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 Science; Planetary Instrument Definition and Development Program FX Manuscript received March 29, 2009, revised June 23, 2009. Current version published October 07, 2009. This work was supported in part by the U. S. Department of Energy under Contract DE-AC02-98CH 10886 and by the NASA Research Opportunities in Space and Earth Science, Planetary Instrument Definition and Development Program NR 14 TC 17 Z9 17 U1 0 U2 10 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 0018-9499 J9 IEEE T NUCL SCI JI IEEE Trans. Nucl. Sci. PD OCT PY 2009 VL 56 IS 5 BP 2843 EP 2849 DI 10.1109/TNS.2009.2028574 PG 7 WC Engineering, Electrical & Electronic; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA 510OX UT WOS:000271100600009 ER PT J AU Peeters, Z Quinn, R Martins, Z Sephton, MA Becker, L van Loosdrecht, MCM Brucato, J Grunthaner, F Ehrenfreund, P AF Peeters, Z. Quinn, R. Martins, Z. Sephton, M. A. Becker, L. van Loosdrecht, M. C. M. Brucato, J. Grunthaner, F. Ehrenfreund, P. TI Habitability on planetary surfaces: interdisciplinary preparation phase for future Mars missions SO INTERNATIONAL JOURNAL OF ASTROBIOLOGY LA English DT Article DE habitability; Mars soil analogues; planetary organics ID CHROMATOGRAPHY-MASS-SPECTROMETRY; ATACAMA DESERT; MERIDIANI-PLANUM; PROTON IRRADIATION; HYDROGEN-PEROXIDE; ORGANIC-COMPOUNDS; MARTIAN REGOLITH; MICROBIAL LIFE; AMINO-ACIDS; CHILE AB Life on Earth is one of the outcomes of the formation and evolution of our solar system and hits adapted to every explored environment on planet Earth. Recent discoveries have shown that life can exist in extreme environments, such as hydrothermal vents, in deserts and in ice lakes in Antarctica. These findings challenge the definition of the 'planetary habitable zone'. The objective of future international planetary exploration programmes is to implement it long-term plan for the robotic and human exploration of solar system bodies. Mars has been a central object of interest in the context of extraterrestrial life. The search for extinct or extant life on Mars is one of the main goals of space missions to the Red Planet during the next decade. In this paper we describe the investigation of the physical and chemical properties of Mars soil analogues collected in arid deserts. We measure the pH, redox potential and ion concentrations, as well as carbon and amino acid abundances of soils collected from the Atacama desert (Chile and Peru) and the Salten Skov sediment from Denmark. The samples show large differences in their measured properties, even when taken only several meters apart. A desert sample and the Salten Skov sediment were exposed to a simulated Mars environment to test the stability of amino acids in the soils. The presented laboratory and field studies provide limits to exobiological models, evidence on the effects of subsurface mineral matrices, support current and planned space missions and address planetary protection issues. C1 [Peeters, Z.; Ehrenfreund, P.] Leiden Inst Chem, NL-2333 CC Leiden, Netherlands. [Peeters, Z.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Quinn, R.] NASA, Ames Res Ctr, SETI Inst, Moffett Field, CA 94035 USA. [Martins, Z.; Sephton, M. A.] Univ London Imperial Coll Sci Technol & Med, Dept Earth Sci & Engn, London SW7 2AZ, England. [Becker, L.] Johns Hopkins Univ, Baltimore, MD 21218 USA. [van Loosdrecht, M. C. M.] Delft Univ Technol, Fac Sci Appl, Dept Biotechnol, NL-2628 BC Delft, Netherlands. [Brucato, J.] Osserv Astrofis Arcetri, INAF, I-50125 Florence, Italy. [Grunthaner, F.] NASA, Jet Prop Lab, Situ Explorat Technol Grp, Pasadena, CA USA. [Ehrenfreund, P.] George Washington Univ, Elliott Sch Int Affairs, Inst Space Policy, Washington, DC 20052 USA. RP Peeters, Z (reprint author), Leiden Inst Chem, Einsteinweg 55, NL-2333 CC Leiden, Netherlands. RI van Loosdrecht, Mark/B-2738-2009; Martins, Zita/H-4860-2015; OI van Loosdrecht, Mark/0000-0003-0658-4775; Martins, Zita/0000-0002-5420-1081; Sephton, Mark/0000-0002-2190-5402; Brucato, John Robert/0000-0002-4738-5521 FU NWO-VI [016.023.003]; ESA; NASA [NNX08AG78G]; Fundacao para a Ciencia e a Tecnologia [SFRH/BD/10518/2002]; Science and Technology Facilities Council (STFC); ASI [1/015/07/0] FX PE and ZP were supported by grant NWO-VI 016.023.003 and ESA grant for Ground based facilities: 'Simulations of organic compounds and micro-organisms in Martian regolith analogues: SocMar'. This work is conducted in the framework of being the Recognized Cooperating Laboratory/Geochemistry for Mars Express. PE is also supported by NASA grant NNX08AG78G and the NASA Astrobiology Institute NAI. ZP is also supported by NASA grant NNG05GL46G and the Goddard Center for Astrobiology. ZM was supported by Fundacao para a Ciencia e a Tecnologia (scholarship SFRH/BD/10518/2002). ZM and MAS also acknowledge financial support from the Science and Technology Facilities Council (STFC). This research was conducted in the framework of the Mars Express Recognized Cooperating Laboratory for geochemistry. JRB activity is supported by ASI contract 1/015/07/0. We thank Lauren Fletcher for logistic support in the Arequipa desert. NR 65 TC 14 Z9 14 U1 0 U2 24 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 1473-5504 EI 1475-3006 J9 INT J ASTROBIOL JI Int. J. Astrobiol. PD OCT PY 2009 VL 8 IS 4 BP 301 EP 315 DI 10.1017/S1473550409990140 PG 15 WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics; Geology GA 541AU UT WOS:000273383800005 ER PT J AU Sullivan, RM Ghosn, LJ AF Sullivan, Roy M. Ghosn, Louis J. TI Shear moduli for non-isotropic, open cell foams using a general elongated Kelvin foam model SO INTERNATIONAL JOURNAL OF ENGINEERING SCIENCE LA English DT Article DE Foams; Elastic constants; Shear modulus; Kelvin foam model; Elongated cell ID ELASTIC PROPERTIES AB Equations for calculating the shear modulus of non-isotropic, open cell foams in the plane perpendicular to the rise direction and in a plane parallel to the rise direction are derived using an elongated Kelvin foam model. This Kelvin foam model is more general than that employed by previous authors as the size and shape of the unit cell are defined by specifying three independent cell dimensions. The equations for the shear compliances are derived as a function of three unit cell dimensions and the section properties of the cell edges. From the compliance equations, the shear modulus equations are obtained and written as a function of the relative density and two unit cell shape parameters. The dependence of the two shear moduli on the relative density and the two shape parameters is demonstrated. Published by Elsevier Ltd. C1 [Sullivan, Roy M.] NASA, Struct & Mat Div, Glenn Res Ctr, Cleveland, OH 44135 USA. [Ghosn, Louis J.] Ohio Aerosp Inst, Cleveland, OH 44142 USA. RP Sullivan, RM (reprint author), NASA, Struct & Mat Div, Glenn Res Ctr, Cleveland, OH 44135 USA. EM Roy.m.sullivan@nasa.gov; Louis.j.ghosn@nasa.gov FU NASA's Space Shuttle Program FX The authors are grateful for funding from the External Tank Project under NASA's Space Shuttle Program. NR 14 TC 9 Z9 9 U1 0 U2 5 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0020-7225 J9 INT J ENG SCI JI Int. J. Eng. Sci. PD OCT PY 2009 VL 47 IS 10 BP 990 EP 1001 DI 10.1016/j.ijengsci.2009.05.005 PG 12 WC Engineering, Multidisciplinary SC Engineering GA 487LM UT WOS:000269275700003 ER PT J AU Helenbrook, BT Powers, M Shen, HH Metzger, PT AF Helenbrook, B. T. Powers, M. Shen, H. H. Metzger, P. T. TI Continuum Modeling and Discrete Element Simulations of Elastic-Quasi-Static Granular Flow in a Compressing Slot SO JOURNAL OF AEROSPACE ENGINEERING LA English DT Article ID THERMALLY-INDUCED LOADS; SHEAR FLOWS; GRAIN BINS; UNIFORM AB The stress generated by the horizontal compression of a vertical column of granular material is investigated. The column is open at the top so that the material is free to flow upward in the slot as it is compressed. This simple geometry has interesting mechanics because both elastic and frictional regimes coexist, and it is also relevant to problems involving the insulating material in cryogenic storage tanks. Two methods are used to investigate this problem: traditional continuum modeling and discrete element simulation. The continuum model assumes that the column consists of a frictional region near the top of the column and a linearly elastic region near the bottom. Analytic solutions are obtained for each region and predictions for the location of the transition are made based on intersections of the two solutions. A discrete element simulation of the same geometry is performed to compare with the results from the continuum model. Various conditions of wall friction and particle stiffness are simulated. Based on the outcome of this comparison, we verify that in a compressing slot there are essentially two distinct regions: a frictional flow region near the top of the column that results in an exponential increase in stress with depth. This eventually saturates leading to a linear-elastic plane strain region. The location of the transition between these two regions depends on the material properties and the state of the compression. C1 [Helenbrook, B. T.; Powers, M.] Clarkson Univ, Dept Mech & Aerosp Engn, Potsdam, NY 13699 USA. [Shen, H. H.] Clarkson Univ, Dept Civil & Environm Engn, Potsdam, NY 13699 USA. [Metzger, P. T.] NASA, Granular Mech & Regolith Operat Lab, Kennedy Space Ctr, FL 32899 USA. RP Helenbrook, BT (reprint author), Clarkson Univ, Dept Mech & Aerosp Engn, Potsdam, NY 13699 USA. EM helenbrk@clarkson.edu RI Metzger, Philip/R-3136-2016 OI Metzger, Philip/0000-0002-6871-5358 NR 21 TC 0 Z9 0 U1 0 U2 6 PU ASCE-AMER SOC CIVIL ENGINEERS PI RESTON PA 1801 ALEXANDER BELL DR, RESTON, VA 20191-4400 USA SN 0893-1321 J9 J AEROSPACE ENG JI J. Aerosp. Eng. PD OCT PY 2009 VL 22 IS 4 BP 415 EP 422 DI 10.1061/(ASCE)0893-1321(2009)22:4(415) PG 8 WC Engineering, Aerospace; Engineering, Civil SC Engineering GA 494UR UT WOS:000269844600009 ER PT J AU Scheuerell, MD Zabel, RW Sandford, BP AF Scheuerell, Mark D. Zabel, Richard W. Sandford, Benjamin P. TI Relating juvenile migration timing and survival to adulthood in two species of threatened Pacific salmon (Oncorhynchus spp.) SO JOURNAL OF APPLIED ECOLOGY LA English DT Article DE Chinook; dams; migration; Oncorhynchus mykiss; Oncorhynchus tshawytscha; steelhead; survival; temperature; timing ID SPRING CHINOOK SALMON; CLIMATE-CHANGE; COLUMBIA RIVER; SNAKE RIVER; EVOLUTIONARY RESPONSES; HYDROPOWER SYSTEM; GROWTH; TSHAWYTSCHA; COMPETITION; MISMATCH AB 1. Migration timing in animals has important effects on life-history transitions. Human activities can alter migration timing of animals, and understanding the effects of such disruptions remains an important goal for applied ecology. Anadromous Pacific salmon (Oncorhynchus spp.) inhabit fresh water as juveniles before migrating to the ocean where they gain >90% of their biomass before returning to fresh water as adults to reproduce. Although construction of dams has delayed juvenile migration for many populations, we currently lack a synthesis of patterns in migration timing and how they relate to subsequent survival to adulthood for Pacific salmon, especially for at-risk populations. 2. We studied two groups of Pacific salmon from the Columbia River basin in the northwestern United States currently listed under the U. S. Endangered Species Act. We examined how the proportion of juveniles surviving to return as adults varied with year of migration, date of arrival in the estuary, water temperature and coastal ocean upwelling using data from over 40 000 individually tagged Chinook salmon Oncorhynchus tshawytscha and steelhead Oncorhynchus mykiss. 3. In general, models with year, day and day(2) had much better support from the data than those with temperature and upwelling. For Chinook salmon, we also found a residual effect of temperature after controlling for day, but the effect was small for steelhead. 4. For both species, juveniles migrating from early to mid-May survived 4-50 times greater than those migrating in mid-June. As expected, however, the estimated peak in survival varied among years, presumably reflecting interannual variation in the nearshore physical environment and trophic dynamics that affect salmon during the critical juvenile life stage. 5. Synthesis and applications. Our results indicate a possible management objective would be to speed arrival to the estuary by increasing springtime river flows. These findings also provide some insight into the mechanisms underlying seasonal differences in survival patterns, but additional studies are needed to better resolve the issue. Future changes to river flow and water temperature associated with climate change and human activities may further alter migration timing, and thus this phenomenon deserves further attention. C1 [Scheuerell, Mark D.; Zabel, Richard W.] NOAA, Natl Marine Fisheries Serv, NW Fisheries Sci Ctr, Seattle, WA 98112 USA. [Sandford, Benjamin P.] NW Fisheries Sci Ctr, Natl Marine Fisheries Serv, Pasco Res Stn, Pasco, WA 99301 USA. RP Scheuerell, MD (reprint author), NOAA, Natl Marine Fisheries Serv, NW Fisheries Sci Ctr, Seattle, WA 98112 USA. EM mark.scheuerell@noaa.gov RI Scheuerell, Mark/N-6683-2016 OI Scheuerell, Mark/0000-0002-8284-1254 NR 40 TC 63 Z9 63 U1 3 U2 48 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0021-8901 J9 J APPL ECOL JI J. Appl. Ecol. PD OCT PY 2009 VL 46 IS 5 BP 983 EP 990 DI 10.1111/j.1365-2664.2009.01693.x PG 8 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 502AB UT WOS:000270425100009 ER PT J AU Omar, AH Winker, DM Kittaka, C Vaughan, MA Liu, ZY Hu, YX Trepte, CR Rogers, RR Ferrare, RA Lee, KP Kuehn, RE Hostetler, CA AF Omar, Ali H. Winker, David M. Kittaka, Chieko Vaughan, Mark A. Liu, Zhaoyan Hu, Yongxiang Trepte, Charles R. Rogers, Raymond R. Ferrare, Richard A. Lee, Kam-Pui Kuehn, Ralph E. Hostetler, Chris A. TI The CALIPSO Automated Aerosol Classification and Lidar Ratio Selection Algorithm SO JOURNAL OF ATMOSPHERIC AND OCEANIC TECHNOLOGY LA English DT Article ID TO-BACKSCATTER RATIO; ATMOSPHERIC BOUNDARY-LAYER; SPECTRAL-RESOLUTION LIDAR; OPTICAL-PROPERTIES; RAMAN LIDAR; TROPOSPHERIC AEROSOL; INDIAN-OCEAN; SAHARAN DUST; ACE-ASIA; EXTINCTION AB Descriptions are provided of the aerosol classification algorithms and the extinction-to-backscatter ratio (lidar ratio) selection schemes for the Cloud-Aerosol Lidar and Infrared Pathfinder Satellite Observations (CALIPSO) aerosol products. One year of CALIPSO level 2 version 2 data are analyzed to assess the veracity of the CALIPSO aerosol-type identification algorithm and generate vertically resolved distributions of aerosol types and their respective optical characteristics. To assess the robustness of the algorithm, the interannual variability is analyzed by using a fixed season (June-August) and aerosol type (polluted dust) over two consecutive years (2006 and 2007). The CALIPSO models define six aerosol types: clean continental, clean marine, dust, polluted continental, polluted dust, and smoke, with 532-nm (1064 nm) extinction-to-backscatter ratios S, of 35 (30), 20 (45) 40 (55), 70 (30) 65 (30), and 70 (40) sr, respectively. This paper presents the global distributions of the CALIPSO aerosol types, the complementary distributions of integrated attenuated backscatter, and the volume depolarization ratio for each type. The aerosol-type distributions are further partitioned according to surface type (land/ocean) and detection resolution (5, 20, and 80 km) for optical and spatial context, because the optically thick layers are found most often at the smallest spatial resolution. Except for clean marine and polluted continental, all the aerosol types are found preferentially at the 80-km resolution. Nearly 80% of the smoke cases and 60% of the polluted dust cases are found over water, whereas dust and polluted continental cases are found over both land and water at comparable frequencies. Because the CALIPSO observables do not sufficiently constrain the determination of the aerosol, the surface type is used to augment the selection criteria. Distributions of the total attenuated color ratios show that the use of surface type in the typing algorithm does not result in abrupt and artificial changes in aerosol type or extinction. C1 [Omar, Ali H.; Winker, David M.; Vaughan, Mark A.; Hu, Yongxiang; Trepte, Charles R.; Ferrare, Richard A.; Lee, Kam-Pui; Hostetler, Chris A.] NASA, Langley Res Ctr, Sci Directorate, Hampton, VA 23681 USA. [Kittaka, Chieko; Rogers, Raymond R.; Kuehn, Ralph E.] Sci Syst & Applicat Int, Hampton, VA USA. [Liu, Zhaoyan] Natl Inst Aerosp, Hampton, VA USA. RP Omar, AH (reprint author), NASA, Langley Res Ctr, Sci Directorate, MS 475, Hampton, VA 23681 USA. EM ali.h.omar@nasa.gov RI Liu, Zhaoyan/A-9604-2009; Liu, Zhaoyan/B-1783-2010; Hu, Yongxiang/K-4426-2012; Omar, Ali/D-7102-2017 OI Liu, Zhaoyan/0000-0003-4996-5738; Omar, Ali/0000-0003-1871-9235 FU CALIPSO; NASA CNES FX We acknowledge the support of CALIPSO, a joint NASA CNES mission, and in particular the algorithm development and data management teams at Langley. We are also indebted to the anonymous reviewers for the many useful suggestions and constructive criticism, all of which have significantly improved this paper. NR 55 TC 272 Z9 284 U1 13 U2 63 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0739-0572 EI 1520-0426 J9 J ATMOS OCEAN TECH JI J. Atmos. Ocean. Technol. PD OCT PY 2009 VL 26 IS 10 BP 1994 EP 2014 DI 10.1175/2009JTECHA1231.1 PG 21 WC Engineering, Ocean; Meteorology & Atmospheric Sciences SC Engineering; Meteorology & Atmospheric Sciences GA 506ZE UT WOS:000270817600002 ER PT J AU Powell, KA Hostetler, CA Liu, ZY Vaughan, MA Kuehn, RE Hunt, WH Lee, KP Trepte, CR Rogers, RR Young, SA Winker, DM AF Powell, Kathleen A. Hostetler, Chris A. Liu, Zhaoyan Vaughan, Mark A. Kuehn, Ralph E. Hunt, William H. Lee, Kam-Pui Trepte, Charles R. Rogers, Raymond R. Young, Stuart A. Winker, David M. TI CALIPSO Lidar Calibration Algorithms. Part I: Nighttime 532-nm Parallel Channel and 532-nm Perpendicular Channel SO JOURNAL OF ATMOSPHERIC AND OCEANIC TECHNOLOGY LA English DT Article AB The Cloud-Aerosol Lidar and Infrared Pathfinder Satellite Observation (CALIPSO) mission was launched in April 2006 and has continuously acquired collocated multisensor observations of the spatial and optical properties of clouds and aerosols in the earth's atmosphere. The primary payload aboard CALIPSO is the Cloud-Aerosol Lidar with Orthogonal Polarization (CALIOP), which makes range-resolved measurements of elastic backscatter at 532 and 1064 nm and linear depolarization ratios at 532 nm. CALIOP measurements are important in reducing uncertainties that currently limit understanding of the global climate system, and it is essential that these measurements be accurately calibrated. This work describes the procedures used to calibrate the 532-nm measurements acquired during the nighttime portions of the CALIPSO orbits. Accurate nighttime calibration of the 532-nm parallel-channel data is fundamental to the success of the CALIOP measurement scheme, because the nighttime calibration is used to infer calibration across the day side of the orbits and all other channels are calibrated relative to the 532-nm parallel channel. The theoretical basis of the molecular normalization technique as applied to space-based lidar measurements is reviewed, and a comprehensive overview of the calibration algorithm implementation is provided. Also included is a description of a data filtering procedure that detects and removes spurious high-energy events that would otherwise introduce large errors into the calibration. Error estimates are derived and comparisons are made to validation data acquired by the NASA airborne high-spectral resolution lidar. Similar analyses are also presented for the 532-nm perpendicular-channel calibration technique. C1 [Powell, Kathleen A.] NASA, Langley Res Ctr, Hampton, VA 23681 USA. [Liu, Zhaoyan] Natl Inst Aerosp, Hampton, VA USA. [Kuehn, Ralph E.; Hunt, William H.] Sci Syst & Applicat Inc, Hampton, VA USA. [Young, Stuart A.] CSIRO Marine & Atmospher Res, Aspendale, Vic, Australia. RP Powell, KA (reprint author), NASA, Langley Res Ctr, MS 475, Hampton, VA 23681 USA. EM kathleen.a.powell@nasa.gov RI Liu, Zhaoyan/A-9604-2009; Liu, Zhaoyan/B-1783-2010; Young, Stuart/A-8641-2011 OI Liu, Zhaoyan/0000-0003-4996-5738; Young, Stuart/0000-0001-6434-9816 NR 25 TC 62 Z9 64 U1 1 U2 8 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 OCT PY 2009 VL 26 IS 10 BP 2015 EP 2033 DI 10.1175/2009JTECHA1242.1 PG 19 WC Engineering, Ocean; Meteorology & Atmospheric Sciences SC Engineering; Meteorology & Atmospheric Sciences GA 506ZE UT WOS:000270817600003 ER PT J AU Vaughan, MA Powell, KA Kuehn, RE Young, SA Winker, DM Hostetler, CA Hunt, WH Liu, ZY McGill, MJ Getzewich, BJ AF Vaughan, Mark A. Powell, Kathleen A. Kuehn, Ralph E. Young, Stuart A. Winker, David M. Hostetler, Chris A. Hunt, William H. Liu, Zhaoyan McGill, Matthew J. Getzewich, Brian J. TI Fully Automated Detection of Cloud and Aerosol Layers in the CALIPSO Lidar Measurements SO JOURNAL OF ATMOSPHERIC AND OCEANIC TECHNOLOGY LA English DT Article ID ALGORITHM; PERFORMANCE; VALIDATION; MODIS AB Accurate knowledge of the vertical and horizontal extent of clouds and aerosols in the earth's atmosphere is critical in assessing the planet's radiation budget and for advancing human understanding of climate change issues. To retrieve this fundamental information from the elastic backscatter lidar data acquired during the Cloud-Aerosol Lidar and Infrared Pathfinder Satellite Observations (CALIPSO) mission, a selective, iterated boundary location (SIBYL) algorithm has been developed and deployed. SIBYL accomplishes its goals by integrating an adaptive context-sensitive profile scanner into an iterated multiresolution spatial averaging scheme. This paper provides an in-depth overview of the architecture and performance of the SIBYL algorithm. It begins with a brief review of the theory of target detection in noise-contaminated signals, and an enumeration of the practical constraints levied on the retrieval scheme by the design of the lidar hardware, the geometry of a space-based remote sensing platform, and the spatial variability of the measurement targets. Detailed descriptions are then provided for both the adaptive threshold algorithm used to detect features of interest within individual lidar profiles and the fully automated multiresolution averaging engine within which this profile scanner functions. The resulting fusion of profile scanner and averaging engine is specifically designed to optimize the trade-offs between the widely varying signal-to-noise ratio of the measurements and the disparate spatial resolutions of the detection targets. Throughout the paper, specific algorithm performance details are illustrated using examples drawn from the existing CALIPSO dataset. Overall performance is established by comparisons to existing layer height distributions obtained by other airborne and space-based lidars. C1 [Vaughan, Mark A.] NASA, Langley Res Ctr, Hampton, VA 23681 USA. [Kuehn, Ralph E.; Hunt, William H.; Getzewich, Brian J.] Sci Syst & Applicat Inc, Hampton, VA USA. [Young, Stuart A.] CSIRO Marine & Atmospher Res, Aspendale, Vic, Australia. [Liu, Zhaoyan] Natl Inst Aerosp, Hampton, VA USA. [McGill, Matthew J.] NASA, Greenbelt, MD USA. RP Vaughan, MA (reprint author), NASA, Langley Res Ctr, Mail Stop 475, Hampton, VA 23681 USA. EM mark.a.vaughan@nasa.gov RI Liu, Zhaoyan/A-9604-2009; Liu, Zhaoyan/B-1783-2010; McGill, Matthew/D-8176-2012; Young, Stuart/A-8641-2011 OI Liu, Zhaoyan/0000-0003-4996-5738; Young, Stuart/0000-0001-6434-9816 FU National Snow and Ice Data Center (NSIDC) at the University of Colorado [GLA08, GLA09] FX The authors wish to acknowledge the many and substantial contributions of the members of the CALIPSO Lidar Science Working Group. We also extend special votes of thanks and appreciation to Sharon Rodier and Karn-Pui Lee, chief architects of the CALIOP level I analysis codes; to Steve Palm, Bill Hart, and Dennis Hlavka for many valuable discussions about space-based lidar data processing in general and layer detection techniques in particular; and to John Hair, Ray Rogers, Mike Obland, and Chip Trepte for their phenomenal and ongoing validation support. The ISCCP D1 data were obtained from the NASA LaRC ASDC. The GLAS GLA08 and GLA09 data were obtained from the National Snow and Ice Data Center (NSIDC) at the University of Colorado. The MODIS level 2 cloud data were obtained from the NASA Goddard Space Flight Center Level I and Atmosphere Archive and Distribution System. NR 36 TC 179 Z9 180 U1 8 U2 39 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0739-0572 EI 1520-0426 J9 J ATMOS OCEAN TECH JI J. Atmos. Ocean. Technol. PD OCT PY 2009 VL 26 IS 10 BP 2034 EP 2050 DI 10.1175/2009JTECHA1228.1 PG 17 WC Engineering, Ocean; Meteorology & Atmospheric Sciences SC Engineering; Meteorology & Atmospheric Sciences GA 506ZE UT WOS:000270817600004 ER PT J AU Wright, CW Walsh, EJ Krabill, WB Shaffer, WA Baig, SR Peng, M Pietrafesa, LJ Garcia, AW Marks, FD Black, PG Sonntag, J Beckley, BD AF Wright, C. W. Walsh, E. J. Krabill, W. B. Shaffer, W. A. Baig, S. R. Peng, M. Pietrafesa, L. J. Garcia, A. W. Marks, F. D., Jr. Black, P. G. Sonntag, J. Beckley, B. D. TI Measuring Storm Surge with an Airborne Wide-Swath Radar Altimeter SO JOURNAL OF ATMOSPHERIC AND OCEANIC TECHNOLOGY LA English DT Article ID SPECTRUM SPATIAL VARIATION; DIRECTIONAL WAVE SPECTRA; SEA-SURFACE; WIND; HURRICANES; MODEL; VERIFICATION; INUNDATION; SYSTEM AB Over the years, hurricane track forecasts and storm surge models, as well the digital terrain and bathymetry data they depend on, have improved significantly. Strides have also been made in the knowledge of the detailed variation of the surface wind field driving the surge. The area of least improvement has been in obtaining data on the temporal/spatial evolution of the mound of water that the hurricane wind and waves push against the shore to evaluate the performance of the numerical models. Tide gauges in the vicinity of the landfall are frequently destroyed by the surge. Survey crews dispatched after the event provide no temporal information and only indirect indications of the maximum water level over land. The landfall of Hurricane Bonnie on 26 August 1998, with a surge less than 2 m. provided an excellent opportunity to demonstrate the potential benefits of direct airborne measurement of the temporal/spatial evolution of the water level over a large area. Despite a 160-m variation in aircraft altitude. an 11.5-m variation in the elevation of the mean sea surface relative to the ellipsoid over the flight track, and the tidal variation over the 5-h data acquisition interval. a survey-quality global positioning system (GPS) aircraft trajectory allowed the NASA scanning radar altimeter carried by a NOAA hurricane research aircraft to demonstrate that an airborne wide-swath radar altimeter could produce targeted measurements of storm surge that would provide an absolute standard for assessing the accuracy of numerical storm surge models. C1 [Wright, C. W.; Walsh, E. J.; Krabill, W. B.] NASA, Goddard Space Flight Ctr, Wallops Isl, VA 23337 USA. [Shaffer, W. A.] NOAA, Natl Weather Serv, Silver Spring, MD 20910 USA. [Baig, S. R.] NOAA, Trop Predict Ctr, Miami, FL USA. [Peng, M.; Pietrafesa, L. J.] N Carolina State Univ, Coll Phys & Math Sci, Raleigh, NC 27695 USA. [Garcia, A. W.] USA, Coastal & Hydraul Lab, Engn R&D Ctr, Vicksburg, MS USA. [Marks, F. D., Jr.; Black, P. G.] NOAA, Atlantic Oceanog & Meteorol Lab, Hurricane Res Div, Miami, FL 33149 USA. [Sonntag, J.] EG&G Tech Serv Inc, Wallops Isl, VA USA. [Beckley, B. D.] SGT Inc, Greenbelt, MD USA. RP Walsh, EJ (reprint author), NOAA, Earth Syst Res Lab, R PSD3,325 Broadway, Boulder, CO 80305 USA. EM edward.walsh@noaa.gov RI Marks, Frank/A-5733-2011 OI Marks, Frank/0000-0003-0371-5514 FU Joint Hurricane Testbed of the NOAA/U.S; Weather Research Program (USWRP) at the Tropical Prediction Center/National Hurricane Center; NASA SRA; NOAA Aircraft Operations Center FX These measurements and this analysis were supported by the NASA Physical Oceanography Program. The analysis was also supported by the Joint Hurricane Testbed of the NOAA/U.S. Weather Research Program (USWRP) at the Tropical Prediction Center/National Hurricane Center. Donald E. Hines maintained the NASA SRA, and the NOAA Aircraft Operations Center is thanked for their expertise in helping install the system and executing the complex flight patterns. E. J. Walsh thanks Hendilk Tolman of NCEP for useful discussion. NR 25 TC 1 Z9 1 U1 1 U2 7 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 OCT PY 2009 VL 26 IS 10 BP 2200 EP 2215 DI 10.1175/2009JTECHO627.1 PG 16 WC Engineering, Ocean; Meteorology & Atmospheric Sciences SC Engineering; Meteorology & Atmospheric Sciences GA 506ZE UT WOS:000270817600016 ER PT J AU Jones, TA Christopher, SA Petersen, W AF Jones, Thomas A. Christopher, Sundar A. Petersen, Walt TI Dual-Polarization Radar Characteristics of an Apartment Fire SO JOURNAL OF ATMOSPHERIC AND OCEANIC TECHNOLOGY LA English DT Article ID ECHOES; CLOUDS; SMOKE AB Dual-polarimetric microwave wavelength radar observations of an apartment fire in Huntsville, Alabama, on 3 March 2008 are examined to determine the radar-observable properties of ash and fire debris lofted into the atmosphere, Dual-polarimetric observations are collected at close range (<20 km) by the 5-cm (C band) Advanced Radar for Meteorological and Operational Research (ARMOR) radar operated by the University of Alabama in Huntsville. Precipitation radars, such as ARMOR, are not sensitive to aerosol-sized (D < 10 mu m) smoke particles, but they are sensitive to the larger ash and burnt debris embedded within the smoke plume. The authors also assess if turbulent eddies caused by the heat of the fire cause Bragg scattering to occur at the 5-cm wavelength. In this example, the mean reflectivity within the debris plume from the 1.3 degrees elevation scan was 9.0 dBZ, with a few values exceeding 20 dBZ. The plume is present more than 20 kin downstream of the fire, with debris lofted at least I km above ground level into the atmosphere. Velocities up to 20 in s(-1) are present within the plume, indicating that the travel time for the debris from its source to the maximum range of detection is less than 20 min. Dual-polarization observations show that backscattered radiation is dominated by nonspherical, large, oblate targets as indicated by nonzero differential reflectivity values (mean = 1.7 dB) and low correlation coefficients (0.49). Boundary layer convective rolls are also observed that have very low reflectivity values (-6.0 dBZ); however, differential reflectivity is much larger (3.2 dB). This is likely the result of noise, because ARMOR differential reflectivity is not reliable for reflectivity values <0 dBZ. Also, copolar correlation is even lower compared to the debris plume (0.42). The remainder of the data mainly consists of atmospheric and ground-clutter noise. The large differential phase values coupled with positive differential reflectivity strongly indicate that the source of much of the return from the debris plume is particle scattering. However, given the significant degree of noise present, a substantial contribution from Bragg scattering cannot be entirely ruled out. C1 [Jones, Thomas A.; Christopher, Sundar A.] Univ Alabama, Dept Atmospher Sci, Huntsville, AL 35805 USA. [Petersen, Walt] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. RP Jones, TA (reprint author), Univ Alabama, Dept Atmospher Sci, 320 Sparkman Dr, Huntsville, AL 35805 USA. EM tjones@nsstc.uah.edu RI Christopher, Sundar/E-6781-2011 FU NOAA [NA06NES4400008, NA07NES4280005]; NASA CALIPSO; MODIS FX This research was partially supported by NOAA Grants NA06NES4400008 and NA07NES4280005 and a NASA CALIPSO science team grant. MODIS data were obtained from the Level 1 and Atmosphere Archive and Distribution System (LAADS) at Goddard Space Flight Center (GSFC). Special thanks to Ms. Elise Johnson and Mr. Christopher Schultz for providing and formatting the ARMOR data used in this research and Ms. Christina Crowe of the Huntsville National Weather Service Office for providing the surface weather observations. We greatly appreciate the comments provided by the anonymous reviewers and the technical overview by Ms. Anita Leroy, which significantly improved the quality of this work. NR 25 TC 8 Z9 9 U1 2 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 OCT PY 2009 VL 26 IS 10 BP 2257 EP 2269 DI 10.1175/2009JTECHA1290.1 PG 13 WC Engineering, Ocean; Meteorology & Atmospheric Sciences SC Engineering; Meteorology & Atmospheric Sciences GA 506ZE UT WOS:000270817600020 ER PT J AU Mohr, KI Molinari, J Thorncroft, CD AF Mohr, Karen I. Molinari, John Thorncroft, Chris D. TI The Interannual Stability of Cumulative Frequency Distributions for Convective System Size and Intensity SO JOURNAL OF CLIMATE LA English DT Article ID WESTERN NORTH PACIFIC; CLIMATE ASSESSMENT; LIGHTNING CHARACTERISTICS; PRECIPITATION FEATURES; PASSIVE MICROWAVE; AFRICAN MONSOON; ICE SCATTERING; DIURNAL CYCLE; EL-NINO; TRMM AB The characteristics of convective system populations in West Africa and the western Pacific tropical cyclone basin were analyzed to investigate whether interannual variability in convective activity in tropical continental and oceanic environments is driven by variations in the number of events during the wet season or by favoring large and/or intense convective systems. Convective systems were defined from Tropical Rainfall Measuring Mission (TRMM) data as a cluster of pixels with an 85-GHz polarization-corrected brightness temperature below 255 K and with an area of at least 64 km(2). The study database consisted of convective systems in West Africa from May to September 1998-2007, and in the western Pacific from May to November 1998-2007. Annual cumulative frequency distributions for system minimum brightness temperature and system area were constructed for both regions. For both regions, there were no statistically significant differences between the annual curves for system minimum brightness temperature. There were two groups of system area curves, split by the TRMM altitude boost in 2001. Within each set, there was no statistically significant interannual variability. Subsetting the database revealed some sensitivity in distribution shape to the size of the sampling area, the length of the sample period, and the climate zone. From a regional perspective, the stability of the cumulative frequency distributions implied that the probability that a convective system would attain a particular size or intensity does not change interannually. Variability in the number of convective events appeared to be more important in determining whether a year is either wetter or drier than normal. C1 [Mohr, Karen I.; Molinari, John; Thorncroft, Chris D.] SUNY Albany, Dept Earth & Atmospher Sci, Albany, NY 12222 USA. RP Mohr, KI (reprint author), NASA, Goddard Space Flight Ctr, Atmospheres Lab, Code 613-1, Greenbelt, MD 20771 USA. EM karen.mohr-1@nasa.gov RI Mohr, Karen/E-4331-2012 FU NASA [NNX07AD45G]; NSF [ATM0538164, ATM0732255] FX We obtained the TRMM data products (1B11 and 3B43) from the NASA Goddard Distributed Active Archive Center (online at http://disc.sci.gsfc.nasa.gov/data/datapool/TRMM/). D. Vollaro produced our Pacific map, A. Mekonnen provided wavelet analyses, and H. Ghiradella translated a French language reference for us. We had useful discussions with R. Carbone, E. Zipser, and the students and postdocs of our West Africa research group: H. Nguyen, A. Mekonnen, S. Hopsch, M. Tanu, S. Nicholls, M. Janiga, and G. Berry. We are grateful to C. Liu and two anonymous reviewers for their helpful comments on this manuscript. This work was supported by the NASA Precipitation Measuring Mission Grant NNX07AD45G and NSF Grants ATM0538164 and ATM0732255. NR 38 TC 5 Z9 5 U1 1 U2 1 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 PY 2009 VL 22 IS 19 BP 5218 EP 5231 DI 10.1175/2009JCLI2940.1 PG 14 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 501ZL UT WOS:000270423300016 ER PT J AU Schubert, S Gutzler, D Wang, HL Dai, A Delworth, T Deser, C Findell, K Fu, R Higgins, W Hoerling, M Kirtman, B Koster, R Kumar, A Legler, D Lettenmaier, D Lyon, B Magana, V Mo, K Nigam, S Pegion, P Phillips, A Pulwarty, R Rind, D Ruiz-Barradas, A Schemm, J Seager, R Stewart, R Suarez, M Syktus, J Ting, MF Wang, CZ Weaver, S Zeng, N AF Schubert, Siegfried Gutzler, David Wang, Hailan Dai, Aiguo Delworth, Tom Deser, Clara Findell, Kirsten Fu, Rong Higgins, Wayne Hoerling, Martin Kirtman, Ben Koster, Randal Kumar, Arun Legler, David Lettenmaier, Dennis Lyon, Bradfield Magana, Victor Mo, Kingtse Nigam, Sumant Pegion, Philip Phillips, Adam Pulwarty, Roger Rind, David Ruiz-Barradas, Alfredo Schemm, Jae Seager, Richard Stewart, Ronald Suarez, Max Syktus, Jozef Ting, Mingfang Wang, Chunzai Weaver, Scott Zeng, Ning TI A US CLIVAR Project to Assess and Compare the Responses of Global Climate Models to Drought-Related SST Forcing Patterns: Overview and Results SO JOURNAL OF CLIMATE LA English DT Article ID SEA-SURFACE TEMPERATURE; PART I; UNITED-STATES; MOIST CONVECTION; NATIONAL CENTER; GREAT-PLAINS; PRECIPITATION; VARIABILITY; PACIFIC; SUMMER AB The U. S. Climate Variability and Predictability (CLIVAR) working group on drought recently initiated a series of global climate model simulations forced with idealized SST anomaly patterns, designed to address a number of uncertainties regarding the impact of SST forcing and the role of land-atmosphere feedbacks on regional drought. The runs were carried out with five different atmospheric general circulation models (AGCMs) and one coupled atmosphere-ocean model in which the model was continuously nudged to the imposed SST forcing. This paper provides an overview of the experiments and some initial results focusing on the responses to the leading patterns of annual mean SST variability consisting of a Pacific El Nino-Southern Oscillation (ENSO)-like pattern, a pattern that resembles the Atlantic multidecadal oscillation (AMO), and a global trend pattern. One of the key findings is that all of the AGCMs produce broadly similar (though different in detail) precipitation responses to the Pacific forcing pattern, with a cold Pacific leading to reduced precipitation and a warm Pacific leading to enhanced precipitation over most of the United States. While the response to the response over the United States tends to occur when the two oceans have anomalies of opposite signs. Further highlights of the response over the United States to the Pacific forcing include precipitation signal-to-noise ratios that peak in spring, and surface temperature signal-to-noise ratios that are both lower and show less agreement among the models than those found for the precipitation response. The response to the positive SST trend forcing pattern is an overall surface warming over the world's land areas, with substantial regional variations that are in part reproduced in runs forced with a globally uniform SST trend forcing. The precipitation response to the trend forcing is weak in all of the models. It is hoped that these early results, as well as those reported in the other contributions to this special issue on drought, will serve to stimulate further analysis of these simulations, as well as suggest new research on the physical mechanisms contributing to hydroclimatic variability and change throughout the world. C1 [Schubert, Siegfried; Wang, Hailan; Koster, Randal; Suarez, Max; Weaver, Scott] NASA, Global Modeling & Assimilat Off, GSFC, Sci & Explorat Directorate, Greenbelt, MD 20771 USA. [Gutzler, David] Univ New Mexico, Dept Earth & Planetary Sci, Albuquerque, NM 87131 USA. [Wang, Hailan; Weaver, Scott] Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA. [Dai, Aiguo; Deser, Clara; Phillips, Adam] Natl Ctr Atmospher Res, Boulder, CO 80307 USA. [Delworth, Tom; Findell, Kirsten] Princeton Univ, Natl Ocean & Atmospher Adm, Geophys Fluid Dynam Lab, Princeton, NJ 08544 USA. [Fu, Rong] Univ Texas Austin, Jackson Sch Geosci, Austin, TX 78712 USA. [Higgins, Wayne; Kumar, Arun; Mo, Kingtse; Pegion, Philip; Schemm, Jae] NOAA, NWS, NCEP, Climate Predict Ctr, Washington, DC USA. [Hoerling, Martin] NOAA, Earth Syst Res Lab, Boulder, CO USA. [Kirtman, Ben] Univ Miami, Rosenstiel Sch Marine & Atmospher Sci, Miami, FL 33149 USA. [Legler, David] US Climate Variabil & Predictabil Res Program, Washington, DC USA. [Lettenmaier, Dennis] Univ Washington, Dept Civil & Environm Engn, Seattle, WA 98195 USA. [Lyon, Bradfield] Columbia Univ, Lamont Doherty Earth Observ, Int Res Inst Climate & Soc, Palisades, NY USA. [Magana, Victor] Univ Nacl Autonoma Mexico, Ctr Atmospher Sci, Mexico City 04510, DF, Mexico. [Nigam, Sumant; Ruiz-Barradas, Alfredo; Zeng, Ning] Univ Maryland, Dept Atmospher & Ocean Sci, College Pk, MD 20742 USA. [Rind, David] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Stewart, Ronald] Univ Manitoba, Dept Geog & Environm, Winnipeg, MB, Canada. [Syktus, Jozef] Environm Protect Agcy, Indooroopilly, Qld, Australia. [Wang, Chunzai] NOAA, Atlantic Oceanog & Meteorol Lab, Phys Oceanog Div, Miami, FL 33149 USA. RP Schubert, S (reprint author), NASA, Global Modeling & Assimilat Off, GSFC, Sci & Explorat Directorate, Greenbelt, MD 20771 USA. EM siegfried.d.schubert@nasa.gov RI Wang, Chunzai /C-9712-2009; Ruiz-Barradas, Alfredo/F-4499-2010; Syktus, Jozef/E-7173-2011; Pegion, Philip/E-5247-2012; Koster, Randal/F-5881-2012; Nigam, Sumant/A-8338-2009; Zeng, Ning/A-3130-2008; lettenmaier, dennis/F-8780-2011; Delworth, Thomas/C-5191-2014; Findell, Kirsten/D-4430-2014; Dai, Aiguo/D-3487-2009 OI Gutzler, David/0000-0001-6476-8412; Wang, Chunzai /0000-0002-7611-0308; Ruiz-Barradas, Alfredo/0000-0003-3633-3950; Syktus, Jozef/0000-0003-1782-3073; Koster, Randal/0000-0001-6418-6383; Zeng, Ning/0000-0002-7489-7629; lettenmaier, dennis/0000-0003-3317-1327; NR 46 TC 125 Z9 127 U1 1 U2 37 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 PY 2009 VL 22 IS 19 BP 5251 EP 5272 DI 10.1175/2009JCLI3060.1 PG 22 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 501ZL UT WOS:000270423300018 ER PT J AU Ballard, CG Anderson, KS Myrabo, L AF Ballard, Christopher G. Anderson, Kurt S. Myrabo, Leik TI Flight Dynamics and Simulation of Laser Propelled Lightcraft SO JOURNAL OF COMPUTATIONAL AND NONLINEAR DYNAMICS LA English DT Article CT ASME International Design Engineering Technical Conferences/Computers and Information in Engineering Conference CY SEP 04-07, 2007 CL Las Vegas, NV SP ASME, Design Engn Div, ASME, Comp & Informat Engn Div AB A seven degree-of-freedom (7DOF) dynamic model was developed to provide insight into the flight behavior of Type 200 and other related lightcraft, and to serve as a research tool for developing future engine-vehicle configurations for laser launching of nanosatellites (1-10 vertical bar kg). Accurate engine, beam, and aerodynamics models are included to improve the predictive capability of the 7DOF code. The aerodynamic forces of lift, drag, and aerodynamic pitching moment were derived from FLUENT (R) computational fluid dynamics predictions, and calibrated against limited existing wind tunnel data. To facilitate 7DOF model validation, simulation results are compared with video analysis of actual flights under comparable conditions. Despite current limitations of the 7DOF model, the results compared well with experimental flight trajectory data. [DOI: 10.1115/1.3187214] C1 [Anderson, Kurt S.; Myrabo, Leik] Rensselaer Polytech Inst, Dept Mech Aerosp & Nucl Engn, Troy, NY 12180 USA. [Ballard, Christopher G.] NASA, Jet Prop Lab, Pasadena, CA 91109 USA. RP Anderson, KS (reprint author), Rensselaer Polytech Inst, Dept Mech Aerosp & Nucl Engn, Troy, NY 12180 USA. EM christopher.g.ballard@jpl.nasa.gov; anderk5@oceania.edu; myrabl@rpi.edu NR 7 TC 5 Z9 5 U1 0 U2 3 PU ASME-AMER SOC MECHANICAL ENG PI NEW YORK PA THREE PARK AVE, NEW YORK, NY 10016-5990 USA SN 1555-1423 J9 J COMPUT NONLIN DYN JI J. Comput. Nonlinear Dyn. PD OCT PY 2009 VL 4 IS 4 AR 041005 DI 10.1115/1.3187214 PG 8 WC Engineering, Mechanical; Mechanics SC Engineering; Mechanics GA 500EB UT WOS:000270279900005 ER PT J AU Wang, W Shu, CW Yee, HC Sjogreen, B AF Wang, Wei Shu, Chi-Wang Yee, H. C. Sjoegreen, Bjoern TI High-order well-balanced schemes and applications to non-equilibrium flow SO JOURNAL OF COMPUTATIONAL PHYSICS LA English DT Article DE Well-balanced schemes; Non-equilibrium flow; Chemical reactions; WENO schemes; TVD schemes; Nozzle flow ID SHALLOW-WATER EQUATIONS; HYPERBOLIC CONSERVATION-LAWS; NONLINEAR DIFFERENTIAL-EQUATIONS; STATE NUMERICAL-SOLUTIONS; SOURCE TERMS; WENO SCHEMES; TVD SCHEMES; EFFICIENT IMPLEMENTATION; RESIDUAL DISTRIBUTION; WAVE-PROPAGATION AB The appearance of the source terms in modeling non-equilibrium flow problems containing finite-rate chemistry or combustion poses additional numerical difficulties beyond that for solving non-reacting flows. A well-balanced scheme, which can preserve certain non-trivial steady state solutions exactly, may help minimize some of these difficulties. In this paper, a simple one-dimensional non-equilibrium model with one temperature is considered. We first describe a general strategy to design high-order well-balanced finite-difference schemes and then study the well-balanced properties of the high-order finite-difference weighted essentially non-oscillatory (WENO) scheme, modified balanced WENO schemes and various total variation diminishing (TVD) schemes. The advantages of using a well-balanced scheme in preserving steady states and in resolving small perturbations of such states will be shown. Numerical examples containing both smooth and discontinuous solutions are included to verify the improved accuracy, in addition to the well-balanced behavior. (C) 2009 Elsevier Inc. All rights reserved C1 [Shu, Chi-Wang] Brown Univ, Div Appl Math, Providence, RI 02912 USA. [Wang, Wei] Stanford Univ, Ctr Turbulence Res, Stanford, CA 94305 USA. [Yee, H. C.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Sjoegreen, Bjoern] Lawrence Livermore Natl Lab, Livermore, CA 94551 USA. RP Shu, CW (reprint author), Brown Univ, Div Appl Math, Providence, RI 02912 USA. EM shu@dam.brown.edu RI Shu, Chi-Wang/A-3216-2013 OI Shu, Chi-Wang/0000-0001-7720-9564 FU DOE/SciDAC SAP [DE-AI02-06ER25796]; Lawrence Livermore National Laboratory [DE-AC52-07NA27344 LLNL-JRNL-409903] FX The authors acknowledge the support of the DOE/SciDAC SAP grant DE-AI02-06ER25796. The work by Bjorn Sjogreen is performed under the auspices of the U.S. Department of Energy by Lawrence Livermore National Laboratory under Contract No. DE-AC52-07NA27344 LLNL-JRNL-409903. NR 34 TC 10 Z9 10 U1 0 U2 3 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0021-9991 J9 J COMPUT PHYS JI J. Comput. Phys. PD OCT 1 PY 2009 VL 228 IS 18 BP 6682 EP 6702 DI 10.1016/j.jcp.2009.05.028 PG 21 WC Computer Science, Interdisciplinary Applications; Physics, Mathematical SC Computer Science; Physics GA 488UG UT WOS:000269375000004 ER PT J AU Ruthruff, E Johnston, JC Remington, RW AF Ruthruff, Eric Johnston, James C. Remington, Roger W. TI How Strategic Is the Central Bottleneck: Can It Be Overcome by Trying Harder? SO JOURNAL OF EXPERIMENTAL PSYCHOLOGY-HUMAN PERCEPTION AND PERFORMANCE LA English DT Article ID DUAL-TASK INTERFERENCE; PSYCHOLOGICAL REFRACTORY-PERIOD; ADAPTIVE EXECUTIVE CONTROL; RESPONSE-SELECTION; IDEOMOTOR COMPATIBILITY; CENTRAL POSTPONEMENT; OVERLAPPING TASKS; 2 THINGS; PERFORMANCE; TIME AB Recent dual-task studies suggest that a bottleneck prevents central mental operations from working on more than one task at a time, especially at relatively low practice levels. It remains highly controversial, however, whether this bottleneck is structural (inherent to human cognitive architecture) or merely a strategic choice. If the strategic hypothesis is testable, it ought to predict that, under sufficiently strong incentives, people could choose to bypass the bottleneck and perform both tasks in parallel. Because the incentives for parallel processing in previous studies have been modest, the authors introduced a novel dual-task paradigm with much greater incentives, induced by strict time deadlines for each task. With this paradigm, bottleneck delays would cause participants to frequently miss the time deadline or make errors, triggering immediate negative consequences (failure feedback). Nevertheless, participants had little success performing central operations in parallel; severe dual-task performance costs were observed, even with relatively easy tasks. These results greatly strengthen the case that the central bottleneck reflects a structural limitation that, at least at modest practice levels, cannot be avoided merely by trying harder. C1 [Ruthruff, Eric] Univ New Mexico, Albuquerque, NM 87131 USA. [Johnston, James C.] NASA, Ames Res Ctr, Washington, DC USA. [Remington, Roger W.] Univ Queensland, Brisbane, Qld 4072, Australia. RP Ruthruff, E (reprint author), 1 Univ New Mexico, Dept Psychol, MSC03 2220, Albuquerque, NM 87131 USA. EM ruthruff@unm.edu FU NASA FX This research was funded, in part, by the Airspace Operations Systems Project of NASA's Airspace Systems Program. NR 43 TC 13 Z9 13 U1 3 U2 8 PU AMER PSYCHOLOGICAL ASSOC PI WASHINGTON PA 750 FIRST ST NE, WASHINGTON, DC 20002-4242 USA SN 0096-1523 J9 J EXP PSYCHOL HUMAN JI J. Exp. Psychol.