FN Thomson Reuters Web of Science™ VR 1.0 PT J AU Schutz, O Meeus, G Sterzik, MF Peeters, E AF Schuetz, O. Meeus, G. Sterzik, M. F. Peeters, E. TI Mid-IR observations of circumstellar disks Part III. A mixed sample of PMS stars and Vega-type objects SO ASTRONOMY & ASTROPHYSICS LA English DT Review DE methods: observational; techniques: spectroscopic; stars: circumstellar matter; infrared: stars; stars: planetary systems: protoplanetary disks; stars: pre-main sequence ID HERBIG-AE/BE STARS; T-TAURI STARS; POLYCYCLIC AROMATIC-HYDROCARBONS; SPITZER-SPACE-TELESCOPE; EXTRASOLAR PLANETARY SYSTEM; MILLIMETER-WAVE PROPERTIES; MAIN-SEQUENCE BINARY; POINT-SOURCE CATALOG; FU ORIONIS OBJECTS; YOUNG STARS AB We present new mid-infrared spectra of 15 targets (1 FU Orionis object, 4 Herbig Ae stars, 5 T Tauri stars, and 5 Vega-type stars), obtained with the TIMMI2 camera at La Silla Observatory (ESO). Three targets are members of the beta Pic moving group (HD 155 555, HD 181 296, and HD 319 139). PAH bands are observed towards the T Tauri star HD 34 700 and the Herbig Ae star PDS 144 N. For HD 34 700, the band profiles indicate processed PAHs. The spectrum of the Vega-type object eta Corvi (HD 109 085), for which a resolved disk at sub-mm wavelengths is known, appears stellar between 8-13 mu m, but a small excess emission was reported by Spitzer observations. Similarly, no indication of circumstellar matter at mid-infrared wavelengths is found towards the Vega-like stars HD 3003, HD 80 951, HD 181 296, and, surprisingly, the T Tauri system HD 155 555. The silicate emission features of the remaining eight sources are modelled with a mixture of silicates of different grain sizes and composition. Unprocessed dust dominates FU Ori, HD 143 006, and CD-43 344. Large amorphous grains are the main dust component around HD 190 073, HD 319 139, KK Oph, and PDS 144 S. Both small grains and crystalline dust is found for the Vega-type HD 123 356, with a dominance of small amorphous grains. We show that the infrared emission of the binary HD 123 356 is dominated by its late-type secondary, but optical spectroscopy is still required to confirm the age of the system and the spectral class of the companion. For most targets, this is their first mid-infrared spectroscopic observation. We investigate trends between stellar, disk, and silicate properties and confirm correlations identified in previous studies. Several objects present an exciting potential for follow-up high-resolution disk studies. C1 [Schuetz, O.; Sterzik, M. F.] European So Observ, Santiago 19, Chile. [Meeus, G.] Astrophys Inst Potsdam, D-14482 Potsdam, Germany. [Peeters, E.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Sterzik, M. F.] SETI Inst, Mountain View, CA 94043 USA. [Peeters, E.] Univ Western Ontario, London, ON N6A 3K7, Canada. RP Schutz, O (reprint author), European So Observ, Alonso de Cordova 3107, Santiago 19, Chile. EM oschuetz@eso.org FU Deutsche Forschungsgemeinschaft (DFG) [ME2061/3-1, ME2061/3-2] FX G. M. acknowledges financial support by the Deutsche Forschungsgemeinschaft (DFG) under grants ME2061/3-1 and /3-2. We would like to thank Alexis Brandeker for the analysis and discussion of the photometric VISIR data of eta Corvi, and Aurora Sicilia-Aguilar for providing the additional data plotted in Fig. 10. This work made use of the SIMBAD astronomical database. We thank the La Silla staff and telescope operators for support during the observations. NR 127 TC 8 Z9 8 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 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD NOV PY 2009 VL 507 IS 1 BP 261 EP 276 DI 10.1051/0004-6361/20066262 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 519QS UT WOS:000271782900026 ER PT J AU Torres-Flores, S de Oliveira, CM de Mello, DF Amram, P Plana, H Epinat, B Iglesias-Paramo, J AF Torres-Flores, S. de Oliveira, C. Mendes de Mello, D. F. Amram, P. Plana, H. Epinat, B. Iglesias-Paramo, J. TI Star formation in the intragroup medium and other diagnostics of the evolutionary stages of compact groups of galaxies SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE galaxies: evolution; galaxies: interactions; galaxies: intergalactic medium; galaxies: kinematics and dynamics ID TIDAL DWARF GALAXIES; ALPHA KINEMATIC SURVEY; STEPHANS-QUINTET; INFRARED PROPERTIES; IRREGULAR GALAXIES; NEARBY UNIVERSE; FORMATION RATES; GAS KINEMATICS; LOCAL UNIVERSE; DATA CUBES AB Context. Compact groups of galaxies are entities that have high densities of galaxies and serve as laboratories to study galaxy interactions, intergalactic star formation and galaxy evolution. Aims. The main goal of this study is to search for young objects in the intragroup medium of seven compact groups of galaxies: HCG 2, 7, 22, 23, 92, 100 and NGC 92 as well as to evaluate the stage of interaction of each group. Methods. We used Fabry-Perot velocity fields and rotation curves together with GALEX NUV and FUV images and optical R-band and HI maps. Results. (i) HCG 7 and HCG 23 are in early stages of interaction; (ii) HCG 2 and HCG 22 are mildly interacting; and (iii) HCG 92, HCG 100 and NGC 92 are in late stages of evolution. We find that all three evolved groups contain populations of young blue objects in the intragroup medium, consistent with ages < 100 Myr, of which several are younger than < 10 Myr. We also report the discovery of a tidal dwarf galaxy candidate in the tail of NGC 92. These three groups, besides containing galaxies that have peculiar velocity fields, also show extended HI tails. Conclusions. Our results indicate that the advanced stage of evolution of a group, together with the presence of intragroup HI clouds, may lead to star formation in the intragroup medium. A table containing all intergalactic HII regions and tidal dwarf galaxies confirmed to date is appended. C1 [Torres-Flores, S.; de Oliveira, C. Mendes] Univ Sao Paulo, Inst Astron Geofis & Ciencias Atmosfer, Dept Astron, Sao Paulo, Brazil. [Torres-Flores, S.; Amram, P.; Plana, H.] Univ Aix Marseille 1, OAMP, Astrophys Lab, F-13388 Marseille 13, France. [Torres-Flores, S.; Amram, P.; Plana, H.] CNRS, F-13388 Marseille, France. [de Mello, D. F.] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA. [de Mello, D. F.] Catholic Univ Amer, Washington, DC 20064 USA. [de Mello, D. F.] Johns Hopkins Univ, Baltimore, MD 21218 USA. [Epinat, B.] Univ Toulouse, CNRS, Lab Astrophys Toulouse Tarbes, F-31400 Toulouse, France. [Plana, H.] Univ Estadual Santa Cruz, Lab Astrofis Teor & Observac, Santa Cruz, Brazil. [Iglesias-Paramo, J.] CSIC, Inst Astrofis Andalucia, E-18008 Granada, Spain. RP Torres-Flores, S (reprint author), Univ Sao Paulo, Inst Astron Geofis & Ciencias Atmosfer, Dept Astron, Sao Paulo, Brazil. EM storres@astro.iag.usp.br RI Mendes de Oliveira, Claudia/F-2391-2012; 7, INCT/H-6207-2013; Astrofisica, Inct/H-9455-2013; Plana, Henri/F-7585-2014; OI Mendes de Oliveira, Claudia/0000-0002-7736-4297; Iglesias-Paramo, Jorge/0000-0003-2726-6370 FU FAPESP [2007/07973-3]; Brazilian agencies FAPESP [2006/56213-9]; CNPq; CAPES; GALEX [NNG06GG45G]; CAPES [3656/08-0]; NASA; Jet Propulsion Laboratory; California Institute of Technology; National Aeronautics and Space Administration FX We would like to thank the referee, Dr. Sonia Temporin, for very useful comments and suggestions which were very important in improving this paper. S.T.-F. acknowledges the financial support of FAPESP through the Doctoral position, under contract 2007/07973-3. C.M.d.O. acknowledges support from the Brazilian agencies FAPESP (projeto tematico 2006/56213-9), CNPq and CAPES. D.F.d.M. acknowledges support from GALEX grant NNG06GG45G. H. P. acknowledges the financial support of CAPES through the Pos-Doctoral position, under contract 3656/08-0. GALEX is a NASA Small Explorer, launched in 2003 April. We 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. This research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. We also acknowledge the usage of the HyperLeda database (http://leda.univ-lyon1.fr). NR 77 TC 20 Z9 20 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 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD NOV PY 2009 VL 507 IS 2 BP 723 EP 746 DI 10.1051/0004-6361/200911878 PG 24 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 522VU UT WOS:000272029000020 ER PT J AU in 't Zand, JJM Jonker, PG Bassa, CG Markwardt, CB Levine, AM AF in 't Zand, J. J. M. Jonker, P. G. Bassa, C. G. Markwardt, C. B. Levine, A. M. TI Monitoring campaign of 1RXS J171824.2-402934, the low-mass X-ray binary with the lowest mass accretion rate SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE accretion, accretion disks; stars: neutron; X-rays: binaries; X-rays: individuals: 1RXS J171824.2-402934; X-rays: individuals: RX J1718.4-4029 ID PHOTOMETRIC STANDARD STARS; RESOLUTION CAMERA HRC; ALL-SKY SURVEY; GALACTIC-CENTER; ULTRACOMPACT BINARIES; TIMING-EXPLORER; DISCOVERY; TRANSIENTS; CATALOG; CALIBRATION AB An X-ray monitoring campaign with Chandra and Swift confirms that 1RXS J171824.2-402934 is accreting at the lowest rate among the known persistently accreting low-mass X-ray binaries. A thermonuclear X-ray burst was detected with the all-sky monitor on RXTE. This is only the second such burst seen in 1RXS J171824.2-402934 in more than 20 Ms of observations done over 19 years. The low burst recurrence rate is in line with the low accretion rate. The persistent nature and low accretion rate can be reconciled within accretion disk theory if the binary system is ultracompact. An unprecedentedly short orbital period of less than approximate to 7 min would be implied. An ultracompact nature, together with the properties of the type I X-ray burst, suggests, in turn, that helium-rich material is accreted. Optical follow-up of the Chandra error region does not reveal an unambiguous counterpart. C1 [in 't Zand, J. J. M.; Jonker, P. G.; Bassa, C. G.] SRON Netherlands Inst Space Res, NL-3584 CA Utrecht, Netherlands. [Jonker, P. G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bassa, C. G.] Radboud Univ Nijmegen, Dept Astrophys, NL-6525 ED Nijmegen, Netherlands. [Markwardt, C. B.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Markwardt, C. B.] NASA, Goddard Space Flight Ctr, Astroparticle Phys Lab, Greenbelt, MD 20771 USA. [Levine, A. M.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. RP in 't Zand, JJM (reprint author), SRON Netherlands Inst Space Res, Sorbonnelaan 2, NL-3584 CA Utrecht, Netherlands. EM jeanz@sron.nl NR 50 TC 8 Z9 8 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 NOV PY 2009 VL 506 IS 2 BP 857 EP 863 DI 10.1051/0004-6361/200912403 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 514DP UT WOS:000271374800034 ER PT J AU Muller, HSP Drouin, BJ Pearson, JC AF Mueller, H. S. P. Drouin, B. J. Pearson, J. C. TI Rotational spectra of isotopic species of methyl cyanide, CH3CN, in their ground vibrational states up to terahertz frequencies SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE molecular data; methods: laboratory; techniques: spectroscopic; radio lines: ISM; ISM: molecules ID MICROWAVE-SPECTRA; MOLECULAR-SPECTROSCOPY; COLOGNE DATABASE; RZ STRUCTURE; LINE SURVEY; GHZ; CONSTANTS; SUBMILLIMETER; METHYLCYANIDE; TRANSITION AB Context. Methyl cyanide is an important trace molecule in star-forming regions. It is one of the more common molecules used to derive kinetic temperatures in such sources. Aims. As preparatory work for Herschel, SOFIA, and in particular ALMA we want to improve the rest frequencies of the main as well as minor isotopologs of methyl cyanide. Methods. The laboratory rotational spectrum of methyl cyanide in natural isotopic composition has been recorded up to 1.63 THz. Results. Transitions with good signal-to-noise ratio could be identified for CH3CN, (CH3CN)-C-13, (CH3CN)-C-13, (CH3CN)-N-15, CH2DCN, and (CH3CN)-C-13-C-13 in their ground vibrational states up to about 1.2 THz. The main isotopic species could be identified even in the highest frequency spectral recordings around 1.6 THz. The highest J' quantum numbers included in the fit are 64 for (CH3CN)-C-13-C-13 and 89 for the main isotopic species. Greatly improved spectroscopic parameters have been obtained by fitting the present data together with previously reported transition frequencies. Conclusions. The present data will be helpful to identify isotopologs of methyl cyanide in the higher frequency bands of instruments such as the recently launched Herschel satellite, the upcoming airplane mission SOFIA or the radio telescope array ALMA. C1 [Mueller, H. S. P.] Univ Cologne, Inst Phys 1, D-50937 Cologne, Germany. [Drouin, B. J.; Pearson, J. C.] CALTECH, Jet Prop Lab, Pasadena, CA 91011 USA. RP Muller, HSP (reprint author), Univ Cologne, Inst Phys 1, Zulpicher Str 77, D-50937 Cologne, Germany. EM hspm@ph1.uni-koeln.de OI Mueller, Holger/0000-0002-0183-8927 FU Bundesministerium fur Bildung und Forschung (BMBF); Deutsches Zentrum fur Luft- und Raumfahrt (DLR); National Aeronautics and Space Administration (NASA) FX H.S.P.M. is very grateful to the Bundesministerium fur Bildung und Forschung (BMBF) for financial support aimed at maintaining the Cologne Database for Molecular Spectroscopy, CDMS. This support has been administered by the Deutsches Zentrum fur Luft- und Raumfahrt (DLR). A part of the present research has been carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration (NASA). NR 40 TC 11 Z9 11 U1 0 U2 9 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD NOV PY 2009 VL 506 IS 3 BP 1487 EP 1499 DI 10.1051/0004-6361/200912932 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 516AV UT WOS:000271514900039 ER PT J AU Camilo, F Ray, PS Ransom, SM Burgay, M Johnson, TJ Kerr, M Gotthelf, EV Halpern, JP Reynolds, J Romani, RW Demorest, P Johnston, S van Straten, W Parkinson, PMS Ziegler, M Dormody, M Thompson, DJ Smith, DA Harding, AK Abdo, AA Crawford, F Freire, PCC Keith, M Kramer, M Roberts, MSE Weltevrede, P Wood, KS AF Camilo, F. Ray, P. S. Ransom, S. M. Burgay, M. Johnson, T. J. Kerr, M. Gotthelf, E. V. Halpern, J. P. Reynolds, J. Romani, R. W. Demorest, P. Johnston, S. van Straten, W. Parkinson, P. M. Saz Ziegler, M. Dormody, M. Thompson, D. J. Smith, D. A. Harding, A. K. Abdo, A. A. Crawford, F. Freire, P. C. C. Keith, M. Kramer, M. Roberts, M. S. E. Weltevrede, P. Wood, K. S. TI RADIO DETECTION OF LAT PSRs J1741-2054 AND J2032+4127: NO LONGER JUST GAMMA-RAY PULSARS SO ASTROPHYSICAL JOURNAL LA English DT Article DE gamma rays: observations; ISM: individual (TeV J2032+4130); open clusters and associations: individual (Cyg OB2); pulsars: individual (PSR J1741-2054, PSR J2032+4127); X-rays: individual (Swift J174157.6-205411) ID SOURCE TEV J2032+4130; LARGE-AREA TELESCOPE; X-RAY; CYGNUS OB2; SOURCE TEV-J2032+4130; CYG-OB2 ASSOCIATION; SPACE-TELESCOPE; MASSIVE STARS; NEUTRON-STAR; LIGHT CURVES AB Sixteen pulsars have been discovered so far in blind searches of photons collected with the Large Area Telescope on the Fermi Gamma-ray Space Telescope. We here report the discovery of radio pulsations from two of them. PSR J1741-2054, with period P = 413 ms, was detected in archival Parkes telescope data and subsequently has been detected at the Green Bank Telescope (GBT). Its received flux varies greatly due to interstellar scintillation and it has a very small dispersion measure of DM = 4.7 pc cm(-3), implying a distance of approximate to 0.4 kpc and possibly the smallest luminosity of any known radio pulsar. At this distance, for isotropic emission, its gamma-ray luminosity above 0.1 GeV corresponds to 28% of the spin-down luminosity of (E) over dot = 9.4 x 10(33) erg s(-1). The gamma-ray profile occupies 1/3 of pulse phase and has three closely spaced peaks with the first peak lagging the radio pulse by delta = 0.29 P. We have also identified a soft Swift source that is the likely X-ray counterpart. In many respects PSR J1741-2054 resembles the Geminga pulsar. The second source, PSR J2032+4127, was detected at the GBT. It has P = 143 ms, and its DM = 115 pc cm(-3) suggests a distance of approximate to 3.6 kpc, but we consider it likely that it is located within the Cyg OB2 stellar association at half that distance. The radio emission is nearly 100% linearly polarized, and the main radio peak precedes by delta = 0.15 P the first of two narrow gamma-ray peaks that are separated by Delta = 0.50 P. The second peak has a harder spectrum than the first one, following a trend observed in young gamma-ray pulsars. Faint, diffuse X-ray emission in a Chandra image is possibly its pulsar wind nebula. The wind of PSR J2032+4127 is responsible for the formerly unidentified HEGRA source TeV J2032+4130. PSR J2032+4127 is coincident in projection with MT91 213, a Be star in Cyg OB2, although apparently not a binary companion of it. C1 [Camilo, F.; Gotthelf, E. V.; Halpern, J. P.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Ray, P. S.; Abdo, A. A.; Wood, K. S.] USN, Res Lab, Div Space Sci, Washington, DC 20375 USA. [Ransom, S. M.; Demorest, P.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. [Burgay, M.] INAF Osservatorio Astron Cagliari, I-09012 Capoterra, Italy. [Johnson, T. J.; Thompson, D. J.; Harding, A. K.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Johnson, T. J.] Univ Maryland, College Pk, MD 20742 USA. [Kerr, M.] Univ Washington, Dept Phys, Seattle, WA 98195 USA. [Reynolds, J.; Johnston, S.; Keith, M.; Weltevrede, P.] CSIRO, Australia Telescope Natl Facil, Epping, NSW 1710, Australia. [Reynolds, J.] Parkes Observ, CSIRO, Parkes, NSW 2870, Australia. [Romani, R. W.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA. [van Straten, W.] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia. [Parkinson, P. M. Saz; Ziegler, M.; Dormody, M.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Dept Phys, Santa Cruz, CA 95064 USA. [Parkinson, P. M. Saz; Ziegler, M.; Dormody, M.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Smith, D. A.] Ctr Etud Nucl Bordeaux Gradignan, IN2P3, CNRS, F-33175 Gradignan, France. [Smith, D. A.] Univ Bordeaux, Ctr Etud Nucl Bordeaux Gradignan, F-33175 Gradignan, France. [Crawford, F.] Franklin & Marshall Coll, Dept Phys & Astron, Lancaster, PA 17604 USA. [Freire, P. C. C.] Arecibo Observ, NAIC, Arecibo, PR 00612 USA. [Kramer, M.] MPIfR, D-53121 Bonn, Germany. [Kramer, M.] Univ Manchester, Jodrell Bank, Ctr Astrophys, Manchester M13 9PL, Lancs, England. [Roberts, M. S. E.] Eureka Sci Inc, Oakland, CA 94602 USA. RP Camilo, F (reprint author), Columbia Univ, Columbia Astrophys Lab, 538 W 120th St, New York, NY 10027 USA. RI Thompson, David/D-2939-2012; Harding, Alice/D-3160-2012; OI Thompson, David/0000-0001-5217-9135; Burgay, Marta/0000-0002-8265-4344; Roberts, Mallory/0000-0002-9396-9720; Ransom, Scott/0000-0001-5799-9714; van Straten, Willem/0000-0003-2519-7375; Ray, Paul/0000-0002-5297-5278 FU CSIRO; National Aeronautics and Space Administration; Department of Energy in the United States; Commissariat a l'Energie Atomique; Centre National de la Recherche Scientifique/Institut National de Physique Nucleaire et de Physique des Particules in France; Agenzia Spaziale Italiana and the Istituto Nazionale di Fisica Nucleare in Italy; Ministry of Education, Culture, Sports, Science and Technology (MEXT); High Energy Accelerator Research Organization (KEK); Japan Aerospace Exploration Agency (JAXA) in Japan; K. A. Wallenberg Foundation; Swedish Research Council; Swedish National Space Board in Sweden FX Facilities: CXO (ACIS-I), Fermi (LAT), GBT (BCPM, GUPPI), Hiltner (RETROCAM), Parkes (PMDAQ), Swift (XRT) NR 70 TC 67 Z9 67 U1 0 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD NOV 1 PY 2009 VL 705 IS 1 BP 1 EP 13 DI 10.1088/0004-637X/705/1/1 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 508CA UT WOS:000270903200001 ER PT J AU Deo, RP Richards, GT Crenshaw, DM Kraemer, SB AF Deo, Rajesh P. Richards, Gordon T. Crenshaw, D. M. Kraemer, S. B. TI THE MID-INFRARED CONTINUA OF SEYFERT GALAXIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: nuclei; galaxies: Seyfert; infrared: galaxies ID SPECTRAL ENERGY-DISTRIBUTIONS; SPITZER-SPACE-TELESCOPE; ACTIVE GALACTIC NUCLEI; MU-M; EMISSION-LINE; INFRARED SPECTROGRAPH; DUST EMISSION; IRS SPECTRA; QUASARS; AGNS AB An analysis of archival mid-infrared (mid-IR) spectra of Seyfert galaxies from the Spitzer Space Telescope observations is presented. We characterize the nature of the mid-IR active nuclear continuum by subtracting a template starburst spectrum from the Seyfert spectra. The long wavelength part of the spectrum contains a strong contribution from the starburst-heated cool dust; this is used to effectively separate starburst-dominated Seyferts from those dominated by the active nuclear continuum. Within the latter category, the strength of the active nuclear continuum drops rapidly beyond similar to 20 mu m. On average, type 2 Seyferts have weaker short-wavelength active nuclear continua as compared to type 1 Seyferts. Type 2 Seyferts can be divided into two types, those with strong polycyclic aromatic hydrocarbon (PAH) bands and those without. The latter type show polarized broad emission lines in their optical spectra. The PAH-dominated type 2 Seyferts and Seyfert 1.8/1.9s show very similar mid-IR spectra. However, after the subtraction of the starburst component, there is a striking similarity in the active nuclear continuum of all Seyfert optical types. PAH-dominated Seyfert 2s and Seyfert 1.8/1.9s tend to show weak active nuclear continua in general. A few type 2 Seyferts with weak/absent PAH bands show a bump in the spectrum between 15 and 20 mu m. We suggest that this bump is the peak of a warm (similar to 200 K) blackbody dust emission, which becomes clearly visible when the short-wavelength continuum is weaker. This warm blackbody emission is also observed in other Seyfert optical subtypes, suggesting a common origin in these active galactic nuclei. C1 [Deo, Rajesh P.; Richards, Gordon T.] Drexel Univ, Dept Phys, Philadelphia, PA 19104 USA. [Crenshaw, D. M.] Georgia State Univ, Dept Phys & Astron, Atlanta, GA 30303 USA. [Kraemer, S. B.] NASA, Goddard Space Flight Ctr, Explorat Univ Div, Greenbelt, MD 20771 USA. [Kraemer, S. B.] Catholic Univ Amer, Greenbelt, MD 20771 USA. RP Deo, RP (reprint author), Drexel Univ, Dept Phys, 3141 Chestnut St, Philadelphia, PA 19104 USA. EM rpd@physics.drexel.edu; gtr@physics.drexel.edu; crenshaw@chara.gsu.edu; kraemer@yancey.gsfc.nasa.gov FU Alfred P. Sloan Research Fellowship; NASA FX We would like to thank Nadia Zakamska for insightful comments on an early draft of this paper. G. T. R. acknowledges support from an Alfred P. Sloan Research Fellowship. This work is based on archival data obtained with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. This research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. This research has also made use of NASA's Astrophysics Data System Bibliographic Services. The IRS was a collaborative venture between Cornell University and Ball Aerospace Corporation funded by NASA through the Jet Propulsion Laboratory and Ames Research Center. SMART was developed at Cornell University and is available through the Spitzer Science Center at Caltech. NR 45 TC 38 Z9 38 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD NOV 1 PY 2009 VL 705 IS 1 BP 14 EP 31 DI 10.1088/0004-637X/705/1/14 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 508CA UT WOS:000270903200002 ER PT J AU Bertincourt, B Helou, G Appleton, P Ogle, P Lagache, G Brooke, T Smith, JD Sheth, K Dale, D Harwit, M Puget, JL Roussel, H AF Bertincourt, B. Helou, G. Appleton, P. Ogle, P. Lagache, G. Brooke, T. Smith, J-D. Sheth, K. Dale, D. Harwit, M. Puget, J-L. Roussel, H. TI A SPITZER UNBIASED ULTRADEEP SPECTROSCOPIC SURVEY SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: starburst; infrared: galaxies ID ULTRALUMINOUS INFRARED GALAXIES; STAR-FORMING GALAXIES; ACTIVE GALACTIC NUCLEI; GOODS-NORTH FIELD; AREA ISO SURVEY; SPACE-TELESCOPE; LUMINOUS GALAXIES; MIDINFRARED SPECTROSCOPY; SUBMILLIMETER GALAXIES; MOLECULAR-HYDROGEN AB We carried out an unbiased, spectroscopic survey using the low-resolution module of the infrared spectrograph (IRS) onboard Spitzer targeting two 2.6 square arcminute regions in the GOODS-North field. The IRS was used in a spectral mapping mode with 5 hr of effective integration time per pixel. One region was covered between 14 and 21 mu m and the other between 20 and 35 mu m. We extracted spectra for 45 sources. About 84% of the sources have reported detections by GOODS at 24 mu m, with a median f(nu)( 24 mu m) similar to 100 mu Jy. All but one source are detected in all four IRAC bands, 3.6 to 8 mu m. We use a new cross-correlation technique to measure redshifts and estimate IRS spectral types; this was successful for similar to 60% of the spectra. Fourteen sources show significant polycyclic aromatic hydrocarbon emission, four mostly SiO absorption, eight present mixed spectral signatures (low PAH and/or SiO) and two show a single line in emission. For the remaining 17, no spectral features were detected. Redshifts range from z similar to 0.2 to z similar to 2.2, with a median of 1. IR luminosities are roughly estimated from 24 mu m flux densities, and have median values of 2.2 x 10(11)L(circle dot) and 7.5 x 10(11)L(circle dot) at z similar to 1 and z similar to 2, respectively. This sample has fewer active galactic nuclei than previous faint samples observed with the IRS, which we attribute to the fainter luminosities reached here. C1 [Bertincourt, B.; Lagache, G.; Puget, J-L.] Univ Paris 11, Inst Astrophys Spatiale, F-91405 Orsay, France. [Bertincourt, B.; Lagache, G.; Puget, J-L.] CNRS, UMR 8617, F-91405 Orsay, France. [Bertincourt, B.; Helou, G.; Appleton, P.; Ogle, P.; Brooke, T.; Sheth, K.] CALTECH, Spitzer Sci Ctr, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA. [Appleton, P.] CALTECH, NASA, Herschel Sci Ctr, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA. [Smith, J-D.] Univ Arizona, Steward Observ, Tucson, AZ USA. [Dale, D.] Univ Wyoming, Dept Phys & Astron, Laramie, WY 82071 USA. [Harwit, M.] Cornell Univ, Ithaca, NY USA. [Roussel, H.] Univ Paris 06, UPMC, Inst Astrophys Paris, F-75014 Paris, France. RP Bertincourt, B (reprint author), Univ Paris 11, Inst Astrophys Spatiale, Batiment 121, F-91405 Orsay, France. EM benjamin.bertincourt@ias.u-psud.fr; guilaine.lagache@ias.u-psud.fr; jean-loup.puget@ias.u-psud.fr OI Appleton, Philip/0000-0002-7607-8766 FU NASA [1407]; French National Agency [ANR-06-BLAN-0170, ANR05-BLAN-0289-02] FX We thank Aaron Stephen for help with the X- ray data. This work is based on observation obtained with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under NASA contract 1407. Support for this work was provided by NASA through an award issued by JPL/Caltech, as well as the French National Agency for Research under programs ANR-06-BLAN-0170 and ANR05-BLAN-0289-02. This research has made use of the NASA/IPAC Extragalactic Databasewhich is operated by JPL/Caltech, under contract with NASA. NR 61 TC 3 Z9 3 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD NOV 1 PY 2009 VL 705 IS 1 BP 68 EP 88 DI 10.1088/0004-637X/705/1/68 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 508CA UT WOS:000270903200007 ER PT J AU Lawler, SM Beichman, CA Bryden, G Ciardi, DR Tanner, AM Su, KYL Stapelfeldt, KR Lisse, CM Harker, DE AF Lawler, S. M. Beichman, C. A. Bryden, G. Ciardi, D. R. Tanner, A. M. Su, K. Y. L. Stapelfeldt, K. R. Lisse, C. M. Harker, D. E. TI EXPLORATIONS BEYOND THE SNOW LINE: SPITZER/IRS SPECTRA OF DEBRIS DISKS AROUND SOLAR-TYPE STARS SO ASTROPHYSICAL JOURNAL LA English DT Article DE infrared: stars; circumstellar matter; planetary systems; Kuiper Belt ID MULTIBAND IMAGING PHOTOMETER; MAIN-SEQUENCE STARS; SUN-LIKE STARS; MU-M; MODEL ATMOSPHERES; SPACE-TELESCOPE; F-DWARF; ABSOLUTE CALIBRATION; PLANETARY SYSTEM; HARPS SEARCH AB We have observed 152 nearby solar-type stars with the Infrared Spectrometer (IRS) on the Spitzer Space Telescope. Including stars that met our criteria but were observed in other surveys, we get an overall success rate for finding excesses in the long-wavelength IRS band (30-34 mu m) of 11.8% +/- 2.4%. The success rate for excesses in the short-wavelength band (8.5-12 mu m) is similar to 1% including sources from other surveys. For stars with no excess at 8.5-12 mu m, the IRS data set 3 sigma limits of around 1000 times the level of zodiacal emission present in our solar system, while at 30 34 mu m data set limits of around 100 times the level of our solar system. Two stars (HD 40136 and HD 10647) show weak evidence for spectral features; the excess emission in the other systems is featureless. If the emitting material consists of large (10 mu m) grains as implied by the lack of spectral features, we find that these grains are typically located at or beyond the snow line, similar to 1-35 AU from the host stars, with an average distance of 14 +/- 6 AU; however, smaller grains could be located at significantly greater distances from the host stars. These distances correspond to dust temperatures in the range similar to 50-450 K. Several of the disks are well modeled by a single dust temperature, possibly indicative of a ring-like structure. However, a single dust temperature does not match the data for other disks in the sample, implying a distribution of temperatures within these disks. For most stars with excesses, we detect an excess at both IRS and Multiband Imaging Photometer for Spitzer (MIPS) wavelengths. Only three stars in this sample show a MIPS 70 mu m excess with no IRS excess, implying that very cold dust is rare around solar-type stars. C1 [Lawler, S. M.] Wesleyan Univ, Dept Astron, Middletown, CT 06459 USA. [Lawler, S. M.; Beichman, C. A.; Ciardi, D. R.] CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA. [Bryden, G.; Tanner, A. M.; Stapelfeldt, K. R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Su, K. Y. L.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Lisse, C. M.] Johns Hopkins Univ, Appl Phys Lab, SD SRE, Laurel, MD 20723 USA. [Harker, D. E.] Univ Calif San Diego, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA. RP Lawler, SM (reprint author), Univ British Columbia, Dept Phys & Astron, 6244 Agr Rd, Vancouver, BC V6T 1Z1, Canada. RI Stapelfeldt, Karl/D-2721-2012; Lisse, Carey/B-7772-2016; OI Lisse, Carey/0000-0002-9548-1526; Harker, David/0000-0001-6397-9082; Ciardi, David/0000-0002-5741-3047; Su, Kate/0000-0002-3532-5580 FU NASA [1407, 960785]; Jet Propulsion Laboratory, California Institute of Technology FX This publication makes use of data products from the Two-Micron All Sky Survey, as well as from IPAC/IRSKY/IBIS, SIMBAD, VizieR, the ROE Debris Disks Database website, and the Extrasolar Planets Encyclopaedia website. The Spitzer Space Telescope is operated by the Jet Propulsion Laboratory, California Institute of Technology, under NASA contract 1407. Development of MIPS was funded by NASA through the Jet Propulsion Laboratory, subcontract 960785. Some of the research described in this publication was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. S. M. L. thanks Seth Redfield and Roy Kilgard for very helpful comments and advice regarding this paper. NR 93 TC 55 Z9 55 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD NOV 1 PY 2009 VL 705 IS 1 BP 89 EP 111 DI 10.1088/0004-637X/705/1/89 PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 508CA UT WOS:000270903200008 ER PT J AU Bradford, CM Aguirre, JE Aikin, R Bock, JJ Earle, L Glenn, J Inami, H Maloney, PR Matsuhara, H Naylor, BJ Nguyen, HT Zmuidzinas, J AF Bradford, C. M. Aguirre, J. E. Aikin, R. Bock, J. J. Earle, L. Glenn, J. Inami, H. Maloney, P. R. Matsuhara, H. Naylor, B. J. Nguyen, H. T. Zmuidzinas, J. TI THE WARM MOLECULAR GAS AROUND THE CLOVERLEAF QUASAR SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: ISM; instrumentation: spectrographs; ISM: clouds; stars: luminosity function, mass function; techniques: spectroscopic ID MAGNETOHYDRODYNAMIC SHOCK-WAVES; INITIAL MASS FUNCTION; STAR-FORMATION RATE; WATER-VAPOR; BROAD-BAND; DENSE GAS; ASTRONOMY-SATELLITE; STARBURST GALAXIES; IRAS F10214+4724; LINE EMISSION AB We present the first broadband lambda = 1 mm spectrum toward the z = 2.56 Cloverleaf quasar, obtained with Z-Spec, a grating spectrograph on the 10.4 m Caltech Submillimeter Observatory. The 190-305 GHz observation band corresponds to the rest frame 272-444 mu m, and we measure the dust continuum as well as all four transitions of carbon monoxide ( CO) lying in this range. The power-law dust emission, F(nu) = 14 mJy (nu/240 GHz)(3.9) is consistent with the published continuum measurements. The CO J = 6 -> 5, J = 8 -> 7, and J = 9 -> 8 measurements are the first, and now provide the highest-J CO information in this source. Our measured CO intensities are very close to the previously published interferometric measurements of J = 7 -> 6, and we use all available transitions and our (13)CO upper limits to constrain the physical conditions in the Cloverleaf molecular gas disk. We find a large mass (2-50 x 10(9)M(circle dot)) of highly excited gas with thermal pressure nT > 10(6) K cm(-3). The ratio of the total CO cooling to the far-IR dust emission exceeds that in the local dusty galaxies, and we investigate the potential heating sources for this bulk of warm molecular gas. We conclude that both UV photons and X-rays likely contribute, and discuss implications for a top-heavy stellar initial mass function arising in the X-ray-irradiated starburst. Finally, we present tentative identifications of other species in the spectrum, including a possible detection of the H(2)O 2(0,2) -> 1(1,1) transition at lambda(rest) = 303 mu m. C1 [Bradford, C. M.; Bock, J. J.; Naylor, B. J.; Nguyen, H. T.; Zmuidzinas, J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Bradford, C. M.; Aikin, R.; Bock, J. J.; Naylor, B. J.; Zmuidzinas, J.] CALTECH, Pasadena, CA 91125 USA. [Aguirre, J. E.; Aikin, R.; Earle, L.; Glenn, J.; Maloney, P. R.] Univ Colorado, Boulder, CO 80303 USA. [Aguirre, J. E.] Univ Penn, Philadelphia, PA 19104 USA. [Inami, H.; Matsuhara, H.] Japan Aerosp & Explorat Agcy, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2298510, Japan. RP Bradford, CM (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. FU NASA SARA [NAGS-11911, NAGS-12788]; NSF [AST-0239270]; Research Corporation Award [RI0928]; NASA GSRP FX We are indebted to the staff of the Caltech Submillimeter Observatory for their help in Z-Spec's commissioning and observing. We acknowledge Peter Ade and his group for some of the filters and Lionel Duband for the 3He/4He refrigerator in Z-Spec, and are grateful for their help in the early integration of the instrument. We benefitted from conversations with Tom Phillips, Paul Goldsmith, Simon Radford, and Andy Harris, as well as helpful comments from Xinyu Dai and an anonymous referee. Finally, we acknowledge the following grants and fellowships: NASA SARA grants NAGS-11911 and NAGS-12788, an NSF Career grant (AST-0239270) and a Research Corporation Award (RI0928) to J. Glenn, a Caltech Millikan and JPL Director's fellowships to C. M. B., a NRAO Jansky fellowship to J. Aguirre, and NASA GSRP fellowship to L. Earle. NR 67 TC 50 Z9 50 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD NOV 1 PY 2009 VL 705 IS 1 BP 112 EP 122 DI 10.1088/0004-637X/705/1/112 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 508CA UT WOS:000270903200009 ER PT J AU Bentz, MC Walsh, JL Barth, AJ Baliber, N Bennert, VN Canalizo, G Filippenko, AV Ganeshalingam, M Gates, EL Greene, JE Hidas, MG Hiner, KD Lee, N Li, WD Malkan, MA Minezaki, T Sakata, Y Serduke, FJD Silverman, JM Steele, TN Stern, D Street, RA Thornton, CE Treu, T Wang, XF Woo, JH Yoshii, Y AF Bentz, Misty C. Walsh, Jonelle L. Barth, Aaron J. Baliber, Nairn Bennert, Vardha Nicola Canalizo, Gabriela Filippenko, Alexei V. Ganeshalingam, Mohan Gates, Elinor L. Greene, Jenny E. Hidas, Marton G. Hiner, Kyle D. Lee, Nicholas Li, Weidong Malkan, Matthew A. Minezaki, Takeo Sakata, Yu Serduke, Frank J. D. Silverman, Jeffrey M. Steele, Thea N. Stern, Daniel Street, Rachel A. Thornton, Carol E. Treu, Tommaso Wang, Xiaofeng Woo, Jong-Hak Yoshii, Yuzuru TI THE LICK AGN MONITORING PROJECT: BROAD-LINE REGION RADII AND BLACK HOLE MASSES FROM REVERBERATION MAPPING OF H beta SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: nuclei; galaxies: Seyfert ID ACTIVE GALACTIC NUCLEI; HOST-GALAXY STARLIGHT; SEYFERT 1 GALAXIES; LUMINOSITY RELATIONSHIP; VELOCITY DISPERSION; OPTICAL CONTINUUM; WIND MODEL; DISK-WIND; NGC 4051; EMISSION AB We have recently completed a 64-night spectroscopic monitoring campaign at the Lick Observatory 3-m Shane telescope with the aim of measuring the masses of the black holes in 12 nearby (z < 0.05) Seyfert 1 galaxies with expected masses in the range similar to 10(6) - 10(7) M(circle dot) and also the well-studied nearby active galactic nucleus (AGN) NGC 5548. Nine of the objects in the sample ( including NGC 5548) showed optical variability of sufficient strength during the monitoring campaign to allow for a time lag to be measured between the continuum fluctuations and the response to these fluctuations in the broad H beta emission. We present here the light curves for all the objects in this sample and the subsequent H beta time lags for the nine objects where these measurements were possible. The H beta lag time is directly related to the size of the broad-line region (BLR) in AGNs, and by combining the H beta lag time with the measured width of the H beta emission line in the variable part of the spectrum, we determine the virial mass of the central supermassive black hole in these nine AGNs. The absolute calibration of the black hole masses is based on the normalization derived by Onken et al., which brings the masses determined by reverberation mapping into agreement with the local M(BH)-sigma(star)relationship for quiescent galaxies. We also examine the time lag response as a function of velocity across the H beta line profile for six of the AGNs. The analysis of four leads to rather ambiguous results with relatively flat time lags as a function of velocity. However, SBS 1116+583A exhibits a symmetric time lag response around the line center reminiscent of simple models for circularly orbiting BLR clouds, and Arp 151 shows an asymmetric profile that is most easily explained by a simple gravitational infall model. Further investigation will be necessary to fully understand the constraints placed on the physical models of the BLR by the velocity-resolved response in these objects. C1 [Bentz, Misty C.; Walsh, Jonelle L.; Barth, Aaron J.; Thornton, Carol E.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. [Baliber, Nairn; Bennert, Vardha Nicola; Greene, Jenny E.; Hidas, Marton G.; Street, Rachel A.; Treu, Tommaso] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Baliber, Nairn; Hidas, Marton G.; Street, Rachel A.] Las Cumbres Observ Global Telescope, Goleta, CA 93117 USA. [Bennert, Vardha Nicola; Canalizo, Gabriela; Hiner, Kyle D.] Univ Calif Riverside, Inst Geophys & Planetary Phys, Riverside, CA 92521 USA. [Canalizo, Gabriela; Hiner, Kyle D.] Univ Calif Riverside, Dept Phys & Astron, Riverside, CA 92521 USA. [Filippenko, Alexei V.; Ganeshalingam, Mohan; Lee, Nicholas; Li, Weidong; Serduke, Frank J. D.; Silverman, Jeffrey M.; Steele, Thea N.; Wang, Xiaofeng] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Gates, Elinor L.] Univ Calif Santa Cruz, Lick Observ, Mt Hamilton, CA 95140 USA. [Greene, Jenny E.] Princeton Univ Observ, Princeton, NJ 08544 USA. [Hidas, Marton G.] Univ Sydney, Sch Phys A28, Sydney, NSW 2006, Australia. [Malkan, Matthew A.; Woo, Jong-Hak] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90024 USA. [Minezaki, Takeo; Sakata, Yu; Yoshii, Yuzuru] Univ Tokyo, Sch Sci, Inst Astron, Tokyo 1810015, Japan. [Sakata, Yu] Univ Tokyo, Sch Sci, Dept Astron, Bunkyo Ku, Tokyo 1130033, Japan. [Stern, Daniel] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Wang, Xiaofeng] Tsinghua Univ, Dept Phys, Beijing 100084, Peoples R China. [Wang, Xiaofeng] Tsinghua Univ, Tsinghua Ctr Astrophys THCA, Beijing 100084, Peoples R China. [Woo, Jong-Hak] Seoul Natl Univ, Dept Phys & Astron, Astron Program, Seoul 151742, South Korea. RP Bentz, MC (reprint author), Univ Calif Irvine, Dept Phys & Astron, 4129 Frederick Reines Hall, Irvine, CA 92697 USA. EM mbentz@uci.edu RI Woo, Jong-Hak/A-2790-2014; Wang, Xiaofeng/J-5390-2015; OI Hidas, Marton/0000-0002-4027-9240 FU NSF [AST-0548198, AST-0607485, AST- 0642621, AST- 0507450]; Space Telescope Science Institute [HF-51249]; NASA [NAS 5-26555] FX We thank the anonymous referee for comments that improved the presentation of this paper. We also thank the excellent staff and support personnel at Lick Observatory for their enormous help during our observing run, and Brad Peterson for helpful conversations and the use of his analysis software. We thank Josh Shiode for his observing help. This work was supported by NSF grants AST-0548198 ( UC Irvine), AST-0607485 ( UC Berkeley), AST- 0642621 ( UC Santa Barbara), and AST- 0507450 ( UC Riverside). J.H.W. gratefully acknowledges support provided by NASA through Hubble Fellowship grant HF-51249 awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS 5-26555. The UC Berkeley researchers also gratefully acknowledge the support of both the Sylvia & Jim Katzman Foundation and the TABASGO Foundation for the continued operation of KAIT. The work of D. S. was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. NR 77 TC 176 Z9 176 U1 0 U2 9 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD NOV 1 PY 2009 VL 705 IS 1 BP 199 EP 217 DI 10.1088/0004-637X/705/1/199 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 508CA UT WOS:000270903200016 ER PT J AU Dicker, SR Mason, BS Korngut, PM Cotton, WD Compiegne, M Devlin, MJ Martin, PG Ade, PAR Benford, DJ Irwin, KD Maddalena, RJ McMullin, JP Shepherd, DS Sievers, A Staguhn, JG Tucker, C AF Dicker, S. R. Mason, B. S. Korngut, P. M. Cotton, W. D. Compiegne, M. Devlin, M. J. Martin, P. G. Ade, P. A. R. Benford, D. J. Irwin, K. D. Maddalena, R. J. McMullin, J. P. Shepherd, D. S. Sievers, A. Staguhn, J. G. Tucker, C. TI 90 GHz AND 150 GHz OBSERVATIONS OF THE ORION M42 REGION. A SUBMILLIMETER TO RADIO ANALYSIS SO ASTROPHYSICAL JOURNAL LA English DT Article DE HII regions; ISM: individual (M42, Orion Nebula); radio continuum: ISM; submillimeter ID H II REGION; MOLECULAR CLOUD; MICROWAVE EMISSION; GALACTIC EMISSION; NEBULA; CONTINUUM; DUST; MAPS; INTERFACE; CAMERA AB We have used the new 90 GHz MUSTANG camera on the Robert C. Byrd Green Bank Telescope (GBT) to map the bright Huygens region of the star-forming region M42 with a resolution of 9" and a sensitivity of 2.8 mJy beam(-1). Ninety GHz is an interesting transition frequency, as MUSTANG detects both the free-free emission characteristic of the HII region created by the Trapezium stars, normally seen at lower frequencies, and thermal dust emission from the background OMC1 molecular cloud, normally mapped at higher frequencies. We also present similar data from the 150 GHz GISMO camera taken on the IRAM 30 m telescope. This map has 15" resolution. By combining the MUSTANG data with 1.4, 8, and 21 GHz radio data from the VLA and GBT, we derive a new estimate of the emission measure averaged electron temperature of T(e) = 11376 +/- 1050 K by an original method relating free-free emission intensities at optically thin and optically thick frequencies. Combining Infrared Space Observatory-long wavelength spectrometer (ISO-LWS) data with our data, we derive a new estimate of the dust temperature and spectral emissivity index within the 80" ISO-LWS beam toward Orion KL/BN, T(d) = 42 +/- 3 K and beta(d) = 1.3 +/- 0.1. We show that both T(d) and beta(d) decrease when going from the HII region and excited OMC1 interface to the denser UV shielded part of OMC1 (Orion KL/BN, Orion S). With a model consisting of only free-free and thermal dust emission, we are able to fit data taken at frequencies from 1.5 GHz to 854 GHz (350 mu m). C1 [Dicker, S. R.; Korngut, P. M.; Devlin, M. J.] Univ Penn, Philadelphia, PA 19104 USA. [Mason, B. S.; Cotton, W. D.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. [Compiegne, M.; Martin, P. G.] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada. [Ade, P. A. R.; Tucker, C.] Cardiff Univ, Cardiff CF24 3YB, S Glam, Wales. [Benford, D. J.; Staguhn, J. G.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Irwin, K. D.] Natl Inst Stand & Technol, Boulder, CO 80305 USA. [Maddalena, R. J.; McMullin, J. P.; Shepherd, D. S.] Natl Radio Astron Observ, Green Bank, WV 24944 USA. [Sievers, A.] IRAM, Nucleo Cent, E-18012 Granada, Spain. [Staguhn, J. G.] Univ Maryland, College Pk, MD 20742 USA. RP Dicker, SR (reprint author), Univ Penn, 209 S 33rd St, Philadelphia, PA 19104 USA. RI Benford, Dominic/D-4760-2012 OI Benford, Dominic/0000-0002-9884-4206 FU NSF [AST-0705185, AST-0607654]; National Radio Astronomy Observatory (NRAO); University of Pennsylvania FX The authors acknowledge all those who worked to make the MUSTANG camera and we would also like to thank the GISMO team and the IRAM staff for their hard work. We thank Rick Arendt and Dale Fixsen for sharing their least-squares imaging code and Darren Dowell for hiswork on the SHARC-II map. The GISMO observations were made possible by support through NSF grant AST-0705185. Funding for the MUSTANG camera was provided by the National Radio Astronomy Observatory (NRAO) and the University of Pennsylvania. Observations were supported by NSF award number AST-0607654. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. NR 39 TC 23 Z9 23 U1 1 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD NOV 1 PY 2009 VL 705 IS 1 BP 226 EP 236 DI 10.1088/0004-637X/705/1/226 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 508CA UT WOS:000270903200018 ER PT J AU Su, KYL Rieke, GH Stapelfeldt, KR Malhotra, R Bryden, G Smith, PS Misselt, KA Moro-Martin, A Williams, JP AF Su, K. Y. L. Rieke, G. H. Stapelfeldt, K. R. Malhotra, R. Bryden, G. Smith, P. S. Misselt, K. A. Moro-Martin, A. Williams, J. P. TI THE DEBRIS DISK AROUND HR 8799 SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; infrared: stars; planetary systems; stars: individual (HR 8799) ID MULTIBAND IMAGING PHOTOMETER; SPITZER-SPACE-TELESCOPE; LAMBDA-BOOTIS PHENOMENON; ABSOLUTE CALIBRATION; SOLAR-SYSTEM; PLANET FORMATION; DUSTY DEBRIS; WARM DUST; MU-M; VEGA-LIKE AB We have obtained a full suite of Spitzer observations to characterize the debris disk around HR 8799 and to explore how its properties are related to the recently discovered set of three massive planets orbiting the star. We distinguish three components to the debris system: (1) warm dust (T similar to 150 K) orbiting within the innermost planet; (2) a broad zone of cold dust (T similar to 45 K) with a sharp inner edge orbiting just outside the outermost planet and presumably sculpted by it; and (3) a dramatic halo of small grains originating in the cold dust component. The high level of dynamical activity implied by this halo may arise due to enhanced gravitational stirring by the massive planets. The relatively young age of HR 8799 places it in an important early stage of development and may provide some help in understanding the interaction of planets and planetary debris, an important process in the evolution of our own solar system. C1 [Su, K. Y. L.; Rieke, G. H.; Smith, P. S.; Misselt, K. A.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Stapelfeldt, K. R.; Bryden, G.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Malhotra, R.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Moro-Martin, A.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Moro-Martin, A.] CSIC INTA, Ctr Astrobiol, Madrid, Spain. [Williams, J. P.] Univ Hawaii, Astron Inst, Honolulu, HI 96822 USA. RP Su, KYL (reprint author), Univ Arizona, Steward Observ, 933 N Cherry Ave, Tucson, AZ 85721 USA. EM ksu@as.arizona.edu RI Stapelfeldt, Karl/D-2721-2012; OI Williams, Jonathan/0000-0001-5058-695X; Malhotra, Renu/0000-0002-1226-3305; Su, Kate/0000-0002-3532-5580 FU NASA [1255094, 1256424] FX This work is based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology. Support for this work was provided by NASA through contract 1255094 and 1256424 issued by JPL/Caltech to the University of Arizona. We thank Chian-Chou Chen for assistance with the JCMT CO data; David Wilner, and Eric Mamajek for discussion of the background cloud; and Ben Zuckerman for pointing out the error in the velocity comparison of the star and the cloud. K. S. also thanks Glenn Schneider and Mike Meyer for the useful discussion. This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France. NR 69 TC 126 Z9 126 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD NOV 1 PY 2009 VL 705 IS 1 BP 314 EP 327 DI 10.1088/0004-637X/705/1/314 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 508CA UT WOS:000270903200026 ER PT J AU LaMassa, SM Heckman, TM Ptak, A Hornschemeier, A Martins, L Sonnentrucker, P Tremonti, C AF LaMassa, Stephanie M. Heckman, Timothy M. Ptak, Andrew Hornschemeier, Ann Martins, Lucimara Sonnentrucker, Paule Tremonti, Christy TI XMM-NEWTON OBSERVATIONS OF A COMPLETE SAMPLE OF OPTICALLY SELECTED TYPE 2 SEYFERT GALAXIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: Seyfert; X-rays: galaxies ID ACTIVE GALACTIC NUCLEI; DIGITAL-SKY-SURVEY; HARD X-RAY; ULTRALUMINOUS INFRARED GALAXIES; STAR-FORMATION HISTORIES; ENERGY-DISTRIBUTIONS; SPECTRAL PROPERTIES; FORMING GALAXIES; HOST GALAXIES; BLACK-HOLES AB The majority of active galactic nuclei (AGNs) suffer from significant obscuration by surrounding dust and gas. The penetrating power and sensitivity of hard X-ray observations allow obscured AGNs to be probed out to high redshifts. However, X-ray surveys in the 2-10 keV band will miss the most heavily obscured AGNs in which the absorbing column density exceeds similar to 10(24) cm(-2) (the Compton-thick AGN). It is, therefore, vital to know the fraction of AGNs that are missed in such X-ray surveys and to determine if these AGNs represent some distinct population in terms of the fundamental properties of AGNs and/or their host galaxies. In this paper, we present the analysis of XMM-Newton X-ray data for a complete sample of 17 low-redshift Type 2 Seyfert galaxies chosen from the Sloan Digital Sky Survey based solely on the high observed flux of the [OIII]lambda 5007 emission line. This line is formed in the narrow-line region hundreds of parsecs away from the central engine. Thus, unlike the X-ray emission, it is not affected by obscuration due to the torus surrounding the black hole. It therefore provides a useful isotropic indicator of the AGN luminosity. As additional indicators of the intrinsic AGN luminosity, we use the Spitzer Space Telescope to measure the luminosities of the mid-infrared continuum and the [OIV] 25.89 mu m narrow emission line. We then use the ratio of the 2-10 keV X-ray luminosity to the [OIII], [OIV], and mid-infrared luminosities to assess the amount of X-ray obscuration and to distinguish between Compton-thick and Compton-thin objects. The various diagnostics of AGN luminosity with heavily obscured hard X-ray emission are in broad agreement. We find that the majority of the sources suffer significant amounts of obscuration: the observed 2-10 keV emission is depressed by more than an order of magnitude in 11 of the 17 cases (as expected for Compton-thick sources). Thus, surveys in the rest-frame 2-10 keV band will be significantly incomplete for obscured AGNs. We find a strong inverse correlation between the ratio of the 2-10 keV X-ray and [OIII] (or [OIV] or mid-IR) fluxes and the equivalent width of the 6.4 keV Fe K alpha line. This demonstrates that the weak hard X-ray continuum emission is due to obscuration (rather than due to intrinsically weak emission). In several cases, the large amount of obscuration is not consistent with the values of absorbing column density derived from simple spectral fits to the data. We run simulations of a more physically realistic model with partial covering of the X-ray source plus Compton scattering, and show that such models are consistent with the data. We show that the distribution of obscuration in the 2-10 keV band in our sample is similar to what is seen in samples selected in the Swift BAT energy band (14-195 keV). This implies that the BAT surveys do recover a significant fraction of the local population of Compton-thick AGNs. Finally, we find no relationship between the amount of X-ray obscuration and the other properties of the AGN and its host galaxy. Hence, Compton-thick and Compton-thin sources do not seem to trace distinct populations. C1 [LaMassa, Stephanie M.; Heckman, Timothy M.; Ptak, Andrew; Sonnentrucker, Paule] Johns Hopkins Univ, Baltimore, MD 21218 USA. [Hornschemeier, Ann] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Martins, Lucimara] Univ Cruzeiro Sul, NAT, Sao Paulo, Brazil. [Tremonti, Christy] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Tremonti, Christy] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. RP LaMassa, SM (reprint author), Johns Hopkins Univ, Baltimore, MD 21218 USA. RI Ptak, Andrew/D-3574-2012; Martins, Lucimara/K-5158-2012; 7, INCT/H-6207-2013; Astrofisica, Inct/H-9455-2013 OI Martins, Lucimara/0000-0001-6505-5190; FU NASA [NNX07AQ36G]; Alexander von Humboldt Foundation FX This work was funded by NASA grant number NNX07AQ36G. The authors thank the anonymous referee for insightful comments and suggestions which improved the quality of the manuscript. C. A. T thanks the Alexander von Humboldt Foundation for their support. NR 64 TC 42 Z9 42 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD NOV 1 PY 2009 VL 705 IS 1 BP 568 EP 586 DI 10.1088/0004-637X/705/1/568 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 508CA UT WOS:000270903200047 ER PT J AU Yu, S Drouin, BJ Pearson, JC AF Yu, Shanshan Drouin, Brian J. Pearson, John C. TI TERAHERTZ SPECTROSCOPY OF THE BENDING VIBRATIONS OF ACETYLENE (C2H2)-C-12 SO ASTROPHYSICAL JOURNAL LA English DT Article DE catalogs; ISM: molecules; methods: laboratory; molecular data; techniques: spectroscopic ID C2H2; SPECTRA; IDENTIFICATION; MOLECULES AB Twenty P-branch transitions of (C2H2)-C-12 have been measured in the 0.8-1.6 THz region of its bending vibrational difference band. The accuracy of these measurements is estimated to be 100 kHz. The (C2H2)-C-12 molecules were generated under room temperature by passing 150 mTorr H2O vapor through calcium carbide (CaC2) powder. The observed transitions were modeled together with prior far-infrared data involving the bending levels with Sigma(t) V-t (t = 4, 5) <= 2. Frequency predictions of (C2H2)-C-12 in the terahertz region have been greatly improved by adding the first data of "microwave" precision. The new measurements and predictions reported here will facilitate the analyses of astronomical observations by the high spectral resolution telescopes such as Herschel, SOFIA, and ALMA. C1 [Yu, Shanshan; Drouin, Brian J.; Pearson, John C.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Yu, S (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM shanshan.yu@jpl.nasa.gov RI Yu, Shanshan/D-8733-2016 FU National Aeronautics and Space Administration; Oak Ridge Associated Universities through a contract with NASA FX The research described in this paper was performed at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. S. Y. is a NASA Postdoctoral fellow, and her research was supported by an appointment to the NASA Postdoctoral Program at the Jet Propulsion Laboratory, administrated by Oak Ridge Associated Universities through a contract with NASA. The authors thank Professor M. Herman for providing an electronic line list of C2H2. NR 20 TC 12 Z9 12 U1 1 U2 13 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD NOV 1 PY 2009 VL 705 IS 1 BP 786 EP 790 DI 10.1088/0004-637X/705/1/786 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 508CA UT WOS:000270903200065 ER PT J AU Welsch, BT Li, Y Schuck, PW Fisher, GH AF Welsch, Brian T. Li, Yan Schuck, Peter W. Fisher, George H. TI WHAT IS THE RELATIONSHIP BETWEEN PHOTOSPHERIC FLOW FIELDS AND SOLAR FLARES? SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun: atmospheric motions; Sun: flares; Sun: magnetic fields ID CORONAL MASS EJECTIONS; MAGNETIC INDUCTION EQUATION; LOCAL CORRELATION TRACKING; QUIET ACTIVE REGIONS; FLUX CANCELLATION; EMERGING FLUX; NEUTRAL LINES; MODEL; EMERGENCE; EVOLUTION AB We estimated photospheric velocities by separately applying the Fourier Local Correlation Tracking and Differential Affine Velocity Estimator methods to 2708 co-registered pairs of SOHO/MDI magnetograms, with nominal 96 minute cadence and similar to 2 '' pixels, from 46 active regions (ARs) from 1996 to 1998 over the time interval tau(45) when each AR was within 45 degrees of disk center. For each magnetogram pair, we computed the reprojected, average estimated radial magnetic field, (B) over tilde (R); and each tracking method produced an independently estimated flow field, u. We then quantitatively characterized these magnetic and flow fields by computing several extensive and intensive properties of each; extensive properties scale with AR size, while intensive properties do not depend directly on AR size. Intensive flow properties included moments of speeds, horizontal divergences, and radial curls; extensive flow properties included sums of these properties over each AR, and a crude proxy for the ideal Poynting flux, S-R = Sigma vertical bar u vertical bar(B) over tilde (2)(R). Several quantities derived from (B) over tilde (R) were also computed, including: F, the total unsigned flux; R, a measure of the unsigned flux near strong-field polarity inversion lines; and (B) over tilde (2)(R). Next, using correlation and discriminant analysis, we investigated the associations between these properties and flares from the GOES flare catalog, when averaged over both tau(45) and shorter time windows of 6 and 24 hr. Our AR sample included both flaring and flare-quiet ARs; the latter did not flare above GOES C1.0 level during tau(45). Among magnetic properties, we found R to be most strongly associated with flare flux. Among extensive flow properties, the proxy Poynting flux, S-R, was most strongly associated with flare flux, at a level comparable to that of R. All intensive flow properties studied were more poorly associated with flare flux than these extensive properties. Past flare activity was also associated with future flare occurrence. The largest coefficients of determination from correlations with flare flux that we performed are similar to 0.25, implying no single variable that we considered can explain the majority of variability in average flare flux. C1 [Welsch, Brian T.; Li, Yan; Fisher, George H.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Schuck, Peter W.] NASA, Goddard Space Flight Ctr, Space Weather Lab, Heliophys Sci Div, Greenbelt, MD 20771 USA. RP Welsch, BT (reprint author), Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. EM welsch@ssl.berkeley.edu RI Fisher, George/G-1380-2015 OI Fisher, George/0000-0002-6912-5704 FU NSF [ATM-0451438, ATM-0752597, ATM-0120950, ATM-0641303, ATM-0551084]; NASA [NNH06AD87I, NNH07AG26I, NNH07CD25C]; AFOSR [F49620-00-C-0004, F49620-03-C-0019] FX The authors appreciate the referee's careful reading of the manuscript and thoughtful comments, which have improved the manuscript. B. T. W. and Y. L. acknowledge the support of NSF grant ATM-0451438, and NSF SHINE award ATM-0752597 for B. T. W. Y. L. additionally acknowledges support from NSF CISM ATM-0120950. P. W. S. acknowledges support from NASA LWS TR& T grant NNH06AD87I, LWS TR& T Strategic Capability grant NNH07AG26I, and ONR. G. H. F. acknowledges support for his development work on FLCT from NSF awards ATM-0641303 and ATM-0551084. The discriminant analysis code we used was kindly supplied by G. Barnes and K. D. Leka, who received funding from AFOSR under contracts F49620-00-C-0004, F49620-03-C-0019, and from NASA under contract NNH07CD25C. We thank the SOHO/MDI team for making their database available and easy to use. MDI is funded through NASA's Solar and Heliospheric Physics program. The SOHO project results from international cooperation between NASA and ESA. B. T. W. also gratefully acknowledges discussions with Maureen Lahiff regarding statistical analysis techniques. NR 73 TC 38 Z9 39 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD NOV 1 PY 2009 VL 705 IS 1 BP 821 EP 843 DI 10.1088/0004-637X/705/1/821 PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 508CA UT WOS:000270903200069 ER PT J AU Zenitani, S Hesse, M Klimas, A AF Zenitani, Seiji Hesse, Michael Klimas, Alex TI RELATIVISTIC TWO-FLUID SIMULATIONS OF GUIDE FIELD MAGNETIC RECONNECTION SO ASTROPHYSICAL JOURNAL LA English DT Article DE magnetic fields; MHD; plasmas; relativity ID PAIR PLASMAS; MAGNETOHYDRODYNAMIC SIMULATIONS; PARTICLE-ACCELERATION; EQUATIONS; MHD AB The nonlinear evolution of relativistic magnetic reconnection in sheared magnetic configuration (with a guide field) is investigated by using two-dimensional relativistic two-fluid simulations. Relativistic guide field reconnection features the charge separation and the guide field compression in and around the outflow channel. As the guide field increases, the composition of the outgoing energy changes from enthalpy-dominated to Poynting-dominated. The inertial effects of the two-fluid model play an important role to sustain magnetic reconnection. Implications for the single-fluid magnetohydrodynamic approach and the physics models of relativistic reconnection are briefly addressed. C1 [Zenitani, Seiji; Hesse, Michael; Klimas, Alex] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Zenitani, S (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM Seiji.Zenitani-1@nasa.gov RI Hesse, Michael/D-2031-2012; Zenitani, Seiji/D-7988-2013; NASA MMS, Science Team/J-5393-2013 OI Zenitani, Seiji/0000-0002-0945-1815; NASA MMS, Science Team/0000-0002-9504-5214 FU NASA Center for Computational Sciences FX The authors are grateful to R. Yoshitake and M. Kuznetsova for helpful comments. The authors also thank the anonymous referee for his/her constructive comments on this manuscript. This research was supported by the NASA Center for Computational Sciences, and NASA's MMS SMART mission. S. Z. gratefully acknowledges support from NASA's postdoctoral program. NR 19 TC 19 Z9 19 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD NOV 1 PY 2009 VL 705 IS 1 BP 907 EP 913 DI 10.1088/0004-637X/705/1/907 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 508CA UT WOS:000270903200076 ER PT J AU Brown, ML Ade, P Bock, J Bowden, M Cahill, G Castro, PG Church, S Culverhouse, T Friedman, RB Ganga, K Gear, WK Gupta, S Hinderks, J Kovac, J Lange, AE Leitch, E Melhuish, SJ Memari, Y Murphy, JA Orlando, A Sullivan, CO Piccirillo, L Pryke, C Rajguru, N Rusholme, B Schwarz, R Taylor, AN Thompson, KL Turner, AH Wu, EYS Zemcov, M AF Brown, M. L. Ade, P. Bock, J. Bowden, M. Cahill, G. Castro, P. G. Church, S. Culverhouse, T. Friedman, R. B. Ganga, K. Gear, W. K. Gupta, S. Hinderks, J. Kovac, J. Lange, A. E. Leitch, E. Melhuish, S. J. Memari, Y. Murphy, J. A. Orlando, A. Sullivan, C. O' Piccirillo, L. Pryke, C. Rajguru, N. Rusholme, B. Schwarz, R. Taylor, A. N. Thompson, K. L. Turner, A. H. Wu, E. Y. S. Zemcov, M. CA QUaD Collaboration TI IMPROVED MEASUREMENTS OF THE TEMPERATURE AND POLARIZATION OF THE COSMIC MICROWAVE BACKGROUND FROM QUaD SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmic microwave background; cosmological parameters; cosmology: observations; polarization ID PROBE WMAP OBSERVATIONS; POWER SPECTRUM; 2003 FLIGHT; COSMOLOGICAL PARAMETERS; BOOMERANG; MAPS; ANISOTROPIES; DESIGN; IMAGER; CAPMAP AB We present an improved analysis of the final data set from the QUaD experiment. Using an improved technique to remove ground contamination, we double the effective sky area and hence increase the precision of our cosmic microwave background (CMB) power spectrum measurements by similar to 30% versus that previously reported. In addition, we have improved our modeling of the instrument beams and have reduced our absolute calibration uncertainty from 5% to 3.5% in temperature. The robustness of our results is confirmed through extensive jackknife tests, and by way of the agreement that we find between our two fully independent analysis pipelines. For the standard six-parameter Lambda CDM model, the addition of QUaD data marginally improves the constraints on a number of cosmological parameters over those obtained from the WMAP experiment alone. The impact of QUaD data is significantly greater for a model extended to include either a running in the scalar spectral index, or a possible tensor component, or both. Adding both the QUaD data and the results from the Arcminute Cosmology Bolometer Array Receiver experiment, the uncertainty in the spectral index running is reduced by similar to 25% compared to WMAP alone, while the upper limit on the tensor-to-scalar ratio is reduced from r < 0.48 tor < 0.33 (95% c. l.). This is the strongest limit on tensors to date from the CMB alone. We also use our polarization measurements to place constraints on parity-violating interactions to the surface of last scattering, constraining the energy scale of Lorentz violating interactions to < 1.5 x 10(-43) GeV (68% c.l.). Finally, we place a robust upper limit on the strength of the lensing B-mode signal. Assuming a single flat band power between l = 200 and l = 2000, we constrain the amplitude of B-modes to be < 0.57 mu K-2 (95% c.l.). C1 [Brown, M. L.] Univ Cambridge, Cavendish Astrophys, Cambridge CB3 OHE, England. [Brown, M. L.] Kavli Inst Cosmol Cambridge, Cambridge CB3 OHA, England. [Ade, P.; Bowden, M.; Gear, W. K.; Gupta, S.; Orlando, A.; Rajguru, N.; Turner, A. H.; Zemcov, M.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Bock, J.; Leitch, E.; Zemcov, M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Bock, J.; Kovac, J.; Lange, A. E.; Leitch, E.; Orlando, A.; Zemcov, M.] CALTECH, Pasadena, CA 91125 USA. [Bowden, M.; Church, S.; Hinderks, J.; Rusholme, B.; Thompson, K. L.; Wu, E. Y. S.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA. [Bowden, M.; Church, S.; Hinderks, J.; Rusholme, B.; Thompson, K. L.; Wu, E. Y. S.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA. [Cahill, G.; Murphy, J. A.; Sullivan, C. O'] Natl Univ Ireland Maynooth, Dept Expt Phys, Maynooth, Kildare, Ireland. [Castro, P. G.; Memari, Y.; Taylor, A. N.] Univ Edinburgh, Royal Observ, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland. [Culverhouse, T.; Friedman, R. B.; Pryke, C.; Schwarz, R.] Univ Chicago, Dept Astron & Astrophys, Enrico Fermi Inst, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Ganga, K.] Univ Paris 07, APC, CNRS, F-75205 Paris 13, France. [Melhuish, S. J.; Piccirillo, L.] Univ Manchester, Sch Phys & Astron, Manchester M13 9PL, Lancs, England. RP Brown, ML (reprint author), Univ Cambridge, Cavendish Astrophys, JJ Thomson Ave, Cambridge CB3 OHE, England. RI Melhuish, Simon/B-1299-2016; OI Melhuish, Simon/0000-0001-8725-4991; Orlando, Angiola/0000-0001-8004-5054 NR 53 TC 189 Z9 189 U1 1 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD NOV 1 PY 2009 VL 705 IS 1 BP 978 EP 999 DI 10.1088/0004-637X/705/1/978 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 508CA UT WOS:000270903200082 ER PT J AU Krick, JE Surace, JA Thompson, D Ashby, MLN Hora, J Gorjian, V Yan, L Frayer, DT Egami, E Lacy, M AF Krick, J. E. Surace, J. A. Thompson, D. Ashby, M. L. N. Hora, J. Gorjian, V. Yan, L. Frayer, D. T. Egami, E. Lacy, M. TI THE INFRARED ARRAY CAMERA DARK FIELD: FAR-INFRARED TO X-RAY DATA SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE cosmology: observations; galaxies: photometry ID SPITZER-SPACE-TELESCOPE; STAR-FORMING GALAXIES; MULTIBAND IMAGING PHOTOMETER; ACTIVE GALACTIC NUCLEI; EXTENDED GROTH STRIP; IRAC SHALLOW SURVEY; HUBBLE DEEP FIELD; 160 MU-M; ABSOLUTE CALIBRATION; STELLAR POPULATIONS AB We present 20 band photometry from the far-IR to X-ray in the Spitzer Infrared Array Camera ( IRAC) dark field. The bias for the near-IR camera on Spitzer is calibrated by observing a similar to 20' diameter "dark" field near the north ecliptic pole roughly every two-to-three weeks throughout the mission duration of Spitzer. The field is unique for its extreme depth, low background, high quality imaging, time-series information, and accompanying photometry including data taken with Akari, Palomar, MMT, KPNO, Hubble, and Chandra. This serendipitous survey contains the deepest mid-IR data taken to date. This data set is well suited for studies of intermediate-redshift galaxy clusters, high-redshift galaxies, the first generation of stars, and the lowest mass brown dwarfs, among others. This paper provides a summary of the data characteristics and catalog generation from all bands collected to date as well as a discussion of photometric redshifts and initial and expected science results and goals. To illustrate the scientific potential of this unique data set, we also present here IRAC color-color diagrams. C1 [Krick, J. E.; Surace, J. A.; Yan, L.; Lacy, M.] CALTECH, Jet Prop Lab, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Thompson, D.] Univ Arizona, Large Binocular Telescope Observ, Tucson, AZ 85721 USA. [Ashby, M. L. N.; Hora, J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Gorjian, V.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Frayer, D. T.] CALTECH, NASA, Herschel Sci Ctr, Pasadena, CA 91109 USA. [Egami, E.] Univ Arizona, Dept Astron, Tucson, AZ 85721 USA. RP Krick, JE (reprint author), CALTECH, Jet Prop Lab, Spitzer Sci Ctr, MS 220-6, Pasadena, CA 91125 USA. EM jkrick@caltech.edu OI Hora, Joseph/0000-0002-5599-4650 FU NASA through a grant from the Space Telescope Science Institute [10521, NAS 5-26555]; NSF [AST97-31180]; Kitt Peak National Observatory; National Aeronautics and Space Administration through Chandra Award [G07-8120, NAS8-03060] FX We thank the anonymous referee for useful suggestions on the manuscript. This research has made use of data 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 work was based on observations obtained with the Hale Telescope, Palomar Observatory as part of a continuing collaboration between the California Institute of Technology, NASA/JPL, and Cornell University, the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA, and the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc. Support for program # 10521 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. FLAMINGOS was designed and constructed by the IR instrumentation group (PI: R. Elston) at the University of Florida, Department of Astronomy, with support from NSF grant AST97-31180 and Kitt Peak National Observatory. Observations reported here were obtained at the MMT Observatory, a joint facility of the Smithsonian Institution and theUniversity of Arizona. Support for this work was provided by the National Aeronautics and Space Administration through Chandra Award Number G07-8120 issued by the Chandra X-ray Observatory Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of the National Aeronautics Space Administration under contract NAS8-03060. NR 55 TC 7 Z9 7 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 NOV PY 2009 VL 185 IS 1 BP 85 EP 97 DI 10.1088/0067-0049/185/1/85 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 514NZ UT WOS:000271402900004 ER PT J AU Stalder, B Chambers, KC Vacca, WD AF Stalder, B. Chambers, K. C. Vacca, William D. TI 58 RADIO SOURCES NEAR BRIGHT NATURAL GUIDE STARS SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE galaxies: evolution; galaxies: formation; galaxies: fundamental parameters; galaxies: high-redshift ID HIGH-REDSHIFT GALAXIES; NEAR-INFRARED SPECTRA; K-Z RELATION; ELLIPTIC GALAXIES; STELLAR POPULATIONS; FORMING GALAXIES; PHOTOMETRIC REDSHIFTS; OPTICAL MORPHOLOGIES; STANDARD STARS; FILTER SET AB We present a preliminary survey of 58 radio sources within the isoplanatic patches (r < 25 '') of bright (11 < R < 12) stars suitable for use as natural guide stars with high-order adaptive optics (AO). An optical and near-infrared imaging survey was conducted utilizing tip-tilt corrections in the optical and AO in the near-infrared. Spectral energy distributions were fit to the multi-band data for the purpose of obtaining photometric redshifts using the Hyperz code. Several of these photometric redshifts were confirmed with spectroscopy, a result that gives more confidence to the redshift distribution for the whole sample. Additional long-wavelength data from Spitzer, SCUBA, SHARC2, and VLA supplement the optical and near-infrared data. We find the sample generally follows and extends the magnitude-redshift relation found for more powerful local radio galaxies. The survey has identified several reasonably bright (H = 19-20) objects at significant redshifts (z > 1) that are now within the capabilities of the current generation of AO-fed integral-field spectrographs. These objects constitute a unique sample that can be used for detailed ground-based AO studies of galactic structure, evolution, and active galactic nucleus formation at high redshift. C1 [Stalder, B.; Chambers, K. C.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Vacca, William D.] NASA, Ames Res Ctr, SOFIA USRA, Moffett Field, CA 94035 USA. RP Stalder, B (reprint author), Harvard Univ, Dept Phys, 17 Oxford St, Cambridge, MA 02138 USA. EM bstalder@physics.harvard.edu; chambers@ifa.hawaii.edu; wvacca@sofia.usra.edu OI Chambers, Kenneth /0000-0001-6965-7789 FU NSF [AST 0098349]; Pan-STARRS Camera Group; NASA FX We thank Michael Connelley, Steve Howell, Elizabeth McGrath, and Barry Rothberg for assisting in some of the imaging and spectroscopy observations for this huge data set. We also acknowledge the telescope support staffs at the University of Hawaii 2.2 m as well as the Infrared Telescope Facility, which is operated by the University of Hawaii under Cooperative Agreement No. NCC 5-538 with the National Aeronautics and Space Administration, Science Mission Directorate, Planetary Astronomy Program. This research was partially supported by the Extragalactic and Cosmology division of NSF under grant AST 0098349 and also partially supported by the Pan-STARRS Camera Group. This research has made use of the NASA/IPAC Extragalactic Database (NED), which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract to the National Aeronautics and Space Administration. This work is partly 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 58 TC 0 Z9 0 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD NOV PY 2009 VL 185 IS 1 BP 124 EP 155 DI 10.1088/0067-0049/185/1/124 PG 32 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 514NZ UT WOS:000271402900006 ER PT J AU Walsh, JL Minezaki, T Bentz, MC Barth, AJ Baliber, N Li, WD Stern, D Bennert, VN Brown, TM Canalizo, G Filippenko, AV Gates, EL Greene, JE Malkan, MA Sakata, Y Street, RA Treu, T Woo, JH Yoshii, Y AF Walsh, Jonelle L. Minezaki, Takeo Bentz, Misty C. Barth, Aaron J. Baliber, Nairn Li, Weidong Stern, Daniel Bennert, Vardha Nicola Brown, Timothy M. Canalizo, Gabriela Filippenko, Alexei V. Gates, Elinor L. Greene, Jenny E. Malkan, Matthew A. Sakata, Yu Street, Rachel A. Treu, Tommaso Woo, Jong-Hak Yoshii, Yuzuru TI THE LICK AGN MONITORING PROJECT: PHOTOMETRIC LIGHT CURVES AND OPTICAL VARIABILITY CHARACTERISTICS SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE galaxies: active; galaxies: nuclei; galaxies: Seyfert ID ACTIVE GALACTIC NUCLEI; BROAD-LINE REGION; BLACK-HOLE MASS; RADIUS-LUMINOSITY RELATIONSHIP; HOST-GALAXY STARLIGHT; NGC 7469; X-RAY; REVERBERATION MEASUREMENTS; SEYFERT-1 GALAXIES; QUASAR VARIABILITY AB The Lick AGN Monitoring Project targeted 13 nearby Seyfert 1 galaxies with the intent of measuring the masses of their central black holes using reverberation mapping. The sample includes 12 galaxies selected to have black holes with masses roughly in the range 10(6)-10(7) M-circle dot, as well as the well-studied active galactic nucleus (AGN) NGC 5548. In conjunction with a spectroscopic monitoring campaign, we obtained broadband B and V images on most nights from 2008 February through 2008 May. The imaging observations were carried out by four telescopes: the 0.76 m Katzman Automatic Imaging Telescope, the 2 m Multicolor Active Galactic Nuclei Monitoring telescope, the Palomar 60 inch (1.5 m) telescope, and the 0.80 m Tenagra II telescope. Having well-sampled light curves over the course of a few months is useful for obtaining the broad-line reverberation lag and black hole mass, and also allows us to examine the characteristics of the continuum variability. In this paper, we discuss the observational methods and the photometric measurements, and present the AGN continuum light curves. We measure various variability characteristics of each of the light curves. We do not detect any evidence for a time lag between the B-and V-band variations, and we do not find significant color variations for the AGNs in our sample. C1 [Walsh, Jonelle L.; Bentz, Misty C.; Barth, Aaron J.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. [Minezaki, Takeo; Sakata, Yu; Yoshii, Yuzuru] Univ Tokyo, Sch Sci, Inst Astron, Tokyo 1810015, Japan. [Baliber, Nairn; Bennert, Vardha Nicola; Street, Rachel A.; Treu, Tommaso] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Baliber, Nairn; Brown, Timothy M.; Street, Rachel A.] Las Cumbres Observ Global Telescope, Goleta, CA 93117 USA. [Li, Weidong; Filippenko, Alexei V.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Stern, Daniel] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Canalizo, Gabriela] Univ Calif Riverside, Dept Phys & Astron, Riverside, CA 92521 USA. [Canalizo, Gabriela] Univ Calif Riverside, Inst Geophys & Planetary Phys, Riverside, CA 92521 USA. [Gates, Elinor L.] Lick Observ, Mt Hamilton, CA 95140 USA. [Greene, Jenny E.] Princeton Univ Observ, Princeton, NJ 08544 USA. [Malkan, Matthew A.; Woo, Jong-Hak] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90024 USA. [Sakata, Yu] Univ Tokyo, Sch Sci, Dept Astron, Bunkyo Ku, Tokyo 1130033, Japan. [Yoshii, Yuzuru] Univ Tokyo, Sch Sci, Res Ctr Early Universe, Bunkyo Ku, Tokyo 1130033, Japan. [Woo, Jong-Hak] Seoul Natl Univ, Dept Phys & Astron, Astron Program, Seoul 151742, South Korea. RP Walsh, JL (reprint author), Univ Calif Irvine, Dept Phys & Astron, 4129 Frederick Reines Hall, Irvine, CA 92697 USA. EM jlwalsh@uci.edu RI Woo, Jong-Hak/A-2790-2014; OI Barth, Aaron/0000-0002-3026-0562 FU National Science Foundation (NSF) [AST-0548198, AST-0607485, AST-0642621, AST-0507450]; TABASGO Foundation (UC Berkeley); Ministry of Education, Culture, Sports, Science & Technology of Japan [07CE2002]; [10041110]; [10304014]; [12640233]; [14047206]; [14253001]; [14540223] FX We thank MansiKasliwal for assistance with the P60 scheduling. This work was supported by National Science Foundation (NSF) grants AST-0548198 (UC Irvine), AST-0607485 (UC Berkeley), AST-0642621 (UC Santa Barbara), and AST-0507450 (UC Riverside), as well as by the TABASGO Foundation (UC Berkeley). KAIT and its ongoing operation were made possible by donations from Sun Microsystems, Inc., the Hewlett-Packard Company, AutoScope Corporation, the Lick Observatory, the NSF, the University of California, the Sylvia & Jim Katzman Foundation, and the TABASGO Foundation. TheMAGNUM project has been supported partly by the Grant-in-Aid of Scientific Research (10041110, 10304014, 12640233, 14047206, 14253001, and 14540223) and the COE Research (07CE2002) of the Ministry of Education, Culture, Sports, Science & Technology of Japan. The work of D. S. was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. A. V. F. thanks the Aspen Center for Physics, where he participated in a workshop on WideFast- Deep Surveys while this paper was nearing completion. This research has made use of the NASA/IPAC Extragalactic Database (NED), which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA. NR 63 TC 23 Z9 23 U1 0 U2 3 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 NOV PY 2009 VL 185 IS 1 BP 156 EP 170 DI 10.1088/0067-0049/185/1/156 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 514NZ UT WOS:000271402900007 ER PT J AU Habib, E Henschke, A Adler, RF AF Habib, Emad Henschke, Amy Adler, Robert F. TI Evaluation of TMPA satellite-based research and real-time rainfall estimates during six tropical-related heavy rainfall events over Louisiana, USA SO ATMOSPHERIC RESEARCH LA English DT Article DE Satellite rainfall; Statistical evaluation; Tropical storms; TRMM ID PRECIPITATION ANALYSIS TMPA; GLOBAL PRECIPITATION; PASSIVE MICROWAVE; RIVER-BASIN; TRMM; PRODUCTS; FLOOD; PREDICTION; RESOLUTION; SCALES AB This study focuses on the evaluation of 3-hourly 0.25 degrees x 0.25 degrees satellite-based rainfall estimates produced by the Tropical Rainfall Measuring Mission (TRMM) Multi-satellite Precipitation Analysis (TMPA). The evaluation is performed during six heavy rainfall events that were generated by tropical storms passing over Louisiana, United States. Two surface-based rainfall datasets from gauge and radar observations are used as a ground reference for evaluating the real-time (RT) version of the TMPA product and the post-real-time bias adjusted research version. The evaluation analysis is performed at the native temporal and spatial scales of the TMPA products, 3-hourly and 0.25 degrees x0.25 degrees. Several graphical and statistical techniques are applied to characterize the deviation of the TMPA estimates from the reference datasets. Both versions of the TMPA products track reasonably well the temporal evolution and fluctuations of surface rainfall during the analyzed storms with moderate to high correlation values of 0.5-0.8. The TMPA estimates reported reasonable levels of rainfall detection especially when light rainfall rates are excluded. On a storm scale, the TMPA products are characterized by varying degrees of bias which was mostly within 25% and 50% for the research and RT products, respectively. Analysis of the error distribution indicated that, on average, the TMPA products tend to overestimate small rain rates and underestimate large rain rates. Compared to the real-time estimates, the research product shows significant improvement in the overall and conditional bias, and in the correlation coefficients, with slight deterioration in the probability of detecting rainfall occurrences. A fair agreement in terms of reproducing the tail of the distribution of rain rates (i.e., probability of surface rainfall exceeding certain thresholds) was observed especially for the RT estimates. Despite the apparent differences with surface rainfall estimates, the results reported in this study highlight the TMPA potential as a valuable resource of high-resolution rainfall information over many areas in the world that lack capabilities for monitoring landfalling tropical storms. (C) 2009 Elsevier B.V. All rights reserved. C1 [Habib, Emad; Henschke, Amy] Univ Louisiana Lafayette, Dept Civil Engn, Lafayette, LA 70504 USA. [Adler, Robert F.] Univ Maryland, College Pk, MD 20742 USA. [Adler, Robert F.] NASA, Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD 20771 USA. RP Habib, E (reprint author), Univ Louisiana Lafayette, Dept Civil Engn, POB 42991, Lafayette, LA 70504 USA. EM habib@louisiana.edu FU NASA/LEQSF; LaSPACE; NASA [NNG05GH22H] FX The authors would like to acknowledge the following sources of support: the Louisiana Board of Regents Support Fund under contract number NASA/LEQSF (2005-2010)LaSPACE and NASA grant number NNG05GH22H and the Research Competitiveness Subprogram of the Louisiana Board of Regents Support Fund, provided to the first author, and the LaSPACE Undergraduate Research Assistantship provided to the second author. The authors also acknowledge Dr. Yang Hong for his input during the early stage of this study and Dr. Dongsoo Kim for providing the quality-controlled version of the HADS gauge dataset. NR 47 TC 65 Z9 66 U1 3 U2 20 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0169-8095 J9 ATMOS RES JI Atmos. Res. PD NOV PY 2009 VL 94 IS 3 BP 373 EP 388 DI 10.1016/j.atmosres.2009.06.015 PG 16 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 513PW UT WOS:000271336300002 ER PT J AU Wagner, EB Charles, JB Cuttino, CM AF Wagner, Erika B. Charles, John B. Cuttino, Charles Marsh TI Opportunities for Research in Space Life Sciences Aboard Commercial Suborbital Flights SO AVIATION SPACE AND ENVIRONMENTAL MEDICINE LA English DT Editorial Material DE spaceflight; microgravity; commercial; tourism AB WAGNER EB, CHARLES JB, CUTTINO CM. Opportunities for research in space life sciences aboard commercial suborbital flights. Aviat Space Environ Med 2009; 80:984-6. The emergence of commercial suborbital spaceflight offers a wide range of new research and development opportunities for those in the space life sciences. Large numbers of diverse flyers, frequent re-flights, and flexible operations provide a fertile ground for both basic and applied science, as well as technology demonstrations. This commentary explores some of the unique features available to the space life science community and encourages engagement with commercial developers and operators during the design phase to help optimize platform designs and operations for future research. C1 [Wagner, Erika B.] MIT, Cambridge, MA 02139 USA. [Charles, John B.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Cuttino, Charles Marsh] Virginia Emergency Phys, Dept Emergency Med, CJW Med Ctr, Richmond, VA USA. RP Wagner, EB (reprint author), MIT, 77 Massachusetts Ave,37-219, Cambridge, MA 02139 USA. EM erika@mit.edu NR 8 TC 1 Z9 1 U1 0 U2 0 PU AEROSPACE MEDICAL ASSOC PI ALEXANDRIA PA 320 S HENRY ST, ALEXANDRIA, VA 22314-3579 USA SN 0095-6562 J9 AVIAT SPACE ENVIR MD JI Aviat. Space Environ. Med. PD NOV PY 2009 VL 80 IS 11 BP 984 EP 986 DI 10.3357/ASEM.2589.2009 PG 3 WC Public, Environmental & Occupational Health; Medicine, General & Internal; Sport Sciences SC Public, Environmental & Occupational Health; General & Internal Medicine; Sport Sciences GA 512RI UT WOS:000271267500012 PM 19911525 ER PT J AU Berg, LK Berkowitz, CM Ogren, JA Hostetler, CA Ferrare, RA Dubey, MK Andrews, E Coulter, RL Hair, JW Hubbe, JM Lee, YN Mazzoleni, C Olfert, J Springston, SR AF Berg, Larry K. Berkowitz, Carl M. Ogren, John A. Hostetler, Chris A. Ferrare, Richard A. Dubey, Manvendra K. Andrews, Elisabeth Coulter, Richard L. Hair, Johnathan W. Hubbe, John M. Lee, Yin-Nan Mazzoleni, Claudio Olfert, Jason Springston, Stephen R. TI OVERVIEW OF THE CUMULUS HUMILIS AEROSOL PROCESSING STUDY SO BULLETIN OF THE AMERICAN METEOROLOGICAL SOCIETY LA English DT Article ID MASS-SPECTROMETER; CLOUD; IMPACTS; FIELD; SIZE; SITE AB The primary goal of the Cumulus Humilis Aerosol Processing Study (CHAPS) was to characterize and contrast freshly emitted aerosols below, within, and above fields of cumuli, and to study changes to the cloud microphysical structure within these same cloud fields in the vicinity of Oklahoma City during June 2007. CHAPS is one of few studies that have had an aerosol mass spectrometer (AMS) sampling downstream of a counterflow virtual impactor (CVI) inlet on an aircraft, allowing the examination of the chemical composition of activated aerosols within the cumuli. The results from CHAPS provide insights into changes in the aerosol chemical and optical properties as aerosols move through shallow cumuli downwind of a moderately sized city. Three instrument platforms were employed during CHAPS, including the U. S. Department of Energy Gulfstream-1 aircraft, which was equipped for in situ sampling of aerosol optical and chemical properties; the NASA Langley King Air B200, which carried the downward-looking NASA Langley High Spectral Resolution Lidar (HSRL) to measure profiles of aerosol backscatter, extinction, and depolarization between the King Air and the surface; and a surface site equipped for continuous in situ measurements of aerosol optical properties, profiles of aerosol backscatter, and meteorological conditions, including total sky cover and thermodynamic profiles of the atmosphere. In spite of record precipitation over central Oklahoma, a total of 8 research flights were made by the G-1 and 18 by the B200, including special satellite verification flights timed to coincide with NASA satellite A-Train overpasses. C1 [Berg, Larry K.; Berkowitz, Carl M.; Hubbe, John M.] Pacific NW Natl Lab, Richland, WA 99352 USA. [Ogren, John A.; Andrews, Elisabeth] NOAA, Earth Syst Res Lab, Boulder, CO USA. [Hostetler, Chris A.; Ferrare, Richard A.; Hair, Johnathan W.] NASA, Langley Res Ctr, Hampton, VA 23665 USA. [Dubey, Manvendra K.; Mazzoleni, Claudio] Los Alamos Natl Lab, Los Alamos, NM USA. [Andrews, Elisabeth] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA. [Coulter, Richard L.] Argonne Natl Lab, Argonne, IL 60439 USA. [Lee, Yin-Nan; Olfert, Jason; Springston, Stephen R.] Brookhaven Natl Lab, Upton, NY 11973 USA. RP Berg, LK (reprint author), POB 999,MSIN K9-30, Richland, WA 99352 USA. EM larry.berg@pnl.gov RI Dubey, Manvendra/E-3949-2010; Mazzoleni, Claudio/E-5615-2011; Ogren, John/M-8255-2015; Berg, Larry/A-7468-2016 OI Dubey, Manvendra/0000-0002-3492-790X; Ogren, John/0000-0002-7895-9583; Berg, Larry/0000-0002-3362-9492 NR 27 TC 23 Z9 23 U1 0 U2 7 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0003-0007 J9 B AM METEOROL SOC JI Bull. Amer. Meteorol. Soc. PD NOV PY 2009 VL 90 IS 11 BP 1653 EP + DI 10.1175/2009BAMS2760.1 PG 17 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 530XU UT WOS:000272627100005 ER PT J AU Chao, WC Yang, B Fu, XH AF Chao, Winston C. Yang, Bo Fu, Xiouhua TI A revised method of presenting wavenumber-frequency power spectrum diagrams that reveals the asymmetric nature of tropical large-scale waves SO CLIMATE DYNAMICS LA English DT Article ID COUPLED EQUATORIAL WAVES; MODELS AB The popular method of presenting wavenumber -frequency power spectrum diagrams for studying tropical large-scale waves in the literature is shown to give an incomplete presentation of these waves. The so-called "convectively coupled Kelvin (mixed Rossby-gravity) waves'' are presented as existing only in the symmetric (anti-symmetric) component of the diagrams. This is obviously not consistent with the published composite/regression studies of "convectively coupled Kelvin waves,'' which illustrate the asymmetric nature of these waves. The cause of this inconsistency is revealed in this note and a revised method of presenting the power spectrum diagrams is proposed. When this revised method is used, "convectively coupled Kelvin waves'' do show anti-symmetric components, and "convectively coupled mixed Rossby-gravity waves (also known as Yanai waves)'' do show a hint of symmetric components. These results bolster a published proposal that these waves should be called "chimeric Kelvin waves,'' "chimeric mixed Rossby-gravity waves,'' etc. This revised method of presenting power spectrum diagrams offers an additional means of comparing the GCM output with observations by calling attention to the capability of GCMs to correctly simulate the asymmetric characteristics of equatorial waves. C1 [Chao, Winston C.] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA. [Yang, Bo; Fu, Xiouhua] Univ Hawaii Manoa, Sch Ocean & Earth Sci & Technol, Int Pacific Res Ctr, Honolulu, HI 96822 USA. RP Chao, WC (reprint author), NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Mail Code 610-1, Greenbelt, MD 20771 USA. EM Winston.c.chao@nasa.gov FU NASA; Japanese Agency for Marine-Earth Science and Technology (JAMSTEC) FX Winston Chao was supported by the Modeling, Analysis and Prediction program of NASA Science Mission Directorate. Bo Yang and Xiouhua Fu were supported by the NASA Earth Science Program, NSF Climate Dynamics Program, and IPRC. IPRC is sponsored by NASA, NOAA, and the Japanese Agency for Marine-Earth Science and Technology (JAMSTEC). Matthew Wheeler provided the WK code for the wavenumber-frequency diagram. MyongIn Lee, Phil Pegion, and Baode Chen of NASA/Goddard/GMAO provided their versions of the WK code for reference purposes. The OLR data used were from Liebmann and Smith of NOAA/CDC. NR 8 TC 6 Z9 7 U1 0 U2 3 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0930-7575 J9 CLIM DYNAM JI Clim. Dyn. PD NOV PY 2009 VL 33 IS 6 BP 843 EP 847 DI 10.1007/s00382-008-0494-3 PG 5 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 505HU UT WOS:000270684100008 ER PT J AU Mathew, G Zwart, SR Smith, SM AF Mathew, Grace Zwart, Sara R. Smith, Scott M. TI Stability of blood analytes after storage in BD SST (TM) tubes for 12 mo SO CLINICAL BIOCHEMISTRY LA English DT Article DE Blood chemical analysis; Clinical chemistry; Serum ID COLLECTION TUBE; GEL; DRUGS; SERUM AB Objectives: We studied the stability of 33 analytes related to clinical chemistry, bone, and vitamin metabolism, after storage in serum separator tubes (SST (TM)). Design and methods: Blood was collected from 6 subjects using SST tubes. Some serum remained in the tube in contact with the barrier gel and was stored at -80 degrees C for 12 mo. Results: Clinically significant changes Occurred only in 1,25-dihydroxyvitamin D and retinol-binding protein. Conclusions: Freezing SST tubes before sample analysis is a viable option for some analytes. (C) 2009 The Canadian Society of Clinical Chemists. Published by Elsevier Inc. All rights reserved. C1 [Zwart, Sara R.; Smith, Scott M.] NASA, Lyndon B Johnson Space Ctr, Human Adaptat & Countermeasures Div, Houston, TX 77058 USA. [Mathew, Grace] Enterprise Advisory Serv Inc, Houston, TX USA. RP Zwart, SR (reprint author), NASA, Lyndon B Johnson Space Ctr, Human Adaptat & Countermeasures Div, Mail Code SK3,2101 NASA Pkwy, Houston, TX 77058 USA. EM sara.zwart-1@nasa.gov FU National Aeronautics; Space Administration's Human Research Program FX Funding support: This research was supported by the National Aeronautics and Space Administration's Human Research Program. NR 11 TC 7 Z9 7 U1 0 U2 2 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0009-9120 J9 CLIN BIOCHEM JI Clin. Biochem. PD NOV PY 2009 VL 42 IS 16-17 BP 1732 EP 1734 DI 10.1016/j.clinbiochem.2009.07.015 PG 3 WC Medical Laboratory Technology SC Medical Laboratory Technology GA 508MO UT WOS:000270935700024 PM 19631634 ER PT J AU Prasad, NR Almanza-Garcia, S Lu, TT AF Prasad, Nadipuram R. Almanza-Garcia, Salvador Lu, Thomas T. TI Anomaly Detection SO CMC-COMPUTERS MATERIALS & CONTINUA LA English DT Article DE Anomaly detection; soft-computing; decision-making; machine intelligence; nonlinear dynamical systems AB The paper presents a revolutionary framework for the modeling, detection, characterization, identification, and machine-learning of anomalous behavior in observed phenomena arising from a large class of unknown and uncertain dynamical systems. An evolved behavior would in general be very difficult to correct unless the specific anomalous event that caused such behavior can be detected early, and any consequence attributed to the specific anomaly following its detection. Substantial investigative time and effort is required to back-track the cause for abnormal behavior and to recreate the event sequence leading to such abnormal behavior. The need to automatically detect anomalous behavior is therefore critical using principles of state motion, and to do so with a human operator in the loop. Human-machine interaction results in a capability for machine self-learning and in producing a robust decision-support mechanism. This is the fundamental concept of intelligent control wherein machine-learning is enhanced by interaction with human operators. C1 [Prasad, Nadipuram R.; Almanza-Garcia, Salvador] New Mexico State Univ, Las Cruces, NM 88003 USA. [Lu, Thomas T.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Prasad, NR (reprint author), New Mexico State Univ, Las Cruces, NM 88003 USA. FU Defense Threat Reduction Agency FX Work reported here was funded in part by the Defense Threat Reduction Agency under a University Associated Research Partnership Program. NR 18 TC 0 Z9 0 U1 0 U2 1 PU TECH SCIENCE PRESS PI NORCROSS PA 6825 JIMMY CARTER BLVD, STE 1850, NORCROSS, GA 30071 USA SN 1546-2218 J9 CMC-COMPUT MATER CON JI CMC-Comput. Mat. Contin. PD NOV PY 2009 VL 14 IS 1 BP 1 EP 22 PG 22 WC Engineering, Multidisciplinary; Materials Science, Multidisciplinary; Mathematics, Interdisciplinary Applications SC Engineering; Materials Science; Mathematics GA 617BA UT WOS:000279254600001 ER PT J AU McCown, F Marshall, CC Nelson, ML AF McCown, Frank Marshall, Catherine C. Nelson, Michael L. TI Why Web Sites Are Lost (and How They're Sometimes Found) SO COMMUNICATIONS OF THE ACM LA English DT Article C1 [McCown, Frank] Harding Univ, Searcy, AR 72149 USA. [Nelson, Michael L.] Old Dominion Univ, Norfolk, VA 23529 USA. [Nelson, Michael L.] NASA, Langley Res Ctr, Washington, DC 20546 USA. RP McCown, F (reprint author), Harding Univ, Searcy, AR 72149 USA. EM fmccown@harding.edu; cathymar@microsoft.com; mln@cs.odu.edu OI Nelson, Michael/0000-0003-3749-8116 NR 6 TC 3 Z9 3 U1 0 U2 0 PU ASSOC COMPUTING MACHINERY PI NEW YORK PA 2 PENN PLAZA, STE 701, NEW YORK, NY 10121-0701 USA SN 0001-0782 J9 COMMUN ACM JI Commun. ACM PD NOV PY 2009 VL 52 IS 11 BP 141 EP 145 DI 10.1145/1592761.1592794 PG 5 WC Computer Science, Hardware & Architecture; Computer Science, Software Engineering; Computer Science, Theory & Methods SC Computer Science GA 512AV UT WOS:000271215300039 ER PT J AU Jamshidi, M AF Jamshidi, Mo TI Special Issue: High Performance Computing Architectures SO COMPUTERS & ELECTRICAL ENGINEERING LA English DT Editorial Material C1 [Jamshidi, Mo] Univ Texas Syst, San Antonio, TX USA. [Jamshidi, Mo] Univ New Mexico, Ctr Autonomous Control Engn, Albuquerque, NM 87131 USA. [Jamshidi, Mo] Univ Texas San Antonio, San Antonio, TX USA. [Jamshidi, Mo] UNM, ECE, Albuquerque, NM USA. [Jamshidi, Mo] NASA, Washington, DC USA. [Jamshidi, Mo] US DOE, Washington, DC 20585 USA. RP Jamshidi, M (reprint author), Univ Texas Syst, San Antonio Campus, San Antonio, TX USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0045-7906 J9 COMPUT ELECTR ENG JI Comput. Electr. Eng. PD NOV PY 2009 VL 35 IS 6 BP III EP IV PG 2 WC Computer Science, Hardware & Architecture; Computer Science, Interdisciplinary Applications; Engineering, Electrical & Electronic SC Computer Science; Engineering GA 523YK UT WOS:000272110800001 ER PT J AU Brown, ME Hintermann, B Higgins, N AF Brown, Molly E. Hintermann, Beat Higgins, Nathaniel TI Markets, Climate Change, and Food Security in West Africa SO ENVIRONMENTAL SCIENCE & TECHNOLOGY LA English DT Article ID LAND-USE C1 [Brown, Molly E.] NASA, Goddard Space Flight Ctr, Biospher Sci Branch, Greenbelt, MD 20771 USA. [Hintermann, Beat] ETH, Ctr Energy Policy & Econ, Swiss Fed Inst Technol, Zurich, Switzerland. [Higgins, Nathaniel] Univ Maryland, Dept Agr & Resource Econ, College Pk, MD 20742 USA. RP Brown, ME (reprint author), NASA, Goddard Space Flight Ctr, Biospher Sci Branch, Greenbelt, MD 20771 USA. EM molly.brown@nasa.gov RI Brown, Molly/E-2724-2010; Brown, Molly/M-5146-2013 OI Brown, Molly/0000-0001-7384-3314; Brown, Molly/0000-0001-7384-3314 FU U.S. Agency for International Development Famine Early Warning Systems Network and through NASA [NN-H-04-Z-YO-010-C] FX This research has been made possible by data, support, and funding from the U.S. Agency for International Development Famine Early Warning Systems Network and through funding from a NASA decision support project (Cooperative Agreement Notice NN-H-04-Z-YO-010-C). NR 30 TC 30 Z9 33 U1 2 U2 17 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0013-936X J9 ENVIRON SCI TECHNOL JI Environ. Sci. Technol. PD NOV 1 PY 2009 VL 43 IS 21 BP 8016 EP 8020 DI 10.1021/es901162d PG 5 WC Engineering, Environmental; Environmental Sciences SC Engineering; Environmental Sciences & Ecology GA 510QT UT WOS:000271106300010 PM 19924916 ER PT J AU Thomas-Keprta, KL Clemett, SJ McKay, DS Gibson, EK Wentworth, SJ AF Thomas-Keprta, K. L. Clemett, S. J. McKay, D. S. Gibson, E. K. Wentworth, S. J. TI Origins of magnetite nanocrystals in Martian meteorite ALH84001 SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Review ID ALLAN HILLS 84001; CARBONATE SYSTEM CACO3-MGCO3-FECO3; ALTERNATIVE SOLUTION MODEL; SOLID-SOLUTION PRECURSORS; THERMAL-DECOMPOSITION; LOW-TEMPERATURE; CATION DIFFUSION; ORDERING MODEL; SIDERITE; SHOCK AB The Martian meteorite ALH84001 preserves evidence of interaction with aqueous fluids while on Mars in the form of microscopic carbonate disks. These carbonate disks are believed to have precipitated 3.9 Ga ago at beginning of the Noachian epoch on Mars during which both the oldest extant Martian surfaces were formed, and perhaps the earliest global oceans. Intimately associated within and throughout these carbonate disks are nanocrystal magnetites (Fe(3)O(4)) with unusual chemical and physical properties, whose origins have become the source of considerable debate. One group of hypotheses argues that these magnetites are the product of partial thermal decomposition of the host carbonate. Alternatively, the origins of magnetite and carbonate may be unrelated; that is, from the perspective of the carbonate the magnetite is allochthonous. For example, the magnetites might have already been present in the aqueous fluids from which the carbonates were believed to have been deposited. We have sought to resolve between these hypotheses through the detailed characterization of the compositional and structural relationships of the carbonate disks and associated magnetites with the orthopyroxene matrix in which they are embedded. Extensive use of focused ion beam milling techniques has been utilized for sample preparation. We then compared our observations with those from experimental thermal decomposition studies of sideritic carbonates under a range of plausible geological heating scenarios. We conclude that the vast majority of the nanocrystal magnetites present in the carbonate disks could not have formed by any of the currently proposed thermal decomposition scenarios. Instead, we find there is considerable evidence in support of an alternative allochthonous origin for the magnetite unrelated to any shock or thermal processing of the carbonates. (C) 2009 Published by Elsevier Ltd. C1 [Thomas-Keprta, K. L.; Clemett, S. J.; Wentworth, S. J.] NASA, Lyndon B Johnson Space Ctr, ESCG, Houston, TX 77058 USA. [McKay, D. S.; Gibson, E. K.] NASA, Lyndon B Johnson Space Ctr, KR, ARES, Houston, TX 77058 USA. RP Thomas-Keprta, KL (reprint author), NASA, Lyndon B Johnson Space Ctr, ESCG, Houston, TX 77058 USA. EM kathie.thomas-keprta-1@nasa.gov; simon.j.clemett@nasa.gov FU NASA Mars Fundamental FX We acknowledge support from the NASA Mars Fundamental program. We thank FEI Corporation, particularly Trisha Rice and Lucille Giannuzzi, for assistance in preparing the FIB sections of ALH84001 carbonate disks. We also acknowledge Giles Graham for assistance with preparing the Texas FIB sections. We gratefully acknowledge the support of Sean and Nathaniel Keprta and Miss B. and O. Clemett. We thank two anonymous reviewers and Christian Koeberl for suggestions that greatly improved this paper. NR 107 TC 39 Z9 42 U1 2 U2 33 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD NOV 1 PY 2009 VL 73 IS 21 BP 6631 EP 6677 DI 10.1016/j.gca.2009.05.064 PG 47 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 541LG UT WOS:000273416600012 ER PT J AU Tape, C Muse, P Simons, M Dong, D Webb, F AF Tape, Carl Muse, Pablo Simons, Mark Dong, Danan Webb, Frank TI Multiscale estimation of GPS velocity fields SO GEOPHYSICAL JOURNAL INTERNATIONAL LA English DT Article DE Wavelet transform; Satellite geodesy; Seismic cycle; Transient deformation; Kinematics of crustal and mantle deformation ID FAULT SLIP RATES; LINEAR-MODEL SELECTION; SPACE GEODETIC STRAIN; 1999 HECTOR MINE; PLATE BOUNDARY; WAVELET FRAMES; POSTSEISMIC DEFORMATION; TECTONIC DEFORMATION; SURFACE DEFORMATION; CROSS-VALIDATION AB P>We present a spherical wavelet-based multiscale approach for estimating a spatial velocity field on the sphere from a set of irregularly spaced geodetic displacement observations. Because the adopted spherical wavelets are analytically differentiable, spatial gradient tensor quantities such as dilatation rate, strain rate and rotation rate can be directly computed using the same coefficients. In a series of synthetic and real examples, we illustrate the benefit of the multiscale approach, in particular, the inherent ability of the method to localize a given deformation field in space and scale as well as to detect outliers in the set of observations. This approach has the added benefit of being able to locally match the smallest resolved process to the local spatial density of observations, thereby both maximizing the amount of derived information while also allowing the comparison of derived quantities at the same scale but in different regions. We also consider the vertical component of the velocity field in our synthetic and real examples, showing that in some cases the spatial gradients of the vertical velocity field may constitute a significant part of the deformation. This formulation may be easily applied either regionally or globally and is ideally suited as the spatial parametrization used in any automatic time-dependent geodetic transient detector. C1 [Tape, Carl; Muse, Pablo; Simons, Mark] CALTECH, Seismol Lab, Pasadena, CA 91125 USA. [Dong, Danan; Webb, Frank] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Tape, C (reprint author), CALTECH, Seismol Lab, Pasadena, CA 91125 USA. EM carltape@gps.caltech.edu RI Simons, Mark/N-4397-2015 OI Simons, Mark/0000-0003-1412-6395 FU Gordon and Betty Moore Foundation FX We are grateful to John Haines, an anonymous reviewer, and editor John Beavan for comments that improved this manuscript. We thank Jean-Philippe Avouac for helpful discussions. We acknowledge the Southern California Integrated GPS Network and its sponsors, the W. M. Keck Foundation, NASA, NSF, USGS and SCEC, for providing data used in this study. This research was supported in part by the Gordon and Betty Moore Foundation. This is Caltech Tectonic Observatory Contribution 112. NR 79 TC 19 Z9 22 U1 1 U2 10 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 NOV PY 2009 VL 179 IS 2 BP 945 EP 971 DI 10.1111/j.1365-246X.2009.04337.x PG 27 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 504XU UT WOS:000270652300019 ER PT J AU Dobrovolskis, AR AF Dobrovolskis, Anthony R. TI Insolation patterns on synchronous exoplanets with obliquity SO ICARUS LA English DT Article DE Celestial mechanics; Extrasolar planets; Resonances; Spin-orbit; Rotational dynamics ID GENERALIZED CASSINIS LAWS; LONG-TERM EVOLUTION; ATMOSPHERIC TIDES; HOT JUPITERS; MOLTEN CORE; TERRESTRIAL PLANETS; HD 209458B; VENUS; ROTATION; SPIN AB A previous paper [Dobrovolskis, A.R., 2007. Icarus 192, 1-23] showed that eccentricity can have profound effects on the climate, habitability, and detectability of extrasolar planets. This complementary study shows that obliquity can have comparable effects. The known exoplanets exhibit a wide range of orbital eccentricities, but those within several million kilometers of their suns are generally in near-circular orbits. This fact is widely attributed to the dissipation of tides in the planets. Tides in a planet affect its spin even more than its orbit, and Such tidally evolved planets often are assumed to be in synchronous rotation, so that their rotation periods are identical to their orbital periods. The canonical example of synchronous spin is the way that our Moon always keeps nearly the same hemisphere facing the Earth. Tides also tend to reduce the planet's obliquity (the angle between its spin and orbital angular velocities). However, orbit precession can cause the rotation to become locked in a "Cassim state", where it retains a nearly constant non-zero obliquity. For example, our Moon maintains an obliquity of about 6.7 degrees with respect to its orbit about the Earth. In comparison, stable Cassini states can exist for practically any obliquity up to similar to 90 degrees, or more for planets of binary stars, or in multi-planet systems with high mutual inclinations, such as are produced by scattering or by the Kozai mechanism. This work considers planets in synchronous rotation with circular orbits, but arbitrary obliquity beta; this affects the distribution of insolation over the planet's surface, particularly near its poles. For beta = 0, one hemisphere bakes in perpetual Sunshine, while the opposite hemisphere experiences eternal darkness. As beta increases, the region of permanent daylight and the antipodal realm of endless night both shrink, while a more temperate area of alternating day and night spreads in longitude, and especially in latitude. The regions of permanent day or night disappear at beta = 90 degrees. The insolation regime passes through several more transitions as beta continues to increase toward 180 degrees, but the surface distribution of insolation remains non-uniform in both latitude and longitude. Thus obliquity, like eccentricity, can protect certain areas of the planet from the worst extremes of temperature and solar radiation, and can improve the planet's habitability. These results also have implications for the direct detectability of extrasolar planets, and for the interpretation of their thermal emissions. (C) 2009 Elsevier Inc. All rights reserved. C1 245 3 NASA, Ames Res Ctr, Lick Observ, UC Santa Cruz, Moffett Field, CA 94035 USA. RP Dobrovolskis, AR (reprint author), 245 3 NASA, Ames Res Ctr, Lick Observ, UC Santa Cruz, Moffett Field, CA 94035 USA. EM dobro@cosmic.arc.nasa.gov NR 70 TC 12 Z9 12 U1 0 U2 4 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD NOV PY 2009 VL 204 IS 1 BP 1 EP 10 DI 10.1016/j.icarus.2009.06.007 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 507VT UT WOS:000270884100001 ER PT J AU Pankine, AA Tamppari, LK Smith, MD AF Pankine, Alexey A. Tamppari, Leslie K. Smith, Michael D. TI Water vapor variability in the north polar region of Mars from Viking MAWD and MGS TES datasets SO ICARUS LA English DT Article DE Mars; Mars, atmosphere; Mars, climate; Mars, polar caps ID THERMAL EMISSION SPECTROMETER; INTERANNUAL VARIABILITY; MARTIAN ATMOSPHERE; LIQUID WATER; ICE; CYCLE; CAP; BEHAVIOR; DUST; TEMPERATURES AB Atmospheric water vapor abundances in Mars' north polar region (NPR, from 60 degrees to 90 degrees N) are mapped as function of latitude and longitude for spring and summer seasons, and their spatial, seasonal, and interannual variability is discussed. Water vapor data are from Mars Global Surveyor (MGS) Thermal Emission Spectrometer (TES) and the Viking Orbiter (VO) Mars Atmospheric Water Detector (MAWD). The data cover three complete northern spring-summer seasons in 1977-1978, 2000-2001 and 2002-2003, and shorter periods of spring-summer seasons during 1975, 1999 and 2004. Long term interannual variability in the averaged NPR abundances may exist, with Viking MAWD observations showing twice as much water vapor during summer as the MGS TES observations more than 10 martian years (MY) later. While the averaged abundances are very similar in TES observations for the same season in different years, the spatial distributions in the early summer season do vary significantly year over year. Spatial and temporal variabilities increase between L(s) similar to 80-140 degrees, which may be related to vapor sublimation from the North Polar Residual Cap (NPRC), or to changes in circulation. Spatial variability is observed on scales of similar to 100 km and temporal variability is observed on scales of <10 sols during summer. During late spring the TES water vapor spatial distribution is seen to correlate with the low topography/low albedo region of northern Acidalia Planitia (270-360 degrees E), and with the dust spatial distribution across the NPR during late spring-early summer. Non-uniform vertical distribution of water vapor, a regolith source or atmospheric circulation 'pooling' of water vapor from the NPRC into the topographic depression may be behind the correlation with low topography/low albedo. Sublimation winds carrying water vapor off the NPRC and lifting surface dust in the areas surrounding the NPRC may explain the correlation between the water vapor and dust spatial distributions. Correlation between water vapor and dust in MAWD data are only observed over low topography/low albedo area. Maximum water vapor abundances are observed at L(s) = 105-115 degrees and outside of the NPRC at 75-80 degrees N; the TES data, however, do not extend over the NPRC and thus, this conclusion may be biased. Some water vapor appears to be released in plumes or 'outbursts' in the MAWD and TES datasets during late spring and early summer. We propose that the sublimation rate of ice varies across the NPRC with varying surface winds, giving rise to the observed 'outbursts' at some seasons. (C) 2009 Elsevier Inc. All rights reserved. C1 [Pankine, Alexey A.; Tamppari, Leslie K.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Smith, Michael D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Pankine, AA (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,MS 183-301, Pasadena, CA 91109 USA. EM alexey.a.pankine@jpl.nasa.gov FU Jet Propulsion Laboratory, California Institute of Technology FX This research was carried out at the Jet Propulsion Laboratory, California Institute of Technology and funded through the Research and Technology Development Fund program. We thank the anonymous reviewer and Prof. Bruce Jakosky for helpful suggestions in improving the manuscript. NR 54 TC 7 Z9 7 U1 0 U2 0 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 J9 ICARUS JI Icarus PD NOV PY 2009 VL 204 IS 1 BP 87 EP 102 DI 10.1016/j.icarus.2009.06.009 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 507VT UT WOS:000270884100007 ER PT J AU Veeder, GJ Davies, AG Matson, DL Johnson, TV AF Veeder, Glenn J. Davies, Ashley Gerard Matson, Dennis L. Johnson, Torrence V. TI Io: Heat flow from dark volcanic fields SO ICARUS LA English DT Review DE Io; Volcanism; Jupiter, Satellites ID INFRARED MAPPING SPECTROMETER; GALILEO PHOTOPOLARIMETER-RADIOMETER; JUPITERS MOON IO; HOT-SPOTS; THERMAL EMISSION; LAVA FLOWS; TIDAL DISSIPATION; ACTIVE VOLCANISM; IMAGING DATA; NIMS DATA AB Dark flow fields on the jovian satellite Io are evidence of current or recent volcanic activity. We have examined the darkest volcanic fields and quantified their thermal emission in order to assess their contribution to Io's total heat flow. Loki Patera, the largest single source of heat flow on Io, is a convenient point of reference. We find that dark volcanic fields are more common in the hemisphere opposite Loki Patera and this large scale concentration is manifested as a maximum in the longitudinal distribution (near similar to 200 degrees W), consistent with USGS global geologic mapping results. In spite of their relatively cool temperatures, dark volcanic fields contribute almost as much to Io's heat flow as Loki Patera itself because of their larger areal extent. As a group, dark volcanic fields provide an asymmetric component of similar to 5% of Io's global heat flow or similar to 5 x 10(12) W. (C) 2009 Elsevier Inc. All rights reserved. C1 [Veeder, Glenn J.; Davies, Ashley Gerard; Matson, Dennis L.; Johnson, Torrence V.