-Hum. Percept. Perform. PD OCT PY 2009 VL 35 IS 5 BP 1368 EP 1384 DI 10.1037/a0015784 PG 17 WC Psychology; Psychology, Experimental SC Psychology GA 503UK UT WOS:000270565900008 PM 19803643 ER PT J AU Murchie, SL Seelos, FP Hash, CD Humm, DC Malaret, E McGovern, JA Choo, TH Seelos, KD Buczkowski, DL Morgan, MF Barnouin-Jha, OS Nair, H Taylor, HW Patterson, GW Harvel, CA Mustard, JF Arvidson, RE McGuire, P Smith, MD Wolff, MJ Titus, TN Bibring, JP Poulet, F AF Murchie, Scott L. Seelos, Frank P. Hash, Christopher D. Humm, David C. Malaret, Erick McGovern, J. Andrew Choo, Teck H. Seelos, Kimberly D. Buczkowski, Debra L. Morgan, M. Frank Barnouin-Jha, Olivier S. Nair, Hari Taylor, Howard W. Patterson, Gerald W. Harvel, Christopher A. Mustard, John F. Arvidson, Raymond E. McGuire, Patrick Smith, Michael D. Wolff, Michael J. Titus, Timothy N. Bibring, Jean-Pierre Poulet, Francois TI Compact Reconnaissance Imaging Spectrometer for Mars investigation and data set from the Mars Reconnaissance Orbiter's primary science phase SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID OMEGA/MARS EXPRESS; RADIATIVE-TRANSFER; DIVERSITY; MINERALS; DEPOSITS; OLIVINE; MISSION; REGION AB The part of the Compact Reconnaissance Imaging Spectrometer (CRISM) for Mars investigation conducted during the Mars Reconnaissance Orbiter's (MRO's) primary science phase was a comprehensive investigation of past aqueous environments, structure of the planet's crust, past climate, and current meteorology. The measurements to implement this investigation include over 9500 targeted observations of surface features taken at spatial resolutions of better than 40 m/pixel, monitoring of seasonal variations in atmospheric aerosols and trace gases, and acquisition of a 200 m/pixel map covering over 55% of Mars in 72 selected wavelengths under conditions of relatively low atmospheric opacity. Key results from these data include recognition of a diversity of aqueous mineral-containing deposits, discovery of a widespread distribution of phyllosilicates in early to middle Noachian units, the first definitive detection of carbonates in bedrock, new constraints on the sequence of events that formed Hesperian-aged, sulfate-rich layered deposits, characterization of seasonal polar processes, and monitoring of the 2007 global dust event. Here we describe CRISM's science investigations during the Primary Science Phase, the data sets that were collected and their calibration and uncertainties, and how they have been processed and made available to the scientific community. We also describe the ongoing investigation during MRO's extended science phase. C1 [Murchie, Scott L.; Seelos, Frank P.; Humm, David C.; McGovern, J. Andrew; Choo, Teck H.; Seelos, Kimberly D.; Buczkowski, Debra L.; Morgan, M. Frank; Barnouin-Jha, Olivier S.; Nair, Hari; Taylor, Howard W.; Patterson, Gerald W.; Harvel, Christopher A.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Bibring, Jean-Pierre; Poulet, Francois] Univ Paris 11, Inst Astrophys Spatiale, F-91405 Orsay, France. [Arvidson, Raymond E.; McGuire, Patrick] Washington Univ, Dept Earth & Planetary Sci, St Louis, MO 63130 USA. [Hash, Christopher D.; Malaret, Erick] Appl Coherent Technol, Herndon, VA 20170 USA. [Mustard, John F.] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA. [Smith, Michael D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Titus, Timothy N.] US Geol Survey, Flagstaff, AZ 86001 USA. [Wolff, Michael J.] Space Sci Inst, Boulder, CO 80301 USA. [McGuire, Patrick] Free Univ Berlin, D-1000 Berlin, Germany. RP Murchie, SL (reprint author), Johns Hopkins Univ, Appl Phys Lab, Johns Hopkins Rd, Laurel, MD 20723 USA. RI Smith, Michael/C-8875-2012; McGuire, Patrick/D-2962-2013; Murchie, Scott/E-8030-2015; Barnouin, Olivier/I-7475-2015; Seelos, Kimberly/F-4647-2015; Humm, David/B-8825-2016; Morgan, Frank/C-5246-2016; Seelos, Frank/C-7875-2016 OI McGuire, Patrick/0000-0001-6592-4966; Murchie, Scott/0000-0002-1616-8751; Barnouin, Olivier/0000-0002-3578-7750; Seelos, Kimberly/0000-0001-7236-0580; Humm, David/0000-0003-1520-261X; Morgan, Frank/0000-0003-3166-7732; Seelos, Frank/0000-0001-9721-941X NR 45 TC 74 Z9 74 U1 1 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 1 PY 2009 VL 114 AR E00D07 DI 10.1029/2009JE003344 PG 15 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 502MM UT WOS:000270464400002 ER PT J AU Banerjee, RK Ashtekar, KD Effat, MA Helmy, TA Kim, E Schneeberger, EW Sinha, RA Gottliebson, WM Back, LH AF Banerjee, Rupak K. Ashtekar, Koustubh D. Effat, Mohamed A. Helmy, Tarek A. Kim, Edward Schneeberger, Eric W. Sinha, Roy A. Gottliebson, William M. Back, Lloyd H. TI Concurrent Assessment of Epicardial Coronary Artery Stenosis and Microvascular Dysfunction Using Diagnostic Endpoints Derived from Fundamental Fluid Dynamics Principles SO JOURNAL OF INVASIVE CARDIOLOGY LA English DT Article DE coronary disease; microcirculation stenosis hemodynamics catheterization ID FRACTIONAL FLOW RESERVE; SEVERITY; RESISTANCE; PRESSURE; INDEX; MICROCIRCULATION; INTERVENTIONS; ANGIOPLASTY AB Background Simultaneously measured pressure and flow distal to coronary stenoses can be combined in conjunction with anatomical measurements to assess the status of both the epicardial and microvascular circulations Methods and Results Assessments of cow nary hemodynamics were performed using fundamental fluid dynamics principles We hypothesized that the pressure-drop coefficient (CDP(e) trans stenotic pressure drop divided by the dynamic pressure in the distal vessel) correlates linearly with epicardial and microcirculatory resistances concurrently In 14 pigs simultaneous measurements of distal coronary arterial pressure and flow were performed using a dual sensor-tipped guidewire in the setting of both normal and disrupted microcirculation with the presence of epicardial coronary lesions of < 50% area stenosis (AS) and > 50% AS The CDPe progressively increased from lesions of < 50% AS to 50% AS and had a higher resolving power (45 +/- 22 to 193 +/- 140 in not mal microcirculation 248 +/- 137 to 351 +/- 140 in disrupted microcirculation) as compared to fractional flow reserve (FFR) and coronary flow reserve (CFR) Strong multiple linear correlation was observed for CDP(e) with combined FFR and CFR (r = 0 72 p < 0 0001) Further the ratio of maximum pressure drop coefficient evaluated at the site of stenosis and its theoretical limiting value of minimum cross-sectional area was also able to distinguish different combinations of coronary artery diseases Conclusions The CDP(e) can be readily obtained during routine pressure and flow measurements during cardiac catheterization It is a promising clinical diagnostic parameter that can independently assess the severity of epicardial stenosis and microvascular impairment C1 [Banerjee, Rupak K.; Ashtekar, Koustubh D.; Sinha, Roy A.] Univ Cincinnati, Dept Mech Engn, Cincinnati, OH USA. [Banerjee, Rupak K.] Univ Cincinnati, Dept Biomed Engn, Cincinnati, OH USA. [Banerjee, Rupak K.] Univ Cincinnati, Dept Internal Med & Cardiol, Cincinnati, OH USA. [Schneeberger, Eric W.] Univ Cincinnati, Dept Cardiothorac Surg, Cincinnati, OH USA. [Schneeberger, Eric W.] Cincinnati Childrens Hosp, Med Ctr, Dept Cardiol, Cincinnati, OH USA. [Back, Lloyd H.] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Banerjee, RK (reprint author), Dept Mech Primary & Biomed Secondary Engn, 598 Rhodes Hall,POB 210072, Cincinnati, OH 45221 USA. FU American Heart Association [0755236B, 0335270N] FX This work is supported by Grant In Aid of Great Rivers Affiliate and National Scientific Development Grant of American Heart Association (Giant reference #s 0755236B and 0335270N) NR 24 TC 24 Z9 25 U1 0 U2 1 PU H M P COMMUNICATIONS PI MALVERN PA 83 GENERAL WARREN BLVD, STE 100, MALVERN, PA 19355 USA SN 1042-3931 J9 J INVASIVE CARDIOL JI J. Invasive Cardiol. PD OCT PY 2009 VL 21 IS 10 BP 511 EP 517 PG 7 WC Cardiac & Cardiovascular Systems SC Cardiovascular System & Cardiology GA 687VU UT WOS:000284807100006 PM 19805837 ER PT J AU Chai, F Liu, GM Xue, HJ Shi, L Chao, Y Tseng, CM Chou, WC Liu, KK AF Chai, Fei Liu, Guimei Xue, Huijie Shi, Lei Chao, Yi Tseng, Chun-Mao Chou, Wen-Chen Liu, Kon-Kee TI Seasonal and Interannual Variability of Carbon Cycle in South China Sea: A Three-Dimensional Physical-Biogeochemical Modeling Study SO JOURNAL OF OCEANOGRAPHY LA English DT Article; Proceedings Paper CT Session on Decadal Changes in Carbon Biogeochemistry in the North Pacific held at the 16th PICES Annual Meeting CY OCT, 2007 CL Victoria, CANADA SP PICES DE Carbon cycle; South China Sea; physical-biogeochemical modeling; seasonal and interannual variability ID NORTH-ATLANTIC OCEAN; PEARL RIVER ESTUARY; TIME-SERIES SITE; EQUATORIAL PACIFIC; PARTIAL-PRESSURE; ATMOSPHERIC CO2; EL-NINO; SUMMER; SINK; DIOXIDE AB The South China Sea (SCS) exhibits strong variations on seasonal to interannual time scale, and the changing Southeast Asian Monsoon has direct impacts on the nutrients and phytoplankton dynamics, as well as the carbon cycle. A Pacific basin-wide physical-biogeochemical model has been developed and used to investigate the physical variations, ecosystem responses, and carbon cycle consequences. The Pacific basin-wide circulation model, based on the Regional Ocean Model Systems (ROMS) with a 50-km spatial resolution, is driven with daily air-sea fluxes derived from the National Centers for Environmental Prediction (NCEP) reanalysis between 1990 and 2004. The biogeochemical processes are simulated with the Carbon, Si(OH)(4), Nitrogen Ecosystem (CoSINE) model consisting of multiple nutrients and plankton functional groups and detailed carbon cycle dynamics. The ROMS-CoSINE model is capable of reproducing many observed features and their variability over the same period at the SouthEast Asian Time-series Study (SEATS) station in the SCS. The integrated air-sea CO2 flux over the entire SCS reveals a strong seasonal cycle, serving as a source of CO2 to the atmosphere in spring, summer and autumn, but acting as a sink of CO2 for the atmosphere in winter. The annual mean sea-to-air CO2 flux averaged over the entire SCS is +0.33 moles CO2 m(-2)year(-1), which indicates that the SCS is a weak source of CO2 to the atmosphere. Temperature has a stronger influence on the seasonal variation of pCO(2) than biological activity, and is thus the dominant factor controlling the oceanic pCO(2) in the SCS. The water temperature, seasonal upwelling and Kuroshio intrusion determine the pCO(2) differences at coast of Vietnam and the northwestern region of the Luzon Island. The inverse relationship between the interannual variability of Chl-a in summer near the coast of Vietnam and NINO3 SST (Sea Surface Temperature) index in January implies that the carbon cycle and primary productivity in the SCS is teleconnected to the Pacific-East Asian large-scale climatic variability. C1 [Chai, Fei; Liu, Guimei; Xue, Huijie; Shi, Lei] Univ Maine, Sch Marine Sci, Orono, ME 04469 USA. [Liu, Guimei] State Ocean Adm, Natl Marine Environm Forecasting Ctr, Beijing 100081, Peoples R China. [Chao, Yi] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Tseng, Chun-Mao] Natl Taiwan Univ, Inst Oceanog, Taipei 106, Taiwan. [Chou, Wen-Chen] Natl Taiwan Ocean Univ, Inst Marine Environm Chem & Ecol, Chilung, Taiwan. [Liu, Kon-Kee] Natl Cent Univ, Inst Hydrol & Ocean Sci, Jhongli 32001, Taiwan. RP Chai, F (reprint author), Univ Maine, Sch Marine Sci, 5706 Aubert Hall, Orono, ME 04469 USA. EM fchai@maine.edu RI Liu, Kon-Kee/K-8855-2012; OI Liu, Kon-Kee/0000-0003-4909-897X; TSENG, CHUN-MAO/0000-0003-1922-3936 NR 74 TC 33 Z9 40 U1 2 U2 36 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0916-8370 J9 J OCEANOGR JI J. Oceanogr. PD OCT PY 2009 VL 65 IS 5 BP 703 EP 720 PG 18 WC Oceanography SC Oceanography GA 490EL UT WOS:000269480900012 ER PT J AU Bidigare, RR Chai, F Landry, MR Lukas, R Hannides, CCS Christensen, SJ Karl, DM Shi, L Chao, Y AF Bidigare, Robert R. Chai, Fei Landry, Michael R. Lukas, Roger Hannides, Cecelia C. S. Christensen, Stephanie J. Karl, David M. Shi, Lei Chao, Yi TI Subtropical ocean ecosystem structure changes forced by North Pacific climate variations SO JOURNAL OF PLANKTON RESEARCH LA English DT Article ID STATION ALOHA; TIME-SERIES; NITROGEN; PRODUCTIVITY; PROCHLOROCOCCUS; SYNECHOCOCCUS; THERMOCLINE; SIMULATION; BIOMASS; MODEL AB Biological responses to basin-scale climate forcing in the subtropical North Pacific Ocean are assessed based on temporal variations in plankton community structure observed at Station. ALOHA and results of a coupled plysical-biogeochemical model. Observational data and model simulations for the period 1990-2004 reveal distinct temporal patterns, with significant increases in net primary productivity, modeled nitrate flux into the euphotic zone and the measured downward of particulate nitrogen during 1999-2004. Concurrent increases in microalgae, cyanobacteria and modeled and measured zooplankton biomass were also observed during this period. We provide evidence that these responses were a consequence of climate forcing that destratified the upper ocean, making it more susceptible to mixing events and nutrient entrainment. These findigs underscore the importance of nitrate flux and plankton community structure, as modulated by climate forcing, in regulating particle export over interannual and decadal time scales. C1 [Bidigare, Robert R.] Univ Hawaii, Hawaii Inst Marine Biol, Kaneohe, HI 96744 USA. [Chai, Fei; Shi, Lei] Univ Maine, Sch Marine Sci, Orono, ME 04469 USA. [Landry, Michael R.] Univ Calif, Scripps Inst Oceanog, La Jolla, CA 92093 USA. [Lukas, Roger; Hannides, Cecelia C. S.; Christensen, Stephanie J.; Karl, David M.] Univ Hawaii, Dept Oceanog, Honolulu, HI 96822 USA. [Chao, Yi] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Bidigare, RR (reprint author), Univ Hawaii, Hawaii Inst Marine Biol, POB 1346, Kaneohe, HI 96744 USA. EM bidigare@hawaii.edu FU National Science Foundation [EF-04245999, OCE-0326616, OCE-0117919, OCE-0327513, OCE-0324666, EF-0424599]; National Aeronautics and Space Administration; Environmental Protection Agency; Gordon arid Betty Moore Foundation and by the State of Hawaii FX This research was supported by grants From the National Science Foundation (EF-04245999 awarded to D.M.K.; OCE-0326616 awarded to RACK and R.R.B.; OCE-0117919 and OCE-0327513 awarded to R.L., OCE-0324666 awarded to M.R.L; arid EF-0424599 awarded to D.M.K. and R.R.B), the National Aeronautics and Space Administration, the Environmental Protection Agency, the Gordon arid Betty Moore Foundation and by the State of Hawaii. NR 41 TC 29 Z9 29 U1 0 U2 11 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0142-7873 EI 1464-3774 J9 J PLANKTON RES JI J. Plankton Res. PD OCT PY 2009 VL 31 IS 10 BP 1131 EP 1139 DI 10.1093/plankt/fbp064 PG 9 WC Marine & Freshwater Biology; Oceanography SC Marine & Freshwater Biology; Oceanography GA 500AQ UT WOS:000270269800002 ER PT J AU Palumbo, D AF Palumbo, Dan TI Estimating sound power radiated from rectangular baffled panels using a radiation factor SO JOURNAL OF THE ACOUSTICAL SOCIETY OF AMERICA LA English DT Article AB A method is introduced which is shown to predict radiated sound power from rectangular baffled panels. The method employs a filtered wavenumber transform to extract the power in the supersonic wavenumbers on the panel and a radiation factor to scale the supersonic power to match the actual radiated sound power. Although empirically derived, the radiation factor is shown to be related to the radiation efficiency of an infinite panel. The radiation factor is simple, depending only on the ratio of the wavenumbers of the panel to the radiation medium, and the method is straightforward to use, requiring only the panel normal velocities. The computation is efficient, as much as two orders of magnitude faster than a Rayleigh integration, thus providing a means of combining sound power predictions with finite element optimizations. A formula is derived which predicts the lowest frequency for which the method is valid as a function of the bin width of the wavenumber transform. The radiation factor method is shown to produce radiated sound power estimates which favorably compare to estimates derived from intensity measurements of physical test specimens and to Rayleigh integral estimates computed using both simulated and measured velocities. [DOI: 10.1121/1.3203930] C1 NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Palumbo, D (reprint author), NASA, Langley Res Ctr, MS 463, Hampton, VA 23681 USA. EM d.l.palumbo@nasa.gov NR 10 TC 3 Z9 3 U1 0 U2 3 PU ACOUSTICAL SOC AMER AMER INST PHYSICS PI MELVILLE PA STE 1 NO 1, 2 HUNTINGTON QUADRANGLE, MELVILLE, NY 11747-4502 USA SN 0001-4966 J9 J ACOUST SOC AM JI J. Acoust. Soc. Am. PD OCT PY 2009 VL 126 IS 4 BP 1827 EP 1837 DI 10.1121/1.3203930 PG 11 WC Acoustics; Audiology & Speech-Language Pathology SC Acoustics; Audiology & Speech-Language Pathology GA 506MJ UT WOS:000270778600019 PM 19813797 ER PT J AU Eldridge, JI Spuckler, CM Markham, JR AF Eldridge, Jeffrey I. Spuckler, Charles M. Markham, James R. TI Determination of Scattering and Absorption Coefficients for Plasma-Sprayed Yttria-Stabilized Zirconia Thermal Barrier Coatings at Elevated Temperatures SO JOURNAL OF THE AMERICAN CERAMIC SOCIETY LA English DT Article ID REFRACTIVE-INDEX; CUBIC ZIRCONIA; RADIATIVE PROPERTIES; SPECTRAL EMITTANCE; INSTRUMENT; TRANSPORT; BEHAVIOR; TISSUE; OXIDES AB The temperature dependence of the scattering and absorption coefficients for a set of freestanding plasma-sprayed 8 wt% yttria-stabilized zirconia (8YSZ) thermal barrier coatings (TBCs) was determined at temperatures up to 1360 degrees C in a wavelength range from 1.2 mu m up to the 8YSZ absorption edge. The scattering and absorption coefficients were determined by fitting the directional-hemispherical reflectance and transmittance values calculated by a four-flux Kubelka-Munk method to the experimentally measured hemispherical-directional reflectance and transmittance values obtained for five 8YSZ thicknesses. The scattering coefficient exhibited a continuous decrease with increasing wavelength and showed no significant temperature dependence. The scattering is primarily attributed to the relatively temperature-insensitive refractive index mismatch between the 8YSZ and its internal voids. The absorption coefficient was very low (<1 cm(-1)) at wavelengths between 2 mu m and the absorption edge and showed a definite temperature dependence that consisted of a shift of the absorption edge to shorter wavelengths and an increase in the weak absorption below the absorption edge with increasing temperature. The shift in the absorption edge with temperature is attributed to strongly temperature-dependent multiphonon absorption. While TBC hemispherical transmittance beyond the absorption edge can be predicted by a simple exponential decrease with thickness, below the absorption edge, typical TBC thicknesses are well below the thickness range where a simple exponential decrease in hemispherical transmittance with TBC thickness is expected. [Correction added after online publication August 11, 2009: "edge to a shorter wavelengths'' has been updated as "edge to shorter wavelengths.''] C1 [Eldridge, Jeffrey I.; Spuckler, Charles M.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. [Markham, James R.] Adv Fuel Res Inc, E Hartford, CT 06108 USA. RP Eldridge, JI (reprint author), NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. EM jeffrey.i.eldridge@nasa.gov NR 32 TC 30 Z9 31 U1 2 U2 25 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0002-7820 J9 J AM CERAM SOC JI J. Am. Ceram. Soc. PD OCT PY 2009 VL 92 IS 10 BP 2276 EP 2285 DI 10.1111/j.1551-2916.2009.03217.x PG 10 WC Materials Science, Ceramics SC Materials Science GA 499AJ UT WOS:000270188300019 ER PT J AU Kubar, TL Hartmann, DL Wood, R AF Kubar, Terence L. Hartmann, Dennis L. Wood, Robert TI Understanding the Importance of Microphysics and Macrophysics for Warm Rain in Marine Low Clouds. Part I: Satellite Observations SO JOURNAL OF THE ATMOSPHERIC SCIENCES LA English DT Article ID DROPLET SIZE DISTRIBUTIONS; BOUNDARY-LAYER CLOUDS; LIQUID WATER PATH; STRATOCUMULUS CLOUDS; EFFECTIVE RADIUS; STRATIFORM CLOUDS; RADIATION BUDGET; DRIZZLE; ALBEDO; RADAR AB The importance of macrophysical variables [cloud thickness, liquid water path (LWP)] and microphysical variables (effective radius r(e), effective droplet concentration N-eff) on warm drizzle intensity and frequency across the tropics and subtropics is studied. In this first part of a two-part study, Moderate Resolution Imaging Spectroradiometer (MODIS) optical and CloudSat cloud radar data are used to understand warm rain in marine clouds. Part 11 uses simple heuristic models. Cloud-top height and LWP substantially increase as drizzle intensity increases. Droplet radius estimated from MODIS also increases with cloud radar reflectivity (dBZ) but levels off as dBZ > 0, except where the influence of continental pollution is present, in which case a monotonic increase of r(e) with drizzle intensity occurs. Off the Asian coast and over the Gulf of Mexico, r(e) values are smaller (by several mu m) and N-eff values are larger compared to more remote marine regions. For heavy drizzle intensity, both r(e) and N-eff values off the Asian coast and over the Gulf of Mexico approach r(e) and N-eff values in more remote marine regions. Drizzle frequency, defined as profiles in which maximum dBZ > -15, increases dramatically and nearly uniformly when cloud tops grow from 1 to 2 km. Drizzle frequencies exceed 90% in all regions when LWPs exceed 250 g m(-2) and N-eff values are below 50 cm(-3), even in regions where drizzle occurs infrequently on the whole. The fact that the relationship among drizzle frequency, LWP, and N-eff is essentially the same for all regions suggests a near universality among tropical and subtropical regions. C1 [Kubar, Terence L.; Hartmann, Dennis L.; Wood, Robert] Univ Washington, Dept Atmospher Sci, Seattle, WA 98195 USA. RP Kubar, TL (reprint author), CALTECH, Jet Prop Lab, MS 183-518,4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM terry.kubar@jpl.nasa.gov RI Wood, Robert/A-2989-2008 OI Wood, Robert/0000-0002-1401-3828 FU NASA [NNG05GA19G, NNX08AG91G] FX This work was supported by NASA Grants NNG05GA19G and NNX08AG91G. The authors thank Sandra Yuter and two anonymous referees for their comments on this manuscript. NR 52 TC 56 Z9 56 U1 3 U2 14 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0022-4928 J9 J ATMOS SCI JI J. Atmos. Sci. PD OCT PY 2009 VL 66 IS 10 BP 2953 EP 2972 DI 10.1175/2009JAS3071.1 PG 20 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 505ZO UT WOS:000270741700001 ER PT J AU Ibrahim, MB Danila, D Simon, TW Gedeon, D Tew, R AF Ibrahim, Mounir B. Danila, Daniel Simon, Terrence W. Gedeon, David Tew, Roy TI Computational Modeling of a Segmented-Involute-Foil Regenerator for Stirling Engines SO JOURNAL OF THERMOPHYSICS AND HEAT TRANSFER LA English DT Article AB A microfabricated, segmented-involute-foil regenerator was numerically investigated using the Fluent commercial software under both steady- and oscillatory-flow conditions and using two- and three-dimensional numerical simulations. Steady-state simulations were performed for Re = 50-2000. The oscillatory-flow conditions were performed for Re(max) = 50 and Re(omega) = 0.229, with the hot end at 310 K and the cold end at 293 K. For the steady-state three-dimensional simulation, both the local friction factor and the local mean Nusselt numbers started to depart from the two-dimensional simulation values upon entering the second layer. At the entrance of every layer, the forced reorientation of the flow results in small rises of both the friction factor and the mean Nusselt number, with subsequent decrease as the flow settles into the new layer. As for the oscillatory-flow simulations, the two-dimensional model was used to study the effects of changing 1) the oscillation amplitude and frequency, 2) the thermal contact resistance between layers, and 3) the solid material. The effects of these parameters on the total regenerator beat loss (convection and conduction) were documented and are expected to be a useful tool for further development of Stirling engine regenerators. C1 [Ibrahim, Mounir B.; Danila, Daniel] Cleveland State Univ, Dept Mech Engn, Cleveland, OH 44115 USA. [Simon, Terrence W.] Univ Minnesota, Dept Mech Engn, Minneapolis, MN 55455 USA. [Gedeon, David] Gedeon Associates, Athens, OH 45701 USA. [Tew, Roy] NASA, John H Glenn Res Ctr Lewis Field, Cleveland, OH 44135 USA. RP Ibrahim, MB (reprint author), Cleveland State Univ, Dept Mech Engn, 1960 E 24th St,Room 261,Stillwell Hall, Cleveland, OH 44115 USA. FU NASA Glenn Research Center at Lewis Field under NASA [NAS3-03124] FX We are grateful for sponsorship of this effort by the NASA Headquarters Science Mission Directorate and the Radioisotope Power System Program and for the support of the NASA Glenn Research Center at Lewis Field under NASA Contract NAS3-03124, for which the Contracting Officer's Technical Representative was Roy Tew. We wish to acknowledge the valuable guidance we received from our team of advisors: James Cairelli (retired) and Randy Bowman, both of NASA Glenn Research Center at Lewis Field, and David Berchowitz at Global Cooling, Inc. NR 12 TC 2 Z9 3 U1 0 U2 8 PU AMER INST AERONAUT ASTRONAUT PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0887-8722 J9 J THERMOPHYS HEAT TR JI J. Thermophys. Heat Transf. PD OCT-DEC PY 2009 VL 23 IS 4 BP 786 EP 800 DI 10.2514/1.40330 PG 15 WC Thermodynamics; Engineering, Mechanical SC Thermodynamics; Engineering GA 509GD UT WOS:000271002100016 ER PT J AU Boyle, RJ Stripf, M AF Boyle, R. J. Stripf, M. TI Simplified Approach to Predicting Rough Surface Transition SO JOURNAL OF TURBOMACHINERY-TRANSACTIONS OF THE ASME LA English DT Article DE aerodynamics; blades; engines; gas turbines; heat transfer; laminar flow; statistical analysis; surface roughness; turbulence ID TURBULENT BOUNDARY-LAYER; HEAT-TRANSFER; PERFORMANCE; FLOWS; VANE AB Turbine vane heat transfer predictions are given for smooth and rough vanes where the experimental data show transition moving forward on the vane as the surface roughness physical height increases. Consistent with smooth vane heat transfer, the transition moves forward for a fixed roughness height as the Reynolds number increases. Comparisons are presented with published experimental data. Some of the data are for a regular roughness geometry with a range of roughness heights, Reynolds numbers, and inlet turbulence intensities. The approach taken in this analysis is to treat the roughness in a statistical sense, consistent with what would be obtained from blades measured after exposure to actual engine environments. An approach is given to determine the equivalent sand grain roughness from the statistics of the regular geometry. This approach is guided by the experimental data. A roughness transition criterion is developed, and comparisons are made with experimental data over the entire range of experimental test conditions. Additional comparisons are made with experimental heat transfer data, where the roughness geometries are both regular and statistical. Using the developed analysis, heat transfer calculations are presented for the second stage vane of a high pressure turbine at hypothetical engine conditions. C1 [Boyle, R. J.] NASA Glenn Res Ctr, Cleveland, OH 44135 USA. [Stripf, M.] Univ Karlsruhe, D-76128 Karlsruhe, Germany. RP Boyle, RJ (reprint author), NASA Glenn Res Ctr, Cleveland, OH 44135 USA. EM robert.j.boyle@grc.nasa.gov; matthias.stripf@its.uni-karlsruhe.de NR 45 TC 4 Z9 5 U1 2 U2 7 PU ASME-AMER SOC MECHANICAL ENG PI NEW YORK PA THREE PARK AVE, NEW YORK, NY 10016-5990 USA SN 0889-504X J9 J TURBOMACH JI J. Turbomach.-Trans. ASME PD OCT PY 2009 VL 131 IS 4 AR 041020 DI 10.1115/1.3072521 PG 11 WC Engineering, Mechanical SC Engineering GA 470NW UT WOS:000267983300019 ER PT J AU West, KL Walker, WA Baird, RW White, W Levine, G Brown, E Schofield, D AF West, Kristi L. Walker, William A. Baird, Robin W. White, Whitney Levine, Gregg Brown, Eric Schofield, David TI Diet of pygmy sperm whales (Kogia breviceps) in the Hawaiian Archipelago SO MARINE MAMMAL SCIENCE LA English DT Article ID VERTICAL DISTRIBUTION C1 [West, Kristi L.; White, Whitney] Hawaii Pacific Univ, Coll Nat Sci, Kaneohe, HI 96744 USA. [Walker, William A.] NOAA, Natl Marine Fisheries Serv, Natl Marine Mammal Lab, Alaska Fisheries Sci Ctr, Seattle, WA 98115 USA. [Baird, Robin W.] Cascadia Res Collect, Olympia, WA 98501 USA. [Brown, Eric] Natl Pk Serv, Kalaupapa, HI 96742 USA. [Schofield, David] NOAA, Pacific Isl Reg Off, Natl Marine Fisheries Serv, Honolulu, HI 96814 USA. RP West, KL (reprint author), Hawaii Pacific Univ, Coll Nat Sci, 45-045 Kamehameha Highway, Kaneohe, HI 96744 USA. EM kwest@hpu.edu FU Prescott grant program FX We would like to thank John Klavitter, Thierry Work, and other stranding responders involved in the collection of the pygmy sperm whale stomach contents. We are also grateful to Jeffery Drazen, Brad Seibel, and Steve Haddock for assistance in the interpretation of our results. Richard Young was particularly helpful in sharing his knowledge on the vertical distribution of Hawaiian cephalopods and provided assistance in the identification of the histioteuthid and mastigoteuthid beaks. Susan Chivers confirmed the species identification of the Midway individual. We also thank Mariana Kuprijanova for her assistance with the references and Nicole Davis for her efforts to track down one of the missing samples. We would also like to thank the Prescott grant program for supporting stranding response efforts in the Pacific Islands region. NR 26 TC 8 Z9 10 U1 1 U2 12 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0824-0469 EI 1748-7692 J9 MAR MAMMAL SCI JI Mar. Mamm. Sci. PD OCT PY 2009 VL 25 IS 4 BP 931 EP 943 DI 10.1111/j.1748-7692.2009.00295.x PG 13 WC Marine & Freshwater Biology; Zoology SC Marine & Freshwater Biology; Zoology GA 509VI UT WOS:000271046600011 ER PT J AU Hatamleh, O Rivero, IV Swain, SE AF Hatamleh, Omar Rivero, Iris V. Swain, Shayla E. TI An investigation of the residual stress characterization and relaxation in peened friction stir welded aluminum-lithium alloy joints SO MATERIALS & DESIGN LA English DT Article DE Non-ferrous metals and alloys; Surface treatment; Fatigue ID FATIGUE-CRACK GROWTH; BUTT JOINTS AB In this investigation the residual stresses generated from friction stir welded (FSW) 2195 aluminum-lithium alloy joints were characterized. The results derived from this research revealed significant levels of tensile residual stresses at the surface and throughout the thickness of the FSW samples. Furthermore, residual stress relaxation at the surface and throughout the thickness of the samples was assessed for laser peened friction stir welded aluminum-lithium joints. To do so the samples were cycled several times at a constant amplitude load. The results indicated that most of the relaxation for the surface residual stresses took place during the first cycle of loading. Also, residual stresses relaxation throughout the thickness of the welded region of unpeened samples significantly exceeded the relaxation exhibited by the laser peened samples. Published by Elsevier Ltd. C1 [Hatamleh, Omar] NASA, Lyndon B Johnson Space Ctr, Struct Branch, Houston, TX 77058 USA. [Rivero, Iris V.; Swain, Shayla E.] Texas Tech Univ, Dept Ind Engn, Lubbock, TX 79409 USA. RP Hatamleh, O (reprint author), NASA, Lyndon B Johnson Space Ctr, Struct Branch, Houston, TX 77058 USA. EM omar.hatamleh-1@nasa.gov NR 17 TC 11 Z9 11 U1 1 U2 12 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0261-3069 J9 MATER DESIGN JI Mater. Des. PD OCT PY 2009 VL 30 IS 9 BP 3367 EP 3373 DI 10.1016/j.matdes.2009.03.038 PG 7 WC Materials Science, Multidisciplinary SC Materials Science GA 469JA UT WOS:000267892200004 ER PT J AU Matlik, JF Farris, TN Haynes, J Swanson, GR Ham-Battista, G AF Matlik, J. F. Farris, T. N. Haynes, J. Swanson, G. R. Ham-Battista, G. TI Prediction of fretting crack location and orientation in a single crystal nickel alloy SO MECHANICS OF MATERIALS LA English DT Article ID DOVETAIL ATTACHMENTS; CONTACTS; SUPERALLOY; STRESSES AB Fretting is a structural damage mechanism that occurs when two clamped surfaces are subjected to an oscillatory loading. A critical location for fretting induced damage has been identified at the blade/disk and blade/damper interfaces of gas turbine engine turbomachinery and space propulsion components. The high-temperature, high-frequency loading environment seen by these components lead to severe stress gradients at the edge-of-contact that could potentially foster crack growth leading to premature component failure. Recently, a high-frequency, high-temperature load frame has been designed for experimentally investigating fretting damage of single crystal nickel materials employed in aircraft and spacecraft turbomachinery [Matlik, J., Farris, T.. Haake, F., Swanson, G., Duke, G., 2007. High-frequency, high-temperature fretting experiments. Wear 261, 1367-1382]. A modeling method for characterizing the fretting stresses of the spherical fretting contact stress behavior in this experiment is developed and described. The calculated fretting stresses for a series of experiments are then correlated to the observed fretting damage. Results show that knowledge of the normal stresses and resolved shear stresses on each crystal plane can aid in predicting fretting fatigue initiated crack locations and orientations. (C) 2009 Elsevier Ltd. All rights reserved. C1 [Matlik, J. F.] Rolls Royce Corp, Design Syst Engn, Indianapolis, IN 46206 USA. [Farris, T. N.] Purdue Univ, Sch Aeronaut & Astronaut, W Lafayette, IN 47907 USA. [Haynes, J.] United Technol Corp, Pratt & Whitney Space Propuls, Jupiter, FL 33478 USA. [Swanson, G. R.] NASA, George C Marshall Space Flight Ctr, EM20, Damage Tolerance Assessment Branch, Huntsville, AL 35812 USA. [Ham-Battista, G.] Sverdrup Technol Inc, MSFC Grp, Huntsville, AL 35806 USA. RP Matlik, JF (reprint author), Rolls Royce Corp, Design Syst Engn, Box 420, Indianapolis, IN 46206 USA. EM John.F.Matlik@rolls-royce.com NR 20 TC 2 Z9 3 U1 2 U2 14 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0167-6636 J9 MECH MATER JI Mech. Mater. PD OCT PY 2009 VL 41 IS 10 BP 1133 EP 1151 DI 10.1016/j.mechmat.2009.04.002 PG 19 WC Materials Science, Multidisciplinary; Mechanics SC Materials Science; Mechanics GA 505NC UT WOS:000270699500009 ER PT J AU Yanovsky, I Leow, AD Lee, S Osher, SJ Thompson, PM AF Yanovsky, Igor Leow, Alex D. Lee, Suh Osher, Stanley J. Thompson, Paul M. TI Comparing registration methods for mapping brain change using tensor-based morphometry SO MEDICAL IMAGE ANALYSIS LA English DT Article DE Image registration; Unbiased nonlinear registration; Information theory; Mutual information; Tensor-based morphometry; Computational anatomy ID FALSE DISCOVERY RATE; ALZHEIMERS-DISEASE; IMAGE REGISTRATION; COMPUTATIONAL ANATOMY; SERIAL MRI; DEFORMATION; ATROPHY; SEGMENTATION; SHAPE; DIFFEOMORPHISMS AB Measures of brain changes can be computed from sequential MRI scans, providing valuable information on disease progression for neuroscientific studies and clinical trials. Tensor-based morphometry (TBM) creates maps of these brain changes, visualizing the 3D profile and rates of tissue growth or atrophy. In this paper, we examine the power of different nonrigid registration models to detect changes in TBM, and their stability when no real changes are present. Specifically, we investigate an asymmetric version of a recently proposed Unbiased registration method, using mutual information as the matching criterion. We compare matching functionals (sum of squared differences and mutual information), as well as large-deformation registration schemes (viscous fluid and inverse-consistent linear elastic registration methods versus Symmetric and Asymmetric Unbiased registration) for detecting changes in serial MRI scans of 10 elderly normal subjects and 10 patients with Alzheimer's Disease scanned at 2-week and 1-year intervals. We also analyzed registration results when matching images corrupted with artificial noise. We demonstrated that the unbiased methods, both symmetric and asymmetric, have higher reproducibility. The unbiased methods were also less likely to detect changes in the absence of any real physiological change. Moreover, they measured biological deformations more accurately by penalizing bias in the corresponding statistical maps. (C) 2009 Elsevier B.V. All rights reserved. C1 [Yanovsky, Igor] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Yanovsky, Igor; Osher, Stanley J.] Univ Calif Los Angeles, Dept Math, Los Angeles, CA 90095 USA. [Leow, Alex D.; Lee, Suh; Thompson, Paul M.] Univ Calif Los Angeles, Sch Med, Lab Neuro Imaging, Los Angeles, CA 90095 USA. RP Yanovsky, I (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM igor.yanovsky@jpl.nasa.gov; feuillet@ucla.edu; slee04@ucla.edu; sjo@math.ucla.edu; thompson@loni.ucla.edu RI Leow, Alex/K-3236-2014 OI Leow, Alex/0000-0002-5660-8651 FU NCRR NIH HHS [U54 RR021813, P41 RR013642, P41 RR013642-11, P41 RR13642, R21 RR019771, R21 RR019771-02, U54 RR021813-05]; NIA NIH HHS [AG016570, P50 AG016570, U01 AG024904, U01 AG024904-04]; NIBIB NIH HHS [EB01651, R21 EB001561, R21 EB001561-03]; NINDS NIH HHS [NS049194] NR 50 TC 34 Z9 34 U1 1 U2 4 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 1361-8415 J9 MED IMAGE ANAL JI Med. Image Anal. PD OCT PY 2009 VL 13 IS 5 BP 679 EP 700 DI 10.1016/j.media.2009.06.002 PG 22 WC Computer Science, Artificial Intelligence; Computer Science, Interdisciplinary Applications; Engineering, Biomedical; Radiology, Nuclear Medicine & Medical Imaging SC Computer Science; Engineering; Radiology, Nuclear Medicine & Medical Imaging GA 499YY UT WOS:000270264200001 PM 19631572 ER PT J AU Fries, M Burchell, M Kearsley, A Steele, A AF Fries, Marc Burchell, Mark Kearsley, Anton Steele, Andrew TI Capture effects in carbonaceous material: A Stardust analogue study SO METEORITICS & PLANETARY SCIENCE LA English DT Article; Proceedings Paper CT Conference on Multiscale Geo-Forensic Examination of Comet 81P/Wild 2 CY OCT 26-28, 2008 CL Timber Cove, CA SP Inst Geophys & Planetary Phys ID RAMAN D-BAND; COMET 81P/WILD-2; HYPERVELOCITY CAPTURE; AEROGEL; PARTICLES; KINETICS; GRAPHITIZATION; IMPACTS; IDENTIFICATION; TEMPERATURE AB It is reasonable to expect that cometary samples returned to Earth by the Stardust space probe have been altered to some degree during capture in aerogel at 6.1 km/s. In order to help interpret the measured structure of these particles with respect to their original cometary nature, a series of coal samples of known structure and chemical composition was fired into aerogel at Stardust capture velocity. This portion of the Study analyzed the surfaces of aerogel-em bedded particles using Raman spectroscopy. Results Show that particle surfaces are largely homogenized during capture regardless of metamorphic grade or chemical composition, apparently to include a devolatilization step during capture processing. This provides a possible mechanism for alteration of some aliphatic compound-rich phases through devolatilization of cometary carbonaceous material followed by re-condensation within the particle. Results also show that the possibility of alteration must be considered for any particular Stardust grain, as examples of both graphitization and amorphization are found in the coal samples. It is evident that Raman G band (similar to 1580 cm(-1)) parameters provide a means of characterizing Stardust carbonaceous material to include identifying those grains which have been Subjected to significant capture alteration. C1 [Fries, Marc] NASA, Jet Prop Lab, Pasadena, CA 91109 USA. [Burchell, Mark] Univ Kent, Sch Phys Sci, Canterbury CT2 7NH, Kent, England. [Kearsley, Anton] Nat Hist Museum, Dept Mineral, London SW7 5BD, England. [Steele, Andrew] Carnegie Inst Sci, Geophys Lab, Washington, DC 20001 USA. RP Fries, M (reprint author), NASA, Jet Prop Lab, 4800 Oak Grove Dr MS 183-301, Pasadena, CA 91109 USA. EM marc.d.fries@jpl.nasa.gov OI Burchell, Mark/0000-0002-2680-8943 NR 40 TC 10 Z9 10 U1 1 U2 5 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD OCT PY 2009 VL 44 IS 10 BP 1465 EP 1474 PG 10 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 537PG UT WOS:000273124800006 ER PT J AU Wirick, S Flynn, GJ Keller, LP Nakamura-Messenger, K Peltzer, C Jacobsen, C Sandford, S Zolensky, M AF Wirick, S. Flynn, G. J. Keller, L. P. Nakamura-Messenger, K. Peltzer, C. Jacobsen, C. Sandford, S. Zolensky, M. TI Organic matter from comet 81P/Wild 2, IDPs, and carbonaceous meteorites; similarities and differences SO METEORITICS & PLANETARY SCIENCE LA English DT Article; Proceedings Paper CT Conference on Multiscale Geo-Forensic Examination of Comet 81P/Wild 2 CY OCT 26-28, 2008 CL Timber Cove, CA SP Inst Geophys & Planetary Phys ID INTERPLANETARY DUST PARTICLES; X-RAY-ABSORPTION; EDGE STRUCTURE SPECTROSCOPY; ELECTRON-MICROSCOPY; FINE-STRUCTURE; RADIATION-DAMAGE; SHELL EXCITATION; STARDUST; SPECTROMICROSCOPY; MOLECULES AB During preliminary examination of 81P/Wild 2 particles collected by the NASA Stardust spacecraft, we analyzed seven, sulfur embedded and ultramicrotomed particles extracted from five different tracks. Sections were analyzed using a scanning transmission X-ray microscope (SXTM) and carbon X-ray absorption near edge structure (XANES) spectra were collected. We compared the carbon XANES spectra of these Wild 2 samples with a database of spectra on thirty-four interplanetary dust particles (IDPs) and with several meteorites. Two of the particles analyzed are iron sulfides and there is evidence that ail aliphatic compound associated with these particles can survive high temperatures. An iron sulfide from ail IDP demonstrates the same phenomenon. Another, mostly carbon free containing particle radiation damaged, something we have not observed in any IDPs we have analyzed or any indigenous organic matter from the carbonaceous meteorites, Tagish Lake, Orgueil, Bells and Murchison. The carbonaceous material associated with this particle showed no mass loss during the initial analysis but chemically changed over a period of two months. The carbon XANES spectra of the other four particles varied more than spectra from IDPs and indigenous organic matter from meteorites. Comparison of the carbon XANES spectra from these particles with 1. the carbon XANES spectra from thirty-four IDPs (<15 micron in size) and 2. the carbon XANES spectra from carbonaceous material From the Tagish Lake, Orgueil, Bells, and Murchison meteorites show that 81P/Wild 2 carbon XANES spectra are more similar to IDP carbon XANES spectra then to the carbon XANES spectra of meteorites. C1 [Wirick, S.; Peltzer, C.; Jacobsen, C.] SUNY Stony Brook, Dept Phys & Astron, Stony Brook, NY 11794 USA. [Flynn, G. J.] SUNY Coll Plattsburgh, Dept Math, Stony Brook, NY 12903 USA. [Flynn, G. J.] SUNY Coll Plattsburgh, Dept Phys, Stony Brook, NY 12903 USA. [Keller, L. P.; Nakamura-Messenger, K.; Zolensky, M.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Sandford, S.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Wirick, S (reprint author), SUNY Stony Brook, Dept Phys & Astron, Stony Brook, NY 11794 USA. EM swirick@bnl.gov RI Jacobsen, Chris/E-2827-2015 OI Jacobsen, Chris/0000-0001-8562-0353 NR 76 TC 18 Z9 18 U1 0 U2 13 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD OCT PY 2009 VL 44 IS 10 BP 1611 EP 1626 PG 16 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 537PG UT WOS:000273124800014 ER PT J AU Druyan, LM Fulakeza, M Lonergan, P Noble, E AF Druyan, Leonard M. Fulakeza, Matthew Lonergan, Patrick Noble, Erik TI Regional climate model simulation of the AMMA Special Observing Period #3 and the pre-Helene easterly wave SO METEOROLOGY AND ATMOSPHERIC PHYSICS LA English DT Article ID TROPICAL ATLANTIC; SYSTEM; PARAMETERIZATION; DISTURBANCES; VARIABILITY; MONSOON; AFRICA AB The study examines results of dynamic downscaling of two global analyses: the National Center for Environmental Prediction/National Center for Atmospheric Research (NCEP/NCAR) reanalysis II and the Global Forecast System final analysis (FNL). Downscaling to a 0.5A degrees grid over West Africa and the adjacent Atlantic Ocean is accomplished by each of two regional models, the Regional Model, version 3 (RM3) of the Center for Climate Systems Research and the Weather, Research and Forecasting model (WRF). Simulations are for September 2006, the African Monsoon Multidisciplinary Analysis (AMMA) Special Observing Period #3 (SOP-3). The aim of this study is to exploit the increased spatial detail in the simulations and representations of climate fields by the regional models to analyze meteorological systems within the SOP-3 area of interest and time frame. In particular, the paper focuses on the regional models' representations of the structure and movement of a prominent easterly wave during September 10-13th, the precursor of Tropical Storm/Hurricane Helene. It describes the RM3 simulated structure of the developing storm in terms of circulation, precipitation, vertical motion, cumulus heating rates, and cross-sections of wind and geopotential height anomalies. Simulated cumulus heating rates within the wave's main precipitation area imply a lowering of the bases of active cumulus in the transition from the African continent to the Atlantic, indicating that the ocean environment promotes greater upward latent heat flux that in turn intensifies overlying storms. RM3 circulation, precipitation patterns, and storm trajectory are reasonably consistent with observational evidence. Experiments show that precipitation rates near 6A degrees N over the eastern North Atlantic are sensitive to vertical thermal stability, such that they are enhanced by warmer in situ sea-surface temperatures (SSTs) and diminished by colder SSTs. However, prescribing colder SST causes increases in precipitation north of 9A degrees N within areas of large scale upward vertical motion where rainfall rates are less sensitive to in situ SSTs. The evaluation of WRF indicates that its storm propagation is too fast over West Africa, where associated WRF precipitation rates are exaggerated, but its performance is improved over the Atlantic. C1 [Druyan, Leonard M.; Fulakeza, Matthew; Lonergan, Patrick] Columbia Univ, NASA, Goddard Inst Space Studies, NYC, New York, NY 10027 USA. [Druyan, Leonard M.; Fulakeza, Matthew; Lonergan, Patrick] Columbia Univ, Ctr Climate Syst Res, New York, NY USA. [Noble, Erik] Univ Colorado, Boulder, CO 80309 USA. RP Druyan, LM (reprint author), Columbia Univ, NASA, Goddard Inst Space Studies, NYC, New York, NY 10027 USA. EM LDruyan@giss.nasa.gov FU National Science Foundation [ATM-0652518]; National Aeronautics and Space Administration (NAMMA) [NNX07A193G]; National Aeronautics and Space Administration FX This research was supported by National Science Foundation grant ATM-0652518, National Aeronautics and Space Administration (NAMMA) grant NNX07A193G, and by the National Aeronautics and Space Administration Climate and Earth Observing System Program. E. Noble is a Fellow of the National Aeronautics and Space Administration Graduate Student Researchers Program. Helpful discussion about cumulus heating rate profiles with Dr. A. Del Genio is acknowledged. We gratefully acknowledge assistance from the WRF help desk at the National Center for Atmospheric Research and helpful consultations concerning WRF with Dr. Jimy Dudhia. TRMM data used in this study were acquired using the GES-DISC Interactive Online Visualization and Analysis Infrastructure (Giovanni) as part of the NASA's Goddard Earth Sciences (GES) Data and Information Services Center (DISC). NCEP reanalysis II data used in this study were obtained on-line from the National Oceanographic and Atmospheric Agency/Earth System Research Laboratory (Physical Sciences Division). FEWS data sets were created at the National Oceanographic and Atmospheric Agency Climate Prediction Center and made available on-line by the International Research Institute for Climate Prediction of Columbia University. NR 23 TC 6 Z9 6 U1 0 U2 3 PU SPRINGER WIEN PI WIEN PA SACHSENPLATZ 4-6, PO BOX 89, A-1201 WIEN, AUSTRIA SN 0177-7971 EI 1436-5065 J9 METEOROL ATMOS PHYS JI Meteorol. Atmos. Phys. PD OCT PY 2009 VL 105 IS 3-4 BP 191 EP 210 DI 10.1007/s00703-009-0044-5 PG 20 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 501MJ UT WOS:000270385700007 ER PT J AU Greenhall, CA AF Greenhall, Charles A. TI Linear invariant estimation of clock phase and trend from noisy phase data SO METROLOGIA LA English DT Article ID FREQUENCY; UNCERTAINTY; PREDICTION; THEOREM; TIME AB We show how to solve two problems of optimal linear estimation from a set of noisy measurements of clock phase. The phase is modelled as a process with stationary dth increments, e. g. a sum of processes with power-law spectra. The additive measurement noise can be any mean-zero process with a known autocovariance function. The estimation targets are the phase at a given time and the coefficient of the overall trend, e. g. the frequency drift. A feasibility condition called 'invariance' is imposed according to the target and the degree of non-stationarity of the phase model. The solution of a set of linear equations gives the regression coefficients and the mean squared error of the best linear invariant estimate. Proofs of these results are available from the online version of this journal. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Greenhall, CA (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,MS 298, Pasadena, CA 91109 USA. EM cgreenhall@jpl.nasa.gov FU Jet Propulsion Laboratory, California Institute of Technology3; National Aeronautics and Space Administration FX This work was performed by the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the . NR 24 TC 2 Z9 2 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0026-1394 J9 METROLOGIA JI Metrologia PD OCT PY 2009 VL 46 IS 5 BP 569 EP 577 DI 10.1088/0026-1394/46/5/022 PG 9 WC Instruments & Instrumentation; Physics, Applied SC Instruments & Instrumentation; Physics GA 501NE UT WOS:000270387800026 ER PT J AU Azua-Bustos, A Gonzalez-Silva, C Mancilla, RA Salas, L Palma, RE Wynne, JJ McKay, CP Vicuna, R AF Azua-Bustos, A. Gonzalez-Silva, C. Mancilla, R. A. Salas, L. Palma, R. E. Wynne, J. J. McKay, C. P. Vicuna, R. TI Ancient Photosynthetic Eukaryote Biofilms in an Atacama Desert Coastal Cave SO MICROBIAL ECOLOGY LA English DT Article ID RED ALGAE RHODOPHYTA; 16S RIBOSOMAL-RNA; CYANIDIUM-CALDARIUM; HYPERARID CORE; MICROBIAL LIFE; NORTHERN CHILE; NATIONAL-PARK; LAMP-FLORA; CYANOBACTERIA; DIVERSITY AB Caves offer a stable and protected environment from harsh and changing outside prevailing conditions. Hence, they represent an interesting habitat for studying life in extreme environments. Here, we report the presence of a member of the ancient eukaryote red algae Cyanidium group in a coastal cave of the hyperarid Atacama Desert. This microorganism was found to form a seemingly monospecific biofilm growing under extremely low photon flux levels. Our work suggests that this species, Cyanidium sp. Atacama, is a new member of a recently proposed novel monophyletic lineage of mesophilic "cave" Cyanidium sp., distinct from the remaining three other lineages which are all thermo-acidophilic. The cave described in this work may represent an evolutionary island for life in the midst of the Atacama Desert. C1 [Azua-Bustos, A.; Mancilla, R. A.; Salas, L.; Vicuna, R.] Pontificia Univ Catolica Chile, Dept Mol Genet & Microbiol, Fac Ciencias Biol, Santiago, Chile. [Gonzalez-Silva, C.] Univ Arturo Prat, Dept Ciencias Quim & Farmaceut, Iquique, Chile. [Wynne, J. J.] No Arizona Univ, USGS, SW Biol Sci Ctr, Flagstaff, AZ 86011 USA. [Wynne, J. J.] No Arizona Univ, Dept Biol Sci, Flagstaff, AZ 86011 USA. [McKay, C. P.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Azua-Bustos, A.; Vicuna, R.] Millennium Inst Fundamental & Appl Biol, Santiago, Chile. [Palma, R. E.] Pontificia Univ Catolica Chile, Fac Ciencias Biol, Dept Ecol, Santiago, Chile. RP Azua-Bustos, A (reprint author), Pontificia Univ Catolica Chile, Dept Mol Genet & Microbiol, Fac Ciencias Biol, Alameda 340, Santiago, Chile. EM ajazua@uc.cl RI mancilla, rodrigo/C-8380-2011; Palma, Eduardo/N-1416-2014; azua-bustos, armando/P-8787-2016 FU Millennium Institute of Fundamental and Applied Biology (Chile) FX This work was supported by the Millennium Institute of Fundamental and Applied Biology (Chile). We also thank the members of Rafael Vicuna's Laboratory for critical comments and insights which helped to improve this manuscript. NR 55 TC 14 Z9 17 U1 0 U2 16 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0095-3628 J9 MICROB ECOL JI Microb. Ecol. PD OCT PY 2009 VL 58 IS 3 BP 485 EP 496 DI 10.1007/s00248-009-9500-5 PG 12 WC Ecology; Marine & Freshwater Biology; Microbiology SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Microbiology GA 495XH UT WOS:000269928300004 PM 19259626 ER PT J AU Gayon-Markt, J Bois, E AF Gayon-Markt, Julie Bois, Eric TI On fitting planetary systems in counter-revolving configurations SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE techniques: radial velocities; planetary systems ID M4 DWARF; GJ-876; STAR AB In Gayon & Bois and Gayon, Bois & Scholl, (i) we studied the theoretical feasibility and efficiency of retrograde mean motion resonances (i. e. two planets are both in orbital resonance and in counter-revolving configuration), (ii) we showed that retrograde resonances can generate interesting mechanisms of stability and (iii) we obtained a dynamical fit involving a counter-revolving configuration that is consistent with the observations of the HD 73526 planetary system. In the present Letter, we present and analyse data reductions assuming counter-revolving configurations for eight compact multiplanetary systems detected through the radial velocity method. In each case, we select the best fit leading to a dynamically stable solution. The resulting data reductions obtained in rms and root chi(2)(nu) values for counter-revolving configurations are of the same order, and sometimes slightly better than for prograde configurations. In the end, these fits tend to show that, over the eight studied multiplanetary systems, six of them could be regulated by a mechanism involving a counter-revolving configuration. C1 [Gayon-Markt, Julie; Bois, Eric] Univ Nice Sophia Antipolis, CNRS, Observ Cote Azur, F-06304 Nice 4, France. [Gayon-Markt, Julie] NASA, Ames Res Ctr, Space Sci & Astrobiol Div, Moffett Field, CA 94035 USA. RP Gayon-Markt, J (reprint author), Univ Nice Sophia Antipolis, CNRS, Observ Cote Azur, BP 4229, F-06304 Nice 4, France. EM julie.gayon@oca.eu FU NASA FX Computations have been done on the 'Mesocentre SIGAMM' machine, hosted by Observatoire de la Coted'Azur. Julie Gayon-Markt is supported through the NASA Postdoctoral Program. NR 17 TC 5 Z9 5 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 OCT PY 2009 VL 399 IS 1 BP L137 EP L140 DI 10.1111/j.1745-3933.2009.00740.x PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 678WM UT WOS:000284113800029 ER PT J AU Miller, L Turner, TJ Reeves, JN AF Miller, L. Turner, T. J. Reeves, J. N. TI The absorption-dominated model for the X-ray spectra of type I active galaxies: MCG-6-30-15 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion, accretion discs; galaxies: active; galaxies: individual: MCG-6-30-15; X-rays: galaxies ID GALACTIC NUCLEI; BLACK-HOLE; XMM-NEWTON; IRON LINE; PHOTOIONIZATION; VARIABILITY; REFLECTION; DISK; ABSORBER; MATTER AB MCG-6-30-15 is the archetypal example of a type I active galaxy showing broad 'red-wing' emission in its X-ray spectrum at energies below the 6.4 keV Fe K alpha emission line and a continuum excess above 20 keV. Miller et al. showed that these spectral features could be caused by clumpy absorbing material, but Reynolds et al. have argued that the observed Fe K alpha line luminosity is inconsistent with this explanation unless the global covering factor of the absorber(s) is very low. However, the Reynolds et al. calculation effectively considers the only source of opacity to be the FeK bound-free transition and neglects the opacity at the line energy: correction to realistic opacity decreases the predicted line flux by a large factor. We also discuss the interpretation of the covering factor and the possible effect of occultation by the accretion disc. Finally, we consider a model for MCG-6-30-15 dominated by clumpy absorption, which is consistent with a global covering factor of 0.45, although models that include the effects of Compton scattering are required to reach a full understanding. Variations in covering fraction may dominate the observed X-ray spectral variability. C1 [Miller, L.] Univ Oxford, Dept Phys, Oxford OX1 3RH, England. [Turner, T. J.] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA. [Turner, T. J.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Reeves, J. N.] Keele Univ, Sch Phys & Geog Sci, Astrophys Grp, Keele ST5 8EH, Staffs, England. RP Miller, L (reprint author), Univ Oxford, Dept Phys, Denys Wilkinson Bldg,Keble Rd, Oxford OX1 3RH, England. EM L.Miller1@physics.ox.ac.uk FU NASA [NNX08AJ41G] FX We are grateful to Tim Kallman for providing and updating XSTAR. Rapid production of XSTAR tables was possible using PVM_XSTAR (Noble et al. 2009). TJT acknowledges NASA grant NNX08AJ41G. NR 36 TC 47 Z9 47 U1 2 U2 2 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD OCT PY 2009 VL 399 IS 1 BP L69 EP L73 DI 10.1111/j.1745-3933.2009.00726.x PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 678WM UT WOS:000284113800015 ER PT J AU Marquis, EA Miller, MK Blavette, D Ringer, SP Sudbrack, CK Smith, GDW AF Marquis, Emmanuelle A. Miller, Michael K. Blavette, Didier Ringer, Simon P. Sudbrack, Chantal K. Smith, George D. W. TI Structural Materials: Understanding Atomic-Scale Microstructures SO MRS BULLETIN LA English DT Article ID GRAIN-BOUNDARY SEGREGATION; FE-CR ALLOYS; NI-AL-CR; MG-SI ALLOYS; PROBE TOMOGRAPHY; SPINODAL DECOMPOSITION; COMPUTER-MODELS; TEMPORAL EVOLUTION; CU ADDITIONS; RPV STEELS AB With the ability to locate and identify atoms in three dimensions, atom-probe tomography (APT) has revolutionized our understanding of structure-property relationships in materials used for structural applications. The atomic-scale details of clusters, second phases, and microstructural defects that control alloy properties have been investigated, providing an unprecedented level of detail on the origins of aging behavior, strength, creep, fracture toughness, corrosion, and irradiation resistance. Moreover, atomic-scale microscopy combined with atomistic simulation and theoretical modeling of material behavior can guide new alloy design. In this article, selected examples highlight how APT has led to a deeper understanding of materials structures and therefore properties, starting with the phase transformations controlling the aging and strengthening behavior of complex Al-, Fe-, and Ni-based alloys systems. The chemistry of interfaces and structural defects that play a crucial role in high-temperature strengthening, fracture, and corrosion resistance are also discussed, with particular reference to Zr- and Al-alloys and FeAl intermetallics. C1 [Ringer, Simon P.] Univ Sydney, Australian Key Ctr Microscopy & Microanal, Sydney, NSW 2006, Australia. [Sudbrack, Chantal K.] NASA, Glenn Res Ctr, Mat & Struct Div, Cleveland, OH USA. [Smith, George D. W.] Univ Oxford, Oxford OX1 2JD, England. [Blavette, Didier] Univ Rouen, F-76821 Mont St Aignan, France. [Blavette, Didier] CNRS, UMR 6634, Grp Phys Mat, F-75700 Paris, France. EM emmanuelle.marquis@materials.ox.ac.uk; millermk@ornl.gov; Didier.blavette@univ-rouen.fr; s.ringer@usyd.edu.au; chantal.k.sudbrack@nasa.gov; george.smith@materials.ox.ac.uk RI Ringer, Simon/E-3487-2012; Blavette, Didier/J-9488-2013; Marquis, Emmanuelle/O-5647-2014 OI Ringer, Simon/0000-0002-1559-330X; Marquis, Emmanuelle/0000-0002-6476-2835 FU UK Engineering Physical Science and Research Council; Australian Research Council; U.S. National Science Foundation, Division of Materials Research; U.S. Department of Energy, Division of Materials Sciences and Engineering FX The research reviewed in this article was originally sponsored, in part, by the UK Engineering Physical Science and Research Council, the Australian Research Council, the U.S. National Science Foundation, Division of Materials Research, the U.S. Department of Energy, Division of Materials Sciences and Engineering, and the Scientific User Facilities Division, Office of Basic Energy Sciences, U.S. Department of Energy for the Oak Ridge National Laboratory SHaRE User Facility. NR 69 TC 20 Z9 20 U1 1 U2 31 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 0883-7694 J9 MRS BULL JI MRS Bull. PD OCT PY 2009 VL 34 IS 10 BP 725 EP 730 PG 6 WC Materials Science, Multidisciplinary; Physics, Applied SC Materials Science; Physics GA 506TD UT WOS:000270798200013 ER PT J AU Nikolaev, P Holmes, W Sosa, E Boul, P Arepalli, S AF Nikolaev, Pavel Holmes, William Sosa, Edward Boul, Peter Arepalli, Sivaram TI Effect of the Laser Heating of Nanotube Nuclei on the Nanotube Type Population SO NANO RESEARCH LA English DT Article; Proceedings Paper CT 4th Workshop on Growth Mechanisms of Single-Wall Carbon Nanotubes CY APR 17-21, 2009 CL Boerne, TX SP NASA, Johnson Space Ctr, Rice Univ, Air Force Res Lab, Dayton DE Nanotube synthesis; pulsed laser vaporization; nanotube population ID WALL CARBON NANOTUBES; CATALYTIC GROWTH; ABLATION PROCESS; DIFFRACTION; ROPES AB Many potential applications of carbon nanotubes are expected to benefit from the availability of single-walled carbon nanotube materials enriched in metallic species, and specifically armchair nanotubes. The present work focuses on the modification of the pulsed laser vaporization (PLV) technique to selectively produce certain carbon nanotube structures. Nanotube nuclei were "warmed-up" with an additional laser pulse, timed to coincide approximately with the nucleation event. The effect of the second laser on the carbon vapor temperature was studied by emission spectroscopy. Nanotube type populations with and without warm-up were compared by means of absorption, photoluminescence, and Raman spectroscopy. It was found that the warm-up of nanotube nuclei with a laser pulse has a noticeable, albeit small, effect on the nanotube population. The intensity of spectral features associated with (9,7) nanotube and its large chiral angle neighbors increased, while small chiral angle nanotubes decreased, with exception of the (15,0) tube. This experiment demonstrates that nanotube population during PLV synthesis can be manipulated in a controlled fashion. C1 [Holmes, William] Univ Texas Dallas, Alan G MacDiarmid NanoTech Inst, Richardson, TX 75080 USA. [Nikolaev, Pavel; Arepalli, Sivaram] Sungkyunkwan Univ, Dept Energy Sci, Suwon 440746, South Korea. [Sosa, Edward; Boul, Peter] NASA, Lyndon B Johnson Space Ctr, ERC Inc, Houston, TX 77258 USA. RP Nikolaev, P (reprint author), Sungkyunkwan Univ, Dept Energy Sci, 300 Cheoncheon Dong, Suwon 440746, South Korea. EM pasha.nikolaev@gmail.com RI Arepalli, Sivaram/A-5372-2010; Nikolaev, Pavel/B-9960-2009 NR 32 TC 2 Z9 2 U1 0 U2 13 PU TSINGHUA UNIV PRESS PI BEIJING PA TSINGHUA UNIV, RM A703, XUEYAN BLDG, BEIJING, 10084, PEOPLES R CHINA SN 1998-0124 J9 NANO RES JI Nano Res. PD OCT PY 2009 VL 2 IS 10 SI SI BP 818 EP 827 DI 10.1007/s12274-009-9086-8 PG 10 WC Chemistry, Physical; Nanoscience & Nanotechnology; Materials Science, Multidisciplinary; Physics, Applied SC Chemistry; Science & Technology - Other Topics; Materials Science; Physics GA 548DM UT WOS:000273939800009 ER PT J AU Migliaccio, M Natoli, P De Troia, G Hikage, C Komatsu, E Ade, PAR Bock, JJ Bond, JR Borrill, J Boscaleri, A Contaldi, CR Crill, BP de Bernardis, P de Gasperis, G de Oliveira-Costa, A Di Stefano, G Hivon, E Kisner, TS Jones, WC Lange, AE Masi, S Mauskopf, PD MacTavish, CJ Melchiorri, A Montroy, TE Netterfield, CB Pascale, E Piacentini, F Polenta, G Ricciardi, S Romeo, G Ruhl, JE Tegmark, M Veneziani, M Vittorio, N AF Migliaccio, M. Natoli, P. De Troia, G. Hikage, C. Komatsu, E. Ade, P. A. R. Bock, J. J. Bond, J. R. Borrill, J. Boscaleri, A. Contaldi, C. R. Crill, B. P. de Bernardis, P. de Gasperis, G. de Oliveira-Costa, A. Di Stefano, G. Hivon, E. Kisner, T. S. Jones, W. C. Lange, A. E. Masi, S. Mauskopf, P. D. MacTavish, C. J. Melchiorri, A. Montroy, T. E. Netterfield, C. B. Pascale, E. Piacentini, F. Polenta, G. Ricciardi, S. Romeo, G. Ruhl, J. E. Tegmark, M. Veneziani, M. Vittorio, N. TI Probing primordial non Gaussianity in the BOOMERanG CMB maps: an analysis based on analytical Minkowski functionals SO NUCLEAR PHYSICS B-PROCEEDINGS SUPPLEMENTS LA English DT Proceedings Paper CT Galileo-Galilei-Institute Conference on Dark Matter and Dark Energy CY JAN 19-MAR 12, 2009 CL Florence, ITALY SP Galileo Galilei Inst ID ANGULAR POWER SPECTRUM; LARGE-SCALE STRUCTURE; 2003 FLIGHT; WMAP OBSERVATIONS; COSMOLOGICAL PARAMETERS; TEMPERATURE ANISOTROPY; INFLATIONARY MODELS; MAKING ALGORITHM; MICROWAVE; BISPECTRUM AB Minkowski functionals are a powerful tool to constrain the Gaussianity of the Cosmic Microwave Background (CMB). In the limit of a weakly non Gaussian field, a perturbative approach can be derived [14] that is completely based on analytical formulae without requiring computationally intensive, dedicated Monte Carlo non Gaussian simulations of the CMB anisotropy. We apply this machinery to an intensity map derived from the 1998 and 2003 flights of BOOMERanG, analyzed here together for the first time. We set limits on the non-linear coupling parameter f(NL) as -1020 < f(NL) < 390 at 95% CL, markedly improving the previous constraints set by 191 whose analysis was limited to the BOOMERanG 2003 dataset. These limits are the most stringent ever set among suborbital experiments. C1 [Migliaccio, M.; Natoli, P.; De Troia, G.; de Gasperis, G.; Vittorio, N.] Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy. [Hikage, C.; Ade, P. A. R.; Mauskopf, P. D.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Komatsu, E.] Univ Texas Austin, Texas Cosmol Ctr, Univ Stn 1, Austin, TX 78712 USA. [Bock, J. J.; Crill, B. P.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Bond, J. R.] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 1A1, Canada. [Borrill, J.; Kisner, T. S.; Ricciardi, S.] Univ Calif Berkeley, Lawrence Berkeley Lab, Computat Res Div, Berkeley, CA 94720 USA. [Boscaleri, A.] CNR, IFAC, Florence, Italy. [Contaldi, C. R.] Univ London Imperial Coll Sci Technol & Med, Theoret Phys Grp, London SW7 2AZ, England. [de Bernardis, P.; Masi, S.; Melchiorri, A.; Piacentini, F.; Polenta, G.; Veneziani, M.] Univ Roma La Sapienza, Dipartimento Fis, I-00185 Rome, Italy. [de Oliveira-Costa, A.; Tegmark, M.] MIT, Dept Phys, Cambridge, MA 02139 USA. [Di Stefano, G.; Romeo, G.] Ist Nazl Geofis & Vulcanol, I-00143 Rome, Italy. [Hivon, E.] Inst Astrophys, F-75014 Paris, France. [Jones, W. C.] Princeton Univ, Dept Phys, Princeton, NJ USA. [Lange, A. E.] CALTECH, Observ Cosmol, Pasadena, CA 91125 USA. [MacTavish, C. J.] Univ London Imperial Coll Sci Technol & Med, Astrophys Grp, London SW7 2AZ, England. [Montroy, T. E.; Ruhl, J. E.] Case Western Reserve Univ, Dept Phys, Cleveland, OH 44106 USA. [Netterfield, C. B.; Pascale, E.] Univ Toronto, Dept Phys, Toronto, ON, Canada. RP Migliaccio, M (reprint author), Univ Roma Tor Vergata, Dipartimento Fis, Via Ric Sci 1, I-00133 Rome, Italy. RI Piacentini, Francesco/E-7234-2010; OI Piacentini, Francesco/0000-0002-5444-9327; de Bernardis, Paolo/0000-0001-6547-6446; Masi, Silvia/0000-0001-5105-1439; ROMEO, Giovanni/0000-0002-5535-7803; Polenta, Gianluca/0000-0003-4067-9196; Ricciardi, Sara/0000-0002-3807-4043; Melchiorri, Alessandro/0000-0001-5326-6003; Hivon, Eric/0000-0003-1880-2733 NR 41 TC 2 Z9 2 U1 0 U2 1 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0920-5632 J9 NUCL PHYS B-PROC SUP JI Nucl. Phys. B-Proc. Suppl. PD OCT PY 2009 VL 194 BP 278 EP 286 DI 10.1016/j.nuclphysbps.2009.07.092 PG 9 WC Physics, Particles & Fields SC Physics GA 525WJ UT WOS:000272247800048 ER PT J AU Cullings, K Courty, PE AF Cullings, Ken Courty, Pierre-Emmanuel TI Saprotrophic capabilities as functional traits to study functional diversity and resilience of ectomycorrhizal community SO OECOLOGIA LA English DT Editorial Material DE Ectomycorrhizae; Saprophytic; Ecosystem function; Enzymes ID YELLOWSTONE-NATIONAL-PARK; VERTICAL-DISTRIBUTION; LIGNIN PEROXIDASE; SOIL HORIZONS; FOREST SOILS; OAK FOREST; LACCASE; FUNGI; STAND; DIFFERENTIATION AB In an accompanying editorial Dr Petr Baldrian made a case casting doubt on our recent work addressing the saprophytic potential of ectomycorrhizal (EM) fungi. Dr Baldrian's statements illustrate a very valid truth: the book is still very much open on this subject. The point he raised that the only logical reason for these fungi to be responding to high carbon demand or decreased host photosynthetic capacity by up-regulating enzymes is for the purpose of carbon acquisition is valid as well. Despite this, he makes the case that there is no compelling evidence that EM fungi exhibit saprophytic activity. The concept central to Dr Baldrian's conclusion is that even though some EM fungi possess the genes necessary for saprophytic behaviour and may even express these genes, EM fungi do not inhabit a position in the soil column that provides access to usable substrate. In this paper we present both previously published and newly obtained data that demonstrate that this assumption is erroneous, and we present arguments that place the saprophytic potential of EM fungi within a broad ecological context. C1 [Cullings, Ken] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Courty, Pierre-Emmanuel] Univ Basel, Inst Bot, CH-4056 Basel, Switzerland. RP Cullings, K (reprint author), NASA, Ames Res Ctr, MS 239-11, Moffett Field, CA 94035 USA. EM cullings1@earthlink.net; pierre.courty@unibas.ch NR 31 TC 40 Z9 40 U1 0 U2 27 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0029-8549 J9 OECOLOGIA JI Oecologia PD OCT PY 2009 VL 161 IS 4 BP 661 EP 664 DI 10.1007/s00442-009-1434-6 PG 4 WC Ecology SC Environmental Sciences & Ecology GA 495AE UT WOS:000269860700002 PM 19685248 ER PT J AU Hizlan, M Lekki, JD Nguyen, BV AF Hizlan, Murad Lekki, John D. Nguyen, Binh V. TI Glenn Research Center quantum communicator receiver design and development SO OPTICAL ENGINEERING LA English DT Article DE optical communications; receiver design; synchronization; quantum optics; photonics ID BINARY SEQUENCES; AUTOCORRELATION AB We investigate, design, and develop a prototype real-time synchronous receiver for the second-generation quantum communicator recently developed at the National Aeronautics and Space Administration (NASA) Glenn Research Center. This communication system exploits the temporal coincidences between simultaneously fired low-power laser sources to communicate at power levels several orders of magnitude less than what is currently achievable through classical means, with the ultimate goal of creating ultra-low-power microsize optical communications and sensing devices. The proposed receiver uses a unique adaptation of the early-late gate method for symbol synchronization and a newly identified 31-bit synchronization word for frame synchronization. This receiver, implemented in a field-programmable gate array (FPGA), also provides a number of significant additional features over the existing non-real-time experimental receiver, such as real-time bit error rate (BER) statistics collection and display, and recovery and display of embedded textual information. It also exhibits an indefinite run time and statistics collection. (c) 2009 Society of Photo-Optical Instrumentation Engineers. [DOI: 10.1117/1.3241989] C1 [Hizlan, Murad] Cleveland State Univ, Dept Elect & Comp Engn, Cleveland, OH 44115 USA. [Lekki, John D.] NASA, Glenn Res Ctr, Opt Instrumentat & NDE Branch, Brookpark, OH 44135 USA. [Nguyen, Binh V.] NASA, Glenn Res Ctr, Digital Commun Branch, Brookpark, OH 44135 USA. RP Hizlan, M (reprint author), Cleveland State Univ, Dept Elect & Comp Engn, 2121 Euclid Ave, Cleveland, OH 44115 USA. EM m.hizlan@csuohio.edu NR 13 TC 0 Z9 0 U1 1 U2 2 PU SPIE-SOC PHOTOPTICAL INSTRUMENTATION ENGINEERS PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98225 USA SN 0091-3286 J9 OPT ENG JI Opt. Eng. PD OCT PY 2009 VL 48 IS 10 AR 105003 DI 10.1117/1.3241989 PG 8 WC Optics SC Optics GA 519DW UT WOS:000271746200022 ER PT J AU Xu, MS Song, WZ Huang, RJ Peng, Y Shirazi, B Lahusen, R Kiely, A Peterson, N Ma, A Anusuya-Rangappa, L Miceli, M McBride, D AF Xu, Mingsen Song, Wen-Zhan Huang, Renjie Peng, Yang Shirazi, Behrooz Lahusen, Richard Kiely, Aaron Peterson, Nina Ma, Andy Anusuya-Rangappa, Lohith Miceli, Michael McBride, Devin TI Design of smart sensing components for volcano monitoring SO PERVASIVE AND MOBILE COMPUTING LA English DT Article DE Wireless sensor network; Volcano monitoring; Situation awareness; Time synchronization AB In a volcano monitoring application, various geophysical and geochemical sensors generate continuous high-fidelity data, and there is a compelling need for real-time raw data for volcano eruption prediction research. It requires the network to support network synchronized sampling, online configurable sensing and situation awareness, which pose significant challenges on sensing component design. Ideally, the resource usages shall be driven by the environment and node situations, and the data quality is optimized under resource constraints. In this paper, we present our smart sensing component design, including hybrid time synchronization, configurable sensing, and situation awareness. Both design details and evaluation results are presented to show their efficiency. Although the presented design is for a volcano monitoring application, its design philosophy and framework can also apply to other similar applications and platforms. (C) 2009 Elsevier B.V. All rights reserved. C1 [Xu, Mingsen; Song, Wen-Zhan; Huang, Renjie; Peng, Yang; Ma, Andy] Washington State Univ, Sensorweb Res Lab, Vancouver, WA 98686 USA. [Kiely, Aaron] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Lahusen, Richard] US Geol Survey, Cascades Volcano Observ, Vancouver, WA USA. [Shirazi, Behrooz; Peterson, Nina; Anusuya-Rangappa, Lohith] Washington State Univ, Sch Elect Engn & Comp Sci, Pullman, WA 99163 USA. [Miceli, Michael] Louisiana State Univ, Sch Comp Sci, Baton Rouge, LA 70803 USA. [McBride, Devin] Seattle Univ, Sch Comp Sci, Seattle, WA 98122 USA. RP Song, WZ (reprint author), Washington State Univ, Sensorweb Res Lab, 14204 NE Salmon Creek Ave, Vancouver, WA 98686 USA. EM mingsen_xu@wsu.edu; songwz@wsu.edu; renjie_huang@wsu.edu; yang_peng@wsu.edu; shirazi@wsu.edu; rlahusen@usgs.gov; Aaron.B.Kiely@jpl.nasa.gov; npicone@eecs.wsu.edu; hama@wsu.edu; lanusuya@eecs.wsu.edu; mmicel2@lsu.edu; mcbrided@seattleu.edu FU National Aeronautics and Space Administration (NASA) ESTO AIST program; U.S. Geological Survey (USGS) Volcano Hazard program [NNX06AE42G]; USGS Cascades Volcano Observatory; NASA Jet Propulsion Laboratory FX This work is supported by National Aeronautics and Space Administration (NASA) ESTO AIST program and U.S. Geological Survey (USGS) Volcano Hazard program under the research grant NNX06AE42G. Partial results of this paper was published in [Y. Peng, R. Lahusen, B. Shirazi, W. Song, Design of smart sensing component for volcano monitoring, in: the 4th IET International Conference on Intelligent Environments, 2008].; This work was done in the OASIS project (http://sensorweb.vancouver.wsu.edu). We greatly appreciate the supports from USGS Cascades Volcano Observatory (John Pallister, Dan Dzurisin, Seth Moran, Mike Lisowski) and NASA Jet Propulsion Laboratory (Steve Chien, Sharon Kedar, Frank Webb, Joshua Doubleday, Danny Tran, Ashley Davies). NR 25 TC 2 Z9 2 U1 0 U2 2 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 1574-1192 J9 PERVASIVE MOB COMPUT JI Pervasive Mob. Comput. PD OCT PY 2009 VL 5 IS 5 BP 639 EP 653 DI 10.1016/j.pmcj.2009.06.004 PG 15 WC Computer Science, Information Systems; Telecommunications SC Computer Science; Telecommunications GA V24FN UT WOS:000208396400019 ER PT J AU Lorenzo, CF Hartley, TT Adams, JL AF Lorenzo, C. F. Hartley, T. T. Adams, J. L. TI The inverted initialization problem for fractional-order derivatives SO PHYSICA SCRIPTA LA English DT Article AB The problem of 'inverted initialization' as it applies to the fractional-order derivative is introduced in this paper. For the inverted initialization problem of fractional derivatives, the history information is not provided for the variable being differentiated, the usual case, but instead is given in terms of the fractional-order derivative of the variable. The case undertaken in this study requires the fractional derivative to be constant during the historic period as opposed to the normal case where the initialization is based on the differentiated variable. An example compares the inverted and normal initializations. C1 [Lorenzo, C. F.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. [Hartley, T. T.; Adams, J. L.] Univ Akron, Akron, OH USA. RP Lorenzo, CF (reprint author), NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. EM Carl.F.Lorenzo@nasa.gov FU NASA Glenn Research Center FX We gratefully acknowledge the support of NASA Glenn Research Center. NR 4 TC 2 Z9 2 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0031-8949 J9 PHYS SCRIPTA JI Phys. Scr. PD OCT PY 2009 VL T136 AR 014029 DI 10.1088/0031-8949/2009/T136/014029 PG 4 WC Physics, Multidisciplinary SC Physics GA 506VA UT WOS:000270803300030 ER PT J AU Neudeck, PG Garverick, SL Spry, DJ Chen, LY Beheim, GM Krasowski, MJ Mehregany, M AF Neudeck, Philip G. Garverick, Steven L. Spry, David J. Chen, Liang-Yu Beheim, Glenn M. Krasowski, Michael J. Mehregany, Mehran TI Extreme temperature 6H-SiC JFET integrated circuit technology SO PHYSICA STATUS SOLIDI A-APPLICATIONS AND MATERIALS SCIENCE LA English DT Article ID FIELD-EFFECT TRANSISTORS; SILICON-CARBIDE; OPERATION; 500-DEGREES-C; IMPLANTATION; OXIDATION; ALUMINUM; DEFECTS; 4H AB Extreme temperature semiconductor integrated circuits (ICs) are being developed for use in the hot sections of aircraft engines and other harsh-environment applications well above the 300 degrees C effective limit of silicon-on-insulator IC technology. This paper reviews progress by the NASA Glenn Research Center and Case Western Reserve University (CWRU) in the development of extreme temperature (up to 500 degrees C) integrated circuit technology based on epitaxial 6H-SiC junction field effect transistors (JFETs). Simple analog amplifier and digital logic gate ICs fabricated and packaged by NASA have now demonstrated thousands of hours of continuous 500 degrees C operation in oxidizing air atmosphere with minimal changes in relevant electrical parameters. Design, modeling, and characterization of transistors and circuits at temperatures from 24 degrees C to 500 degrees C are also described. CWRU designs for improved extreme temperature SiC MET differential amplifier circuits are demonstrated. Areas for further technology maturation, needed prior to beneficial system insertion, are discussed. [GRAPHICS] Optical micrograph of a 500 degrees C durable 6H-SiC JFET differential amplifier IC chip fabricated at NASA prior to packaging. Digitized waveforms measured during the 1st (solid black) and 6519th (dashed grey) hour of 500 degrees C operational testing show no change in output characteristics. (C) 2009 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim C1 [Neudeck, Philip G.; Chen, Liang-Yu] NASA, Glenn Res Ctr, Ohio Aerosp Inst, Cleveland, OH 44135 USA. [Garverick, Steven L.; Mehregany, Mehran] Case Western Reserve Univ, Dept Elect Engn & Comp Sci, Cleveland, OH 44106 USA. RP Neudeck, PG (reprint author), NASA, Glenn Res Ctr, Ohio Aerosp Inst, 21000 Brookpk Rd,MS 77-1, Cleveland, OH 44135 USA. EM Neudeck@nasa.gov; Steven.garverick@case.edu FU NASA Aeronautics Research Mission Directorate; NASA Glenn Research Center; DARPA [NBCH1050002] FX The NASA work is presently funded by the NASA Aeronautics Research Mission Directorate in both the Aviation Safety and Fundamental Aeronautics Programs under the Integrated Vehicle Health Management, Subsonic Fixed Wing, and Supersonics Projects. Prior-year funding for the NASA work included the Glennan Microsystems Initiative, Ultra Efficient Engine Technology, Propulsion 2 1, and NASA Electronics Parts and Packaging programs. The NASA work was carried out by the NASA Glenn Research Center. Process development and fabrication of the NASA devices was carried out primarily by D. Spry, G. Beheim, C. Chang, R. Okojie, L. Evans, R. Meredith, and T. Ferrier. The NASA high-temperature chip packaging was developed and implemented by L. Y. Chen. The NASA authors are also grateful for the assistance of J. Flatico, D. Lucko, J. Jordan, K. Laster, J. Gonzalez, R. Lotenero, R. Buttlet, M. Mrdenovich, B. Osborn, D. Androjna, A. Trunek, G. Hunter, and L. Matus. The Case Western Reserve University work is supported by DARPA Grant #NBCH1050002. Process development and fabrication of the CWRU devices was carried out by Dr. Xiao-An Fu, now a faculty member in the Department of Chemical Engineering at University of Louisville. The CWRU authors are also grateful for the technical contributions of Amita Patel and Chompoonoot Anupongongarch. NR 54 TC 56 Z9 56 U1 1 U2 11 PU WILEY-V C H VERLAG GMBH PI WEINHEIM PA PO BOX 10 11 61, D-69451 WEINHEIM, GERMANY SN 1862-6300 J9 PHYS STATUS SOLIDI A JI Phys. Status Solidi A-Appl. Mat. PD OCT PY 2009 VL 206 IS 10 BP 2329 EP 2345 DI 10.1002/pssa.200925188 PG 17 WC Materials Science, Multidisciplinary; Physics, Applied; Physics, Condensed Matter SC Materials Science; Physics GA 517HX UT WOS:000271605200012 ER PT J AU Long, DA Havey, DK Okumura, M Pickett, HM Miller, CE Hodges, JT AF Long, D. A. Havey, D. K. Okumura, M. Pickett, H. M. Miller, C. E. Hodges, J. T. TI Laboratory measurements and theoretical calculations of O-2 A band electric quadrupole transitions SO PHYSICAL REVIEW A LA English DT Article DE absorption coefficients; electric moments; infrared spectra; molecular electronic states; oxygen; quadrupole moments; spectral line intensity ID OXYGEN-A-BAND; RING-DOWN SPECTROSCOPY; HIGH-RESOLUTION; ABSORPTION-SPECTROSCOPY; CAVITY RING; MOLECULAR-OXYGEN; LINE PARAMETERS; RAMAN-SPECTRUM; HIGH-PRECISION; GROUND-STATE AB Frequency-stabilized cavity ring-down spectroscopy was utilized to measure electric quadrupole transitions within the O-16(2) A band, b (1)Sigma(+)(g)<- X (3)Sigma(-)(g)(0,0). We report quantitative measurements (relative uncertainties in intensity measurements from 4.4% to 11%) of nine ultraweak transitions in the O-N, O-P, S-R, and S-T branches with line intensities ranging from 3x10(-30) to 2x10(-29) cm molec.(-1). A thorough discussion of relevant noise sources and uncertainties in this experiment and other cw-cavity ring-down spectrometers is given. For short-term averaging (t < 100 s), we estimate a noise-equivalent absorption of 2.5x10(-10) cm(-1) Hz(-1/2). The detection limit was reduced further by co-adding up to 100 spectra to yield a minimum detectable absorption coefficient equal to 1.8x10(-11) cm(-1), corresponding to a line intensity of similar to 2.5x10(-31) cm molec.(-1). We discuss calculations of electric quadrupole line positions based on a simultaneous fit of the ground and upper electronic state energies which have uncertainties < 3 MHz, and we present calculations of electric quadrupole matrix elements and line intensities. The electric quadrupole line intensity calculations and measurements agreed on average to 5%, which is comparable to our average experimental uncertainty. The calculated electric quadrupole band intensity was 1.8(1)x10(-27) cm molec.(-1) which is equal to only similar to 8x10(-6) of the magnetic dipole band intensity. C1 [Long, D. A.; Okumura, M.] CALTECH, Div Chem & Chem Engn, Pasadena, CA 91125 USA. [Havey, D. K.; Hodges, J. T.] Natl Inst Stand & Technol, Proc Measurements Div, Gaithersburg, MD 20899 USA. [Pickett, H. M.; Miller, C. E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Long, DA (reprint author), CALTECH, Div Chem & Chem Engn, Pasadena, CA 91125 USA. RI Havey, Daniel/C-1997-2009; Hodges, Joseph/B-4578-2009; Okumura, Mitchio/I-3326-2013 OI Okumura, Mitchio/0000-0001-6874-1137 FU National Aeronautics and Space Administration FX The research at the Jet Propulsion Laboratory (JPL), California Institute of Technology, was performed under contract with the National Aeronautics and Space Administration. NR 51 TC 34 Z9 33 U1 2 U2 20 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 OCT PY 2009 VL 80 IS 4 AR 042513 DI 10.1103/PhysRevA.80.042513 PG 12 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 513VB UT WOS:000271351000089 ER PT J AU Prange, MP Rehr, JJ Rivas, G Kas, JJ Lawson, JW AF Prange, M. P. Rehr, J. J. Rivas, G. Kas, J. J. Lawson, John W. TI Real space calculation of optical constants from optical to x-ray frequencies SO PHYSICAL REVIEW B LA English DT Article ID ABSORPTION FINE-STRUCTURE; DIELECTRIC-CONSTANT; AMORPHOUS-CARBON; SCATTERING; SPECTRA; PHOTOABSORPTION; SPECTROSCOPY; EXCITATIONS; FORMULATION; SYSTEMS AB We present a theory of linear optical constants based on the single-particle density operator and implemented in an extension of the real space multiple scattering code known as FEFF. This approach avoids the need to compute wave functions explicitly and yields efficient calculations for frequencies ranging from the IR to hard x-rays, which is applicable to arbitrary aperiodic systems. The approach is illustrated with calculations of optical properties and applications for several materials and compared with existing tabulations. C1 [Prange, M. P.; Rehr, J. J.; Kas, J. J.] Univ Washington, Dept Phys, Seattle, WA 98195 USA. [Rivas, G.] Univ Autonoma Ciudad Juarez, Inst Ingn & Tecnol, Juarez 32310, Mexico. [Lawson, John W.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Prange, MP (reprint author), Univ Washington, Dept Phys, Seattle, WA 98195 USA. RI Yambo, MBPT Code/O-4564-2015 NR 53 TC 17 Z9 17 U1 3 U2 10 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 OCT PY 2009 VL 80 IS 15 AR 155110 DI 10.1103/PhysRevB.80.155110 PG 14 WC Physics, Condensed Matter SC Physics GA 513VK UT WOS:000271352000043 ER PT J AU Rahman, R Lansbergen, GP Park, SH Verduijn, J Klimeck, G Rogge, S Hollenberg, LCL AF Rahman, Rajib Lansbergen, G. P. Park, Seung H. Verduijn, J. Klimeck, Gerhard Rogge, S. Hollenberg, Lloyd C. L. TI Orbital Stark effect and quantum confinement transition of donors in silicon SO PHYSICAL REVIEW B LA English DT Article ID NEMO 3-D; STATES; COMPUTER; ATOM; DOTS; SEMICONDUCTORS AB Adiabatic shuttling of single impurity bound electrons to gate-induced surface states in semiconductors has attracted much attention in recent times, mostly in the context of solid-state quantum computer architecture. A recent transport spectroscopy experiment for the first time was able to probe the Stark shifted spectrum of a single donor in silicon buried close to a gate. Here, we present the full theoretical model involving large-scale quantum mechanical simulations that was used to compute the Stark shifted donor states in order to interpret the experimental data. Use of atomistic tight-binding technique on a domain of over a million atoms helped not only to incorporate the full band structure of the host, but also to treat realistic device geometries and donor models, and to use a large enough basis set to capture any number of donor states. The method yields a quantitative description of the symmetry transition that the donor electron undergoes from a three-dimensional Coulomb confined state to a two-dimensional (2D) surface state as the electric field is ramped up adiabatically. In the intermediate field regime, the electron resides in a superposition between the atomic donor states and the 2D surface states. In addition to determining the effect of field and donor depth on the electronic structure, the model also provides a basis to distinguish between a phosphorus and an arsenic donor based on their Stark signature. The method also captures valley-orbit splitting in both the donor well and the interface well, a quantity critical to silicon qubits. The work concludes with a detailed analysis of the effects of screening on the donor spectrum. C1 [Rahman, Rajib; Park, Seung H.; Klimeck, Gerhard] Purdue Univ, Network Computat Nanotechnol, W Lafayette, IN 47907 USA. [Lansbergen, G. P.; Verduijn, J.; Rogge, S.] Delft Univ Technol, Kavli Inst Nanosci, NL-2628 CJ Delft, Netherlands. [Klimeck, Gerhard] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Hollenberg, Lloyd C. L.] Univ Melbourne, Sch Phys, Ctr Quantum Comp Technol, Melbourne, Vic 3010, Australia. RP Rahman, R (reprint author), Purdue Univ, Network Computat Nanotechnol, W Lafayette, IN 47907 USA. EM rrahman@purdue.edu; lloydch@unimelb.edu.au RI Hollenberg, Lloyd/B-2296-2010; Lansbergen, Gabriel/A-7895-2011; Klimeck, Gerhard/A-1414-2012; Rogge, Sven/G-3709-2010; OI Klimeck, Gerhard/0000-0001-7128-773X; Rahman, Rajib/0000-0003-1649-823X FU Australian Research Council, the Australian Government; U. S. National Security Agency (NSA); Army Research Office (ARO) [W911NF-08-1-0527] FX This work was supported by the Australian Research Council, the Australian Government, and the U. S. National Security Agency (NSA) and the Army Research Office (ARO) under Contract No. W911NF-08-1-0527. Part of the development of NEMO-3D was initially performed at JPL, Caltech under a contract with NASA. NCN/nanohub.org computational resources were used in this work. S. R. also acknowledges the support of Dutch Foundation for Fundamental Research on Matter (FOM) and the EU FP7 project AFSID. NR 63 TC 51 Z9 51 U1 0 U2 11 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1098-0121 J9 PHYS REV B JI Phys. Rev. B PD OCT PY 2009 VL 80 IS 16 AR 165314 DI 10.1103/PhysRevB.80.165314 PG 10 WC Physics, Condensed Matter SC Physics GA 513VL UT WOS:000271352100089 ER PT J AU Rahman, R Park, SH Boykin, TB Klimeck, G Rogge, S Hollenberg, LCL AF Rahman, Rajib Park, Seung H. Boykin, Timothy B. Klimeck, Gerhard Rogge, Sven Hollenberg, Lloyd C. L. TI Gate-induced g-factor control and dimensional transition for donors in multivalley semiconductors SO PHYSICAL REVIEW B LA English DT Article AB The dependence of the g factors of semiconductor donors on applied electric and magnetic fields is of immense importance in spin-based quantum computation and in semiconductor spintronics. The donor g-factor Stark shift is sensitive to the orientation of the electric and magnetic fields and is strongly influenced by the band-structure and spin-orbit interactions of the host. Using a multimillion atom tight-binding framework, the spin-orbit Stark parameters are computed for donors in multivalley semiconductors, silicon, and germanium. Comparison with limited experimental data shows good agreement for a donor in silicon. Results for gate-induced transition from three-dimensional to two-dimensional wave-function confinement show that the corresponding g-factor shift in Si is experimentally observable, and at modest B field, O(1 T) can exceed the Stark shift of the hyperfine interaction. C1 [Rahman, Rajib; Park, Seung H.; Klimeck, Gerhard] Purdue Univ, Network Computat Nanotechnol, W Lafayette, IN 47907 USA. [Boykin, Timothy B.] Univ Alabama, Dept Elect Engn, Huntsville, AL 35899 USA. [Klimeck, Gerhard] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Rogge, Sven] Delft Univ Technol, Kavli Inst Nanosci, NL-2628 CJ Delft, Netherlands. [Hollenberg, Lloyd C. L.] Univ Melbourne, Sch Phys, Ctr Quantum Comp Technol, Melbourne, Vic 3010, Australia. RP Rahman, R (reprint author), Purdue Univ, Network Computat Nanotechnol, W Lafayette, IN 47907 USA. EM rrahman@purdue.edu; lloydch@unimelb.edu.au RI Hollenberg, Lloyd/B-2296-2010; Klimeck, Gerhard/A-1414-2012; Rogge, Sven/G-3709-2010; OI Klimeck, Gerhard/0000-0001-7128-773X; Rahman, Rajib/0000-0003-1649-823X FU Australian Research Council; NSA; ARO [W911NF-08-1-052]; NASA FX This work was supported by the Australian Research Council, NSA, and ARO (Contract No. W911NF-08-1-052). Part of the development of NEMO-3D was performed at JPL, Caltech under a contract with NASA. NCN/nanohub.org computer resources were used. NR 0 TC 24 Z9 24 U1 0 U2 7 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1098-0121 J9 PHYS REV B JI Phys. Rev. B PD OCT PY 2009 VL 80 IS 15 AR 155301 DI 10.1103/PhysRevB.80.155301 PG 5 WC Physics, Condensed Matter SC Physics GA 513VK UT WOS:000271352000076 ER PT J AU Menegoni, E Galli, S Bartlett, JG Martins, CJAP Melchiorri, A AF Menegoni, Eloisa Galli, Silvia Bartlett, James G. Martins, C. J. A. P. Melchiorri, Alessandro TI New constraints on variations of the fine structure constant from CMB anisotropies SO PHYSICAL REVIEW D LA English DT Article ID POWER SPECTRUM; TIME-VARIATION; 2003 FLIGHT; POLARIZATION; BOOMERANG; ALPHA AB We demonstrate that recent measurements of cosmic microwave background temperature and polarization anisotropy made by the ACBAR, QUAD, and BICEP experiments substantially improve the cosmological constraints on possible variations of the fine structure constant in the early universe. This data, combined with the five year observations from the WMAP mission, yield the constraint alpha/alpha(0) = 0 0.987 +/- 0.012 at 68% C.L. The inclusion of the new Hubble Space Telescope constraints on the Hubble constant further increases the accuracy to alpha/alpha(0) = 1.001 +/- 0.007 at 68% C.L., bringing possible deviations from the current value below the 1% level and improving previous constraints by a factor of similar to 3. C1 [Menegoni, Eloisa; Galli, Silvia; Melchiorri, Alessandro] Univ Roma La Sapienza, Dept Phys, I-00185 Rome, Italy. [Menegoni, Eloisa; Galli, Silvia; Melchiorri, Alessandro] Univ Roma La Sapienza, Ist Nazl Fis Nucl, I-00185 Rome, Italy. [Galli, Silvia; Bartlett, James G.] Univ Paris Diderot, Lab Astroparticule & Cosmol APC, F-75205 Paris 13, France. [Bartlett, James G.