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Veeder, GJ (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Glenn.Veeder@jpl.nasa.gov FU Jet Propulsion Laboratory, California Institute of Technology; NASA PGG; NASA OPR FX This work was carried out at the jet Propulsion Laboratory, California Institute of Technology, under contract to NASA. GJV and DLM are supported by a grant from the NASA PG&G program. AGD is supported by a grant from the NASA OPR program. We thank Dr. D.A. Williams and an anonymous reviewer for helpful comments on the manuscript. NR 105 TC 12 Z9 12 U1 2 U2 3 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 J9 ICARUS JI Icarus PD NOV PY 2009 VL 204 IS 1 BP 239 EP 253 DI 10.1016/j.icarus.2009.06.027 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 507VT UT WOS:000270884100017 ER PT J AU Chien, S Silverman, D Davies, AG Mandl, D AF Chien, Steve Silverman, Dorothy Davies, Ashley Gerard Mandl, Daniel TI Onboard Science Processing Concepts for the HyspIRI Mission SO IEEE INTELLIGENT SYSTEMS LA English DT Editorial Material ID VOLCANISM; HYPERION; MODIS; EO-1 C1 [Chien, Steve; Silverman, Dorothy] CALTECH, Jet Prop Lab, Artificial Intelligence Grp, Pasadena, CA 91125 USA. RP Chien, S (reprint author), CALTECH, Jet Prop Lab, Artificial Intelligence Grp, Pasadena, CA 91125 USA. EM steve.chien@jpl.nasa.gov; dotsspot@gmail.com; ashley.davies@jpl.nasa.gov; daniel.mandl@gsfc.nasa.gov NR 18 TC 16 Z9 16 U1 1 U2 5 PU IEEE COMPUTER SOC PI LOS ALAMITOS PA 10662 LOS VAQUEROS CIRCLE, PO BOX 3014, LOS ALAMITOS, CA 90720-1314 USA SN 1541-1672 J9 IEEE INTELL SYST JI IEEE Intell. Syst. PD NOV-DEC PY 2009 VL 24 IS 6 BP 12 EP 19 PG 8 WC Computer Science, Artificial Intelligence; Engineering, Electrical & Electronic SC Computer Science; Engineering GA 529JL UT WOS:000272511900003 ER PT J AU Wilson, WC Malocha, DC Kozlovski, N Gallagher, DR Fisher, B Pavlina, J Saldanha, N Puccio, D Atkinson, GM AF Wilson, W. C. Malocha, D. C. Kozlovski, N. Gallagher, D. R. Fisher, B. Pavlina, J. Saldanha, N. Puccio, D. Atkinson, G. M. TI Orthogonal Frequency Coded SAW Sensors for Aerospace SHM Applications SO IEEE SENSORS JOURNAL LA English DT Article DE Orthogonal frequency code (OFC); structural health monitoring; surface acoustic wave (SAW) detector AB National Aeronautics and Space Administration (NASA) aeronautical programs require structural health monitoring (SHM) to ensure the safety of the crew and the vehicles. Future SHM sensors need to be small, lightweight, inexpensive, and wireless. Orthogonal frequency coded (OFC) surface acoustic wave (SAW) reflectors and transducers have been recently introduced for use in communication, as well as in sensor and radio-frequency identification (RFID) tag applications (Malocha et al., 2004, Puccio et al., 2004). The OFC SAW technology approach has been investigated by NASA for possible inclusion in ground, space flight, and space exploration sensor applications. In general, SAW technology has advantages over other potentially competitive technologies, because the devices can operate in ranges from cryogenic to furnace temperature. SAW devices can also be small, rugged, passive, wireless, and radiation hard and can operate with variable frequency and bandwidth. SAW sensor embodiments can provide onboard device sensor integration or can provide integration with an external sensor that uses the SAW device for encoding the sensor information and transmission to the receiver. SAW OFC device technology can provide RFID tags and sensors with low loss, large operating temperatures, and a multiuse sensor platform. This paper will discuss the key parameters for OFC device design, which includes reflector and transducer design, coding diversity approaches, and insertion loss considerations. Examples of several OFC device sensors and RFID tags are presented to show the current state-of-the-art performance for several NASA applications. Projections for future sensor and RFID tag platform performance are discussed, along with some of the current challenges and issues of the technology. C1 [Wilson, W. C.] Virginia Commonwealth Univ, Richmond, VA 23298 USA. [Wilson, W. C.] NASA, Langley Res Ctr, Hampton, VA 23681 USA. [Malocha, D. C.; Kozlovski, N.; Gallagher, D. R.; Fisher, B.; Pavlina, J.; Saldanha, N.] Univ Cent Florida, Orlando, FL 32816 USA. [Puccio, D.] Quartzdyne Inc, Salt Lake City, UT 84123 USA. [Atkinson, G. M.] Virginia Commonwealth Univ, Richmond, VA 23284 USA. RP Wilson, WC (reprint author), Virginia Commonwealth Univ, Med Coll Virginia Campus, Richmond, VA 23298 USA. EM William.C.Wilson@nasa.gov FU National Aeronautics and Space Administration (NASA) Graduate Student Research Program Fellowships [NNK04OA28C, NNK05OB31C, NNK06OM24C]; University of Central Florida-Florida Solar Energy Center; Mnemonics Corporation; Aeronautics Research Mission Directorate FX This work was supported in part by the National Aeronautics and Space Administration (NASA) Graduate Student Research Program Fellowships, in part by the University of Central Florida-Florida Solar Energy Center, in part by the NASA Small Business Technology Transfer (STTR) Phase I under Contract NNK04OA28C, in part by the NASA contracts and industrial collaboration with Applied Sensor Research and Development Corporation, Phase II STTR under Contract NNK05OB31C, Contract NNK06OM24C, and Contract NNK06OM24C, in part by the Mnemonics Corporation, and in part by the NASA Integrated Vehicle Heath Management Project, which is part of the Aviation Safety Program under the Aeronautics Research Mission Directorate. NR 28 TC 23 Z9 24 U1 0 U2 12 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1530-437X EI 1558-1748 J9 IEEE SENS J JI IEEE Sens. J. PD NOV PY 2009 VL 9 IS 11 BP 1546 EP 1556 DI 10.1109/JSEN.2009.2027403 PG 11 WC Engineering, Electrical & Electronic; Instruments & Instrumentation; Physics, Applied SC Engineering; Instruments & Instrumentation; Physics GA 503PB UT WOS:000270548800006 ER PT J AU Wolf, MT Burdick, JW AF Wolf, Michael T. Burdick, Joel W. TI A Bayesian Clustering Method for Tracking Neural Signals Over Successive Intervals SO IEEE TRANSACTIONS ON BIOMEDICAL ENGINEERING LA English DT Article DE Bayesian classification; clustering; expectation-maximization (EM); multitarget tracking; neuron tracking; spike sorting ID ACTION-POTENTIALS; CONTROL ALGORITHM; SPIKE DETECTION; REAL-TIME; CLASSIFICATION; RECORDINGS AB This paper introduces a new, unsupervised method for sorting and tracking the action potentials of individual neurons in multiunit extracellular recordings. Presuming the data are divided into short, sequential recording intervals, the core of our strategy relies upon an extension of a traditional mixture model approach that incorporates clustering results from the preceding interval in a Bayesian manner, while still allowing for signal nonstationarity and changing numbers of recorded neurons. As a natural byproduct of the sorting method, current and prior signal clusters can be matched over time in order to track persisting neurons. We also develop techniques to use prior data to appropriately seed the clustering algorithm and select the model class. We present results in a principal components space; however, the algorithm may be applied in any feature space where the distribution of a neuron's spikes may be modeled as Gaussian. Applications of this signal classification method to recordings from macaque parietal cortex show that it provides significantly more consistent clustering and tracking results than traditional methods based on expectation-maximization optimization of mixture models. This consistent tracking ability is crucial for intended applications of the method. C1 [Wolf, Michael T.; Burdick, Joel W.] CALTECH, Div Engn & Appl Sci, Pasadena, CA 91125 USA. RP Wolf, MT (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM wolf@jpl.nasa.gov; jwb@robotics.caltech.edu FU NEI NIH HHS [R01 EY015545] NR 30 TC 7 Z9 7 U1 0 U2 1 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 0018-9294 J9 IEEE T BIO-MED ENG JI IEEE Trans. Biomed. Eng. PD NOV PY 2009 VL 56 IS 11 BP 2649 EP 2659 DI 10.1109/TBME.2009.2027604 PG 11 WC Engineering, Biomedical SC Engineering GA 511BV UT WOS:000271139800012 PM 19643700 ER PT J AU Truong-Loi, ML Freeman, A Dubois-Fernandez, PC Pottier, E AF Truong-Loi, My-Linh Freeman, Anthony Dubois-Fernandez, Pascale C. Pottier, Eric TI Estimation of Soil Moisture and Faraday Rotation From Bare Surfaces Using Compact Polarimetry SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article; Proceedings Paper CT IEEE International Geoscience and Remote Sensing Symposium (IGARSS 2008) CY JUL 06-11, 2008 CL Boston, MA SP IEEE, IEEE Geosci & Remote Sensing Soc DE Bare soil surfaces; compact polarimetry (CP); Faraday rotation (FR); soil moisture ID SAR DATA; SYMMETRY PROPERTIES; SPACEBORNE SAR; CALIBRATION; RADAR; CLASSIFICATION; BEHAVIOR AB The potential of compact polarimetry (CP) mode at longer wavelengths in a space environment for surface parameter estimation is investigated. CP consists of transmitting a single polarization while receiving two polarizations. At longer wavelengths, one of the main challenges associated with CP from space is Faraday rotation (FR) estimation and correction. In this paper, an estimation procedure for FR is presented, which relies on the scattering properties of bare surfaces. The selection of the bare surfaces is based on a new parameter, the conformity coefficient computed from CP measurements. This parameter is shown to be FR invariant. Once estimated, the FR can be corrected over the whole image. A simple approximation to sigma(o)(HH) and sigma(o)(VV) based on CP measurements over bare soil surfaces is presented, from which soil moisture can be estimated using the 1995 Dubois et al. algorithm. The results obtained using CP are shown to be in good agreement with those obtained from the standard Dubois et al. algorithm using fully polarimetric data. This implies that, for soil moisture, CP can be used instead of HH and VV dual-polarized measurements. C1 [Truong-Loi, My-Linh; Dubois-Fernandez, Pascale C.] Off Natl Etud & Rech Aerosp, DEMR, F-13661 Salon De Provence, France. [Truong-Loi, My-Linh; Pottier, Eric] Univ Rennes 1, Inst Elect & Telecommun Rennes, F-35065 Rennes, France. [Truong-Loi, My-Linh] Ctr Natl Etud Spatiales, F-31401 Toulouse, France. [Freeman, Anthony] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Truong-Loi, ML (reprint author), Off Natl Etud & Rech Aerosp, DEMR, F-13661 Salon De Provence, France. EM My-Linh.Truong-Loi@onera.fr RI Dubois-Fernandez, Pascale/A-6743-2012 NR 19 TC 35 Z9 37 U1 2 U2 9 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 0196-2892 J9 IEEE T GEOSCI REMOTE JI IEEE Trans. Geosci. Remote Sensing PD NOV PY 2009 VL 47 IS 11 BP 3608 EP 3615 DI 10.1109/TGRS.2009.2031428 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 511CB UT WOS:000271140400002 ER PT J AU Yurchak, BS AF Yurchak, Boris S. TI Radar Volume Backscatter From Spatially Extended Geophysical Targets in a "Slice" Approach SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article; Proceedings Paper CT IEEE International Geoscience and Remote Sensing Symposium (IGARSS 2008) CY JUL 06-11, 2008 CL Boston, MA SP IEEE, IEEE Geosci & Remote Sensing Soc DE Radar scattering; remote sensing ID COHERENT SCATTERING; CLOUD; PARTICLES; SNOW; DISTRIBUTIONS AB This paper presents an assessment of the radar backscatter from a spatially extended geophysical target (SEGT) based on a semiempirical (SE) model. An SEGT is any geophysical object that is at least semitransparent to radar illumination (clouds, rain, snowfall in the atmosphere, thick snow cover of the ground). The existing SE model does not take into account the statistical properties of the SEGT's media. To improve the SE model, a so-called "slice" approach is applied. In this approach, the particles located close to the wavefront of the radar illumination are assumed to produce backscatter that is mainly coherent. This method allows the contribution of the microphysical parameters of the scattering media to the volume component of the radar cross section to be described more comprehensively than the SE model based on the incoherent approach. It is shown that the slice concept results in the original SE model in the particular case when the particle number fluctuation within the slices pertains to the Poisson law. C1 Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Yurchak, BS (reprint author), Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM boris.s.yurchak@nasa.gov NR 41 TC 2 Z9 2 U1 0 U2 2 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 0196-2892 J9 IEEE T GEOSCI REMOTE JI IEEE Trans. Geosci. Remote Sensing PD NOV PY 2009 VL 47 IS 11 BP 3690 EP 3696 DI 10.1109/TGRS.2009.2015444 PG 7 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA 511CB UT WOS:000271140400011 ER PT J AU Padmanabhan, S Reising, SC Vivekanandan, J Iturbide-Sanchez, F AF Padmanabhan, Sharmila Reising, Steven C. Vivekanandan, Jothiram Iturbide-Sanchez, Flavio TI Retrieval of Atmospheric Water Vapor Density With Fine Spatial Resolution Using Three-Dimensional Tomographic Inversion of Microwave Brightness Temperatures Measured by a Network of Scanning Compact Radiometers SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article; Proceedings Paper CT IEEE International Geoscience and Remote Sensing Symposium (IGARSS 2008) CY JUL 06-11, 2008 CL Boston, MA SP IEEE, IEEE Geosci & Remote Sensing Soc DE Atmospheric measurement; electromagnetic tomography; humidity measurement; microwave radiometry; remote sensing; water vapor ID ABSORPTION; PROFILES; VARIABILITY; IMPACT; LIDAR; BIAS AB Quantitative precipitation forecasting is currently limited by the paucity of observations on sufficiently fine temporal and spatial scales. Three-dimensional water vapor fields can be retrieved with improved spatial coverage from measurements obtained using a network of scanning microwave radiometers. To investigate this potential, an observation system simulation experiment was performed in which synthetic examples of retrievals using a network of radiometers were compared with results from the Weather Research and Forecasting model at a grid scale of 500 m. These comparisons show that the 3-D water vapor field can be retrieved with an accuracy of better than 15%-20%. A ground-based demonstration network of three compact microwave radiometers was deployed at the Atmospheric Radiation Measurement Southern Great Plains site in Oklahoma. Results using these network measurements demonstrated the first retrieval of the 3-D water vapor field in the troposphere at fine spatial and temporal resolutions. C1 [Padmanabhan, Sharmila; Reising, Steven C.; Iturbide-Sanchez, Flavio] Colorado State Univ, Microwave Syst Lab, Dept Elect & Comp Engn, Ft Collins, CO 80523 USA. [Vivekanandan, Jothiram] Natl Ctr Atmospher Res, Earth Observing Lab, Boulder, CO 80301 USA. RP Padmanabhan, S (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. EM sharmila.padmanabhan@jpl.nasa.gov; Steven.Reising@ColoState.edu; vivek@ucar.edu; Flavio.Iturbide@noaa.gov RI Iturbide-Sanchez, Flavio/F-9186-2014 OI Iturbide-Sanchez, Flavio/0000-0002-8539-0073 NR 43 TC 16 Z9 16 U1 0 U2 2 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 0196-2892 J9 IEEE T GEOSCI REMOTE JI IEEE Trans. Geosci. Remote Sensing PD NOV PY 2009 VL 47 IS 11 BP 3708 EP 3721 DI 10.1109/TGRS.2009.2031107 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 511CB UT WOS:000271140400013 ER PT J AU Lim, BH Ruf, CS AF Lim, Boon H. Ruf, Christopher S. TI A High-Resolution Full-Earth Disk Model for Evaluating Synthetic Aperture Passive Microwave Observations From GEO SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article; Proceedings Paper CT IEEE International Geoscience and Remote Sensing Symposium (IGARSS 2008) CY JUL 06-11, 2008 CL Boston, MA SP IEEE, IEEE Geosci & Remote Sensing Soc DE Microwave radiometry; remote sensing; synthetic aperture imaging ID RADIOMETERS; ARRAY; PRECIPITATION; CALIBRATION; EMISSIVITY; CHANNELS; WATER; LAND AB A proposed instrument for deployment on next-generation Geostationary Operational Environmental Satellite (GOES) platforms is the Geostationary Synthetic Thinned Aperture Radiometer (GeoSTAR). A high-resolution full-Earth disk model has been developed to aid in the design of the instrument and to characterize sensor performance. A number of ancillary geophysical data fields are used as inputs into a radiative-transfer model that also accounts for the propagation and viewing geometries from a geostationary Earth orbit (GEO). The model produces high-resolution (10 km x 10 km) simulated full-Earth disk microwave images from GEO. The model is used as a tool to examine several critical aspects of GeoSTAR performance and design. Differential image processing is assessed as a means of mitigating the effects of the Gibbs phenomenon; its performance is found to be excellent, even with nonideal a priori information. The spatial resolution and precision of images generated at 50 GHz are evaluated. The magnitude of the highest spatial-frequency components sampled by GeoSTAR is found to be well above its minimum detectable signal. However, the differential image processing removes most of the high-frequency content, which is due to static high-contrast boundaries in the scene. Most of the residual high-frequency content lies at or below the instrument noise floor. C1 [Lim, Boon H.] NASA, Jet Prop Lab, Instrument Syst Implementat & Concepts Sect, Pasadena, CA 91109 USA. [Ruf, Christopher S.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Coll Engn, Ann Arbor, MI 48109 USA. RP Lim, BH (reprint author), NASA, Jet Prop Lab, Instrument Syst Implementat & Concepts Sect, Pasadena, CA 91109 USA. EM boon.h.lim@jpl.nasa.gov; cruf@umich.edu RI Ruf, Christopher/I-9463-2012 NR 33 TC 4 Z9 4 U1 0 U2 3 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 0196-2892 J9 IEEE T GEOSCI REMOTE JI IEEE Trans. Geosci. Remote Sensing PD NOV PY 2009 VL 47 IS 11 BP 3731 EP 3741 DI 10.1109/TGRS.2009.2031172 PG 11 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA 511CB UT WOS:000271140400015 ER PT J AU Misra, S Mohammed, PN Guner, B Ruf, CS Piepmeier, JR Johnson, JT AF Misra, Sidharth Mohammed, Priscilla N. Guener, Baris Ruf, Christopher S. Piepmeier, Jeffrey R. Johnson, Joel T. TI Microwave Radiometer Radio-Frequency Interference Detection Algorithms: A Comparative Study SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article; Proceedings Paper CT IEEE International Geoscience and Remote Sensing Symposium (IGARSS 2008) CY JUL 06-11, 2008 CL Boston, MA SP IEEE, IEEE Geosci & Remote Sensing Soc DE Detectors; noise measurement; radiometry; radio spectrum management; remote sensing ID MITIGATION; RFI; KURTOSIS; LAND; SEA AB Two algorithms used in microwave radiometry for radio-frequency interference (RFI) detection and mitigation are the pulse detection algorithm and the kurtosis detection algorithm. The relative performance of the algorithms is compared both analytically and empirically. Their probabilities of false alarm under RFI-free conditions and of detection when RFI is present are examined. The downlink data rate required to implement each algorithm in a spaceborne application is also considered. The kurtosis algorithm is compared to a pulse detection algorithm operating under optimal RFI detection conditions. The performance of both algorithms is also analyzed as a function of varying characteristics of the RFI. The RFI detection probabilities of both algorithms under varying subsampling conditions are compared and validated using data obtained from a field campaign. Implementation details, resource usage, and postprocessing requirements are also addressed for both algorithms. C1 [Misra, Sidharth; Ruf, Christopher S.] Univ Michigan, Space Phys Res Lab, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. [Mohammed, Priscilla N.; Piepmeier, Jeffrey R.] NASA, Goddard Space Flight Ctr, Microwave Instrument Technol Branch, Greenbelt, MD 20771 USA. [Mohammed, Priscilla N.] Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21250 USA. [Guener, Baris] Halliburton Energy Serv, Houston, TX 77032 USA. [Johnson, Joel T.] Ohio State Univ, Electrosci Lab, Dept Elect & Comp Engn, Columbus, OH 43210 USA. RP Misra, S (reprint author), Univ Michigan, Space Phys Res Lab, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. EM cruf@umich.edu RI Ruf, Christopher/I-9463-2012 NR 25 TC 34 Z9 35 U1 0 U2 2 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 0196-2892 J9 IEEE T GEOSCI REMOTE JI IEEE Trans. Geosci. Remote Sensing PD NOV PY 2009 VL 47 IS 11 BP 3742 EP 3754 DI 10.1109/TGRS.2009.2031104 PG 13 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA 511CB UT WOS:000271140400016 ER PT J AU Ruan, S Zhou, YK Yu, FL Pattipati, KR Willett, P Patterson-Hine, A AF Ruan, Sui Zhou, Yunkai Yu, Feili Pattipati, Krishna R. Willett, Peter Patterson-Hine, Ann TI Dynamic Multiple-Fault Diagnosis With Imperfect Tests SO IEEE TRANSACTIONS ON SYSTEMS MAN AND CYBERNETICS PART A-SYSTEMS AND HUMANS LA English DT Article DE Approximate Bayesian revision; determinisitic simulated annealing; dynamic fault diagnosis; functional HMMMs; hidden Markov models (HMMs); Lagrangian relaxation; multiple faults ID UNRELIABLE TESTS; ALGORITHMS; SYSTEMS AB In this paper, we consider a model for the dynamic multiple-fault diagnosis (DMFD) problem arising in online monitoring of complex systems and present a solution. This problem involves real-time inference of the most likely set of faults and their time-evolution based on blocks of unreliable test outcomes over time. In the DMFD problem, there is a finite set of mutually independent fault states, and a finite set of sensors (tests) is used to monitor their status. We model the dependence of test outcomes on the fault states via the traditional D-matrix (fault dictionary). The tests are imperfect in the sense that they can have missed detections, false alarms, or may be available asynchronously. Based on the imperfect observations over time, the problem is to identify the most likely evolution of fault states over time. The DMFD problem is an intractable NP-hard combinatorial optimization problem. Consequently, we decompose the DMFD problem into a series of decoupled subproblems, one for each sample epoch. For a single-epoch MFD, we develop a fast and high-quality deterministic simulated annealing method. Based on the sequential inferences, a local search-and-update scheme is applied to further improve the solution. Finally, we discuss how the method can be extended to dependent faults. C1 [Ruan, Sui; Yu, Feili; Pattipati, Krishna R.; Willett, Peter] Univ Connecticut, Dept Elect & Comp Engn, Storrs, CT 06269 USA. [Zhou, Yunkai] So Methodist Univ, Dept Math, Dallas, TX 75275 USA. [Patterson-Hine, Ann] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Ruan, S (reprint author), Amer Airlines Inc, Dept Revenue Management & Planning, Ft Worth, TX 76155 USA. EM yzhou@smu.edu; yu02001@engr.uconn.edu; krishna@engr.uconn.edu; willett@engr.uconn.edu; apatterson-hine@mail.arc.nasa.gov OI Willett, Peter/0000-0001-8443-5586 FU Office of Naval Research [00014-00-1-0101, N00014-06-1-0080]; NASA Ames Research Center [NAG2-1635] FX This work was supported in part by the Office of Naval Research under Contract 00014-00-1-0101 and N00014-06-1-0080 and in part by the NASA Ames Research Center under Contract NAG2-1635. This paper was recommended by Associate Editor H. Pham. NR 26 TC 13 Z9 19 U1 1 U2 8 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 1083-4427 J9 IEEE T SYST MAN CY A JI IEEE Trans. Syst. Man Cybern. Paart A-Syst. Hum. PD NOV PY 2009 VL 39 IS 6 BP 1224 EP 1236 DI 10.1109/TSMCA.2009.2025572 PG 13 WC Computer Science, Cybernetics; Computer Science, Theory & Methods SC Computer Science GA 508QI UT WOS:000270947600008 ER PT J AU Oza, N Castle, JP Stutz, J AF Oza, Nikunj Castle, J. Patrick Stutz, John TI Classification of Aeronautics System Health and Safety Documents SO IEEE TRANSACTIONS ON SYSTEMS MAN AND CYBERNETICS PART C-APPLICATIONS AND REVIEWS LA English DT Article DE Nonnegative matrix factorization (NMF); support vector machines (SVMs); text classification ID NONNEGATIVE MATRIX FACTORIZATION AB Most complex aerospace systems have many text reports on safety, maintenance, and associated issues. The Aviation Safety Reporting System (ASRS) spans several decades and contains over 700 000 reports. The Aviation Safety Action Plan (ASAP) contains over 12 000 reports from various airlines. Problem categorizations have been developed for both ASRS and ASAP to enable identification of system problems. However, repository volume and complexity make human analysis difficult. Multiple experts are needed, and they often disagree on classifications. Even the same person has classified the same document differently at different times due to evolving experiences. Consistent classification is necessary to support tracking trends in problem categories over time. A decision support system that performs consistent document classification quickly and over large repositories would be useful. We discuss the results of two algorithms we have developed to classify ASRS and ASAP documents. The first is Mariana-a support vector machine (SVM) with simulated annealing, which is used to optimize hyperparameters for the model. The second method is classification built on top of nonnegative matrix factorization (NMF), which attempts to find a model that represents document features that add up in various combinations to form documents. We tested both methods on ASRS and ASAP documents with the latter categorized two different ways. We illustrate the potential of NMF to provide document features that are interpretable and indicative of topics. We also briefly discuss the tool that we have incorporated Mariana into in order to allow human experts to provide feedback on the document categorizations. C1 [Oza, Nikunj; Stutz, John] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Castle, J. Patrick] Mission Control Technol, Moffett Field, CA 94035 USA. RP Oza, N (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM nikunj.c.oza@nasa.gov; john.c.stutz@nasa.gov NR 20 TC 13 Z9 14 U1 2 U2 5 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 1094-6977 J9 IEEE T SYST MAN CY C JI IEEE Trans. Syst. Man Cybern. Part C-Appl. Rev. PD NOV PY 2009 VL 39 IS 6 BP 670 EP 680 DI 10.1109/TSMCC.2009.2020788 PG 11 WC Computer Science, Artificial Intelligence; Computer Science, Cybernetics; Computer Science, Interdisciplinary Applications SC Computer Science GA 506FZ UT WOS:000270761100007 ER PT J AU Sherrit, S Lamberti, N Pappalardo, M AF Sherrit, Stewart Lamberti, Nicola Pappalardo, Massimo TI Comment on "The Use of Real or Complex Coupling Coefficients for Lossy Piezoelectric Materials" SO IEEE TRANSACTIONS ON ULTRASONICS FERROELECTRICS AND FREQUENCY CONTROL LA English DT Article DE Couplings; Materials; Equations; Mathematical model; Permittivity; Frequency domain analysis; Data mining AB We show that the claims of a recent paper on coupling which states that the complex coupling has mathematical difficulties and is inconsistent with a specific experiment are incorrect. C1 [Sherrit, Stewart] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Lamberti, Nicola] Univ Salerno, Dipartimento Ingn Informaz & Ingn Elettr, Fisciano, Italy. [Pappalardo, Massimo] Univ Roma III, Dept Elect Engn, Rome, Italy. RP Sherrit, S (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. EM ssherrit@jpl.nasa.gov OI Lamberti, Nicola/0000-0002-0972-7084 FU National Aeronautics and Space Administration FX The research described in this publication was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration NR 9 TC 0 Z9 0 U1 0 U2 2 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 0885-3010 J9 IEEE T ULTRASON FERR JI IEEE Trans. Ultrason. Ferroelectr. Freq. Control PD NOV PY 2009 VL 56 IS 11 BP 2334 EP 2336 DI 10.1109/TUFFC.2009.1320 PG 3 WC Acoustics; Engineering, Electrical & Electronic SC Acoustics; Engineering GA 515NJ UT WOS:000271478600001 PM 19942519 ER PT J AU Gunapala, SD Liu, HC Razeghi, M AF Gunapala, S. D. Liu, H. C. Razeghi, M. TI PROCEEDINGS OF THE INTERNATIONAL CONFERENCE ON QUANTUM STRUCTURE INFRARED PHOTODETECTORS (QSIP) 2009 Preface SO INFRARED PHYSICS & TECHNOLOGY LA English DT Editorial Material C1 [Gunapala, S. D.] CALTECH, NASA, Jet Prop Lab, Pasadena, CA 91109 USA. RP Gunapala, SD (reprint author), CALTECH, NASA, Jet Prop Lab, M-S 302-306,4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM sarath.d.gunapala@jpl.nasa.gov NR 0 TC 0 Z9 0 U1 0 U2 2 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 1350-4495 J9 INFRARED PHYS TECHN JI Infrared Phys. Technol. PD NOV PY 2009 VL 52 IS 6 BP 215 EP 215 DI 10.1016/j.infrared.2009.05.039 PG 1 WC Instruments & Instrumentation; Optics; Physics, Applied SC Instruments & Instrumentation; Optics; Physics GA 539GB UT WOS:000273240700001 ER PT J AU Wilson, DW AF Wilson, Daniel W. TI Electromagnetic modeling of multi-wavelength QWIP optical coupling structures SO INFRARED PHYSICS & TECHNOLOGY LA English DT Article; Proceedings Paper CT International Conference on Quantum Structure Infrared Photodetector CY JAN 18-23, 2009 CL Yosemite, CA SP NASA, Jet Propuls Lab, NASA, AF Res Lab, NASA, Army Res Lab, NASA, Defense Adv Res Projects Agcy, NASA, Missile Defense Agcy, Calif Inst Technol, Georgia Inst Technol, FLIR, QWIPT Technol, QmagiQ Wafer Technol DE Quantum-well infrared photodetectors; Finite-element modeling; Electromagnetic modeling ID WELL INFRARED PHOTODETECTORS; QUASI-RANDOM GRATINGS; WAVE ANALYSIS; ARRAY; IMPLEMENTATION; DETECTORS AB Quantum-well infrared photodetector (QWIP) materials can be engineered to be optically absorbing over a wide range of wavelengths. This enables multi-band focal plane arrays to be realized. However, some of this flexibility is lost due to the required optical coupling structure that converts normally incident light to horizontal propagation to allow absorption. Such coupling structures are typically strongly wavelength-dependent and must be tuned to the waveband of interest. In this study, we perform electromagnetic simulations to understand and optimize optical coupling structures for multi-band QWIPs. (C) 2009 Elsevier B.V. All rights reserved. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Wilson, DW (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM daniel.w.wilson@jpl.nasa.gov NR 20 TC 5 Z9 5 U1 3 U2 6 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 1350-4495 EI 1879-0275 J9 INFRARED PHYS TECHN JI Infrared Phys. Technol. PD NOV PY 2009 VL 52 IS 6 BP 224 EP 228 DI 10.1016/j.infrared.2009.05.030 PG 5 WC Instruments & Instrumentation; Optics; Physics, Applied SC Instruments & Instrumentation; Optics; Physics GA 539GB UT WOS:000273240700003 ER PT J AU Ting, DZY Bandara, SV Mumolo, J Keo, SA Nguyen, J Liu, HC Song, CY Chang, YC Rafol, SB Hill, CJ Gunapala, SD Soibel, A Liu, JK Blazejewski, E AF Ting, David Z. -Y. Bandara, Sumith V. Mumolo, Jason Keo, Sam A. Nguyen, Jean Liu, H. C. Song, C. Y. Chang, Yia-Chung Rafol, Sir B. Hill, Cory J. Gunapala, Sarath D. Soibel, Alexander Liu, John K. Blazejewski, Edward TI Dots, QWISPs, and BIRDs SO INFRARED PHYSICS & TECHNOLOGY LA English DT Article; Proceedings Paper CT International Conference on Quantum Structure Infrared Photodetector CY JAN 18-23, 2009 CL Yosemite, CA SP NASA, Jet Propuls Lab, NASA, AF Res Lab, NASA, Army Res Lab, NASA, Defense Adv Res Projects Agcy, NASA, Missile Defense Agcy, Calif Inst Technol, Georgia Inst Technol, FLIR, QWIPT Technol, QmagiQ Wafer Technol DE Infrared detector; Quantum well; Quantum dot; QWIP; Superlattice ID INFRARED PHOTODETECTORS; RESPONSIVITY; DETECTORS; ISLANDS; ARRAYS AB We report work on several quantum structure based infrared detectors. We describe the concept of the submonolayer quantum dot based infrared photodetectors, report device results, and present imaging results from a megapixel focal plane array. We describe the concept and experimental progress of the quantum well intra-subband photodetector (QWISP), which is closely related to the quantum well infrared photodetector (QWIP), but uses the dopant-assisted intra-subband absorption mechanism in quantum wells for normal-incidence far infrared/terahertz radiation detection. We discuss aspects of superlattice heterostructure based barrier infrared detectors (BIRDs). (C) 2009 Elsevier B.V. All rights reserved. C1 [Ting, David Z. -Y.; Bandara, Sumith V.; Mumolo, Jason; Keo, Sam A.; Nguyen, Jean; Hill, Cory J.; Gunapala, Sarath D.; Soibel, Alexander; Liu, John K.; Blazejewski, Edward] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Liu, H. C.; Song, C. Y.] CNR, Inst Microstruct Sci, Ottawa, ON K1A 0R6, Canada. [Chang, Yia-Chung] U Illinois Urbana Champaign, Dept Phys, Urbana, IL 61801 USA. [Rafol, Sir B.] Infravis Syst, Altadena, CA 91001 USA. RP Ting, DZY (reprint author), CALTECH, Jet Prop Lab, M-S 302-231,4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM David.Z.Ting@jpl.nasa.gov RI Chang, Yia-Chung/F-4239-2011; Soibel, Alexander/A-1313-2007 NR 33 TC 10 Z9 11 U1 1 U2 10 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 1350-4495 J9 INFRARED PHYS TECHN JI Infrared Phys. Technol. PD NOV PY 2009 VL 52 IS 6 BP 294 EP 298 DI 10.1016/j.infrared.2009.05.020 PG 5 WC Instruments & Instrumentation; Optics; Physics, Applied SC Instruments & Instrumentation; Optics; Physics GA 539GB UT WOS:000273240700018 ER PT J AU Rhiger, DR Kvaas, RE Harris, SF Hill, CJ AF Rhiger, David R. Kvaas, Robert E. Harris, Sean F. Hill, Cory J. TI Characterization of LWIR diodes on InAs/GaSb Type-II superlattice material SO INFRARED PHYSICS & TECHNOLOGY LA English DT Article; Proceedings Paper CT International Conference on Quantum Structure Infrared Photodetector CY JAN 18-23, 2009 CL Yosemite, CA SP NASA, Jet Propuls Lab, NASA, AF Res Lab, NASA, Army Res Lab, NASA, Defense Adv Res Projects Agcy, NASA, Missile Defense Agcy, Calif Inst Technol, Georgia Inst Technol, FLIR, QWIPT Technol, QmagiQ Wafer Technol DE Superlattices; Infrared detectors; Surface passivation; Carrier lifetime ID GAAS AB Long wavelength infrared (LWIR) focal plane arrays (FPAs) built on Type-II strained layer InAs/GaSb superlattice materials are emerging as an alternative to LWIR HgCdTe. We have made progress in the development of this technology in a collaborative effort between Raytheon Vision Systems and jet Propulsion Laboratory, resulting in successful devices with LWIR cutoff wavelengths. We report here two investigations related to wafer processing and superlattice material characteristics. The critical interface between the superlattice and the silicon dioxide passivation was examined at the atomic scale by high resolution transmission electron microscopy (HRTEM), showing a conformal coating on an InAs/GaSb mesa sidewall, which undulates with the superlattice periodicity due to differential etching. Electron energy loss spectroscopy (EELS) showed that oxides of the superlattice elements were present but minimal, and some occasional arsenic precipitates were observed at the passivation interface. Our previous analysis of the current-voltage curves was extended further to reveal the minority carrier lifetimes responsible for producing the generation-recombination (GR) and the diffusion dark currents. Lifetimes at 78 K were found to be 6 and 20 ns in the GR and diffusion processes, respectively. Lifetimes from both mechanisms track together with temperature. A HgCdTe diode was analyzed in the same manner for comparison. (C) 2009 Elsevier B.V. All rights reserved. C1 [Rhiger, David R.; Kvaas, Robert E.; Harris, Sean F.] Raytheon Vis Syst, Goleta, CA 93117 USA. [Hill, Cory J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Rhiger, DR (reprint author), Raytheon Vis Syst, 75 Coromar Dr, Goleta, CA 93117 USA. EM drhiger@raytheon.com NR 13 TC 20 Z9 20 U1 1 U2 10 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 1350-4495 J9 INFRARED PHYS TECHN JI Infrared Phys. Technol. PD NOV PY 2009 VL 52 IS 6 BP 304 EP 309 DI 10.1016/j.infrared.2009.05.009 PG 6 WC Instruments & Instrumentation; Optics; Physics, Applied SC Instruments & Instrumentation; Optics; Physics GA 539GB UT WOS:000273240700020 ER PT J AU Nguyen, J Ting, DZ Hill, CJ Soibel, A Keo, SA Gunapala, SD AF Nguyen, Jean Ting, David Z. Hill, Cory J. Soibel, Alexander Keo, Sam A. Gunapala, Sarath D. TI Dark current analysis of InAs/GaSb superlattices at low temperatures SO INFRARED PHYSICS & TECHNOLOGY LA English DT Article; Proceedings Paper CT International Conference on Quantum Structure Infrared Photodetector CY JAN 18-23, 2009 CL Yosemite, CA SP NASA, Jet Propuls Lab, NASA, AF Res Lab, NASA, Army Res Lab, NASA, Defense Adv Res Projects Agcy, NASA, Missile Defense Agcy, Calif Inst Technol, Georgia Inst Technol, FLIR, QWIPT Technol, QmagiQ Wafer Technol DE Infrared detector; Superlattices; Dark current ID DETECTORS AB A limitation to the advancement of the strained-layer superlattice technology for infrared detection is unwanted high dark currents and low R(0)A values, especially at long-wavelengths. In this paper, we discuss dark current characteristics of LWIR InAs/GaSb type-II superlattice detectors. Comparing devices with different dominant mechanisms, a more thorough analysis at low temperatures is provided. (C) 2009 Published by Elsevier B.V. C1 [Nguyen, Jean; Ting, David Z.; Hill, Cory J.; Soibel, Alexander; Keo, Sam A.; Gunapala, Sarath D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Nguyen, J (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM jean.nguyen@jpl.nasa.gov RI Soibel, Alexander/A-1313-2007 NR 13 TC 25 Z9 25 U1 2 U2 22 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 1350-4495 J9 INFRARED PHYS TECHN JI Infrared Phys. Technol. PD NOV PY 2009 VL 52 IS 6 BP 317 EP 321 DI 10.1016/j.infrared.2009.05.022 PG 5 WC Instruments & Instrumentation; Optics; Physics, Applied SC Instruments & Instrumentation; Optics; Physics GA 539GB UT WOS:000273240700022 ER PT J AU Hill, CJ Soibel, A Keo, SA Mumolo, JM Ting, DZ Gunapala, SD AF Hill, Cory J. Soibel, Alexander Keo, Sam A. Mumolo, Jason M. Ting, David Z. Gunapala, Sarath D. TI Demonstration of large format mid-wavelength infrared focal plane arrays based on superlattice and BIRD detector structures SO INFRARED PHYSICS & TECHNOLOGY LA English DT Article; Proceedings Paper CT International Conference on Quantum Structure Infrared Photodetector CY JAN 18-23, 2009 CL Yosemite, CA SP NASA, Jet Propuls Lab, NASA, AF Res Lab, NASA, Army Res Lab, NASA, Defense Adv Res Projects Agcy, NASA, Missile Defense Agcy, Calif Inst Technol, Georgia Inst Technol, FLIR, QWIPT Technol, QmagiQ Wafer Technol DE Superlattice; Infrared; Photodetector AB We have demonstrated the use of bulk antimonide based materials and type-II antimonide based superlattices in the development of large area mid-wavelength infrared (MWIR) focal plane arrays (FPAs). Barrier infrared photodetectors (BIRDs) and superlattice-based infrared photodetectors are expected to outperform traditional III-V MWIR and LWIR imaging technologies and are expected to offer significant advantages over II-VI material based FPAs. We have used molecular beam epitaxy (MBE) technology to grow InAs/GaSb superlattice pin photodiodes and bulk InAsSb structures on GaSb substrates. The coupled quantum well superlattice device offers additional control in wavelength tuning via quantum well sizes and interface composition, while the BIRD structure allows for device fabrication without additional passivation. As a demonstration of the large area imaging capabilities of this technology, we have fabricated mid-wavelength 1024 x 1024 pixels superlattice imaging FPAs and 640 x 512 MWIR arrays based on the BIRD concept. These initial FPA have produced excellent infrared imagery. (C) 2009 Published by Elsevier B.V. C1 [Hill, Cory J.; Soibel, Alexander; Keo, Sam A.; Mumolo, Jason M.; Ting, David Z.; Gunapala, Sarath D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Hill, CJ (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM cory.j.hill@jpl.nasa.gov RI Soibel, Alexander/A-1313-2007 NR 13 TC 16 Z9 18 U1 0 U2 15 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 1350-4495 J9 INFRARED PHYS TECHN JI Infrared Phys. Technol. PD NOV PY 2009 VL 52 IS 6 BP 348 EP 352 DI 10.1016/j.infrared.2009.09.007 PG 5 WC Instruments & Instrumentation; Optics; Physics, Applied SC Instruments & Instrumentation; Optics; Physics GA 539GB UT WOS:000273240700028 ER PT J AU Rafol, D Gunapala, S Bandara, S Law, KK AF Rafol, Don Gunapala, Sarath Bandara, Sumith Law, K. K. TI Spatial and temporal NEDT in the frequency domain SO INFRARED PHYSICS & TECHNOLOGY LA English DT Article; Proceedings Paper CT International Conference on Quantum Structure Infrared Photodetector CY JAN 18-23, 2009 CL Yosemite, CA SP NASA, Jet Propuls Lab, NASA, AF Res Lab, NASA, Army Res Lab, NASA, Defense Adv Res Projects Agcy, NASA, Missile Defense Agcy, Calif Inst Technol, Georgia Inst Technol, FLIR, QWIPT Technol, QmagiQ Wafer Technol DE QWIP; MIR; FPA; NUC; NEDT; Pattern noise AB It is widely accepted from noise models that the extracted performance parameters such as spatial and temporal NEDT do not depend on the number of samples, which are used to estimate the noise values. Experimental studies have determined that noise values depend on the number of sampled data because of other noise contribution or its frequency dependence. This, however, creates ambiguities since unique values NEDT cannot be established without fixing the number of frames to be utilized. However in the frequency domain, values of parameters can be easily established at certain frequency. In the frequency domain it is also easier to study the noise contribution originating from various noise sources such as from the ROIC. This presentation will present preliminary analysis of spatial and temporal noise in the frequency domain by utilizing the power of FFT analysis. (C) 2009 Elsevier B.V. All rights reserved C1 [Rafol, Don] EPIR Technol, Bolingbrook, IL 60440 USA. [Bandara, Sumith] AMSRD CER NV ST IFT, Night Vis & Elect Sesnors Directorate, Ft Belvoir, VA USA. [Law, K. K.] NAWCWD, China Lake, CA 93555 USA. [Gunapala, Sarath] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Rafol, D (reprint author), EPIR Technol, 590 Territorial Dr,Unit B, Bolingbrook, IL 60440 USA. EM rafol@sbcglobal.net; sarath.d.gunapala@jpl.nasa.gov; sumith.bandara@us.army.mil; kk.law@navy.mil NR 6 TC 0 Z9 0 U1 1 U2 2 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 1350-4495 J9 INFRARED PHYS TECHN JI Infrared Phys. Technol. PD NOV PY 2009 VL 52 IS 6 BP 371 EP 379 DI 10.1016/j.infrared.2009.05.038 PG 9 WC Instruments & Instrumentation; Optics; Physics, Applied SC Instruments & Instrumentation; Optics; Physics GA 539GB UT WOS:000273240700032 ER PT J AU Simolon, B Aziz, N Cogan, S Kurth, E Lam, S Petronio, S Woolaway, J Bandara, S Gunapala, S Mumolo, J AF Simolon, Brian Aziz, Naseem Cogan, Scott Kurth, Eric Lam, Simon Petronio, Susan Woolaway, James Bandara, Sumith Gunapala, Sarath Mumolo, Jason TI High performance two-color one megapixel CMOS ROIC for QWIP detectors SO INFRARED PHYSICS & TECHNOLOGY LA English DT Article; Proceedings Paper CT International Conference on Quantum Structure Infrared Photodetector CY JAN 18-23, 2009 CL Yosemite, CA SP NASA, Jet Propuls Lab, NASA, AF Res Lab, NASA, Army Res Lab, NASA, Defense Adv Res Projects Agcy, NASA, Missile Defense Agcy, Calif Inst Technol, Georgia Inst Technol, FLIR, QWIPT Technol, QmagiQ Wafer Technol DE QWIP; CMOS; Readout integrated circuits; Multiplexing; Two-color; Megapixel AB FUR Systems, Inc. has designed and fabricated the ISC0501 CMOS readout integrated circuit (ROIC) for quantum well infrared photocletectors (QWIPs). The ISC0501 is a two-color 1024 x 1024 format array with a 30 mu m pixel pitch. The ROIC contains a separate analog signal path for each wavelength band. Separate signal paths allow the two-colors to have optimized detector biases, integration times, offsets and gains. This architecture also allows both colors to simultaneously sample a scene and readout the pixel data. This paper will describe the interface, design and features of the ROIC as well as a summary of the characterization test results. A sample image is included from a focal plane array (FPA) built by the jet Propulsion Laboratory (JPL) using the ISC0501 ROIC with QWIP detectors designed by JPL (C) 2009 Elsevier B.V. All rights reserved. C1 [Simolon, Brian; Aziz, Naseem; Cogan, Scott; Kurth, Eric; Lam, Simon; Petronio, Susan; Woolaway, James] FLIR Syst Inc, Goleta, CA 93117 USA. [Bandara, Sumith; Gunapala, Sarath; Mumolo, Jason] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Simolon, B (reprint author), FLIR Syst Inc, 70 Castilian Dr, Goleta, CA 93117 USA. EM brian.simolon@flir.com NR 4 TC 3 Z9 3 U1 0 U2 2 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 1350-4495 J9 INFRARED PHYS TECHN JI Infrared Phys. Technol. PD NOV PY 2009 VL 52 IS 6 BP 391 EP 394 DI 10.1016/j.infrared.2009.05.015 PG 4 WC Instruments & Instrumentation; Optics; Physics, Applied SC Instruments & Instrumentation; Optics; Physics GA 539GB UT WOS:000273240700035 ER PT J AU Gunapala, SD Bandara, SV Liu, JK Mumolo, JM Ting, DZ Hill, CJ Nguyen, J Simolon, B Woolaway, J Wang, SC Li, W LeVan, PD Tidrow, MZ AF Gunapala, S. D. Bandara, S. V. Liu, J. K. Mumolo, J. M. Ting, D. Z. Hill, C. J. Nguyen, J. Simolon, B. Woolaway, J. Wang, S. C. Li, W. LeVan, P. D. Tidrow, M. Z. TI 1024 x 1024 Format pixel co-located simultaneously readable dual-band QWIP focal plane SO INFRARED PHYSICS & TECHNOLOGY LA English DT Article; Proceedings Paper CT International Conference on Quantum Structure Infrared Photodetector CY JAN 18-23, 2009 CL Yosemite, CA SP NASA, Jet Propuls Lab, NASA, AF Res Lab, NASA, Army Res Lab, NASA, Defense Adv Res Projects Agcy, NASA, Missile Defense Agcy, Calif Inst Technol, Georgia Inst Technol, FLIR, QWIPT Technol, QmagiQ Wafer Technol DE Infrared detectors; Quantum wells; QWIP; Dualband; Infrared imaging; Focal plane arrays ID WELL INFRARED DETECTORS; ARRAYS; CAMERA AB This paper reports the first demonstration of the megapixel-simultaneously-readable and pixel-co-registered dual-band quantum well infrared photodetector (QWIP) focal plane array (FPA). The dual-band QWIP device was developed by stacking two multi-quantum-well stacks tuned to absorb two different infrared wavelengths. The full width at half maximum (FWHM) of the mid-wave infrared (MWIR) band extends from 4.4 to 5.1 mu m and the FWHM of a long-wave infrared (LWIR) band extends from 7.8 to 8.8 mu m. Dual-band QWIP detector arrays were hybridized with custom fabricated direct injection read out integrated circuits (ROICs) using the indium bump hybridization technique. The initial dual-band megapixel QWIP FPAs were cooled to 70 K operating temperature. The preliminary data taken from the first megapixel QWIP FPA has shown system NE Delta T of 27 and 40 mK for MWIR and LWIR bands, respectively. (C) 2009 Elsevier B.V. All rights reserved. C1 [Gunapala, S. D.; Bandara, S. V.; Liu, J. K.; Mumolo, J. M.; Ting, D. Z.; Hill, C. J.; Nguyen, J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Simolon, B.; Woolaway, J.] FLIR Syst Inc, Indigo Operat, Goleta, CA 93117 USA. [Wang, S. C.; Li, W.] Global Commun Semicond Inc, Torrance, CA 90505 USA. [LeVan, P. D.] USAF, Res Lab, Kirtland AFB, NM 87117 USA. [Tidrow, M. Z.] Missile Def Agcy, AS, Washington, DC 20301 USA. RP Gunapala, SD (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM sarath.d.gunapala@jpl.nasa.gov NR 14 TC 8 Z9 12 U1 1 U2 8 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 1350-4495 J9 INFRARED PHYS TECHN JI Infrared Phys. Technol. PD NOV PY 2009 VL 52 IS 6 BP 395 EP 398 DI 10.1016/j.infrared.2009.05.019 PG 4 WC Instruments & Instrumentation; Optics; Physics, Applied SC Instruments & Instrumentation; Optics; Physics GA 539GB UT WOS:000273240700036 ER PT J AU Soibel, A Bandara, SV Ting, DZ Liu, JK Mumolo, JM Rafol, SB Johnson, WR Wilson, DW Gunapala, SD AF Soibel, A. Bandara, Sumith V. Ting, David Z. Liu, John K. Mumolo, Jason M. Rafol, Sir B. Johnson, William R. Wilson, Daniel W. Gunapala, Sarath D. TI A super-pixel QWIP focal plane array for imaging multiple waveband temperature sensor SO INFRARED PHYSICS & TECHNOLOGY LA English DT Article; Proceedings Paper CT International Conference on Quantum Structure Infrared Photodetector CY JAN 18-23, 2009 CL Yosemite, CA SP NASA, Jet Propuls Lab, NASA, AF Res Lab, NASA, Army Res Lab, NASA, Defense Adv Res Projects Agcy, NASA, Missile Defense Agcy, Calif Inst Technol, Georgia Inst Technol, FLIR, QWIPT Technol, QmagiQ Wafer Technol DE Infrared; Infrared FPA; QWIP ID WELL INFRARED PHOTODETECTORS; WAVELENGTH AB The multi-waveband temperature sensor (MWTS) array, in which each super-pixel (2 x 2 pixel cell) operates at four distinct thermal infrared (IR) wavebands is being developed. Using this high spatial resolution, four-band thermal IR band detector array, accurate temperature measurements on the surface of an object can be made without prior knowledge of its exact emissivity. This multi-band detector involves intersubband transition in III-V semiconductor-based quantum layered structures. Each detector stack absorbs photons within the specified wavelength band while allowing the transmission of photons in other spectral bands, thus efficiently permitting multi-band detection. This produces multiple, spectrally resolved images of the scene that are recorded simultaneously in a single snapshot on the FPA. From the multispectral images and calibration information about the system, computational algorithms are used to evaluate the temperature on the surface of a target. (C) 2009 Elsevier B.V. All rights reserved. C1 [Soibel, A.; Bandara, Sumith V.; Ting, David Z.; Liu, John K.; Mumolo, Jason M.; Rafol, Sir B.; Johnson, William R.; Wilson, Daniel W.; Gunapala, Sarath D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Soibel, A (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Alexander.Soibel@jpl.nass.gov RI Soibel, Alexander/A-1313-2007 NR 13 TC 4 Z9 4 U1 0 U2 5 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 1350-4495 J9 INFRARED PHYS TECHN JI Infrared Phys. Technol. PD NOV PY 2009 VL 52 IS 6 BP 403 EP 407 DI 10.1016/j.infrared.2009.05.010 PG 5 WC Instruments & Instrumentation; Optics; Physics, Applied SC Instruments & Instrumentation; Optics; Physics GA 539GB UT WOS:000273240700038 ER PT J AU Jhabvala, M Reuter, D Choi, K Jhabvala, C Sundaram, M AF Jhabvala, M. Reuter, D. Choi, K. Jhabvala, C. Sundaram, M. TI QWIP-based thermal infrared sensor for the Landsat Data Continuity Mission SO INFRARED PHYSICS & TECHNOLOGY LA English DT Article; Proceedings Paper CT International Conference on Quantum Structure Infrared Photodetector CY JAN 18-23, 2009 CL Yosemite, CA SP NASA, Jet Propuls Lab, NASA, AF Res Lab, NASA, Army Res Lab, NASA, Defense Adv Res Projects Agcy, NASA, Missile Defense Agcy, Calif Inst Technol, Georgia Inst Technol, FLIR, QWIPT Technol, QmagiQ Wafer Technol DE QWIP; Infrared detectors; Landsat; Quantum well structures AB The thermal infrared sensor (TIRS) is a QWIP based instrument intended to supplement the Operational Land Imager (OLI) for the Landsat Data Continuity Mission (LDCM) [See Landsat project description at: http://landsathandbook.gsfc.nasa.gov/handbook/handbook-htmis/chapterl/chapterl.html, [1]. The LDCM is planned to be launched in late 2012 and will continue the 35 year legacy of the Landsat program as Landsat 7 degrades. The LDCM is a joint NASA-US Geological Survey (USGS) mission. The TIRS instrument is a far infrared imager operating in the push broom mode with two IR channels: 10.8 mu m and 12 mu m. The focal plane will contain three 640 x 512 QWIP arrays mounted on a silicon substrate. The readout integrated circuit (ROIC) is intended to be the Indigo 9803. The focal plane operating temperature will be 43 K (nominally). Bandpass filters will define the precise spectral response of the focal plane. Two QWIP designs will be pursued, the corrugated structure and the grating structure. NASA/Goddard, the Army Research Lab and QmagiQ will work closely together to obtain the suite of arrays that will best meet the mission requirements (primarily adequate conversion efficiency at the required wavelengths). This paper will describe the design and fabrication of the TIRS instrument with particular emphasis on the QWIP detectors. The QWIP parameters that are driving the mission requirements include spectral response, dark current, conversion efficiency, read noise, temperature stability, pixel uniformity and pixel yield. Additional mechanical constraints such as co-registration between the three arrays, filter design and assembly and testing will also be discussed. Published by Elsevier B.V. C1 [Jhabvala, M.; Reuter, D.; Jhabvala, C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Choi, K.] USA, Res Lab, Adelphi, MD 20783 USA. [Sundaram, M.] QmagiQ LLC, Nashua, NH 03063 USA. RP Jhabvala, M (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM murzy.d.jhabvala@nasa.gov NR 5 TC 19 Z9 20 U1 0 U2 10 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 1350-4495 J9 INFRARED PHYS TECHN JI Infrared Phys. Technol. PD NOV PY 2009 VL 52 IS 6 BP 424 EP 429 DI 10.1016/j.infrared.2009.05.027 PG 6 WC Instruments & Instrumentation; Optics; Physics, Applied SC Instruments & Instrumentation; Optics; Physics GA 539GB UT WOS:000273240700042 ER PT J AU Johnson, WR Hook, SJ Mouroulis, P Wilson, DW Gunapala, SD Hill, CJ Mumolo, JM Eng, BT AF Johnson, William R. Hook, Simon J. Mouroulis, Pantazis Wilson, Daniel W. Gunapala, Sarath D. Hill, Cory J. Mumolo, Jason M. Eng, Bjorn T. TI Quantum well earth science testbed SO INFRARED PHYSICS & TECHNOLOGY LA English DT Article; Proceedings Paper CT International Conference on Quantum Structure Infrared Photodetector CY JAN 18-23, 2009 CL Yosemite, CA SP NASA, Jet Propuls Lab, NASA, AF Res Lab, NASA, Army Res Lab, NASA, Defense Adv Res Projects Agcy, NASA, Missile Defense Agcy, Calif Inst Technol, Georgia Inst Technol, FLIR, QWIPT Technol, QmagiQ Wafer Technol DE QWIP; Imaging; Spectroscopy; Dyson ID OPTICAL DESIGN; SPECTROMETER AB A thermal hyperspectral imager is underdevelopment which utilizes the compact Dyson optical configuration and the broadband (8-12 mu m) quantum well infrared photodetector (QWIP) focal plane array technology. The Dyson configuration uses a single monolithic prism-like grating design which allows for a high throughput instrument (F/1.6) with minimal ghosting, stray light and large swath width. The configuration has the potential to be the optimal high resolution imaging spectroscopy solution for aerial and space remote sensing applications due to its small form factor and relatively low power requirements. The planned instrument specifications are discussed as well as thermal design trade-offs. The current design uses a single high power cryocooler which allows operation of the QWIP at 40 K with adequate temperature stability. Calibration testing results (noise equivalent temperature difference, spectral linearity and spectral bandwidth) and laboratory emissivity plots from samples are shown using an operational testbed unit which has similar specifications as the final airborne system. Field testing of the testbed unit was performed to acquire plots of emissivity for various known standard minerals (quartz, opal, alunite). A comparison is made using data from the ASTER spectral library. The current single band (8-9 mu m) testbed utilizes the high uniformity and operability of the QWIP array and shows excellent laboratory and field spectroscopic results. (C) 2009 Elsevier B.V. All rights reserved. C1 [Johnson, William R.; Hook, Simon J.; Mouroulis, Pantazis; Wilson, Daniel W.; Gunapala, Sarath D.; Hill, Cory J.; Mumolo, Jason M.; Eng, Bjorn T.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Johnson, WR (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM William.R.Johnson@jpl.nasa.gov NR 11 TC 3 Z9 3 U1 0 U2 4 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 1350-4495 J9 INFRARED PHYS TECHN JI Infrared Phys. Technol. PD NOV PY 2009 VL 52 IS 6 BP 430 EP 433 DI 10.1016/j.infrared.2009.05.006 PG 4 WC Instruments & Instrumentation; Optics; Physics, Applied SC Instruments & Instrumentation; Optics; Physics GA 539GB UT WOS:000273240700043 ER PT J AU Wolpert, DH AF Wolpert, David H. TI Trembling hand perfection for mixed quantal/best response equilibria SO INTERNATIONAL JOURNAL OF GAME THEORY LA English DT Article DE Quantal response equilibrium; Trembling hand perfection; Entropy ID GAMES AB The quantal response equilibrium (QRE) is a powerful alternative to full rationality equilibrium concepts. At a QRE, all joint moves have non-zero probability. However in "mixed scenarios", where some players use quantal response and some use best response, equilibrium strategy profiles can have joint moves with zero probability. This raises the question of applying the trembling hand refinement to such mixed scenarios. To address this I first show how to reformulate the QRE as a "best response" equilibrium where expected utilities are replaced by more general objective functions. I then show that under this reformulation the two popular types of trembling hand perfection can differ when some players use quantal response and some use best response. I end by showing that one of those types of trembling hand perfection cannot be used to remove certain troubling kinds of equilibrium in such mixed scenarios, while the other type can. The conclusion is that only the one type of trembling hand perfection should be applied when we allow some players to be quantal response and some to be best response. C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Wolpert, DH (reprint author), NASA, Ames Res Ctr, MS 269-1, Moffett Field, CA 94035 USA. EM david.h.wolpert@nasa.gov NR 20 TC 1 Z9 1 U1 0 U2 4 PU SPRINGER HEIDELBERG PI HEIDELBERG PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY SN 0020-7276 J9 INT J GAME THEORY JI Int. J. Game Theory PD NOV PY 2009 VL 38 IS 4 BP 539 EP 551 DI 10.1007/s00182-009-0169-2 PG 13 WC Economics; Mathematics, Interdisciplinary Applications; Social Sciences, Mathematical Methods; Statistics & Probability SC Business & Economics; Mathematics; Mathematical Methods In Social Sciences GA 522WD UT WOS:000272029900006 ER PT J AU Bajracharya, M Moghaddam, B Howard, A Brennan, S Matthies, LH AF Bajracharya, Max Moghaddam, Baback Howard, Andrew Brennan, Shane Matthies, Larry H. TI A Fast Stereo-based System for Detecting and Tracking Pedestrians from a Moving Vehicle SO INTERNATIONAL JOURNAL OF ROBOTICS RESEARCH LA English DT Article; Proceedings Paper CT 13th International Symposium on Robotics Research (ISSR) CY NOV 26-29, 2007 CL Hiroshima, JAPAN SP Int Fdn Robot Res DE pedestrian detection; human detection; stereo; tracking AB In this paper we describe a fully integrated system for detecting, localizing, and tracking pedestrians from a moving vehicle. The system can reliably detect upright pedestrians to a range of 40 m in lightly cluttered urban environments. The system uses range data from stereo vision to segment the scene into regions of interest, from which shape features are extracted and used to classify pedestrians. The regions are tracked using shape and appearance features. Tracking is used to temporally filter classifications to improve performance and to estimate the velocity of pedestrians for use in path planning. The end-to-end system runs at 5 Hz on 1,024 x 768 imagery using a standard 2.4 GHz Intel Core 2 Quad processor, and has been integrated and tested on multiple ground vehicles and environments. We show performance on a diverse set of datasets with groundtruth in outdoor environments with varying degrees of pedestrian density and clutter. In highly cluttered urban environments, the detection rates are on a par with state-of-the-art but significantly slower systems. C1 [Bajracharya, Max; Moghaddam, Baback; Howard, Andrew; Brennan, Shane; Matthies, Larry H.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Bajracharya, M (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM maxb@robotics.jpl.nasa.gov NR 28 TC 28 Z9 29 U1 0 U2 7 PU SAGE PUBLICATIONS LTD PI LONDON PA 1 OLIVERS YARD, 55 CITY ROAD, LONDON EC1Y 1SP, ENGLAND SN 0278-3649 J9 INT J ROBOT RES JI Int. J. Robot. Res. PD NOV-DEC PY 2009 VL 28 IS 11-12 BP 1466 EP 1485 DI 10.1177/0278364909341884 PG 20 WC Robotics SC Robotics GA 511JR UT WOS:000271160800006 ER PT J AU Morelli, EA Smith, MS AF Morelli, Eugene A. Smith, Mark S. TI Real-Time Dynamic Modeling: Data Information Requirements and Flight-Test Results SO JOURNAL OF AIRCRAFT LA English DT Article; Proceedings Paper CT AIAA Atmospheric Flight Mechanics Conference CY AUG 18-21, 2008 CL Honolulu, HI SP AIAA ID PARAMETER-ESTIMATION; IDENTIFICATION; AIRCRAFT; SYSTEM AB Practical aspects or identifying dynamic models for aircraft in real time were studied. Topics included the formulation of am equation-error method in the frequency domain to estimate nondimensional stability and control derivatives in real time, data information content for accurate modeling results, speed of convergence. and data information management techniques such as data forgetting, incorporating prior information, and optimized excitation. Real-time dynamic modeling was applied to simulation data and flight-test data from a modified F-15B fighter aircraft and to operational flight data from a subscale jet transport aircraft. Estimated parameter standard errors, prediction cases, and comparisons with results from postflight analysis using the output-error method in the time domain were used to demonstrate the accuracy of the identified real-time models. C1 [Morelli, Eugene A.] NASA, Langley Res Ctr, Dynam Syst & Control Branch, Hampton, VA 23681 USA. [Smith, Mark S.] NASA, Dryden Flight Res Ctr, Aerodynam Branch, Edwards AFB, CA 93523 USA. RP Morelli, EA (reprint author), NASA, Langley Res Ctr, Dynam Syst & Control Branch, Mail Stop 308, Hampton, VA 23681 USA. NR 18 TC 13 Z9 13 U1 1 U2 3 PU AMER INST AERONAUT ASTRONAUT PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0021-8669 J9 J AIRCRAFT JI J. Aircr. PD NOV-DEC PY 2009 VL 46 IS 6 BP 1894 EP 1905 DI 10.2514/1.40764 PG 12 WC Engineering, Aerospace SC Engineering GA 532CS UT WOS:000272722300007 ER PT J AU Schwarz, JB Dowell, EH Thomas, JP Hall, KC Rausch, RD Bertels, RE AF Schwarz, Jordan B. Dowell, Earl H. Thomas, Jeffrey P. Hall, Kenneth C. Rausch, Russ D. Bertels, Robert E. TI Improved Flutter Boundary Prediction for an Isolated Two-Degree-of-Freedom Airfoil SO JOURNAL OF AIRCRAFT LA English DT Article; Proceedings Paper CT AIAA/ASME/ASCE/AHS/ASC 49th Structures Structural Dynamic and Materials Conference CY APR 07-10, 2008 CL Schaumburg, IL SP Amer Inst Aeronaut & Astronaut, ASME, ASCE, AHS, ASC AB A novel method of computing the flutter boundary for all isolated airfoil based on a high-fidelity computational fluid dynamics model reveals unusual behavior in a critical transonic range. Inviscid and viscous predictions of the flutter boundary for the two airfoils examined differ substantially in this critical region and become sensitive to Mach number and grid topology due to complicated shock/boundary-layer interactions. Computational fluid dynamics predictions of the flutter boundary for a NACA 0012 section airfoil are also compared with previous experimental results. C1 [Schwarz, Jordan B.; Dowell, Earl H.; Thomas, Jeffrey P.; Hall, Kenneth C.] Duke Univ, Dept Mech Engn & Mat Sci, Durham, NC 27708 USA. [Rausch, Russ D.; Bertels, Robert E.] NASA, Langley Res Ctr, Aeroelast Branch, Hampton, VA 23681 USA. RP Schwarz, JB (reprint author), Dynam Concepts Inc, Huntsville, AL USA. NR 6 TC 4 Z9 5 U1 0 U2 5 PU AMER INST AERONAUT ASTRONAUT PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0021-8669 J9 J AIRCRAFT JI J. Aircr. PD NOV-DEC PY 2009 VL 46 IS 6 BP 2069 EP 2076 DI 10.2514/1.30703 PG 8 WC Engineering, Aerospace SC Engineering GA 532CS UT WOS:000272722300022 ER PT J AU Liao, L Meneghini, R Tian, L Heymsfield, GM AF Liao, Liang Meneghini, Robert Tian, Lin Heymsfield, Gerald M. TI Measurements and Simulations of Nadir-Viewing Radar Returns from the Melting Layer at X and W Bands SO JOURNAL OF APPLIED METEOROLOGY AND CLIMATOLOGY LA English DT Article ID REMOTE-SENSING APPLICATIONS; MICROPHYSICAL PROCESSES; 2-WAVELENGTH RADAR; PART I; MODEL; HYDROMETEORS; SNOWFLAKES; PRECIPITATION; DISTRIBUTIONS; PARTICLES AB Simulated radar signatures within the melting layer in stratiform rain-namely, the radar bright band-are checked by means of comparisons with simultaneous measurements of the bright band made by the ER-2 Doppler radar (EDOP; X band) and Cloud Radar System (CRS; W band) airborne Doppler radars during the Cirrus Regional Study of Tropical Anvils and Cirrus Layers-Florida-Area Cirrus Experiment (CRYSTAL-FACE) campaign in 2002. A stratified-sphere model, allowing the fractional water content to vary along the radius of the particle, is used to compute the scattering properties of individual melting snowflakes. Using the effective dielectric constants computed by the conjugate gradient-fast Fourier transform numerical method for X and W bands and expressing the fractional water content of a melting particle as an exponential function in particle radius, it is found that at X band the simulated radar brightband profiles are in an excellent agreement with the measured profiles. It is also found that the simulated W-band profiles usually resemble the shapes of the measured brightband profiles even though persistent offsets between them are present. These offsets, however, can be explained by the attenuation caused by cloud water and water vapor at W band. This is confirmed by comparisons of the radar profiles made in the rain regions where the unattenuated W-band reflectivity profiles can be estimated through the X-and W-band Doppler velocity measurements. The brightband model described in this paper has the potential to be used effectively for both radar and radiometer algorithms relevant to the satellite-based Tropical Rainfall Measuring Mission and Global Precipitation Measuring Mission. C1 [Liao, Liang; Tian, Lin] Univ Maryland, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21201 USA. RP Liao, L (reprint author), NASA, Goddard Space Flight Ctr, Goddard Earth Sci & Technol Ctr UMBC, Code 613-1, Greenbelt, MD 20771 USA. EM liang.liao-1@nasa.gov FU NASA [NNH06ZDA001N-PMM] FX We thank Dr. Lihua Li, Mr. Ed Zenker, Dr. Steven Bidwell, and Dr. Paul Racette for EDOP and CRS data processing and engineering support. This work is supported by Dr. R. Kakar of NASA Headquarters under NASA's Precipitation Measurement Mission (PMM) Grant NNH06ZDA001N-PMM. NR 33 TC 6 Z9 6 U1 1 U2 2 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 1558-8424 J9 J APPL METEOROL CLIM JI J. Appl. Meteorol. Climatol. PD NOV PY 2009 VL 48 IS 11 BP 2215 EP 2226 DI 10.1175/2009JAMC2033.1 PG 12 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 523LX UT WOS:000272076000002 ER PT J AU Cantrell, JH AF Cantrell, John H. TI Ultrasonic harmonic generation from fatigue-induced dislocation substructures in planar slip metals and assessment of remaining fatigue life SO JOURNAL OF APPLIED PHYSICS LA English DT Article ID DAMAGE ACCUMULATION; ELASTIC-CONSTANTS; ORGANIZATION; BEHAVIOR; COPPER AB An analytical model is presented of the microelastic-plastic nonlinearities resulting from the interactions of a stress perturbation with dislocation Substructures and cracks that evolve during cyclic fatigue of planar slip metals. The interactions are quantified by a material nonlinearity parameter beta extracted from acoustic (ultrasonic) harmonic generation measurements The beta parameter for a given fatigue state is highly sensitive to the volume fractions of active persistent Luders bands (PLBs) and PLB internal stresses, as well as to the densities. loop lengths. and dipole heights of the dislocation monopoles and dipoles that form the PLBs The beta parameter is predicted to increase monotonically with the increase in the hardness of the metal during cyclic loading, thus allowing all unambiguous assessment of the remaining life of the material. The model is applied to the calculation of beta as a function of percent full fatigue life of IN100 nickel-base superalloy. The theoretical predictions are in good agreement with experimental measurements reported in the literature of IN100 samples fatigued In strain-control led, low cycle. fully reversed loading (C) 2009 American Institute of Physics. [doi: 10.1063/1.3254223] C1 NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Cantrell, JH (reprint author), NASA, Langley Res Ctr, Mail Stop 231, Hampton, VA 23681 USA. NR 30 TC 19 Z9 21 U1 1 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 0021-8979 J9 J APPL PHYS JI J. Appl. Phys. PD NOV 1 PY 2009 VL 106 IS 9 AR 093516 DI 10.1063/1.3254223 PG 6 WC Physics, Applied SC Physics GA 529YP UT WOS:000272555700032 ER PT J AU Hu, YX Winker, D Vaughan, M Lin, B Omar, A Trepte, C Flittner, D Yang, P Nasiri, SL Baum, B Sun, WB Liu, ZY Wang, Z Young, S Stamnes, K Huang, JP Kuehn, R Holz, R AF Hu, Yongxiang Winker, David Vaughan, Mark Lin, Bing Omar, Ali Trepte, Charles Flittner, David Yang, Ping Nasiri, Shaima L. Baum, Bryan Sun, Wenbo Liu, Zhaoyan Wang, Zhien Young, Stuart Stamnes, Knut Huang, Jianping Kuehn, Ralph Holz, Robert TI CALIPSO/CALIOP Cloud Phase Discrimination Algorithm SO JOURNAL OF ATMOSPHERIC AND OCEANIC TECHNOLOGY LA English DT Article ID OPTICAL-PROPERTIES; MICROPHYSICAL PROPERTIES; LIDAR DEPOLARIZATION; MULTIPLE-SCATTERING; CIRRUS CLOUDS; ICE CRYSTALS; MIDLATITUDE; POLARIZATION; SENSITIVITY AB The current cloud thermodynamic phase discrimination by Cloud-Aerosol Lidar Pathfinder Satellite Observations (CALIPSO) is based on the depolarization of backscattered light measured by its lidar [Cloud-Aerosol Lidar with Orthogonal Polarization (CALIOP)]. It assumes that backscattered light from ice crystals is depolarizing, whereas water clouds, being spherical, result in minimal depolarization. However, because of the relationship between the CALIOP field of view (FOV) and the large distance between the satellite and clouds and because of the frequent presence of oriented ice crystals, there is often a weak correlation between measured depolarization and phase, which thereby creates significant uncertainties in the current CALIOP phase retrieval. For water clouds, the CALIOP-measured depolarization can be large because of multiple scattering, whereas horizontally oriented ice particles depolarize only weakly and behave similarly to water clouds. Because of the nonunique depolarization-cloud phase relationship, more constraints are necessary to uniquely determine cloud phase. Based on theoretical and modeling studies, an improved cloud phase determination algorithm has been developed. Instead of depending primarily on layer-integrated depolarization ratios, this algorithm differentiates cloud phases by using the spatial correlation of layer-integrated attenuated backscatter and layer-integrated particulate depolarization ratio. This approach includes a two-step process: 1) use of a simple two-dimensional threshold method to provide a preliminary identification of ice clouds containing randomly oriented particles, ice clouds with horizontally oriented particles, and possible water clouds and 2) application of a spatial coherence analysis technique to separate water clouds from ice clouds containing horizontally oriented ice particles. Other information, such as temperature, color ratio, and vertical variation of depolarization ratio, is also considered. The algorithm works well for both the 0.3 degrees and 3 degrees off-nadir lidar pointing geometry. When the lidar is pointed at 0.38 off nadir, half of the opaque ice clouds and about one-third of all ice clouds have a significant lidar backscatter contribution from specular reflections from horizontally oriented particles. At 3 degrees off nadir, the lidar backscatter signals for roughly 30% of opaque ice clouds and 20% of all observed ice clouds are contaminated by horizontally oriented crystals. C1 [Hu, Yongxiang; Winker, David; Vaughan, Mark; Lin, Bing; Omar, Ali; Trepte, Charles; Flittner, David] NASA, Langley Res Ctr, Climate Sci Branch, Hampton, VA 23681 USA. [Yang, Ping; Nasiri, Shaima L.] Texas A&M Univ, College Stn, TX USA. [Baum, Bryan; Holz, Robert] Univ Wisconsin, Ctr Space Sci & Engn, Madison, WI 53706 USA. [Sun, Wenbo] Hampton Univ, Ctr Atmospher Sci, Hampton, VA 23668 USA. [Liu, Zhaoyan] Natl Inst Aerosp, Hampton, VA USA. [Wang, Zhien] Univ Wyoming, Laramie, WY 82071 USA. [Young, Stuart] CSIRO Marine & Atmospher Res, Aspendale, Vic, Australia. [Stamnes, Knut] Stevens Inst Technol, Hoboken, NJ 07030 USA. [Huang, Jianping; Kuehn, Ralph] SSAI, Hampton, VA USA. RP Hu, YX (reprint author), NASA, Langley Res Ctr, Climate Sci Branch, MS 475, Hampton, VA 23681 USA. EM yongxiang.hu-1@nasa.gov RI Liu, Zhaoyan/A-9604-2009; Liu, Zhaoyan/B-1783-2010; Baum, Bryan/B-7670-2011; Yang, Ping/B-4590-2011; Wang, Zhien/F-4857-2011; Nasiri, Shaima/C-8044-2011; Young, Stuart/A-8641-2011; Hu, Yongxiang/K-4426-2012; Omar, Ali/D-7102-2017 OI Liu, Zhaoyan/0000-0003-4996-5738; Baum, Bryan/0000-0002-7193-2767; Young, Stuart/0000-0001-6434-9816; Omar, Ali/0000-0003-1871-9235 FU CALIPSO project; NASA [NNX08AF81G, NNX08AF78A] FX This study is supported by the CALIPSO project. The authors thank Dr. M. Platt for providing constructive comments on the manuscript. The authors are grateful for the insightful comments offered by the anonymous reviewers. Bryan Baum's research is supported by NASA Grants NNX08AF81G and NNX08AF78A. NR 22 TC 114 Z9 117 U1 4 U2 26 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0739-0572 J9 J ATMOS OCEAN TECH JI J. Atmos. Ocean. Technol. PD NOV PY 2009 VL 26 IS 11 BP 2293 EP 2309 DI 10.1175/2009JTECHA1280.1 PG 17 WC Engineering, Ocean; Meteorology & Atmospheric Sciences SC Engineering; Meteorology & Atmospheric Sciences GA 521FA UT WOS:000271904500002 ER PT J AU Winker, DM Vaughan, MA Omar, A Hu, YX Powell, KA Liu, ZY Hunt, WH Young, SA AF Winker, David M. Vaughan, Mark A. Omar, Ali Hu, Yongxiang Powell, Kathleen A. Liu, Zhaoyan Hunt, William H. Young, Stuart A. TI Overview of the CALIPSO Mission and CALIOP Data Processing Algorithms SO JOURNAL OF ATMOSPHERIC AND OCEANIC TECHNOLOGY LA English DT Article ID CIRRUS CLOUD CLIMATOLOGY; TO-BACKSCATTER RATIO; TROPOSPHERIC AEROSOL; LIDAR; SPACE; EXTINCTION; RETRIEVAL; PERFORMANCE; PROFILES; FACILITY AB The Cloud-Aerosol Lidar with Orthogonal Polarization (CALIOP) is a two-wavelength polarization lidar performs global profiling of aerosols and clouds in the troposphere and lower stratosphere. CALIOP is the primary instrument on the Cloud-Aerosol Lidar and Infrared Pathfinder Satellite Observations (CALIPSO) satellite, which has flown in formation with the NASA A-train constellation of satellites since May 2006. The global, multiyear dataset obtained from CALIOP provides a new view of the earth's atmosphere and will lead to an improved understanding of the role of aerosols and clouds in the climate system. A suite of algorithms has been developed to identify aerosol and cloud layers and to retrieve a variety of optical and microphysical properties. CALIOP represents a significant advance over previous space lidars, and the algorithms that have been developed have many innovative aspects to take advantage of its capabilities. This paper provides a brief overview of the CALIPSO mission, the CALIOP instrument and data products, and an overview of the algorithms used to produce these data products. C1 [Winker, David M.; Vaughan, Mark A.; Omar, Ali; Hu, Yongxiang; Powell, Kathleen A.] NASA, Langley Res Ctr, Hampton, VA 23681 USA. [Liu, Zhaoyan] Natl Inst Aerosp, Hampton, VA USA. [Hunt, William H.] Sci Syst & Applicat Inc, Hampton, VA USA. [Young, Stuart A.] CSIRO Marine & Atmospher Res, Aspendale, Vic, Australia. RP Winker, DM (reprint author), NASA, Langley Res Ctr, MS 475, Hampton, VA 23681 USA. EM david.m.winker@nasa.gov RI Liu, Zhaoyan/A-9604-2009; Liu, Zhaoyan/B-1783-2010; Young, Stuart/A-8641-2011; Hu, Yongxiang/K-4426-2012; Omar, Ali/D-7102-2017 OI Liu, Zhaoyan/0000-0003-4996-5738; Young, Stuart/0000-0001-6434-9816; Omar, Ali/0000-0003-1871-9235 FU NASA; CNES FX The authors wish to acknowledge the support and successful cooperation of NASA and CNES, which made the CALIPSO mission possible. NR 39 TC 584 Z9 594 U1 16 U2 109 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0739-0572 EI 1520-0426 J9 J ATMOS OCEAN TECH JI J. Atmos. Ocean. Technol. PD NOV PY 2009 VL 26 IS 11 BP 2310 EP 2323 DI 10.1175/2009JTECHA1281.1 PG 14 WC Engineering, Ocean; Meteorology & Atmospheric Sciences SC Engineering; Meteorology & Atmospheric Sciences GA 521FA UT WOS:000271904500003 ER PT J AU Smith, GL Priestley, KJ Hess, PC Currey, C Spence, P AF Smith, G. Louis Priestley, Kory J. Hess, Phillip C. Currey, Chris Spence, Peter TI Validation of Geolocation of Measurements of the Clouds and the Earth's Radiant Energy System (CERES) Scanning Radiometers aboard Three Spacecraft SO JOURNAL OF ATMOSPHERIC AND OCEANIC TECHNOLOGY LA English DT Article AB The Clouds and the Earth's Radiant Energy System (CERES) instrument is a scanning radiometer for measuring Earth-emitted and -reflected solar radiation to understand Earth's energy balance. One CERES instrument was placed into orbit aboard the Tropical Rainfall Measuring Mission (TRMM) in 1997; two were aboard the Terra spacecraft, launched in 1999; and two were aboard the Aqua spacecraft, launched in 2002. These measurements are used together with data from higher-resolution instruments to generate a number of data products. The nominal footprint size of the pixel at Earth's surface is 16 km in the cross-scan direction and 23 km in the scan direction for the TRMM platform and 36 km in the cross-scan direction and 46 km in the scan direction for the Terra and Aqua platforms. It is required that the location on Earth of each pixel be known to 1-2 km to use the CERES data with the higher-resolution instruments on a pixel basis. A technique has been developed to validate the computed geolocation of the measurements by use of coastlines. Scenes are chosen in which the reflected solar radiation changes abruptly from the land surface to the darker ocean surface and the Earth-emitted radiation changes from the warm land to the cool ocean, or vice versa, so that scenes can be detected both day and night. The computed coastline location is then compared with the World Bank II map. The method has been applied to data from the three spacecraft and shows that the pixel geolocations are accurate to within 10% of the pixel size and that the geolocation is adequate for current scientific investigations. C1 [Smith, G. Louis; Priestley, Kory J.; Currey, Chris] NASA, Langley Res Ctr, Hampton, VA 23681 USA. [Smith, G. Louis] Natl Inst Aerosp, Hampton, VA USA. [Hess, Phillip C.] Space Syst Applicat Inc, Hampton, VA USA. [Spence, Peter] Sci Applicat Int Corp, Hampton, VA USA. RP Smith, GL (reprint author), NASA, Langley Res Ctr, Mail Stop 420, Hampton, VA 23681 USA. EM george.l.smith@larc.nasa.gov FU Earth Observation Office of the Washington, D.C.; NASA; Science Directorate of the Langley Research Center (LaRC); National Institute for Aerospace; Space Science Applications, Inc. FX The authors gratefully acknowledge the support by the CERES Program, which is funded by the Earth Observation Office of the Washington, D.C., office of NASA, and by the Science Directorate of the Langley Research Center (LaRC). GLS is funded by contract between LaRC and the National Institute for Aerospace, and PCH is funded by contract between LaRC and Space Science Applications, Inc. NR 21 TC 11 Z9 12 U1 0 U2 1 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0739-0572 J9 J ATMOS OCEAN TECH JI J. Atmos. Ocean. Technol. PD NOV PY 2009 VL 26 IS 11 BP 2379 EP 2391 DI 10.1175/2009JTECHA1207.1 PG 13 WC Engineering, Ocean; Meteorology & Atmospheric Sciences SC Engineering; Meteorology & Atmospheric Sciences GA 521FA UT WOS:000271904500008 ER PT J AU Nugent, PW Shaw, JA Pust, NJ Piazzolla, S AF Nugent, Paul W. Shaw, Joseph A. Pust, Nathan J. Piazzolla, Sabino TI Correcting Calibrated Infrared Sky Imagery for the Effect of an Infrared Window SO JOURNAL OF ATMOSPHERIC AND OCEANIC TECHNOLOGY LA English DT Article ID EMITTED RADIANCE INTERFEROMETER; SYSTEM AB A method is demonstrated for deriving a correction for the effects of an infrared window when used to weatherproof a radiometrically calibrated thermal infrared imager. The technique relies on initial calibration of two identical imagers without windows and subsequently operating the imagers side by side: one with a window and one without. An equation is presented that expresses the scene radiance in terms of through-window radiance and the transmittance, reflectance, and emissivity of the window. The window's optical properties are determined as a function of angle over the imager's field of view through a matrix inversion using images observed simultaneously with and without a window. The technique is applied to calibrated sky images from infrared cloud imager systems. Application of this window correction algorithm to data obtained months before or after the algorithm was derived leads to an improvement from 0.46 to 0.91 for the correlation coefficient between data obtained simultaneously from imagers with and without a window. Once the window correction has been determined, the windowed imager can operate independently and provide accurate measurements of sky radiance. C1 [Nugent, Paul W.; Shaw, Joseph A.; Pust, Nathan J.] Montana State Univ, Elect & Comp Engn Dept, Bozeman, MT 59717 USA. [Piazzolla, Sabino] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Shaw, JA (reprint author), Montana State Univ, Elect & Comp Engn Dept, 610 Cobleigh Hall, Bozeman, MT 59717 USA. EM jshaw@ece.montana.edu NR 13 TC 0 Z9 0 U1 1 U2 5 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0739-0572 J9 J ATMOS OCEAN TECH JI J. Atmos. Ocean. Technol. PD NOV PY 2009 VL 26 IS 11 BP 2403 EP 2412 DI 10.1175/2009JTECHA1288.1 PG 10 WC Engineering, Ocean; Meteorology & Atmospheric Sciences SC Engineering; Meteorology & Atmospheric Sciences GA 521FA UT WOS:000271904500010 ER PT J AU Zheng, YH Zhang, YL Kozyra, JU Albert, J Bortnik, J Gallagher, DL Kessel, RL AF Zheng, Yihua Zhang, Yongliang Kozyra, Janet U. Albert, Jay Bortnik, Jacob Gallagher, Dennis L. Kessel, Ramona L. TI Toward an integrated view of inner magnetosphere and radiation belts Preface SO JOURNAL OF ATMOSPHERIC AND SOLAR-TERRESTRIAL PHYSICS LA English DT Editorial Material C1 [Zheng, Yihua; Zhang, Yongliang] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Kozyra, Janet U.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. [Albert, Jay] USAF, Res Lab, Space Vehicles Directorate, Hanscom AFB, MA USA. [Bortnik, Jacob] Univ Calif Los Angeles, Dept Atmospher & Ocean Sci, Los Angeles, CA USA. [Gallagher, Dennis L.] NASA, George C Marshall Space Flight Ctr, Dept Space Sci, Natl Space Sci & Technol Ctr, Huntsville, AL 35812 USA. [Kessel, Ramona L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Zheng, YH (reprint author), Johns Hopkins Univ, Appl Phys Lab, 11100 Johns Hopkins Rd, Laurel, MD 20723 USA. EM yihua.zheng@jhuapl.edu NR 0 TC 0 Z9 0 U1 0 U2 0 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1364-6826 J9 J ATMOS SOL-TERR PHY JI J. Atmos. Sol.-Terr. Phys. PD NOV PY 2009 VL 71 IS 16 BP 1613 EP 1613 DI 10.1016/j.jastp.2009.04.013 PG 1 WC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences SC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences GA 512KY UT WOS:000271249000001 ER PT J AU Glocer, A Toth, G Fok, M Gombosi, T Liemohn, M AF Glocer, A. Toth, G. Fok, M. Gombosi, T. Liemohn, M. TI Integration of the radiation belt environment model into the space weather modeling framework SO JOURNAL OF ATMOSPHERIC AND SOLAR-TERRESTRIAL PHYSICS LA English DT Article DE Modeling; Radiation belts; Inner Magnetosphere; MHD ID DAWN-DUSK ASYMMETRY; ELECTRON-FLUXES; RING CURRENT; MAGNETOSPHERE; MAGNETOHYDRODYNAMICS; SIMULATIONS; FIELD; SALAMMBO; EVENTS; SOLAR AB We have integrated the Fok radiation belt environment (RBE) model into the space weather modeling framework (SWMF). RBE is coupled to the global magnetohydrodynamics component (represented by the Block-Adaptive-Tree Solar-wind Roe-type Upwind Scheme, BATS-R-US, code) and the Ionosphere Electrodynamics component of the SWMF, following initial results using the Weimer empirical model for the ionospheric potential. The radiation belt (RB) model solves the convection-diffusion equation of the plasma in the energy range of 10 keV to a few MeV. In stand-alone mode RBE uses Tsyganenko's empirical models for the magnetic field, and Weimer's empirical model for the ionospheric potential. In the SWMF the BATS-R-US model provides the time dependent magnetic field by efficiently tracing the closed magnetic field-lines and passing the geometrical and field strength information to RBE at a regular cadence. The ionosphere electrodynamics component uses a two-dimensional vertical potential solver to provide new potential maps to the HE model at regular intervals. We discuss the coupling algorithm and show some preliminary results with the coupled code. We run our newly coupled model for periods of steady solar wind conditions and compare our results to the RB model using an empirical magnetic field and potential model. We also simulate the RB for an active time period and find that there are substantial differences in the RB model results when changing either the magnetic field or the electric field, including the creation of an outer belt enhancement via rapid inward transport on the time scale of tens of minutes. (C) 2009 Elsevier Ltd. All rights reserved. C1 [Glocer, A.; Toth, G.; Gombosi, T.; Liemohn, M.] Univ Michigan, Ctr Space Environm Modeling, Ann Arbor, MI 48109 USA. [Fok, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA. RP Glocer, A (reprint author), Univ Michigan, Ctr Space Environm Modeling, 2426 Space Res Bldg, Ann Arbor, MI 48109 USA. EM aglocer@umich.edu RI Gombosi, Tamas/G-4238-2011; Glocer, Alex/C-9512-2012; Fok, Mei-Ching/D-1626-2012; Liemohn, Michael/H-8703-2012; Toth, Gabor/B-7977-2013 OI Gombosi, Tamas/0000-0001-9360-4951; Glocer, Alex/0000-0001-9843-9094; Liemohn, Michael/0000-0002-7039-2631; Toth, Gabor/0000-0002-5654-9823 NR 39 TC 15 Z9 15 U1 0 U2 4 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1364-6826 EI 1879-1824 J9 J ATMOS SOL-TERR PHY JI J. Atmos. Sol.-Terr. Phys. PD NOV PY 2009 VL 71 IS 16 SI SI BP 1653 EP 1663 DI 10.1016/j.jastp.2009.01.003 PG 11 WC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences SC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences GA 512KY UT WOS:000271249000007 ER PT J AU Grebowsky, JM Benson, RF Webb, PA Truhlik, V Bilitza, D AF Grebowsky, Joseph M. Benson, Robert F. Webb, Phillip A. Truhlik, Vladimir Bilitza, Dieter TI Altitude variation of the plasmapause signature in the main ionospheric trough SO JOURNAL OF ATMOSPHERIC AND SOLAR-TERRESTRIAL PHYSICS LA English DT Article DE Plasmapause; Ionosphere; Midlatitude; Trough ID LIGHT-ION TROUGH; ELECTRON-DENSITY PROFILES; MID-LATITUDE TROUGH; MAGNETOSPHERIC CONVECTION; PROBE MEASUREMENTS; MODEL AB The projection of the plasmapause magnetic-field lines to low altitudes, where the light-ion chemistry is dominated by O+, tends to occur near the minimum electron density in the main (midlatitude) electron density trough at night. With increasing altitude in the trough. where H+ emerges as the dominant ion on the low-latitude boundary, we have found cases where the plasmapause field lines are located on the sharp low-latitude side of the trough as expected if this topside ionosphere H+ distribution varies in step with the plasmapause gradient in the distant plasmasphere. These conclusions are based on near-equatorial crossings of the plasmapause (corresponding to the steep gradient in the dominant species H+) by the Explorer-45 satellite as determined from electric-field measurements by Maynard and Cauffman in the early 1970s and ISIS-2 ionospheric topside-sounder measurements. The former data have now been converted to digital form and made available at http://nssdcftp.gsfc.nasa.gov. The latter provide samples of nearly coincident observations of ionospheric main trough crossings near the same magnetic-field lines of the Explorer 45-determined equatorial plasmapause. The ISIS-2 vertical electron density profiles are used to infer where the F-region transitions from an O+ to a H+ dominated plasma through the main trough boundaries. Published by Elsevier Ltd. C1 [Grebowsky, Joseph M.] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Planetary Magnetospheres Lab, Greenbelt, MD 20771 USA. [Benson, Robert F.] NASA, Goddard Space Flight Ctr, Geospace Phys Lab, Heliophys Sci Div, Greenbelt, MD 20771 USA. [Webb, Phillip A.] NASA, Goddard Space Flight Ctr, GEST UMBC Space Weather Lab, Heliophys Sci Div, Greenbelt, MD 20771 USA. [Truhlik, Vladimir] Acad Sci Czech Republic, Inst Atmospher Phys, Prague, Czech Republic. [Bilitza, Dieter] NASA, Goddard Space Flight Ctr, GMU Heliospher Phys Lab, Heliophys Sci Div, Greenbelt, MD 20771 USA. RP Grebowsky, JM (reprint author), NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Planetary Magnetospheres Lab, Code 695, Greenbelt, MD 20771 USA. EM joseph.m.grebowsky@nasa.gov RI Grebowsky, Joseph/I-7185-2013; Truhlik, Vladimir/H-6971-2014 OI Truhlik, Vladimir/0000-0002-6624-4388 FU Characterizing the composition of large midlatitude topside ionospheric and plasmaspheric gradients; Grant Agency of the Academy of Sciences of the Czech Republic [A300420603]; National Space Club Scholars Program FX This work is based on a NASA Living with A Star (LWS) supported research effort "Characterizing the composition of large midlatitude topside ionospheric and plasmaspheric gradients" led by R. Benson. It is part of a larger LWS Targeted Research and Technology (TR&T) research group effort focusing on "Global Distribution, Sources and Effects of Large Density Gradients" led by R. Heelis. V.T. was Supported, in part, by grant A300420603 of the Grant Agency of the Academy of Sciences of the Czech Republic. We acknowledge the industrious work of Sahil S. Shah, a High School Senior supported by the National Space Club Scholars Program, for scanning and digitizing the Explorer 45 data. Helpful comments of the two referees are also acknowledged. The ISIS topside-sounder data were provided by NASA's Space Physics Data Facility and National Space Science Data Center. NR 32 TC 3 Z9 3 U1 0 U2 0 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1364-6826 EI 1879-1824 J9 J ATMOS SOL-TERR PHY JI J. Atmos. Sol.-Terr. Phys. PD NOV PY 2009 VL 71 IS 16 SI SI BP 1669 EP 1676 DI 10.1016/j.jastp.2009.05.016 PG 8 WC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences SC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences GA 512KY UT WOS:000271249000009 ER PT J AU Cicia, AM Driggers, WB Ingram, GW Kneebone, J Tsang, PCW Koester, DM Sulikowski, JA AF Cicia, A. M. Driggers, W. B., III Ingram, G. W., Jr. Kneebone, J. Tsang, P. C. W. Koester, D. M. Sulikowski, J. A. TI Size and age estimates at sexual maturity for the little skate Leucoraja erinacea from the western Gulf of Maine, USA SO JOURNAL OF FISH BIOLOGY LA English DT Article DE elasmobranch; hormones; oxytetracycline; rajidae; reproduction ID RHIZOPRIONODON-TERRAENOVAE RICHARDSON; ATLANTIC SHARPNOSE SHARK; REPRODUCTIVE-BIOLOGY; WINTER SKATE; ELASMOBRANCH FISHES; AMBLYRAJA-RADIATA; GONAD DEVELOPMENT; STEROID-HORMONES; SOUTHERN AFRICA; LIFE-HISTORY AB Size and age estimates at sexual maturity were determined for 162 male and 273 female little skates Leucoraja erinacea collected from the western Gulf of Maine. Maturity ogives suggest that 50% maturity in females occurs at age 9.5 years and 480 mm total length (L(T)), whereas 50% maturity in males occurs at a slightly younger age of 7.7 years and smaller size of 460 mm L(T). Age estimates were made from 389 L. erinacea ranging in size from 93 to 570 mm L(T). The index of average per cent error and age-bias plots indicated that the ageing methods were precise and non-biased. Additionally, annual periodicity of band formation was validated with oxytetracycline in eight individuals (three males and five females) ranging in age from 3 to 12 years. In conclusion, results from this study indicate that L. erinacea exhibits characteristics that make other elasmobranch populations highly susceptible to overexploitation. C1 [Cicia, A. M.; Sulikowski, J. A.] Univ New England, Ctr Marine Sci, Biddeford, ME 04005 USA. [Driggers, W. B., III; Ingram, G. W., Jr.] SE Fisheries Sci Ctr, Natl Marine Fisheries Serv, Mississippi Labs, Pascagoula, MS 39568 USA. [Kneebone, J.; Tsang, P. C. W.] Univ New Hampshire, Dept Anim & Nutr Sci, Durham, NH 03824 USA. [Koester, D. M.] Univ New England, Coll Osteopath Med, Dept Anat, Biddeford, ME 04005 USA. RP Cicia, AM (reprint author), Univ New England, Ctr Marine Sci, 11 Hills Beach Rd, Biddeford, ME 04005 USA. EM acicia@mail.une.edu FU College of Arts and Sciences Dean Office; Biology Department FX We thank C. Felch of the F. V. Lady Victoria and J. King of the Massachusetts (DMR) for the collection of the skates. We further extend our gratitude to N. Furey and A. Wargo for their help in animal dissections and for the maintenance of the skates at the UNE MSC. This project was supported by a UNE Honors Program, College of Arts and Sciences Dean Office and the Biology Department. MSC contribution number 21. NR 47 TC 9 Z9 9 U1 0 U2 9 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0022-1112 J9 J FISH BIOL JI J. Fish Biol. PD NOV PY 2009 VL 75 IS 7 BP 1648 EP 1666 DI 10.1111/j.1095-8649.2009.02392.x PG 19 WC Fisheries; Marine & Freshwater Biology SC Fisheries; Marine & Freshwater Biology GA 528JT UT WOS:000272441000010 PM 20738640 ER PT J AU Rademacher, BJ Lu, P Strahan, AL Cerimele, CJ AF Rademacher, Branden J. Lu, Ping Strahan, Alan L. Cerimele, Christopher J. TI In-Flight Trajectory Planning and Guidance for Autonomous Parafoils SO JOURNAL OF GUIDANCE CONTROL AND DYNAMICS LA English DT Article; Proceedings Paper CT AIAA Guidance, Navigation and Control Conference CY AUG 18-21, 2009 CL Honolulu, HI SP AIAA ID CURVATURE; VEHICLE; MASS AB This paper presents a framework for onboard trajectory planning and guidance for a large class of autonomously guided parafoils. The problem is for the parafoil to reach a given location at a specified altitude with a specified final heading. Through appropriate change of the independent variable, the trajectory planning problem is converted from a three-dimensional free-final-time problem to a two-dimensional fixed-final-time problem. Using the well-known Dubins path synthesis and known parafoil performance parameters, a concept of altitude margin is developed as a quantitative measure of the available maneuvering energy for use in trajectory planning. A hybrid strategy using two methods to generate kinematically feasible fixed-time trajectories is presented, each targeting a different range of initial values of the altitude margin. The trajectory can be replanned onboard in every guidance cycle, making the guidance effectively closed-loop, or replanned whenever the actual deviation of the actual condition from the reference trajectory exceeds a threshold. The proposed planning and guidance algorithm applies to a large class of parafoil canopies and payloads, which encompasses wide variations in the lift-to-drag ratio, wing loading, and maximum turn rate. The guidance logic has the potential of requiring little or no tuning to accommodate variations in canopy performance. Monte Carlo simulations are conducted to evaluate the effectiveness of the algorithm with dispersions in canopy performance, loading, wind profile errors, navigation uncertainty, using lateral control only, and using both longitudinal and lateral control. C1 [Rademacher, Branden J.; Lu, Ping] Iowa State Univ, Dept Aerosp Engn, Ames, IA 50011 USA. [Cerimele, Christopher J.] NASA, Lyndon B Johnson Space Ctr, Flight Mech & Trajectory Design Branch, Houston, TX 77058 USA. RP Rademacher, BJ (reprint author), Iowa State Univ, Dept Aerosp Engn, 2271 Howe Hall,Room 1200, Ames, IA 50011 USA. EM plu@iastate.edu NR 29 TC 14 Z9 15 U1 0 U2 6 PU AMER INST AERONAUT ASTRONAUT PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0731-5090 J9 J GUID CONTROL DYNAM JI J. Guid. Control Dyn. PD NOV-DEC PY 2009 VL 32 IS 6 BP 1697 EP 1712 DI 10.2514/1.44862 PG 16 WC Engineering, Aerospace; Instruments & Instrumentation SC Engineering; Instruments & Instrumentation GA 527KV UT WOS:000272366900001 ER PT J AU Bailey, RE Jackson, EB Goodrich, KH Al Ragsdale, W Neuhaus, J Barnes, J AF Bailey, Randall E. Jackson, E. Bruce Goodrich, Kenneth H. Al Ragsdale, W. Neuhaus, Jason Barnes, Jim TI Investigation of Reaction Control System Design on Spacecraft Handling Qualities for Docking SO JOURNAL OF GUIDANCE CONTROL AND DYNAMICS LA English DT Article; Proceedings Paper CT AIAA Atmospheric Flight Mechanics Conference CY AUG 18-21, 2008 CL Honolulu, HI SP AIAA ID PROXIMITY OPERATIONS AB A program of research, development, test, and evaluation is planned for the development of spacecraft handling qualities guidelines. In this first experiment, the effects of reaction control system design characteristics and rotational control laws were evaluated during simulated proximity operations and docking. Also, the influence of piloting demands resulting from varying closure rates was assessed. The pilot-in-the-loop simulation results showed that significantly different spacecraft handling qualities result from the design of the reaction control system. In particular, cross coupling between translational and rotational motions significantly affected handling qualities as reflected by Cooper-Harper pilot ratings and pilot workload, as reflected by Task Load Index ratings. This influence is masked (but only slightly) by the rotational control system mode. Although rotational control augmentation using rate command/attitude hold can reduce the workload (principally, physical workload) created by cross coupling, the handling qualities are not significantly improved. The attitude and rate deadbands of the rate command/attitude hold introduced significant mental workload and control compensation to evaluate when deadband firings would occur, assess their impact on docking performance, and apply control inputs to mitigate that impact. C1 [Bailey, Randall E.] NASA, Langley Res Ctr, Crew Syst & Aviat Operat Branch, Hampton, VA 23681 USA. [Jackson, E. Bruce; Goodrich, Kenneth H.] NASA, Langley Res Ctr, Dynam Syst & Guidance Branch, Hampton, VA 23681 USA. [Al Ragsdale, W.; Neuhaus, Jason] Unisys Corp, Simulat Dev & Anal Branch, Hampton, VA 23681 USA. [Barnes, Jim] ARINC Inc, Simulat Dev & Anal Branch, Hampton, VA 23666 USA. RP Bailey, RE (reprint author), NASA, Langley Res Ctr, Crew Syst & Aviat Operat Branch, Mail Stop 152, Hampton, VA 23681 USA. NR 21 TC 7 Z9 7 U1 1 U2 4 PU AMER INST AERONAUT ASTRONAUT PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0731-5090 J9 J GUID CONTROL DYNAM JI J. Guid. Control Dyn. PD NOV-DEC PY 2009 VL 32 IS 6 BP 1723 EP 1735 DI 10.2514/1.44688 PG 13 WC Engineering, Aerospace; Instruments & Instrumentation SC Engineering; Instruments & Instrumentation GA 527KV UT WOS:000272366900003 ER PT J AU Boskovic, JD Jackson, JA Mehra, RK Nguyen, NT AF Boskovic, Jovan D. Jackson, Joseph A. Mehra, Raman K. Nguyen, Nhan T. TI Multiple-Model Adaptive Fault-Tolerant Control of a Planetary Lander SO JOURNAL OF GUIDANCE CONTROL AND DYNAMICS LA English DT Article; Proceedings Paper CT AIAA Guidance, Navigation and Control Conference and Exhibit CY AUG 18-21, 2008 CL Honolulu, HI SP Amer Inst Aeronaut & Astronaut (AIAA) ID FLIGHT CONTROL-DESIGN; FAILURES; SYSTEM; DAMAGE AB In this paper we present an approach to fault-tolerant control based on multiple models, switching, and tuning and its implementation to a hardware-in-the-loop simulation of Delta Clipper Experimental dynamics. The Delta Clipper Experimental is characterized by large control input redundancy, which made it an ideal test bed for evaluation of advanced fault-tolerant and adaptive reconfigurable control strategies. The overall failure detection, identification, and accommodation architecture is an upgraded version of our Fast Online Actuator Reconfiguration Enhancement (FLARE) system. The FLARE approach is based on representing different possible fault and failure scenarios using multiple observers, such that the case of nominal (no-failure) operation is covered along with the loss-of-effectiveness, lock-in-place, and hardover failures of the flight control effectors. Based on a suitably chosen performance criterion, the FLARE system quickly detects single or multiple failures and reconfigures the controls, thus achieving either the original desired performance or graceful performance degradation. In the first stage of the project, the FLARE system was tested on a medium-fidelity simulation of Delta Clipper Experimental dynamics, resulting in excellent performance over a large range of single and multiple faults and failures. Following that, in collaboration with Boeing Phantom Works, the FLARE run-time code was installed at their site and tested on a hardware-in-the-loop test bed consisting of an electromechanical actuator actuating a gimballed engine as a part of a simulation of the Delta Clipper Experimental dynamics. A large number of hardware-in-the-loop simulations were run to cover a dense test-case matrix, including cases of up to 10 simultaneous control effector failures. In all cases FLARE was able to quickly and accurately detect the failures and reconfigure the controls, resulting in excellent overall system performance. In this paper we describe the Delta Clipper Experimental and its dynamics model, along with the multiple models, switching, and tuning based modification of our FLARE system. This is followed by a description of the experimental test bed and a discussion of the results obtained through hardware-in-the-loop testing. C1 [Boskovic, Jovan D.] Sci Syst Co Inc, Intelligent & Autonomous Control Syst Grp, Woburn, MA 01801 USA. [Jackson, Joseph A.] Sci Syst Co Inc, Intelligent & Autonomous Control Syst, Woburn, MA 01801 USA. [Nguyen, Nhan T.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Boskovic, JD (reprint author), Sci Syst Co Inc, Intelligent & Autonomous Control Syst Grp, 500 W Cummings Pk,Suite 3000, Woburn, MA 01801 USA. EM jovan@ssci.com; jjackson@ssci.com; rkm@ssci.com; Nhan.T.Nguyen@nasa.gov NR 17 TC 37 Z9 43 U1 1 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 NOV-DEC PY 2009 VL 32 IS 6 BP 1812 EP 1826 DI 10.2514/1.42719 PG 15 WC Engineering, Aerospace; Instruments & Instrumentation SC Engineering; Instruments & Instrumentation GA 527KV UT WOS:000272366900010 ER PT J AU Anderson, RL Lo, MW AF Anderson, Rodney L. Lo, Martin W. TI Role of Invariant Manifolds in Low-Thrust Trajectory Design SO JOURNAL OF GUIDANCE CONTROL AND DYNAMICS LA English DT Article AB This paper demonstrates the significant role that invariant manifolds play in the dynamics of low-thrust trajectories moving through unstable regions in the three-body problem. It shows that an optimization algorithm incorporating no knowledge of invariant manifolds converges on low-thrust trajectories that use the invariant manifolds of unstable resonant orbits to traverse resonances. It is determined that the algorithm could both change the energy through thrusting to a level where the invariant manifolds could more easily be used, as well as use thrusting to move the trajectory along the invariant manifolds. Knowledge of this relationship has the potential to be very useful in developing initial guesses and new control laws for these optimization algorithms. In particular, this approach can speed up the convergence of the optimization process, retain the essential geometric and topological characteristics of the initial design, and provide a more accurate estimate of the Delta V and fuel usage based on the initial trajectory. C1 [Anderson, Rodney L.] Univ Colorado, Colorado Ctr Astrodynam Res, Boulder, CO 80309 USA. [Lo, Martin W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Anderson, RL (reprint author), Univ Colorado, Colorado Ctr Astrodynam Res, Campus Box 431, Boulder, CO 80309 USA. OI Anderson, Rodney/0000-0001-5336-2775 FU NASA Advanced Information Systems Research Program FX Many thanks to Try Lam and Greg Whiffen for supplying the low-thrust trajectory developed in Mystic. Thanks also to Greg Whiffen for adapting his Mystic code to the circular restricted three-body problem for the trajectory and for his consultations on Mystic. The authors would like to thank George Bom and Bob Easton for their support and their many helpful discussions. This work was conducted in part at the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA. It was Supported in part by the Prometheus Project as well as the Episode Project and the Wool Project of the NASA Advanced Information Systems Research Program. The parallel computation used in this investigation was provided by the Jet Propulsion Laboratory Supercomputer Project and the Jet Propulsion Laboratory Supercomputing and Visualization Facility. NR 24 TC 20 Z9 20 U1 0 U2 5 PU AMER INST AERONAUT ASTRONAUT PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0731-5090 J9 J GUID CONTROL DYNAM JI J. Guid. Control Dyn. PD NOV-DEC PY 2009 VL 32 IS 6 BP 1921 EP 1930 DI 10.2514/1.37516 PG 10 WC Engineering, Aerospace; Instruments & Instrumentation SC Engineering; Instruments & Instrumentation GA 527KV UT WOS:000272366900019 ER PT J AU Stebner, A Padula, S Noebe, R Lerch, B Quinn, D AF Stebner, Aaron Padula, Santo, II Noebe, Ronald Lerch, Bradley Quinn, Dane TI Development, Characterization, and Design Considerations of Ni19.5Ti50.5Pd25Pt5 High-temperature Shape Memory Alloy Helical Actuators SO JOURNAL OF INTELLIGENT MATERIAL SYSTEMS AND STRUCTURES LA English DT Article DE shape memory alloy; shape memory spring; helical actuator; high temperature; shape memory effect; thermal actuator; NiTiPdPt; NiTi ID WIND-TUNNEL TEST; CRYSTALLOGRAPHY AB Shape memory alloys (SMAs) have been used in various applications since their discovery. However, their use as actuation devices in high-temperature environments has been limited due to the temperature constraints of commercially available materials. Recently, SMAs that produce good work characteristics at elevated temperatures have been developed at NASA's Glenn Research Center. One such alloy, Ni19.5Ti50.5Pd25Pt5, has shown repeatable strain recovery on the order of 2.5% in the presence of an externally applied stress at temperatures greater than 250 degrees C. Based on these findings, potential applications for this alloy are being explored and further work is being done to assess the use of this alloy in various structural forms. In this article, the characterization of Ni19.5Ti50.5Pd25Pt5 helical actuators is reported, including their mechanical responses and how variations in their responses correlate to changes in geometric parameters and training loads. Finally, implementation of previously published SMA spring design methodology in future SMA helical actuator development is considered through comparison of the observed and predicted responses. C1 [Stebner, Aaron] Northwestern Univ, Dept Mech Engn, Evanston, IL 60208 USA. [Padula, Santo, II; Noebe, Ronald; Lerch, Bradley] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. [Quinn, Dane] Univ Akron, Dept Mech Engn, Auburn Sci & Engn Ctr, Akron, OH 44325 USA. RP Stebner, A (reprint author), Northwestern Univ, Dept Mech Engn, 2145 Sheridan Rd, Evanston, IL 60208 USA. EM a-stebner@u.northwestern.edu RI Quinn, Dane/D-4757-2009; Stebner, Aaron/A-7685-2015 OI Quinn, Dane/0000-0001-7790-7768; FU NASA's Graduate Student Researchers Program; Fundamental Aeronautics Program; Telezygology, Inc.; GSRP Fellowship FX This work was funded through NASA's Graduate Student Researchers Program, the Fundamental Aeronautics Program - Subsonic Fixed Wing Project, and Telezygology, Inc. The authors acknowledge and thank Dr Dexter Johnson for sponsoring the primary author's GSRP Fellowship. The authors also thank the journal reviewers and Dr Raj Vaidyanathan for tremendous feedback on early versions of this manuscript. NR 34 TC 24 Z9 24 U1 0 U2 10 PU SAGE PUBLICATIONS LTD PI LONDON PA 1 OLIVERS YARD, 55 CITY ROAD, LONDON EC1Y 1SP, ENGLAND SN 1045-389X J9 J INTEL MAT SYST STR JI J. Intell. Mater. Syst. Struct. PD NOV PY 2009 VL 20 IS 17 BP 2107 EP 2126 DI 10.1177/1045389X09347018 PG 20 WC Materials Science, Multidisciplinary SC Materials Science GA 514RV UT WOS:000271414200007 ER PT J AU Crucian, B Sams, C AF Crucian, Brian Sams, Clarence TI Immune system dysregulation during spaceflight: clinical risk for exploration-class missions SO JOURNAL OF LEUKOCYTE BIOLOGY LA English DT Letter DE adaptive immunity; innate immunity; space flight ID ASTRONAUTS; VIRUS; REACTIVATION C1 [Crucian, Brian] NASA, JSC Wyle, Houston, TX 77059 USA. [Sams, Clarence] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. RP Crucian, B (reprint author), NASA, JSC Wyle, 1290 Hercules Dr, Houston, TX 77059 USA. EM brian.crucian-1@nasa.gov NR 14 TC 31 Z9 36 U1 4 U2 13 PU FEDERATION AMER SOC EXP BIOL PI BETHESDA PA 9650 ROCKVILLE PIKE, BETHESDA, MD 20814-3998 USA SN 0741-5400 J9 J LEUKOCYTE BIOL JI J. Leukoc. Biol. PD NOV PY 2009 VL 86 IS 5 BP 1017 EP 1018 DI 10.1189/jlb.0709500 PG 2 WC Cell Biology; Hematology; Immunology SC Cell Biology; Hematology; Immunology GA 512SJ UT WOS:000271270600001 PM 19875627 ER PT J AU Trease, B Kota, S AF Trease, Brian Kota, Sridhar TI Design of Adaptive and Controllable Compliant Systems With Embedded Actuators and Sensors SO JOURNAL OF MECHANICAL DESIGN LA English DT Article CT ASME International Design Engineering Technical Conference/Computers and Information in Engineering Conference CY SEP 10-13, 2006 CL Philadelphia, PA SP ASME ID SMART STRUCTURES; TOPOLOGY OPTIMIZATION; OPTIMAL PLACEMENT; MECHANISMS; ALGORITHMS; LOCATION AB We present a framework for the design of a compliant system, i.e., the concurrent design of a compliant mechanism with embedded actuators and sensors. Our methods simultaneously synthesize optimal structural topology and component placement for maximum energy efficiency and adaptive performance, while satisfying various weight and performance constraints. The goal of this research is to lay an algorithmic framework for distributed actuation and sensing within a compliant active structure. Key features of the methodology include (1) the simultaneous optimization of the location, orientation, and size of actuators (and sensors) concurrent with the compliant transmission topology, and (2) the implementation of controllability and observability concepts (both arising from consideration of control) in compliant systems design. The methods used include genetic algorithms, graph searches for connectivity, and multiple load cases implemented with linear finite element analysis. Actuators, modeled as both force generators and structural compliant elements, are included as topology variables in the optimization. The results from the controllability problem are used to motivate and describe the analogous extension to observability for sensing. Results are provided for several studies, including (1) concurrent actuator placement and topology design for a compliant amplifier, (2) a shape-morphing aircraft wing demonstration with three controlled output nodes, and (3) a load-distribution sensing wing structure with internal sensors. Central to this method is the concept of structure/component orthogonality, which refers to the unique system response for each component (actuator or sensor) it contains. [DOI:10.1115/1.3149848] C1 [Trease, Brian] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Kota, Sridhar] Univ Michigan, Dept Mech Engn, Ann Arbor, MI 48109 USA. RP Trease, B (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM trease@asme.org; kota@umich.edu NR 33 TC 10 Z9 11 U1 5 U2 23 PU ASME-AMER SOC MECHANICAL ENG PI NEW YORK PA THREE PARK AVE, NEW YORK, NY 10016-5990 USA SN 1050-0472 J9 J MECH DESIGN JI J. Mech. Des. PD NOV PY 2009 VL 131 IS 11 AR 111001 DI 10.1115/1.3149848 PG 12 WC Engineering, Mechanical SC Engineering GA 507BP UT WOS:000270825300001 ER PT J AU Nitschke, W Russell, MJ AF Nitschke, Wolfgang Russell, Michael J. TI Hydrothermal Focusing of Chemical and Chemiosmotic Energy, Supported by Delivery of Catalytic Fe, Ni, Mo/W, Co, S and Se, Forced Life to Emerge SO JOURNAL OF MOLECULAR EVOLUTION LA English DT Review DE Origin of life; Hydrothermal vent; Chemiosmosis; Chemoautotrophy; LUCA ID IRON-SULFUR CLUSTERS; INORGANIC PYROPHOSPHATE; EARLY EVOLUTION; GENETIC-CODE; AMINO-ACIDS; EARLY EARTH; RHODOSPIRILLUM-RUBRUM; H+-PYROPHOSPHATASE; COEVOLUTION THEORY; ESCHERICHIA-COLI AB Energised by the protonmotive force and with the intervention of inorganic catalysts, at base Life reacts hydrogen from a variety of sources with atmospheric carbon dioxide. It seems inescapable that life emerged to fulfil the same role (i.e., to hydrogenate CO(2)) on the early Earth, thus outcompeting the slow geochemical reduction to methane. Life would have done so where hydrothermal hydrogen interfaced a carbonic ocean through inorganic precipitate membranes. Thus we argue that the first carbon-fixing reaction was the molybdenum-dependent, proton-translocating formate hydrogenlyase system described by Andrews et al. (Microbiology 143: 3633-3647, 1997), but driven in reverse. Alkaline on the inside and acidic and carbonic on the outside - a submarine chambered hydrothermal mound built above an alkaline hydrothermal spring of long duration - offered just the conditions for such a reverse reaction imposed by the ambient protonmotive force. Assisted by the same inorganic catalysts and potential energy stores that were to evolve into the active centres of enzymes supplied variously from ocean or hydrothermal system, the formate reaction enabled the rest of the acetyl coenzyme-A pathway to be followed exergonically, first to acetate, then separately to methane. Thus the two prokaryotic domains both emerged within the hydrothermal mound-the acetogens were the forerunners of the Bacteria and the methanogens were the forerunners of the Archaea. C1 [Russell, Michael J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Nitschke, Wolfgang] CNRS, Lab Bioenerget & Ingn Prot, UPR9036, IFR88, F-13402 Marseille 20, France. RP Russell, MJ (reprint author), CALTECH, Jet Prop Lab, Sect 3220,MS 183-601,4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM michael.j.russell@jpl.nasa.gov OI Nitschke, Wolfgang/0000-0003-2084-3032 FU French Agence Nationale pour la Recherche [ANR06-BLAN-0384]; NASA's Astrobiology Institute (Icy Worlds) FX We thank Anne-Lise Ducluzeau, Allan Hall, Isik Kanik, Bill Martin, Randall Mielke, Shawn McGlynn, Carola Schulzke and Anne Volbeda for help and support. WN was financially supported by the French Agence Nationale pour la Recherche (ANR06-BLAN-0384). MJR's research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration: Exobiology and Evolutionary Biology and supported by NASA's Astrobiology Institute (Icy Worlds). NR 117 TC 57 Z9 57 U1 7 U2 49 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0022-2844 J9 J MOL EVOL JI J. Mol. Evol. PD NOV PY 2009 VL 69 IS 5 BP 481 EP 496 DI 10.1007/s00239-009-9289-3 PG 16 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA 530FJ UT WOS:000272574100008 PM 19911220 ER PT J AU Ram, RS Yu, S Gordon, I Bernath, PF AF Ram, R. S. Yu, S. Gordon, I. Bernath, P. F. TI Fourier transform infrared emission spectroscopy of new systems of NiS SO JOURNAL OF MOLECULAR SPECTROSCOPY LA English DT Article DE Fourier transform emission spectroscopy; Near infrared spectroscopy; Rotational analysis; Transition metal sulfides ID LASER-INDUCED FLUORESCENCE; LOW-LYING STATES; ROTATIONAL ANALYSIS; EXCITED-STATES; IDENTIFICATION; TRANSITION; NICL; RESOLUTION; SPECTRUM; OXIDES AB The emission spectrum of NiS has been investigated in the near infrared in the 2000-7500 cm(-1) region using a Fourier transform spectrometer. New bands observed in the 3000-5000 cm(-1) region have been assigned to a (3)Pi(i)-X(3)Sigma(-) transition analogous to the transition of NiO observed in the near infrared [R.S. Ram and P.F. Bernath, J. Mol. Spectrosc. 155 (1992) 315-325]. The 0-0 band of NiS consists of (3)Pi(0+)-X(3)Sigma(-)(1) (4399 cm(-1)), (3)Pi(0-)-X(3)Sigma(-) (4257 cm(-1)), (3)Pi(1)-X(3)Sigma(-)(0+) (3938 cm(-1)), and (3)Pi(2)-X(3)Sigma(-)(1) (3325 cm(-1)) sub-bands. To higher wavenumbers, another [Omega = 1] - X(3)Sigma(-)(0+) transition has been observed with a 0-0 R head near 5887 cm(-1). This transition has been assigned as (1)Pi-X(3)Sigma(-)(0+), although a (3)Pi(1)-X(3)Sigma(-)(0+) assignment is also possible. Several vibrational bands belonging to different sub-bands were rotationally analyzed and spectroscopic constants evaluated. Our spectroscopic constants for the ground state agree well with the values reported in the microwave Study by Yamamoto et al. [T. Yamamoto, N. Tanimoto, T. Okabayashi. Phys. Chem. Chem. Phys. 9 (2007) 3744-3748]. (C) 2009 Elsevier Inc. All rights reserved. C1 [Ram, R. S.; Bernath, P. F.] Univ Arizona, Dept Chem, Tucson, AZ 85721 USA. [Yu, S.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Gordon, I.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bernath, P. F.] Univ Waterloo, Dept Chem, Waterloo, ON N2L 3G1, Canada. [Bernath, P. F.] Univ York, Dept Chem, York YO10 5DD, N Yorkshire, England. RP Ram, RS (reprint author), Univ Arizona, Dept Chem, Room 133,Old Chem Bldg,1306 E Univ Blvd, Tucson, AZ 85721 USA. EM rram@u.arizona.edu RI Bernath, Peter/B-6567-2012; Yu, Shanshan/D-8733-2016; OI Bernath, Peter/0000-0002-1255-396X; Gordon, Iouli/0000-0003-4763-2841 FU NASA; Natural Sciences and Engineering Research Council (NSERC) of Canada; UK Engineering and Physical Sciences Research Council (EPSRC) FX The research described here was partially supported by funds from the NASA laboratory astrophysics program. Some support was also provided by the Natural Sciences and Engineering Research Council (NSERC) of Canada and the UK Engineering and Physical Sciences Research Council (EPSRC). NR 32 TC 1 Z9 1 U1 0 U2 11 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0022-2852 J9 J MOL SPECTROSC JI J. Mol. Spectrosc. PD NOV-DEC PY 2009 VL 258 IS 1-2 BP 20 EP 25 DI 10.1016/j.jms.2009.08.013 PG 6 WC Physics, Atomic, Molecular & Chemical; Spectroscopy SC Physics; Spectroscopy GA 528BJ UT WOS:000272414800004 ER PT J AU Kisiel, Z Pszczolkowski, L Drouin, BJ Brauer, CS Yu, SS Pearson, JC AF Kisiel, Zbigniew Pszczolkowski, Lech Drouin, Brian J. Brauer, Carolyn S. Yu, Shanshan Pearson, John C. TI The rotational spectrum of acrylonitrile up to 1.67 THz SO JOURNAL OF MOLECULAR SPECTROSCOPY LA English DT Article DE THz spectroscopy; Rotational spectrum; Interstate interactions; Coriolis coupling; Fermi resonance; Astrophysical species ID SUBMILLIMETER-WAVE SPECTRUM; CHLORINE NITRATE CLONO2; ELECTRIC-DIPOLE MOMENTS; VINYL CYANIDE; VIBRATION-ROTATION; MILLIMETER-WAVE; MOLECULAR-STRUCTURE; HYPERFINE-STRUCTURE; MICROWAVE-SPECTRUM; DIETHYL-ETHER AB The rotational spectrum of acrylonitrile was studied up to 1.67 THz by recording and analysing several extended spectral segments spanning a total of over 540 GHz. The spectra were obtained with cascaded harmonic multiplication techniques, and the ground state data set was extended to over 3000 lines, J = 129, and includes transitions up to K(a) = 30. At high-J and K(a) several manifestations of a perturbation between the ground state and the lowest excited vibrational state, v(11) = 1, were observed. The perturbed frequencies were successfully fitted with a coupled fit of the two states resulting in E(11) = 228.29991(2) cm(-1). The results reported for the parent species of acrylonitrile should allow confident prediction of the major features over the whole envelope of the measurable rotational spectrum. New measurements and spectroscopic constants for the ground states of the three single (13)C isotopic species and for the (15)N species are also reported. (C) 2009 Elsevier Inc. All rights reserved. C1 [Kisiel, Zbigniew; Pszczolkowski, Lech] Polish Acad Sci, Inst Phys, PL-02668 Warsaw, Poland. [Drouin, Brian J.; Brauer, Carolyn S.; Yu, Shanshan; Pearson, John C.