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Martins, C. J. A. P.] Univ Porto, Ctr Astrofis, P-4150762 Oporto, Portugal. [Martins, C. J. A. P.] Univ Cambridge, DAMTP, Cambridge CB3 0WA, England. RP Menegoni, E (reprint author), Univ Roma La Sapienza, Dept Phys, Piazzale Aldo Moro 2, I-00185 Rome, Italy. OI Martins, Carlos/0000-0002-4886-9261; Melchiorri, Alessandro/0000-0001-5326-6003 FU FSE; POPH-QREN funds; National Aeronautics and Space Administration FX The work of C. M. is funded by a Ciencia2007 Research Contract, supported by FSE and POPH-QREN funds. The work of J. G. B. was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. NR 25 TC 32 Z9 32 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 OCT PY 2009 VL 80 IS 8 AR 087302 DI 10.1103/PhysRevD.80.087302 PG 3 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 513WB UT WOS:000271353700139 ER PT J AU Hesse, M Zenitani, S Kuznetsova, M Klimas, A AF Hesse, Michael Zenitani, Seiji Kuznetsova, Masha Klimas, Alex TI A simple, analytical model of collisionless magnetic reconnection in a pair plasma SO PHYSICS OF PLASMAS LA English DT Article AB A set of conservation equations is utilized to derive balance equations in the reconnection diffusion region of a symmetric pair plasma. The reconnection electric field is assumed to have the function to maintain the current density in the diffusion region and to impart thermal energy to the plasma by means of quasiviscous dissipation. Using these assumptions it is possible to derive a simple set of equations for diffusion region parameters in dependence on inflow conditions and on plasma compressibility. These equations are solved by means of a simple, iterative procedure. The solutions show expected features such as dominance of enthalpy flux in the reconnection outflow, as well as combination of adiabatic and quasiviscous heating. Furthermore, the model predicts a maximum reconnection electric field of E*=0.4, normalized to the parameters at the inflow edge of the diffusion region. (C) 2009 American Institute of Physics. [doi: 10.1063/1.3246005] C1 [Hesse, Michael; Zenitani, Seiji; Kuznetsova, Masha; Klimas, Alex] NASA, Goddard Space Flight Ctr, Space Weather Lab, Greenbelt, MD 20771 USA. RP Hesse, M (reprint author), NASA, Goddard Space Flight Ctr, Space Weather Lab, Code 674, Greenbelt, MD 20771 USA. RI Hesse, Michael/D-2031-2012; Kuznetsova, Maria/F-6840-2012; 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's MMS mission FX This research was supported by NASA's MMS mission. One of us (S.Z.) gratefully acknowledges support from NASA's postdoctoral program. The authors acknowledge helpful comments from Karl Schindler. NR 18 TC 14 Z9 14 U1 0 U2 7 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 1070-664X J9 PHYS PLASMAS JI Phys. Plasmas PD OCT PY 2009 VL 16 IS 10 AR 102106 DI 10.1063/1.3246005 PG 10 WC Physics, Fluids & Plasmas SC Physics GA 513YK UT WOS:000271359900008 ER PT J AU Temkin, A AF Temkin, Aaron TI Recollections of Samuel Goudsmit's humor SO PHYSICS TODAY LA English DT Letter C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD USA. RP Temkin, A (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD USA. EM aaron.temkin-1@nasa.gov NR 0 TC 0 Z9 0 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 0031-9228 J9 PHYS TODAY JI Phys. Today PD OCT PY 2009 VL 62 IS 10 BP 10 EP 10 PG 1 WC Physics, Multidisciplinary SC Physics GA 503TA UT WOS:000270561600003 ER PT J AU Schmidt, G AF Schmidt, Gavin TI Wrong but useful SO PHYSICS WORLD LA English DT Article C1 NASA, Goddard Inst Space Studies, New York, NY 10025 USA. RP Schmidt, G (reprint author), NASA, Goddard Inst Space Studies, New York, NY 10025 USA. EM gavin.a.schmidt@nasa.gov RI Schmidt, Gavin/D-4427-2012 OI Schmidt, Gavin/0000-0002-2258-0486 NR 0 TC 0 Z9 0 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0953-8585 J9 PHYS WORLD JI Phys. World PD OCT PY 2009 VL 22 IS 10 BP 33 EP 35 PG 3 WC Physics, Multidisciplinary SC Physics GA 517NH UT WOS:000271621100039 ER PT J AU Helled, R Schubert, G Anderson, JD AF Helled, Ravit Schubert, Gerald Anderson, John D. TI Jupiter and Saturn rotation periods SO PLANETARY AND SPACE SCIENCE LA English DT Article DE Jupiter; Saturn; Atmospheres; Dynamics; Rotation period ID RADIO OCCULTATION MEASUREMENTS; GRAVITY-FIELD; TRACKING DATA; ZONAL FLOW; ATMOSPHERE; STABILITY; WINDS AB Anderson and Schubert [2007. Saturn's Gravitational field, internal rotation, and interior structure. Science 317, 1384-1387 (paper 1)] proposed that Saturn's rotation period can be ascertained by minimizing the dynamic heights of the 100 mbar isosurface with respect to the geoid; they derived a rotation period of 10 h 32 m 35 s. We investigate the same approach for Jupiter to see if the Jovian rotation period is predicted by minimizing the dynamical heights of its isobaric (I bar pressure level) surface using zonal wind data. A rotation period of 9 h 54 m 29.7 s is found. Further, we investigate the minimization method by fitting Pioneer and Voyager occultation radii for both Jupiter and Saturn. Rotation periods of 9 h 55 m 30 s and 10 h 32 m 35 s are found to minimize the dynamical heights for Jupiter and Saturn, respectively. Though there is no dynamical principle requiring the minimization of the dynamical heights of an isobaric surface, the successful application of the method to Jupiter lends support to its relevance for Saturn. We derive Jupiter and Saturn rotation periods using equilibrium theory to explain the difference between equatorial and polar radii. Rotation periods of 9 h 55 m 20s and 10 h 31 m 49s are found for Jupiter and Saturn, respectively. We show that both Jupiter's and Saturn's shapes can be derived using solid-body rotation, suggesting that zonal winds have a minor effect on the planetary shape for both planets. The agreement in the values of Saturn's rotation period predicted by the different approaches supports the conclusion that the planet's period of rotation is about 10 h 32 m. (C) 2009 Elsevier Ltd. All rights reserved. C1 [Helled, Ravit; Schubert, Gerald] Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90095 USA. [Helled, Ravit; Schubert, Gerald] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90095 USA. [Anderson, John D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Helled, R (reprint author), Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90095 USA. EM rhelled@ess.ucla.edu; schubert@ucla.edu; jdandy@earthlink.net FU NASA through the Southwest Research Institute; NASA PGG; PA programs FX The authors thank Andy Ingersoll and an anonymous referee for valuable comments and suggestions. R.H. and J.D.A. acknowledge support from NASA through the Southwest Research Institute. G.S. acknowledges support from the NASA PGG and PA programs. NR 25 TC 14 Z9 14 U1 0 U2 3 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0032-0633 J9 PLANET SPACE SCI JI Planet Space Sci. PD OCT PY 2009 VL 57 IS 12 BP 1467 EP 1473 DI 10.1016/j.pss.2009.07.008 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 514AH UT WOS:000271365200015 ER PT J AU Shevchenko, VG Tungalag, N Chiorny, VG Gaftonyuk, NM Krugly, YN Harris, AW Young, JW AF Shevchenko, Vasilij G. Tungalag, N. Chiorny, Vasilij G. Gaftonyuk, Ninel M. Krugly, Yury N. Harris, Alan W. Young, James W. TI CCD-photometry and pole coordinates for eight asteroids SO PLANETARY AND SPACE SCIENCE LA English DT Article DE Asteroids; Photometry; Lightcurve; Rotation period; Pole coordinates ID MAIN-BELT ASTEROIDS; FOLLOW-UP PROGRAM; ROTATIONAL PROPERTIES; LIGHTCURVES; PERIODS; HILDA; SHAPE AB The long time photometric observations were carried out for eight asteroids: (122) Gerda, (153) Hilda, (190) Ismene, (221) Eos, (411) Xanthe, (679) Pax, (700) Auravictrix, (787) Moskva. New rotation periods have been determined for the asteroids (153) Hilda (5.959 h) and (411) Xanthe (11.408 h), and known rotation periods for some of the others have been confirmed. Using our data and others data we have estimated new pole coordinates for the observed asteroids. (C) 2009 Elsevier Ltd. All rights reserved. C1 [Shevchenko, Vasilij G.; Chiorny, Vasilij G.; Krugly, Yury N.] Kharkiv Karazin Natl Univ, Inst Astron, UA-61022 Kharkov, Ukraine. [Tungalag, N.] Acad Sci, Res Inst Geophys & Astron, Ulaanbaatar, Mongol Peo Rep. [Gaftonyuk, Ninel M.] Crimean Astrophys Observ, UA-98680 Crimea, Simeiz, Ukraine. [Harris, Alan W.] Space Sci Inst, Orange, CA 91011 USA. [Young, James W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Shevchenko, VG (reprint author), Kharkiv Karazin Natl Univ, Inst Astron, Sumska St 35, UA-61022 Kharkov, Ukraine. EM shevchenko@astron.kharkov.ua RI Shevchenko, Vasilij/H-1366-2011 OI Shevchenko, Vasilij/0000-0003-1000-223X FU INTAS [03-70-567] FX The authors are grateful to the DLR Institute of Planetary Exploration (Berlin, Germany) for the provision of the CCD-camera and the image reduction software. Since June 2006 observations using 0.7 m telescope have been carried out with a CCD-camera obtained thanks to INTAS Grant Ref. no 03-70-567. We thank the reviewers for their constructive reviews which helped to improve the paper. NR 40 TC 2 Z9 2 U1 0 U2 0 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0032-0633 J9 PLANET SPACE SCI JI Planet Space Sci. PD OCT PY 2009 VL 57 IS 12 BP 1514 EP 1520 DI 10.1016/j.pss.2009.08.001 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 514AH UT WOS:000271365200020 ER PT J AU Howes, A Lewis, RL Vera, A AF Howes, Andrew Lewis, Richard L. Vera, Alonso TI Rational Adaptation Under Task and Processing Constraints: Implications for Testing Theories of Cognition and Action SO PSYCHOLOGICAL REVIEW LA English DT Article DE rational adaptation; bounded optimality; cognitive architecture; theory comparison; response ordering; dual task ID PSYCHOLOGICAL REFRACTORY-PERIOD; STATISTICAL DECISION-THEORY; DUAL-TASK; COMPUTATIONAL MODELS; INTERACTIVE BEHAVIOR; RESPONSE-SELECTION; MENTAL-IMAGERY; CHOICE TASKS; PERFORMANCE; VARIABILITY AB The authors assume that individuals adapt rationally to a utility function given constraints imposed by their cognitive architecture and the local task environment. This assumption underlies a new approach to modeling and understanding cognition-cognitively bounded rational analysis-that sharpens the predictive acuity of general, integrated theories of cognition and action. Such theories provide the necessary computational means to explain the flexible nature of human behavior but in doing so introduce extreme degrees of freedom in accounting for data. The new approach narrows the space of predicted behaviors through analysis of the payoff achieved by alternative strategies, rather than through fitting strategies and theoretical parameters to data. It extends and complements established approaches, including computational cognitive architectures, rational analysis, optimal motor control, bounded rationality, and signal detection theory. The authors illustrate the approach with a reanalysis of an existing account of psychological refractory period (PRP) dual-task performance and the development and analysis of a new theory of ordered dual-task responses. These analyses yield several novel results, including a new understanding of the role of strategic variation in existing accounts of PRP and the first predictive, quantitative account showing how the details of ordered dual-task phenomena emerge from the rational control of a cognitive system subject to the combined constraints of internal variance, motor interference, and a response selection bottleneck. C1 [Howes, Andrew] Univ Manchester, Manchester Business Sch, Manchester M15 6PB, Lancs, England. [Lewis, Richard L.] Univ Michigan, Dept Psychol, Ann Arbor, MI 48109 USA. [Vera, Alonso] NASA, Ames Res Ctr, Human Syst Integrat Div, Moffett Field, CA 94035 USA. RP Howes, A (reprint author), Univ Manchester, Manchester Business Sch, MBS E,Booth St W, Manchester M15 6PB, Lancs, England. EM Andrew.Howes@mbs.ac.uk FU NASA FX The work was supported by the NASA Aviation Operations Safety Program, by the NASA Intelligent Systems Program, and by the Office of Naval Research. We thank David Meyer and Eric Schumacher for providing theraw data for the experiments reported in Schumacher et al. (1999) as well as John Anderson, Nick Chater, Alina Chu, Wai Tat Fu, Wayne Gray, Collin Green, Bonnie John, Jonathon Kopecky, Stelios Lelis, Michael McCurdy, David Meyer, Hal Pashler, Stephen J. Payne, Roger Remington, Mason Smith, Yuan-Chi Tseng, and Richard M. Young for providing useful comments on this work. NR 98 TC 53 Z9 53 U1 2 U2 11 PU AMER PSYCHOLOGICAL ASSOC PI WASHINGTON PA 750 FIRST ST NE, WASHINGTON, DC 20002-4242 USA SN 0033-295X EI 1939-1471 J9 PSYCHOL REV JI Psychol. Rev. PD OCT PY 2009 VL 116 IS 4 BP 717 EP 751 DI 10.1037/a0017187 PG 35 WC Psychology; Psychology, Multidisciplinary SC Psychology GA 506KW UT WOS:000270774700002 PM 19839682 ER PT J AU Kane, SR von Braun, K AF Kane, Stephen R. von Braun, Kaspar TI Exoplanetary Transit Constraints Based upon Secondary Eclipse Observations SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article ID PLANET HD 189733B; EXTRASOLAR PLANET; LIGHT CURVES; ORBITAL ECCENTRICITY; THERMAL EMISSION; PHOTOMETRY; DETECTABILITY; PARAMETERS; COMPANION; 209458B AB Transiting extrasolar planets provide an opportunity to study the mass-radius relation of planets as well as their internal structure. The existence of a secondary eclipse enables further study of the thermal properties of the the planet by observing at infrared wavelengths. The probability of an observable secondary eclipse depends upon the orbital parameters of the planet, particularly eccentricity and argument of periastron. Here we provide analytical expressions for these probabilities, investigate their properties, and calculate their values for the known extrasolar planets. We furthermore quantitatively discuss constraints on existence and observability of primary transits if a secondary eclipse is observed. Finally, we calculate the a posteriori transit probabilities of the known extrasolar planets, and we present several case studies in which orbital constraints resulting from the presence of a secondary eclipse may be applied in observing campaigns. C1 [Kane, Stephen R.; von Braun, Kaspar] CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA. RP Kane, SR (reprint author), CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA. EM skane@ipac.caltech.edu RI Kane, Stephen/B-4798-2013 NR 31 TC 11 Z9 11 U1 0 U2 1 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 OCT PY 2009 VL 121 IS 884 BP 1096 EP 1103 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 500BP UT WOS:000270272400008 ER PT J AU Colavita, MM Serabyn, E Millan-Gabet, R Koresko, CD Akeson, RL Booth, AJ Mennesson, BP Ragland, SD Appleby, EC Berkey, BC Cooper, A Crawford, SL Creech-Eakman, MJ Dahl, W Felizardo, C Garcia-Gathright, JI Gathright, JT Herstein, JS Hovland, EE Hrynevych, MA Ligon, ER Medeiros, DW Moore, JD Morrison, D Paine, CG Palmer, DL Panteleeva, T Smith, B Swain, MR Smythe, RF Summers, KR Tsubota, K Tyau, C Vasisht, G Wetherell, E Wizinowich, PL Woillez, JM AF Colavita, M. M. Serabyn, E. Millan-Gabet, R. Koresko, C. D. Akeson, R. L. Booth, A. J. Mennesson, B. P. Ragland, S. D. Appleby, E. C. Berkey, B. C. Cooper, A. Crawford, S. L. Creech-Eakman, M. J. Dahl, W. Felizardo, C. Garcia-Gathright, J. I. Gathright, J. T. Herstein, J. S. Hovland, E. E. Hrynevych, M. A. Ligon, E. R. Medeiros, D. W. Moore, J. D. Morrison, D. Paine, C. G. Palmer, D. L. Panteleeva, T. Smith, B. Swain, M. R. Smythe, R. F. Summers, K. R. Tsubota, K. Tyau, C. Vasisht, G. Wetherell, E. Wizinowich, P. L. Woillez, J. M. TI Keck Interferometer Nuller Data Reduction and On-Sky Performance SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article ID STARS AB We describe the Keck Interferometer nuller theory of operation, data reduction, and on-sky performance, particularly as it applies to the nuller exozodiacal dust key science program that was carried out between 2008 February and 2009 January. We review the nuller implementation, including the detailed phasor processing involved in implementing the null-peak mode used for science data and the sequencing used for science observing. We then describe the Level 1 reduction to convert the instrument telemetry streams to raw null leakages, and the Level 2 reduction to provide calibrated null leakages. The Level 1 reduction uses conservative, primarily linear processing, implemented consistently for science and calibrator stars. The Level 2 processing is more flexible, and uses diameters for the calibrator stars measured contemporaneously with the interferometer's K-band cophasing system in order to provide the requisite accuracy. Using the key science data set of 462 total scans, we assess the instrument performance for sensitivity and systematic error. At 2.0 Jy we achieve a photometrically-limited null leakage uncertainty of 0.25% rms per 10 minutes of integration time in our broadband channel. From analysis of the Level 2 reductions, we estimate a systematic noise floor for bright stars of similar to 0.2% rms null leakage uncertainty per observing cluster in the broadband channel. A similar analysis is performed for the narrowband channels. We also provide additional information needed for science reduction, including details on the instrument beam pattern and the basic astrophysical response of the system, and references to the data reduction and modeling tools. C1 [Colavita, M. M.; Serabyn, E.; Booth, A. J.; Mennesson, B. P.; Crawford, S. L.; Creech-Eakman, M. J.; Garcia-Gathright, J. I.; Hovland, E. E.; Ligon, E. R.; Moore, J. D.; Paine, C. G.; Palmer, D. L.; Swain, M. R.; Smythe, R. F.; Vasisht, G.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Millan-Gabet, R.; Koresko, C. D.; Akeson, R. L.; Felizardo, C.; Herstein, J. S.] CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA. [Ragland, S. D.; Appleby, E. C.; Berkey, B. C.; Cooper, A.; Dahl, W.; Gathright, J. T.; Hrynevych, M. A.; Medeiros, D. W.; Morrison, D.; Panteleeva, T.; Smith, B.; Summers, K. R.; Tsubota, K.; Tyau, C.; Wetherell, E.; Wizinowich, P. L.; Woillez, J. M.] WM Keck Observ, Kamuela, HI 96743 USA. RP Colavita, MM (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Mark.Colavita@jpl.nasa.gov NR 18 TC 34 Z9 34 U1 1 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6280 EI 1538-3873 J9 PUBL ASTRON SOC PAC JI Publ. Astron. Soc. Pac. PD OCT PY 2009 VL 121 IS 884 BP 1120 EP 1138 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 500BP UT WOS:000270272400011 ER PT J AU Sorbjan, Z Wolff, M Smith, MD AF Sorbjan, Zbigniew Wolff, Michael Smith, Michael D. TI Thermal structure of the atmospheric boundary layer on Mars based on Mini-TES observations SO QUARTERLY JOURNAL OF THE ROYAL METEOROLOGICAL SOCIETY LA English DT Article DE depth of Martian convective boundary layer; potential temperature on Mars; turbulent heat flux on Mars ID RADIO OCCULTATION MEASUREMENTS; LARGE-EDDY SIMULATIONS; MARTIAN SURFACE-LAYER; SHALLOW CONVECTION; VIKING LANDER; GUSEV CRATER; MODEL; PATHFINDER; SPIRIT; SITES AB This paper presents and discusses the vertical profiles of the potential temperature in the Martian boundary layer. The profiles were remotely sensed from on-board the Spirit Mars Exploration Rover during the first 702 sols of its operation in 2004-2005. The rover carried the Miniature Thermal Emission Spectrometer (Mini-TES), which allowed it to retrieve temperature profiles up to a level 2 km above the ground surface. The data analysed here permit a reconstruction of the diurnal and seasonal structure of the lower part of the Martian convective boundary layer, an evaluation of the boundary layer depth, and a computation of the temperature heat flux. Copyright (C) 2009 Royal Meteorological Society C1 [Sorbjan, Zbigniew] Marquette Univ, Dept Phys, Milwaukee, WI 53201 USA. [Sorbjan, Zbigniew] Polish Acad Sci, Inst Geophys, Warsaw, Poland. [Sorbjan, Zbigniew; Wolff, Michael] Space Sci Inst, Boulder, CO USA. [Smith, Michael D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Sorbjan, Z (reprint author), Marquette Univ, Dept Phys, POB 1181, Milwaukee, WI 53201 USA. EM zbigniew.sorbjan@mu.edu RI Smith, Michael/C-8875-2012 FU NASA FX We thank Hannu Savijarvi for graciously allowing us to use his single-column Martian model. We are grateful to four anonymous reviewers for their helpful comments. The performed research has been supported by NASA through the Mars Exploration Rover Project, a portion of which was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. NR 33 TC 7 Z9 7 U1 0 U2 6 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0035-9009 EI 1477-870X J9 Q J ROY METEOR SOC JI Q. J. R. Meteorol. Soc. PD OCT PY 2009 VL 135 IS 644 BP 1776 EP 1787 DI 10.1002/qj.510 PN A PG 12 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 520GZ UT WOS:000271832000010 ER PT J AU Juarez, MD AF Juarez, Manuel de la Torre TI Taylor-Proudman columns in non-hydrostatic divergent baroclinic and barotropic flows SO QUARTERLY JOURNAL OF THE ROYAL METEOROLOGICAL SOCIETY LA English DT Article DE Taylor-Proudman theorem; non-hydrostatic atmospheres; geostrophy ID GREAT RED SPOT; CORIOLIS-FORCE; DYNAMICS; FLUID; ATMOSPHERES; VORTICES; PLANETS; CASSINI; MOTION; MODEL AB The Taylor-Proudman theorem states that the velocity of slow, steady flow in a rotating incompressible fluid does not change along the direction of the rotation axis. This fundamental result has been invoked to explain blocking phenomena observed over topographic features in oceanic and atmospheric flows on Earth and atmospheric patterns observed in giant gas planets even in cases where the assumption of incompressibility fails. The possible existence of Taylor-Proudman columns is analyzed here for a less restrictive family of non-hydrostatic divergent density-stratified flows, including situations where the stratification gradient and rotation axis are not parallel. The results show that Taylor-Proudman-like constraints are possible in baroclinic inviscid and viscous nonlinear flows of constant vorticity, Beltrami flows and low-Rossby-number flows. It is found that (1) the baroclinic term is moderated by a factor of the order of the Rossby number, (2) a conservation law can be found for baroclinic flows and (3) Taylor-Proudman columns will be eroded in viscous flows. One particular result stressed in this note is its interpretation in equatorial regions, where the rotation axis is perpendicular to the main stratification gradient, and it is argued that Taylor-Proudman columns could be difficult to discern with observational parameters from convective cells with only zonal and vertical transport. Copyright (C) 2009 Royal Meteorological Society C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Juarez, MD (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM mtj@jpl.nasa.gov FU National Aeronautics and Space Administration FX The research described in this paper was carried out at the Jet Propulsion Laboratory/California Institute of Technology, under a contract with the National Aeronautics and Space Administration. The author is indebted to J-Y K. Cho for highlighting the Tassoul (2000) analysis and to A. Showman for pointing Out the Vasavada & Showman (2005) discussion. NR 33 TC 1 Z9 1 U1 0 U2 2 PU JOHN WILEY & SONS LTD PI CHICHESTER PA THE ATRIUM, SOUTHERN GATE, CHICHESTER PO19 8SQ, W SUSSEX, ENGLAND SN 0035-9009 J9 Q J ROY METEOR SOC JI Q. J. R. Meteorol. Soc. PD OCT PY 2009 VL 135 IS 645 SI SI BP 2179 EP 2184 DI 10.1002/qj.483 PN B PG 6 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 543KF UT WOS:000273575200020 ER PT J AU Zhou, D O'Sullivan, D Semones, E Zapp, N Benton, ER AF Zhou, D. O'Sullivan, D. Semones, E. Zapp, N. Benton, E. R. TI Research on sensitivity fading of CR-39 detectors during long time exposure SO RADIATION MEASUREMENTS LA English DT Article; Proceedings Paper CT 24th International Conference on Nuclear Tracks in Solids CY SEP 01-05, 2008 CL Bologna, ITALY SP Int Nucl Track Soc, Italian Natl Inst Nucl Phys, Univ Bologna, Dept Phys DE CR-39; Sensitivity fading and correction; Radiation measurement ID LOW-EARTH-ORBIT; DIFFERENT DOSIMETERS; STATION; SPECTRA; OXYGEN AB CR-39 PNTDs (Plastic Nuclear Track Detectors) have been widely used in radiation research for many years. Experiments with long-term exposure during space mission LDEF (Long Duration Exposure Facility, 5.7 years), EUROMIR95 (similar to 6 months), Matroshka-1 (616 days), Matroshka-2 (367 days) and ISS-Expeditions (> similar to 6 months) indicate that fading of CR-39 sensitivity exists and the longer the exposure time, the more the fading. Due to fading the values of etch rate ratio and LET (Linear Energy Transfer) as well as the radiation quantities were smaller than expected. In the past, there was no appropriate method and formula which could be used to deal with the sensitivity fading of CR-39 detectors, so all the results obtained from CR-39 exposed for long time are questionable. To solve CR-39 fading problem for ISS-Expedition and Matroshka work, a study on the sensitivity fading of CR-39 was conducted and a practical method was developed. The method is based on the internal LET calibration using GCR events identified as iron peak nuclei at similar to 1 GeV/n (similar to 100 keV/mu m in CR-39), combined with identification of the particles' charge using the effective etch rate ratio and fractional etch rate gradient. A correction formula for etch rate ratio as a function of exposure time was found using data of ISS-Expedition and Matroshka exposures. This paper introduces the correction method for the fading of CR-39 sensitivity and the method to determine particles' charge using CR-39 detectors, presents the correction formula for the sensitivity fading of CR-39 and compares the radiation quantities obtained without and with fading correction for CR-39 sensitivity for recent ISS-Expedition and Matroshka space missions. Published by Elsevier Ltd. C1 [Zhou, D.; Semones, E.; Zapp, N.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Zhou, D.] Univ Space Res Assoc, Houston, TX 77058 USA. [O'Sullivan, D.] Dublin Inst Adv Studies, Dublin 2, Ireland. [Benton, E. R.] Eril Res Inc, Stillwater, OK 74074 USA. RP Zhou, D (reprint author), NASA, Lyndon B Johnson Space Ctr, 2101 Nasa Pkwy, Houston, TX 77058 USA. EM dazhuang.zhou-1@nasa.gov NR 15 TC 4 Z9 5 U1 2 U2 4 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1350-4487 J9 RADIAT MEAS JI Radiat. Meas. PD OCT-NOV PY 2009 VL 44 IS 9-10 BP 909 EP 912 DI 10.1016/j.radmeas.2009.09.004 PG 4 WC Nuclear Science & Technology SC Nuclear Science & Technology GA 538CP UT WOS:000273162100046 ER PT J AU Kuhne, WW Gersey, BB Wilkins, R Wu, HL Wender, SA George, V Dynan, WS AF Kuhne, Wendy W. Gersey, Brad B. Wilkins, Richard Wu, Honglu Wender, Stephen A. George, Varghese Dynan, William S. TI Biological Effects of High-Energy Neutrons Measured In Vivo Using a Vertebrate Model SO RADIATION RESEARCH LA English DT Article ID PROPORTIONAL COUNTER MICRODOSIMETER; MEDAKA ORYZIAS-LATIPES; GERM-CELL MUTAGENESIS; IONIZING-RADIATION; BOMB SURVIVORS; FISH; EQUIVALENT; INDUCTION; APOPTOSIS; ORGANISM AB Interaction of solar protons and galactic cosmic radiation with the atmosphere and other materials produces high-energy secondary neutrons from below 1 to 1000 MeV and higher. Although secondary neutrons may provide an appreciable component of the radiation dose equivalent received by space and high-altitude air travelers, the biological effects remain poorly defined, particularly in vivo in intact organisms. Here we describe the acute response of Japanese medaka (Oryzias latipes) embryos to a beam of high-energy spallation neutrons that mimics the energy spectrum of secondary neutrons encountered aboard spacecraft and high-altitude aircraft. To determine RBE, embryos were exposed to 0-0.5 Gy of high-energy neutron radiation or 0-15 Gy of reference gamma radiation. The radiation response was measured by imaging apoptotic cells in situ in defined volumes of the embryo, an assay that provides a quantifiable, linear dose response. The slope of the dose response in the developing head, relative to reference gamma radiation, indicates an RBE of 24.9 (95% CI 13.6-40.7). A higher RBE of 48.1 (95% CI 30.0-66.4) was obtained based on overall survival. A separate analysis of apoptosis in muscle showed an overall nonlinear response, with the greatest effects at doses of less than 0.3 Gy. Results of this experiment indicate that medaka are a useful model for investigating biological damage associated with high-energy neutron exposure. (C) 2009 by Radiation Research society C1 [Kuhne, Wendy W.] Med Coll Georgia, IMMAG CA 3053, Inst Mol Med & Genet, Augusta, GA 30912 USA. [George, Varghese] Med Coll Georgia, Dept Biostat, Augusta, GA 30912 USA. [Gersey, Brad B.; Wilkins, Richard] Prairie View A&M Univ, Ctr Appl Radiat Res, Prairie View, TX USA. [Wu, Honglu] NASA, Lyndon B Johnson Space Ctr, Human Adaptat & Countermeasures Div, Houston, TX 77058 USA. [Wender, Stephen A.] Los Alamos Natl Lab, Los Alamos Neutron Sci Ctr, Los Alamos, NM USA. RP Kuhne, WW (reprint author), Med Coll Georgia, IMMAG CA 3053, Inst Mol Med & Genet, Augusta, GA 30912 USA. EM wkuhne@mcg.edu OI Wender, Stephen/0000-0002-2446-5115 FU U.S. Department of Energy Low Dose Radiation Research Program [DOE FG02-03ERG3649]; National Research Service Award [1F32ES015663-01]; National Aeronautics and Space Administration [NCC9-114] FX Funding was provided by a grant award from U.S. Department of Energy Low Dose Radiation Research Program (DOE FG02-03ERG3649), a National Research Service Award to Wendy Kuhne (1F32ES015663-01), and a grant award from the National Aeronautics and Space Administration (NCC9-114) to the Center for Applied Radiation Research, Prairie View A&M University. Neutron beam time was supported by the U.S. Department of Energy. We thank Katsuya Miyake and the Medical College of Georgia Cell Imaging Core Facility for assistance with microscopy and data analysis. We thank Li Fang Zhang in the Biostatistics Group at the Medical College of Georgia for her contributions to data analysis. We extend special thanks to Art Bridge at the LANSCE facility and Lingling Ding at the Medical College of Georgia for their assistance with logistical support in this project. NR 33 TC 11 Z9 11 U1 0 U2 1 PU RADIATION RESEARCH SOC PI LAWRENCE PA 810 E TENTH STREET, LAWRENCE, KS 66044 USA SN 0033-7587 J9 RADIAT RES JI Radiat. Res. PD OCT PY 2009 VL 172 IS 4 BP 473 EP 480 DI 10.1667/RR1556.1 PG 8 WC Biology; Biophysics; Radiology, Nuclear Medicine & Medical Imaging SC Life Sciences & Biomedicine - Other Topics; Biophysics; Radiology, Nuclear Medicine & Medical Imaging GA 503VI UT WOS:000270568900008 PM 19772468 ER PT J AU Montesano, PM Nelson, R Sun, G Margolis, H Kerber, A Ranson, KJ AF Montesano, P. M. Nelson, R. Sun, G. Margolis, H. Kerber, A. Ranson, K. J. TI MODIS tree cover validation for the circumpolar taiga-tundra transition zone SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE MODIS; Validation; Tree cover; Ecotone; Transition; Taiga; Tundra; Circumpolar ID GLOBAL CARBON-CYCLE; FOREST COVER; SATELLITE-OBSERVATIONS; CONTINUOUS FIELD; CLIMATE-CHANGE; NORTH-AMERICA; AVHRR DATA; VEGETATION; ALGORITHM; PRODUCTS AB A validation of the 2005 500 m MODIS vegetation continuous fields (VCF) tree cover product in the circumpolar taiga-tundra ecotone was performed using high resolution Quickbird imagery. Assessing the VCF's performance near the northern limits of the boreal forest can help quantify the accuracy of the product within this vegetation transition area. The circumpolar region was divided into 7 longitudinal zones and validation sites were selected in areas of varying tree cover where Quickbird imagery is available in Google Earth. Each site was linked to the corresponding VCF pixel and overlaid with a regular dot grid within the VCF pixel's boundary to estimate percent tree crown cover in the area. Percent tree crown cover was estimated using Quickbird imagery for 396 sites throughout the circumpolar region and related to the VCFs estimates of canopy cover for 2000-2005. Regression results of VCF inter-annual comparisons (2000-2005) and VCF-Quickbird image-interpreted estimates indicate that: (1) Pixel-level, inter-annual comparisons of VCF estimates of percent canopy cover were linearly related (mean R-2 = 0.77) and exhibited an average root mean square error (RMSE) of 10.1% and an average root mean square difference (RMSD) of 7.3%. (2) A comparison of image-interpreted percent tree crown cover estimates based on dot counts on Quickbird color images by two different interpreters were more variable (R-2 = 0.73, RMSE = 14.8%, RMSD = 18.7%) than VCF inter-annual comparisons. (3) Across the circumpolar boreal region, 2005 VCF-Quickbird comparisons were linearly related, with an R-2 = 0.57, a RMSE = 13.4% and a RMSD = 21.3%, with a tendency to over-estimate areas of low percent tree cover and anomalous VCF results in Scandinavia. The relationship of the VCF estimates and ground reference indicate to potential users that the VCFs tree cover values for individual pixels, particularly those below 20% tree cover, may not be precise enough to monitor 500 m pixel-level tree cover in the taiga-tundra transition zone. (C) 2009 Elsevier Inc. All rights reserved. C1 [Montesano, P. M.] Sci Syst & Applicat Inc, Lanham, MD 20706 USA. [Nelson, R.; Kerber, A.; Ranson, K. J.] NASA, Goddard Space Flight Ctr, Biospher Sci Branch, Greenbelt, MD 20771 USA. [Sun, G.] Univ Maryland, Dept Geog, College Pk, MD 20742 USA. [Margolis, H.] Univ Laval, Ctr Etud Foret, Quebec City, PQ G1K 7P4, Canada. RP Montesano, PM (reprint author), Sci Syst & Applicat Inc, Lanham, MD 20706 USA. EM paul.m.montesano@nasa.gov RI Ranson, Kenneth/G-2446-2012; Nelson, Ross/H-8266-2014 OI Ranson, Kenneth/0000-0003-3806-7270; NR 50 TC 48 Z9 49 U1 2 U2 14 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0034-4257 J9 REMOTE SENS ENVIRON JI Remote Sens. Environ. PD OCT PY 2009 VL 113 IS 10 BP 2130 EP 2141 DI 10.1016/j.rse.2009.05.021 PG 12 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA 487MA UT WOS:000269277200008 ER PT J AU Chopping, M Nolin, A Moisen, GG Martonchik, JV Bull, M AF Chopping, Mark Nolin, Anne Moisen, Gretchen G. Martonchik, John V. Bull, Michael TI Forest canopy height from the Multiangle Imaging SpectroRadiometer (MISR) assessed with high resolution discrete return lidar SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE Forest; Canopy; Height; Cover; Biomass; Multiangle; Model; Inversion; Mapping ID REMOTE-SENSING DATA; BIDIRECTIONAL REFLECTANCE MODEL; ANGLE SPECTRAL DATA; BACKGROUND REFLECTANCE; UNDERSTORY VEGETATION; BIOPHYSICAL STRUCTURE; VERTICAL STRUCTURE; COVER; INVERSION; CARBON AB In this study retrievals of forest canopy height were obtained through adjustment of a simple geometric-optical (GO) model against red band surface bidirectional reflectance estimates from NASA's Multiangle Imaging SpectroRadiometer (MISR), mapped to a 250 m grid. The soil-understory background contribution was partly isolated prior to inversion using regression relationships with the isotropic, geometric, and volume scattering kernel weights of a Li-Ross kernel-driven bidirectional reflectance distribution function (BRDF) model. The height retrievals were assessed using discrete return lidar data acquired over sites in Colorado as part of the Cold Land Processes Experiment (CLPX) and used with fractional crown cover retrievals to obtain aboveground woody biomass estimates. For all model runs with reasonable backgrounds and initial b/r (vertical to horizontal crown radii) values <2.0, root mean square error (RMSE) distributions were centered between 2.5 and 3.7 m while R(2) distributions were centered between 0.4 and 0.7. The MISR/GO aboveground biomass estimates predicted via regression on fractional cover and mean canopy height for the CLPX sites showed good agreement with U.S. Forest Service Interior West map data (adjusted R(2) = 0.84). The implication is that multiangle sensors such as MISR can provide spatially contiguous retrievals of forest canopy height, cover, and aboveground woody biomass that are potentially useful in mapping distributions of aboveground carbon stocks, tracking disturbance, and in initializing, constraining, and validating ecosystem models. This is important because the MISR record is spatially comprehensive and extends back to the year 2000 and the launch of the NASA Earth Observing System (EOS) Terra satellite; it might thus provide a similar to 10-year baseline record that would enhance exploitation of data from the NASA Deformation, Ecosystem Structure and Dynamics of Ice (DESDynl) mission, as well as furthering realization of synergies with active instruments. (C) 2009 Elsevier Inc. All rights reserved. C1 [Chopping, Mark] Montclair State Univ, Dept Earth & Environm Studies, Montclair, NJ 07043 USA. [Nolin, Anne] Oregon State Univ, Dept Geosci, Corvallis, OR 97331 USA. [Moisen, Gretchen G.] US Forest Serv, USDA, Rocky Mt Res Stn, Ogden, UT 84401 USA. [Martonchik, John V.; Bull, Michael] NASA, Jet Prop Lab, Pasadena, CA 91109 USA. RP Chopping, M (reprint author), Montclair State Univ, Dept Earth & Environm Studies, Montclair, NJ 07043 USA. EM chopping@pegasus.montclair.edu FU NASA Earth Observing System [NNX08AE71G] FX This research was supported by NASA Earth Observing System grant NNX08AE71G to MC (Technical Manager: Dr. William Emanuel). The MISR data were obtained from the NASA Langley Atmospheric Science Data Center. The CLPX data were provided courtesy of National Snow and Ice Data Center, Boulder. We thank Xiaohong Chopping: David Diner (MISR Scientist, NASA/JPL) and the MISR Science Team; Molly McAllister (National Snow and Ice Data Center, University of Colorado, Boulder, CO); Chad Poole (Spectrum Mapping LLC, Albuquerque, NM); Ron Tymcio and Tracey Frescino (US Forest Service, Rocky Mountain Research Station, Ogden, UT); Matt Smith and the Global Land Cover Facility (University of Maryland, College Park, MD): Joseph Youn and Michael Stoppay (Computer Operations for Research and Education, College of Science and Mathematics, Montclair State University); and all participants in CLPX NR 54 TC 24 Z9 26 U1 0 U2 13 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0034-4257 J9 REMOTE SENS ENVIRON JI Remote Sens. Environ. PD OCT PY 2009 VL 113 IS 10 BP 2172 EP 2185 DI 10.1016/j.rse.2009.05.017 PG 14 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA 487MA UT WOS:000269277200012 ER PT J AU Hulley, GC Hook, SJ Baldridge, AM AF Hulley, Glynn C. Hook, Simon J. Baldridge, Alice M. TI Validation of the North American ASTER Land Surface Emissivity Database (NAALSED) version 2.0 using pseudo-invariant sand dune sites SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE Emissivity; ASTER; Validation; Sand dunes; NAALSED ID CALIBRATION; SENSORS; TEMPERATURE; RETRIEVALS; CLIMATE; MODIS; FIELD AB Knowledge of the Land Surface Emissivity (LSE) in the Thermal Infrared (TIR: 8-12 mu m) part of the electromagnetic spectrum is essential to derive accurate Land Surface Temperatures (LSTs) from spaceborne TIR measurements. This study focuses on validation of the emissivity product in the North American ASTER Land Surface Emissivity Database (NAALSED) v2.0 - a mean seasonal, gridded emissivity product produced at 100 in spatial resolution using all Advanced Spaceborne Thermal Emission and Reflection Radiometer (ASTER) scenes from 2000 to 2008 over North America (http://emissivity.jpl.nasa.gov). The NAALSED emissivity product was validated over bare surfaces with laboratory measurements of sand samples collected at nine pseudo-invariant sand dune sites located in the western/southwestern USA. The nine sand dune sites cover a broad range of surface emissivities in the TIR. Results show that the absolute mean emissivity difference between NAALSED and the laboratory results for the nine validation sites and all five ASTER TIR bands was 0.016 (1.6%). This emissivity difference is equivalent to approximately a 1 K error in the land surface temperature for a material at 300 K in the TIR. (C) 2009 Published by Elsevier Inc. C1 [Hulley, Glynn C.; Hook, Simon J.; Baldridge, Alice M.] 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 FU Jet Propulsion Laboratory; California Institute of Technology; National Aeronautics and Space Administration FX The research described in this paper was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under the contract with the National Aeronautics and Space Administration. We kindly thank Dr. Tom Schmugge from New Mexico State University for assisting us with field work at White Sands, and also Dr. Joshua Bandfield for providing the basalt samples from Moses Lake, WA. ASTER data was provided by NASA/GSFC/METI/ERSDAC/JAROS, and U.S./Japan ASTER Science Team. NR 30 TC 34 Z9 35 U1 1 U2 11 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0034-4257 J9 REMOTE SENS ENVIRON JI Remote Sens. Environ. PD OCT PY 2009 VL 113 IS 10 BP 2224 EP 2233 DI 10.1016/j.rse.2009.06.005 PG 10 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA 487MA UT WOS:000269277200017 ER PT J AU Wal, RLV Berger, GM Kulis, MJ Hunter, GW Xu, JC Evans, L AF Wal, Randy L. Vander Berger, Gordon M. Kulis, Michael J. Hunter, Gary W. Xu, Jennifer C. Evans, Laura TI Synthesis Methods, Microscopy Characterization and Device Integration of Nanoscale Metal Oxide Semiconductors for Gas Sensing SO SENSORS LA English DT Article DE metal oxide; gas sensor; nanostructure; integration; nanorods; catalyst; gas detector; gas analysis ID LOW-TEMPERATURE; ZNO NANOWIRES; GROWTH; NANOSTRUCTURES; TRANSPORT; ARRAYS; PHOTOLUMINESCENCE; NANOCRYSTALLINE; NANOBELTS; NANORODS AB A comparison is made between SnO2, ZnO, and TiO2 single-crystal nanowires and SnO2 polycrystalline nanofibers for gas sensing. Both nanostructures possess a one-dimensional morphology. Different synthesis methods are used to produce these materials: thermal evaporation-condensation (TEC), controlled oxidation, and electrospinning. Advantages and limitations of each technique are listed. Practical issues associated with harvesting, purification, and integration of these materials into sensing devices are detailed. For comparison to the nascent form, these sensing materials are surface coated with Pd and Pt nanoparticles. Gas sensing tests, with respect to H-2, are conducted at ambient and elevated temperatures. Comparative normalized responses and time constants for the catalyst and noncatalyst systems provide a basis for identification of the superior metal-oxide nanostructure and catalyst combination. With temperature-dependent data, Arrhenius analyses are made to determine activation energies for the catalyst-assisted systems. C1 [Wal, Randy L. Vander] Penn State Univ, Dept Energy & Mineral Engn, Energy Inst, University Pk, PA 16802 USA. [Wal, Randy L. Vander] Penn State Univ, PSIEE, University Pk, PA 16802 USA. [Berger, Gordon M.; Kulis, Michael J.] NCSER, Cleveland, OH 44135 USA. [Hunter, Gary W.; Xu, Jennifer C.; Evans, Laura] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Wal, RLV (reprint author), Penn State Univ, Dept Energy & Mineral Engn, Energy Inst, 203 Hosler Bldg, University Pk, PA 16802 USA. EM RandyVW@psu.edu; Gordon.M.Berger@grc.nasa.gov; Michael.J.Kulis@grc.nasa.gov; Gary.W.Hunter@grc.nasa.gov; Jennifer.C.Xu@grc.nasa.gov; Laura.Evans@grc.nasa.gov FU NASA; Penn State Institutes of Energy and the Environment; Keystone Innovation Starter Kit, (KISK) [C000032466] FX This work is presently funded by the NASA Aeronautics Research Mission Directorate in both the Aviation Safety and Fundamental Aeronautics programs under the Integrated Vehicle Health Management, Subsonic Fixed Wing, and Supersonics projects. Prior-year NASA funding for this work included the NASA Glenn Strategic Research Fund (SRF) and the Independent Research and Development Program. Sensor testing was performed by D. Androjna. Dr. R. Vander Wal also acknowledges support through the Penn State Institutes of Energy and the Environment and the Keystone Innovation Starter Kit, (KISK), Contract No. C000032466 with Penn State University. NR 49 TC 4 Z9 4 U1 5 U2 29 PU MDPI AG PI BASEL PA ST ALBAN-ANLAGE 66, CH-4052 BASEL, SWITZERLAND SN 1424-8220 J9 SENSORS-BASEL JI Sensors PD OCT PY 2009 VL 9 IS 10 BP 7866 EP 7902 DI 10.3390/s91007866 PG 37 WC Chemistry, Analytical; Electrochemistry; Instruments & Instrumentation SC Chemistry; Electrochemistry; Instruments & Instrumentation GA 512QT UT WOS:000271265800015 ER PT J AU Bone, LA van Driel-Gesztelyi, L Culhane, JL Aulanier, G Liewer, P AF Bone, L. A. van Driel-Gesztelyi, L. Culhane, J. L. Aulanier, G. Liewer, P. TI Formation, Interaction and Merger of an Active Region and a Quiescent Filament Prior to Their Eruption on 19 May 2007 SO SOLAR PHYSICS LA English DT Article DE Corona, active; Helicity, magnetic; Magnetic fields, corona; Prominences, formation and evolution ID MAGNETIC-FIELDS; PROMINENCE; EVOLUTION AB We report observations of the formation of two filaments -aEuro parts per thousand one active and one quiescent, and their subsequent interactions prior to eruption. The active region filament appeared on 17 May 2007, followed by the quiescent filament about 24 hours later. In the 26 hour interval preceding the eruption, which occurred at around 12:50 UT on 19 May 2007, we see the two filaments attempting to merge and filament material is repeatedly heated suggesting magnetic reconnection. The filament structure is observed to become increasingly dynamic preceding the eruption with two small hard X-ray sources seen close to the active part of the filament at around 01:38 UT on 19 May 2007 during one of the activity episodes. The final eruption on 19 May at about 12:51 UT involves a complex CME structure, a flare and a coronal wave. A magnetic cloud is observed near Earth by the STEREO-B and WIND spacecraft about 2.7 days later. Here we describe the behaviour of the two filaments in the period prior to the eruption and assess the nature of their dynamic interactions. C1 [Bone, L. A.; van Driel-Gesztelyi, L.; Culhane, J. L.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. [van Driel-Gesztelyi, L.; Aulanier, G.] Observ Paris, CNRS, LESIA, UMR 8109, F-92195 Meudon, France. [van Driel-Gesztelyi, L.] Hungarian Acad Sci, Konkoly Observ, Budapest, Hungary. [Liewer, P.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP van Driel-Gesztelyi, L (reprint author), Univ Coll London, Mullard Space Sci Lab, Holmbury St Mary, Dorking RH5 6NT, Surrey, England. EM lvdg@mssl.ucl.ac.uk FU Leverhume Emeritus Fellowship; European Commission [218816] FX We thank Astrid Veronig for making Kanzelhohe data available and Cristina Mandrini for the Argentine HASTA H alpha data. We are grateful to Jingxiu Wang for coordinating our access to Ha data from Huairou and Yunnan Observatories, and Kazunari Shibata for the Hida Observatory H alpha data. We are grateful to the SOHO/MDI, TRACE, Hinode/XRT, STEREO/SECCHI and RHESSI Teams for their open data policy. SOHO is a cooperative mission between ESA and NASA. RHESSI is a NASA small explorer mission. Hinode is a Japanese mission developed and launched by ISAS/JAXA, with NAOJ as domestic partner and NASA and STFC (UK) as international partners. It is operated by these agencies in co-operation with ESA and NSC ( Norway). The STEREO/SECCHI data used here are produced by an international consortium of the Naval Research Laboratory ( USA), Lockheed Martin Solar and Astrophysics Laboratory ( USA), NASA Goddard Space Flight Center ( USA), Rutherford Appleton Laboratory ( UK), University of Birmingham ( UK), Max-Planck-Institut fur Sonnensystemforschung ( Germany), Centre Spatiale de Liege ( Belgium), Institut d'Optique Theorique et Applique ( France), Institute d'Astrophysique Spatiale ( France). L. A. B. acknowledges financial assistance from the Science & Technology Facilities Council ( STFC) of the UK. J.L.C. acknowledges the award of Leverhume Emeritus Fellowship. L.vD.G.'s work was partially supported by the European Commission through the SOTERIA Network (EU FP7 Space Science Project No. 218816). We are grateful to an anonymous referee for constructive comments, which helped us to improve the paper. NR 19 TC 22 Z9 22 U1 0 U2 2 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-0938 J9 SOL PHYS JI Sol. Phys. PD OCT PY 2009 VL 259 IS 1-2 BP 31 EP 47 DI 10.1007/s11207-009-9427-5 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 508AJ UT WOS:000270898200003 ER PT J AU Kramar, M Jones, S Davila, J Inhester, B Mierla, M AF Kramar, M. Jones, S. Davila, J. Inhester, B. Mierla, M. TI On the Tomographic Reconstruction of the 3D Electron Density for the Solar Corona from STEREO COR1 Data SO SOLAR PHYSICS LA English DT Article DE Sun: corona; Sun: magnetic fields; Methods: data analysis; Techniques: tomography; Techniques: image processing ID WHITE-LIGHT IMAGES; ROTATIONAL TOMOGRAPHY; MAGNETIC FIELDS; CALIBRATION AB We present for the first time a three-dimensional reconstruction of the electron density in the corona at distances from 1.5R (aS (TM)) to 4R (aS (TM)) using COR1 STEREO observations. The reconstruction is performed using a regularized tomography inversion method for two biweekly periods corresponding to Carrington Rotations 2058 and 2066. Images from the two STEREO spacecraft are used to compare the reconstructed density structures with coronal features located by triangulation. We find that the location of a bright tip of a helmet streamer obtained from the tomographic reconstruction is in good agreement with the location obtained by triangulation. The reconstructed density structure of the equatorial streamer belt is largely consistent with the variation of the current sheet derived from a potential magnetic field extrapolation for most of the equatorial region and for an MHD model of the corona. A zero-value density region in the reconstruction is identified with a low-density region seen in an EUVI image below the reconstruction domain. C1 [Kramar, M.; Mierla, M.