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Kisiel, Z (reprint author), Polish Acad Sci, Inst Phys, Al Lotnikow 32-46, PL-02668 Warsaw, Poland. EM kisiel@ifpan.edu.pl RI Yu, Shanshan/D-8733-2016; Kisiel, Zbigniew/K-8798-2016; Pszczolkowski, Lech/S-3018-2016 OI Kisiel, Zbigniew/0000-0002-2570-3154; FU Polish Ministry of Science and Higher Education [N-N202-0541-33] FX This paper presents research carried out at the jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. The Warsaw authors acknowledge financial support from the Polish Ministry of Science and Higher Education, Grant No. N-N202-0541-33. NR 36 TC 20 Z9 20 U1 2 U2 11 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0022-2852 J9 J MOL SPECTROSC JI J. Mol. Spectrosc. PD NOV-DEC PY 2009 VL 258 IS 1-2 BP 26 EP 34 DI 10.1016/j.jms.2009.08.011 PG 9 WC Physics, Atomic, Molecular & Chemical; Spectroscopy SC Physics; Spectroscopy GA 528BJ UT WOS:000272414800005 ER PT J AU Jin, X Dong, CM Kurian, J McWilliams, JC Chelton, DB Li, ZJ AF Jin, Xin Dong, Changming Kurian, Jaison McWilliams, James C. Chelton, Dudley B. Li, Zhijin TI SST-Wind Interaction in Coastal Upwelling: Oceanic Simulation with Empirical Coupling SO JOURNAL OF PHYSICAL OCEANOGRAPHY LA English DT Article ID SEA-SURFACE TEMPERATURE; CALIFORNIA CURRENT SYSTEM; ATMOSPHERIC BOUNDARY-LAYER; EKMANS THEORY; STRESS CURL; WEST-COAST; MODEL; ADJUSTMENT; VELOCITY; FLOW AB Observations, primarily from satellites, have shown a statistical relationship between the surface wind stress and underlying sea surface temperature (SST) on intermediate space and time scales, in many regions inclusive of eastern boundary upwelling current systems. In this paper, this empirical SST-wind stress relationship is utilized to provide a simple representation of mesoscale air-sea coupling for an oceanic model forced by surface winds, namely, the Regional Oceanic Modeling System (ROMS). This model formulation is applied to an idealized upwelling problem with prevailing equatorward winds to determine the coupling consequences on flow, SST, stratification, and wind evolutions. The initially uniform wind field adjusts through coupling to a cross-shore profile with weaker nearshore winds, similar to realistic ones. The modified wind stress weakens the nearshore upwelling circulation and increases SST in the coastal zone. The SST-induced wind stress curl strengthens offshore upwelling through Ekman suction. The total curl-driven upwelling exceeds the coastal upwelling. The SST-induced changes in the nearshore wind stress field also strengthen and broaden the poleward undercurrent. The coupling also shows significant impact on the developing mesoscale eddies by damaging cyclonic eddies more than anticyclonic eddies, which leads to dominance by the latter. Dynamically, this is a consequence of cyclones with stronger SST gradients that induce stronger wind perturbations in this particular upwelling problem and that are therefore generally more susceptible to disruption than anticyclones at finite Rossby number. The net effect is a weakening of eddy kinetic energy. C1 [Jin, Xin; Dong, Changming; Kurian, Jaison; McWilliams, James C.] Univ Calif Los Angeles, IGPP, Los Angeles, CA 90095 USA. [Chelton, Dudley B.] Oregon State Univ, Coll Ocean & Atmospher Sci, Corvallis, OR 97331 USA. [Li, Zhijin] NASA, Jet Prop Lab, Pasadena, CA USA. RP Jin, X (reprint author), Univ Calif Los Angeles, IGPP, 405 Hilgard Ave, Los Angeles, CA 90095 USA. EM xjin@ucla.edu FU Cooperative Institute for Oceanographic Satellite Studies at Oregon State University; NASA [NNX08AI84G, NNX08AL91G]; Jet Propulsion Laboratory [1283973, 1283976] FX We appreciate support from a grant from the Cooperative Institute for Oceanographic Satellite Studies at Oregon State University, Grants NNX08AI84G and NNX08AL91G from NASA, and Contracts 1283973 and 1283976 from the Jet Propulsion Laboratory for funding of Ocean Vector Winds Science Team activities. Comments and suggestions from two anonymous reviewers helped to improve the paper. Computations were made at the National Center for Supercomputing Applications. NR 45 TC 38 Z9 38 U1 4 U2 13 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0022-3670 J9 J PHYS OCEANOGR JI J. Phys. Oceanogr. PD NOV PY 2009 VL 39 IS 11 BP 2957 EP 2970 DI 10.1175/2009JPO4205.1 PG 14 WC Oceanography SC Oceanography GA 521HU UT WOS:000271912200015 ER PT J AU Brophy, JR Garner, CE Mikes, S AF Brophy, John R. Garner, Charles E. Mikes, Steven TI Dawn Ion Propulsion System: Initial Checkout After Launch SO JOURNAL OF PROPULSION AND POWER LA English DT Article; Proceedings Paper CT AIAA/ASME/SAE/ASEE 44th Joint Propulsion Conference and Exhibit CY JUL 20-23, 2008 CL Hartford, CT SP AIAA, ASME, SAE, ASEE ID MISSION AB The first 80 days after launch of the Dawn mission were dedicated to the checkout of the spacecraft with a major emphasis on the ion propulsion system. All three ion thrusters, all three thruster-gimbal assemblies, both power processor units, both digital interface and control units, and the entire xenon feed system were completely checked out, and every component was found to he in good health. Direct thrust measurements agreed well with preflight expected values for all three thrusters over the entire throttle range. Measurements of the thruster-produced roll-torque verified that each thruster produced less than the maximum allowed value of 60 mu Nm at full power. Thruster electrical operating parameters and power processor unit efficiencies also agreed well with preflight expected values based on acceptance test data. Two of the three ion thrusters were fully checked out within 30 days after launch. Checkout of all three thrusters was completed 64 days after launch. Deterministic thrusting with the ion propulsion system began on 17 December 2007. C1 [Brophy, John R.; Garner, Charles E.; Mikes, Steven] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Brophy, JR (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 16 TC 4 Z9 4 U1 1 U2 5 PU AMER INST AERONAUT ASTRONAUT PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0748-4658 J9 J PROPUL POWER JI J. Propul. Power PD NOV-DEC PY 2009 VL 25 IS 6 BP 1189 EP 1202 DI 10.2514/1.40480 PG 14 WC Engineering, Aerospace SC Engineering GA 529DY UT WOS:000272497300004 ER PT J AU Mento, CA Sung, CJ Ibarreta, AF Schneider, SJ AF Mento, Christopher A. Sung, Chih-Jen Ibarreta, Alfonso F. Schneider, Steven J. TI Catalyzed Ignition of Using Methane/Hydrogen Fuel in a Microtube for Microthruster Applications SO JOURNAL OF PROPULSION AND POWER LA English DT Article ID VAPORIZING LIQUID MICROTHRUSTER; COMBUSTION; THRUSTER; PLATINUM; PERFORMANCE; MIXTURES; METHANE; ISSUES AB Catalyzed combustion of propellants in a microtube serves as a model of a microthruster that has potential applications for micropropulsion for small satellites/spacecraft. The effect of hydrogen addition on fuel-rich methane/oxygen ignition within a 0.40-mm-diam platinum microtube is investigated experimentally. All tests are conducted in a vacuum chamber with an ambient pressure of 0.0136 atm to simulate high-altitude conditions. Experimental results show that the critical temperature needed to catalytically lightoff fuel-rich methane/oxygen mixtures is reduced by the addition of small amounts of hydrogen to the mixture. Two-stage ignition phenomena are observed for low levels of hydrogen addition (2-7% by volume), with the first and second ignition conditions corresponding to the reactions of hydrogen and methane, respectively. The effects of changing flow rate (residence time), equivalence ratio, and amount of hydrogen addition on the critical ignition temperature are investigated. The ability of the catalyst to sustain chemical reactions once the input power is turned off is also explored and, for most cases, self-sustainability is realized. Various microtube performance parameters are estimated for all experiments, which include thrust, specific impulse, and power required to ignite reactions within the microtube. C1 [Mento, Christopher A.; Sung, Chih-Jen; Ibarreta, Alfonso F.] Case Western Reserve Univ, Dept Mech & Aerosp Engn, Cleveland, OH 44106 USA. [Schneider, Steven J.] NASA, John H Glenn Res Ctr, Multidisciplinary Design Anal & Optimizat Branch, Cleveland, OH 44135 USA. RP Sung, CJ (reprint author), Univ Connecticut, Dept Mech Engn, Storrs, CT 06269 USA. EM cmento@flowsciences.com; cjsung@engr.uconn.edu; aibarreta@exponent.com; Steven.J.Schneider@grc.nasa.gov FU NASA Microgravity Combustion Program with Merrill King; NASA Graduate Student Researchers Program FX This work was supported by the NASA Microgravity Combustion Program with Merrill King as contract monitor. The first author would also like to acknowledge fellowship support by the NASA Graduate Student Researchers Program. NR 32 TC 1 Z9 1 U1 1 U2 5 PU AMER INST AERONAUT ASTRONAUT PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0748-4658 J9 J PROPUL POWER JI J. Propul. Power PD NOV-DEC PY 2009 VL 25 IS 6 BP 1203 EP 1210 DI 10.2514/1.42592 PG 8 WC Engineering, Aerospace SC Engineering GA 529DY UT WOS:000272497300005 ER PT J AU Wang, TS Guidos, M AF Wang, Ten-See Guidos, Mike TI Transient Three-Dimensional Side-Load Analysis of a Film-Cooled Nozzle SO JOURNAL OF PROPULSION AND POWER LA English DT Article; Proceedings Paper CT AIAA 38th Fluid Dynamics Conference CY JUN 23-26, 2008-3008 CL Seattle, WA SP AIAA ID PERFORMANCE AB Transient three-dimensional numerical investigations on the side-load physics of an engine encompassing a film-cooled nozzle extension and a regeneratively cooled thrust chamber were performed. The objectives of this study are. to identify the side-load physics and to compute the associated aerodynamic side load. The computational methodology is based on an unstructured-grid pressure-based computational fluid dynamics formulation and a. transient inlet history based on an engine system simulation. Computations simulating engine startup at ambient. pressures corresponding to sea level and three high altitudes were performed. In addition, computations for both engine startup and shutdown transients for a stub nozzle operating at sea level were also performed. For engine startups with the nozzle extension attached, computational results show that the dominant side-load physics are the turbine-exhaust-gas-assisted asymmetric Mach disk flow and the subsequent jump of the separation line, which generated the peak side load that decreases as the ambient pressure decreases. For the stub nozzle operating at sea level, the peak side load reduces drastically. The computed side-load physics and the associated peak side load for the sea-level cases agree reasonably well with those of available data from the tests of a similar engine. C1 [Wang, Ten-See] NASA, George C Marshall Space Flight Ctr, Fluid Dynam Branch, Prop Struct Thermal & Fluids Anal Div, Huntsville, AL 35812 USA. [Guidos, Mike] NASA, George C Marshall Space Flight Ctr, Liquid Engine & Main Prop Syst Branch, Prop Syst Design & Integrat Div, Huntsville, AL 35812 USA. RP Wang, TS (reprint author), NASA, George C Marshall Space Flight Ctr, Fluid Dynam Branch, Prop Struct Thermal & Fluids Anal Div, Mail Stop ER42, Huntsville, AL 35812 USA. NR 31 TC 11 Z9 12 U1 1 U2 3 PU AMER INST AERONAUT ASTRONAUT PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0748-4658 J9 J PROPUL POWER JI J. Propul. Power PD NOV-DEC PY 2009 VL 25 IS 6 BP 1272 EP 1280 DI 10.2514/1.41025 PG 9 WC Engineering, Aerospace SC Engineering GA 529DY UT WOS:000272497300013 ER PT J AU Li, ZQ Goloub, P Dubovik, O Blarel, L Zhang, WX Podvin, T Sinyuk, A Sorokin, M Chen, HB Holben, B Tanre, D Carlini, M Buis, JP AF Li, Zhengqiang Goloub, Philippe Dubovik, Oleg Blarel, Luc Zhang, Wenxing Podvin, Thierry Sinyuk, Alexander Sorokin, Mikhail Chen, Hongbin Holben, Brent Tanre, Didier Carlini, Marius Buis, Jean-Pierre TI Improvements for ground-based remote sensing of atmospheric aerosol properties by additional polarimetric measurements SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Article DE Aerosol; Remote sensing; Polarization; Calibration; Retrieval ID SKY RADIANCE MEASUREMENTS; PLANETARY-ATMOSPHERES; OPTICAL-PROPERTIES; DIRECT SOLAR; RETRIEVAL; SUN; POLARIZATION; CALIBRATION; SCATTERING; RADIATION AB We discuss the improvements in the aerosol properties characterization resulting from the additional multi-wavelength polarization measurements measured by a new CIMEL polarized sun/sky-photometer, CE318-DP. In order to process direct-sun, sky and polarization measurements in a wide spectral range (340-1640 nm), we developed new calibration methods and strategies, e.g. using the Langley plot method to calibrate both direct-sun irradiance and sky radiance, as well as combining laboratory facilities with a vicarious method to calibrate the polarized sky measurements. For studying the impact of new polarimetric measurements on the retrievals of aerosol properties, we have processed an extensive record of field measurements using an updated Dubovik and King retrieval algorithm [Dubovik O, Sinyuk A, Lapyonok T, Holben BN, Mishchenko, MI, et al. Application of spheroid models to account for aerosol particle nonsphericity in remote sensing of desert dust. J Geophys Res 2006:111:D11208.]. A preliminary analysis shows that adding polarization in the inversion can reduce possible errors (notably for about 30% of our field cases) in the fine mode size distribution, real part of refractive index and particle shape parameter retrievals, especially for small particles. (C) 2009 Elsevier Ltd. All rights reserved. C1 [Li, Zhengqiang; Goloub, Philippe; Dubovik, Oleg; Blarel, Luc; Podvin, Thierry; Tanre, Didier] Univ Lille 1, Opt Atmospher Lab, F-59655 Villeneuve Dascq, France. [Sinyuk, Alexander; Sorokin, Mikhail; Holben, Brent] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Carlini, Marius; Buis, Jean-Pierre] CIMEL Elect, F-75011 Paris, France. [Zhang, Wenxing; Chen, Hongbin] Chinese Acad Sci, Inst Atmospher Phys, Beijing 100029, Peoples R China. RP Li, ZQ (reprint author), Univ Lille 1, Opt Atmospher Lab, F-59655 Villeneuve Dascq, France. EM zhengqiang.li@univ-lille1.fr RI li, zhengqiang/C-5678-2013; Dubovik, Oleg/A-8235-2009 OI li, zhengqiang/0000-0002-7795-3630; Dubovik, Oleg/0000-0003-3482-6460 NR 15 TC 41 Z9 46 U1 6 U2 18 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0022-4073 EI 1879-1352 J9 J QUANT SPECTROSC RA JI J. Quant. Spectrosc. Radiat. Transf. PD NOV PY 2009 VL 110 IS 17 BP 1954 EP 1961 DI 10.1016/j.jqsrt.2009.04.009 PG 8 WC Optics; Spectroscopy SC Optics; Spectroscopy GA 489OF UT WOS:000269429200013 ER PT J AU Mishchenko, MI Geogdzhayev, IV Liu, L Lacis, AA Cairns, B Travis, LD AF Mishchenko, Michael I. Geogdzhayev, Igor V. Liu, Li Lacis, Andrew A. Cairns, Brian Travis, Larry D. TI Toward unified satellite climatology of aerosol properties: What do fully compatible MODIS and MISR aerosol pixels tell us? (vol 110, pg 402, 2009) SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Correction C1 [Mishchenko, Michael I.; Geogdzhayev, Igor V.; Liu, Li; Lacis, Andrew A.; Cairns, Brian; Travis, Larry D.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. RP Mishchenko, MI (reprint author), NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA. EM mmishchenko@giss.nasa.gov RI Lacis, Andrew/D-4658-2012; Mishchenko, Michael/D-4426-2012 NR 1 TC 1 Z9 1 U1 0 U2 3 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0022-4073 J9 J QUANT SPECTROSC RA JI J. Quant. Spectrosc. Radiat. Transf. PD NOV PY 2009 VL 110 IS 17 BP 1962 EP 1963 DI 10.1016/j.jqsrt.2009.05.015 PG 2 WC Optics; Spectroscopy SC Optics; Spectroscopy GA 489OF UT WOS:000269429200014 ER PT J AU Milos, FS Chen, YK AF Milos, F. S. Chen, Y. -K. TI Two-Dimensional Ablation, Thermal Response, and Sizing Program for Pyrolyzing Ablators SO JOURNAL OF SPACECRAFT AND ROCKETS LA English DT Article; Proceedings Paper CT AIAA 46th Aerospace Sciences Meeting and Exhibit CY JAN 07-10, 2008 CL Reno, NV SP Amer Inst Aeronaut & Astronaut AB The purpose of this paper is to describe and demonstrate new capabilities in the two-dimensional implicit thermal response and ablation program. These expanded capabilities include grid options for flight and arcjet geometries, a sizing algorithm for the flight-type geometry, and an orthotropic thermal conductivity model. Applications to analysis of an orthotropic low-density carbon-phenolic material in arcjet and flight environments relevant to the Orion crew module are presented. For the arcjet environment, multidimensional conduction effects strongly influence the in-depth thermal response. For a lunar return flight environment, in the shoulder region of the crew module (where the radius of curvature is smallest), the thermal response is influenced by multidimensional conduction and by the orientation of the orthotropic material. C1 [Milos, F. S.; Chen, Y. -K.] NASA, Ames Res Ctr, Thermal Protect Mat & Syst Branch, Moffett Field, CA 94035 USA. RP Milos, FS (reprint author), NASA, Ames Res Ctr, Thermal Protect Mat & Syst Branch, Mail Stop 234-1, Moffett Field, CA 94035 USA. NR 23 TC 13 Z9 13 U1 1 U2 2 PU AMER INST AERONAUT ASTRONAUT PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0022-4650 J9 J SPACECRAFT ROCKETS JI J. Spacecr. Rockets PD NOV-DEC PY 2009 VL 46 IS 6 BP 1089 EP 1099 DI 10.2514/1.36575 PG 11 WC Engineering, Aerospace SC Engineering GA 534NE UT WOS:000272903600001 ER PT J AU Palmer, GE Pulsonetti, M Wood, WA Alter, S Gnoffo, P Tang, C AF Palmer, Grant E. Pulsonetti, Maria Wood, William A. Alter, Steve Gnoffo, Peter Tang, Chun TI Computational Assessment of Thermal Protection System Damage Experienced During STS-118 SO JOURNAL OF SPACECRAFT AND ROCKETS LA English DT Article; Proceedings Paper CT AIAA 40th Thermophysics Conference CY JUN 23-26, 2008 CL Seattle, WA SP AIAA AB In response to thermal protection system tile damage that occurred during the ascent portion of space shuttle mission STS-118, rapid turnaround computational fluid dynamic simulations were performed on the damage site during the mission. The purpose of the computational effort was to provide insight into the flow physics and determine heating augmentation bump factors in and around the damage site. Damage analysis teams at the NASA Ames and NASA Langley Research Centers used automated local cavity simulation procedures to generate 12 three-dimensional simulations in less than 18 h during the mission. The computational fluid dynamic results compared closely with the engineering results used as inputs to the vehicle thermal analysis models and supported the recommendation of the damage assessment team to fly the Orbiter back as is without requiring the astronauts to perform a damage site repair in situ. C1 [Palmer, Grant E.] ELORET Corp, Reacting Flow Environm Branch, Sunnyvale, CA 94086 USA. [Pulsonetti, Maria; Wood, William A.; Alter, Steve; Gnoffo, Peter] NASA, Langley Res Ctr, Aerothermodynam Branch, Hampton, VA 23681 USA. [Tang, Chun] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Palmer, GE (reprint author), ELORET Corp, Reacting Flow Environm Branch, Mail Stop 230-2, Sunnyvale, CA 94086 USA. NR 12 TC 0 Z9 0 U1 0 U2 2 PU AMER INST AERONAUT ASTRONAUT PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0022-4650 J9 J SPACECRAFT ROCKETS JI J. Spacecr. Rockets PD NOV-DEC PY 2009 VL 46 IS 6 BP 1110 EP 1116 DI 10.2514/1.40478 PG 7 WC Engineering, Aerospace SC Engineering GA 534NE UT WOS:000272903600003 ER PT J AU Sengupta, A Kelsch, R Roeder, J Wernet, M Witkowski, A Kandis, M AF Sengupta, Anita Kelsch, Richard Roeder, James Wernet, Mark Witkowski, Allen Kandis, Mike TI Supersonic Performance of Disk-Gap-Band Parachutes Constrained to a 0-Degree Trim Angle SO JOURNAL OF SPACECRAFT AND ROCKETS LA English DT Article; Proceedings Paper CT AIAA Atmospheric Flight Mechanics Conference CY AUG 18-21, 2008 CL Honolulu, HI SP AIAA AB Supersonic wind-tunnel tests of 0.813 m disk-gap-band parachutes were conducted in a 10 x 10 ft cross section of a closed-loop wind tunnel. Four-percent-scale parachutes were attached to a 4%-scale Mars Science Laboratory (Viking-type) entry vehicle to simulate the free-flight configuration. The parachutes were tested from Mach 2 to 2.5 over a Reynolds number Re range of 2 x 10(5) to 1.3 x 10(6), representative of the Mars flight deployment envelope. A constrained parachute configuration was investigated to quantify the effect of parachute trim angle with respect to alignment with the entry-vehicle wake. In the constrained configuration, the parachutes were supported at the vent, using a rod that restricted parachute translation along a single axis. This was investigated for fixed trim angles of 0 and 10 degrees from the velocity vector. In the unconstrained configuration, the parachute was permitted to translate as well as trim and cone, in a manner similar to free flight. Nonintrusive test diagnostics were selected. An in-line load cell provided measurement of unsteady and mean parachute normal force. High-speed shadowgraph video of the upstream parachute flowfield was used to capture bow-shock motion and standoff distance. Stereo particle image velocimetry of the flowfield upstream of the parachute provided spatially resolved measurements of all three velocity components. Multiple high-speed-video views were used to document the supersonic inflation, parachute trim angle, projected area, and frequency of area oscillations. In addition, reflective targets placed in the interior of the canopy enabled photogrammetric reconstruction of the canopy-fabric motion (in both time and space) from the high-speed-video data. C1 [Sengupta, Anita] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Kelsch, Richard] NASA, John H Glenn Res Ctr Lewis Field, Appl Struct Mech Branch, Cleveland, OH 44135 USA. [Roeder, James] NASA, John H Glenn Res Ctr Lewis Field, Aeropower & Prop Test Engn Branch, Cleveland, OH 44135 USA. [Witkowski, Allen; Kandis, Mike] Pioneer Aerosp Corp, S Windsor, CT 06074 USA. RP Sengupta, A (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,Mail Stop T1723-118, Pasadena, CA 91109 USA. NR 23 TC 6 Z9 6 U1 0 U2 1 PU AMER INST AERONAUT ASTRONAUT PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0022-4650 J9 J SPACECRAFT ROCKETS JI J. Spacecr. Rockets PD NOV-DEC PY 2009 VL 46 IS 6 BP 1155 EP 1163 DI 10.2514/1.41223 PG 9 WC Engineering, Aerospace SC Engineering GA 534NE UT WOS:000272903600008 ER PT J AU Bilimoria, KD AF Bilimoria, Karl D. TI Effects of Control Power and Guidance Cues on Lunar Lander Handling Qualities SO JOURNAL OF SPACECRAFT AND ROCKETS LA English DT Article; Proceedings Paper CT AIAA Space 2008 Conference and Exposition CY SEP 08-12, 2008 CL San Diego, CA SP Amer Inst Aeronaut & Astronaut ID ATTITUDE-CONTROL; SPACECRAFT; MODULE AB A piloted simulation was conducted to study handling qualities for a precision lunar landing task from final approach to touchdown. The experiment variables were control power and guidance cues. A dynamics and control model was derived from Apollo Lunar Module data, and new feedback guidance laws were designed to help the pilot follow a reference trajectory. The experiment was conducted on the large motion base Vertical Motion Simulator at the NASA Ames Research Center. Six pilot astronauts served as evaluation pilots, providing Cooper-Harper ratings, Task Load Index ratings, and qualitative comment. The piloting task was to fly a final approach profile from 500 ft altitude located 1351) ft up range of the designated landing site with a 250 ft lateral offset, and touch down with a position accuracy of 15 ft. Following guidance cues presented on cockpit displays, the pilots were able to accomplish this task for control powers ranging from 100 to 15% of the nominal (Apollo) value. The handling qualities were satisfactory (Level 1) at nominal control power, and degraded nonlinearly as control power decreased. Without guidance cues, in the limited time available for this experiment, the evaluation pilots were unable to develop a flying technique for the precision landing task with lateral offset approach. This highlights the need for guidance cues in future lunar operations that may require precision landing capability. C1 NASA, Ames Res Ctr, Flight Trajectory Dynam & Controls Branch, Moffett Field, CA 94035 USA. RP Bilimoria, KD (reprint author), NASA, Ames Res Ctr, Flight Trajectory Dynam & Controls Branch, Mail Stop 210-10, Moffett Field, CA 94035 USA. EM Karl.Bilimoria@nasa.gov NR 34 TC 9 Z9 10 U1 0 U2 4 PU AMER INST AERONAUT ASTRONAUT PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0022-4650 J9 J SPACECRAFT ROCKETS JI J. Spacecr. Rockets PD NOV-DEC PY 2009 VL 46 IS 6 BP 1261 EP 1271 DI 10.2514/1.40187 PG 11 WC Engineering, Aerospace SC Engineering GA 534NE UT WOS:000272903600018 ER PT J AU Mueller, E Bilimoria, KD Frost, C AF Mueller, Eric Bilimoria, Karl D. Frost, Chad TI Dynamic Coupling and Control Response Effects on Spacecraft Handling Qualities During Docking SO JOURNAL OF SPACECRAFT AND ROCKETS LA English DT Article; Proceedings Paper CT AIAA Guidance, Navigation and Control Conference CY AUG 18-21, 2008 CL Honolulu, HI SP Amer Inst Aeronaut & Astronaut AB NASA is developing a new generation of spacecraft to replace the Space Shuttle and return astronauts to the moon. These spacecraft will have a manual control capability for several mission tasks, and the ease and precision with which pilots can execute these tasks will have an important effect on mission risk and training costs. A simulation evaluated the handling qualities of a generic space vehicle based on dynamics similar to one of these spacecraft, NASA's Crew Exploration Vehicle, during the last segment of the docking task with a space station. This handling qualities evaluation looked at four different translational control systems, called response types, that map pilot inputs to thruster firings in a way that gives predictable and useful vehicle responses. These response types were flown with three levels of translation-into-rotation dynamic coupling arising from a longitudinal offset between the reaction control system thrusters and the vehicle's center of mass. The results indicate that greater translation-into-rotation coupling is strongly correlated with degraded handling qualities, but that different response types do not have a major effect on pilot workload, final docking performance, or handling qualities. C1 [Mueller, Eric; Bilimoria, Karl D.] NASA, Ames Res Ctr, Flight Trajectory Dynam & Controls Branch, Moffett Field, CA 94035 USA. [Frost, Chad] NASA, Ames Res Ctr, Intelligent Syst Div, Moffett Field, CA 94035 USA. RP Mueller, E (reprint author), NASA, Ames Res Ctr, Flight Trajectory Dynam & Controls Branch, Mail Stop 210-10, Moffett Field, CA 94035 USA. EM eric.mueller@nasa.gov; karl.bilimoria@nasa.gov; chad.r.frost@nasa.gov NR 30 TC 7 Z9 8 U1 1 U2 4 PU AMER INST AERONAUT ASTRONAUT PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0022-4650 J9 J SPACECRAFT ROCKETS JI J. Spacecr. Rockets PD NOV-DEC PY 2009 VL 46 IS 6 BP 1288 EP 1297 DI 10.2514/1.41924 PG 10 WC Engineering, Aerospace SC Engineering GA 534NE UT WOS:000272903600020 ER PT J AU Whitson, PA Pietrzyk, RA Jones, JA Nelman-Gonzalez, M Hudson, EK Sams, CF AF Whitson, Peggy A. Pietrzyk, Robert A. Jones, Jeffrey A. Nelman-Gonzalez, Mayra Hudson, Edgar K. Sams, Clarence F. TI Effect of Potassium Citrate Therapy on the Risk of Renal Stone Formation During Spaceflight SO JOURNAL OF UROLOGY LA English DT Article DE kidney; kidney calculi; space flight; potassium citrate; uric acid ID MAGNESIUM CITRATE; SPACE-FLIGHT AB Purpose: Exposure to microgravity affects human physiology and results in changes in urinary chemical composition during and after spaceflight, favoring an increased risk of renal stones. We assessed the efficacy of potassium citrate to decrease the stone risk during and after spaceflight. Materials and Methods: The study was done in 30 long duration spaceflight crew members to the space stations Mir and International Space Station. Before, during and after spaceflight 24-hour urine samples were collected to assess the renal stone risk. Potassium citrate (20 mEq) was ingested daily by International Space Station crew members in a double-blind, placebo controlled study. Mir crew members performed the identical protocol but did not ingest medication. Results: Potassium citrate treated crew members had decreased urinary calcium excretion and maintained the calcium oxalate supersaturation risk at preflight levels compared to that in controls. Increased urinary pH in the treatment group decreased the risk of uric acid stones. Conclusions: Results from this investigation suggest that supplementation with potassium citrate may decrease the risk of renal stone formation during and immediately after spaceflight. C1 [Pietrzyk, Robert A.; Nelman-Gonzalez, Mayra] Wyle Integrated Sci & Engn Grp, Human Adaptat & Countermeasures Div, Houston, TX 77058 USA. [Whitson, Peggy A.] NASA, Lyndon B Johnson Space Ctr, Astronaut Off, Houston, TX 77058 USA. [Jones, Jeffrey A.] NASA, Lyndon B Johnson Space Ctr, Space Med Div, Houston, TX 77058 USA. [Sams, Clarence F.] NASA, Lyndon B Johnson Space Ctr, Human Adaptat & Countermeasures Div, Houston, TX 77058 USA. [Hudson, Edgar K.] JES Tech, Houston, TX USA. RP Pietrzyk, RA (reprint author), Wyle Integrated Sci & Engn Grp, Human Adaptat & Countermeasures Div, 1290 Hercules Dr,Suite 120, Houston, TX 77058 USA. EM robert.pietrzyk-1@nasa.gov FU Mineral Metabolism Laboratory; Center for Mineral Metabolism and General Clinical Research Center; University of Texas Southwestern Medical Center, Dallas; NASA Johnson Space Center Clinical Laboratory; NASA Johnson Space Center Nutritional Biochemistry Laboratory; Johnson Space Center, Houston, Texas and Gagarin Cosmonaut Training Center, Star City, Russia FX Dr. C. Y. C Pak, Dr. J. Zerwekh and J. Koska, Mineral Metabolism Laboratory, Center for Mineral Metabolism and General Clinical Research Center, University of Texas Southwestern Medical Center, Dallas, Texas provided expertise. Mission (R) Pharmacal provided KCIT and placebo. Urinalysis was done at the NASA Johnson Space Center Clinical Laboratory. Lithium was measured at the NASA Johnson Space Center Nutritional Biochemistry Laboratory. Urine was collected at Johnson Space Center, Houston, Texas and Gagarin Cosmonaut Training Center, Star City, Russia. NR 14 TC 14 Z9 14 U1 0 U2 2 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0022-5347 J9 J UROLOGY JI J. Urol. PD NOV PY 2009 VL 182 IS 5 BP 2490 EP 2496 DI 10.1016/j.juro.2009.07.010 PG 7 WC Urology & Nephrology SC Urology & Nephrology GA 506EO UT WOS:000270756900138 PM 19765769 ER PT J AU Usabiaga, J Erol, A Bebis, G Boyle, R Twombly, X AF Usabiaga, Jorge Erol, Ali Bebis, George Boyle, Richard Twombly, Xander TI Global hand pose estimation by multiple camera ellipse tracking SO MACHINE VISION AND APPLICATIONS LA English DT Article DE Virtual environments; Ellipse tracking; Model-based tracking; Hand pose estimation ID IMAGE AB Immersive virtual environments with life-like interaction capabilities have very demanding requirements including high-precision motion capture and high-processing speed. These issues raise many challenges for computer vision-based motion estimation algorithms. In this study, we consider the problem of hand tracking using multiple cameras and estimating its 3D global pose (i.e., position and orientation of the palm). Our interest is in developing an accurate and robust algorithm to be employed in an immersive virtual training environment, called "Virtual GloveboX" (VGX) (Twombly et al. in J Syst Cybern Inf 2:30-34, 2005), which is currently under development at NASA Ames. In this context, we present a marker-based, hand tracking and 3D global pose estimation algorithm that operates in a controlled, multi-camera, environment built to track the user's hand inside VGX. The key idea of the proposed algorithm is tracking the 3D position and orientation of an elliptical marker placed on the dorsal part of the hand using model-based tracking approaches and active camera selection. It should be noted that, the use of markers is well justified in the context of our application since VGX naturally allows for the use of gloves without disrupting the fidelity of the interaction. Our experimental results and comparisons illustrate that the proposed approach is more accurate and robust than related approaches. A byproduct of our multi-camera ellipse tracking algorithm is that, with only minor modifications, the same algorithm can be used to automatically re-calibrate (i.e., fine-tune) the extrinsic parameters of a multi-camera system leading to more accurate pose estimates. C1 [Usabiaga, Jorge; Erol, Ali; Bebis, George] Univ Nevada, Comp Vis Lab, Reno, NV 89557 USA. [Boyle, Richard; Twombly, Xander] NASA, Ames Res Ctr, BioVis Lab, Moffett Field, CA 94035 USA. RP Bebis, G (reprint author), Univ Nevada, Comp Vis Lab, Reno, NV 89557 USA. EM usabiaga@cse.unr.edu; aerol@cse.unr.edu; bebis@cse.unr.edu; rboyle@mail.arc.nasa.gov; xtwombly@mail.arc.nasa.gov FU NASA [NCC5-583] FX This work was supported by NASA under grant # NCC5-583 NR 21 TC 7 Z9 7 U1 0 U2 5 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0932-8092 J9 MACH VISION APPL JI Mach. Vis. Appl. PD NOV PY 2009 VL 21 IS 1 BP 1 EP 15 DI 10.1007/s00138-008-0137-z PG 15 WC Computer Science, Artificial Intelligence; Computer Science, Cybernetics; Engineering, Electrical & Electronic SC Computer Science; Engineering GA 505ZI UT WOS:000270740800001 ER PT J AU Martinez, JE Erol, A Bebis, G Boyle, R Twombly, X AF Martinez, Javier E. Erol, Ali Bebis, George Boyle, Richard Twombly, Xander TI Integrating perceptual level of detail with head-pose estimation and its uncertainty SO MACHINE VISION AND APPLICATIONS LA English DT Article DE Virtual environments; Perceptual level of detail; Head-pose estimation; Uncertainty estimation ID ALGORITHMS AB Immersive virtual environments with life-like interaction capabilities can provide a high fidelity view of the virtual world and seamless interaction methods to the user. High demanding requirements, however, raise many challenges in the development of sensing technologies and display systems. The focus of this study is on improving the performance of human-computer interaction by rendering optimizations guided by head pose estimates and their uncertainties. This work is part of a larger study currently being under investigation at NASA Ames, called "Virtual GloveboX" (VGX). VGX is a virtual simulator that aims to provide advanced training and simulation capabilities for astronauts to perform precise biological experiments in a glovebox aboard the International Space Station (ISS). Our objective is to enhance the virtual experience by incorporating information about the user's viewing direction into the rendering process. In our system, viewing direction is approximated by estimating head orientation using markers placed on a pair of polarized eye-glasses. Using eye-glasses does not pose any constraints in our operational environment since they are an integral part of a stereo display used in VGX. During rendering, perceptual level of detail methods are coupled with head-pose estimation to improve the visual experience. A key contribution of our work is incorporating head pose estimation uncertainties into the level of detail computations to account for head pose estimation errors. Subject tests designed to quantify user satisfaction under different modes of operation indicate that incorporating uncertainty information during rendering improves the visual experience of the user. C1 [Martinez, Javier E.; Erol, Ali; Bebis, George] Univ Nevada, Comp Vis Lab, Reno, NV 89557 USA. [Boyle, Richard; Twombly, Xander] NASA, Ames Res Ctr, BioVis Lab, Moffett Field, CA 94035 USA. RP Bebis, G (reprint author), Univ Nevada, Comp Vis Lab, Reno, NV 89557 USA. EM javier@cse.unr.edu; aerol@cse.unr.edu; bebis@cse.unr.edu; rboyle@mail.arc.nasa.gov; xtwombly@mail.arc.nasa.gov FU NASA [NCC5-583] FX This work was supported by NASA under grant # NCC5-583. NR 26 TC 0 Z9 0 U1 0 U2 1 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0932-8092 EI 1432-1769 J9 MACH VISION APPL JI Mach. Vis. Appl. PD NOV PY 2009 VL 21 IS 1 BP 69 EP 83 DI 10.1007/s00138-008-0142-2 PG 15 WC Computer Science, Artificial Intelligence; Computer Science, Cybernetics; Engineering, Electrical & Electronic SC Computer Science; Engineering GA 505ZI UT WOS:000270740800006 ER PT J AU Vasudevan, RV Mushotzky, RF Winter, LM Fabian, AC AF Vasudevan, R. V. Mushotzky, R. F. Winter, L. M. Fabian, A. C. TI Optical-to-X-ray emission in low-absorption AGN: results from the Swift-BAT 9-month catalogue SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE black hole physics; galaxies: active; galaxies: Seyfert ID ACTIVE GALACTIC NUCLEI; BLACK-HOLE MASS; SPECTRAL ENERGY-DISTRIBUTION; DIGITAL SKY SURVEY; SEYFERT 1 GALAXIES; BROAD-LINE REGION; HOST GALAXIES; RADIATION PRESSURE; LUMINOSITY; QUASARS AB We present simultaneous optical-to-X-ray spectral energy distributions (SEDs) from Swift's X-ray and UV-optical telescopes (XRTs and UVOTs) for a well-selected sample of 26 low-redshift (z < 0.1) active galactic nuclei (AGN) from the Swift/Burst Alert Telescope 9-month catalogue, the largest well-studied, hard X-ray-selected survey of local AGN to date. Our sub-sample consists of AGN with low intrinsic X-ray absorption (N(H) < 1022 cm-2) and minimal spectral complexity, to more accurately recover the intrinsic accretion luminosity in these sources. We perform a correction for host galaxy contamination in all available UVOT filter images to recover the intrinsic AGN emission and estimate intrinsic dust extinction from the resultant nuclear SEDs. Black hole mass estimates are determined from the host galaxy Two-Micron All-Sky Survey K-band bulge luminosity. Accretion rates determined from our SEDs are on average low (Eddington ratios lambda(Edd) less than or similar to 0.1) and hard X-ray bolometric corrections cluster at similar to 10-20, in contrast with the higher values seen for quasars. An average SED for the 22 low accretion rate (lambda(Edd) < 0.1) objects is presented, with and without correction for extinction. Significant dust reddening is found in some objects despite the selection of low N(H) objects, emphasizing the complex relationship between these two types of absorption. We do not find a correlation of the optical-to-X-ray spectral index with the Eddington ratio, regardless of the optical reference wavelength chosen for defining the spectral index. An anticorrelation of bolometric correction with black hole mass may reinforce 'cosmic downsizing' scenarios, since the higher bolometric corrections at low mass would boost accretion rates in local, lower mass black holes. We also perform a basic analysis of the UVOT-derived host galaxy colours for our sample and find hosts cluster near the 'green valley' of the colour-magnitude diagram, but better quality images are needed for a more definitive analysis. The low accretion rates and bolometric corrections found for this representative low-redshift sample are of particular importance for studies of AGN accretion history. C1 [Vasudevan, R. V.; Fabian, A. C.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Mushotzky, R. F.] NASA, Goddard Space Flight Ctr, High Energy Astrophys Lab, Greenbelt, MD 20771 USA. [Winter, L. M.] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA. RP Vasudevan, RV (reprint author), Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England. EM ranjan@ast.cam.ac.uk FU Science and Technology Facilities Council (STFC); Royal Society FX RVV acknowledges support from the Science and Technology Facilities Council (STFC) and ACF thanks the Royal Society for Support. We thank the Swift/BAT team for the 9-month AGN catalogue data. We thank Stephen Holland for help with UVOT data analysis and Alice Breeveld for kindly providing and customizing her PSF generation code for UVOT images. We thank Jack Tueller for the use of results derived from the eight-channel BAT data and Kevin Schawinksi for providing host galaxy colours and magnitudes from his paper for comparison with our study. We thank Richard McMahon for help in understanding the correct use of the data in the 2MASS catalogues. We also thank the anonymous referee for useful comments and suggestions which improved this work. This research has made use of the NED and the NASA/IPAC Infrared Science Archive, which are operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. NR 65 TC 61 Z9 61 U1 0 U2 0 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD NOV 1 PY 2009 VL 399 IS 3 BP 1553 EP 1575 DI 10.1111/j.1365-2966.2009.15371.x PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 508BP UT WOS:000270902100035 ER PT J AU Byckling, K Osborne, JP Wheatley, PJ Wynn, GA Beardmore, A Braito, V Mukai, K West, RG AF Byckling, K. Osborne, J. P. Wheatley, P. J. Wynn, G. A. Beardmore, A. Braito, V. Mukai, K. West, R. G. TI Swift observations of GW Lib: a unique insight into a rare outburst SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion; accretion discs; stars: dwarf novae; novae; cataclysmic variables; X-rays: binaries; X-rays: stars ID X-RAY OBSERVATIONS; NOVA VW HYDRI; ACCRETING WHITE-DWARF; SS-CYGNI; CATACLYSMIC VARIABLES; EXOSAT OBSERVATIONS; WZ SGE; EMISSION; ULTRAVIOLET; SUPEROUTBURST AB The second known outburst of the WZ Sge type dwarf nova GW Lib was observed in 2007 April. We have obtained unique multiwavelength data of this outburst which lasted similar to 26 days. The American Association of Variable Star Observers (AAVSO) recorded the outburst in the optical, which was also monitored by Wide Angle Search for Planets, with a peak V magnitude of similar to 8. The outburst was followed in the ultraviolet and X-ray wavelengths by the Swift ultraviolet/optical and X-ray telescopes. The X-ray flux at optical maximum was found to be three orders of magnitude above the pre-outburst quiescent level, whereas X-rays are normally suppressed during dwarf nova outbursts. A distinct supersoft X-ray component was also detected at optical maximum, which probably arises from an optically thick boundary layer. Follow-up Swift observations taken 1 and 2 years after the outburst show that the post-outburst quiescent X-ray flux remains an order of magnitude higher than the pre-outburst flux. The long interoutburst time-scale of GW Lib with no observed normal outbursts support the idea that the inner disc in GW Lib is evacuated or the disc viscosity is very low. C1 [Byckling, K.; Osborne, J. P.; Wynn, G. A.; Beardmore, A.; Braito, V.; West, R. G.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Wheatley, P. J.] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. [Mukai, K.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Byckling, K (reprint author), Univ Leicester, Dept Phys & Astron, Univ Rd, Leicester LE1 7RH, Leics, England. EM kjkb2@star.le.ac.uk OI Braito, Valentina/0000-0002-2629-4989; Wheatley, Peter/0000-0003-1452-2240 FU European Commission [MEST-CT-2004-007512]; STFC FX KB acknowledges funding from the European Commission under the Marie Curie Host Fellowship for Early Stage Research Training SPARTAN, Contract No MEST-CT-2004-007512, University of Leicester, UK. The authors also acknowledge the support of STFC. We acknowledge with thanks the variable star observations from the AAVSO International Data base contributed by observers worldwide and used in this research. We thank the Swift science team and planners for their support of these target-of-opportunity observations. Swift data were extracted from the Swift science archive at http://www.swift.le.ac.uk. This work made use of data supplied by the UK Swift Science Data Centre at the University of Leicester. The WASP Consortium consists of astronomers primarily from Queen's University Belfast, Keele, Leicester, The Open University, and St Andrews, the Isaac Newton Group (La Palma), the Instituto de Astrofisica de Canarias (Tenerife) and the South African Astronomical Observatory. The SuperWASP-N and WASP-S Cameras were constructed and operated with funds made available from Consortium Universities and the UK's Science and Technology Facilities Council. WASP-South is hosted by the South African Astronomical Observatory (SAAO), and we are grateful for their support and assistance. We thank M. R. Goad for helpful comments on this paper. NR 52 TC 11 Z9 11 U1 0 U2 0 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD NOV 1 PY 2009 VL 399 IS 3 BP 1576 EP 1586 DI 10.1111/j.1365-2966.2009.15378.x PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 508BP UT WOS:000270902100036 ER PT J AU Carn, SA Krueger, AJ Krotkov, NA Yang, K Evans, K AF Carn, Simon A. Krueger, Arlin J. Krotkov, Nickolay A. Yang, Kai Evans, Keith TI Tracking volcanic sulfur dioxide clouds for aviation hazard mitigation SO NATURAL HAZARDS LA English DT Article DE Sulfur dioxide; Volcanic clouds; Aviation hazards; Ultraviolet remote sensing ID OZONE MONITORING INSTRUMENT; MAPPING SPECTROMETER; ERUPTION CLOUD; ASH CLOUDS; MISSION; TOMS; SO2; RETRIEVAL; AVHRR; GOME AB Satellite measurements of volcanic sulfur dioxide (SO2) emissions can provide critical information for aviation hazard mitigation, particularly when ash detection techniques fail. Recent developments in space-based SO2 monitoring are discussed, focusing on daily, global ultraviolet (UV) measurements by the Ozone Monitoring Instrument (OMI) on NASA's Aura satellite. OMI's high sensitivity to SO2 permits long-range tracking of volcanic clouds in the upper troposphere and lower stratosphere (UTLS) and accurate mapping of their perimeters to facilitate avoidance. Examples from 2006 to 2007 include eruptions of Soufriere Hills (Montserrat), Rabaul (Papua New Guinea), Nyamuragira (DR Congo), and Jebel at Tair (Yemen). A tendency for some volcanic clouds to occupy the jet stream suggests an increased threat to aircraft that exploit this phenomenon. Synergy between NASA A-Train sensors such as OMI and the Atmospheric Infrared Sounder (AIRS) on the Aqua satellite can provide critical information on volcanic cloud altitude. OMI and AIRS SO2 data products are being produced in near real-time for distribution to Volcanic Ash Advisory Centers (VAACs) via a NOAA website. Operational issues arising from these improved SO2 measurements include the reliability of SO2 as proxy for co-erupted ash, the duration of VAAC advisories for long-lived volcanic clouds, and the potential effects of elevated concentrations of SO2 and sulfate aerosol in ash-poor clouds on aircraft and avionics (including cumulative effects after multiple inadvertent transits through dilute clouds). Further research is required in these areas. Aviation community assistance is sought through continued reporting of sulfurous odors or other indications of diffuse volcanic cloud encounters, in order to validate the satellite retrievals. C1 [Carn, Simon A.; Krueger, Arlin J.; Evans, Keith] Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, Baltimore, MD 21250 USA. [Krotkov, Nickolay A.; Yang, Kai] Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol GEST Ctr, Baltimore, MD 21250 USA. [Krotkov, Nickolay A.; Yang, Kai] NASA, Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD 20771 USA. RP Carn, SA (reprint author), Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, 1000 Hilltop Circle, Baltimore, MD 21250 USA. EM scarn@umbc.edu RI Krotkov, Nickolay/E-1541-2012 OI Krotkov, Nickolay/0000-0001-6170-6750 FU NASA Science Mission Directorate's Earth-Sun System Division; Royal Dutch Meteorological Institute (KNMI); Netherlands Agency for Aerospace Programs (NIVR); NOAA Air Resources Laboratory (ARL) FX Funding for this work was provided by the NASA Science Mission Directorate's Earth-Sun System Division. The OMI project is managed by Royal Dutch Meteorological Institute (KNMI) and the Netherlands Agency for Aerospace Programs (NIVR). The NOAA Air Resources Laboratory (ARL) is acknowledged for provision of the HYSPLIT model and READY website (http://www.arl.noaa.gov/ready.html) used in this work. NR 53 TC 68 Z9 68 U1 0 U2 25 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0921-030X EI 1573-0840 J9 NAT HAZARDS JI Nat. Hazards PD NOV PY 2009 VL 51 IS 2 BP 325 EP 343 DI 10.1007/s11069-008-9228-4 PG 19 WC Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences; Water Resources SC Geology; Meteorology & Atmospheric Sciences; Water Resources GA 501ML UT WOS:000270385900007 ER PT J AU van der Werf, GR Morton, DC DeFries, RS Olivier, JGJ Kasibhatla, PS Jackson, RB Collatz, GJ Randerson, JT AF van der Werf, G. R. Morton, D. C. DeFries, R. S. Olivier, J. G. J. Kasibhatla, P. S. Jackson, R. B. Collatz, G. J. Randerson, J. T. TI CO2 emissions from forest loss SO NATURE GEOSCIENCE LA English DT Editorial Material ID CARBON; DEFORESTATION C1 [van der Werf, G. R.] Vrije Univ Amsterdam, Fac Earth & Life Sci, NL-1081 HV Amsterdam, Netherlands. [Morton, D. C.; Collatz, G. J.] NASA, Goddard Space Flight Ctr, Hydrospher & Biospher Sci Lab, Greenbelt, MD 20771 USA. [DeFries, R. S.] Columbia Univ, Dept Ecol Evolut & Environm Biol, New York, NY 10027 USA. [Olivier, J. G. J.] Netherlands Environm Assessment Agcy, NL-3720 AH Bilthoven, Netherlands. [Kasibhatla, P. S.; Jackson, R. B.] Duke Univ, Nicholas Sch Environm, Durham, NC 27708 USA. [Randerson, J. T.] Univ Calif Irvine, Earth Syst Sci Dept, Irvine, CA 92697 USA. RP van der Werf, GR (reprint author), Vrije Univ Amsterdam, Fac Earth & Life Sci, Boelelaan 1085, NL-1081 HV Amsterdam, Netherlands. EM guido.van.der.werf@falw.vu.nl RI collatz, george/D-5381-2012; Morton, Douglas/D-5044-2012; van der Werf, Guido/M-8260-2016; OI van der Werf, Guido/0000-0001-9042-8630; Kasibhatla, Prasad/0000-0003-3562-3737 NR 23 TC 432 Z9 438 U1 21 U2 137 PU NATURE PUBLISHING GROUP PI NEW YORK PA 75 VARICK ST, 9TH FLR, NEW YORK, NY 10013-1917 USA SN 1752-0894 J9 NAT GEOSCI JI Nat. Geosci. PD NOV PY 2009 VL 2 IS 11 BP 737 EP 738 DI 10.1038/ngeo671 PG 2 WC Geosciences, Multidisciplinary SC Geology GA 514IU UT WOS:000271388500004 ER PT J AU Wang, YF Xu, HF Merino, E Konishi, H AF Wang, Yifeng Xu, Huifang Merino, Enrique Konishi, Hiromi TI Generation of banded iron formations by internal dynamics and leaching of oceanic crust SO NATURE GEOSCIENCE LA English DT Article ID DEPOSITION; KINETICS; HISTORY; ORIGIN; MODEL AB The chemical signatures and mineralogy of banded iron formations have the potential to provide information about the ocean environment on early Earth(1-7). Their formation requires iron- and silicon-rich fluids, but the mechanisms by which the alternating layers of Si- and Fe-rich rock formed remain controversial(8-11). Here we use thermodynamic calculations to show that Fe- and Si- rich fluids can be generated by hydrothermal leaching of low-Al oceanic crustal rocks such as komatiites. We find that positive feedbacks occur among the chemical reactions when hydrothermal fluids mix with ambient sea water. These feedbacks lead to alternating precipitation of Fe and Si minerals, owing to the formation of complexes between Fe(II) and silicic acid. We suggest that the small-scale (<1 cm) banding was produced by internal dynamics of the geochemical system, rather than any external forcing. As the Archaean eon progressed, the oceanic crust produced was rich in Al-12. When Al-rich crust undergoes hydrothermal alteration, Fe is locked in Al-Fe silicate minerals. This results in iron-depleted hydrothermal fluids, and thus prevents the deposition of Fe- rich minerals. We therefore conclude that the widespread cessation of banded iron formation deposition 1.7 billion years ago reflects the changing composition of the oceanic crust. C1 [Wang, Yifeng] Sandia Natl Labs, Albuquerque, NM 87185 USA. [Xu, Huifang; Konishi, Hiromi] Univ Wisconsin, Dept Geol & Geophys, Madison, WI 53706 USA. [Xu, Huifang; Konishi, Hiromi] Univ Wisconsin, NASA, Astrobiol Inst, Madison, WI 53706 USA. [Merino, Enrique] Indiana Univ, Dept Geol Sci, Bloomington, IN 47405 USA. RP Wang, YF (reprint author), Sandia Natl Labs, POB 5800, Albuquerque, NM 87185 USA. EM ywang@sandia.gov FU United States Department of Energy's National Nuclear Security Administration [DE-AC04-94AL85000]; DOE Sandia LDRD Program; NASA Astrobiology Institute [N07-5489]; NSF [EAR-0810150] FX Sandia is a multiprogram laboratory operated by Sandia Corporation, a Lockheed Martin company for the United States Department of Energy's National Nuclear Security Administration under contract DE-AC04-94AL85000. This work is partly supported by DOE Sandia LDRD Program and NASA Astrobiology Institute under grant N07-5489 and NSF (EAR-0810150). The authors thank C. Jove-Colonand C.Bryan of Sandia National Laboratories, C. Klein of University of New Mexico, K. C. Condie of New Mexico Institute of Technology and P.Brown, E.Roden, C. Johnson and J.Valley of the University of Wiscons in for their comments on an early draft of this paper and M. Diman for the artwork of Fig.1. H.X. also thanks D.F. Blake of NASA Ames Research Center, D.Ojakangas of the University of Minnesota-Duluth, P.Fralick of Lakehead University, P.Pufahl of Acadia University and Alumni Geology Field Experience Fund of the Department of Geology and Geophysics of University of Wiscons in for their help with a field trip and C. Klein of University of New Mexico for donating his BIF collection. NR 29 TC 29 Z9 35 U1 3 U2 30 PU NATURE PUBLISHING GROUP PI NEW YORK PA 75 VARICK ST, 9TH FLR, NEW YORK, NY 10013-1917 USA SN 1752-0894 J9 NAT GEOSCI JI Nat. Geosci. PD NOV PY 2009 VL 2 IS 11 BP 781 EP 784 DI 10.1038/NGEO652 PG 4 WC Geosciences, Multidisciplinary SC Geology GA 514IU UT WOS:000271388500021 ER PT J AU Colavita, MM AF Colavita, M. Mark TI Adverse effects in dual-feed interferometry SO NEW ASTRONOMY REVIEWS LA English DT Article ID PALOMAR TESTBED INTERFEROMETER; INFRARED INTERFEROMETRY AB Narrow-angle dual-star interferometric astrometry can provide very high accuracy in the presence of the Earth's turbulent atmosphere. However, to exploit the high atmospherically-limited accuracy requires control of systematic errors in measurement of the interferometer baseline, internal OPDs, and fringe phase. In addition, as high photometric SNR is required, care must be taken to maximize throughput and coherence to obtain high accuracy on faint stars. This article reviews the key aspects of the dual-star approach and implementation, the main contributors to the systematic error budget, and the coherence terms in the photometric error budget. (C) 2010 Elsevier B.V. All rights reserved. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Colavita, MM (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM m.m.colavita@jpl.nasa.gov FU National Aeronautics and Space Administration FX This work was performed at the Jet Propulsion Laboratory, California Institute of Technology, under contract with National Aeronautics and Space Administration. NR 18 TC 5 Z9 5 U1 0 U2 0 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 1387-6473 J9 NEW ASTRON REV JI New Astron. Rev. PD NOV-DEC PY 2009 VL 53 IS 11-12 BP 344 EP 352 DI 10.1016/j.newar.2010.07.004 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 671EI UT WOS:000283482700010 ER PT J AU Pott, JU Woillez, J Akeson, RL Berkey, B Colavita, MM Cooper, A Eisner, JA Ghez, AM Graham, JR Hillenbrand, L Hrynewych, M Medeiros, D Millan-Gabet, R Monnier, J Morrison, D Panteleeva, T Quataert, E Randolph, B Smith, B Summers, K Tsubota, K Tyau, C Weinberg, N Wetherell, E Wizinowich, PL AF Pott, Jorg-Uwe Woillez, Julien Akeson, Rachel L. Berkey, Ben Colavita, Mark M. Cooper, Andrew Eisner, Josh A. Ghez, Andrea M. Graham, James R. Hillenbrand, Lynne Hrynewych, Michael Medeiros, Drew Millan-Gabet, Rafael Monnier, John Morrison, Douglas Panteleeva, Tatyana Quataert, Eliot Randolph, Bill Smith, Brett Summers, Kellee Tsubota, Kevin Tyau, Colette Weinberg, Nevin Wetherell, Ed Wizinowich, Peter L. TI Astrometry with the Keck Interferometer: The ASTRA project and its science SO NEW ASTRONOMY REVIEWS LA English DT Article ID STAR ADAPTIVE OPTICS; GALACTIC-CENTER; STELLAR ORBITS; BLACK-HOLE; PLANETS AB The sensitivity and astrometry upgrade ASTRA of the Keck Interferometer is introduced. After a brief overview of the underlying interferometric principles, the technology and concepts of the upgrade are presented. The interferometric dual-field technology of ASTRA will provide the KI with the means to observe two objects simultaneously, and measure the distance between them with a precision eventually better than 100 mu as. This astrometric functionality of ASTRA will add a unique observing tool to fields of astrophysical research as diverse as exo-planetary kinematics, binary astrometry, and the investigation of stars accelerated by the massive black hole in the center of the Milky Way as discussed in this contribution. (C) 2010 Elsevier B.V. All rights reserved. C1 [Pott, Jorg-Uwe; Woillez, Julien; Berkey, Ben; Cooper, Andrew; Hrynewych, Michael; Medeiros, Drew; Morrison, Douglas; Panteleeva, Tatyana; Randolph, Bill; Smith, Brett; Summers, Kellee; Tsubota, Kevin; Tyau, Colette; Wetherell, Ed; Wizinowich, Peter L.] WM Keck Observ, Kamuela, HI 96743 USA. [Pott, Jorg-Uwe; Ghez, Andrea M.] Univ Calif Los Angeles, Dept Astron, Los Angeles, CA 90095 USA. [Akeson, Rachel L.; Hillenbrand, Lynne; Millan-Gabet, Rafael] NASA, Exoplanet Sci Inst, CALTECH, Pasadena, CA 91125 USA. [Colavita, Mark M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Eisner, Josh A.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Graham, James R.; Quataert, Eliot; Weinberg, Nevin] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Monnier, John] Univ Michigan, Ann Arbor, MI 48109 USA. RP Pott, JU (reprint author), WM Keck Observ, Kamuela, HI 96743 USA. EM jpott@mpia.de FU W.M. Keck Foundation; National Aeronautics and Space Administration; National Science Foundation FX The W.M. Keck Observatory is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W.M. Keck Foundation. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. The Keck Interferometer is funded by the National Aeronautics and Space Administration. The ASTRA upgrade is funded by the Major Research Instrumentation Program of the National Science Foundation. NR 22 TC 6 Z9 6 U1 0 U2 0 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 1387-6473 J9 NEW ASTRON REV JI New Astron. Rev. PD NOV-DEC PY 2009 VL 53 IS 11-12 BP 363 EP 372 DI 10.1016/j.newar.2010.07.009 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 671EI UT WOS:000283482700012 ER PT J AU La Tessa, C Di Fino, L Larosa, M Lee, K Mancusi, D Matthia, D Narici, L Zaconte, V AF La Tessa, C. Di Fino, L. Larosa, M. Lee, K. Mancusi, D. Matthiae, D. Narici, L. Zaconte, V. TI Simulation of ALTEA calibration data with PHITS, FLUKA and GEANT4 SO NUCLEAR INSTRUMENTS & METHODS IN PHYSICS RESEARCH SECTION B-BEAM INTERACTIONS WITH MATERIALS AND ATOMS LA English DT Article DE ALTEA; PHITS; FLUKA; GEANT4; Monte Carlo; Energy spectrum; delta rays ID ACCURATE UNIVERSAL PARAMETERIZATION; ABSORPTION CROSS-SECTIONS; RELATIVISTIC HEAVY-IONS; PARTICLE-TRANSPORT; MODEL AB The ALTEA-Space detector has been calibrated by testing its response to several monochromatic beams. These measurements provided energy-deposition spectra in silicon of 100, 600 and 1000 MeV/nucleon (12)C and 200 and 600 MeV/nucleon (48)Ti. The results have been compared to three Monte Carlo transport codes, namely PHITS, GEANT4 and FLUKA. Median, full width at half maximum (FWHM) and interquartile range (IQR) have been calculated for all datasets to characterize location, width and asymmetry of the energy-deposition spectra. Particular attention has been devoted to the influence of,5 rays on the shape of the energy-deposition spectrum, both with the help of analytical calculations and Monte Carlo simulations. The two approaches proved that, in this range of projectile charge, projectile energy and detector size, the leakage of secondary electrons might introduce a difference between the energy-loss and energy-deposition spectrum, in particular by changing the location, width and symmetry of the distribution. The overall agreement between the Monte Carlo predictions and the measurements is fair and makes PHITS, FLUKA and GEANT4 all possible candidates for simulating ALTEA-Space experiment. (C) 2009 Elsevier B.V. All rights reserved. C1 [La Tessa, C.; Di Fino, L.; Larosa, M.; Narici, L.; Zaconte, V.] Univ Roma Tor Vergata, Dept Phys, I-00133 Rome, Italy. [Mancusi, D.] Univ Liege, B-4000 Liege, Belgium. [Lee, K.] NASA, Lyndon B Johnson Space Ctr, Space Radiat Anal Grp, Houston, TX 77058 USA. [Matthiae, D.] German Aerosp Ctr, Inst Aerosp Med, D-51147 Cologne, Germany. RP Narici, L (reprint author), Univ Roma Tor Vergata, Dept Phys, Via Ric Sci 1, I-00133 Rome, Italy. EM livio.narici@roma2.infn.it OI Mancusi, Davide/0000-0002-2518-8228; Matthia, Daniel/0000-0003-1507-0143 FU ASI [MoMa-ALTEA] FX The authors acknowledge A. De Simone for the help with GEANT4 simulations and ASI (grant MoMa-ALTEA) for the finantial contribution. NR 28 TC 2 Z9 2 U1 1 U2 3 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0168-583X J9 NUCL INSTRUM METH B JI Nucl. Instrum. Methods Phys. Res. Sect. B-Beam Interact. Mater. Atoms PD NOV PY 2009 VL 267 IS 21-22 BP 3549 EP 3557 DI 10.1016/j.nimb.2009.06.086 PG 9 WC Instruments & Instrumentation; Nuclear Science & Technology; Physics, Atomic, Molecular & Chemical; Physics, Nuclear SC Instruments & Instrumentation; Nuclear Science & Technology; Physics GA 524EA UT WOS:000272125400011 ER PT J AU Cooke, MP van Dongen, BE Talbot, HM Semiletov, I Shakhova, N Guo, L Gustafsson, O AF Cooke, Martin P. van Dongen, Bart E. Talbot, Helen M. Semiletov, Igor Shakhova, Natalia Guo, Laodong Gustafsson, Orjan TI Bacteriohopanepolyol biomarker composition of organic matter exported to the Arctic Ocean by seven of the major Arctic rivers SO ORGANIC GEOCHEMISTRY LA English DT Review ID TRAP MASS-SPECTROMETRY; HOPANE SERIES; PROKARYOTIC TRITERPENOIDS; BACTERIAL TRITERPENOIDS; METHANOTROPHIC BACTERIA; SHELF WATERS; SEDIMENTARY BACTERIOHOPANEPOLYOLS; METHYLOBACTERIUM-ORGANOPHILUM; INTACT BACTERIOHOPANEPOLYOLS; RHODOPSEUDOMONAS-ACIDOPHILA AB Bacteriohopanepolyols (BHPs) are a diverse group of membrane lipids produced by a wide variety of bacteria and can be used as molecular biomarkers for bacterial processes and populations in both modern and ancient environments. A group of BHPs, including adenosylhopane and structurally related compounds, have been identified as being specific to soils, enabling the transport of terrestrial organic matter (terrOM) to the marine realm to be monitored. Estuary surface sediment samples were obtained from the five Great Russian Arctic Rivers (GRARs: Ob, Yenisey, Lena, Indigirka and Kolyma) and river sediments were obtained from two North American Rivers (Yukon and Mackenzie). Analysis of the BHP signatures, using high performance liquid chromatography-tandem mass spectrometry (HPLC-MSn), indicated the presence of 15 different BHPs originating from a variety of different bacteria, as well as a significant presence of terrestrially derived OM. Total BHP abundance and the contribution of the "soil-marker" BHPs to the total BHP pool increased eastwards among the GRAR sediments. This suggests increasing terrestrial OM or increased preservation of OM as a result of shorter periods of permafrost thawing. The North American rivers showed greatly differing BHP levels between the Yukon and Mackenzie rivers, with a greater BHP input and thus a relatively higher soil OM contribution from the Yukon. The Indigirka River basin in the eastern Siberian Arctic appeared to be the epicentre in the pan-Arctic BHP distribution trend, with the highest "soil-marker" BHPs but the lowest tetrafunctionalised BHPs. Aminobacteriohopanepentol, an indicator of aerobic methane oxidation, was observed in all the sediments, with the source being either the marine environment or methane producing terrestrial environments. (C) 2009 Elsevier Ltd. All rights reserved. C1 [Cooke, Martin P.; Talbot, Helen M.] Univ Newcastle, Sch Civil Engn & Geosci, Newcastle Upon Tyne NE1 7RU, Tyne & Wear, England. [van Dongen, Bart E.] Univ Manchester, Sch Earth Atmospher & Environm Sci, Manchester M13 9PL, Lancs, England. [van Dongen, Bart E.] Univ Manchester, Williamson Res Ctr Mol Environm Sci, Manchester M13 9PL, Lancs, England. [Semiletov, Igor; Shakhova, Natalia] Univ Alaska, Int Arctic Res Ctr, Fairbanks, AK 99775 USA. [Semiletov, Igor; Shakhova, Natalia] Russian Acad Sci, Far E Branch, Pacific Oceanol Inst, Vladivostok 690041, Russia. [Guo, Laodong] Univ So Mississippi, Stennis Space Ctr, Dept Marine Sci, Hattiesburg, MS 39406 USA. [Gustafsson, Orjan] Stockholm Univ, Dept Appl Environm Sci ITM, SE-10691 Stockholm, Sweden. RP Cooke, MP (reprint author), Univ Newcastle, Sch Civil Engn & Geosci, Drummond Bldg, Newcastle Upon Tyne NE1 7RU, Tyne & Wear, England. EM m.p.cooke@ncl.ac.uk RI Guo, Laodong/F-6045-2010; Semiletov, Igor/B-3616-2013; OI Guo, Laodong/0000-0002-5010-1630; van Dongen, Bart/0000-0003-1189-142X FU Engineering and Physical Science Research Council (EPSRC); HEFCE; Swedish Research Council [621-2004-4039, 629-2002-2309]; Swedish Foundation for Strategic Environmental Research [2002-057]; Far-Eastern Branch of Russian Academy of Sciences (FEBRAS); University Alaska Fair-banks [NA17RJ1224]; Russian Foundation for Basic Research [04-05-64819]; NSF [EAR 0554781, OPP 0436179] FX The project was financially supported in part by funding from the Engineering and Physical Science Research Council (EPSRC) to M.P.C., the Science Research Infrastructure Fund (SRIF) from HEFCE for funding the purchase of the Thermo Electron Finnigan LCQ ion trap mass spectrometer, the Swedish Research Council (VR contract No. 621-2004-4039), a senior research fellowship to O.G. (VR contract No. 629-2002-2309), the Swedish Foundation for Strategic Environmental Research (Mistra contract No. 2002-057), the Far-Eastern Branch of Russian Academy of Sciences (FEBRAS), the International Arctic Research Center of the University Alaska Fair-banks (by the Cooperative Institute for Arctic Research through NOAA Cooperative Agreement NA17RJ1224), the Russian Foundation for Basic Research (No. 04-05-64819) and NSF grants to LG. (EAR #0554781 and OPP #0436179). We thank O. Dudarev and A. Charkin for assistance during sampling, P. Donohoe for assistance with mass spectrometry, and M. Blumenberg and P. Schaeffer for valuable comments. NR 102 TC 26 Z9 26 U1 1 U2 31 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0146-6380 J9 ORG GEOCHEM JI Org. Geochem. PD NOV PY 2009 VL 40 IS 11 BP 1151 EP 1159 DI 10.1016/j.orggeochem.2009.07.014 PG 9 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 524AN UT WOS:000272116300005 ER PT J AU Franks, S Masek, JG Headley, RMK Gasch, J Arvidson, T AF Franks, Shannon Masek, Jeffrey G. Headley, Rachel M. K. Gasch, John Arvidson, Terry TI Large Area Scene Selection Interface (LASSI): Methodology of Selecting Landsat Imagery for the Global Land Survey 2005. SO PHOTOGRAMMETRIC ENGINEERING AND REMOTE SENSING LA English DT Review ID DATA SET; COVER AB The Global Land Survey (GLS) 2005 is a cloud-free, orthorectified collection of Landsat imagery acquired during the 2004 to 2007 epoch intended to support global land-cover and ecological monitoring. Due to the numerous complexities in selecting imagery for the GLS2005, NASA and the U.S. Geological Survey (USGS) sponsored the development of an automated scene selection tool, the Large Area Scene Selection Interface (LASSI), to aid in the selection of imagery for this data set. This innovative approach to scene selection applied a user-defined weighting system to various scene parameters: image cloud cover, image vegetation greenness, choice of sensor, and the ability of the Landsat-7 Scan Line Corrector (SLC)-off pair to completely fill image gaps, among others. The parameters considered in scene selection were weighted according to their relative importance to the data set, along with the algorithm's sensitivity to that weight. This paper describes the methodology and analysis that established the parameter weighting strategy, as well as the post-screening processes used in selecting the optimal data set for GLS2005. C1 [Franks, Shannon] Stinger Ghaffarian Technol Inc, Goddard Space Flight Ctr Code 614 4, Greenbelt, MD 20771 USA. [Franks, Shannon] Univ Maryland, Dept Geog, College Pk, MD 20742 USA. [Masek, Jeffrey G.] NASA, Goddard Space Flight Ctr, Biospher Sci Branch Code 614 4, Greenbelt, MD 20771 USA. [Headley, Rachel M. K.] EROS, USGS Ctr, Sioux Falls, SD 57198 USA. [Gasch, John] Emalico LLC, Goddard Space Flight Ctr Code 428 1, Greenbelt, MD 20771 USA. [Arvidson, Terry] Lockheed Martin, Goddard Space Flight Ctr Code 614 4, Greenbelt, MD 20771 USA. RP Franks, S (reprint author), Stinger Ghaffarian Technol Inc, Goddard Space Flight Ctr Code 614 4, Greenbelt, MD 20771 USA. EM Shannon.franks@nasa.gov RI Masek, Jeffrey/D-7673-2012 FU NASA FX We would like to thank the NASA Land Cover Land Use Change (LCLUC) program for their support in funding the work. We also thank Darrel Williams for added support through the Landsat Project Science Office. This work could not be accomplished without Dr. Robert A. Morris and Dr. Lina Khatib at the Computational Sciences Division of NASA Ames Research Center for developing the Global Map Generator (GMG) algorithm, which serves as the heart of LASSI. Lastly, we appreciate the reviewers' constructive comments. NR 9 TC 13 Z9 15 U1 0 U2 1 PU AMER SOC PHOTOGRAMMETRY PI BETHESDA PA 5410 GROSVENOR LANE SUITE 210, BETHESDA, MD 20814-2160 USA SN 0099-1112 J9 PHOTOGRAMM ENG REM S JI Photogramm. Eng. Remote Sens. PD NOV PY 2009 VL 75 IS 11 BP 1287 EP 1296 PG 10 WC Geography, Physical; Geosciences, Multidisciplinary; Remote Sensing; Imaging Science & Photographic Technology SC Physical Geography; Geology; Remote Sensing; Imaging Science & Photographic Technology GA 522UM UT WOS:000272024500007 ER PT J AU Huang, SL Connaughton, Z Potter, CS Genovese, V Crabtree, RL Fu, PD AF Huang, Shengli Connaughton, Zachary Potter, Christopher S. Genovese, Vanessa Crabtree, Robert L. Fu, Pinde TI MODELING NEAR-SURFACE AIR TEMPERATURE FROM SOLAR RADIATION AND LAPSE RATE: NEW DEVELOPMENT ON SHORT-TERM MONTHLY AND DAILY APPROACH SO PHYSICAL GEOGRAPHY LA English DT Article DE montane eco-system; surface temperature; temperature anomalies; inverse distance weighting; Yellowstone National Park ID INTERPOLATION AB Short-term monthly mean temperature (T(m)) and short-term daily mean temperature (T(d)) rather than long-term monthly and daily mean temperature ((T) over bar (m) and (T) over bar (d)) are preferred for some ecosystem studies such as carbon source and sink, pine beetle mortality, and snow melting. The recent progress of modeling T(m) and T(d) (based on the previous work on (T) over bar (m)) supported by climatologically aided interpolation (CAI) is reported over the mountainous Yellowstone National Park. With the spatial scale of a 30 m digital elevation model (DEM), the slope, aspect, and shadows cast by surrounding topography, which could not be well captured by very coarse DEM, could be taken into account. Data from 12 months (Jan-Dec 2008) and 12 dates (25 Jan-Dec 2008) were used to demonstrate the approach. Inverse distance weighting (IDW) interpolations of limited temperature anomalies were adopted to represent the deviations from normality. (T) over bar (m), as a preexisting climatology surface, was added to deviations in order to model T(m). Linear temporal interpolation of adjacent (T) over bar (m) was used to create a climatology surface, which was then added to deviations in order to model T(d). Results show the mean absolute errors (MAEs) for T(m) ranged from 0.75 degrees C to 1.78 degrees C, while the MAEs for T(d) ranged from 1.14 degrees C to 2.02 degrees C. The four factors of elevation, seasonal change of lapse rate, temperature difference caused by variation in solar radiation, and preexisting climatology surface for the CAI approach were comprehensively considered in this approach. C1 [Huang, Shengli; Potter, Christopher S.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Huang, Shengli; Crabtree, Robert L.] Yellowstone Ecol Res Ctr, Bozeman, MT 59718 USA. [Connaughton, Zachary] Montana State Univ, Dept Mech Engn, Bozeman, MT 59715 USA. [Genovese, Vanessa] Calif State Univ, Seaside, CA 93955 USA. [Fu, Pinde] Environm Syst Res Inst ESRI Inc, Redlands, CA 92373 USA. RP Huang, SL (reprint author), NASA, Ames Res Ctr, Mail Stop 242-4, Moffett Field, CA 94035 USA. FU NASA [NNS06AA23G] FX We thank NASA for providing financial support (contract No. NNS06AA23G). This research was also supported by an appointment to the NASA Postdoctoral Program at the Ames Research Center, administered by Oak Ridge Associated Universities through a contract with NASA. We also thank Mrs. Mei Peng for collecting and pre-processing weather data. NR 12 TC 2 Z9 2 U1 2 U2 4 PU BELLWETHER PUBL LTD PI COLUMBIA PA 8640 GUILFORD RD, STE 200, COLUMBIA, MD 21046 USA SN 0272-3646 J9 PHYS GEOGR JI Phys. Geogr. PD NOV-DEC PY 2009 VL 30 IS 6 BP 517 EP 527 DI 10.2747/0272-3646.30.6.517 PG 11 WC Environmental Sciences; Geography, Physical; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Physical Geography; Geology; Meteorology & Atmospheric Sciences GA 532FC UT WOS:000272729800003 ER PT J AU Guha, S Erkmen, BI AF Guha, Saikat Erkmen, Baris I. TI Gaussian-state quantum-illumination receivers for target detection SO PHYSICAL REVIEW A LA English DT Article DE error statistics; laser beams; object detection; optical frequency conversion; optical receivers; optical sensors; optical transmitters; quantum communication; quantum entanglement; quantum optics AB The signal half of an entangled twin beam, generated using spontaneous parametric downconversion, interrogates a region of space that is suspected of containing a target and has high loss and high (entanglement-breaking) background noise. A joint measurement is performed on the returned light and the idler beam that was retained at the transmitter. An optimal quantum receiver, whose implementation is not yet known, was shown to achieve 6 dB gain in the error-probability exponent relative to that achieved with a single coherent-state (classical) laser transmitter and the optimum receiver. We present two structured optical receivers that achieve up to 3 dB gain in the error exponent over that attained with the classical sensor. These are designs of quantum-optical sensors for target detection, which can be readily implemented in a proof-of-concept experiment, that appreciably outperform the best classical sensor in the low-signal-brightness, high-loss, and high-noise operating regime. C1 [Guha, Saikat] BBN Technol, Disrupt Informat Proc, Cambridge, MA 02138 USA. [Erkmen, Baris I.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Guha, S (reprint author), BBN Technol, Disrupt Informat Proc, Cambridge, MA 02138 USA. FU National Aeronautics and Space Administration FX The authors thank J. H. Shapiro for making the observation about generalizing the coherent-state performance bound to arbitrary signal-idler classically-correlated transmitters. The authors also thank F. Wong, S. Lloyd, and Z. Dutton for valuable discussions. S. G. thanks the DARPA Quantum Sensors Program and BBN Technologies. B. I. E.' s contribution to the research described in this paper was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. NR 11 TC 44 Z9 47 U1 0 U2 14 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1050-2947 J9 PHYS REV A JI Phys. Rev. A PD NOV PY 2009 VL 80 IS 5 AR 052310 DI 10.1103/PhysRevA.80.052310 PG 4 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 526RH UT WOS:000272310000045 ER PT J AU Mishchenko, MI Dlugach, JM Liu, L AF Mishchenko, Michael I. Dlugach, Janna M. Liu, Li TI Azimuthal asymmetry of the coherent backscattering cone: Theoretical results SO PHYSICAL REVIEW A LA English DT Article DE backscatter; light coherence; light polarisation; light scattering; Maxwell equations ID SOLAR-SYSTEM BODIES; WEAK-LOCALIZATION; MULTIPLE-SCATTERING; POLARIZED-LIGHT; ELECTROMAGNETIC-WAVES; SPHERICAL-PARTICLES; GALILEAN SATELLITES; MEDIA; ABSORPTION; CLUSTERS AB The azimuthal asymmetry of the polarized backscattering cone and the intimately related polarization opposition effect (POE) are corollaries of the theory of coherent backscattering (CB) valid in the asymptotic limit of very small particle packing density. In this paper we use numerically exact solutions of the Maxwell equations to study the evolution of these and other manifestations of CB as the packing density in a multiparticle group increases from zero to values typical of actual particle suspensions and particulate surfaces. Our results reveal a remarkable robustness of virtually all effects predicted by the low-density concept of CB and allow us to conclude that the azimuthal asymmetry and POE observed in the laboratory for densely packed discrete random media are indeed caused by CB. C1 [Mishchenko, Michael I.; Liu, Li] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Dlugach, Janna M.] Natl Acad Sci Ukraine, Main Astron Observ, UA-03680 Kiev, Ukraine. RP Mishchenko, MI (reprint author), NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA. EM mmishchenko@giss.nasa.gov RI Mishchenko, Michael/D-4426-2012 NR 51 TC 24 Z9 24 U1 2 U2 4 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 2469-9926 EI 2469-9934 J9 PHYS REV A JI Phys. Rev. A PD NOV PY 2009 VL 80 IS 5 AR 053824 DI 10.1103/PhysRevA.80.053824 PG 10 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 526RH UT WOS:000272310000170 ER PT J AU Delaire, O May, AF McGuire, MA Porter, WD Lucas, MS Stone, MB Abernathy, DL Ravi, VA Firdosy, SA Snyder, GJ AF Delaire, O. May, A. F. McGuire, M. A. Porter, W. D. Lucas, M. S. Stone, M. B. Abernathy, D. L. Ravi, V. A. Firdosy, S. A. Snyder, G. J. TI Phonon density of states and heat capacity of La3-xTe4 SO PHYSICAL REVIEW B LA English DT Article DE band structure; bonds (chemical); Debye temperature; lanthanum alloys; neutron diffraction; phonons; specific heat; tellurium alloys; vacancies (crystal) ID THERMOELECTRIC-MATERIALS; CHALCOGENIDES; TH3P4 AB The phonon density of states (DOS) of La3-xTe4 compounds (x=0.0,0.18,0.32) was measured at 300, 520, and 780 K, using inelastic neutron scattering. A significant stiffening of the phonon DOS and a large broadening of features were observed upon introduction of vacancies on La sites (increasing x). Heat-capacity measurements were performed at temperatures 1.85 < T < 1200 K and were analyzed to quantify the contributions of phonons and electrons. The Debye temperature and the electronic coefficient of heat capacity determined from these measurements are consistent with the neutron-scattering results, and with previously reported first-principles calculations. Our results indicate that La vacancies in La3-xTe4 strongly scatter phonons and this source of scattering appears to be independent of temperature. The stiffening of the phonon DOS induced by the introduction of vacancies is explained in terms of the electronic structure and the change in bonding character. The temperature dependence of the phonon DOS is captured satisfactorily by the quasiharmonic approximation. C1 [Delaire, O.; Lucas, M. S.; Stone, M. B.; Abernathy, D. L.] Oak Ridge Natl Lab, Neutron Scattering Sci Div, Oak Ridge, TN 37831 USA. [May, A. F.; Snyder, G. J.] CALTECH, Pasadena, CA 91125 USA. [McGuire, M. A.; Porter, W. D.] Oak Ridge Natl Lab, Div Mat Sci & Technol, Oak Ridge, TN 37831 USA. [Ravi, V. A.; Firdosy, S. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Ravi, V. A.] Calif State Polytech Univ Pomona, Dept Chem & Mat Engn, Pomona, CA 91768 USA. RP Delaire, O (reprint author), Oak Ridge Natl Lab, Neutron Scattering Sci Div, Oak Ridge, TN 37831 USA. RI McGuire, Michael/B-5453-2009; May, Andrew/E-5897-2011; Snyder, G. Jeffrey/E-4453-2011; Stone, Matthew/G-3275-2011; Abernathy, Douglas/A-3038-2012; Snyder, G/I-2263-2015; BL18, ARCS/A-3000-2012 OI McGuire, Michael/0000-0003-1762-9406; May, Andrew/0000-0003-0777-8539; Snyder, G. Jeffrey/0000-0003-1414-8682; Stone, Matthew/0000-0001-7884-9715; Abernathy, Douglas/0000-0002-3533-003X; FU Scientific User Facilities Division, Office of Basic Energy Sciences, U. S. DOE. High-temperature; U. S. Department of Energy, Office of Energy Efficiency and Renewable Energy; NSF [DMR- 0520547.] FX We thank David Singh for providing us with the numerical data for the electronic DOS of La3Te4 published in Ref. 27, and for helpful discussions. We thank Rebecca A. Mills for help with the neutron- scattering furnace. This work was partially supported by the Division of Materials Science and Engineering, Basic Energy Sciences, U. S. DOE. Work performed at the California Institute of Technology was done with the assistance of the Jet Propulsion Laboratory, under a contract with the National Aeronautics and Space Administration. The Research at Oak Ridge National Laboratory's Spallation Neutron Source was sponsored by the Scientific User Facilities Division, Office of Basic Energy Sciences, U. S. DOE. High-temperature calorimetry measurements were conducted at Oak Ridge National Laboratory's High Temperature Materials Laboratory, sponsored by the U. S. Department of Energy, Office of Energy Efficiency and Renewable Energy, Vehicle Technologies Program. This work benefitted from DANSE software developed under NSF under Award No. DMR- 0520547. NR 35 TC 39 Z9 39 U1 4 U2 38 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 2469-9950 EI 2469-9969 J9 PHYS REV B JI Phys. Rev. B PD NOV PY 2009 VL 80 IS 18 AR 184302 DI 10.1103/PhysRevB.80.184302 PG 9 WC Physics, Condensed Matter SC Physics GA 526RO UT WOS:000272310900058 ER PT J AU Abbott, BP Abbott, R Adhikari, R Ajith, P Allen, B Allen, G Amin, RS Anderson, SB Anderson, WG Arain, MA Araya, M Armandula, H Armor, P Aso, Y Aston, S Aufmuth, P Aulbert, C Babak, S Baker, P Ballmer, S Barker, C Barker, D Barr, B Barriga, P Barsotti, L Barton, MA Bartos, I Bassiri, R Bastarrika, M Behnke, B Benacquista, M Betzwieser, J Beyersdorf, PT Bilenko, IA Billingsley, G Biswas, R Black, E Blackburn, JK Blackburn, L Blair, D Bland, B Bodiya, TP Bogue, L Bork, R Boschi, V Bose, S Brady, PR Braginsky, VB Brau, JE Bridges, DO Brinkmann, M Brooks, AF Brown, DA Brummit, A Brunet, G Bullington, A Buonanno, A Burmeister, O Byer, RL Cadonati, L Camp, JB Cannizzo, J Cannon, KC Cao, J Cardenas, L Caride, S Castaldi, G Caudill, S Cavaglia, M Cepeda, C Chalermsongsak, T Chalkley, E Charlton, P Chatterji, S Chelkowski, S Chen, Y Christensen, N Chung, CTY Clark, D Clark, J Clayton, JH Cokelaer, T Colacino, CN Conte, R Cook, D Corbitt, TRC Cornish, N Coward, D Coyne, DC Creighton, JDE Creighton, TD Cruise, AM Culter, RM Cumming, A Cunningham, L Danilishin, SL Danzmann, K Daudert, B Davies, G Daw, EJ DeBra, D Degallaix, J Dergachev, V Desai, S DeSalvo, R Dhurandhar, S Diaz, M Di Credico, A Dietz, A Donovan, F Dooley, KL Doomes, EE Drever, RWP Dueck, J Duke, I Dumas, JC Dwyer, JG Echols, C Edgar, M Effler, A Ehrens, P Espinoza, E Etzel, T Evans, M Evans, T Fairhurst, S Faltas, Y Fan, Y Fazi, D Fehrmann, H Finn, LS Flasch, K Foley, S Forrest, C Fotopoulos, N Franzen, A Frede, M Frei, M Frei, Z Freise, A Frey, R Fricke, T Fritschel, P Frolov, VV Fyffe, M Galdi, V Garofoli, JA Gholami, I Giaime, JA Giampanis, S Giardina, KD Goda, K Goetz, E Goggin, LM Gonzalez, G Gorodetsky, ML Gossler, S Gouaty, R Grant, A Gras, S Gray, C Gray, M Greenhalgh, RJS Gretarsson, AM Grimaldi, F Grosso, R Grote, H Grunewald, S Guenther, M 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Raics, Z Rainer, N Rakhmanov, M Raymond, V Reed, CM Reed, T Rehbein, H Reid, S Reitze, DH Riesen, R Riles, K Rivera, B Roberts, P Robertson, NA Robinson, C Robinson, EL Roddy, S Rover, C Rollins, J Romano, JD Romie, JH Rowan, S Rudiger, A Russell, P Ryan, K Sakata, S de la Jordana, LS Sandberg, V Sannibale, V Santamaria, L Saraf, S Sarin, P Sathyaprakash, BS Sato, S Satterthwaite, M Saulson, PR Savage, R Savov, P Scanlan, M Schilling, R Schnabel, R Schofield, R Schulz, B Schutz, BF Schwinberg, P Scott, J Scott, SM Searle, AC Sears, B Seifert, F Sellers, D Sengupta, AS Sergeev, A Shapiro, B Shawhan, P Shoemaker, DH Sibley, A Siemens, X Sigg, D Sinha, S Sintes, AM Slagmolen, BJJ Slutsky, J Smith, JR Smith, MR Smith, ND Somiya, K Sorazu, B Stein, A Stein, LC Steplewski, S Stochino, A Stone, R Strain, KA Strigin, S Stroeer, A Stuver, AL Summerscales, TZ Sun, KX Sung, M Sutton, PJ Szokoly, GP Talukder, D Tang, L Tanner, DB Tarabrin, SP Taylor, JR Taylor, R Thacker, J Thorne, KA Thuring, A Tokmakov, KV Torres, C Torrie, C Traylor, G Trias, M Ugolini, D Ulmen, J Urbanek, K Vahlbruch, H Vallisneri, M Van Den Broeck, C van der Sluys, MV van Veggel, AA Vass, S Vaulin, R Vecchio, A Veitch, J Veitch, P Veltkamp, C Villar, A Vorvick, C Vyachanin, SP Waldman, SJ Wallace, L Ward, RL Weidner, A Weinert, M Weinstein, AJ Weiss, R Wen, L Wen, S Wette, K Whelan, JT Whitcomb, SE Whiting, BF Wilkinson, C Willems, PA Williams, HR Williams, L Willke, B Wilmut, I Winkelmann, L Winkler, W Wipf, CC Wiseman, AG Woan, G Wooley, R Worden, J Wu, W Yakushin, I Yamamoto, H Yan, Z Yoshida, S Zanolin, M Zhang, J Zhang, L Zhao, C Zotov, N Zucker, ME zur Mulhlen, H Zweizig, J AF Abbott, B. P. Abbott, R. Adhikari, R. Ajith, P. Allen, B. Allen, G. Amin, R. S. Anderson, S. B. Anderson, W. G. Arain, M. A. Araya, M. Armandula, H. Armor, P. Aso, Y. Aston, S. Aufmuth, P. Aulbert, C. Babak, S. Baker, P. Ballmer, S. Barker, C. Barker, D. Barr, B. Barriga, P. Barsotti, L. Barton, M. A. Bartos, I. Bassiri, R. Bastarrika, M. Behnke, B. Benacquista, M. Betzwieser, J. Beyersdorf, P. T. Bilenko, I. A. Billingsley, G. Biswas, R. Black, E. Blackburn, J. K. Blackburn, L. Blair, D. Bland, B. Bodiya, T. P. Bogue, L. Bork, R. Boschi, V. Bose, S. Brady, P. R. Braginsky, V. B. Brau, J. E. Bridges, D. O. Brinkmann, M. Brooks, A. F. Brown, D. A. Brummit, A. Brunet, G. Bullington, A. Buonanno, A. Burmeister, O. Byer, R. L. Cadonati, L. Camp, J. B. Cannizzo, J. Cannon, K. C. Cao, J. Cardenas, L. Caride, S. Castaldi, G. Caudill, S. Cavaglia, M. Cepeda, C. Chalermsongsak, T. Chalkley, E. Charlton, P. Chatterji, S. Chelkowski, S. Chen, Y. Christensen, N. Chung, C. T. Y. Clark, D. Clark, J. Clayton, J. H. Cokelaer, T. Colacino, C. N. Conte, R. Cook, D. Corbitt, T. R. C. Cornish, N. Coward, D. Coyne, D. C. Creighton, J. D. E. Creighton, T. D. Cruise, A. M. Culter, R. M. Cumming, A. Cunningham, L. Danilishin, S. L. Danzmann, K. Daudert, B. Davies, G. Daw, E. J. DeBra, D. Degallaix, J. Dergachev, V. Desai, S. DeSalvo, R. Dhurandhar, S. Diaz, M. Di Credico, A. Dietz, A. Donovan, F. Dooley, K. L. Doomes, E. E. Drever, R. W. P. Dueck, J. Duke, I. Dumas, J. -C. Dwyer, J. G. Echols, C. Edgar, M. Effler, A. Ehrens, P. Espinoza, E. Etzel, T. Evans, M. Evans, T. Fairhurst, S. Faltas, Y. Fan, Y. Fazi, D. Fehrmann, H. Finn, L. S. Flasch, K. Foley, S. Forrest, C. Fotopoulos, N. Franzen, A. Frede, M. Frei, M. Frei, Z. Freise, A. Frey, R. Fricke, T. Fritschel, P. Frolov, V. V. Fyffe, M. Galdi, V. Garofoli, J. A. Gholami, I. Giaime, J. A. Giampanis, S. Giardina, K. D. Goda, K. Goetz, E. Goggin, L. M. Gonzalez, G. Gorodetsky, M. L. Gossler, S. Gouaty, R. Grant, A. Gras, S. Gray, C. Gray, M. Greenhalgh, R. J. S. Gretarsson, A. M. Grimaldi, F. Grosso, R. Grote, H. Grunewald, S. Guenther, M. Gustafson, E. K. Gustafson, R. Hage, B. Hallam, J. M. Hammer, D. Hammond, G. D. Hanna, C. Hanson, J. Harms, J. Harry, G. M. Harry, I. W. Harstad, E. D. Haughian, K. Hayama, K. Heefner, J. Heng, I. S. Heptonstall, A. Hewitson, M. Hild, S. Hirose, E. Hoak, D. Hodge, K. A. Holt, K. Hosken, D. J. Hough, J. Hoyland, D. Hughey, B. Huttner, S. H. Ingram, D. R. Isogai, T. Ito, M. Ivanov, A. Johnson, B. Johnson, W. W. Jones, D. I. Jones, G. Jones, R. Ju, L. Kalmus, P. Kalogera, V. Kandhasamy, S. Kanner, J. Kasprzyk, D. Katsavounidis, E. Kawabe, K. Kawamura, S. Kawazoe, F. Kells, W. Keppel, D. G. Khalaidovski, A. Khalili, F. Y. Khan, R. Khazanov, E. King, P. Kissel, J. S. Klimenko, S. Kokeyama, K. Kondrashov, V. Kopparapu, R. Koranda, S. Kozak, D. Krishnan, B. Kumar, R. Kwee, P. Lam, P. K. Landry, M. Lantz, B. Lazzarini, A. Lei, H. Lei, M. Leindecker, N. Leonor, I. Li, C. Lin, H. Lindquist, P. E. Littenberg, T. B. Lockerbie, N. A. Lodhia, D. Longo, M. Lormand, M. Lu, P. Lubinski, M. Lucianetti, A. Lueck, H. Machenschalk, B. MacInnis, M. Mageswaran, M. Mailand, K. Mandel, I. Mandic, V. Marka, S. Marka, Z. Markosyan, A. Markowitz, J. Maros, E. Martin, I. W. Martin, R. M. Marx, J. N. Mason, K. Matichard, F. Matone, L. Matzner, R. A. Mavalvala, N. McCarthy, R. McClelland, D. E. McGuire, S. C. McHugh, M. McIntyre, G. McKechan, D. J. A. McKenzie, K. Mehmet, M. Melatos, A. Melissinos, A. C. Menendez, D. F. Mendell, G. Mercer, R. A. Meshkov, S. Messenger, C. Meyer, M. S. Miller, J. Minelli, J. Mino, Y. Mitrofanov, V. P. Mitselmakher, G. Mittleman, R. Miyakawa, O. Moe, B. Mohanty, S. D. Mohapatra, S. R. P. Moreno, G. Morioka, T. Mors, K. Mossavi, K. MowLowry, C. Mueller, G. Mueller-Ebhardt, H. Muhammad, D. Mukherjee, S. Mukhopadhyay, H. Mullavey, A. Munch, J. Murray, P. G. Myers, E. Myers, J. Nash, T. Nelson, J. Newton, G. Nishizawa, A. Numata, K. O'Dell, J. O'Reilly, B. O'Shaughnessy, R. Ochsner, E. Ogin, G. H. Ottaway, D. J. Ottens, R. S. Overmier, H. Owen, B. J. Pan, Y. Pankow, C. Papa, M. A. Parameshwaraiah, V. Patel, P. Pedraza, M. Penn, S. Perraca, A. Pierro, V. Pinto, I. M. Pitkin, M. Pletsch, H. J. Plissi, M. V. Postiglione, F. Principe, M. Prix, R. Prokhorov, L. Puncken, O. Quetschke, V. Raab, F. J. Rabeling, D. S. Radkins, H. Raffai, P. Raics, Z. Rainer, N. Rakhmanov, M. Raymond, V. Reed, C. M. Reed, T. Rehbein, H. Reid, S. Reitze, D. H. Riesen, R. Riles, K. Rivera, B. Roberts, P. Robertson, N. A. Robinson, C. Robinson, E. L. Roddy, S. Roever, C. Rollins, J. Romano, J. D. Romie, J. H. Rowan, S. Ruediger, A. Russell, P. Ryan, K. Sakata, S. Sancho de la Jordana, L. Sandberg, V. Sannibale, V. Santamaria, L. Saraf, S. Sarin, P. Sathyaprakash, B. S. Sato, S. Satterthwaite, M. Saulson, P. R. Savage, R. Savov, P. Scanlan, M. Schilling, R. Schnabel, R. Schofield, R. Schulz, B. Schutz, B. F. Schwinberg, P. Scott, J. Scott, S. M. Searle, A. C. Sears, B. Seifert, F. Sellers, D. Sengupta, A. S. Sergeev, A. Shapiro, B. Shawhan, P. Shoemaker, D. H. Sibley, A. Siemens, X. Sigg, D. Sinha, S. Sintes, A. M. Slagmolen, B. J. J. Slutsky, J. Smith, J. R. Smith, M. R. Smith, N. D. Somiya, K. Sorazu, B. Stein, A. Stein, L. C. Steplewski, S. Stochino, A. Stone, R. Strain, K. A. Strigin, S. Stroeer, A. Stuver, A. L. Summerscales, T. Z. Sun, K. -X. Sung, M. Sutton, P. J. Szokoly, G. P. Talukder, D. Tang, L. Tanner, D. B. Tarabrin, S. P. Taylor, J. R. Taylor, R. Thacker, J. Thorne, K. A. Thuering, A. Tokmakov, K. V. Torres, C. Torrie, C. Traylor, G. Trias, M. Ugolini, D. Ulmen, J. Urbanek, K. Vahlbruch, H. Vallisneri, M. Van Den Broeck, C. van der Sluys, M. V. van Veggel, A. A. Vass, S. Vaulin, R. Vecchio, A. Veitch, J. Veitch, P. Veltkamp, C. Villar, A. Vorvick, C. Vyachanin, S. P. Waldman, S. J. Wallace, L. Ward, R. L. Weidner, A. Weinert, M. Weinstein, A. J. Weiss, R. Wen, L. Wen, S. Wette, K. Whelan, J. T. Whitcomb, S. E. Whiting, B. F. Wilkinson, C. Willems, P. A. Williams, H. R. Williams, L. Willke, B. Wilmut, I. Winkelmann, L. Winkler, W. Wipf, C. C. Wiseman, A. G. Woan, G. Wooley, R. Worden, J. Wu, W. Yakushin, I. Yamamoto, H. Yan, Z. Yoshida, S. Zanolin, M. Zhang, J. Zhang, L. Zhao, C. Zotov, N. Zucker, M. E. zur Muelhlen, H. Zweizig, J. CA LIGO Sci Collaboration TI Search for gravitational-wave bursts in the first year of the fifth LIGO science run SO PHYSICAL REVIEW D LA English DT Article ID DETECTORS; COLLAPSE AB We present the results obtained from an all-sky search for gravitational-wave (GW) bursts in the 64-2000 Hz frequency range in data collected by the LIGO detectors during the first year (November 2005-November 2006) of their fifth science run. The total analyzed live time was 268.6 days. Multiple hierarchical data analysis methods were invoked in this search. The overall sensitivity expressed in terms of the root-sum-square (rss) strain amplitude h(rss) for gravitational-wave bursts with various morphologies was in the range of 6x10(-22) Hz(-1/2) to a fewx10(-21) Hz(-1/2). No GW signals were observed and a frequentist upper limit of 3.75 events per year on the rate of strong GW bursts was placed at the 90% confidence level. As in our previous searches, we also combined this rate limit with the detection efficiency for selected waveform morphologies to obtain event rate versus strength exclusion curves. In sensitivity, these exclusion curves are the most stringent to date. C1 [Abbott, B. P.; Abbott, R.; Adhikari, R.; Anderson, S. B.; Araya, M.; Armandula, H.; Aso, Y.; Ballmer, S.; Barton, M. A.; Betzwieser, J.; Billingsley, G.; Black, E.; Blackburn, J. K.; Bork, R.; Boschi, V.; Brooks, A. F.; Cannon, K. C.; Cardenas, L.; Cepeda, C.; Chalermsongsak, T.; Chatterji, S.; Coyne, D. C.; Daudert, B.; DeSalvo, R.; Echols, C.; Ehrens, P.; Espinoza, E.; Etzel, T.; Fazi, D.; Gustafson, E. K.; Hanna, C.; Heefner, J.; Heptonstall, A.; Hodge, K. A.; Ivanov, A.; Kalmus, P.; Kells, W.; Keppel, D. G.; King, P.; Kondrashov, V.; Kozak, D.; Lazzarini, A.; Lei, M.; Lindquist, P. E.; Mageswaran, M.; Mailand, K.; Maros, E.; Marx, J. N.; McIntyre, G.; Meshkov, S.; Miyakawa, O.; Nash, T.; Ogin, G. H.; Patel, P.; Pedraza, M.; Robertson, N. A.; Russell, P.; Sannibale, V.; Searle, A. C.; Sears, B.; Sengupta, A. S.; Smith, M. R.; Stochino, A.; Taylor, R.; Torrie, C.; Vass, S.; Villar, A.; Wallace, L.; Ward, R. L.; Weinstein, A. J.; Whitcomb, S. E.; Willems, P. A.; Yamamoto, H.; Zhang, L.; Zweizig, J.] CALTECH, LIGO, Pasadena, CA 91125 USA. [Babak, S.; Behnke, B.; Chen, Y.; Gholami, I.; Grunewald, S.; Krishnan, B.; Machenschalk, B.; Papa, M. A.; Robinson, E. L.; Santamaria, L.; Schutz, B. F.; Whelan, J. T.] Max Planck Inst, Albert Einstein Inst, D-14476 Golm, Germany. 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[Chen, Y.; Li, C.; Mino, Y.; Savov, P.; Somiya, K.; Vallisneri, M.; Wen, L.] CALTECH, CaRT, Pasadena, CA 91125 USA. [Clark, J.; Cokelaer, T.; Davies, G.; Dietz, A.; Fairhurst, S.; Harry, I. W.; Jones, G.; McKechan, D. J. A.; Robinson, C.; Sathyaprakash, B. S.; Schutz, B. F.; Sutton, P. J.; Van Den Broeck, C.] Cardiff Univ, Cardiff CF24 3AA, S Glam, Wales. [Christensen, N.; Isogai, T.] Carleton Coll, Northfield, MN 55057 USA. [Charlton, P.] Charles Sturt Univ, Wagga Wagga, NSW 2678, Australia. [Bartos, I.; Dwyer, J. G.; Khan, R.; Marka, S.; Marka, Z.; Matone, L.; Raics, Z.; Rollins, J.] Columbia Univ, New York, NY 10027 USA. [Gretarsson, A. M.; Zanolin, M.] Embry Riddle Aeronaut Univ, Prescott, AZ 86301 USA. [Colacino, C. N.; Frei, Z.; Raffai, P.; Szokoly, G. P.] Eotvos Lorand Univ, ELTE, H-1053 Budapest, Hungary. [Penn, S.] Hobart & William Smith Coll, Geneva, NY 14456 USA. [Khazanov, E.; Sergeev, A.] Inst Appl Phys, Nizhnii Novgorod 603950, Russia. [Dhurandhar, S.; Mukhopadhyay, H.] Interuniv Ctr Astron & Astrophys, Pune 411007, Maharashtra, India. [Aufmuth, P.; Danzmann, K.; Franzen, A.; Hage, B.; Kwee, P.; Lueck, H.; Thuering, A.; Vahlbruch, H.; Willke, B.; zur Muelhlen, H.] Leibniz Univ Hannover, D-30167 Hannover, Germany. [Barker, C.; Barker, D.; Bland, B.; Cook, D.; Effler, A.; Gray, C.; Guenther, M.; Ingram, D. R.; Johnson, B.; Kawabe, K.; Landry, M.; McCarthy, R.; Mendell, G.; Moreno, G.; Myers, E.; Myers, J.; Parameshwaraiah, V.; Raab, F. J.; Radkins, H.; Reed, C. M.; Rivera, B.; Ryan, K.; Sandberg, V.; Savage, R.; Schwinberg, P.; Sigg, D.; Vorvick, C.; Wilkinson, C.; Worden, J.] Hanford Observ, LIGO, Richland, WA 99352 USA. [Bogue, L.; Bridges, D. O.; Evans, T.; Fricke, T.; Frolov, V. V.; Fyffe, M.; Giaime, J. A.; Giardina, K. D.; Hanson, J.; Hoak, D.; Holt, K.; Lormand, M.; Meyer, M. S.; Muhammad, D.; O'Reilly, B.; Overmier, H.; Riesen, R.; Roddy, S.; Romie, J. H.; Sellers, D.; Sibley, A.; Stuver, A. L.; Thacker, J.; Thorne, K. A.; Torres, C.; Traylor, G.; Wooley, R.; Yakushin, I.] Livingston Observ, LIGO, Livingston, LA 70754 USA. [Barsotti, L.; Blackburn, L.; Bodiya, T. P.; Brunet, G.; Cao, J.; Corbitt, T. R. C.; Donovan, F.; Duke, I.; Evans, M.; Foley, S.; Fritschel, P.; Goda, K.; Grimaldi, F.; Harry, G. M.; Hughey, B.; Katsavounidis, E.; MacInnis, M.; Markowitz, J.; Mason, K.; Mavalvala, N.; Mittleman, R.; Sarin, P.; Shapiro, B.; Shoemaker, D. H.; Smith, N. D.; Stein, A.; Stein, L. C.; Waldman, S. J.; Weiss, R.; Wipf, C. C.; Zucker, M. E.] MIT, LIGO, Cambridge, MA 02139 USA. [Amin, R. S.; Caudill, S.; Giaime, J. A.; Gonzalez, G.; Gouaty, R.; Johnson, W. W.; Kissel, J. S.; Matichard, F.; Slutsky, J.; Sung, M.; Wen, S.] Louisiana State Univ, Baton Rouge, LA 70803 USA. [Reed, T.; Scanlan, M.; Zotov, N.] Louisiana Tech Univ, Ruston, LA 71272 USA. [McHugh, M.] Loyola Univ, New Orleans, LA 70118 USA. [Baker, P.; Cornish, N.; Littenberg, T. B.] Montana State Univ, Bozeman, MT 59717 USA. [Bilenko, I. A.; Braginsky, V. B.; Danilishin, S. L.; Gorodetsky, M. L.; Khalili, F. Y.; Mitrofanov, V. P.; Prokhorov, L.; Strigin, S.; Tarabrin, S. P.; Vyachanin, S. P.] Moscow MV Lomonosov State Univ, Moscow 119992, Russia. [Camp, J. B.; Cannizzo, J.; Numata, K.; Stroeer, A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Kawamura, S.; Kokeyama, K.; Morioka, T.; Nishizawa, A.; Sakata, S.; Sato, S.] Natl Inst Nat Sci, Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan. [Kalogera, V.; Mandel, I.; Raymond, V.; van der Sluys, M. V.] Northwestern Univ, Evanston, IL 60208 USA. [Whelan, J. T.] Rochester Inst Technol, Rochester, NY 14623 USA. [Brummit, A.; Greenhalgh, R. J. S.; O'Dell, J.; Wilmut, I.] Rutherford Appleton Lab, HSIC, Didcot OX11 0QX, Oxon, England. [Beyersdorf, P. T.] San Jose State Univ, San Jose, CA 95192 USA. [Saraf, S.] Sonoma State Univ, Rohnert Pk, CA 94928 USA. [Yoshida, S.] SE Louisiana Univ, Hammond, LA 70402 USA. [Doomes, E. E.; McGuire, S. C.] Southern Univ, Baton Rouge, LA 70813 USA. [Doomes, E. E.; McGuire, S. C.] A&M Coll, Baton Rouge, LA 70813 USA. [Allen, G.; Bullington, A.; Byer, R. L.; Clark, D.; DeBra, D.; Lantz, B.; Leindecker, N.; Lu, P.; Markosyan, A.; Sinha, S.; Sun, K. -X.; Ulmen, J.; Urbanek, K.] Stanford Univ, Stanford, CA 94305 USA. [Brown, D. A.; Di Credico, A.; Garofoli, J. A.; Hirose, E.; Saulson, P. R.; Smith, J. R.] Syracuse Univ, Syracuse, NY 13244 USA. [Desai, S.; Finn, L. S.; Kopparapu, R.; Menendez, D. F.; Minelli, J.; O'Shaughnessy, R.; Owen, B. J.; Williams, H. R.] Penn State Univ, University Pk, PA 16802 USA. [Chung, C. T. Y.; Melatos, A.] Univ Melbourne, Parkville, Vic 3010, Australia. [Cavaglia, M.] Univ Mississippi, University, MS 38677 USA. [Daw, E. J.] Univ Sheffield, Sheffield S10 2TN, S Yorkshire, England. [Frei, M.; Matzner, R. A.] Univ Texas Austin, Austin, TX 78712 USA. [Benacquista, M.; Creighton, T. D.; Grosso, R.; Hayama, K.; Lei, H.; Mukherjee, S.; Rakhmanov, M.; Romano, J. D.; Stone, R.; Tang, L.] Univ Texas Brownsville & Texas Southmost Coll, Brownsville, TX 78520 USA. [Ugolini, D.] Trinity Univ, San Antonio, TX 78212 USA. [Sancho de la Jordana, L.; Sintes, A. M.; Trias, M.] Univ Illes Balears, E-07122 Palma de Mallorca, Spain. [Diaz, M.; Hosken, D. J.; Mohanty, S. D.; Munch, J.; Ottaway, D. J.; Veitch, P.] Univ Adelaide, Adelaide, SA 5005, Australia. [Aston, S.; Chelkowski, S.; Cruise, A. M.; Culter, R. M.; Freise, A.; Hallam, J. M.; Hild, S.; Kasprzyk, D.; Lodhia, D.; Perraca, A.; Vecchio, A.; Veitch, J.] Univ Birmingham, Birmingham B15 2TT, W Midlands, England. [Arain, M. A.; Faltas, Y.; Klimenko, S.; Lin, H.; Lucianetti, A.; Martin, R. M.; Mitselmakher, G.; Mueller, G.; Ottens, R. S.; Pankow, C.; Quetschke, V.; Reitze, D. H.; Tanner, D. B.; Whiting, B. F.; Williams, L.; Wu, W.] Univ Florida, Gainesville, FL 32611 USA. [Barr, B.; Bassiri, R.; Bastarrika, M.; Chalkley, E.; Cumming, A.; Cunningham, L.; Dooley, K. L.; Edgar, M.; Grant, A.; Hammond, G. D.; Haughian, K.; Heng, I. S.; Hough, J.; Huttner, S. H.; Jones, R.; Kumar, R.; Lubinski, M.; Martin, I. W.; Miller, J.; Murray, P. G.; Nelson, J.; Newton, G.; Pitkin, M.; Plissi, M. V.; Reid, S.; Robertson, N. A.; Rowan, S.; Scott, J.; Sorazu, B.; Strain, K. A.; Tokmakov, K. V.; van Veggel, A. A.; Woan, G.] Univ Glasgow, Glasgow G12 8QQ, Lanark, Scotland. [Buonanno, A.; Kanner, J.; Ochsner, E.; Pan, Y.; Shawhan, P.] Univ Maryland, College Pk, MD 20742 USA. [Cadonati, L.; Mohapatra, S. R. P.] Univ Massachusetts, Amherst, MA 01003 USA. [Caride, S.; Dergachev, V.; Goetz, E.; Gustafson, R.; Riles, K.; Zhang, J.] Univ Michigan, Ann Arbor, MI 48109 USA. [Harms, J.; Kandhasamy, S.; Mandic, V.] Univ Minnesota, Minneapolis, MN 55455 USA. [Brau, J. E.; Frey, R.; Harstad, E. D.; Ito, M.; Leonor, I.; Schofield, R.] Univ Oregon, Eugene, OR 97403 USA. [Forrest, C.; Melissinos, A. C.] Univ Rochester, Rochester, NY 14627 USA. [Conte, R.; Postiglione, F.] Univ Salerno, I-84084 Salerno, Italy. [Castaldi, G.; Galdi, V.; Longo, M.; Pierro, V.; Pinto, I. M.; Principe, M.] Univ Sannio Benevento, I-82100 Benevento, Italy. [Jones, D. I.] Univ Southampton, Southampton SO17 1BJ, Hants, England. [Lockerbie, N. A.] Univ Strathclyde, Glasgow G1 1XQ, Lanark, Scotland. [Barriga, P.; Blair, D.; Coward, D.; Dumas, J. -C.; Fan, Y.; Gras, S.; Hoyland, D.; Ju, L.; Wen, L.; Yan, Z.; Zhao, C.] Univ Western Australia, Crawley, WA 6009, Australia. [Allen, B.; Anderson, W. G.; Armor, P.; Biswas, R.; Brady, P. R.; Clayton, J. H.; Creighton, J. D. E.; Flasch, K.; Fotopoulos, N.; Goggin, L. M.; Hammer, D.; Koranda, S.; Mercer, R. A.; Moe, B.; Papa, M. A.; Siemens, X.; Vaulin, R.; Wiseman, A. G.] Univ Wisconsin, Milwaukee, WI 53201 USA. [Bose, S.; Steplewski, S.; Talukder, D.] Washington State Univ, Pullman, WA 99164 USA. RP Abbott, BP (reprint author), CALTECH, LIGO, Pasadena, CA 91125 USA. RI Santamaria, Lucia/A-7269-2012; Prokhorov, Leonid/I-2953-2012; Gorodetsky, Michael/C-5938-2008; Strigin, Sergey/I-8337-2012; Mitrofanov, Valery/D-8501-2012; Bilenko, Igor/D-5172-2012; Allen, Bruce/K-2327-2012; Chen, Yanbei/A-2604-2013; Barker, David/A-5671-2013; Zhao, Chunnong/C-2403-2013; Ju, Li/C-2623-2013; Pitkin, Matthew/I-3802-2013; Schutz, Bernard/B-1504-2010; Galdi, Vincenzo/B-1670-2008; Hammond, Giles/B-7861-2009; Hammond, Giles/A-8168-2012; Finn, Lee Samuel/A-3452-2009; McClelland, David/E-6765-2010; Hild, Stefan/A-3864-2010; Rowan, Sheila/E-3032-2010; Strain, Kenneth/D-5236-2011; Raab, Frederick/E-2222-2011; Martin, Iain/A-2445-2010; Lueck, Harald/F-7100-2011; Kawazoe, Fumiko/F-7700-2011; Freise, Andreas/F-8892-2011; Kawabe, Keita/G-9840-2011; Harms, Jan/J-4359-2012; Bartos, Imre/A-2592-2017; Frey, Raymond/E-2830-2016; Sergeev, Alexander/F-3027-2017; Ward, Robert/I-8032-2014; Vyatchanin, Sergey/J-2238-2012; Khazanov, Efim/B-6643-2014; Lucianetti, Antonio/G-7383-2014; Lam, Ping Koy/A-5276-2008; Danilishin, Stefan/K-7262-2012; Khalili, Farit/D-8113-2012; Vecchio, Alberto/F-8310-2015; Mow-Lowry, Conor/F-8843-2015; Khan, Rubab/F-9455-2015; Ottaway, David/J-5908-2015; Postiglione, Fabio/O-4744-2015; Sigg, Daniel/I-4308-2015; Pinto, Innocenzo/L-3520-2016 OI Gorodetsky, Michael/0000-0002-5159-2742; Allen, Bruce/0000-0003-4285-6256; Zhao, Chunnong/0000-0001-5825-2401; Pitkin, Matthew/0000-0003-4548-526X; Galdi, Vincenzo/0000-0002-4796-3600; Finn, Lee Samuel/0000-0002-3937-0688; McClelland, David/0000-0001-6210-5842; Strain, Kenneth/0000-0002-2066-5355; Lueck, Harald/0000-0001-9350-4846; Papa, M.Alessandra/0000-0002-1007-5298; Kanner, Jonah/0000-0001-8115-0577; Aulbert, Carsten/0000-0002-1481-8319; Freise, Andreas/0000-0001-6586-9901; Mandel, Ilya/0000-0002-6134-8946; Whiting, Bernard F/0000-0002-8501-8669; Veitch, John/0000-0002-6508-0713; Principe, Maria/0000-0002-6327-0628; Matichard, Fabrice/0000-0001-8982-8418; Pinto, Innocenzo M./0000-0002-2679-4457; Minelli, Jeff/0000-0002-5330-912X; Santamaria, Lucia/0000-0002-5986-0449; Pierro, Vincenzo/0000-0002-6020-5521; Hallam, Jonathan Mark/0000-0002-7087-0461; Sorazu, Borja/0000-0002-6178-3198; Stuver, Amber/0000-0003-0324-5735; Nishizawa, Atsushi/0000-0003-3562-0990; Zweizig, John/0000-0002-1521-3397; O'Shaughnessy, Richard/0000-0001-5832-8517; Frey, Raymond/0000-0003-0341-2636; Stein, Leo/0000-0001-7559-9597; Ward, Robert/0000-0001-5503-5241; Whelan, John/0000-0001-5710-6576; LONGO, Maurizio/0000-0001-8325-4003; Fairhurst, Stephen/0000-0001-8480-1961; Boschi, Valerio/0000-0001-8665-2293; Lam, Ping Koy/0000-0002-4421-601X; Danilishin, Stefan/0000-0001-7758-7493; Vecchio, Alberto/0000-0002-6254-1617; Khan, Rubab/0000-0001-5100-5168; Postiglione, Fabio/0000-0003-0628-3796; Sigg, Daniel/0000-0003-4606-6526; NR 41 TC 66 Z9 65 U1 3 U2 14 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1550-7998 J9 PHYS REV D JI Phys. Rev. D PD NOV PY 2009 VL 80 IS 10 AR 102001 DI 10.1103/PhysRevD.80.102001 PG 26 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 526SI UT WOS:000272313300004 ER PT J AU Abbott, BP Abbott, R Adhikari, R Ajith, P Allen, B Allen, G Amin, RS Anderson, SB Anderson, WG Arain, MA Araya, M Armandula, H Armor, P Aso, Y Aston, S Aufmuth, P Aulbert, C Babak, S Baker, P Ballmer, S Barker, C Barker, D Barr, B Barriga, P Barsotti, L Barton, MA Bartos, I Bassiri, R Bastarrika, M Behnke, B Benacquista, M Betzwieser, J Beyersdorf, PT Bilenko, IA Billingsley, G Biswas, R Black, E Blackburn, JK Blackburn, L Blair, D Bland, B Bodiya, TP Bogue, L Bork, R Boschi, V Bose, S Brady, PR Braginsky, VB Brau, JE Bridges, DO Brinkmann, M Brooks, AF Brown, DA Brummit, A Brunet, G Bullington, A Buonanno, A Burmeister, O Byer, RL Cadonati, L Camp, JB Cannizzo, J Cannon, KC Cao, J Cardenas, L Caride, S Castaldi, G Caudill, S Cavaglia, M Cepeda, C Chalermsongsak, T Chalkley, E Charlton, P Chatterji, S Chelkowski, S Chen, Y Christensen, N Chung, CTY Clark, D Clark, J Clayton, JH Cokelaer, T Colacino, CN Conte, R Cook, D Corbitt, TRC Cornish, N Coward, D Coyne, DC Di Credico, A Creighton, JDE Creighton, TD Cruise, AM Culter, RM Cumming, A Cunningham, L Danilishin, SL Danzmann, K Daudert, B Davies, G Daw, EJ DeBra, D Degallaix, J Dergachev, V Desai, S DeSalvo, R Dhurandhar, S Diaz, M Dietz, A Donovan, F Dooley, KL Doomes, EE Drever, RWP Dueck, J Duke, I Dumas, JC Dwyer, JG Echols, C Edgar, M Effler, A Ehrens, P Espinoza, E Etzel, T Evans, M Evans, T Fairhurst, S Faltas, Y Fan, Y Fazi, D Fehrmann, H Finn, LS Flasch, K Foley, S Forrest, C Fotopoulos, N Franzen, A Frede, M Frei, M Frei, Z Freise, A Frey, R Fricke, T Fritschel, P Frolov, VV Fyffe, M Galdi, V Garofoli, JA Gholami, I Giaime, JA Giampanis, S Giardina, KD Goda, K Goetz, E Goggin, LM Gonzalez, G Gorodetsky, ML Gossler, S Gouaty, R Grant, A Gras, S Gray, C Gray, M Greenhalgh, RJS Gretarsson, AM Grimaldi, F Grosso, R Grote, H Grunewald, S Guenther, M Gustafson, EK Gustafson, R Hage, B Hallam, JM Hammer, D Hammond, GD Hanna, C Hanson, J Harms, J Harry, GM Harry, IW Harstad, ED Haughian, K Hayama, K Heefner, J Heng, IS Heptonstall, A Hewitson, M Hild, S Hirose, E Hoak, D Hodge, KA Holt, K Hosken, DJ Hough, J Hoyland, D Hughey, B Huttner, SH Ingram, DR Isogai, T Ito, M Ivanov, A Johnson, B Johnson, WW Jones, DI Jones, G Jones, R Ju, L Kalmus, P Kalogera, V Kandhasamy, S Kanner, J Kasprzyk, D Katsavounidis, E Kawabe, K Kawamura, S Kawazoe, F Kells, W Keppel, DG Khalaidovski, A Khalili, FY Khan, R Khazanov, E King, P Kissel, JS Klimenko, S Kokeyama, K Kondrashov, V Kopparapu, R Koranda, S Kozak, D Krishnan, B Kumar, R Kwee, P Lam, PK Landry, M Lantz, B Lazzarini, A Lei, H Lei, M Leindecker, N Leonor, I Li, C Lin, H Lindquist, PE Littenberg, TB Lockerbie, NA Lodhia, D Longo, M Lormand, M Lu, P Lubinski, M Lucianetti, A Luck, H Machenschalk, B MacInnis, M Mageswaran, M Mailand, K Mandel, I Mandic, V Marka, S Marka, Z Markosyan, A Markowitz, J Maros, E Martin, IW Martin, RM Marx, JN Mason, K Matichard, F Matone, L Matzner, RA Mavalvala, N McCarthy, R McClelland, DE McGuire, SC McHugh, M McIntyre, G McKechan, DJA McKenzie, K Mehmet, M Melatos, A Melissinos, AC Menendez, DF Mendell, G Mercer, RA Meshkov, S Messenger, C Meyer, MS Miller, J Minelli, J Mino, Y Mitrofanov, VP Mitselmakher, G Mittleman, R Miyakawa, O Moe, B Mohanty, SD Mohapatra, SRP Moreno, G Morioka, T Mors, K Mossavi, K MowLowry, C Mueller, G Muller-Ebhardt, H Muhammad, D Mukherjee, S Mukhopadhyay, H Mullavey, A Munch, J Murray, PG Myers, E Myers, J Nash, T Nelson, J Newton, G Nishizawa, A Numata, K O'Dell, J O'Reilly, B O'Shaughnessy, R Ochsner, E Ogin, GH Ottaway, DJ Ottens, RS Overmier, H Owen, BJ Pan, Y Pankow, C Papa, MA Parameshwaraiah, V Patel, P Pedraza, M Penn, S Perraca, A Pierro, V Pinto, IM Pitkin, M Pletsch, HJ Plissi, MV Postiglione, F Principe, M Prix, R Prokhorov, L Puncken, O Quetschke, V Raab, FJ Rabeling, DS Radkins, H Raffai, P Raics, Z Rainer, N Rakhmanov, M Raymond, V Reed, CM Reed, T Rehbein, H Reid, S Reitze, DH Riesen, R Riles, K Rivera, B Roberts, P Robertson, NA Robinson, C Robinson, EL Roddy, S Rover, C Rollins, J Romano, JD Romie, JH Rowan, S Rudiger, A Russell, P Ryan, K Sakata, S de la Jordana, LS Sandberg, V Sannibale, V Santamaria, L Saraf, S Sarin, P Sathyaprakash, BS Sato, S Satterthwaite, M Saulson, PR Savage, R Savov, P Scanlan, M Schilling, R Schnabel, R Schofield, R Schulz, B Schutz, BF Schwinberg, P Scott, J Scott, SM Searle, AC Sears, B Seifert, F Sellers, D Sengupta, AS Sergeev, A Shapiro, B Shawhan, P Shoemaker, DH Sibley, A Siemens, X Sigg, D Sinha, S Sintes, AM Slagmolen, BJJ Slutsky, J Smith, JR Smith, MR Smith, ND Somiya, K Sorazu, B Stein, A Stein, LC Steplewski, S Stochino, A Stone, R Strain, KA Strigin, S Stroeer, A Stuver, AL Summerscales, TZ Sun, KX Sung, M Sutton, PJ Szokoly, GP Talukder, D Tang, L Tanner, DB Tarabrin, SP Taylor, JR Taylor, R Thacker, J Thorne, KA Thorne, KS Thuring, A Tokmakov, KV Torres, C Torrie, C Traylor, G Trias, M Ugolini, D Ulmen, J Urbanek, K Vahlbruch, H Vallisneri, M Van Den Broeck, C van der Sluys, MV van Veggel, AA Vass, S Vaulin, R Vecchio, A Veitch, J Veitch, P Veltkamp, C Villadsen, J Villar, A Vorvick, C Vyachanin, SP Waldman, SJ Wallace, L Ward, RL Weidner, A Weinert, M Weinstein, AJ Weiss, R Wen, L Wen, S Wette, K Whelan, JT Whitcomb, SE Whiting, BF Wilkinson, C Willems, PA Williams, HR Williams, L Willke, B Wilmut, I Winkelmann, L Winkler, W Wipf, CC Wiseman, AG Woan, G Wooley, R Worden, J Wu, W Yakushin, I Yamamoto, H Yan, Z Yoshida, S Zanolin, M Zhang, J Zhang, L Zhao, C Zotov, N Zucker, ME zur Muhlen, H Zweizig, J AF Abbott, B. P. Abbott, R. Adhikari, R. Ajith, P. Allen, B. Allen, G. Amin, R. S. Anderson, S. B. Anderson, W. G. Arain, M. A. Araya, M. Armandula, H. Armor, P. Aso, Y. Aston, S. Aufmuth, P. Aulbert, C. Babak, S. Baker, P. Ballmer, S. Barker, C. Barker, D. Barr, B. Barriga, P. Barsotti, L. Barton, M. A. Bartos, I. Bassiri, R. Bastarrika, M. Behnke, B. Benacquista, M. Betzwieser, J. Beyersdorf, P. T. Bilenko, I. A. Billingsley, G. Biswas, R. Black, E. Blackburn, J. K. Blackburn, L. Blair, D. Bland, B. Bodiya, T. P. Bogue, L. Bork, R. Boschi, V. Bose, S. Brady, P. R. Braginsky, V. B. Brau, J. E. Bridges, D. O. Brinkmann, M. Brooks, A. F. Brown, D. A. Brummit, A. Brunet, G. Bullington, A. Buonanno, A. Burmeister, O. Byer, R. L. Cadonati, L. Camp, J. B. Cannizzo, J. Cannon, K. C. Cao, J. Cardenas, L. Caride, S. Castaldi, G. Caudill, S. Cavaglia, M. Cepeda, C. Chalermsongsak, T. Chalkley, E. Charlton, P. Chatterji, S. Chelkowski, S. Chen, Y. Christensen, N. Chung, C. T. Y. Clark, D. Clark, J. Clayton, J. H. Cokelaer, T. Colacino, C. N. Conte, R. Cook, D. Corbitt, T. R. C. Cornish, N. Coward, D. Coyne, D. C. Di Credico, A. Creighton, J. D. E. Creighton, T. D. Cruise, A. M. Culter, R. M. Cumming, A. Cunningham, L. Danilishin, S. L. Danzmann, K. Daudert, B. Davies, G. Daw, E. J. DeBra, D. Degallaix, J. Dergachev, V. Desai, S. DeSalvo, R. Dhurandhar, S. Diaz, M. Dietz, A. Donovan, F. Dooley, K. L. Doomes, E. E. Drever, R. W. P. Dueck, J. Duke, I. Dumas, J. -C. Dwyer, J. G. Echols, C. Edgar, M. Effler, A. Ehrens, P. Espinoza, E. Etzel, T. Evans, M. Evans, T. Fairhurst, S. Faltas, Y. Fan, Y. Fazi, D. Fehrmann, H. Finn, L. S. Flasch, K. Foley, S. Forrest, C. Fotopoulos, N. Franzen, A. Frede, M. Frei, M. Frei, Z. Freise, A. Frey, R. Fricke, T. Fritschel, P. Frolov, V. V. Fyffe, M. Galdi, V. Garofoli, J. A. Gholami, I. Giaime, J. A. Giampanis, S. Giardina, K. D. Goda, K. Goetz, E. Goggin, L. M. Gonzalez, G. Gorodetsky, M. L. Gossler, S. Gouaty, R. Grant, A. Gras, S. Gray, C. Gray, M. Greenhalgh, R. J. S. Gretarsson, A. M. Grimaldi, F. Grosso, R. Grote, H. Grunewald, S. Guenther, M. Gustafson, E. K. Gustafson, R. Hage, B. Hallam, J. M. Hammer, D. Hammond, G. D. Hanna, C. Hanson, J. Harms, J. Harry, G. M. Harry, I. W. Harstad, E. D. Haughian, K. Hayama, K. Heefner, J. Heng, I. S. Heptonstall, A. Hewitson, M. Hild, S. Hirose, E. Hoak, D. Hodge, K. A. Holt, K. Hosken, D. J. Hough, J. Hoyland, D. Hughey, B. Huttner, S. H. Ingram, D. R. Isogai, T. Ito, M. Ivanov, A. Johnson, B. Johnson, W. W. Jones, D. I. Jones, G. Jones, R. Ju, L. Kalmus, P. Kalogera, V. Kandhasamy, S. Kanner, J. Kasprzyk, D. Katsavounidis, E. Kawabe, K. Kawamura, S. Kawazoe, F. Kells, W. Keppel, D. G. Khalaidovski, A. Khalili, F. Y. Khan, R. Khazanov, E. King, P. Kissel, J. S. Klimenko, S. Kokeyama, K. Kondrashov, V. Kopparapu, R. Koranda, S. Kozak, D. Krishnan, B. Kumar, R. Kwee, P. Lam, P. K. Landry, M. Lantz, B. Lazzarini, A. Lei, H. Lei, M. Leindecker, N. Leonor, I. Li, C. Lin, H. Lindquist, P. E. Littenberg, T. B. Lockerbie, N. A. Lodhia, D. Longo, M. Lormand, M. Lu, P. Lubinski, M. Lucianetti, A. Lueck, H. Machenschalk, B. MacInnis, M. Mageswaran, M. Mailand, K. Mandel, I. Mandic, V. Marka, S. Marka, Z. Markosyan, A. Markowitz, J. Maros, E. Martin, I. W. Martin, R. M. Marx, J. N. Mason, K. Matichard, F. Matone, L. Matzner, R. A. Mavalvala, N. McCarthy, R. McClelland, D. E. McGuire, S. C. McHugh, M. McIntyre, G. McKechan, D. J. A. McKenzie, K. Mehmet, M. Melatos, A. Melissinos, A. C. Menendez, D. F. Mendell, G. Mercer, R. A. Meshkov, S. Messenger, C. Meyer, M. S. Miller, J. Minelli, J. Mino, Y. Mitrofanov, V. P. Mitselmakher, G. Mittleman, R. Miyakawa, O. Moe, B. Mohanty, S. D. Mohapatra, S. R. P. Moreno, G. Morioka, T. Mors, K. Mossavi, K. MowLowry, C. Mueller, G. Muller-Ebhardt, H. Muhammad, D. Mukherjee, S. Mukhopadhyay, H. Mullavey, A. Munch, J. Murray, P. G. Myers, E. Myers, J. Nash, T. Nelson, J. Newton, G. Nishizawa, A. Numata, K. O'Dell, J. O'Reilly, B. O'Shaughnessy, R. Ochsner, E. Ogin, G. H. Ottaway, D. J. Ottens, R. S. Overmier, H. Owen, B. J. Pan, Y. Pankow, C. Papa, M. A. Parameshwaraiah, V. Patel, P. Pedraza, M. Penn, S. Perraca, A. Pierro, V. Pinto, I. M. Pitkin, M. Pletsch, H. J. Plissi, M. V. Postiglione, F. Principe, M. Prix, R. Prokhorov, L. Puncken, O. Quetschke, V. Raab, F. J. Rabeling, D. S. Radkins, H. Raffai, P. Raics, Z. Rainer, N. Rakhmanov, M. Raymond, V. Reed, C. M. Reed, T. Rehbein, H. Reid, S. Reitze, D. H. Riesen, R. Riles, K. Rivera, B. Roberts, P. Robertson, N. A. Robinson, C. Robinson, E. L. Roddy, S. Roever, C. Rollins, J. Romano, J. D. Romie, J. H. Rowan, S. Rudiger, A. Russell, P. Ryan, K. Sakata, S. Sancho de la Jordana, L. Sandberg, V. Sannibale, V. Santamaria, L. Saraf, S. Sarin, P. Sathyaprakash, B. S. Sato, S. Satterthwaite, M. Saulson, P. R. Savage, R. Savov, P. Scanlan, M. Schilling, R. Schnabel, R. Schofield, R. Schulz, B. Schutz, B. F. Schwinberg, P. Scott, J. Scott, S. M. Searle, A. C. Sears, B. Seifert, F. Sellers, D. Sengupta, A. S. Sergeev, A. Shapiro, B. Shawhan, P. Shoemaker, D. H. Sibley, A. Siemens, X. Sigg, D. Sinha, S. Sintes, A. M. Slagmolen, B. J. J. Slutsky, J. Smith, J. R. Smith, M. R. Smith, N. D. Somiya, K. Sorazu, B. Stein, A. Stein, L. C. Steplewski, S. Stochino, A. Stone, R. Strain, K. A. Strigin, S. Stroeer, A. Stuver, A. L. Summerscales, T. Z. Sun, K. -X. Sung, M. Sutton, P. J. Szokoly, G. P. Talukder, D. Tang, L. Tanner, D. B. Tarabrin, S. P. Taylor, J. R. Taylor, R. Thacker, J. Thorne, K. A. Thorne, K. S. Thuring, A. Tokmakov, K. V. Torres, C. Torrie, C. Traylor, G. Trias, M. Ugolini, D. Ulmen, J. Urbanek, K. Vahlbruch, H. Vallisneri, M. Van Den Broeck, C. van der Sluys, M. V. van Veggel, A. A. Vass, S. Vaulin, R. Vecchio, A. Veitch, J. Veitch, P. Veltkamp, C. Villadsen, J. Villar, A. Vorvick, C. Vyachanin, S. P. Waldman, S. J. Wallace, L. Ward, R. L. Weidner, A. Weinert, M. Weinstein, A. J. Weiss, R. Wen, L. Wen, S. Wette, K. Whelan, J. T. Whitcomb, S. E. Whiting, B. F. Wilkinson, C. Willems, P. A. Williams, H. R. Williams, L. Willke, B. Wilmut, I. Winkelmann, L. Winkler, W. Wipf, C. C. Wiseman, A. G. Woan, G. Wooley, R. Worden, J. Wu, W. Yakushin, I. Yamamoto, H. Yan, Z. Yoshida, S. Zanolin, M. Zhang, J. Zhang, L. Zhao, C. Zotov, N. Zucker, M. E. zur Muehlen, H. Zweizig, J. CA LIGO Sci Collaboration TI Search for high frequency gravitational-wave bursts in the first calendar year of LIGO's fifth science run SO PHYSICAL REVIEW D LA English DT Article ID VIRGO AB We present an all-sky search for gravitational waves in the frequency range 1 to 6 kHz during the first calendar year of LIGO's fifth science run. This is the first untriggered LIGO burst analysis to be conducted above 3 kHz. We discuss the unique properties of interferometric data in this regime. 161.3 days of triple-coincident data were analyzed. No gravitational events above threshold were observed and a frequentist upper limit of 5.4 year(-1) on the rate of strong gravitational-wave bursts was placed at a 90% confidence level. Implications for specific theoretical models of gravitational-wave emission are also discussed. C1 [Abbott, B. P.; Abbott, R.; Adhikari, R.; Anderson, S. B.; Arain, M. A.; Araya, M.; Armandula, H.; Aso, Y.; Ballmer, S.; Barton, M. A.; Betzwieser, J.; Billingsley, G.; Black, E.; Blackburn, J. K.; Bork, R.; Boschi, V.; Brooks, A. F.; Cannon, K. C.; Cardenas, L.; Cepeda, C.; Chalermsongsak, T.; Chatterji, S.; Coyne, D. C.; Daudert, B.; DeSalvo, R.; Echols, C.; Effler, A.; Ehrens, P.; Espinoza, E.; Etzel, T.; Fazi, D.; Gustafson, E. K.; Hanna, C.; Heefner, J.; Heptonstall, A.; Hodge, K. A.; Ivanov, A.; Kalmus, P.; Kells, W.; Keppel, D. G.; King, P.; Kondrashov, V.; Kozak, D.; Lazzarini, A.; Lei, M.; Lindquist, P. E.; Mageswaran, M.; Mailand, K.; Maros, E.; Marx, J. N.; McIntyre, G.; Meshkov, S.; Miyakawa, O.; Nash, T.; Ogin, G. H.; Patel, P.; Pedraza, M.; Robertson, N. A.; Russell, P.; Sannibale, V.; Searle, A. C.; Sears, B.; Sengupta, A. S.; Smith, M. R.; Stochino, A.; Taylor, R.; Torrie, C.; Vass, S.; Villar, A.; Wallace, L.; Ward, R. L.; Weinstein, A. J.; Whitcomb, S. E.; Willems, P. A.; Yamamoto, H.; Zhang, L.; Zweizig, J.] CALTECH, LIGO, Pasadena, CA 91125 USA. [Babak, S.; Behnke, B.; Chen, Y.; Gholami, I.; Grunewald, S.; Krishnan, B.; Machenschalk, B.; Papa, M. A.; Robinson, E. L.; Santamaria, L.; Schutz, B. F.; Whelan, J. T.] Max Planck Inst Gravitat Phys, Albert Einstein Inst, D-14476 Golm, Germany. [Ajith, P.; Allen, B.; Aulbert, C.; Brinkmann, M.; Burmeister, O.; Danzmann, K.; Degallaix, J.; Dueck, J.; Fehrmann, H.; Frede, M.; Giampanis, S.; Gossler, S.; Grote, H.; Hewitson, M.; Kawazoe, F.; Khalaidovski, A.; Lueck, H.; Mehmet, M.; Messenger, C.; Mors, K.; Mossavi, K.; Muller-Ebhardt, H.; Pletsch, H. J.; Prix, R.; Puncken, O.; Rainer, N.; Rehbein, H.; Roever, C.; Rudiger, A.; Schilling, R.; Schnabel, R.; Schulz, B.; Seifert, F.; Taylor, J. R.; Veltkamp, C.; Weidner, A.; Weinert, M.; Willke, B.; Winkelmann, L.; Winkler, W.] Max Planck Inst Gravitat Phys, Albert Einstein Inst, D-30167 Hannover, Germany. [Roberts, P.; Summerscales, T. Z.] Andrews Univ, Berrien Springs, MI 49104 USA. [Gray, M.; Lam, P. K.; McClelland, D. E.; McKenzie, K.; MowLowry, C.; Mullavey, A.; Rabeling, D. S.; Satterthwaite, M.; Scott, S. M.; Slagmolen, B. J. J.; Wette, K.] Australian Natl Univ, Canberra, ACT 0200, Australia. [Chen, Y.; Li, C.; Mino, Y.; Savov, P.; Somiya, K.; Thorne, K. S.; Vallisneri, M.; Wen, L.] CALTECH, CaRT, Pasadena, CA 91125 USA. [Clark, J.; Cokelaer, T.; Davies, G.; Dietz, A.; Fairhurst, S.; Harry, I. W.; Jones, G.; McKechan, D. J. A.; Robinson, C.; Sathyaprakash, B. S.; Schutz, B. F.; Sutton, P. J.; Van Den Broeck, C.] Cardiff Univ, Cardiff CF24 3AA, S Glam, Wales. 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[Ugolini, D.] Trinity Univ, San Antonio, TX 78212 USA. [Sancho de la Jordana, L.; Sintes, A. M.; Trias, M.] Univ Illes Balears, E-07122 Palma de Mallorca, Spain. [Hosken, D. J.; Munch, J.; Ottaway, D. J.; Veitch, P.] Univ Adelaide, Adelaide, SA 5005, Australia. [Aston, S.; Chelkowski, S.; Cruise, A. M.; Culter, R. M.; Freise, A.; Hallam, J. M.; Hild, S.; Kasprzyk, D.; Lodhia, D.; Perraca, A.; Vecchio, A.; Veitch, J.] Univ Birmingham, Birmingham B15 2TT, W Midlands, England. [Dooley, K. L.; Faltas, Y.; Klimenko, S.; Lin, H.; Lucianetti, A.; Martin, R. M.; Mitselmakher, G.; Mueller, G.; Ottens, R. S.; Pankow, C.; Quetschke, V.; Reitze, D. H.; Tanner, D. B.; Whiting, B. F.; Williams, L.; Wu, W.] Univ Florida, Gainesville, FL 32611 USA. [Barr, B.; Bassiri, R.; Bastarrika, M.; Chalkley, E.; Cumming, A.; Cunningham, L.; Edgar, M.; Grant, A.; Hammond, G. D.; Haughian, K.; Heng, I. S.; Hough, J.; Huttner, S. H.; Jones, R.; Kumar, R.; Martin, I. W.; Miller, J.; Murray, P. 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I.] Univ Southampton, Southampton SO17 1BJ, Hants, England. [Lockerbie, N. A.] Univ Strathclyde, Glasgow G1 1XQ, Lanark, Scotland. [Barriga, P.; Blair, D.; Coward, D.; Dumas, J. -C.; Fan, Y.; Gras, S.; Hoyland, D.; Ju, L.; Wen, L.; Yan, Z.; Zhao, C.] Univ Western Australia, Crawley, WA 6009, Australia. [Allen, B.; Anderson, W. G.; Armor, P.; Biswas, R.; Brady, P. R.; Clayton, J. H.; Creighton, J. D. E.; Flasch, K.; Fotopoulos, N.; Goggin, L. M.; Hammer, D.; Koranda, S.; Mercer, R. A.; Moe, B.; Papa, M. A.; Siemens, X.; Vaulin, R.; Wiseman, A. G.] Univ Wisconsin, Milwaukee, WI 53201 USA. [Bose, S.; Steplewski, S.; Talukder, D.] Washington State Univ, Pullman, WA 99164 USA. RP Abbott, BP (reprint author), CALTECH, LIGO, Pasadena, CA 91125 USA. RI Finn, Lee Samuel/A-3452-2009; Santamaria, Lucia/A-7269-2012; Prokhorov, Leonid/I-2953-2012; Gorodetsky, Michael/C-5938-2008; Strigin, Sergey/I-8337-2012; Mitrofanov, Valery/D-8501-2012; Bilenko, Igor/D-5172-2012; Allen, Bruce/K-2327-2012; Chen, Yanbei/A-2604-2013; Barker, David/A-5671-2013; Zhao, Chunnong/C-2403-2013; Ju, Li/C-2623-2013; Pitkin, Matthew/I-3802-2013; Kawabe, Keita/G-9840-2011; Hammond, Giles/A-8168-2012; Galdi, Vincenzo/B-1670-2008; Hammond, Giles/B-7861-2009; McClelland, David/E-6765-2010; Hild, Stefan/A-3864-2010; Schutz, Bernard/B-1504-2010; Rowan, Sheila/E-3032-2010; Strain, Kenneth/D-5236-2011; Raab, Frederick/E-2222-2011; Martin, Iain/A-2445-2010; Lueck, Harald/F-7100-2011; Kawazoe, Fumiko/F-7700-2011; Freise, Andreas/F-8892-2011; Harms, Jan/J-4359-2012; Bartos, Imre/A-2592-2017; Frey, Raymond/E-2830-2016; Sergeev, Alexander/F-3027-2017; Ward, Robert/I-8032-2014; Vyatchanin, Sergey/J-2238-2012; Khazanov, Efim/B-6643-2014; Lucianetti, Antonio/G-7383-2014; Lam, Ping Koy/A-5276-2008; Danilishin, Stefan/K-7262-2012; Khalili, Farit/D-8113-2012; Vecchio, Alberto/F-8310-2015; Mow-Lowry, Conor/F-8843-2015; Khan, Rubab/F-9455-2015; Ottaway, David/J-5908-2015; Postiglione, Fabio/O-4744-2015; Sigg, Daniel/I-4308-2015; Pinto, Innocenzo/L-3520-2016 OI Finn, Lee Samuel/0000-0002-3937-0688; Gorodetsky, Michael/0000-0002-5159-2742; Allen, Bruce/0000-0003-4285-6256; Zhao, Chunnong/0000-0001-5825-2401; Pitkin, Matthew/0000-0003-4548-526X; Papa, M.Alessandra/0000-0002-1007-5298; Kanner, Jonah/0000-0001-8115-0577; Aulbert, Carsten/0000-0002-1481-8319; Freise, Andreas/0000-0001-6586-9901; Mandel, Ilya/0000-0002-6134-8946; Whiting, Bernard F/0000-0002-8501-8669; Veitch, John/0000-0002-6508-0713; Principe, Maria/0000-0002-6327-0628; Galdi, Vincenzo/0000-0002-4796-3600; McClelland, David/0000-0001-6210-5842; Strain, Kenneth/0000-0002-2066-5355; Lueck, Harald/0000-0001-9350-4846; Matichard, Fabrice/0000-0001-8982-8418; Pinto, Innocenzo M./0000-0002-2679-4457; Minelli, Jeff/0000-0002-5330-912X; Santamaria, Lucia/0000-0002-5986-0449; Pierro, Vincenzo/0000-0002-6020-5521; Hallam, Jonathan Mark/0000-0002-7087-0461; Sorazu, Borja/0000-0002-6178-3198; Stuver, Amber/0000-0003-0324-5735; Nishizawa, Atsushi/0000-0003-3562-0990; Zweizig, John/0000-0002-1521-3397; O'Shaughnessy, Richard/0000-0001-5832-8517; Frey, Raymond/0000-0003-0341-2636; Stein, Leo/0000-0001-7559-9597; Ward, Robert/0000-0001-5503-5241; Whelan, John/0000-0001-5710-6576; LONGO, Maurizio/0000-0001-8325-4003; Fairhurst, Stephen/0000-0001-8480-1961; Boschi, Valerio/0000-0001-8665-2293; Lam, Ping Koy/0000-0002-4421-601X; Danilishin, Stefan/0000-0001-7758-7493; Vecchio, Alberto/0000-0002-6254-1617; Khan, Rubab/0000-0001-5100-5168; Postiglione, Fabio/0000-0003-0628-3796; Sigg, Daniel/0000-0003-4606-6526; NR 31 TC 27 Z9 27 U1 3 U2 16 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1550-7998 J9 PHYS REV D JI Phys. Rev. D PD NOV PY 2009 VL 80 IS 10 AR 102002 DI 10.1103/PhysRevD.80.102002 PG 14 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 526SI UT WOS:000272313300005 ER PT J AU Calabrese, E Cooray, A Martinelli, M Melchiorri, A Pagano, L Slosar, A Smoot, GF AF Calabrese, Erminia Cooray, Asantha Martinelli, Matteo Melchiorri, Alessandro Pagano, Luca Slosar, Anze Smoot, George F. TI CMB lensing constraints on dark energy and modified gravity scenarios SO PHYSICAL REVIEW D LA English DT Article ID MICROWAVE BACKGROUND ANISOTROPIES; COSMOLOGICAL MODEL; ANGULAR VARIATIONS; PERTURBATIONS AB Weak gravitational lensing leaves a characteristic imprint on the cosmic microwave background temperature and polarization angular power spectra. Here, we investigate the possible constraints on the integrated lensing potential from future cosmic microwave background angular spectra measurements expected from Planck and EPIC. We find that Planck and EPIC will constrain the amplitude of the integrated projected potential responsible for lensing at 6% and 1% level, respectively, with very little sensitivity to the shape of the lensing potential. We discuss the implications of such a measurement in constraining dark energy and modified gravity scalar-tensor theories. We then discuss the impact of a wrong assumption on the weak lensing potential amplitude on cosmological parameter inference. C1 [Calabrese, Erminia; Martinelli, Matteo; Melchiorri, Alessandro; Pagano, Luca] Univ Roma La Sapienza, Dept Phys, I-00185 Rome, Italy. [Calabrese, Erminia; Martinelli, Matteo; Melchiorri, Alessandro; Pagano, Luca] Univ Roma La Sapienza, Ist Nazl Fis Nucl, I-00185 Rome, Italy. [Calabrese, Erminia; Cooray, Asantha] Univ Calif Irvine, Dept Phys & Astron, Ctr Cosmol, Irvine, CA 92697 USA. [Martinelli, Matteo] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Pagano, Luca] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Slosar, Anze; Smoot, George F.] Univ Calif Berkeley, Berkeley Ctr Cosmol Phys, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. [Slosar, Anze; Smoot, George F.