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA. [Jones, S.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA. [Jones, S.; Davila, J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Inhester, B.] Max Planck Inst Sonnensyst Forsch, D-37191 Katlenburg Lindau, Germany. [Mierla, M.] Royal Observ Belgium, B-1180 Brussels, Belgium. [Mierla, M.] Acad Romana, Astron Inst, Bucharest 040557, Romania. RP Kramar, M (reprint author), Catholic Univ Amer, Dept Phys, 620 Michigan Ave NE, Washington, DC 20064 USA. EM kramar@helio.gsfc.nasa.gov NR 23 TC 23 Z9 23 U1 0 U2 0 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-0938 J9 SOL PHYS JI Sol. Phys. PD OCT PY 2009 VL 259 IS 1-2 BP 109 EP 121 DI 10.1007/s11207-009-9401-2 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 508AJ UT WOS:000270898200007 ER PT J AU Mierla, M Inhester, B Marque, C Rodriguez, L Gissot, S Zhukov, AN Berghmans, D Davila, J AF Mierla, M. Inhester, B. Marque, C. Rodriguez, L. Gissot, S. Zhukov, A. N. Berghmans, D. Davila, J. TI On 3D Reconstruction of Coronal Mass Ejections: I. Method Description and Application to SECCHI-COR Data SO SOLAR PHYSICS LA English DT Article DE Corona, structures; Coronal mass ejections, initiation and propagation ID STEREO MISSION; CONE MODEL; SPACECRAFT; GEOMETRY; IMAGES; LASCO; CMES AB The data from SECCHI-COR1 and SECCHI-COR2 coronagraphs onboard the STEREO mission, which was launched in October 2006, provide us with the first-ever stereoscopic images of the Sun's corona. These observations were found to be useful in inferring the three-dimensional structure of coronal mass ejections (CMEs) and their propagation direction in space. We apply four methods for reconstructing CMEs: i) Forward modeling technique; ii) Local correlation tracking (to identify the same feature in COR Ahead and COR Behind images) plus tie-point reconstruction technique; iii) Center of mass of the structures in a given epipolar plane plus tie-point reconstruction technique; iv) Polarization ratio technique. The four techniques are applied to three structured CMEs observed by COR1 and COR2 instruments, respectively, on 15 May 2007, 31 August 2007, and 25 March 2008. A comparison of the results obtained from the application of the four reconstruction algorithms is presented and discussed. C1 [Mierla, M.; Marque, C.; Rodriguez, L.; Gissot, S.; Zhukov, A. N.; Berghmans, D.] Royal Observ Belgium, Solar Terr Ctr Excellence, SIDC, B-1180 Brussels, Belgium. [Mierla, M.] Acad Romana, Astron Inst, Bucharest 040557, Romania. [Inhester, B.] Max Planck Inst Sonnensyst Forsch, D-37191 Katlenburg Lindau, Germany. [Zhukov, A. N.] Moscow MV Lomonosov State Univ, Skobeltsyn Inst Nucl Phys, Moscow 119992, Russia. [Davila, J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Mierla, M (reprint author), Royal Observ Belgium, Solar Terr Ctr Excellence, SIDC, Ringlaan 3, B-1180 Brussels, Belgium. EM marilena@oma.be; binhest@mps.mpg.de; josephmdavila@gmail.com FU Naval Research Laboratory (USA); Lockheed Martin Solar and Astrophysics Lab (USA); NASA Goddard Space Flight Center (USA); Rutherford Appleton Laboratory (UK); University of Birmingham (UK); Max-Planck-Institut for Solar System Research (Germany); Centre Spatiale de Liege (Belgium); Institut d'Optique Theorique et Appliquee (France); Institut d'Astrophysique Spatiale (France) FX M. M. would like to thank ROB for the financial support and for the facilities to carry out this work. The authors thank to A. Thernisien for providing the model data and for the productive discussions. We also thank W. Thompson, M. Kramar, N. Srivastava and G. Stenborg for fruitful discussions. We acknowledge the SECCHI/STEREO consortium for providing the data. The SECCHI data used here were produced by an international consortium of the Naval Research Laboratory (USA), Lockheed Martin Solar and Astrophysics Lab (USA), NASA Goddard Space Flight Center (USA), Rutherford Appleton Laboratory (UK), University of Birmingham (UK), Max-Planck-Institut for Solar System Research (Germany), Centre Spatiale de Liege (Belgium), Institut d'Optique Theorique et Appliquee (France), Institut d'Astrophysique Spatiale (France). We also thank the anonymous referee for useful comments and suggestions. NR 28 TC 33 Z9 36 U1 2 U2 6 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-0938 J9 SOL PHYS JI Sol. Phys. PD OCT PY 2009 VL 259 IS 1-2 BP 123 EP 141 DI 10.1007/s11207-009-9416-8 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 508AJ UT WOS:000270898200008 ER PT J AU Xie, H St Cyr, OC Gopalswamy, N Yashiro, S Krall, J Kramar, M Davila, J AF Xie, H. St Cyr, O. C. Gopalswamy, N. Yashiro, S. Krall, J. Kramar, M. Davila, J. TI On the Origin, 3D Structure and Dynamic Evolution of CMEs Near Solar Minimum SO SOLAR PHYSICS LA English DT Article DE Corona mass ejections; 3D reconstruction; Flux rope model fit ID CORONAL MASS EJECTIONS; FLUX ROPES; MAGNETIC RECONNECTION; PROMINENCE; GEOMETRY; MODEL; LASCO; TRANSIENT; FLARE; MOTION AB We have conducted a statistical study 27 coronal mass ejections (CMEs) from January 2007 - June 2008, using the stereoscopic views of STEREO SECCHI A and B combined with SOHO LASCO observations. A flux-rope model, in conjunction with 3D triangulations, has been used to reconstruct the 3D structures and determine the actual speeds of CMEs. The origin and the dynamic evolution of the CMEs are investigated using COR1, COR2 and EUVI images. We have identified four types of solar surface activities associated with CMEs: i) total eruptive prominence (totEP), ii) partially eruptive prominence (PEP), iii) X-ray flare, and iv) X-type magnetic structure (X-line). Among the 27 CMEs, 18.5% (5 of 27) are associated with totEPs, 29.6% (8 of 27) are associated with PEPs, 26% (7 of 27) are flare related, and 26% (7 of 27) are associated with X-line structures, and 43% (3 of 7) are associated with both X-line structures and PEPs. Three (11%) could not be associated with any detectable activity. The mean actual speeds for totEP-CMEs, PEP-CMEs, flare-CMEs, and X-line-CMEs are 404 km s(-1),247 km s(-1),909 km s(-1), and 276 km s(-1), respectively; the average mean values of edge-on and broadside widths for the 27 CMEs are 52 and 85 degrees, respectively. We found that slow CMEs (Va parts per thousand currency sign400 km s(-1)) tend to deflect towards and propagate along the streamer belts due to the deflections by the strong polar magnetic fields of corona holes, while some faster CMEs show opposite deflections away from the streamer belts. C1 [Xie, H.; Yashiro, S.; Kramar, M.] Catholic Univ Amer, Washington, DC 20064 USA. [St Cyr, O. C.; Gopalswamy, N.; Davila, J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Krall, J.] USN, Res Lab, Div Plasma Phys, Washington, DC 20375 USA. RP Xie, H (reprint author), Catholic Univ Amer, Washington, DC 20064 USA. EM hong.xie@nasa.gov RI Gopalswamy, Nat/D-3659-2012 FU NASA [NNX07A110G] FX The authors are thankful to William Thompson for developing solar software that assisted the data processing and 3D triangulations. H. X. would like to thank Holly Gilbert, Jim Klimchuk, and Bernard Kliem for valuable discussions. M. K. thanks Gordon Petrie for useful comments about potential field reconstruction methods, and Janet Luhmann whose potential field reconstruction code was used. H. X. is partially supported by NASA grant NNX07A110G. NR 53 TC 11 Z9 11 U1 0 U2 1 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-0938 EI 1573-093X J9 SOL PHYS JI Sol. Phys. PD OCT PY 2009 VL 259 IS 1-2 BP 143 EP 161 DI 10.1007/s11207-009-9422-x PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 508AJ UT WOS:000270898200009 ER PT J AU Gopalswamy, N Thompson, WT Davila, JM Kaiser, ML Yashiro, S Makela, P Michalek, G Bougeret, JL Howard, RA AF Gopalswamy, N. Thompson, W. T. Davila, J. M. Kaiser, M. L. Yashiro, S. Maekelae, P. Michalek, G. Bougeret, J. -L. Howard, R. A. TI Relation Between Type II Bursts and CMEs Inferred from STEREO Observations SO SOLAR PHYSICS LA English DT Article DE Coronal mass ejections; Type II radio bursts; Shocks; Flares; Dynamic spectrum ID CORONAL MASS EJECTIONS; RADIO-BURSTS; SOLAR ERUPTIONS; SHOCK-WAVES; NEAR-SUN; ACCELERATION; MISSION; LASCO AB The inner coronagraph (COR1) of the Solar Terrestrial Relations Observatory (STEREO) mission has made it possible to observe CMEs in the spatial domain overlapping with that of the metric type II radio bursts. The type II bursts were associated with generally weak flares (mostly B and C class soft X-ray flares), but the CMEs were quite energetic. Using CME data for a set of type II bursts during the declining phase of solar cycle 23, we determine the CME height when the type II bursts start, thus giving an estimate of the heliocentric distance at which CME-driven shocks form. This distance has been determined to be similar to 1.5R (s) (solar radii), which coincides with the distance at which the Alfv,n speed profile has a minimum value. We also use type II radio observations from STEREO/WAVES and Wind/WAVES observations to show that CMEs with moderate speed drive either weak shocks or no shock at all when they attain a height where the Alfv,n speed peaks (similar to 3R (s) -aEuro parts per thousand 4R (s)). Thus the shocks seem to be most efficient in accelerating electrons in the heliocentric distance range of 1.5R (s) to 4R (s). By combining the radial variation of the CME speed in the inner corona (CME speed increase) and interplanetary medium (speed decrease) we were able to correctly account for the deviations from the universal drift-rate spectrum of type II bursts, thus confirming the close physical connection between type II bursts and CMEs. The average height (similar to 1.5R (s)) of STEREO CMEs at the time of type II bursts is smaller than that (2.2R (s)) obtained for SOHO (Solar and Heliospheric Observatory) CMEs. We suggest that this may indicate, at least partly, the density reduction in the corona between the maximum and declining phases, so a given plasma level occurs closer to the Sun in the latter phase. In two cases, there was a diffuse shock-like feature ahead of the main body of the CME, indicating a standoff distance of 1R (s) -aEuro parts per thousand 2R (s) by the time the CME left the LASCO field of view. C1 [Gopalswamy, N.; Thompson, W. T.; Davila, J. M.; Kaiser, M. L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA. [Yashiro, S.] Interferometrics, Herndon, VA USA. [Maekelae, P.; Michalek, G.] Catholic Univ Amer, Washington, DC 20064 USA. [Bougeret, J. -L.] Observ Paris, Meudon, France. [Howard, R. A.] USN, Res Lab, Washington, DC 20375 USA. RP Gopalswamy, N (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD USA. EM nat.gopalswamy@nasa.gov RI Gopalswamy, Nat/D-3659-2012; Thompson, William/D-7376-2012 FU Naval Research Laboratory (USA); Lockheed Martin Solar and Astrophysical Laboratory (USA); NASA Goddard Space Flight Center (USA); Max Planck Institut fur Sonnensystemforschung (Germany); Centre Spatial de Liege (Belgium); University of Birmingham (UK); Rutherford Appleton Laboratory (UK); Institut d'Optique (France); Institute d'Astrophysique Spatiale (France) FX The SECCHI instrument was constructed by a consortium of international institutions: the Naval Research Laboratory (USA), the Lockheed Martin Solar and Astrophysical Laboratory (USA), the NASA Goddard Space Flight Center (USA), the Max Planck Institut fur Sonnensystemforschung (Germany), the Centre Spatial de Liege (Belgium), the University of Birmingham (UK), the Rutherford Appleton Laboratory (UK), the Institut d'Optique (France), and the Institute d'Astrophysique Spatiale (France). The S/WAVES instrument was built by a consortium including Observatoire de Paris (France), University of California at Berkeley (USA), University of Minnesota (USA), NASA Goddard Space FlightCenter (USA), and AAS Space Research Institute (Austria). SOHO is a project of international collaboration between ESA and NASA. We thank the anonymous referee for helpful comments. NR 37 TC 78 Z9 78 U1 0 U2 6 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-0938 J9 SOL PHYS JI Sol. Phys. PD OCT PY 2009 VL 259 IS 1-2 BP 227 EP 254 DI 10.1007/s11207-009-9382-1 PG 28 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 508AJ UT WOS:000270898200014 ER PT J AU Reiner, MJ Goetz, K Fainberg, J Kaiser, ML Maksimovic, M Cecconi, B Hoang, S Bale, SD Bougeret, JL AF Reiner, M. J. Goetz, K. Fainberg, J. Kaiser, M. L. Maksimovic, M. Cecconi, B. Hoang, S. Bale, S. D. Bougeret, J. -L. TI Multipoint Observations of Solar Type III Radio Bursts from STEREO and Wind SO SOLAR PHYSICS LA English DT Article DE Solar radio emissions; Intrinsic radiation characteristics ID CORONA; SPACECRAFT; ELECTRONS; ANTENNAS; ORIGIN; AU AB The twin STEREO and the Wind spacecraft make remote multipoint measurements of interplanetary radio sources of solar origin from widely separated vantage points. One year after launch, the angular separation between the STEREO spacecraft reached 45A degrees, which was ideal for locating solar type III radio sources in the heliosphere by three-spacecraft triangulation measurements from STEREO and Wind. These triangulated source locations enable intrinsic properties of the radio source, such as its beaming characteristics, to be deduced. We present the first three-point measurements of the beaming characteristics for two solar type III radio bursts that were simultaneously observed by the three spacecraft in December of 2007 and in January of 2008. These analyses suggest that individual type III bursts exhibit a wide beaming pattern that is approximately beamed along the direction tangent to the Parker spiral magnetic field line at the source location. C1 [Reiner, M. J.; Fainberg, J.; Kaiser, M. L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20071 USA. [Reiner, M. J.] Catholic Univ Amer, Washington, DC 20064 USA. [Goetz, K.] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA. [Maksimovic, M.; Cecconi, B.; Hoang, S.; Bougeret, J. -L.] Univ Paris Diderot, LESIA, CNRS, UPMC,Observ Paris, F-92190 Meudon, France. [Bale, S. D.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. RP Reiner, MJ (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20071 USA. EM michael.reiner@nasa.gov; goetz@space.umn.edu; joseph.fainberg@nasa.gov; michael.l.kaiser@nasa.gov; milan.maksimovic@obspm.fr; baptiste.cecconi@obspm.fr; song.hoang@obspm.fr; BALE@sunspot.ssl.berkeley.edu; Jean-Louis.Bougeret@obspm.fr RI Bale, Stuart/E-7533-2011 OI Bale, Stuart/0000-0002-1989-3596 NR 27 TC 20 Z9 20 U1 0 U2 2 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-0938 J9 SOL PHYS JI Sol. Phys. PD OCT PY 2009 VL 259 IS 1-2 BP 255 EP 276 DI 10.1007/s11207-009-9404-z PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 508AJ UT WOS:000270898200015 ER PT J AU Louarn, P Dieval, C Genot, V Lavraud, B Opitz, A Fedorov, A Sauvaud, JA Larson, D Galvin, A Acuna, MH Luhmann, J AF Louarn, P. Dieval, C. Genot, V. Lavraud, B. Opitz, A. Fedorov, A. Sauvaud, J. A. Larson, D. Galvin, A. Acuna, M. H. Luhmann, J. TI On the Temporal Variability of the "Strahl" and Its Relationship with Solar Wind Characteristics: STEREO SWEA Observations SO SOLAR PHYSICS LA English DT Article ID VELOCITY DISTRIBUTION-FUNCTIONS; HELIOS PLASMA-EXPERIMENT; EXOSPHERIC THEORY; ALFVEN WAVES; PITCH-ANGLE; ELECTRONS; SPACECRAFT; CORONA; FLUX AB The "strahl" is a specific population of the solar wind, constituted by strongly field aligned electrons flowing away from the Sun, with energies > 60 eV. Using the Solar Wind Electron Analyzer (SWEA) onboard STEREO, we investigate the short time scale fluctuations of this population. It is shown that its phase space density (PSD) at times presents fluctuations larger than 50% at scales of the order of minutes and less. The fluctuations are particularly strong for periods of a few tens of hours in high-speed streams, following the crossing of the corotating interaction region, when the strahl is also the most collimated in pitch angle. The amplitude of the fluctuations tends to decrease in conjunction with a broadening in pitch angle. Generally, the strongly fluctuating strahl is observed when the magnetic field is also highly perturbed. That SWEA is able to perform a very rapid 3D analysis at a given energy is essential since it can be demonstrated that the observed magnetic turbulence can only marginally perturb the PSD measurements. C1 [Louarn, P.; Dieval, C.; Genot, V.; Lavraud, B.; Opitz, A.; Fedorov, A.; Sauvaud, J. A.] UPS, CNRS, CESR, F-31028 Toulouse 4, France. [Larson, D.; Luhmann, J.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Galvin, A.] Univ New Hampshire, Inst Study Earth Oceans & Space, Durham, NH 03824 USA. [Acuna, M. H.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Louarn, P (reprint author), UPS, CNRS, CESR, 9 Ave Colonel Roche, F-31028 Toulouse 4, France. EM philippe.louarn@cesr.fr RI Galvin, Antoinette/A-6114-2013 FU CNES; CNRS; Universite Paul Sabatier, Toulouse FX This work has been supported by CNES, CNRS, and Universite Paul Sabatier, Toulouse. NR 28 TC 5 Z9 5 U1 1 U2 4 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-0938 J9 SOL PHYS JI Sol. Phys. PD OCT PY 2009 VL 259 IS 1-2 BP 311 EP 321 DI 10.1007/s11207-009-9402-1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 508AJ UT WOS:000270898200018 ER PT J AU Simunac, KDC Kistler, LM Galvin, AB Lee, MA Popecki, MA Farrugia, C Moebius, E Blush, LM Bochsler, P Wurz, P Klecker, B Wimmer-Schweingruber, RF Thompson, B Luhmann, JG Russell, CT Howard, RA AF Simunac, K. D. C. Kistler, L. M. Galvin, A. B. Lee, M. A. Popecki, M. A. Farrugia, C. Moebius, E. Blush, L. M. Bochsler, P. Wurz, P. Klecker, B. Wimmer-Schweingruber, R. F. Thompson, B. Luhmann, J. G. Russell, C. T. Howard, R. A. TI In Situ Observations of Solar Wind Stream Interface Evolution SO SOLAR PHYSICS LA English DT Article ID COROTATING INTERACTION REGIONS; LARGE-SCALE STRUCTURE; CORONAL HOLES; INTERPLANETARY MEDIUM; STEREO; ACE AB The heliocentric orbits of the two STEREO satellites are similar in radius and ecliptic latitude, with separation in longitude increasing by about 45A degrees per year. This arrangement provides a unique opportunity to study the evolution of stream interfaces near 1 AU over time scales of hours to a few days, much less than the period of a Carrington rotation. Assuming nonevolving solar wind sources that corotate with the Sun, we calculated the expected time and longitude of arrival of stream interfaces at the Ahead observatory based on the in situ solar wind speeds measured at the Behind observatory. We find agreement to within 5A degrees between the expected and actual arrival longitude until the spacecraft are separated by more than 20A degrees in heliocentric inertial longitude. This corresponds to about one day between the measurement times. Much larger deviations, up to 25A degrees in longitude, are observed after 20A degrees separation. Some of the deviations can be explained by a latitude difference between the spacecraft, but other deviations most likely result from evolution of the source region. Both remote and in situ measurements show that changes at the source boundary can occur on a time scale much shorter than one solar rotation. In 32 of 41 cases, the interface was observed earlier than expected at STEREO/Ahead. C1 [Simunac, K. D. C.; Kistler, L. M.; Galvin, A. B.; Lee, M. A.; Popecki, M. A.; Farrugia, C.; Moebius, E.; Bochsler, P.] Univ New Hampshire, Ctr Space Sci, Durham, NH 03824 USA. [Blush, L. M.; Bochsler, P.; Wurz, P.] Univ Bern, Inst Phys, Bern, Switzerland. [Klecker, B.] Max Planck Inst Extraterr Phys, D-37075 Garching, Germany. [Wimmer-Schweingruber, R. F.] Univ Kiel, Inst Expt & Appl Phys, Kiel, Germany. [Thompson, B.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Luhmann, J. G.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Russell, C. T.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90095 USA. [Howard, R. A.] USN, Res Lab, EO Hulburt Ctr Space Res, Washington, DC 20375 USA. RP Simunac, KDC (reprint author), Univ New Hampshire, Ctr Space Sci, Durham, NH 03824 USA. EM ksimunac@cisunix.unh.edu RI Thompson, Barbara/C-9429-2012; Galvin, Antoinette/A-6114-2013; Russell, Christopher/E-7745-2012; OI Russell, Christopher/0000-0003-1639-8298; Moebius, Eberhard/0000-0002-2745-6978 FU NASA [NAS5-00132] FX This work was supported under NASA Contract No. NAS5-00132. This work utilizes data obtained by the Global Oscillation Network Group (GONG) Program, managed by the National Solar Observatory, which is operated by AURA, Inc., under a cooperative agreement with the National Science Foundation. The GONG data were acquired by instruments operated by the Big Bear Solar Observatory, High Altitude Observatory, Learmonth Solar Observatory, Udaipur Solar Observatory, Instituto de Astrofisica de Canarias, and Cerro Tololo Interamerican Observatory. The authors are grateful to the IMPACT team for their data. The SECCHI instrument was constructed by a consortium of international institutions: the Naval Research Laboratory (USA), the Lockheed Martin Solar and Astrophysical Laboratory (USA), the NASA Goddard Space Flight Center (USA), the Max Planck Institut fur Sonnensystemforschung (Germany), the Centre Spatial de Liege (Belgium), the University of Birmingham (UK), the Rutherford Appleton Laboratory (UK), the Institut d'Optique (France), and the Institute d'Astrophysique Spatiale (France). NR 24 TC 12 Z9 13 U1 0 U2 0 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-0938 J9 SOL PHYS JI Sol. Phys. PD OCT PY 2009 VL 259 IS 1-2 BP 323 EP 344 DI 10.1007/s11207-009-9393-y PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 508AJ UT WOS:000270898200019 ER PT J AU Jian, LK Russell, CT Luhmann, JG Galvin, AB MacNeice, PJ AF Jian, L. K. Russell, C. T. Luhmann, J. G. Galvin, A. B. MacNeice, P. J. TI Multi-Spacecraft Observations: Stream Interactions and Associated Structures SO SOLAR PHYSICS LA English DT Article DE Solar wind; Stream interaction; Shock; Multi-spacecraft observation ID COROTATING INTERACTION REGIONS; CORONAL MASS EJECTIONS; SOLAR-WIND; MAGNETIC-FIELDS; PLASMA; ULYSSES; AU; INSTRUMENTATION; PIONEER-10; EVOLUTION AB The stream interaction region (SIR), formed when a fast stream overtakes a preceding slow stream, is the predominant large-scale solar wind structure at this early phase of the STEREO mission. Using multi-spacecraft observations from STEREO A and B, ACE, Wind, and Ulysses in 2007, we analyze three stream interaction events in depth in May, August, and November of 2007, respectively, when the spacecraft had quite different spatial separations. We attempt to determine the causes of the differences in the SIR properties, whether they are spatial or temporal variations, and also to examine the steepening or widening of the SIR during its radial evolution. The presence and characteristics of associated shocks, the relation to the heliospheric current sheet, and other structures are also studied. C1 [Jian, L. K.; Russell, C. T.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90095 USA. [Luhmann, J. G.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Galvin, A. B.] Univ New Hampshire, Dept Phys, Durham, NH 03824 USA. [MacNeice, P. J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Jian, LK (reprint author), Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90095 USA. EM jlan@igpp.ucla.edu; ctrussel@igpp.ucla.edu; jgluhman@ssl.berkeley.edu; toni.galvin@unh.edu; Peter.J.MacNeice@nasa.gov RI Jian, Lan/B-4053-2010; MacNeice, Peter/F-5587-2012; Russell, Christopher/E-7745-2012; Galvin, Antoinette/A-6114-2013 OI Jian, Lan/0000-0002-6849-5527; Russell, Christopher/0000-0003-1639-8298; FU NASA STEREO [NAS5-03131] FX This research is supported by the NASA STEREO program through Grant NAS5-03131 administered by UC Berkeley. We sincerely thank all the PIs for making the data available. We gratefully acknowledge MWO and CCMC staff for providing us the photospheric magnetic dada and coronal modeling. We also thank R. J. Forsyth for helping us confirm Ulysses shock identifications. NR 32 TC 14 Z9 14 U1 0 U2 3 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-0938 J9 SOL PHYS JI Sol. Phys. PD OCT PY 2009 VL 259 IS 1-2 BP 345 EP 360 DI 10.1007/s11207-009-9445-3 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 508AJ UT WOS:000270898200020 ER PT J AU Leitner, M Farrugia, CJ Galvin, A Simunac, KDC Biernat, HK Osherovich, VA AF Leitner, M. Farrugia, C. J. Galvin, A. Simunac, K. D. C. Biernat, H. K. Osherovich, V. A. TI The Solar Wind Quasi-Invariant Observed by STEREO A and B at Solar Minimum 2007 and Comparison with Two Other Minima SO SOLAR PHYSICS LA English DT Article DE Solar wind; Solar cycle minima; Coronal mass ejections; Log-normal distribution ID PLASMA AB The solar wind quasi-invariant (QI) is defined as the ratio of the solar wind magnetic energy density to the plasma kinetic energy density (i.e., the inverse square of the Alfv,n Mach number). Previous work has found this quantity to be a good proxy for solar activity, correlating very well with the sunspot number at various heliospheric distances. It has the advantage of being locally determined from in situ measurements and can thus function as a heliospheric index of solar activity. Using STEREO A, STEREO B, and Wind data we obtain the distribution of QIs during the current solar activity minimum (March to December 2007). (1) We investigate whether this minimum is indeed weaker than previous ones by comparing this QI distribution with those during two other solar activity minima: 1995, using Wind data, and 1974, using Helios data at 1 AU. We find that, on average, QI(2007) is lower than during the previous two minima, indicating weaker solar activity. It also implies weaker MHD effects in solar wind flow around planetary magnetospheres, which, in turn, alters the solar wind's interaction with them. (2) In all three solar cycle minima considered we find that the QI distributions are reasonably well represented by a log-normal distribution, for which we give the respective mean and standard deviations. These values are used in comparing the QIs over the three solar minima. C1 [Leitner, M.] Univ Innsbruck, Inst Astro & Particle Phys, A-6020 Innsbruck, Austria. [Farrugia, C. J.; Galvin, A.; Simunac, K. D. C.] Univ New Hampshire, Ctr Space Sci, Durham, NH 03824 USA. [Farrugia, C. J.; Galvin, A.; Simunac, K. D. C.] Univ New Hampshire, Dept Phys, Durham, NH 03824 USA. [Biernat, H. K.] Austrian Acad Sci, Space Res Inst, A-8010 Graz, Austria. [Osherovich, V. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Leitner, M (reprint author), Univ Innsbruck, Inst Astro & Particle Phys, Technikerstr 25-8, A-6020 Innsbruck, Austria. EM m.leitner@uibk.ac.at; charlie.farrugia@unh.edu; toni.galvin@unh.edu; ksimunac@cisunix.unh.edu; helfried.biernat@oeaw.ac.at RI Galvin, Antoinette/A-6114-2013 FU Austrian "Fonds zur Forderung der wissenschaftlichen Forschung" [P20131-N16, P20145-N16]; NASA [NAS5-00132, NNX08AD11G] FX We thank Rainer Schwenn for providing us with Helios data. This work is supported by the Austrian "Fonds zur Forderung der wissenschaftlichen Forschung" under Project Nos. P20131-N16 and P20145-N16 and by NASA STEREO Grant No. NAS5-00132 to UNH. CJF also acknowledges the support of NASA Wind Grant No. NNX08AD11G. NR 17 TC 9 Z9 9 U1 0 U2 0 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-0938 J9 SOL PHYS JI Sol. Phys. PD OCT PY 2009 VL 259 IS 1-2 BP 381 EP 388 DI 10.1007/s11207-009-9412-z PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 508AJ UT WOS:000270898200022 ER PT J AU Flom, Y Wang, L Powell, MM Soffa, MA Rommel, ML AF Flom, Yury Wang, Len Powell, Mollie M. Soffa, Matthew A. Rommel, Monica L. TI Evaluating Margins of Safety in Brazed Joints SO WELDING JOURNAL LA English DT Editorial Material C1 [Flom, Yury; Wang, Len; Powell, Mollie M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA. [Soffa, Matthew A.; Rommel, Monica L.] ITT Space Syst Div, Rochester, NY USA. RP Flom, Y (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD USA. EM yury.a.flom@nasa.gov FU Dr. George Alcorn (GSFC) FX The authors would like to acknowledge David Puckett (NASA GSFC), Clint Casey (ITT), S. R. Lin (Aerospace Corp.), Ge Wang (NGST), and the other dedicated employees who contributed to this study. They would also like to thank Dr. George Alcorn (GSFC) for his continuous support of this effort. NR 13 TC 4 Z9 4 U1 0 U2 0 PU AMER WELDING SOC PI MIAMI PA 550 N W LEJEUNE RD, MIAMI, FL 33126 USA SN 0043-2296 J9 WELD J JI Weld. J. PD OCT PY 2009 VL 88 IS 10 BP 31 EP 37 PG 7 WC Metallurgy & Metallurgical Engineering SC Metallurgy & Metallurgical Engineering GA 502IZ UT WOS:000270453500006 ER PT J AU Ofman, L Balikhin, M Russell, CT Gedalin, M AF Ofman, L. Balikhin, M. Russell, C. T. Gedalin, M. TI Collisionless relaxation of ion distributions downstream of laminar quasi-perpendicular shocks SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID TERMINATION SHOCK; MACH NUMBER; PICKUP IONS; BOW SHOCKS; HIGH-BETA; THERMALIZATION; WAVES AB Directed flow of incident ions provides the free energy which is redistributed in a shock among heated ions and electrons, accelerated particles, and magnetic compression. In low Mach number laminar shock the main channel of conversion is into downstream gyrating ions. Just behind the shock transition the ion distribution is substantially nongyrotropic, which results in spatially periodic variations of the ion pressure and, consequently, in time stationary downstream oscillations of the magnetic field. In the absence of significant level of nonstationarity, gyrotropization is due to the gyrophase mixing and slow. Theoretical analysis of the phenomenon and supporting hybrid simulations are presented. It is shown that these oscillations are more likely to be observed at low Mach number low beta shocks, while at higher Mach numbers or higher beta they may be obscured by waves crossing the shocks. C1 [Ofman, L.] CUA, Greenbelt, MD 20771 USA. [Ofman, L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Ofman, L.] Tel Aviv Univ, Dept Geophys & Planetary Sci, IL-69978 Tel Aviv, Israel. [Balikhin, M.] Univ Sheffield, ACSE, Sheffield S1 3JD, S Yorkshire, England. [Russell, C. T.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90095 USA. [Gedalin, M.] Ben Gurion Univ Negev, Dept Phys, IL-84105 Beer Sheva, Israel. RP Ofman, L (reprint author), CUA, Greenbelt, MD 20771 USA. RI Gedalin, Michael/A-5153-2012 OI Gedalin, Michael/0000-0003-1236-4787 FU Royal Society; ISSI; ISF [275/07]; University of Sheffield; NASA [NNX08AV88G, NNX08AF85G] FX [26] Wolfgang Baumjohann thanks Gary Zank and another reviewer for their assistance in evaluating this paper. NR 22 TC 22 Z9 22 U1 0 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 SEP 30 PY 2009 VL 114 AR A09106 DI 10.1029/2009JA014365 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 502MT UT WOS:000270465200004 ER PT J AU Bursik, MI Kobs, SE Burns, A Braitseva, OA Bazanova, LI Melekestsev, IV Kurbatov, A Pieri, DC AF Bursik, M. I. Kobs, S. E. Burns, A. Braitseva, O. A. Bazanova, L. I. Melekestsev, I. V. Kurbatov, A. Pieri, D. C. TI Volcanic plumes and wind: Jetstream interaction examples and implications for air traffic SO JOURNAL OF VOLCANOLOGY AND GEOTHERMAL RESEARCH LA English DT Article DE Avachinsky; Kliuchevskoi; Inyo Craters; Kamchatka; California; explosive eruption; volcanic plume; tephra ID TEPHRA; CALIFORNIA; CRATERS; REGION AB Volcanic plumes interact with the wind at all scales. On smaller scales, wind affects local eddy structure: on larger scales, wind shapes the entire plume trajectory. The polar jets or jetstreams are regions of high [generally eastbound] winds that span the globe from 30 to 60 degrees in latitude, centered at an altitude of about 10 km. They can be hundreds of kilometers wide, but as little as 1 km in thickness. Core windspeeds are up to 130 m/s. Modern transcontinental and transoceanic air routes are configured to take advantage of the jetstream. Eastbound commercial jets can save both time and fuel by flying within it; westbound aircraft generally seek to avoid it. Using both an integral model of plume motion that is formulated within a plume-centered coordinate system (BENT) as well as the Active Tracer High-resolution Atmospheric Model (ATHAM), we have calculated plume trajectories and rise heights under different wind conditions. Model plume trajectories compare well with the observed plume trajectory of the Sept 30/Oct 1, 1994, eruption of Kliuchevskoi Volcano, Kamchatka, Russia, for which measured maximum windspeed was 30-40 m/s at about 12 km. Tephra fall patterns for some prehistoric eruptions of Avachinsky Volcano, Kamchatka, and Inyo Craters, CA, USA, are anomalously elongated and inconsistent with simple models of tephra dispersal in a constant windfield. The Avachinsky deposit is modeled well by BENT using a windspeed that varies with height. Two potentially useful conclusions can be made about air routes and volcanic eruption plumes under jetstream conditions. The first is that by taking advantage of the jetstream, aircraft are flying within an airspace that is also preferentially occupied by volcanic eruption clouds and particles. The second is that, because eruptions with highly variable mass eruption rate pump volcanic particles into the jetstream under these conditions, it is difficult to constrain the tephra grain size distribution and mass loading present within a downwind volcanic plume or cloud that has interacted with the jetstream. Furthermore. anomalously large particles and high mass loadings could be present within the cloud, if it was in fact formed by an eruption with a high mass eruption rate. In terms of interpretation of tephra dispersal patterns, the results suggest that extremely elongated isopach or isopleth patterns may often be the result of eruption into the jetstream, and that estimation of the mass eruption rate from these elongated patterns should be considered cautiously. (C) 2009 Elsevier B.V. All rights reserved. C1 [Bursik, M. I.; Kobs, S. E.; Burns, A.] SUNY Buffalo, Dept Geol, Buffalo, NY 14260 USA. [Braitseva, O. A.; Bazanova, L. I.; Melekestsev, I. V.] Russian Acad Sci, Inst Volcanol & Seismol, Petropavlovsk Kamchatski 683006, Russia. [Kurbatov, A.] Univ Maine, Climate Change Inst, Orono, ME 04469 USA. [Pieri, D. C.] CALTECH, Jet Prop Lab, Div Earth & Space Sci, Pasadena, CA 91109 USA. RP Bursik, MI (reprint author), SUNY Buffalo, Dept Geol, Buffalo, NY 14260 USA. EM mib@geology.buffalo.edu FU National Science Foundation [EAR0711464, EAR0538227]; National Aeronautics and Space Administration; California Institute of Technology; Science Applications International Corp FX This research was supported in part by grants from the National Science Foundation (EAR0711464 and EAR0538227), National Aeronautics and Space Administration, the California Institute of Technology, and Science Applications International Corp. Part of the work (D. Pieri) was performed at the jet Propulsion Laboratory, California Institute of Technology, under contract to the NASA Geology Program. The creators of ATHAM (H. Graf et al.) are thanked for sharing the source code and allowing its use by other researchers; A. Burns' modeling of the Kliuchevskoi plume with ATHAM was completed following a stay at MPI, Hamburg, for which we are grateful. M. Melnyk assisted with particle analysis in the laboratory; V. Kirianov is thanked for the radiosonde wind profile for Kliuchevskoi. Larry Mastin, Amanda Clarke and an anonymous reviewer are thanked for numerous helpful comments. NR 20 TC 20 Z9 21 U1 2 U2 11 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 SEP 30 PY 2009 VL 186 IS 1-2 BP 60 EP 67 DI 10.1016/j.jvolgeores.2009.01.021 PG 8 WC Geosciences, Multidisciplinary SC Geology GA 498DN UT WOS:000270117100006 ER PT J AU Hecht, JH Alexander, MJ Walterscheid, RL Gelinas, LJ Vincent, RA MacKinnon, AD Woithe, JM May, PT Skinner, WR Mlynczak, MG Russell, JM AF Hecht, J. H. Alexander, M. J. Walterscheid, R. L. Gelinas, L. J. Vincent, R. A. MacKinnon, A. D. Woithe, J. M. May, P. T. Skinner, W. R. Mlynczak, M. G. Russell, J. M., III TI Imaging of atmospheric gravity waves in the stratosphere and upper mesosphere using satellite and ground-based observations over Australia during the TWPICE campaign SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID OH AIRGLOW; LOWER THERMOSPHERE; RADAR OBSERVATIONS; MIDDLE ATMOSPHERE; MF RADAR; NIGHTGLOW; THUNDERSTORM; EMISSION; IMAGES; MODEL AB During the Tropical Warm Pool International Cloud Experiment (TWPICE) an intense tropical low was situated between Darwin and Alice Springs, Australia. Observations made on 31 January 2006 by the Atmospheric Infrared Sounder instrument on the NASA Aqua satellite imaged the presence of atmospheric gravity waves (AGWs), at approximately 40 km altitude, with horizontal wavelengths between 200 and 400 km that were originating from the region of the storm. Airglow images obtained from Alice Springs (about 600 km from the center of the low) showed the presence of similar waves with observed periods of 1 to 2 h. The images also revealed the presence of 30- to 45-km-horizontal-wavelength AGWs with shorter observed periods of near 15 to 25 min. Ray tracing calculations show that (1) some of the long wavelength waves traveled on rays, without ducting, to the altitudes where the observations were obtained, and (2) shorter-period waves rapidly reached 85 km altitude at a horizontal distance close to the storm, thus occurring over Alice Springs only if they were trapped or ducted. The mesospheric inversion layer seen in the measured temperature data almost forms such a trapped region. The winds therefore critically control the formation of the trapped region. Wind profiles deduced from the available data show the plausibility for the formation of such a trapped region. Variations in the wind, however, would make ideal trapped region conditions short-lived, and this may account for the sporadic nature of the short-period wave observations. C1 [Hecht, J. H.; Walterscheid, R. L.; Gelinas, L. J.] Aerosp Corp, Dept Space Sci, Los Angeles, CA 90009 USA. [Alexander, M. J.] NW Res Associates Inc, Colorado Res Associates Div, Boulder, CO 80301 USA. [Vincent, R. A.; MacKinnon, A. D.; Woithe, J. M.] Univ Adelaide, Dept Phys & Math Phys, Adelaide, SA 5005, Australia. [May, P. T.] Ctr Australian Weather & Climate Res, Melbourne, Vic 3001, Australia. [Skinner, W. R.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. [Mlynczak, M. G.] NASA, Langley Res Ctr, Climate Sci Branch, Hampton, VA 23681 USA. [Russell, J. M., III] Hampton Univ, Ctr Atmospher Sci, Hampton, VA 23668 USA. RP Hecht, JH (reprint author), Aerosp Corp, Dept Space Sci, POB 92957,Mail Stop M2-260, Los Angeles, CA 90009 USA. EM james.hecht@aero.org; alexand@cora.nwra.com; richard.walterscheid@aero.org; lynette.gelinas@aero.org; robert.vincent@physics.adelaide.edu.au; andrew.mackinnon@physics.adelaide.edu.au; jwoithe@physics.adelaide.edu.au; pmay@bom.gov.au; wskinner@umich.edu; martin.g.mlynczak@nasa.gov; james.russell@hamptonu.edu RI Mlynczak, Martin/K-3396-2012 FU NSF [ATM-0737557, ATM-0436516]; NASA [NAG5-13025, NNH04CC54C, NNH08AH43I, NAG5 5049]; Australian Research Council [DP0558361]; Department of Energy; UK Natural Environment Research Council (NERC) [NE/C512688/1]; Australian National Marine Research Facility; Australian Bureau of Meteorology; Kyoto University Active Geosphere Investigation (KAGI) FX Thanks go to Peter Strickland and Jeremy Ward for the considerable help at Alice Springs. Elizabeth Ebert of the Centre for Australian Weather at the Bureau of Meteorology in Melbourne, Australia, provided the rainfall data. The Aerospace Corporation's results could not have been obtained without the invaluable help given by Kirk Crawford in all aspects of this project. J. H. H., R. L. W., and L. J. G. were supported by NSF grants ATM-0737557 and ATM-0436516 and by NASA grant NAG5-13025. M. J. A. was supported by the NASA program Earth System Science Research using data and products from TERRA, AQUA, and ACRIM Satellites, contracts NNH04CC54C and NNH08AH43I. R. A. V. acknowledges support from Australian Research Council grant DP0558361. The authors acknowledge the SABER science team for their role in developing the scientific algorithms for the SABER temperatures. W. R. S. was supported in part by NASA grant NAG5 5049. P. T. M. acknowledges the support of the Department of Energy Atmospheric Radiation Measurement Program. TWP-ICE was supported under the auspices of the U. S. Department of Energy ARM Program, the ARM Uninhabited Aerospace Vehicle (UAV) Program, NASA CloudSat, the UK Natural Environment Research Council (NERC) grant NE/C512688/1, the NERC Airborne Remote Sensing Facility, the Australian National Marine Research Facility, the Australian Bureau of Meteorology, and the Kyoto University Active Geosphere Investigation (KAGI) for the 21st century COE program. Centre for Australian Weather and Climate Research is a partnership between the Australian Bureau of Meteorology and CSIRO. Vaisala generously donated the radiosonde base stations. The Charles Darwin University, Darwin RAAF Base, and the Tiwi Island Land Council all made extensive facilities available to the experiment. The initial version of the wavelet software was provided by C. Torrence and G. Compo and is available at http://paos. colorado. edu/ research/wavelets/. NR 51 TC 20 Z9 21 U1 0 U2 4 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD SEP 29 PY 2009 VL 114 AR D18123 DI 10.1029/2008JD011259 PG 20 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 502MA UT WOS:000270463100001 ER PT J AU McCarty, W Jedlovec, G Miller, TL AF McCarty, Will Jedlovec, Gary Miller, Timothy L. TI Impact of the assimilation of Atmospheric Infrared Sounder radiance measurements on short-term weather forecasts SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID SSI ANALYSIS SYSTEM; ERROR ANALYSIS; AIRS; TOVS; PREDICTION; AIRS/AMSU/HSB; RETRIEVAL; ALGORITHM; PRODUCTS; MISSION AB Advanced spaceborne instruments have the ability to improve the horizontal and vertical characterization of temperature and water vapor in the atmosphere through the explicit use of hyperspectral thermal infrared radiance measurements. The incorporation of these measurements into a data assimilation system provides a means to continuously characterize a three-dimensional, instantaneous atmospheric state necessary for the time integration of numerical weather forecasts. Measurements from the National Aeronautics and Space Administration (NASA) Atmospheric Infrared Sounder (AIRS) are incorporated into the grid point statistical interpolation (GSI) three-dimensional variational (3D-Var) assimilation system to provide improved initial conditions for use in a mesoscale modeling framework mimicking that of the operational North American Mesoscale (NAM) model. The methodologies for the incorporation of the measurements into the system are presented. Though the measurements have been shown to have a positive impact in global modeling systems, the measurements are further constrained in this system as the model top is physically lower than the global systems and there is no ozone characterization in the background state. For a study period, the measurements are shown to have positive impact on both the analysis state as well as subsequently spawned short-term (0-48 h) forecasts, particularly in forecasted geopotential height and precipitation fields. At 48 h, height anomaly correlations showed an improvement in forecast skill of 2.3 h relative to a system without the AIRS measurements. Similarly, the equitable threat and bias scores of precipitation forecasts of 25 mm (6 h)(-1) were shown to be improved by 8% and 7%, respectively. C1 [McCarty, Will] Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Goddard Space Flight Ctr, Global Modeling & Assimilat Off,NASA, Greenbelt, MD 20771 USA. [Jedlovec, Gary; Miller, Timothy L.] NASA, George C Marshall Space Flight Ctr, Earth Sci Off, Huntsville, AL 35812 USA. [McCarty, Will] Univ Alabama, Dept Atmospher Sci, Huntsville, AL 35899 USA. RP McCarty, W (reprint author), Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Goddard Space Flight Ctr, Global Modeling & Assimilat Off,NASA, Mail Code 610-1,8800 Greenbelt Rd, Greenbelt, MD 20771 USA. EM will.mccarty@nasa.gov RI McCarty, Will/E-9359-2012 FU NASA [NNG05GQ55H] FX This work was supported by NASA Headquarters under the NASA Earth and Space Science Fellowship Program grant NNG05GQ55H and by Tsengdar Lee of NASA Science Mission Directorate's Earth Science Division in support of the SPoRT program at the NASA Marshall Space Flight Center. The authors would also like to thank Stephen Lord of NCEP, Lars Peter Riishogaard of the JCSDA, and John Le Marshall, formerly of the JCSDA, for providing the computational resources required for this study. NR 39 TC 19 Z9 19 U1 0 U2 3 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD SEP 29 PY 2009 VL 114 AR D18122 DI 10.1029/2008JD011626 PG 14 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 502MA UT WOS:000270463100002 ER PT J AU Tangborn, A Cooper, R Pawson, S Sun, ZB AF Tangborn, Andrew Cooper, Robert Pawson, Steven Sun, Zhibin TI Chemical Source Inversion Using Assimilated Constituent Observations in an Idealized Two-Dimensional System SO MONTHLY WEATHER REVIEW LA English DT Article ID KALMAN FILTER; ATMOSPHERIC TRANSPORT; TRACER OBSERVATIONS; SURFACE EMISSIONS; MODEL; SENSITIVITY AB A source inversion technique for chemical constituents is presented that uses assimilated constituent observations rather than directly using the observations. The method is tested with a simple model problem, which is a two-dimensional Fourier-Galerkin transport model combined with a Kalman filter for data assimilation. Inversion is carried out using a Green's function method and observations are simulated from a true state with added Gaussian noise. The forecast state uses the same spectral model but differs by an unbiased Gaussian model error and emissions models with constant errors. The numerical experiments employ both simulated in situ and satellite observation networks. Source inversion was carried out either by directly using synthetically generated observations with added noise or by first assimilating the observations and using the analyses to extract observations. Twenty identical twin experiments were conducted for each set of source and observation configurations, and it was found that in the limiting cases of a very few localized observations or an extremely large observation network there is little advantage to carrying out assimilation first. For intermediate observation densities, the source inversion error standard deviation is decreased by 50% to 90% when the observations are assimilated with the Kalman filter before carrying out the Green's function inversion. C1 [Tangborn, Andrew; Pawson, Steven] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA. [Cooper, Robert] Williams Coll, Dept Phys, Williamstown, MA 01267 USA. [Sun, Zhibin] Univ Maryland, Dept Math & Stat, Baltimore, MD 21201 USA. RP Tangborn, A (reprint author), NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Code 610, Greenbelt, MD 20771 USA. EM andrew.v.tangborn@nasa.gov RI Pawson, Steven/I-1865-2014 OI Pawson, Steven/0000-0003-0200-717X FU NASA Modeling, Analysis, and Prediction (MAP) program; GSFC Laboratory FX This work is funded by the NASA Modeling, Analysis, and Prediction (MAP) program. R. Cooper was funded by the GSFC Laboratory for Atmospheres summer intern program. The authors gratefully acknowledge the helpful comments of the reviewers. NR 28 TC 0 Z9 0 U1 0 U2 1 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0027-0644 J9 MON WEATHER REV JI Mon. Weather Rev. PD SEP 29 PY 2009 VL 137 IS 9 BP 3013 EP 3025 DI 10.1175/2009MWR2775.1 PG 13 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 501LA UT WOS:000270382200017 ER PT J AU Mu, QZ Jones, LA Kimball, JS McDonald, KC Running, SW AF Mu, Qiaozhen Jones, Lucas A. Kimball, John S. McDonald, Kyle C. Running, Steven W. TI Satellite assessment of land surface evapotranspiration for the pan-Arctic domain SO WATER RESOURCES RESEARCH LA English DT Article ID NET PRIMARY PRODUCTION; GROSS PRIMARY PRODUCTION; CARBON-DIOXIDE; GAS-EXCHANGE; STOMATAL CONDUCTANCE; PRIMARY PRODUCTIVITY; VEGETATION INDEXES; ENERGY BALANCE; WATER-BALANCE; CO2 EXCHANGE AB Regional evapotranspiration (ET), including water loss from plant transpiration and soil evaporation, is essential to understanding interactions between land-atmosphere surface energy and water balances. Vapor pressure deficit (VPD) and surface air temperature are key variables for stomatal conductance and ET estimation. We developed an algorithm to estimate ET using the Penman-Monteith approach driven by Moderate Resolution Imaging Spectroradiometer (MODIS)-derived vegetation data and daily surface meteorological inputs including incoming solar radiation, air temperature, and VPD. The model was applied using alternate daily meteorological inputs, including (1) site level weather station observations, (2) VPD and air temperature derived from the Advanced Microwave Scanning Radiometer (AMSR-E) on the EOS Aqua satellite, and (3) Global Modeling and Assimilation Office (GMAO) reanalysis meteorology-based surface air temperature, humidity, and solar radiation data. Model performance was assessed across a North American latitudinal transect of six eddy covariance flux towers representing northern temperate grassland, boreal forest, and tundra biomes. Model results derived from the three meteorology data sets agree well with observed tower fluxes (r > 0.7; P < 0.003; root mean square error of latent heat flux < 30 W m(-2)) and capture spatial patterns and seasonal variability in ET. The MODIS-AMSR-E-derived ET results also show similar accuracy to ET results derived from GMAO, while ET estimation error was generally more a function of algorithm parameterization than differences in meteorology drivers. Our results indicate significant potential for regional mapping and monitoring daily land surface ET using synergistic information from satellite optical IR and microwave remote sensing. C1 [Mu, Qiaozhen; Jones, Lucas A.; Running, Steven W.] Univ Montana, Numer Terradynam Simulat Grp, Coll Forestry & Conservat, Missoula, MT 59812 USA. [Kimball, John S.] Univ Montana, Flathead Lake Biol Stn, Polson, MT 59860 USA. [McDonald, Kyle C.] CALTECH, Jet Prop Lab, NASA, Pasadena, CA 91109 USA. RP Mu, QZ (reprint author), Univ Montana, Numer Terradynam Simulat Grp, Coll Forestry & Conservat, Missoula, MT 59812 USA. RI Mu, Qiaozhen/G-5695-2010 FU NASA FX We gratefully thank Maosheng Zhao for providing and processing GMAO data and useful comments on this paper. This work was supported by grants from the Terrestrial Hydrology Program of NASA's Earth Science Enterprise and National Science Foundation's Office of Polar Programs. Portions of the research described in this paper were carried out at the Jet Propulsion Laboratory, California Institute of Technology, under contract to NASA. We thank the principal investigators and research teams of Ameriflux, BERMS, and FLUXNET Canada for providing tower-based meteorological data for use in this study; tower site principal investigators include Steve Wofsy and Allison Dunn (OBS site), T. Andy Black and Alan Barr (OAS site), Lawrence Flanagan (LTH site), and Yoshinobu Harazono of the National Institute for Agro-Environmental Sciences, Tsukuba, Japan (BRW2 site), and Walter C. Oechel (BRW1 site). NR 95 TC 30 Z9 30 U1 0 U2 21 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0043-1397 EI 1944-7973 J9 WATER RESOUR RES JI Water Resour. Res. PD SEP 29 PY 2009 VL 45 AR W09420 DI 10.1029/2008WR007189 PG 20 WC Environmental Sciences; Limnology; Water Resources SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Water Resources GA 502NF UT WOS:000270466500001 ER PT J AU Silan, JL Niemann, DL Ribaya, BP Rahman, M Meyyappan, M Nguyen, CV AF Silan, Jeremy L. Niemann, Darrell L. Ribaya, Bryan P. Rahman, Mahmud Meyyappan, M. Nguyen, Cattien V. TI Carbon nanotube pillar arrays for achieving high emission current densities SO APPLIED PHYSICS LETTERS LA English DT Article ID FIELD EMITTERS AB We introduce an innovative geometry carbon nanotube (CNT) field emitter array capable of achieving stable and high current densities. Arrays of toroid CNT pillars were grown directly on bulk metal alloy substrates and on patterned metal catalyst on silicon substrates. Compared to a solid CNT pillar array (CPA), this toroid CPA (tCPA) provides a larger edge area for achieving a higher stable current density of 50 mA/cm(2) at an applied dc field of less than 8 V/mu m. Electrostatic simulation data confirming the field enhancement at the inner and outer edges of the tCPA are also presented. (C) 2009 American Institute of Physics. [doi:10.1063/1.3216584] C1 [Silan, Jeremy L.; Nguyen, Cattien V.] NASA, Ames Res Ctr, ELORET Corp, Moffett Field, CA 94035 USA. [Silan, Jeremy L.; Niemann, Darrell L.; Ribaya, Bryan P.; Rahman, Mahmud] Santa Clara Univ, Electron Devices Lab, Dept Elect Engn, Santa Clara, CA 95053 USA. RP Silan, JL (reprint author), NASA, Ames Res Ctr, ELORET Corp, Moffett Field, CA 94035 USA. EM cattien.v.nguyen@nasa.gov NR 11 TC 15 Z9 15 U1 0 U2 9 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 SEP 28 PY 2009 VL 95 IS 13 AR 133111 DI 10.1063/1.3216584 PG 3 WC Physics, Applied SC Physics GA 502KL UT WOS:000270458000057 ER PT J AU Liu, XM Johnson, PV Malone, CP Young, JA Shemansky, DE Kanik, I AF Liu, Xianming Johnson, Paul V. Malone, Charles P. Young, Jason A. Shemansky, Donald E. Kanik, Isik TI Electron-impact excitation and emission cross sections of the H-2 B ' (1)Sigma(+)(u) and D (1)Pi(u) states and rotational dependence of photodissociation cross sections of the B ' (1)Sigma(+)(u) and D (1)Pi(u) continua SO JOURNAL OF PHYSICS B-ATOMIC MOLECULAR AND OPTICAL PHYSICS LA English DT Review ID HUBBLE-SPACE-TELESCOPE; QUANTUM-DEFECT THEORY; HOPKINS ULTRAVIOLET TELESCOPE; RESOLUTION LASER SPECTROSCOPY; DIFFUSE INTERSTELLAR BANDS; VIBRATIONALLY EXCITED H-2; MINIMUM 1-SIGMA-G+ STATES; 2ND DISSOCIATION LIMIT; MOLECULAR-HYDROGEN; TRANSITION MOMENTS AB Rotational and vibrational dependence of photodissociation cross sections and oscillator strengths to the continuum levels of the H-2 B' (1)Sigma(+)(u) and D (1)Pi(u) states have been examined. The electron-impact excitation, dissociation and emission cross sections of the B' (1)Sigma(+)(u) - X (1)Sigma(+)(g) and D (1)Pi(u) - X (1)Sigma(+)(g) band systems have been obtained for the first time over a wide energy range by using calculated continuum oscillator strengths along with previously published discrete transition probabilities and Lyman and Werner bands excitation functions. The present B' (1)Sigma(+)(u) photodissociation cross section from the J(i) = 0 level is in excellent agreement with that obtained by Glass-Maujean (1986 Phys. Rev. A 33 346-50). Photoexcitation from the X (1)Sigma(+)(g) (v(i) = 0) state to the D (1)Pi(u) continuum is found to be weak. The present calculation shows significant contribution of quasi-resonance, which arises from transitions to the quasi-bound levels above the dissociation limit but stabilized by the centrifugal potential. The quasi-resonance is largely responsible for the significant rotational dependence of the continuum oscillator strength of the B' (1)Sigma(+)(u) - X (1)Sigma(+)(g) (0) transition, which, in turn, leads to the noticeable temperature dependence of electron-impact excitation and emission cross sections. B' (1)Sigma(+)(u) - X (1)Sigma(+)(g) and D (1)Pi(u) - X (1)Sigma(+)(g) electron-impact excitation, emission, and dissociation cross sections, important for modelling dayglow and auroral activity in the atmospheres of the outer planets, are presented. C1 [Liu, Xianming; Johnson, Paul V.; Malone, Charles P.; Young, Jason A.; Kanik, Isik] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Malone, Charles P.] Calif State Univ Fullerton, Dept Phys, Fullerton, CA 92834 USA. [Shemansky, Donald E.] Space Environm Technol, Planetary & Space Sci Div, Pasadena, CA 91107 USA. RP Liu, XM (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM xianming@jpl.nasa.gov; paul.v.johnson@jpl.nasa.gov; isik.kanik@jpl.nasa.gov RI Malone, Charles/A-6294-2010; Johnson, Paul/D-4001-2009 OI Malone, Charles/0000-0001-8418-1539; Johnson, Paul/0000-0002-0186-8456 FU NASA's Outer Planets and Planetary Atmospheres Research programs [NASA-NNG06GH76G]; University of Colorado FX The analysis described in this paper was carried out at Jet Propulsion Laboratory (JPL), California Institute of Technology and Space Environment Technologies ( SET). We gratefully acknowledge financial support through NASA's Outer Planets and Planetary Atmospheres Research programs. XL acknowledges the support of the NASA/JPL Senior Postdoctoral Fellowship, which is administered by Oak Ridge Associated Universities through a contract with NASA. DES acknowledges the supported by the Cassini UVIS contract with the University of Colorado and NASA-NNG06GH76G issued to SET through the NASA Planetary Atmospheres Program. The authors wish to thank Professor Robert Le Roy for the LEVEL 8 and BCONT 2.2 computer programs. NR 125 TC 6 Z9 6 U1 0 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0953-4075 J9 J PHYS B-AT MOL OPT JI J. Phys. B-At. Mol. Opt. Phys. PD SEP 28 PY 2009 VL 42 IS 18 AR 185203 DI 10.1088/0953-4075/42/18/185203 PG 13 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 492AL UT WOS:000269625900014 ER PT J AU Young, JA Malone, CP Johnson, PV Liu, X Ajello, JM Kanik, I AF Young, J. A. Malone, C. P. Johnson, P. V. Liu, X. Ajello, J. M. Kanik, I. TI Dissociative excitation of NO2 by electron impact SO JOURNAL OF PHYSICS B-ATOMIC MOLECULAR AND OPTICAL PHYSICS LA English DT Article ID EMISSION CROSS-SECTION; OXYGEN-CONTAINING MOLECULES; ULTRAVIOLET EMISSION; EXTREME-ULTRAVIOLET; VACUUM-ULTRAVIOLET; NITROGEN-DIOXIDE; NITRIC-OXIDE; IONIZATION; N2O; NM AB Electron-impact-induced vacuum ultraviolet emissions are measured for NO2, a species important to discharge phenomena and ozone decomposition in the Earth's atmosphere. A calibrated spectrum for 100 eV incident electrons is presented, along with cross sections for strong emission features between 80 and 160 nm. The dominant NI (2p(3) S-4 degrees -3s P-4) emission at 120.1 nm is compared with that of N-2 and used to provide an absolute calibration for all measured cross sections. In addition, 10-300 eV excitation functions for the NI (120.1 nm) and OI (130.4 nm) emissions are presented and interpreted. Comparisons are made with similar measurements of related species, in particular N2O and NO. Of interest, it was found that, on average, the variation in the intensity of oxygen and nitrogen emissions could be reasonably explained by the difference in the number of constituent oxygen and nitrogen atoms in each target. C1 [Young, J. A.; Malone, C. P.; Johnson, P. V.; Liu, X.; Ajello, J. M.; Kanik, I.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Malone, C. P.] Calif State Univ Fullerton, Dept Phys, Fullerton, CA 92834 USA. RP Young, JA (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. RI Malone, Charles/A-6294-2010; Johnson, Paul/D-4001-2009 OI Malone, Charles/0000-0001-8418-1539; Johnson, Paul/0000-0002-0186-8456 FU National Aeronautics and Space Administration ( NASA); NASA/JPL Senior Fellowship FX This work was performed at the Jet Propulsion Laboratory (JPL), California Institute of Technology ( Caltech), under a contract with the National Aeronautics and Space Administration ( NASA). We gratefully acknowledge financial support through NASA's Outer Planets Research and Planetary Atmospheres programs. XL acknowledges the support of the NASA/JPL Senior Fellowship, which is administered by Oak Ridge Associated Universities through a contract with NASA. NR 45 TC 1 Z9 1 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0953-4075 J9 J PHYS B-AT MOL OPT JI J. Phys. B-At. Mol. Opt. Phys. PD SEP 28 PY 2009 VL 42 IS 18 AR 185201 DI 10.1088/0953-4075/42/18/185201 PG 10 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 492AL UT WOS:000269625900012 ER PT J AU Lavraud, B Borovsky, JE Genot, V Schwartz, SJ Birn, J Fazakerley, AN Dunlop, MW Taylor, MGGT Hasegawa, H Rouillard, AP Berchem, J Bogdanova, Y Constantinescu, D Dandouras, I Eastwood, JP Escoubet, CP Frey, H Jacquey, C Panov, E Pu, ZY Shen, C Shi, J Sibeck, DG Volwerk, M Wild, JA AF Lavraud, B. Borovsky, J. E. Genot, V. Schwartz, S. J. Birn, J. Fazakerley, A. N. Dunlop, M. W. Taylor, M. G. G. T. Hasegawa, H. Rouillard, A. P. Berchem, J. Bogdanova, Y. Constantinescu, D. Dandouras, I. Eastwood, J. P. Escoubet, C. P. Frey, H. Jacquey, C. Panov, E. Pu, Z. Y. Shen, C. Shi, J. Sibeck, D. G. Volwerk, M. Wild, J. A. TI Tracing solar wind plasma entry into the magnetosphere using ion-to-electron temperature ratio SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID INTERPLANETARY MAGNETIC-FIELD; KELVIN-HELMHOLTZ VORTICES; LATITUDE BOUNDARY-LAYER; KINETIC ALFVEN WAVES; DAYSIDE MAGNETOPAUSE; GEOTAIL OBSERVATIONS; EARTHS MAGNETOSPHERE; SHEET; TRANSPORT; REGION AB When the solar wind Mach number is low, typically such as in magnetic clouds, the physics of the bow shock leads to a downstream ion-to-electron temperature ratio that can be notably lower than usual. We utilize this property to trace solar wind plasma entry into the magnetosphere by use of Cluster measurements in the vicinity of the dusk magnetopause during the passage of a magnetic cloud at Earth on November 25, 2001. The ion-to-electron temperature ratio was indeed low in the magnetosheath (T(i)/T(e) similar to 3). In total, three magnetopause boundary layer intervals are encountered on that day. They all show that the low ion-to-electron temperature ratio can be preserved as the plasma enters the magnetosphere, and both with and without the observation of Kelvin-Helmholtz activity. This suggests that the ion-to-electron temperature ratio in the magnetopause boundary layer, which is usually high, is not prescribed by the heating characteristics of the plasma entry mechanism that formed these boundary layers. In the future, this property may be used to (1) further trace plasma entry into inner regions and (2) determine the preferred entry mechanisms if other theoretical, observational and simulation works can give indications on which mechanisms may alter this ratio. Citation: Lavraud, B., et al. (2009), Tracing solar wind plasma entry into the magnetosphere using ion-to-electron temperature ratio, Geophys. Res. Lett., 36, L18109, doi: 10.1029/2009GL039442. C1 [Lavraud, B.; Genot, V.; Dandouras, I.; Jacquey, C.] Univ Toulouse, Ctr Etud Spatiale Rayonnements, F-31028 Toulouse 4, France. [Berchem, J.] Univ Calif Los Angeles, IGPP, Los Angeles, CA 90095 USA. [Borovsky, J. E.; Birn, J.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA. [Bogdanova, Y.] La Trobe Univ, Dept Phys, Melbourne, Vic 3086, Australia. [Constantinescu, D.] Tech Univ Carolo Wilhelmina Braunschweig, Inst Geophys & Extraterr Phys, D-38106 Braunschweig, Germany. [Dunlop, M. W.; Rouillard, A. P.] Rutherford Appleton Lab, Didcot OX11 0QX, Oxon, England. [Eastwood, J. P.; Frey, H.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Taylor, M. G. G. T.; Escoubet, C. P.] ESA, Estec, NL-2200 AG Noordwijk, Netherlands. [Fazakerley, A. N.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. [Hasegawa, H.] JAXA, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2298510, Japan. [Panov, E.; Volwerk, M.] Space Res Inst, A-8042 Graz, Austria. [Pu, Z. Y.] Peking Univ, Sch Earth & Space Sci, Beijing 100871, Peoples R China. [Schwartz, S. J.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, London SW7 2AZ, England. [Shen, C.; Shi, J.] Chinese Acad Sci, Ctr Space Sci & Appl Res, Beijing 100080, Peoples R China. [Sibeck, D. G.] NASA, GSFC, Greenbelt, MD 20771 USA. [Wild, J. A.] Univ Lancaster, Dept Commun Syst, Lancaster LA1 4WA, England. [Lavraud, B.; Genot, V.; Dandouras, I.; Jacquey, C.] CNRS, UMR 5187, Toulouse, France. RP Lavraud, B (reprint author), Univ Toulouse, Ctr Etud Spatiale Rayonnements, 9 Ave Colonel Roche,BP 44346, F-31028 Toulouse 4, France. EM benoit.lavraud@cesr.fr RI Hasegawa, Hiroshi/A-1192-2007; Constantinescu, Ovidiu Dragos/C-4350-2012; Sibeck, David/D-4424-2012; dunlop, malcolm/F-1347-2010; Constantinescu, Dragos/A-6007-2013; OI Hasegawa, Hiroshi/0000-0002-1172-021X; Dandouras, Iannis/0000-0002-7121-1118; Frey, Harald/0000-0001-8955-3282; Wild, James/0000-0001-8025-8869 FU ISSI (Bern, Switzerland) FX The authors acknowledge the support of ISSI (Bern, Switzerland) for the organization of a combined Cluster-THEMIS study team. We are grateful for the use the AMDA/CDPP tool which allowed conditional searches of low Mach number intervals. We thank the OMNI data team for providing the solar wind data, as well as the ACE teams. NR 34 TC 15 Z9 15 U1 3 U2 7 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 SEP 25 PY 2009 VL 36 AR L18109 DI 10.1029/2009GL039442 PG 6 WC Geosciences, Multidisciplinary SC Geology GA 499OZ UT WOS:000270235200001 ER PT J AU Rawlins, MA Ye, H Yang, D Shiklomanov, A McDonald, KC AF Rawlins, M. A. Ye, H. Yang, D. Shiklomanov, A. McDonald, K. C. TI Divergence in seasonal hydrology across northern Eurasia: Emerging trends and water cycle linkages SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID RIVER DISCHARGE; ARCTIC-OCEAN; PRECIPITATION; SIBERIA; CLIMATOLOGY; PERMAFROST; IMPACTS; ALASKA; BASIN; LAND AB Discharge from large Eurasia rivers increased during the 20th century, yet much remains unknown regarding details of this increasing freshwater flux. Here, for the three largest Eurasian basins (the Ob, Yenisei, and Lena) we examine the nature of annual and seasonal discharge trends by investigating the flow changes along with those for precipitation, snow depth, and snow water equivalent. On the basis of a multiperiod trend analysis and examination of station data, we propose two characteristic regimes to explain the long-term discharge increase from these large Eurasian rivers. Over the early decades from approximately 1936 to 1965, annual precipitation correlates well with annual discharge, and positive discharge trends are concurrent with summer/fall discharge increases. The latter decades were marked by a divergence between winter/spring flows, which increased, amid summer/fall discharge declines. A comparison of cold season precipitation (CSP) and spring discharge trends across subbasins of the Ob, Yenisei, and Lena shows limited agreement with one precipitation data set but good agreement (R-2 > 0.90) when a second is used. While natural variability in the Arctic system tends to mask these emerging trends, spatial and temporal changes can generally be characterized by increased solid precipitation, primarily to the north, along with a drier hydrography during the warm season. C1 [Rawlins, M. A.; McDonald, K. C.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Ye, H.] Calif State Univ Los Angeles, Dept Geog & Urban Anal, Los Angeles, CA 90032 USA. [Yang, D.] Univ Alaska Fairbanks, Dept Civil & Environm Engn, Water & Environm Res Ctr, Fairbanks, AK 99775 USA. [Shiklomanov, A.] Univ New Hampshire, Complex Syst Res Ctr, Durham, NH 03824 USA. RP Rawlins, MA (reprint author), CALTECH, Jet Prop Lab, Mail Stop 300-233,4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM michael.rawlins@jpl.nasa.gov FU NSF [ARC-0612062, OPP-0230083]; NASA LCLUC [NNG06GE43G]; National Aeronautics and Space Administration FX The authors gratefully acknowledge support from NSF grants ARC-0612062 and OPP-0230083 and NASA LCLUC NNG06GE43G. The lead author was also supported by an appointment to the NASA Postdoctoral Program. We thank Jennifer Adam and two anonymous reviewers for their comments and suggestions which helped to improve the manuscript. We also thank Baisheng Ye for providing the reconstructed discharge data for the Lena basin. 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 63 TC 31 Z9 31 U1 0 U2 7 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 SEP 24 PY 2009 VL 114 AR D18119 DI 10.1029/2009JD011747 PG 14 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 499PE UT WOS:000270235700004 ER PT J AU Lakhina, GS Singh, SV Kakad, AP Goldstein, ML Vinas, AF Pickett, JS AF Lakhina, G. S. Singh, S. V. Kakad, A. P. Goldstein, M. L. Vinas, A. F. Pickett, J. S. TI A mechanism for electrostatic solitary structures in the Earth's magnetosheath SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID WEAK DOUBLE-LAYERS; ELECTRIC-FIELD STRUCTURES; AURORAL PLASMA PROCESSES; ACOUSTIC DOUBLE-LAYERS; PHASE-SPACE HOLES; SATELLITE-OBSERVATIONS; WAVES; SOLITONS; CLUSTER; ION AB Electrostatic solitary waves (ESWs) have been observed in the Earth's magnetosheath region by Cluster. A mechanism for the generation of these structures in terms of electron-acoustic solitons and double layers is discussed. The model simulates the magnetosheath plasma by a four-component plasma system consisting of core electrons, two counterstreaming electron beams, and one type of ions. The analysis is based on the fluid equations and the Poisson equation, and employs the Sagdeev pseudopotential techniques to investigate the solitary waves. The electric field amplitudes, the time durations, and the propagation speeds of the solitary structures predicted by the model are in good agreement with the observed electric fields, pulse widths, and speeds of the electrostatic bipolar pulses. C1 [Lakhina, G. S.; Singh, S. V.; Kakad, A. P.] Indian Inst Geomagnetism, New Panvel W 410218, Navi Mumbai, India. [Goldstein, M. L.; Vinas, A. F.] NASA, Goddard Space Flight Ctr, Geospace Phys Lab, Greenbelt, MD 20771 USA. [Pickett, J. S.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. RP Lakhina, GS (reprint author), Indian Inst Geomagnetism, Plot 5,Sector 18, New Panvel W 410218, Navi Mumbai, India. EM lakhina@iigs.iigm.res.in RI Lakhina, Gurbax /C-9295-2012; Goldstein, Melvyn/B-1724-2008; Singh, satyavir/C-8949-2012; OI Singh, satyavir/0000-0003-2758-7713; Lakhina, Gurbax /0000-0002-8956-486X FU Indian National Science Academy, New Delhi; NASA Goddard Space Flight Center [NNX07AI24G] FX G. S. L. thanks the Indian National Science Academy, New Delhi, for the support under the Senior Scientist scheme. J.S.P. acknowledges support from NASA Goddard Space Flight Center under grant NNX07AI24G. NR 53 TC 35 Z9 35 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 SEP 24 PY 2009 VL 114 AR A09212 DI 10.1029/2009JA014306 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 499PU UT WOS:000270237600002 ER PT J AU Rockstrom, J Steffen, W Noone, K Persson, A Chapin, FS Lambin, EF Lenton, TM Scheffer, M Folke, C Schellnhuber, HJ Nykvist, B de Wit, CA Hughes, T van der Leeuw, S Rodhe, H Sorlin, S Snyder, PK Costanza, R Svedin, U Falkenmark, M Karlberg, L Corell, RW Fabry, VJ Hansen, J Walker, B Liverman, D Richardson, K Crutzen, P Foley, JA AF Rockstrom, Johan Steffen, Will Noone, Kevin Persson, Asa Chapin, F. Stuart, III Lambin, Eric F. Lenton, Timothy M. Scheffer, Marten Folke, Carl Schellnhuber, Hans Joachim Nykvist, Bjorn de Wit, Cynthia A. Hughes, Terry van der Leeuw, Sander Rodhe, Henning Sorlin, Sverker Snyder, Peter K. Costanza, Robert Svedin, Uno Falkenmark, Malin Karlberg, Louise Corell, Robert W. Fabry, Victoria J. Hansen, James Walker, Brian Liverman, Diana Richardson, Katherine Crutzen, Paul Foley, Jonathan A. TI A safe operating space for humanity SO NATURE LA English DT Article ID SOCIAL-ECOLOGICAL SYSTEMS; HUMAN IMPACT; BIODIVERSITY; CLIMATE; PERSPECTIVE; RESILIENCE; CONSEQUENCES; ECOSYSTEMS; PHOSPHORUS; SHIFTS C1 [Rockstrom, Johan; Steffen, Will; Noone, Kevin; Persson, Asa; Folke, Carl; Nykvist, Bjorn; Sorlin, Sverker; Costanza, Robert; Svedin, Uno; Falkenmark, Malin; Karlberg, Louise; Walker, Brian] Stockholm Univ, Stockholm Resilience Ctr, S-10691 Stockholm, Sweden. [Rockstrom, Johan; Persson, Asa; Nykvist, Bjorn; Karlberg, Louise] Stockholm Environm Inst, S-10691 Stockholm, Sweden. [Steffen, Will] Australian Natl Univ, ANU Climate Change Inst, Canberra, ACT 0200, Australia. [Noone, Kevin; de Wit, Cynthia A.] Stockholm Univ, Dept Appl Environm Sci, S-10691 Stockholm, Sweden. [Chapin, F. Stuart, III] Univ Alaska Fairbanks, Inst Arctic Biol, Fairbanks, AK 99775 USA. [Lambin, Eric F.] Catholic Univ Louvain, Dept Geog, B-1348 Louvain, Belgium. [Lenton, Timothy M.] Univ E Anglia, Sch Environm Sci, Norwich NR4 7TJ, Norfolk, England. [Scheffer, Marten] Wageningen Univ, Aquat Ecol & Water Qual Management Grp, NL-6700 HB Wageningen, Netherlands. [Folke, Carl] Royal Swedish Acad Sci, Beijer Inst Ecol Econ, S-10405 Stockholm, Sweden. [Schellnhuber, Hans Joachim] Potsdam Inst Climate Impact Res, D-14412 Potsdam, Germany. [Schellnhuber, Hans Joachim] Univ Oxford, Tyndall Ctr, Oxford OX1 3QY, England. [Schellnhuber, Hans Joachim; Liverman, Diana] Univ Oxford, Environm Change Inst, Oxford OX1 3QY, England. [Hughes, Terry] James Cook Univ, ARC Ctr Excellence Coral Reef Studies, Townsville, Qld 4811, Australia. [van der Leeuw, Sander] Arizona State Univ, Sch Human Evolut & Social Change, Tempe, AZ 85287 USA. [Rodhe, Henning] Stockholm Univ, Dept Meteorol, S-10691 Stockholm, Sweden. [Sorlin, Sverker] Royal Inst Technol, Div Hist Sci & Technol, S-10044 Stockholm, Sweden. [Snyder, Peter K.] Univ Minnesota, Dept Soil Water & Climate, St Paul, MN 55108 USA. [Costanza, Robert] Univ Vermont, Gund Inst Ecol Econ, Burlington, VT 05405 USA. [Falkenmark, Malin] Stockholm Int Water Inst, S-11151 Stockholm, Sweden. [Corell, Robert W.] H John Heinz III Ctr Sci Econ & Environm, Washington, DC 20006 USA. [Fabry, Victoria J.] Calif State Univ San Marcos, Dept Biol Sci, San Marcos, CA 92096 USA. [Hansen, James] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Walker, Brian] Commonwealth Sci & Ind Org, Sustainable Ecosyst, Canberra, ACT 2601, Australia. [Liverman, Diana] Univ Arizona, Inst Environm, Tucson, AZ 85721 USA. [Richardson, Katherine] Fac Nat Sci, DK-2200 Copenhagen N, Denmark. [Crutzen, Paul] Max Planck Inst Chem, D-55020 Mainz, Germany. [Foley, Jonathan A.] Univ Minnesota, Inst Environm, St Paul, MN 55108 USA. RP Rockstrom, J (reprint author), Stockholm Univ, Stockholm Resilience Ctr, Kraftriket 2B, S-10691 Stockholm, Sweden. RI Steffen, Will/C-7651-2011; Walker, Brian/F-2386-2011; Schellnhuber, Hans Joachim/B-2607-2012; Scheffer, Marten/C-1852-2012; Crutzen, Paul/F-6044-2012; de Wit, Cynthia/J-8063-2012; Snyder, Peter/H-3063-2013; Hughes, Terry/L-4721-2013; Richardson, Katherine/D-7592-2014; Costanza, Robert/A-4912-2008; OI Schellnhuber, Hans Joachim/0000-0001-7453-4935; de Wit, Cynthia/0000-0001-8497-2699; Hughes, Terry/0000-0002-5257-5063; Richardson, Katherine/0000-0003-3785-2787; Costanza, Robert/0000-0001-6348-8734; Chapin III, F Stuart/0000-0002-2558-9910; Rockstrom, Johan/0000-0001-8988-2983 NR 46 TC 2082 Z9 2136 U1 267 U2 1657 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 EI 1476-4687 J9 NATURE JI Nature PD SEP 24 PY 2009 VL 461 IS 7263 BP 472 EP 475 DI 10.1038/461472a PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 497SP UT WOS:000270082900020 PM 19779433 ER PT J AU Serrador, JM Schlegel, TT Black, FO Wood, SJ AF Serrador, Jorge M. Schlegel, Todd T. Black, F. Owen Wood, Scott J. TI Vestibular effects on cerebral blood flow SO BMC NEUROSCIENCE LA English DT Article ID INNERVATING OTOLITH ORGANS; SQUIRREL-MONKEY; ORTHOSTATIC STRESS; NEURONS; STIMULATION; DYNAMICS; NUCLEUS; HUMANS; TRANSLATION; PHYSIOLOGY AB Background: Humans demonstrate a number of unique adaptations that allow for the maintenance of blood pressure and brain blood flow when upright. While several physiological systems, including cerebral autoregulation, are involved in this adaptation the unique role the vestibular system plays in helping to maintain brain blood flow is just beginning to be elucidated. In this study, we tested the hypothesis that stimulation of the vestibular system, specifically the otoliths organs, would result in changes in cerebral blood flow. Results: To test our hypothesis, we stimulated the vestibular organs of 25 healthy subjects by pitch tilt (stimulates both canals and otoliths) and by translation on a centrifuge (stimulates otoliths and not the canals) at five frequencies: 0.5, 0.25, 0.125 and 0.0625 Hz for 80 sec and 0.03125 Hz for 160 sec. Changes in cerebral flow velocity (by transcranial Doppler) and blood pressure (by Finapres) were similar during both stimuli and dependent on frequency of stimulation (P < 0.01). However, changes in cerebral blood flow were in opposition to changes in blood pressure and not fully dependent on changes in end tidal CO(2). Conclusion: The experimental results support our hypothesis and provide evidence that activation of the vestibular apparatus, specifically the otolith organs, directly affects cerebral blood flow regulation, independent of blood pressure and end tidal CO(2) changes. C1 [Serrador, Jorge M.] Harvard Univ, Beth Israel Deaconess Med Ctr, Sch Med, Boston, MA 02215 USA. [Schlegel, Todd T.; Wood, Scott J.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Black, F. Owen] Legacy Hlth Syst, Neurotol Res, Portland, OR USA. [Wood, Scott J.] Univ Space Res Assoc, Houston, TX USA. [Serrador, Jorge M.] Natl Univ Ireland Galway, Galway, Ireland. RP Serrador, JM (reprint author), Harvard Univ, Beth Israel Deaconess Med Ctr, Sch Med, Boston, MA 02215 USA. EM serrador@hms.harvard.edu; todd.t.schlegel@nasa.gov; fob@neurotology.org; scott.j.wood@nasa.gov FU National Institutes of Health Institute on Deafness & Other Communication Disorders [R03DC5545, R03DC5547, R01DC0205]; NASA [NNJ04HI13G]; Science Foundation Ireland FX The authors would like to thank Valerie Stallings and Julie Leduc for their assistance in data collection and analysis and Sarah La Rose in the creation of the illustration of anatomical connections. This work was supported by the National Institutes of Health Institute on Deafness & Other Communication Disorders grants R03DC5545 (Serrador), R03DC5547 (Wood), R01DC0205 (Black) and NASA grant NNJ04HI13G (Serrador). Dr. Serrador is the recipient of an E. T. S. Walton Visitor Award from Science Foundation Ireland. NR 26 TC 10 Z9 11 U1 1 U2 4 PU BIOMED CENTRAL LTD PI LONDON PA 236 GRAYS INN RD, FLOOR 6, LONDON WC1X 8HL, ENGLAND SN 1471-2202 J9 BMC NEUROSCI JI BMC Neurosci. PD SEP 23 PY 2009 VL 10 AR 119 DI 10.1186/1471-2202-10-119 PG 9 WC Neurosciences SC Neurosciences & Neurology GA 503SM UT WOS:000270559900001 PM 19775430 ER PT J AU Boardsen, SA Slavin, JA Anderson, BJ Korth, H Solomon, SC AF Boardsen, Scott A. Slavin, James A. Anderson, Brian J. Korth, Haje Solomon, Sean C. TI Comparison of ultra-low-frequency waves at Mercury under northward and southward IMF SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID MESSENGERS 1ST FLYBY; ULF WAVES; MAGNETOSPHERE AB Narrow-band ultra-low-frequency (ULF) waves at frequencies greater than the He(+) cyclotron frequency (f(cHe+)) were detected during MESSENGER's first two Mercury flybys. The waves were observed primarily between closest approach (CA) and the outbound magnetopause. The magnetosphere was very quiet during the first flyby (M1) and highly disturbed during the second flyby (M2); that ULF waves were observed during both flybys despite these different magnetospheric conditions is remarkable. The wave frequency structure in the boundary layer (BL) was similar between M1 and M2. Between CA and the BL, for M1 the wave frequency rose systematically from fcHe+ to the proton cyclotron frequency (f(cH+)), while during M2 two frequency bands were observed, one near the He(++) cyclotron frequency and one near f(cH+). The main difference in the waves between the two flybys, apart from their frequency structure, was their power, which was 4 to 5 times larger during M2 than during M1. Citation: Boardsen, S. A., J. A. Slavin, B. J. Anderson, H. Korth, and S. C. Solomon (2009), Comparison of ultra-low-frequency waves at Mercury under northward and southward IMF, Geophys. Res. Lett., 36, L18106, doi:10.1029/2009GL039525. C1 [Boardsen, Scott A.; Slavin, James A.] NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Greenbelt, MD 20771 USA. [Anderson, Brian J.; Korth, Haje] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Solomon, Sean C.] Carnegie Inst Washington, Dept Terr Magnetism, Washington, DC 20015 USA. [Boardsen, Scott A.] Univ Maryland, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21201 USA. RP Boardsen, SA (reprint author), NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Mail Stop 674, Greenbelt, MD 20771 USA. EM scott.a.boardsen@nasa.gov RI Anderson, Brian/I-8615-2012; Slavin, James/H-3170-2012 OI Slavin, James/0000-0002-9206-724X FU NASA Discovery Program [NAS5-97271]; Hopkins University Applied Physics Laboratory; Carnegie Institution of Washington [NASW-00002] FX The MESSENGER project is supported by the NASA Discovery Program under contracts NAS5-97271 to the Johns Hopkins University Applied Physics Laboratory and NASW-00002 to the Carnegie Institution of Washington. NR 15 TC 10 Z9 10 U1 0 U2 1 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 SEP 23 PY 2009 VL 36 AR L18106 DI 10.1029/2009GL039525 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 499OX UT WOS:000270235000002 ER PT J AU Vermote, E Ellicott, E Dubovik, O Lapyonok, T Chin, M Giglio, L Roberts, GJ AF Vermote, Eric Ellicott, Evan Dubovik, Oleg Lapyonok, Tatyana Chin, Mian Giglio, Louis Roberts, Gareth J. TI An approach to estimate global biomass burning emissions of organic and black carbon from MODIS fire radiative power SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID SATELLITE; ENERGY; ALGORITHM; AEROSOLS; TROPICS; AFRICA; IMPACT; FOREST AB Biomass burning is the main global source of fine primary carbonaceous aerosols in the form of organic carbon (OC) and black carbon (BC). We present an approach to estimate biomass burning aerosol emissions based on the measurement of radiative energy released during combustion. We make use of both Aqua and Terra MODIS observations to estimate the fire radiative energy using a simple model to parameterize the fire diurnal cycle based on the long-term ratio between Terra and Aqua MODIS FRP. The parameterization is developed using cases of frequent (up to 12 times daily) MODIS observations, geostationary data from SEVIRI, and precessing observations from TRMM VIRS. FRE-based emission coefficients for the organic and black carbon (OCBC) component of fine mode aerosols are computed from multiple regions encompassing grassland/savanna, tropical forest, and extratropical forest biomes using OCBC emission estimates derived from the MODIS fine mode aerosol product and an inverse aerosol transport model. The values of emission coefficients for OCBC retrieved were 2.7 +/- 0.3 g/MJ for grassland/savanna, 8.6 +/- 0.8 g/MJ for tropical forest, and 14.4 +/- 0.8 g/MJ for extratropical forest. The FRE monthly data are then used to estimate OCBC emissions from biomass burning on a global basis. For 2001 to 2007, our annual estimates are comparable to previously published values. According to our estimate, the OCBC emissions are the largest for 2003 (18.8 Tg), roughly 20% above average and primarily driven by wildland fires in the Lake Baikal region (Russia). C1 [Vermote, Eric; Ellicott, Evan] Univ Maryland, Dept Geog, College Pk, MD 20740 USA. [Dubovik, Oleg] Univ Sci & Technol Lille 1, Opt Atmospher Lab, F-59655 Lille, France. [Chin, Mian] NASA, Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD 20771 USA. [Lapyonok, Tatyana; Giglio, Louis] Sci Syst & Applicat Inc, Lanham, MD 20706 USA. [Lapyonok, Tatyana] NASA, Goddard Space Flight Ctr, Terr Phys Lab, Greenbelt, MD 20771 USA. [Roberts, Gareth J.] Kings Coll London, Dept Geog, London WC2R 2LS, England. RP Vermote, E (reprint author), Univ Maryland, Dept Geog, 4321 Hartwick Rd,Suite 209, College Pk, MD 20740 USA. EM eric@ltdri.org RI Vermote, Eric/K-3733-2012; Chin, Mian/J-8354-2012; Dubovik, Oleg/A-8235-2009 OI Dubovik, Oleg/0000-0003-3482-6460 NR 52 TC 60 Z9 60 U1 2 U2 18 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 SEP 23 PY 2009 VL 114 AR D18205 DI 10.1029/2008JD011188 PG 22 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 499PD UT WOS:000270235600003 ER PT J AU Houghton, RA Hall, F Goetz, SJ AF Houghton, R. A. Hall, Forrest Goetz, Scott J. TI Importance of biomass in the global carbon cycle SO JOURNAL OF GEOPHYSICAL RESEARCH-BIOGEOSCIENCES LA English DT Article ID LAND-USE CHANGE; ABOVEGROUND LIVE BIOMASS; TERM ECOLOGICAL CHANGES; ATMOSPHERIC CO2 GROWTH; FOREST INVENTORY DATA; ANNUAL NET FLUX; TROPICAL FORESTS; BRAZILIAN AMAZON; CLIMATE-CHANGE; WOODY BIOMASS AB Our knowledge of the distribution and amount of terrestrial biomass is based almost entirely on ground measurements over an extremely small, and possibly biased sample, with many regions still unmeasured. Our understanding of changes in terrestrial biomass is even more rudimentary, although changes in land use, largely tropical deforestation, are estimated to have reduced biomass, globally. At the same time, however, the global carbon balance requires that terrestrial carbon storage has increased, albeit the exact magnitude, location, and causes of this residual terrestrial sink are still not well quantified. A satellite mission capable of measuring aboveground woody biomass could help reduce these uncertainties by delivering three products. First, a global map of aboveground woody biomass density would halve the uncertainty of estimated carbon emissions from land use change. Second, an annual, global map of natural disturbances could define the unknown but potentially large proportion of the residual terrestrial sink attributable to biomass recovery from such disturbances. Third, direct measurement of changes in aboveground biomass density (without classification of land cover or carbon modeling) would indicate the magnitude and distribution of at least the largest carbon sources (from deforestation and degradation) and sinks (from woody growth). The information would increase our understanding of the carbon cycle, including better information on the magnitude, location, and mechanisms responsible for terrestrial sources and sinks of carbon. This paper lays out the accuracy, spatial resolution, and coverage required for a satellite mission that would generate these products. C1 [Houghton, R. A.; Goetz, Scott J.] Woods Hole Res Ctr, Falmouth, MA 02543 USA. [Hall, Forrest] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Houghton, RA (reprint author), Woods Hole Res Ctr, POB 296, Falmouth, MA 02543 USA. EM rhoughton@whrc.org RI Goetz, Scott/A-3393-2015 OI Goetz, Scott/0000-0002-6326-4308 FU National Aeronautics and Space Administration FX The authors are indebted to members of the DESDynI Science Study Group whose extensive discussions contributed much to this analysis. Ralph Dubayah, Steve Frolking, George Hurtt, Sassan Saatchi, and Robert Treuhaft provided helpful comments on earlier drafts. Work was supported by the National Aeronautics and Space Administration through the Terrestrial Ecology Program. NR 92 TC 121 Z9 131 U1 10 U2 78 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-8953 J9 J GEOPHYS RES-BIOGEO JI J. Geophys. Res.-Biogeosci. PD SEP 23 PY 2009 VL 114 AR G00E03 DI 10.1029/2009JG000935 PG 13 WC Environmental Sciences; Geosciences, Multidisciplinary SC Environmental Sciences & Ecology; Geology GA 499PH UT WOS:000270236100004 ER PT J AU Waugh, DW Oman, L Newman, PA Stolarski, RS Pawson, S Nielsen, JE Perlwitz, J AF Waugh, D. W. Oman, L. Newman, P. A. Stolarski, R. S. Pawson, S. Nielsen, J. E. Perlwitz, J. TI Effect of zonal asymmetries in stratospheric ozone on simulated Southern Hemisphere climate trends SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article AB Stratospheric ozone is represented in most climate models by prescribing zonal-mean fields. We examine the impact of this on Southern Hemisphere (SH) trends using a chemistry climate model (CCM): multi-decadal simulations with interactive stratospheric chemistry are compared with parallel simulations using the same model in which the zonal-mean ozone is prescribed. Prescribing zonal-mean ozone results in a warmer Antarctic stratosphere when there is a large ozone hole, with much smaller differences at other times. As a consequence, Antarctic temperature trends for 1960 to 2000 and 2000 to 2050 in the CCM are underestimated when zonal-mean ozone is prescribed. The impacts of stratospheric changes on the tropospheric circulation (i.e., summertime trends in the SH annular mode) are also underestimated. This shows that SH trends related to ozone depletion and recovery are underestimated when interactions between stratospheric ozone and climate are approximated by an imposed zonal-mean ozone field. Citation: Waugh, D. W., L. Oman, P. A. Newman, R. S. Stolarski, S. Pawson, J. E. Nielsen, and J. Perlwitz (2009), Effect of zonal asymmetries in stratospheric ozone on simulated Southern Hemisphere climate trends, Geophys. Res. Lett., 36, L18701, doi:10.1029/2009GL040419. C1 [Waugh, D. W.; Oman, L.] Johns Hopkins Univ, Dept Earth & Planetary Sci, Baltimore, MD 21218 USA. [Newman, P. A.; Stolarski, R. S.] NASA, Atmospher Chem & Dynam Branch, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Pawson, S.; Nielsen, J. E.] NASA, Global Modeling & Assimilat Off, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Perlwitz, J.] Univ Colorado, Cooperat Inst Res Environm Sci, NOAA, Boulder, CO 80309 USA. RP Waugh, DW (reprint author), Johns Hopkins Univ, Dept Earth & Planetary Sci, 320 Olin Bldg,3400 N Charles St, Baltimore, MD 21218 USA. EM waugh@jhu.edu RI Perlwitz, Judith/B-7201-2008; Newman, Paul/D-6208-2012; Oman, Luke/C-2778-2009; Stolarski, Richard/B-8499-2013; Pawson, Steven/I-1865-2014; Waugh, Darryn/K-3688-2016 OI Perlwitz, Judith/0000-0003-4061-2442; Newman, Paul/0000-0003-1139-2508; Oman, Luke/0000-0002-5487-2598; Stolarski, Richard/0000-0001-8722-4012; Pawson, Steven/0000-0003-0200-717X; Waugh, Darryn/0000-0001-7692-2798 FU NASA MAP; NSF FX This research was supported by the NASA MAP and NSF Large-scale Climate Dynamics programs. Computational resources were provided through NASA's High-End Computing program. NR 21 TC 41 Z9 42 U1 0 U2 9 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD SEP 22 PY 2009 VL 36 AR L18701 DI 10.1029/2009GL040419 PG 6 WC Geosciences, Multidisciplinary SC Geology GA 499OT UT WOS:000270234600009 ER PT J AU Murchie, SL Mustard, JF Ehlmann, BL Milliken, RE Bishop, JL McKeown, NK Dobrea, EZN Seelos, FP Buczkowski, DL Wiseman, SM Arvidson, RE Wray, JJ Swayze, G Clark, RN Marais, DJD McEwen, AS Bibring, JP AF Murchie, Scott L. Mustard, John F. Ehlmann, Bethany L. Milliken, Ralph E. Bishop, Janice L. McKeown, Nancy K. Dobrea, Eldar Z. Noe Seelos, Frank P. Buczkowski, Debra L. Wiseman, Sandra M. Arvidson, Raymond E. Wray, James J. Swayze, Gregg Clark, Roger N. Marais, David J. Des McEwen, Alfred S. Bibring, Jean-Pierre TI A synthesis of Martian aqueous mineralogy after 1 Mars year of observations from the Mars Reconnaissance Orbiter SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Review ID NORTH POLAR-REGION; MERIDIANI-PLANUM; VALLES-MARINERIS; OMEGA/MARS EXPRESS; RADIATIVE-TRANSFER; SILICATE MINERALS; LAYERED DEPOSITS; TERRA-MERIDIANI; WATER ACTIVITY; CANDOR-CHASMA AB Martian aqueous mineral deposits have been examined and characterized using data acquired during Mars Reconnaissance Orbiter's (MRO) primary science phase, including Compact Reconnaissance Imaging Spectrometer for Mars hyperspectral images covering the 0.4-3.9 mu m wavelength range, coordinated with higher-spatial resolution HiRISE and Context Imager images. MRO's new high-resolution measurements, combined with earlier data from Thermal Emission Spectrometer; Thermal Emission Imaging System; and Observatoire pour la Mineralogie, L'Eau, les Glaces et l'Activitie on Mars Express, indicate that aqueous minerals are both diverse and widespread on the Martian surface. The aqueous minerals occur in 9-10 classes of deposits characterized by distinct mineral assemblages, morphologies, and geologic settings. Phyllosilicates occur in several settings: in compositionally layered blankets hundreds of meters thick, superposed on eroded Noachian terrains; in lower layers of intracrater depositional fans; in layers with potential chlorides in sediments on intercrater plains; and as thousands of deep exposures in craters and escarpments. Carbonate-bearing rocks form a thin unit surrounding the Isidis basin. Hydrated silica occurs with hydrated sulfates in thin stratified deposits surrounding Valles Marineris. Hydrated sulfates also occur together with crystalline ferric minerals in thick, layered deposits in Terra Meridiani and in Valles Marineris and together with kaolinite in deposits that partially infill some highland craters. In this paper we describe each of the classes of deposits, review hypotheses for their origins, identify new questions posed by existing measurements, and consider their implications for ancient habitable environments. On the basis of current data, two to five classes of Noachian-aged deposits containing phyllosilicates and carbonates may have formed in aqueous environments with pH and water activities suitable for life. C1 [Murchie, Scott L.; Seelos, Frank P.; Buczkowski, Debra L.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Wiseman, Sandra M.; Arvidson, Raymond E.] Washington Univ, Dept Earth & Planetary Sci, St Louis, MO 63130 USA. [Bibring, Jean-Pierre] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Bishop, Janice L.] SETI Inst, Mountain View, CA 94043 USA. [Swayze, Gregg; Clark, Roger N.] US Geol Survey, Lakewood, CO 80225 USA. [Marais, David J. Des] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Mustard, John F.; Ehlmann, Bethany L.] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA. [McEwen, Alfred S.] Univ Paris 11, Inst Astrophys Spatiale, F-91405 Orsay, France. [McKeown, Nancy K.] Univ Calif Santa Cruz, Dept Earth & Planetary Sci, Santa Cruz, CA 95064 USA. [Milliken, Ralph E.; Dobrea, Eldar Z. Noe] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Wray, James J.