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Smoot, George F.] Ewha Womans Univ, Inst Early Universe, Seoul, South Korea. [Smoot, George F.] Ewha Adv Acad, Seoul, South Korea. [Smoot, George F.] Univ Paris Diderot, Chaire Blaise Pascal, F-75205 Paris 13, France. RP Calabrese, E (reprint author), Univ Roma La Sapienza, Dept Phys, Ple Aldo Moro 2, I-00185 Rome, Italy. OI Melchiorri, Alessandro/0000-0001-5326-6003; Martinelli, Matteo/0000-0002-6943-7732 FU NSF CAREER [AST-0605427]; Berkeley Center for Cosmological Physics; ASI [I/016/07/0 COFIS] FX Research work of E. C. at UC Irvine was supported by the NSF CAREER under Contract No. AST-0605427. A. M. thanks the University of California Irvine for hospitality. A. S. acknowledges financial support from the Berkeley Center for Cosmological Physics. This research has been supported by the ASI under Contract No. I/016/07/0 COFIS. M. M. thanks D. Spergel and the University of Princeton for hospitality. L. P. thanks G. Rocha and the Jet Propulsion Laboratory for hospitality. NR 47 TC 24 Z9 24 U1 0 U2 1 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 2470-0010 EI 2470-0029 J9 PHYS REV D JI Phys. Rev. D PD NOV PY 2009 VL 80 IS 10 AR 103516 DI 10.1103/PhysRevD.80.103516 PG 10 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 526SI UT WOS:000272313300029 ER PT J AU Cutler, C Holz, DE AF Cutler, Curt Holz, Daniel E. TI Ultrahigh precision cosmology from gravitational waves SO PHYSICAL REVIEW D LA English DT Article ID HUBBLE-SPACE-TELESCOPE; RAY BURST PROGENITORS; COMPACT BINARIES; IA SUPERNOVAE; BLACK-HOLES; CONSTANT; PROSPECTS; UNIVERSE; GRAVITY; MERGERS AB We show that the Big Bang Observer (BBO), a proposed space-based gravitational-wave (GW) detector, would provide ultraprecise measurements of cosmological parameters. By detecting similar to 3x10(5) compact-star binaries, and utilizing them as standard sirens, BBO would determine the Hubble constant to similar to 0.1%, and the dark-energy parameters w(0) and w(a) to similar to 0.01 and similar to 0.1, respectively. BBO's dark-energy figure-of-merit would be approximately an order of magnitude better than all other proposed, dedicated dark-energy missions. To date, BBO has been designed with the primary goal of searching for gravitational waves from inflation, down to the level Omega(GW)similar to 10(-17); this requirement determines BBO's frequency band (deci-Hz) and its sensitivity requirement (strain measured to similar to 10(-24)). To observe an inflationary GW background, BBO would first have to detect and subtract out similar to 3x10(5) merging compact-star binaries, out to a redshift z similar to 5. It is precisely this carefully measured foreground which would enable high-precision cosmology. BBO would determine the luminosity distance to each binary to similar to percent accuracy. In addition, BBO's angular resolution would be sufficient to uniquely identify the host galaxy for the majority of binaries; a coordinated optical/infrared observing campaign could obtain the redshifts. Combining the GW-derived distances and the electromagnetically-derived redshifts for such a large sample of objects, out to such high redshift, naturally leads to extraordinarily tight constraints on cosmological parameters. We emphasize that such "standard siren" measurements of cosmology avoid many of the systematic errors associated with other techniques: GWs offer a physics-based, absolute measurement of distance. In addition, we show that BBO would also serve as an exceptionally powerful gravitational-lensing mission, and we briefly discuss other astronomical uses of BBO, including providing an early warning system for all short/hard gamma-ray bursts. C1 [Cutler, Curt] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Holz, Daniel E.] Los Alamos Natl Lab, Div Theoret, Los Alamos, NM 87545 USA. RP Cutler, C (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 73 TC 51 Z9 51 U1 1 U2 1 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 2470-0010 EI 2470-0029 J9 PHYS REV D JI Phys. Rev. D PD NOV PY 2009 VL 80 IS 10 AR 104009 DI 10.1103/PhysRevD.80.104009 PG 15 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 526SI UT WOS:000272313300044 ER PT J AU McKenzie, K Spero, RE Shaddock, DA AF McKenzie, Kirk Spero, Robert E. Shaddock, Daniel A. TI Performance of arm locking in LISA SO PHYSICAL REVIEW D LA English DT Article ID LASER FREQUENCY STABILIZATION; PHASE; DELAY; INTERFEROMETRY; MODEL AB For the Laser Interferometer Space Antenna (LISA) to reach its design sensitivity, the coupling of the free-running laser frequency noise to the signal readout must be reduced by more than 14 orders of magnitude. One technique employed to reduce the laser frequency noise will be arm locking, where the laser frequency is locked to the LISA arm length. In this paper we detail an implementation of arm locking. We investigate orbital effects (changing arm lengths and Doppler frequencies), the impact of errors in the Doppler knowledge that can cause pulling of the laser frequency, and the noise limit of arm locking. Laser frequency pulling is examined in two regimes: at lock acquisition and in steady state. The noise performance of arm locking is calculated with the inclusion of the dominant expected noise sources: ultrastable oscillator (clock) noise, spacecraft motion, and shot noise. We find that clock noise and spacecraft motion limit the performance of dual arm locking in the LISA science band. Studying these issues reveals that although dual arm locking [A. Sutton and D. A. Shaddock, Phys. Rev. D 78, 082001 (2008)] has advantages over single (or common) arm locking in terms of allowing high gain, it has disadvantages in both laser frequency pulling and noise performance. We address this by proposing a modification to the dual arm-locking sensor, a hybrid of common and dual arm-locking sensors. This modified dual arm-locking sensor has the laser frequency pulling characteristics and low-frequency noise coupling of common arm locking, but retains the control system advantages of dual arm locking. We present a detailed design of an arm-locking controller and perform an analysis of the expected performance when used with and without laser prestabilization. We observe that the sensor phase changes beneficially near unity-gain frequencies of the arm-locking controller, allowing a factor of 10 more gain than previously believed, without degrading stability. With a time-delay error of 3 ns (equivalent of 1 m interspacecraft ranging error), time-delay interferometry (TDI) is capable of suppressing 300 Hz/Hz of laser frequency noise to the required level. We show that if no interspacecraft laser links fail, arm locking alone surpasses this noise performance for the entire mission. If one interspacecraft laser link fails, arm locking alone will achieve this performance for all but approximately 1 h per year, when the arm length mismatch of the two remaining arms passes through zero. Therefore, the LISA sensitivity can be realized with arm locking and time-delay interferometry only, without any form of prestabilization. C1 [McKenzie, Kirk; Spero, Robert E.; Shaddock, Daniel A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Shaddock, Daniel A.] Australian Natl Univ, Ctr Gravitat Phys, Canberra, ACT 0200, Australia. RP McKenzie, K (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. RI Shaddock, Daniel/A-7534-2011 OI Shaddock, Daniel/0000-0002-6885-3494 NR 33 TC 9 Z9 9 U1 0 U2 1 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1550-7998 J9 PHYS REV D JI Phys. Rev. D PD NOV PY 2009 VL 80 IS 10 AR 102003 DI 10.1103/PhysRevD.80.102003 PG 28 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 526SI UT WOS:000272313300006 ER PT J AU Sittler, EC Ali, A Cooper, JF Hartle, RE Johnson, RE Coates, AJ Young, DT AF Sittler, E. C., Jr. Ali, A. Cooper, J. F. Hartle, R. E. Johnson, R. E. Coates, A. J. Young, D. T. TI Heavy ion formation in Titan's ionosphere: Magnetospheric introduction of free oxygen and a source of Titan's aerosols? SO PLANETARY AND SPACE SCIENCE LA English DT Review DE Titan; Saturn's magnetosphere; Heavy negative ions; Oxygen; Aerosols; Astrobiology ID POLYCYCLIC AROMATIC-HYDROCARBONS; MASS PROTOSTAR IRAS-04368+2557; FULLERENE RADICAL CATIONS; ELECTRON-ATTACHMENT; SATURNIAN SYSTEM; COUPLING PHOTOCHEMISTRY; INFRARED OBSERVATIONS; PLANETARY SCIENCE; ORGANIC-CHEMISTRY; UPPER-ATMOSPHERE AB Discovery by Cassini's plasma instrument of heavy positive and negative ions within Titan's upper atmosphere and ionosphere has advanced our understanding of ion neutral chemistry within Titan's upper atmosphere, primarily composed of molecular nitrogen, with similar to 2.5% methane. The external energy flux transforms Titan's upper atmosphere and ionosphere into a medium rich in complex hydrocarbons, nitriles and haze particles extending from the surface to 1200km altitudes. The energy sources are solar UV, solar X-rays, Saturn's magnetospheric ions and electrons, solar wind and shocked magnetosheath ions and electrons, galactic cosmic rays (GCR) and the ablation of incident meteoritic dust from Enceladus' E-ring and interplanetary medium. Here it is proposed that the heavy atmospheric ions detected in situ by Cassini for heights > 950 km, are the likely seed particles for aerosols detected by the Huygens probe for altitudes < 100 km. These seed particles may be in the form of polycyclic aromatic hydrocarbons (PAH) containing both carbon and hydrogen atoms C,,H,. There could also be hollow shells of carbon atoms, such as C-60, called fullerenes which contain no hydrogen. The fullerenes may compose a significant fraction of the seed particles with PAHs contributing the rest. As shown by Cassini, the upper atmosphere is bombarded by magnetospheric plasma composed of protons, H-2(+) and water group ions. The latter provide keV oxygen, hydroxyl and water ions to Titan's upper atmosphere and can become trapped within the fullerene molecules and ions. Pickup keV N-2(+), N+ and CH4+ can also be implanted inside of fullerenes. Attachment of oxygen ions to PAH molecules is uncertain, but following thermalization O+ can interact with abundant CH4 contributing to the CO and CO2 observed in Titan's atmosphere. If an exogenic keV O+ ion is implanted into the haze particles, it could become free oxygen within those aerosols that eventually fall onto Titan's surface. The process of freeing oxygen within aerosols could be driven by cosmic ray interactions with aerosols at all heights. This process could drive pre-biotic chemistry within the descending aerosols. Cosmic ray interactions with grains at the surface, including water frost depositing on grains from cryovolcanism, would further add to abundance of trapped free oxygen. Pre-biotic chemistry could arise within surface microcosms of the composite organic-ice grains, in part driven by free oxygen in the presence of organics and any heat sources, thereby raising the astrobiological potential for microscopic equivalents of Darwin's "warm ponds" on Titan. Published by Elsevier Ltd. C1 [Sittler, E. C., Jr.; Ali, A.; Cooper, J. F.; Hartle, R. E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA. [Ali, A.] Univ Maryland, College Pk, MD 20742 USA. [Johnson, R. E.] Univ Virginia, Charlottesville, VA USA. [Young, D. T.] SW Res Inst, San Antonio, TX USA. RP Sittler, EC (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD USA. EM Edward.C.Sittler@nasa.gov RI Cooper, John/D-4709-2012; Coates, Andrew/C-2396-2008 OI Coates, Andrew/0000-0002-6185-3125 FU NASA jet Propulsion Laboratory [1243218]; NASA Cassini Data Analysis Program (CDAP) FX This work was supported at NASA Goddard Space Flight center in part by the Cassini Plasma Spectrometer (CAPS) Project through NASA jet Propulsion Laboratory contract 1243218 with the Southwest Research Institute in San Antonio, Texas. Additional support was provided at Goddard by the NASA Cassini Data Analysis Program (CDAP). NR 130 TC 38 Z9 38 U1 0 U2 28 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0032-0633 J9 PLANET SPACE SCI JI Planet Space Sci. PD NOV PY 2009 VL 57 IS 13 SI SI BP 1547 EP 1557 DI 10.1016/j.pss.2009.07.017 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 526JM UT WOS:000272284300004 ER PT J AU Nixon, CA Jennings, DE Flaud, JM Bezard, B Teanby, NA Irwin, PGJ Ansty, TM Coustenis, A Vinatier, S Flasar, FM AF Nixon, C. A. Jennings, D. E. Flaud, J-M. Bezard, B. Teanby, N. A. Irwin, P. G. J. Ansty, T. M. Coustenis, A. Vinatier, S. Flasar, F. M. TI Titan's prolific propane: The Cassini CIRS perspective SO PLANETARY AND SPACE SCIENCE LA English DT Article DE Titan atmosphere; Atmospheric abundances, outer planets; Propane; Infrared spectroscopy; Abundance retrieval ID COMPOSITE INFRARED SPECTROMETER; ISOTOPIC-RATIOS; SPECTROSCOPIC DATABASE; LATITUDINAL VARIATIONS; RADIATIVE-TRANSFER; THERMAL EMISSION; SPECTRAL REGION; D/H RATIO; ATMOSPHERE; STRATOSPHERE AB Although propane gas (C3H8) was first detected in the stratosphere of Titan by the Voyager IRIS infrared spectrometer in 1980, obtaining an accurate measurement of its abundance has proved difficult. All existing measurements have been made by modeling the nu(26) band at 748cm(-1): however, different analyzes over time have yielded quite different results, and it also suffers from confusion with the strong nearby nu(5) band of acetylene. In this paper we select large spectral averages of data from the Cassini Composite Infrared Spectrometer (CIRS) obtained in limb-viewing mode at low latitudes (30 degrees S-30 degrees N), greatly increasing the path length and hence signal-to-noise ratio for optically thin trace species such as propane. By modeling and subtracting the emissions of other gas species, we demonstrate that at least six infrared bands of propane are detected by CIRS, including two not previously identified in Titan spectra. Using a new linelist for the range 1300-1400 cm(-1), along with an existing GEISA list, we retrieve propane abundances from two bands at 748 and 1376 cm(-1). At 748 cm(-1) we retrieve 4.2 +/- 0.5 x 10(-7) (1 - sigma error) at 2 mbar, in good agreement with previous studies, although lack of hotbands in the present spectral atlas remains a problem. We also determine 5.7 +/- 0.8 x 10(-7) at 2 mbar from the 1376 cm(-1) band - a value that is probably affected by systematic errors including continuum gradients due to haze and also an imperfect model of the nu(6) band of ethane. This study clearly shows for the first time the ubiquity of propane's emission bands across the thermal infrared spectrum of Titan, and points to an urgent need for further laboratory spectroscopy work, both to provide the line positions and intensities needed to model these bands, and also to further characterize haze spectral opacity. The present lack of accurate modeling capability for propane is an impediment not only for the measurement of propane itself, but also for the search for the emissions of new molecules in many spectral regions. (C) 2009 Elsevier Ltd. All rights reserved. C1 [Nixon, C. A.; Jennings, D. E.; Flasar, F. M.] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Planetary Syst Lab, Greenbelt, MD 20771 USA. [Nixon, C. A.] Univ Maryland, College Pk, MD 20742 USA. [Flaud, J-M.] Univ Paris Est, CNRS, F-94010 Creteil, France. [Flaud, J-M.] Univ Paris 07, CNRS, F-94010 Creteil, France. [Bezard, B.; Coustenis, A.; Vinatier, S.] Observ Paris, CNRS, LESIA, F-92195 Meudon, France. [Teanby, N. A.; Irwin, P. G. J.] Univ Oxford, Clarendon Lab, Oxford OX1 3PU, England. [Ansty, T. M.] Cornell Univ, Ithaca, NY 14853 USA. RP Nixon, CA (reprint author), NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Planetary Syst Lab, Code 693, Greenbelt, MD 20771 USA. EM conor.a.nixon@nasa.gov RI Nixon, Conor/A-8531-2009; Flasar, F Michael/C-8509-2012; OI Nixon, Conor/0000-0001-9540-9121; Teanby, Nicholas/0000-0003-3108-5775; Irwin, Patrick/0000-0002-6772-384X NR 52 TC 28 Z9 28 U1 1 U2 4 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0032-0633 J9 PLANET SPACE SCI JI Planet Space Sci. PD NOV PY 2009 VL 57 IS 13 SI SI BP 1573 EP 1585 DI 10.1016/j.pss.2009.06.021 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 526JM UT WOS:000272284300006 ER PT J AU Hartogh, P Lellouch, E Crovisier, J Banaszkiewicz, M Bensch, F Bergin, EA Billebaud, F Biver, N Blake, GA Blecka, MI Blommaert, J Bockelee-Morvan, D Cavalie, T Cernicharo, J Courtin, R Davis, G Decin, L Encrenaz, P Encrenaz, T Gonzalez, A de Graauw, T Hutsemekers, D Jarchow, C Jehin, E Kidger, M Kuppers, M de Lange, A Lara, LM Lis, DC Lorente, R Manfroid, J Medvedev, AS Moreno, R Naylor, DA Orton, G Portyankina, G Rengel, M Sagawa, H Sanchez-Portal, M Schieder, R Sidher, S Stam, D Swinyard, B Szutowicz, S Thomas, N Thornhill, G Vandenbussche, B Verdugo, E Waelkens, C Walker, H AF Hartogh, P. Lellouch, E. Crovisier, J. Banaszkiewicz, M. Bensch, F. Bergin, E. A. Billebaud, F. Biver, N. Blake, G. A. Blecka, M. I. Blommaert, J. Bockelee-Morvan, D. Cavalie, T. Cernicharo, J. Courtin, R. Davis, G. Decin, L. Encrenaz, P. Encrenaz, T. Gonzalez, A. de Graauw, T. Hutsemekers, D. Jarchow, C. Jehin, E. Kidger, M. Kueppers, M. de lange, A. Lara, L-M. Lis, D. C. Lorente, R. Manfroid, J. Medvedev, A. S. Moreno, R. Naylor, D. A. Orton, G. Portyankina, G. Rengel, M. Sagawa, H. Sanchez-Portal, M. Schieder, R. Sidher, S. Stam, D. Swinyard, B. Szutowicz, S. Thomas, N. Thornhill, G. Vandenbussche, B. Verdugo, E. Waelkens, C. Walker, H. TI Water and related chemistry in the solar system. A guaranteed time key programme for Herschel SO PLANETARY AND SPACE SCIENCE LA English DT Review DE Herschel space observatory; Water; Mars; Giant planets; Titan; Comets ID ASTRONOMY-SATELLITE OBSERVATIONS; GENERAL-CIRCULATION MODEL; CARBON-ISOTOPE RATIOS; MARTIAN ATMOSPHERE; VERTICAL-DISTRIBUTION; D/H RATIO; HALE-BOPP; SUBMILLIMETER OBSERVATIONS; JUPITERS STRATOSPHERE; PHOTOCHEMICAL MODEL AB "Water and related chemistry in the Solar System" is a Herschel Space Observatory Guaranteed-Time Key Programme. This project, approved by the European Space Agency, aims at determining the distribution, the evolution and the origin of water in Mars, the outer planets, Titan, Enceladus and the comets. It addresses the broad topic of water and its isotopologues in planetary and cometary atmospheres. The nature of cometary activity and the thermodynamics of cometary comae will be investigated by studying water excitation in a sample of comets. The D/H ratio, the key parameter for constraining the origin and evolution of Solar System species, will be measured for the first time in a Jupiter-family comet. A comparison with existing and new measurements of D/H in Oort-cloud comets will constrain the composition of pre-solar cometary grains and possibly the dynamics of the protosolar nebula. New measurements of D/H in giant planets, similarly constraining the composition of protoplanetary ices, will be obtained. The D/H and other isotopic ratios, diagnostic of Mars' atmosphere evolution, will be accurately measured in H2O and CO. The role of water vapor in Mars' atmospheric chemistry will be studied by monitoring vertical profiles of H2O and HDO and by searching for several other species (and CO and H2O isotopes). A detailed study of the source of water in the upper atmosphere of the Giant Planets and Titan will be performed. By monitoring the water abundance, vertical profile, and input fluxes in the various objects, and when possible with the help of mapping observations, we will discriminate between the possible sources of water in the outer planets (interplanetary dust particles, cometary impacts, and local sources). In addition to these interconnected objectives, serendipitous searches will enhance our knowledge of the composition of planetary and cometary atmospheres. (C) 2009 Elsevier Ltd. All rights reserved. C1 [Hartogh, P.; Cavalie, T.; Gonzalez, A.; Jarchow, C.; Medvedev, A. S.; Rengel, M.; Sagawa, H.] Max Planck Inst Solar Syst Res, D-37191 Katlenburg Lindau, Germany. [Lellouch, E.; Crovisier, J.; Biver, N.; Bockelee-Morvan, D.; Courtin, R.; Encrenaz, T.; Moreno, R.] Observ Paris, LESIA, Paris, France. [Banaszkiewicz, M.; Blecka, M. I.; Szutowicz, S.] Polish Acad Sci, Space Res Ctr, PL-01237 Warsaw, Poland. [Bensch, F.] Univ Bonn, Argelander Inst Astron, D-5300 Bonn, Germany. [Bensch, F.] German Aerosp Ctr, DLR, Bonn, Germany. [Bergin, E. A.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Billebaud, F.] Univ Bordeaux, Lab Astrophys Bordeaux, Bordeaux, France. [Billebaud, F.] CNRS INSU, UMR 5804, Floirac, France. [Blake, G. A.] CALTECH, Pasadena, CA USA. [Blommaert, J.; Decin, L.; Vandenbussche, B.; Waelkens, C.] Katholieke Univ Leuven, Inst Sterrenkunde, Louvain, Belgium. [Cernicharo, J.] INTA, CAB CSIC, Lab Mol Astrophys, Madrid, Spain. [Davis, G.] Joint Astron Ctr, Hilo, HI 96720 USA. [Encrenaz, P.] Observ Paris, LERMA, Paris, France. [Gonzalez, A.; Lara, L-M.] CSIC, Inst Astrofis Andalucia, Granada, Spain. [de Graauw, T.] Leiden Univ, NL-2300 RA Leiden, Netherlands. [Hutsemekers, D.; Jehin, E.; Manfroid, J.] Univ Liege, Inst Astrophys & Geophys, B-4000 Liege, Belgium. [Jehin, E.] European So Observ, Santiago, Chile. [Kidger, M.; Lorente, R.; Sanchez-Portal, M.; Thornhill, G.; Verdugo, E.] European Space Agcy, European Space Astron Ctr, Herschel Sci Ctr, Madrid, Spain. [Kueppers, M.] European Space Agcy, European Space Astron Ctr, Rosetta Sci Operat Ctr, Madrid, Spain. [Naylor, D. A.] Univ Lethbridge, Dept Phys & Astron, Lethbridge, AB T1K 3M4, Canada. [Orton, G.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Portyankina, G.; Thomas, N.] Univ Bern, Inst Phys, CH-3012 Bern, Switzerland. [Schieder, R.] Univ Cologne, Inst Phys 1, D-5000 Cologne 41, Germany. [Sidher, S.; Swinyard, B.; Walker, H.] Rutherford Appleton Lab, Space Sci & Technol Dept, Rutherford, NJ USA. RP Hartogh, P (reprint author), Max Planck Inst Solar Syst Res, D-37191 Katlenburg Lindau, Germany. EM hartogh@mps.mpg.de OI Medvedev, Alexander/0000-0003-2713-8977 NR 115 TC 49 Z9 49 U1 4 U2 20 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0032-0633 J9 PLANET SPACE SCI JI Planet Space Sci. PD NOV PY 2009 VL 57 IS 13 SI SI BP 1596 EP 1606 DI 10.1016/j.pss.2009.07.009 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 526JM UT WOS:000272284300008 ER PT J AU Cooper, JF Cooper, PD Sittler, EC Sturner, SJ Rymer, AM AF Cooper, John F. Cooper, Paul D. Sittler, Edward C. Sturner, Steven J. Rymer, Abigail M. TI Old Faithful model for radiolytic gas-driven cryovolcanism at Enceladus SO PLANETARY AND SPACE SCIENCE LA English DT Review DE Enceladus; Energetic particles; Radiolysis; Oxidants; Water; Cryovolcanism ID NEUTRAL MASS-SPECTROMETER; AMORPHOUS WATER ICE; GEYSER-LIKE PLUMES; HYDROGEN-PEROXIDE; SATURNS MAGNETOSPHERE; GALILEAN SATELLITES; ENERGETIC PARTICLES; INNER MAGNETOSPHERE; PROTON IRRADIATION; ION IRRADIATION AB A new model is presented on how chemically driven cryovolcanism might contribute to episodic outgassing at the icy moon Enceladus and potentially elsewhere including Europa and Kuiper Belt Objects. Exposed water ices can become oxidized from radiolytic chemical alteration of near-surface water ice by space environment irradiation. In contact with primordially abundant reductants such as NH(3), CH(4), and other hydrocarbons, the product oxidants can react exothermically to produce volatile gases driving cryovolcanism via gas-piston forces on any subsurface liquid reservoirs. Radiolytic oxidants such as H(2)O(2) and O(2) can continuously accumulate deep in icy regoliths and be conveyed by rheological flows to subsurface chemical reaction zones over million-year time scales indicated by cratering ages for active regions of Enceladus and Europa. Surface blanketing with cryovolcanic plume ejecta would further accelerate regolith burial of radiolytic oxidants. Episodic heating from transient gravitational tides, radioisotope decay, impacts, or other geologic events might occasionally accelerate chemical reaction rates and ignite the exothermic release of cumulative radiolytic oxidant energy. The time history for the suggested "Old Faithful" model of radiolytic gas-driven cryovolcanism at Enceladus and elsewhere therefore consists of long periods of chemical energy accumulation punctuated by much briefer episodes of cryovolcanic activity. The most probable sequence for detection of activity in the current epoch is a long evolutionary phase of slow but continuous oxidant accumulation over billions of years followed by continuous but variable high activity over the past 10(7)-10(8) years. Detectable cryovolcanic activity could then later decline due to near-total oxidation of the theologically accessible ice crust and depletion the accessible reductant abundances, as may have already occurred for Europa in the more intense radiation environment of Jupiter's magnetosphere. Astrobiological potential of Enceladus could correspondingly be higher than at Europa due to a less extreme state of oxidation and greater residual abundance of organics. Published by Elsevier Ltd. C1 [Cooper, John F.] NASA, Goddard Space Flight Ctr, Heliospher Phys Lab, Greenbelt, MD 20771 USA. [Cooper, Paul D.] George Mason Univ, Dept Chem & Biochem, Fairfax, VA 22030 USA. [Sittler, Edward C.] NASA, Goddard Space Flight Ctr, Geospace Phys Lab, Greenbelt, MD 20771 USA. [Sturner, Steven J.] NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA. [Sturner, Steven J.] NASA, Goddard Space Flight Ctr, Astroparticle Phys Lab, Greenbelt, MD 20771 USA. [Rymer, Abigail M.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. RP Cooper, JF (reprint author), NASA, Goddard Space Flight Ctr, Heliospher Phys Lab, Code 672,8800 Greenbelt Rd, Greenbelt, MD 20771 USA. EM John.F.Cooper@nasa.gov RI Cooper, John/D-4709-2012 FU Cassini Plasma Spectrometer (CAPS) Project through NASA jet Propulsion Laboratory [1243218]; NASA Outer Planets Research and Planetary Atmospheres programs; Space Physics Data Facility project of the NASA Heliophysics program FX This work was supported at NASA Goddard Space Flight center in part by the Cassini Plasma Spectrometer (CAPS) Project through NASA jet Propulsion Laboratory contract 1243218 with the Southwest Research Institute in San Antonio, Texas. Additional support was provided at Goddard by the NASA Outer Planets Research and Planetary Atmospheres programs, and by the Space Physics Data Facility project of the NASA Heliophysics program. NR 109 TC 17 Z9 17 U1 2 U2 19 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0032-0633 J9 PLANET SPACE SCI JI Planet Space Sci. PD NOV PY 2009 VL 57 IS 13 SI SI BP 1607 EP 1620 DI 10.1016/j.pss.2009.08.002 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 526JM UT WOS:000272284300009 ER PT J AU Patnaik, SN Pai, SS Coroneos, RM AF Patnaik, S. N. Pai, S. S. Coroneos, R. M. TI Reliability-based design optimization of airframe components SO PROCEEDINGS OF THE INSTITUTION OF MECHANICAL ENGINEERS PART G-JOURNAL OF AEROSPACE ENGINEERING LA English DT Article DE optimization; deterministic; stochastic; risk; industrial; CometBoards; distribution; normal; Weibull; strain energy; inverted S graph AB A stochastic design optimization (SDO) methodology has been developed to design components of an airframe structure. The design is obtained as a function of the risk or reliability. Uncertainties in load, strength, and material properties are treated as distribution functions. Design constraints and optimum weight become functions of reliability. Weight versus reliability traces out an inverted S-shaped graph. The centre of the graph corresponds to 50 per cent probability of success. A heavy design with weight approaching infinity could be produced for a near-zero rate of failure. Weight can be reduced to a small value for the most failure-prone design. Reliability can be changed for different components of an airframe structure. The SDO capability is obtained by combining three codes. MSC/Nastran is the deterministic analysis tool, the fast probability integration of the NESSUS (numerical evaluation of stochastic structures under stress) software is the probabilistic calculator, and NASA (National Aeronautics and Space Administration) Glenn Research Center's testbed CometBoards is the optimizer. The SDO capability requires a finite-element model, a material model, a load model, and a design model. The stochastic optimization concept is illustrated considering an academic example and a real-life raked wingtip structure of the Boeing 767-400 extended range airliner made of metallic and composite materials. C1 [Patnaik, S. N.] Ohio Aerosp Inst, Cleveland, OH 44142 USA. [Pai, S. S.; Coroneos, R. M.] NASA, Glenn Res Ctr, Cleveland, OH USA. RP Patnaik, SN (reprint author), Ohio Aerosp Inst, Brook Pk, Cleveland, OH 44142 USA. EM Surya.N.Patnaik@nasa.gov NR 26 TC 0 Z9 0 U1 0 U2 3 PU PROFESSIONAL ENGINEERING PUBLISHING LTD PI WESTMINISTER PA 1 BIRDCAGE WALK, WESTMINISTER SW1H 9JJ, ENGLAND SN 0954-4100 J9 P I MECH ENG G-J AER JI Proc. Inst. Mech. Eng. Part G-J. Aerosp. Eng. PD NOV PY 2009 VL 223 IS G7 BP 1019 EP 1036 DI 10.1243/09544100JAERO444 PG 18 WC Engineering, Aerospace; Engineering, Mechanical SC Engineering GA 529CY UT WOS:000272494600016 ER PT J AU Gull, TR AF Gull, T. R. TI The Variable 6307 angstrom Emission Line in the Spectrum of Eta Carinae: Blueshifted [S III] lambda 6313 from the Interacting Winds SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article AB The 6307 angstrom emission line in the spectrum of eta Car, found by Martin et al., is blue-shifted [S III] lambda 6313 emission originating from the outer wind structures of the massive binary system. We realized the identification while analyzing multiple forbidden emission lines not normally seen in the spectra of massive stars. The high spatial and moderate spectral resolutions of HST/STIS resolve forbidden lines of Fe(+), N(+), Fe(+2), S(+2), Ne(+2), and Ar(+2) into spatially and velocity-resolved ropelike features originating from collisionally-excited ions photoionized by UV photons or collisions. While the [Fe II] emission extends across a velocity range of +/- 500 km s(-1) out to 0.7 '', more highly ionized forbidden emissions ([N II], [Fe III], [S III], [Ar III], and [Ne III]) range in velocity from -500 to +200 km s(-1), but spatially extend out to only 0.4 ''. The [Fe II] defines the outer regions of the massive primary wind. The [N II], [Fe III] emissions define the the outer wind interaction regions directly photoionized by far-UV radiation. Variations in emission of [S III] lambda lambda 9533, 9071, and 6313 suggest density ranges of 10(6) - 10(10) cm(-3) for electron temperatures ranging from 8000 to 13,000 K. Mapping the temporal changes of the emission structure at critical phases of the 5.54 yr period will provide important diagnostics of the interacting winds. C1 NASA, Goddard Space Flight Ctr, Explorat Universe Div, Lab Extrasolar Planets & Stellar Astrophys, Greenbelt, MD 20771 USA. RP Gull, TR (reprint author), NASA, Goddard Space Flight Ctr, Explorat Universe Div, Lab Extrasolar Planets & Stellar Astrophys, Greenbelt, MD 20771 USA. RI Gull, Theodore/D-2753-2012 OI Gull, Theodore/0000-0002-6851-5380 FU NASA/ESA Hubble Space Telescope [7302, 8036, 8483, 8619, 9083, 9337, 9420, 9973, 10957, 11273]; Space Telescope Imaging Spectrograph Science Team; Space Telescope Science Institute; Association of Universities for Research in Astronomy, Inc; NASA [NAS5-26555] FX The observations were accomplished with the NASA/ESA Hubble Space Telescope. Support for Program numbers 7302, 8036, 8483, 8619, 9083, 9337, 9420, 9973, 10957, and 11273 was provided by NASA directly to the Space Telescope Imaging Spectrograph Science Team and through grants from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. All analysis was done using STIS IDT software tools on data available through the HST eta Car Treasury public archive. NR 11 TC 0 Z9 0 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6280 J9 PUBL ASTRON SOC PAC JI Publ. Astron. Soc. Pac. PD NOV PY 2009 VL 121 IS 885 BP 1213 EP 1217 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 511UB UT WOS:000271193700006 ER PT J AU Boss, AP Weinberger, AJ Anglada-Escude, G Thompson, IB Burley, G Birk, C Pravdo, SH Shaklan, SB Gatewood, GD Majewski, SR Patterson, RJ AF Boss, Alan P. Weinberger, Alycia J. Anglada-Escude, Guillem Thompson, Ian B. Burley, Gregory Birk, Christoph Pravdo, Steven H. Shaklan, Stuart B. Gatewood, George D. Majewski, Steven R. Patterson, Richard J. TI The Carnegie Astrometric Planet Search Program SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article ID EXTRA-SOLAR PLANETS; LOW-MASS STARS; BROWN DWARF; PRECISION ASTROMETRY; MICROLENSING EVENT; RADIAL-VELOCITY; VISUAL ORBIT; NEARBY; PHOTOMETRY; DISCOVERY AB We are undertaking an astrometric search for gas giant planets and brown dwarfs orbiting nearby low-mass dwarf stars with the 2.5 m du Pont Telescope at the Las Campanas Observatory in Chile. We have built two specialized astrometric cameras, the Carnegie Astrometric Planet Search Cameras (CAPSCam-S and CAPSCam-N), using two Teledyne HAWAII-2RG HyViSI arrays, with the cameras' design having been optimized for high-accuracy astrometry of M dwarf stars. We describe two independent CAPSCam data reduction approaches and present a detailed analysis of the observations to date of one of our target stars, NLTT 48256. Observations of NLTT 48256 taken since 2007 July with CAPSCam-S imply that astrometric accuracies of around 0.3 mas hr(-1) are achievable, sufficient to detect a Jupiter-mass companion orbiting 1 AU from a late M dwarf 10 pc away with a signal-to-noise ratio (S/N) of about 4. We plan to follow about 100 nearby (primarily within about 10 pc) low-mass stars, principally late M, L, and T dwarfs, for 10 yr or more, in order to detect very low-mass companions with orbital periods long enough to permit the existence of habitable, Earth-like planets on shorter-period orbits. These stars are generally too faint and red to be included in ground-based Doppler planet surveys, which are often optimized for FGK dwarfs. The smaller masses of late M dwarfs also yield correspondingly larger astrometric signals for a given mass planet. Our search will help to determine whether gas giant planets form primarily by core accretion or by disk instability around late M dwarf stars. C1 [Boss, Alan P.; Weinberger, Alycia J.; Anglada-Escude, Guillem] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC 20015 USA. [Thompson, Ian B.; Burley, Gregory; Birk, Christoph] Carnegie Observ, Pasadena, CA 91101 USA. [Pravdo, Steven H.; Shaklan, Stuart B.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Gatewood, George D.] Univ Pittsburgh, Allegheny Observ, Pittsburgh, PA 15214 USA. [Majewski, Steven R.; Patterson, Richard J.] Univ Virginia, Dept Astron, Charlottesville, VA 22903 USA. RP Boss, AP (reprint author), Carnegie Inst Sci, Dept Terr Magnetism, 5241 Broad Branch Rd NW, Washington, DC 20015 USA. RI Patterson, Richard/F-5690-2013 OI Patterson, Richard/0000-0003-1494-8399 NR 62 TC 26 Z9 26 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6280 EI 1538-3873 J9 PUBL ASTRON SOC PAC JI Publ. Astron. Soc. Pac. PD NOV PY 2009 VL 121 IS 885 BP 1218 EP 1231 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 511UB UT WOS:000271193700007 ER PT J AU Pasachoff, JM Jacobson, WA Sterling, AC AF Pasachoff, Jay M. Jacobson, William A. Sterling, Alphonse C. TI Limb Spicules from the Ground and from Space SO SOLAR PHYSICS LA English DT Article DE TRACE; Swedish 1-m solar telescope; Hinode; Sun: spicules; Sun: chromosphere; Solar dynamics observatory ID CHROMOSPHERIC FINE-STRUCTURE; DAMPED ALFVEN WAVES; SOLAR SPICULES; TRANSITION REGION; NUMERICAL SIMULATIONS; DYNAMIC FIBRILS; DARK MOTTLES; H-ALPHA; JETS; TRACE AB We amassed statistics for quiet-sun chromosphere spicules at the limb using ground-based observations from the Swedish 1-m Solar Telescope on La Palma and simultaneously from NASA's Transition Region and Coronal Explorer (TRACE) spacecraft. The observations were obtained in July 2006. With the 0.2 arcsecond resolution obtained after maximizing the ground-based resolution with the Multi-Object Multi-Frame Blind Deconvolution (MOMFBD) program, we obtained specific statistics for sizes and motions of over two dozen individual spicules, based on movies compiled at 50-second cadence for the series of five wavelengths observed in a very narrow band at H alpha, on-band and at +/- 0.035 nm and +/- 0.070 nm (10 s at each wavelength) using the SOUP filter, and had simultaneous observations in the 160 nm EUV continuum from TRACE. The MOMFBD restoration also automatically aligned the images, facilitating the making of Dopplergrams at each off-band pair. We studied 40 H alpha spicules, and 14 EUV spicules that overlapped H alpha spicules; we found that their dynamical and morphological properties fit into the framework of several previous studies. From a preliminary comparison with spicule theories, our observations are consistent with a reconnection mechanism for spicule generation, and with UV spicules being a sheath region surrounding the H alpha spicules. C1 [Pasachoff, Jay M.; Jacobson, William A.] Williams Coll, Hopkins Observ, Williamstown, MA 01267 USA. [Pasachoff, Jay M.] CALTECH, Pasadena, CA 91125 USA. [Sterling, Alphonse C.] NASA, MSFC, Space Sci Off VP62, Huntsville, AL 35805 USA. RP Pasachoff, JM (reprint author), Williams Coll, Hopkins Observ, Williamstown, MA 01267 USA. EM jay.m.pasachoff@williams.edu FU NASA [NNG04GF99G, NNG04GK44G]; NASA's Marshall Space Flight Center [NNM07AA01G]; NASA's Office of Space Science FX We thank Mats Lofdahl of the Royal Swedish Academy of Sciences for his work on Multi-Object Multi-Frame Blind Deconvolution of the Swedish 1-m Solar Telescope data and Michiel van Noort there for helpful assistance. We thank Evan Tingle (Keck Northeast Astronomy Consortium Summer Fellow from Wesleyan University, sponsored by a Research Experiences for Undergraduates grant from the National Science Foundation) for his collaboration with data reduction. We are grateful to C. Alex Young (NASA's Goddard Space Flight Center) and Daniel B. Seaton ( formerly Williams College, then University of New Hampshire, and now Royal Observatory of Belgium) for consultation on alignment of images. We thank former Williams College students Anne Jaskot and Megan Bruck for their participation while obtaining the data at the Swedish 1-m Solar Telescope and Jennifer Yee (KNAC Summer Fellow from Swarthmore College) for work on earlier SST spicule data. Bruck also worked on arranging MOMFBD. We appreciate the earlier undergraduate thesis work at Williams College on SST and TRACE data of Kamen Kozarev ( now at Boston University) and Owen Westbrook ( now at M. I. T.). We thank Bart De Pontieu (Lockheed Martin Solar and Astrophysics Laboratory) for assistance during the first of the three SST data runs, and Rolf Kever and the Telescope Operators for their help also on site. We thank Leon Golub, Edward DeLuca, and Jonathan Cirtain (Harvard-Smithsonian Center for Astrophysics) for consultations on the TRACE data reduction. We thank Steven P. Souza of Williams College's Astronomy Department for computing assistance and advice.; J.M.P. thanks Michael Brown and the Division of Geological and Planetary Sciences of the California Institute of Technology for sabbatical hospitality during the preparation of this paper.; Our work was funded in part by NASA grants NNG04GF99G and NNG04GK44G from the Solar Terrestrial Program and grant NNM07AA01G from NASA's Marshall Space Flight Center. A.C.S. was supported by funding from NASA's Office of Space Science through the Living with a Star, the Solar Physics Supporting Research and Technology, and the Sun-Earth Connection Guest Investigator Programs. NR 76 TC 31 Z9 32 U1 1 U2 4 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 NOV PY 2009 VL 260 IS 1 BP 59 EP 82 DI 10.1007/s11207-009-9430-x PG 24 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 521YP UT WOS:000271962900005 ER PT J AU Kundu, MR Grechnev, VV White, SM Schmahl, EJ Meshalkina, NS Kashapova, LK AF Kundu, M. R. Grechnev, V. V. White, S. M. Schmahl, E. J. Meshalkina, N. S. Kashapova, L. K. TI High-Energy Emission from a Solar Flare in Hard X-rays and Microwaves SO SOLAR PHYSICS LA English DT Article DE Flares, impulsive phase; Radio bursts, microwave (mm, cm); X-ray bursts, hard ID COLLAPSING MAGNETIC TRAPS; BURSTS; ELECTRONS; WAVELENGTHS; PARTICLES; RADIO; EXPRESSIONS; MILLIMETER; NOBEYAMA; IMAGER AB We investigate accelerated electron energy spectra for different sources in a large flare using simultaneous observations obtained with two instruments, the Nobeyama Radio Heliograph (NoRH) at 17 and 34 GHz, and the Reuven Ramaty High Energy Solar Spectroscopic Imager (RHESSI) at hard X-rays. This flare is one of the few in which emission up to energies exceeding 200 keV can be imaged in hard X-rays. Furthermore, we can investigate the spectra of individual sources up to this energy. We discuss and compare the HXR and microwave spectra and morphology. Although the event overall appears to correspond to the standard scenario with magnetic reconnection under an eruptive filament, several of its features do not seem to be consistent with popular flare models. In particular we find that (1) microwave emissions might be optically thick at high frequencies despite a low peak frequency in the total flux radio spectrum, presumably due to the inhomogeneity of the emitting source; (2) magnetic fields in high-frequency radio sources might be stronger than sometimes assumed; (3) sources spread over a very large volume can show matching evolution in their hard X-ray spectra that may provide a challenge to acceleration models. Our results emphasize the importance of studies of sunspot-associated flares and total flux measurements of radio bursts in the millimeter range. C1 [Grechnev, V. V.; Meshalkina, N. S.; Kashapova, L. K.] Inst Solar Terr Phys, Irkutsk 664033, Russia. [Kundu, M. R.; White, S. M.; Schmahl, E. J.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Schmahl, E. J.] NASA, Goddard Space Flight Ctr, Astron & Solar Phys Lab, Greenbelt, MD 20771 USA. RP Grechnev, VV (reprint author), Inst Solar Terr Phys, Irkutsk 664033, Russia. EM kundu@astro.umd.edu; grechnev@iszf.irk.ru; white@astro.umd.edu; ed@astro.umd.edu FU NSF [ATM 02-33907]; NASA [NAG 5-12860, NNG05-GI-91G, NAG 510180, NNG06-GB-636]; Russian Foundation [07-02-00101] FX The research of MRK and SMW for this paper was supported by NSF grant ATM 02-33907 and NASA grants NAG 5-12860 and NNG05-GI-91G. The research of EJS was supported by NASA grants NAG 510180 and NNG06-GB-636. The research of VVG and NSM was supported by the Russian Foundation of Basic Research under grant 07-02-00101. NR 33 TC 21 Z9 22 U1 0 U2 1 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-0938 J9 SOL PHYS JI Sol. Phys. PD NOV PY 2009 VL 260 IS 1 BP 135 EP 156 DI 10.1007/s11207-009-9437-3 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 521YP UT WOS:000271962900009 ER PT J AU Trudel, M Fisher, J Orsi, JA Morris, JFT Thiess, ME Sweeting, RM Hinton, S Fergusson, EA Welch, DW AF Trudel, M. Fisher, J. Orsi, J. A. Morris, J. F. T. Thiess, M. E. Sweeting, R. M. Hinton, S. Fergusson, E. A. Welch, D. W. TI Distribution and Migration of Juvenile Chinook Salmon Derived from Coded Wire Tag Recoveries along the Continental Shelf of Western North America SO TRANSACTIONS OF THE AMERICAN FISHERIES SOCIETY LA English DT Article ID CALIFORNIA CURRENT SYSTEM; ONCORHYNCHUS-TSHAWYTSCHA; COHO SALMON; BRITISH-COLUMBIA; PACIFIC SALMON; LIFE-HISTORY; SNAKE RIVER; POPULATION-STRUCTURE; SOUTHEASTERN ALASKA; MARINE DISTRIBUTION AB The effects of ocean conditions on highly migratory species such as salmon are difficult to assess owing to the diversity of environments they encounter during their marine life. In this study, we reconstructed the initial ocean migration routes of juvenile Chinook salmon Oncorhynchus tshawytscha originating from Oregon to Southeast Alaska using coded wire tag recovery data from Canadian Department of Fisheries and Oceans and National Marine Fisheries Service research surveys conducted between 1995 and 2006. Over this 12-year period, 1,862 coded-wire-tagged juvenile Chinook salmon were recovered along the coasts of Oregon, Washington, British Columbia, and Alaska from March to November. Except for those from the Columbia River, most juvenile Chinook salmon remained within 100-200 km of their natal rivers until their second year at sea, irrespective of their freshwater history and adult run timing. Northward migration of most coastal stocks was initiated during their second or possibly third year at sea, whereas the Strait of Georgia and Puget Sound stocks primarily migrated onto the continental shelf after their first year at sea. In contrast, Columbia River Chinook salmon generally undertook a rapid northward migration that varied among life histories and stocks. Columbia River spring Chinook salmon were recovered as far north as Prince William Sound, Alaska, during their first summer at sea, whereas very few Columbia River fall Chinook salmon were recovered north of Vancouver Island. In addition to northern migrants, a fraction of the Columbia River spring and fall Chinook salmon actively migrated south of the Columbia River. The stock-specific initial ocean migration routes described in this study will aid in the identification of the appropriate spatial and temporal scales for assessing the processes regulating Chinook salmon recruitment in the marine environment. C1 [Trudel, M.; Morris, J. F. T.; Thiess, M. E.; Sweeting, R. M.; Welch, D. W.] Fisheries & Oceans Canada, Pacific Biol Stn, Nanaimo, BC V9T 6N7, Canada. [Trudel, M.] Univ Victoria, Dept Biol, Victoria, BC V8W 3N5, Canada. [Fisher, J.] Oregon State Univ, Coll Atmospher & Ocean Sci, Corvallis, OR 97331 USA. [Orsi, J. A.; Fergusson, E. A.] Natl Marine Fisheries Serv, Alaska Fisheries Sci Ctr, Auke Bay Labs, Juneau, AK 99801 USA. [Hinton, S.] Natl Marine Fisheries Serv, NW Fisheries Sci Ctr, Point Adams Field Stn, Hammond, OR 97121 USA. [Welch, D. W.] Univ Victoria, Sch Earth & Ocean Sci, Victoria, BC V8N 2Y2, Canada. RP Trudel, M (reprint author), Fisheries & Oceans Canada, Pacific Biol Stn, 3190 Hammond Bay Rd, Nanaimo, BC V9T 6N7, Canada. EM marc.trudel@dfo-mpo.gc.ca RI Trudel, Marc/H-1955-2012 FU Fisheries and Oceans Canada; NOAA Fisheries; Bonneville Power Administration; U.S. GLOBEC Northeast Pacific program FX We thank the crews of the Canadian Coast Guard ship W. E. Ricker, fishing vessels Frosti, Sea Eagle, and Viking Storm, and NOAA ships David Starr Jordan, John N. Cobb, and Miller Freeman, as well as the numerous technicians for their assistance with the field work and laboratory analysis. We also thank B. Beckman, D. Teel, S. Tucker, R. McNicol and L. Weitkamp for useful comments on earlier versions of this manuscript. Funding was provided by Fisheries and Oceans Canada, NOAA Fisheries, the Bonneville Power Administration, and the U.S. GLOBEC Northeast Pacific program. NR 60 TC 57 Z9 61 U1 3 U2 14 PU AMER FISHERIES SOC PI BETHESDA PA 5410 GROSVENOR LANE SUITE 110, BETHESDA, MD 20814-2199 USA SN 0002-8487 J9 T AM FISH SOC JI Trans. Am. Fish. Soc. PD NOV PY 2009 VL 138 IS 6 BP 1369 EP 1391 DI 10.1577/T08-181.1 PG 23 WC Fisheries SC Fisheries GA 589DC UT WOS:000277124500014 ER PT J AU Daly, EA Brodeur, RD Weitkamp, LA AF Daly, Elizabeth A. Brodeur, Richard D. Weitkamp, Laurie A. TI Ontogenetic Shifts in Diets of Juvenile and Subadult Coho and Chinook Salmon in Coastal Marine Waters: Important for Marine Survival? SO TRANSACTIONS OF THE AMERICAN FISHERIES SOCIETY LA English DT Article ID COLUMBIA RIVER PLUME; PACIFIC SALMON; ONCORHYNCHUS-KISUTCH; COMMUNITY STRUCTURE; OCEANOGRAPHIC CONDITIONS; CALIFORNIA CURRENT; NORTH-AMERICA; FISH LARVAE; FOOD-HABITS; WEST-COAST AB Successfully shifting to a more piscivorous diet may be an important factor in the growth and survival of juvenile coho salmon Oncorhynchus kisutch and Chinook salmon O. tshawytscha during their first summer in the northern California Current. Nonmetric multidimensional scaling and cluster analysis of diets by size showed several distinct groupings as the salmon grew during their first marine summer. These size-based diet differences were clearly driven by increased rates of piscivory for both species. Fish prey composition, feeding intensity, and fish prey-predator length ratios all significantly increased for coho salmon at approximately 240 mm fork length when they changed from diets dominated by juvenile rockfishes Sebastes spp., the larvae of crabs Cancer spp., and adult euphausiids to one of predominantly juvenile forage fish. As Chinook salmon grew, they gradually increased the proportional contribution (by weight) of fish prey in their diets-from 55% in the smallest length-class examined (80-100 mm) to 95% in the largest one (. 375 mm). Chinook salmon fed in the same marine environments as coho salmon and consistently ate more and longer fish prey at a given size than coho salmon but had lower overall feeding intensity, perhaps owing to a higher level of prey selection. Relating subsequent interannual adult salmon returns to juvenile diets showed mixed results. During lower-survival years, coho salmon ate fewer and smaller fish prey, while subyearling Chinook salmon had less total food and more empty stomachs. We did not find consistent trophic patterns for yearling Chinook salmon in relation to their ultimate survival. C1 [Daly, Elizabeth A.] Oregon State Univ, Hatfield Marine Sci Ctr, Cooperat Inst Marine Resources Studies, Newport, OR 97365 USA. [Brodeur, Richard D.; Weitkamp, Laurie A.] Oregon State Univ, Hatfield Marine Sci Ctr, NW Fisheries Sci Ctr, Natl Marine Fisheries Serv, Newport, OR 97365 USA. RP Daly, EA (reprint author), Oregon State Univ, Hatfield Marine Sci Ctr, Cooperat Inst Marine Resources Studies, Newport, OR 97365 USA. EM elizabeth.daly@noaa.gov FU Bonneville Power Administration; U.S. Global Ocean Ecosystems (GLOBEC) Northeast Pacific Program FX We thank the many National Oceanic and Atmospheric Administration and Oregon State University personnel who assisted in the field collections and laboratory dissections of the salmon. Jackie Noskov, Robert Schabetsberger, Carolyn Knight, and Rob Boley assisted with the analyses of the diets. Ed Casillas, Robert Emmett, Rebecca Baldwin, and three anonymous reviewers provided comments on earlier drafts of this manuscript. Many thanks to Cheryl Morgan for database management, and Susan Hinton for organizing our field collections. Funding was provided by the Bonneville Power Administration and the U.S. Global Ocean Ecosystems (GLOBEC) Northeast Pacific Program. This is contribution 636 of the U. S. GLOBEC Program. Reference to trade names does not imply endorsement by the U. S. Government. NR 48 TC 40 Z9 39 U1 1 U2 25 PU AMER FISHERIES SOC PI BETHESDA PA 5410 GROSVENOR LANE SUITE 110, BETHESDA, MD 20814-2199 USA SN 0002-8487 J9 T AM FISH SOC JI Trans. Am. Fish. Soc. PD NOV PY 2009 VL 138 IS 6 BP 1420 EP 1438 DI 10.1577/T08-226.1 PG 19 WC Fisheries SC Fisheries GA 589DC UT WOS:000277124500017 ER PT J AU Tucker, S Trudel, M Welch, DW Candy, JR Morris, JFT Thiess, ME Wallace, C Teel, DJ Crawford, W Farley, EV Beacham, TD AF Tucker, S. Trudel, M. Welch, D. W. Candy, J. R. Morris, J. F. T. Thiess, M. E. Wallace, C. Teel, D. J. Crawford, W. Farley, E. V., Jr. Beacham, T. D. TI Seasonal Stock-Specific Migrations of Juvenile Sockeye Salmon along the West Coast of North America: Implications for Growth SO TRANSACTIONS OF THE AMERICAN FISHERIES SOCIETY LA English DT Article ID HISTOCOMPATIBILITY COMPLEX VARIATION; ONCORHYNCHUS-NERKA SMOLTS; PACIFIC-SALMON; BRITISH-COLUMBIA; COHO SALMON; CHINOOK SALMON; CONTINENTAL-SHELF; SOUTHEAST ALASKA; SURVIVAL RATES; FRASER-RIVER AB Knowledge of the migratory habits of juvenile Pacific salmon Oncorhynchus spp. is required to test the hypothesis that ocean food resources are a limiting factor in their production. Using DNA stock identification techniques, we reconstructed the regional and seasonal changes in the stock composition of juvenile sockeye salmon O. nerka (n = 4,062) collected from coastal Washington to the Alaska Peninsula in coastal trawl surveys from May to February 1996-2007. Individuals were allocated to 14 regional populations. The majority were allocated to stocks from the Fraser River system (42%), while west coast Vancouver Island stocks accounted for 15% of the total catch; Nass and Skeena River sockeye salmon constituted 14% and Rivers Inlet 6% of the total. The remainder of the stocks identified individually contributed less than 5% of the sockeye salmon analyzed. These proportions generally reflected the abundance of those populations. In spring and summer, the majority of fish were caught in close proximity to their rivers of origin, lending further support to the allocations. By fall, sockeye salmon were caught as far north and west as the Alaska Peninsula, the majority being caught from central British Columbia to Southeast Alaska. Juvenile sockeye salmon generally disappeared from the coast by winter, suggesting dispersion into the Gulf of Alaska. Within each region, the proportional stock composition changed as the seasons progressed, with northward (and in some cases, rapid) migration along the coast. We also demonstrated stock-specific differences in migration patterns. For each stock identified, body size and energy density were higher at northern latitudes, suggesting that there is an environmental or food web influence on growth or that faster growing fish initiated their northward migration earlier. C1 [Tucker, S.; Trudel, M.; Welch, D. W.; Candy, J. R.; Morris, J. F. T.; Thiess, M. E.; Wallace, C.; Beacham, T. D.] Fisheries & Oceans Canada, Pacific Biol Stn, Nanaimo, BC V9T 6N7, Canada. [Trudel, M.] Univ Victoria, Dept Biol, Victoria, BC V8W 3N5, Canada. [Teel, D. J.] NOAA Fisheries, NW Fisheries Sci Ctr, Manchester Res Lab, Manchester, WA 98353 USA. [Crawford, W.] Fisheries & Oceans Canada, Inst Ocean Sci, Sidney, BC V8L 4B2, Canada. [Farley, E. V., Jr.] Natl Marine Fisheries Serv, Auke Bay Lab, Juneau, AK 99801 USA. RP Tucker, S (reprint author), Fisheries & Oceans Canada, Pacific Biol Stn, 3190 Hammond Bay Rd, Nanaimo, BC V9T 6N7, Canada. EM strahan.tucker@dfo-mpo.gc.ca RI Trudel, Marc/H-1955-2012 FU Bonneville Power Administration; Fisheries and Oceans Canada; World Wildlife Fund; Department of Fisheries and Oceans FX We thank the crews of CCGS W. E. Ricker, FV Ocean Selector, and FV Frosti, numerous scientists, and technicians for their assistance with the field work and laboratory analysis and the Bonneville Power Administration, Fisheries and Oceans Canada, and the World Wildlife Fund for their financial support. We also thank Sue Grant from the Department of Fisheries and Oceans for providing information on stock sizes. NR 57 TC 42 Z9 44 U1 3 U2 30 PU AMER FISHERIES SOC PI BETHESDA PA 5410 GROSVENOR LANE SUITE 110, BETHESDA, MD 20814-2199 USA SN 0002-8487 J9 T AM FISH SOC JI Trans. Am. Fish. Soc. PD NOV PY 2009 VL 138 IS 6 BP 1458 EP 1480 DI 10.1577/T08-211.1 PG 23 WC Fisheries SC Fisheries GA 589DC UT WOS:000277124500019 ER PT J AU DellaCorte, C AF DellaCorte, Christopher TI Superconductivity and 'frictionless' systems SO TRIBOLOGY & LUBRICATION TECHNOLOGY LA English DT Letter C1 NASA, Glenn Res Ctr, Cleveland, OH USA. RP DellaCorte, C (reprint author), NASA, Glenn Res Ctr, Cleveland, OH USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU SOC TRIBOLOGISTS & LUBRICATION ENGINEERS PI PARK RIDGE PA 840 BUSSE HIGHWAY, PARK RIDGE, IL 60068 USA SN 1545-858X J9 TRIBOL LUBR TECHNOL JI Tribol. Lubr. Technol. PD NOV PY 2009 VL 65 IS 11 BP 7 EP 7 PG 1 WC Engineering, Mechanical SC Engineering GA 520VC UT WOS:000271876600003 ER PT J AU Righter, K Pando, K Danielson, LR AF Righter, K. Pando, K. Danielson, L. R. TI Experimental evidence for sulfur-rich martian magmas: Implications for volcanism and surficial sulfur sources SO EARTH AND PLANETARY SCIENCE LETTERS LA English DT Article DE sulfur; basalt; magma; sulfate; Mars ID OXYGEN FUGACITY; SILICATE MELTS; SULFIDE SATURATION; MAFIC MAGMAS; HYDROTHERMAL ALTERATION; ACHONDRITIC METEORITES; EMPIRICAL EQUATIONS; OMEGA/MARS EXPRESS; MERIDIANI-PLANUM; SNC METEORITES AB It has been proposed that sulfur outgassing by volcanism on Mars contributes to the sulfur budget and volatile cycle at and near the surface (Farquhar et al., 2000; Halevy et al., 2007). However, it remains unclear if shergottites and martian magmas are sulfide saturated or under-saturated and therefore how much sulfur, they can contribute via volcanism. Expressions derived from experimental studies allow prediction of S contents, though they are not calibrated for shergottitic liquids, which are FeO-rich and Al(2)O(3)-Poor compared to the terrestrial experimental dataset upon which the models have been based. We have carried out new experiments designed to test current S saturation models, and then show that existing calibrations are not suitable for high FeO and low Al(2)O(3) Compositions characteristic of shergottitic liquids. The new results show that existing models either under-predict by a factor of 2, or over-predict by a factor of 2-3, the S contents of sulfide saturated shergottitic liquids. Primitive shergottite magmas are capable of dissolving no more than similar to 4000 ppm S at sulfide saturation. Melting of the martian mantle, and subsequent volcanism provides more than enough sulfur for the sulfate-rich soil and layered deposits recognized on the surface of Mars. Published by Elsevier B.V. C1 [Righter, K.; Pando, K.] NASA, Lyndon B Johnson Space Ctr, ESCG Hamilton Sunstrund, Houston, TX 77058 USA. [Danielson, L. R.] NASA, Lyndon B Johnson Space Ctr, ESCG Jacobs Technol, Houston, TX 77058 USA. RP Righter, K (reprint author), NASA, Lyndon B Johnson Space Ctr, ESCG Hamilton Sunstrund, 2101 NASA Pkwy, Houston, TX 77058 USA. EM kevin.righter-1@nasa.gov FU NASA Mars Fundamental Research program FX This research is supported by a grant to KR from the NASA Mars Fundamental Research program. We thank L. Le and A. Peslier for assistance with the electron microprobe. We also thank K. Edgett, H. Newsom, and P. Wallace for discussions about aspects of this work. Reviews by C. Li and an anonymous reviewer led to improvements to the presentation. NR 77 TC 39 Z9 39 U1 1 U2 18 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0012-821X J9 EARTH PLANET SC LETT JI Earth Planet. Sci. Lett. PD OCT 30 PY 2009 VL 288 IS 1-2 BP 235 EP 243 DI 10.1016/j.epsl.2009.09.027 PG 9 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 532YX UT WOS:000272788500024 ER PT J AU Egbert, GD Erofeeva, SY Han, SC Luthcke, SB Ray, RD AF Egbert, G. D. Erofeeva, S. Y. Han, S. -C. Luthcke, S. B. Ray, R. D. TI Assimilation of GRACE tide solutions into a numerical hydrodynamic inverse model SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID GLOBAL OCEAN; SYSTEM; EARTH AB We assimilate localized mass anomalies inferred from GRACE ranging measurements into a hydrodynamic model to improve tidal solutions around Antarctica for the M-2, S-2, and O-1 constituents. The variational approach used accounts for the spatial averaging of tidal elevations implicit in the mass anomaly parametrization used for the GRACE tidal analysis, as well as spatial correlation of errors in the resulting estimates. The inverse solution shows better agreement with independent station tide measurements around Antarctica, and it reduces cross-over residuals for ICESat laser altimeter data over the Filchner, Ronne and Ross Ice Shelves, demonstrating that GRACE data can provide useful constraints for improving hydrodynamic tidal models at high latitudes. Citation: Egbert, G. D., S. Y. Erofeeva, S.-C. Han, S. B. Luthcke, and R. D. Ray (2009), Assimilation of GRACE tide solutions into a numerical hydrodynamic inverse model, Geophys. Res. Lett., 36, L20609, doi: 10.1029/2009GL040376. C1 [Egbert, G. D.; Erofeeva, S. Y.] Oregon State Univ, Coll Ocean & Atmospher Sci, Corvallis, OR 97331 USA. [Han, S. -C.; Luthcke, S. B.; Ray, R. D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Han, S. -C.] Univ Maryland Baltimore Cty, GEST, Baltimore, MD 21228 USA. RP Egbert, GD (reprint author), Oregon State Univ, Coll Ocean & Atmospher Sci, 104 COAS Admin Bldg, Corvallis, OR 97331 USA. EM egbert@coas.oregonstate.edu; richard.ray@nasa.gov RI Ray, Richard/D-1034-2012; Luthcke, Scott/D-6283-2012; Han, Shin-Chan/A-2022-2009; OI Egbert, Gary/0000-0003-1276-8538 FU National Aeronautics and Space Administration's GRACE; International Polar Year projects FX We thank D. Rowlands and J.-P. Boy for help with processing of GRACE data. This work was supported by the National Aeronautics and Space Administration's GRACE and International Polar Year projects. NR 19 TC 11 Z9 11 U1 0 U2 5 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD OCT 30 PY 2009 VL 36 AR L20609 DI 10.1029/2009GL040376 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 513HW UT WOS:000271314300002 ER PT J AU Lee, JN Wu, DL Manney, GL Schwartz, MJ AF Lee, Jae N. Wu, Dong L. Manney, Gloria L. Schwartz, Michael J. TI Aura Microwave Limb Sounder observations of the Northern Annular Mode: From the mesosphere to the upper troposphere SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID ARCTIC OSCILLATION; PART I; VARIABILITY; STRATOSPHERE; CIRCULATION; HEMISPHERE; TRANSPORT; CLIMATE; MIDDLE AB Vertical structure and evolution of the wintertime Northern Hemisphere Annular Mode (NAM), the first Empirical Orthogonal Function (EOF) of geopotential height anomalies, are constructed from the 2005-2009 Aura Microwave Limb Sounder (MLS) measurements in the entire middle atmosphere between 316 hPa (similar to 9 km) and 0.001 hPa (similar to 90 km). This is the first report of NAM structure extending into the mesosphere. The mode appears to be robust and it accounts for up to 70% of middle-atmospheric variance before decreasing in the upper mesosphere. The vertical connection of the NAM modes suggests strong dynamic coupling between the mesosphere and stratosphere. Time evolution of the NAM suggests that the significant NAM anomalies typically appear first in the mesosphere and progress downward. NAM patterns derived from MLS observations are consistent with those derived from long-term reanalysis below the middle stratosphere. The NAM indexes show the mesospheric cooling signals during the major stratospheric sudden warmings (SSWs) in 2006 and 2009. Citation: Lee, J. N., D. L. Wu, G. L. Manney, and M. J. Schwartz (2009), Aura Microwave Limb Sounder observations of the Northern Annular Mode: From the mesosphere to the upper troposphere, Geophys. Res. Lett., 36, L20807, doi: 10.1029/2009GL040678. C1 [Lee, Jae N.; Wu, Dong L.; Manney, Gloria L.; Schwartz, Michael J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Manney, Gloria L.] New Mexico Inst Min & Technol, Socorro, NM 87801 USA. RP Lee, JN (reprint author), CALTECH, Jet Prop Lab, MS 169-237,4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM jae.nyung.lee@jpl.nasa.gov RI Schwartz, Michael/F-5172-2016; Wu, Dong/D-5375-2012 OI Schwartz, Michael/0000-0001-6169-5094; FU NASA FX We thank the MLS Science Team for their continuing support, especially Jung H. Chae, and Robert P. Thurstans. We also thank to Kirstin Kruger, Varavut Limpasuvan, Alexander Ruzmaikin, Joan Feynman for inspiring discussions and two anonymous reviewers for suggestions and comments that have lead to significant improvements of the paper. 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. Research at the Jet Propulsion Laboratory, California Institute of Technology, is done under contract with the National Aeronautics and Space Administration. NR 33 TC 14 Z9 15 U1 1 U2 5 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD OCT 30 PY 2009 VL 36 AR L20807 DI 10.1029/2009GL040678 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 513HW UT WOS:000271314300007 ER PT J AU Jiang, JH Su, H Massie, ST Colarco, PR Schoeberl, MR Platnick, S AF Jiang, Jonathan H. Su, Hui Massie, Steven T. Colarco, Peter R. Schoeberl, Mark R. Platnick, Steven TI Aerosol-CO relationship and aerosol effect on ice cloud particle size: Analyses from Aura Microwave Limb Sounder and Aqua Moderate Resolution Imaging Spectroradiometer observations SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID MODIS; VALIDATION; PRODUCTS; AFRICA AB We examine the relation between Aqua Moderate Resolution Imaging Spectroradiometer (MODIS) aerosol optical thickness (AOT) and Aura Microwave Limb Sounder upper tropospheric (UT) carbon monoxide (CO) to address when CO can be used as a proxy for aerosols. Ice cloud effective radii (r(e)), also from Aqua MODIS, are also analyzed to investigate possible aerosol effects on ice clouds. Our analysis focuses on five regions where ice clouds are collocated with high UT CO loadings: South America (SAM), southern Africa (SAF), northern Africa (NAF), South Asia (SAS), and East Asia (EAS). We find three levels of AOT to CO sensitivity. High AOT sensitivity to CO is characterized by a rapid increase of AOT when CO increases. SAM in August-November and SAF in June September fall into this category. Moderate AOT sensitivity to CO is characterized by moderate increase of AOT with CO. It includes SAF in October-May, NAF in January March, SAS in all months, and EAS in August-September. The other months for each region fall into the low sensitivity category. The variations of sensitivity in different regions and seasons result from different emission sources coupled with dynamic influence. CO can be used as an aerosol proxy for the "high'' and "moderate'' sensitivity cases. During those times, r(e) for polluted clouds is smaller than that for clean clouds, suggesting an indirect effect of aerosol on ice clouds. CO is not a good aerosol index in the low sensitivity cases, in which polluted clouds defined by CO loadings do not show significant differences from clean clouds in r(e). C1 [Jiang, Jonathan H.; Su, Hui] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Colarco, Peter R.; Schoeberl, Mark R.; Platnick, Steven] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Massie, Steven T.] Natl Ctr Atmospher Res, Boulder, CO 80307 USA. RP Jiang, JH (reprint author), CALTECH, Jet Prop Lab, Mail Stop 183-701,4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM jonathan.h.jiang@jpl.nasa.gov RI Platnick, Steven/J-9982-2014; Colarco, Peter/D-8637-2012 OI Platnick, Steven/0000-0003-3964-3567; Colarco, Peter/0000-0003-3525-1662 FU NASA [ROSES05 ACMAP, ROSES06-IDS]; National Science Foundation FX We thank the NASA ROSES05 ACMAP and ROSES06-IDS programs for support. The work was conducted jointly at the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA; at the National Center for Atmospheric Research, supported by the National Science Foundation; and at the NASA Goddard Space Flight Center. NR 23 TC 14 Z9 14 U1 0 U2 8 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD OCT 30 PY 2009 VL 114 AR D20207 DI 10.1029/2009JD012421 PG 8 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 513JJ UT WOS:000271318200006 ER PT J AU Leone, G Davies, AG Wilson, L Williams, DA Keszthelyi, LP Jaeger, WL Turtle, EP AF Leone, Giovanni Davies, Ashley Gerard Wilson, Lionel Williams, David A. Keszthelyi, Laszlo P. Jaeger, Windy L. Turtle, Elizabeth P. TI Volcanic history, geologic analysis and map of the Prometheus Patera region on Io SO JOURNAL OF VOLCANOLOGY AND GEOTHERMAL RESEARCH LA English DT Article DE Io; Prometheus; volcano; geology; tectonics ID INFRARED MAPPING SPECTROMETER; GALILEO OBSERVATIONS; MAGMA; ERUPTION; NIMS; LITHOSPHERE; MOUNTAINS; SSI; CONSTRAINTS; TEMPERATURE AB Data from Jupiter's moon Io returned by the Galileo spacecraft have been used to create a geologic map of Prometheus Patera, its associated flow field, and nearby features. We have identified the location of the vent that fed the Prometheus flow field during the Galileo epoch in the north-eastern portion of the main Prometheus flow field. This vent is the probable source of a small sulphur-rich plume. Previous studies suggested that the vent may be atop a tectonic fault but we find that the vent is offset from the putative fault. It is plausible that, in the past, magma exploited the fault to reach the surface at Prometheus Patera, but subsequent magma cooling in the conduit could have caused an obstruction preventing further eruptions from providing significant contributions to the Prometheus flow field. We also speculate on how a new Prometheus plumbing system may be fed by mafic magmas after melt stalls in magma reservoirs during its ascent through the lithosphere from the mantle. (C) 2009 Elsevier B.V. All rights reserved. C1 [Leone, Giovanni; Wilson, Lionel] Univ Lancaster, Lancaster Environm Ctr, Lancaster LA1 4YQ, England. [Davies, Ashley Gerard] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Williams, David A.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [Keszthelyi, Laszlo P.; Jaeger, Windy L.] US Geol Survey, Astrogeol Team, Flagstaff, AZ 86001 USA. [Turtle, Elizabeth P.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. RP Leone, G (reprint author), Univ Lancaster, Lancaster Environm Ctr, Lancaster LA1 4YQ, England. EM g.leone@lancaster.ac.uk RI Turtle, Elizabeth/K-8673-2012 OI Turtle, Elizabeth/0000-0003-1423-5751 FU NASA FX Part of this work was carried out at the jet Propulsion Laboratory-California Institute of Technology, under contract to NASA. We gratefully acknowledge the support of the NASA Planetary Geology and Geophysics Program and Outer Planets Research Program. Giovanni Leone thanks Bob Pappalardo for a travel grant contribution to work at JPL The authors thank Jani Radebaugh and Paul Geissler for their reviews of the manuscript. NR 67 TC 9 Z9 9 U1 0 U2 4 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0377-0273 J9 J VOLCANOL GEOTH RES JI J. Volcanol. Geotherm. Res. PD OCT 30 PY 2009 VL 187 IS 1-2 BP 93 EP 105 DI 10.1016/j.jvolgeores.2009.07.019 PG 13 WC Geosciences, Multidisciplinary SC Geology GA 516KG UT WOS:000271540400008 ER PT J AU Arneth, A Unger, N Kulmala, M Andreae, MO AF Arneth, Almut Unger, Nadine Kulmala, Markku Andreae, Meinrat O. TI Clean the Air, Heat the Planet? SO SCIENCE LA English DT Editorial Material ID CLIMATE; POLLUTION; AEROSOLS C1 [Arneth, Almut] Lund Univ, Dept Phys Geog & Ecosyst Anal, S-22362 Lund, Sweden. [Arneth, Almut; Kulmala, Markku] Univ Helsinki, Dept Phys, FIN-00014 Helsinki, Finland. [Unger, Nadine] Columbia Univ, Ctr Climate Syst Res, NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Andreae, Meinrat O.] Max Planck Inst Chem, Biogeochem Dept, D-55020 Mainz, Germany. RP Arneth, A (reprint author), Lund Univ, Dept Phys Geog & Ecosyst Anal, S-22362 Lund, Sweden. EM almut.arneth@nateko.lu.se RI Arneth, Almut/B-2702-2013; Unger, Nadine/M-9360-2015; Kulmala, Markku/I-7671-2016; Andreae, Meinrat/B-1068-2008 OI Kulmala, Markku/0000-0003-3464-7825; Andreae, Meinrat/0000-0003-1968-7925 NR 20 TC 55 Z9 56 U1 4 U2 44 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 EI 1095-9203 J9 SCIENCE JI Science PD OCT 30 PY 2009 VL 326 IS 5953 BP 672 EP 673 DI 10.1126/science.1181568 PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 512GB UT WOS:000271233200019 PM 19900919 ER PT J AU Shindell, DT Faluvegi, G Koch, DM Schmidt, GA Unger, N Bauer, SE AF Shindell, Drew T. Faluvegi, Greg Koch, Dorothy M. Schmidt, Gavin A. Unger, Nadine Bauer, Susanne E. TI Improved Attribution of Climate Forcing to Emissions SO SCIENCE LA English DT Article ID LAND-CARBON SINK; TROPOSPHERIC OZONE; AIR-QUALITY; WARMING POTENTIALS; REGIONAL EMISSIONS; AEROSOLS; IMPACT; PREINDUSTRIAL; AGREEMENTS; PRECURSORS AB Evaluating multicomponent climate change mitigation strategies requires knowledge of the diverse direct and indirect effects of emissions. Methane, ozone, and aerosols are linked through atmospheric chemistry so that emissions of a single pollutant can affect several species. We calculated atmospheric composition changes, historical radiative forcing, and forcing per unit of emission due to aerosol and tropospheric ozone precursor emissions in a coupled composition-climate model. We found that gas-aerosol interactions substantially alter the relative importance of the various emissions. In particular, methane emissions have a larger impact than that used in current carbon-trading schemes or in the Kyoto Protocol. Thus, assessments of multigas mitigation policies, as well as any separate efforts to mitigate warming from short-lived pollutants, should include gas-aerosol interactions. C1 [Shindell, Drew T.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. Columbia Univ, New York, NY 10025 USA. RP Shindell, DT (reprint author), NASA, Goddard Inst Space Studies, New York, NY 10025 USA. EM drew.t.shindell@nasa.gov RI Shindell, Drew/D-4636-2012; Schmidt, Gavin/D-4427-2012; Bauer, Susanne/P-3082-2014; Unger, Nadine/M-9360-2015 OI Schmidt, Gavin/0000-0002-2258-0486; FU NASA FX We thank the NASA Atmospheric Chemistry Modeling and Analysis Program for supporting this work. NR 30 TC 322 Z9 334 U1 13 U2 188 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 EI 1095-9203 J9 SCIENCE JI Science PD OCT 30 PY 2009 VL 326 IS 5953 BP 716 EP 718 DI 10.1126/science.1174760 PG 3 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 512GB UT WOS:000271233200034 PM 19900930 ER PT J AU Huang, XC Schwenke, DW Lee, TJ AF Huang, Xinchuan Schwenke, David W. Lee, Timothy J. TI An Approach to Include the Effects of Diffuse Functions in Potential Energy Surface Calculations SO JOURNAL OF PHYSICAL CHEMISTRY A LA English DT Article ID ANHARMONIC-FORCE FIELD; BASIS-SET CONVERGENCE; VIBRATIONAL FREQUENCIES; CO2 AB A new approach is proposed and investigated for approximately including the effects of diffuse functions in one-particle basis sets when high accuracy is desired. The method is cost-effective for use in computing quartic force fields (QFFs), global potential energy surfaces (PESs), or other situations when a large part of the PES is needed. It is conservatively estimated that the use of this approximation leads to a computational savings of a factor of five, and it is argued that this could be significantly larger if input/output wait times are considered. It can be used when extrapolation to the one-particle basis set limit is performed, or it can be used simply to approximate the effect of diffuse functions for a larger basis set. The new approach is based on scaling the diffuse function effect for a smaller basis set to approximate the effect for a larger basis or an extrapolated energy in which larger basis set(s) are used. The scale factor is written as a function of the geometrical coordinates of the molecule and thus it includes a geometry dependence. We report results where the scale factor is a constant, includes through gradient terms, includes through second derivative terms, and includes through diagonal second and third derivative terms. The method has been tested in the calculation of accurate QFFs, equilibrium structures, and harmonic and fundamental vibrational frequencies for NH(2)(-), OH(-), H(2)O, and CH(3)OH. It is found that including up through diagonal second derivative terms leads to reliable fundamental vibrational frequencies and is cost-effective. It is also concluded that the use of a 5Z-quality basis set is essential if high accuracy is desired for these properties, even with extrapolation to the one-particle basis set limit. C1 [Huang, Xinchuan; Schwenke, David W.; Lee, Timothy J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Lee, TJ (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM Timothy.J.Lee@nasa.gov RI HUANG, XINCHUAN/A-3266-2013; Lee, Timothy/K-2838-2012; schwenke, david/I-3564-2013 FU NASA [PID 1022, PID 40645] FX We gratefully acknowledge support from the NASA Herschel GO Program, Cycle 0 TR/LA PID 1022, and the NASA Spitzer GO Program, Cycle 4, AR-4 Science Program PID 40645. X.H. acknowledges the support by an appointment to the NASA Postdoctoral Program at the Ames Research Center, administered by Oak Ridge Associated Universities through a contract with NASA. NR 24 TC 6 Z9 6 U1 0 U2 5 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 1089-5639 J9 J PHYS CHEM A JI J. Phys. Chem. A PD OCT 29 PY 2009 VL 113 IS 43 BP 11954 EP 11962 DI 10.1021/jp9036364 PG 9 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 508EO UT WOS:000270911400056 PM 19702284 ER PT J AU Tanvir, NR Fox, DB Levan, AJ Berger, E Wiersema, K Fynbo, JPU Cucchiara, A Kruhler, T Gehrels, N Bloom, JS Greiner, J Evans, PA Rol, E Olivares, F Hjorth, J Jakobsson, P Farihi, J Willingale, R Starling, RLC Cenko, SB Perley, D Maund, JR Duke, J Wijers, RAMJ Adamson, AJ Allan, A Bremer, MN Burrows, DN Castro-Tirado, AJ Cavanagh, B Postigo, AD Dopita, MA Fatkhullin, TA Fruchter, AS Foley, RJ Gorosabel, J Kennea, J Kerr, T Klose, S Krimm, HA Komarova, VN Kulkarni, SR Moskvitin, AS Mundell, CG Naylor, T Page, K Penprase, BE Perri, M Podsiadlowski, P Roth, K Rutledge, RE Sakamoto, T Schady, P Schmidt, BP Soderberg, AM Sollerman, J Stephens, AW Stratta, G Ukwatta, TN Watson, D Westra, E Wold, T Wolf, C AF Tanvir, N. R. Fox, D. B. Levan, A. J. Berger, E. Wiersema, K. Fynbo, J. P. U. Cucchiara, A. Kruehler, T. Gehrels, N. Bloom, J. S. Greiner, J. Evans, P. A. Rol, E. Olivares, F. Hjorth, J. Jakobsson, P. Farihi, J. Willingale, R. Starling, R. L. C. Cenko, S. B. Perley, D. Maund, J. R. Duke, J. Wijers, R. A. M. J. Adamson, A. J. Allan, A. Bremer, M. N. Burrows, D. N. Castro-Tirado, A. J. Cavanagh, B. de Ugarte Postigo, A. Dopita, M. A. Fatkhullin, T. A. Fruchter, A. S. Foley, R. J. Gorosabel, J. Kennea, J. Kerr, T. Klose, S. Krimm, H. A. Komarova, V. N. Kulkarni, S. R. Moskvitin, A. S. Mundell, C. G. Naylor, T. Page, K. Penprase, B. E. Perri, M. Podsiadlowski, P. Roth, K. Rutledge, R. E. Sakamoto, T. Schady, P. Schmidt, B. P. Soderberg, A. M. Sollerman, J. Stephens, A. W. Stratta, G. Ukwatta, T. N. Watson, D. Westra, E. Wold, T. Wolf, C. TI A gamma-ray burst at a redshift of z approximate to 8.2 SO NATURE LA English DT Article ID REIONIZATION; AFTERGLOW; SWIFT; EVOLUTION; FRACTION; UNIVERSE; GALAXY; PROBE; GRBS AB Long-duration gamma-ray bursts (GRBs) are thought to result from the explosions of certain massive stars(1), and some are bright enough that they should be observable out to redshifts of z > 20 using current technology(2-4). Hitherto, the highest redshift measured for any object was z = 6.96, for a Lyman-alpha emitting galaxy(5). Here we report that GRB 090423 lies at a redshift of z approximate to 8.2, implying that massive stars were being produced and dying as GRBs similar to 630 Myr after the Big Bang. The burst also pinpoints the location of its host galaxy. C1 [Tanvir, N. R.; Wiersema, K.; Evans, P. A.; Farihi, J.; Willingale, R.; Starling, R. L. C.; Duke, J.; Page, K.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Fox, D. B.; Cucchiara, A.; Burrows, D. N.; Kennea, J.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Levan, A. J.] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. [Berger, E.; Foley, R. J.; Soderberg, A. M.; Westra, E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Fynbo, J. P. U.; Hjorth, J.; Maund, J. R.; Sollerman, J.; Watson, D.] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen, Denmark. [Kruehler, T.; Greiner, J.; Olivares, F.] Max Planck Inst Extraterr Phys, D-85740 Garching, Germany. [Kruehler, T.] Tech Univ Munich, D-85748 Garching, Germany. [Gehrels, N.; Krimm, H. A.; Sakamoto, T.; Ukwatta, T. N.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Bloom, J. S.; Cenko, S. B.; Perley, D.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Rol, E.; Wijers, R. A. M. J.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1090 GE Amsterdam, Netherlands. [Jakobsson, P.] Univ Iceland, Inst Sci, Ctr Astrophys & Cosmol, IS-107 Reykjavik, Iceland. [Adamson, A. J.; Cavanagh, B.; Kerr, T.; Wold, T.] Joint Astron Ctr, Hilo, HI 96720 USA. [Allan, A.; Naylor, T.] Univ Exeter, Sch Phys, Exeter EX4 4QL, Devon, England. [Bremer, M. N.] Univ Bristol, HH Wills Phys Lab, Bristol BS8 1TL, Avon, England. [Castro-Tirado, A. J.; Gorosabel, J.] CSIC, Inst Astrofis Andalucia, E-18080 Granada, Spain. [de Ugarte Postigo, A.] European So Observ, Santiago 19, Chile. [Dopita, M. A.; Schmidt, B. P.] Australian Natl Univ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia. [Fatkhullin, T. A.; Komarova, V. N.; Moskvitin, A. S.] Special Astrophys Observ, Nizhnii Arkhyz 369167, Russia. [Fruchter, A. S.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Klose, S.] Thuringer Landessternwarte Tautenburg, D-07778 Tautenburg, Germany. [Krimm, H. A.; Sakamoto, T.] CRESST, Greenbelt, MD 20771 USA. [Krimm, H. A.] Univ Space Res Assoc, Columbia, MD 21044 USA. [Kulkarni, S. R.] CALTECH, Dept Astron, Pasadena, CA 91125 USA. [Mundell, C. G.] Liverpool John Moores Univ, Astrophys Res Inst, Birkenhead CH41 1LD, Merseyside, England. [Penprase, B. E.] Pomona Coll, Dept Phys & Astron, Claremont, CA 91711 USA. [Perri, M.; Stratta, G.] ASI Sci Data Ctr, I-00044 Frascati, Italy. [Podsiadlowski, P.; Wolf, C.] Univ Oxford, Dept Phys, Oxford OX1 3RH, England. [Roth, K.; Stephens, A. W.] Gemini Observ, Hilo, HI 96720 USA. [Rutledge, R. E.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Schady, P.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. [Sollerman, J.] Stockholm Univ, Dept Astron, Oskar Klein Ctr, S-10691 Stockholm, Sweden. [Ukwatta, T. N.] George Washington Univ, Washington, DC 20052 USA. RP Tanvir, NR (reprint author), Univ Leicester, Dept Phys & Astron, Univ Rd, Leicester LE1 7RH, Leics, England. EM nrt3@star.le.ac.uk RI Jakobsson, Pall/L-9950-2015; Stratta, Maria Giuliana/L-3045-2016; Gehrels, Neil/D-2971-2012; Fynbo, Johan/L-8496-2014; Hjorth, Jens/M-5787-2014; Dopita, Michael/P-5413-2014; Naylor, Tim /A-9465-2015; Watson, Darach/E-4521-2015 OI Jakobsson, Pall/0000-0002-9404-5650; Stratta, Maria Giuliana/0000-0003-1055-7980; Wijers, Ralph/0000-0002-3101-1808; Fynbo, Johan/0000-0002-8149-8298; Hjorth, Jens/0000-0002-4571-2306; Dopita, Michael/0000-0003-0922-4986; Watson, Darach/0000-0002-4465-8264 FU Clay Fellowship FX We thank Ph. Yock, B. Allen, P. Kubanek, M. Jelinek and S. Guziy for their assistance with the BOOTES-3 YA telescope observations (Supplementary Information). This work was partly 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 US National Science Foundation on behalf of the Gemini partnership: the National Science Foundation (United States), the Science and Technology Facilities Council (United Kingdom), the National Research Council (Canada), CONICYT (Chile), the Australian Research Council (Australia), the Ministerio da Ciencia e Tecnologia (Brazil) and SECYT (Argentina). This work was also partly based on observations made using ESO telescopes at the La Silla or Paranal observatories by G. Carraro, L. Schmidtobreick, G. Marconi, J. Smoker, V. Ivanov, E. Mason and M. Huertas-Company. The UKIRT is operated by the Joint Astronomy Centre on behalf of the UK Science and Technology Facilities Council. R. J. F. acknowledges a Clay Fellowship. NR 27 TC 353 Z9 357 U1 4 U2 20 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD OCT 29 PY 2009 VL 461 IS 7268 BP 1254 EP 1257 DI 10.1038/nature08459 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 511TF UT WOS:000271190800042 PM 19865165 ER PT J AU Salvaterra, R Della Valle, M Campana, S Chincarini, G Covino, S D'Avanzo, P Fernandez-Soto, A Guidorzi, C Mannucci, F Margutti, R Thoene, CC Antonelli, LA Barthelmy, SD De Pasquale, M D'Elia, V Fiore, F Fugazza, D Hunt, LK Maiorano, E Marinoni, S Marshall, FE Molinari, E Nousek, J Pian, E Racusin, JL Stella, L Amati, L Andreuzzi, G Cusumano, G Fenimore, EE Ferrero, P Giommi, P Guetta, D Holland, ST Hurley, K Israel, GL Mao, J Markwardt, CB Masetti, N Pagani, C Palazzi, E Palmer, DM Piranomonte, S Tagliaferri, G Testa, V AF Salvaterra, R. Della Valle, M. Campana, S. Chincarini, G. Covino, S. D'Avanzo, P. Fernandez-Soto, A. Guidorzi, C. Mannucci, F. Margutti, R. Thoene, C. C. Antonelli, L. A. Barthelmy, S. D. De Pasquale, M. D'Elia, V. Fiore, F. Fugazza, D. Hunt, L. K. Maiorano, E. Marinoni, S. Marshall, F. E. Molinari, E. Nousek, J. Pian, E. Racusin, J. L. Stella, L. Amati, L. Andreuzzi, G. Cusumano, G. Fenimore, E. E. Ferrero, P. Giommi, P. Guetta, D. Holland, S. T. Hurley, K. Israel, G. L. Mao, J. Markwardt, C. B. Masetti, N. Pagani, C. Palazzi, E. Palmer, D. M. Piranomonte, S. Tagliaferri, G. Testa, V. TI GRB 090423 at a redshift of z approximate to 8.1 SO NATURE LA English DT Article ID GAMMA-RAY BURSTS; REIONIZATION; ENVIRONMENTS; LUMINOSITY; EVOLUTION; GALAXIES; EPOCH; PROBE; MASS AB Gamma-ray bursts (GRBs) are produced by rare types of massive stellar explosion. Their rapidly fading afterglows are often bright enough at optical wavelengths that they are detectable at cosmological distances. Hitherto, the highest known redshift for a GRB was z = 6.7 (ref. 1), for GRB 080913, and for a galaxy was z = 6.96 (ref. 2). Here we report observations of GRB 090423 and the near-infrared spectroscopic measurement of its redshift, z = 8.1(-0.3)(+0.1). This burst happened when the Universe was only about 4 per cent of its current age(3). Its properties are similar to those of GRBs observed at low/intermediate redshifts, suggesting that the mechanisms and progenitors that gave rise to this burst about 600,000,000 years after the Big Bang are not markedly different from those producing GRBs about 10,000,000,000 years later. C1 [Salvaterra, R.; Campana, S.; Chincarini, G.; Covino, S.; D'Avanzo, P.; Margutti, R.; Thoene, C. C.; Fugazza, D.; Molinari, E.; Mao, J.; Tagliaferri, G.] Osserv Astron Brera, INAF, I-23807 Merate, LC, Italy. [Della Valle, M.] Osserv Astron Capodimonte, INAF, I-80131 Naples, Italy. [Della Valle, M.] European So Observ, D-85748 Garching, Germany. [Della Valle, M.] Int Ctr Relativist Astrophys, I-65122 Pescara, Italy. [Chincarini, G.; D'Avanzo, P.; Margutti, R.] Univ Milano Bicocca, Dipartimento Fis G Occhialini, I-20126 Milan, Italy. [Fernandez-Soto, A.] Univ Cantabria, CSIC, Inst Fis Cantabria, E-39005 Santander, Spain. [Guidorzi, C.] Univ Ferrara, Dipartimento Fis, I-44100 Ferrara, Italy. [Mannucci, F.; Hunt, L. K.] Osserv Astrofis Arcetri, INAF, I-50125 Florence, Italy. [Antonelli, L. A.; D'Elia, V.; Fiore, F.; Stella, L.; Guetta, D.; Israel, G. L.; Piranomonte, S.; Testa, V.] Osserv Astron Roma, INAF, I-00040 Monte Porzio Catone, Rome, Italy. [Barthelmy, S. D.; Marshall, F. E.; Holland, S. T.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [De Pasquale, M.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. [Maiorano, E.; Amati, L.; Masetti, N.; Palazzi, E.] IASF Bologna, INAF, I-40129 Bologna, Italy. [Marinoni, S.; Molinari, E.; Andreuzzi, G.] Fdn Galileo Galilei, INAF, Brena Baja 38712, TF, Spain. [Marinoni, S.] Univ Bologna, I-40127 Bologna, Italy. [Nousek, J.; Racusin, J. L.; Pagani, C.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Pian, E.] Trieste Astron Observ, INAF, I-34143 Trieste, Italy. [Pian, E.] Scuola Normale Super Pisa, I-56100 Pisa, Italy. [Cusumano, G.; Palmer, D. M.] Ist Astrofis Spaziale & Fis Cosm Palermo, INAF, I-90146 Palermo, Italy. [Fenimore, E. E.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA. [Ferrero, P.] Thuringer Landessternwarte Tautenburg, D-07778 Tautenburg, Germany. [Giommi, P.] ESRIN, ASDC, ASI Sci Data Ctr, I-00044 Frascati, Italy. [Holland, S. T.] Univ Space Res Assoc, Columbia, MD 21044 USA. [Holland, S. T.; Markwardt, C. B.] Ctr Res & Explorat Space Sci & Technol, Greenbelt, MD 20771 USA. [Hurley, K.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Markwardt, C. B.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. RP Salvaterra, R (reprint author), Osserv Astron Brera, INAF, Via E Bianchi 46, I-23807 Merate, LC, Italy. EM salvaterra@mib.infn.it RI Racusin, Judith/D-2935-2012; Barthelmy, Scott/D-2943-2012; Palazzi, Eliana/N-4746-2015; Fernandez-Soto, Alberto/A-2443-2009; Amati, Lorenzo/N-5586-2015; OI D'Elia, Valerio/0000-0002-7320-5862; Palazzi, Eliana/0000-0002-8691-7666; Salvaterra, Ruben/0000-0002-9393-8078; Della Valle, Massimo/0000-0003-3142-5020; Israel, GianLuca/0000-0001-5480-6438; Thone, Christina/0000-0002-7978-7648; Hunt, Leslie/0000-0001-9162-2371; Covino, Stefano/0000-0001-9078-5507; Masetti, Nicola/0000-0001-9487-7740; Tagliaferri, Gianpiero/0000-0003-0121-0723; Testa, Vincenzo/0000-0003-1033-1340; Pian, Elena/0000-0001-8646-4858; Antonelli, Lucio Angelo/0000-0002-5037-9034; Fiore, Fabrizio/0000-0002-4031-4157; giommi, paolo/0000-0002-2265-5003; Fernandez-Soto, Alberto/0000-0002-5732-3121; Molinari, Emilio/0000-0002-1742-7735; guetta, dafne/0000-0002-7349-1109; Amati, Lorenzo/0000-0001-5355-7388; Campana, Sergio/0000-0001-6278-1576; mannucci, filippo/0000-0002-4803-2381; Cusumano, Giancarlo/0000-0002-8151-1990 FU Agenzia Spaziale Italiana; Ministero dell'Universita e della Ricerca; Ministero degli Affari Esteri; NASA; US National Science Foundation FX We acknowledge the TNG staff for useful support during target-of-opportunity observations, in particular A. Fiorenzano, N. Sacchi and A. G. de Gurtubai Escudero. Wethank A. Ferrara for discussions. This research was supported by the Agenzia Spaziale Italiana, the Ministero dell'Universita e della Ricerca, the Ministero degli Affari Esteri, NASA and the US National Science Foundation. NR 29 TC 291 Z9 295 U1 1 U2 12 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD OCT 29 PY 2009 VL 461 IS 7268 BP 1258 EP 1260 DI 10.1038/nature08445 PG 3 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 511TF UT WOS:000271190800043 PM 19865166 ER PT J AU Poole, LR Pitts, MC Thomason, LW AF Poole, Lamont R. Pitts, Michael C. Thomason, Larry W. TI Comment on "A tropical 'NAT-like' belt observed from space" by H. Chepfer and V. Noel SO GEOPHYSICAL RESEARCH LETTERS LA English DT Editorial Material ID STRATOSPHERIC AEROSOLS; CONTAINING PARTICLES; CLOUDS; TROPOPAUSE C1 [Poole, Lamont R.] Sci Syst & Applicat Inc, Hampton, VA 23666 USA. [Pitts, Michael C.; Thomason, Larry W.] NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Poole, LR (reprint author), Sci Syst & Applicat Inc, Hampton, VA 23666 USA. EM lamont.r.poole@nasa.gov NR 12 TC 4 Z9 4 U1 0 U2 2 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD OCT 27 PY 2009 VL 36 AR L20803 DI 10.1029/2009GL038506 PG 2 WC Geosciences, Multidisciplinary SC Geology GA 513HQ UT WOS:000271313700001 ER PT J AU Hall, DK Nghiem, SV Schaaf, CB DiGirolamo, NE Neumann, G AF Hall, Dorothy K. Nghiem, Son V. Schaaf, Crystal B. DiGirolamo, Nicolo E. Neumann, Gregory TI Evaluation of surface and near-surface melt characteristics on the Greenland ice sheet using MODIS and QuikSCAT data SO JOURNAL OF GEOPHYSICAL RESEARCH-EARTH SURFACE LA English DT Article ID IN-SITU MEASUREMENTS; ACCURACY ASSESSMENT; MICROWAVE-FREQUENCIES; RADIATION PROPERTIES; DIELECTRIC-CONSTANT; ARCTIC SURFACE; ALBEDO PRODUCT; LAYERED MEDIA; RECENT TRENDS; MASS-LOSS AB The Greenland ice sheet has been the focus of much attention recently because of increasing melt in response to regional climate warming and can be studied using Moderate Resolution Imaging Spectroradiometer (MODIS) and Quick Scatterometer (QuikSCAT) data. To improve our ability to measure surface melt, we use remote sensing data products to study surface and near-surface melt characteristics of the Greenland ice sheet for the 2007 melt season when record melt extent and runoff occurred. MODIS daily land surface temperature (LST), MODIS daily snow albedo, and a special diurnal melt product derived from QuikSCAT (QS) scatterometer data, are all effective in measuring the evolution of melt on the ice sheet. These daily products, produced from different parts of the electromagnetic spectrum, are sensitive to different geophysical features, though QS- and MODIS-derived melt generally show excellent correspondence when surface melt is present. Values derived from the MODIS daily snow albedo product drop in response to melt and change with apparent grain size changes. For the 2007 melt season, the MODIS LST and QS products detect 766,184 km(2) +/- 8% and 862,769 km(2) +/- 3% of melt, respectively. The QS product detects about 11% greater melt extent than is detected by the MODIS LST product probably because QS is more sensitive to surface melt and can also see subsurface melt. The consistency of the response of the different products demonstrates unequivocally that physically meaningful melt/freeze boundaries are detected. We have demonstrated that when these products are used together we can improve the precision in mapping surface and near-surface melt extent on the Greenland ice sheet. C1 [Hall, Dorothy K.] NASA, Goddard Space Flight Ctr, Cryospher Sci Branch, Greenbelt, MD 20771 USA. [DiGirolamo, Nicolo E.] Sci Syst & Applicat Inc, Lanham, MD 20706 USA. [Nghiem, Son V.; Neumann, Gregory] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Schaaf, Crystal B.] Boston Univ, Dept Geog, Boston, MA 02215 USA. [Schaaf, Crystal B.] Boston Univ, Ctr Remote Sensing, Boston, MA 02215 USA. RP Hall, DK (reprint author), NASA, Goddard Space Flight Ctr, Cryospher Sci Branch, Code 614-1, Greenbelt, MD 20771 USA. EM dorothy.k.hall@nasa.gov RI Hall, Dorothy/D-5562-2012 FU NASA; Cryospheric Sciences Program FX The authors thank George Riggs at SSAI for discussions concerning the MODIS daily snow albedo product and comparisons with the MODIS BRDF/Albedo product. We also thank Zhengming Wan at University of California at Santa Barbara for many valuable discussions about the MODIS Land Surface Temperature product and its validation. We also thank one anonymous reviewer and Jason Box at Ohio State University and Thomas Mote at University of Georgia for their very helpful reviews. The work carried out at Goddard Space Flight Center was supported by NASA's Earth Observing System (EOS) Program and the Cryospheric Sciences Program. The research carried out at the Jet Propulsion Laboratory, California Institute of Technology, was also supported by NASA. NR 74 TC 22 Z9 22 U1 2 U2 10 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9003 EI 2169-9011 J9 J GEOPHYS RES-EARTH JI J. Geophys. Res.-Earth Surf. PD OCT 27 PY 2009 VL 114 AR F04006 DI 10.1029/2009JF001287 PG 13 WC Geosciences, Multidisciplinary SC Geology GA 513JM UT WOS:000271318500004 ER PT J AU Khazendar, A Rignot, E Larour, E AF Khazendar, A. Rignot, E. Larour, E. TI Roles of marine ice, rheology, and fracture in the flow and stability of the Brunt/Stancomb-Wills Ice Shelf SO JOURNAL OF GEOPHYSICAL RESEARCH-EARTH SURFACE LA English DT Article ID WEDDELL SEA; SAR INTERFEROMETRY; ANTARCTICA; DYNAMICS; FRONT; ACCUMULATION; ASSIMILATION; TEMPERATURE; POLYNYA; BENEATH AB Marine ice, sometimes as part of an ice melange, significantly affects ice shelf flow and ice fracture. The highly heterogeneous structure of the Brunt/Stancomb-Wills Ice Shelf (BSW) system in the east Weddell Sea offers a rare setting for uncovering the difference in rheology between meteoric and marine ice. Here, we use data assimilation to infer the rheology of the Brunt/Stancomb-Wills Ice Shelf by an inverse control method that combines interferometric synthetic aperture radar measurements with numerical modeling. We then apply the inferred rheology to support the hypothesis attributing the observed 1970s ice shelf flow acceleration to a change in the stiffness of the ice melange area connecting Brunt proper with Stancomb-Wills and to examine the consequences of frontal rift propagation. We conclude that while the Brunt/Stancomb-Wills system is currently not susceptible to extreme fragmentation similar to that of the Larsen B Ice Shelf in 2002, our inverse and forward modeling results emphasize its vulnerability to destabilization by relatively rapid changes in the ice melange properties, resulting from the interaction of its marine ice component with ocean water, or by the further propagation of a frontal rift. C1 [Khazendar, A.; Rignot, E.; Larour, E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Rignot, E.] Univ Calif Irvine, Irvine, CA 92697 USA. RP Khazendar, A (reprint author), CALTECH, Jet Prop Lab, Mail Stop 300-319,4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM ala.khazendar@jpl.nasa.gov RI Rignot, Eric/A-4560-2014 OI Rignot, Eric/0000-0002-3366-0481 FU NASA FX Part of this work was performed by the first author as a fellow of the NRC/Oak Ridge Associated Universities NASA Postdoctoral Program. He would like to thank A. Humbert, B. Kulessa, A. Luckman, K. Makinson, and K. Nicholls for informative discussions. We much appreciate the thorough and highly informative comments of O. Sergienko, two anonymous reviewers, and the Associate Editor. This work was performed at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration, with support from NASA's Cryospheric Sciences Program. NR 62 TC 34 Z9 34 U1 0 U2 9 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-EARTH JI J. Geophys. Res.-Earth Surf. PD OCT 27 PY 2009 VL 114 AR F04007 DI 10.1029/2008JF001124 PG 9 WC Geosciences, Multidisciplinary SC Geology GA 513JM UT WOS:000271318500001 ER PT J AU Bautz, MW Miller, ED Sanders, JS Arnaud, KA Mushotzky, RF Porter, FS Hayashida, K Henry, JP Hughes, JP Kawaharada, M Makishima, K Sato, M Tamura, T AF Bautz, Marshall W. Miller, Eric D. Sanders, Jeremy S. Arnaud, Keith A. Mushotzky, Richard F. Porter, F. Scott Hayashida, Kiyoshi Henry, J. Patrick Hughes, John P. Kawaharada, Madoka Makishima, Kazuo Sato, Mitsuhiro Tamura, Takayuki TI Suzaku Observations of Abell 1795: Cluster Emission to r(200) SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN LA English DT Article DE galaxies: clusters: intracluster medium; galaxies: clusters: individual (Abell 1795); galaxies: clusters: X-rays ID X-RAY-CLUSTERS; RELAXED GALAXY CLUSTERS; WIND CHARGE-EXCHANGE; XMM-NEWTON; VIRIAL RADIUS; SOLAR-WIND; SURFACE BRIGHTNESS; GAS TEMPERATURE; PROFILES; MASS AB We report Suzaku observations of the galaxy cluster Abell 1795 that extend to r(200) approximate to 2 Mpc, the radius within which the mean cluster mass density is 200 times the cosmic critical density. These observations are the first to probe the state of the intracluster medium in this object at r > 1.3 Mpc. We sample two disjoint sectors in the cluster outskirts (1.3 Mpc < r < 1.9 Mpc) and detect X-ray emission in only one of them to a limiting (3 sigma) soft X-ray surface brightness of B0.5-2keV = 1.8 x 10(-12) erg s(-1) cm(-2) deg(-2), it level less than 20% of the cosmic X-ray background brightness. We trace the run of temperature with radius at r > 0.4 Mpc and find that it falls relatively rapidly (T-deprojected proportional to r(-0.9)), reaching a value about one third of its peak at the largest radius we can measure it. Assuming the intracluster medium is in hydrostatic equilibrium and is polytropic, we find a polytropic index of Gamma = 1.3(-0.2)(+0.3) and we estimate a mass of (4.1(-0.3)(+0.5)) x 10(14) M-circle dot within 1.3 Mpc, somewhat (2.7 sigma) lower than that reported by previous observers. However, our observations provide evidence for departure from hydrostatic equilibrium at radii as small as r similar to 1.3 Mpc approximate to r(500) in this apparently regular and symmetrical cluster. C1 [Bautz, Marshall W.; Miller, Eric D.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Sanders, Jeremy S.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Arnaud, Keith A.; Mushotzky, Richard F.; Porter, F. Scott] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Hayashida, Kiyoshi] Osaka Univ, Grad Sch Sci, Dept Earth & Space Sci, Toyonaka, Osaka 5600043, Japan. [Henry, J. Patrick] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Hughes, John P.] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. [Kawaharada, Madoka; Makishima, Kazuo; Sato, Mitsuhiro] Univ Tokyo, Dept Phys, Bunkyo Ku, Tokyo 1130033, Japan. [Tamura, Takayuki] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2298510, Japan. RP Bautz, MW (reprint author), MIT, Kavli Inst Astrophys & Space Res, 77 Massachusetts Ave, Cambridge, MA 02139 USA. EM mwb@space.mit.edu RI Porter, Frederick/D-3501-2012; Tamura, Takayuki/K-8236-2012; XRAY, SUZAKU/A-1808-2009; OI Porter, Frederick/0000-0002-6374-1119; Sanders, Jeremy/0000-0003-2189-4501 FU NASA [NNG05GM92G, NNGG05GP87G, NNG06GC04G] FX We thank Alexey Vikhlinin and Steve Snowden for providing temperature data from Chandra and XMM-Newton, respectively, and Helen Russell for useful discussions about deprojection. MWB and EDM were supported in part by NASA grant NNG05GM92G to MIT. J. Hughes acknowledges support from NASA grant NNGG05GP87G. J. P. Henry acknowledges support from NASA grant NNG06GC04G. NR 48 TC 98 Z9 98 U1 0 U2 3 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0004-6264 EI 2053-051X J9 PUBL ASTRON SOC JPN JI Publ. Astron. Soc. Jpn. PD OCT 25 PY 2009 VL 61 IS 5 BP 1117 EP 1133 DI 10.1093/pasj/61.5.1117 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 513ZY UT WOS:000271364100019 ER PT J AU Hopfner, M Pitts, MC Poole, LR AF Hoepfner, M. Pitts, M. C. Poole, L. R. TI Comparison between CALIPSO and MIPAS observations of polar stratospheric clouds SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID LIMB EMISSION-SPECTRA; ACID TRIHYDRATE NAT; LIDAR MEASUREMENTS; WINTER 2002/2003; CIRRUS CLOUDS; PSCS; AEROSOL; MICROPHYSICS; WAVES; SIMULATIONS AB Polar stratospheric cloud (PSC) detection, top height, and composition as derived from measurements by the infrared emission limb sounder Michelson Interferometer for Passive Atmospheric Sounding (MIPAS) on Envisat and the Cloud-Aerosol Lidar and Infrared Pathfinder Satellite Observation (CALIPSO) lidar have been compared. The comparisons are based on coincident observations from the 2006 and 2007 Antarctic and the 2006/2007 and 2007/2008 Arctic winters. During the middle of the Antarctic season, very good agreement in common PSC detection (around 90%) has been found. At the beginning and end of the Antarctic PSC season and in the Arctic, the frequency of common PSC detection is generally less (60-70%) which can be explained by cloud inhomogeneity and viewing geometry differences. MIPAS PSC top heights are about 0-2 km lower than CALIPSO top heights with larger offsets at higher altitudes. The negative bias of MIPAS PSC top heights can be modeled under the assumptions of limited horizontal cloud extent and a field-of-view-dependent sensitivity. The comparisons further show a high degree of consistency between PSC composition derived from the fundamentally different classification approaches of the two instruments. Remaining differences can be explained considering the physical limitations of each approach and the definition of composition boundaries within the classification scheme of each instrument. C1 [Hoepfner, M.] Karlsruhe Inst Technol, Inst Meteorol & Climate Res, D-76021 Karlsruhe, Germany. [Pitts, M. C.] NASA, Langley Res Ctr, Hampton, VA 23681 USA. [Poole, L. R.] Sci Syst & Applicat Inc, Hampton, VA 23666 USA. RP Hopfner, M (reprint author), Karlsruhe Inst Technol, Inst Meteorol & Climate Res, Postfach 3640, D-76021 Karlsruhe, Germany. EM michael.hoepfner@kit.edu; michael.c.pitts@nasa.gov; lamont.r.poole@nasa.gov RI Hopfner, Michael/A-7255-2013 OI Hopfner, Michael/0000-0002-4174-9531 FU Hal Maring, NASA Radiation Sciences program manager; NASA Headquarters Earth Science Division; NASA [NNL07AA00C] FX We thank the European Space Agency for providing MIPAS spectra. CALIPSO PSC research is supported by Hal Maring, NASA Radiation Sciences program manager, and the NASA Headquarters Earth Science Division. Support for L. Poole is provided under NASA contract NNL07AA00C. NR 54 TC 19 Z9 19 U1 2 U2 6 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD OCT 24 PY 2009 VL 114 AR D00H05 DI 10.1029/2009JD012114 PG 15 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 510ZA UT WOS:000271131800001 ER PT J AU Cao, CY Vermote, E Xiong, XX AF Cao, Changyong Vermote, Eric Xiong, Xiaoxiong TI Using AVHRR lunar observations for NDVI long-term climate change detection SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID HIGH-RESOLUTION RADIOMETER; NEAR-INFRARED CHANNELS; ON-ORBIT CALIBRATION; MODIS; SPACECRAFT; BANDS; MOON AB The Moon is believed to be an irrefutably stable calibration reference target for studying climate change from satellites, as demonstrated in several lunar calibration studies of satellite radiometers. However, the potential of using advanced very high resolution radiometer (AVHRR) lunar observations for climate change detection has not been recognized in the past. At the same time, it is known that despite past efforts, there are still significant uncertainties in determining the long-term trend of climate change using such indices as the Normalized Difference Vegetation Index (NDVI), partly because most AVHRR calibrations to date lack the stability required for climate change detection. This study demonstrates a novel method using the AVHRR lunar band ratio as a stability reference for long-term NDVI change detection. It shows that despite the incomplete lunar observations and complex space view mechanisms, the AVHRR lunar observations can be used to ensure the stability of the Earth observations at a better than +/- 1% (1 sigma) level for the lifetime of the AVHRR instrument in the long-term detection of NDVI trends. This method is compared with the Vermote and Kaufman high-altitude bright cloud method used by the NASA Long-Term Data Record (LTDR) project, and preliminary results are very encouraging. The lunar band ratio method has been tested for NOAA11, 14, and 16AVHRR and is applicable to all AVHRRs since the early 1980s. It is conceived that the Lunar Band Ratio serves as an important stability reference for ensuring the long-term confidence for the detection of climate change. The AVHRR lunar band ratio is also useful for deriving the calibration for the problematic band 2 from that of band 1 for establishing a consistent AVHRR fundamental climate data record for a variety of climate applications. C1 [Cao, Changyong] NOAA, Ctr Satellite Applicat & Res, NESDIS, Camp Springs, MD USA. [Vermote, Eric] Univ Maryland, Dept Geog, College Pk, MD 20742 USA. [Xiong, Xiaoxiong] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20770 USA. RP Cao, CY (reprint author), NOAA, Ctr Satellite Applicat & Res, NESDIS, 5200 Auth Rd,E-RA1,Room 810,WWB, Camp Springs, MD USA. EM changyong.cao@noaa.gov RI Cao, Changyong/F-5578-2010; Vermote, Eric/K-3733-2012 NR 24 TC 9 Z9 9 U1 1 U2 8 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD OCT 23 PY 2009 VL 114 AR D20105 DI 10.1029/2009JD012179 PG 9 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 510YZ UT WOS:000271131700004 ER PT J AU Ehlmann, BL Mustard, JF Swayze, GA Clark, RN Bishop, JL Poulet, F Marais, DJD Roach, LH Milliken, RE Wray, JJ Barnouin-Jha, O Murchie, SL AF Ehlmann, Bethany L. Mustard, John F. Swayze, Gregg A. Clark, Roger N. Bishop, Janice L. Poulet, Francois Marais, David J. Des Roach, Leah H. Milliken, Ralph E. Wray, James J. Barnouin-Jha, Olivier Murchie, Scott L. TI Identification of hydrated silicate minerals on Mars using MRO-CRISM: Geologic context near Nili Fossae and implications for aqueous alteration SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Review ID RESOLUTION REFLECTANCE SPECTROSCOPY; SPECTRAL CHARACTERISTICS; HYDROTHERMAL ALTERATION; INFRARED-SPECTROSCOPY; EMISSION-SPECTROSCOPY; WATER; PHYLLOSILICATES; SERPENTINES; KAOLINITE; DEPOSITS AB The Noachian terrain west of the Isidis basin hosts a diverse collection of alteration minerals in rocks comprising varied geomorphic units within a 100,000 km 2 region in and near the Nili Fossae. Prior investigations in this region by the Observatoire pour l'Mineralogie, l'Eau, les Glaces, et l'Activite (OMEGA) instrument on Mars Express revealed large exposures of both mafic minerals and iron magnesium phyllosilicates in stratigraphic context. Expanding on the discoveries of OMEGA, the Compact Reconnaissance Imaging Spectrometer for Mars (CRISM) aboard the Mars Reconnaissance Orbiter (MRO) has found more spatially widespread and mineralogically diverse alteration minerals than previously realized, which represent multiple aqueous environments. Using CRISM near-infrared spectral data, we detail the basis for identification of iron and magnesium smectites (including both nontronite and more Mg-rich varieties), chlorite, prehnite, serpentine, kaolinite, potassium mica (illite or muscovite), hydrated (opaline) silica, the sodium zeolite analcime, and magnesium carbonate. The detection of serpentine and analcime on Mars is reported here for the first time. We detail the geomorphic context of these minerals using data from high-resolution imagers onboard MRO in conjunction with CRISM. We find that the distribution of alteration minerals is not homogeneous; rather, they occur in provinces with distinctive assemblages of alteration minerals. Key findings are (1) a distinctive stratigraphy, in and around the Nili Fossae, of kaolinite and magnesium carbonate in bedrock units always overlying Fe/Mg smectites and (2) evidence for mineral phases and assemblages indicative of low-grade metamorphic or hydrothermal aqueous alteration in cratered terrains. The alteration minerals around the Nili Fossae are more typical of those resulting from neutral to alkaline conditions rather than acidic conditions, which appear to have dominated much of Mars. Moreover, the mineralogic diversity and geologic context of alteration minerals found in the region around the Nili Fossae indicates several episodes of aqueous activity in multiple distinct environments. C1 [Ehlmann, Bethany L.; Mustard, John F.; Roach, Leah H.] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA. [Barnouin-Jha, Olivier; Murchie, Scott L.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Bishop, Janice L.; Marais, David J. Des] NASA, Ames Res Ctr, Mountain View, CA 94035 USA. [Swayze, Gregg A.; Clark, Roger N.] US Geol Survey, Denver, CO 80225 USA. [Milliken, Ralph E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Poulet, Francois] Univ Paris 11, Inst Astrophys Spatiale, CNRS, F-91405 Orsay, France. [Wray, James J.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. [Bishop, Janice L.] SETI Inst, Mountain View, CA USA. RP Ehlmann, BL (reprint author), Brown Univ, Dept Geol Sci, Providence, RI 02912 USA. RI Wray, James/B-8457-2008; Murchie, Scott/E-8030-2015; Barnouin, Olivier/I-7475-2015 OI Wray, James/0000-0001-5559-2179; Murchie, Scott/0000-0002-1616-8751; Barnouin, Olivier/0000-0002-3578-7750 NR 117 TC 203 Z9 204 U1 5 U2 45 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 OCT 23 PY 2009 VL 114 AR E00D08 DI 10.1029/2009JE003339 PG 33 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 510ZP UT WOS:000271133400002 ER PT J AU Sunshine, JM Farnham, TL Feaga, LM Groussin, O Merlin, F Milliken, RE A'Hearn, MF AF Sunshine, Jessica M. Farnham, Tony L. Feaga, Lori M. Groussin, Olivier Merlin, Frederic Milliken, Ralph E. A'Hearn, Michael F. TI Temporal and Spatial Variability of Lunar Hydration As Observed by the Deep Impact Spacecraft SO SCIENCE LA English DT Article ID SPECTRAL PROPERTIES; WATER; MONTMORILLONITE; MIXTURES; MINERALS AB The Moon is generally anhydrous, yet the Deep Impact spacecraft found the entire surface to be hydrated during some portions of the day. Hydroxyl (OH) and water (H(2)O) absorptions in the near infrared were strongest near the North Pole and are consistent with <0.5 weight percent H(2)O. Hydration varied with temperature, rather than cumulative solar radiation, but no inherent absorptivity differences with composition were observed. However, comparisons between data collected 1 week (a quarter lunar day) apart show a dynamic process with diurnal changes in hydration that were greater for mare basalts (similar to 70%) than for highlands (similar to 50%). This hydration loss and return to a steady state occurred entirely between local morning and evening, requiring a ready daytime source of water-group ions, which is consistent with a solar wind origin. C1 [Sunshine, Jessica M.; Farnham, Tony L.; Feaga, Lori M.; Merlin, Frederic; A'Hearn, Michael F.] Univ Maryland, College Pk, MD 20742 USA. [Groussin, Olivier] Lab Astrophys Marseille, F-13388 Marseille, France. [Milliken, Ralph E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Sunshine, JM (reprint author), Univ Maryland, College Pk, MD 20742 USA. EM jess@astro.umd.edu FU NASA Discovery Program [NNM07AA99C, NNG06GJ31G] FX EPOXI, the Deep Impact extended mission, is supported by the NASA Discovery Program under contract NNM07AA99C to the University of Maryland. The Deep Impact spacecraft and HRI-IR instrument were built by Ball Aerospace. We gratefully acknowledge the efforts and support of the EPOXI project team at the Jet Propulsion Laboratory in acquiring the data presented here and the continuing work of members of the EPOXI science team in improving the instrument calibration. Laboratory spectra of lunar soils were acquired with the NASA/Keck RELAB, a multi-user facility supported by NASA grant NNG06GJ31G. We also thank R. Clark for discussions on the spectral interpretations of the 3-mm feature and L. McFadden for comments that improved this manuscript. NR 17 TC 157 Z9 163 U1 3 U2 20 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 J9 SCIENCE JI Science PD OCT 23 PY 2009 VL 326 IS 5952 BP 565 EP 568 DI 10.1126/science.1179788 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 509LN UT WOS:000271019400039 PM 19779149 ER PT J AU Pieters, CM Goswami, JN Clark, RN Annadurai, M Boardman, J Buratti, B Combe, JP Dyar, MD Green, R Head, JW Hibbitts, C Hicks, M Isaacson, P Klima, R Kramer, G Kumar, S Livo, E Lundeen, S Malaret, E McCord, T Mustard, J Nettles, J Petro, N Runyon, C Staid, M Sunshine, J Taylor, LA Tompkins, S Varanasi, P AF Pieters, C. M. Goswami, J. N. Clark, R. N. Annadurai, M. Boardman, J. Buratti, B. Combe, J. -P. Dyar, M. D. Green, R. Head, J. W. Hibbitts, C. Hicks, M. Isaacson, P. Klima, R. Kramer, G. Kumar, S. Livo, E. Lundeen, S. Malaret, E. McCord, T. Mustard, J. Nettles, J. Petro, N. Runyon, C. Staid, M. Sunshine, J. Taylor, L. A. Tompkins, S. Varanasi, P. TI Character and Spatial Distribution of OH/H2O on the Surface of the Moon Seen by M-3 on Chandrayaan-1 SO SCIENCE LA English DT Article ID LUNAR POLES; WATER ICE; EPITHERMAL NEUTRONS; OPTICAL-CONSTANTS; HYDROGEN; PROSPECTOR AB The search for water on the surface of the anhydrous Moon had remained an unfulfilled quest for 40 years. However, the Moon Mineralogy Mapper (M-3) on Chandrayaan-1 has recently detected absorption features near 2.8 to 3.0 micrometers on the surface of the Moon. For silicate bodies, such features are typically attributed to hydroxyl- and/or water-bearing materials. On the Moon, the feature is seen as a widely distributed absorption that appears strongest at cooler high latitudes and at several fresh feldspathic craters. The general lack of correlation of this feature in sunlit M-3 data with neutron spectrometer hydrogen abundance data suggests that the formation and retention of hydroxyl and water are ongoing surficial processes. Hydroxyl/water production processes may feed polar cold traps and make the lunar regolith a candidate source of volatiles for human exploration. C1 [Pieters, C. M.; Head, J. W.; Isaacson, P.; Klima, R.; Mustard, J.; Nettles, J.] Brown Univ, Providence, RI 02912 USA. [Goswami, J. N.] Phys Res Lab, Ahmadabad 380009, Gujarat, India. [Goswami, J. N.; Annadurai, M.] Indian Space Res Org, Bangalore 562140, Karnataka, India. [Clark, R. N.; Livo, E.] US Geol Survey, Denver, CO 80225 USA. [Boardman, J.] Analyt Imaging & Geophys, Boulder, CO 80303 USA. [Buratti, B.; Green, R.; Hicks, M.; Lundeen, S.; Varanasi, P.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Combe, J. -P.; Kramer, G.; McCord, T.] Bear Fight Ctr, Winthrop, WA 98862 USA. [Dyar, M. D.] Mt Holyoke Coll, S Hadley, MA 01075 USA. [Hibbitts, C.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Kumar, S.] Natl Remote Sensing Agcy, Hyderabad, Andhra Pradesh, India. [Malaret, E.] Appl Coherent Technol Corp, Herndon, VA 22070 USA. [Petro, N.] NASA Goddard, Greenbelt, MD 20771 USA. [Runyon, C.] Coll Charleston, Charleston, SC 29424 USA. [Staid, M.] Planetary Sci Inst, Tucson, AZ 85719 USA. [Sunshine, J.] Univ Maryland, College Pk, MD 20742 USA. [Taylor, L. A.] Univ Tennessee, Knoxville, TN 37996 USA. [Tompkins, S.] Def Adv Res Projects Agcy, Arlington, VA 22203 USA. RP Pieters, CM (reprint author), Brown Univ, Providence, RI 02912 USA. EM carle_pieters@brown.edu RI Petro, Noah/F-5340-2013; Hibbitts, Charles/B-7787-2016 OI Hibbitts, Charles/0000-0001-9089-4391 FU NASA's Discovery program [NNM05AB26C, NNG06GJ31G] FX M3 is funded as a Mission of Opportunity under NASA's Discovery program contract NNM05AB26C to Brown University. Lunar reflectance spectra were acquired using the NASA/Keck Reflectance Experiment Laboratory, a multiuser facility supported by NASA grant NNG06GJ31G. A portion of this research was carried out at the JPL, California Institute of Technology, under a contract with NASA. We thank the team of engineers at JPL who designed and built M3 ( led by T. Glavich and M. White) and the Chandrayaan-1 mission operations team ( led by N. S. Hegde, with M3 implementation largely by S. Gomathi), whose mission support has made M3 data possible. The M3 team is honored to be a guest instrument on India's first mission to the Moon. NR 23 TC 237 Z9 253 U1 12 U2 49 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 J9 SCIENCE JI Science PD OCT 23 PY 2009 VL 326 IS 5952 BP 568 EP 572 DI 10.1126/science.1178658 PG 5 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 509LN UT WOS:000271019400040 PM 19779151 ER PT J AU Zong, QG Wang, YF Yang, B Zhang, H Tian, AM Dunlop, M Fritz, TA Kistler, LM Korth, A Daly, PW Pedersen, A AF Zong, Q. -G. Wang, Y. F. Yang, B. Zhang, H. Tian, A. M. Dunlop, M. Fritz, T. A. Kistler, L. M. Korth, A. Daly, P. W. Pedersen, A. TI Vortex-like plasma flow structures observed by Cluster at the boundary of the outer radiation belt and ring current: A link between the inner and outer magnetosphere SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID KELVIN-HELMHOLTZ INSTABILITY; FIELD-ALIGNED CURRENT; GEOTAIL OBSERVATIONS; MAGNETOTAIL BOUNDARY; EARTHS MAGNETOSPHERE; MAGNETIC-FIELD; CURRENT SHEET; SOLAR-CYCLE; VORTICES; SPACECRAFT AB Two vortex-like plasma flow structures have been observed at the outer radiation belt and/or the ring current region on 11 April 2002, from 0415 to 0635 UT, when the Cluster fleet entered (in the Southern Hemisphere) and exited (in the Northern Hemisphere) the boundary layer of the inner magnetosphere near 2130 MLT. On 11 April 2002 during the period of interest, the solar wind speed was high, and the geomagnetic activity was moderate. These two vortices have opposite rotation directions and are characterized by bipolar signatures in the flow V(x) components with peak-to-peak amplitudes of about 40 km/s. The inflection points of the plasma flow coincide precisely with the local maxima of the duskward core flow V(y) (30 km/s) which exceed the surrounding flow by 3-4 times in magnitude for both vortices. A pair of bidirectional current sheets and bipolar electric fields (E(y)) are found to be closely associated with these vortices. Whereas magnetic field disturbances are observed only in B(x) and B(y) components, the magnetic magnitude stays almost unchanged. Vortices observed both inbound and outbound at the boundary of the radiation belt at nearly the same location (L shell and latitude), suggesting they may last for more than 140 min. The scale sizes of the two vortices are about 810 km and 1138 km, respectively. Interestingly, it is found that Earth's ionospheric singly charged oxygen are precipitating in the vortex dynamic process, having energies less than 1 keV and having a strong field-aligned pitch angle distribution. These plasma flow vortices are suggested to be formed at the interface between the enhanced ionospheric outflow stream from the polar ionosphere and a sudden braking and/or azimuthal deflection of bursty bulk flows generated by the tail reconnection. These observed flow vortices provide a link among the inner magnetosphere, the tail plasma sheet, and the Earth's ionosphere by coupling magnetic shear stresses and plasma flow momentum. C1 [Zong, Q. -G.; Wang, Y. F.; Yang, B.; Tian, A. M.] Peking Univ, Inst Space Phys & Appl Technol, Beijing 100871, Peoples R China. [Zong, Q. -G.] Univ Massachusetts, Ctr Atmospher Res, Lowell, MA 01854 USA. [Zhang, H.