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. RP Murchie, SL (reprint author), Johns Hopkins Univ, Appl Phys Lab, Johns Hopkins Rd, Laurel, MD 20723 USA. EM scott.murchie@jhuapl.edu RI Wray, James/B-8457-2008; Murchie, Scott/E-8030-2015; Seelos, Frank/C-7875-2016 OI Wray, James/0000-0001-5559-2179; Murchie, Scott/0000-0002-1616-8751; Seelos, Frank/0000-0001-9721-941X FU Jet Propulsion Laboratory [852950] FX The authors thank the CRISM, HiRISE, CTX, and MRO operations team for collecting the data that made the results in this paper possible. This work was supported by MRO funding through subcontract 852950 from the Jet Propulsion Laboratory. NR 137 TC 205 Z9 207 U1 10 U2 53 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 SEP 22 PY 2009 VL 114 AR E00D06 DI 10.1029/2009JE003342 PG 30 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 499PM UT WOS:000270236700003 ER PT J AU Kato, S AF Kato, Seiji TI Interannual Variability of the Global Radiation Budget SO JOURNAL OF CLIMATE LA English DT Article ID AVAILABLE POTENTIAL-ENERGY; 10-YEAR DATA SET; EL-NINO; TROPICAL OCEAN; SYSTEM CERES; ATMOSPHERE; CIRCULATIONS; TRANSPORTS; CLIMATE; REGIONS AB Interannual variability of the global radiation budget, regions that contribute to its variability, and what limits albedo variability are investigated using Clouds and the Earth's Radiant Energy System (CERES) data taken from March 2000 through February 2004. Area-weighted mean top-of-atmosphere (TOA) reflected shortwave, longwave, and net irradiance standard deviations computed from monthly anomalies over a 1 degrees x 1 degrees region are 9.6, 7.6, and 7.6 W m(-2), respectively. When standard deviations are computed from global monthly anomalies, they drop to 0.5, 0.4, and 0.4 W m(-2), respectively. Clouds are mostly responsible for the variation. Regions with a large standard deviation of TOA shortwave and longwave irradiance at TOA are the tropical western and central Pacific, which is caused by shifting from La Nina to El Nino during this period. However, a larger standard deviation of 300-1000-hPa thickness anomalies occurs in the polar region instead of the tropics. The correlation coefficient between atmospheric net irradiance anomalies and 300-1000-hPa thickness anomalies is negative. These indicate that temperature anomalies in the atmosphere are mostly a result of anomalies in longwave and dynamical processes that transport energy poleward, instead of albedo anomalies by clouds directly affecting temperature anomalies in the atmosphere. With simple zonal-mean thermodynamic energy equations it is demonstrated that temperature anomalies decay exponentially with time by longwave emission and by dynamical processes. As a result, the mean meridional temperature gradient is maintained. Therefore, mean meridional circulations are not greatly altered by albedo anomalies on an annual time scale, which in turn provides small interannual variability of the global mean albedo. C1 NASA, Langley Res Ctr, Climate Sci Branch, Hampton, VA 23681 USA. RP Kato, S (reprint author), NASA, Langley Res Ctr, Climate Sci Branch, Mail Stop 420, Hampton, VA 23681 USA. EM seiji.kato@nasa.gov FU NASA FX NOAAOISSTV2data andNCEP NCAR reanalysis-derived data were provided by the NOAA/OAR/ESRL PSD, Boulder, Colorado, from their Website (http://www. cdc. noaa. gov/). I thank Drs. Thomas Ackerman, Alan Betts, Norman Loeb, Ehrhard Raschke, Fred Rose, Graeme Stephens, Bruce Wielicki, Takmeng Wong, Robert Woods, and Kuan-man Xu, and one anonymous reviewer for useful comments and constructive discussions. I also thank Dr. Graeme Stephens for encouraging me to work on this subject. The work was supported by the NASA Science Mission Directorate through the CERES and NASA Energy Water Cycle Study (NEWS) projects. NR 29 TC 21 Z9 21 U1 0 U2 10 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 SEP 21 PY 2009 VL 22 IS 18 BP 4893 EP 4907 DI 10.1175/2009JCLI2795.1 PG 15 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 496ZT UT WOS:000270021000011 ER PT J AU Thureau, ND Monnier, JD Traub, WA Millan-Gabet, R Pedretti, E Berger, JP Garcia, MR Schloerb, FP Tannirkulam, AK AF Thureau, N. D. Monnier, J. D. Traub, W. A. Millan-Gabet, R. Pedretti, E. Berger, J. -P. Garcia, M. R. Schloerb, F. P. Tannirkulam, A. -K. TI Imaging the asymmetric dust shell around CI Cam with long baseline optical interferometry SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE techniques: high angular resolution; techniques: interferometric; circumstellar matter; stars: individual: CI Cam ID HERBIG AE/BE STARS; X-RAY TRANSIENT; SPECTROSCOPIC OBSERVATIONS; IOTA INTERFEROMETER; CAMELOPARDALIS; EMISSION; OUTBURST; PHOTOMETRY; J0421+560; OBJECTS AB We present the first high angular resolution observation of the B[e] star/X-ray transient object CI Cam, performed with the two-telescope Infrared Optical Telescope Array (IOTA), its upgraded three-telescope version (IOTA3T) and the Palomar Testbed Interferometer (PTI). Visibilities and closure phases were obtained using the IONIC-3 integrated optics beam combiner. CI Cam was observed in the near-infrared H and K spectral bands, wavelengths well suited to measure the size and study the geometry of the hot dust surrounding CI Cam. The analysis of the visibility data over an 8 yr period from soon after the 1998 outburst to 2006 shows that the dust visibility has not changed over the years. The visibility data show that CI Cam is elongated which confirms the disc-shape of the circumstellar environment and totally rules out the hypothesis of a spherical dust shell. Closure phase measurements show direct evidence of asymmetries in the circumstellar environment of CI Cam and we conclude that the dust surrounding CI Cam lies in an inhomogeneous disc seen at an angle. The near-infrared dust emission appears as an elliptical skewed Gaussian ring with a major axis a = 7.58 +/- 0.24 mas, an axis ratio r = 0.39 +/- 0.03 and a position angle theta = 35 degrees +/- 2 degrees. C1 [Thureau, N. D.; Pedretti, E.] Univ St Andrews, Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland. [Monnier, J. D.; Tannirkulam, A. -K.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Traub, W. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Millan-Gabet, R.] CALTECH, Michelson Sci Ctr, Pasadena, CA 91125 USA. [Berger, J. -P.] LAOG, Grenoble, France. [Garcia, M. R.] Ctr Astrophys, Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Schloerb, F. P.] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. RP Thureau, ND (reprint author), Univ St Andrews, Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland. EM nt15@st-andrews.ac.uk FU European Community's through an International Outgoing Marie-Curie [OIF - 002990]; Centre National de Recherche Scientifique (CNRS, France); Centre National d'Etudes Spatiales (CNES, France); Ohio State University; MDM consortium; MIT; NSF [AST-9605012]; Michelson Postdoctoral Fellowship; Scottish Universities Physics Association (SUPA); NASA [NAS8-03060] FX M. R. Garcia acknowledges partial support from NASA Contract NAS8-03060 to the Chandra X-ray Center. NR 45 TC 10 Z9 10 U1 0 U2 1 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 SEP 21 PY 2009 VL 398 IS 3 BP 1309 EP 1316 DI 10.1111/j.1365-2966.2009.14949.x PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 493JB UT WOS:000269731500020 ER PT J AU Barber, RJ Miller, S Dello Russo, N Mumma, MJ Tennyson, J Guio, P AF Barber, R. J. Miller, S. Dello Russo, N. Mumma, M. J. Tennyson, J. Guio, P. TI Water in the near-infrared spectrum of comet 8P/Tuttle SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE line: formation; line: identification ID ROTATIONAL-EXCITATION; VOLATILE COMPOSITION; IMPACT; RELEASE; NUCLEI; RATES AB High-resolution spectra of comet 8P/Tuttle were obtained in the frequency range 3449.0-3462.2 cm(-1) on 2008 January 3 UT using CGS4 with echelle grating on United Kingdom Infrared Telescope. In addition to observing solar pumped fluorescent lines of H(2)O, the long integration time (152 min on target) enabled eight weaker H(2)O features to be assigned, most of which had not previously been identified in cometary spectra. These transitions, which are from higher energy upper states, are similar in character to the so-called SH lines recorded in the post Deep Impact spectrum of comet Tempel 1. We have identified certain characteristics that these lines have in common, and which in addition to helping to define this new class of cometary line give some clues to the physical processes involved in their production. Finally, we derive an H(2)O rotational temperature of 62 +/- 5K and a water production rate of (1.4 +/- 0.3) x 10(28) molecules s(-1). C1 [Barber, R. J.; Miller, S.; Tennyson, J.; Guio, P.] UCL, Dept Phys & Astron, London WC1E 6BT, England. [Dello Russo, N.] Johns Hopkins Univ, Appl Phys Lab, Dept Space, Laurel, MD 20723 USA. [Mumma, M. J.] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA. RP Barber, RJ (reprint author), UCL, Dept Phys & Astron, Gower St, London WC1E 6BT, England. EM rjb@star.ucl.ac.uk RI Guio, Patrick/A-6271-2008; Tennyson, Jonathan/I-2222-2012; mumma, michael/I-2764-2013; Dello Russo, Neil/G-2727-2015 OI Guio, Patrick/0000-0002-1607-5862; Tennyson, Jonathan/0000-0002-4994-5238; Dello Russo, Neil/0000-0002-8379-7304 FU UKIRT FX We are grateful to have been granted observing time on UKIRT, and acknowledge the assistance that we have received from the directors and staff of the observatory. We also wish to acknowledge the very helpful comments of the anonymous referee, which have assisted in the development of this paper. NR 35 TC 19 Z9 19 U1 0 U2 1 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 SEP 21 PY 2009 VL 398 IS 3 BP 1593 EP 1600 DI 10.1111/j.1365-2966.2009.15239.x PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 493JB UT WOS:000269731500047 ER PT J AU Koopmans, LVE Bolton, A Treu, T Czoske, O Auger, MW Barnabe, M Vegetti, S Gavazzi, R Moustakas, LA Burles, S AF Koopmans, L. V. E. Bolton, A. Treu, T. Czoske, O. Auger, M. W. Barnabe, M. Vegetti, S. Gavazzi, R. Moustakas, L. A. Burles, S. TI THE STRUCTURE AND DYNAMICS OF MASSIVE EARLY-TYPE GALAXIES: ON HOMOLOGY, ISOTHERMALITY, AND ISOTROPY INSIDE ONE EFFECTIVE RADIUS SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE galaxies: structure; gravitational lensing ID LENS ACS SURVEY; ABSOLUTE MAGNITUDE RELATION; SUPERMASSIVE BLACK-HOLES; COLD DARK MATTER; ELLIPTIC GALAXIES; FUNDAMENTAL PLANE; SPHERICAL GALAXIES; GRAVITATIONAL LENSES; INTERNAL STRUCTURE; SAURON PROJECT AB Based on 58 SLACS strong-lens early-type galaxies (ETGs) with direct total-mass and stellar-velocity dispersion measurements, we find that inside one effective radius maassive elliptical galaxies with M(eff) greater than or similar to 3 x 10(10) M(circle dot.) are well approximated by a power-law ellipsoid, with an average logarithmic density slope of equivalent to -d log(rho(tot))/d log(r) = 2.085(-0.018)(+0.025) and sigma(gamma') less than or similar to 0.20(-0.02)(+0.04) (random error on mean) for isotropic orbits with beta(r) = 0, +/- 0.1 (syst.) intrinsic scatter (all errors indicate the 68% CL). We find no correlation of gamma'(LD) with galaxy mass (M(eff)), rescaled radius (i.e., R(einst)/R(eff)) or redshift, despite intrinsic differences in density-slope between galaxies. Based on scaling relations, the average logarithmic density slope can be derived in an alternative manner, fully independent from dynamics, yielding = 1.959 +/- 0.077. Agreement between the two values is reached for = 0.45 +/- 0.25, consistent with mild radial anisotropy. This agreement supports the robustness of our results, despite the increase in mass-to-light ratio with total galaxy mass: M(eff) proportional to L(V,eff)(1.363 +/- 0.056). We conclude that massive ETGs are structurally close to homologous with close to isothermal total density profiles (less than or similar to 10% intrinsic scatter) and have at most some mild radial anisotropy. Our results provide new observational limits on galaxy formation and evolution scenarios, covering 4 Gyr look-back time. C1 [Koopmans, L. V. E.; Czoske, O.; Barnabe, M.; Vegetti, S.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands. [Bolton, A.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Treu, T.; Auger, M. W.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Gavazzi, R.] Univ Paris 06, CNRS, UMR7095, Inst Astrophys Paris, F-75014 Paris, France. [Moustakas, L. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Burles, S.] MIT, Dept Phys, Cambridge, MA 02139 USA. [Burles, S.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. RP Koopmans, LVE (reprint author), Univ Groningen, Kapteyn Astron Inst, POB 800, NL-9700 AV Groningen, Netherlands. EM koopmans@astro.rug.nl; bolton@ifa.hawaii.edu; ttreu@physics.ucsb.edu; gavazzi@iap.fr; leonidas@jpl.nasa.gov; burles@mit.edu OI Moustakas, Leonidas/0000-0003-3030-2360 FU NSF; NASA [10174, 10587, 10886, 10494, 10798, 11202] FX L. K. is supported through an NWO-VIDI program subsidy. T. T. acknowledges support from the NSF through CAREER award, by the Sloan and Packard Foundations. The work of LAM was carried out at JPL/Caltech, under a contract with NASA. Support for HST programs 10174, 10587, 10886, 10494, 10798, and 11202 was provided by NASA through a grant from the STScI. NR 46 TC 150 Z9 150 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD SEP 20 PY 2009 VL 703 IS 1 BP L51 EP L54 DI 10.1088/0004-637X/703/1/L51 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 492AQ UT WOS:000269626600012 ER PT J AU Burke, WJ de la Beaujardiere, O Gentile, LC Hunton, DE Pfaff, RF Roddy, PA Su, YJ Wilson, GR AF Burke, W. J. de la Beaujardiere, O. Gentile, L. C. Hunton, D. E. Pfaff, R. F. Roddy, P. A. Su, Y. -J. Wilson, G. R. TI C/NOFS observations of plasma density and electric field irregularities at post-midnight local times SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID EQUATORIAL IONOSPHERE; DISTURBANCE DYNAMO; STORM; BUBBLES AB We report on plasma densities and electric fields measured by the C/NOFS satellite between 10 and 20 June 2008. Midway through the interval, geomagnetic conditions changed from quiescent to disturbed as a high speed stream (HSS) in the solar wind passed Earth. During the HSS passage C/NOFS encountered post-midnight irregularities that ranged from strong equatorial plasma bubbles to longitudinally broad depletions. At the leading edge of the HSS the interplanetary magnetic field rapidly intensified and rotated causing auroral electrojet currents to rise and fall within a few hours. As the electrojet relaxed, C/NOFS witnessed a rapid transition from a weakly to a strongly disturbed equatorial ionosphere that lasted similar to 10 hours. Eastward polarization electric fields intensified within locally depleted flux tubes. We discuss relative contributions of gravity-driven currents, overshielding electric fields and disturbance dynamos as drivers of post-midnight depletions. Citation: Burke, W.J., O. de La Beaujardiere, L. C. Gentile, D. E. Hunton, R. F. Pfaff, P. A. Roddy, Y.- J. Su, and G. R. Wilson (2009), C/NOFS observations of plasma density and electric field irregularities at post-midnight local times, Geophys. Res. Lett., 36, L00C09, doi: 10.1029/2009GL038879. C1 [Burke, W. J.; de la Beaujardiere, O.; Gentile, L. C.; Hunton, D. E.; Roddy, P. A.; Su, Y. -J.; Wilson, G. R.] USAF, Res Lab, Space Vehicles Directorate, Hanscom AFB, MA 01731 USA. [Pfaff, R. F.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Burke, WJ (reprint author), USAF, Res Lab, Space Vehicles Directorate, 29 Randolph Rd, Hanscom AFB, MA 01731 USA. EM afrl.rvb.pa@hanscom.af.mil RI Pfaff, Robert/F-5703-2012 OI Pfaff, Robert/0000-0002-4881-9715 FU Air Force Research Laboratory; Department of Defense Space Test Program; National Aeronautics and Space Administration; Naval Research Laboratory; Aerospace Corporation; Air Force Office of Scientific Research Task [2301SDA5]; Air Force [FA8718-08-C-0012] FX The C/NOFS mission is supported by the Air Force Research Laboratory, the Department of Defense Space Test Program, the National Aeronautics and Space Administration, the Naval Research Laboratory, and the Aerospace Corporation. This analysis was supported by Air Force Office of Scientific Research Task 2301SDA5 and Air Force contract FA8718-08-C-0012 with Boston College. NR 20 TC 34 Z9 35 U1 0 U2 3 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 SEP 19 PY 2009 VL 36 AR L00C09 DI 10.1029/2009GL038879 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 497JM UT WOS:000270055300001 ER PT J AU Ray, RD Luthcke, SB Boy, JP AF Ray, R. D. Luthcke, S. B. Boy, J. -P. TI Qualitative comparisons of global ocean tide models by analysis of intersatellite ranging data SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS LA English DT Article ID GRACE; EARTH; ASSIMILATION; GRAVIMETRY; ALTIMETRY; TRACKING; SURFACE; SYSTEM AB Four global ocean tide models are compared in terms of their contribution to Gravity Recovery and Climate Experiment (GRACE) satellite-to-satellite tracking residuals. The residuals are computed relative to a comprehensive model of Earth's time-varying gravity, including allowance for mass motions in the atmosphere, ocean, terrestrial hydrology, and mantle, in addition to tides. For each analyzed tide model, 4 years of GRACE range rate data are processed. Range and range acceleration residuals are tidally analyzed by geographic location. All four global tide models are shown to be error prone in various ways, leaving tidally coherent residuals especially in polar regions but also in some lower-latitude regions. Considerable power in the solar semidiurnal S-2 tide in low latitudes suggests errors in our adopted model of atmospheric tides, which is based on 3 hourly European Centre for Medium-Range Weather Forecasts operational analyses. Anomalies in the mu(2) tidal constituent over some shallow seas suggest the presence of unmodeled nonlinear compound tides, in this case 2MS(2). Similarly, anomalies in the nonlinear M-4 tide are seen if this constituent is omitted from the models. Errors in assumed seawater density may be contributing to some residuals. C1 [Ray, R. D.; Luthcke, S. B.; Boy, J. -P.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Boy, J. -P.] IPGS, EOST, Strasbourg, France. RP Ray, RD (reprint author), NASA, Goddard Space Flight Ctr, Mail Code 698, Greenbelt, MD 20771 USA. EM richard.ray@nasa.gov RI Ray, Richard/D-1034-2012; Luthcke, Scott/D-6283-2012; Boy, Jean-Paul/E-6677-2017 OI Boy, Jean-Paul/0000-0003-0259-209X FU National Aeronautics and Space Administration's GRACE project FX We thank D. Rowlands and S. Bettadpur for useful discussions. This work was supported by the National Aeronautics and Space Administration's GRACE project. NR 47 TC 16 Z9 16 U1 0 U2 4 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9275 J9 J GEOPHYS RES-OCEANS JI J. Geophys. Res.-Oceans PD SEP 18 PY 2009 VL 114 AR C09017 DI 10.1029/2009JC005362 PG 11 WC Oceanography SC Oceanography GA 497KE UT WOS:000270057300005 ER PT J AU Bland, PA Spurny, P Towner, MC Bevan, AWR Singleton, AT Bottke, WF Greenwood, RC Chesley, SR Shrbeny, L Borovicka, J Ceplecha, Z McClafferty, TP Vaughan, D Benedix, GK Deacon, G Howard, KT Franchi, IA Hough, RM AF Bland, Philip A. Spurny, Pavel Towner, Martin C. Bevan, Alex W. R. Singleton, Andrew T. Bottke, William F., Jr. Greenwood, Richard C. Chesley, Steven R. Shrbeny, Lukas Borovicka, Jiri Ceplecha, Zdenek McClafferty, Terence P. Vaughan, David Benedix, Gretchen K. Deacon, Geoff Howard, Kieren T. Franchi, Ian A. Hough, Robert M. TI An Anomalous Basaltic Meteorite from the Innermost Main Belt SO SCIENCE LA English DT Article ID IRON-METEORITES; PARENT BODY; ASTEROIDS; VESTA; ACHONDRITE; CHONDRITES; REGION; ORIGIN; BODIES; SYSTEM AB Triangulated observations of fireballs allow us to determine orbits and fall positions for meteorites. The great majority of basaltic meteorites are derived from the asteroid 4 Vesta. We report on a recent fall that has orbital properties and an oxygen isotope composition that suggest a distinct parent body. Although its orbit was almost entirely contained within Earth's orbit, modeling indicates that it originated from the innermost main belt. Because the meteorite parent body would likely be classified as a V-type asteroid, V-type precursors for basaltic meteorites unrelated to Vesta may reside in the inner main belt. This starting location is in agreement with predictions of a planetesimal evolution model that postulates the formation of differentiated asteroids in the terrestrial planet region, with surviving fragments concentrated in the innermost main belt. C1 [Bland, Philip A.; Towner, Martin C.; Shrbeny, Lukas] Univ London Imperial Coll Sci Technol & Med, Dept Earth Sci & Engn, IARC, London SW7 2AZ, England. [Spurny, Pavel; Shrbeny, Lukas; Borovicka, Jiri; Ceplecha, Zdenek] Acad Sci Czech Republic, Astron Inst, CZ-25165 Ondrejov, Czech Republic. [Bevan, Alex W. R.; Deacon, Geoff] Western Australian Museum, Dept Earth & Planetary Sci, Welshpool Dc, WA 6986, Australia. [Singleton, Andrew T.] Univ London Imperial Coll Sci Technol & Med, Dept Phys, Space & Atmospher Phys Grp, London SW7 2AZ, England. [Bottke, William F., Jr.] SW Res Inst, Boulder, CO 80302 USA. [Greenwood, Richard C.; Franchi, Ian A.] Open Univ, PSSRI, Milton Keynes MK7 6AA, Bucks, England. [Chesley, Steven R.] CALTECH, Jet Prop Lab, Solar Syst Dynam Grp, Pasadena, CA 91109 USA. [McClafferty, Terence P.] Curtin Univ Technol, Off Res & Dev, Perth, WA 6845, Australia. [Benedix, Gretchen K.; Howard, Kieren T.] Nat Hist Museum, Dept Mineral, IARC, London SW7 5BD, England. [Hough, Robert M.] ARRC, CRCLEME, CSIRO Explorat & Min, Perth, WA 6151, Australia. RP Bland, PA (reprint author), Univ London Imperial Coll Sci Technol & Med, Dept Earth Sci & Engn, IARC, London SW7 2AZ, England. EM p.a.bland@imperial.ac.uk RI Borovicka, Jiri/F-4257-2014; Shrbeny, Lukas/G-9040-2014; Spurny, Pavel/G-9044-2014; OI Benedix, Gretchen/0000-0003-0990-8878 FU UK Science and Technology Facilities Council [PP/C502406/1, ST/F003072/1]; Czech Science Foundation [205/08/0411]; EU [MRTN-CT-2006-035519]; Czech Academy of Sciences [AV0Z10030501]; Western Australian Museum FX Supported by UK Science and Technology Facilities Council grants PP/C502406/1 and ST/F003072/1; grant 205/08/0411 of the Czech Science Foundation; and EU grant MRTN-CT-2006-035519. P. S. thanks the Czech Academy of Sciences for support through institutional research project AV0Z10030501. We also thank the people of the Nullarbor, and M. Cupak, M. Halik, J. Ullrich, A. Forte, M. Creasy, L. Beazley, T. Smith, C. Daw, T. Kennedy, G. Kennedy, W. Moore, T. Davies, and the trustees of the Western Australian Museum for their help and support over the course of this project, and Australia Post for in-kind sponsorship. NR 23 TC 48 Z9 48 U1 0 U2 5 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 SEP 18 PY 2009 VL 325 IS 5947 BP 1525 EP 1527 DI 10.1126/science.1174787 PG 3 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 495JS UT WOS:000269887900034 PM 19762639 ER PT J AU Yorks, JE McGill, M Rodier, S Vaughan, M Hu, YX Hlavka, D AF Yorks, John E. McGill, Matt Rodier, Sharon Vaughan, Mark Hu, Yongxiang Hlavka, Dennis TI Radiative effects of African dust and smoke observed from Clouds and the Earth's Radiant Energy System (CERES) and Cloud-Aerosol Lidar with Orthogonal Polarization (CALIOP) data SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID ANGULAR-DISTRIBUTION MODELS; TERRA SATELLITE; FLUX ESTIMATION; FIELD CAMPAIGN; SAFARI 2000; ATMOSPHERE; CALIPSO; TOP; EXTINCTION; INSTRUMENT AB Cloud and aerosol effects have a significant impact on the atmospheric radiation budget in the tropical Atlantic because of the spatial and temporal extent of desert dust and smoke from biomass burning in the atmosphere. The influences of African dust and smoke aerosols on cloud radiative properties over the tropical Atlantic Ocean were analyzed for the month of July for 3 years (2006-2008) using colocated data collected by the Cloud-Aerosol Lidar with Orthogonal Polarization (CALIOP) and Clouds and the Earth's Radiant Energy System (CERES) instruments on the Cloud-Aerosol Lidar and Infrared Pathfinder Satellite Observations (CALIPSO) and Aqua satellites. Aerosol layer height and type can be accurately determined using CALIOP data through directly measured parameters such as optical depth, volume depolarization ratio, attenuated backscatter, and color ratio. On average, clouds below 5 km had a daytime instantaneous shortwave (SW) radiative flux of 270.2 +/- 16.9 W/m(2) and thin cirrus clouds had a SW radiative flux of 208.0 +/- 12.7 W/m(2). When dust aerosols interacted with clouds below 5 km, as determined from CALIPSO, the SW radiative flux decreased to 205.4 +/- 13.0 W/m(2). Similarly, smoke aerosols decreased the SW radiative flux of low clouds to a value of 240.0 +/- 16.6 W/m(2). These decreases in SW radiative flux were likely attributed to the aerosol layer height and changes in cloud microphysics. CALIOP lidar observations, which more accurately identify aerosol layer height than passive instruments, appear essential for better understanding of cloud-aerosol interactions, a major uncertainty in predicting the climate system. C1 [Yorks, John E.; Rodier, Sharon; Hlavka, Dennis] Sci Syst & Applicat Inc, Lanham, MD USA. [McGill, Matt] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Vaughan, Mark; Hu, Yongxiang] NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Yorks, JE (reprint author), Sci Syst & Applicat Inc, Lanham, MD USA. EM john.e.yorks@nasa.gov RI McGill, Matthew/D-8176-2012; Hu, Yongxiang/K-4426-2012; OI Hlavka, Dennis/0000-0002-2976-7243 FU NASA FX NASA's Radiation Sciences Program funded this study. Special thanks go to all the members of the CALIPSO and CERES science team for making the instrument data available and providing insight on retrieval uncertainties. NR 40 TC 9 Z9 9 U1 1 U2 4 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD SEP 17 PY 2009 VL 114 AR D00H04 DI 10.1029/2009JD012000 PG 10 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 497JU UT WOS:000270056200003 ER PT J AU Gibson, SE Kozyra, JU de Toma, G Emery, BA Onsager, T Thompson, BJ AF Gibson, S. E. Kozyra, J. U. de Toma, G. Emery, B. A. Onsager, T. Thompson, B. J. TI If the Sun is so quiet, why is the Earth ringing? A comparison of two solar minimum intervals SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID CORONAL HOLES; GEOMAGNETIC STORMS; MAGNETIC-FIELD; WIND; CYCLES; MAGNETOSPHERE; ACCELERATION; STREAMS AB Observations from the recent Whole Heliosphere Interval (WHI) solar minimum campaign are compared to last cycle's Whole Sun Month (WSM) to demonstrate that sunspot numbers, while providing a good measure of solar activity, do not provide sufficient information to gauge solar and heliospheric magnetic complexity and its effect at the Earth. The present solar minimum is exceptionally quiet, with sunspot numbers at their lowest in 75 years and solar wind magnetic field strength lower than ever observed. Despite, or perhaps because of, a global weakness in the heliospheric magnetic field, large near-equatorial coronal holes lingered even as the sunspots disappeared. Consequently, for the months surrounding the WHI campaign, strong, long, and recurring high-speed streams in the solar wind intercepted the Earth in contrast to the weaker and more sporadic streams that occurred around the time of last cycle's WSM campaign. In response, geospace and upper atmospheric parameters continued to ring with the periodicities of the solar wind in a manner that was absent last cycle minimum, and the flux of relativistic electrons in the Earth's outer radiation belt was elevated to levels more than three times higher in WHI than in WSM. Such behavior could not have been predicted using sunspot numbers alone, indicating the importance of considering variation within and between solar minima in analyzing and predicting space weather responses at the Earth during solar quiet intervals, as well as in interpreting the Sun's past behavior as preserved in geological and historical records. C1 [Gibson, S. E.; de Toma, G.; Emery, B. A.] Natl Ctr Atmospher Res, High Altitude Observ, Boulder, CO 80307 USA. [Kozyra, J. U.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. [Onsager, T.] NOAA, Space Weather Predict Ctr, Boulder, CO 80305 USA. [Thompson, B. J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Gibson, SE (reprint author), Natl Ctr Atmospher Res, High Altitude Observ, POB 3000, Boulder, CO 80307 USA. EM sgibson@ucar.edu RI Thompson, Barbara/C-9429-2012 FU NASA-LWS [NNH05AA49I]; NASALWS [NNH05AB54I]; NASASRT [NNG05GM48G, NNX08AQ15G, NNX08AV83G]; NSF FX The Whole Heliosphere Interval (WHI) is coordinated under the auspices of the International Heliophysical Year, and we acknowledge David Webb's leadership role in WHI. We also thank the participants of the WHI Data and Modeling Assessment Workshop (August 2008, Boulder, Colorado) for working group discussions and P. Riley for showing us early model results for WHI that helped frame our understanding of the system. OMNI solar wind and IMF data include Wind and ACE satellite data time-shifted to the Earth's magnetosphere. The intercalibrated NOAA and DMSP auroral electron powers are from the CEDAR Database, which is supported by the NSF. SOHO is a project of international collaboration between ESA and NASA. G.d.T.'s work was supported by NASA-LWS grant NNH05AA49I, B.A.E.'s work was supported by NASALWS grant NNH05AB54I, and J.U.K.' s work was supported by NASASRT grants NNG05GM48G, NNX08AQ15G, and NNX08AV83G. NCAR is sponsored by the NSF. NR 42 TC 84 Z9 86 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 SEP 17 PY 2009 VL 114 AR A09105 DI 10.1029/2009JA014342 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 497KT UT WOS:000270058800002 ER PT J AU Keika, K Nakamura, R Baumjohann, W Angelopoulos, V Kabin, K Glassmeier, KH Sibeck, DG Magnes, W Auster, HU Fornacon, KH McFadden, JP Carlson, CW Lucek, EA Carr, CM Dandouras, I Rankin, R AF Keika, K. Nakamura, R. Baumjohann, W. Angelopoulos, V. Kabin, K. Glassmeier, K. H. Sibeck, D. G. Magnes, W. Auster, H. U. Fornacon, K. H. McFadden, J. P. Carlson, C. W. Lucek, E. A. Carr, C. M. Dandouras, I. Rankin, R. TI Deformation and evolution of solar wind discontinuities through their interactions with the Earth's bow shock SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID INTERPLANETARY TANGENTIAL DISCONTINUITIES; SPACECRAFT; MAGNETOSPHERE; PERFORMANCE; INSTRUMENT; NORMALS; PLASMA; SHAPE AB The present study examines the interaction of solar wind discontinuities with the Earth's bow shock, using multipoint observations in the magnetosheath by Time History of Events and Macroscale Interactions During Substorms (THEMIS), Cluster, and Double Star TC1. We focus on the deformation and evolution of two discontinuities observed on 21 June 2007, one of which involves a density increase and a magnetic field decrease, while the other is accompanied by a density decrease and a magnetic field increase. In the magnetosheath, the discontinuities are deformed into a concave shape; that is, the normal is inclined toward dusk (dawn) on the dawnside (duskside). The density-increase (-decrease) discontinuity is being compressed (expanded) as it propagates in the magnetosheath. We conclude that the compression (expansion) is due to antisunward (sunward) motion of the bow shock which is initiated or enhanced by the impact of the discontinuity on the bow shock. The steepening of B-z reversal followed by an overshoot of the total magnetic field, which appears at the trailing edge of the density-decrease discontinuity, is also discussed. C1 [Keika, K.; Nakamura, R.; Baumjohann, W.; Magnes, W.] Austrian Acad Sci, Space Res Inst, A-8042 Graz, Austria. [Angelopoulos, V.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90095 USA. [Glassmeier, K. H.; Auster, H. U.; Fornacon, K. H.] Tech Univ Carolo Wilhelmina Braunschweig, Inst Geophys & Extraterr Phys, D-38106 Braunschweig, Germany. [McFadden, J. P.; Carlson, C. W.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Lucek, E. A.; Carr, C. M.] Univ London Imperial Coll Sci Technol & Med, Space & Atmospher Phys Grp, London SW7 2AZ, England. [Dandouras, I.] Univ Toulouse 3, Ctr Etud Spatiale Rayonnements, CNRS, UMR 5187, F-31028 Toulouse 4, France. [Kabin, K.; Rankin, R.] Univ Alberta, Dept Phys, Edmonton, AB T6G 2J1, Canada. [Sibeck, D. G.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Keika, K.] New Jersey Inst Technol, Ctr Solar Terr Res, Newark, NJ 07102 USA. [Glassmeier, K. H.] Max Planck Inst Solar Syst Res, Katlenburg Lindau, Germany. RP Keika, K (reprint author), Austrian Acad Sci, Space Res Inst, Schmiedlstr 6, A-8042 Graz, Austria. EM kunihiro.keika@oeaw.ac.at RI Sibeck, David/D-4424-2012; Baumjohann, Wolfgang/A-1012-2010; Rankin, Robert/C-5435-2013; Nakamura, Rumi/I-7712-2013; OI Baumjohann, Wolfgang/0000-0001-6271-0110; Rankin, Robert/0000-0003-0151-6343; Nakamura, Rumi/0000-0002-2620-9211; Dandouras, Iannis/0000-0002-7121-1118 FU NASA [NAS5-02099]; German Ministerium fur Wirtschaft und Technologie; German Zentrum fur Luft- und Raumfahrt [50QP0402]; Canadian Space Agency FX Wind and ACE data are provided by Coordinated Data Analysis Web (CDAWeb), NASA. We are grateful to H. Eichelberger and G. Laky for helping with the Cluster and Double Star data analysis. We thank A. Retino for his helpful comments. THEMIS was made possible and is supported in the United States by NASA NAS5-02099. The work of the IGEP team at the Technical University of Braunschweig was financially supported by the German Ministerium fur Wirtschaft und Technologie and the German Zentrum fur Luft- und Raumfahrt under grant 50QP0402. K. Kabin and R. Rankin are supported by the Canadian Space Agency. Figures 14 and 15 are drawn by Mayuko Keika. NR 43 TC 9 Z9 9 U1 0 U2 2 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD SEP 17 PY 2009 VL 114 AR A00C26 DI 10.1029/2008JA013481 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 497KT UT WOS:000270058800001 ER PT J AU Keihm, S Brown, S Teixeira, J Desai, S Lu, W Fetzer, E Ruf, C Huang, XL Yung, Y AF Keihm, S. Brown, S. Teixeira, J. Desai, S. Lu, W. Fetzer, E. Ruf, C. Huang, X. L. Yung, Y. TI Ocean water vapor and cloud liquid water trends from 1992 to 2005 TOPEX Microwave Radiometer data SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID 1D+4D-VAR ASSIMILATION; INSTRUMENT DESCRIPTION; CORRECTION ALGORITHM; ATMOSPHERIC WATER; CLIMATE; CALIBRATION; PERFORMANCE; RADIANCES; SEASAT; TMR AB The continuous 1992-2005 data set of the TOPEX Microwave Radiometer (TMR) has been reprocessed to provide global, zonal, and regional scale histories of overocean integrated water vapor (IWV) and cloud liquid water (CLW). Results indicate well-defined trends in IWV on global and hemisphere scales, with values of 1.8 +/- 0.4%/decade (60 degrees S-60 degrees N), 2.4 +/- 0.4%/decade (0-60 degrees N), and 1.0 +/- 0.5%/decade (0-60 degrees S). The uncertainties represent 1 standard deviation of the regressed slope parameter adjusted for lag 1 autocorrelation. These results are comparable to earlier results based on analyses of the multiinstrument SSM/I ocean measurements beginning in 1988. For the 1992-2005 interval, comparisons between SSM/I- and TMR-derived IWV trends show remarkable agreement, with global trends differing by less than 0.3%/decade, comparable to the statistical uncertainty level and about one-sixth of the global TMR-derived trend. Latitudinal and regional analyses of IWV trends show large variability about the global mean, with synoptic scale variations of IWV trends ranging from similar to-8 to +8%/decade. Averaged over 5 degrees latitude bands the IWV trends reveal a near zero minimum in the Southern Tropical Pacific and maximum values of similar to 4%/decade over the 30-40N latitude band. Comparisons with band latitude averaged SST data over the same 1992-2005 interval roughly match a delta_IWV/delta_SST trend scaling of similar to 11%/K, consistent with previously observed tropical and midlatitude seasonal variability. TMR-derived CLW trends are fractionally comparable to the IWV trends. The CLW values are 1.5 +/- 0.6%/decade (60 degrees S-60 degrees N), 2.0 +/- 0.8%/decade (0-60 degrees N), and 1.1 +/- 0.8%/decade (0-60 degrees S). When scaled to global mean CLW derived from SSM/I and compared seasonally, the TMR CLW variations exhibit excellent tracking with the SSM/I results. Unlike IWV, however, the CLW statistical uncertainties do not likely reflect the dominant error component in the retrieved trends. The 1992-2005 CLW trend estimates were particularly sensitive to short-term trends in the first and last 2 years of the TMR archive. Additional errors difficult to quantify include strong aliasing effects from precipitation cells and uncertainties in the radiative transfer models utilized in the generation of the TMR CLW algorithm. C1 [Keihm, S.; Brown, S.; Teixeira, J.; Desai, S.; Lu, W.; Fetzer, E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Ruf, C.; Huang, X. L.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. [Yung, Y.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. RP Keihm, S (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM stephen.j.keihm@jpl.nasa.gov RI Huang, Xianglei/G-6127-2011; Ruf, Christopher/I-9463-2012 OI Huang, Xianglei/0000-0002-7129-614X; NR 44 TC 2 Z9 2 U1 0 U2 3 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD SEP 16 PY 2009 VL 114 AR D18101 DI 10.1029/2009JD012145 PG 18 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 497JS UT WOS:000270056000003 ER PT J AU Murchie, S Roach, L Seelos, F Milliken, R Mustard, J Arvidson, R Wiseman, S Lichtenberg, K Andrews-Hanna, J Bishop, J Bibring, JP Parente, M Morris, R AF Murchie, Scott Roach, Leah Seelos, Frank Milliken, Ralph Mustard, John Arvidson, Raymond Wiseman, Sandra Lichtenberg, Kimberly Andrews-Hanna, Jeffrey Bishop, Janice Bibring, Jean-Pierre Parente, Mario Morris, Richard TI Evidence for the origin of layered deposits in Candor Chasma, Mars, from mineral composition and hydrologic modeling SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID PALEO-FLUID FLOW; MERIDIANI-PLANUM; VALLES-MARINERIS; REFLECTANCE SPECTROSCOPY; TERRA-MERIDIANI; HISTORY; REGION; DIVERSITY; SULFATES; HEMATITE AB New results from the Compact Reconnaissance Imaging Spectrometer for Mars and High Resolution Imaging Science Experiment and Context Imager cameras on Mars Reconnaissance Orbiter provide insights into the origin of interior layered deposits in Valles Marineris from analysis of a thick, well-exposed section in western Candor Chasma. Most of the deposit is dominated spectrally by nanophase ferric oxide like that found in the globally distributed eolian dust, with the addition of a prevalent component of monohydrated sulfates. A rippled mantle containing both pyroxene and monohydrated sulfate emanates from discrete layers, which are interpreted as interbedded basaltic sand. Ferric minerals are observed in most of the sulfate-rich layers, and locally a coarse-grained grayer component has been concentrated from the layers by sorting. Polyhydrated sulfates are concentrated in discrete layers high in the section, implying chasma-scale changes in brine chemistry during formation of the layered deposits. Hydrological models were constructed in order to assess whether evaporite deposition from groundwater discharge could have trapped eolian sediments to form the observed deposits. The predicted thickness and extent of the evaporite-trapped sediment is consistent with the distribution of interior layered deposits in Candor Chasma as well as in other chasmata of Valles Marineris. In this scenario, eolian dust and sand were trapped and lithified by evaporites formed by evaporation of groundwater discharge that was highly localized within the chasmata. Sulfates precipitated in the resulting saline conditions, and diagenetic alteration formed crystalline ferric minerals including hematite. This model links the layered deposits in Valles Marineris and those in Meridiani Planum to a common regional process. C1 [Murchie, Scott; Seelos, Frank] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Roach, Leah; Mustard, John] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA. [Milliken, Ralph] CALTECH, Jet Prop Lab, NASA, Pasadena, CA 91109 USA. [Andrews-Hanna, Jeffrey] Colorado Sch Mines, Dept Geophys, Golden, CO 80401 USA. [Arvidson, Raymond; Wiseman, Sandra; Lichtenberg, Kimberly] Washington Univ, Dept Earth & Planetary Sci, St Louis, MO 63130 USA. [Bibring, Jean-Pierre] Inst Astrophys Spatiale, F-91405 Orsay, France. [Bishop, Janice] SETI Inst, Mountain View, CA 94043 USA. [Morris, Richard] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Parente, Mario] Stanford Univ, Dept Elect Engn, Stanford, CA 94305 USA. [Bishop, Janice] NASA, Ames Res Ctr, Mountain View, CA USA. RP Murchie, S (reprint author), Johns Hopkins Univ, Appl Phys Lab, Johns Hopkins Rd, Laurel, MD 20723 USA. EM scott.murchie@jhuapl.edu RI Murchie, Scott/E-8030-2015; Seelos, Frank/C-7875-2016 OI Murchie, Scott/0000-0002-1616-8751; Seelos, Frank/0000-0001-9721-941X FU MRO [852950] FX The authors thank the CRISM, HiRISE, CTX, and MRO operations team for collecting the data that made the results in this paper possible. This work was supported by MRO funding through subcontract 852950 from the Jet Propulsion Laboratory. NR 65 TC 91 Z9 92 U1 0 U2 7 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9097 EI 2169-9100 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD SEP 16 PY 2009 VL 114 AR E00D05 DI 10.1029/2009JE003343 PG 15 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 497KH UT WOS:000270057600001 ER PT J AU Breech, B Matthaeus, WH Cranmer, SR Kasper, JC Oughton, S AF Breech, B. Matthaeus, W. H. Cranmer, S. R. Kasper, J. C. Oughton, S. TI Electron and proton heating by solar wind turbulence SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID INTERSTELLAR PICKUP PROTONS; ALFVENIC TURBULENCE; ULYSSES OBSERVATIONS; SPATIAL TRANSPORT; POLAR WIND; DISSIPATION; FLUCTUATIONS; PLASMA; 1-AU; EVOLUTION AB Previous formulations of heating and transport associated with strong magnetohydrodynamic (MHD) turbulence are generalized to incorporate separate internal energy equations for electrons and protons. Electron heat conduction is included. Energy is supplied by turbulent heating that affects both electrons and protons and is exchanged between them via collisions. Comparison to available Ulysses data shows that a reasonable accounting for the data is provided when (1) the energy exchange timescale is very long and (2) the deposition of heat due to turbulence is divided, with 60% going to proton heating and 40% into electron heating. Heat conduction, determined here by an empirical fit, plays a major role in describing the electron data. C1 [Breech, B.] NASA, Goddard Space Flight Ctr, Lab Solar & Space Phys, Greenbelt, MD 20716 USA. [Matthaeus, W. H.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA. [Matthaeus, W. H.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA. [Cranmer, S. R.; Kasper, J. C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Oughton, S.] Univ Waikato, Dept Math, Hamilton 3240, New Zealand. RP Breech, B (reprint author), NASA, Goddard Space Flight Ctr, Lab Solar & Space Phys, Mail Code 673,8800 Greenbelt Rd, Greenbelt, MD 20716 USA. EM babreech@gmail.com RI Kasper, Justin/D-1152-2010; Oughton, Sean/A-3380-2012 OI Kasper, Justin/0000-0002-7077-930X; Oughton, Sean/0000-0002-2814-7288 FU National Aeronautics and Space Administration (NASA) [NNG04GE77G, NNX06AG95G, NNX09AB27G, NNX08AI47G, NNX08AW07G]; NSF [ATM 0752135] FX Amitava Bhattacharjee thanks the reviewers for their assistance in evaluating this paper. NR 45 TC 45 Z9 45 U1 0 U2 0 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 SEP 16 PY 2009 VL 114 AR A09103 DI 10.1029/2009JA014354 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 497KS UT WOS:000270058700003 ER PT J AU Iyuke, SE Mamvura, TA Liu, K Sibanda, V Meyyappan, M Varadan, VK AF Iyuke, S. E. Mamvura, T. A. Liu, K. Sibanda, V. Meyyappan, M. Varadan, V. K. TI Process synthesis and optimization for the production of carbon nanostructures SO NANOTECHNOLOGY LA English DT Article ID CHEMICAL-VAPOR-DEPOSITION; LARGE-SCALE SYNTHESIS; FLOATING CATALYST; FIELD-EMISSION; NANOTUBES; SUPPORT; CVD AB A swirled fluidized bed chemical vapour deposition (SFCVD) reactor has been manufactured and optimized to produce carbon nanostructures on a continuous basis using in situ formation of floating catalyst particles by thermal decomposition of organometallic ferrocene. During the process optimization, carbon nanoballs were produced in the absence of a catalyst at temperatures higher than 1000 degrees C, while carbon nanofibres, single-walled carbon nanotubes, helical carbon nanotubes, multi-walled carbon nanotubes (MWCNTs) and carbon nanofibres (CNFs) were produced in the presence of a catalyst at lower temperatures of between 750 and 900 degrees C. The optimum conditions for producing carbon nanostructures were a temperature of 850 degrees C, acetylene flow rate of 100 ml min(-1), and acetylene gas was used as the carbon source. All carbon nanostructures produced have morphologies and diameters ranging from 15 to 200 nm and wall thicknesses between 0.5 and 0.8 nm. In comparison to the quantity of MWCNTs produced with other methods described in the literature, the SFCVD technique was superior to floating catalytic CVD (horizontal fixed bed) and microwave CVD but inferior to rotary tube CVD. C1 [Iyuke, S. E.; Mamvura, T. A.; Liu, K.; Sibanda, V.] Univ Witwatersrand, Fac Engn & Built Environm, Sch Chem & Met Engn, ZA-2050 Wits, Johannesburg, South Africa. [Iyuke, S. E.; Liu, K.] Univ Witwatersrand, DST NRF Ctr Excellence Strong Mat, ZA-2050 Wits, Johannesburg, South Africa. [Liu, K.] Cent S Univ, Sch Resources Proc & Bioengn, Changsha 410083, Hunan, Peoples R China. [Meyyappan, M.] NASA, Ames Res Ctr, Ctr Nanotechnol, Moffett Field, CA 94035 USA. [Varadan, V. K.] Univ Arkansas, Dept Elect Engn, HiDEC, Fayetteville, AR 72701 USA. RP Iyuke, SE (reprint author), Univ Witwatersrand, Fac Engn & Built Environm, Sch Chem & Met Engn, ZA-2050 Wits, Johannesburg, South Africa. EM sunny.iyuke@wits.ac.za RI Liu, Kun/F-9118-2010 FU National Research Foundation (NRF); NRF Focus Area; NRF Nanotechnology flagship programme; DST/NRF Centre of Excellence FX The authors acknowledge the financial support from the National Research Foundation (NRF) under a South Africa-China collaborative research grant, NRF Focus Area, NRF Nanotechnology flagship programme, DST/NRF Centre of Excellence. The student bursaries provided by the Wits University are much appreciated. NR 22 TC 6 Z9 7 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0957-4484 J9 NANOTECHNOLOGY JI Nanotechnology PD SEP 16 PY 2009 VL 20 IS 37 AR 375602 DI 10.1088/0957-4484/20/37/375602 PG 10 WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary; Physics, Applied SC Science & Technology - Other Topics; Materials Science; Physics GA 488GR UT WOS:000269337800012 PM 19706958 ER PT J AU Truhlik, V Bilitza, D Triskova, L AF Truhlik, V. Bilitza, D. Triskova, L. TI Latitudinal variation of the topside electron temperature at different levels of solar activity SO ADVANCES IN SPACE RESEARCH LA English DT Article DE Electron temperature; Solar activity variation; Latitudinal dependence ID UPPER IONOSPHERE; F-REGION; CYCLE VARIATIONS; MODEL; PLASMASPHERE; SATELLITE; ALTITUDE; ISIS-1; IRI AB A database of electron temperature (T(e)) measurements comprising of most of the available satellite measurements in the topside ionosphere is used for studying the solar activity variations of the electron temperature T(e) at different latitudes, altitudes, local times and seasons. The T(e) data are grouped into three levels of solar activity (low, medium, high) at four altitude ranges, for day and night, and for equinox and solstices. We find that in general T(e) changes with solar activity are small and comparable in magnitude with seasonal changes but much smaller than the changes with altitude, latitude, and from day to night. In all cases, except at low altitude during daytime, T(e) increases with increasing solar activity. But this increase is not linear as assumed in most empirical T(e) models but requires at least a parabolic approximation. At 550 kill during daytime negative as well as positive correlation is found with solar activity. Our global data base allows to quantity the latitude range and seasonal conditions for which these correlations occur. A negative correlation with solar activity is found in the invdip latitude range from 20 to 55 degrees during equinox and from 20 degrees onward during winter. In the low latitude (20 to -20 degrees invdip) F-region there is almost no change with solar activity during solstice and a positive correlation during equinox. A positive correlation is also observed during summer from 30 degrees onward. (C) 2009 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 [Truhlik, V.; Triskova, L.] Inst Atmospher Phys, Prague 14131 4, Czech Republic. [Bilitza, D.] SPDF, GSFC, Greenbelt, MD 20771 USA. [Bilitza, D.] George Mason Univ, Fairfax, VA 22030 USA. RP Truhlik, V (reprint author), Inst Atmospher Phys, Bocni 2, Prague 14131 4, Czech Republic. EM vtr@ufa.cas.cz RI Triskova, Ludmila/H-6503-2014; Truhlik, Vladimir/H-6971-2014 OI Truhlik, Vladimir/0000-0002-6624-4388 FU Academy of Sciences of the Czech Republic [A300420603]; NASA [NNH06CD17C] FX We are very grateful to K.