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20770 USA. [Dunlop, M.] CCLRC Rutherford Appleton Lab, Didcot OX11 0QX, Oxon, England. [Fritz, T. A.] Boston Univ, Ctr Space Phys, Boston, MA 02215 USA. [Korth, A.; Daly, P. W.] Max Planck Inst Sonnensyst Forsch, D-37191 Katlenburg Lindau, Germany. [Kistler, L. M.] Univ New Hampshire, Ctr Space Sci, Durham, NH 03824 USA. [Pedersen, A.] Univ Oslo, Dept Phys, N-0316 Oslo, Norway. RP Zong, QG (reprint author), Peking Univ, Inst Space Phys & Appl Technol, Beijing 100871, Peoples R China. EM qiugang_zong@uml.edu RI dunlop, malcolm/F-1347-2010 FU National Natural Science Foundation of China [40831061]; China Scholarship Council FX This work is partly supported by the National Natural Science Foundation of China grant 40831061. One of the authors (Biao Yang) is grateful to China Scholarship Council for the financial support. NR 45 TC 14 Z9 15 U1 0 U2 4 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD OCT 22 PY 2009 VL 114 AR A10211 DI 10.1029/2009JA014388 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 510ZX UT WOS:000271134300004 ER PT J AU Jennings, DE Romani, PN Bjoraker, GL Sada, PV Nixon, CA Lunsford, AW Boyle, RJ Hesman, BE McCabe, GH AF Jennings, Donald E. Romani, Paul N. Bjoraker, Gordon L. Sada, Pedro V. Nixon, Conor A. Lunsford, Allen W. Boyle, Robert J. Hesman, Brigette E. McCabe, George H. TI C-12/C-13 Ratio in Ethane on Titan and Implications for Methane's Replenishment SO JOURNAL OF PHYSICAL CHEMISTRY A LA English DT Article ID COMPOSITE INFRARED SPECTROMETER; ISOTOPIC-RATIOS; CASSINI/CIRS; ABUNDANCES; ATMOSPHERE; SATURN; N-14/N-15; SPECTRA AB The C-12/C-13 abundance ratio in ethane in the atmosphere of Titan has been measured at 822 cm(-1) from high spectral resolution ground-based observations. The value, 89(8), coincides with the telluric standard and also agrees with the ratio seen in the outer planets. It is almost identical to the result for ethane on Titan found by the composite infrared spectrometer (CIRS) on Cassini. The C-12/C-13 ratio for ethane is higher than the ratio measured in atmospheric methane by Cassini/Huygens GCMS, 82.3(1), representing an enrichment of C-12 in the ethane that might be explained by a kinetic isotope effect of approximately 1.1 in the formation of methyl radicals. If methane is being continuously resupplied to balance photochemical destruction, then we expect the isotopic composition in the ethane product to equilibrate at close to the same C-11/C-13 ratio as that in the supply. The telluric value of the ratio in ethane then implies that the methane reservoir is primordial. C1 [Jennings, Donald E.; Romani, Paul N.; Bjoraker, Gordon L.; Nixon, Conor A.; Lunsford, Allen W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Sada, Pedro V.] Univ Monterrey, Dept Fis & Math, Graza Garcia 66238, NL, Mexico. [Nixon, Conor A.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Lunsford, Allen W.] Catholic Univ Amer, Washington, DC 20064 USA. [Boyle, Robert J.] Dickinson Coll, Dept Phys & Astron, Carlisle, PA 17013 USA. [Hesman, Brigette E.] Natl Radio Astron Observ, Pete V Domenici Sci Operat Ctr, Socorro, NM 87801 USA. [McCabe, George H.] CMA Consulting Serv, Latham, NY 12110 USA. RP Jennings, DE (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM donald.e.jennings@nasa.gov RI Nixon, Conor/A-8531-2009; Romani, Paul/D-2729-2012; Bjoraker, Gordon/D-5032-2012; Jennings, Donald/D-7978-2012 OI Nixon, Conor/0000-0001-9540-9121; FU NASA's Cassini Project; Planetary Astronomy Program FX We thank C. Plymate and E. Galayda of the McMath-Pierce Telescope for observing run support. Funding for this work came from NASA's Cassini Project and Planetary Astronomy Program. NR 31 TC 12 Z9 12 U1 0 U2 2 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 1089-5639 J9 J PHYS CHEM A JI J. Phys. Chem. A PD OCT 22 PY 2009 VL 113 IS 42 BP 11101 EP 11106 DI 10.1021/jp903637d PG 6 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 505EA UT WOS:000270670700003 PM 19552394 ER PT J AU Wilson, EH Atreya, SK AF Wilson, Eric H. Atreya, Sushil K. TI Titan's Carbon Budget and the Case of the Missing Ethane SO JOURNAL OF PHYSICAL CHEMISTRY A LA English DT Article ID VOYAGER INFRARED OBSERVATIONS; METHANE CYCLE; ATMOSPHERE; PHOTOCHEMISTRY; SURFACE; HYDROCARBONS; PHOTOLYSIS; PROFILES; CHANNELS; HUYGENS AB The retrieval of data from the Cassini-Huygens mission has revealed much about Titan's atmospheric-surface system and has precipitated more questions. One of these questions involves the lack of large reservoirs of ethane that were predicted by a variety of studies prior to the arrival of the Cassini-Huygens spacecraft. Using an updated and comprehensive photochemical model, we examine the nature of Titan's carbon budget, initiated by the destruction of methane, and the role that ethane condensation plays in this budget. Model results show that 40% of methane destruction results in ethane formation, with a net production rate of 2.7 x 10(9) molecules cm(-2) s(-1), due primarily to acetylenic catalysis in Titan's stratosphere. This corresponds to a liquid ethane layer of several hundred meters over geologic time. However, episodic methane outgassing, subsurface sequestration, and chemical processing of Titan's surface are likely responsible for the limiting of ethane condensate on Titan's surface to less than 10 m globally averaged. C1 [Wilson, Eric H.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Wilson, Eric H.; Atreya, Sushil K.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. RP Wilson, EH (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr M-S 169-237, Pasadena, CA 91109 USA. EM titansat74@yahoo.com NR 41 TC 31 Z9 31 U1 0 U2 9 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 1089-5639 J9 J PHYS CHEM A JI J. Phys. Chem. A PD OCT 22 PY 2009 VL 113 IS 42 BP 11221 EP 11226 DI 10.1021/jp905535a PG 6 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 505EA UT WOS:000270670700017 PM 19827852 ER PT J AU Kleinbohl, A Schofield, JT Kass, DM Abdou, WA Backus, CR Sen, B Shirley, JH Lawson, WG Richardson, MI Taylor, FW Teanby, NA McCleese, DJ AF Kleinboehl, Armin Schofield, John T. Kass, David M. Abdou, Wedad A. Backus, Charles R. Sen, Bhaswar Shirley, James H. Lawson, W. Gregory Richardson, Mark I. Taylor, Fredric W. Teanby, Nicholas A. McCleese, Daniel J. TI Mars Climate Sounder limb profile retrieval of atmospheric temperature, pressure, and dust and water ice opacity SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID ORBITER LASER ALTIMETER; RADIATIVE-TRANSFER; THERMAL STRUCTURE; GLOBAL SURVEYOR; MU-M; AEROSOL; ABSORPTION; H2O; CO2 AB The Mars Climate Sounder (MCS) onboard the Mars Reconnaissance Orbiter is the latest of a series of investigations devoted to improving the understanding of current Martian climate. MCS is a nine-channel passive midinfrared and far-infrared filter radiometer designed to measure thermal emission in limb and on-planet geometries from which vertical profiles of atmospheric temperature, water vapor, dust, and condensates can be retrieved. Here we describe the algorithm that is used to retrieve atmospheric profiles from MCS limb measurements for delivery to the Planetary Data System. The algorithm is based on a modified Chahine method and uses a fast radiative transfer scheme based on the Curtis-Godson approximation. It retrieves pressure and vertical profiles of atmospheric temperature, dust opacity, and water ice opacity. Water vapor retrievals involve a different approach and will be reported separately. Pressure can be retrieved to a precision of 1-2% and is used to establish the vertical coordinate. Temperature profiles are retrieved over a range from 5-10 to 80-90 km altitude with a typical altitude resolution of 4-6 km and a precision between 0.5 and 2 K over most of this altitude range. Dust and water ice opacity profiles also achieve vertical resolutions of about 5 km and typically have precisions of 10(-4)-10(-5) km(-1) at 463 cm(-1) and 843 cm(-1), respectively. Examples of temperature profiles as well as dust and water ice opacity profiles from the first year of the MCS mission are presented, and atmospheric features observed during periods employing different MCS operational modes are described. An intercomparison with historical temperature measurements from the Mars Global Surveyor mission shows good agreement. C1 [Kleinboehl, Armin; Schofield, John T.; Kass, David M.; Abdou, Wedad A.; Backus, Charles R.; Sen, Bhaswar; Shirley, James H.; McCleese, Daniel J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Lawson, W. Gregory; Richardson, Mark I.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Taylor, Fredric W.; Teanby, Nicholas A.] Univ Oxford, Clarendon Lab, Oxford OX1 3PU, England. RP Kleinbohl, A (reprint author), CALTECH, Jet Prop Lab, Mail Stop 169-237,4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM armin.kleinboehl@jpl.nasa.gov OI Teanby, Nicholas/0000-0003-3108-5775 FU National Aeronautics and Space Administration FX We would like to thank the MRO spacecraft and MCS instrument operations teams who made these measurements possible. We also wish to thank Joshua Bandfield and Timothy Glotch for contributing spectroscopic parameters of dust. We are indebted to Michael Wolff for providing limb scattering calculations in addition to his review of the manuscript. Furthermore, we acknowledge Nicholas Heavens for helpful comments on the manuscript. Work at the Jet Propulsion Laboratory, California Institute of Technology, was performed under a contract with the National Aeronautics and Space Administration. NR 40 TC 69 Z9 69 U1 1 U2 6 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9097 EI 2169-9100 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD OCT 21 PY 2009 VL 114 AR E10006 DI 10.1029/2009JE003358 PG 30 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 510ZO UT WOS:000271133300001 ER PT J AU Li, HB Dowell, CD Goodman, A Hildebrand, R Novak, G AF Li, Hua-Bai Dowell, C. Darren Goodman, Alyssa Hildebrand, Roger Novak, Giles TI ANCHORING MAGNETIC FIELD IN TURBULENT MOLECULAR CLOUDS SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: clouds; ISM: magnetic fields; polarization; stars: formation; turbulence ID SUBMILLIMETER POLARIZATION; STAR-FORMATION; CORES; ALIGNMENT; DENSITY; REGIONS; MODELS; DR21 AB One of the key problems in star formation research is to determine the role of magnetic fields. Starting from the atomic intercloud medium which has density n(H) similar to 1 cm(-3), gas must accumulate from a volume several hundred pc across in order to form a typical molecular cloud. Star formation usually occurs in cloud cores, which have linear sizes below 1 pc and densities n(H2) > 10(5) cm(-3). With current technologies, it is hard to probe magnetic fields at scales lying between the accumulation length and the size of cloud cores, a range corresponds to many levels of turbulent eddy cascade, and many orders of magnitude of density amplification. For field directions detected from the two extremes, however, we show here that a significant correlation is found. Comparing this result with molecular cloud simulations, only the sub-Alfvenic cases result in field orientations consistent with our observations. C1 [Li, Hua-Bai; Goodman, Alyssa] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Dowell, C. Darren] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA. [Hildebrand, Roger] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [Hildebrand, Roger] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Novak, Giles] Northwestern Univ, Dept Phys & Astron, Evanston, IL 60208 USA. [Dowell, C. Darren] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Hildebrand, Roger] Univ Chicago, Dept Phys, Chicago, IL 60637 USA. RP Li, HB (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 78, Cambridge, MA 02138 USA. EM hli@cfa.harvard.edu RI Goodman, Alyssa/A-6007-2010 OI Goodman, Alyssa/0000-0003-1312-0477 FU Smithsonian Astrophysics Observatory; NSF [AST-0505124, AST-0540882] FX We appreciate the referee, whose comments have made our article much better. We are grateful to T. K. Sridharan, Zhi-Yun Li, Paolo Padoan, Telemachos Ch. Mouschovias, Yasuo Fukui, Alex Lazarian, and John Scalo for insightful discussions and comments. H. L. appreciates the helps from Tingting Wu on collecting and preliminarily analyzing the optical data. We thank Scott Paine and Robert Kimberk for proofreading many versions of themanuscript. H. L.'s research is funded through a postdoctoral fellowship from the Smithsonian Astrophysics Observatory. R. H. acknowledges NSF grant AST-0505124 for support of the submillimeter observations. The Caltech Submillimeter Observatory is funded through the NSF grant AST-0540882. NR 38 TC 12 Z9 12 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 20 PY 2009 VL 704 IS 2 BP 891 EP 897 DI 10.1088/0004-637X/704/2/891 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 502UQ UT WOS:000270486200058 ER PT J AU Krimm, HA Yamaoka, K Sugita, S Ohno, M Sakamoto, T Barthelmy, SD Gehrels, N Hara, R Norris, JP Ohmori, N Onda, K Sato, G Tanaka, H Tashiro, M Yamauchi, M AF Krimm, H. A. Yamaoka, K. Sugita, S. Ohno, M. Sakamoto, T. Barthelmy, S. D. Gehrels, N. Hara, R. Norris, J. P. Ohmori, N. Onda, K. Sato, G. Tanaka, H. Tashiro, M. Yamauchi, M. TI TESTING THE E-peak-E-iso RELATION FOR GRBs DETECTED BY SWIFT AND SUZAKU-WAM SO ASTROPHYSICAL JOURNAL LA English DT Review DE gamma rays: bursts ID GAMMA-RAY BURSTS; PROMPT EMISSION; SPECTRAL CATALOG; ALERT TELESCOPE; HUBBLE DIAGRAM; REDSHIFT; ENERGY; AFTERGLOW; ENERGETICS; BAT AB One of the most prominent, yet controversial associations derived from the ensemble of prompt-phase observations of gamma-ray bursts (GRBs) is the apparent correlation in the source frame between the peak energy (E-peak) of the nu F(nu) spectrum and the isotropic radiated energy, E-iso. Since most GRBs have E-peak above the energy range (15-150 keV) of the Burst Alert Telescope (BAT) on Swift, determining accurate E-peak values for large numbers of Swift bursts has been difficult. However, by combining data from Swift/BAT and the Suzaku Wideband All-Sky Monitor (WAM), which covers the energy range from 50 to 5000 keV, for bursts which are simultaneously detected, one can accurately fit E-peak and E-iso and test the relationship between them for the Swift sample. Between the launch of Suzaku in 2005 July and the end of 2009 April, there were 48 GRBs that triggered both Swift/BAT and WAM, and an additional 48 bursts that triggered Swift and were detected by WAM, but did not trigger. A BAT-WAM team has cross-calibrated the two instruments using GRBs, and we are now able to perform joint fits on these bursts to determine their spectral parameters. For those bursts with spectroscopic redshifts, we can also calculate the isotropic energy. Here, we present the results of joint Swift/BAT-Suzaku/WAM spectral fits for 91 of the bursts detected by the two instruments. We show that the distribution of spectral fit parameters is consistent with distributions from earlier missions and confirm that Swift bursts are consistent with earlier reported relationships between E-peak and isotropic energy. We show through time-resolved spectroscopy that individual burst pulses are also consistent with this relationship. C1 [Krimm, H. A.; Sakamoto, T.] CRESST, Greenbelt, MD 20771 USA. [Krimm, H. A.; Sakamoto, T.; Barthelmy, S. D.; Gehrels, N.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Krimm, H. A.] Univ Space Res Assoc, Columbia, MD 21044 USA. [Yamaoka, K.; Sugita, S.] Aoyama Gakuin Univ, Dept Math & Phys, Kanagawa 2298558, Japan. [Sugita, S.] RIKEN, Wako, Saitama 3510198, Japan. [Ohno, M.; Sato, G.] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, JAXA, Sagamihara, Kanagawa 2298510, Japan. [Sakamoto, T.] Univ Maryland, Joint Ctr Astrophys, Baltimore, MD 21250 USA. [Hara, R.; Ohmori, N.; Tanaka, H.; Yamauchi, M.] Miyazaki Univ, Dept Appl Phys, Miyazaki 8892192, Japan. [Norris, J. P.] Univ Denver, Dept Phys & Astron, Denver, CO 80208 USA. [Onda, K.; Tashiro, M.] Saitama Univ, Dept Phys, Sakura Ku, Saitama 3388570, Japan. RP Krimm, HA (reprint author), CRESST, Greenbelt, MD 20771 USA. RI Barthelmy, Scott/D-2943-2012; Gehrels, Neil/D-2971-2012; XRAY, SUZAKU/A-1808-2009 FU Swift project; Japanese Ministry of Education, Culture, Sports, Science and Technology (MEXT) [19047001 KY] FX H. A. K. and T. S. are supported by the Swift project. This research is supported in part by a Grant-in-Aid for Science Research (19047001 KY) of the Japanese Ministry of Education, Culture, Sports, Science and Technology (MEXT). We appreciate the helpful communication with C. Guidorzi about using the log-likelihood function for our fits. We also thank the anonymous referee for his/her insightful comments and suggestions that significantly improved the paper. NR 133 TC 53 Z9 53 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 OCT 20 PY 2009 VL 704 IS 2 BP 1405 EP 1432 DI 10.1088/0004-637X/704/2/1405 PG 28 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 502UQ UT WOS:000270486200032 ER PT J AU Hansen, FK Banday, AJ Gorski, KM Eriksen, HK Lilje, PB AF Hansen, F. K. Banday, A. J. Gorski, K. M. Eriksen, H. K. Lilje, P. B. TI POWER ASYMMETRY IN COSMIC MICROWAVE BACKGROUND FLUCTUATIONS FROM FULL SKY TO SUB-DEGREE SCALES: IS THE UNIVERSE ISOTROPIC? SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmic microwave background; cosmology: observations; methods: data analysis; methods: statistical ID ANISOTROPY-PROBE DATA; DIRECTIONAL SPHERICAL WAVELETS; 5-YEAR WMAP DATA; NON-GAUSSIANITY; VIIH MODELS; SPECTRUM ESTIMATION; GABOR TRANSFORMS; MAPS; TEMPERATURE AB We repeat and extend the analysis of Eriksen et al. and Hansen et al., testing the isotropy of the cosmic microwave background fluctuations. We find that the hemispherical power asymmetry previously reported for the largest scales l = 2-40 extends to much smaller scales. In fact, for the full multipole range l = 2-600, significantly more power is found in the hemisphere centered at (theta = 107 degrees +/- 10 degrees, phi = 226 degrees +/- 10 degrees) in galactic co-latitude and longitude than in the opposite hemisphere, consistent with the previously detected direction of asymmetry for l = 2-40. We adopt a model selection test where the direction and amplitude of asymmetry, as well as the multipole range, are free parameters. A model with an asymmetric distribution of power for l = 2-600 is found to be preferred over the isotropic model at the 0.4% significance level, taking into account the additional parameters required to describe it. A similar direction of asymmetry is found independently in all six subranges of 100 multipoles between l = 2-600. None of our 9800 isotropic simulated maps show a similarly consistent direction of asymmetry over such a large multipole range. No known systematic effects or foregrounds are found to be able to explain the asymmetry. C1 [Hansen, F. K.; Eriksen, H. K.; Lilje, P. B.] Univ Oslo, Inst Theoret Astrophys, N-0315 Oslo, Norway. [Hansen, F. K.; Eriksen, H. K.; Lilje, P. B.] Univ Oslo, Ctr Math Applicat, N-0316 Oslo, Norway. [Banday, A. J.] Max Planck Inst Astrophys, D-85741 Garching, Germany. [Banday, A. J.] Ctr Etud Spatiale Rayonnements, 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. [Gorski, K. M.] CALTECH, Pasadena, CA 91125 USA. RP Hansen, FK (reprint author), Univ Oslo, Inst Theoret Astrophys, POB 1029 Blindern, N-0315 Oslo, Norway. EM frodekh@astro.uio.no; banday@MPA-Garching.MPG.DE; Krzysztof.M.Gorski@jpl.nasa.gov; h.k.k.eriksen@astro.uio.no; per.lilje@astro.uio.no RI Lilje, Per/A-2699-2012; OI Lilje, Per/0000-0003-4324-7794 FU Research Council of Norway; NASA Office of Space Science FX We acknowledge the use of the HEALPix (Gorski et al. 2005) package. F. K. H. is thankful for an OYI grant from the Research Council of Norway. We acknowledge the use of the NOTUR super computing facilities. 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 44 TC 102 Z9 103 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 OCT 20 PY 2009 VL 704 IS 2 BP 1448 EP 1458 DI 10.1088/0004-637X/704/2/1448 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 502UQ UT WOS:000270486200034 ER PT J AU Pravdo, SH Tsuboi, Y Uzawa, A Ezoe, Y AF Pravdo, Steven H. Tsuboi, Yohko Uzawa, Akiko Ezoe, Yuichiro TI X-RAYS FROM THE POWER SOURCES OF THE CEPHEUS A STAR-FORMING REGION SO ASTROPHYSICAL JOURNAL LA English DT Article DE infrared: stars; stars: formation; stars: pre-main sequence; X-rays: stars ID HERBIG-HARO OBJECTS; SPITZER-SPACE-TELESCOPE; YOUNG STELLAR POPULATION; OB3 MOLECULAR CLOUD; MAIN-SEQUENCE STARS; RHO-OPHIUCHI CLOUD; A EAST; MASSIVE PROTOSTAR; SOURCE EXTRACTION; INFRARED IMAGES AB We report an observation of X-ray emission from the exciting region of Cepheus A with the Chandra/ACIS instrument. What had been an unresolved X-ray source comprising the putative power sources is now resolved into at least three point-like sources, each with similar X-ray properties and differing radio and submillimeter properties. The sources are HW9, HW3c, and a new source that is undetected at other wavelengths "h10." They each have inferred X-ray luminosities >= 10(31) erg s(-1) with hard spectra, T >= 10(7) K, and high low-energy absorption equivalent to tens to as much as a hundred magnitudes of visual absorption. The star usually assumed to be the most massive and energetic, HW2, is not detected with an upper limit about seven times lower than the detections. The X-rays may arise via thermal bremsstrahlung in diffuse emission regions associated with a gyrosynchrotron source for the radio emission, or they could arise from powerful stellar winds. We also analyzed the Spitzer/IRAC mid-IR observation from this star formation region and present the X-ray results and mid-IR classifications of the nearby stars. HH 168 is not as underluminous in X-rays as previously reported. C1 [Pravdo, Steven H.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Tsuboi, Yohko; Uzawa, Akiko] Chuo Univ, Fac Sci & Engn, Dept Phys, Bunkyo Ku, Tokyo 1128551, Japan. [Ezoe, Yuichiro] Tokyo Metropolitan Univ, Dept Phys, Tokyo 1920397, Japan. RP Pravdo, SH (reprint author), CALTECH, Jet Prop Lab, 306-431,4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM spravdo@jpl.nasa.gov; tsuboi@phys.chuo-u.ac.jp; akiko@phys.chuo-u.ac.jp; ezoe@phys.metro-u.ac.jp FU National Aeronautics and Space Administration; National Science Foundation; NASA [NAS 8-01128]; Ministry of Education, Culture, Sports, Science and Technology [20540237] FX The research described in this paper was performed in part by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. We thank T. Thompson for assistance with the Spitzer data reduction, and G. Garmire and P. Broos for assistance with the Chandra data reduction. This research has made use of the NASA/IPAC Infrared Science Archive including the Spitzer archive, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France. 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 was supported by NASA contract NAS 8-01128. Y.T. acknowledges support from the Grants-in-Aid for Scientific Research (number 20540237) by the Ministry of Education, Culture, Sports, Science and Technology. Y.T. also acknowledges T. Maeda, Y. Sugawara, and H. Kobayashi for help with the data analysis. Government sponsorship acknowledged. NR 66 TC 13 Z9 13 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 20 PY 2009 VL 704 IS 2 BP 1495 EP 1505 DI 10.1088/0004-637X/704/2/1495 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 502UQ UT WOS:000270486200038 ER PT J AU Swain, MR Tinetti, G Vasisht, G Deroo, P Griffith, C Bouwman, J Chen, P Yung, Y Burrows, A Brown, LR Matthews, J Rowe, JF Kuschnig, R Angerhausen, D AF Swain, M. R. Tinetti, G. Vasisht, G. Deroo, P. Griffith, C. Bouwman, J. Chen, Pin Yung, Y. Burrows, A. Brown, L. R. Matthews, J. Rowe, J. F. Kuschnig, R. Angerhausen, D. TI WATER, METHANE, AND CARBON DIOXIDE PRESENT IN THE DAYSIDE SPECTRUM OF THE EXOPLANET HD 209458b SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems; techniques: spectroscopic ID EXTRASOLAR PLANET; HOT JUPITERS; EMISSION-SPECTRUM; ATMOSPHERE; PHOTOMETRY; SIGNATURES; SPACE AB Using the NICMOS instrument on the Hubble Space Telescope, we have measured the dayside spectrum of HD 209458b between 1.5 and 2.5 mu m. The emergent spectrum is dominated by features due to the presence of methane (CH4) and water vapor (H2O), with smaller contributions from carbon dioxide (CO2). Combining this near-infrared spectrum with existing mid-infrared measurements shows the existence of a temperature inversion and confirms the interpretation of previous photometry measurements. We find a family of plausible solutions for the molecular abundance and detailed temperature profile. Observationally resolving the ambiguity between abundance and temperature requires either (1) improved wavelength coverage or spectral resolution of the dayside emission spectrum or (2) a transmission spectrum where abundance determinations are less sensitive to the temperature structure. C1 [Swain, M. R.; Vasisht, G.; Deroo, P.; Chen, Pin; Brown, L. R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Tinetti, G.] UCL, London WC1E 6BT, England. [Griffith, C.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Bouwman, J.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Yung, Y.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Burrows, A.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Matthews, J.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 171, Canada. [Rowe, J. F.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Kuschnig, R.] Univ Vienna, Inst Astron, A-1180 Vienna, Austria. [Angerhausen, D.] Univ Stuttgart, Inst Space Syst, D-70569 Stuttgart, Germany. RP Swain, MR (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. RI Chen, Pin/B-1112-2008; OI Chen, Pin/0000-0003-1195-9666; Tinetti, Giovanna/0000-0001-6058-6654 FU Royal Society FX We appreciate the Director's Time Award for these observations, and we thank Tommy Wiklind, Beth Padillo, and other members of the Space Telescope Science Institute staff for assistance in planning the observations. We also thank Jonathan Tennyson and Bob Barber for help with the water line list. G.T. was supported by the Royal Society. A portion of the research described in this paper was carried out at the Jet Propulsion Laboratory, under a contact with the National Aeronautics and Space Administration. NR 26 TC 144 Z9 147 U1 2 U2 14 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 20 PY 2009 VL 704 IS 2 BP 1616 EP 1621 DI 10.1088/0004-637X/704/2/1616 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 502UQ UT WOS:000270486200045 ER PT J AU Roming, PWA Pritchard, TA Brown, PJ Holland, ST Immler, S Stockdale, CJ Weiler, KW Panagia, N Van Dyk, SD Hoversten, EA Milne, PA Oates, SR Russell, B Vandrevala, C AF Roming, P. W. A. Pritchard, T. A. Brown, P. J. Holland, S. T. Immler, S. Stockdale, C. J. Weiler, K. W. Panagia, N. Van Dyk, S. D. Hoversten, E. A. Milne, P. A. Oates, S. R. Russell, B. Vandrevala, C. TI MULTI-WAVELENGTH PROPERTIES OF THE TYPE IIb SN 2008ax SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE radio continuum: stars; supernovae: individual (SN 2008ax); ultraviolet: stars; X-rays: stars ID SWIFT ULTRAVIOLET/OPTICAL TELESCOPE; HOBBY-EBERLY TELESCOPE; X-RAY-EMISSION; LIGHT CURVES; MASS-LOSS; SUPERNOVA; RADIO; 1993J; EVOLUTION; IB AB We present the UV, optical, X-ray, and radio properties of the Type IIb SN 2008ax discovered in NGC 4490. The observations in the UV are one of the earliest of a Type IIb supernova (SN). On approximately day 4 after the explosion, a dramatic upturn in the u and uvw1 (lambda(c) = 2600 angstrom) light curves occurred after an initial rapid decline which is attributed to adiabatic cooling after the initial shock breakout. This rapid decline and upturn is reminiscent of the Type IIb SN 1993J on day 6 after the explosion. Optical/near-IR spectra taken around the peak reveal prominent H alpha, He I, and Ca II absorption lines. A fading X-ray source is also located at the position of SN 2008ax, implying an interaction of the SN shock with the surrounding circumstellar material and a mass-loss rate of the progenitor of (M) over dot = (9 +/- 3) x 10(-6) M(circle dot) yr(-1). The unusual time evolution (14 days) of the 6 cm peak radio luminosity provides further evidence that themass-loss rate is low. Combining the UV, optical, X-ray, and radio data with models of helium exploding stars implies the progenitor of SN 2008ax was an unmixed star in an interacting binary. Modeling of the SN light curve suggests a kinetic energy (E(k)) of 0.5 x 10(51) erg, an ejecta mass (M(ej)) of 2.9 M(circle dot), and a nickel mass (M(Ni)) of 0.06 M(circle dot). C1 [Roming, P. W. A.; Pritchard, T. A.; Brown, P. J.; Hoversten, E. A.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Holland, S. T.] Univ Space Res Assoc, Columbia, MD 21044 USA. [Holland, S. T.] Ctr Res & Explorat Space Sci & Technol, Greenbelt, MD 20771 USA. [Immler, S.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Immler, S.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Stockdale, C. J.; Vandrevala, C.] Marquette Univ, Dept Phys, Milwaukee, WI 53201 USA. [Weiler, K. W.] USN, Res Lab, Washington, DC 20375 USA. [Panagia, N.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Panagia, N.] Osserv Astrofis Catania, INAF CT, I-95123 Catania, Italy. [Van Dyk, S. D.] CALTECH, Spitzer Sci Ctr, IPAC, Pasadena, CA 91125 USA. [Milne, P. A.] Univ Arizona, Dept Astron, Tucson, AZ 85721 USA. [Oates, S. R.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. [Russell, B.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA. RP Roming, PWA (reprint author), Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA. EM roming@astro.psu.edu OI Van Dyk, Schuyler/0000-0001-9038-9950 FU NASA [NAS5-00136, NNX09AC90G] FX We thank Alicia Soderberg for suggestions regarding this work, which is sponsored at PSU by NASA contract NAS5-00136 and at Marquette by NASA award NNX09AC90G. The HET of UT-Austin, PSU, Stanford, Ludwig-Maximilians-Universitat Munchen, and Georg-August-Universitat Gottingen, is named in honor of William Hobby and Robert Eberly. NR 49 TC 38 Z9 38 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD OCT 20 PY 2009 VL 704 IS 2 BP L118 EP L123 DI 10.1088/0004-637X/704/2/L118 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 508JR UT WOS:000270927500010 ER PT J AU Tenenbaum, ED Milam, SN Woolf, NJ Ziurys, LM AF Tenenbaum, E. D. Milam, S. N. Woolf, N. J. Ziurys, L. M. TI MOLECULAR SURVIVAL IN EVOLVED PLANETARY NEBULAE: DETECTION OF H2CO, c-C3H2, AND C2H IN THE HELIX SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE astrochemistry; ISM: molecules; planetary nebulae: individual (NGC 7293); radio lines: ISM ID CIRCUMSTELLAR ENVELOPE; CARBON-CHEMISTRY; STAR IRC+10216; DIFFUSE CLOUDS; LINE SURVEY; FORMALDEHYDE; ABUNDANCES; NGC-7293; RADICALS; GLOBULES AB H2CO, c-C3H2, and C2H have been identified in the neutral envelope of the highly evolved planetary nebula (PN), the Helix (also know as NGC 7293). Emission from these species were detected toward a peak position in CO, 372 '' east of the central star, using the facilities of the Arizona Radio Observatory (ARO). C2H and c-C3H2 were identified on the basis of their 3 mm transitions, measured with the ARO 12 m, while five lines of H2CO were observed using the 12 m at 2 and 3 mm and the ARO Submillimeter Telescope at 1 mm. From a radiative transfer analysis of the formaldehyde emission, the molecular material was determined to have a density of n(H-2) similar to 3 x 10(5) cm(-3), with a kinetic temperature of T-kin similar to 20 K. Column densities for C2H, H2CO, and c-C3H2 of N-tot similar to 1.4 x 10(13) cm(-2), 1.1 x 10(12) cm(-2), and 3 x 10(11) cm(-2), respectively, were derived, corresponding to fractional abundances relative to H-2 of f(H2CO) = 1 x 10(-7) , f (c-C3H2) = 3 x 10(-8), and f (C2H) = 1 x 10(-6). The physical conditions found support the notion that molecules in evolved PNe survive in dense clumps in pressure equilibrium, shielded from photodissociation. The presence of H2CO, c-C3H2, and C2H, along with the previously observed species CN, HNC, HCN, and HCO+, indicates that a relatively complex chemistry can occur in the late stages of PN evolution, despite potentially destructive ultraviolet radiation. These molecules have also been observed in diffuse clouds, suggesting a possible connection between molecular material in evolved PNe and the diffuse ISM. C1 [Tenenbaum, E. D.; Woolf, N. J.; Ziurys, L. M.] Univ Arizona, Dept Astron, Tucson, AZ 85721 USA. [Tenenbaum, E. D.; Woolf, N. J.; Ziurys, L. M.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Tenenbaum, E. D.; Ziurys, L. M.] Univ Arizona, Dept Chem & Biochem, Tucson, AZ 85721 USA. [Milam, S. N.] NASA, Ames Res Ctr, SETI Inst, Moffett Field, CA 94035 USA. [Ziurys, L. M.] Univ Arizona, Arizona Radio Observ, Tucson, AZ 85721 USA. RP Tenenbaum, ED (reprint author), Univ Arizona, Dept Astron, 933 N Cherry Ave, Tucson, AZ 85721 USA. EM emilyt@as.arizona.edu; Stefanie.N.Milam@nasa.gov; nwoolf@as.arizona.edu; lziurys@as.arizona.edu RI Milam, Stefanie/D-1092-2012 OI Milam, Stefanie/0000-0001-7694-4129 FU NSF [AST-0607803] FX We thank A. Faure and N. Troscompt for their unpublished para-H2CO collisional rates. This research is funded by NSF grant AST-0607803. E. D. T. acknowledges support from the NSF Graduate Research Fellowship Program. NR 37 TC 21 Z9 21 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD OCT 20 PY 2009 VL 704 IS 2 BP L108 EP L112 DI 10.1088/0004-637X/704/2/L108 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 508JR UT WOS:000270927500008 ER PT J AU Veerapaneni, SK Gueyffier, D Biros, G Zorin, D AF Veerapaneni, Shravan K. Gueyffier, Denis Biros, George Zorin, Denis TI A numerical method for simulating the dynamics of 3D axisymmetric vesicles suspended in viscous flows SO JOURNAL OF COMPUTATIONAL PHYSICS LA English DT Article DE Particulate flows; Integral equations; Axisymmetric flows; Numerical methods; Fluid membranes; Inextensible vesicles; Moving boundaries ID FLUID MEMBRANES; MODEL AB We extend [Shravan K. Veerapaneni, Denis Gueyffier, Denis Zorin, George Biros, A boundary integral method for simulating the dynamics of inextensible vesicles suspended in a viscous fluid in 21), journal of Computational Physics 228(7) (2009) 2334-2353] to the case of three-dimensional axisymmetric vesicles of spherical or toroidal topology immersed in viscous flows. Although the main components of the algorithm are similar in spirit to the 2D case-spectral approximation in space, semi-implicit time-stepping scheme-the main differences are that the bending and viscous force require new analysis, the linearization for the semi-implicit schemes must be redeived, a fully implicit scheme must be used for the toroidal topology to eliminate a CFL-type restriction and a novel numerical scheme for the evaluation of the 3D Stokes single layer potential on an axisymmetric surface is necessary to speed up the calculations. By introducing these novel components, we obtain a time-scheme that experimentally is unconditionally stable, has low cost per time step, and is third-order accurate in time. We present numerical results to analyze the cost and convergence rates of the scheme. To verify the solver, we compare it to a constrained variational approach to compute equilibrium shapes that does not involve interactions with a viscous fluid. To illustrate the applicability of method, we consider a few vesicle-flow interaction problems: the sedimentation of a vesicle, interactions of one and three vesicles with a background Poiseuille flow. (C) 2009 Elsevier Inc. All rights reserved. C1 [Veerapaneni, Shravan K.; Zorin, Denis] NYU, Courant Inst Math Sci, New York, NY 10012 USA. [Gueyffier, Denis] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Biros, George] Georgia Inst Technol, Coll Comp, Atlanta, GA 30332 USA. RP Veerapaneni, SK (reprint author), NYU, Courant Inst Math Sci, 251 Mercer St, New York, NY 10012 USA. EM shravan@cims.nyu.edu; dgueyffier@giss.nasa.gov; gbiros@gmail.com; dzorin@cims.nyu.edu RI Gueyffier, Denis/I-4265-2014 OI Gueyffier, Denis/0000-0002-4759-3857 NR 26 TC 34 Z9 34 U1 0 U2 23 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 OCT 20 PY 2009 VL 228 IS 19 BP 7233 EP 7249 DI 10.1016/j.jcp.2009.06.020 PG 17 WC Computer Science, Interdisciplinary Applications; Physics, Mathematical SC Computer Science; Physics GA 491MF UT WOS:000269582300007 ER PT J AU Muniz, AR Meyyappan, M Maroudas, D AF Muniz, Andre R. Meyyappan, M. Maroudas, Dimitrios TI On the hydrogen storage capacity of carbon nanotube bundles SO APPLIED PHYSICS LETTERS LA English DT Article ID ATOMIC-HYDROGEN; GLOW-DISCHARGE; HIGH COVERAGES; FUNCTIONALIZATION; CHEMISORPTION; ADSORPTION AB An analytical model is presented to describe the effect of carbon nanotube (CNT) swelling upon hydrogenation on the hydrogen storage capacity of single-walled CNT bundles; the model is properly parameterized using atomistic calculations for the relationship between CNT swelling and the degree of hydrogenation as measured by the coverage of the CNTs by chemisorbed atomic H. The model generates experimentally testable hypotheses, which can be used to explain the lower H storage capacities reported for CNT bundles and the experimentally observed nonuniformity of hydrogenation of CNT bundles. (C) 2009 American Institute of Physics. [doi: 10.1063/1.3253711] C1 [Muniz, Andre R.; Maroudas, Dimitrios] Univ Massachusetts, Dept Chem Engn, Amherst, MA 01003 USA. [Meyyappan, M.] NASA, Ames Res Ctr, Ctr Nanotechnol, Moffett Field, CA 94035 USA. RP Maroudas, D (reprint author), Univ Massachusetts, Dept Chem Engn, Amherst, MA 01003 USA. EM maroudas@ecs.umass.edu OI Muniz, Andre/0000-0002-8784-012X FU National Science Foundation [CMMI-0531171, CBET-0613501]; CAPES FX This work was supported by the National Science Foundation through Grant Nos. CMMI-0531171 and CBET-0613501 and by a CAPES/Fulbright Fellowship to A. R. M. NR 18 TC 12 Z9 12 U1 0 U2 6 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 J9 APPL PHYS LETT JI Appl. Phys. Lett. PD OCT 19 PY 2009 VL 95 IS 16 AR 163111 DI 10.1063/1.3253711 PG 3 WC Physics, Applied SC Physics GA 512BU UT WOS:000271218200053 ER PT J AU Dou, XK Li, T Xu, JY Liu, HL Xue, XH Wang, S Leblanc, T McDermid, IS Hauchecorne, A Keckhut, P Bencherif, H Heinselman, C Steinbrecht, W Mlynczak, MG Russell, JM AF Dou, Xiankang Li, Tao Xu, Jiyao Liu, Han-Li Xue, Xianghui Wang, Shui Leblanc, Thierry McDermid, I. Stuart Hauchecorne, Alain Keckhut, Philippe Bencherif, Hassan Heinselman, Craig Steinbrecht, Wolfgang Mlynczak, M. G. Russell, J. M., III TI Seasonal oscillations of middle atmosphere temperature observed by Rayleigh lidars and their comparisons with TIMED/SABER observations SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID SEMIANNUAL OSCILLATION; MESOSPHERIC TEMPERATURES; EQUATORIAL WAVES; LOW-LATITUDES; CLIMATOLOGY; TIDES; OZONE; WIND; UARS AB The long-term temperature data sets obtained by Rayleigh lidars at six different locations from low to high latitudes within the Network for the Detection of Atmospheric Composition Change (NDACC) were used to derive the annual oscillations (AO) and semiannual oscillations (SAO) of middle atmosphere temperature: Reunion Island (21.8 degrees S); Mauna Loa Observatory, Hawaii (19.5 degrees N); Table Mountain Facility, California (34.4 degrees N); Observatoire de Haute Provence, France (43.9 degrees N); Hohenpeissenberg, Germany (47.8 degrees N); Sondre Stromfjord, Greenland (67.0 degrees N). The results were compared with those derived from the Sounding of the Atmosphere using Broadband Emission Radiometry (SABER) instrument onboard the Thermosphere-Ionosphere-Mesosphere Energetics and Dynamics (TIMED) satellite. The zonal mean temperatures at similar latitudes show good agreement. The observations also reveal that the AO dominates the seasonal oscillations in both the stratosphere and the mesosphere at middle and high latitudes, with the amplitudes increasing poleward. The SAO oscillations are weaker at all six sites. The oscillations in the upper mesosphere are usually stronger than those in the upper stratosphere with a local minimum near 50-65 km. The upper mesospheric signals are clearly out of phase with upper stratospheric signals. Some differences between lidar and SABER results were found in both the stratosphere and mesosphere. These could be due to: the difference in data sampling between ground-based and space-based instruments, the length of data set, the tidal aliasing owing to the temperature AO and SAO since lidar data are nighttime only, and lidar temperature analysis algorithms. The seasonal oscillations of tidal amplitudes derived from SABER observations suggests that the tidal aliasing of the lidar temperature AO and SAO in the upper mesosphere may over- or under-estimate the real temperature oscillations, depending on the tidal phases. In addition, the possibly unrealistic seasonal oscillations embedded in the climatological models (e.g., MSIS or CIRA) at the reference point for lidar temperature analysis may also affect the lidar results in the top part of the profiles (usually in the upper mesosphere). C1 [Dou, Xiankang; Li, Tao; Xue, Xianghui; Wang, Shui] Univ Sci & Technol China, Sch Earth & Space Sci, Natl Geophys Observ, Hefei 230026, Anhui, Peoples R China. [Xu, Jiyao] Chinese Acad Sci, Key Lab Space Weather, Beijing 100080, Peoples R China. [Liu, Han-Li] Natl Ctr Atmospher Res, High Altitude Observ, Boulder, CO 80301 USA. [Leblanc, Thierry; McDermid, I. Stuart] CALTECH, Jet Prop Lab, Table Mt Facil, Wrightwood, CA 92397 USA. [Hauchecorne, Alain; Keckhut, Philippe] CNRS, Inst Pierre Simon Laplace, Serv Aeron, F-91371 Verrieres Le Buisson, France. [Bencherif, Hassan] Univ La Reunion, Lab Atmosphere & Cyclones, F-97715 St Denis, France. [Heinselman, Craig] SRI Int, Menlo Pk, CA 94025 USA. [Steinbrecht, Wolfgang] German Weather Serv, Meteorol Observ Hohenpeissenberg, D-82383 Hohenpeissenberg, Germany. [Mlynczak, M. G.] NASA, Langley Res Ctr, Hampton, VA 23681 USA. [Russell, J. M., III] Hampton Univ, Ctr Atmospher Sci, Hampton, VA 23668 USA. RP Dou, XK (reprint author), Univ Sci & Technol China, Sch Earth & Space Sci, Natl Geophys Observ, 96 Jinzhai Rd, Hefei 230026, Anhui, Peoples R China. EM litao@ustc.edu.cn RI Liu, Han-Li/A-9549-2008; Bencherif, Hassan/F-1671-2010; Steinbrecht, Wolfgang/G-6113-2010; Mlynczak, Martin/K-3396-2012; Hauchecorne, Alain/A-8489-2013; Dou, xiankang/M-9106-2013; Li, Tao/J-8950-2014; Xue, Xianghui/E-1225-2012 OI Liu, Han-Li/0000-0002-6370-0704; Steinbrecht, Wolfgang/0000-0003-0680-6729; Li, Tao/0000-0002-5100-4429; Xue, Xianghui/0000-0002-4541-9900 FU University of Science and Technology of China; Chinese Academy of Sciences ( CAS) [kzcx2-yw-123]; National Natural Sciences Foundation of China (NSFC) [40674087, 40890165]; China Meteorological Administration [GYHY20070613]; NSFC [40974084]; CAS; European Commission [FOP6-2005-Global-4-036677]; University Corporation for Atmospheric; National Science Foundation FX The work described in this paper was carried out at the University of Science and Technology of China with the support of Chinese Academy of Sciences ( CAS) KIP Pilot project kzcx2-yw-123, National Natural Sciences Foundation of China (NSFC) funds 40674087 and 40890165, China Meteorological Administration grant GYHY20070613, NSFC fund 40974084, and the CAS One Hundred Talent Program. The lidar temperature data are archived at the NDACC Data and Handling Facility and are publicly available (see http://www.ndacc.org). We acknowledge the support of the European Commission through the GEO-MON Integrated Project under the Sixth Framework Program ( contract FOP6-2005-Global-4-036677). The National Center for Atmospheric Research is operated by the University Corporation for Atmospheric Research under the sponsorship of the National Science Foundation. NR 32 TC 12 Z9 13 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 OCT 17 PY 2009 VL 114 AR D20103 DI 10.1029/2008JD011654 PG 11 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 508OX UT WOS:000270943800001 ER PT J AU Wilson, LB Cattell, CA Kellogg, PJ Goetz, K Kersten, K Kasper, JC Szabo, A Meziane, K AF Wilson, L. B., III Cattell, C. A. Kellogg, P. J. Goetz, K. Kersten, K. Kasper, J. C. Szabo, A. Meziane, K. TI Low-frequency whistler waves and shocklets observed at quasi-perpendicular interplanetary shocks SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID EARTHS BOW SHOCK; AMPLITUDE MAGNETIC-STRUCTURES; COLLISIONLESS SHOCKS; ISEE-2 OBSERVATIONS; UPSTREAM WAVES; SOLAR-WIND; PARALLEL SHOCK; IONS UPSTREAM; FORESHOCK; PLASMA AB We present observations of low-frequency waves (0.25 Hz < f < 10 Hz) at five quasi-perpendicular interplanetary (IP) shocks observed by the Wind spacecraft. Four of the five IP shocks had oblique precursor whistler waves propagating at angles with respect to the magnetic field of 20 degrees-50 degrees and large propagation angles with respect to the shock normal; thus they do not appear to be phase standing. One event, the strongest in our study and likely supercritical, had low-frequency waves consistent with steepened magnetosonic waves called shocklets. The shocklets are seen in association with diffuse ion distributions. Both the shocklets and precursor whistlers are often seen simultaneously with anisotropic electron distributions unstable to the whistler heat flux instability. The IP shock with upstream shocklets showed much stronger electron heating across the shock ramp than the four events without upstream shocklets. These results may offer new insights into collisionless shock dissipation and wave-particle interactions in the solar wind. C1 [Wilson, L. B., III; Cattell, C. A.; Kellogg, P. J.; Goetz, K.; Kersten, K.] Univ Minnesota, Dept Phys & Astron, Minneapolis, MN 55455 USA. [Kasper, J. C.] Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Szabo, A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Meziane, K.] Univ New Brunswick, Dept Phys, Fredericton, NB E3B 5A3, Canada. RP Wilson, LB (reprint author), Univ Minnesota, Dept Phys & Astron, 116 Church St SE, Minneapolis, MN 55455 USA. EM wilson@physics.umn.edu; cattell@fields.space.umn.edu; pauljkellogg@gmail.com; goetz@umn.edu; kkersten@physics.umn.edu; jkasper@cfa.harvard.edu; adam.szabo-1@nasa.gov; karim@unb.ca RI Kasper, Justin/D-1152-2010; Wilson III, Lynn/D-4425-2012; OI Kasper, Justin/0000-0002-7077-930X; Wilson III, Lynn/0000-0002-4313-1970; Cattell, Cynthia/0000-0002-3805-320X FU NESSF [NNX07AU72H, NNX07AI05G] FX [49] Zuyin Pu thanks the reviewers for their assistance in evaluating this paper. NR 38 TC 33 Z9 33 U1 1 U2 6 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD OCT 17 PY 2009 VL 114 AR A10106 DI 10.1029/2009JA014376 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 508PK UT WOS:000270945100004 ER PT J AU Thorn, DB Gu, MF Brown, GV Beiersdorfer, P Porter, FS Kilbourne, CA Kelley, RL AF Thorn, Daniel B. Gu, Ming F. Brown, Gregory V. Beiersdorfer, Peter Porter, F. Scott Kilbourne, Caroline A. Kelley, Richard L. TI Precision Measurement of the K-Shell Spectrum from Highly Charged Xenon with an Array of X-Ray Calorimeters SO PHYSICAL REVIEW LETTERS LA English DT Article ID HELIUM-LIKE IONS; CONFIGURATION-INTERACTION CALCULATIONS; LAMB SHIFT; GROUND-STATE; FE-XXV; HYDROGENLIKE; URANIUM; MICROCALORIMETER; TRANSITIONS; ENERGIES AB We present a measurement of the K-shell spectrum from highly charged xenon ions recorded with a high-energy x-ray calorimeter spectrometer array that can distinguish between various theories for the atomic structure of the two electron system. The array was designed to provide high resolution with high quantum efficiency in the 10-60 keV x-ray range which allows us to resolve blends that afflicted previous measurements. A precision of better than 2 eV was achieved in the measurement of the Xe(52+) and Xe(53+) K-shell transitions located near 31 keV, which is an order of magnitude better than previously reported. C1 [Thorn, Daniel B.; Gu, Ming F.; Brown, Gregory V.; Beiersdorfer, Peter] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA. [Porter, F. Scott; Kilbourne, Caroline A.; Kelley, Richard L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Thorn, DB (reprint author), Extreme Matter Inst, Darmstadt, Germany. EM dbthorn@gsi.de RI Porter, Frederick/D-3501-2012; Kelley, Richard/K-4474-2012 OI Porter, Frederick/0000-0002-6374-1119; FU U.S. Department of Energy by Lawrence Livermore National Laboratory [DE-AC52-07NA27344]; NASA Astronomy and Physics Research and Analysis Program (APRA); NASA/GSFC FX We gratefully acknowledge fruitful discussions with Mau Chen, as well as expert technical support on EBIT by Ed Magee, and thank John Gygax and Jonathan King for help in building and designing the ECS spectrometer. This work was performed under the auspices of the U.S. Department of Energy by Lawrence Livermore National Laboratory under Contract No. DE-AC52-07NA27344 and supported by NASA Astronomy and Physics Research and Analysis Program (APRA) grants to LLNL and NASA/GSFC. NR 30 TC 17 Z9 17 U1 0 U2 5 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 0031-9007 J9 PHYS REV LETT JI Phys. Rev. Lett. PD OCT 16 PY 2009 VL 103 IS 16 AR 163001 DI 10.1103/PhysRevLett.103.163001 PG 4 WC Physics, Multidisciplinary SC Physics GA 508AP UT WOS:000270899500019 PM 19905691 ER PT J AU Nicolau, E Gonzalez-Gonzalez, I Flynn, M Griebenow, K Cabrera, CR AF Nicolau, Eduardo Gonzalez-Gonzalez, Ileana Flynn, Michael Griebenow, Kai Cabrera, Carlos R. TI Bioelectrochemical degradation of urea at platinized boron doped diamond electrodes for bioregenerative systems SO ADVANCES IN SPACE RESEARCH LA English DT Article DE Urea; Wastewater; Bioelectrochemistry; Boron-doped diamond; Urease; Bioreactor ID AMMONIA OXIDATION; ELECTROCHEMISTRY; ELECTROCATALYSTS; CREATININE; SPACE AB The recovery of potable water from space mission wastewater is critical for the life support and environmental health of crew members in long-term missions. NASA estimates reveal that at manned space missions 1.91 kg/person day of urine is produced, with urea and various salts as its main components. In this research we explore the utilization of urease (EC 3.5.1.5, 15,000 U/g) along with a platinized boron doped diamond electrode (Pt-BDD) to degrade urea. Urea is directly degraded to nitrogen by the in situ utilization of the reaction products as a strategy to increase the amount of clean water in future space expeditions. The biochemical reaction of urease produces ammonia and carbon dioxide from urea. Thereafter, ammonia is electrooxidized at the interface of the Pt-BDD producing molecular nitrogen. The herein presented system has been proven to have 20% urea conversion efficiency. This research has potential applications for future long-term space missions since the reaction byproducts could be used for a biomass subsystem (in situ resource recovery), while generating electricity from the same process. (C) 2009 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 [Nicolau, Eduardo; Gonzalez-Gonzalez, Ileana; Griebenow, Kai; Cabrera, Carlos R.] Univ Puerto Rico, Dept Chem, Rio Piedras, PR 00931 USA. [Nicolau, Eduardo; Gonzalez-Gonzalez, Ileana; Griebenow, Kai; Cabrera, Carlos R.] Univ Puerto Rico, NASA Ctr Adv Nanoscale Mat, Rio Piedras, PR 00931 USA. [Flynn, Michael] NASA, Ames Res Ctr, Bioengn Branch, Moffett Field, CA 94035 USA. RP Griebenow, K (reprint author), Univ Puerto Rico, Dept Chem, Rio Piedras Campus,POB 23346, Rio Piedras, PR 00931 USA. EM kai.griebenow@gmail.com; ccabrera@uprrp.edu OI Cabrera, Carlos/0000-0002-3342-8666 FU NASA Center for Advanced Nanoscale Materials [NNX08BA48A] FX This work was financially supported in part by NASA Center for Advanced Nanoscale Materials under Grant No. NNX08BA48A and the NASA Graduate Student Researchers Program under Grant No. NNX08AV42H. The authors also acknowledge the UPR Materials Characterization Center and its personnel for their technical help during the attainment of thiswork. E. Nicolau acknowledges Jos6 Fonseca-Vega for his help and useful discussions. NR 22 TC 7 Z9 9 U1 3 U2 26 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0273-1177 J9 ADV SPACE RES JI Adv. Space Res. PD OCT 15 PY 2009 VL 44 IS 8 BP 965 EP 970 DI 10.1016/j.asr.2009.04.003 PG 6 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA 504UW UT WOS:000270644300011 ER PT J AU Kim, HI Kim, H Pang, ES Ryu, EK Beegle, LW Loo, JA Goddard, WA Kanik, I AF Kim, Hugh I. Kim, Hyungjun Pang, Eric S. Ryu, Ernest K. Beegle, Luther W. Loo, Joseph A. Goddard, William A. Kanik, Isik TI Structural Characterization of Unsaturated Phosphatidylcholines Using Traveling Wave Ion Mobility Spectrometry SO ANALYTICAL CHEMISTRY LA English DT Article ID MASS-SPECTROMETRY; ELECTROSPRAY-IONIZATION; GAS-PHASE; DRIFT-GAS; PHOSPHORYLATED PEPTIDES; PROTEIN COMPLEXES; SELECTIVITY; SEPARATION; DYNAMICS; TOFMS AB A number of phosphatidylcholine (PC) cations spanning a mass range of 400-1000 Da are investigated using electrospray ionization mass spectrometry coupled with traveling wave ion mobility spectrometry (TWIMS). A high correlation between mass and mobility is demonstrated with saturated phosphatidylcholine cations in N(2). A significant deviation from this mass-mobility correlation line is observed for the unsaturated PC cation. We found that the double bond in the acyl chain causes a 5% reduction in drift time. The drift time is reduced at a rate of similar to 1% for each additional double bond. Theoretical collision cross sections of PC cations exhibit good agreement with experimentally evaluated values. Collision cross sections are determined using the recently derived relationship between mobility and drift time in TWIMS stacked ring ion guide (SRIG) and compared to estimated collision cross sections using an empiric calibration method. Computational analysis was performed using the modified trajectory (TJ) method with nonspherical. N(2) molecules as the drift gas. The difference between estimated collision cross sections and theoretical collision cross sections of PC cations is related to the sensitivity of the PC cation collision cross sections to the details of the ion-neutral interactions. ne origin of the observed correlation and deviation between mass and mobility of PC cations is discussed in terms of the structural rigidity of these molecules using molecular dynamic simulations. C1 [Kim, Hugh I.; Ryu, Ernest K.; Beegle, Luther W.; Kanik, Isik] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Kim, Hyungjun; Goddard, William A.] CALTECH, Beckman Inst, Mat & Proc Simulat Ctr, Pasadena, CA 91125 USA. [Pang, Eric S.; Loo, Joseph A.] Univ Calif Los Angeles, Dept Chem & Biochem, Los Angeles, CA 90095 USA. RP Kim, HI (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM hugh.i.kim@jpl.nasa.gov RI Beegle, Luther/A-6354-2010; Kim, Hugh/G-4476-2011; Kim, Hyungjun/B-4527-2013 FU NASA's Astrobiology Science and Technology Instrument Developmen Planetary Instrument Definition and Development; Mars Instrument Development programs; NIH [RR20004]; National Research Foundation of Korea funded by the Ministry of Education, Science and Technology [R31-2008-000-10055-0] 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), The University of California Los Angeles Mass Spectrometry and Proteomics Technology Center, and the Material and Process Simulation Center, Beckman Institute, California Institute of Technology. Financial support through NASA's Astrobiology Science and Technology Instrument Developmen Planetary Instrument Definition and Development, and Mars Instrument Development programs is gratefully acknowledged. J.A.L. acknowledges support from the NIH (RR20004). H.K and W.A.G. acknowledge support from the WCU (World Class University) program through the National Research Foundation of Korea funded by the Ministry of Education, Science and Technology (R31-2008-000-10055-0). H.LK and H.K. contributed equally to this work. NR 48 TC 41 Z9 41 U1 2 U2 23 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0003-2700 J9 ANAL CHEM JI Anal. Chem. PD OCT 15 PY 2009 VL 81 IS 20 BP 8289 EP 8297 DI 10.1021/ac900672a PG 9 WC Chemistry, Analytical SC Chemistry GA 505DZ UT WOS:000270670600004 PM 19764704 ER PT J AU La Duc, MT Osman, S Vaishampayan, P Piceno, Y Andersen, G Spry, JA Venkateswaran, K AF La Duc, Myron T. Osman, Shariff Vaishampayan, Parag Piceno, Yvette Andersen, Gary Spry, J. A. Venkateswaran, Kasthuri TI Comprehensive Census of Bacteria in Clean Rooms by Using DNA Microarray and Cloning Methods SO APPLIED AND ENVIRONMENTAL MICROBIOLOGY LA English DT Article ID MICROBIAL DIVERSITY; SEQUENCE DATA; ENVIRONMENT; SPACECRAFT; ARB AB A census of clean room surface-associated bacterial populations was derived from the results of both the cloning and sequencing of 16S rRNA genes and DNA microarray (PhyloChip) analyses. Samples from the Lockheed Martin Aeronautics Multiple Testing Facility (LMA-MTF), the Kennedy Space Center Payload Hazard and Servicing Facility (KSC-PHSF), and the Jet Propulsion Laboratory Spacecraft Assembly Facility (JPL-SAF) clean rooms were collected during the various assembly phases of the Phoenix and Mars Science Laboratory (MSL) spacecraft. Clone library-derived analyses detected a larger bacterial diversity prior to the arrival of spacecraft hardware in these clean room facilities. PhyloChip results were in agreement with this trend but also unveiled the presence of anywhere from 9- to 70-fold more bacterial taxa than cloning approaches. Among the facilities sampled, the JPL-SAF (MSL mission) housed a significantly less diverse bacterial population than either the LMA-MTF or KSC-PHSF (Phoenix mission). Bacterial taxa known to thrive in arid conditions were frequently detected in MSL-associated JPL-SAF samples, whereas proteobacterial lineages dominated Phoenix-associated KSC-PHSF samples. Comprehensive bacterial censuses, such as that reported here, will help space-faring nations preemptively identify contaminant biomatter that may compromise extraterrestrial life detection experiments. The robust nature and high sensitivity of DNA microarray technologies should prove beneficial to a wide range of scientific, electronic, homeland security, medical, and pharmaceutical applications and to any other ventures with a vested interest in monitoring and controlling contamination in exceptionally clean environments. C1 [La Duc, Myron T.; Vaishampayan, Parag; Spry, J. A.; Venkateswaran, Kasthuri] CALTECH, Jet Prop Lab, NASA, Biotechnol & Planetary Protect Grp, Pasadena, CA 91109 USA. [Osman, Shariff; Piceno, Yvette; Andersen, Gary] Lawrence Berkeley Natl Lab, Berkeley, CA USA. RP Venkateswaran, K (reprint author), CALTECH, Jet Prop Lab, NASA, Biotechnol & Planetary Protect Grp, Mail Stop 89,Oak Grove Dr, Pasadena, CA 91109 USA. EM kjvenkat@jpl.nasa.gov RI Piceno, Yvette/I-6738-2016; Andersen, Gary/G-2792-2015 OI Piceno, Yvette/0000-0002-7915-4699; Andersen, Gary/0000-0002-1618-9827 FU [DE-AC02-05CH11231] FX We thank K. Buxbaum and C. Conley for valuable advice and encouragement. We also thank Todd DeSantis for his input and support using the Greengenes suite of tools (www.greengenes.lbl.gov). NR 36 TC 49 Z9 49 U1 0 U2 11 PU AMER SOC MICROBIOLOGY PI WASHINGTON PA 1752 N ST NW, WASHINGTON, DC 20036-2904 USA SN 0099-2240 J9 APPL ENVIRON MICROB JI Appl. Environ. Microbiol. PD OCT 15 PY 2009 VL 75 IS 20 BP 6559 EP 6567 DI 10.1128/AEM.01073-09 PG 9 WC Biotechnology & Applied Microbiology; Microbiology SC Biotechnology & Applied Microbiology; Microbiology GA 503QD UT WOS:000270552500018 PM 19700540 ER PT J AU Zak, M AF Zak, Michail TI Quantum-inspired teleportation SO CHAOS SOLITONS & FRACTALS LA English DT Article AB Based upon quantum-inspired entanglement in quantum-classical hybrids, a simple algorithm for instantaneous transmissions of non-intentional messages (chosen at random) to remote distances is proposed. A special class of situations when such transmissions are useful is outlined. Application of such a quantum-inspired teleportation, i.e. instantaneous transmission of conditional information on remote distances for security of communications is discussed. Similarities and differences between quantum systems and quantum-classical hybrids are emphasized. (C) 2009 Published by Elsevier Ltd. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Zak, M (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM michail.zak@gmail.com FU National Aeronautics and Space Administration FX The research described in this paper was performed at Jet Propulsion Laboratory California Institute of Technology under contract with National Aeronautics and Space Administration. NR 12 TC 1 Z9 1 U1 1 U2 4 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0960-0779 J9 CHAOS SOLITON FRACT JI Chaos Solitons Fractals PD OCT 15 PY 2009 VL 42 IS 1 BP 306 EP 315 DI 10.1016/j.chaos.2008.12.003 PG 10 WC Mathematics, Interdisciplinary Applications; Physics, Multidisciplinary; Physics, Mathematical SC Mathematics; Physics GA 514YZ UT WOS:000271434200042 ER PT J AU Bland, PA Jackson, MD Coker, RF Cohen, BA Webber, JBW Lee, MR Duffy, CM Chater, RJ Ardakani, MG McPhail, DS McComb, DW Benedix, GK AF Bland, Philip A. Jackson, Matthew D. Coker, Robert F. Cohen, Barbara A. Webber, J. Beau W. Lee, Martin R. Duffy, Christina M. Chater, Richard J. Ardakani, Mahmoud G. McPhail, David S. McComb, David W. Benedix, Gretchen K. TI Why aqueous alteration in asteroids was isochemical: High porosity not equal high permeability SO EARTH AND PLANETARY SCIENCE LETTERS LA English DT Article DE meteorite; carbonaceous chondrite; asteroidal alteration; permeability; isochemical alteration; fluid flow; closed/open system ID CHONDRITE PARENT BODIES; EARLY SOLAR-SYSTEM; OXYGEN ISOTOPIC COMPOSITION; X-RAY-DIFFRACTION; CARBONACEOUS CHONDRITES; MODAL MINERALOGY; CM2 CHONDRITES; CI CHONDRITES; METEORITES; CHONDRULES AB Carbonaceous chondrite meteorites are the most compositionally primitive rocks in the solar system, but the most chemically pristine (Cl1 and CM2 chondrites) have experienced pervasive aqueous alteration, apparently within asteroid parent bodies. Unfractionated soluble elements suggest very limited flow of liquid water, indicting a closed-system at scales large than 100's mu m, consistent with data from oxygen isotopes, and meteorite petrography. However, numerical studies persistently predict large-scale (10's km) water transport in model asteroids, either in convecting cells, or via 'exhalation' flow - an open-system at scales up to 10's km. These models have tended to use permeabilites in the range 10(-13) to 10(-11) m(2). we show that the permeability of plausible chondritic starting materials lies in the range 10(-19) to 10(-17) m(2) (0.1-10 mu D): around six orders-of-magnitude lower than previously assumed. This low permeability is largely a result of the extreme fine grain-size of primitive chondritic materials. Applying these permeability estimates in numerical models, we predict very limited liquid water flow (distances of 100's mu m at most), even in a high porosity, water-saturated asteroid, with a high thermal gradient, over millions of years. Isochemical alteration, with flow over minimal lengthscales, is not a special circumstance. It is inevitable, once we consider the fundamental material properties of these rocks. To achieve large-scale flow it would require average matrix grain sizes in primitive materials of 10's-100's mu m - orders of magnitude larger than observed. Finally, in addition to reconciling numerical modelling with meteorite data, our work explains several other features of these enigmatic rocks, most particularly, why the most chemically primitive meteorites are also the most altered. (C) 2009 Elsevier B.V. All rights reserved. C1 [Bland, Philip A.; Jackson, Matthew D.; Duffy, Christina M.] Univ London Imperial Coll Sci Technol & Med, IARC, Dept Earth Sci & Engn, London SW7 2AZ, England. [Bland, Philip A.; Benedix, Gretchen K.] Nat Hist Museum, Dept Mineral, IARC, London SW7 5BD, England. [Coker, Robert F.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA. [Cohen, Barbara A.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. [Webber, J. Beau W.] Univ Kent, Sch Phys Sci, Canterbury CT2 7NR, Kent, England. [Webber, J. Beau W.] Inst Petr Engn, Edinburgh EH14 4AS, Midlothian, Scotland. [Lee, Martin R.] Univ Glasgow, Dept Geog & Earth Sci, Glasgow G12 8QQ, Lanark, Scotland. [Chater, Richard J.; Ardakani, Mahmoud G.; McPhail, David S.; McComb, David W.] Univ London Imperial Coll Sci Technol & Med, Dept Mat, London SW7 2AZ, England. RP Bland, PA (reprint author), Univ London Imperial Coll Sci Technol & Med, IARC, Dept Earth Sci & Engn, S Kensington Campus, London SW7 2AZ, England. EM p.a.bland@imperial.ac.uk RI Lee, Martin/D-9169-2011; Jackson, Matthew/N-5121-2014; Webber, J B W/C-4317-2008; McComb, David/A-7808-2010; OI Lee, Martin/0000-0002-6004-3622; Webber, J B W/0000-0002-8967-4671; Benedix, Gretchen/0000-0003-0990-8878 FU Royal Society; Science & Technology Facilities Council (STFC) [PPA/G/S/2003/00071] FX We acknowledge the financial support from the Royal Society, and the Science & Technology Facilities Council (STFC) under grant number PPA/G/S/2003/00071: PAB thanks Ed Young and Richard Ash for the numerous useful discussions on this topic. The final draft of the paper benefited from comments by two anonymous reviewers. NR 66 TC 45 Z9 45 U1 2 U2 15 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0012-821X J9 EARTH PLANET SC LETT JI Earth Planet. Sci. Lett. PD OCT 15 PY 2009 VL 287 IS 3-4 BP 559 EP 568 DI 10.1016/j.epsl.2009.09.004 PG 10 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 522PQ UT WOS:000272010800029 ER PT J AU Szynkiewicz, A Moore, CH Glamoclija, M Pratt, LM AF Szynkiewicz, Anna Moore, Craig H. Glamoclija, Mihaela Pratt, Lisa M. TI Sulfur isotope signatures in gypsiferous sediments of the Estancia and Tularosa Basins as indicators of sulfate sources, hydrological processes, and microbial activity SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Article ID RIO-GRANDE RIFT; SOUTHWESTERN NORTH-AMERICA; SANDS DUNE FIELD; NEW-MEXICO; MERIDIANI-PLANUM; OMEGA/MARS EXPRESS; INORGANIC SULFUR; BURNS FORMATION; MARINE SULFATE; ICE AGES AB In order to reconstruct paleo-environmental conditions for the saline playa lakes of the Rio Grande Rift, we investigated sediment sulfate sources using sulfur isotope compositions of dissolved SO(4)(2-) ions in modern surface water, groundwater, and SO(4)(2-) precipitated in the form of gypsum sediments deposited during the Pleistocene and Holocene in the Tularosa and Estancia Basins. The major sulfate sources are Lower and Middle Permian marine evaporites (delta(34)S of 10.9-14.4 parts per thousand), but the diverse physiography of the Tularosa Basin led to a complex drainage system which contributed sulfates from various sources depending on the climate at the time of sedimentation. As inferred from sulfur isotope mass balance constraints, weathering of sulfides of magmatic/hydrothermal and sedimentary origin associated with climate oscillations during Last Glacial Maximum contributed about 35-50% of the sulfates and led to deposition of gypsum with delta(34)S values of -1.2 parts per thousand to 2.2 parts per thousand which are substantially lower than Permian evaporates. In the Estancia Basin, microbial sulfate reduction appears to overprint sulfur isotopic signatures that might elucidate past groundwater flows. A Rayleigh distillation model indicates that about 3-18% of sulfates from an inorganic groundwater pool (delta(34)S of 12.6-13.8 parts per thousand) have been metabolized by bacteria and preserved as partially to fully reduced sulfur-bearing minerals species (elemental sulfur, monosulfides, disulfides) with distinctly negative delta(34)S values (-42.3 parts per thousand to -20.3 parts per thousand) compared to co-existing gypsum (-3.8 parts per thousand to 22.4 parts per thousand). For the Tularosa Basin microbial sulfate reduction had negligible effect on delta(34)S value of the gypsiferous sediments most likely because of higher annual temperatures (15-33 degrees C) and lower organic carbon content (median 0.09%) in those sediments leading to more efficient oxidation of H(2)S and/or smaller rates of sulfate reduction compared to the saline playas of the Estancia Basin (5-28 degrees C; median 0.46% of organic carbon). The White Sands region of the Tularosa Basin is frequently posited as a hydrothermal analogue for Mars. High temperatures of groundwater (33.3 degrees C) and high delta(18)O(H(2)O) values (1.1 parts per thousand) in White Sands, however, are controlled predominantly by seasonal evaporation rather than the modern influx of hydrothermal fluids. Nevertheless, it is possible that some of the geochemical processes in White Sands, such as sulfide weathering during climate oscillations and upwelling of highly mineralized waters, might be considered as valid terrestrial analogues for the sulfate cycle in places such as Meridiani Planum on Mars. (C) 2009 Elsevier Ltd. All rights reserved. C1 [Szynkiewicz, Anna; Moore, Craig H.; Pratt, Lisa M.] Indiana Univ, Dept Geol Sci, Bloomington, IN 47408 USA. [Szynkiewicz, Anna; Pratt, Lisa M.] Indiana Univ, NASA, Astrobiol Inst Team, Bloomington, IN 47405 USA. [Glamoclija, Mihaela] Carnegie Inst Washington, Geophys Lab, Washington, DC 20015 USA. RP Szynkiewicz, A (reprint author), Indiana Univ, Dept Geol Sci, 1001E 10th St, Bloomington, IN 47408 USA. EM aaszynkiewicz@utep.edu FU NASA [NNA 04CC03A] FX This study was funded by NASA Grant NNA 04CC03A awarded to L. M. Pratt through the NASA Astrobiology Institute. We sincerely thank (i) Bruce Allen for discussion and field assistance in the Estancia Basin and for providing the spring and sediment samples for the northern Tularosa Basin; (ii) Dave Love for discussion and recommending sampling sites for the Tularosa Basin; and (iii) David Bustos from the White Sands National Monument and Mara Weisenberger from the San Andres Wildlife Refuge for field assistance in the White Sands region. Esther Singer was a NASA Astrobiology Summer Intern who provided tireless field assistance and skilled help in processing numerous sediment samples for sulfur sequential extraction during the summer of 2007. We gratefully recognize Peter Sauer, Ericka Elswick, Adam Johnson, Steve Studley, Arndt Schimmelmann, Magdalena Modelska and Marta Kurasiewicz for technical assistance. We thank Associate Editor Sidney Hemming and four anonymous reviewers for valuable comments and suggestions that contributed significantly to the clarity of this manuscript. NR 83 TC 14 Z9 14 U1 4 U2 26 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD OCT 15 PY 2009 VL 73 IS 20 BP 6162 EP 6186 DI 10.1016/j.gca.2009.07.009 PG 25 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 541LF UT WOS:000273416500014 ER PT J AU Fike, DA Finke, N Zha, J Blake, G Hoehler, TM Orphan, VJ AF Fike, David A. Finke, Niko Zha, Jessica Blake, Garrett Hoehler, Tori M. Orphan, Victoria J. TI The effect of sulfate concentration on (sub)millimeter-scale sulfide delta S-34 in hypersaline cyanobacterial mats over the diurnal cycle SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Review ID SULFUR ISOTOPE FRACTIONATION; SOLAR LAKE SINAI; MICROBIAL MAT; REDUCING BACTERIA; ELEMENTAL SULFUR; MARINE-SEDIMENTS; ANOXYGENIC PHOTOSYNTHESIS; TEMPERATURE-DEPENDENCE; ANAEROBIC OXIDATION; COMMUNITY STRUCTURE AB Substantial isotopic fractionations are associated with many microbial sulfur metabolisms and measurements of the bulk delta S-34 isotopic composition of sulfur species (predominantly sulfates and/or sulfides) have been a key component in developing our understanding of both modern and ancient biogeochemical cycling. However, the interpretations of bulk delta S-34 measurements are often non-unique, making reconstructions of paleoenvironmental conditions or microbial ecology challenging. In particular, the link between the mu m-scale microbial activity that generates isotopic signatures and their eventual preservation as a bulk rock value in the geologic record has remained elusive, in large part because of the difficulty of extracting sufficient material at small scales. Here we investigate the potential for small-scale (similar to 100 mu m-1 cm) delta S-34 variability to provide additional constraints for environmental and/or ecological reconstructions. We have investigated the impact of sulfate concentrations (0.2, 1, and 80 mMSO(4)) on the delta S-34 composition of hydrogen sulfide produced over the diurnal (day/night) cycle in cyanobacterial mats from Guerrero Negro, Baja California Sur, Mexico. Sulfide was captured as silver sulfide on the surface of a 2.5 cm metallic silver disk partially submerged beneath the mat surface. Subsequent analyses were conducted on a Cameca 7f-GEO secondary ion mass spectrometer (SIMS) to record spatial delta S-34 variability within the mats under different environmental conditions. Isotope measurements were made in a 2-dimensional grid for each incubation, documenting both lateral and vertical isotopic variation within the mats. Typical grids consisted of similar to 400-800 individual measurements covering a lateral distance of similar to 1 mm and a vertical depth of similar to 5-15 mm. There is a large isotopic enrichment (similar to 10-20 parts per thousand) in the uppermost mm of sulfide in those mats where [SO4] was non-limiting (field and lab incubations at 80 mM). This is attributed to rapid recycling of sulfur (elevated sulfate reduction rates and extensive sulfide oxidation) at and above the chemocline. This isotopic gradient is observed in both day and night enrichments and suggests that, despite the close physical association between cyanobacteria and select sulfate-reducing bacteria, photosynthetic forcing has no substantive impact on delta S-34 in these cyanobacterial mats. Perhaps equally surprising, large, spatially-coherent delta S-34 oscillations (similar to 20-30 parts per thousand over 1 mm) occurred at depths up to similar to 1.5 cm below the mat surface. These gradients must arise in situ from differential microbial metabolic activity and fractionation during sulfide production at depth. Sulfate concentrations were the dominant control on the spatial variability of sulfide delta S-34. Decreased sulfate concentrations diminished both vertical and lateral delta S-34 variability, suggesting that small-scale variations of delta S-34 can be diagnostic for reconstructing past sulfate concentrations, even when original sulfate delta S-34 is unknown. (C) 2009 Elsevier Ltd. All rights reserved. C1 [Fike, David A.; Orphan, Victoria J.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Fike, David A.] Washington Univ, Dept Earth & Planetary Sci, St Louis, MO 63130 USA. [Fike, David A.] Washington Univ, McDonnell Ctr Space Sci, St Louis, MO 63130 USA. [Finke, Niko; Hoehler, Tori M.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Finke, Niko] Univ So Denmark, Nord Ctr Earth Evolut, DK-5230 Odense M, Denmark. [Zha, Jessica] Johns Hopkins Univ, Baltimore, MD 21218 USA. [Blake, Garrett] Pitzer Coll, Claremont, CA 91711 USA. RP Fike, DA (reprint author), CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. EM dfike@levee.wustl.edu; vorphan@gps.caltech.edu RI Fike, David/D-3634-2011; Orphan, Victoria/K-1002-2014 OI Fike, David/0000-0003-2848-0328; Orphan, Victoria/0000-0002-5374-6178 FU National Aeronautics and Space Administration [NAI02-003-0001]; NASA [07-EXOB07-0093]; Caltech O. K. Earl Postdoctoral Fellowship; EU [MOIF-CT-2005-22154] FX We would like to acknowledge the Gordon and Betty Moore Foundation and the Caltech Center for Geochemical and Cosmochemical Microanalysis for funding (to V. J. O.) as well as support from National Aeronautics and Space Administration grant NAI02-003-0001 issued through the Astrobiology Program and NASA grant 07-EXOB07-0093 issued through the Exobiology Program. D. A. F. was additionally supported by the Caltech O. K. Earl Postdoctoral Fellowship. N.F. was supported by an EU-Marie Curie Postdoctoral Fellowship Contract MOIF-CT-2005-22154. We would like to thank Y. Guan and J. Eiler for analytical assistance and invaluable discussions, and T. Lyons for conventional delta34S analysis of aqueous sulfate. We are also indebted to the NASA Ames group (K. Turk, M. Kubo, L. Jahnke and D. Des Marais) for support and assistance with sample collections. NR 105 TC 16 Z9 16 U1 0 U2 26 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD OCT 15 PY 2009 VL 73 IS 20 BP 6187 EP 6204 DI 10.1016/j.gca.2009.07.006 PG 18 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 541LF UT WOS:000273416500015 ER PT J AU Puchtel, IS Walker, RJ Brandon, AD Nisbet, EG AF Puchtel, I. S. Walker, R. J. Brandon, A. D. Nisbet, E. G. TI Pt-Re-Os and Sm-Nd isotope and HSE and REE systematics of the 2.7 Ga Belingwe and Abitibi komatiites SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Review ID PLATINUM-GROUP ELEMENTS; EARTHS UPPER-MANTLE; GREENSTONE-BELT; HIGHLY SIDEROPHILE; OSMIUM ISOTOPE; EARLY DIFFERENTIATION; ARCHEAN MANTLE; MUNRO-TOWNSHIP; MAGMA OCEAN; RE-187-OS-187 SYSTEMATICS AB High-precision Pt-Re-Os and Sm-Nd isotope and highly siderophile element (HSE) and rare earth element (REE) abundance data are reported for two 2.7 b.y. old komatiite lava flows, Tony's flow (TN) from the Belingwe greenstone belt, Zimbabwe, and the PH-II flow (PH) from Munro Township in the Abitibi greenstone belt, Canada. The emplaced lavas are calculated to have contained similar to 25% (TN) and similar to 28% (PH) MgO. These lavas were derived from mantle sources characterized by strong depletions in highly incompatible lithophile trace elements, such as light REE (Ce/Sm-N = 0.64 +/- 0.02 (TN) and 0.52 +/- 0.01 (PH), epsilon Nd-143(T) = +2.9 +/- 0.2 in both sources). Pt-190-Os-186 and Re-187-Os-187 isochrons generated for each flow yield ages consistent with respective emplacement ages obtained using other chronometers. The calculated precise initial Os-186/Os-188 = 0.1198318 +/- 3 (TN) and 0.1198316 +/- 5 (PH) and Os-187/Os-188 = 0.10875 +/- 17 (TN) and 0.10873 +/- 15 (PH) require time-integrated Pt-190/Os-188 and Re-187/Os-188 of 0.00178 +/- 11 and 0.407 +/- 8 (TN) and 0.00174 +/- 18 and 0.415 +/- 5 (PH). These parameters, which by far represent the most precise and accurate estimates of time-integrated Pt/Os and Re/Os of the Archean mantle, are best matched by those of enstatite chondrites. The data also provide evidence for a remarkable similarity in the composition of the sources of these komatiites with respect to both REE and HSE. The calculated absolute HSE abundances in the TN and PH komatiite sources are within or slightly below the range of estimates for the terrestrial Primitive Upper Mantle (PUM). Assuming a chondritic composition of the bulk silicate Earth, the strong depletions in LREE, yet chondritic Re/Os in the komatiite sources are apparently problematic because early Earth processes capable of fractionating the LREE might also be expected to fractionate Re/Os. This apparent discrepancy could be reconciled via a two-stage model, whereby the moderate LREE depletion in the sources of the komatiites initially occurred within the first 100 Ma of Earth's history as a result of either global magma ocean differentiation or extraction and subsequent long-term isolation of early crust, whereas HSE were largely added subsequently via late accretion. The komatiite formation, preceded by derivation of basaltic magmas, was a result of second-stage, large-degree dynamic melting in mantle plumes. (C) 2009 Elsevier Ltd. All rights reserved. C1 [Puchtel, I. S.; Walker, R. J.] Univ Maryland, Dept Geol, College Pk, MD 20742 USA. [Brandon, A. D.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Nisbet, E. G.] Univ London, Dept Earth Sci, Egham TW20 0EX, Surrey, England. RP Puchtel, IS (reprint author), Univ Maryland, Dept Geol, College Pk, MD 20742 USA. EM ipuchtel@umd.edu RI Walker, Richard/K-6869-2016 OI Walker, Richard/0000-0003-0348-2407 FU NSF [EAR-0635690] FX We thank Tony Martin, who discovered the freshest Reliance Fm. outcrop, for generous long-term collaboration and ongoing support. We are thankful to Mike Lesher and Rebecca Sproule for help with collecting drill core samples from the Pyke Hill area and to Martin Menzies for editorial handling. The final version of the manuscript has greatly benefitted from thoughtful and constructive reviews by Steve Shirey and Nick Arndt. This work was made possible through the support by the NSF Grant EAR-0635690 to ISP; this support is gratefully acknowledged. NR 112 TC 33 Z9 33 U1 3 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 OCT 15 PY 2009 VL 73 IS 20 BP 6367 EP 6389 DI 10.1016/j.gca.2009.07.022 PG 23 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 541LF UT WOS:000273416500026 ER PT J AU Berthet, S Malavergne, V Righter, K AF Berthet, S. Malavergne, V. Righter, K. TI Melting of the Indarch meteorite (EH4 chondrite) at 1 GPa and variable oxygen fugacity: Implications for early planetary differentiation processes SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Article ID LOWER-MANTLE CONDITIONS; ANHYDROUS PERIDOTITE KLB-1; CORE FORMATION; CHEMICAL-COMPOSITION; TERRESTRIAL PLANETS; OXIDATION-STATE; SILICATE MELTS; HIGH-PRESSURE; EARTHS CORE; ENSTATITE CHONDRITES AB In order to derive constraints on planetary differentiation processes, and ultimately the formation of the Earth, it is required to study a variety of meteoritic materials and to investigate their melting relations and elemental partitioning at variable pressures, temperatures, and oxygen fugacities (f(O2)). This study reports the first high pressure (HP) and high temperature (HT) investigation of an enstatite chondrite (Indarch). Four series of experiments exploring various f(O2) conditions have been carried out at 1 GPa in a piston-cylinder apparatus using the EH4 chondrite Indarch. We show that temperature and redox conditions have important effects on the phase equilibria of the meteorite: the solidus and liquidus temperatures of the silicate portion increase with decreasing f(O2), and the stability fields of various phases are modified. Olivine and pyroxene are stable around 1.5 log f(O2) unit below the iron-wustite buffer (IW-1.5), whereas quartz and pyroxene is the stable assemblage under the most reducing conditions, between IW-5.0 and IW-4.0, due to reduction of the silicate. While these changes are occurring in the silicate, the metal gains Si from the silicate, (Fe, Mg, Mn, Ca, Cr)-bearing sulfides are observed at f(O2) less than IW-4, and the partitioning of Ni and Mo are both affected by the presence of Si in Fe-S-C liquids. The f(O2) has also a significant effect on the liquid metal-liquid silicate partitioning behavior of Si and S, two possible light elements in planetary cores, and of the slightly siderophile elements Cr and Mn. With decreasing f(O2), S becomes increasingly lithophile, Si becomes increasingly siderophile, and Cr and Mn both become strongly siderophile and chalcophile. The partitioning behavior of these elements places new constraints on models of core segregation for the Earth and other differentiated bodies. (C) 2009 Elsevier Ltd. All rights reserved. C1 [Berthet, S.; Malavergne, V.] Univ Paris Est, Lab Geomat, F-77454 Champs Sur Marne, France. [Berthet, S.; Malavergne, V.] Lunar & Planetary Inst, Houston, TX 77058 USA. [Righter, K.] NASA, Lyndon B Johnson Space Ctr, Mail Code KT, Houston, TX 77058 USA. RP Malavergne, V (reprint author), Univ Paris Est, Lab Geomat, F-77454 Champs Sur Marne, France. EM malavergne@univ-mlv.fr FU LPI; NASA FX We thank Meenakshi Wadhwa from Arizona State University (SESE) and previously the Field Museum of Natural History, Chicago, for providing us with the aliquot and the thin section of Indarch, Craig Schwandt and Loan Le from the NASA Johnson Space Center for their great assistance on the electron microprobe. The careful comments of F. J. Ryerson, A. Corgne, and two anonymous reviewers are greatly appreciated. This study was supported by LPI contribution #1417 to SB and VM and NASA RTOP to KR. NR 100 TC 26 Z9 26 U1 0 U2 14 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD OCT 15 PY 2009 VL 73 IS 20 BP 6402 EP 6420 DI 10.1016/j.gca.2009.07.030 PG 19 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 541LF UT WOS:000273416500028 ER PT J AU Brandon, AD Lapen, TJ Debaille, V Beard, BL Rankenburg, K Neal, C AF Brandon, Alan D. Lapen, Thomas J. Debaille, Vinciane Beard, Brian L. Rankenburg, Kai Neal, Clive TI Re-evaluating Nd-142/Nd-144 in lunar mare basalts with implications for the early evolution and bulk Sm/Nd of the Moon SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Article ID ENRICHED HADEAN RESERVOIR; FORMING GIANT IMPACT; ANGRA-DOS-REIS; MAGMA OCEAN; SM-ND; EARLY DIFFERENTIATION; NEUTRON-CAPTURE; ND-142 EVIDENCE; LU-HF; ISOTOPE FRACTIONATION AB The Moon likely accreted from melt and vapor ejected during a cataclysmic collision between Proto-Earth and a Mars-sized impactor very early in solar system history. The identical W, O, K, and Cr isotope compositions between materials from the Earth and Moon require that the material from the two bodies were well-homogenized during the collision process. As such, the ancient isotopic signatures preserved in lunar samples provide constraints on the bulk composition of the Earth. Two recent studies to obtain high-precision Nd-142/Nd-144 ratios of lunar mare basalts yielded contrasting results. In one study, after correction of neutron fluence effects imparted to the Nd isotope compositions of the samples, the coupled Nd-142-Nd-143 systematics were interpreted to be consistent with a bulk Moon having a chondritic Sm/Nd ratio [Rankenburg K., Brandon A. D. and Neal C. R. (2006) Neodymium isotope evidence for a chondritic composition of the Moon. Science 312, 1369 1372]. The other study found that their data on the same and similar lunar mare basalts were consistent with a bulk Moon having a superchondritic Sm/Nd ratio [Boyet M. and Carlson R. W. (2007) A highly depleted Moon or a non-magma origin for the lunar crust? Earth Planet. Sci. Lett. 262, 505-516]. Delineating between these two potential scenarios has key ramifications for a comprehensive understanding of the formation and early evolution of the Moon and for constraining the types of materials available for accretion into large terrestrial planets such as Earth. To further examine this issue, the same six lunar mare basalt samples measured in Rankenburg et al. [Rankenburg K., Brandon A. D. and Neal C. R. (2006) Neodymium isotope evidence for a chondritic composition of the Moon. Science 312, 1369-1372] were re-measured for high-precision Nd isotopes using a multidynamic routine with reproducible internal and external precisions to better than +/-3 ppm (2 sigma) for Nd-142/Nd-144 ratios. The measurements were repeated in a distinct second analytical campaign to further test their reproducibility. Evaluation of accuracy and neutron fluence corrections indicates that the multidynamic Nd isotope measurements in this study and the 3 in Boyet and Carlson [Boyet M. and Carlson R. W. (2007) A highly depleted Moon or a non-magma origin for the lunar crust? Earth Planet. Sci. Lett. 262, 505-516] are reproducible, while static measurements in the previous two studies show analytical artifacts and cannot be used at the resolution of 10 ppm to determine a bulk Moon with either chondritic or superchondritic Sm/Nd ratios. The multidynamic data are best explained by a bulk Moon with a superchondritic Sm/Nd ratio that is similar to the present-day average for depleted MORB. Hafnium isotope data were collected on the same aliquots measured for their Nd-142/Nd-144 isotope ratios in order to assess if the correlation line for Nd-142-Nd-143 systematics reflect mixing processes or times at which lunar mantle sources formed. Based on the combined Nd-142-Nd-143-Hf-176 obtained we conclude that the Nd-142-Nd-143 correlation line measured in this study is best interpreted as an isochron with an age of 229(-20)(+24)Ma after the onset of nebular condensation. The uncertainties in the data permit the sources of these samples to have formed over a 44 Ma time interval. These new results for lunar mare basalts are thus consistent with a later Sm-Nd isotope closure time of their source regions than some recent studies have postulated, and a superchondritic bulk Sm/Nd ratio of the Moon and Earth. The superchondritic Sm/Nd signature was inherited from the materials that accreted to make up the Earth-Moon system. Although collisional erosion of crust from planetesimals is favored here to remove subchondritic Sm/Nd portions and drive the bulk of these bodies to superchondritic in composition, removal of explosive basalt material via gravitational escape from such bodies, or chondrule sorting in the inner solar system, may also explain the compositional features that deviate from average chondrites that make up the Earth-Moon system. This inferred superchondritic nature for the Earth similar to the modern convecting mantle means that there is no reason to invoke a missing, subchondritic reservoir to mass balance the Earth back to chondritic for Sm/Nd ratios. However, to account for the subchondritic Sm/Nd ratios of continental crust, a second superchondritic Sm/Nd mantle reservoir is required. Published by Elsevier Ltd. C1 [Brandon, Alan D.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Lapen, Thomas J.] Univ Houston, Houston, TX 77204 USA. [Debaille, Vinciane] Univ Libre Brussels, Dept Sci Terre & Environm, B-1050 Brussels, Belgium. [Beard, Brian L.] Univ Wisconsin, Dept Geol & Geophys, Madison, WI 53706 USA. [Rankenburg, Kai] Free Univ Berlin, Inst Geol Wissensch, D-12249 Berlin, Germany. [Neal, Clive] Univ Notre Dame, Dept Civil Engn & Geol Sci, Notre Dame, IN 46556 USA. RP Brandon, AD (reprint author), NASA, Lyndon B Johnson Space Ctr, Mail Code KR,2101 Nasa Pkwy, Houston, TX 77058 USA. EM alan.d.brandon@nasa.gov FU NASA FX This work was supported by a NASA Cosmochemistry grant to A. D. B. NASA and the Swiss Natural History Museum are thanked for providing samples. Vickie Bennett is thanked for helping to jointly develop the multidynamic method for high-precision measurements with A. D. B. in 2006 on the JSC Triton and for measuring several standard runs listed in this paper in 2008 while in residence at JSC. Maud Boyet and Richard Carlson are thanked for allowing us to use their unpublished 145Nd/144Nd on the lunar samples they obtained 142Nd/144Nd for and presented in Boyet and Carlson (2007). We thank Minako Righter for assistance in the clean laboratory at the University of Houston. We thank Richard Carlson, Mathieu Touboul, and Mukul Sharma for constructive journal reviews. NR 77 TC 41 Z9 43 U1 1 U2 31 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD OCT 15 PY 2009 VL 73 IS 20 BP 6421 EP 6445 DI 10.1016/j.gca.2009.07.015 PG 25 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 541LF UT WOS:000273416500029 ER PT J AU Koster, RD Wang, HL Schubert, SD Suarez, MJ Mahanama, S AF Koster, Randal D. Wang, Hailan Schubert, Siegfried D. Suarez, Max J. Mahanama, Sarith TI Drought-Induced Warming in the Continental United States under Different SST Regimes SO JOURNAL OF CLIMATE LA English DT Article ID SOIL-MOISTURE; CLIMATE; TEMPERATURE; SURFACE; MODEL; RECONSTRUCTION; PRECIPITATION; CIRCULATION AB The U.S. Climate Variability and Predictability (U.S. CLIVAR) Drought Working Group (DWG) recently performed a series of experiments in which a number of AGCMs were forced with different leading patterns of global SST variability. These experiments provide a unique opportunity to examine how different SST regimes affect temperature over the continental United States. Herein, the focus is on a particular aspect of June-August (JJA) near-surface air temperature: the temperature during relatively dry years for a given SST regime. For most of the models participating in the DWG experiments, a cold Pacific produces greater warming in the central United States during relatively dry years than a warm Pacific does for the following two separate reasons: (i) the cold Pacific leads on average, across all years, to drier conditions, and (ii) the particular evaporation regime induced by the cold Pacific enhances the impact of evaporation feedback on temperature, that is, the sensitivity of temperature to within-climate variations in moisture availability. These results are supported, to a large extent, by the observational record. C1 [Koster, Randal D.; Wang, Hailan; Schubert, Siegfried D.; Suarez, Max J.; Mahanama, Sarith] NASA GSFC, GMAO, Greenbelt, MD 20771 USA. [Wang, Hailan; Mahanama, Sarith] UMBC GEST, Baltimore, MD USA. RP Koster, RD (reprint author), NASA GSFC, GMAO, Code 610-1, Greenbelt, MD 20771 USA. EM randal.d.koster@nasa.gov RI Koster, Randal/F-5881-2012 OI Koster, Randal/0000-0001-6418-6383 FU NASA; NOAA; NSF FX This work was carried out as part of the U.S. CLIVAR Drought Working Group activity supported by NASA, NOAA, and NSF to coordinate and compare climate model simulations forced with a common set of idealized SST patterns. The authors thank NASA's Global Modeling and Assimilation Office (GMAO) for making the NSIPP1 runs available, the Lamont-Doherty Earth Observatory of Columbia University versity for making their CCM3 runs available, NOAA's Environmental Modeling Center (EMC) and Climate Prediction Center (CPC) for making the GFS runs available, NOAA's Geophysical Fluid Dynamics Laboratory (GFDL) for making the AM2.1 runs available, the National Center for Atmospheric Research (NCAR) for making the CAM3.5 runs available, and the Center for Ocean Land Atmosphere (COLA) and the University of Miami's Rosenstiel School of Marine and Atmospheric Science for making the CCSM3.0 coupled model runs available. NR 24 TC 10 Z9 10 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 OCT 15 PY 2009 VL 22 IS 20 BP 5385 EP 5400 DI 10.1175/2009JCLI3075.1 PG 16 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 510HY UT WOS:000271080000006 ER PT J AU Weaver, SJ Schubert, S Wang, H AF Weaver, Scott J. Schubert, Siegfried Wang, Hailan TI Warm Season Variations in the Low-Level Circulation and Precipitation over the Central United States in Observations, AMIP Simulations, and Idealized SST Experiments SO JOURNAL OF CLIMATE LA English DT Article ID NORTH-AMERICAN MONSOON; US GREAT-PLAINS; SURFACE TEMPERATURE; SUMMERTIME PRECIPITATION; INTERANNUAL VARIABILITY; MOISTURE TRANSPORT; JET; REGIME; HEMISPHERE; DROUGHT AB Sea surface temperature (SST) linkages to central U.S. low-level circulation and precipitation variability are investigated from the perspective of the Great Plains low-level jet (GPLLJ) and recurring modes of SST variability. The observed and simulated links are first examined via GPLLJ index regressions to precipitation, SST, and large-scale circulation fields in the NCEP-NCAR and North American Regional Reanalysis (NARR) reanalyses, and NASA's Seasonal-to-Interannual Prediction Project (NSIPP1) and Community Climate Model, version 3 (CCM3) ensemble mean Atmospheric Model Intercomparison Project (AMIP) simulations for the 1949-2002 (1979-2002 for NARR) period. Characteristics of the low-level circulation and its related precipitation are further examined in the U.S. Climate Variability and Predictability (CLIVAR) Drought Working Group idealized climate model simulations (NSIPP1 and CCM3) forced with varying polarities of recurring modes of SST variability. It is found that the observed and simulated correlations of the GPLLJ index to Atlantic and Pacific SST, large-scale atmospheric circulation, and Great Plains precipitation variability for 1949-2002 are robust during the July-September (JAS) season and show connections to a distinct global-scale SST variability pattern, one similar to that used in forcing the NSIPP1 and CCM3 idealized simulations, and a subtropical Atlantic-based sea level pressure (SLP) anomaly with a maximum over the Gulf of Mexico. The idealized simulations demonstrate that a warm Pacific and/or a cold Atlantic are influential over regional hydroclimate features including the monthly preference for maximum GPLLJ and precipitation in the seasonal cycle. Furthermore, it appears that the regional expression of globally derived SST variability is important for generating an anomalous atmospheric low-level response of consequence to the GPLLJ, especially when the SST anomaly is positioned over a regional maximum in climatological SST, and in this case the Western Hemisphere warm pool. C1 [Weaver, Scott J.; Wang, Hailan] Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA. [Schubert, Siegfried] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Weaver, Scott J.] NOAA Climate Predict Ctr, Camp Springs, MD USA. RP Weaver, SJ (reprint author), NOAA NWS NCEP, Climate Predict Ctr, 5200 Auth Rd,Rm 605, Camp Springs, MD 20746 USA. EM scott.weaver@noaa.gov FU NASA; NOAA; NSF FX This project was carried out as part of a U.S. CLIVAR Drought Working Group activity supported by NASA, NOAA, and NSF to coordinate and compare climate model simulations forced with a common set of idealized SST patterns. The authors thank NASA's Global Modeling and Assimilation Office (GMAO) for making the NSIPP1 runs available, the Lamont-Doherty Earth Observatory of Columbia University for making their CCM3 runs available, NOAA's Climate Prediction Center (CPC)/Climate Test Bed (CTB) for making the GFS runs available, NOAA's Geophysical Fluid Dynamics Laboratory (GFDL) for making the AM2.1 runs available, the National Center for Atmospheric Research (NCAR) for making the CAM3.5 runs available, and the Center for Ocean-Land-Atmosphere (COLA) and the University of Miami's Rosenstiel School of Marine and Atmospheric Science for making the CCSM3.0 coupled model runs available. The NASA/GMAO contributions to this project were supported by funding from the NASA Energy and Water Cycle Study (NEWS) program and the NASA Modeling and Analysis Program (MAP). The authors also thank three anonymous reviewers for their constructive comments, which greatly enhanced the quality of the manuscript. NR 35 TC 35 Z9 35 U1 1 U2 10 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0894-8755 EI 1520-0442 J9 J CLIMATE JI J. Clim. PD OCT 15 PY 2009 VL 22 IS 20 BP 5401 EP 5420 DI 10.1175/2009JCLI2984.1 PG 20 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 510HY UT WOS:000271080000007 ER PT J AU Kahn, BH Teixeira, J AF Kahn, Brian H. Teixeira, Joao TI A Global Climatology of Temperature and Water Vapor Variance Scaling from the Atmospheric Infrared Sounder SO JOURNAL OF CLIMATE LA English DT Article ID WAVE-NUMBER SPECTRA; GENERAL-CIRCULATION MODEL; MARINE STRATOCUMULUS; ENERGY-SPECTRUM; LIQUID WATER; 2-DIMENSIONAL TURBULENCE; COMMERCIAL AIRCRAFT; LAYER CLOUDS; VARIABILITY; CONVECTION AB A global climatology of height-resolved variance scaling within the troposphere is presented using derived temperature (T) and water vapor (q) profiles from the Atmospheric Infrared Sounder ( AIRS). The power-law exponent of T variance scaling approaches 1.0 outside of the tropics at scales >500-800 km, but it is closer to 0.3 at scales <500 km, similar to exponents obtained from aircraft campaigns, numerical modeling, and theoretical studies. The T exponents in the tropics at all scales become less than 0.3, with a similar pattern observed within the boundary layer in some extratropical regions. For q, the variance scaling differs substantially from T with exponents near 0.5-0.6 in parts of the tropics and subtropics with little to no scale break, showing some consistency with a very limited set of aircraft and satellite studies. Scaling differences as a function of land and ocean, altitude, and cloudy- and clear-sky scenes are quantified. Both T and q exponents indicate peak magnitudes in the midtroposphere and reductions are observed near the boundary layer and upper troposphere. Seasonal variations of T and q scaling reveal a stronger seasonal cycle over land than ocean, especially for T at large length scales. While the zonal variations of T and q exponents vary significantly for scales <500 km, the seasonal variations are much smaller in magnitude. The exponents derived from AIRS could eventually be extrapolated to smaller scales in the absence of additional scale breaks <150 km to provide useful information for constraining subgrid-scale cloud parameterizations. C1 [Kahn, Brian H.; Teixeira, Joao] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Kahn, BH (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,Mail Stop 169-237, Pasadena, CA 91109 USA. EM brian.h.kahn@jpl.nasa.gov FU AIRS project; ONR Award [N0001408IP20064] FX Acknowledgments. During the course of this study, the AIRS and Cloudsat projects provided funding support for BHK. JT was supported by the AIRS project and by ONR Award Number N0001408IP20064. The authors thank Bob Cahalan, Anthony Davis, Eric Fetzer, Alexander Ruzmaikin, Pier Siebesma, Robert Wood, and Mark Zelinka for helpful guidance and discussions, and the anonymous reviewers for comments that led to improvements in the manuscript. AIRS data were obtained through the Goddard Earth Sciences Data and Information Services Center (online at http://daac.gsfc.nasa.gov/). 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 61 TC 23 Z9 23 U1 3 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 OCT 15 PY 2009 VL 22 IS 20 BP 5558 EP 5576 DI 10.1175/2009JCLI2934.1 PG 19 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 510HY UT WOS:000271080000017 ER PT J AU Shige, S Takayabu, YN Kida, S Tao, WK Zeng, XP Yokoyama, C L'Ecuyer, T AF Shige, Shoichi Takayabu, Yukari N. Kida, Satoshi Tao, Wei-Kuo Zeng, Xiping Yokoyama, Chie L'Ecuyer, Tristan TI Spectral Retrieval of Latent Heating Profiles from TRMM PR Data. Part IV: Comparisons of Lookup Tables from Two- and Three-Dimensional Cloud-Resolving Model Simulations SO JOURNAL OF CLIMATE LA English DT Review ID RAINFALL MEASURING MISSION; SOUTH CHINA SEA; ATMOSPHERE RESPONSE EXPERIMENT; PASSIVE MICROWAVE RETRIEVALS; LARGE-SCALE DYNAMICS; PACIFIC WARM POOL; TOGA COARE; CONVECTIVE SYSTEMS; PRECIPITATION RADAR; MOISTURE BUDGETS AB The spectral latent heating (SLH) algorithm was developed to estimate latent heating profiles for the Tropical Rainfall Measuring Mission Precipitation Radar (TRMM PR). The method uses TRMM PR information (precipitation-top height, precipitation rates at the surface and melting level, and rain type) to select heating profiles from lookup tables (LUTs). LUTs for the three rain types-convective, shallow stratiform, and anvil rain (deep stratiform with a melting level)-were derived from numerical simulations of tropical cloud systems from the Tropical Ocean and Global Atmosphere Coupled Ocean-Atmosphere Response Experiment (TOGA COARE) using a cloud-resolving model (CRM). The two-dimensional (2D) CRM was used in previous studies. The availability of exponentially increasing computer capabilities has resulted in three-dimensional (3D) CRM simulations for multiday periods becoming increasingly prevalent. In this study, LUTs from the 2D and 3D simulations are compared. Using the LUTs from 3D simulations results in less agreement between the SLH-retrieved heating and sounding-based heating for the South China Sea Monsoon Experiment (SCSMEX). The level of SLH-estimated maximum heating is lower than that of the sounding-derived maximum heating. This is explained by the fact that using the 3D LUTs results in stronger convective heating and weaker stratiform heating above the melting level than is the case if using the 2D LUTs. More condensate is generated in and carried from the convective region in the 3D model than in the 2D model, and less condensate is produced by the stratiform region's own upward motion. C1 [Shige, Shoichi; Kida, Satoshi] Osaka Prefecture Univ, Dept Aerosp Engn, Osaka, Japan. [Takayabu, Yukari N.; Yokoyama, Chie] Univ Tokyo, Ctr Climate Syst Res, Chiba, Japan. [Takayabu, Yukari N.] Japan Agcy Marine Earth Sci & Technol, Inst Observat Res Global Change, Kanagawa, Japan. [Tao, Wei-Kuo; Zeng, Xiping] NASA, Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD 20771 USA. [Zeng, Xiping] Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA. [L'Ecuyer, Tristan] Colorado State Univ, Dept Atmospher Sci, Ft Collins, CO 80523 USA. RP Shige, S (reprint author), Kyoto Univ, Grad Sch Sci, Div Earth & Planetary Sci, Sakyo Ku, Kyoto 6068502, Japan. EM shige@kugi.kyoto-u.ac.jp RI Zhang, YIng/F-5751-2011; L'Ecuyer, Tristan/C-7040-2013; L'Ecuyer, Tristan/E-5607-2012; PMM, JAXA/K-8537-2016 OI L'Ecuyer, Tristan/0000-0002-7584-4836; FU JAXA/EORC Tropical Rainfall Measuring Mission (TRMM) FX This study is supported by the JAXA/EORC Tropical Rainfall Measuring Mission (TRMM) project. The authors thank Prof. C. Schumacher and an anonymous reviewer for their constructive comments that improved the clarity of the presentation in this paper. NR 113 TC 20 Z9 20 U1 0 U2 4 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0894-8755 J9 J CLIMATE JI J. Clim. PD OCT 15 PY 2009 VL 22 IS 20 BP 5577 EP 5594 DI 10.1175/2009JCLI2919.1 PG 18 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 510HY UT WOS:000271080000018 ER PT J AU Mannucci, AJ Tsurutani, BT Kelley, MC Iijima, BA Komjathy, A AF Mannucci, Anthony J. Tsurutani, Bruce T. Kelley, Michael C. Iijima, Byron A. Komjathy, Attila TI Local time dependence of the prompt ionospheric response for the 7, 9, and 10 November 2004 superstorms SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID GEOMAGNETIC STORM; LATITUDE IONOSPHERE; EQUATORIAL; REGION; SYSTEM AB In this paper, we study the local time response of the low-latitude ionosphere during the sequence of geomagnetic storms occurring on 7, 9, and 10 November 2004. Three distinct storm main phases leading to peak negative Dst index of at least -250 nT occur during this period. We analyze total electron content (TEC) measurements from the global network of GPS receivers available from the International Global Navigation Satellite Systems (GNSS) Service. Average TEC within the geomagnetic latitude band +/- 25 degrees is computed as a function of local time for several hours following storm commencement. We find that significant TEC increases are observed on 7 November (increase of 100%) and 9 November (50%). During 7 November, the increases tend to occur during solar local times 1200-1600 LT. During 9 November, the largest TEC increases tend to occur at earlier local times (similar to 1000-1200 LT). No daytime TEC increase is observed on 10 November, although the K-p index suggests that this storm is comparable in intensity to the 7 November storm. Vertical drift measurements from the Jicamarca radar (Peruvian sector) for the 7 and 9 November storm periods suggest large (2-3 mV/m) low-latitude "prompt penetration'' eastward electric fields (PPEF), consistent with observed increases in TEC. For the 10 November storm, published estimates of electric fields using the dual-magnetometer technique near the Japanese sector, which is near similar to 1400 LT at storm onset, suggest the absence of eastward directed electric fields during daytime. A time series analysis of TEC in the Japanese sector throughout the 7-11 November period reveals significant daytime TEC reduction of 33% relative to quiet conditions. Reduced TEC occurs coincident with the onset of the 10 November storm period, persisting into the 11th. Global Ultraviolet Imager (GUVI) retrievals of thermospheric atomic oxygen to nitrogen ratio suggest depleted oxygen in the southern hemisphere that may contribute to the TEC reduction on 10 November. Solar rotation reduces solar X-ray and EUV fluxes from 10 through 12 November, which may be a contributing factor to reduced TEC on 10 and 11 November. In conclusion, we postulate that an additional source of electric field is present on 10 November during daytime that counteracts the PPEF of magnetospheric origin. C1 [Mannucci, Anthony J.; Tsurutani, Bruce T.; Iijima, Byron A.; Komjathy, Attila] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Kelley, Michael C.] Cornell Univ, Sch Elect & Comp Engn, Ithaca, NY 14853 USA. RP Mannucci, AJ (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,Mailstop 138-308, Pasadena, CA 91109 USA. EM tony.mannucci@jpl.nasa.gov FU NASA's Living With A Star Targeted Research and Technology program; NASA MODA 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. Authors A. J. M. and B. T. acknowledge support of NASA's Living With A Star Targeted Research and Technology program. We gratefully acknowledge the following data providers: World Data Center For Geomagnetism, Kyoto, Japan; International GNSS Service for GPS data; and CDAWeb at NASA's Space Physics Data Facility for interplanetary data. The GUVI data used here are provided through support from the NASA MO&DA program. The GUVI instrument was designed and built by The Aerospace Corporation and The Johns Hopkins University. The principal investigator is Andrew B. Christensen and the chief scientist and co-PI is Larry J. Paxton. NR 39 TC 20 Z9 20 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 OCT 15 PY 2009 VL 114 AR A10308 DI 10.1029/2009JA014043 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 508PI UT WOS:000270944900002 ER PT J AU Metz, JM Grotzinger, JP Mohrig, D Milliken, R Prather, B Pirmez, C McEwen, AS Weitz, CM AF Metz, Joannah M. Grotzinger, John P. Mohrig, David Milliken, Ralph Prather, Bradford Pirmez, Carlos McEwen, Alfred S. Weitz, Catherine M. TI Sublacustrine depositional fans in southwest Melas Chasma SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID DEEP-SEA FAN; VALLES-MARINERIS; ALLUVIAL FANS; DISTRIBUTARY CHANNELS; TURBIDITY CURRENTS; SEDIMENTARY PROCESSES; SUBMARINE CHANNELS; MERIDIANI-PLANUM; MARTIAN GULLIES; MISSISSIPPI FAN AB Two depositional fan complexes have been identified on the floor of southwest Melas Chasma. The western fan complex is located near the center of an enclosed basin in southwest Melas Chasma and is composed of multiple lobes with dendritic finger-like terminations. These fans are very flat and have a morphology unlike any other fan that has been previously identified on Mars. On the basis of the morphologic similarity of the western fan complex to the Mississippi submarine fan complex, we suggest that it may be a deep subaqueous fan depositional system. There are numerous channels on the surface of the western fan complex, and measurements of channel length, width, and sinuosity are consistent with channels observed on terrestrial submarine fans. The eastern Melas depositional fans are less well preserved and may be of deltaic or sublacustrine origin. Recognition of the fans supports earlier suggestions for the presence of a former lake in Melas Chasma and indicates that a significant body of water was present and stable at the surface of Mars for at least 10(2) to 10(4) years. C1 [Metz, Joannah M.; Grotzinger, John P.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Mohrig, David] Univ Texas Austin, Dept Geol Sci, Austin, TX 78712 USA. [Milliken, Ralph] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Pirmez, Carlos] Shell Explorat & Prod Co, Houston, TX 77001 USA. [Prather, Bradford] Shell Explorat & Prod Co, Houston, TX 77079 USA. [McEwen, Alfred S.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Weitz, Catherine M.] Planetary Sci Inst, Tucson, AZ 85719 USA. RP Metz, JM (reprint author), CALTECH, Div Geol & Planetary Sci, 1200 E Calif Blvd, Pasadena, CA 91125 USA. RI Mohrig, David/O-1758-2013 NR 94 TC 33 Z9 33 U1 3 U2 15 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD OCT 14 PY 2009 VL 114 AR E10002 DI 10.1029/2009JE003365 PG 17 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 508PC UT WOS:000270944300002 ER PT J AU Renno, NO Bos, BJ Catling, D Clark, BC Drube, L Fisher, D Goetz, W Hviid, SF Keller, HU Kok, JF Kounaves, SP Leer, K Lemmon, M Madsen, MB Markiewicz, WJ Marshall, J McKay, C Mehta, M Smith, M Zorzano, MP Smith, PH Stoker, C Young, SMM AF Renno, Nilton O. Bos, Brent J. Catling, David Clark, Benton C. Drube, Line Fisher, David Goetz, Walter Hviid, Stubbe F. Keller, Horst Uwe Kok, Jasper F. Kounaves, Samuel P. Leer, Kristoffer Lemmon, Mark Madsen, Morten Bo Markiewicz, Wojciech J. Marshall, John McKay, Christopher Mehta, Manish Smith, Miles Zorzano, M. P. Smith, Peter H. Stoker, Carol Young, Suzanne M. M. TI Possible physical and thermodynamical evidence for liquid water at the Phoenix landing site SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID VOLATILE WEAK ELECTROLYTES; AQUEOUS-SOLUTIONS; MARS; ICE; STABILITY; DELIQUESCENCE; TEMPERATURES; CHEMISTRY; MIXTURES; MINERALS AB The objective of the Phoenix mission is to determine if Mars' polar region can support life. Since liquid water is a basic ingredient for life, as we know it, an important goal of the mission is to determine if liquid water exists at the landing site. It is believed that a layer of Martian soil preserves ice by forming a barrier against high temperatures and sublimation, but that exposed ice sublimates without the formation of the liquid phase. Here we show possible independent physical and thermodynamical evidence that besides ice, liquid saline water exists in areas disturbed by the Phoenix Lander. Moreover, we show that the thermodynamics of freeze-thaw cycles can lead to the formation of saline solutions with freezing temperatures lower than current summer ground temperatures on the Phoenix landing site on Mars' Arctic. Thus, we hypothesize that liquid saline water might occur where ground ice exists near the Martian surface. The ideas and results presented in this article provide significant new insights into the behavior of water on Mars. C1 [Renno, Nilton O.; Kok, Jasper F.; Mehta, Manish] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. [Renno, Nilton O.; Kok, Jasper F.] Univ Michigan, Appl Phys Program, Ann Arbor, MI 48109 USA. [Bos, Brent J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Catling, David] Univ Washington, Dept Earth & Space Sci, Seattle, WA 98195 USA. [Clark, Benton C.] Space Sci Inst, Boulder, CO 80301 USA. [Drube, Line; Hviid, Stubbe F.; Leer, Kristoffer; Madsen, Morten Bo] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark. [Fisher, David] Univ Ottawa, Geol Survey Canada, Ottawa, ON, Canada. [Goetz, Walter; Keller, Horst Uwe; Markiewicz, Wojciech J.] Max Planck Inst Solar Syst Res, Katlenburg Lindau, Germany. [Kounaves, Samuel P.] Tufts Univ, Dept Chem, Medford, MA 02155 USA. [Lemmon, Mark] Texas A&M Univ, Dept Atmospher Sci, College Stn, TX USA. [Marshall, John] SETI Inst, Carl Sagan Ctr, Mountain View, CA USA. [McKay, Christopher; Stoker, Carol] NASA, Ames Res Ctr, Mountain View, CA USA. [Smith, Miles] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Zorzano, M. P.] Ctr Astrobiol, Madrid, Spain. [Smith, Peter H.] Univ Arizona, Dept Planetary Sci, Tucson, AZ 85721 USA. [Young, Suzanne M. M.] Univ New Hampshire, Dept Chem, Durham, NH 03824 USA. RP Renno, NO (reprint author), Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. RI Lemmon, Mark/E-9983-2010; Catling, David/D-2082-2009; Madsen, Morten/D-2082-2011; Zorzano, Maria-Paz/C-5784-2015; Kok, Jasper/A-9698-2008; Zorzano, Maria-Paz/F-2184-2015; OI Kounaves, Samuel/0000-0002-2629-4831; Lemmon, Mark/0000-0002-4504-5136; Madsen, Morten/0000-0001-8909-5111; Zorzano, Maria-Paz/0000-0002-4492-9650; Kok, Jasper/0000-0003-0464-8325; Zorzano, Maria-Paz/0000-0002-4492-9650; Catling, David/0000-0001-5646-120X FU NASA; NSF [ATM 0622539] FX We thank NASA for funding the Phoenix mission, including this study, and for funding M. Mehta though a Graduate Research Fellowship. Graduate student J. Kok was funded by NSF award ATM 0622539. We thank Robb Gillespie and Steven Rogacki for their assistance with the laboratory experiments on the Phoenix landing thruster. We thank Lucas Renno for help with the interpretation of the images of the spheroids. Finally, we thank John Barker and three anonymous reviewers for constructive criticisms and suggestions that improved the manuscript substantially. NR 51 TC 76 Z9 77 U1 2 U2 26 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 OCT 14 PY 2009 VL 114 AR E00E03 DI 10.1029/2009JE003362 PG 11 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 508PC UT WOS:000270944300001 ER PT J AU Velicogna, I AF Velicogna, I. TI Increasing rates of ice mass loss from the Greenland and Antarctic ice sheets revealed by GRACE SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID BALANCE; SYSTEM AB We use monthly measurements of time-variable gravity from the GRACE (Gravity Recovery and Climate Experiment) satellite gravity mission to determine the ice mass-loss for the Greenland and Antarctic Ice Sheets during the period between April 2002 and February 2009. We find that during this time period the mass loss of the ice sheets is not a constant, but accelerating with time, i.e., that the GRACE observations are better represented by a quadratic trend than by a linear one, implying that the ice sheets contribution to sea level becomes larger with time. In Greenland, the mass loss increased from 137 Gt/yr in 2002-2003 to 286 Gt/yr in 2007-2009, i.e., an acceleration of -30 +/- 11 Gt/yr(2) in 2002-2009. In Antarctica the mass loss increased from 104 Gt/yr in 2002-2006 to 246 Gt/yr in 2006-2009, i. e., an acceleration of -26 +/- 14 Gt/yr(2) in 2002-2009. The observed acceleration in ice sheet mass loss helps reconcile GRACE ice mass estimates obtained for different time periods. Citation: Velicogna, I. (2009), Increasing rates of ice mass loss from the Greenland and Antarctic ice sheets revealed by GRACE, Geophys. Res. Lett., 36, L19503, doi: 10.1029/2009GL040222. C1 [Velicogna, I.] Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA 92697 USA. [Velicogna, I.] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Velicogna, I (reprint author), Univ Calif Irvine, Dept Earth Syst Sci, 3226 Croul Hall, Irvine, CA 92697 USA. EM isabella@uci.edu FU NASA's Cryospheric Science Program; Solid Earth and Natural Hazards Program; Terrestrial Hydrology Program; NSF Office of Polar Programs FX This work was performed at the University of California Irvine and at the Jet Propulsion Laboratory, California Institute of Technology and was supported by grants from NASA's Cryospheric Science Program, Solid Earth and Natural Hazards Program, Terrestrial Hydrology Program and by the NSF Office of Polar Programs. NR 23 TC 309 Z9 317 U1 10 U2 92 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD OCT 13 PY 2009 VL 36 AR L19503 DI 10.1029/2009GL040222 PG 4 WC Geosciences, Multidisciplinary SC Geology GA 508OM UT WOS:000270942700005 ER PT J AU de Asis, ED Leung, J Wood, S Nguyen, CV AF de Asis, Edward D., Jr. Leung, Joseph Wood, Sally Nguyen, Cattien V. TI High spatial resolution single multiwalled carbon nanotube electrode for stimulation, recording, and whole cell voltage clamping of electrically active cells SO APPLIED PHYSICS LETTERS LA English DT Article ID FROG SARTORIUS MUSCLE; ACTION POTENTIALS; MEMBRANE; SYNAPSES; NETWORKS; RELEASE; NEURONS; FIBRES; FIBERS; SYSTEM AB We report the stimulation, recording, and voltage clamp of muscle fibers using a 30 nm diameter single multiwalled carbon nanotube electrode (sMWNT electrode) tip. Because of the lower access resistance, the sMWNT electrode conducts extracellular and intracellular stimulation more efficiently compared to glass micropipettes. The sMWNT electrode records field potentials and action potentials and performs whole cell voltage clamping of single fibers. (C) 2009 American Institute of Physics. [doi:10.1063/1.3247885] C1 [de Asis, Edward D., Jr.; Wood, Sally] Santa Clara Univ, Sch Engn, Dept Elect Engn, Santa Clara, CA 95053 USA. [de Asis, Edward D., Jr.; Wood, Sally] Santa Clara Univ, Sch Engn, Dept Bioengn, Santa Clara, CA 95053 USA. [Nguyen, Cattien V.] NASA, Ames Res Ctr, ELORET Corp, Moffett Field, CA 94035 USA. RP de Asis, ED (reprint author), Santa Clara Univ, Sch Engn, Dept Elect Engn, 500 El Camino Real, Santa Clara, CA 95053 USA. EM cattien.v.nguyen@nasa.gov NR 25 TC 10 Z9 10 U1 1 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 0003-6951 J9 APPL PHYS LETT JI Appl. Phys. Lett. PD OCT 12 PY 2009 VL 95 IS 15 AR 153701 DI 10.1063/1.3247885 PG 3 WC Physics, Applied SC Physics GA 508FU UT WOS:000270915700083 ER PT J AU Skilton, JL Pandey-Pommier, M Hinton, JA Cheung, CC Aharonian, FA Brucker, J Dubus, G Fiasson, A Funk, S Gallant, Y Marcowith, A Reimer, O AF Skilton, J. L. Pandey-Pommier, M. Hinton, J. A. Cheung, C. C. Aharonian, F. A. Brucker, J. Dubus, G. Fiasson, A. Funk, S. Gallant, Y. Marcowith, A. Reimer, O. TI The radio counterpart of the likely TeV binary HESS J0632+057 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE radio continuum: stars; X-rays: binaries ID X-RAY BINARY; ENERGY GAMMA-RAYS; LS 5039; SKY SURVEY; STARS; EMISSION; DISCOVERY; LS-5039; I+61-DEGREES-303; PERIASTRON AB The few known gamma-ray binary systems are all associated with variable radio and X-ray emission. The TeV source HESS J0632+057, apparently associated with the Be star MWC 148, is plausibly I new member of this class. Following the identification of a variable X-ray counterpart to the TeV source we conducted Giant Metrewave Radio Telescope (GMRT) and Very Large Array (VLA) observations in 2008 June-September to search for the radio counterpart of this object. A point-like radio source at the position of the star is detected in both 1280-MHz GMRT and 5-GHz VLA observations, with an average spectral index, alpha, of similar to 0.6. In the VLA data there is significant flux variability oil similar to month time-scales around the mean flux density of approximate to 0.3 mJy. These radio properties (and the overall spectral energy distribution) are consistent with an interpretation of HESS J0632+057 as a lower power analogue of the established gamma-ray binary systems. C1 [Skilton, J. L.; Hinton, J. A.] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England. [Pandey-Pommier, M.] Leiden Observ, NL-2300 RA Leiden, Netherlands. [Cheung, C. C.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Aharonian, F. A.] Dublin Inst Adv Studies, Dublin 2, Ireland. [Brucker, J.] Univ Erlangen Nurnberg, Inst Phys, D-91058 Erlangen, Germany. [Dubus, G.] Univ Grenoble 1, Lab Astrophys Grenoble, INSU, CNRS, F-38041 Grenoble 9, France. [Fiasson, A.; Gallant, Y.; Marcowith, A.] Univ Montpellier 2, Lab Phys Theor & Astroparticules, CNRS, IN2P3, F-34095 Montpellier 5, France. [Fiasson, A.] CNRS, Lab Annecy Le Vieux Phys Particules, IN2P3, F-74941 Annecy Le Vieux, France. [Funk, S.; Reimer, O.] SLAC, Kavli Inst Particle Astrophys & Cosmol, Menlo Pk, CA 94025 USA. [Reimer, O.] Univ Innsbruck, Inst Astro & Particle Phys, A-6020 Innsbruck, Austria. RP Skilton, JL (reprint author), Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England. EM J.L.Skilton03@leeds.ac.uk RI Reimer, Olaf/A-3117-2013; Funk, Stefan/B-7629-2015 OI Reimer, Olaf/0000-0001-6953-1385; Funk, Stefan/0000-0002-2012-0080 FU UK Science and Technology Facilities Council (STFC) Advanced Fellowship; NASA Postdoctoral Program at Goddard Space Flight Center; European Community [ERC-StG-200911] FX We thank the staff of the GMRT who made these observations possible. We thank Dr S. Roy and Professor V. Kulkarni of NCRA for the help provided during the GMRT observation and data transmission to the Leiden Observatory, H. E. Wheelwright and J. J Stead for useful discussions and all anonymous referee for helpful comments. JAH is supported by a UK Science and Technology Facilities Council (STFC) Advanced Fellowship. CCC is supported by an appointment to the NASA Postdoctoral Program at Goddard Space Flight Center, administered by Oak Ridge Associated Universities through it contract with NASA. GD is supported by European Community contract ERC-StG-200911. NR 37 TC 28 Z9 28 U1 0 U2 0 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD OCT 11 PY 2009 VL 399 IS 1 BP 317 EP 322 DI 10.1111/j.1365-2966.2009.15272.x PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 511KN UT WOS:000271163200026 ER PT J AU Tanner, A Beichman, C Bryden, G Lisse, C Lawler, S AF Tanner, Angelle Beichman, Charles Bryden, Geoff Lisse, Carey Lawler, Samantha TI SURVEY OF NEARBY FGK STARS AT 160 mu m WITH SPITZER SO ASTROPHYSICAL JOURNAL LA English DT Article DE infrared: stars; planetary systems ID SOLAR-TYPE STARS; MULTIBAND IMAGING PHOTOMETER; DEBRIS DISKS; KUIPER-BELT; MIPS SURVEY; DUST; PLANET AB The Spitzer Space Telescope has advanced debris disk science tremendously with a wealth of information on debris disks around nearby A, F, G, K, and M stars at 24 and 70 mu m with the MIPS photometer and at 8-34 mu m with IRS. Here we present 160 mu m observations of a small subset of these stars. At this wavelength, the stellar photospheric emission is negligible and any detected emission corresponds to cold dust in extended Kuiper Belt analogs. However, the Spitzer 160 mu m observations are limited in sensitivity by the large beam size which results in significant "noise" due to cirrus and extragalactic confusion. In addition, the 160 mu m measurements suffer from the added complication of a light leak next to the star's position whose flux is proportional to the near-infrared flux of the star. We are able to remove the contamination from the leak and report 160 mu m measurements or upper limits for 24 stars. Three stars (HD 10647, HD 207129, and HD 115617) have excesses at 160 mu m that we use to constrain the properties of the debris disks around them. A more detailed model of the spectral energy distribution of HD 10647 reveals that the 70 and 160 mu m emission could be due to small water ice particles at a distance of 100 AU, consistent with Hubble Space Telescope optical imaging of circumstellar material in the system. C1 [Tanner, Angelle] Georgia State Univ, Dept Phys & Astron, Atlanta, GA 30302 USA. [Tanner, Angelle; Bryden, Geoff] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Beichman, Charles] CALTECH, NASA Exoplanet Sci Inst, Pasadena, CA 91125 USA. [Lisse, Carey] Johns Hopkins Univ, Appl Phys Lab, SD SRE, Laurel, MD 20723 USA. [Lawler, Samantha] Wesleyan Univ, Van Vleck Observ, Dept Astron, Middletown, CT 06459 USA. RP Tanner, A (reprint author), Georgia State Univ, Dept Phys & Astron, Atlanta, GA 30302 USA. EM angelle.tanner@gmail.com RI Lisse, Carey/B-7772-2016 OI Lisse, Carey/0000-0002-9548-1526 FU National Aeronautics and Space Administration; University of Massachusetts; Infrared Processing and Analysis Center/California Institute of Technology; National Science Foundation FX The research described in this publication was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. NR 22 TC 21 Z9 21 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 10 PY 2009 VL 704 IS 1 BP 109 EP 116 DI 10.1088/0004-637X/704/1/109 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 499KR UT WOS:000270219500009 ER PT J AU Absil, O Mennesson, B Le Bouquin, JB Di Folco, E Kervella, P Augereau, JC AF Absil, Olivier Mennesson, Bertrand Le Bouquin, Jean-Baptiste Di Folco, Emmanuel Kervella, Pierre Augereau, Jean-Charles TI AN INTERFEROMETRIC STUDY OF THE FOMALHAUT INNER DEBRIS DISK. I. NEAR-INFRARED DETECTION OF HOT DUST WITH VLTI/VINCI SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; stars: individual (Fomalhaut); techniques: interferometric ID BALMER LINE-PROFILES; A-TYPE STARS; PLANETARY SYSTEM; VLTI; CHARA/FLUOR; VELOCITIES; EMISSION; MODELS; ORIGIN; IMAGES AB The innermost parts of dusty debris disks around main-sequence stars are currently poorly known due to the high contrast and small angular separation with their parent stars. Using near-infrared interferometry, we aim to detect the signature of hot dust around the nearby A4 V star Fomalhaut, which has already been suggested to harbor a warm dust population in addition to a cold dust ring located at about 140 AU. Archival data obtained with the VINCI instrument at the VLTI are used to study the fringe visibility of the Fomalhaut system at projected baseline lengths ranging from 4 m to 140 m in the K band. A significant visibility deficit is observed at short baselines with respect to the expected visibility of the sole stellar photosphere. This is interpreted as the signature of resolved circumstellar emission, producing a relative flux of 0.88% +/- 0.12% with respect to the stellar photosphere. While our interferometric data cannot directly constrain the morphology of the excess emission source, complementary data from the literature allow us to discard an off-axis point-like object as the source of circumstellar emission. We argue that the thermal emission from hot dusty grains located within 6 AU from Fomalhaut is the most plausible explanation for the detected excess. Our study also provides a revised limb-darkened diameter for Fomalhaut (theta(LD) = 2.223 +/- 0.022 mas), taking into account the effect of the resolved circumstellar emission. C1 [Absil, Olivier] Univ Liege, Dept Astrophys Geophys & Oceanog, B-4000 Sart Tilman Par Liege, Belgium. [Absil, Olivier; Augereau, Jean-Charles] Univ Grenoble 1, F-38041 Grenoble, France. [Absil, Olivier; Augereau, Jean-Charles] CNRS, LAOG, UMR 5571, F-38041 Grenoble, France. [Mennesson, Bertrand] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Le Bouquin, Jean-Baptiste] European So Observ, Santiago 19, Chile. [Di Folco, Emmanuel; Kervella, Pierre] CNRS, LESIA, UMR 8109, F-92195 Meudon, France. [Di Folco, Emmanuel; Kervella, Pierre] Observ Paris, F-92195 Meudon, France. RP Absil, O (reprint author), Univ Liege, Dept Astrophys Geophys & Oceanog, 17 Allee Six, B-4000 Sart Tilman Par Liege, Belgium. OI Absil, Olivier/0000-0002-4006-6237 FU European Commission; F.R.S.-FNRS Postdoctoral Fellowship; International Space Science Institute; EGIDE/PHC Procope program [17843ZE] FX O.A. acknowledges the financial support from the European Commission's Sixth Framework Program as a Marie Curie Intra-European Fellow(EIF) while at LAOG, and from a F.R.S.-FNRS Postdoctoral Fellowship while at IAGL. This research was partly funded by the International Space Science Institute ("Exozodiacal Dust Disks and Darwin"working group) and by an EGIDE/PHC Procope program (No. 17843ZE). NR 37 TC 42 Z9 42 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 OCT 10 PY 2009 VL 704 IS 1 BP 150 EP 160 DI 10.1088/0004-637X/704/1/150 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 499KR UT WOS:000270219500013 ER PT J AU Cotton, WD Ragland, S Pluzhnik, E Danchi, WC Traub, WA Willson, LA Lacasse, MG AF Cotton, W. D. Ragland, S. Pluzhnik, E. Danchi, W. C. Traub, W. A. Willson, L. A. Lacasse, M. G. TI SIO MASERS IN ASYMMETRIC MIRAS. I. R LEONIS SO ASTROPHYSICAL JOURNAL LA English DT Article DE radio lines: stars; stars: AGB and post-AGB; stars: atmospheres ID LATE-TYPE STARS; VARIABLE-STARS; VLBA OBSERVATIONS; SHELL AB This is the first paper in a series of multi-epoch observations of the SiO masers at 7 mm wavelength in several asymptotic giant branch (AGB) stars. This is a sample of Mira variable stars showing evidence of asymmetric structure in the infrared which were observed interferometrically in the infrared by Infrared Optical Telescope Array and with Very Long Baseline Array measurements of the SiO masers. In this paper, we present the observations of R Leonis (R Leo). During the period of observations, this star shows extended emission with large-scale coherent patterns in the radial velocity, possibly the result of ejecting a substantial amount of material, largely to the west. This is interpreted as an event in which material is expelled in a collimated flow, possibly following an energetic event. If common, these events may help explain the asymmetric nature of the planetary nebulae that develop from AGB stars. The systemic velocity of R Leo is estimated to be +1.0 +/- 0.3 km s(-1). All observed radial velocities are well below the escape velocity. C1 [Cotton, W. D.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. [Ragland, S.; Pluzhnik, E.] Calif Assoc Res Astron, Kamuela, HI 96743 USA. [Danchi, W. C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Traub, W. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Willson, L. A.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50014 USA. [Lacasse, M. G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Cotton, WD (reprint author), Natl Radio Astron Observ, 520 Edgemont Rd, Charlottesville, VA 22903 USA. EM bcotton@nrao.edu FU NSF [AST-0456047] FX We acknowledge support from NSF through grant AST-0456047. NR 13 TC 5 Z9 5 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 10 PY 2009 VL 704 IS 1 BP 170 EP 182 DI 10.1088/0004-637X/704/1/170 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 499KR UT WOS:000270219500015 ER PT J AU Kilper, G Gilbert, H Alexander, D AF Kilper, Gary Gilbert, Holly Alexander, David TI MASS COMPOSITION IN PRE-ERUPTION QUIET SUN FILAMENTS SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun: coronal mass ejections (CMEs); Sun: filaments; Sun: prominences ID QUIESCENT PROMINENCE; ERUPTING-PROMINENCE; MODEL PROMINENCES; TRANSITION REGION; PLASMA PARAMETERS; SOLAR FILAMENTS; CME; SPECTRUM; HELIUM; CORONA AB Filament eruptions are extremely important phenomena due to their association with coronal mass ejections and their effects on space weather. Little is known about the filament mass and composition in the eruption process, since most of the related research has concentrated on the evolution and disruption of the magnetic field. Following up on our previous work, we present here an analysis of nineteen quiet Sun filament eruptions observed by Mauna Loa Solar Observatory in H alpha and He I 10830 angstrom that has identified a compositional precursor common to all of these eruptions. There is a combined trend of an apparent increase in the homogenization of the filament mass composition, with concurrent increases in absorption in H alpha and He I and in the level of activity, all starting at least one day prior to eruption. This finding suggests that a prolonged period of mass motions, compositional mixing, and possibly even extensive mass loading is occurring during the build up of these eruptions. C1 [Kilper, Gary; Gilbert, Holly; Alexander, David] Rice Univ, Dept Phys & Astron, Houston, TX 77005 USA. [Gilbert, Holly] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Kilper, G (reprint author), Rice Univ, Dept Phys & Astron, 6100 Main St, Houston, TX 77005 USA. EM garyk1@gmail.com RI Gilbert, Holly/C-7215-2012 FU NASA GSRP [NNX07AK31H, NNX07AI10G S02] FX The research was supported by NASA GSRP grant NNX07AK31H, NASA grant NNX07AI10G S02, and partially by an appointment to the NASA Postdoctoral Program at Goddard Space Flight Center, administered by Oak Ridge Associated Universities through a contract with NASA. NR 30 TC 8 Z9 8 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 10 PY 2009 VL 704 IS 1 BP 522 EP 530 DI 10.1088/0004-637X/704/1/522 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 499KR UT WOS:000270219500041 ER PT J AU Schmelz, JT Kashyap, VL Saar, SH Dennis, BR Grigis, PC Lin, L DeLuca, EE Holman, GD Golub, L Weber, MA AF Schmelz, J. T. Kashyap, V. L. Saar, S. H. Dennis, B. R. Grigis, P. C. Lin, L. DeLuca, E. E. Holman, G. D. Golub, L. Weber, M. A. TI SOME LIKE IT HOT: CORONAL HEATING OBSERVATIONS FROM HINODE X-RAY TELESCOPE AND RHESSI SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun: corona; Sun: X-rays, gamma rays ID SOLAR ACTIVE REGIONS; ATOMIC DATABASE; EMISSION-LINES; ABUNDANCES; RECONSTRUCTION; SPECTRA; MISSION; CHIANTI; PLASMA; SHEETS AB We have used Hinode X-Ray Telescope observations and RHESSI upper limits together to characterize the differential emission measure (DEM) from a quiescent active region. We find a relatively smooth DEM curve with the expected active region peak at log T = 6.4. We also find a high-temperature component with significant emission measure at log T greater than or similar to 7. This curve is consistent with previous observations of quiescent active regions in that it does not produce observable Fe XIX lines. It is different from that generated with X-Ray Telescope (XRT) data alone-RHESSI rules out the possibility of a separate high-temperature component with a peak of approximately log T = 7.4. The strength and position of the high-temperature peak in this XRT-only analysis was, however, poorly determined; adding RHESSI flux upper limits in the 4-13 keV energy range provide a strong high-temperature constraint which greatly improves the multi-thermal findings. The results of the present work as well as those from a growing number of papers on this subject imply that our previous understanding of the temperature distribution in active regions has been limited. Hot plasma (log T approximate to 7) appears to be prevalent, although in relatively small quantities as predicted by nanoflare models. Other models may need to be adjusted or updated to account for these new results. C1 [Schmelz, J. T.] Univ Memphis, Dept Phys, Memphis, TN 38152 USA. [Schmelz, J. T.; Kashyap, V. L.; Saar, S. H.; Grigis, P. C.; DeLuca, E. E.; Golub, L.; Weber, M. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Dennis, B. R.; Holman, G. D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Lin, L.] Univ New Hampshire, Inst Study Earth Oceans & Space, Durham, NH 03824 USA. RP Schmelz, JT (reprint author), Univ Memphis, Dept Phys, Memphis, TN 38152 USA. EM jschmelz@memphis.edu RI Dennis, Brian/C-9511-2012; Holman, Gordon/C-9548-2012; DeLuca, Edward/L-7534-2013 OI DeLuca, Edward/0000-0001-7416-2895 FU NASA [NNG05GM44G, NAS8-39073]; NSF [ATM-0402729] FX We thank Piet Martens, Fabio Reale, and Jim Klimchuk for helpful discussions. Richard Schwartz measured the RHESSI background data used here to compute upper limits and provided the instrument response. Hinode is a Japanese mission developed and launched by ISAS/JAXA, with NAOJ as domestic partner and NASA and STFC (UK) as international partners. It is operated by these agencies in co-operation with ESA and the NSC (Norway). Solar physics research at the University of Memphis is supported by a Hinode subcontract from NASA/SAO as well as NSF ATM-0402729. V. K. acknowledges support from NASA-LWSTRT Grant NNG05GM44G and NASA contract NAS8-39073 to the Chandra X-ray Center. NR 26 TC 31 Z9 31 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 10 PY 2009 VL 704 IS 1 BP 863 EP 869 DI 10.1088/0004-637X/704/1/863 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 499KR UT WOS:000270219500067 ER PT J AU Muzerolle, J Flaherty, K Balog, Z Furlan, E Smith, PS Allen, L Calvet, N D'Alessio, P Megeath, ST Muench, A Rieke, GH Sherry, WH AF Muzerolle, James Flaherty, Kevin Balog, Zoltan Furlan, Elise Smith, Paul S. Allen, Lori Calvet, Nuria D'Alessio, Paola Megeath, S. Thomas Muench, August Rieke, George H. Sherry, William H. TI EVIDENCE FOR DYNAMICAL CHANGES IN A TRANSITIONAL PROTOPLANETARY DISK WITH MID-INFRARED VARIABILITY SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE accretion, accretion disks; planetary systems: protoplanetary disks; stars: pre-main sequence ID PRE-MAIN-SEQUENCE; SPITZER-SPACE-TELESCOPE; YOUNG STELLAR OBJECTS; MULTIBAND IMAGING PHOTOMETER; ALL-SKY SURVEY; MASS STARS; INFRARED SPECTROGRAPH; INTERSTELLAR CLOUDS; MOLECULAR CLOUD; C2D SURVEY AB We present multi-epoch Spitzer Space Telescope observations of the transitional disk LRLL 31 in the 2-3 Myr old star-forming region IC 348. Our measurements show remarkable mid-infrared variability on timescales as short as one week. The infrared continuum emission exhibits systematic wavelength-dependent changes that suggest corresponding dynamical changes in the inner disk structure and variable shadowing of outer disk material. We propose several possible sources for the structural changes, including a variable accretion rate or a stellar or planetary companion embedded in the disk. Our results indicate that variability studies in the infrared can provide important new constraints on protoplanetary disk behavior. C1 [Muzerolle, James] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Muzerolle, James; Flaherty, Kevin; Balog, Zoltan; Smith, Paul S.; Rieke, George H.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Balog, Zoltan] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Furlan, Elise] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Allen, Lori; Muench, August] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Allen, Lori] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Calvet, Nuria] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [D'Alessio, Paola] UNAM, Ctr Radioastron & Astrofis, Morelia, Michoacan, Mexico. [Megeath, S. Thomas] Univ Toledo, Dept Phys & Astron, Toledo, OH 43606 USA. [Sherry, William H.] Natl Solar Observ, Tucson, AZ 85719 USA. RP Muzerolle, J (reprint author), Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA. OI Muench, August/0000-0003-0666-6367; Furlan, Elise/0000-0001-9800-6248 FU NASA [1407, 960785] FX This work is based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under NASA contract 1407. Support for this work was provided by NASA through Contract Number 960785 issued by JPL/Caltech. We acknowledge K. Luhman for assistance with spectral typing the SpeX spectrum. NR 37 TC 52 Z9 52 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD OCT 10 PY 2009 VL 704 IS 1 BP L15 EP L19 DI 10.1088/0004-637X/704/1/L15 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 499KT UT WOS:000270219700004 ER PT J AU Baldridge, AM Hook, SJ Crowley, JK Marion, GM Kargel, JS Michalski, JL Thomson, BJ de Souza, CR Bridges, NT Brown, AJ AF Baldridge, A. M. Hook, S. J. Crowley, J. K. Marion, G. M. Kargel, J. S. Michalski, J. L. Thomson, B. J. de Souza Filho, C. R. Bridges, N. T. Brown, A. J. TI Contemporaneous deposition of phyllosilicates and sulfates: Using Australian acidic saline lake deposits to describe geochemical variability on Mars SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID SOUTHERN WESTERN-AUSTRALIA; MARTIAN GEOLOGIC RECORD; OMEGA/MARS EXPRESS; MERIDIANI-PLANUM; YILGARN BLOCK; SOIL; ENVIRONMENT; SURFACE; MINERALIZATION; FERROLYSIS AB Studies of the origin of the Martian sulfate and phyllosilicate deposits have led to the hypothesis that there was a marked, global-scale change in the Mars environment from circum-neutral pH aqueous alteration in the Noachian to an acidic evaporitic system in the late Noachian to Hesperian. However, terrestrial studies suggest that two different geochemical systems need not be invoked to explain such geochemical variation. Western Australian acidic playa lakes have large pH differences separated vertically and laterally by only a few tens of meters, demonstrating how highly variable chemistries can coexist over short distances in natural environments. We suggest diverse and variable Martian aqueous environments where the coetaneous formation of phyllosilicates and sulfates at the Australian sites are analogs for regions where phyllosilicates and sulfates coexist on Mars. In these systems, Fe and alkali earth phyllosilicates represent deep facies associated with upwelling neutral to alkaline groundwater, whereas aluminous phyllosilicates and sulfates represent near-surface evaporitic facies formed from more acidic brines. Citation: Baldridge, A. M., S. J. Hook, J. K. Crowley, G. M. Marion, J. S. Kargel, J. L. Michalski, B. J. Thomson, C. R. de Souza Filho, N. T. Bridges, and A. J. Brown (2009), Contemporaneous deposition of phyllosilicates and sulfates: Using Australian acidic saline lake deposits to describe geochemical variability on Mars, Geophys. Res. Lett., 36, L19201, doi:10.1029/2009GL040069. C1 [Baldridge, A. M.; Hook, S. J.; Bridges, N. T.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Brown, A. J.] SETI Inst, Mountain View, CA 94043 USA. [Crowley, J. K.] US Geol Survey, Reston, VA 20192 USA. [de Souza Filho, C. R.] Univ Estadual Campinas, Dept Geol & Nat Resources, BR-13083970 Campinas, SP, Brazil. [Kargel, J. S.] Univ Arizona, Dept Hydrol & Water Resources, Tucson, AZ 85721 USA. [Marion, G. M.] Desert Res Inst, Reno, NV 89512 USA. [Michalski, J. L.] Univ Paris 11, Inst Astrophys Spatiale, F-91405 Orsay, France. [Thomson, B. J.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. RP Baldridge, AM (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM alice.m.baldridge@jpl.nasa.gov RI Bridges, Nathan/D-6341-2016; OI Thomson, Bradley/0000-0001-8635-8932 NR 45 TC 33 Z9 34 U1 1 U2 12 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD OCT 9 PY 2009 VL 36 AR L19201 DI 10.1029/2009GL040069 PG 6 WC Geosciences, Multidisciplinary SC Geology GA 505MC UT WOS:000270696700006 ER PT J AU Spreen, G Kern, S Stammer, D Hansen, E AF Spreen, Gunnar Kern, Stefan Stammer, Detlef Hansen, Edmond TI Fram Strait sea ice volume export estimated between 2003 and 2008 from satellite data SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID THICKNESS AB Satellite-based estimates of monthly sea ice volume exports through Fram Strait for the years 2003 to 2008 are presented. These are obtained from individual satellite observations of sea ice thickness, area, and drift. First, sea ice freeboard is inferred from ICESat laser altimeter observations and then converted to ice thickness estimates. Sea ice area and drift are derived from AMSR-E 89 GHz data. Retrieved sea ice thickness estimates compare within 0.5 m with the few ULS data available in the Fram Strait. The mean, minimum, and maximum observed monthly Fram Strait sea ice volume export amounts to 217, 92, and 420 km(3)/month, respectively. In comparison to former Fram Strait sea ice volume export estimates obtained during the 1990s our estimates are slightly smaller (-33 km(3)/month) but are within the natural variability and no significant change of the total amount of Fram Strait sea ice export can be observed. Citation: Spreen, G., S. Kern, D. Stammer, and E. Hansen (2009), Fram Strait sea ice volume export estimated between 2003 and 2008 from satellite data, Geophys. Res. Lett., 36, L19502, doi:10.1029/2009GL039591. C1 [Hansen, Edmond] Norwegian Polar Res Inst, Polar Environm Ctr, N-9296 Tromso, Norway. [Spreen, Gunnar; Kern, Stefan; Stammer, Detlef] Univ Hamburg, Inst Oceanog, D-20146 Hamburg, Germany. RP Spreen, G (reprint author), CALTECH, Jet Prop Lab, MS 300-323,4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM gunnar.spreen@jpl.nasa.gov; stefan.kern@zmaw.de; detlef.stammer@zmaw.de; edmond.hansen@npolar.no RI Spreen, Gunnar/A-4533-2010 OI Spreen, Gunnar/0000-0003-0165-8448 FU German Science Foundation [SFB 512, TP E1] FX This study was funded in part by the German Science Foundation (SFB 512, TP E1). Data provision by the National Snow and Ice Data Center, Boulder, USA and CERSAT, IFREMER, Brest, France are greatly acknowledged as are the helpful comments of two anonymous reviewers. NR 18 TC 41 Z9 41 U1 0 U2 5 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD OCT 9 PY 2009 VL 36 AR L19502 DI 10.1029/2009GL039591 PG 6 WC Geosciences, Multidisciplinary SC Geology GA 505MC UT WOS:000270696700002 ER PT J AU Shoji, M Omura, Y Tsurutani, BT Verkhoglyadova, OP Lembege, B AF Shoji, Masafumi Omura, Yoshiharu Tsurutani, Bruce T. Verkhoglyadova, Olga P. Lembege, Bertrand TI Mirror instability and L-mode electromagnetic ion cyclotron instability: Competition in the Earth's magnetosheath SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID SOLAR-WIND; ANISOTROPY INSTABILITIES; NUMERICAL-SIMULATION; WAVES; PLASMA; MAGNETOPAUSE; ULYSSES; MAGNETOSPHERE; DEPLETION; JUPITER AB We performed both two- nd three-dimensional hybrid simulations of the competing processes between the L-mode electromagnetic ion cyclotron (EMIC) and mirror instabilities, assuming anisotropic energetic ions with T(perpendicular to)/T(parallel to) = 4.0. In the two-imensional model, the energy of the EMIC waves is higher at the linear growth phase because its growth rate is larger than that of the mirror mode. In the three-dimensional model, however, the energy of the mirror mode waves is larger than that of the EMIC waves for all times because the wave number spectra of mirror mode waves form torus-like structures. We also theoretically derived a necessary condition for the dominance of the mirror instability. As the mirror mode waves relax the temperature anisotropy effectively, the linear growth rates of the EMIC waves become smaller before saturation. The EMIC waves cause heating of protons trapped by the nonlinear potentials due to coexistence of forward and backward propagating waves and inverse cascading. They terminate the linear growth of EMIC waves. Because of these parallel heatings, the temperature anisotropy decreases to the threshold of the mirror instability and thus the mirror mode wave saturates. At the nonlinear stage, coalescence of the mirror mode waves takes place in both models. The quick dissipation of the EMIC waves occurs due to the heating by the nonlinear processes. On the other hand, the coalescence is a much slower process than the nonlinear processes of EMIC waves, and thus the mirror mode waves remain in the three-dimensional model. C1 [Shoji, Masafumi; Omura, Yoshiharu; Lembege, Bertrand] Kyoto Univ, Res Inst Sustainable Humanosphere, Kyoto 6110011, Japan. [Tsurutani, Bruce T.; Verkhoglyadova, Olga P.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Lembege, Bertrand] CNRS, IPSL, UVSQ, LATMOS, F-78140 Velizy Villacoublay, France. RP Shoji, M (reprint author), Kyoto Univ, Res Inst Sustainable Humanosphere, Kyoto 6110011, Japan. EM shouji@rish.kyoto-u.ac.jp RI Omura, Yoshiharu/P-8565-2014; OI Omura, Yoshiharu/0000-0002-6683-3940; Verkhoglyadova, Olga/0000-0002-9295-9539 FU Japan Society for the Promotion of Science (JSPS); Creative Scientific Research "The Basic Study of Space Weather Prediction'' of the Ministry of Education, Science, Sports and Culture of Japan [17GS0208]; Jet Propulsion Laboratory, California Institute of Technology; National Aeronautics and Space Administration FX Computation in the present study was performed with the KDK system of Research Institute for Sustainable Humanosphere (RISH) and Academic Center for Computing and Media Studies at Kyoto University as a collaborative research project. The present study was supported in part by a Grant-in-Aid for Research Fellows from the Japan Society for the Promotion of Science (JSPS). This work was partially supported by 17GS0208 for Creative Scientific Research "The Basic Study of Space Weather Prediction'' of the Ministry of Education, Science, Sports and Culture of Japan. Portions of this work were performed at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. NR 31 TC 26 Z9 27 U1 0 U2 1 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD OCT 9 PY 2009 VL 114 AR A10203 DI 10.1029/2008JA014038 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 505PU UT WOS:000270707400001 ER PT J AU Schmidt, BE Thomas, PC Bauer, JM Li, JY McFadden, LA Mutchler, MJ Radcliffe, SC Rivkin, AS Russell, CT Parker, JW Stern, SA AF Schmidt, B. E. Thomas, P. C. Bauer, J. M. Li, J. -Y. McFadden, L. A. Mutchler, M. J. Radcliffe, S. C. Rivkin, A. S. Russell, C. T. Parker, J. Wm. Stern, S. A. TI The Shape and Surface Variation of 2 Pallas from the Hubble Space Telescope SO SCIENCE LA English DT Article ID TRIAXIAL ELLIPSOID DIMENSIONS; ADAPTIVE OPTICS; CERES; IMAGES; VESTA; ASTEROIDS AB We obtained Hubble Space Telescope images of 2 Pallas in September 2007 that reveal distinct color and albedo variations across the surface of this large asteroid. Pallas's shape is an ellipsoid with radii of 291 (+/- 9), 278 (+/- 9), and 250 (+/- 9) kilometers, implying a density of 2400 (+/- 250) kilograms per cubic meter-a value consistent with a body that formed from water-rich material. Our observations are consistent with the presence of an impact feature, 240 (+/- 25) kilometers in diameter, within Pallas's ultraviolet-dark terrain. Our observations imply that Pallas is an intact protoplanet that has undergone impact excavation and probable internal alteration. C1 [Schmidt, B. E.; Russell, C. T.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90095 USA. [Thomas, P. C.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. [Bauer, J. M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Li, J. -Y.; McFadden, L. A.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Mutchler, M. J.] STScI, Baltimore, MD USA. [Radcliffe, S. C.] Hydraulx, Santa Monica, CA 90401 USA. [Rivkin, A. S.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Parker, J. Wm.; Stern, S. A.] SW Res Inst, Boulder, CO 80302 USA. RP Schmidt, BE (reprint author), Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90095 USA. EM britneys@ucla.edu RI McFadden, Lucy-Ann/I-4902-2013; Rivkin, Andrew/B-7744-2016; OI McFadden, Lucy-Ann/0000-0002-0537-9975; Rivkin, Andrew/0000-0002-9939-9976; Schmidt, Britney/0000-0001-7376-8510 FU NASA [NAS 5-26555]; STScI [HST-GO-11115.01] FX Based on observations made with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy Inc. under NASA contract NAS 5-26555. The observations are associated with program 11115. Supported by STScI grant HST-GO-11115.01 (C. T. R.). NR 27 TC 22 Z9 22 U1 0 U2 2 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 J9 SCIENCE JI Science PD OCT 9 PY 2009 VL 326 IS 5950 BP 275 EP 278 DI 10.1126/science.1177734 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 504EX UT WOS:000270599500039 PM 19815773 ER PT J AU Hill, CJ Soibel, A Ting, DZY Keo, SA Mumolo, JM Nguyen, J Lee, M Gunapala, SD AF Hill, C. J. Soibel, A. Ting, D. Z. -Y. Keo, S. A. Mumolo, J. M. Nguyen, J. Lee, M. Gunapala, S. D. TI High temperature operation of long-wavelength infrared superlattice detector with supressed dark current SO ELECTRONICS LETTERS LA English DT Article ID PHOTODIODES AB Superlattice (SL) photodetectors operating with a cutoff wavelength of lambda = 10 mu m are demonstrated to respond up to a temperature of T = 140 K with a nonunity gain enabling a high responsivity of R = 25 A/W. The improvement in detector performance is achieved by the optimisation of SL heterodiode design in which suppression of dark current is realised without significant impact on the photocurrent. C1 [Hill, C. J.; Soibel, A.; Ting, D. Z. -Y.; Keo, S. A.; Mumolo, J. M.; Nguyen, J.; Lee, M.; Gunapala, S. D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Hill, CJ (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM asoibel@jpl.nasa.gov RI Soibel, Alexander/A-1313-2007 FU Missile Defense Agency; National Aeronautics and Space Administration FX The authors thank S. Bandara, J. K. Liu, and B. Yang for helpful discussions, and M. Tidrow, R. Liang, T. Luchik, A. Larson, M. Hermann, E. Kolawa, and P. Dimotakis for encouragement and support. The research described in this Letter was sponsored by the Missile Defense Agency, and was carried out at the Jet Propulsion Laboratory, California Institute of Technology, through an agreement with the National Aeronautics and Space Administration. NR 7 TC 11 Z9 11 U1 0 U2 3 PU INST ENGINEERING TECHNOLOGY-IET PI HERTFORD PA MICHAEL FARADAY HOUSE SIX HILLS WAY STEVENAGE, HERTFORD SG1 2AY, ENGLAND SN 0013-5194 J9 ELECTRON LETT JI Electron. Lett. PD OCT 8 PY 2009 VL 45 IS 21 BP 1089 EP U65 DI 10.1049/el.2009.1560 PG 2 WC Engineering, Electrical & Electronic SC Engineering GA 512VI UT WOS:000271279000021 ER PT J AU Wang, LL Qu, JJ Xiong, XX Hao, XJ AF Wang, Lingli Qu, John J. Xiong, Xiaoxiong Hao, Xianjun TI Analysis of seven-year moderate resolution imaging spectroradiometer vegetation water indices for drought and fire activity assessment over Georgia of the United States SO JOURNAL OF APPLIED REMOTE SENSING LA English DT Article DE vegetation drought; drought index; fire activity; vegetation water indices; MODIS ID FOREST-FIRES; SOYBEANS; CORN AB Using a seven-year history of the satellite measurements and meteorology data over Georgia, USA, this study investigated the capability of a series of satellite-derived vegetation water indices for drought monitoring, as well as the connection between fire occurrence and drought conditions. The vegetation water indices are normalized calculations between MODIS near infrared band 2 and shortwave infrared bands 5, 6, 7, and the difference between bands 6 and 7, denoted by NDWI2, 5, NDWI2, (6), NDWI2, (7) and NMDI, respectively. Results show that the drought conditions indicated by NMDI, NDWI2, (6) and NDWI2, 7 agree well with what have been identified by meteorology data. NMDI, however, has demonstrated more dependable results regarding seasonal moisture variations, as well as stronger responses to drought conditions than NDWI2, (6), and NDWI2, (7). The annual fire number exhibits high correspondence to drought conditions. Drought intensity also influenced fire extent and the most widespread fires occurred during the driest years. Analysis reveals that NMDI can be used as an effective indicator for fire risk monitoring. It is expected that this research will greatly benefit many applications, such as monitoring drought and detecting fire danger potential. C1 [Wang, Lingli; Qu, John J.; Hao, Xianjun] George Mason Univ, EastFIRE Lab, ESTC, Coll Sci, Fairfax, VA 22030 USA. [Xiong, Xiaoxiong] NASA, Goddard Space Flight Ctr, Biospher Sci Branch, Greenbelt, MD 20771 USA. RP Wang, LL (reprint author), George Mason Univ, EastFIRE Lab, ESTC, Coll Sci, Fairfax, VA 22030 USA. EM Lwang2@gmu.edu RI Hao, Xianjun/F-7253-2016; Hao, Xianjun/C-9543-2011 OI Hao, Xianjun/0000-0002-8186-6839; Hao, Xianjun/0000-0002-8186-6839 NR 25 TC 6 Z9 6 U1 0 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 OCT 8 PY 2009 VL 3 AR 033555 DI 10.1117/1.3256138 PG 12 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA 520YP UT WOS:000271886000003 ER PT J AU Kurtz, NT Markus, T Cavalieri, DJ Sparling, LC Krabill, WB Gasiewski, AJ Sonntag, JG AF Kurtz, Nathan T. Markus, Thorsten Cavalieri, Donald J. Sparling, Lynn C. Krabill, William B. Gasiewski, Albin J. Sonntag, John G. TI Estimation of sea ice thickness distributions through the combination of snow depth and satellite laser altimetry data SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS LA English DT Article ID OCEAN; PROJECT; CLIMATE; ALBEDO; REGION; MODEL AB Combinations of sea ice freeboard and snow depth measurements from satellite data have the potential to provide a means to derive global sea ice thickness values. However, large differences in spatial coverage and resolution between the measurements lead to uncertainties when combining the data. High-resolution airborne laser altimeter retrievals of snow-ice freeboard and passive microwave retrievals of snow depth taken in March 2006 provide insight into the spatial variability of these quantities as well as optimal methods for combining high-resolution satellite altimeter measurements with low-resolution snow depth data. The aircraft measurements show a relationship between freeboard and snow depth for thin ice allowing the development of a method for estimating sea ice thickness from satellite laser altimetry data at their full spatial resolution. This method is used to estimate snow and ice thicknesses for the Arctic basin through the combination of freeboard data from ICESat, snow depth data over first-year ice from AMSR-E, and snow depth over multiyear ice from climatological data. Due to the nonlinear dependence of heat flux on ice thickness, the impact on heat flux calculations when maintaining the full resolution of the ICESat data for ice thickness estimates is explored for typical winter conditions. Calculations of the basin-wide mean heat flux and ice growth rate using snow and ice thickness values at the similar to 70 m spatial resolution of ICESat are found to be approximately one-third higher than those calculated from 25-km mean ice thickness values. C1 [Kurtz, Nathan T.; Sparling, Lynn C.] Univ Maryland, Dept Phys, Baltimore, MD 21201 USA. [Markus, Thorsten; Cavalieri, Donald J.] NASA, Goddard Space Flight Ctr, Hydrospher & Biospher Sci Lab, Greenbelt, MD 20771 USA. [Krabill, William B.] NASA, Goddard Space Flight Ctr, Wallops Flight Facil, Wallops Isl, VA 23337 USA. [Gasiewski, Albin J.] Univ Colorado, Dept Elect & Comp Engn, Boulder, CO 80309 USA. [Sonntag, John G.] NASA, Goddard Space Flight Ctr, Wallops Flight Facil, EG&G Tech Serv, Wallops Isl, VA USA. RP Kurtz, NT (reprint author), Univ Maryland Baltimore Cty, Dept Phys, 1000 Hilltop Circle, Baltimore, MD 21250 USA. EM nkurtz1@umbc.edu RI Markus, Thorsten/D-5365-2012 FU NASA's Cryosphere Program FX We thank the mission and flight crew for their invaluable contributions to the AMSR-E 2006 campaign and the associate editor and two anonymous reviewers for their thorough reading of the manuscript and their constructive comments and suggestions. This work has been supported through NASA's Cryosphere Program. NR 37 TC 22 Z9 23 U1 0 U2 2 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-OCEANS JI J. Geophys. Res.-Oceans PD OCT 8 PY 2009 VL 114 AR C10007 DI 10.1029/2009JC005292 PG 16 WC Oceanography SC Oceanography GA 505OR UT WOS:000270704200001 ER PT J AU Manizza, M Follows, MJ Dutkiewicz, S McClelland, JW Menemenlis, D Hill, CN Townsend-Small, A Peterson, BJ AF Manizza, M. Follows, M. J. Dutkiewicz, S. McClelland, J. W. Menemenlis, D. Hill, C. N. Townsend-Small, A. Peterson, B. J. TI Modeling transport and fate of riverine dissolved organic carbon in the Arctic Ocean SO GLOBAL BIOGEOCHEMICAL CYCLES LA English DT Article ID SEA-ICE; MATTER; FLUX; WATER; THICKNESS; CLIMATE; BUDGET AB The spatial distribution and fate of riverine dissolved organic carbon ( DOC) in the Arctic may be significant for the regional carbon cycle but are difficult to fully characterize using the sparse observations alone. Numerical models of the circulation and biogeochemical cycles of the region can help to interpret and extrapolate the data and may ultimately be applied in global change sensitivity studies. Here we develop and explore a regional, three-dimensional model of the Arctic Ocean in which, for the first time, we explicitly represent the sources of riverine DOC with seasonal discharge based on climatological field estimates. Through a suite of numerical experiments, we explore the distribution of DOC-like tracers with realistic riverine sources and a simple linear decay to represent remineralization through microbial degradation. The model reproduces the slope of the DOC-salinity relationship observed in the eastern and western Arctic basins when the DOC tracer lifetime is about 10 years, consistent with published inferences from field data. The new empirical parameterization of riverine DOC and the regional circulation and biogeochemical model provide new tools for application in both regional and global change studies. C1 [Manizza, M.; Follows, M. J.; Dutkiewicz, S.; Hill, C. N.] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 01239 USA. [McClelland, J. W.] Univ Texas Austin, Inst Marine Sci, Port Aransas, TX 78373 USA. [Menemenlis, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Peterson, B. J.] Marine Biol Lab, Woods Hole, MA 02543 USA. [Townsend-Small, A.] Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA 92697 USA. RP Manizza, M (reprint author), MIT, Dept Earth Atmospher & Planetary Sci, 77 Massachusetts Ave, Cambridge, MA 01239 USA. EM mmanizza@ocean.mit.edu RI Follows, Michael/G-9824-2011; McClelland, James/C-5396-2008 OI McClelland, James/0000-0001-9619-8194 FU National Science Foundation FX This study has been carried out in the framework of the ECCO2 Project (http:W//ecco2.org), and it is also part of the project Synthesis of Arctic System Science I. M. M. and M. J. F. are grateful to National Science Foundation for financial support. M. M. thanks Jean-Michel Campin and Baylor Fox-Kemper for their valuable help with MITgcm, Alan Condron for useful discussions on Arctic circulation, and NASA for providing excellent support for scientific computation. We also thank Dennis Hansell and Nicholas Bates for constructive comments and guidance during the development of this study. Comments from two anonymous reviewers helped us to improve the weak parts of the initial version of our manuscript. NR 50 TC 32 Z9 32 U1 2 U2 18 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0886-6236 J9 GLOBAL BIOGEOCHEM CY JI Glob. Biogeochem. Cycle PD OCT 7 PY 2009 VL 23 AR GB4006 DI 10.1029/2008GB003396 PG 10 WC Environmental Sciences; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Geology; Meteorology & Atmospheric Sciences GA 505MG UT WOS:000270697100001 ER PT J AU Shi, QQ Pu, ZY Soucek, J Zong, QG Pu, ZY Xie, L Chen, Y Zhang, H Li, L Xia, LD Liu, ZX Lucek, E Fazakerley, AN Reme, H AF Shi, Q. Q. Pu, Z. Y. Soucek, J. Zong, Q. -G. Pu, Z. Y. Xie, L. Chen, Y. Zhang, H. Li, L. Xia, L. D. Liu, Z. X. Lucek, E. Fazakerley, A. N. Reme, H. TI Spatial structures of magnetic depression in the Earth's high-altitude cusp: Cluster multipoint observations SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID MIRROR-MODE STRUCTURES; LINEAR INSTABILITY; HYBRID SIMULATIONS; SOLAR-WIND; MAGNETOSHEATH; FIELD; MAGNETOSPHERE; HOLES; IDENTIFICATION; SPACECRAFT AB Magnetic depression structures (magnetic holes) of short time duration from seconds to minutes have been studied using Cluster data in the high-latitude cusp. Our multispacecraft analysis revealed that the magnetic depressions are spatial structures traveling across the spacecraft, and this result was further strengthened by the calculation of the boundary normal directions and velocities using various methods. In this article, we show that multiple properties of the magnetic depressions are consistent with those of mirror structures observed in the magnetosheath or solar wind. The plasma in the cusp is rarely unstable with respect to mirror instability. However, as has been shown by previous studies, once a large magnetic hole is created by mirror instability, it becomes relatively stable and can survive for extended periods of time even if surrounding plasma conditions drop well below the mirror threshold. Although local generation of these structures cannot be completely ruled out in some cases, we propose an interpretation of the magnetic depressions observed in the cusp as mirror structures generated upstream and convected to the cusp by plasma flow. Specifically, the magnetic holes could be generated in the magnetosheath and enter the cusp due to the open geometry of the cusp magnetic field. C1 [Shi, Q. Q.; Pu, Z. Y.; Zong, Q. -G.; Pu, Z. Y.; Xie, L.] Peking Univ, Inst Space Phys & Appl Technol, Beijing 100871, Peoples R China. [Fazakerley, A. N.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. [Shi, Q. Q.; Chen, Y.; Li, L.; Xia, L. D.] Shandong Univ, Sch Space Sci & Phys, Weihai 264209, Shandong, Peoples R China. [Liu, Z. X.] Chinese Acad Sci, Key Lab Space Weather, Ctr Space Sci & Appl Res, Beijing 100080, Peoples R China. [Lucek, E.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Space & Atmospher Phys Grp, London SW7 2AZ, England. [Reme, H.] Univ Toulouse 3, Ctr Etud Spatiale Rayonnements, F-31028 Toulouse, France. [Soucek, J.] Acad Sci Czech Republic, Inst Atmospher Phys, Dept Space Phys, Prague 11720, Czech Republic. [Zhang, H.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Reme, H.] CNRS, UMR 5187, Toulouse, France. RP Shi, QQ (reprint author), Peking Univ, Inst Space Phys & Appl Technol, Beijing 100871, Peoples R China. EM sqq@pku.edu.cn; zypu@pku.edu.cn RI Chen, Yao/B-7255-2011; Xia, Lidong/B-8836-2011; Soucek, Jan/G-3424-2014 OI Xia, Lidong/0000-0001-8938-1038; Soucek, Jan/0000-0003-0462-6804 FU NNSFC [40604022, 40731056, 40874086, 40831061, 40890162] FX This work is supported by NNSFC grants 40604022, 40731056, 40874086, 40831061, and 40890162. We are grateful to the instrument teams of FGM, CIS, and PEACE Cluster instruments and to Cluster Active Archive (CAA) for providing Cluster data. We also thank the CDAWeb for the ACE data used in this work. We thank T. L. Zhang and Z. Lin for their helpful discussions. NR 55 TC 18 Z9 22 U1 0 U2 5 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD OCT 7 PY 2009 VL 114 AR A10202 DI 10.1029/2009JA014283 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 505PS UT WOS:000270707200001 ER PT J AU Qiu, S Krishnan, VB Padula, SA Noebe, RD Brown, DW Clausen, B Vaidyanathan, R AF Qiu, S. Krishnan, V. B. Padula, S. A., II Noebe, R. D. Brown, D. W. Clausen, B. Vaidyanathan, R. TI Measurement of the lattice plane strain and phase fraction evolution during heating and cooling in shape memory NiTi SO APPLIED PHYSICS LETTERS LA English DT Article ID NEUTRON-DIFFRACTION; SUPERELASTIC NITI; TIC COMPOSITES; REFINEMENT; TEXTURE; SPECTRA AB We report on in situ neutron diffraction measurements during heating and cooling through the phase transformation in shape memory NiTi. The lattice plane specific strain evolution remains linear with temperature and is not influenced by intergranular stresses, enabling the determination of the thermal expansion tensor of B19' NiTi. The neutron measurements are consistent with macroscopic dilatometric measurements and a 30 000 grain polycrystalline self-consistent model. The accommodative nature of B19' NiTi results in macroscopic shape changes being offset (with temperature) from the start and finish of the transformation. The texture does not evolve in the absence of biasing stresses. (C) 2009 American Institute of Physics. [doi: 10.1063/1.3245308] C1 [Qiu, S.; Krishnan, V. B.; Vaidyanathan, R.] Univ Cent Florida, AMPAC, Orlando, FL 32816 USA. [Qiu, S.; Krishnan, V. B.; Vaidyanathan, R.] Univ Cent Florida, Mech Mat & Aerosp Engn Dept, Orlando, FL 32816 USA. [Padula, S. A., II; Noebe, R. D.] NASA, Glenn Res Ctr, Mat & Struct Div, Cleveland, OH 44135 USA. [Brown, D. W.; Clausen, B.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA. RP Qiu, S (reprint author), Univ Cent Florida, AMPAC, Orlando, FL 32816 USA. EM raj@mail.ucf.edu RI Clausen, Bjorn/B-3618-2015 OI Clausen, Bjorn/0000-0003-3906-846X FU NASA Fundamental Aeronautics Program; Supersonics Project [NNX08AB51A]; NSF [DMR-0239512]; Office of Basic Energy Sciences (DOE) FX S. Q., V. B. K., and R. V. acknowledge funding from the NASA Fundamental Aeronautics Program, Supersonics Project (Grant No. NNX08AB51A) and NSF (Grant No. CAREER DMR-0239512). The authors thank T. Sisneros, S. Kabra, J. Wall, and C. Aydiner at LANL for technical support. This work has benefited from the use of the Lujan Neutron Scattering Center at LANSCE, which is funded by the Office of Basic Energy Sciences (DOE). LANL is operated by Los Alamos National Security LLC under DOE under Contract No. DE-AC52-06NA25396. NR 23 TC 23 Z9 23 U1 0 U2 13 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 J9 APPL PHYS LETT JI Appl. Phys. Lett. PD OCT 5 PY 2009 VL 95 IS 14 AR 141906 DI 10.1063/1.3245308 PG 3 WC Physics, Applied SC Physics GA 505DW UT WOS:000270670200022 ER PT J AU Ray, RD AF Ray, Richard D. TI Secular changes in the solar semidiurnal tide of the western North Atlantic Ocean SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID FUNDY; MAINE; GULF; BAY; TRENDS; RANGE AB An analysis of twentieth century tide gauge records reveals that the solar semidiurnal tide S(2) has been decreasing in amplitude along the eastern coast of North America and at the mid-ocean site Bermuda. In relative terms the observed rates are unusually large, of order 10% per century. Periods of greatest change, however, are inconsistent among the stations, and roughly half the stations show increasing amplitude since the late 1990s. Excepting the Gulf of Maine, lunar tides are either static or slightly increasing in amplitude; a few stations show decreases. Large changes in solar, but not lunar, tides suggest causes related to variable radiational forcing, but the hypothesis is at present unproven. Citation: Ray, R. D. (2009), Secular changes in the solar semidiurnal tide of the western North Atlantic Ocean, Geophys. Res. Lett., 36, L19601, doi:10.1029/2009GL040217. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 21114 USA. RP Ray, RD (reprint author), NASA, Goddard Space Flight Ctr, Code 698, Greenbelt, MD 21114 USA. EM richard.ray@nasa.gov RI Ray, Richard/D-1034-2012 FU NASA Ocean Surface Topography program FX Work of this kind owes immeasurably to generations of anonymous tide-gauge operators. Their sea-level records have been refined, compiled, and archived by the University of Hawaii Sea Level Center and the British Oceanographic Data Centre, from which I obtained the hourly data used here. It is a pleasure to thank David Cartwright, Chris Garrett, Florent Lyard and Philip Woodworth for useful suggestions. This work was supported by the NASA Ocean Surface Topography program. NR 18 TC 18 Z9 18 U1 0 U2 2 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD OCT 2 PY 2009 VL 36 AR L19601 DI 10.1029/2009GL040217 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 502LW UT WOS:000270462600004 ER PT J AU Cooper, G Sant, M Asiyo, C AF Cooper, George Sant, Minakshi Asiyo, Cynthia TI Gas chromatography-mass spectrometry resolution of sugar acid enantiomers on a permethylated beta-cyclodextrin stationary phase SO JOURNAL OF CHROMATOGRAPHY A LA English DT Article DE Gas chromatography-mass spectrometry; Enantiomers; Sugar acid; Aldonic acid; Cyclodextrin; Chiralsil-Dex CB ID SEPARATION AB Analysis of compounds in meteorites revealed a need to simultaneously characterize multiple enantiomers of sugar acids (aldonic acids) present in trace amounts. Analyses by gas chromatography-mass spectrometry demonstrated that all but two of the three-carbon through six-carbon straight-chained sugar acid enantiomer pairs could be resolved using a single derivatization procedure and one set of GC parameters. Compounds were analyzed as their ethyl ester/O-triflouroacetyl, isopropyl ester/O-triflouroacetyl and isopropyl ester/O-pentafluoropropionyl derivatives on a capillary column containing permethylated beta-cyclodextrin (Chirasil-Dex CB) as the stationary phase. Characteristic mass fragments are related to the ester groups while several ions are also common to derivatized monosaccharides. Published by Elsevier B.V. C1 [Cooper, George; Sant, Minakshi; Asiyo, Cynthia] NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA. RP Cooper, G (reprint author), NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA. EM gcooper@mail.arc.nasa.gov FU NASA FX The authors are grateful to Dr. S. Pizzarello, Dr. J. Blank, and anonymous reviewers for their helpful suggestions and comments on the manuscript. We thank N. Ahuja, D. Nguyen, C. Reed and M. Carter for assistance with preparation of C-6 aldonic acids. This work was supported by NASA's Astrobiology Program. NR 22 TC 9 Z9 9 U1 0 U2 9 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0021-9673 J9 J CHROMATOGR A JI J. Chromatogr. A PD OCT 2 PY 2009 VL 1216 IS 40 BP 6838 EP 6843 DI 10.1016/j.chroma.2009.07.073 PG 6 WC Biochemical Research Methods; Chemistry, Analytical SC Biochemistry & Molecular Biology; Chemistry GA 500QD UT WOS:000270317500009 PM 19716135 ER PT J AU Hulley, GC Hook, SJ Manning, E Lee, SY Fetzer, E AF Hulley, Glynn C. Hook, Simon J. Manning, Evan Lee, Sung-Yung Fetzer, Eric TI Validation of the Atmospheric Infrared Sounder (AIRS) version 5 land surface emissivity product over the Namib and Kalahari deserts SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID TEMPERATURE; TRENDS AB Hyperspectral infrared sounders require accurate knowledge of the land surface emissivity (LSE) to retrieve important climate variables such as surface temperature, air temperature, and total water vapor from space. This study provides a method for validating and assessing the Atmospheric Infrared Sounder (AIRS) version 5 LSE product using high-spatial resolution data (90 m) from the Advanced Spaceborne Thermal Emission and Reflection Radiometer (ASTER) which has five bands in the thermal infrared region (8-12 mu m, 1250-833 cm(-1)) and high-spectral resolution laboratory measurements of sand samples collected over the Namib and Kalahari deserts in southern Africa. Results indicate that the mean, absolute daytime LSE difference between AIRS and the laboratory results for six wavelengths in window regions between 3.9 and 11.4 mu m (2564-877 cm(-1)) was 2.3% over the Namib and 0.70% over the Kalahari, while the mean difference with ASTER was 2.3% over the Namib and 2.26% over the Kalahari for four bands between 8 and 12 mu m. Systematic modeling and surface dependent AIRS LSE retrieval errors such as large discrepancies between day and nighttime shortwave LSE (up to 15%), unphysical values (LSE > 1), and large daytime temporal variations in the shortwave region (up to 30%) are further discussed. C1 [Hulley, Glynn C.; Hook, Simon J.; Manning, Evan; Lee, Sung-Yung; Fetzer, Eric] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Hulley, GC (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM glynn.hulley@jpl.nasa.gov NR 31 TC 21 Z9 22 U1 0 U2 8 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD OCT 2 PY 2009 VL 114 AR D19104 DI 10.1029/2009JD012351 PG 11 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 502MB UT WOS:000270463200001 ER PT J AU Arvidson, RE Bonitz, RG Robinson, ML Carsten, JL Volpe, RA Trebi-Ollennu, A Mellon, MT Chu, PC Davis, KR Wilson, JJ Shaw, AS Greenberger, RN Siebach, KL Stein, TC Cull, SC Goetz, W Morris, RV Ming, DW Keller, HU Lemmon, MT Sizemore, HG Mehta, M AF Arvidson, R. E. Bonitz, R. G. Robinson, M. L. Carsten, J. L. Volpe, R. A. Trebi-Ollennu, A. Mellon, M. T. Chu, P. C. Davis, K. R. Wilson, J. J. Shaw, A. S. Greenberger, R. N. Siebach, K. L. Stein, T. C. Cull, S. C. Goetz, W. Morris, R. V. Ming, D. W. Keller, H. U. Lemmon, M. T. Sizemore, H. G. Mehta, M. TI Results from the Mars Phoenix Lander Robotic Arm experiment SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID PHYSICAL-PROPERTIES; MARTIAN SURFACE; LANDING SITE; SOIL; LOCALIZATION AB The Mars Phoenix Lander was equipped with a 2.4 m Robotic Arm (RA) with an Icy Soil Acquisition Device capable of excavating trenches in soil deposits, grooming hard icy soil surfaces with a scraper blade, and acquiring icy soil samples using a rasp tool. A camera capable of imaging the scoop interior and a thermal and electrical conductivity probe were also included on the RA. A dozen trench complexes were excavated at the northern plains landing site and 31 samples (including water-ice-bearing soils) were acquired for delivery to instruments on the Lander during the 152 sol mission. Deliveries included sprinkling material from several centimeters height to break up cloddy soils on impact with instrument portals. Excavations were done on the side of the Humpty Dumpty and the top of the Wonderland polygons, and in nearby troughs. Resistive forces encountered during backhoe operations show that soils above the 3-5 cm deep icy soil interfaces are stronger with increasing depth. Further, soils are similar in appearance and properties to the weakly cohesive crusty and cloddy soils imaged and excavated by the Viking Lander 2, which also landed on the northern plains. Adsorbed H2O is inferred to be responsible for the variable nature and cohesive strength of the soils. Backhoe blade chatter marks on excavated icy soil surfaces, combined with rasp motor currents, are consistent with laboratory experiments using grain-supported icy soil deposits, as is the relatively rapid decrease in icy soil strength over time as the ice sublimated on Mars. C1 [Arvidson, R. E.; Shaw, A. S.; Greenberger, R. N.; Siebach, K. L.; Stein, T. C.; Cull, S. C.] Washington Univ, Dept Earth & Planetary Sci, St Louis, MO 63130 USA. [Bonitz, R. G.; Robinson, M. L.; Carsten, J. L.; Volpe, R. A.; Trebi-Ollennu, A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Chu, P. C.; Davis, K. R.; Wilson, J. J.] Honeybee Robot Spacecraft Mech Corp, New York, NY 10001 USA. [Goetz, W.; Keller, H. U.] Max Planck Inst Sonnensyst Forsch, D-37191 Katlenburg Lindau, Germany. [Lemmon, M. T.] Texas A&M Univ, Dept Atmospher Sci, College Stn, TX 77843 USA. [Mehta, M.] Univ Michigan, Ann Arbor, MI 48109 USA. [Mellon, M. T.; Sizemore, H. G.] Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80303 USA. [Morris, R. V.; Ming, D. W.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77508 USA. RP Arvidson, RE (reprint author), Washington Univ, Dept Earth & Planetary Sci, Campus Box 1169,1 Brookings Dr, St Louis, MO 63130 USA. EM arvidson@wunder.wustl.edu RI Lemmon, Mark/E-9983-2010; Mellon, Michael/C-3456-2016; OI Lemmon, Mark/0000-0002-4504-5136; Siebach, Kirsten/0000-0002-6628-6297; Greenberger, Rebecca/0000-0003-1583-0261 FU National Aeronautics and Space Administration FX We thank the capable team of engineers and scientists who made the Phoenix mission possible and we thank NASA for its support of our endeavors. Part of this research and the work of R. Bonitz, M. Robinson, R. Volpe, A. Trebi-Ollennu, and J. Carsten 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 41 Z9 41 U1 1 U2 14 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9097 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD OCT 2 PY 2009 VL 114 AR E00E02 DI 10.1029/2009JE003408 PG 21 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 502MN UT WOS:000270464600001 ER PT J AU Baker, DN Odstrcil, D Anderson, BJ Arge, CN Benna, M Gloeckler, G Raines, JM Schriver, D Slavin, JA Solomon, SC Killen, RM Zurbuchen, TH AF Baker, Daniel N. Odstrcil, Dusan Anderson, Brian J. Arge, C. Nick Benna, Mehdi Gloeckler, George Raines, Jim M. Schriver, David Slavin, James A. Solomon, Sean C. Killen, Rosemary M. Zurbuchen, Thomas H. TI Space environment of Mercury at the time of the first MESSENGER flyby: Solar wind and interplanetary magnetic field modeling of upstream conditions SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID MAGNETOSPHERE; TRANSPORT; EXOSPHERE AB The first flyby of Mercury by the Mercury Surface, Space Environment, Geochemistry and Ranging (MESSENGER) spacecraft occurred on 14 January 2008. In order to provide contextual information about the solar wind (SW) properties and the interplanetary magnetic field near the planet, we have used an empirical modeling technique combined with a numerical physics-based SW model. The Wang-Sheeley-Arge (WSA) method uses solar photospheric magnetic field observations (from Earth-based instruments) in order to estimate inner heliospheric conditions out to 21.5 solar radii from the Sun. This information is then used as input to the global numerical magnetohydrodynamic model, ENLIL, which calculates SW velocity, density, temperature, and magnetic field strength and polarity throughout the inner heliosphere. The present paper shows WSA-ENLIL conditions computed for the several week period encompassing the first flyby. This information is used in conjunction with MESSENGER magnetometer data (and the only limited available MESSENGER SW plasma data) to help understand the Mercury flyby results. The in situ spacecraft data, in turn, can also be used iteratively to improve the model accuracy for inner heliospheric "space weather" purposes. Looking to the future, we discuss how with such modeling we can estimate relatively continuously the SW properties near Mercury and at the cruise location of MESSENGER now, for upcoming flybys, and toward the time of spacecraft orbit insertion in 2011. C1 [Baker, Daniel N.] Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80309 USA. [Odstrcil, Dusan] NOAA, Boulder, CO 80303 USA. [Odstrcil, Dusan] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA. [Anderson, Brian J.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Arge, C. Nick] USAF, Res Lab, Kirtland AFB, NM 87117 USA. [Benna, Mehdi] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA. [Gloeckler, George; Raines, Jim M.; Zurbuchen, Thomas H.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. [Killen, Rosemary M.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Schriver, David] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90095 USA. [Slavin, James A.] NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Greenbelt, MD 20771 USA. [Solomon, Sean C.] Carnegie Inst Washington, Dept Terr Magnetism, Washington, DC 20015 USA. RP Baker, DN (reprint author), Univ Colorado, Atmospher & Space Phys Lab, 1234 Innovat Dr, Boulder, CO 80309 USA. EM daniel.baker@lasp.colorado.edu RI Anderson, Brian/I-8615-2012; Slavin, James/H-3170-2012; Benna, Mehdi/F-3489-2012 OI Slavin, James/0000-0002-9206-724X; FU NASA Discovery Program [NASW-00002]; National Science Foundation Center for Integrated Space Weather Modeling (CISM); [NAS5-97271] FX Wolfgang Baumjohann thanks the reviewers for their assistance in evaluating this paper. NR 17 TC 30 Z9 30 U1 0 U2 2 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD OCT 2 PY 2009 VL 114 AR A10101 DI 10.1029/2009JA014287 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 502MU UT WOS:000270465300001 ER PT J AU Christiansen, EL Nagy, K Lear, DM Prior, TG AF Christiansen, Eric L. Nagy, Kornel Lear, Dana M. Prior, Thomas G. TI Space station MMOD shielding SO ACTA ASTRONAUTICA LA English DT Article ID DEBRIS AB This paper describes the International Space Station (ISS) micro-meteoroid orbital debris (MMOD) impact shielding including the requirements for protection as well as technical approaches to meeting the requirements. Current activities in providing MMOD protection for ISS are described, including efforts to augment MMOD protection by adding shields on-orbit. Another activity is to observe MMOD impact damage on ISS elements and returned hardware, and to compare the observed damage with predicted damage using Bumper code risk assessment software. A conclusion of this paper is that ISS will be protected adequately from MMOD impact after completing augmentation of ISS shielding for service module, and after improving MMOD protection for Soyuz and Progress vehicles. Another conclusion is that impact damage observed to the ISS mini-pressurized logistics module matches the distribution of impacts predicted by Bumper code. (C) 2009 Published by Elsevier Ltd. C1 [Christiansen, Eric L.; Lear, Dana M.; Prior, Thomas G.] NASA, Lyndon B Johnson Space Ctr, ESCG KX, Houston, TX 77058 USA. RP Christiansen, EL (reprint author), NASA, Lyndon B Johnson Space Ctr, ESCG KX, Houston, TX 77058 USA. EM Eric.L.Christiansen@nasa.gov; Kornel.Nagy@nasa.gov; Dana.M.Lear@nasa.gov; Thomas.G.Prior@nasa.gov NR 12 TC 5 Z9 5 U1 0 U2 7 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0094-5765 J9 ACTA ASTRONAUT JI Acta Astronaut. PD OCT-NOV PY 2009 VL 65 IS 7-8 BP 921 EP 929 DI 10.1016/j.actaastro.2008.01.046 PG 9 WC Engineering, Aerospace SC Engineering GA 491TC UT WOS:000269601500003 ER PT J AU Quadrelli, MB West, J AF Quadrelli, Marco B. West, John TI Sensitivity studies of the deployment of a square inflatable solar sail with vanes SO ACTA ASTRONAUTICA LA English DT Article DE Solar sail; Attitude dynamics; Attitude control; Dynamic stability AB This paper summarizes the results of numerical experiments to determine the sensitivity of the final attitude of an inflatable solar sail with vanes after deployment to various parameters affecting the deployment process. These parameters are: in- and out-of-plane asymmetries during deployment, length inflation profile. and vane deployment failures. We show how robust the sail deployment is to geometric asymmetries before a 35 degrees off-Sun angle is reached. Differential delays in the time to inflate the booms and a boom sweep-back angle affect the stability favorably. Adjacent vane failures to deploy affect the stability unfavorably, while the failure of opposing vanes is acceptable. Realistic boom length rate profiles obtained during ground tests are used in the Simulation showing that failing adjacent vanes in conjunction with initial inflation delays in adjacent booms represent the worst case. We also demonstrate that by feeding back attitude and attitude rate measurements so that a corrective action is taken during the deployment, the final attitude can be maintained very close to the initial attitude, thus mitigating the attitude changes incurred during deployment. (C) 2009 Elsevier Ltd. All rights reserved. C1 [Quadrelli, Marco B.] CALTECH, Jet Prop Lab, Guidance & Control Anal Grp, Guidance Navigat & Control Sect, Pasadena, CA 91109 USA. [West, John] CALTECH, Jet Prop Lab, Near Earth Mission Architecture Grp, Mission & Syst Architecture Sect, Pasadena, CA 91109 USA. RP Quadrelli, MB (reprint author), CALTECH, Jet Prop Lab, Guidance & Control Anal Grp, Guidance Navigat & Control Sect, Mail Stop 198-326, Pasadena, CA 91109 USA. EM Marco.B.Quadrelli@jpl.nasa.gov FU Jet Propulsion Laboratory, California Institute of Technology FX This research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and SpaceAdministration. The authors are grateful to Dr. Gurkirpal Singh of JPL for valuable discussions. NR 11 TC 5 Z9 6 U1 4 U2 13 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0094-5765 J9 ACTA ASTRONAUT JI Acta Astronaut. PD OCT-NOV PY 2009 VL 65 IS 7-8 BP 1007 EP 1027 DI 10.1016/j.actaastro.2009.03.015 PG 21 WC Engineering, Aerospace SC Engineering GA 491TC UT WOS:000269601500012 ER PT J AU Korakianitis, T Boruta, M Jerovsek, J Meitner, PL AF Korakianitis, T. Boruta, M. Jerovsek, J. Meitner, P. L. TI Performance of a single nutating disk engine in the 2 to 500 kW power range SO APPLIED ENERGY LA English DT Article DE Advanced power generation; Novel engine; Nutating disk; Engine performance; High thermal efficiency; Low fuel consumption; Power; Power density AB A new type of internal combustion engine with distinct advantages over conventional piston-engines and gas turbines in small power ranges is presented. The engine has analogies with piston engine operation, but like gas turbines it has dedicated spaces and devices for compression, burning and expansion. The engine operates on a modified limited-pressure thermodynamic cycle. The core of the engine is a nutating non-rotating disk, with the center of its hub mounted in the middle of a Z-shaped shaft. The two ends of the shaft rotate, while the disk nutates. The motion of the disk circumference prescribes a portion of a sphere. In the single-disk configuration a portion of the surface area of the disk is used for intake and compression, a portion is used to seal against a center casing, and the remaining portion is used for expansion and exhaust. The compressed air is admitted to an external accumulator, and then into an external combustion chamber before it is admitted to the power side of the disk. The external combustion chamber enables the engine to operate on a variable compression ratio cycle. Variations in cycle temperature ratio and compression ratio during normal operation enable the engine to effectively become a variable-cycle engine, allowing significant flexibility for optimizing efficiency or power output. The thermal efficiency is similar to that of medium sized diesel engines. For the same engine volume and weight this engine produces approximately twice the power of a two-stroke engine and four times the power of a four-stroke engine. The computed sea-level engine performance at design and off-design conditions in the 2 to 500 kW power range is presented. (C) 2009 Elsevier Ltd. All rights reserved. C1 [Korakianitis, T.] Univ London, Sch Mat Sci & Engn, London, England. [Boruta, M.; Jerovsek, J.] Kinet BEI LLC, S Elgin, IL USA. [Meitner, P. L.] USA, Res Lab, Glenn Res Ctr, Cleveland, OH USA. RP Korakianitis, T (reprint author), Univ London, Sch Mat Sci & Engn, London, England. EM theodosios@alum.mit.edu NR 23 TC 11 Z9 11 U1 0 U2 2 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0306-2619 EI 1872-9118 J9 APPL ENERG JI Appl. Energy PD OCT PY 2009 VL 86 IS 10 BP 2213 EP 2221 DI 10.1016/j.apenergy.2009.01.006 PG 9 WC Energy & Fuels; Engineering, Chemical SC Energy & Fuels; Engineering GA 446NU UT WOS:000266129100042 ER PT J AU Navarro-Gonzalez, R Iniguez, E de la Rosa, J McKay, CP AF Navarro-Gonzalez, Rafael Iniguez, Enrique de la Rosa, Jose McKay, Christopher P. TI Characterization of Organics, Microorganisms, Desert Soils, and Mars-like Soils by Thermal Volatilization Coupled to Mass Spectrometry and Their Implications for the Search for Organics on Mars by Phoenix and Future Space Missions SO ASTROBIOLOGY LA English DT Article DE Astrobiology; Mars; Mass spectrometry; Organic matter; Planetary instrumentation ID EVOLVED GAS ANALYZER; MARTIAN SOIL; EXTRACTION TECHNIQUE; NITRIC-OXIDE; CHROMATOGRAPHY; MATTER; LIFE; PYROLYSIS; DECOMPOSITION; EXPLORATION AB A key goal for astrobiology is the search for evidence of life on Mars. Because liquid water is a fundamental environmental requirement for life, the recent set of missions to Mars have focused on a strategy known as "follow the water.'' Since life is made of organic molecules, a logical next step is "follow the organics.'' However, organics are expected to be present at very low levels on Mars, which would make their detection challenging. Viking was unable to detect organics at parts per billion (ppb), but the effective upper limit could be higher due to the low efficiency of the thermal volatilization (TV) step in releasing organics. Due to its ease of use, TV is still the method selected for current and future NASA and ESA missions. Here, we show that when organics are present in the soil at levels above 1500 parts per million (ppm), there are several characteristic organic fragments detected by TV-mass spectrometry; however, when the levels are below < 150 ppm, TV oxidizes them, and no organic fragments are released. Instead, nitric oxide (NO) is produced and can be used to determine quantitatively the organic content if the C/N ratio is determined. Any atmospheric NO sorbed or mineral nitrogen (e. g., nitrates) present in the soil would release NO by TV at distinctive temperature regimes that would not overlap with the organic nitrogen source. Therefore, we suggest that monitoring NO provides the best chance for Phoenix and other future Mars missions to detect nitrogen-containing organics in the soil or ice. C1 [Navarro-Gonzalez, Rafael; Iniguez, Enrique; de la Rosa, Jose] Univ Nacl Autonoma Mexico, Inst Ciencias Nucl, Lab Quim Plasmas & Estudios Planetarios, Mexico City 04510, DF, Mexico. [McKay, Christopher P.] NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA. RP Navarro-Gonzalez, R (reprint author), Univ Nacl Autonoma Mexico, Inst Ciencias Nucl, Lab Quim Plasmas & Estudios Planetarios, Ciudad Univ,Apartado Postal 70-543, Mexico City 04510, DF, Mexico. EM navarro@nucleares.unam.mx RI Iniguez, Enrique/D-5208-2009; Gonzalez, Rafael/D-1748-2009; De la Rosa, Jose/A-3573-2010 OI Iniguez, Enrique/0000-0001-8062-8225; FU National Autonomous University of Mexico [IN 107107]; National Council of Science and Technology of Mexico (CONACyT) [45810-F] FX Funding for this research comes from grants from the National Autonomous University of Mexico (IN 107107) and the National Council of Science and Technology of Mexico (CONACyT 45810-F). C. P. M. acknowledges support from the Phoenix mission. R. N.-G. also acknowledges Rosa Estela Navarro-Gonzalez from the Institute of Cellular Physiology of the National Autonomous University of Mexico for providing some of the biomolecules or microorganisms used in this study. NR 61 TC 15 Z9 16 U1 3 U2 22 PU MARY ANN LIEBERT INC PI NEW ROCHELLE PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA SN 1531-1074 J9 ASTROBIOLOGY JI Astrobiology PD OCT PY 2009 VL 9 IS 8 BP 703 EP 715 DI 10.1089/ast.2008.0284 PG 13 WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics; Geology GA 509DF UT WOS:000270993600002 PM 19845443 ER PT J AU Beaty, DW Allen, CC Bass, DS Buxbaum, KL Campbell, JK Lindstrom, DJ Miller, SL Papanastassiou, DA AF Beaty, David W. Allen, Carlton C. Bass, Deborah S. Buxbaum, Karen L. Campbell, James K. Lindstrom, David J. Miller, Sylvia L. Papanastassiou, Dimitri A. TI Planning Considerations for a Mars Sample Receiving Facility: Summary and Interpretation of Three Design Studies SO ASTROBIOLOGY LA English DT Article DE Mars; Sample Receiving Facility (SRF); Mars Sample Return (MSR); Curation; Biosafety; Test protocol; Sample preservation; Containment; Clean room; NASA; Planetary protection ID RETURN; CURATION AB It has been widely understood for many years that an essential component of a Mars Sample Return mission is a Sample Receiving Facility (SRF). The purpose of such a facility would be to take delivery of the flight hardware that lands on Earth, open the spacecraft and extract the sample container and samples, and conduct an agreed-upon test protocol, while ensuring strict containment and contamination control of the samples while in the SRF. Any samples that are found to be non-hazardous (or are rendered non-hazardous by sterilization) would then be transferred to long-term curation. Although the general concept of an SRF is relatively straightforward, there has been considerable discussion about implementation planning. The Mars Exploration Program carried out an analysis of the attributes of an SRF to establish its scope, including minimum size and functionality, budgetary requirements (capital cost, operating costs, cost profile), and development schedule. The approach was to arrange for three independent design studies, each led by an architectural design firm, and compare the results. While there were many design elements in common identified by each study team, there were significant differences in the way human operators were to interact with the systems. In aggregate, the design studies provided insight into the attributes of a future SRF and the complex factors to consider for future programmatic planning. C1 [Beaty, David W.; Bass, Deborah S.; Buxbaum, Karen L.; Campbell, James K.; Miller, Sylvia L.] CALTECH, Jet Prop Lab, Mars Program Off, Pasadena, CA 91109 USA. [Allen, Carlton C.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Lindstrom, David J.] NASA Headquarters, Washington, DC USA. RP Bass, DS (reprint author), CALTECH, Jet Prop Lab, Mars Program Off, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Deborah.Bass@jpl.nasa.gov NR 32 TC 6 Z9 6 U1 1 U2 9 PU MARY ANN LIEBERT INC PI NEW ROCHELLE PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA SN 1531-1074 J9 ASTROBIOLOGY JI Astrobiology PD OCT PY 2009 VL 9 IS 8 BP 745 EP 758 DI 10.1089/ast.2009.0339 PG 14 WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics; Geology GA 509DF UT WOS:000270993600005 PM 19845446 ER PT J AU Maule, J Wainwright, N Steele, A Monaco, L Morris, H Gunter, D Damon, M Wells, M AF Maule, Jake Wainwright, Norm Steele, Andrew Monaco, Lisa Morris, Heather Gunter, Daniel Damon, Michael Wells, Mark TI Rapid Culture-Independent Microbial Analysis Aboard the International Space Station (ISS) SO ASTROBIOLOGY LA English DT Article DE International Space Station (ISS); Crew health; Planetary protection; Contamination control ID MICROBIOLOGICAL PROFILES; NONCULTURABLE STATE; HOSPITAL FABRICS; DRINKING-WATER; ENDOTOXIN; BACTERIA; LIMULUS; RESUSCITATION; CONTAMINATION; COAGULATION AB A new culture-independent system for microbial monitoring, called the Lab-On-a-Chip Application Development Portable Test System (LOCAD-PTS), was operated aboard the International Space Station (ISS). LOCAD-PTS was launched to the ISS aboard Space Shuttle STS-116 on December 9, 2006, and has since been used by ISS crews to monitor endotoxin on cabin surfaces. Quantitative analysis was performed within 15 minutes, and sample return to Earth was not required. Endotoxin (a marker of Gram-negative bacteria and fungi) was distributed throughout the ISS, despite previous indications that most bacteria on ISS surfaces were Gram-positive. Endotoxin was detected at 24 out of 42 surface areas tested and at every surface site where colony-forming units (cfu) were observed, even at levels of 4-120 bacterial cfu per 100 cm(2), which is below NASA in-flight requirements (< 10,000 bacterial cfu per 100 cm(2)). Absent to low levels of endotoxin (< 0.24 to 1.0 EU per 100 cm(2); defined in endotoxin units, or EU) were found on 31 surface areas, including on most panels in Node 1 and the US Lab. High to moderate levels (1.01 to 14.7 EU per 100 cm(2)) were found on 11 surface areas, including at exercise, hygiene, sleeping, and dining facilities. Endotoxin was absent from airlock surfaces, except the Extravehicular Hatch Handle (> 3.78 EU per 100 cm(2)). Based upon data collected from the ISS so far, new culture-independent requirements (defined in EU) are suggested, which are verifiable in flight with LOCAD-PTS yet high enough to avoid false alarms. The suggested requirements are intended to supplement current ISS requirements (defined in cfu) and would serve a dual purpose of safeguarding crew health (internal spacecraft surfaces < 20 EU per 100 cm(2)) and monitoring forward contamination during Constellation missions (surfaces periodically exposed to the external environment, including the airlock and space suits, < 0.24 EU per 100 cm(2)). C1 [Maule, Jake; Damon, Michael] BAE Syst, Huntsville, AL 35806 USA. [Wainwright, Norm] Charles River Labs, Charleston, SC USA. [Steele, Andrew] Carnegie Inst Sci, Geophys Lab, Washington, DC USA. [Monaco, Lisa; Morris, Heather] Jacobs Technol Inc, Huntsville, AL USA. [Gunter, Daniel] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. [Wells, Mark] Univ Alabama, Huntsville, AL 35899 USA. RP Maule, J (reprint author), BAE Syst, 308 Voyager Way, Huntsville, AL 35806 USA. EM giles.maule-1@nasa.gov FU NASA's Exploration Technology Development Program; Advanced Environmental Monitoring and Control FX We would like to thank NASA's Exploration Technology Development Program and the Advanced Environmental Monitoring and Control project for funding this work. Special thanks to astronauts Suni Williams, Peggy Whitson, Dan Tani, Greg Chamitoff, Mike Fincke, Sandy Magnus, Mike Barratt, Koichi Wakata, and Tim Kopra (Expeditions 14 to 20) who operated LOCAD-PTS aboard the ISS between March 2007 and September 2009. We are grateful to Payload Integration Managers Lorrie Hellier and Jeff Durham, ISS Program Scientist Julie Robinson, Increment Payload Manager Christian Maender, and ISS Increment Scientists Vic Cooley, Kenol Jules, Jorge Sotomayor, and Jennifer Comella, for facilitating on-orbit operations. We'd especially like to thank our friends and colleagues at NASA Johnson Space Center: Duane Pierson, Mark Ott, Victoria Castro, Willy Wong, Anthony Jeevarajan, Bekki Bruce, Jeff Jones, and Dan Burbank for their continual input and support of LOCADPTS as a tool to further human space exploration. NR 67 TC 10 Z9 11 U1 5 U2 24 PU MARY ANN LIEBERT INC PI NEW ROCHELLE PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA SN 1531-1074 J9 ASTROBIOLOGY JI Astrobiology PD OCT PY 2009 VL 9 IS 8 BP 759 EP 775 DI 10.1089/ast.2008.0319 PG 17 WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics; Geology GA 509DF UT WOS:000270993600006 PM 19845447 ER PT J AU Straughn, AN Pirzkal, N Meurer, GR Cohen, SH Windhorst, RA Malhotra, S Rhoads, J Gardner, JP Hathi, NP Jansen, RA Grogin, N Panagia, N Alighieri, SD Gronwall, C Walsh, J Pasquali, A Xu, C AF Straughn, Amber N. Pirzkal, Norbert Meurer, Gerhardt R. Cohen, Seth H. Windhorst, Rogier A. Malhotra, Sangeeta Rhoads, James Gardner, Jonathan P. Hathi, Nimish P. Jansen, Rolf A. Grogin, Norman Panagia, Nino Alighieri, Sperello di Serego Gronwall, Caryl Walsh, Jeremy Pasquali, Anna Xu, Chun TI EMISSION-LINE GALAXIES FROM THE HUBBLE SPACE TELESCOPE PROBING EVOLUTION AND REIONIZATION SPECTROSCOPICALLY (PEARS) GRISM SURVEY. I. THE SOUTH FIELDS SO ASTRONOMICAL JOURNAL LA English DT Article DE catalogs; galaxies: starburst; techniques: spectroscopic ID H-II-REGIONS; STAR-FORMATION RATE; ULTRA DEEP FIELD; ALPHA LUMINOSITY FUNCTION; LYMAN-BREAK GALAXIES; STIS PARALLEL SURVEY; SPIRAL GALAXIES; O-II; RADIAL-DISTRIBUTION; STARBURST GALAXIES AB We present results of a search for emission-line galaxies (ELGs) in the southern fields of the Hubble Space Telescope Probing Evolution And Reionization Spectroscopically (PEARS) grism survey. The PEARS South Fields consist of five Advanced Camera for Surveys pointings (including the Hubble Ultra Deep Field) with the G800L grism for a total of 120 orbits, revealing thousands of faint object spectra in the GOODS-South region of the sky. ELGs are one subset of objects that are prevalent among the grism spectra. Using a two-dimensional detection and extraction procedure, we find 320 emission lines originating from 226 galaxy "knots" within 192 individual galaxies. Line identification results in 118 new grism-spectroscopic redshifts for galaxies in the GOODS-South Field. We measure emission-line fluxes using standard Gaussian fitting techniques. At the resolution of the grism data, the H beta and [O III] doublet are blended. However, by fitting two Gaussian components to the H beta and [O III] features, we find that many of the PEARS ELGs have high[O III]/H beta ratios compared to other galaxy samples of comparable luminosities. The star formation rates of the ELGs are presented, as well as a sample of distinct giant star-forming regions at z similar to 0.1-0.5 across individual galaxies. We find that the radial distances of these H II regions in general reside near the galaxies' optical continuum half-light radii, similar to those of giant H II regions in local galaxies. C1 [Straughn, Amber N.; Gardner, Jonathan P.] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Pirzkal, Norbert; Grogin, Norman; Panagia, Nino] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Meurer, Gerhardt R.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Cohen, Seth H.; Windhorst, Rogier A.; Malhotra, Sangeeta; Rhoads, James; Jansen, Rolf A.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [Hathi, Nimish P.] Univ Calif Riverside, Dept Phys & Astron, Riverside, CA 92521 USA. [Alighieri, Sperello di Serego] INAF Osservatorio Astrofis Arcetri, I-50125 Florence, Italy. [Gronwall, Caryl] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Walsh, Jeremy] ESO Space Telescope European Coordinating Facil, D-85748 Garching, Germany. [Pasquali, Anna] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Xu, Chun] Acad Sinica, Shanghai Inst Tech Phys, Shanghai 200083, Peoples R China. RP Straughn, AN (reprint author), NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Astrophys Sci Div, Code 665, Greenbelt, MD 20771 USA. EM Amber.N.Straughn@nasa.gov RI di Serego Alighieri, Sperello/E-4067-2010; Hathi, Nimish/J-7092-2014 OI di Serego Alighieri, Sperello/0000-0001-8769-2692; Hathi, Nimish/0000-0001-6145-5090 FU NASA [NAS 5-26555]; STScI [HST-GO-10530, HST-GO-9793] FX We thank Mark Dickinson for useful discussions. This research was supported in part by the NASA/UNCFSP Harriett G. Jenkins Predoctoral Fellowship program and by an appointment to the NASA Postdoctoral Program at Goddard Space Flight Center, administered by Oak Ridge Associated Universities through a contract with NASA ( ANS), as well as by grants HST-GO-10530 & HST-GO-9793 from STScI, which is operated by AURA for NASA under contract NAS 5-26555. We thank the anonymous referee for helpful comments that improved the paper. NR 59 TC 22 Z9 22 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD OCT PY 2009 VL 138 IS 4 BP 1022 EP 1031 DI 10.1088/0004-6256/138/4/1022 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 493WD UT WOS:000269768500002 ER PT J AU Solano, E von Braun, K Velasco, A Ciardi, DR Gutierrez, R McElroy, DL Lopez, M Abajian, M Garcia, M Ali, B Sarro, LM Berriman, GB Bryden, G Chan, B Good, J Kane, SR Laity, AC Lau, C Payne, AN Plavchan, P Ramirez, S Schmitz, M Stauffer, JR Wyatt, PL Zhang, A AF Solano, E. von Braun, K. Velasco, A. Ciardi, D. R. Gutierrez, R. McElroy, D. L. Lopez, M. Abajian, M. Garcia, M. Ali, B. Sarro, L. M. Berriman, G. B. Bryden, G. Chan, B. Good, J. Kane, S. R. Laity, A. C. Lau, C. Payne, A. N. Plavchan, P. Ramirez, S. Schmitz, M. Stauffer, J. R. Wyatt, P. L. Zhang, A. TI The LAEX and NASA portals for CoRoT public data SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE astronomical data bases: miscellaneous; catalogs; surveys; stars: fundamental parameters; planetary systems; stars: variables: general ID VARIABLE-STARS; PLANETARY OCCULTATIONS; FIELD; SEARCH; TELESCOPE; TRANSITS; NGC-2301; TRES-2 AB Aims. We describe here the main functionalities of the LAEX (Laboratorio de Astrofisica Estelar y Exoplanetas/Laboratory for Stellar Astrophysics and Exoplanets) and NASA portals for CoRoT Public Data. The CoRoT archive at LAEX was opened to the community in January 2009 and is managed in the framework of the Spanish Virtual Observatory. NStED (NASA Star and Exoplanet Database) serves as the CoRoT portal for the US astronomical community. NStED is a general purpose stellar and exoplanet archive with the aim of providing support for NASA's planet finding and characterisation goals, and the planning and support of NASA and other space missions. CoRoT data at LAEX and NStED can be accessed at http://sdc.laeff.inta.es/corotfa/ and http://nsted.ipac.caltech.edu, respectively. Methods. Based on considerable experience with astronomical archives, the aforementioned archives are designed with the aim of delivering science-quality data in a simple and efficient way. Results. LAEX and NStED not only provide access to CoRoT Public Data but furthermore serve a variety of observed and calculated astrophysical data. In particular, NStED provides scientifically validated information on stellar and planetary data related to the search for and characterization of extrasolar planets, and LAEX makes any information from Virtual Observatory services available to the astronomical community. C1 [Solano, E.; Velasco, A.; Gutierrez, R.; Lopez, M.] LAEX, CSIC, INTA, Ctr Astrobiol, Madrid 28691, Spain. [von Braun, K.; Ciardi, D. R.; McElroy, D. L.; Abajian, M.; Berriman, G. B.; Chan, B.; Good, J.; Kane, S. R.; Laity, A. C.; Lau, C.; Plavchan, P.; Ramirez, S.; Wyatt, P. L.; Zhang, A.] NASA, Exoplanet Sci Inst, Washington, DC USA. [von Braun, K.; Ciardi, D. R.; McElroy, D. L.; Abajian, M.; Ali, B.; Berriman, G. B.; Good, J.; Kane, S. R.; Laity, A. C.; Plavchan, P.; Ramirez, S.; Schmitz, M.; Stauffer, J. R.; Wyatt, P. L.; Zhang, A.] CALTECH, Pasadena, CA 91125 USA. [Garcia, M.] Univ Pablo Olavide, Area Lenguajes & Sistemas Informat, Seville 41013, Spain. [Sarro, L. M.] Univ Nacl Educ Distancia, Dpt Inteligencia Artificial, Madrid 28040, Spain. [Bryden, G.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Chan, B.; Lau, C.] Raytheon Informat Syst, Pasadena, CA USA. Australian Natl Univ, Mt Stromlo Observ, Canberra, ACT, Australia. RP Solano, E (reprint author), LAEX, CSIC, INTA, Ctr Astrobiol, POB 78, Madrid 28691, Spain. EM esm@laeff.inta.es RI Kane, Stephen/B-4798-2013; Sarro, Luis/L-8082-2014; Solano, Enrique/C-2895-2017; OI Ciardi, David/0000-0002-5741-3047 NR 17 TC 0 Z9 0 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD OCT PY 2009 VL 506 IS 1 BP 455 EP 463 DI 10.1051/0004-6361/200912386 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 509XN UT WOS:000271052700049 ER PT J AU Beckmann, V Soldi, S Ricci, C Alfonso-Garzon, J Courvoisier, TJL Domingo, A Gehrels, N Lubinski, P Mas-Hesse, JM Zdziarski, AA AF Beckmann, V. Soldi, S. Ricci, C. Alfonso-Garzon, J. Courvoisier, T. J. -L. Domingo, A. Gehrels, N. Lubinski, P. Mas-Hesse, J. M. Zdziarski, A. A. TI The second INTEGRAL AGN catalogue SO ASTRONOMY & ASTROPHYSICS LA English DT Review DE galaxies: active; galaxies: Seyfert; X-rays: galaxies; surveys; catalogs ID ACTIVE GALACTIC NUCLEI; BLACK-HOLE MASS; ALL-SKY SURVEY; SEYFERT 2 GALAXIES; X-RAY VARIABILITY; XMM-NEWTON; COMPTON REFLECTION; HOST GALAXIES; INSTRUMENT DESCRIPTION; OPTICAL SPECTROSCOPY AB Aims. The INTEGRAL mission provides a large data set for studying the hard X-ray properties of AGN and allows testing of the unified scheme for AGN. Methods. We present analysis of INTEGRAL IBIS/ISGRI, JEM-X, and OMC data for 199 AGN supposedly detected by INTEGRAL above 20 keV. Results. The data analysed here allow significant spectral extraction on 148 objects and an optical variability study of 57 AGN. The slopes of the hard X-ray spectra of Seyfert 1 and Seyfert 2 galaxies are found to be consistent within the uncertainties, whereas higher cut-off energies and lower luminosities we measured for the more absorbed/type 2 AGN. The intermediate Seyfert 1.5 objects exhibit hard X-ray spectra consistent with those of Seyfert 1. When applying a Compton reflection model, the underlying continua appear the same in Seyfert 1 and 2 with Gamma similar or equal to 2, and the reflection strength is about R similar or equal to 1, when assuming different inclination angles. A significant correlation is found between the hard X-ray and optical luminosity and the mass of the central black hole in the sense that the more luminous objects appear to be more massive. There is also a general trend toward the absorbed sources and type 2 AGN having lower Eddington ratios. The black hole mass appears to form a fundamental plane together with the optical and X-ray luminosity of the form L-V proportional to (LXMBH0.2)-M-0.6, similar to what is found between L-R, L-X, and M-BH. Conclusions. The transition from the type 1 to type 2 AGN appears to be smooth. The type 2 AGN are less luminous and have less accreting super massive black holes. The unified model for Seyfert galaxies seems to hold, showing in hard X-rays that the central engine is the same in Seyfert 1 and 2, but seen under different inclination angles and absorption. The fundamental plane links the accretion mechanism with the bulge of the host galaxy and with the mass of the central engine in the same way in all types of Seyfert galaxies. C1 [Beckmann, V.; Ricci, C.; Courvoisier, T. J. -L.; Lubinski, P.] ISDC Data Ctr Astrophys, CH-1290 Versoix, Switzerland. [Beckmann, V.; Ricci, C.; Courvoisier, T. J. -L.] Univ Geneva, Astron Observ, CH-1290 Sauverny, Switzerland. [Beckmann, V.] Univ Paris Diderot, APC Lab, F-75205 Paris 13, France. [Soldi, S.] Univ Paris Diderot, Lab AIM CNRS CEA DSM, CEA Saclay, DSM IRFU SAp,UMR 7158, F-91191 Gif Sur Yvette, France. [Alfonso-Garzon, J.; Domingo, A.; Mas-Hesse, J. M.] INTA, CSIC, Ctr Astrobiol LAEX, Madrid 28691, Spain. [Gehrels, N.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Lubinski, P.; Zdziarski, A. A.] Ctr Astron M Kopernika, PL-00716 Warsaw, Poland. RP Beckmann, V (reprint author), ISDC Data Ctr Astrophys, Chemin Ecogia 16, CH-1290 Versoix, Switzerland. EM beckmann@apc.univ-paris7.fr RI Gehrels, Neil/D-2971-2012; Mas-Hesse, J. Miguel /K-6805-2014; Domingo, Albert/L-9071-2014; Alfonso-Garzon, Julia/H-6446-2015 OI Mas-Hesse, J. Miguel /0000-0002-8823-9723; Domingo, Albert/0000-0001-9764-6411; Alfonso-Garzon, Julia/0000-0003-0852-3474 NR 124 TC 81 Z9 81 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD OCT PY 2009 VL 505 IS 1 BP 417 EP 439 DI 10.1051/0004-6361/200912111 PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 502DU UT WOS:000270436000038 ER PT J AU Huber, D Matthews, JM Croll, B Obbrugger, M Gruberbauer, M Guenther, DB Weiss, WW Rowe, JF Kallinger, T Kuschnig, R Scholtz, AL Moffat, AFJ Rucinski, SM Sasselov, D Walker, GAH AF Huber, D. Matthews, J. M. Croll, B. Obbrugger, M. Gruberbauer, M. Guenther, D. B. Weiss, W. W. Rowe, J. F. Kallinger, T. Kuschnig, R. Scholtz, A. L. Moffat, A. F. J. Rucinski, S. M. Sasselov, D. Walker, G. A. H. TI A search for p-modes and other variability in the binary system 85 Pegasi using MOST photometry SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE techniques: photometric; stars: individual: 85 Peg; stars: oscillations; stars: rotation; starspots; binaries: general ID SOLAR-LIKE OSCILLATIONS; MAIN-SEQUENCE STARS; LINE-DATA-BASE; DIFFERENTIAL ROTATION; STELLAR OSCILLATIONS; ABUNDANCE ANALYSIS; EPSILON-OPHIUCHI; ASTEROSEISMOLOGY; GRANULATION; SPACE AB Context. Asteroseismology has great potential for the study of metal-poor stars due to its sensitivity to determine stellar ages. Solid detections of oscillation frequencies in stars with well constrained fundamental parameters, combined with a known rotation period, should significantly advance our understanding of stellar structure and evolution in context with metallicity effects. Aims. Our goal was to detect p-mode oscillations in the metal-poor sub-dwarf 85 Peg A and to search for variability on longer timescales. Methods. We have obtained continuous high-precision optical photometry of the binary system 85 Pegasi with the MOST (Microvariability & Oscillations of STars) space telescope in two seasons (2005 & 2007). The light curves were analyzed using traditional Fourier techniques. Furthermore, we redetermined v sin i for 85 Peg A using high resolution spectra obtained through the ESO archive, and used photometric spot modeling to interpret long periodic variations. Results. Our frequency analysis yields no convincing evidence for p-modes significantly above a noise level of 4 ppm. Using simulated p-mode patterns we provide upper rms amplitude limits for 85 Peg A. After removal of instrumental trends the light curve shows evidence for variability with a period of about 11 d and this periodicity is also seen in the follow up run in 2007; however, as different methods to remove instrumental trends in the 2005 run yield vastly different results, the exact shape and periodicity of the 2005 variability remain uncertain. Our re-determined v sin i value for 85 Peg A is comparable to previous studies and we provide realistic uncertainties for this parameter. Using these values in combination with simple photometric spot models we are able to reconstruct the observed variations. Conclusions. The null-detection of p-modes in 85 Peg A is consistent with theoretical values for pulsation amplitudes in this star. The detected long-periodic variation in the 85 Peg system must await confirmation by further observations with similar or better precision and long-term stability. If the 11 d periodicity is real, rotational modulation of surface features on one of the components is the most likely explanation. C1 [Huber, D.; Obbrugger, M.; Gruberbauer, M.; Weiss, W. W.; Kallinger, T.; Kuschnig, R.] Univ Vienna, Inst Astron, A-1180 Vienna, Austria. [Huber, D.] Univ Sydney, Sch Phys, Sydney Inst Astron, Sydney, NSW 2006, Australia. [Matthews, J. M.; Kallinger, T.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. [Croll, B.; Rucinski, S. M.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada. [Gruberbauer, M.; Guenther, D. B.] St Marys Univ, Dept Phys & Astron, Halifax, NS B3H 3C3, Canada. [Rowe, J. F.] NASA, Moffett Field, CA 94035 USA. [Scholtz, A. L.] Vienna Univ Technol, Inst Commun & Radiofrequency Engn, A-1040 Vienna, Austria. [Moffat, A. F. J.] Univ Montreal, Dept Phys, Montreal, PQ H3C 3J7, Canada. [Sasselov, D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Huber, D (reprint author), Univ Vienna, Inst Astron, Turkenschanzstr 17, A-1180 Vienna, Austria. EM huber@astro.univie.ac.at FU Natural Sciences & Engineering Research Council (NSERC) Canada FX We are grateful for discussions with Pierre Demarque. We are also thankful to Gerald Handler for critical discussions concerning the p-mode detection limit. M. G., M.O., T. K., W. W. W. and R. K. are supported by the Austrian Fonds zur Forderung der wissenschaftlichen Forschung, project number P17580-N02. The Austrian participation in the MOST project is funded by the Austrian Research Promotion Agency (FFG). B. C., D. B. G., J.M.M., A.F.J.M., and S. R. acknowledge funding from the Natural Sciences & Engineering Research Council (NSERC) Canada. NR 60 TC 1 Z9 1 U1 0 U2 2 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD OCT PY 2009 VL 505 IS 2 BP 715 EP 725 DI 10.1051/0004-6361/200912139 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 504ST UT WOS:000270638600027 ER PT J AU Smits, R Lorimer, DR Kramer, M Manchester, R Stappers, B Jin, CJ Nan, RD Li, D AF Smits, R. Lorimer, D. R. Kramer, M. Manchester, R. Stappers, B. Jin, C. J. Nan, R. D. Li, D. TI Pulsar science with the Five hundred metre Aperture Spherical Telescope SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: neutron; stars: pulsars: general; telescopes ID DATA-ANALYSIS SYSTEMS; BLACK-HOLE BINARIES; GRAVITATIONAL-WAVES; MILLISECOND PULSARS; POPULATION ANALYSIS; SUPERNOVA-REMNANTS; ANDROMEDA GALAXY; ECLIPSING BINARY; M33; DISCOVERY AB With a collecting area of 70 000 m(2), the Five hundred metre Aperture Spherical Telescope (FAST) will allow for great advances in pulsar astronomy. We have performed simulations to estimate the number of previously unknown pulsars FAST will find with its 19-beam or possibly 100-beam receivers for different survey strategies. With the 19-beam receiver, a total of 5200 previously unknown pulsars could be discovered in the Galactic plane, including about 460 millisecond pulsars (MSPs). Such a survey would take just over 200 days with eight hours survey time per day. We also estimate that, with about 80 six-hour days, a survey of M 31 and M 33 could yield 50-100 extra-Galactic pulsars. A 19-beam receiver would produce just under 500 MB of data per second and requires about 9 tera-ops to perform the major part of a real time analysis. We also simulate the logistics of high-precision timing of MSPs with FAST. Timing of the 50 brightest MSPs to a signal-to-noise of 500 would take about 24 h per epoch. C1 [Smits, R.; Kramer, M.; Stappers, B.] Univ Manchester, Jodrell Bank, Ctr Astrophys, Sch Phys & Astron, Manchester M13 9PL, Lancs, England. [Lorimer, D. R.] W Virginia Univ, Dept Phys, Morgantown, WV 26506 USA. [Lorimer, D. R.] Green Bank Observ, Natl Radio Astron Observ, Green Bank, WV 24944 USA. [Kramer, M.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Manchester, R.] CSIRO, Australia Telescope Natl Facil, Epping, NSW 1710, Australia. [Jin, C. J.; Nan, R. D.] Chinese Acad Sci, Natl Astron Observ, Beijing 100012, Peoples R China. [Li, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Smits, R (reprint author), Univ Manchester, Jodrell Bank, Ctr Astrophys, Sch Phys & Astron, Alan Turing Bldg,Oxford Rd, Manchester M13 9PL, Lancs, England. EM Roy.Smits@manchester.ac.uk FU European Community [011938]; West Virginia EPSCoR FX We would like to thank the referee, Scott Ransom, for his useful suggestions and comments. The authors have made use of the ATNF Pulsar Catalogue which can be found at http://www.atnf.csiro.au/research/pulsar/psrcat. This effort/activity is supported by the European Community Framework Programme 6, Square Kilometre Array Design Studies (SKADS), contract No. 011938. D.R.L. is supported by a Research Challenge Grant from West Virginia EPSCoR. NR 35 TC 33 Z9 37 U1 0 U2 1 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD OCT PY 2009 VL 505 IS 2 BP 919 EP 926 DI 10.1051/0004-6361/200911939 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 504ST UT WOS:000270638600045 ER PT J AU Marcaide, JM Marti-Vidal, I Alberdi, A Perez-Torres, MA Ros, E Diamond, PJ Guirado, JC Lara, L Shapiro, II Stockdale, CJ Weiler, KW Mantovani, F Preston, RA Schilizzi, RT Sramek, RA Trigilio, C Van Dyk, SD Whitney, AR AF Marcaide, J. M. Marti-Vidal, I. Alberdi, A. Perez-Torres, M. A. Ros, E. Diamond, P. J. Guirado, J. C. Lara, L. Shapiro, I. I. Stockdale, C. J. Weiler, K. W. Mantovani, F. Preston, R. A. Schilizzi, R. T. Sramek, R. A. Trigilio, C. Van Dyk, S. D. Whitney, A. R. TI A decade of SN 1993J: discovery of radio wavelength effects in the expansion rate SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE galaxies: clusters: individual: M 81; radio continuum: stars; supernovae: general; supernovae: individual: SN 1993J; techniques: interferometric ID HUBBLE-SPACE-TELESCOPE; IIB SUPERNOVA 1993J; CIRCUMSTELLAR INTERACTION; OPTICAL-SPECTRA; SN-1993J VLBI; NEBULAR PHASE; LIGHT CURVES; MASS-LOSS; X-RAYS; M81 AB We studied the growth of the shell-like radio structure of supernova SN1993J in M 81 from September 1993 to October 2003 with very-long-baseline interferometry (VLBI) observations at the wavelengths of 3.6, 6, and 18 cm. We developed a method to accurately determine the outer radius (R) of any circularly symmetric compact radio structure such as SN1993J. The source structure of SN 1993J remains circularly symmetric (with deviations from circularity under 2%) over almost 4000 days. We characterize the decelerated expansion of SN 1993J until approximately day 1500 after explosion with an expansion parameter m = 0.845 +/- 0.005 (R proportional to t(m)). However, from that day onwards the expansion differs when observed at 6 and 18 cm. Indeed, at 18 cm, the expansion can be well characterized by the same m as before day 1500, while at 6 cm the expansion appears more decelerated, and is characterized by another expansion parameter, m(6) = 0.788 +/- 0.015. Therefore, since about day 1500 onwards, the radio source size has been progressively smaller at 6 cm than at 18 cm. These findings differ significantly from those of other authors in the details of the expansion. In our interpretation, the supernova expands with a single expansion parameter, m = 0.845 +/- 0.005, and the 6 cm results beyond day 1500 are caused by physical effects, perhaps also coupled to instrumental limitations. Two physical effects may be involved: (a) a changing opacity of the ejecta to the 6 cm radiation; and (b) a radial decrease of the magnetic field in the emitting region. We also found that at 6 cm about 80% of the radio emission from the backside of the shell behind the ejecta is absorbed (our average estimate, since we cannot determine any possible evolution of the opacity), and the width of the radio shell is (31 +/- 2)% of the outer radius. The shell width at 18 cm depends on the degree of assumed absorption. For 80% absorption, the width is (33.5 +/- 1.7)%, and for 100% absorption, it is (37.8 +/- 1.3)%. A comparison of our VLBI results with optical spectral line velocities shows that the deceleration is more pronounced in the radio than in the optical. This difference might be due to a progressive penetration of ejecta instabilities into the shocked circumstellar medium, as also suggested by other authors. C1 [Marcaide, J. M.; Marti-Vidal, I.; Perez-Torres, M. A.; Ros, E.; Guirado, J. C.] Univ Valencia, Dept Astron, Valencia, Spain. [Marti-Vidal, I.; Ros, E.] Max Planck Inst Radioastron, D-5300 Bonn, Germany. [Alberdi, A.; Perez-Torres, M. A.] CSIC, Inst Astrofis Andalucia, Granada, Spain. [Diamond, P. J.] Univ Manchester, Jodrell Bank Observ, Manchester, Lancs, England. [Lara, L.] Univ Granada, Granada, Spain. [Shapiro, I. I.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Stockdale, C. J.] Marquette Univ, Milwaukee, WI 53233 USA. [Weiler, K. W.] USN, Res Lab, Washington, DC 20375 USA. [Mantovani, F.] INAF, Ist Radioastron, Bologna, Italy. [Preston, R. A.] NASA, Jet Prop Lab, Pasadena, CA USA. [Schilizzi, R. T.] Int SKA Project Off, Dwingeloo, Netherlands. [Sramek, R. A.] Natl Radio Astron Observ, Socorro, NM 87801 USA. [Trigilio, C.] INAF, Ist Radioastron, Noto, Italy. [Van Dyk, S. D.] Spitzer Sci Ctr, Pasadena, CA USA. [Whitney, A. R.] MIT, Haystack Observ, Westford, MA 01886 USA. RP Marcaide, JM (reprint author), Univ Valencia, Dept Astron, Valencia, Spain. EM J.M.Marcaide@uv.es RI Marti-Vidal, Ivan/A-8799-2017; OI Marti-Vidal, Ivan/0000-0003-3708-9611; Ros, Eduardo/0000-0001-9503-4892; Van Dyk, Schuyler/0000-0001-9038-9950 NR 79 TC 22 Z9 22 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 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD OCT PY 2009 VL 505 IS 3 BP 927 EP 945 DI 10.1051/0004-6361/200912133 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 508DF UT WOS:000270907100001 ER PT J AU Sauter, J Wolf, S Launhardt, R Padgett, DL Stapelfeldt, KR Pinte, C Duchene, G Menard, F McCabe, CE Pontoppidan, K Dunham, M Bourke, TL Chen, JH AF Sauter, J. Wolf, S. Launhardt, R. Padgett, D. L. Stapelfeldt, K. R. Pinte, C. Duchene, G. Menard, F. McCabe, C. -E. Pontoppidan, K. Dunham, M. Bourke, T. L. Chen, J. -H. TI The circumstellar disc in the Bok globule CB 26 Multi-wavelength observations and modelling of the dust disc and envelope SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE circumstellar matter; planetary systems: protoplanetary disks; radiative transfer; stars: formation; stars: individual: CB 26 ID MULTIBAND IMAGING PHOTOMETER; TAURI CIRCUMBINARY RING; MU-M; RADIATIVE-TRANSFER; ABSOLUTE CALIBRATION; GG-TAURI; SIZE DISTRIBUTION; BUTTERFLY STAR; SPITZER; EXTINCTION AB Context. Circumstellar discs are expected to be the nursery of planets. Grain growth within such discs is the first step in the planet formation process. The Bok globule CB 26 harbours such a young disc. Aims. We present a detailed model of the edge-on circumstellar disc and its envelope in the Bok globule CB 26. Methods. The model is based on HST near-infrared maps in the I, J, H, and K bands, OVRO and SMA radio maps at 1.1 mm, 1.3 mm and 2.7 mm, and the spectral energy distribution (SED) from 0.9 mu m to 3 mm. New photometric and spectroscopic data from the Spitzer Space Telescope and the Caltech Submilimeter Observatory are also part of our analysis. Using the self-consistent radiative transfer code MC3D, the model we construct is able to discriminate between parameter sets and dust properties of both envelope and disc. Results. We find that the data are fit by a disc that has an inner hole with a radius of 45 +/- 5 AU. Based on a dust model including silicate and graphite, the maximum grain size needed to reproduce the spectral millimetre index is 2.5 mu m. Features seen in the near-infrared images, dominated by scattered light, can be described as a result of a rotating envelope. Conclusions. Successful employment of ISM dust in both the disc and envelope hint that grain growth may not yet play a significant role for the appearance of this system. A large inner hole implies that CB 26 is a circumbinary disc. C1 [Sauter, J.; Wolf, S.] Univ Kiel, Inst Theoret Phys & Astrophys, D-24098 Kiel, Germany. [Sauter, J.; Launhardt, R.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Pontoppidan, K.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Stapelfeldt, K. R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Pinte, C.] Univ Exeter, Sch Phys, Exeter EX4 4QL, Devon, England. [Pinte, C.; Duchene, G.; Menard, F.] UJF, CNRS, Lab Astrophys Grenoble, CNRS,UMR 5571, F-38041 Grenoble 9, France. [Duchene, G.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Dunham, M.; Chen, J. -H.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Bourke, T. L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Sauter, J (reprint author), Univ Kiel, Inst Theoret Phys & Astrophys, Leibnizstr 15, D-24098 Kiel, Germany. EM jsauter@mpia.de RI Stapelfeldt, Karl/D-2721-2012 FU DFG [759]; CNRS/INSU, France; Agence Nationale pour la Recherche of France [ANR-07-BLAN-0221]; NASA [10603, 30765]; European Commission [PIEF-GA2008-220891]; Smithsonian Institution; Academia Sinica FX The authors thank all members of the GEODE-team for their help in this project. J. Sauter thanks Owen Matthews, Jens Rodmann, and Arjan Bik for enlightening discussions. This work is supported by the DFG through the research group 759 "The Formation of Planets: The Critical First Growth Phase". F. Menard thanks financial support from Programme national de Physique Stellaire (PNPS) of CNRS/INSU, France and from Agence Nationale pour la Recherche of France under contract ANR-07-BLAN-0221. This work has been supported by NASA funding from the Space Telescope Science Institute, HST general observer program 10603; and by NASA funding from the Jet Propulsion Laboratory, under Spitzer general observer program 30765. C. Pinte acknowledges the funding from the European Commission's Seventh Framework Program as a Marie Curie Intra-European Fellow (PIEF-GA2008-220891). 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. NR 61 TC 29 Z9 29 U1 0 U2 2 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD OCT PY 2009 VL 505 IS 3 BP 1167 EP 1182 DI 10.1051/0004-6361/200912397 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 508DF UT WOS:000270907100020 ER PT J AU Van Winckel, H Evans, TL Briquet, M De Cat, P Degroote, P De Meester, W De Ridder, J Deroo, P Desmet, M Drummond, R Eyer, L Groenewegen, MAT Kolenberg, K Kilkenny, D Ladjal, D Lefever, K Maas, T Marang, F Martinez, P Ostensen, RH Raskin, G Reyniers, M Royer, P Saesen, S Uytterhoeven, K Vanautgaerden, J Vandenbussche, B van Wyk, F Vuckovic, M Waelkens, C Zima, W AF Van Winckel, H. Evans, T. Lloyd Briquet, M. De Cat, P. Degroote, P. De Meester, W. De Ridder, J. Deroo, P. Desmet, M. Drummond, R. Eyer, L. Groenewegen, M. A. T. Kolenberg, K. Kilkenny, D. Ladjal, D. Lefever, K. Maas, T. Marang, F. Martinez, P. Ostensen, R. H. Raskin, G. Reyniers, M. Royer, P. Saesen, S. Uytterhoeven, K. Vanautgaerden, J. Vandenbussche, B. van Wyk, F. Vuckovic, M. Waelkens, C. Zima, W. TI Post-AGB stars with hot circumstellar dust: binarity of the low-amplitude pulsators SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: AGB and post-AGB; stars: binaries: general; stars: binaries: spectroscopic; stars: chemically peculiar; stars: evolution ID RV-TAURI STARS; LOW-RESOLUTION SPECTROSCOPY; PLANETARY-NEBULAE; RED-RECTANGLE; DISCS; DEPLETION; CEPHEIDS; SYSTEM; IRAS-08544-4431; CLASSIFICATION AB Context. The influence of binarity on the late stages of stellar evolution remains an open issue. Aims. While the first binary post-AGB stars were serendipitously discovered, the distinct characteristics of their spectral energy distribution (SED) allowed us to launch a more systematic search for binaries. We selected post-AGB objects, which exhibit a broad dust excess starting either at H or K, pointing to the presence of a gravitationally bound dusty disc in the system. We initiated an extensive multiwavelength study of those systems and here report on our radial velocity and photometric monitoring results for six stars of early F type, which are pulsators of small amplitude. Methods. To determine the radial velocity of low signal-to-noise ratio time-series data, we constructed dedicated autocorrelation masks based on high signal-to-noise ratio spectra, used in our published chemical studies. The radial velocity variations were analysed in detail to differentiate between pulsational variability and variability caused by orbital motion. When available, the photometric monitoring data were used to complement the time series of radial velocity data and to establish the nature of the pulsation. Finally, orbital minimalisation was performed to constrain the orbital elements. Results. All of the six objects are binaries with orbital periods ranging from 120 to 1800 days. Five systems have non-circular orbits. The mass functions range from 0.004 to 0.57 M(circle dot) and the companions are probably unevolved objects of (very) low initial mass. We argue that these binaries must have evolved through a phase of strong binary interaction when the primary was a cool supergiant. Although the origin of the circumstellar disc is not well understood, the disc is generally believed to have formed during this strong interaction phase. The eccentric orbits of these highly evolved objects remain poorly understood. In one object, the line-of-sight grazes the edge of the puffed-up inner rim of the disc. Conclusions. These results corroborate our earlier statement that evolved objects in binary stars create a Keplerian dusty circumbinary disc. With the measured orbits and mass functions, we conclude that the circumbinary discs seem to have a major impact on the evolution of a significant fraction of binary systems. C1 [Van Winckel, H.; Briquet, M.; De Cat, P.; Degroote, P.; De Meester, W.; De Ridder, J.; Deroo, P.; Desmet, M.; Drummond, R.; Eyer, L.; Groenewegen, M. A. T.; Kolenberg, K.; Ladjal, D.; Lefever, K.; Maas, T.; Ostensen, R. H.; Raskin, G.; Reyniers, M.; Royer, P.; Saesen, S.; Uytterhoeven, K.; Vanautgaerden, J.; Vandenbussche, B.; Vuckovic, M.; Waelkens, C.; Zima, W.] Katholieke Univ Leuven, Inst Sterrenkunde, B-3001 Louvain, Belgium. [Evans, T. Lloyd] Univ St Andrews, Sch Phys & Astron, SUPA, St Andrews KY16 9SS, Fife, Scotland. [De Cat, P.; Groenewegen, M. A. T.] Observ Royal Belgique, B-1180 Brussels, Belgium. [Deroo, P.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Drummond, R.; Lefever, K.] Belgian Inst Space Aeron, B-1180 Brussels, Belgium. [Eyer, L.] Observ Geneva, CH-1290 Sauverny, Switzerland. [Kolenberg, K.] Univ Vienna, Inst Astron, A-1180 Vienna, Austria. [Reyniers, M.] Royal Meteorol Inst Belgium, Dept Observat, B-1180 Brussels, Belgium. [Kilkenny, D.] Univ Western Cape, Dept Phys, ZA-7535 Bellville, Western Cape, South Africa. [Marang, F.; Martinez, P.; van Wyk, F.] S African Astron Observ, ZA-7935 Observatory, South Africa. [Uytterhoeven, K.] Univ Paris Diderot, Lab AIM, CEA, DSM,CNRS, Paris, France. [Uytterhoeven, K.] CEA, IRFU, SAp, Ctr Saclay, F-91191 Gif Sur Yvette, France. RP Van Winckel, H (reprint author), Katholieke Univ Leuven, Inst Sterrenkunde, Celestijnenlaan 200B, B-3001 Louvain, Belgium. EM Hans.VanWinckel@ster.kuleuven.be RI Van Winckel, Hans/I-7863-2013 OI Van Winckel, Hans/0000-0001-5158-9327 FU Fund for Scientific Research of Flanders (FWO) [G.0178.02, G.0703.08, G.0332.06, G.0470.07]; Research Council of K.U. Leuven [GOA/2008/04] FX The authors want to acknowledge the Geneva Observatory and its staff for the generous time allocation on the Swiss Euler telescope. The IvS acknowledges support from the Fund for Scientific Research of Flanders (FWO) under the grants G.0178.02., G.0703.08, G.0332.06 and G.0470.07. This research was made possible thanks to support from the Research Council of K.U. Leuven under grant GOA/2008/04. We would like to express our appreciation to Grzegorz Pojmanski for his efforts to provide and maintain the ASAS data in a form accessible to the astronomical community. NR 68 TC 74 Z9 74 U1 0 U2 1 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD OCT PY 2009 VL 505 IS 3 BP 1221 EP U321 DI 10.1051/0004-6361/200912332 PG 24 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 508DF UT WOS:000270907100024 ER PT J AU Williams, PE Cuntz, M AF Williams, P. E. Cuntz, M. TI A method for the treatment of supergranulation advection by giant cells SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE convection; methods: numerical; Sun: helioseismology; Sun: photosphere; turbulence; waves ID STEADY PHOTOSPHERIC FLOWS; VELOCITY-FIELDS; SOLAR ATMOSPHERE; SUN; ROTATION; GRANULATION; NETWORK; SURFACE; SEARCH AB Aims. We present a new method for the treatment of the advection of solar supergranulation by giant cells, a large-scale analogue to the observed property of granule advection by supergranules. Methods. The proposed method is derived from a description of solar convection via spherical harmonics and spectral coefficients, allowing the investigation of the influence of a giant cell component on a realistic supergranule signal. Results. We show that a supergranule pattern derived from real data, as well as a simplified test signal, can be advected by a giant cell component of various sizes. Conclusions. The identified behaviour is in analogy to observed supergranulation patterns, including those based on MDI Dopplergrams, which show wavelike supergranulation patterns, even after the removal of the geometric projection effect. Our method is an important step towards the construction of future models involving supergranule flow patterns advected by a giant cell flow. Nevertheless, additional efforts are required to obtain a final verification of giant cells as a separate component of the solar photospheric convection spectrum. C1 [Williams, P. E.; Cuntz, M.] Univ Texas Arlington, Dept Phys, Arlington, TX 76019 USA. RP Williams, PE (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM peter.williams@nasa.gov; cuntz@uta.edu FU NASA's Office of Space Science FX This work was supported by NASA's Office of Space Science through a grant from its Solar and Heliospheric Supporting Research and Technology Program. We also acknowledge valuable discussions with D. H. Hathaway and welcome the comments of an anonymous referee. SOHO is a project of international cooperation between ESA and NASA. NR 29 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 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD OCT PY 2009 VL 505 IS 3 BP 1265 EP 1268 DI 10.1051/0004-6361/200811499 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 508DF UT WOS:000270907100029 ER PT J AU Abdo, AA Ackermann, M Ajello, M Ampe, J Anderson, B Atwood, WB Axelsson, M Bagagli, R Baldini, L Ballet, J Barbiellini, G Bartelt, J Bastieri, D Baughman, BM Bechtol, K Bederede, D Bellardi, F Bellazzini, R Belli, F Berenji, B Bisello, D Bissaldi, E Bloom, ED Bogaert, G Bogart, JR Bonamente, E Borgland, AW Bourgeois, P Bouvier, A Bregeon, J Brez, A Brigida, M Bruel, P Burnett, TH Busetto, G Caliandro, GA Cameron, RA Campell, M Caraveo, PA Carius, S Carlson, P Casandjian, JM Cavazzuti, E Ceccanti, M Cecchi, C Charles, E Chekhtman, A Cheung, CC Chiang, J Chipaux, R Cillis, AN Ciprini, S Claus, R Cohen-Tanugi, J Condamoor, S Conrad, J Corbet, R Cutini, S Davis, DS DeKlotz, M Dermer, CD de Angelis, A de Palma, F Digel, SW Dizon, P Dormody, M Silva, EDE Drell, PS Dubois, R Dumora, D Edmonds, Y Fabiani, D Farnier, C Favuzzi, C Ferrara, EC Ferreira, O Fewtrell, Z Flath, DL Fleury, P Focke, WB Fouts, K Frailis, M Freytag, D Fukazawa, Y Funk, S Fusco, P Garganov, F Gasparrini, D Gehrelscao, N Germani, S Giebels, B Giglietto, N Giordano, F Glanzman, T Godfrey, G Goodman, J Grenier, IA Grondin, MH Grove, JE Guillemot, L Guiriec, S Hakimi, M Haller, G Hanabata, Y Hart, PA Hascall, P Hays, E Huffer, M Hughes, RE Johannesson, G Johnson, AS Johnson, RP Johnson, TJ Johnson, WN Kamae, T Katagiri, H Kataoka, J Kavelaars, A Kelly, H Kerr, M Klamra, W Knodlseder, J Kocian, ML Kuehn, F Kuss, M Latronico, L Lavalley, C Leas, B Lee, B Lee, SH Lemoine-Goumard, M Longo, F Loparco, F Lott, B Lovellette, MN Lubrano, P Lung, DK Madejski, GM Makeev, A Marangelli, B Marchetti, M Massai, MM May, D Mazzenga, G Mazziotta, MN McEnery, JE McGlynn, S Meurer, C Michelson, PF Minuti, M Mirizzi, N Mitra, P Mitthumsiri, W Mizuno, T Moiseev, AA Mongelli, M Monte, C Monzani, ME Moretti, E Morselli, A Moskalenko, IV Murgia, S Nelson, D Nilsson, L Nishino, S Nolan, PL Nuss, E Ohno, M Ohsugi, T Omodei, N Orlando, E Ormes, JF Ozaki, M Paccagnella, A Paneque, D Panetta, JH Parent, D Pelassa, V Pepe, M Pesce-Rollins, M Picozza, P Pinchera, M Piron, F Porter, TA Raino, S Rando, R Rapposelli, E Raynor, W Razzano, M Reimer, A Reimer, O Reposeur, T Reyes, LC Ritz, S Robinson, S Rochester, LS Rodriguez, AY Romani, RW Roth, M Ryde, F Sacchetti, A Sadrozinski, HFW Saggini, N Sanchez, D Sander, A Sapozhnikov, L Saxton, OH Parkinson, PMS Sellerholm, A Sgro, C Siskind, EJ Smith, DA Smith, PD Spandre, G Spinelli, P Starck, JL Stephens, TE Strickman, MS Strong, AW Sugizaki, M Suson, DJ Tajima, H Takahashi, H Takahashi, T Tanaka, T Tenze, A Thayer, JB Thayer, JG Thompson, DJ Tibaldo, L Tibolla, O Torres, DF Tosti, G Tramacere, A Turri, M Usher, TL Vilchez, N Virmani, N Vitale, V Wai, LL Waite, AP Wang, P Winer, BL Wood, DL Wood, KS Yasuda, H Ylinen, T Ziegler, M AF Abdo, A. A. Ackermann, M. Ajello, M. Ampe, J. Anderson, B. Atwood, W. B. Axelsson, M. Bagagli, R. Baldini, L. Ballet, J. Barbiellini, G. Bartelt, J. Bastieri, D. Baughman, B. M. Bechtol, K. Bederede, D. Bellardi, F. Bellazzini, R. Belli, F. Berenji, B. Bisello, D. Bissaldi, E. Bloom, E. D. Bogaert, G. Bogart, J. R. Bonamente, E. Borgland, A. W. Bourgeois, P. Bouvier, A. Bregeon, J. Brez, A. Brigida, M. Bruel, P. Burnett, T. H. Busetto, G. Caliandro, G. A. Cameron, R. A. Campell, M. Caraveo, P. A. Carius, S. Carlson, P. Casandjian, J. M. Cavazzuti, E. Ceccanti, M. Cecchi, C. Charles, E. Chekhtman, A. Cheung, C. C. Chiang, J. Chipaux, R. Cillis, A. N. Ciprini, S. Claus, R. Cohen-Tanugi, J. Condamoor, S. Conrad, J. Corbet, R. Cutini, S. Davis, D. S. DeKlotz, M. Dermer, C. D. de Angelis, A. de Palma, F. Digel, S. W. Dizon, P. Dormody, M. do Couto e Silva, E. Drell, P. S. Dubois, R. Dumora, D. Edmonds, Y. Fabiani, D. Farnier, C. Favuzzi, C. Ferrara, E. C. Ferreira, O. Fewtrell, Z. Flath, D. L. Fleury, P. Focke, W. B. Fouts, K. Frailis, M. Freytag, D. Fukazawa, Y. Funk, S. Fusco, P. Garganov, F. Gasparrini, D. Gehrelscao, N. Germani, S. Giebels, B. Giglietto, N. Giordano, F. Glanzman, T. Godfrey, G. Goodman, J. Grenier, I. A. Grondin, M. -H. Grove, J. E. Guillemot, L. Guiriec, S. Hakimi, M. Haller, G. Hanabata, Y. Hart, P. A. Hascall, P. Hays, E. Huffer, M. Hughes, R. E. Johannesson, G. Johnson, A. S. Johnson, R. P. Johnson, T. J. Johnson, W. N. Kamae, T. Katagiri, H. Kataoka, J. Kavelaars, A. Kelly, H. Kerr, M. Klamra, W. Knoedlseder, J. Kocian, M. L. Kuehn, F. Kuss, M. Latronico, L. Lavalley, C. Leas, B. Lee, B. Lee, S. -H. Lemoine-Goumard, M. Longo, F. Loparco, F. Lott, B. Lovellette, M. N. Lubrano, P. Lung, D. K. Madejski, G. M. Makeev, A. Marangelli, B. Marchetti, M. Massai, M. M. May, D. Mazzenga, G. Mazziotta, M. N. McEnery, J. E. McGlynn, S. Meurer, C. Michelson, P. F. Minuti, M. Mirizzi, N. Mitra, P. Mitthumsiri, W. Mizuno, T. Moiseev, A. A. Mongelli, M. Monte, C. Monzani, M. E. Moretti, E. Morselli, A. Moskalenko, I. V. Murgia, S. Nelson, D. Nilsson, L. Nishino, S. Nolan, P. L. Nuss, E. Ohno, M. Ohsugi, T. Omodei, N. Orlando, E. Ormes, J. F. Ozaki, M. Paccagnella, A. Paneque, D. Panetta, J. H. Parent, D. Pelassa, V. Pepe, M. Pesce-Rollins, M. Picozza, P. Pinchera, M. Piron, F. Porter, T. A. Raino, S. Rando, R. Rapposelli, E. Raynor, W. Razzano, M. Reimer, A. Reimer, O. Reposeur, T. Reyes, L. C. Ritz, S. Robinson, S. Rochester, L. S. Rodriguez, A. Y. Romani, R. W. Roth, M. Ryde, F. Sacchetti, A. Sadrozinski, H. F. -W. Saggini, N. Sanchez, D. Sander, A. Sapozhnikov, L. Saxton, O. H. Parkinson, P. M. Saz Sellerholm, A. Sgro, C. Siskind, E. J. Smith, D. A. Smith, P. D. Spandre, G. Spinelli, P. Starck, J. -L. Stephens, T. E. Strickman, M. S. Strong, A. W. Sugizaki, M. Suson, D. J. Tajima, H. Takahashi, H. Takahashi, T. Tanaka, T. Tenze, A. Thayer, J. B. Thayer, J. G. Thompson, D. J. Tibaldo, L. Tibolla, O. Torres, D. F. Tosti, G. Tramacere, A. Turri, M. Usher, T. L. Vilchez, N. Virmani, N. Vitale, V. Wai, L. L. Waite, A. P. Wang, P. Winer, B. L. Wood, D. L. Wood, K. S. Yasuda, H. Ylinen, T. Ziegler, M. TI The on-orbit calibration of the Fermi Large Area Telescope SO ASTROPARTICLE PHYSICS LA English DT Article DE GLAST; Fermi; FGST; LAT; Telescope; Gamma-ray; Calibrations ID RAY-SPACE-TELESCOPE; BEAM TEST; TRACKER; PULSAR; CALORIMETER; DETECTOR; READOUT; DESIGN; MODEL AB The Large Area Telescope (LAT) on-board the Fermi Gamma-ray Space Telescope began its on-orbit operations on June 23, 2008. Calibrations, defined in a generic sense, correspond to synchronization of trigger signals, optimization of delays for latching data, determination of detector thresholds, gains and responses, evaluation of the perimeter of the South Atlantic Anomaly (SAA), measurements of live time, of absolute time, and internal and spacecraft boresight alignments. Here we describe on-orbit calibration results obtained using known astrophysical sources, galactic cosmic rays, and charge injection into the front-end electronics of each detector. Instrument response functions will be described in a separate publication. This paper demonstrates the stability of calibrations and describes minor changes observed since launch. These results have been used to calibrate the LAT datasets to be publicly released in August 2009. (C) 2009 Elsevier B.V. All rights reserved. C1 [Ackermann, M.; Ajello, M.; Bartelt, J.; Bechtol, K.; Berenji, B.; Bloom, E. D.; Bogart, J. R.; Borgland, A. W.; Bouvier, A.; Cameron, R. A.; Campell, M.; Charles, E.; Chiang, J.; Claus, R.; Condamoor, S.; Digel, S. W.; do Couto e Silva, E.; Drell, P. S.; Dubois, R.; Edmonds, Y.; Flath, D. L.; Focke, W. B.; Fouts, K.; Freytag, D.; Funk, S.; Glanzman, T.; Godfrey, G.; Goodman, J.; Hakimi, M.; Haller, G.; Hart, P. A.; Huffer, M.; Johannesson, G.; Johnson, A. S.; Kamae, T.; Kavelaars, A.; Kelly, H.; Kocian, M. L.; Lee, S. -H.; Madejski, G. M.; Michelson, P. F.; Mitra, P.; Mitthumsiri, W.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Nelson, D.; Nolan, P. L.; Paneque, D.; Panetta, J. H.; Rochester, L. S.; Romani, R. W.; Sapozhnikov, L.; Saxton, O. H.; Sugizaki, M.; Tajima, H.; Tanaka, T.; Thayer, J. B.; Thayer, J. G.; Tramacere, A.; Turri, M.; Usher, T. L.; Wai, L. L.; Waite, A. P.; Wang, P.] Stanford Univ, WW Hansen Expt Phys Lab, Kavli Inst Particle Astrophys & Cosmol, Dept Phys, Stanford, CA 94305 USA. [Ackermann, M.; Ajello, M.; Bartelt, J.; Bechtol, K.; Berenji, B.; Bloom, E. D.; Bogart, J. R.; Borgland, A. W.; Bouvier, A.; Cameron, R. A.; Campell, M.; Charles, E.; Chiang, J.; Claus, R.; Condamoor, S.; Digel, S. W.; do Couto e Silva, E.; Drell, P. S.; Dubois, R.; Edmonds, Y.; Flath, D. L.; Focke, W. B.; Fouts, K.; Freytag, D.; Funk, S.; Glanzman, T.; Godfrey, G.; Goodman, J.; Hakimi, M.; Haller, G.; Hart, P. A.; Huffer, M.; Johannesson, G.; Johnson, A. S.; Kamae, T.; Kavelaars, A.; Kelly, H.; Kocian, M. L.; Lee, S. -H.; Madejski, G. M.; Michelson, P. F.; Mitra, P.; Mitthumsiri, W.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Nelson, D.; Nolan, P. L.; Paneque, D.; Panetta, J. H.; Rochester, L. S.; Romani, R. W.; Sapozhnikov, L.; Saxton, O. H.; Sugizaki, M.; Tajima, H.; Tanaka, T.; Thayer, J. B.; Thayer, J. G.; Tramacere, A.; Turri, M.; Usher, T. L.; Wai, L. L.; Waite, A. P.; Wang, P.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA. [Abdo, A. A.; Ampe, J.; Chekhtman, A.; Dermer, C. D.; Fewtrell, Z.; Grove, J. E.; Johnson, W. N.; Leas, B.; Lovellette, M. N.; Makeev, A.; May, D.; Raynor, W.; Strickman, M. S.; Wood, D. L.; Wood, K. S.] USN, Res Lab, Div Space Sci, Washington, DC 20375 USA. [Abdo, A. A.] Natl Acad Sci, Natl Res Council Res Associate, Washington, DC 20001 USA. [Anderson, B.; Atwood, W. B.; Dormody, M.; Johnson, R. P.; Porter, T. A.; Sadrozinski, H. F. -W.; Parkinson, P. M. Saz; Ziegler, M.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA. [Anderson, B.; Atwood, W. B.; Dormody, M.; Johnson, R. P.; Porter, T. A.; Sadrozinski, H. F. -W.; Parkinson, P. M. Saz; Ziegler, M.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Axelsson, M.] Stockholm Univ, Dept Astron, SE-10691 Stockholm, Sweden. [Axelsson, M.; Carlson, P.; Conrad, J.; Klamra, W.; McGlynn, S.; Meurer, C.; Ryde, F.; Sellerholm, A.; Ylinen, T.] AlbaNova, Oskar Klein Ctr Cosmo Particle Phys, SE-10691 Stockholm, Sweden. [Bagagli, R.; Baldini, L.; Bellardi, F.; Bellazzini, R.; Bregeon, J.; Brez, A.; Ceccanti, M.; Fabiani, D.; Kuss, M.; Latronico, L.; Massai, M. M.; Minuti, M.; Omodei, N.; Pesce-Rollins, M.; Pinchera, M.; Rapposelli, E.; Razzano, M.; Saggini, N.; Sgro, C.; Spandre, G.; Tenze, A.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy. [Ballet, J.; Casandjian, J. M.; Grenier, I. 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[Belli, F.; Marchetti, M.; Mazzenga, G.; Picozza, P.; Vitale, V.] Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy. [Bissaldi, E.; Orlando, E.; Strong, A. W.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Bogaert, G.; Bruel, P.; Ferreira, O.; Fleury, P.; Giebels, B.; Sanchez, D.] Ecole Polytech, CNRS, IN2P3, Lab Leprince Ringuet, F-91128 Palaiseau, France. [Bonamente, E.; Cecchi, C.; Ciprini, S.; Germani, S.; Lubrano, P.; Pepe, M.; Tosti, G.] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy. [Bonamente, E.; Cecchi, C.; Ciprini, S.; Germani, S.; Lubrano, P.; Pepe, M.; Tosti, G.] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy. [Brigida, M.; Caliandro, G. A.; de Palma, F.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Giordano, F.; Loparco, F.; Marangelli, B.; Mirizzi, N.; Monte, C.; Raino, S.; Spinelli, P.] Univ Bari, Dipartimento Fis M Merlin, I-70126 Bari, Italy. [Brigida, M.; Caliandro, G. A.; de Palma, F.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Giordano, F.; Loparco, F.; Marangelli, B.; Mirizzi, N.; Monte, C.; Raino, S.; Spinelli, P.] Politecn Bari, I-70126 Bari, Italy. [Brigida, M.; Caliandro, G. A.; de Palma, F.; Favuzzi, C.; Fusco, P.; Garganov, F.; Giglietto, N.; Giordano, F.; Loparco, F.; Marangelli, B.; Mazziotta, M. N.; Mirizzi, N.; Mongelli, M.; Monte, C.; Raino, S.; Sacchetti, A.; Spinelli, P.] Ist Nazl Fis Nucl, Sez Bari, I-70126 Bari, Italy. [Burnett, T. H.; Kerr, M.; Robinson, S.; Roth, M.] Univ Washington, Dept Phys, Seattle, WA 98195 USA. [Caraveo, P. A.] Ist Astrofis Spaziale & Fis Cosm, INAF, I-20133 Milan, Italy. [Carius, S.; Nilsson, L.] Univ Kalmar, Sch Pure & Appl Nat Sci, SE-39182 Kalmar, Sweden. [Carlson, P.; Conrad, J.; Klamra, W.; McGlynn, S.; Ryde, F.; Ylinen, T.] Royal Inst Technol KTH, Dept Phys, SE-10691 Stockholm, Sweden. [Cavazzuti, E.; Cutini, S.; Gasparrini, D.] ASI, Sci Data Ctr, I-00044 Frascati, Italy. [Chekhtman, A.; Makeev, A.] George Mason Univ, Fairfax, VA 22030 USA. [Cheung, C. C.; Cillis, A. N.; Corbet, R.; Davis, D. S.; Ferrara, E. C.; Gehrelscao, N.; Hays, E.; Johnson, T. J.; McEnery, J. E.; Ritz, S.; Thompson, D. J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Chipaux, R.] CEA Saclay, IRFU, Serv Phys Particules, F-91191 Gif Sur Yvette, France. [Chipaux, R.] CEA Saclay, IRFU SEDI, F-91191 Gif Sur Yvette, France. [Cohen-Tanugi, J.; Farnier, C.; Lavalley, C.; Nuss, E.; Pelassa, V.; Piron, F.] Univ Montpellier 2, CNRS, IN2P3, Lab Phys Theor & Astroparticules, Montpellier, France. [Conrad, J.; Meurer, C.; Sellerholm, A.] Stockholm Univ, Dept Phys, SE-10691 Stockholm, Sweden. [Corbet, R.; Davis, D. S.] Univ Maryland Baltimore Cty, Baltimore, MD 21250 USA. [DeKlotz, M.] Stellar Solut Inc, Palo Alto, CA 94306 USA. [de Angelis, A.; Frailis, M.] Univ Udine, Dipartimento Fis, I-33100 Udine, Italy. [de Angelis, A.; Frailis, M.] Ist Nazl Fis Nucl, Sez Trieste, Grp Coll Udine, I-33100 Udine, Italy. [Dumora, D.; Grondin, M. -H.; Guillemot, L.; Lemoine-Goumard, M.; Lott, B.; Parent, D.; Reposeur, T.; Smith, D. A.] Univ Bordeaux, Ctr Etud Nucl Bordeaux Gradignan, UMR 5797, F-33175 Gradignan, France. [Dizon, P.; Virmani, N.] ATK Space Prod, Beltsville, MD 20705 USA. [Dumora, D.; Grondin, M. -H.; Guillemot, L.; Lemoine-Goumard, M.; Lott, B.; Parent, D.; Reposeur, T.; Smith, D. A.] Ctr Etud Nucl Bordeaux Gradignan, CNRS, IN2P3, UMR 5797, F-33175 Gradignan, France. [Fukazawa, Y.; Hanabata, Y.; Katagiri, H.; Mizuno, T.; Nishino, S.; Ohsugi, T.; Takahashi, H.; Yasuda, H.] Hiroshima Univ, Dept Phys Sci, Hiroshima 7398526, Japan. [Gehrelscao, N.; Johnson, T. J.; Moiseev, A. A.] Univ Maryland, College Pk, MD 20742 USA. [Guiriec, S.] Univ Alabama, Huntsville, AL 35899 USA. [Hascall, P.; Lee, B.; Lung, D. K.] Orbital Network Engn, Cupertino, CA 95014 USA. [Kataoka, J.] Tokyo Inst Technol, Dept Phys, Meguro, Tokyo 1528551, Japan. [Kataoka, J.] Waseda Univ, Shinjuku Ku, Tokyo 1698050, Japan. [Knoedlseder, J.; Vilchez, N.] UPS, CNRS, Ctr Etud Spatiale Rayonnements, F-31028 Toulouse 4, France. [Moiseev, A. A.] NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA. [Nilsson, L.] Matfakta Kalmar AB, S-30477 Kalmar, Sweden. [Ohno, M.; Ozaki, M.; Takahashi, T.] JAXA, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2298510, Japan. [Ormes, J. F.] Univ Denver, Dept Phys & Astron, Denver, CO 80208 USA. [Paccagnella, A.] Univ Padua, Dipartimento Ingn Informaz, I-35131 Padua, Italy. [Reimer, A.; Reimer, O.] Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria. [Reimer, A.; Reimer, O.] Univ Innsbruck, Inst Theoret Phys, A-6020 Innsbruck, Austria. [Reyes, L. C.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Robinson, S.] Pacific NW Natl Lab, Richland, WA 99352 USA. [Rodriguez, A. Y.; Torres, D. F.] CSIC, IEEC, Inst Ciencies Espai, Barcelona 08193, Spain. [Siskind, E. J.] NYCB Real Time Comp Inc, Lattingtown, NY 11560 USA. [Stephens, T. E.] NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA. [Stephens, T. E.] USRA, Columbia, MD 21044 USA. [Suson, D. J.] Purdue Univ Calumet, Dept Chem & Phys, Hammond, IN 46323 USA. [Tibolla, O.] Max Planck Inst Kernphys, D-69029 Heidelberg, Germany. [Torres, D. F.] Inst Catalana Recerca & Estudis Avancats, Barcelona, Spain. [Tramacere, A.] CIFS, I-10133 Turin, Italy. [Wai, L. L.] Yahoo Inc, Sunnyvale, CA 94089 USA. RP Silva, EDE (reprint author), Stanford Univ, WW Hansen Expt Phys Lab, Kavli Inst Particle Astrophys & Cosmol, Dept Phys, Stanford, CA 94305 USA. EM eduardo@slac.stanford.edu RI Hays, Elizabeth/D-3257-2012; Johnson, Neil/G-3309-2014; Reimer, Olaf/A-3117-2013; Funk, Stefan/B-7629-2015; Loparco, Francesco/O-8847-2015; Johannesson, Gudlaugur/O-8741-2015; Moskalenko, Igor/A-1301-2007; Mazziotta, Mario /O-8867-2015; Sgro, Carmelo/K-3395-2016; Bissaldi, Elisabetta/K-7911-2016; Torres, Diego/O-9422-2016; Starck, Jean-Luc/D-9467-2011; Thompson, David/D-2939-2012; McEnery, Julie/D-6612-2012; Chipaux, Remi/G-1145-2010; Baldini, Luca/E-5396-2012; lubrano, pasquale/F-7269-2012; Morselli, Aldo/G-6769-2011; Nolan, Patrick/A-5582-2009; Kuss, Michael/H-8959-2012; giglietto, nicola/I-8951-2012; Tosti, Gino/E-9976-2013; Saz Parkinson, Pablo Miguel/I-7980-2013; Ozaki, Masanobu/K-1165-2013; Rando, Riccardo/M-7179-2013 OI Giordano, Francesco/0000-0002-8651-2394; Picozza, Piergiorgio/0000-0002-7986-3321; Stephens, Thomas/0000-0003-3065-6871; De Angelis, Alessandro/0000-0002-3288-2517; Frailis, Marco/0000-0002-7400-2135; Caraveo, Patrizia/0000-0003-2478-8018; Bastieri, Denis/0000-0002-6954-8862; Omodei, Nicola/0000-0002-5448-7577; Pesce-Rollins, Melissa/0000-0003-1790-8018; Gargano, Fabio/0000-0002-5055-6395; Reimer, Olaf/0000-0001-6953-1385; Funk, Stefan/0000-0002-2012-0080; Loparco, Francesco/0000-0002-1173-5673; Johannesson, Gudlaugur/0000-0003-1458-7036; Moskalenko, Igor/0000-0001-6141-458X; Mazziotta, Mario /0000-0001-9325-4672; Bissaldi, Elisabetta/0000-0001-9935-8106; Torres, Diego/0000-0002-1522-9065; Rando, Riccardo/0000-0001-6992-818X; Sgro', Carmelo/0000-0001-5676-6214; Moretti, Elena/0000-0001-5477-9097; Cutini, Sara/0000-0002-1271-2924; Gasparrini, Dario/0000-0002-5064-9495; Tramacere, Andrea/0000-0002-8186-3793; Baldini, Luca/0000-0002-9785-7726; Starck, Jean-Luc/0000-0003-2177-7794; Thompson, David/0000-0001-5217-9135; lubrano, pasquale/0000-0003-0221-4806; Morselli, Aldo/0000-0002-7704-9553; giglietto, nicola/0000-0002-9021-2888; FU Istituto Nazionale di Astrofisica in Italy FX Additional support for science analysis during the operations phase is gratefully acknowledged from the Istituto Nazionale di Astrofisica in Italy. NR 30 TC 88 Z9 88 U1 0 U2 5 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 OCT-NOV PY 2009 VL 32 IS 3-4 BP 193 EP 219 DI 10.1016/j.astropartphys.2009.08.002 PG 27 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 526GT UT WOS:000272276400005 ER PT J AU Stark, CC Kuchner, MJ Traub, WA Monnier, JD Serabyn, E Colavita, M Koresko, C Mennesson, B Keller, LD AF Stark, Christopher C. Kuchner, Marc J. Traub, Wesley A. Monnier, John D. Serabyn, Eugene Colavita, Mark Koresko, Chris Mennesson, Bertrand Keller, Luke D. TI 51 OPHIUCHUS: A POSSIBLE BETA PICTORIS ANALOG MEASURED WITH THE KECK INTERFEROMETER NULLER SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; infrared: stars; interplanetary medium; planetary systems ID HERBIG-AE/BE STARS; CIRCUMSTELLAR DISKS; DEBRIS DISK; DUST; SPECTROSCOPY; EMISSION; SYSTEMS; YOUNG; AU; CO AB We present observations of the 51 Ophiuchi circumstellar disk made with the Keck interferometer operating in nulling mode at N band. We model these data simultaneously with VLTI-MIDI visibility data and a Spitzer IRS spectrum using a variety of optically thin dust cloud models and an edge-on optically thick disk model. We find that single-component optically thin disk models and optically thick disk models are inadequate to reproduce the observations, but an optically thin two-component disk model can reproduce all of the major spectral and interferometric features. Our preferred disk model consists of an inner disk of blackbody grains extending to similar to 4 AU and an outer disk of small silicate grains extending out to similar to 1200 AU. Our model is consistent with an inner "birth" disk of continually colliding parent bodies producing an extended envelope of ejected small grains. This picture resembles the disks around Vega, AU Microscopii, and beta Pictoris, supporting the idea that 51 Ophiuchius may be a beta Pictoris analog. C1 [Stark, Christopher C.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA. [Kuchner, Marc J.] NASA, Goddard Space Flight Ctr, Exoplanets & Stellar Astrophys Lab, Greenbelt, MD 20771 USA. [Traub, Wesley A.; Serabyn, Eugene; Colavita, Mark; Mennesson, Bertrand] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Monnier, John D.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Koresko, Chris] Argon ST, Fairfax, VA 22033 USA. [Keller, Luke D.] Ithaca Coll, Dept Phys, Ithaca, NY 14850 USA. RP Stark, CC (reprint author), Univ Maryland, Dept Phys, Box 197,082 Regents Dr, College Pk, MD 20742 USA. EM starkc@umd.edu RI Kuchner, Marc/E-2288-2012 FU National Aeronautics and Space Administration; Goddard Space Flight Center; Harvard-Smithsonian Center for Astrophysics FX We thank the National Aeronautics and Space Administration and Goddard Space Flight Center for support of this research through funding from the Graduate Student Researchers Program, and the Harvard-Smithsonian Center for Astrophysics and NASA's Navigator Program for their financial support via the Keck Interferometer Nuller Shared Risk Science Program. 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. The authors also thank Rachel Akeson and Rafael Millan-Gabet for their help in making these observations possible. NR 35 TC 14 Z9 14 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 1 PY 2009 VL 703 IS 2 BP 1188 EP 1197 DI 10.1088/0004-637X/703/2/1188 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 495XS UT WOS:000269929500002 ER PT J AU Hollenbach, D Gorti, U AF Hollenbach, David Gorti, U. TI DIAGNOSTIC LINE EMISSION FROM EXTREME ULTRAVIOLET AND X-RAY-ILLUMINATED DISKS AND SHOCKS AROUND LOW-MASS STARS SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; infrared: stars; planetary systems: protoplanetary disks; stars: formation; stars: winds, outflows; X-rays: stars ID T-TAURI STARS; NE-II EMISSION; EFFECTIVE COLLISION STRENGTHS; IRRADIATED PROTOPLANETARY DISKS; HIGH-RESOLUTION SPECTROSCOPY; CENTRIFUGALLY DRIVEN WINDS; FINE-STRUCTURE LEVELS; MAIN-SEQUENCE STARS; YOUNG STARS; ATOMIC DATA AB Extreme ultraviolet (EUV; 13.6 eV < h nu less than or similar to 100 eV) and X-rays in the 0.1-2 keV band can heat the surfaces of disks around young, low-mass stars to thousands of degrees and ionize species with ionization potentials greater than 13.6 eV. Shocks generated by protostellar winds can also heat and ionize the same species close to the star/disk system. These processes produce diagnostic lines (e.g., [Ne II] 12.8 mu m and [O I] 6300 angstrom) that we model as functions of key parameters such as EUV luminosity and spectral shape, X-ray luminosity and spectral shape, and wind mass loss rate and shock speed. Comparing our models with observations, we conclude that either internal shocks in the winds or X-rays incident on the disk surfaces often produce the observed [Ne II] line, although there are cases where EUV may dominate. Shocks created by the oblique interaction of winds with disks are unlikely [Ne II] sources because these shocks are too weak to ionize Ne. Even if [Ne II] is mainly produced by X-rays or internal wind shocks, the neon observations typically place upper limits of less than or similar to 10(42) s(-1) on the EUV photon luminosity of these young low-mass stars. The observed [O I] 6300 angstrom line has both a low velocity component (LVC) and a high velocity component. The latter likely arises in internal wind shocks. For the former we find that X-rays likely produce more [O I] luminosity than either the EUV layer, the transition layer between the EUV and X-ray layer, or the shear layer where the protostellar wind shocks and entrains disk material in a radial flow across the surface of the disk. Our soft X-ray models produce [O I] LVCs with luminosities up to 10(-4) L(circle dot), but may not be able to explain the most luminous LVCs. C1 [Hollenbach, David; Gorti, U.] SETI Inst, Mountain View, CA 94043 USA. [Gorti, U.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Hollenbach, D (reprint author), SETI Inst, 515 N Whisman Rd, Mountain View, CA 94043 USA. FU NASA FX We thank R. Alexander, C. Clarke, J. Drake, B. Ercolano, A. Glassgold, M. Gudel, M. Kaufman, R. Meijerink, J. Najita, D. Neufeld, and I. Pascucci for helpful discussions and allowing us access to prepublication drafts of papers. We also thank R. Alexander for his helpful and thorough referee report and E. Feigelson, the editor, for helpful comments on the X-ray flare size, time variability, and spectral shape. We acknowledge financial support from NASA's Origins Program, Astrobiology Program, and Astrophysical Theory Program. NR 100 TC 45 Z9 45 U1 1 U2 8 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 1 PY 2009 VL 703 IS 2 BP 1203 EP 1223 DI 10.1088/0004-637X/703/2/1203 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 495XS UT WOS:000269929500004 ER PT J AU Abdo, AA Ackermann, M Ajello, M Atwood, WB Axelsson, M Baldini, L Ballet, J Barbiellini, G Bastieri, D Baughman, BM Bechtol, K Bellazzini, R Berenji, B Bloom, ED Bonamente, E Borgland, AW Bregeon, J Brez, A Brigida, M Bruel, P Burnett, TH Caliandro, GA Cameron, RA Caraveo, PA Carlson, P Casandjian, JM Cecchi, C Celik, O Chekhtman, A Cheung, CC Ciprini, S Claus, R Cohen-Tanugi, J Conrad, J Cutini, S Dermer, CD de Angelis, A de Palma, F Digel, SW Silva, EDE Drell, PS Dubois, R Dumora, D Farnier, C Favuzzi, C Fegan, SJ Focke, WB Frailis, M Fukazawa, Y Funk, S Fusco, P Gargano, F Gasparrini, D Gehrels, N Germani, S Giebels, B Giglietto, N Giordano, F Glanzman, T Godfrey, G Grenier, IA Grondin, MH Grove, JE Guillemot, L Guiriec, S Hanabata, Y Harding, AK Hayashida, M Hays, E Hughes, RE Johannesson, G Johnson, AS Johnson, RP Johnson, WN Kamae, T Katagiri, H Kawai, N Kerr, M Knodlseder, J Kocian, ML Kuehn, F Kuss, M Lande, J Latronico, L Lemoine-Goumard, M Longo, F Loparco, F Lott, B Lovellette, MN Lubrano, P Makeev, A Mazziotta, MN McEnery, JE Meurer, C Michelson, PF Mitthumsiri, W Mizuno, T Moiseev, AA Monte, C Monzani, ME Morselli, A Moskalenko, IV Murgia, S Nolan, PL Norris, JP Nuss, E Ohsugi, T Okumura, A Omodei, N Orlando, E Ormes, JF Ozaki, M Paneque, D Panetta, JH Parent, D Pepe, M Pesce-Rollins, M Piron, F Pohl, M Porter, TA Raino, S Rando, R Razzano, M Reimer, A Reimer, O Reposeur, T Ritz, S Rochester, LS Rodriguez, AY Ryde, F Sadrozinski, HFW Sanchez, D Sander, A Parkinson, PMS Schalk, TL Sellerholm, A Sgro, C Smith, DA Smith, PD Spandre, G Spinelli, P Starck, JL Stecker, FW Strickman, MS Strong, AW Suson, DJ Tajima, H Takahashi, H Takahashi, T Tanaka, T Thayer, JB Thayer, JG Thompson, DJ Tibaldo, L Torres, DF Tosti, G Tramacere, A Uchiyama, Y Usher, TL Vasileiou, V Vilchez, N Vitale, V Waite, AP Wang, P Winer, BL Wood, KS Ylinen, T Ziegler, M AF Abdo, A. A. Ackermann, M. Ajello, M. Atwood, W. B. Axelsson, M. Baldini, L. Ballet, J. Barbiellini, G. Bastieri, D. Baughman, B. M. Bechtol, K. Bellazzini, R. Berenji, B. Bloom, E. D. Bonamente, E. Borgland, A. W. Bregeon, J. Brez, A. Brigida, M. Bruel, P. Burnett, T. H. Caliandro, G. A. Cameron, R. A. Caraveo, P. A. Carlson, P. Casandjian, J. M. Cecchi, C. Celik, Oe. Chekhtman, A. Cheung, C. C. Ciprini, S. Claus, R. Cohen-Tanugi, J. Conrad, J. Cutini, S. Dermer, C. D. de Angelis, A. de Palma, F. Digel, S. W. do Couto e Silva, E. Drell, P. S. Dubois, R. Dumora, D. Farnier, C. Favuzzi, C. Fegan, S. J. Focke, W. B. Frailis, M. Fukazawa, Y. Funk, S. Fusco, P. Gargano, F. Gasparrini, D. Gehrels, N. Germani, S. Giebels, B. Giglietto, N. Giordano, F. Glanzman, T. Godfrey, G. Grenier, I. A. Grondin, M. -H. Grove, J. E. Guillemot, L. Guiriec, S. Hanabata, Y. Harding, A. K. Hayashida, M. Hays, E. Hughes, R. E. Johannesson, G. Johnson, A. S. Johnson, R. P. Johnson, W. N. Kamae, T. Katagiri, H. Kawai, N. Kerr, M. Knoedlseder, J. Kocian, M. L. Kuehn, F. Kuss, M. Lande, J. Latronico, L. Lemoine-Goumard, M. Longo, F. Loparco, F. Lott, B. Lovellette, M. N. Lubrano, P. Makeev, A. Mazziotta, M. N. McEnery, J. E. Meurer, C. Michelson, P. F. Mitthumsiri, W. Mizuno, T. Moiseev, A. A. Monte, C. Monzani, M. E. Morselli, A. Moskalenko, I. V. Murgia, S. Nolan, P. L. Norris, J. P. Nuss, E. Ohsugi, T. Okumura, A. Omodei, N. Orlando, E. Ormes, J. F. Ozaki, M. Paneque, D. Panetta, J. H. Parent, D. Pepe, M. Pesce-Rollins, M. Piron, F. Pohl, M. Porter, T. A. Raino, S. Rando, R. Razzano, M. Reimer, A. Reimer, O. Reposeur, T. Ritz, S. Rochester, L. S. Rodriguez, A. Y. Ryde, F. Sadrozinski, H. F. -W. Sanchez, D. Sander, A. Parkinson, P. M. Saz Schalk, T. L. Sellerholm, A. Sgro, C. Smith, D. A. Smith, P. D. Spandre, G. Spinelli, P. Starck, J. -L. Stecker, F. W. Strickman, M. S. Strong, A. W. Suson, D. J. Tajima, H. Takahashi, H. Takahashi, T. Tanaka, T. Thayer, J. B. Thayer, J. G. Thompson, D. J. Tibaldo, L. Torres, D. F. Tosti, G. Tramacere, A. Uchiyama, Y. Usher, T. L. Vasileiou, V. Vilchez, N. Vitale, V. Waite, A. P. Wang, P. Winer, B. L. Wood, K. S. Ylinen, T. Ziegler, M. TI FERMI LAT OBSERVATION OF DIFFUSE GAMMA RAYS PRODUCED THROUGH INTERACTIONS BETWEEN LOCAL INTERSTELLAR MATTER AND HIGH-ENERGY COSMIC RAYS SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmic rays; diffuse radiation; gamma rays: observations ID NEAR-EARTH ORBIT; EGRET OBSERVATIONS; GALACTIC PLANE; BESS SPECTROMETER; AREA TELESCOPE; HELIUM SPECTRA; CO SURVEY; EMISSION; GALAXY; RADIATION AB Observations by the Large Area Telescope (LAT) on the Fermi mission of diffuse gamma-rays in a mid-latitude region in the third quadrant (Galactic longitude l from 200 degrees to 260 degrees and latitude vertical bar b vertical bar from 22 degrees to 60 degrees) are reported. The region contains no known large molecular cloud and most of the atomic hydrogen is within 1 kpc of the solar system. The contributions of gamma-ray point sources and inverse Compton scattering are estimated and subtracted. The residual gamma-ray intensity exhibits a linear correlation with the atomic gas column density in energy from 100 MeV to 10 GeV. The measured integrated gamma-ray emissivity is (1.63 +/- 0.05) x 10(-26) photons s(-1)sr(-1) H-atom(-1) and (0.66 +/- 0.02) x 10(-26) photons s(-1)sr(-1) H-atom(-1) above 100 MeV and above 300 MeV, respectively, with an additional systematic error of similar to 10%. The differential emissivity from 100 MeV to 10 GeV agrees with calculations based on cosmic ray spectra consistent with those directly measured, at the 10% level. The results obtained indicate that cosmic ray nuclei spectra within 1 kpc from the solar system in regions studied are close to the local interstellar spectra inferred from direct measurements at the Earth within similar to 10%. C1 [Abdo, A. A.; Chekhtman, A.; Dermer, C. D.; Grove, J. E.; Johnson, W. N.; Lovellette, M. N.; Makeev, A.; Mizuno, T.; Strickman, M. S.; Wood, K. S.] USN, Res Lab, Div Space Sci, Washington, DC 20375 USA. [Abdo, A. A.] Natl Acad Sci, Natl Res Council Res Associate, Washington, DC 20001 USA. [Ackermann, M.; Ajello, M.; Bechtol, K.; Berenji, B.; Bloom, E. D.; Borgland, A. W.; Cameron, R. A.; Claus, R.; Digel, S. W.; do Couto e Silva, E.; Drell, P. S.; Dubois, R.; Focke, W. B.; Funk, S.; Glanzman, T.; Godfrey, G.; Hayashida, M.; Johannesson, G.; Johnson, A. S.; Kamae, T.; Kocian, M. L.; Lande, J.; Michelson, P. F.; Mitthumsiri, W.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Nolan, P. L.; Paneque, D.; Panetta, J. H.; Reimer, A.; Reimer, O.; Rochester, L. S.; Tajima, H.; Tanaka, T.; Thayer, J. B.; Thayer, J. G.; Tramacere, A.; Uchiyama, Y.; Usher, T. L.; Waite, A. P.; Wang, P.] Stanford Univ, WW Hansen Expt Phys Lab, Kavli Inst Particle Astrophys & Cosmol, Dept Phys, Stanford, CA 94305 USA. [Ackermann, M.; Ajello, M.; Bechtol, K.; Berenji, B.; Bloom, E. D.; Borgland, A. W.; Cameron, R. A.; Claus, R.; Digel, S. W.; do Couto e Silva, E.; Drell, P. S.; Dubois, R.; Focke, W. B.; Funk, S.; Glanzman, T.; Godfrey, G.; Hayashida, M.; Johannesson, G.; Johnson, A. S.; Kamae, T.; Kocian, M. L.; Lande, J.; Michelson, P. F.; Mitthumsiri, W.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Nolan, P. L.; Paneque, D.; Panetta, J. H.; Reimer, A.; Reimer, O.; Rochester, L. S.; Tajima, H.; Tanaka, T.; Thayer, J. B.; Thayer, J. G.; Tramacere, A.; Uchiyama, Y.; Usher, T. L.; Waite, A. P.; Wang, P.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA. [Atwood, W. B.; Johnson, R. P.; Porter, T. A.; Sadrozinski, H. F. -W.; Parkinson, P. M. Saz; Schalk, T. L.; Ziegler, M.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Dept Phys, Santa Cruz, CA 95064 USA. [Atwood, W. B.; Johnson, R. P.; Porter, T. A.; Sadrozinski, H. F. -W.; Parkinson, P. M. Saz; Schalk, T. L.; Ziegler, M.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Axelsson, M.] Stockholm Univ, Dept Astron, SE-10691 Stockholm, Sweden. [Axelsson, M.; Carlson, P.; Conrad, J.; Meurer, C.; Ryde, F.; Sellerholm, A.; Ylinen, T.] AlbaNova, Oskar Klein Ctr Cosmo Particle Phys, SE-10691 Stockholm, Sweden. [Baldini, L.; Bellazzini, R.; Bregeon, J.; Brez, A.; Kuss, M.; Latronico, L.; Omodei, N.; Pesce-Rollins, M.; Razzano, M.; Sgro, C.; Spandre, G.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy. [Ballet, J.; Casandjian, J. M.; Grenier, I. A.; Starck, J. -L.] Univ Paris Diderot, CNRS, Lab AIM, CEA IRFU,Serv Astrophys,CEA Saclay, F-91191 Gif Sur Yvette, France. [Barbiellini, G.; Longo, F.] Univ Trieste, Dipartmento Fis, I-34127 Trieste, Italy. [Barbiellini, G.; Longo, F.] Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy. [Bastieri, D.; Rando, R.; Tibaldo, L.] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy. [Bastieri, D.; Rando, R.; Tibaldo, L.] Univ Padua, Dipartimento Fis G Galilei, I-35131 Padua, Italy. [Baughman, B. M.; Hughes, R. E.; Kuehn, F.; Sander, A.; Smith, P. D.; Winer, B. L.] Ohio State Univ, Dept Phys, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA. [Bonamente, E.; Cecchi, C.; Ciprini, S.; Germani, S.; Lubrano, P.; Pepe, M.; Tosti, G.] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy. [Bonamente, E.; Cecchi, C.; Ciprini, S.; Germani, S.; Lubrano, P.; Pepe, M.; Tosti, G.] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy. [Brigida, M.; Caliandro, G. A.; de Palma, F.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Giordano, F.; Loparco, F.; Monte, C.; Raino, S.; Spinelli, P.] Univ Politecn Bari, Dipartimento Fis M Merlin, I-70126 Bari, Italy. [Brigida, M.; Caliandro, G. A.; de Palma, F.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Giordano, F.; Loparco, F.; Monte, C.; Raino, S.; Spinelli, P.] Ist Nazl Fis Nucl, Sez Bari, I-70126 Bari, Italy. [Bruel, P.; Fegan, S. J.; Giebels, B.; Sanchez, D.] Ecole Polytech, CNRS, Lab Leprince Ringuet, IN2P3, F-91128 Palaiseau, France. [Burnett, T. H.; Kerr, M.] Univ Washington, Dept Phys, Seattle, WA 98195 USA. [Caraveo, P. A.] Ist Astrofis Spaziale & Fis Cosm, INAF, I-20133 Milan, Italy. [Carlson, P.; Conrad, J.; Ryde, F.; Ylinen, T.] Royal Inst Technol, KTH, Dept Phys, SE-10691 Stockholm, Sweden. [Chekhtman, A.; Makeev, A.] George Mason Univ, Fairfax, VA 22030 USA. [Cohen-Tanugi, J.; Farnier, C.; Guiriec, S.; Nuss, E.; Piron, F.] Univ Montpellier 2, Lab Phys Theor & Astroparticules, IN2P3, CNRS, Montpellier, France. [Conrad, J.; Meurer, C.; Sellerholm, A.] Stockholm Univ, Dept Phys, SE-10691 Stockholm, Sweden. [Cutini, S.; Gasparrini, D.] Agenzia Spaziale Italiana Sci Data Ctr, I-00044 Frascati, Roma, Italy. [de Angelis, A.; Frailis, M.] Univ Udine, Dipartimento Fis, I-33100 Udine, Italy. [de Angelis, A.; Frailis, M.] Ist Nazl Fis Nucl, Sez Trieste, Grp Coll Udine, I-33100 Udine, Italy. [Dumora, D.; Grondin, M. -H.; Guillemot, L.; Lemoine-Goumard, M.; Lott, B.; Parent, D.; Reposeur, T.; Smith, D. A.] Univ Bordeaux, Ctr Etud Nucl Bordeaux Gradignan, UMR 5797, F-33175 Gradignan, France. [Dumora, D.; Grondin, M. -H.; Guillemot, L.; Lemoine-Goumard, M.; Lott, B.; Parent, D.; Reposeur, T.; Smith, D. A.] CNRS, Ctr Etud Nucl Bordeaux Gradignan, UMR 5797, IN2P3, F-33175 Gradignan, France. [Fukazawa, Y.; Hanabata, Y.; Katagiri, H.; Mizuno, T.; Ohsugi, T.; Takahashi, H.] Hiroshima Univ, Dept Phys Sci, Hiroshima 7398526, Japan. [Gehrels, N.; Moiseev, A. A.] Univ Maryland, College Pk, MD 20742 USA. [Guiriec, S.] Univ Alabama, Huntsville, AL 35899 USA. [Kawai, N.] Tokyo Inst Technol, Dept Phys, Meguro, Tokyo 1528551, Japan. [Kawai, N.] RIKEN, Inst Phys & Chem Res, Cosm Radiat Lab, Wako, Saitama 3510198, Japan. [Knoedlseder, J.; Vilchez, N.] CNRS, UPS, Ctr Etud Spatiale Rayonnements, F-31028 Toulouse 4, France. [Moiseev, A. A.; Vasileiou, V.] NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA. [Morselli, A.; Vitale, V.] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, I-00133 Rome, Italy. [Norris, J. P.; Ormes, J. F.] Univ Denver, Dept Phys & Astron, Denver, CO 80208 USA. [Okumura, A.] Univ Tokyo, Dept Phys, Grad Sch Sci, Bunkyo Ku, Tokyo 1130033, Japan. [Orlando, E.; Strong, A. W.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Ozaki, M.; Takahashi, T.; Uchiyama, Y.] JAXA, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2298510, Japan. [Pohl, M.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. [Reimer, A.; Reimer, O.] Leopold Franzens Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria. [Rodriguez, A. Y.; Torres, D. F.] CSIC, IEEC, Inst Ciencies Espai, Barcelona 08193, Spain. [Suson, D. J.] Purdue Univ Calumet, Dept Chem & Phys, Hammond, IN 46323 USA. [Torres, D. F.] Inst Catalana Recerca & Estudis Avancats, Barcelona, Spain. [Tramacere, A.] CIFS, I-10133 Turin, Italy. [Vasileiou, V.] Univ Maryland Baltimore Cty, Baltimore, MD 21250 USA. [Vitale, V.] Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy. [Ylinen, T.] Univ Kalmar, Sch Pure & Appl Nat Sci, SE-39182 Kalmar, Sweden. RP Abdo, AA (reprint author), USN, Res Lab, Div Space Sci, Washington, DC 20375 USA. EM mizuno@hep01.hepl.hiroshima-u.ac.jp RI Tosti, Gino/E-9976-2013; Ozaki, Masanobu/K-1165-2013; Starck, Jean-Luc/D-9467-2011; Thompson, David/D-2939-2012; Stecker, Floyd/D-3169-2012; Harding, Alice/D-3160-2012; Gehrels, Neil/D-2971-2012; McEnery, Julie/D-6612-2012; Baldini, Luca/E-5396-2012; lubrano, pasquale/F-7269-2012; Morselli, Aldo/G-6769-2011; Nolan, Patrick/A-5582-2009; Kuss, Michael/H-8959-2012; giglietto, nicola/I-8951-2012; Rando, Riccardo/M-7179-2013; Hays, Elizabeth/D-3257-2012; Johnson, Neil/G-3309-2014; Reimer, Olaf/A-3117-2013; Funk, Stefan/B-7629-2015; Gargano, Fabio/O-8934-2015; Loparco, Francesco/O-8847-2015; Johannesson, Gudlaugur/O-8741-2015; Moskalenko, Igor/A-1301-2007; Mazziotta, Mario /O-8867-2015; Sgro, Carmelo/K-3395-2016; Torres, Diego/O-9422-2016; OI Starck, Jean-Luc/0000-0003-2177-7794; Thompson, David/0000-0001-5217-9135; lubrano, pasquale/0000-0003-0221-4806; Morselli, Aldo/0000-0002-7704-9553; giglietto, nicola/0000-0002-9021-2888; Reimer, Olaf/0000-0001-6953-1385; Funk, Stefan/0000-0002-2012-0080; Gargano, Fabio/0000-0002-5055-6395; Loparco, Francesco/0000-0002-1173-5673; Johannesson, Gudlaugur/0000-0003-1458-7036; Moskalenko, Igor/0000-0001-6141-458X; Mazziotta, Mario /0000-0001-9325-4672; Torres, Diego/0000-0002-1522-9065; Rando, Riccardo/0000-0001-6992-818X; Sgro', Carmelo/0000-0001-5676-6214; Giordano, Francesco/0000-0002-8651-2394; SPINELLI, Paolo/0000-0001-6688-8864; De Angelis, Alessandro/0000-0002-3288-2517; Frailis, Marco/0000-0002-7400-2135; Caraveo, Patrizia/0000-0003-2478-8018; Bastieri, Denis/0000-0002-6954-8862; Omodei, Nicola/0000-0002-5448-7577; Pesce-Rollins, Melissa/0000-0003-1790-8018; Axelsson, Magnus/0000-0003-4378-8785; Cutini, Sara/0000-0002-1271-2924; Berenji, Bijan/0000-0002-4551-772X; Gasparrini, Dario/0000-0002-5064-9495; Tramacere, Andrea/0000-0002-8186-3793; Baldini, Luca/0000-0002-9785-7726 FU National Aeronautics and Space Administration; Department of Energy in the United States; Commissariat a l'Energie Atomique; Centre National de la Recherche Scientifique/Institut National de Physique Nucleaire et de Physique des Particules in France; Agenzia Spaziale Italiana; Istituto Nazionale di Fisica Nucleare in Italy; Ministry of Education, Culture, Sports, Science and Technology (MEXT); High Energy Accelerator Research Organization (KEK); Japan Aerospace Exploration Agency (JAXA) in Japan; Swedish Research Council, and the Swedish National Space Board in Sweden 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 Swedish Research Council, and the Swedish National Space Board in Sweden. Additional support for science analysis during the operations phase from the following agencies is also gratefully acknowledged: the Istituto Nazionale di Astrofisica in Italy and the K. A. Wallenberg Foundation in Sweden. NR 48 TC 75 Z9 76 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 OCT 1 PY 2009 VL 703 IS 2 BP 1249 EP 1256 DI 10.1088/0004-637X/703/2/1249 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 495XS UT WOS:000269929500007 ER PT J AU Behar, E AF Behar, Ehud TI DENSITY PROFILES IN SEYFERT OUTFLOWS SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: individual (IRAS 13349+2438, NGC 3783, NGC 7469, NGC 5548, MCG-6-30-15); galaxies: ISM; techniques: spectroscopic; X-rays: galaxies ID ACTIVE GALACTIC NUCLEI; SOFT-X-RAY; THERMAL-INSTABILITY; KEY INGREDIENT; CHANDRA-LETGS; WARM ABSORBER; SPECTROSCOPY; WINDS; GAS; ABSORPTION AB For the past decade, ionized outflows of a few 100 km s(-1) from nearby Seyfert galaxies have been studied in great detail using high-resolution X-ray absorption spectra. A recurring feature of these outflows is their broad ionization distribution including essentially ions ( e. g., of Fe) from neutral to fully ionized. The absorption measure distribution (AMD) is defined as the distribution of column density with ionization parameter vertical bar dN(H)/d(log xi)vertical bar. AMDs of Seyfert outflows can span up to 5 orders of magnitude in.. We present the AMD of five outflows and show that they are all rather flat, perhaps slightly rising toward high ionization. More quantitatively, a power-law fit for log AMD proportional to (log xi)(a) yields slopes of 0 < a < 0.4. These slopes tightly constrain the density profiles of the wind, which until now could be addressed only by theory. If the wind is distributed on large scales, the measured slopes imply a generic density radial profile of n proportional to r(-alpha) with 1 < alpha < 1.3. This scaling rules out a mass conserving radial flow of n proportional to r(-2), or a constant density absorber, but is consistent with a nonspherical MHD outflow model in which n proportional to r(-1) along any given line of sight. On the other hand, if ionization variations are a result of local (delta r) density gradients, e.g., as in the turbulent interstellar medium (ISM), the AMD slopes imply density scaling of n proportional to delta r(-alpha) with 0.7 < alpha < 1.0, which is quite different from the scaling of approximately n proportional to delta r(0.4) found in the Milky Way ISM and typical of incompressible turbulence. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Behar, Ehud] Technion Israel Inst Technol, Dept Phys, IL-32000 Haifa, Israel. RP Behar, E (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM behar@milkyway.gsfc.nasa.gov NR 29 TC 27 Z9 27 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 1 PY 2009 VL 703 IS 2 BP 1346 EP 1351 DI 10.1088/0004-637X/703/2/1346 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 495XS UT WOS:000269929500016 ER PT J AU Strohmayer, TE Mushotzky, RF AF Strohmayer, Tod E. Mushotzky, Richard F. TI EVIDENCE FOR AN INTERMEDIATE-MASS BLACK HOLE IN NGC 5408 X-1 SO ASTROPHYSICAL JOURNAL LA English DT Article DE black hole physics; galaxies: individual (NGC 5408); stars: oscillations; X-rays: stars; X-rays: galaxies ID QUASI-PERIODIC OSCILLATIONS; X-RAY SOURCE; XTE J1550-564; QPO FREQUENCY; GRO J1655-40; VARIABILITY; OUTBURST; STELLAR; GX-339-4; BINARY AB We report the discovery with XMM-Newton of correlated spectral and timing behavior in the ultraluminous X-ray source (ULX) NGC 5408 X-1. An approximate to 100 ks pointing with XMM/Newton obtained in 2008 January reveals a strong 10 mHz quasi-periodic oscillation (QPO) in the > 1 keV flux, as well as flat-topped, band-limited noise breaking to a power law. The energy spectrum is again dominated by two components, a 0.16 keV thermal disk and a power law with an index of approximate to 2.5. These new measurements, combined with results from our previous 2006 January pointing in which we first detected QPOs, show for the first time in a ULX a pattern of spectral and temporal correlations strongly analogous to that seen in Galactic black hole (BH) sources, but at much higher X-ray luminosity and longer characteristic timescales. We find that the QPO frequency is proportional to the inferred disk flux, while the QPO and broadband noise amplitude (rms) are inversely proportional to the disk flux. Assuming that QPO frequency scales inversely with the BH mass at a given power-law spectral index we derive mass estimates using the observed QPO frequency-spectral index relations from five stellar-mass BH systems with dynamical mass constraints. The results from all sources are consistent with a mass range for NGC 5408 X-1 from 1000 to 9000 M(circle dot). We argue that these are conservative limits, and a more likely range is from 2000 to 5000 M(circle dot). Moreover, the recent relation from Gierlinski et al. that relates the BH mass to the strength of variability at high frequencies (above the break in the power spectrum) is also indicative of such a high mass for NGC 5408 X-1. Importantly, none of the above estimates appears consistent with a BH mass less than approximate to 1000 M(circle dot) for NGC 5408 X-1. We argue that these new findings strongly support the conclusion that NGC 5408 X-1 harbors an intermediate-mass BH. C1 [Strohmayer, Tod E.; Mushotzky, Richard F.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. RP Strohmayer, TE (reprint author), NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. EM tod.strohmayer@nasa.gov; richard.mushotzky@nasa.gov NR 37 TC 52 Z9 52 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 1 PY 2009 VL 703 IS 2 BP 1386 EP 1393 DI 10.1088/0004-637X/703/2/1386 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 495XS UT WOS:000269929500020 ER PT J AU Zhang, B Zhang, BB Virgili, FJ Liang, EW Kann, DA Wu, XF Proga, D Lv, HJ Toma, K Meszaros, P Burrows, DN Roming, PWA Gehrels, N AF Zhang, Bing Zhang, Bin-Bin Virgili, Francisco J. Liang, En-Wei Kann, D. Alexander Wu, Xue-Feng Proga, Daniel Lv, Hou-Jun Toma, Kenji Meszaros, Peter Burrows, David N. Roming, Peter W. A. Gehrels, Neil TI DISCERNING THE PHYSICAL ORIGINS OF COSMOLOGICAL GAMMA-RAY BURSTS BASED ON MULTIPLE OBSERVATIONAL CRITERIA: THE CASES OF z=6.7 GRB 080913, z=8.2 GRB 090423, AND SOME SHORT/HARD GRBs SO ASTROPHYSICAL JOURNAL LA English DT Review DE gamma rays: bursts ID AFTERGLOW LIGHT CURVES; STANDARD ENERGY RESERVOIR; COMPACT OBJECT MERGERS; SWIFT XRT DATA; X-RAY; HOST GALAXY; SHORT-DURATION; PEAK-ENERGY; OPTICAL AFTERGLOW; SPECTRAL LAGS AB The two high-redshift gamma- ray bursts, GRB 080913 at z = 6.7 and GRB 090423 at z = 8.2, recently detected by Swift appear as intrinsically short, hard GRBs. They could have been recognized by BATSE as short/hard GRBs should they have occurred at z <= 1. In order to address their physical origin, we perform a more thorough investigation on two physically distinct types (Type I/II) of cosmological GRBs and their observational characteristics. We reiterate the definitions of Type I/II GRBs and then review the following observational criteria and their physical motivations: supernova (SN) association, specific star-forming rate (SFR) of the host galaxy, location offset, duration, hardness, spectral lag, statistical correlations, energetics and collimation, afterglow properties, redshift distribution, luminosity function, and gravitational wave signature. Contrary to the traditional approach of assigning the physical category based on the gamma- ray properties (duration, hardness, and spectral lag), we take an alternative approach to define the Type I and Type II Gold Samples using several criteria that are more directly related to the GRB progenitors (SN association, host galaxy type, and specific SFR). We then study the properties of the two Gold Samples and compare them with the traditional long/soft and short/ hard samples. We find that the Type II Gold Sample reasonably tracks the long/soft population, although it includes several intrinsically short (shorter than 1 s in the rest frame) GRBs. The Type I Gold Sample only has five GRBs, four of which are not strictly short but have extended emission. Other short/ hard GRBs detected in the Swift era represent the BATSE short/ hard sample well, but it is unclear whether all of them belong to Type I. We suggest that some (probably even most) high-luminosity short/ hard GRBs instead belong to Type II. Based on multiple observational criteria, we suggest that GRB 080913 and GRB 090423 are more likely Type II events. In general, we acknowledge that it is not always straightforward to discern the physical categories of GRBs, and re-emphasize the importance of invoking multiple observational criteria. We cautiously propose an operational procedure to infer the physical origin of a given GRB with available multiple observational criteria, with various caveats laid out. C1 [Zhang, Bing; Zhang, Bin-Bin; Virgili, Francisco J.; Proga, Daniel] Univ Nevada, Dept Phys & Astron, Las Vegas, NV 89154 USA. [Liang, En-Wei; Lv, Hou-Jun] Guangxi Univ, Dept Phys, Guangxi 530004, Peoples R China. [Kann, D. Alexander] Thuringer Landessternwarte Tautenburg, D-07778 Tautenburg, Germany. [Wu, Xue-Feng; Toma, Kenji; Meszaros, Peter; Burrows, David N.; Roming, Peter W. A.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Wu, Xue-Feng] Chinese Acad Sci, Purple Mt Observ, Nanjing 210008, Peoples R China. [Meszaros, Peter] Penn State Univ, Dept Phys, University Pk, PA 16801 USA. [Gehrels, Neil] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Zhang, B (reprint author), Univ Nevada, Dept Phys & Astron, Las Vegas, NV 89154 USA. RI Gehrels, Neil/D-2971-2012; Zhang, Binbin/C-9035-2013; Wu, Xuefeng/G-5316-2015 OI Zhang, Binbin/0000-0003-2002-116X; Wu, Xuefeng/0000-0002-6299-1263 NR 320 TC 143 Z9 147 U1 2 U2 13 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD OCT 1 PY 2009 VL 703 IS 2 BP 1696 EP 1724 DI 10.1088/0004-637X/703/2/1696 PG 29 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 495XS UT WOS:000269929500040 ER PT J AU Makarov, VV Eggleton, PP AF Makarov, V. V. Eggleton, P. P. TI THE ORIGIN OF BRIGHT X-RAY SOURCES IN MULTIPLE STARS SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: close; stars: activity; stars: individual (AB Dor, BO Mic, TZ CrB) ID ALL-SKY SURVEY; ACTIVE-CHROMOSPHERE STARS; CLOSE BINARY-SYSTEMS; CONTACT BINARIES; ADDITIONAL COMPONENTS; MAGNETIC BRAKING; TIDAL FRICTION; EVOLUTION; CATALOG; HYADES AB Luminous X-ray stars are very often found in visual double or multiple stars. Binaries with periods of a few days possess the highest degree of coronal X-ray activity among regular, non-relativistic stars because of their fast, tidally driven rotation. But the orbital periods in visual double stars are too large for any direct interaction between the companions to take place. We suggest that most of the strongest X-ray components in resolved binaries are yet-undiscovered short-period binaries, and that a few aremerged remnants of such binaries. The omnipresence of short-period active stars, e. g., of BY-Dra-type binaries, in multiple systems is explained via the dynamical evolution of triple stars with large mutual inclinations. The dynamical perturbation on the inner pair pumps up the eccentricity in a cyclic manner, a phenomenon known asKozai cycling. At times of close periapsis, tidal friction reduces the angular momentum of the binary, causing it to shrink. When the orbital period of the inner pair drops to a fewdays, fast surface rotation of the companions is driven by tidal forces, boosting activity by a few orders of magnitude. If the period drops still further, a merger may take place leaving a rapidly rotating active dwarf with only a distant companion. C1 [Makarov, V. V.] CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA. [Eggleton, P. P.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA. RP Makarov, VV (reprint author), CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA. EM valeri.makarov@jpl.nasa.gov; eggleton1@llnl.gov OI Makarov, Valeri/0000-0003-2336-7887 FU U.S. Department of Energy by Lawrence Livermore National Laboratory [DE-AC5207NA27344] FX The research described in this paper was carried out partly at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. This work was also performed partly under the auspices of the U.S. Department of Energy by Lawrence Livermore National Laboratory under Contract DE-AC5207NA27344. This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France; and data products from the 2MASS, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center, California Institute of Technology, funded by NASA and the NSF. NR 39 TC 10 Z9 10 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 1 PY 2009 VL 703 IS 2 BP 1760 EP 1765 DI 10.1088/0004-637X/703/2/1760 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 495XS UT WOS:000269929500045 ER PT J AU Dorodnitsyn, A Kallman, T AF Dorodnitsyn, A. Kallman, T. TI AN AXISYMMETRIC HYDRODYNAMICAL MODEL FOR THE TORUS WIND IN ACTIVE GALACTIC NUCLEUS. III. SPECTRA FROM THREE-DIMENSIONAL RADIATION TRANSFER CALCULATIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE acceleration of particles; galaxies: active; hydrodynamics; methods: numerical; quasars: absorption lines; X-rays: galaxies ID SOFT-X-RAY; P CYGNI PROFILES; ACCRETION DISK; GRATING SPECTROMETER; LINE FORMATION; CHANDRA; NGC-1068; FLOWS; SPECTROSCOPY; DYNAMICS AB We calculate a series of synthetic X-ray spectra from outflows originating from the obscuring torus in active galactic nuclei (AGNs). Such modeling includes 2.5-dimensional hydrodynamical simulations of an X-ray excited torus wind, including the effects of X-ray heating, ionization, and radiation pressure. Three-dimensional radiation transfer calculations are performed in the three-dimensional Sobolev approximation. Synthetic X-ray line spectra and individual profiles of several strong lines are shown at different inclination angles, observing times, and for different characteristics of the torus. Our calculations show that rich synthetic warm absorber spectra from three-dimensional modeling are typically observed at a larger range of inclinations than was previously inferred from simple analysis of the transmitted spectra. In general, our results are supportive of warm absorber models based on the hypothesis of an "X-ray excited funnel flow" and are consistent with characteristics of such flows inferred from observations of warm absorbers from Seyfert 1 galaxies. C1 [Dorodnitsyn, A.; Kallman, T.] NASA, Goddard Space Flight Ctr, High Energy Astrophys Lab, Greenbelt, MD 20771 USA. [Dorodnitsyn, A.] Space Res Inst, Moscow 117997, Russia. RP Dorodnitsyn, A (reprint author), NASA, Goddard Space Flight Ctr, High Energy Astrophys Lab, Code 662, Greenbelt, MD 20771 USA. FU NASA Goddard Space Flight Center; NASA Astrophysics Theory Program [05-ATP05-18] FX This research was supported by an appointment to the NASA Postdoctoral Program at the NASA Goddard Space Flight Center, administered by Oak Ridge Associated Universities through a contract with NASA, and by grants from the NASA Astrophysics Theory Program 05-ATP05-18. NR 33 TC 9 Z9 9 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 1 PY 2009 VL 703 IS 2 BP 1797 EP 1809 DI 10.1088/0004-637X/703/2/1797 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 495XS UT WOS:000269929500049 ER PT J AU Hosokawa, T Omukai, K AF Hosokawa, Takashi Omukai, Kazuyuki TI LOW-METALLICITY PROTOSTARS AND THE MAXIMUM STELLAR MASS RESULTING FROM RADIATIVE FEEDBACK: SPHERICALLY SYMMETRIC CALCULATIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; stars: early-type; stars: evolution; stars: formation; stars: pre-main sequence ID DENSE MOLECULAR CORES; STAR-FORMATION; 1ST STARS; UPPER LIMIT; PRIMORDIAL STAR; ACCRETION; EVOLUTION; CLUSTER; PHYSICS; CLOUDS AB The final mass of a newborn star is set at the epoch when the mass accretion onto the star is terminated. We study the evolution of accreting protostars and the limits of accretion in low-metallicity environments under spherical symmetry. Accretion rates onto protostars are estimated via the temperature evolution of prestellar cores with different metallicities. The derived rates increase with decreasing metallicity, from. <(M)over dot> similar or equal to 10(-6) M(circle dot) yr(-1) at Z = Z(circle dot) to 10(-3) M(circle dot) yr(-1) at Z = 0. With the derived accretion rates, the protostellar evolution is numerically calculated. We find that, at lower metallicity, the protostar has a larger radius and reaches the zero-age main sequence (ZAMS) at higher stellar mass. Using this protostellar evolution, we evaluate the upper stellar mass limit where the mass accretion is hindered by radiative feedback. We consider the effects of radiation pressure exerted on the accreting envelope, and expansion of an Hii region. The mass accretion is finally terminated by radiation pressure on dust grains in the envelope for Z greater than or similar to 10(-3) Z(circle dot) and by the expanding Hii region for lower metallicity. The mass limit from these effects increases with decreasing metallicity from M(*) similar or equal to 10 M(circle dot) at Z = Z(circle dot) to similar or equal to 300 M(circle dot) at Z = 10(-6) Z(circle dot). The termination of accretion occurs after the central star arrives at the ZAMS at all metallicities, which allows us to neglect protostellar evolution effects in discussing the upper mass limit by stellar feedback. The fragmentation induced by line cooling in low-metallicity clouds yields prestellar cores with masses large enough that the final stellar mass is set by the feedback effects. Although relaxing the assumption of spherical symmetry will alter feedback effects, our results will be a benchmark for more realistic evolution to be explored in future studies. C1 [Hosokawa, Takashi] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Hosokawa, Takashi; Omukai, Kazuyuki] Natl Astron Observ, Div Theoret Astron, Mitaka, Tokyo 1818588, Japan. RP Hosokawa, T (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM takashi.hosokawa@jpl.nasa.gov; omukai@th.nao.ac.jp FU Japan Society for the Promotion of Science for Young Scientists; Ministry of Education, Science and Culture of Japan [18740117, 19047004, 21684007] FX The authors thank Neal Turner for his help to revise the manuscript. This study is supported in part by Research Fellowships of the Japan Society for the Promotion of Science for Young Scientists (T.H.) and by the Grants-in-Aid by the Ministry of Education, Science and Culture of Japan (18740117, 19047004, 21684007: K.O.). NR 36 TC 21 Z9 21 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 1 PY 2009 VL 703 IS 2 BP 1810 EP 1818 DI 10.1088/0004-637X/703/2/1810 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 495XS UT WOS:000269929500050 ER PT J AU Datta, A Bhatnagar, S Carilli, CL AF Datta, A. Bhatnagar, S. Carilli, C. L. TI DETECTION OF SIGNALS FROM COSMIC REIONIZATION USING RADIO INTERFEROMETRIC SIGNAL PROCESSING SO ASTROPHYSICAL JOURNAL LA English DT Article DE early universe; intergalactic medium; methods: data analysis; radio lines: general; techniques: interferometric ID HIGH DYNAMIC-RANGE; FOREGROUND SUBTRACTION; WIDEFIELD ARRAY; EPOCH; SIMULATIONS; TOMOGRAPHY; EMISSION AB Observations of the HI 21 cm transition line promises to be an important probe into the cosmic dark ages and epoch of reionization. One of the challenges for the detection of this signal is the accuracy of the foreground source removal. This paper investigates the extragalactic point source contamination and how accurately the bright sources (greater than or similar to 1 Jy) should be removed in order to reach the desired rms noise and be able to detect the 21 cm transition line. Here, we consider position and flux errors in the global sky model for these bright sources as well as the frequency independent residual calibration errors. The synthesized beam is the only frequency dependent term included here. This work determines the level of accuracy for the calibration and source removal schemes and puts forward constraints for the design of the cosmic reionization data reduction scheme for the upcoming low frequency arrays such as, Murchison Widefield Array, Precision Array to Probe Epoch of Reionization, etc. We show that in order to detect the reionization signal the bright sources need to be removed from the data sets with a positional accuracy of similar to 0.1 arcsec. Our results also demonstrate that the efficient foreground source removal strategies can only tolerate a frequency independent antenna based mean residual calibration error of less than or similar to 0.2% in amplitude or less than or similar to 0.degrees 2 in phase, if they are constant over each days of observations (6 hr). In future papers, we will extend this analysis to the power-spectral domain and also include the frequency-dependent calibration errors and direction-dependent errors (ionosphere, primary beam, etc.). C1 [Datta, A.] New Mexico Inst Min & Technol, Socorro, NM 87801 USA. [Datta, A.; Bhatnagar, S.; Carilli, C. L.] Natl Radio Astron Observ, Socorro, NM 87801 USA. [Carilli, C. L.] NASA, Ames Res Ctr, Lunar Sci Inst, Moffett Field, CA 94035 USA. RP Datta, A (reprint author), New Mexico Inst Min & Technol, Socorro, NM 87801 USA. EM adatta@nrao.edu FU Max-Planck Society; Alexander von Humboldt Foundation; National Radio Astronomy Observatory; NASA [NNA09DB30A] FX A. D. and C. C. are grateful for support from the Max-Planck Society and the Alexander von Humboldt Foundation through the Max Planck Forshungspreise 2005. A. D. is also grateful for support from the National Radio Astronomy Observatory through the Graduate Internship Program. The LUNAR consortium (http://lunar.colorado.edu), headquartered at the University of Colorado, is funded by the NASA Lunar Science Institute (via Cooperative Agreement NNA09DB30A) to investigate concepts for astrophysical observatories on the Moon. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. NR 29 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 OCT 1 PY 2009 VL 703 IS 2 BP 1851 EP 1862 DI 10.1088/0004-637X/703/2/1851 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 495XS UT WOS:000269929500054 ER PT J AU Seager, S Deming, D AF Seager, S. Deming, D. TI ON THE METHOD TO INFER AN ATMOSPHERE ON A TIDALLY LOCKED SUPER EARTH EXOPLANET AND UPPER LIMITS TO GJ 876d SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems; stars: individual: (GJ 876); techniques: photometric ID EXTRA-SOLAR PLANETS; NEPTUNE-MASS PLANET; STAR TAU-BOOTIS; M-DWARF GJ-436; M-CIRCLE-PLUS; HD 189733B; TERRESTRIAL EXOPLANETS; HOT JUPITERS; HARPS SEARCH; MISSION AB We develop a method to infer or rule out the presence of an atmosphere on a tidally locked hot super Earth. The question of atmosphere retention is a fundamental one, especially for planets orbiting M stars due to the star's long-duration active phase and corresponding potential for stellar-induced planetary atmospheric escape and erosion. Tidally locked planets with no atmosphere are expected to show a Lambertian-like thermal phase curve, causing the combined light of the planet-star system to vary with planet orbital phase. We report Spitzer 8 mu m IRAC observations of GJ 876 taken over 32 continuous hours and reaching a relative photometric precision of 3.9 x 10(-4) per point for 25.6 s time sampling. This translates to a 3 sigma limit of 5.13 x 10(-5) on a planet thermal phase curve amplitude. Despite the almost photon-noise-limited data, we are unable to conclusively infer the presence of an atmosphere or rule one out on the non-transiting short-period super Earth GJ 876d. The limiting factor in our observations was the miniscule, monotonic photometric variation of the slightly active host M star, because the partial sine wave due to the planet has a component in common with the stellar linear trend. The proposed method is nevertheless very promising for transiting hot super Earths with the James Webb Space Telescope and is critical for establishing observational constraints for atmospheric escape. C1 [Seager, S.] MIT, Dept Earth Atmospher & Planetary Sci, Dept Phys, Cambridge, MA 02139 USA. [Deming, D.] NASA, Goddard Space Flight Ctr, Planetary Syst Branch, Greenbelt, MD 20771 USA. RP Seager, S (reprint author), MIT, Dept Earth Atmospher & Planetary Sci, Dept Phys, 77 Massachusetts Ave, Cambridge, MA 02139 USA. FU NASA FX We thank Feng Tian, Andrew West, Brad Hager, Leslie Rogers, and Lindy Elkins-Tanton for many useful discussions. We thank Eugenio Rivera and Greg Laughlin for providing an unpublished updated ephemeris for GJ 876d, Pedro Sada for communicating his GJ 876 photometry in advance of publication, and Heather Knutson for showing us her unpublished photometry of the M dwarf companion to 189733. We thank an anonymous reviewer for a careful read of our paper. We thank the Spitzer Science Center staff for their efficient scheduling of our observations and for assistance in finding the best pre-flash source. This work is based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech. NR 39 TC 25 Z9 25 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 OCT 1 PY 2009 VL 703 IS 2 BP 1884 EP 1889 DI 10.1088/0004-637X/703/2/1884 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 495XS UT WOS:000269929500057 ER PT J AU Furlan, E Watson, DM McClure, MK Manoj, P Espaillat, C D'Alessio, P Calvet, N Kim, KH Sargent, BA Forrest, WJ Hartmann, L AF Furlan, E. Watson, Dan M. McClure, M. K. Manoj, P. Espaillat, C. D'Alessio, P. Calvet, N. Kim, K. H. Sargent, B. A. Forrest, W. J. Hartmann, L. TI DISK EVOLUTION IN THE THREE NEARBY STAR-FORMING REGIONS OF TAURUS, CHAMAELEON, AND OPHIUCHUS SO ASTROPHYSICAL JOURNAL LA English DT Review DE circumstellar matter; infrared: stars; stars: formation; stars: pre-main sequence ID MAIN-SEQUENCE STARS; SPITZER-SPACE-TELESCOPE; INTERSTELLAR SILICATE MINERALOGY; AURIGA MOLECULAR CLOUD; YOUNG STELLAR OBJECTS; INITIAL MASS FUNCTION; SPECTRAL ENERGY-DISTRIBUTIONS; INFRARED SPECTROGRAPH SPECTRA; HERBIG AE/BE STARS; PROTOPLANETARY DISKS AB We analyze samples of Spitzer Infrared Spectrograph spectra of T Tauri stars in the Ophiuchus, Taurus, and Chamaeleon I star-forming regions, whose median ages lie in the < 1-2 Myr range. The median mid-infrared spectra of objects in these three regions are similar in shape, suggesting, on average, similar disk structures. When normalized to the same stellar luminosity, the medians follow each other closely, implying comparable mid-infrared excess emission from the circumstellar disks. We use the spectral index between 13 and 31 mu m and the equivalent width of the 10 mu m silicate emission feature to identify objects whose disk configuration departs from that of a continuous, optically thick accretion disk. Transitional disks, whose steep 13-31 mu m spectral slope and near-IR flux deficit reveal inner disk clearing, occur with about the same frequency of a few percent in all three regions. Objects with unusually large 10 mu m equivalent widths are more common (20%-30%); they could reveal the presence of disk gaps filled with optically thin dust. Based on their medians and fraction of evolved disks, T Tauri stars in Taurus and Chamaeleon I are very alike. Disk evolution sets in early, since already the youngest region, the Ophiuchus core (L1688), has more settled disks with larger grains. Our results indicate that protoplanetary disks show clear signs of dust evolution at an age of a few Myr, even as early as similar to 1 Myr, but age is not the only factor determining the degree of evolution during the first few million years of a disk's lifetime. C1 [Furlan, E.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Watson, Dan M.; McClure, M. K.; Manoj, P.; Kim, K. H.; Sargent, B. A.; Forrest, W. J.] Univ Rochester, Dept Phys & Astron, Rochester, NY 14627 USA. [McClure, M. K.; Espaillat, C.; Calvet, N.; Hartmann, L.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [D'Alessio, P.] Univ Nacl Autonoma Mexico, Ctr Radioastron & Astrofis, Morelia 58089, Michoacan, Mexico. [Furlan, E.] Univ Calif Los Angeles, NASA, Astrobiol Inst, Los Angeles, CA 90095 USA. RP Furlan, E (reprint author), CALTECH, JPL, Mail Stop 264-767,4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Elise.Furlan@jpl.nasa.gov; dmw@pas.rochester.edu; melisma@umich.edu; manoj@pas.rochester.edu; ccespa@umich.edu; p.dalessio@astrosmo.unam.mx; ncalvet@umich.edu; khkim@pas.rochester.edu; bsargent@pas.rochester.edu; forrest@pas.rochester.edu; lhartm@umich.edu OI McClure, Melissa/0000-0003-1878-327X; Furlan, Elise/0000-0001-9800-6248 FU NASA [1407, NNG05GI26G, NNG06GJ32G, NNX08AH94G]; CONACyT, Mexico FX We thank the referee for a thoughtful review that led us to improve this paper. This work is based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory (JPL), California Institute of Technology (Caltech), under NASA contract 1407. Support for this work was provided by NASA through contract number 1257184 issued by JPL/Caltech. E. F. was partly supported by a NASA Postdoctoral Program Fellowship, administered by Oak Ridge Associated Universities through a contract with NASA, and partly supported by NASA through the Spitzer Space Telescope Fellowship Program, through a contract issued by JPL/Caltech under a contract with NASA. N. C. and L. H. acknowledge support from NASAOrigins grants NNG05GI26G, NNG06GJ32G, and NNX08AH94G. P. D. acknowledges grants from CONACyT, Mexico. 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/Caltech, funded by NASA and the NSF. It has also made use of the SIMBAD and VizieR databases, operated at CDS (Strasbourg, France), NASA's Astrophysics Data System Abstract Service; and of the NASA/IPAC Infrared Science Archive operated by JPL, Caltech, under contract with NASA. NR 140 TC 80 Z9 81 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 1 PY 2009 VL 703 IS 2 BP 1964 EP 1983 DI 10.1088/0004-637X/703/2/1964 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 495XS UT WOS:000269929500065 ER PT J AU Turner, NJ Drake, JF AF Turner, N. J. Drake, J. F. TI ENERGETIC PROTONS, RADIONUCLIDES, AND MAGNETIC ACTIVITY IN PROTOSTELLAR DISKS SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; instabilities; MHD; solar system: formation; stars: formation ID CLASSICAL-T-TAURI; YOUNG STELLAR OBJECTS; X-RAY-EMISSION; PROTOPLANETARY DISKS; IONIZATION FRACTION; ACCRETION DISKS; DEAD ZONE; MAGNETOROTATIONAL INSTABILITY; INTERSTELLAR CLOUDS; CHANDRA OBSERVATION AB We calculate the location of the magnetically inactive dead zone in the minimum-mass protosolar disk, under ionization scenarios including stellar X-rays, long- or short-lived radionuclide decay, and energetic protons arriving from the general interstellar medium, from a nearby supernova explosion, from the disk corona, or from the corona of the young star. The disk contains a dead zone in all scenarios except those with small dust grains removed and a fraction of the short-lived radionuclides remaining in the gas. All the cases without exception have an "undead zone" where intermediate resistivities prevent magneto-rotational turbulence while allowing shear-generated large-scale magnetic fields. The mass column in the undead zone is typically greater than the column in the turbulent surface layers. The results support the idea that the dead and undead zones are robust consequences of cold, dusty gas with mass columns exceeding 1000 g cm(-2). C1 [Turner, N. J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Drake, J. F.] Univ Maryland, Inst Phys Sci & Technol, Dept Phys, College Pk, MD 20742 USA. RP Turner, NJ (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM neal.turner@jpl.nasa.gov NR 74 TC 39 Z9 39 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 1 PY 2009 VL 703 IS 2 BP 2152 EP 2159 DI 10.1088/0004-637X/703/2/2152 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 495XS UT WOS:000269929500082 ER PT J AU Trouille, L Barger, AJ Cowie, LL Yang, Y Mushotzky, RF AF Trouille, L. Barger, A. J. Cowie, L. L. Yang, Y. Mushotzky, R. F. TI THE OPTX PROJECT. III. X-RAY VERSUS OPTICAL SPECTRAL TYPE FOR ACTIVE GALACTIC NUCLEI SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology: observations; galaxies: active ID DEEP-FIELD-NORTH; CHANDRA MULTIWAVELENGTH PROJECT; POINT-SOURCE CATALOG; MEDIUM SENSITIVITY SURVEY; XMM-NEWTON OBSERVATIONS; MS SOURCE CATALOGS; SEYFERT 2 GALAXIES; ALL-SKY SURVEY; LUMINOSITY FUNCTION; HELLAS2XMM SURVEY AB We compare the optical spectral types with the X-ray spectral properties for a uniformly selected (sources with fluxes greater than the 3 sigma level and above a flux limit of f(2-8 keV) > 3.5 x 10(-15) erg cm(-2) s(-1)), highly spectroscopically complete (> 80% for f(2-8 keV) > 10(-14) erg cm(-2) s(-1) and > 60% below) 2-8 keV X-ray sample observed in three Chandra fields (CLANS, CLASXS, and the CDF-N) that cover similar to 1.2 deg(2). For our sample of 645 spectroscopically observed sources, we confirm that there is significant overlap of the X-ray spectral properties, as determined by the effective photon indices, Gamma(eff), obtained from the ratios of the 0.5-2 keV to 2-8 keV counts, for the different optical spectral types. For example, broad-line active galactic nuclei (AGNs) are expected to be unobscured and hence X-ray soft (Gamma(eff) >= 1.2), yet we find 20% +/- 3% have Gamma(eff) >= 1.2. Non-broad-line AGNs are expected to be obscured and hence X-ray hard (Gamma(eff) < 1.2), yet we find 33% +/- 4% have Gamma(eff) >= 1.2. Thus, one cannot use the X-ray spectral classifications and the optical spectral classifications equivalently. Since it is not understood how X-ray and optical classifications relate to the obscuration of the central engine, we strongly advise against a mixed classification scheme, as it can only complicate the interpretation of X-ray AGN samples. We confirm the dependence of optical spectral type on X-ray luminosity, and for z < 1, we find a similar luminosity dependence of Gamma(eff). However, this dependence breaks down at higher redshifts due to the highly redshift-dependent nature of Gamma(eff). We therefore also caution that any classification scheme which depends on Gamma(eff) is likely to suffer from serious redshift bias. C1 [Trouille, L.; Barger, A. J.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. [Barger, A. J.] Univ Hawaii, Dept Phys & Astron, Honolulu, HI 96822 USA. [Barger, A. J.; Cowie, L. L.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Yang, Y.] Univ Illinois, Dept Astron, Urbana, IL 61801 USA. [Mushotzky, R. F.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Trouille, L (reprint author), Univ Wisconsin, Dept Astron, 475 N Charter St, Madison, WI 53706 USA. FU National Science Foundation Graduate Research Fellowship; NSF [AST 0239425, AST 0708793, AST 0407374, AST 0709356]; Wisconsin Alumni Research Foundation; David and Lucile Packard Foundation FX L. T. was supported by a National Science Foundation Graduate Research Fellowship and a Wisconsin Space Grant Consortium Graduate Fellowship Award during portions of this work. We also gratefully acknowledge support from NSF grants AST 0239425 and AST 0708793 (A.J.B.) and AST 0407374 and AST 0709356 (L.L.C.), the University of Wisconsin Research Committee with funds granted by the Wisconsin Alumni Research Foundation and the David and Lucile Packard Foundation (A.J.B.). A.J.B. thanks the Aspen Center for Physics for hospitality during the completion of this work. This article is part of L. T.' s PhD thesis work at the University of WisconsinMadison. NR 83 TC 24 Z9 24 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 1 PY 2009 VL 703 IS 2 BP 2160 EP 2170 DI 10.1088/0004-637X/703/2/2160 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 495XS UT WOS:000269929500083 ER PT J AU Schmoll, S Miller, JM Volonteri, M Cackett, E Reynolds, CS Fabian, AC Brenneman, LW Miniutti, G Gallo, LC AF Schmoll, S. Miller, J. M. Volonteri, M. Cackett, E. Reynolds, C. S. Fabian, A. C. Brenneman, L. W. Miniutti, G. Gallo, L. C. TI CONSTRAINING THE SPIN OF THE BLACK HOLE IN FAIRALL 9 WITH SUZAKU SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; black hole physics; galaxies: active; relativity; X-rays: galaxies ID ACTIVE GALACTIC NUCLEI; X-RAY REFLECTION; XMM-NEWTON; CHAOTIC ACCRETION; ENERGY EXTRACTION; EMISSION-LINES; IRON; VARIABILITY; MCG-6-30-15; EVOLUTION AB We report on the results of spectral fits made to data obtained from a 168 ks Suzaku observation of the Seyfert 1 galaxy Fairall 9. The source is clearly detected out to 30 keV. The observed spectrum is fairly simple; it is well described by a power law with soft excess and disk reflection. A broad iron line is detected, and easily separated from distinct narrow components owing to the resolution of the CCDs in the X-ray Imaging Spectrometer (XIS). The broad line is revealed to be asymmetric, consistent with a disk origin. We fit the XIS and Hard X-ray Detector spectra with relativistically blurred disk reflection models. With the assumption that the inner disk extends to the innermost stable circular orbit, the best-fit model implies a black hole spin parameter of a = 0.60 +/- 0.07 and excludes extremal values at a high level of confidence. We discuss this result in the context of Seyfert observations and models of the cosmic distribution of black hole spin. C1 [Schmoll, S.; Miller, J. M.; Volonteri, M.; Cackett, E.] Univ Michigan, Dept Astron & Astrophys, Ann Arbor, MI 48109 USA. [Reynolds, C. S.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Fabian, A. C.] Univ Cambridge, Inst Astron, Cambridge CB3 OHA, England. [Brenneman, L. W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Miniutti, G.] Max Planck Inst Extraterr Phys, D-85741 Garching, Germany. [Miniutti, G.] Lab APC, UMR 7164, F-75205 Paris 13, France. [Miniutti, G.] LAEFF, Ctr Astrobiol CSIC INTA, LAEX, E-28691 Madrid, ES, Spain. [Gallo, L. C.] St Marys Univ, Dept Phys & Astron, Halifax, NS B3H 3CS, Canada. RP Schmoll, S (reprint author), Univ Michigan, Dept Astron & Astrophys, 500 Church St, Ann Arbor, MI 48109 USA. EM schmoll@umich.edu RI Miniutti, Giovanni/L-2721-2014; XRAY, SUZAKU/A-1808-2009 OI Miniutti, Giovanni/0000-0003-0707-4531; FU NASA through the Chandra Fellowship Program [PF890052] FX We thank the anonymous referee for helpful comments that improved this work. J. M. M. gratefully acknowledges funding from NASA through the Suzaku guest investigator program. E. M. C. gratefully acknowledges support provided by NASA through the Chandra Fellowship Program, grant number PF890052. We thank the US and Japanese Suzaku teams for executing this observation. We acknowledge helpful discussions with Koji Mukai and Oleg Gnedin. This work has made use of the facilities and tools available through HEASARC, operated by GSFC for NASA. NR 37 TC 51 Z9 53 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 OCT 1 PY 2009 VL 703 IS 2 BP 2171 EP 2176 DI 10.1088/0004-637X/703/2/2171 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 495XS UT WOS:000269929500084 ER PT J AU Sheldon, ES Johnston, DE Scranton, R Koester, BP Mckay, TA Oyaizu, H Cunha, C Lima, M Lin, H Frieman, JA Wechsler, RH Annis, J Mandelbaum, R Bahcall, NA Fukugita, M AF Sheldon, Erin S. Johnston, David E. Scranton, Ryan Koester, Benjamin P. McKay, Timothy A. Oyaizu, Hiroaki Cunha, Carlos Lima, Marcos Lin, Huan Frieman, Joshua A. Wechsler, Risa H. Annis, James Mandelbaum, Rachel Bahcall, Neta A. Fukugita, Masataka TI CROSS-CORRELATION WEAK LENSING OF SDSS GALAXY CLUSTERS. I. MEASUREMENTS SO ASTROPHYSICAL JOURNAL LA English DT Article DE dark matter; galaxies: clusters: general; gravitational lensing; large-scale structure of universe ID DIGITAL SKY SURVEY; SPECTROSCOPIC TARGET SELECTION; MASS CORRELATION-FUNCTION; DARK-MATTER HALOES; LARGE-SCALE BIAS; REDSHIFT SURVEY; DENSITY PROFILE; DATA RELEASE; SAMPLE; CALIBRATION AB This is the first in a series of papers on the weak lensing effect caused by clusters of galaxies in Sloan Digital Sky Survey. The photometrically selected cluster sample, known as MaxBCG, includes similar to 130,000 objects between redshift 0.1 and 0.3, ranging in size from small groups to massive clusters. We split the clusters into bins of richness and luminosity and stack the surface density contrast to produce mean radial profiles. The mean profiles are detected over a range of scales, from the inner halo (25 kpc h(-1)) well into the surrounding large-scale structure (30 Mpc h(-1)), with a significance of 15 to 20 in each bin. The signal over this large range of scales is best interpreted in terms of the cluster-mass cross-correlation function. We pay careful attention to sources of systematic error, correcting for them where possible. The resulting signals are calibrated to the similar to 10% level, with the dominant remaining uncertainty being the redshift distribution of the background sources. We find that the profiles scale strongly with richness and luminosity. We find that the signal within a given richness bin depends upon luminosity, suggesting that luminosity is more closely correlated with mass than galaxy counts. We split the samples by redshift but detect no significant evolution. The profiles are not well described by power laws. In a subsequent series of papers, we invert the profiles to three-dimensional mass profiles, show that they are well fit by a halo model description, measure mass-to-light ratios, and provide a cosmological interpretation. C1 [Sheldon, Erin S.] Brookhaven Natl Lab, New York, NY 11973 USA. [Sheldon, Erin S.] New York Univ, Dept Phys, Ctr Cosmol & Particle Phys, New York, NY 10003 USA. [Johnston, David E.] CALTECH, Dept Astron, Pasadena, CA 91125 USA. [Johnston, David E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Scranton, Ryan] Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA. [Koester, Benjamin P.; Oyaizu, Hiroaki; Cunha, Carlos; Lima, Marcos; Frieman, Joshua A.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Koester, Benjamin P.; Oyaizu, Hiroaki; Cunha, Carlos; Frieman, Joshua A.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [McKay, Timothy A.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA. [McKay, Timothy A.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [McKay, Timothy A.] Univ Michigan, Michigan Ctr Theoret Phys, Ann Arbor, MI 48109 USA. [Lima, Marcos] Univ Chicago, Dept Phys, Chicago, IL 60637 USA. [Lin, Huan; Frieman, Joshua A.; Annis, James] Fermilab Natl Accelerator Lab, Batavia, IL 60510 USA. [Wechsler, Risa H.] Stanford Univ, Dept Phys, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA. [Wechsler, Risa H.] Stanford Univ, Stanford Linear Accelerator Ctr, Stanford, CA 94305 USA. [Mandelbaum, Rachel] Princeton Univ, Dept Phys, Princeton, NJ 08544 USA. [Bahcall, Neta A.] Princeton Univ Observ, Princeton, NJ 08544 USA. [Fukugita, Masataka] Univ Tokyo, Inst Cosm Ray Res, Kashiwa, Chiba 2778582, Japan. RP Sheldon, ES (reprint author), Brookhaven Natl Lab, New York, NY 11973 USA. RI Lima, Marcos/E-8378-2010; McKay, Timothy/C-1501-2009; Mandelbaum, Rachel/N-8955-2014 OI McKay, Timothy/0000-0001-9036-6150; Mandelbaum, Rachel/0000-0003-2271-1527 FU NSF [AST-0428465, AST-044327]; U.S. Department of Energy [DEAC0298CH10886, DE-FG0208ER41567]; Alfred P. Sloan Foundation; National Science Foundation; National Aeronautics and Space Administration; Japanese Monbukagakusho; Max Planck Society; Higher Education Funding Council for England FX E. S. S. was supported in part by NSF grant AST-0428465 and the U.S. Department of Energy under contract No. DEAC0298CH10886. B. P. K. and T. A. M. gratefully acknowledge support from NSF grant AST-044327 and the Michigan Center for Theoretical Physics. D. E. J. received partial support from the U.S. Department of Energy under contract number DE-FG0208ER41567. The research described in this paperwas performed in part at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. Funding for the SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation, the ParticipatingInstitutions, 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/. NR 80 TC 89 Z9 89 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 1 PY 2009 VL 703 IS 2 BP 2217 EP 2231 DI 10.1088/0004-637X/703/2/2217 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 495XS UT WOS:000269929500087 ER PT J AU Sheldon, ES Johnston, DE Masjedi, M Mckay, TA Blanton, MR Scranton, R Wechsler, RH Koester, BP Hansen, SM Frieman, JA Annis, J AF Sheldon, Erin S. Johnston, David E. Masjedi, Morad McKay, Timothy A. Blanton, Michael R. Scranton, Ryan Wechsler, Risa H. Koester, Benjamin P. Hansen, Sarah M. Frieman, Joshua A. Annis, James TI CROSS-CORRELATION WEAK LENSING OF SDSS GALAXY CLUSTERS. III. MASS-TO-LIGHT RATIOS SO ASTROPHYSICAL JOURNAL LA English DT Article DE dark matter; galaxies: clusters: general; gravitational lensing; large-scale structure of universe ID DIGITAL SKY SURVEY; NEAR-INFRARED PROPERTIES; HALO OCCUPATION NUMBER; LARGE-SCALE BIAS; DARK-MATTER; LUMINOSITY FUNCTIONS; DEPENDENCE; PROFILES; SEQUENCE; MAXBCG AB We present measurements of the excess mass-to-light ratio (M/L) measured around MaxBCG galaxy clusters observed in the Sloan Digital Sky Survey. This red-sequence cluster sample includes objects from small groups with M(200) similar to 5 x 10(12) h(-1) M(circle dot) to clusters with M(200) similar to 10(15) h(-1) M(circle dot). Using cross-correlation weak lensing, we measure the excess mass density profile above the universal mean Delta rho(r) = rho(r) - (rho) over bar for clusters in bins of richness and optical luminosity. We also measure the excess luminosity density Delta l(r) = l(r) - (l) over bar measured in the z = 0.25 i band. For both mass and light, we de-project the profiles to produce three-dimensional mass and light profiles over scales from 25 h(-1) kpc to 22 h(-1) Mpc. From these profiles we calculate the cumulative excess mass Delta M(r) and excess light Delta L(r) as a function of separation from the BCG. On small scales, where rho(r) >> (rho) over bar the integrated mass-to-light profile (Delta M/Delta L)(r) may be interpreted as the cluster M/L. We find the (Delta M/Delta L)(200), the M/L within r(200), scales with cluster mass as a power law with index 0.33 +/- 0.02. On large scales, where rho(r) similar to (rho) over bar the Delta M/Delta L approaches an asymptotic value independent of cluster richness. For small groups, the mean (Delta M/Delta L)(200) is much smaller than the asymptotic value, while for large clusters (Delta M/Delta L)(200) is consistent with the asymptotic value. This asymptotic value should be proportional to the mean M/L of the universe < M/L >. We find < M/L > b(M/L)(-2) = 362 +/- 54h (statistical). There is additional uncertainty in the overall calibration at the similar to 10% level. The parameter b(M/L)(2) is primarily a function of the bias of the L less than or similar to L(*) galaxies used as light tracers, and should be of order unity. Multiplying by the luminosity density in the same bandpass we find Omega(m)b(M/L)(-2) = 0.20 +/- 0.03, independent of the Hubble parameter. C1 [Sheldon, Erin S.] Brookhaven Natl Lab, Upton, NY 11973 USA. [Sheldon, Erin S.; Masjedi, Morad; Blanton, Michael R.] New York Univ, Dept Phys, Ctr Cosmol & Particle Phys, New York, NY 10003 USA. [Johnston, David E.] CALTECH, Dept Astron, Pasadena, CA 91125 USA. [Johnston, David E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [McKay, Timothy A.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA. [McKay, Timothy A.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [McKay, Timothy A.] Univ Michigan, Michigan Ctr Theoret Phys, Ann Arbor, MI 48109 USA. [Scranton, Ryan] Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA. [Wechsler, Risa H.] Stanford Univ, Stanford Linear Accelerator Ctr, Stanford, CA 94305 USA. [Wechsler, Risa H.] Stanford Univ, Dept Phys, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA. [Koester, Benjamin P.; Hansen, Sarah M.; Frieman, Joshua A.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Koester, Benjamin P.; Hansen, Sarah M.; Frieman, Joshua A.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Frieman, Joshua A.; Annis, James] Fermilab Natl Accelerator Lab, Batavia, IL 60510 USA. RP Sheldon, ES (reprint author), Brookhaven Natl Lab, Upton, NY 11973 USA. RI McKay, Timothy/C-1501-2009 OI McKay, Timothy/0000-0001-9036-6150 FU NSF [AST-0428465, AST-044327]; U.S. Department of Energy [DE-AC0298CH10886, FG0208ER41567] FX E. S. S. was supported by NSF grant AST-0428465 and the U.S. Department of Energy under contract No. DE-AC0298CH10886. B. P. K. and T. A. M. gratefully acknowledge support from NSF grant AST-044327 and the Michigan Center for Theoretical Physics. D. E. J. received partial support from the U. S. Department of Energy under contract number DE-FG0208ER41567. The research described in this paperwas performed in part at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. NR 63 TC 54 Z9 54 U1 1 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 1 PY 2009 VL 703 IS 2 BP 2232 EP 2248 DI 10.1088/0004-637X/703/2/2232 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 495XS UT WOS:000269929500088 ER PT J AU Abdo, AA Allen, BT Aune, T Berley, D Chen, C Christopher, GE DeYoung, T Dingus, BL Ellsworth, RW Gonzalez, MM Goodman, JA Hays, E Hoffman, CM Huentemeyer, PH Kolterman, BE Linnemann, JT McEnery, JE Morgan, T Mincer, AI Nemethy, P Pretz, J Ryan, JM Parkinson, PMS Shoup, A Sinnis, G Smith, AJ Vasileiou, V Walker, GP Williams, DA Yodh, GB AF Abdo, A. A. Allen, B. T. Aune, T. Berley, D. Chen, C. Christopher, G. E. DeYoung, T. Dingus, B. L. Ellsworth, R. W. Gonzalez, M. M. Goodman, J. A. Hays, E. Hoffman, C. M. Huentemeyer, P. H. Kolterman, B. E. Linnemann, J. T. McEnery, J. E. Morgan, T. Mincer, A. I. Nemethy, P. Pretz, J. Ryan, J. M. Parkinson, P. M. Saz Shoup, A. Sinnis, G. Smith, A. J. Vasileiou, V. Walker, G. P. Williams, D. A. Yodh, G. B. TI MILAGRO OBSERVATIONS OF MULTI-TeV EMISSION FROM GALACTIC SOURCES IN THE FERMI BRIGHT SOURCE LIST (vol 700, pg L127, 2009) SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Correction C1 [Abdo, A. A.; Linnemann, J. T.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. [Allen, B. T.; Chen, C.; Yodh, G. B.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. [Aune, T.; Parkinson, P. M. Saz; Williams, D. A.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA. [Berley, D.; Goodman, J. A.; Smith, A. J.; Vasileiou, V.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA. [Christopher, G. E.; Kolterman, B. E.; Mincer, A. I.; Nemethy, P.] New York Univ, Dept Phys, New York, NY 10003 USA. [DeYoung, T.] Penn State Univ, Dept Phys, University Pk, PA 16802 USA. [Dingus, B. L.; Hoffman, C. M.; Pretz, J.; Sinnis, G.; Walker, G. P.] Los Alamos Natl Lab, Grp P 23, Los Alamos, NM 87545 USA. [Ellsworth, R. W.] George Mason Univ, Dept Phys & Astron, Fairfax, VA 22030 USA. [Gonzalez, M. M.] Univ Nacl Autonoma Mexico, Inst Astron, Mexico City 04510, DF, Mexico. [Hays, E.; McEnery, J. E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Huentemeyer, P. H.] Univ Utah, Dept Phys, Salt Lake City, UT 84112 USA. [Ryan, J. M.] Univ New Hampshire, Dept Phys, Durham, NH 03824 USA. [Shoup, A.] Ohio State Univ, Lima, OH 45804 USA. [Vasileiou, V.] NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA. [Vasileiou, V.] Univ Maryland, Baltimore, MD 21250 USA. RP Abdo, AA (reprint author), USN, Res Lab, Div Space Sci, Washington, DC 20375 USA. RI McEnery, Julie/D-6612-2012; Hays, Elizabeth/D-3257-2012 NR 1 TC 3 Z9 3 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD OCT 1 PY 2009 VL 703 IS 2 BP L185 EP L185 DI 10.1088/0004-637X/703/2/L185 PG 1 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 496XV UT WOS:000270014600021 ER PT J AU Krimm, HA Markwardt, CB Deloye, CJ Romano, P Chakrabarty, D Campana, S Cummings, JC Galloway, DK Gehrels, N Hartman, JM Kaaret, P Morgan, EH Tueller, J AF Krimm, H. A. Markwardt, C. B. Deloye, C. J. Romano, P. Chakrabarty, D. Campana, S. Cummings, J. C. Galloway, D. K. Gehrels, N. Hartman, J. M. Kaaret, P. Morgan, E. H. Tueller, J. TI DISCOVERY OF THE ACCRETION-POWERED MILLISECOND PULSAR SWIFT J1756.9-2508 WITH A LOW-MASS COMPANION (vol 668, pg L147, 2007) SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Correction C1 [Krimm, H. A.; Markwardt, C. B.; Cummings, J. C.] CRESST, Greenbelt, MD 20771 USA. [Krimm, H. A.; Markwardt, C. B.; Cummings, J. C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Krimm, H. A.] Univ Space Res Assoc, Columbia, MD 21044 USA. [Markwardt, C. B.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Deloye, C. J.] Northwestern Univ, Dept Phys & Astron, Evanston, IL 60208 USA. [Romano, P.] INAF IASF Palermo, I-90146 Palermo, Italy. [Chakrabarty, D.; Hartman, J. M.; Morgan, E. H.] MIT, Dept Phys, Cambridge, MA 02139 USA. [Chakrabarty, D.; Hartman, J. M.; Morgan, E. H.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Campana, S.] INAF Osservatorio Astron Brera, I-23807 Merate, LC, Italy. [Cummings, J. C.] Univ Maryland, Joint Ctr Astrophys, Baltimore, MD 21250 USA. [Galloway, D. K.] Monash Univ, Ctr Stellar & Planetary Astrophys, Clayton, Vic 3800, Australia. [Gehrels, N.; Tueller, J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Kaaret, P.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. RP Krimm, HA (reprint author), CRESST, Greenbelt, MD 20771 USA. RI Gehrels, Neil/D-2971-2012; Tueller, Jack/D-5334-2012 NR 1 TC 1 Z9 1 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD OCT 1 PY 2009 VL 703 IS 2 BP L183 EP L183 DI 10.1088/0004-637X/703/2/L183 PG 1 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 496XV UT WOS:000270014600019 ER PT J AU Isaksen, ISA Granier, C Myhre, G Berntsen, TK Dalsoren, SB Gauss, M Klimont, Z Benestad, R Bousquet, P Collins, W Cox, T Eyring, V Fowler, D Fuzzi, S Jockel, P Laj, P Lohmann, U Maione, M Monks, P Prevot, ASH Raes, F Richter, A Rognerud, B Schulz, M Shindell, D Stevenson, DS Storelvmo, T Wang, WC van Weele, M Wild, M Wuebbles, D AF Isaksen, I. S. A. Granier, C. Myhre, G. Berntsen, T. K. Dalsoren, S. B. Gauss, M. Klimont, Z. Benestad, R. Bousquet, P. Collins, W. Cox, T. Eyring, V. Fowler, D. Fuzzi, S. Joeckel, P. Laj, P. Lohmann, U. Maione, M. Monks, P. Prevot, A. S. H. Raes, F. Richter, A. Rognerud, B. Schulz, M. Shindell, D. Stevenson, D. S. Storelvmo, T. Wang, W. -C. van Weele, M. Wild, M. Wuebbles, D. TI Atmospheric composition change: Climate-Chemistry interactions SO ATMOSPHERIC ENVIRONMENT LA English DT Review DE Atmosphere climate chemistry; Feedbacks modelling ID GENERAL-CIRCULATION MODEL; SECONDARY ORGANIC AEROSOL; CLOUD CONDENSATION NUCLEI; AIR-POLLUTION TRANSPORT; 11-YEAR SOLAR-CYCLE; MIXED-PHASE CLOUDS; TROPOSPHERIC OZONE; COSMIC-RAYS; CARBONACEOUS PARTICLES; SATELLITE MEASUREMENTS AB Chemically active climate compounds are either primary compounds like methane (CH4), removed by oxidation in the atmosphere, or secondary compounds like ozone (O-3), sulfate and organic aerosols, both formed and removed in the atmosphere. Man-induced climate-chemistry interaction is a two-way process: Emissions of pollutants change the atmospheric composition contributing to climate change through the aforementioned climate components, and climate change, through changes in temperature, dynamics, the hydrological cycle, atmospheric stability, and biosphere-atmosphere interactions, affects the atmospheric composition and oxidation processes in the troposphere. Here we present progress in our understanding of processes of importance for climate-chemistry interactions, and their contributions to changes in atmospheric composition and climate forcing. A key factor is the oxidation potential involving compounds like O-3 and the hydroxyl radical (OH). Reported studies represent both current and future changes. Reported results include new estimates of radiative forcing based on extensive model studies of chemically active climate compounds like O-3, and of particles inducing both direct and indirect effects. Through EU projects like ACCENT, QUANTIFY, and the AeroCom project, extensive studies on regional and sector-wise differences in the impact on atmospheric distribution are performed. Studies have shown that land-based emissions have a different effect on climate than ship and aircraft emissions, and different measures are needed to reduce the climate impact. Several areas where climate change can affect the tropospheric oxidation process and the chemical composition are identified. This can take place through enhanced stratospheric-tropospheric exchange of ozone, more frequent periods with stable conditions favoring pollution build up over industrial areas, enhanced temperature induced biogenic emissions, methane releases from permafrost thawing, and enhanced concentration through reduced biospheric uptake. During the last 5-10 years, new observational data have been made available and used for model validation and the study of atmospheric processes. Although there are significant uncertainties in the modeling of composition changes, access to new observational data has improved modeling capability. Emission scenarios for the coming decades have a large uncertainty range, in particular with respect to regional trends, leading to a significant uncertainty range in estimated regional composition changes and climate impact. (C) 2009 Elsevier Ltd. All rights reserved. C1 [Isaksen, I. S. A.; Myhre, G.; Berntsen, T. K.; Dalsoren, S. B.; Rognerud, B.] Univ Oslo, Dept Geosci, Oslo, Norway. [Isaksen, I. S. A.; Myhre, G.; Berntsen, T. K.; Dalsoren, S. B.] CICERO, Oslo, Norway. [Granier, C.] Univ Paris 06, UMR7620, Paris, France. [Granier, C.] CNRS, Serv Aeron, UMR7620, Paris, France. [Granier, C.] NOAA, Div Chem Sci, Earth Syst Res Lab, Boulder, CO USA. [Granier, C.] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO USA. [Gauss, M.; Benestad, R.] Norwegian Meteorol Inst, Oslo, Norway. [Klimont, Z.] Int Inst Appl Syst Anal, A-2361 Laxenburg, Austria. [Bousquet, P.] Inst Pierre Simon Laplace, Serv Aeron, Paris, France. [Collins, W.] Met Off, Hadley Ctr, Exeter, Devon, England. [Cox, T.] Univ Cambridge, Ctr Atmospher Sci, Cambridge, England. [Eyring, V.] Inst Phys Atmosphare, Deutsch Zent Luft & Raumfahrt, D-82234 Wessling, Germany. [Fowler, D.] Ctr Ecol & Hydrol, Penicuik EH26 0QB, Midlothian, Scotland. [Fuzzi, S.] CNR, Inst Sci Amtosfera & Clima, I-40126 Bologna, Italy. [Joeckel, P.] Max Planck Inst Chem, D-55128 Mainz, Germany. [Laj, P.] Univ Blaise Pascal, Lab Meteorol Phys, Observ Phys Globe Clermont Ferrand, CNRS, F-63177 Clermont Ferrand, France. [Laj, P.] Univ Grenoble 1, CNRS, Lab Glaciol & Geophys Environm, F-38400 St Martin Dheres, France. [Lohmann, U.; Storelvmo, T.; Wild, M.] ETH, Inst Atmospher & Climate Sci, Zurich, Switzerland. [Maione, M.] Univ Urbino, Ist Sci Chim T Bruner, I-61029 Urbino, Italy. [Monks, P.] Univ Leicester, Dept Chem, Leicester LE1 7RH, Leics, England. [Prevot, A. S. H.] Paul Scherrer Inst, Lab Atmospher Chem, Villigen, Switzerland. [Raes, F.] European Commiss Joint Res Ctr, Inst Environm, Ispra, Italy. [Richter, A.] Univ Bremen, Inst Environm Phys, Bremen, Germany. [Schulz, M.] CEA, CNRS, LSCE, F-91198 Gif Sur Yvette, France. [Shindell, D.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Stevenson, D. S.] Univ Edinburgh, Sch Geosci, Edinburgh, Midlothian, Scotland. [Wang, W. -C.] SUNY Albany, Atmospher Sci Res Ctr, Albany, NY 12222 USA. [van Weele, M.] Royal Netherlands Meteorol Inst, Sect Atmospher Composit, NL-3730 AE De Bilt, Netherlands. [Wuebbles, D.] Univ Illinois, Dept Atmospher Sci, Urbana, IL 61801 USA. RP Isaksen, ISA (reprint author), Univ Oslo, Dept Geosci, Oslo, Norway. EM ivar.isaksen@geo.uio.no RI Prevot, Andre/C-6677-2008; Fuzzi, Sandro/F-2675-2010; Jockel, Patrick/C-3687-2009; Shindell, Drew/D-4636-2012; Wild, Martin/J-8977-2012; Granier, Claire/D-5360-2013; Lohmann, Ulrike/B-6153-2009; Schulz, Michael/A-6930-2011; Collins, William/A-5895-2010; fowler, david/B-5446-2010; Myhre, Gunnar/A-3598-2008; Richter, Andreas/C-4971-2008; Stevenson, David/C-8089-2012; Klimont, Zbigniew/P-7641-2015; Monks, Paul/H-6468-2016; Eyring, Veronika/O-9999-2016; Manager, CSD Publications/B-2789-2015; OI Prevot, Andre/0000-0002-9243-8194; Fuzzi, Sandro/0000-0002-5275-2381; Jockel, Patrick/0000-0002-8964-1394; Granier, Claire/0000-0001-7344-7995; Lohmann, Ulrike/0000-0001-8885-3785; Schulz, Michael/0000-0003-4493-4158; Collins, William/0000-0002-7419-0850; fowler, david/0000-0002-2999-2627; Myhre, Gunnar/0000-0002-4309-476X; Richter, Andreas/0000-0003-3339-212X; Stevenson, David/0000-0002-4745-5673; Klimont, Zbigniew/0000-0003-2630-198X; Monks, Paul/0000-0001-9984-4390; Eyring, Veronika/0000-0002-6887-4885; Rognerud, Bjorg/0000-0001-5958-4547 FU EU; ACCENT FX Significant parts of the work reported in this article are based on studies performed in the EU projects ACCENT, ATTICA, QUANTIFY, EUCAARI and HYMN. We are thankful to Dr. Corinna Hoose for making Fig. 28 available and to Dr. Keith Shine for valuable discussions and for his contribution to the article. We are thankful to the ACCENT project office for their support in the preparation of the article. NR 437 TC 112 Z9 115 U1 11 U2 134 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 OCT PY 2009 VL 43 IS 33 SI SI BP 5138 EP 5192 DI 10.1016/j.atmosenv.2009.08.003 PG 55 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA 517FL UT WOS:000271598500003 ER PT J AU Wang, DH Li, X Tao, WK Wang, Y AF Wang, Donghai Li, Xiaofan Tao, Wei-Kuo Wang, Yuan TI Effects of vertical wind shear on convective development during a landfall of severe tropical storm Bilis (2006) SO ATMOSPHERIC RESEARCH LA English DT Article DE Vertical wind shear; Perturbation kinetic energy; Cloud-resolving model simulation ID CLOUD-RESOLVING MODEL; SQUALL LINES; MICROSCALE STRUCTURE; MESOSCALE PROCESSES; FRONTAL RAINBANDS; SIMULATIONS; RADIATION; SYSTEMS; PARAMETERIZATION; PRECIPITATION AB Effects of vertical wind shear on convective development during the landfall of tropical storm Bilis (2006) are investigated with a pair of sensitivity experiments using a two-dimensional cloud-resolving model. The validated simulation data from Wang et al. [Wang, D., Li, X., Tao, W.-K., Liu, Y., Zhou, H., 2009: Torrential rainfall processes associated with a landfall of severe tropical storm Bilis (2006): A two-dimensional cloud-resolving modeling study. Atmos. Res., 91, 94-104.] are used as the control experiment. The difference between the control and sensitivity experiments is that vertically varying zonal winds in the control experiment are replaced by their mass-weighted means in the sensitivity experiment. The imposed vertical velocity with ascending motion in the upper troposphere and descending motion in the lower troposphere is responsible for dominant stratiform rainfall on 15 July. The vertical wind shear does not have important impacts on development of stratiform rainfall. One day later, imposed upward motion extends to the lower troposphere. The inclusion of negative vertical wind shear produces well-organized convection and strong convective rainfall because it causes kinetic energy transfer from large-scale forcing to perturbation circulations. (C) 2009 Elsevier B.V. All rights reserved. C1 [Wang, Donghai] Chinese Acad Meteorol Sci, State Key Lab Severe Weather, Beijing, Peoples R China. [Wang, Donghai] Sci Syst & Applicat Inc, Lanham, MD USA. [Li, Xiaofan] NOAA, NESDIS, Off Res & Applicat, Camp Springs, MD USA. [Tao, Wei-Kuo] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Wang, Yuan] Nanjing Univ, Key Lab Mesoscale Severe Weather, Minist Educ, Dept Atmospher Sci, Nanjing 210008, Peoples R China. RP Wang, DH (reprint author), Chinese Acad Meteorol Sci, State Key Lab Severe Weather, Beijing, Peoples R China. EM d.wang@hotmail.com RI Li, Xiaofan/F-5605-2010; Li, Xiaofan/G-2094-2014 FU State Key Basic Research Development Program [2009CB421504, 2004CB418300]; National Natural Science Foundation [40633016, 40830958] FX The authors thank two anonymous reviewers for their constructive comments. This research was supported by the State Key Basic Research Development Program (2009CB421504 and 2004CB418300), and the National Natural Science Foundation under the Grant Nos. 40633016 and 40830958. NR 46 TC 21 Z9 22 U1 0 U2 8 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0169-8095 J9 ATMOS RES JI Atmos. Res. PD OCT PY 2009 VL 94 IS 2 BP 270 EP 275 DI 10.1016/j.atmosres.2009.06.004 PG 6 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 498EI UT WOS:000270119400011 ER PT J AU Cavanagh, PR Gopalakrishnan, R Rice, AJ Genc, KO Maender, CC Nystrom, PG Johnson, MJ Kuklis, MM Humphreys, BT AF Cavanagh, Peter R. Gopalakrishnan, Raghavan Rice, Andrea J. Genc, Kerim O. Maender, Christian C. Nystrom, Peter G. Johnson, Micah J. Kuklis, Matthew M. Humphreys, Bradley T. TI An Ambulatory Biomechanical Data Collection System for Use in Space: Design and Validation SO AVIATION SPACE AND ENVIRONMENTAL MEDICINE LA English DT Article DE Spaceflight; foot forces; joint angles; EMG; biomechanics ID LONG-DURATION SPACEFLIGHT; WEIGHT-BEARING; MICROGRAVITY; WALKING; GAIT; COUNTERMEASURES; ADAPTATIONS; DISEASE; FORCES; MOTION AB CAVANAGH PR, GOPALAKRISHNAN R, RICE AJ, GENC KO, MAENDER CC, NYSTROM PG, JOHNSON MJ, KUKLIS MM, HUMPHREYS BT. An ambulatory biomechanical data collection system for use in space: design and validation. Aviat Space Environ Med 2009; 80:870-81. Introduction: Loss in bone mineral density and muscle strength in astronauts following long-duration spaceflight have been well documented, but the altered force and movement environments in microgravity which may contribute to these changes have not been well characterized. This paper describes the instrumentation, software, and data collection procedures developed for the "Foot" experiment that was conducted on the International Space Station (ISS) to provide insight into the biomechanics of daily activity in a microgravity environment. Methods: The instrumentation used for data collection included the Ambulatory Data Acquisition System (ADAS), ADAS electromyography (EMG) modules, the Joint Excursion System, and the Total Force-Foot Ground interface system, which were all integrated into a specially designed Lower Extremity Monitoring Suit. There were 14 total channels of data that were collected at sampling rates between 8 Hz and 1024 Hz, including 7 channels of EMG, 4 channels of joint angle data, 2 channels of in-shoe ground reaction force, and a marker channel for event recording. Data were typically collected for between 6.5 and 11.8 h of activity during 4 d on Earth and 4-7 d in flight. Results: Exemplar data sets collected preflight on astronauts in 1 g to validate the instrumentation are presented. Discussion: We conclude that the system provides valid and useful biomechanical information on long-term activity. The analysis of data collected on-orbit using the system described here will be presented in a series of future papers characterizing the biomechanics of astronaut activity during complete working days on the Earth and on the ISS. C1 [Cavanagh, Peter R.; Rice, Andrea J.; Genc, Kerim O.] Univ Washington, Dept Orthoped & Sports Med, Seattle, WA 98195 USA. [Gopalakrishnan, Raghavan; Kuklis, Matthew M.] Cleveland Clin, Dept Biomed Engn, Cleveland, OH 44106 USA. [Genc, Kerim O.] Case Western Reserve Univ, Dept Biomed Engn, Cleveland, OH 44106 USA. [Maender, Christian C.; Nystrom, Peter G.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Johnson, Micah J.] Lockheed Martin, Houston, TX USA. [Humphreys, Bradley T.] ZIN Technol Inc, Brookpark, OH USA. RP Cavanagh, PR (reprint author), Univ Washington, Dept Orthoped & Sports Med, BB 1065D,1959 NE Pacific St,Box 36500, Seattle, WA 98195 USA. EM cavanagh@u.washington.edu RI Gopalakrishnan, Raghavan/F-1213-2015 OI Gopalakrishnan, Raghavan/0000-0002-9038-9392 FU NASA [NCC 9 153] FX This work was supported by NASA cooperative agreement NCC 9 153. The remarkable cooperation of the subjects is acknowledged. We are also grateful to the many individuals at Penn State University, the Cleveland Clinic, NASA Johnson Space Center, Lockheed Martin, Wyle Laboratories, and Baylor College of Medicine who made this experiment possible. NR 38 TC 6 Z9 6 U1 0 U2 6 PU AEROSPACE MEDICAL ASSOC PI ALEXANDRIA PA 320 S HENRY ST, ALEXANDRIA, VA 22314-3579 USA SN 0095-6562 J9 AVIAT SPACE ENVIR MD JI Aviat. Space Environ. Med. PD OCT PY 2009 VL 80 IS 10 BP 870 EP 881 DI 10.3357/ASEM.2266.2009 PG 12 WC Public, Environmental & Occupational Health; Medicine, General & Internal; Sport Sciences SC Public, Environmental & Occupational Health; General & Internal Medicine; Sport Sciences GA 501ZD UT WOS:000270422500006 PM 19817239 ER PT J AU Everett, ME O'Connor, DP DeWitt, JK AF Everett, Meghan E. O'Connor, Daniel P. DeWitt, John K. TI Lower Limb Position During Treadmill Jogging and Fast Running in Microgravity SO AVIATION SPACE AND ENVIRONMENTAL MEDICINE LA English DT Article DE microgravity; locomotion; kinematics AB EVERETT ME, O'CONNOR DP, DEWITT JK. Lower limb position during treadmill jogging and fast running in microgravity. Aviat Space Environ Med 2009; 80:882-6. Introduction: The second-generation ISS treadmill has a faster maximum operating speed than the current ISS treadmill. In normal gravity (1 G), bone loading benefits and cardiorespiratory stress are directly related to locomotion speed. A kinematic comparison of locomotion between 1 G and microgravity will provide information to evaluate the potential efficacy of fast running as an in-flight exercise countermeasure. Methods: Subjects exercised on a treadmill at 3.13 m . s(-1) (8.5 min . mi(-1)) (JOG; N = 6) and 5.36 m . s(-1) (5 min . mi(-1)) (RUN; N = 5) in microgravity during parabolic flight and in 1 G. During microgravity trials, subjects performed locomotion using a subject loading system (in a configuration identical to ISS) with similar to 80% bodyweight loading. Kinematic analyses of joint position at heel strike were performed using video software. Results: During the JOG trials, differences were found in thigh angle (microgravity = 54.09 degrees +/- 4.87; 1 G = 64.04 degrees +/- 3.12, mean +/- SD) and knee angle (microgravity = 33.17 degrees +/- 8.68; 1 G = 21.28 degrees +/- 5.22), indicating a more squatted position at heel strike in microgravity. No kinematic differences were found during the RUN condition. Discussion: The subject loading system and decreased external load throughout the stride in microgravity may account for the observed kinematic differences during JOG. The kinematic compensations for microgravity during JOG may result in in-flight adaptations that are different from expected based on 1-G studies. However, similar kinematics between gravity conditions during RUN suggest in-flight training may provide benefits similar to 1 G. C1 [Everett, Meghan E.; DeWitt, John K.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Everett, Meghan E.; O'Connor, Daniel P.] Univ Houston, Houston, TX USA. RP Everett, ME (reprint author), Wyle Hac 2611,1290 Hercules Ave, Houston, TX 77058 USA. EM Meghan.e.everet@nasa.gov NR 12 TC 5 Z9 5 U1 0 U2 2 PU AEROSPACE MEDICAL ASSOC PI ALEXANDRIA PA 320 S HENRY ST, ALEXANDRIA, VA 22314-3579 USA SN 0095-6562 J9 AVIAT SPACE ENVIR MD JI Aviat. Space Environ. Med. PD OCT PY 2009 VL 80 IS 10 BP 882 EP 886 DI 10.3357/ASEM.2414.2009 PG 5 WC Public, Environmental & Occupational Health; Medicine, General & Internal; Sport Sciences SC Public, Environmental & Occupational Health; General & Internal Medicine; Sport Sciences GA 501ZD UT WOS:000270422500007 PM 19817240 ER PT J AU Stothers, R AF Stothers, Richard TI ANCIENT METEOROLOGICAL OPTICS SO CLASSICAL JOURNAL LA English DT Article AB Presocratic, Peripatetic, Epicurean and Stoic theories that aimed to explain Aristotle's four fundamental phenomena of meteorological optics are compared with one another and with modern theories. Notable recorded instances of these and associated phenomena are cataloged. Aristotle's streak, Octavian's halo, Vitellius' antisun and Constantine's and Cyril's crosses are identified. C1 [Stothers, Richard] NASA, Washington, DC 20546 USA. RP Stothers, R (reprint author), NASA, Washington, DC 20546 USA. NR 39 TC 3 Z9 3 U1 0 U2 0 PU CLASSICAL ASSOC MIDDLE WEST SOUTH, INC PI ASHLAND PA PO BOX 5005, RANDOLPH-MACON COLL, ASHLAND, VA 23005-5505 USA SN 0009-8353 EI 2327-5812 J9 CLASSICAL J JI Class. J. PD OCT-NOV PY 2009 VL 105 IS 1 BP 27 EP 42 PG 16 WC Classics SC Classics GA V45HV UT WOS:000209808600003 ER PT J AU Scaife, AA Kucharski, F Folland, CK Kinter, J Bronnimann, S Fereday, D Fischer, AM Grainger, S Jin, EK Kang, IS Knight, JR Kusunoki, S Lau, NC Nath, MJ Nakaegawa, T Pegion, P Schubert, S Sporyshev, P Syktus, J Yoon, JH Zeng, N Zhou, T AF Scaife, A. A. Kucharski, F. Folland, C. K. Kinter, J. Broennimann, S. Fereday, D. Fischer, A. M. Grainger, S. Jin, E. K. Kang, I. S. Knight, J. R. Kusunoki, S. Lau, N. C. Nath, M. J. Nakaegawa, T. Pegion, P. Schubert, S. Sporyshev, P. Syktus, J. Yoon, J. H. Zeng, N. Zhou, T. TI The CLIVAR C20C project: selected twentieth century climate events SO CLIMATE DYNAMICS LA English DT Article DE CLIVAR Climate of the twentieth century project; Climate sensitivity; Southern Oscillation; Sahel rainfall; North Atlantic Oscillation; Atmospheric models; Model evaluation; Regional climate ID SEA-SURFACE TEMPERATURE; NORTH-ATLANTIC OSCILLATION; ATMOSPHERIC GENERAL-CIRCULATION; SAHEL RAINFALL; MODELS; VARIABILITY; SIMULATIONS; UNCERTAINTY; PREDICTIONS; PACIFIC AB We use a simple methodology to test whether a set of atmospheric climate models with prescribed radiative forcings and ocean surface conditions can reproduce twentieth century climate variability. Globally, rapid land surface warming since the 1970s is reproduced by some models but others warm too slowly. In the tropics, air-sea coupling allows models to reproduce the Southern Oscillation but its strength varies between models. We find a strong relationship between the Southern Oscillation in global temperature and the rate of global warming, which could in principle be used to identify models with realistic climate sensitivity. This relationship and a weak response to ENSO suggests weak sensitivity to changes in sea surface temperature in some of the models used here. In the tropics, most models reproduce part of the observed Sahel drought. In the extratropics, models do not reproduce the observed increase in the North Atlantic Oscillation in response to forcings, through internal variability, or as a combination of both. C1 [Scaife, A. A.; Folland, C. K.; Fereday, D.; Knight, J. R.] Met Off, Hadley Ctr, Exeter, Devon, England. [Kucharski, F.] Earth Syst Phys Sect, Abdus Salam Int Ctr Theoret Phys, Trieste, Italy. [Kinter, J.; Jin, E. K.] Ctr Ocean Land Atmosphere Studies, Fairfax, VA USA. [Kinter, J.; Jin, E. K.] George Mason Univ, Fairfax, VA 22030 USA. [Broennimann, S.; Fischer, A. M.] ETH, Inst Atmospher & Climate Sci, Zurich, Switzerland. [Grainger, S.] Ctr Australian Weather & Climate Res, Melbourne, Vic, Australia. [Kang, I. S.] Seoul Natl Univ, Sch Earth Environm Sci, Seoul, South Korea. [Kusunoki, S.; Nakaegawa, T.] Japan Meteorol Agcy, Meteorol Res Inst, Tokyo, Japan. [Lau, N. C.; Nath, M. J.] Geophys Fluid Dynam Lab, Princeton, NJ USA. [Pegion, P.; Schubert, S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Sporyshev, P.] Voeikov Main Geophys Observ, St Petersburg, Russia. [Yoon, J. H.; Zeng, N.] Univ Maryland, Baltimore, MD 21201 USA. [Zhou, T.] Inst Atmospher Sci, LASG, Beijing, Peoples R China. RP Scaife, AA (reprint author), Met Off, Hadley Ctr, Exeter, Devon, England. EM adam.scaife@metoffice.gov.uk RI ZHOU, Tianjun/C-3195-2012; Bronnimann, Stefan/A-5737-2008; Syktus, Jozef/E-7173-2011; Pegion, Philip/E-5247-2012; Zeng, Ning/A-3130-2008; Folland, Chris/I-2524-2013; YOON, JIN-HO/A-1672-2009; Sporyshev, Petr/P-7323-2015; 안, 민섭/D-9972-2015 OI ZHOU, Tianjun/0000-0002-5829-7279; Bronnimann, Stefan/0000-0001-9502-7991; Syktus, Jozef/0000-0003-1782-3073; Zeng, Ning/0000-0002-7489-7629; YOON, JIN-HO/0000-0002-4939-8078; Sporyshev, Petr/0000-0002-4047-8178; FU UK Met Office's Hadley Centre [GA01101, CBC/2B/0417]; NSF [0332910]; NOAA [NA04OAR4310034]; NASA [NNG04GG46G]; Russian Foundation; Australian Climate Change Science Program of the Australian Greenhouse Office; ETH Zurich [PP-1/04-1] FX This work contributes to the CLIVAR Climate of the twentieth Century project: http://www.iges.org/c20c/home.html and was carried out with support from the UK Met Office's Hadley Centre climate research program: joint Defra and MoD Programme, (Defra) GA01101 (MoD) CBC/2B/0417 Annex C5. We thank Dr J. Murphy for useful comments and Drs B. Booth, M. Collins and G. Harris for coupled ocean atmosphere data from the Hadley Centre model and Dr D. Rowell for the Sahel rainfall data. J. Kinter and K. Jin were supported by research grants from NSF ( 0332910), NOAA (NA04OAR4310034) and NASA (NNG04GG46G). P. Sporyshev was supported by the Russian Foundation for Basic Research. S. Grainger was supported by the Australian Climate Change Science Program of the Australian Greenhouse Office. The development and maintenance of CCM SOCOL was funded by ETH Zurich grant PP-1/04-1. NR 66 TC 58 Z9 65 U1 1 U2 14 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 OCT PY 2009 VL 33 IS 5 BP 603 EP 614 DI 10.1007/s00382-008-0451-1 PG 12 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 486IE UT WOS:000269188800002 ER PT J AU Kucharski, F Scaife, AA Yoo, JH Folland, CK Kinter, J Knight, J Fereday, D Fischer, AM Jin, EK Kroger, J Lau, NC Nakaegawa, T Nath, MJ Pegion, P Rozanov, E Schubert, S Sporyshev, PV Syktus, J Voldoire, A Yoon, JH Zeng, N Zhou, T AF Kucharski, F. Scaife, A. A. Yoo, J. H. Folland, C. K. Kinter, J. Knight, J. Fereday, D. Fischer, A. M. Jin, E. K. Kroeger, J. Lau, N. -C. Nakaegawa, T. Nath, M. J. Pegion, P. Rozanov, E. Schubert, S. Sporyshev, P. V. Syktus, J. Voldoire, A. Yoon, J. H. Zeng, N. Zhou, T. TI The CLIVAR C20C project: skill of simulating Indian monsoon rainfall on interannual to decadal timescales. Does GHG forcing play a role? SO CLIMATE DYNAMICS LA English DT Article DE Climate variability; Multimodel ensembles; Indian monsoon; ENSO-monsoon relation; Interannual-to-decadal predictability ID ASIAN SUMMER MONSOON; ENSO RELATIONSHIP; AIR-TEMPERATURE; VARIABILITY; ATLANTIC AB The ability of atmospheric general circulation models (AGCMs), that are forced with observed sea surface temperatures (SSTs), to simulate the Indian monsoon rainfall (IMR) variability on interannual to decadal timescales is analyzed in a multimodel intercomparison. The multimodel ensemble has been performed within the CLIVAR International "Climate of the 20th Century" (C20C) Project. This paper is part of a C20C intercomparison of key climate time series. Whereas on the interannual timescale there is modest skill in reproducing the observed IMR variability, on decadal timescale the skill is much larger. It is shown that the decadal IMR variability is largely forced, most likely by tropical sea surface temperatures (SSTs), but as well by extratropical and especially Atlantic Multidecadal Oscillation (AMO) related SSTs. In particular there has been a decrease from the late 1950s to the 1990s that corresponds to a general warming of tropical SSTs. Using a selection of control integrations from the World Climate Research Programme's (WCRP's) Coupled Model Intercomparison Project phase 3 (CMIP3), it is shown that the increase of greenhouse gases (GHG) in the twentieth century has not significantly contributed to the observed decadal IMR variability. C1 [Kucharski, F.; Yoo, J. H.; Kroeger, J.] Abdus Salam Int Ctr Theoret Phys, Earth Syst Phys Sect, Trieste, Italy. [Scaife, A. A.; Folland, C. K.; Knight, J.; Fereday, D.] MOHC, Exeter, Devon, England. [Kinter, J.; Jin, E. K.] Ctr Ocean Land Atmosphere Studies, Calverton, MD USA. [Fischer, A. M.] ETH, Inst Atmospher & Climate Sci, Zurich, Switzerland. [Jin, E. K.] George Mason Univ, Fairfax, VA 22030 USA. [Lau, N. -C.; Nath, M. J.] Geophys Fluid Dynam Lab, Princeton, NJ USA. [Nakaegawa, T.] Japan Meteorol Agcy, Meteorol Res Inst, Tokyo, Japan. [Pegion, P.; Schubert, S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Rozanov, E.] World Radiat Ctr, Phys Meteorol Observ, Davos, Switzerland. [Sporyshev, P. V.] Voeikov Main Geophys Observ, St Petersburg, Russia. [Syktus, J.] Queensland Climate Change Ctr Excellence, Brisbane, Qld, Australia. [Voldoire, A.] Meteo France CNRS, CNRM GAME, Toulouse, France. [Yoon, J. H.; Zeng, N.] Univ Maryland, College Pk, MD 20742 USA. [Zhou, T.] LASG, Inst Atmospher Sci, Beijing, Peoples R China. RP Kucharski, F (reprint author), Abdus Salam Int Ctr Theoret Phys, Earth Syst Phys Sect, Trieste, Italy. EM kucharsk@ictp.it RI Syktus, Jozef/E-7173-2011; Pegion, Philip/E-5247-2012; Zeng, Ning/A-3130-2008; Folland, Chris/I-2524-2013; YOON, JIN-HO/A-1672-2009; Rozanov, Eugene/A-9857-2012; Sporyshev, Petr/P-7323-2015; ZHOU, Tianjun/C-3195-2012 OI Syktus, Jozef/0000-0003-1782-3073; Zeng, Ning/0000-0002-7489-7629; YOON, JIN-HO/0000-0002-4939-8078; Rozanov, Eugene/0000-0003-0479-4488; Sporyshev, Petr/0000-0002-4047-8178; ZHOU, Tianjun/0000-0002-5829-7279 FU Defra and MoD Integrated Climate Programme [GA01101, CBC/2B/0417]; NSF [0332910]; NOAA [NA04OAR4310034]; NASA [NNG04GG46G]; National Basic Research Program of China [2006CB403603]; European Commissions [GOCE-CT-2003-505539] FX A. Scaife and C. Folland were supported by the Defra and MoD Integrated Climate Programme-GA01101, CBC/2B/0417_Annex C5. J. Kinter and E. K. Jin were supported by research grants from NSF ( 0332910), NOAA (NA04OAR4310034) and NASA (NNG04GG46G). The MGO participation ( P. Sporyshev) was supported by the Russian Foundation for Basic Research. T. Zhou was supported by the National Basic Research Program of China under grant number 2006CB403603. J. Kroger and F. Kucharski were partially supported by the ENSEMBLES project funded by the European Commissions 6th Framework Programme, Contract GOCE-CT-2003-505539. We wish to thank Xunqiang Bi ( ICTP) for preparing the CMIP3 data and the two anonymous reviewers for their constructive comments that helped to improve the manuscript. NR 30 TC 34 Z9 38 U1 0 U2 9 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 OCT PY 2009 VL 33 IS 5 BP 615 EP 627 DI 10.1007/s00382-008-0462-y PG 13 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 486IE UT WOS:000269188800003 ER PT J AU Thrower, FP Hard, JJ AF Thrower, Frank P. Hard, Jeffrey J. TI Effects of a single event of close inbreeding on growth and survival in steelhead SO CONSERVATION GENETICS LA English DT Article DE Oncorhynchus mykiss; Inbreeding depression; Captive broodstock; Supplementation ID TROUT SALMO-GAIRDNERI; RAINBOW-TROUT; ONCORHYNCHUS-MYKISS; GENETIC-VARIATION; FRESH-WATER; CONSERVATION BIOLOGY; PACIFIC SALMON; DEPRESSION; POPULATIONS; EXTINCTION AB For two populations of Alaskan steelhead ( Oncorhynchus mykiss) of common ancestry we evaluated effects of inbreeding in second-generation descendants of wild fish by comparing progeny of full-sibling matings to those of non-inbred controls to determine if a single event of close inbreeding has significant effects on survival and growth in captivity or the wild. In captivity, both survival and size were highly variable between inbred and control types within each line and among the five broods during five periods of freshwater culture. However, no consistent patterns of inbreeding enhancement or depression between types within lines across years were evident. In contrast, in the wild marine environment, 34 of 34 pairwise comparisons between inbred and control types in body size of returning adults after 2 or 3 years at liberty in the ocean were consistent with inbreeding depression with significant inbreeding depression varying from 2.9% for female length to 20.0% for female weight. Survival of marked juveniles (smolts) to adults in the wild marine environment was consistently and significantly lower in inbred types for both lines, for an average inbreeding depression of 78.8%. The results underscore the potential problems that can arise from using protective culture technologies, including captive broodstocks, to supplement endangered populations, and they highlight the genetic hazards that can be faced by small wild populations. This study demonstrates that high natural mortality or selection increases the amount of inbreeding depression detected in survival. Inbreeding effects on survival and growth in captivity can be poor indicators of survival and growth in a wild marine environment. C1 [Thrower, Frank P.] Alaska Fisheries Sci Ctr, Auke Bay Labs, Natl Marine Fisheries Serv, Juneau, AK 99801 USA. [Hard, Jeffrey J.] NW Fisheries Sci Ctr, Conservat Biol Div, Natl Marine Fisheries Serv, Seattle, WA 98112 USA. RP Thrower, FP (reprint author), Alaska Fisheries Sci Ctr, Auke Bay Labs, Natl Marine Fisheries Serv, 17109 Pt Lena Loop Rd, Juneau, AK 99801 USA. EM Frank.Thrower@noaa.gov RI Hard, Jeffrey/C-7229-2009 FU Alaska Fisheries Science Center; Office of Protected Resources; NOAA Fisheries FX We thank all the personnel involved with this 10 year project at the Little Port Walter Marine Research Station, particularly Ty and Don Cummins, John Joyce, Adrian Celewycz, Bill Heard and Brad Weinlaeder, without whose help the research would not have been possible. This research was funded by the Alaska Fisheries Science Center and the Office of Protected Resources, NOAA Fisheries. NR 51 TC 16 Z9 16 U1 2 U2 20 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 1566-0621 EI 1572-9737 J9 CONSERV GENET JI Conserv. Genet. PD OCT PY 2009 VL 10 IS 5 BP 1299 EP 1307 DI 10.1007/s10592-008-9709-8 PG 9 WC Biodiversity Conservation; Genetics & Heredity SC Biodiversity & Conservation; Genetics & Heredity GA 505YF UT WOS:000270737400010 ER PT J AU Heckendorn, P Weisenstein, D Fueglistaler, S Luo, BP Rozanov, E Schraner, M Thomason, LW Peter, T AF Heckendorn, P. Weisenstein, D. Fueglistaler, S. Luo, B. P. Rozanov, E. Schraner, M. Thomason, L. W. Peter, T. TI The impact of geoengineering aerosols on stratospheric temperature and ozone SO ENVIRONMENTAL RESEARCH LETTERS LA English DT Article DE geoengineering; Mt Pinatubo eruption; ozone depletion; stratospheric aerosols; albedo ID CHEMISTRY-CLIMATE MODEL; PINATUBO VOLCANIC AEROSOL; GENERAL-CIRCULATION MODEL; MT-PINATUBO; 2-DIMENSIONAL MODEL; ANTARCTIC OZONE; POLAR VORTEX; DEPLETION; ERUPTION; SCHEMES AB Anthropogenic greenhouse gas emissions are warming the global climate at an unprecedented rate. Significant emission reductions will be required soon to avoid a rapid temperature rise. As a potential interim measure to avoid extreme temperature increase, it has been suggested that Earth's albedo be increased by artificially enhancing stratospheric sulfate aerosols. We use a 3D chemistry climate model, fed by aerosol size distributions from a zonal mean aerosol model, to simulate continuous injection of 1-10 Mt/a into the lower tropical stratosphere. In contrast to the case for all previous work, the particles are predicted to grow to larger sizes than are observed after volcanic eruptions. The reason is the continuous supply of sulfuric acid and hence freshly formed small aerosol particles, which enhance the formation of large aerosol particles by coagulation and, to a lesser extent, by condensation. Owing to their large size, these particles have a reduced albedo. Furthermore, their sedimentation results in a non-linear relationship between stratospheric aerosol burden and annual injection, leading to a reduction of the targeted cooling. More importantly, the sedimenting particles heat the tropical cold point tropopause and, hence, the stratospheric entry mixing ratio of H2O increases. Therefore, geoengineering by means of sulfate aerosols is predicted to accelerate the hydroxyl catalyzed ozone destruction cycles and cause a significant depletion of the ozone layer even though future halogen concentrations will be significantly reduced. C1 [Heckendorn, P.; Luo, B. P.; Rozanov, E.; Schraner, M.; Peter, T.] ETH, Inst Atmospher & Climate Sci, CH-8092 Zurich, Switzerland. [Weisenstein, D.] AER, Lexington, MA USA. [Fueglistaler, S.] Univ Cambridge, DAMTP, Cambridge CB2 1TN, England. [Rozanov, E.] PMOD WRC, Davos, Switzerland. [Thomason, L. W.] NASA, Langley Res Ctr, Hampton, VA 23665 USA. RP Heckendorn, P (reprint author), ETH, Inst Atmospher & Climate Sci, CH-8092 Zurich, Switzerland. EM patricia.heckendorn@env.ethz.ch RI Rozanov, Eugene/A-9857-2012; Fueglistaler, Stephan/I-5803-2013 OI Rozanov, Eugene/0000-0003-0479-4488; FU ETH Zurich; NASA; EU [SCOUT-O3] FX PK is funded by ETH Zurich (S-ENETH project TUMSS), DW by NASA ACMAP program, BPL by the EU project SCOUT-O3, MS and ER by the ETH Zurich Polyproject 'Variability of the Sun and Global Climate Phase I + II'. We would like to thank Andreas Fischer, Stefan Broennimann, Marco Giorgetta, Gera Stenchikov, Manu Thomas, Claudia Timmreck, Simone Tilmes and Sebastian Schmidt for helpful discussions. NR 59 TC 87 Z9 87 U1 5 U2 64 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 OCT-DEC PY 2009 VL 4 IS 4 AR 045108 DI 10.1088/1748-9326/4/4/045108 PG 12 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA 534ME UT WOS:000272900500053 ER PT J AU Rawlins, MA Serreze, MC Schroeder, R Zhang, XD McDonald, KC AF Rawlins, Michael A. Serreze, Mark C. Schroeder, Ronny Zhang, Xiangdong McDonald, Kyle C. TI Diagnosis of the record discharge of Arctic-draining Eurasian rivers in 2007 SO ENVIRONMENTAL RESEARCH LETTERS LA English DT Article DE SWE; river discharge; NAO; atmospheric circulation ID NORTH-ATLANTIC OSCILLATION; OCEAN; BASIN; PRECIPITATION; REANALYSIS; PERMAFROST; SIBERIA; SYSTEM; AIR AB Aggregate annual discharge from the six largest Arctic-draining Eurasian rivers achieved an all-time record high in 2007, accentuating a long-term upward trend that argues for intensification of the Arctic hydrologic cycle. This record discharge was due in part to strong positive anomalies in late winter snow water equivalent across much of northern Eurasia. These anomalies arose in response to an unusual pattern of atmospheric circulation in late 2006 and early 2007, characterized by an extreme northeastward extension of the Icelandic Low and a contraction of the Siberian High. Positive net precipitation anomalies then continued into summer, further contributing to discharge. C1 [Rawlins, Michael A.; Schroeder, Ronny; McDonald, Kyle C.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Serreze, Mark C.] Univ Colorado, Cooperat Inst Res Environm Sci, Natl Snow & Ice Data Ctr, Boulder, CO 80309 USA. [Zhang, Xiangdong] Univ Alaska Fairbanks, Int Arctic Res Ctr, Fairbanks, AK 99775 USA. RP Rawlins, MA (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM michael.rawlins@jpl.nasa.gov RI Zhang, Xiangdong/A-9711-2009 OI Zhang, Xiangdong/0000-0001-5893-2888 FU NASA; NSF [ARC-0531302, ARC-0805821] FX The NCEP-NCAR reanalysis data were obtained from the NOAA-ESRL Physical Sciences Division web site at http://www. cdc. noaa. gov/. The lead author was supported by a Fellowship from the NASA Postdoctoral Program, administered by Oak Ridge Associated Universities. This study was also supported by NSF grants ARC-0531302 and ARC-0805821. Portions of this work were carried out at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. NR 35 TC 19 Z9 20 U1 0 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 OCT-DEC PY 2009 VL 4 IS 4 AR 045011 DI 10.1088/1748-9326/4/4/045011 PG 7 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA 534ME UT WOS:000272900500028 ER PT J AU Tchebakova, NM Parfenova, E Soja, AJ AF Tchebakova, N. M. Parfenova, E. Soja, A. J. TI The effects of climate, permafrost and fire on vegetation change in Siberia in a changing climate SO ENVIRONMENTAL RESEARCH LETTERS LA English DT Article DE climate change; forest fire; permafrost; vegetation; Siberia ID NORTHERN EURASIA; BOREAL FOREST; MODEL; PARAMETERS AB Observations and general circulation model projections suggest significant temperature increases in Siberia this century that are expected to have profound effects on Siberian vegetation. Potential vegetation change across Siberia was modeled, coupling our Siberian BioClimatic Model with several Hadley Centre climate change scenarios for 2020, 2050 and 2080, with explicit consideration of permafrost and fire activity. In the warmer and drier climate projected by these scenarios, Siberian forests are predicted to decrease and shift northwards and forest-steppe and steppe ecosystems are predicted to dominate over half of Siberia due to the dryer climate by 2080. Despite the large predicted increases in warming, permafrost is not predicted to thaw deep enough to sustain dark (Pinus sibirica, Abies sibirica, and Picea obovata) taiga. Over eastern Siberia, larch (Larix dahurica) taiga is predicted to continue to be the dominant zonobiome because of its ability to withstand continuous permafrost. The model also predicts new temperate broadleaf forest and forest-steppe habitats by 2080. Potential fire danger evaluated with the annual number of high fire danger days (Nesterov index is 4000-10 000) is predicted to increase by 2080, especially in southern Siberia and central Yakutia. In a warming climate, fuel load accumulated due to replacement of forest by steppe together with frequent fire weather promotes high risks of large fires in southern Siberia and central Yakutia, where wild fires would create habitats for grasslands because the drier climate would no longer be suitable for forests. C1 [Tchebakova, N. M.; Parfenova, E.] Russian Acad Sci, Siberian Branch, VN Sukachev Inst Forest, Krasnoyarsk 660036, Russia. [Soja, A. J.] NASA Langley Res Ctr, NIA, Hampton, VA 23681 USA. RP Tchebakova, NM (reprint author), Russian Acad Sci, Siberian Branch, VN Sukachev Inst Forest, Krasnoyarsk 660036, Russia. EM ncheby@forest.akadem.ru; Amber.J.Soja@nasa.gov NR 49 TC 65 Z9 68 U1 6 U2 58 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 OCT-DEC PY 2009 VL 4 IS 4 AR 045013 DI 10.1088/1748-9326/4/4/045013 PG 9 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA 534ME UT WOS:000272900500030 ER PT J AU Kibanova, D Nieto-Camacho, A Cervini-Silva, J AF Kibanova, Daria Nieto-Camacho, Antonio Cervini-Silva, Javiera TI Lipid Peroxidation Induced by Expandable Clay Minerals SO ENVIRONMENTAL SCIENCE & TECHNOLOGY LA English DT Article ID OXIDATIVE STRESS; DIOCTAHEDRAL SMECTITES; RAT-BRAIN; ACID; CHEMISTRY; IRON; NONTRONITES; PARTICLES; MECHANISM; ELEMENTS AB Small-sized environmental particles such as 2:1 phyllosilicates induce oxidative stress, a primary indicator of cell damage and toxicity. Herein, potential hazards of clay particle uptake are addressed. This paper reports that the content and distribution of structural Fe influence the ability of expandable clay minerals to induce lipid peroxidation (LP), a major indicator of oxidative stress, in biological matrices. Three smectite clays, hectorite (SHCa-1) and two nontronites (NAu-1) and (NAu-2) containing varying total content and coordination environment of structural Fe, were selected. Screening and monitoring of LP was conducted using a thiobarbituric acid reactive substances (TBARS) assay, The higher content of TBARS in nontronites than that in SHCa-1 suspensions was explained because structural Fe contributes to LP. The observed lack of correlation between TBARS content and the extent of Fe dissolution indicated that the formation of TBARS is surface controlled. Results showing a high TBARS content in SHCa-1 but not in nontronite supernatant solutions was explained because the former contains distinct soluble chemical component(s) that could (i) induce LP by its (their) own right and (ii) whose chemical affinity for organic ligands used as inhibitors is weak. Clays serve as stronger inductors than 2,2'-azobis(2-amidinopropane) dihydrochloride (AAPH) but are much weaker than FeSO4. The outcome of this work shows that LP is clay surface-controlled and dependent on clay structural composition. C1 [Cervini-Silva, Javiera] Univ Autonoma Metropolitana, Unidad Cuajimalpa UAM C, Dept Proc & Technol, Div Ciencias Nat & Ingn, Mexico City 01120, DF, Mexico. [Kibanova, Daria] Univ Nacl Autonoma Mexico, Fac Quim, Mexico City 04510, DF, Mexico. [Nieto-Camacho, Antonio] Univ Nacl Autonoma Mexico, Inst Quim, Mexico City 04510, DF, Mexico. [Cervini-Silva, Javiera] NASA, Astrobiol Inst, Berkeley, CA 94720 USA. [Cervini-Silva, Javiera] Univ Calif Berkeley, Lawrence Berkeley Lab, Div Earth Sci, Berkeley, CA 94720 USA. RP Cervini-Silva, J (reprint author), Univ Autonoma Metropolitana, Unidad Cuajimalpa UAM C, Dept Proc & Technol, Div Ciencias Nat & Ingn, Artificios 40,6 Piso, Mexico City 01120, DF, Mexico. EM jcervini@igeograf.unam.mx FU DGAPA-UNAM; UNAM [IN116007-2]; CONACYT [61670]; ECACORE FX The authors express gratitude to M. Sc. Pilar Fernandez Lomelin [Instituto de Geogralia, Universidad Nacional Autonoma de Mexico, (UNAM)l for technical support and Dr. Hugo Destaillats (Lawrence Berkeley National Laboratory) for helpful comments. D.K. is thankful for the support of a DGAPA-UNAM undergraduate scholarship. This project was supported in part by UNAM (PUNTA-PAPIIT Grant IN116007-2), CONACYT (SEP-CONACYT Ciencia Basica 2006, Grant 61670), and by ECACORE 2020 (SEMARNAT-CONACYT). NR 45 TC 14 Z9 15 U1 4 U2 17 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0013-936X EI 1520-5851 J9 ENVIRON SCI TECHNOL JI Environ. Sci. Technol. PD OCT 1 PY 2009 VL 43 IS 19 BP 7550 EP 7555 DI 10.1021/es9007917 PG 6 WC Engineering, Environmental; Environmental Sciences SC Engineering; Environmental Sciences & Ecology GA 498JT UT WOS:000270136500063 PM 19848175 ER PT J AU Charland, KML Buckeridge, DL Sturtevant, JL Melton, F Reis, BY Mandl, KD Brownstein, JS AF Charland, K. M. L. Buckeridge, D. L. Sturtevant, J. L. Melton, F. Reis, B. Y. Mandl, K. D. Brownstein, J. S. TI Effect of environmental factors on the spatio-temporal patterns of influenza spread SO EPIDEMIOLOGY AND INFECTION LA English DT Article DE Climate; geographical position; influenza; meteorological variables; solar radiation ID RESPIRATORY SYNCYTIAL VIRUS; VITAMIN-D; IMMUNE-SYSTEM; SURVEILLANCE; MELATONIN; ILLNESS; INACTIVATION; TEMPERATURE; INFECTIONS; VARIABLES AB Although spatio-temporal patterns of influenza spread often suggest that environmental factors play a role, their effect on the geographical variation in the timing of annual epidemics has not been assessed. We examined the effect of solar radiation, dew point, temperature and geographical position on the city-specific timing of epidemics in the USA. Using paediatric in-patient data from hospitals in 35 cities for each influenza season in the study period 2000-2005, we determined 'epidemic timing' by identifying the week of peak influenza activity. For each city we calculated averages of daily climate measurements for 1 October to 31 December. Bayesian hierarchical models were used to assess the strength of association between each variable and epidemic timing. Of the climate variables only solar radiation was significantly related to epidemic timing (95% CI -0.027 to -0.0032). Future studies may elucidate biological mechanisms intrinsically linked to solar radiation that contribute to epidemic timing in temperate regions. C1 [Charland, K. M. L.; Sturtevant, J. L.; Reis, B. Y.; Mandl, K. D.; Brownstein, J. S.] Harvard Mit Div Hlth Sci & Technol, Childrens Hosp Informat Program, Boston, MA USA. [Charland, K. M. L.; Buckeridge, D. L.] McGill Univ, MCHI, Montreal, PQ, Canada. [Charland, K. M. L.; Reis, B. Y.; Mandl, K. D.; Brownstein, J. S.] Childrens Hosp Boston, Div Emergency Med, Boston, MA USA. [Charland, K. M. L.; Reis, B. Y.; Mandl, K. D.; Brownstein, J. S.] Harvard Univ, Sch Med, Dept Pediat, Boston, MA 02115 USA. [Sturtevant, J. L.] Harvard Univ, Sch Publ Hlth, Dept Epidemiol, Boston, MA 02115 USA. [Melton, F.] Calif State Univ Monterey Bay, Seaside, CA USA. [Melton, F.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Charland, KML (reprint author), 1 Autumn St,Room 439, Boston, MA 02215 USA. EM Katia.Charland@childrens.harvard.edu FU NIAID NIH HHS [R21AI073591-01]; NLM NIH HHS [R21LM009263-01] NR 38 TC 19 Z9 21 U1 0 U2 7 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 0950-2688 J9 EPIDEMIOL INFECT JI Epidemiol. Infect. PD OCT PY 2009 VL 137 IS 10 BP 1377 EP 1387 DI 10.1017/S0950268809002283 PG 11 WC Public, Environmental & Occupational Health; Infectious Diseases SC Public, Environmental & Occupational Health; Infectious Diseases GA 498EH UT WOS:000270119300003 PM 19296868 ER PT J AU Jehle, D Fitelson, B AF Jehle, David Fitelson, Branden TI WHAT IS THE "EQUAL WEIGHT VIEW"? SO EPISTEME-A JOURNAL OF INDIVIDUAL AND SOCIAL EPISTEMOLOGY LA English DT Article AB In this paper, we investigate various possible (Bayesian) precisifications of the (somewhat vague) statements of "the equal weight view" (EWV) that have appeared in the recent literature on disagreement. We will show that the renditions of (EWV) that immediately suggest themselves are untenable from a Bayesian point of view. In the end, we will propose some tenable (but not necessarily desirable) interpretations of (EWV). Our aim here will not be to defend any particular Bayesian precisification of (EWV), but rather to raise awareness about some of the difficulties inherent in formulating such precisifications. C1 [Fitelson, Branden] Univ Calif Berkeley, Dept Philosophy, Berkeley, CA USA. [Fitelson, Branden] NASA, Goddard Space Flight Ctr, Argonne Natl Lab, Greenbelt, MD USA. [Fitelson, Branden] Univ Wisconsin, Madison, WI 53706 USA. [Fitelson, Branden] Univ Illinois, Urbana, IL 61801 USA. [Fitelson, Branden] Stanford Univ, Stanford, CA 94305 USA. [Fitelson, Branden] San Jose State Univ, San Jose, CA 95192 USA. NR 20 TC 17 Z9 17 U1 1 U2 1 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 1742-3600 EI 1750-0117 J9 EPISTEME-J INDIV SOC JI Episteme PD OCT PY 2009 VL 6 IS 3 BP 280 EP 293 DI 10.3366/E1742360009000719 PG 14 WC Philosophy SC Philosophy GA V32UT UT WOS:000208976800005 ER PT J AU Park, J Palumbo, DL AF Park, J. Palumbo, D. L. TI Damping of Structural Vibration Using Lightweight Granular Materials SO EXPERIMENTAL MECHANICS LA English DT Article DE Vibration control; Particle damping; Acoustic-structure interaction; Sandwich structures ID MEDIA AB An investigation of the vibration damping capability of granular treatments is presented. Cavities in aluminum and sandwich beams were filled with the lightweight particles made of polyimide. For analysis of vibration damping, the complex stiffness of structures before and after damping treatment was measured. Particles of different sizes, weights and polymer composition were used in the damping treatments. Large, frequency-dependent variations in structural loss factor depending on the types of particles were observed. This behavior was predicted by the Rayleigh-Ritz method. The frame wave propagation characteristics of the particles were measured and used in the numerical simulation. The acoustic-structure interaction between particles and structures enhances the dissipation of vibration energy. C1 [Park, J.] Hanyang Univ, Sch Mech Engn, Seoul 133791, South Korea. [Palumbo, D. L.] NASA, Langley Res Ctr, Struct Acoust Branch, Hampton, VA 23681 USA. RP Park, J (reprint author), Hanyang Univ, Sch Mech Engn, 17 Haengdang Dong, Seoul 133791, South Korea. EM parkj@hanyang.ac.kr; daniel.l.palumbo@nasa.gov FU Hanyang University [HY-2005] FX This work was supported by the research fund of Hanyang University (HY-2005). NR 17 TC 10 Z9 10 U1 2 U2 12 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0014-4851 J9 EXP MECH JI Exp. Mech. PD OCT PY 2009 VL 49 IS 5 BP 697 EP 705 DI 10.1007/s11340-008-9181-x PG 9 WC Materials Science, Multidisciplinary; Mechanics; Materials Science, Characterization & Testing SC Materials Science; Mechanics GA 480ZZ UT WOS:000268777400009 ER PT J AU Mielke, AF Elam, KA AF Mielke, Amy F. Elam, Kristie A. TI Dynamic measurement of temperature, velocity, and density in hot jets using Rayleigh scattering SO EXPERIMENTS IN FLUIDS LA English DT Article; Proceedings Paper CT 14th International Symposium on Applications of Laser Techniques to Fluid Mechanics CY JUL 07-10, 2008 CL Lisbon, PORTUGAL ID BRILLOUIN-SCATTERING; FLOWS; GAS; FLUCTUATIONS; THERMOMETRY; MODEL AB A molecular Rayleigh scattering technique is utilized to measure gas temperature, velocity, and density in unseeded gas flows at sampling rates up to 10 kHz, providing fluctuation information up to 5 kHz based on the Nyquist theorem. A high-power continuous-wave laser beam is focused at a point in an air flow field and Rayleigh scattered light is collected and fiber-optically transmitted to a Fabry-Perot interferometer for spectral analysis. Photomultiplier tubes operated in the photon counting mode allow high-frequency sampling of the total signal level and the circular interference pattern to provide dynamic density, temperature, and velocity measurements. Mean and root mean square velocity, temperature, and density, as well as power spectral density calculations, are presented for measurements in a hydrogen-combustor heated jet facility with a 50.8-mm diameter nozzle at NASA John H. Glenn Research Center at Lewis Field. The Rayleigh measurements are compared with particle image velocimetry data and computational fluid dynamics predictions. This technique is aimed at aeronautics research related to identifying noise sources in free jets, as well as applications in supersonic and hypersonic flows where measurement of flow properties, including mass flux, is required in the presence of shocks and ionization occurrence. C1 [Mielke, Amy F.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. [Elam, Kristie A.] Jacobs Sverdrup, Cleveland, OH 44135 USA. RP Mielke, AF (reprint author), NASA, Glenn Res Ctr, 21000 Brookpk Rd,MS 77-1, Cleveland, OH 44135 USA. EM amy.f.mielke@nasa.gov NR 29 TC 4 Z9 4 U1 1 U2 7 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0723-4864 J9 EXP FLUIDS JI Exp. Fluids PD OCT PY 2009 VL 47 IS 4-5 BP 673 EP 688 DI 10.1007/s00348-009-0708-4 PG 16 WC Engineering, Mechanical; Mechanics SC Engineering; Mechanics GA 507QR UT WOS:000270870000011 ER PT J AU Reese, C Hillgruber, N Sturdevant, M Wertheimer, A Smoker, W Focht, R AF Reese, Carl Hillgruber, Nicola Sturdevant, Molly Wertheimer, Alex Smoker, William Focht, Rick TI Spatial and temporal distribution and the potential for estuarine interactions between wild and hatchery chum salmon (Oncorhynchus keta) in Taku Inlet, Alaska SO FISHERY BULLETIN LA English DT Article ID JUVENILE PACIFIC SALMON; PRINCE-WILLIAM-SOUND; SIZE-SELECTIVE MORTALITY; PINK SALMON; SOUTHEASTERN ALASKA; BRITISH-COLUMBIA; ATLANTIC SALMON; MARINE WATERS; PUGET-SOUND; PRIOR RESIDENCE AB We investigated estuarine spatial and temporal overlap of wild and marked hatchery chum salmon (Oncorhynchus keta) fry; the latter included two distinct size groups released near the Taku River estuary (Taku Inlet) in Southeast Alaska (early May releases of similar to 1.9 g and late May releases of similar to 3.9 g wet weight). Our objectives were to compare abundance, body size, and condition of wild chum salmon fry and hatchery chum salmon fry raised under early and late rearing strategies in different habitats of Taku Inlet and to document environmental factors that could potentially explain the distribution, size, and abundance of these chum salmon fry. We used a sampling design stratified into inner and outer inlet and neritic and littoral habitats. Hatchery fry were rare in the inner estuary in both years but outnumbered wild fry 20:1 in the outer estuary. Hatchery fry were significantly larger than wild fry in both littoral and neritic samples. Abundances of wild and hatchery fry were positively correlated in the outer inlet, indicating the formation of mixed schools of hatchery and wild fry. Spatial and temporal overlap was greatest between wild and early hatchery fry in the outer inlet in both habitats. The early hatchery release coincided with peak abundances of wild fry in the outer inlet, and the distribution of wild and early hatchery fry overlapped for about three weeks. Our results demonstrate that the timing of release of hatchery fry may affect interactions with wild fry. C1 [Reese, Carl] Alaska Dept Environm Conservat, Juneau, AK 99801 USA. [Reese, Carl; Hillgruber, Nicola; Smoker, William] Univ Alaska Fairbanks, Sch Fisheries & Ocean Sci, Juneau, AK 99801 USA. [Sturdevant, Molly; Wertheimer, Alex] Natl Marine Fisheries Serv, Auke Bay Labs, Alaska Fisheries Sci Ctr, Juneau, AK 99801 USA. [Focht, Rick] Douglas Isl Pink & Chum Inc, Juneau, AK 99801 USA. RP Reese, C (reprint author), Alaska Dept Environm Conservat, 410 Willoughby Ave, Juneau, AK 99801 USA. EM carl.reese@alaska.gov FU Alaska Department of Fish and Game; Pacific Coast Salmon Restoration Fund through the Southeast Sustainable Salmon Fund FX This research was supported by the Alaska Department of Fish and Game and the Pacific Coast Salmon Restoration Fund through the Southeast Sustainable Salmon Fund. Otolith marks were read by D. Tersteeg, B. Meredith, and M. Wunderlich of Douglas Island Pink and Chum, Inc. We would like to thank S. Heinl of Alaska Department of Fish and Game for suggestions and background information, and E. Fergusson for laboratory and database assistance. C. Farrington, B. White, L. Mullins, R. Vinzant, E. Venturini, J. Barton, J. Haas, T. Miles, and others assisted us in the field. We are grateful for the expert support provided by R. Dobrydnia, Master of the FV Teasha, Ketchikan, Alaska. We also appreciate the insightful, constructive comments provided by three anonymous reviewers who helped us to substantially improve the manuscript. NR 57 TC 5 Z9 6 U1 0 U2 1 PU NATL MARINE FISHERIES SERVICE SCIENTIFIC PUBL OFFICE PI SEATTLE PA 7600 SAND POINT WAY NE BIN C15700, SEATTLE, WA 98115 USA SN 0090-0656 J9 FISH B-NOAA JI Fish. Bull. PD OCT PY 2009 VL 107 IS 4 BP 433 EP 450 PG 18 WC Fisheries SC Fisheries GA 513HE UT WOS:000271312500003 ER PT J AU Stoner, AW AF Stoner, Allan W. TI Prediction of discard mortality for Alaskan crabs after exposure to freezing temperatures, based on a reflex impairment index SO FISHERY BULLETIN LA English DT Article ID AIR EXPOSURE; SNOW CRAB; COLLATERAL MORTALITY; CHIONOECETES-BAIRDI; HANDLING MORTALITY; WATER TEMPERATURE; TANNER CRABS; SPIDER CRAB; LOBSTER; FISHERY AB Millions of crabs are sorted and discarded in freezing conditions each year in Alaskan fisheries for Tanner crab (Chionoecetes bairdi) and snow crab (C. opilio). However, cold exposures vary widely over the fishing season and among different vessels, and mortalities are difficult to estimate. A shipboard experiment was conducted to determine whether simple behavioral observations can be used to evaluate crab condition after low-temperature exposures. Crabs were systematically subjected to cold in seven different exposure treatments. They were then tested for righting behavior and six different reflex actions and held to monitor mortality. Crabs lost limbs, showed reflex impairment, and died in direct proportion to increases in cold exposure. Righting behavior was a poor predictor of mortality, whereas reflex impairment (scored as the sum of reflex actions that were lost) was an excellent predictor. This composite index could be measured quickly and easily in hand, and logistic regression revealed that the relationship between reflex impairment and mortality correctly predicted 80.0% of the mortality and survival for C. bairdi, and 79.4% for C. opilio. These relationships provide substantial improvements over earlier approaches to mortality estimation and were independent of crab size and exposure temperature. C1 NOAA, Fisheries Behav Ecol Program, Alaska Fisheries Sci Ctr, Natl Marine Fisheries Serv, Newport, OR 97365 USA. RP Stoner, AW (reprint author), NOAA, Fisheries Behav Ecol Program, Alaska Fisheries Sci Ctr, Natl Marine Fisheries Serv, 2030 S Marine Sci Dr, Newport, OR 97365 USA. EM al.stoner@noaa.gov FU North Pacific Research Board [711] FX This research was supported by a grant from the North Pacific Research Board (project no. 711). C. Rose, J.E. Munk, P. Iseri, D. Benjamin, and C. Hammond assisted with the field operations, and the captain and crew of FV Pacific Explorer helped to set up experimental systems. M. W. Davis provided guidance in experimental protocols and data interpretation. Helpful suggestions for the manuscript were made by M. Carls, M. W. Davis, J.E. Munk, and B. G. Stevens. NR 39 TC 9 Z9 9 U1 1 U2 7 PU NATL MARINE FISHERIES SERVICE SCIENTIFIC PUBL OFFICE PI SEATTLE PA 7600 SAND POINT WAY NE BIN C15700, SEATTLE, WA 98115 USA SN 0090-0656 J9 FISH B-NOAA JI Fish. Bull. PD OCT PY 2009 VL 107 IS 4 BP 451 EP 463 PG 13 WC Fisheries SC Fisheries GA 513HE UT WOS:000271312500004 ER PT J AU Cox, MK Heintz, R AF Cox, M. Keith Heintz, Ron TI Electrical phase angle as a new method to measure fish condition SO FISHERY BULLETIN LA English DT Article ID BIOELECTRICAL-IMPEDANCE ANALYSIS; SALMON SALMO-SALAR; PROXIMATE COMPOSITION; BODY-COMPOSITION; ATLANTIC SALMON; SEASONAL-CHANGES; MUSCLE; TROUT; WATER AB In this study, phase angle (the ratio of resistance and reactance of tissue to applied electrical current) is presented as a possible new method to measure fish condition. Condition indices for fish have historically been based on simple weight-at-length relationships, or on costly and time-consuming laboratory procedures that measure specific physiological parameters. Phase angle is introduced to combine the simplicity of a quick field-based measurement with the specificity of laboratory analysis by directly measuring extra- and intracellular water distribution within an organism, which is indicative of its condition. Phase angle, which can be measured in the field or laboratory in the time it takes to measure length and weight, was measured in six species of fish at different states (e.g., fed vs. fasted, and postmortem) and under different environmental treatments (wild vs. hatchery, winter vs. spring). Phase angle reflected different states of condition. Phase angles <15 degrees indicated fish in poor condition, and phase angles >15 degrees indicated fish that were in better condition. Phase angle was slightly affected by temperatures (slope=-0.19) in the 0-8 degrees C range and did not change in fish placed on ice for <12 hours. Phase angle also decreased over time in postmortem fish because of cell membrane degradation and subsequent water movement from intra- to extracellular (interstitial) spaces. Phase angle also reflected condition of specific anatomical locations within the fish. C1 [Cox, M. Keith; Heintz, Ron] NOAA, Natl Marine Fisheries Serv, Alaska Fisheries Sci Ctr, Auke Bay Labs, Juneau, AK 99801 USA. RP Cox, MK (reprint author), NOAA, Natl Marine Fisheries Serv, Alaska Fisheries Sci Ctr, Auke Bay Labs, 11305 Glacier Hwy, Juneau, AK 99801 USA. EM Keith.Cox@noaa.gov FU NOAA Alaska Fisheries Science Center FX The authors would like to thank NOAA Alaska Fisheries Science Center for providing funding for this project and K. Hartman (West Virginia University), J. Silverstein (USDA), J. Margraf (University of Alaska, Fairbanks), N. Parker (Juneau Douglas High School), and J. J. Vollenweider (Auke Bay Laboratories) for providing fish data. NR 32 TC 12 Z9 12 U1 2 U2 6 PU NATL MARINE FISHERIES SERVICE SCIENTIFIC PUBL OFFICE PI SEATTLE PA 7600 SAND POINT WAY NE BIN C15700, SEATTLE, WA 98115 USA SN 0090-0656 J9 FISH B-NOAA JI Fish. Bull. PD OCT PY 2009 VL 107 IS 4 BP 477 EP 487 PG 11 WC Fisheries SC Fisheries GA 513HE UT WOS:000271312500006 ER PT J AU Martinson, EC Helle, JH Scarnecchia, DL Stokes, HH AF Martinson, Ellen C. Helle, John H. Scarnecchia, Dennis L. Stokes, Houston H. TI Growth and survival of sockeye salmon (Oncorhynchus nerka) from Karluk Lake and River, Alaska, in relation to climatic and oceanic regimes and indices, 1922-2000 SO FISHERY BULLETIN LA English DT Article ID SIZE-SELECTIVE MORTALITY; PINK SALMON; NORTHEAST PACIFIC; BRITISH-COLUMBIA; MARINE GROWTH; ABUNDANCE; RATES; TEMPERATURE; COMPETITION; GORBUSCHA AB We examined whether the relationship between climate and salmon production was linked through the effect of climate on the growth of sockeye salmon (Oncorhynchus nerka) at sea. Smolt length and juvenile, immature, and maturing growth rates were estimated from increments on scales of adult sockeye salmon that returned to the Karluk River and Lake system on Kodiak Island, Alaska, over 77 years, 1924-2000. Survival was higher during the warm climate regimes and lower during the cool regime. Growth was not correlated with survival, as estimated from the residuals of the Ricker stock-recruitment model. Juvenile growth was correlated with an atmospheric forcing index and immature growth was correlated with the amount of coastal precipitation, but the magnitude of winter and spring coastal downwelling in the Gulf of Alaska and the Pacific Northwest atmospheric patterns that influence the directional bifurcation of the Pacific Current were not related to the growth of Karluk sockeye salmon. However, indices of sea surface temperature, coastal precipitation, and atmospheric circulation in the eastern North Pacific were correlated with the survival of Karluk sockeye salmon. Winter and spring precipitation and atmospheric circulation are possible processes linking survival to climate variation in Karluk sockeye salmon. C1 [Martinson, Ellen C.; Helle, John H.] NOAA, Auke Bay Labs, Alaska Fisheries Sci Ctr, Natl Marine Fisheries Serv,Ted Stevens Marine Res, Juneau, AK 99801 USA. [Scarnecchia, Dennis L.] Univ Idaho, Dept Fish & Wildlife Resources, Moscow, ID 83844 USA. [Stokes, Houston H.] Univ Illinois, Chicago, IL 60607 USA. RP Martinson, EC (reprint author), NOAA, Auke Bay Labs, Alaska Fisheries Sci Ctr, Natl Marine Fisheries Serv,Ted Stevens Marine Res, 17109 Point Lena Loop Rd, Juneau, AK 99801 USA. EM Ellen.Martinson@noaa.gov NR 39 TC 5 Z9 5 U1 0 U2 7 PU NATL MARINE FISHERIES SERVICE SCIENTIFIC PUBL OFFICE PI SEATTLE PA 7600 SAND POINT WAY NE BIN C15700, SEATTLE, WA 98115 USA SN 0090-0656 J9 FISH B-NOAA JI Fish. Bull. PD OCT PY 2009 VL 107 IS 4 BP 488 EP 500 PG 13 WC Fisheries SC Fisheries GA 513HE UT WOS:000271312500007 ER PT J AU Wu, LL Beard, BL Roden, EE Johnson, CM AF Wu, Lingling Beard, Brian L. Roden, Eric E. Johnson, Clark M. TI Influence of pH and dissolved Si on Fe isotope fractionation during dissimilatory microbial reduction of hematite SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Article ID FE(III) OXIDE REDUCTION; CRYSTAL-CHEMISTRY; IRON ISOTOPES; FERROUS IRON; FE(II)-FE(III) ELECTRON; MOSSBAUER-SPECTROSCOPY; SURFACE CATALYSIS; AQUEOUS-SOLUTION; MINERAL SURFACE; FECL2 SOLUTIONS AB Microbial dissimilatory iron reduction (DIR) has been identified as a mechanism for production of aqueous Fe(II) that has low (56)Fe/(54)Fe ratios in modern and ancient suboxic environments that contain ferric oxides or hydroxides. These studies suggest that DIR could have played an important role in producing distinct Fe isotope compositions in Precambrian banded iron formations or other marine sedimentary rocks. However, the applicability of experimental studies of Fe isotope fractionation produced by DIR in geochemically simple systems to ancient marine environments remains unclear. Here we report Fe isotope fractionations produced during dissimilatory microbial reduction of hematite by Geobacter sulfurreducens in the presence and absence of dissolved Si at neutral and alkaline pH. Hematite reduction was significantly decreased by Si at alkaline (but not neutral) pH, presumably due to Si polymerization at the hematite surface. The presence of Si altered Fe isotope fractionation factors between aqueous Fe(II) or sorbed Fe(II) and reactive Fe(III), reflecting changes in bonding environment of the reactive Fe(III) component at the oxide surface. Despite these changes in isotopic fractionations, our results demonstrate that microbial Fe(III) oxide reduction produces Fe(II) with negative delta(56)Fe values under conditions of variable pH and dissolved Si, similar to the large inventory of negative delta(56)Fe in Neoarchean and Paleoproterozoic age marine sedimentary rocks. (C) 2009 Elsevier Ltd. All rights reserved. C1 Univ Wisconsin, Dept Geosci, Madison, WI 53706 USA. Univ Wisconsin, NASA, Astrobiol Inst, Madison, WI 53706 USA. RP Wu, LL (reprint author), Univ Wisconsin, Dept Geol & Geophys, 1215 W Dayton St, Madison, WI 53706 USA. EM lwu@geology.wisc.edu RI Wu, Lingling/E-4087-2010 OI Wu, Lingling/0000-0002-8211-5754 FU NASA Astrobiology Institute; National Science Foundation FX The authors thank Nita Sahai for insightful discussions about changes in bonding environments for Fe(III) in hematite in the presence of Si. Evgenya S. Shebobolina is thanked for her help with bacterial culturing. Tao Wu is thanked for his help in the preliminary experiments. Constructive criticism by Matthew S. Fantle and an anonymous reviewer and the Associate Editor, James Farquhar, improved the manuscript. This research was supported by the NASA Astrobiology Institute, as well as the National Science Foundation, Research in Biogeosciences Program. NR 75 TC 26 Z9 29 U1 6 U2 33 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD OCT 1 PY 2009 VL 73 IS 19 BP 5584 EP 5599 DI 10.1016/j.gca.2009.06.026 PG 16 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 541LE UT WOS:000273416400005 ER PT J AU Cardace, D Morris, JD AF Cardace, Dawn Morris, Julie D. TI Geochemical evidence for sediment accretion in the Costa Rica Frontal Prism SO GEOLOGY LA English DT Article ID SUBDUCTION EROSION; CONVERGENT MARGINS; ZONES; PLATE; CRUST AB We report new geochemical data for marine sediments sampled in the frontal prism associated with the Costa Rica subduction zone during Leg 205 of the Ocean Drilling Program (ODP). We describe variation in sediment geochemistry with depth as the decollement zone, the interface between overriding and downgoing tectonic plates, is approached. This variation can be explained by three-component mixing of ash, lower plate sediments (LPS), and frontal prism or upper plate sediments (UPS). We detect in-mixing of LPS in localized sediment intervals, amounting to tens of vertical meters of LPS incorporation; no persuasive evidence of LPS transfer into the prism has been shown until this contribution. This inference of fine structure in the prism provides new insight into how tectonic kneading of sediments occurs in decollement zones. C1 [Cardace, Dawn] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Morris, Julie D.] Natl Sci Fdn, Ocean Sci Div, Arlington, VA 22230 USA. RP Cardace, D (reprint author), NASA, Ames Res Ctr, M-S 239-4, Moffett Field, CA 94035 USA. EM dawn.cardacc-1@nasa.gov FU U. S. National Science Foundation; U. S. Science Support Program FX This research used samples and data provided by the Ocean Drilling Program, sponsored by the U. S. National Science Foundation and participating countries under management of Joint Oceanographic Institutions, Inc. Funding was provided by the U. S. Science Support Program. We are grateful to Mike Underwood, Paola Vannucchi, Miriam Kastner, and the Leg 205 Shipboard Scientific Party. Comments from David Scholl, Harold Tobin, and one anonymous reviewer significantly improved this manuscript. NR 21 TC 4 Z9 4 U1 1 U2 4 PU GEOLOGICAL SOC AMER, INC PI BOULDER PA PO BOX 9140, BOULDER, CO 80301-9140 USA SN 0091-7613 J9 GEOLOGY JI Geology PD OCT PY 2009 VL 37 IS 10 BP 891 EP 894 DI 10.1130/G25631A.1 PG 4 WC Geology SC Geology GA 501MV UT WOS:000270386900008 ER PT J AU Warny, S Askin, RA Hannah, MJ Mohr, BAR Raine, JI Harwood, DM Florindo, F Levy, R Acton, G Atkins, C Bassett, K Berg, M Bibby, T Blair, S Blank, L Browne, G Del Carlo, P Dooley, J Drew, S Dunbar, G Field, B Fielding, C Frank, T Frisch-Gleason, R Grelle, T Handwerger, D Hoffmann, S Hubbard, J Huffman, L Ishman, S Johnson, K Jovane, L Konfirst, M Krissek, L Kuhn, G Lacy, L Lehmann, R Magens, D Mankoff, K Millan, C Nielsen, S Olney, M Panter, K Passchier, S Patterson, T Paulsen, T Pekar, S Persico, D Petrushak, S Pierdominici, S Pound, K Reed, J Reichelt, L Riesselman, C Sandroni, S Schmitt, D di Clemente, GS Speece, M Strada, E Szymcek, P Talarico, F Taviani, M Tuzzi, E Williams, R Wonik, T AF Warny, Sophie Askin, Rosemary A. Hannah, Michael J. Mohr, Barbara A. R. Raine, J. Ian Harwood, David M. Florindo, Fabio Levy, Richard (Rich) Acton, Gary Atkins, Clifford (Cliff) Bassett, Kari Berg, Megan Bibby, Theodore (Ted) Blair, Stacie Blank, Leslie Browne, Gregory (Greg) Del Carlo, Paola Dooley, Julia Drew, Scott Dunbar, Gavin Field, Bradley (Brad) Fielding, Christopher (Chris) Frank, Tracy Frisch-Gleason, Robin Grelle, Thomas Handwerger, David (Dave) Hoffmann, Stefan Hubbard, Joanna Huffman, Louise Ishman, Scott Johnson, Katherine (Katie) Jovane, Luigi Konfirst, Matthew (Matt) Krissek, Lawrence (Larry) Kuhn, Gerhard (Gerd) Lacy, Laura Lehmann, Rainer Magens, Diana Mankoff, Kenneth (Ken) Millan, Cristina Nielsen, Simon Olney, Matthew (Matt) Panter, Kurt Passchier, Sandra Patterson, Taylor Paulsen, Timothy (Tim) Pekar, Stephen (Steve) Persico, Davide Petrushak, Steven (Steve) Pierdominici, Simona Pound, Katherine (Kate) Reed, Joshua (Josh) Reichelt, Lucia (Lucy) Riesselman, Christina Sandroni, Sonia Schmitt, Douglas (Doug) di Clemente, Graziano Scotto Speece, Marvin (Marv) Strada, Eleonora Szymcek, Phillip (Phill) Talarico, Franco Taviani, Marco Tuzzi, Eva Williams, Robert (Bob) Wonik, Thomas CA SMS Sci Team TI Palynomorphs from a sediment core reveal a sudden remarkably warm Antarctica during the middle Miocene SO GEOLOGY LA English DT Article ID DINOFLAGELLATE CYST DISTRIBUTION; NORTH-SEA BASIN; CLIMATE; PLIOCENE; STRATIGRAPHY; VEGETATION; GREENLAND; OLIGOCENE; TRANSECT; BELGIUM AB An exceptional triple palynological signal (unusually high abundance of marine, freshwater, and terrestrial palynomorphs) recovered from a core collected during the 2007 ANDRILL (Antarctic geologic drilling program) campaign in the Ross Sea, Antarctica, provides constraints for the Middle Miocene Climatic Optimum. Compared to elsewhere in the core, this signal comprises a 2000-fold increase in two species of dinoflagellate cysts, a synchronous five-fold increase in freshwater algae, and up to an 80-fold increase in terrestrial pollen, including a proliferation of woody plants. Together, these shifts in the palynological assemblages ca. 15.7 Ma ago represent a relatively short period of time during which Antarctica became abruptly much warmer. Land temperatures reached 10 degrees C (January mean), estimated annual sea-surface temperatures ranged from 0 to 11.5 degrees C, and increased freshwater input lowered the salinity during a short period of sea-ice reduction. C1 [Warny, Sophie; Askin, Rosemary A.] Louisiana State Univ, Dept Geol & Geophys, Baton Rouge, LA 70803 USA. [Warny, Sophie; Askin, Rosemary A.] Louisiana State Univ, Museum Nat Sci, Baton Rouge, LA 70803 USA. [Hannah, Michael J.] Victoria Univ Wellington, Sch Geog Environm & Earth Sci, Antarctic Res Ctr, Wellington, New Zealand. [Mohr, Barbara A. R.] Museum Nat Hist, D-10115 Berlin, Germany. [Raine, J. Ian; Levy, Richard (Rich); Browne, Gregory (Greg); Field, Bradley (Brad)] GNS Sci, Lower Hutt, New Zealand. [Harwood, David M.; Fielding, Christopher (Chris); Frank, Tracy; Tuzzi, Eva] Univ Nebraska, Dept Geosci, Lincoln, NE 68588 USA. [Harwood, David M.; Huffman, Louise; Lacy, Laura; Reed, Joshua (Josh)] Univ Nebraska, ANDRILL Sci Management Off, Lincoln, NE 68588 USA. [Florindo, Fabio] Ist Nazl Geofis & Vulcanol, I-00143 Rome, Italy. [Acton, Gary] Univ Calif Davis, Dept Geol, Davis, CA 95616 USA. [Atkins, Clifford (Cliff)] Victoria Univ Wellington, Sch Geog Environm & Earth Sci, Wellington 6005, New Zealand. [Bassett, Kari] Univ Canterbury, Dept Geol Sci, Christchurch, New Zealand. [Bibby, Theodore (Ted); Blair, Stacie; Petrushak, Steven (Steve)] Florida State Univ, Dept Geol Sci, Tallahassee, FL 32306 USA. [Blank, Leslie] Raytheon Polar Serv, Centennial, CO USA. [Del Carlo, Paola] Ist Nazl Geofis & Vulcanol, Sezione Pisa, I-56126 Pisa, Italy. [Drew, Scott; Krissek, Lawrence (Larry); Millan, Cristina] Ohio State Univ, Sch Earth Sci, Columbus, OH 43210 USA. [Dunbar, Gavin] Victoria Univ Wellington, Antarctic Res Ctr, Wellington 6005, New Zealand. [Grelle, Thomas; Wonik, Thomas] LIAG, Hannover, Germany. Victoria Univ Wellington, Sch Earth Sci, Wellington 4007, New Zealand. [Hoffmann, Stefan] Univ Gottingen, Dept Sedimentol & Environm Geol, D-37077 Gottingen, Germany. [Ishman, Scott] SO Illinois Univ Carbondale, Dept Geol, Carbondale, IL 62901 USA. [Johnson, Katherine (Katie)] Geomarine Res, Auckland 1072, New Zealand. [Jovane, Luigi] Univ Calif Davis, Paleomagnet Lab, Dept Geol, Davis, CA 95616 USA. [Konfirst, Matthew (Matt)] No Illinois Univ, Dept Geol & Environm Geosci, De Kalb, IL 60115 USA. [Kuhn, Gerhard (Gerd); Magens, Diana] Alfred Wegener Inst, Dept Marine Geophys, D-27515 Bremerhaven, Germany. [Mankoff, Kenneth (Ken)] NASA GISS, New York, NY 10025 USA. [Nielsen, Simon] Japan Agcy Marine Earth Sci & Technol, Ctr Deep Earth Explorat, Yokohama, Kanagawa 2360001, Japan. [Olney, Matthew (Matt)] Univ S Florida, Dept Geol, Tampa, FL 33620 USA. [Panter, Kurt] Bowling Green State Univ, Earth & Environm Stud, Bowling Green, OH 43403 USA. [Passchier, Sandra] Montclair State Univ, Earth & Environm Stud, Montclair, NJ 07043 USA. [Patterson, Taylor; Speece, Marvin (Marv)] Montana Tech Univ Montana, Dept Geophys Engn, Butte, MT 59701 USA. [Paulsen, Timothy (Tim)] Univ Wisconsin Oshkosh, Dept Geol, Oshkosh, WI 54901 USA. [Pekar, Stephen (Steve)] Queens Coll, Sch Earth & Environm Sci, Flushing, NY 11367 USA. [Persico, Davide] Univ Parma, Dipartimento Sci Terra, I-43100 Parma, Italy. [Pierdominici, Simona] Ist Nazl Geofis & Vulcanol, I-00143 Rome, Italy. [Pound, Katherine (Kate)] St Cloud State Univ, Dept Earth & Atmospher Sci, St Cloud, MN 56301 USA. [Reichelt, Lucia (Lucy)] Alfred Wegener Inst, D-27568 Bremerhaven, Germany. [Riesselman, Christina] Stanford Univ, Geol & Environm Sci, Stanford, CA 94305 USA. [Sandroni, Sonia] Sez Sci Terra Siena, Museo Nazl Antartide, I-53100 Siena, Italy. [Schmitt, Douglas (Doug)] Univ Alberta, Inst Geophys Res, Dept Phys, Edmonton, AB T6G 2G7, Canada. [di Clemente, Graziano Scotto; Talarico, Franco] Secondary Sch Luigi Stefanini, I-31100 Treviso, Italy. [Strada, Eleonora] Univ Siena, Dipartimento Sci Terra, I-53100 Siena, Italy. [Taviani, Marco] CNR, ISMAR Bologna, I-40129 Bologna, Italy. RP Warny, S (reprint author), Louisiana State Univ, Dept Geol & Geophys, E235 Howe Russell, Baton Rouge, LA 70803 USA. EM swarny@lsu.edu; askin@bresnan.net; Michael.hannah@vuw.ac.nz; Barbara.mohr@museum.hu-berlin.de; I.Raine@gns.cri.nz; dharwood1@unl.edu; florindo@ingv.it; r.levy@gns.cri.nz; gdacton@ucdavis.edu; cliff.atkins@vuw.ac.nz; kari.bassett@canterbury.ac.nz; meganberg@mac.com; tcb03c@fsu.edu; blair@quartz.gly.fsu.edu; G.Browne@gns.cri.nz; delcarlo@pi.ingv.it; dooleyj@christina.k12.de.us; drew.37@osu.edu; gavin.dunbar@vuw.ac.nz; brad.field@gns.cri.nz; cfielding2@unl.edu; tfrank2@unl.edu; gleason@aaps.k12.mi.us; t.grelle@liag-hannover.de; dave@xmission.com; s.hoffmann@geo.uni-goettingen.de; hubbard_joanna@asdk12.org; lhuffman@andrill.org; sishman@siu.edu; k.johnson@geomarine.org.nz; jovane@geology.ucdavis.edu; mk@mattkonfirst.com; krissek@mps.ohio-state.edu; gerhard.kuhn@awi.de; llacy2@unl.edu; rainer.lehmann@gmx.net; Diana.Magens@awi.de; mankoff@giss.nasa.gov; millan.2@osu.edu; simon.n@jamstec.go.jp; cyclingolney@yahoo.co.uk; kpanter@bgsu.edu; passchiers@mail.montclair.edu; paulsen@uwosh.edu; stephen.pekar@qc.cuny.edu; davide.persico@unipr.it; gneissguy2000@yahoo.com; pierdominici@ingv.it; kspound@stcloudstate.edu; jareed@andrill.org; lreichelt@gmx.de; criessel@stanford.edu; sandroni@unisi.it; doug@phys.ualberta.ca; grscott@tin.it; mspeece@mtech.edu; strada2@unisi.it; pszymcek@gmail.com; talarico@unisi.it; marco.taviani@bo.ismar.cnr.it; evatuzzi@libero.it; bbermk@xtra.co.nz; Thomas.wonik@liag-hannover.de RI Raine, James/D-5124-2009; Warny, Sophie/A-8226-2013; Hannah, Michael/H-1083-2015; Florindo, Fabio/F-4119-2010; Passchier, Sandra/B-1993-2008; Jovane, Luigi/E-7536-2012 OI Raine, James/0000-0001-5294-2102; Hannah, Michael/0000-0002-2275-0086; Florindo, Fabio/0000-0002-6058-9748; Passchier, Sandra/0000-0001-7204-7025; Jovane, Luigi/0000-0003-4348-4714 FU U. S. Antarctic Program; Raytheon Polar Services Corporation; Antarctica New Zealand; U. S. National Science Foundation; New Zealand Foundation for Research Science and Technology; Italian Antarctic Research Program; German Science Foundation; Alfred Wegener Institute FX The ANDRILL (Antarctic geologic drilling) Program is a multinational collaboration between the Antarctic programs of Germany, Italy, New Zealand, and the United States. Antarctica New Zealand is the project operator and has developed the drilling system in collaboration with Alex Pyne at Victoria University of Wellington and Webster Drilling and Exploration. The U. S. Antarctic Program and Raytheon Polar Services Corporation supported the science team at McMurdo Station, while Antarctica New Zealand supported the drilling team at Scott Base. Scientific studies are jointly supported by the U. S. National Science Foundation, New Zealand Foundation for Research Science and Technology, the Italian Antarctic Research Program, the German Science Foundation, and the Alfred Wegener Institute. We are grateful to Vanessa Bowman and Rex Harland for their careful review of the manuscript. NR 35 TC 53 Z9 54 U1 1 U2 20 PU GEOLOGICAL SOC AMER, INC PI BOULDER PA PO BOX 9140, BOULDER, CO 80301-9140 USA SN 0091-7613 EI 1943-2682 J9 GEOLOGY JI Geology PD OCT PY 2009 VL 37 IS 10 BP 955 EP 958 DI 10.1130/G30139A.1 PG 4 WC Geology SC Geology GA 501MV UT WOS:000270386900024 ER PT J AU Aung, K Burnett, J Smith, SM Dyer, C AF Aung, K. Burnett, J. Smith, S. M. Dyer, C. TI TOCOPHEROL IN ELDER SELF-NEGLECT SO GERONTOLOGIST LA English DT Meeting Abstract C1 [Aung, K.] Univ Texas Hlth Sci Ctr San Antonio, San Antonio, TX 78229 USA. [Aung, K.] Univ Texas Houston, Sch Publ Hlth, Houston, TX USA. [Burnett, J.; Dyer, C.] Univ Texas Hlth Sci Ctr Houston, Houston, TX USA. [Smith, S. M.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU GERONTOLOGICAL SOC AMER PI WASHINGTON PA 1030 15TH ST NW, STE 250, WASHINGTON, DC 20005202-842 USA SN 0016-9013 J9 GERONTOLOGIST JI Gerontologist PD OCT PY 2009 VL 49 SU 2 BP 72 EP 72 PG 1 WC Gerontology SC Geriatrics & Gerontology GA 519UI UT WOS:000271793900342 ER PT J AU Buccello-Stout, R Cromwell, RL Bloomberg, J AF Buccello-Stout, R. Cromwell, R. L. Bloomberg, J. TI CHARACTERIZATION OF THE HEAD STABILIZATION RESPONSE TO A LATERAL PERTURBATION DURING WALKING IN OLDER ADULTS SO GERONTOLOGIST LA English DT Meeting Abstract C1 [Buccello-Stout, R.; Cromwell, R. L.] Univ Space Res Assoc, Houston, TX USA. [Bloomberg, J.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU GERONTOLOGICAL SOC AMER PI WASHINGTON PA 1030 15TH ST NW, STE 250, WASHINGTON, DC 20005202-842 USA SN 0016-9013 J9 GERONTOLOGIST JI Gerontologist PD OCT PY 2009 VL 49 SU 2 BP 288 EP 288 PG 1 WC Gerontology SC Geriatrics & Gerontology GA 519UK UT WOS:000271794100394 ER PT J AU White, MA de Beurs, KM Didan, K Inouye, DW Richardson, AD Jensen, OP O'Keefe, J Zhang, G Nemani, RR van Leeuwen, WJD Brown, JF de Wit, A Schaepman, M Lin, XM Dettinger, M Bailey, AS Kimball, J Schwartz, MD Baldocchi, DD Lee, JT Lauenroth, WK AF White, Michael A. de Beurs, Kirsten M. Didan, Kamel Inouye, David W. Richardson, Andrew D. Jensen, Olaf P. O'Keefe, John Zhang, Gong Nemani, Ramakrishna R. van Leeuwen, Willem J. D. Brown, Jesslyn F. de Wit, Allard Schaepman, Michael Lin, Xioamao Dettinger, Michael Bailey, Amey S. Kimball, John Schwartz, Mark D. Baldocchi, Dennis D. Lee, John T. Lauenroth, William K. TI Intercomparison, interpretation, and assessment of spring phenology in North America estimated from remote sensing for 1982-2006 SO GLOBAL CHANGE BIOLOGY LA English DT Article DE bloom; budburst; climate change; flower; growing season; land surface phenology; seasonality ID SATELLITE SENSOR DATA; NDVI TIME-SERIES; CLIMATE-CHANGE; UNITED-STATES; PLANT PHENOLOGY; DECIDUOUS FOREST; FOURIER-ANALYSIS; CARBON-DIOXIDE; TRENDS; VARIABILITY AB Shifts in the timing of spring phenology are a central feature of global change research. Long-term observations of plant phenology have been used to track vegetation responses to climate variability but are often limited to particular species and locations and may not represent synoptic patterns. Satellite remote sensing is instead used for continental to global monitoring. Although numerous methods exist to extract phenological timing, in particular start-of-spring (SOS), from time series of reflectance data, a comprehensive intercomparison and interpretation of SOS methods has not been conducted. Here, we assess 10 SOS methods for North America between 1982 and 2006. The techniques include consistent inputs from the 8 km Global Inventory Modeling and Mapping Studies Advanced Very High Resolution Radiometer NDVIg dataset, independent data for snow cover, soil thaw, lake ice dynamics, spring streamflow timing, over 16 000 individual measurements of ground-based phenology, and two temperature-driven models of spring phenology. Compared with an ensemble of the 10 SOS methods, we found that individual methods differed in average day-of-year estimates by +/- 60 days and in standard deviation by +/- 20 days. The ability of the satellite methods to retrieve SOS estimates was highest in northern latitudes and lowest in arid, tropical, and Mediterranean ecoregions. The ordinal rank of SOS methods varied geographically, as did the relationships between SOS estimates and the cryospheric/hydrologic metrics. Compared with ground observations, SOS estimates were more related to the first leaf and first flowers expanding phenological stages. We found no evidence for time trends in spring arrival from ground- or model-based data; using an ensemble estimate from two methods that were more closely related to ground observations than other methods, SOS trends could be detected for only 12% of North America and were divided between trends towards both earlier and later spring. C1 [White, Michael A.; Zhang, Gong] Utah State Univ, Dept Watershed Sci, Logan, UT 84322 USA. [de Beurs, Kirsten M.] Virginia Polytech Inst & State Univ, Dept Geog, Blacksburg, VA 24061 USA. [Didan, Kamel] Univ Arizona, Inst Study Planet Earth, Tucson, AZ USA. [Inouye, David W.] Univ Maryland, Dept Biol, College Pk, MD 20742 USA. [Richardson, Andrew D.] Univ New Hampshire, Complex Syst Res Ctr, Durham, NH 03824 USA. [Jensen, Olaf P.] Univ Wisconsin, Ctr Limnol, Madison, WI 53706 USA. [O'Keefe, John] Harvard Forest, Petersham, MA USA. [Nemani, Ramakrishna R.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [van Leeuwen, Willem J. D.] Univ Arizona, Off Arid Lands Studies, Tucson, AZ USA. [van Leeuwen, Willem J. D.] Univ Arizona, Dept Geog & Reg Dev, Tucson, AZ USA. [Brown, Jesslyn F.] Earth Resources Observat & Sci EROS Ctr, US Geol Survey, Land Sci Div, Sioux Falls, SD USA. [de Wit, Allard; Schaepman, Michael] Wageningen UR, Ctr Geoinformat, Wageningen, Netherlands. [Lin, Xioamao] Campbell Sci Inc, Logan, UT USA. [Dettinger, Michael] Univ Calif San Diego, Scripps Inst Oceanog, US Geol Survey, La Jolla, CA 92093 USA. [Bailey, Amey S.] Hubbard Brook Expt Forest, Campton, NH USA. [Kimball, John] Univ Montana, Flathead Lake Biol Stn, Div Biol Sci, Polson, MT 59860 USA. [Schwartz, Mark D.] Univ Wisconsin, Dept Geog, Milwaukee, WI 53201 USA. [Baldocchi, Dennis D.] Univ Calif Berkeley, Dept Environm Sci Policy & Management, Berkeley, CA 94720 USA. [Lee, John T.] Univ Maine, Dept PSE, Environm Phys Grp, Orono, ME USA. [Lauenroth, William K.] Colorado State Univ, Grad Degree Program Ecol, Ft Collins, CO 80523 USA. [Lauenroth, William K.] Colorado State Univ, Warner Coll Nat Resources, Ft Collins, CO 80523 USA. RP White, MA (reprint author), Utah State Univ, Dept Watershed Sci, Logan, UT 84322 USA. EM mikew.usu@gmail.com RI Brown, Jesslyn/C-9888-2010; Jensen, Olaf/E-4947-2011; Richardson, Andrew/F-5691-2011; Inouye, David/C-2997-2011; Baldocchi, Dennis/A-1625-2009; Schaepman, Michael/B-9213-2009; OI Brown, Jesslyn/0000-0002-9976-1998; de Wit, Allard/0000-0002-5517-6404; Richardson, Andrew/0000-0002-0148-6714; Inouye, David/0000-0003-2076-7834; Baldocchi, Dennis/0000-0003-3496-4919; Schaepman, Michael/0000-0002-9627-9565; White, Michael/0000-0002-0238-8913 FU MAW; NASA [NNG04G043G, NNA05CS25A]; NSF [02-4277, ATM-9510342, 9809460, 0085224, DEB 981022, 9211775, 8702328, OPP-9911278, 9911681, 9732281, 9615411, 9615563, 9615942, 9615949, 9400722, 9415411, 9318529, BSR 9019055, 8806635, 8507493]; DDB; Office of Science (BER); US DOE [DE-FG02-06ER64308]; ADR; Northeastern States Research Cooperative FX We gratefully acknowledge agency support: MAW, NASA grants NNG04G043G and NNA05CS25A and NSF grant 02-4277; DDB, the Office of Science (BER), US DOE grant DE-FG02-06ER64308 and NSF grant DEB 0639235; MDS, NSF grants ATM-9510342, 9809460, and 0085224; ADR, the Northeastern States Research Cooperative and the U.S. Department of Energy's Office of Science (BER) through the Northeastern Regional Center of the National Institute for Climatic Change Research. We thank Samuel Hiatt for technical assistance. Logistical support and/or data were provided by the Niwot Ridge Long-Term Ecological Research (LTER) project and the Mountain Research Station (BIR 9115097). Data was supported by the NSF LTER Program at Konza Prairie Biological Station. Data sets were provided by the Arctic LTER. This material is based upon work supported by the National Science Foundation under Grants DEB 981022, 9211775, 8702328; OPP-9911278, 9911681, 9732281, 9615411, 9615563, 9615942, 9615949, 9400722, 9415411, 9318529; BSR 9019055, 8806635, 8507493. Data sets were provided by the Forest Science Data Bank, a partnership between the Department of Forest Science, Oregon State University, and the U.S. Forest Service Pacific Northwest Research Station, Corvallis, Oregon. Significant funding for collection of these data was provided by the National Science Foundation LTER program (NSF Grant numbers BSR 9011663 8811906 0423662; DEB 9632921, 0217631, 9411976, 0080529 and 0217774). Data sets were provided by the Shortgrass Steppe LTER group, a partnership between Colorado State University, United States Department of Agriculture, Agricultural Research Service, and the U.S. Forest Service Pawnee National Grassland. Data sets were provided by the Shortgrass Steppe LTER group, a partnership between Colorado State University, United States Department of Agriculture, Agricultural Research Service, and the U.S. Forest Service Pawnee National Grassland. Data sets were provided by the Sevilleta LTER program. NR 67 TC 325 Z9 350 U1 17 U2 204 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 OCT PY 2009 VL 15 IS 10 BP 2335 EP 2359 DI 10.1111/j.1365-2486.2009.01910.x PG 25 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 491KO UT WOS:000269577800001 ER PT J AU Ghose, S Watson, KA Cano, RJ Britton, SM Jensen, BJ Connell, JW Herring, HM Lineberry, QJ AF Ghose, Sayata Watson, Kent A. Cano, Roberto J. Britton, Sean M. Jensen, Brian J. Connell, John W. Herring, Helen M. Lineberry, Quentin J. TI High Temperature VARTM of Phenylethynyl Terminated Imides SO HIGH PERFORMANCE POLYMERS LA English DT Article DE phenylethynyl terminated imides; VARTM; voids; acid digestion ID COMPOSITES; RESINS AB Depending on the part type and quantity, fabrication of composite structures using vacuum-assisted resin transfer molding (VARTM) can be more affordable than conventional autoclave techniques. Recent efforts have focused on adapting VARTM for the fabrication of high temperature composites. Due to their low melt viscosity and long melt stability, certain phenylethynyl terminated imides (PETI) can be processed into composites using high temperature VARTM (HT-VARTM). However, one of the disadvantages of the current HT-VARTM resin systems has been the high porosity of the resultant composites. For aerospace applications, the desired void fraction of less than 2% has not yet been achieved. In the current study, two PETI resins, LaRC PETI-330 and LaRC PETI-8 have been used to make test specimens using HT-VARTM. The resins were infused into ten layers of IM7-6K carbon fiber 5-harness satin fabric at 260 or 280 degrees C and cured at temperature up to 371 degrees C. Initial runs yielded composites with high void content, typically greater than 7% by weight. A thermogravimetric-mass spectroscopic study was conducted to determine the source of volatiles leading to high porosity. It was determined that under the thermal cycle used for laminate fabrication, the phenylethynyl endcap was undergoing degradation leading to volatile evolution. This finding was unexpected as high quality composite laminates have been fabricated under higher pressures using these resin systems. The amount of weight loss experienced during the thermal cycle was only about 1% by weight, but this led to a significant amount of volatiles in a closed system. By modifying the thermal cycle used in laminate fabrication, the void content was significantly reduced (typically similar to 3% or less). The results of this work are presented herein. C1 [Ghose, Sayata; Watson, Kent A.] Natl Inst Aerosp, Hampton, VA 23666 USA. [Cano, Roberto J.; Britton, Sean M.; Jensen, Brian J.; Connell, John W.] NASA, Langley Res Ctr, Hampton, VA 23681 USA. [Herring, Helen M.] Lockheed Martin Engn & Sci Co, Hampton, VA 23666 USA. [Lineberry, Quentin J.] Western Kentucky Univ, NASA, GSRP, Bowling Green, KY 42101 USA. RP Ghose, S (reprint author), Natl Inst Aerosp, Hampton, VA 23666 USA. EM sayata.ghose-1@nasa.gov NR 16 TC 8 Z9 8 U1 2 U2 14 PU SAGE PUBLICATIONS LTD PI LONDON PA 1 OLIVERS YARD, 55 CITY ROAD, LONDON EC1Y 1SP, ENGLAND SN 0954-0083 J9 HIGH PERFORM POLYM JI High Perform. Polym. PD OCT PY 2009 VL 21 IS 5 BP 653 EP 672 DI 10.1177/0954008309339935 PG 20 WC Polymer Science SC Polymer Science GA 506EY UT WOS:000270757900012 ER PT J AU Wickens, CD Hooey, BL Gore, BF Sebok, A Koenicke, CS AF Wickens, Christopher D. Hooey, Becky L. Gore, Brian F. Sebok, Angelia Koenicke, Corey S. TI Identifying Black Swans in NextGen: Predicting Human Performance in Off-Nominal Conditions SO HUMAN FACTORS LA English DT Article ID PILOT PERFORMANCE; CHANGE BLINDNESS; DISPLAY; FLIGHT; SYSTEMS; MANAGEMENT; ATTENTION; AWARENESS; AVIATION; DESIGN AB Objective: The objective is to validate a computational model of visual attention against empirical data-derived from a meta-analysis-of pilots' failure to notice safety-critical unexpected events. Background: Many aircraft accidents have resulted, in part, because of failure to notice nonsalient unexpected events outside of foveal vision, illustrating the phenomenon of change blindness. A model of visual noticing, N-SEEV (noticing-salience, expectancy, effort, and value), was developed to predict these failures. Method: First, 25 studies that reported objective data on miss rate for unexpected events in high-fidelity cockpit simulations were identified, and their miss rate data pooled across five variables (phase of flight, event expectancy, event location, presence of a head-up display, and presence of a highway-in-the-sky display). Second, the parameters of the N-SEEV model were tailored to mimic these dichotomies. Results: The N-SEEV model output predicted variance in the obtained miss rate (r = .73). The individual miss rates of all six dichotomous conditions were predicted within 14%, and four of these were predicted within 7%. Conclusion: The N-SEEV model, developed on the basis of an independent data set, was able to successfully predict variance in this safety-critical measure of pilot response to abnormal circumstances, as collected from the literature. Applications: As new technology and procedures are envisioned for the future airspace, it is important to predict if these may compromise safety in terms of pilots' failing to notice unexpected events. Computational models such as N-SEEV support cost-effective means of making such predictions. C1 [Wickens, Christopher D.; Koenicke, Corey S.] Alion Sci Corp, Micro Anal & Design, Boulder, CO 80301 USA. [Hooey, Becky L.; Gore, Brian F.] San Jose State Univ, Res Fdn, NASA, Ames Res Ctr, Moffett Field, CA USA. RP Wickens, CD (reprint author), Alion Sci Corp, Micro Anal & Design, 4949 Pearl E Circle,Suite 300, Boulder, CO 80301 USA. EM cwickens@alionscience.com FU National Aeronautics and Space Administration's (NASA) [NNX08AE87A] FX This research was supported by a cooperative agreement from National Aeronautics and Space Administration's (NASA) NextGen-Airspace Project (Airspace Super Density Operations, NRA No. NNX08AE87A) to San Jose State University (PI: Brian. F. Gore@nasa.gov). The authors would like to thank NASA's technical monitor (Dr. David Foyle) for his overview of the project and all reviewers for their comments on the present document. The authors acknowledge the invaluable contributions of Jason McCarley and Kelly Steelman-Allen for N-SEEV (noticing-salience, expectancy, effort, and value) model implementation, of Ellen Salud and Shaun Hutchins for work on the meta-analysis, and of Julie Bzostek for model evaluation. NR 51 TC 15 Z9 16 U1 1 U2 13 PU SAGE PUBLICATIONS INC PI THOUSAND OAKS PA 2455 TELLER RD, THOUSAND OAKS, CA 91320 USA SN 0018-7208 J9 HUM FACTORS JI Hum. Factors PD OCT PY 2009 VL 51 IS 5 BP 638 EP 651 DI 10.1177/0018720809349709 PG 14 WC Behavioral Sciences; Engineering, Industrial; Ergonomics; Psychology, Applied; Psychology SC Behavioral Sciences; Engineering; Psychology GA 548MB UT WOS:000273965900002 PM 20196290 ER PT J AU Thomas, PC James, PB Calvin, WM Haberle, R Malin, MC AF Thomas, P. C. James, P. B. Calvin, W. M. Haberle, R. Malin, M. C. TI Residual south polar cap of Mars: Stratigraphy, history, and implications of recent changes SO ICARUS LA English DT Article DE Mars, Polar caps; Mars, Atmosphere; Mars, Climate ID ORBITER CAMERA OBSERVATIONS; GLOBAL DUST STORM; INTERANNUAL VARIABILITY; WATER ICE; SUMMER TEMPERATURES; CO2 FROST; VIKING; TES; ATMOSPHERE; REGRESSION AB The residual south polar cap (RSPC) of Mars includes a group of different depositional units of CO2 ice undergoing a variety of erosional processes. Complete summer coverage of the RSPC by similar to 6-m/pixel data of the Context Imager (CTX) on Mars Reconnaissance Orbiter (MRO) has allowed mapping and inventory of the units in the RSPC. Unit maps and estimated thicknesses indicate the total volume of the RSPC is currently <380 km(3), and represents less than 3% of the total mass of the current Mars atmosphere. Scarp retreat rates in the CO2 ice derived from comparison of High Resolution Imaging Science Experiment (HiRISE) data with earlier images are comparable to those obtained for periods up to 3 Mars years earlier. These rates, combined with sizes of depressions suggest that the oldest materials were deposited more than 125 Mars years ago. Most current erosion is by backwasting of scarps 1-12 m in height. This backwasting is initiated by a series of scarp-parallel fractures. In the older, thicker unit these fractures form about every Mars year; in thinner, younger materials they form less frequently. Some areas of the older, thicker unit are lost by downwasting rather than by the scarp retreat. A surprising finding from the HiRISE data is the scarcity of visible layering of RSPC materials, a result quite distinct from previous interpretations of layers in lower resolution images. Layers similar to 0.1 m thick are exposed on the upper surfaces of some areas, but their timescale of deposition is not known. Late summer albedo changes mapped by the CTX images indicate local recycling of ice, although the amounts may be morphologically insignificant. Compact Reconnaissance Imaging Spectrometer for Mars (CRISM) data show that the primary material of all the different forms of the RSPC is CO2 ice with only small admixtures of water ice and dust. (C) 2009 Elsevier Inc. All rights reserved. C1 [Thomas, P. C.] Cornell Univ, Ctr Radiophys & Space Res, Ithaca, NY 14853 USA. [James, P. B.] Space Sci Inst, Boulder, CO 80301 USA. [Calvin, W. M.] Univ Nevada, Dept Geol Sci, Reno, NV 89577 USA. [Haberle, R.] NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA. [Malin, M. C.] Malin Space Sci Syst, San Diego, CA 92191 USA. RP Thomas, PC (reprint author), Cornell Univ, Ctr Radiophys & Space Res, Ithaca, NY 14853 USA. EM pct2@cornell.edu FU Mars Reconnaissance Orbiter FX J. Lougen and L. Posiolova targeted the south polar CTX images that make this study possible. We thank those who targeted and made available the CRISM and HiRISE data so helpful to this study. A variety of technical help was provided by T. Clancy, M. Wolff, S. Lee, B. Cantor, K. Edgett, S. Davis, J. Eagle, B. Carcich, K. Consroe, and G. Patton. Patrick Russell and Sarah Milkovich provided very helpful reviews. Funded in part by the Mars Reconnaissance Orbiter project. NR 59 TC 19 Z9 19 U1 0 U2 9 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD OCT PY 2009 VL 203 IS 2 BP 352 EP 375 DI 10.1016/j.icarus.2009.05.014 PG 24 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 599HW UT WOS:000277903000002 ER PT J AU Parente, M Bishop, JL Bell, JF AF Parente, M. Bishop, J. L. Bell, J. F., III TI Spectral unmixing for mineral identification in pancam images of soils in Gusev crater, Mars SO ICARUS LA English DT Article DE Mars; Surface; Spectroscopy; Data reduction techniques; Image processing; Mineralogy ID ENDMEMBER EXTRACTION ALGORITHMS; REFLECTANCE SPECTROSCOPY; MOSSBAUER-SPECTROSCOPY; MIXTURE ANALYSIS; PATHFINDER; DUST; DISCRIMINATION; ANALOG; SITE; ROCK AB The objective of this work is to propose an automated unmixing technique for the analysis of 11-channel Mars Exploration Rover Panoramic Camera (MER(Pancam) spectra. Our approach is to provide a screening tool for identifying unique/distinct reflectance spectra. We demonstrate the utility of this unmixing technique in a study of the mineralogy of the bright salty soils exposed by the rover wheels in images of Gusev crater regions known as Paso Robles (Sols 400.426), Arad (Sol 721), and Tyrone (Sol 790). The unmixing algorithm is based on a novel derivation of the Nonnegative Matrix Factorization technique and includes added features that preclude the adverse effects of low abundance materials that would otherwise skew the unmixing. In order to create a full 11-channel spectrum out of the left and right eye stereo pairs, we also developed a new registration procedure that includes rectification and disparity calculation of the images. We identified two classes of endmember spectra for the bright soils imaged on Sols 426 and 790. One of these endmember classes is also observed for soils imaged on Sols 400 and 721 and has a unique spectral shape that is distinct from most iron oxide, sulfate and silicate spectra and differs from typical martian surface spectra. Instead, its unique spectral character resembles the spectral shape of the ferric sulfate minerals flbroferrite (Fe3+(SO4)(OH) center dot 5H(2)O) and ferricopiapite((Fe3+.Al.Mg) Fe-5(3+) (SO4)(6)(OH)(2) center dot 20H(2)O) and the phosphate mineral ferristrunzite ((Mn2+. Fe-2(3+))(2)(PO4)(2)(OH)(2) center dot 6H(2)O). The other endmember class is less consistent with specific minerals and is likely a mixture of altered volcanic material and some bright salts. Further analyses of data from Sols 400 and 790 using an anomaly detection algorithm as a tool for detecting low abundance materials additionally suggests the identification of the sulfate mineral paracoquimbite (Fe-2(SO4)(3) center dot 9H(2)O). This spectral study of Pancam images of the bright S- and P-enriched soils of Gusev crater identifies specific ferric sulfate and ferric phosphate minerals that are consistent with the unique spectral properties observed here in the 0.4-1 mu m range. (C) 2009 Elsevier Inc. All rights reserved. C1 [Parente, M.] Stanford Univ, Stanford, CA 94305 USA. [Bishop, J. L.] NASA, SETI Inst, Ames Res Ctr, Mountain View, CA 94043 USA. [Bell, J. F., III] Cornell Univ, Ithaca, NY 14853 USA. RP Parente, M (reprint author), Stanford Univ, Packard Elect Engn Bldg,Room 260,350 Serra Mall, Stanford, CA 94305 USA. EM mario.parente@stanford.edu FU Mars Data Analysis Program [NNX06AD88] FX Funding for this project was provided by the Mars Data Analysis Program (Grant #NNX06AD88). The authors thank W. Farrand and J. Johnson for helpful editorial comments. Spectra made available to the project by M. Lane, D. Dyar, and E. Clouds are much appreciated. NR 76 TC 12 Z9 12 U1 0 U2 10 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD OCT PY 2009 VL 203 IS 2 BP 421 EP 436 DI 10.1016/j.icarus.2009.04.029 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 599HW UT WOS:000277903000006 ER PT J AU Milani, A Chesley, SR Sansaturio, ME Bernardi, F Valsecchi, GB Arratia, O AF Milani, Andrea Chesley, Steven R. Sansaturio, Maria Eugenia Bernardi, Fabrizio Valsecchi, Giovanni B. Arratia, Oscar TI Long term impact risk for (101955) 1999 RQ(36) SO ICARUS LA English DT Article DE Asteroids; Dynamics; Impact processes; Orbit determination ID EARTH; ENCOUNTERS AB The potentially hazardous Asteroid (101955) 1999 RQ(36) has a possibility of colliding with the Earth in the latter half of the 22nd century, well beyond the traditional 100-year time horizon for routine impact monitoring. The probabilities accumulate to a total impact probability of approximately 10(-3), with a pair of closely related routes to impact in 2182 comprising more than half of the total. The analysis of impact possibilities so far in the future is strongly dependent on the action of the Yarkovsky effect, which raises new challenges in the careful assessment of longer term impact hazards. Even for asteroids with very precisely determined orbits, a future close approach to Earth can scatter the possible trajectories to the point that the problem becomes like that of a newly discovered asteroid with a weakly determined orbit. If the scattering takes place late enough so that the target plane uncertainty is dominated by Yarkovsky accelerations then the thermal properties of the asteroid, which are typically unknown, play a major role ill the impact assessment. In contrast, if the strong planetary interaction takes place sooner, while the Yarkovsky dispersion is still relatively small compared to that derived from the measurements, then precise modeling of the nongravitational acceleration may be unnecessary. (C) 2009 Elsevier Inc. All rights reserved. C1 [Milani, Andrea; Bernardi, Fabrizio] Univ Pisa, Dept Math, I-56127 Pisa, Italy. [Chesley, Steven R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Sansaturio, Maria Eugenia; Arratia, Oscar] Univ Valladolid, ETS Ingn Ind, E-47011 Valladolid, Spain. [Bernardi, Fabrizio; Valsecchi, Giovanni B.] INAF, IASF Roma, I-00133 Rome, Italy. RP Milani, A (reprint author), Univ Pisa, Dept Math, Largo Pontecorvo 5, I-56127 Pisa, Italy. EM milani@dm.unipi.it RI Arratia, Oscar/B-2599-2017; OI Arratia, Oscar/0000-0001-6825-6895; Valsecchi, Giovanni/0000-0002-2915-1465 FU Italian Space Agency [ASI/INAF 1/015/07/0]; Spanish Ministerio de Ciencia y Tecnologia [AYA2007-64592]; Junta de Castilla y Leon [VA060A07]; National Aeronautics and Space Administration FX The authors have been supported by: the Italian Space Agency, under contract ASI/INAF 1/015/07/0, Tasks 3130 and 3430 (A.M., G.B.V. and F.B.); the Spanish Ministerio de Ciencia y Tecnologia through the grant AYA2007-64592 and by the Junta de Castilla y Leon through the grant VA060A07 (M.E.S. and O.A.). The work of S.R.C. was conducted at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. NR 23 TC 32 Z9 32 U1 0 U2 4 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD OCT PY 2009 VL 203 IS 2 BP 460 EP 471 DI 10.1016/j.icarus.2009.05.029 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 599HW UT WOS:000277903000009 ER PT J AU Veres, P Jedicke, R Wainscoat, R Granvik, M Chesley, S Abe, S Denneau, L Grav, T AF Veres, Peter Jedicke, Robert Wainscoat, Richard Granvik, Mikael Chesley, Steve Abe, Shinsuke Denneau, Larry Grav, Tommy TI Detection of Earth-impacting asteroids with the next generation all-sky surveys SO ICARUS LA English DT Article DE Asteroids; Near-Earth objects; Meteors; Impact processes ID SURVEY SIMULATIONS; SIZE DISTRIBUTION; OBJECTS; SYSTEM; ORBITS; DISTRIBUTIONS; PROSPECTS; PROGRAM; NETWORK; COMET AB We have performed a simulation of a next generation sky survey's (Pan-STARES 1) efficiency for detecting Earth-impacting asteroids. The steady-state sky-plane distribution of the impactors long before impact is concentrated towards small solar elongations (Chesley, SR., Spahr TB., 2004. In: Belton, MTS., Morgan, T.H., Samarashinha, N.H., Yeomans, D.K. (Eds.), Mitigation of Hazardous Comets and Asteroids. Cambridge University Press, Cambridge, pp. 22-37) but we find that there is interesting and potentially exploitable behavior in the sky-plane distribution in the months leading up to impact. The next generation surveys will find most of the dangerous impactors (>140 m diameter) during their decade-long survey missions though there is the potential to miss difficult objects with long synodic periods appearing in the direction of the Sun, as well as objects with long orbital periods that spend much of their time far from the Sun and Earth. A space-based platform that can observe close to the Sun may be needed to identify many of the potential impactors that spend much of their time interior to the Earth's orbit. The next generation surveys have a good chance of imaging a bolide like 2008 TC3 before it enters the atmosphere but the difficulty will lie in obtaining enough images in advance of impact to allow an accurate pre-impact orbit to be computed. (C) 2009 Elsevier Inc. All rights reserved. C1 [Jedicke, Robert; Wainscoat, Richard; Granvik, Mikael; Denneau, Larry] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Veres, Peter] Comenius Univ, Fac Math Phys & Informat, Bratislava 84248, Slovakia. [Chesley, Steve] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Abe, Shinsuke] Natl Cent Univ, Inst Astron, Jhongli 320, Taoyuan County, Taiwan. [Grav, Tommy] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. RP Jedicke, R (reprint author), Univ Hawaii, Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA. EM jedicke@ifa.hawaii.edu OI Granvik, Mikael/0000-0002-5624-1888 FU National Aeronautics and Space Administration [NNX07AL28G]; United States Air Force Research Laboratory (AFRL, Albuquerque, NM) [F29601-02-1-0268.]; National Science Foundation [AST-0551161, AST-0132798]; Department of Energy; LSSTC Institutional Members; National Scholarship Programme of the Slovak Republic; European Social Fund; Comenius University [UK/399/2008]; VEGA [1/0636/09] FX This work was performed in collaboration with Spacewatch, LSSTC, CMU's AUTON lab, and the AstDyS team (Andrea Milani, Giovanni Gronchi and Zoran Knezevic). Steve Chesley's work was conducted at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. The design and construction of the Panoramic Survey Telescope and Rapid Response System by the University of Hawaii Institute for Astronomy is funded by the United States Air Force Research Laboratory (AFRL, Albuquerque, NM) through Grant No. F29601-02-1-0268. MOPS is also supported by a grant (NNX07AL28G) to Robert Jedicke from the NASA NEOO program. Andrea Milani, Giovanni Gronchi and Zoran Knezevic of the AstDyS group provided critical orbit determination software to the MOPS team. The MOPS is currently being developed in association with the Large Synoptic Survey Telescope Corporation (LSSTC). The LSSTC's research and development effort is funded in part by the National Science Foundation under Scientific Program Order No. 9 (AST-0551161) through Cooperative Agreement AST-0132798. Additional funding to the LSSTC comes from private donations, in-kind support at Department of Energy laboratories and other LSSTC Institutional Members. Veres was supported by the National Scholarship Programme of the Slovak Republic, the European Social Fund, a Grant from Comenius University (No. UK/399/2008) and VEGA Grant No. 1/0636/09. NR 60 TC 17 Z9 17 U1 3 U2 7 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 J9 ICARUS JI Icarus PD OCT PY 2009 VL 203 IS 2 BP 472 EP 485 DI 10.1016/j.icarus.2009.05.010 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 599HW UT WOS:000277903000010 ER PT J AU Hurford, TA Bills, BG Helfenstein, P Greenberg, R Hoppa, GV Hamilton, DP AF Hurford, T. A. Bills, B. G. Helfenstein, P. Greenberg, R. Hoppa, G. V. Hamilton, D. P. TI Geological implications of a physical libration on Enceladus SO ICARUS LA English DT Article DE Tectonics; Enceladus ID EUROPA; FEATURES AB Given the non-spherical shape of Enceladus [Thomas et al., 2007], the satellite will experience gravitational torques that will cause it to physically librate as it orbits Saturn. Physical libration would produce a diurnal oscillation in the longitude of Enceladus' tidal bulge, which could have a profound effect on the diurnal tidal stresses experienced by the surface of the satellite. Although Cassini ISS has placed an observational upper limit on the amplitude of Enceladus' libration, smaller amplitudes can still have geologically significant consequences. Here we present the first detailed description of how physical libration affects tidal stresses and how those stresses might then affect geological processes including crack formation and propagation, south polar eruption activity, and tidal heating. Our goal is to provide a framework for testing the hypothesis that geologic features on Enceladus are produced by tidal stresses from diurnal librations of the satellite. Published by Elsevier Inc. C1 [Hurford, T. A.] NASA, Goddard Space Flight Ctr, Planetary Syst Lab, Greenbelt, MD 20771 USA. [Bills, B. G.] Jet Prop Lab, Pasadena, CA 90119 USA. [Bills, B. G.] Univ Calif San Diego, Scripps Inst Oceanog, Inst Geophys & Planetary Phys, La Jolla, CA 92093 USA. [Helfenstein, P.] Cornell Univ, CRSR, Ithaca, NY 14853 USA. [Greenberg, R.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Hoppa, G. V.] Raytheon Co, Woburn, MA 01801 USA. [Hamilton, D. P.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. RP Hurford, TA (reprint author), NASA, Goddard Space Flight Ctr, Planetary Syst Lab, Greenbelt, MD 20771 USA. EM terry.a.hurford@nasa.gov RI Hurford, Terry/F-2625-2012 FU NASA FX This work was supported by NASA Grants issued to T.H. and P.H. through the Cassini Data Analysis Program. NR 32 TC 18 Z9 19 U1 0 U2 17 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 J9 ICARUS JI Icarus PD OCT PY 2009 VL 203 IS 2 BP 541 EP 552 DI 10.1016/j.icarus.2009.04.025 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 599HW UT WOS:000277903000015 ER PT J AU Newman, SF Buratti, BJ Brown, RH Jaumann, R Bauer, J Momary, T AF Newman, Sarah F. Buratti, B. J. Brown, R. H. Jaumann, R. Bauer, J. Momary, T. TI Water ice crystallinity and grain sizes on Dione SO ICARUS LA English DT Article DE Geological processes; Ices; IR spectroscopy; Saturn, Satellites ID ENCELADUS SURFACE; INFRARED-SPECTRA; SOLAR-SYSTEM; CASSINI-VIMS; IRRADIATION; TETHYS; RHEA AB Saturn's satellite Dione is becoming an increasingly important object in the outer Solar System, as evidence for its current activity accumulates. Infrared observations of the surface can provide clues to the history of the body and currently active processes. Using data from the Cassini Visual and Infrared Mapping Spectrometer (VIMS), we perform three sets of analyses that are sensitive to the ice state, temperature, thermal history, grain size and composition of surface ice. These are calculation of a "crystallinity factor", spectral ratios and water ice band depths. In our analysis, we focus on the dichotomy between the wispy and dark terrain on Dione's trailing hemisphere, to better understand the source of the different materials and their current properties. Our results suggest two different scenarios: (1) the ice from the wispy region has a higher crystallinity and water ice content than the dark region or (2) the wispy region contains larger grains. Both of these models imply recent geologic activity on Diane. Published by Elsevier Inc. C1 [Newman, Sarah F.; Buratti, B. J.; Bauer, J.; Momary, T.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Brown, R. H.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Jaumann, R.] German Aerosp Ctr DLR, D-12489 Berlin, Germany. RP Newman, SF (reprint author), Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA. EM sfdnewman@gmail.com FU National Aeronautics and Space Administration; New Graduate Hire Program FX This work was carried out by the Jet Propulsion Laboratory, Caltech, under contract to the National Aeronautics and Space Administration. We acknowledge support from the Cassini project and from the New Graduate Hire Program at J.P.L. NR 29 TC 3 Z9 3 U1 0 U2 2 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD OCT PY 2009 VL 203 IS 2 BP 553 EP 559 DI 10.1016/j.icarus.2009.04.034 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 599HW UT WOS:000277903000016 ER PT J AU DiSanti, MA Villanueva, GL Milam, SN Zack, LN Bonev, BP Mumma, MJ Ziurys, LM Anderson, WM AF DiSanti, Michael A. Villanueva, Geronimo L. Milam, Stefanie N. Zack, Lindsay N. Bonev, Boncho P. Mumma, Michael J. Ziurys, Lucy M. Anderson, William M. TI A multi-wavelength study of parent volatile abundances in Comet C/2006 M4 (SWAN) SO ICARUS LA English DT Article DE Comets, Composition; Comets, Origin ID O1 HALE-BOPP; C/1995 O1; CARBON-MONOXIDE; ORGANIC COMPOSITION; KUIPER-BELT; INFRARED OBSERVATIONS; WATER PRODUCTION; OORT CLOUD; FRAGMENT-C; SOLID CO AB Volatile organic emissions were detected post-perihelion in the long-period Comet C/2006 M4 (SWAN) in October and November 2006. Our study combines target-of-opportunity infrared observations using the Cryogenic Echelle Spectrometer (CSHELL) at the NASA-IR-FE 3-in telescope, and millimeter wavelength observations using the Arizona Radio Observatory (ARO) 12-m telescope. Five parent volatiles were measured with CSHELL (H(2)O, CO, CH(3)OH, CH(4), and C(2)H(6)), and two additional species (HCN and CS) were measured with the ARO 12-m. These revealed highly depleted CO and somewhat enriched CH3OH compared with abundances observed in the dominant group of long-period (Oort cloud) comets in our sample and similar to those observed recently in Comet 8P/Tuttle. This may indicate highly efficient H-atom addition to CO at very low temperature (similar to 10-20 K) on the surfaces of interstellar (pre-cometary) grains. Comet C/2006 M4 had nearly "normal" C(2)H(6) and CH(4), suggesting a processing history similar to that experienced by the dominant group. When compared with estimated water production at the time of the millimeter observations. HCN was slightly depleted compared with the normal abundance in comets based on IR observations but was consistent with the majority of values from the millimeter. The ratio CS/HCN in C/2006 M4 was within the range measured in ten comets at millimeter wavelengths. The higher apparent H-atom conversion efficiency compared with most comets may indicate that the icy grains incorporated into C/2006 M4 were exposed to higher H-atom densities, or alternatively to similar densities but for a longer period of time. (C) 2009 Elsevier Inc. All rights reserved. C1 [DiSanti, Michael A.; Villanueva, Geronimo L.; Bonev, Boncho P.; Mumma, Michael J.; Anderson, William M.] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA. [Villanueva, Geronimo L.; Bonev, Boncho P.; Anderson, William M.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA. [Milam, Stefanie N.] SETI Inst, Moffett Field, CA 94035 USA. [Milam, Stefanie N.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Zack, Lindsay N.; Ziurys, Lucy M.] Univ Arizona, Dept Chem, Dept Astron, Tucson, AZ 85721 USA. RP DiSanti, MA (reprint author), NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA. EM michael.a.disanti@nasa.gov RI Milam, Stefanie/D-1092-2012; mumma, michael/I-2764-2013 OI Milam, Stefanie/0000-0001-7694-4129; FU NASA [RTOP 344-32-98, RTOP 344-53-51, CAN-02-OSS-02] FX This work was supported by the NASA Planetary Astronomy (RTOP 344-32-98) and Astrobiology (RTOP 344-53-51) Programs. Research at the Arizona Radio Observatory was supported by the NASA Astrobiology Institute under Cooperative Agreement No. CAN-02-OSS-02 issued through the Office of Space Sciences. We thank IRTF director Alan Tokunaga for granting target-of-opportunity observations on short notice, and Eric Volquardsen and Paul Sears for their expertise and assistance in conducting these difficult daytime CSHELL observations of C/2006 M4 (SWAN). The NASA-IRTF is operated by the University of Hawaii under Cooperative Agreement NCC 5-538 with the NASA-OSS Planetary Astronomy Program. The authors 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 62 TC 10 Z9 10 U1 0 U2 2 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 J9 ICARUS JI Icarus PD OCT PY 2009 VL 203 IS 2 BP 589 EP 598 DI 10.1016/j.icarus.2009.05.026 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 599HW UT WOS:000277903000019 ER PT J AU Barnes, R Quinn, TR Lissauer, JJ Richardson, DC AF Barnes, Rory Quinn, Thomas R. Lissauer, Jack J. Richardson, Derek C. TI N-Body simulations of growth from 1 km planetesimals at 0.4 AU SO ICARUS LA English DT Article DE Origin, Solar system; Planetesimals; Planetary formation; Earth ID TERRESTRIAL PLANET FORMATION; GRAVITATIONAL-INSTABILITY; PROTOPLANETARY DISK; RUNAWAY GROWTH; SOLAR NEBULA; ACCRETION; EVOLUTION; DYNAMICS; SYSTEMS; ACCUMULATION AB We present N-body simulations of planetary accretion beginning with 1 km radius planetesimals in orbit about a 1 M star at 0.4 AU. The initial disk of planetesimals contains too many bodies for any current N-body code to integrate; therefore, we model a sample patch of the disk. Although this greatly reduces the number of bodies, we still track in excess of 10 particles. We consider three initial velocity distributions and monitor the growth of the planetesimals. The masses of some particles increase by more than a factor of 100. Additionally, the escape speed of the largest particle grows considerably faster than the velocity dispersion of the particles, suggesting impending runaway growth, although no particle grows large enough to detach itself from the power law size-frequency distribution. These results are in general agreement with previous statistical and analytical results. We compute rotation rates by assuming conservation of angular momentum around the center of mass at impact and that merged planetesimals relax to spherical shapes. At the end of our simulations, the majority of bodies that have undergone at least one merger are rotating faster than the breakup frequency. This implies that the assumption of completely inelastic collisions (perfect accretion), which is made in most simulations of planetary growth at sizes 1 km and above, is inappropriate. Our simulations reveal that, subsequent to the number of particles in the patch having been decreased by mergers to half its initial value, the presence of larger bodies in neighboring regions of the disk may limit the validity of simulations employing the patch approximation. (C) 2009 Elsevier Inc. All rights reserved. C1 [Barnes, Rory; Quinn, Thomas R.] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Barnes, Rory] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Lissauer, Jack J.] NASA, Ames Res Ctr, Space Sci & Astrobiol Div, Moffett Field, CA 94035 USA. [Richardson, Derek C.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. RP Barnes, R (reprint author), Univ Washington, Dept Astron, Seattle, WA 98195 USA. EM rory@astro.washington.edu OI Richardson, Derek C/0000-0002-0054-6850 NR 52 TC 10 Z9 10 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 J9 ICARUS JI Icarus PD OCT PY 2009 VL 203 IS 2 BP 626 EP 643 DI 10.1016/j.icarus.2009.03.042 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 599HW UT WOS:000277903000022 ER PT J AU Hudson, RL Moore, MH Raines, LL AF Hudson, R. L. Moore, M. H. Raines, L. L. TI Ethane ices in the outer Solar System: Spectroscopy and chemistry SO ICARUS LA English DT Article DE Ices, IR spectroscopy; Trans-neptunian objects; Cosmic rays; Organic chemistry ID DIFFUSE INTERSTELLAR-MEDIUM; PLUTO; METHANE; HYDROCARBONS; CONSTRAINTS; ACETYLENE; TRITON; PHASE AB We report recent experiments on ethane ices made at temperatures applicable to the outer Solar System. New near- and mid-infrared data for crystalline and amorphous ethane, including new spectra for a seldom-studied solid phase that exists at 35-55 K, are presented along with radiation-chemical experiments showing the formation of more-complex hydrocarbons. Published by Elsevier Inc. C1 [Hudson, R. L.; Raines, L. L.] Eckerd Coll, Dept Chem, St Petersburg, FL 33711 USA. [Hudson, R. L.; Moore, M. H.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Hudson, RL (reprint author), Eckerd Coll, Dept Chem, 4200 54th Ave S, St Petersburg, FL 33711 USA. EM hudsonrl@eckerd.edu RI Hudson, Reggie/E-2335-2012 FU NASA [NAG-5-1843]; NASA Astrobiology Institute through the Goddard Center for Astrobiology FX NASA funding through the Planetary Geology and Geophysics, Cassini Data Analysis, and Planetary Atmospheres programs is acknowledged. RLH also acknowledges the support or NASA for Grant NAG-5-1843. LLR worked on this project as a summer astrobiology intern at the Goddard Space Flight Center, and all authors received partial support: from the NASA Astrobiology Institute through the Goddard Center for Astrobiology. The experimental assistance of Paul Cooper and Robert Ferrante is acknowledged, as is the work of Zan Peeters on IR band strengths. NR 21 TC 21 Z9 21 U1 1 U2 9 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 J9 ICARUS JI Icarus PD OCT PY 2009 VL 203 IS 2 BP 677 EP 680 DI 10.1016/j.icarus.2009.06.026 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 599HW UT WOS:000277903000026 ER PT J AU Rabbani, T Munier, S Dorchies, D Malaterre, PO Bayen, A Litrico, X AF Rabbani, Tarek Munier, Simon Dorchies, David Malaterre, Pierre-Olivier Bayen, Alexandre Litrico, Xavier TI Flatness-Based Control of Open-Channel Flow in an Irrigation Canal Using SCADA SO IEEE CONTROL SYSTEMS MAGAZINE LA English DT Article ID SYSTEMS C1 [Litrico, Xavier] Cemagref, French Publ Res Inst Environm Engn, Montpellier, France. [Bayen, Alexandre] Minist Def, Lab Rech Balist & Aerodynam, Autonomous Nav Lab, Vernon, France. [Bayen, Alexandre] Univ Calif Berkeley, Dept Civil & Environm Engn, Berkeley, CA 94720 USA. [Litrico, Xavier] Cemagref, UMR G EAU, F-34196 Montpellier 5, France. RP Rabbani, T (reprint author), NASA, Ames Res Ctr, Washington, DC 20546 USA. EM trabbani@berkeley.edu RI Munier, Simon/D-3849-2011; Dorchies, David/E-2325-2015 OI Dorchies, David/0000-0002-6595-7984 FU France-Berkeley Fund FX The financial help of the France-Berkeley Fund is gratefully acknowledged. We thank Celine Hugodot, director of the Canal de Gignac, for her help concerning the experiments. NR 15 TC 19 Z9 19 U1 0 U2 9 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 1066-033X J9 IEEE CONTR SYST MAG JI IEEE Control Syst. Mag. PD OCT PY 2009 VL 29 IS 5 BP 22 EP 30 DI 10.1109/MCS.2009.933524 PG 9 WC Automation & Control Systems SC Automation & Control Systems GA 498LB UT WOS:000270140500004 ER PT J AU Bedrossian, NS Bhatt, S Kang, W Ross, IM AF Bedrossian, Nazareth S. Bhatt, Sagar Kang, Wei Ross, I. Michael TI Zero-Propellant Maneuver Guidance ROTATING THE INTERNATIONAL SPACE STATION WITH COMPUTATIONAL DYNAMIC OPTIMIZATION SO IEEE CONTROL SYSTEMS MAGAZINE LA English DT Article ID PSEUDOSPECTRAL METHODS; CONVERGENCE; SYSTEMS C1 [Bedrossian, Nazareth S.] NASA, Lyndon B Johnson Space Ctr, Washington, DC 20546 USA. [Bedrossian, Nazareth S.] Charles Stark Draper Lab Inc, Houston, TX 77058 USA. [Kang, Wei] Naval Postgrad Sch, Fac Appl Math, Montreal, PQ, Canada. RP Bedrossian, NS (reprint author), NASA, Lyndon B Johnson Space Ctr, Washington, DC 20546 USA. EM naz@draper.com FU NASA [NNJ06HC37C] FX The thesis [ 25] was joint research between The Charles Stark Draper Laboratory, Inc., under NASA contract NNJ06HC37C and Prof. Yin Zhang of the Computational and Applied Mathematics department at Rice University. The last author gratefully acknowledges partial funding provided by NASA Glenn Research Center to perform a preliminary ZPM analysis using pseudospectral dynamic optimization. NR 34 TC 16 Z9 20 U1 1 U2 6 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 1066-033X J9 IEEE CONTR SYST MAG JI IEEE Control Syst. Mag. PD OCT PY 2009 VL 29 IS 5 BP 53 EP 73 DI 10.1109/MCS.2009.934089 PG 21 WC Automation & Control Systems SC Automation & Control Systems GA 498LB UT WOS:000270140500007 ER PT J AU Walker, JP Kim, EJ England, AW AF Walker, Jeffrey P. Kim, Edward J. England, Anthony W. TI Introduction to the Special Issue on Airborne Field Campaigns for Soil Moisture SO IEEE GEOSCIENCE AND REMOTE SENSING LETTERS LA English DT Editorial Material DE Special issues and sections; Soil moisture; Soil properties; Soil texture; SMOS mission; SMAP mission C1 [Walker, Jeffrey P.] Univ Melbourne, Dept Civil & Environm Engn, Melbourne, Vic 3010, Australia. [Kim, Edward J.] NASA, Goddard Space Flight Ctr, Hydrospher & Biospher Sci Lab, Greenbelt, MD 20771 USA. [England, Anthony W.] Univ Michigan, Coll Engn, Ann Arbor, MI 48109 USA. RP Walker, JP (reprint author), Univ Melbourne, Dept Civil & Environm Engn, Melbourne, Vic 3010, Australia. RI Walker, Jeffrey/D-2624-2009 NR 0 TC 5 Z9 5 U1 0 U2 5 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 1545-598X J9 IEEE GEOSCI REMOTE S JI IEEE Geosci. Remote Sens. Lett. PD OCT PY 2009 VL 6 IS 4 BP 623 EP 624 DI 10.1109/LGRS.2009.2026982 PG 2 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA 506GD UT WOS:000270761500001 ER PT J AU Bindlish, R Jackson, T Sun, RJ Cosh, M Yueh, S Dinardo, S AF Bindlish, Rajat Jackson, Thomas Sun, Ruijing Cosh, Michael Yueh, Simon Dinardo, Steve TI Combined Passive and Active Microwave Observations of Soil Moisture During CLASIC SO IEEE GEOSCIENCE AND REMOTE SENSING LETTERS LA English DT Article DE Active/passive microwave observations; hydrology; soil moisture; Soil Moisture Active Passive (SMAP) ID VEGETATION; SENSOR; BAND AB An important research direction in advancing higher spatial resolution and better accuracy in soil moisture remote sensing is the integration of active and passive microwave observations. In an effort to address this objective, an airborne instrument, the passive/active L-band sensor (PALS), was flown over two watersheds as part of the cloud and land surface interaction campaign (CLASIC) conducted in Oklahoma in 2007. Eleven flights were conducted over each watershed during the field campaign. Extensive ground observations (soil moisture, soil temperature, and vegetation) were made concurrent with the PALS measurements. Extremely wet conditions were encountered. As expected from previous research, the radiometer-based retrievals were better than the radar retrievals. The standard error of estimates (SEEs) of the retrieved soil moisture using only the PALS radiometer data were 0.048 m(3)/m(3) for Fort Cobb (FC) and 0.067 m(3)/m(3) for the Little Washita ( LW) watershed. These errors were higher than typically observed, which is likely the result of the unusually high soil moisture and standing water conditions. The radar-only-based retrieval SEEs were 0.092 m(3)/m(3) for FC and 0.079 m(3)/m(3) for LW. Radar retrievals in the FC domain were particularly poor due to the high vegetation water content of the agricultural fields. These results indicate the potential for estimating soil moisture for low-vegetation water content domains from radar observations using a simple vegetation model. Results also showed the compatibility between passive and active microwave observations and the potential for combining the two approaches. C1 [Bindlish, Rajat] ARS, Sci Syst & Applicat Inc, Hydrol & Remote Sensing Lab, USDA, Beltsville, MD 20705 USA. [Yueh, Simon; Dinardo, Steve] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Bindlish, R (reprint author), ARS, Sci Syst & Applicat Inc, Hydrol & Remote Sensing Lab, USDA, Beltsville, MD 20705 USA. RI Cosh, MIchael/A-8858-2015 OI Cosh, MIchael/0000-0003-4776-1918 FU National Aeronautics and Space Administration FX Manuscript received September 15, 2008; revised January 22, 2009. Current version published October 14, 2009. The work described in this letter was supported by the National Aeronautics and Space Administration. NR 10 TC 29 Z9 30 U1 0 U2 8 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 1545-598X J9 IEEE GEOSCI REMOTE S JI IEEE Geosci. Remote Sens. Lett. PD OCT PY 2009 VL 6 IS 4 BP 644 EP 648 DI 10.1109/LGRS.2009.2028441 PG 5 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA 506GD UT WOS:000270761500006 ER PT J AU Lary, DJ Remer, LA MacNeill, D Roscoe, B Paradise, S AF Lary, D. J. Remer, L. A. MacNeill, D. Roscoe, B. Paradise, S. TI Machine Learning and Bias Correction of MODIS Aerosol Optical Depth SO IEEE GEOSCIENCE AND REMOTE SENSING LETTERS LA English DT Article DE Aerosol optical depth (AOD); machine learning; neural networks; support vector machines (SVMs) ID SUPPORT VECTOR MACHINES AB Machine-learning approaches ( neural networks and support vector machines) are used to explore the reasons for a persistent bias between aerosol optical depth (AOD) retrieved from the MODerate resolution Imaging Spectroradiometer (MODIS) and the accurate ground-based Aerosol Robotic Network. While this bias falls within the expected uncertainty of the MODIS algorithms, there is room for algorithm improvement. The results of the machine-learning approaches suggest a link between the MODIS AOD biases and surface type. MODIS-derived AOD may be showing dependence on the surface type either because of the link between surface type and surface reflectance or because of the covariance between aerosol properties and surface type. C1 [Lary, D. J.] Univ Maryland, Joint Ctr Earth Syst Technol, Catonsville, MD 21228 USA. [Lary, D. J.] NASA, Goddard Space Flight Ctr, Software Integrat & Visualizat Off, Greenbelt, MD 20771 USA. [MacNeill, D.; Roscoe, B.] NASA, Goddard Space Flight Ctr, DEVELOP Program, Greenbelt, MD 20771 USA. [Paradise, S.] NASA, Jet Prop Lab, Pasadena, CA 91109 USA. RP Lary, DJ (reprint author), Univ Maryland, Joint Ctr Earth Syst Technol, Catonsville, MD 21228 USA. RI Lary, David/A-6163-2010 FU National Aeronautics and Space Administration (NASA) [NNG06GB78G, NNX06AG04G, NNX06AF29G, NNX07AD49G] FX Manuscript received February 18, 2009; revised March 16, 2009 and April 22, 2009. First published July 7, 2009; current version published October 14, 2009. This work was supported in part by the National Aeronautics and Space Administration (NASA) through the Awards NNG06GB78G, NNX06AG04G, NNX06AF29G, and NNX07AD49G and in part by the NASA Goddard Space Flight Center student DEVELOP Program. NR 20 TC 28 Z9 28 U1 7 U2 13 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1545-598X EI 1558-0571 J9 IEEE GEOSCI REMOTE S JI IEEE Geosci. Remote Sens. Lett. PD OCT PY 2009 VL 6 IS 4 BP 694 EP 698 DI 10.1109/LGRS.2009.2023605 PG 5 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA 506GD UT WOS:000270761500017 ER PT J AU Rengarajan, SR Zawadzki, MS Hodges, RE AF Rengarajan, Sembiam R. Zawadzki, Mark S. Hodges, Richard E. TI Design, Analysis, and Development of a Large Ka-Band Slot Array for Digital Beam-Forming Application SO IEEE TRANSACTIONS ON ANTENNAS AND PROPAGATION LA English DT Article DE Array design; method of moments (MoM); slot arrays; waveguide arrays ID RECTANGULAR WAVE-GUIDES; SHUNT SLOTS AB This paper discusses the design, analysis, and development of a large Ka-band slot array for digital beam-forming application. The array consists of 160 x 160 elements in 16 subarrays for producing 16 digital beams in the receive mode.. Infinite array mutual coupling model has been employed in the design and analysis models. Challenges posed in meeting the pattern and return loss specifications because of manufacturing tolerances are discussed. Measured return loss and pattern characteristics of 10 x 40 slot array modules as well as results on a 1 m x 1 m demonstration array are presented. C1 [Rengarajan, Sembiam R.] Calif State Univ Northridge, Northridge, CA 91330 USA. [Rengarajan, Sembiam R.; Zawadzki, Mark S.; Hodges, Richard E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Rengarajan, SR (reprint author), Calif State Univ Northridge, Northridge, CA 91330 USA. EM srengarajan@csun.edu; mark.s.zawadzki@jpl.nasa.gov; richard.e.hodges@jpl.nasa.gov FU National Aeronautics and Space Administration FX This work was supported by the Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, under a contract with National Aeronautics and Space Administration. NR 15 TC 14 Z9 14 U1 0 U2 3 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 0018-926X J9 IEEE T ANTENN PROPAG JI IEEE Trans. Antennas Propag. PD OCT PY 2009 VL 57 IS 10 BP 3103 EP 3109 DI 10.1109/TAP.2009.2028674 PG 7 WC Engineering, Electrical & Electronic; Telecommunications SC Engineering; Telecommunications GA 505UP UT WOS:000270723600016 ER PT J AU Pogorzelski, RJ AF Pogorzelski, Ronald J. TI Extended Probe Instrument Calibration (EPIC) for Accurate Spherical Near-Field Antenna Measurements SO IEEE TRANSACTIONS ON ANTENNAS AND PROPAGATION LA English DT Article DE Anechoic chambers (electromagnetic); antenna measurements; near-field far-field transformation AB A probe calibration technique is described that removes artifacts from spherical near-field antenna measurements. The technique is based on preliminary calibration measurements of a known antenna, a process that characterizes the probe and any stationary objects in the measurement chamber including the walls in terms of a set of correction coefficients. These coefficients are then used in a correction algorithm that recovers the correct antenna pattern from the corrupted measurement data. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Pogorzelski, RJ (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM pogo@jpl.nasa.gov NR 7 TC 3 Z9 3 U1 0 U2 0 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 0018-926X J9 IEEE T ANTENN PROPAG JI IEEE Trans. Antennas Propag. PD OCT PY 2009 VL 57 IS 10 BP 3366 EP 3371 DI 10.1109/TAP.2009.2029392 PG 6 WC Engineering, Electrical & Electronic; Telecommunications SC Engineering; Telecommunications GA 505UP UT WOS:000270723600054 ER PT J AU Zhang, T Hou, ZW Johnson, RW Del Castillo, L Moussessian, A Greenwell, R Blalock, BJ AF Zhang, Tan Hou, Zhenwei Johnson, R. Wayne Del Castillo, Linda Moussessian, Alina Greenwell, Robert Blalock, Benjamin J. TI Flexible Electronics: Thin Silicon Die on Flexible Substrates SO IEEE TRANSACTIONS ON ELECTRONICS PACKAGING MANUFACTURING LA English DT Article DE Flexible electronics; flip chip; thinned die assembly AB Silicon thinned to 50 mu m and less is flexible allowing the fabrication of flexible and conformable electronics. Two techniques have been developed to achieve this goal using thinned die: die flip chip bonded onto flexible substrates [polyimide and liquid crystal polymer (LCP)] and die flip chip laminated onto LCP films. A key to achieving each of these techniques is the thinning of die to a thickness of 50 mu m or thinner. Conventional grinding and polishing can be used to thin to 50 mu m. At 50 mu m, the active die becomes flexible and must be handled by temporarily bonding it to a holder die for assembly. Both reflow solder and thermocompression assembly methods are used. In the case of solder assembly, underfill is used to reinforce the solder joints. With thermocompression bonding of the die to an LCP substrate, the LCP adheres to the die surface, eliminating the need for underfill. C1 [Zhang, Tan; Hou, Zhenwei; Johnson, R. Wayne] Auburn Univ, Dept Elect & Comp Engn, Auburn, AL 36849 USA. [Del Castillo, Linda; Moussessian, Alina] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Greenwell, Robert; Blalock, Benjamin J.] Univ Tennessee, Dept Elect Engn & Comp Sci, Knoxville, TN 37996 USA. RP Zhang, T (reprint author), GE Global Res Ctr, Niskayuna, NY 12309 USA. EM ki4bsd@gmail.com; hou.zhenwei@seagate.com; johnsr7@aubrun.edu; linda.y.delcastillo@jpl.nasa.gov; alina.moussessian@jpl.nasa.gov; rgreenwe@utk.edu; bblalock@eecs.utk.edu FU Jet Propulsion Laboratory/California Institute of Technology Director's Research and Development Fund; NASA FX This work was supported in part by the This work was supported in part by the Jet Propulsion Laboratory/California Institute of Technology Director's Research and Development Fund and in part by the NASA Electronic Parts and Packaging Program. NR 17 TC 17 Z9 17 U1 0 U2 10 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1521-334X J9 IEEE T ELECTRON PACK JI IEEE Trans. Electron. Packag. Manuf. PD OCT PY 2009 VL 32 IS 4 BP 291 EP 300 DI 10.1109/TEPM.2009.2028880 PG 10 WC Engineering, Manufacturing SC Engineering GA 511KJ UT WOS:000271162700010 ER PT J AU Yueh, SH Dinardo, SJ Akgiray, A West, R Cline, DW Elder, K AF Yueh, Simon H. Dinardo, Steve J. Akgiray, Ahmed West, Richard Cline, Donald W. Elder, Kelly TI Airborne Ku-Band Polarimetric Radar Remote Sensing of Terrestrial Snow Cover SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE Microwave remote sensing; radar; snow ID PASSIVE MICROWAVE RESPONSE; SIR-C/X-SAR; DRY SNOW; 35 GHZ; BACKSCATTERING; PARAMETERS; WIND AB Characteristics of the Ku-band polarimetric scatterometer (POLSCAT) data acquired from five sets of aircraft flights in the winter months of 2006-2008 for the second Cold Land Processes Experiment (CLPX-II) in Colorado are described in this paper. The data showed the response of the Ku-band radar echoes to snowpack changes for various types of background vegetation in the study site in north central Colorado. We observed about 0.15-0.5-dB increases in backscatter for every 1 cm of snow-water-equivalent (SWE) accumulation for areas with short vegetation (sagebrush and pasture). The region with the smaller amount of biomass, signified by the backscatter in November, seemed to have the stronger backscatter response to SWE in decibels. The data also showed the impact of surface hoar growth and freeze/thaw cycles, which created large snow-grain sizes, ice crust layers, and ice lenses and consequently increased the radar signals by a few decibels. The copolarized HH/VV backscatter ratio seems to indicate double-bounce scattering between the ground surface and snow or vegetation. The cross-polarized backscatter [vertical-horizontal (VH)] showed not only the influence of vegetation but also the strong response to snow accumulation. The observed HV/VV ratio suggests the importance of multiple scattering or nonspherical scattering geometry of snow grain in the dense-media radiative transfer scattering model. Comparison of the POLSCAT and QuikSCAT data was made and confirmed the effects of mixed terrain covers in the coarse-resolution QuikSCAT data. C1 [Yueh, Simon H.; Dinardo, Steve J.; Akgiray, Ahmed; West, Richard] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Cline, Donald W.] NOAA, Natl Operat Hydrol Remote Sensing Ctr, Natl Weather Serv, Chanhassen, MN 55317 USA. [Elder, Kelly] US Forest Serv, Rocky Mt Res Stn, USDA, Ft Collins, CO 80526 USA. RP Yueh, SH (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM syueh@jpl.nasa.gov; Steve.Dinardo@jpl.nasa.gov; Ahmed.Akgiray@jpl.nasa.gov; richard.west@jpl.nasa.gov; Donald.Cline@noaa.gov; kelder@fs.fed.us FU National Operational Hydrologic Remote Sensing Center; U.S. Forest Service FX The work described in this paper that was performed by the Jet Propulsion Laboratory, California Institute of Technology, Pasadena, was carried out under a contract with the National Aeronautics and Space Administration. Also, the work described here included the contributions by the National Operational Hydrologic Remote Sensing Center and the U.S. Forest Service. NR 23 TC 28 Z9 30 U1 1 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 OCT PY 2009 VL 47 IS 10 BP 3347 EP 3364 DI 10.1109/TGRS.2009.2022945 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 498JR UT WOS:000270136200006 ER PT J AU Bingham, AW McCleese, S Stough, T Deen, RG Hussey, K Toole, N AF Bingham, Andrew W. McCleese, Sean Stough, Timothy Deen, Robert G. Hussey, Kevin Toole, Nicholas TI Earth Science Datacasting: Informed Pull and Information Integration SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE Data distribution; data fusion; data management; Earth science; information extraction; near real time; Really Simple Syndication (RSS) ID ARCHIVES AB The intent of Datacasting is to empower consumers of Earth science data with the ability to extract from a stream of data granules (or files) precisely those granules that are required to meet a predefined need, for example, "Acquire from a MODIS L2 data stream only the granules that contain information about a wild fire in Southern California." Our approach to solving this problem has been to take the concept of Really Simple Syndication (RSS) feeds, for delivering regularly changing web content, and extend this to represent a stream of data granules and deliver regularly changing Earth science data content. In essence, this project is doing for Earth science what Podcasting has done for audio and video. Where Podcasting extended RSS to revolutionize how users access audio and video content provided by various media outlets, so Datacasting extends RSS to provide users with the ability to download data granules provided by Earth science data providers as the data are made available. Moreover, we have taken the concept one step further by creating a solution for filtering on the metadata of a feed in order to identify granules of interest based on user-defined criteria. In this paper, we also show how Datacasting feeds can be combined with other RSS-based feeds to identify relationships between information sources and extract new knowledge, as well as aid the development of new geo-based web services not currently envisaged. C1 [Bingham, Andrew W.; McCleese, Sean; Stough, Timothy; Deen, Robert G.; Hussey, Kevin; Toole, Nicholas] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Bingham, AW (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM andrew.bingham@jpl.nasa.gov; Sean.W.Mccleese@jpl.nasa.gov; stough@jpl.nasa.gov; Robert.G.Deen-104297@jpl.nasa.gov; Kevin.J.Hussey@jpl.nasa.gov; Nicholas.T.Toole@jpl.nasa.gov FU Jet Propulsion Laboratory, California Institute of Technology [NNH05ZDA001N] FX This work was conducted at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the NASA ACCESS Program, 2005, Research Opportunities in Space and Earth Sciences NNH05ZDA001N. NR 11 TC 2 Z9 2 U1 0 U2 2 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 0196-2892 J9 IEEE T GEOSCI REMOTE JI IEEE Trans. Geosci. Remote Sensing PD OCT PY 2009 VL 47 IS 10 BP 3570 EP 3580 DI 10.1109/TGRS.2009.2022324 PG 11 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA 498JR UT WOS:000270136200024 ER PT J AU Carini, GA Chen, W De Geronimo, G Gaskin, JA Keister, JW Li, Z Ramsey, BD Rehak, P Siddons, DP AF Carini, Gabriella A. Chen, Wei De Geronimo, Gianluigi Gaskin, Jessica A. Keister, Jeffrey W. Li, Zheng Ramsey, Brian D. Rehak, Pavel Siddons, David P. TI Performance of a Thin-window Silicon Drift Detector X-Ray Fluorescence Spectrometer SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE LA English DT Article DE Bias voltage; silicon drift detector with hexagonal shaped cathode; thin rectifying p-n junction entrance window with minimum "dead" layer silicon; X-ray energy spectrum ID SPECTROSCOPY AB Several sets of hexagonal Silicon Drift Detector (SDD) arrays were produced by Brookhaven National Laboratory (BNL) and by the commercial vendor, KETEK. These detector arrays were tested at BNL. Each array consists of 14 independent SDD detectors (pixels) and two additional test pixels located at two corners of the array. The side of the detector upon which the X-ray radiation is incident (window side) has a thin junction covering the entire active area. The opposite side (device side) contains a drift-field electrode structure in the form of a hexagonal spiral and an electron collecting anode. There are four guard rings surrounding the 14-pixel array area on each side of the detector. Within each array, seven pixels have aluminum field plates - interrupted spirals (hat stabilize the electric potential under the Si-SiO(2) interface, while the other seven do not. Three bias voltages are applied to control the drift field in the silicon volume; one is applied to a rectifying contact surrounding the central anode (one for each pixel), one is applied to the detector entrance window (common to the full array), and a third Was is applied to a contact oil the outer portion of the spiral, common to all pixels in the array. Some arrays were recently tested in NSLS beam line U3C at BNL. For this work, we installed the complete assemblies in the vacuum and cooled them to -27 degrees C. During this beam run. we collected spectra for energies ranging between 350 and 900 eV in several pixels, some with field plates and others without. The detailed testing results of several arrays are reported here. C1 [Carini, Gabriella A.; Chen, Wei; De Geronimo, Gianluigi; Keister, Jeffrey W.; Li, Zheng; Rehak, Pavel; Siddons, David P.] Brookhaven Natl Lab, Upton, NY 11973 USA. [Gaskin, Jessica A.; Ramsey, Brian D.] NASA, MSFC, Natl Space Sci & Technol Ctr, Huntsville, AL 35805 USA. RP Carini, GA (reprint author), Brookhaven Natl Lab, Upton, NY 11973 USA. FU U. S. Department of Energy [DE-AC02-98CH 10886]; NASA Research Opportunities in Space and Earth Scie