-I. Oyama, J. Smilauer, M. Hairston, F. Rich, K.W. Min, and P.K. Bhuyan for providing data from Hinotori, Intercosmos (19, 24, and 25), DMSP (1712, F13, F14, and F15), DMSP (F10 and F11), KOMPSAT-1 and SROSS C2 satellites, respectively. We are also grateful to NASA's National Space Science Data Center (NSSDC) and Space Physics Data Facility (SPDF) for providing the other satellite Te data and also the Modelweb interface. We also thank Katerina Podolska, BSc., employee of the Institute of Atmospheric Physics for help with processing of the huge amount of DMSP data. This study was supported by the Grant A300420603 of the Grant Agency of the Academy of Sciences of the Czech Republic and by NASA Grant NNH06CD17C. NR 21 TC 9 Z9 9 U1 0 U2 4 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 SEP 15 PY 2009 VL 44 IS 6 BP 693 EP 700 DI 10.1016/j.asr.2009.04.029 PG 8 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA 491QT UT WOS:000269594900007 ER PT J AU Bilitza, D AF Bilitza, D. TI Evaluation of the IRI-2007 model options for the topside electron density SO ADVANCES IN SPACE RESEARCH LA English DT Article DE IRI; Topside ionosphere; Electron density; Topside sounder; NeQuick ID IRI; PROFILES; IONOSPHERE; NEQUICK AB The international Reference Ionosphere (IRI) 2007 provides two new options for the topside electron density profile: (a) it correction of the IRI-2001 model, and (b) the NeQuick topside formula. We use the large volume of Alouette 1, 2 and ISIS 1, 2 topside sounder data to evaluate these two new options with special emphasis oil the uppermost topside where IRI-2001 showed the largest discrepancies. We will also study the accurate representation of profiles in the equatorial anomaly region where the profile function has to accommodate two latitudinal maxima (crests) at lower altitudes but only a single maximum (at the equator) higher up. In addition to IRI-2001 and the two new IRI-2007 options we also include the Intercosmos-based topside model of Triskova, Truhlik, and Smilauer [Triskova, L., Truhlik, V., Smilauer, J. An empirical topside electron density model for calculation of absolute ion densities in IRI. Adv. Space Res. 37 (5), 928-934, 2006] (TTS model) in our analysis. We find that overall IRI-2007-NeQ gives the best results but IRI-2007-corrected provides a more realistic representation of the altitudinal-latitudinal structure in the equatorial anomaly region. The applicability of the TTS model is limited by the fact that it is not normalized to the F2 peak density and height. (C) 2009 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 [Bilitza, D.] GSFC, Heliophys Lab, Greenbelt, MD 20771 USA. [Bilitza, D.] George Mason Univ, Fairfax, VA 22030 USA. RP Bilitza, D (reprint author), GSFC, Heliophys Lab, Code 672, Greenbelt, MD 20771 USA. EM dieter.bilitza-1@nasa.gov FU NSF [0417666]; NASA [05-LWS05-161] FX We gratefully acknowledge NASA's NSSDC and SPDF for providing the Alouette and ISIS topside sounder data. This study was supported through NSF Grant 0417666 and NASA Living With a Star Grant 05-LWS05-161. NR 17 TC 38 Z9 38 U1 0 U2 3 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 SEP 15 PY 2009 VL 44 IS 6 BP 701 EP 706 DI 10.1016/j.asr.2009.04.036 PG 6 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA 491QT UT WOS:000269594900008 ER PT J AU Zak, M AF Zak, Michail TI Quantum-inspired resonance for associative memory SO CHAOS SOLITONS & FRACTALS LA English DT Article AB A new kind of dynamics for simulations based upon quantum-classical hybrid is discussed. The model is represented by a modified Madelung equation in which the quantum potential is replaced by different, specially chosen potentials. As a result, the dynamics attains both quantum and classical properties: it preserves superposition and entanglement of random solutions, while allowing one to measure its state variables using classical methods. Such an optimal combination of characteristics is a perfect match for quantum-inspired information processing. In this paper, the retrieval of stored items from an exponentially large unsorted database is performed by quantum-inspired resonance using polynomial resources due to quantum-like superposition effect. (C) 2008 Elsevier Ltd. All rights reserved. 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 NR 11 TC 2 Z9 2 U1 0 U2 1 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 SEP 15 PY 2009 VL 41 IS 5 BP 2306 EP 2312 DI 10.1016/j.chaos.2008.09.023 PG 7 WC Mathematics, Interdisciplinary Applications; Physics, Multidisciplinary; Physics, Mathematical SC Mathematics; Physics GA 476RF UT WOS:000268460600018 ER PT J AU Rao, MN Nyquist, LE Sutton, SR Dreibus, G Garrison, DH Herrin, J AF Rao, M. N. Nyquist, L. E. Sutton, S. R. Dreibus, G. Garrison, D. H. Herrin, J. TI Fluid-evaporation records preserved in salt assemblages in Meridiani rocks SO EARTH AND PLANETARY SCIENCE LETTERS LA English DT Article DE Mars; Meridiani Planum; Opportunity APXS data; Martian fluids; progressive evaporation; chemical divide; sulfate; chlorine and bromine ID X-RAY SPECTROMETER; MARTIAN METEORITES; BRINE EVOLUTION; BURNS FORMATION; MARS; PLANUM; CHEMISTRY; SOILS; VOLATILES; ORIGIN AB We studied the inter-relationships between the major anions (SO3, Cl, and Br) and cations (FeO, CaO and MgO) using elemental abundances determined by APXS in salt assemblages of RATted (abraded) rocks at Meridiani to characterize the behavior of fluids that infiltrated into this region on Mars. A Plot Of SO3 versus Cl for the abraded rocks yielded an unusual pattern, whereas the SO3/Cl ratios versus Cl for the same rocks showed a monotonically decreasing trend represented by a hyperbola. The systematic behavior of the SO3 and Cl data in the documented rocks at Meridiani suggests that these anions behaved conservatively during fluid-rock interactions. These results further indicate that two kinds of fluids, referred to as SOL-I and SOL-II, infiltrated into Endurance/Eagle/Fram craters, where they underwent progressive evaporative concentration. SOL-I is a low pH fluid consisting of high SO3 and low Cl and high Br, (this fluid infiltrated all the way to the crater-top region), whereas SOL-II fluid of high pH with low SO3 and high Cl and low Br reached only an intermediary level known as the Whatanga contact at Endurance. Based on the FeO/MgO as well as CaO/MgO versus SO3/Cl diagram for rocks above the Whatanga contact, the cation and anion relationships in this system suggest that the Fe2+/SO4 and Ca2+/SO4 ratios in SOL-I fluids at Meridiani were > 1 before the onset of evaporation based on the "chemical divide" considerations. Below the Whatanga contact, relatively dilute SOL-II fluids seem to have infiltrated and dissolved/flushed away the easily soluble Mg-sulfate/chloride phases (along with Br) without significantly altering the SO3/Cl ratios in the residual salt assemblages. Further, Cl/Br versus Br in rocks above the Whatanga contact show a hyperbolic trend suggesting that Cl and Br behaved conservatively similar to SO3 and Cl in the SOL-I fluids at Meridiani. Our results are consistent with a scenario involving two episodes (SOL-I and SOL-II) of groundwater recharge at Meridiani Planum. (C) 2009 Elsevier B.V. All rights reserved. C1 [Rao, M. N.; Garrison, D. H.; Herrin, J.] NASA, Lyndon B Johnson Space Ctr, Jacobs Engn & Sci Contracting Grp, Houston, TX 77058 USA. [Nyquist, L. E.] NASA, Lyndon B Johnson Space Ctr, Astromat Res & Explorat Sci KR, Houston, TX 77058 USA. [Sutton, S. R.] Univ Chicago, Dept Geol Sci, Chicago, IL 60637 USA. [Dreibus, G.] Max Planck Inst Chem, D-55122 Mainz, Germany. RP Rao, MN (reprint author), NASA, Lyndon B Johnson Space Ctr, Jacobs Engn & Sci Contracting Grp, Bldg 31,NASA Rd 1, Houston, TX 77058 USA. EM nageswara.rao@nasa.gov OI Herrin, Jason/0000-0002-2452-244X FU NASA Mars Fundamental Research Program FX We thank Heinrich Wanke, Don Bogard, and Dave McKay for comments and Sue Wentworth, C.-Y. Shih and Ramarao Inguva for assistance during this work. We are grateful to Richard Carlson, Ralf Gellert and an anonymous reviewer for providing valuable suggestions and comments, which improved the paper significantly. We are particularly grateful to Dr. Blair F. Jones (USGS, Reston, VA) for reviewing our paper independently and providing valuable suggestions. This work is supported by NASA Mars Fundamental Research Program contract to Larry Nyquist. NR 49 TC 8 Z9 8 U1 0 U2 7 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0012-821X EI 1385-013X J9 EARTH PLANET SC LETT JI Earth Planet. Sci. Lett. PD SEP 15 PY 2009 VL 286 IS 3-4 BP 396 EP 403 DI 10.1016/j.epsl.2009.07.007 PG 8 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 513XU UT WOS:000271358300006 ER PT J AU Campbell, AJ Danielson, L Righter, K Seagle, CT Wang, YB Prakapenka, VB AF Campbell, Andrew J. Danielson, Lisa Righter, Kevin Seagle, Christopher T. Wang, Yanbin Prakapenka, Vitali B. TI High pressure effects on the iron-iron oxide and nickel-nickel oxide oxygen fugacity buffers SO EARTH AND PLANETARY SCIENCE LETTERS LA English DT Article DE oxygen fugacity; high pressure; equations of state ID DIAMOND-ANVIL CELL; X-RAY-DIFFRACTION; SILICATE PARTITION-COEFFICIENTS; INDUCED COORDINATION CHANGES; HIGH-TEMPERATURE; CORE FORMATION; LOWER-MANTLE; EARTHS MANTLE; MAGMA OCEAN; STATE AB The chemical potential of oxygen in natural and experimental samples is commonly reported relative to a specific oxygen fugacity (fO(2)) buffer. These buffers are precisely known at 1 bar, but under high pressures corresponding to the conditions of the deep Earth, oxygen fugacity buffers are poorly calibrated. Reference (1 bar) fO(2) buffers can be integrated to high pressure conditions by integrating the difference in volume between the solid phases, provided that their equations of state are known. In this work, the equations of state and volume difference between the metal-oxide pairs Fe-FeO and Ni-NiO were measured using synchrotron X-ray diffraction in a multi-anvil press and laser heated diamond anvil cells. The results were used to construct high pressure fO(2) buffer curves for these systems. The difference between the Fe-FeO and Ni-NiO buffers is observed to decrease significantly, by several log units, over 80 GPa. The results can be used to improve interpretation of high pressure experiments, specifically Fe-Ni exchange between metallic and oxide phases. (C) 2009 Elsevier B.V. All rights reserved. C1 [Campbell, Andrew J.] Univ Maryland, Dept Geol, College Pk, MD 20742 USA. [Danielson, Lisa; Righter, Kevin] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Seagle, Christopher T.] Univ Chicago, Dept Geophys Sci, Chicago, IL 60637 USA. [Wang, Yanbin; Prakapenka, Vitali B.] Univ Chicago, Consortium Adv Radiat Sources, Argonne, IL 60439 USA. RP Campbell, AJ (reprint author), Univ Maryland, Dept Geol, College Pk, MD 20742 USA. EM ajc@umd.edu RI Seagle, Christopher/D-5000-2009; OI Wang, Yanbin/0000-0001-5716-3183 FU COMPRES; NSF Cooperative Agreement EAR [06-49658]; National Science Foundation - Earth Sciences [EAR-0622171]; Department of Energy - Geosciences [DE-FG02-94ER14466]; State of Illinois; U. S. Department of Energy, Office of Science, Office of Basic Energy Sciences [DE-AC02-06CH11357]; NSF [EAR-0635722]; NASA Cosmochemistry program; DOE-NNSA FX We are grateful to Graham Taylor, Genna Davidson, and Helen Nguyen for their assistance with data processing. Kurt Leinenweber helpfully provided the octahedral assemblies that were specifically designed for synchrotron X-ray diffraction experiments. Comments from two anonymous reviewers guided improvements to the manuscript. This research was partially supported by COMPRES, the Consortium for Materials Properties Research in Earth Sciences under NSF Cooperative Agreement EAR 06-49658. Portions of this work were performed at GeoSoilEnviroCARS (Sector 13), Advanced Photon Source (APS), Argonne National Laboratory. GeoSoilEnviroCARS is supported by the National Science Foundation - Earth Sciences (EAR-0622171), Department of Energy - Geosciences (DE-FG02-94ER14466) and the State of Illinois. Use of the Advanced Photon Source was supported by the U. S. Department of Energy, Office of Science, Office of Basic Energy Sciences, under Contract No. DE-AC02-06CH11357. This work was supported by NSF grant EAR-0635722 (AJC) and an RTOP from the NASA Cosmochemistry program (KR). CTS acknowledges support from DOE-NNSA through the Carnegie/DOE Alliance Center (CDAC). NR 53 TC 49 Z9 49 U1 3 U2 27 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 SEP 15 PY 2009 VL 286 IS 3-4 BP 556 EP 564 DI 10.1016/j.epsl.2009.07.022 PG 9 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 513XU UT WOS:000271358300021 ER PT J AU Roberts, CD LeGrande, AN Tripati, AK AF Roberts, Christopher D. LeGrande, Allegra N. Tripati, Aradhna K. TI Climate sensitivity to Arctic seaway restriction during the early Paleogene SO EARTH AND PLANETARY SCIENCE LETTERS LA English DT Article DE paleoclimate; climate modeling; Paleogene; Arctic Ocean; Azolla; PETM ID EOCENE THERMAL MAXIMUM; CARBON-DIOXIDE CONCENTRATIONS; SURFACE TEMPERATURES; OCEAN TEMPERATURES; EQUABLE CLIMATES; MARINE ARCHAEA; COASTAL OCEAN; WATER-COLUMN; PALEOCENE; ISOTOPE AB The opening and closing of ocean gateways affects the global distribution of heat salt and moisture, potentially driving climatic change on regional to global scales. Between 65 and 45 million years ago (Ma), during the early Paleogene, exchange between the Arctic and global oceans occurred through two narrow and shallow seaways, the Greenland-Norway seaway and the Turgai Strait. Sediments from the Arctic Ocean suggest that, during this interval, the surface ocean was warm, brackish, and episodically enabled the freshwater fern Azolla to bloom. The precise mechanisms responsible for the development of these conditions in the Paleogene Arctic remain uncertain. Here we show results from an isotope-enabled, atmosphere-ocean general circulation model, which indicate that Northern Hemisphere climate would have been very sensitive to the degree of oceanic exchange through the Arctic seaways. We also present modelled estimates of seawater and calcite delta O-18 for the Paleogene. By restricting these seaways, we simulate freshening of the surface Arctic Ocean to similar to 6 psu and warming of sea-surface temperatures by 2 degrees C in the North Atlantic and 5-10 degrees C in the Labrador Sea. Our results may help explain the occurrence of low-salinity tolerant taxa in the Arctic Ocean during the Eocene and provide a mechanism for enhanced warmth in the north western Atlantic. We propose that the formation of a volcanic land-bridge between Greenland and Europe could have caused increased ocean convection and warming of intermediate waters in the Atlantic. If true, this result is consistent with the theory that bathymetry changes may have caused thermal destabilisation of methane clathrates and supports a tectonic trigger hypothesis for the Paleocene Eocene Thermal Maximum (PETM). (C) 2009 Elsevier B.V. All rights reserved. C1 [Roberts, Christopher D.; Tripati, Aradhna K.] Univ Cambridge, Dept Earth Sci, Cambridge CB2 3EQ, England. [LeGrande, Allegra N.] Columbia Univ, NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [LeGrande, Allegra N.] Columbia Univ, Ctr Climate Syst Res, New York, NY 10025 USA. RP Roberts, CD (reprint author), Univ Cambridge, Dept Earth Sci, Cambridge CB2 3EQ, England. EM cdr30@cam.ac.uk RI Tripati, Aradhna/C-9419-2011; Roberts, Christopher/F-6197-2011; LeGrande, Allegra/D-8920-2012 OI Tripati, Aradhna/0000-0002-1695-1754; LeGrande, Allegra/0000-0002-5295-0062 FU Natural Environment Research Council [NER/S/A/2006/14070, NE/D009049/1]; National Science Foundation (ATM) [0753660]; Magdalene College FX We thank NASA GISS for institutional support and acknowledge financial support from the Natural Environment Research Council (studentship NER/S/A/2006/14070 and fellowship NE/D009049/1), the National Science Foundation (ATM 0753660), and Magdalene College. We thank G. Schmidt for helpful discussions and K. Bice and J. Sewall for providing us with gridded data for the boundary conditions. Constructive reviews from four anonymous reviewers improved this manuscript. NR 80 TC 31 Z9 31 U1 1 U2 11 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0012-821X EI 1385-013X J9 EARTH PLANET SC LETT JI Earth Planet. Sci. Lett. PD SEP 15 PY 2009 VL 286 IS 3-4 BP 576 EP 585 DI 10.1016/j.epsl.2009.07.026 PG 10 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 513XU UT WOS:000271358300024 ER PT J AU Romanek, CS Jimenez-Lopez, C Navarro, AR Sanchez-Roman, M Sahai, N Coleman, M AF Romanek, Christopher S. Jimenez-Lopez, Concepcion Rodriguez Navarro, Alejandro Sanchez-Roman, Monica Sahai, Nita Coleman, Max TI Inorganic synthesis of Fe-Ca-Mg carbonates at low temperature SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Article ID EARLY DIAGENETIC SIDERITE; OXYGEN-ISOTOPE FRACTIONATION; PRECAMBRIAN IRON-FORMATIONS; HYDROUS FERRIC-OXIDE; CRYSTAL-GROWTH; SYSTEM CACO3-MGCO3-FECO3; DISSIMILATORY REDUCTION; ELEMENTAL COMPOSITION; SUBSOLIDUS RELATIONS; MAGNESIAN CALCITE AB A set of free-drift experiments was undertaken to synthesize carbonates of mixed cation content (Fe, Ca, Mg) from solution at 25 and 70 degrees C to better understand the relationship between the mineralogy and composition of these phases and the solutions from which they precipitate. Metastable solid solutions formed at 25 degrees C which are not predicted from the extrapolation of higher temperature equilibrium assemblages; instead, solids formed that were intermediary in chemical composition to known magnesite-siderite and dolomite solid solutions. A calcite-siderite solid solution precipitated at 25 degrees C, with the percentage of CaCO(3) in the solid being proportional to the aqueous Ca/Fe ratio of the solution, while Mg was excluded from the crystal structure except at relatively high aqueous Mg/Ca and Mg/Fe ratios and a low Ca content. Alternatively, at 70 degrees C Mg was the predominant cation of the solid solutions. These results are compatible with the hypothesis that the relative dehydration energies of Fe, Ca and Mg play an important role in the formation of mixed cation carbonates in nature. (C) 2009 Elsevier Ltd. All rights reserved. C1 [Romanek, Christopher S.; Sanchez-Roman, Monica] Univ Georgia, Dept Geol, Athens, GA 30602 USA. [Romanek, Christopher S.; Sanchez-Roman, Monica] Univ Georgia, NASA, Astrobiol Inst, Athens, GA 30602 USA. [Romanek, Christopher S.; Sanchez-Roman, Monica] Savannah River Ecol Lab, Aiken, SC 29802 USA. [Jimenez-Lopez, Concepcion] Univ Granada, Fac Ciencias, Dept Microbiol, E-18071 Granada, Spain. [Rodriguez Navarro, Alejandro] Univ Granada, Fac Ciencias, Dept Mineral & Petr, E-18071 Granada, Spain. [Sahai, Nita] Univ Wisconsin, Dept Geol & Geophys, Madison, WI 53706 USA. [Sahai, Nita] Univ Wisconsin, NASA, Astrobiol Inst, Madison, WI 53706 USA. [Coleman, Max] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Coleman, Max] CALTECH, NASA, Astrobiol Inst, Pasadena, CA 91109 USA. RP Romanek, CS (reprint author), Univ Kentucky, Dept Earth & Environm Sci, Lexington, KY 40506 USA. EM c.romanek@uky.edu; cjl@ugr.es FU MEC (Spain) [GL2004-03910, CGL2007-63859]; Fulbright/MEC Program; NSF [0208036]; ACS [47792-AC2]; JPL's Research and Technology Development Program [01 STCR-R.07.023.01 1]; NASA's Astrobiology Institute; NASA's Ancient Martian Meteorite program; US Department of Energy [DE-FC09-96-SR 18546]; University of Georgia Research Foundation; Junta de Andalucia research [BIO-103] FX CJL acknowledges support from grants CGL2004-03910 and CGL2007-63859 from MEC (Spain) and the Fulbright/MEC Program. NS acknowledges funding support from NSF EAR CAREER 0208036 and ACS PRF 47792-AC2. The contribution of MC was carried out at the Jet Propulsion Laboratory (JPL), California Institute of Technology, under contract with the National Aeronautics and Space Administration (NASA), partly supported by JPL's Research and Technology Development Program (grant 01 STCR-R.07.023.01 1). This work was also supported in part by NASA's Astrobiology Institute, NASA's Ancient Martian Meteorite program, and the US Department of Energy through Financial Assistance Award No. DE-FC09-96-SR 18546 to the University of Georgia Research Foundation. Lindy Paddock, Brian Jackson, John Shields and the Junta de Andalucia research group BIO-103 are acknowledged for analytical assistance. Finally, J. Morse and A. Mucci are thanked for reviewing previous versions of this manuscript. NR 83 TC 27 Z9 27 U1 3 U2 46 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 SEP 15 PY 2009 VL 73 IS 18 BP 5361 EP 5376 DI 10.1016/j.gca.2009.05.065 PG 16 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 489EB UT WOS:000269401600010 ER PT J AU Tobler, DJ Shaw, S Benning, LG AF Tobler, Dominique J. Shaw, Sam Benning, Liane G. TI Quantification of initial steps of nucleation and growth of silica nanoparticles: An in-situ SAXS and DLS study SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Article ID COLLOIDAL SILICA; NANOCOLLOID FORMATION; AQUEOUS-SOLUTIONS; KINETICS; PRECIPITATION; AGGREGATION; PARTICLES; SIZE; POLYMERIZATION; MECHANISMS AB The initial steps of silica polymerization and silica nanoparticle formation have been studied in-situ and in real-time. The experiments were carried out in near neutral pH (7-8) solutions with initial silica concentrations of 640 and 1600 ppm ([SiO(2)]) and ionic strengths (IS) of 0.02, 0.05, 0.11 and 0.22 M. The polymerization reactions were induced by neutralizing a high pH silica solution (from pH 12 to 7) and monitored by the time-dependent depletion in monosilicic acid concentration over time. The accompanied nucleation and growth of silica nanoparticles (i.e., change in particle size over time) was followed in-situ using time-resolved synchrotron-based Small Angle X-ray Scattering (SAXS) and conventional Dynamic Light Scattering (DLS) combined with scanning and (cryo)-transmission electron microscopy (SEM/cryo-TEM). The critical nucleus diameter was quantified (1.4-2 nm) and results from SAXS and DLS showed that over 3 It the particle diameter increased to a final size of similar to 8 nm. SEM and TEM photomicrographs verified the SAXS and DLS data and confirmed the spherical and hydrous structure of the forming silica nanoparticles. Furthermore, fractal analysis (i.e., fractal dimension, D(m) similar to 2.2) indicated that the formed particles consisted of open, polymeric, low-density structures. For the nucleation and growth of silica nanoparticles a 3-stage growth process is proposed: (1) homogeneous and instantaneous nucleation of silica nanoparticles, (2) 3-D, surface-controlled particle growth following 1st order reaction kinetics and (3) Ostwald ripening and particle aggregation. (C) 2009 Elsevier Ltd. All rights reserved. C1 [Tobler, Dominique J.; Shaw, Sam; Benning, Liane G.] Univ Leeds, Sch Earth & Environm, Earth & Biosphere Inst, Leeds LS2 9JT, W Yorkshire, England. RP Tobler, DJ (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM tobler@see.leeds.ac.uk RI Shaw, Sam/D-6869-2011; Benning, Liane/E-7071-2011; Tobler, Dominique/G-3213-2012; Shaw, Sam/A-3528-2017 OI Benning, Liane/0000-0001-9972-5578; Tobler, Dominique/0000-0001-8532-1855; Shaw, Sam/0000-0002-6353-5454 FU Earth and Biosphere Institute (University of Leeds, UK); University of Leeds FX The authors thank Wim Bras and the station scientists from the Dutch-Belgian beamline (DUBBLE) at the European Synchrotron Radiation Facility (ESRF), Grenoble, France, for bearritime and technical assistance. We also specifically thank Mike Hounslow (Chemical and Process Engineering, University of Sheffield, UK) for help and guidance of how to use the Chronomal approach for the evaluation of our SAXS data and for explaining the mathematical background behind this kinetic model. D.J.T. acknowledge John Harrington, Adrian Hick and David Parcej for their assistance with FEG-SEM, TEM and cryo-TEM work, respectively. Many thanks also to Susanne Patel and Jennifer Green from Particles CIC (University of Leeds, UK) for help with DLS logistics. Financial support via a PhD fellowship for DJT from the Earth and Biosphere Institute (University of Leeds, UK), and research funds for LGB from the University of Leeds are acknowledged. The authors thank the three anonymous reviewers for their valued comments. NR 76 TC 55 Z9 56 U1 3 U2 64 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 SEP 15 PY 2009 VL 73 IS 18 BP 5377 EP 5393 DI 10.1016/j.gca.2009.06.002 PG 17 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 489EB UT WOS:000269401600011 ER PT J AU MacPherson, GJ Mittlefehldt, DW Lipschutz, ME Clayton, RN Bullock, ES Ivanov, AV Mayeda, TK Wang, MS AF MacPherson, Glenn J. Mittlefehldt, David W. Lipschutz, Michael E. Clayton, Robert N. Bullock, Emma S. Ivanov, Andrei V. Mayeda, Toshiko K. Wang, Ming-Sheng TI The Kaidun chondrite breccia: Petrology, oxygen isotopes, and trace element abundances SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Article ID CARBONACEOUS CHONDRITE; AQUEOUS ALTERATION; ENSTATITE CHONDRITE; MATRIX MINERALOGY; CM CHONDRITES; TAGISH LAKE; METEORITE; CHONDRULES; CI; GEOCHEMISTRY AB Oxygen isotope and trace element data for 13 samples of the Kaidun chondritic breccia reaffirm the complex polymict nature of this unique meteorite. Bulk Kaidun samples most closely resemble CR chondrites, but the matrix is Cl-like. Two separated clasts are CR-like but have some properties that resemble CM, two clasts are enstatite chondrites (one EL and one EH), one clast is an aubrite-like metal-rich impact melt, and one clast is a unique layered olivine-bearing pyroxenite with the isotopic composition of an aubrite. Yet, although each clast resembles a known meteorite group, all deviate in some respect from the norms for those groups. Collectively, Kaidun has sampled materials not yet represented in the world meteorite collections and which greatly extend the definitions of known meteorite groups. Phyllosilicates in Kaidun span a very wide range in composition and vary from clast to clast, suggesting that the aqueous alteration experienced by the clasts predated assembly of the Kaidun parent body. Published by Elsevier Ltd. C1 [MacPherson, Glenn J.; Bullock, Emma S.] Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, Washington, DC 20560 USA. [Mittlefehldt, David W.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Lipschutz, Michael E.; Wang, Ming-Sheng] Purdue Univ, Dept Chem, BRWN WTHR, W Lafayette, IN 47907 USA. [Clayton, Robert N.; Mayeda, Toshiko K.] Univ Chicago, Enciro Fermi Inst, Chicago, IL 60637 USA. [Ivanov, Andrei V.] VI Vernadskii Inst Geochem & Analyt Chem, Moscow 119991, Russia. RP MacPherson, GJ (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, Washington, DC 20560 USA. EM macphers@si.edu FU NASA [NNG04GK47G, NNX07AJ05G, NAGW-3396]; NSF [9526747]; U.S. Department of Energy [DE-FG07-011D1414] FX Drs. Jcffrey Grossman, Herbert Palme, Ed Scott, and Michael Weisberg provided detailed and very helpful reviews of the manuscript over several versions, and we are indebted to them for their time and patience. Dr. Jeffrey Post graciously helped with the X-ray diffraction study of the metal phase in sample #01.3.01. This research was supported by NASA Grants NNG04GK47G and NNX07AJ05G (GJM), NAGW-3396 (MEL), and NSF Grant 9526747 (RNC). The NASA Cosmochemistry Program financed DWM's participation. We thank the staff of the University of Missouri Research Reactor for their aid and the U.S. Department of Energy for reactor support under Grant DE-FG07-011D14146. We thank Mr. H. Mirzaci for invaluable aid. NR 46 TC 14 Z9 14 U1 0 U2 5 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 SEP 15 PY 2009 VL 73 IS 18 BP 5493 EP 5511 DI 10.1016/j.gca.2009.06.012 PG 19 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 489EB UT WOS:000269401600019 ER PT J AU McKay, CP Molaro, JL Marinova, MM AF McKay, Christopher P. Molaro, Jamie L. Marinova, Margarita M. TI High-frequency rock temperature data from hyper-arid desert environments in the Atacama and the Antarctic Dry Valleys and implications for rock weathering SO GEOMORPHOLOGY LA English DT Article DE Rock; Rock weather; Rock weathering; Surface weather; Grain-scale; Temperature; Thermal; Stress; Stress gradient; Thermal shock; Thermal stress fatigue; Cracking; Flaking; Spalling; Antarctica; Beacon; Fryxell; Dry Valleys; Atacama; Desert; Arid; Damping depth ID THERMAL-STRESS; GRAIN SCALE; COLD; REGION; ISLAND; LIFE AB In desert environments with low water and salt contents. rapid thermal variations may be an important source of rock weathering. We have obtained temperature measurements of the surface of rocks in hyper-arid hot and cold desert environments at a rate of 1/s over several days. The values of temperature change over 1-second intervals were similar in hot and cold deserts despite a 30 degrees C difference in absolute rock surface temperature. The average percentage of the time dT/dt>2 degrees C/min was similar to 8 +/- 3%, >4 degrees C/min was 1 +/- 0.9%, and >8 degrees C/min was 0.02 +/- 0.03%. The maximum change over a I-second interval was similar to 10 degrees C/min. When sampled to simulate data taken over intervals longer than 1 s, we found a reduction in time spent above the 2 degrees C/min temperature gradient threshold. For 1-minute samples, the time spent above any given threshold was about two orders of magnitude lower than the corresponding value for 1-second sampling. We suggest that a rough measure of efficacy of weathering as a function of frequency is the product of the percentage of time spent above a given threshold value multiplied by the damping depth for the corresponding frequency. This product has a broad maximum for periods between 3 and 10 s. Published by Elsevier B.V. C1 [McKay, Christopher P.; Molaro, Jamie L.] NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA. [Marinova, Margarita M.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. RP McKay, CP (reprint author), NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA. EM christopher.mckay@nasa.gov RI Molaro, Jamie/C-6769-2014 OI Molaro, Jamie/0000-0002-5867-9410 FU NASA; ASTEP; IPY FX This work was supported by funding from NASA ASTEP and IPY programs. We thank the members of the field teams for help in all aspects of the fieldwork. The air temperature data from the Antarctic sites as obtained form the McMurdo LTER database. We thank the reviewers for comments that improved the paper. NR 22 TC 28 Z9 28 U1 1 U2 15 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0169-555X J9 GEOMORPHOLOGY JI Geomorphology PD SEP 15 PY 2009 VL 110 IS 3-4 BP 182 EP 187 DI 10.1016/j.geomorph.2009.04.005 PG 6 WC Geography, Physical; Geosciences, Multidisciplinary SC Physical Geography; Geology GA 491CA UT WOS:000269553300013 ER PT J AU Hodyss, R Parkinson, CD Johnson, PV Stern, JV Goguen, JD Yung, YL Kanik, I AF Hodyss, Robert Parkinson, Christopher D. Johnson, Paul V. Stern, Julie V. Goguen, Jay D. Yung, Yuk L. Kanik, Isik TI Methanol on Enceladus SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID MU-M; HYDROGEN-PEROXIDE; FROZEN METHANOL; ION IRRADIATION; ICE MIXTURES; CASSINI; SPECTROSCOPY; SPECTRA; SURFACE; CH3OH AB Near infrared spectra of the surface of Enceladus returned by Cassini show the presence of an absorption feature at 3.53 mm, ascribed by Brown et al. (2006) to "short chain organics," and by Newman et al. (2007) to hydrogen peroxide. We assign this feature tentatively to methanol. Variations in the peak position of the feature suggest that methanol in the "tiger stripes" region may be segregated from the water ice, and not homogeneously distributed in the ice matrix. The photolytic destruction of methanol implies that methane or methanol itself must be continually deposited on the surface. On Enceladus, methanol may be generated photochemically from a mixed methane/water ice, or deposited from the plume itself. The variation in the concentration of methanol over the surface could be used to distinguish between these two processes. Citation: Hodyss, R., C. D. Parkinson, P. V. Johnson, J. V. Stern, J. D. Goguen, Y. L. Yung, and I. Kanik (2009), Methanol on Enceladus, Geophys. Res. Lett., 36, L17103, doi:10.1029/2009GL039336. C1 [Hodyss, Robert; Johnson, Paul V.; Stern, Julie V.; Goguen, Jay D.; Kanik, Isik] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Parkinson, Christopher D.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. [Yung, Yuk L.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. RP Hodyss, R (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM robert.p.hodyss@jpl.nasa.gov RI Johnson, Paul/D-4001-2009 OI Johnson, Paul/0000-0002-0186-8456 FU National Aeronautics and Space Administration (NASA) [NNG06GF33G]; JPL's Research and Technology Development FX This work was performed at the Jet Propulsion Laboratory (JPL), California Institute of Technology, under a contract with the National Aeronautics and Space Administration (NASA). YLY was supported by NASA grant NNG06GF33G to the California Institute of Technology. Financial support through JPL's Research and Technology Development program is gratefully acknowledged. We thank Bonnie Buratti and James Bauer (JPL) for providing the Cassini VIMS data, and Arthur L. Lane (JPL) for useful discussions. NR 21 TC 9 Z9 9 U1 1 U2 10 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 SEP 15 PY 2009 VL 36 AR L17103 DI 10.1029/2009GL039336 PG 3 WC Geosciences, Multidisciplinary SC Geology GA 497JD UT WOS:000270054400003 ER PT J AU Doney, RL Agui, JH Sen, S AF Doney, Robert L. Agui, Juan H. Sen, Surajit TI Energy partitioning and impulse dispersion in the decorated, tapered, strongly nonlinear granular alignment: A system with many potential applications SO JOURNAL OF APPLIED PHYSICS LA English DT Article ID SOLITON-LIKE PULSES; HERTZIAN CHAINS; QUARTZ BEADS; WAVES; PROPAGATION; IMPACT; BACKSCATTERING; CONTACT; COLUMNS; ALLOY AB Rapid absorption of impulses using light-weight, small, reusable systems is a challenging problem. An axially aligned set of progressively shrinking elastic spheres, a "tapered chain," has been shown to be a versatile and scalable shock absorber in earlier simulational, theoretical, and experimental works by several authors. We have recently shown (see R. L. Doney and S. Sen, Phys. Rev. Lett. 97, 155502 (2006)) that the shock absorption ability of a tapered chain can be dramatically enhanced by placing small interstitial grains between the regular grains in the tapered chain systems. Here we focus on a detailed study of the problem introduced in the above mentioned letter, present extensive dynamical simulations using parameters for a titanium-aluminum-vanadium alloy Ti(6)Al(4)V, derive attendant hard-sphere analyses based formulae to describe energy dispersion, and finally discuss some preliminary experimental results using systems with chrome spheres and small Nitinol interstitial grains to present the underlying nonlinear dynamics of this so-called decorated tapered granular alignment. We are specifically interested in small systems, comprised of several grains. This is because in real applications, mass and volume occupied must inevitably be minimized. Our conclusion is that the decorated tapered chain offers enhanced energy dispersion by locking in much of the input energy in the grains of the tapered chain rather than in the small interstitial grains. Thus, the present study offers insights into how the shock absorption capabilities of these systems can be pushed even further by improving energy absorption capabilities of the larger grains in the tapered chains. We envision that these scalable, decorated tapered chains may be used as shock absorbing components in body armor, armored vehicles, building applications and in perhaps even in applications in rehabilitation science. (C) 2009 American Institute of Physics. [doi:10.1063/1.3190485] C1 [Doney, Robert L.] USA, Res Lab, Aberdeen Proving Ground, MD 21005 USA. [Agui, Juan H.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. [Sen, Surajit] SUNY Buffalo, Dept Phys, Buffalo, NY 14260 USA. RP Doney, RL (reprint author), USA, Res Lab, Aberdeen Proving Ground, MD 21005 USA. EM bdoney@arl.army.mil; juan.h.agui@nasa.gov; sen@dynamics.physics.buffalo.edu FU U. S. Army Research Office FX We are grateful to Professor M. Nakagawa, Professor S. Job, and Professor F. Melo for many valuable discussions on the TCs. R. L. D. thanks the U. S. Army Research Laboratory for their continuing financial support of this work. S. S. acknowledges support from the U. S. Army Research Office. NR 65 TC 12 Z9 12 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 0021-8979 J9 J APPL PHYS JI J. Appl. Phys. PD SEP 15 PY 2009 VL 106 IS 6 AR 064905 DI 10.1063/1.3190485 PG 13 WC Physics, Applied SC Physics GA 501JP UT WOS:000270378100157 ER PT J AU Huang, XC Lee, TJ AF Huang, Xinchuan Lee, Timothy J. TI Accurate ab initio quartic force fields for NH2- and CCH- and rovibrational spectroscopic constants for their isotopologs SO JOURNAL OF CHEMICAL PHYSICS LA English DT Article ID BASIS-SET CONVERGENCE; VIBRATIONAL FREQUENCIES; MOLECULAR ANIONS; ENERGY; C2H; NH-2(-); CODE AB A series of high-quality, purely ab initio, quartic force fields (QFFs), computed using a procedure we recently proposed, is reported for NH2- and CCH-. The singles and doubles coupled-cluster method with a perturbational estimate of the effects of connected triple excitations, denoted CCSD (T), was used with TZ, QZ, and 5Z quality basis sets and was combined with extrapolation to the one-particle basis-set limit, core-correlation effects, scalar relativistic effects, and higher-order correlation effects to yield accurate QFFs. A "best-guess" reference geometry was determined at the CCSD (T)/5Z level of theory. Analytical transformation removes nonzero gradients to facilitate a second-order perturbation theory spectroscopic analysis. The QFF is transformed into Morse/cosine coordinates in order to perform exact vibrational configuration interaction computations. Equilibrium structures, vibrational frequencies, rotational constants, and selected spectroscopic constants are reported in comparison with experimental values and previous theoretical studies. Higher-order correlation effects are found comparable to core-correlation effects in magnitude, e. g., similar to 10 cm(-1) for fundamentals, but are of opposite sign. For CCH-, a thorough discussion is presented on effective rotational constants B-0. It is concluded that the "best" QFF should incorporate all the small corrections mentioned above. Correspondingly, the best vibrational fundamentals of CCH- are estimated at 502.0 cm(-1) (nu(2)), 1800.9 cm(-1) (nu(3)), and 3204.3 cm(-1) (nu(1)), while the best vibrational fundamentals of NH2- are at 3118.5 cm(-1) (nu(1)), 1447.8 cm(-1) (nu(2)), and 3186.5 cm(-1) (nu(3)). Excellent agreement with high-resolution experiments has been obtained for fundamentals-e.g., 1-3 cm(-1) deviation for the symmetric and antisymmetric stretches of NH2-, 3121.93 cm(-1) (nu(1)) and 3190.29 cm(-1) (nu(3)), respectively. Isotopic effects are studied and presented to aid future experimental analyses. The present study should facilitate future characterizations of NH2- and CCH- from astronomical observations or other high-resolution laboratory studies. (C) 2009 American Institute of Physics. [doi:10.1063/1.3212560] C1 [Lee, Timothy J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Huang, Xinchuan] SETI Inst, Mountain View, CA 94043 USA. RP Lee, TJ (reprint author), NASA, Ames Res Ctr, MS 245-1, Moffett Field, CA 94035 USA. EM xinchuan.huang-1@nasa.gov; timothy.j.lee@nasa.gov RI HUANG, XINCHUAN/A-3266-2013; Lee, Timothy/K-2838-2012 FU NASA/SETI Institute Cooperative Agreement [NNX09AI49A]; Spitzer Space Telescope GO program [PID 40645] FX 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. Part of this work was financially supported by NASA/SETI Institute Cooperative Agreement NNX09AI49A. Support from the Spitzer Space Telescope GO program (Cycle- 4 AR-4 PID 40645) is gratefully acknowledged. Helpful comments from Dr. Christopher Dateo are gratefully acknowledged. NR 29 TC 49 Z9 49 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 0021-9606 J9 J CHEM PHYS JI J. Chem. Phys. PD SEP 14 PY 2009 VL 131 IS 10 AR 104301 DI 10.1063/1.3212560 PG 15 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 494LP UT WOS:000269814800013 ER PT J AU Campbell, J AF Campbell, Joel TI Some exact results for the Schrodinger wave equation with a time-dependent potential SO JOURNAL OF PHYSICS A-MATHEMATICAL AND THEORETICAL LA English DT Article ID HARMONIC-OSCILLATOR-TYPE; DELTA; HAMILTONIANS; PROPAGATOR; INVARIANTS AB The time-dependent Schrodinger equation with a time-dependent delta function potential is solved exactly for many special cases. In all other cases the problem can be reduced to an integral equation of the Volterra type. It is shown that by knowing the wavefunction at the origin, one may derive the wavefunction everywhere. Thus, the problem is reduced from a PDE in two variables to an integral equation in one. These results are used to compare adiabatic versus sudden changes in the potential. It is shown that adiabatic changes in the potential lead to the conservation of the normalization of the probability density. C1 NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Campbell, J (reprint author), NASA, Langley Res Ctr, MS 488, Hampton, VA 23681 USA. EM joel.f.campbell@nasa.gov NR 19 TC 5 Z9 5 U1 1 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 1751-8113 J9 J PHYS A-MATH THEOR JI J. Phys. A-Math. Theor. PD SEP 11 PY 2009 VL 42 IS 36 AR 365212 DI 10.1088/1751-8113/42/36/365212 PG 7 WC Physics, Multidisciplinary; Physics, Mathematical SC Physics GA 487BP UT WOS:000269245700018 ER PT J AU Zhao, JW Hartlep, T Kosovichev, AG Mansour, NN AF Zhao, Junwei Hartlep, Thomas Kosovichev, A. G. Mansour, N. N. TI IMAGING THE SOLAR TACHOCLINE BY TIME-DISTANCE HELIOSEISMOLOGY SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun: activity; Sun: helioseismology; Sun: interior; Sun: magnetic fields ID MICHELSON DOPPLER IMAGER; DIFFERENTIAL ROTATION; CONVECTION ZONE; REALISTIC SIMULATIONS; ACTIVE REGIONS; INTERIOR; INTERFACE; DYNAMO; BASE AB The solar tachocline at the bottom of the convection zone is an important region for the dynamics of the Sun and the solar dynamo. In this region, the sound speed inferred by global helioseismology exhibits a bump of approximately 0.4% relative to the standard solar model. Global helioseismology does not provide any information on possible latitudinal variations or asymmetries between the northern and southern hemisphere. Here, we develop a time-distance helioseismology technique, including surface- and deep-focusing measurement schemes and a combination of both, for two-dimensional tomographic imaging of the solar tachocline that infers radial and latitudinal variations in the sound speed. We test the technique using artificial solar oscillation data obtained from numerical simulations. The technique successfully recovers major features of the simplified tachocline models. The technique is then applied to SOHO/MDI medium-l data and provides for the first time a full two-dimensional sound-speed perturbation image of the solar tachocline. The one-dimensional radial profile obtained by latitudinal averaging of the image is in good agreement with the previous global helioseismology result. It is found that the amplitude of the sound-speed perturbation at the tachocline varies with latitude, but it is not clear whether this is in part or fully an effect of instrumental distortion. Our initial results demonstrate that time-distance helioseismology can be used to probe the deep interior structure of the Sun, including the solar tachocline. C1 [Zhao, Junwei; Kosovichev, A. G.] Stanford Univ, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA. [Hartlep, Thomas; Mansour, N. N.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Zhao, JW (reprint author), Stanford Univ, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA. RI Zhao, Junwei/A-1177-2007; OI Hartlep, Thomas/0000-0002-5062-9507 NR 29 TC 10 Z9 10 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 SEP 10 PY 2009 VL 702 IS 2 BP 1150 EP 1156 DI 10.1088/0004-637X/702/2/1150 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 487BI UT WOS:000269245000030 ER PT J AU Brenneman, LW Reynolds, CS AF Brenneman, Laura W. Reynolds, Christopher S. TI RELATIVISTIC BROADENING OF IRON EMISSION LINES IN A SAMPLE OF ACTIVE GALACTIC NUCLEI SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; black hole physics; galaxies: active; galaxies: Seyfert; X-rays: galaxies ID X-RAY-SPECTRUM; XMM-NEWTON OBSERVATIONS; SEYFERT 1 GALAXIES; K-ALPHA EMISSION; BLACK-HOLE SPIN; ASCA OBSERVATIONS; INTRINSIC ABSORPTION; GRATING SPECTROMETER; COMPTON REFLECTION; WARM ABSORBER AB We present a uniform X-ray spectral analysis of eight type-1 active galactic nuclei that have been previously observed with relativistically broadened iron emission lines. Utilizing data from the XMM-Newton European Photon Imaging Camera (EPIC-pn) we carefully model the spectral continuum, taking complex intrinsic absorption and emission into account. We then proceed to model the broad Fe K alpha feature in each source with two different accretion disk emission line codes, as well as a self-consistent, ionized accretion disk spectrum convolved with relativistic smearing from the inner disk. Comparing the results, we show that relativistic blurring of the disk emission is required to explain the spectrum in most sources, even when one models the full reflection spectrum from the photoionized disk. C1 [Brenneman, Laura W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Reynolds, Christopher S.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. RP Brenneman, LW (reprint author), NASA, Goddard Space Flight Ctr, Mail Code 662, Greenbelt, MD 20771 USA. NR 70 TC 35 Z9 35 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 SEP 10 PY 2009 VL 702 IS 2 BP 1367 EP 1386 DI 10.1088/0004-637X/702/2/1367 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 487BI UT WOS:000269245000048 ER PT J AU Attard, M Houde, M Novak, G Li, HB Vaillancourt, JE Dowell, CD Davidson, J Shinnaga, H AF Attard, Michael Houde, Martin Novak, Giles Li, Hua-bai Vaillancourt, John E. Dowell, C. Darren Davidson, Jacqueline Shinnaga, Hiroko TI MAGNETIC FIELDS AND INFALL MOTIONS IN NGC 1333 IRAS 4 SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: individual (NGC 1333 IRAS 4); ISM: magnetic fields; ISM: molecules; polarization; stars: formation; submillimeter ID POLARIZED DUST EMISSION; MOLECULAR CLOUD CORES; STAR-FORMATION; NGC-1333 IRAS-4; INTERSTELLAR CLOUDS; PROFILES; COLLAPSE; OUTFLOW; MODELS; LINE AB We present single-dish 350 mu m dust continuum polarimetry as well as HCN and HCO+ J = 4 -> 3 rotational emission spectra obtained on NGC 1333 IRAS 4. The polarimetry indicates a uniform field morphology over a 20 '' radius from the peak continuum flux of IRAS 4A, in agreement with models of magnetically supported cloud collapse. The field morphology around IRAS 4B appears to be quite distinct, however, with indications of depolarization observed toward the peak flux of this source. Inverse P Cygni profiles are observed in the HCN J = 4 -> 3 line spectra toward IRAS 4A, providing a clear indication of infall gas motions. Taken together, the evidence gathered here appears to support the scenario that IRAS 4A is a cloud core in a critical state of support against gravitational collapse. C1 [Attard, Michael; Houde, Martin] Univ Western Ontario, Dept Phys & Astron, London, ON N6A 3K7, Canada. [Novak, Giles] Northwestern Univ, Dept Phys & Astron, Evanston, IL 60208 USA. [Li, Hua-bai] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Vaillancourt, John E.; Dowell, C. Darren] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA. [Dowell, C. Darren] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Davidson, Jacqueline] Univ Western Australia, Sch Phys, Crawley, WA 6009, Australia. [Shinnaga, Hiroko] CALTECH, Submillimeter Observ, Hilo, HI 96720 USA. RP Attard, M (reprint author), Univ Western Ontario, Dept Phys & Astron, London, ON N6A 3K7, Canada. EM mattard@uwo.ca FU NSERC; Canada Foundation for Innovation; Ontario Innovation Trust; Western's Academic Development Fund; NSF [AST 05-40882, AST 02-43156, AST 05-05230, AST 05-05124] FX Our group is grateful for the assistance of the Caltech Sub-millimeter Observatory staff in installing and observing with SHARP and the heterodyne receiver. We also acknowledge the help provided by Jose Girart, Megan Krejny, Roger Hildebrand, Tristan Matthews, Larry Kirby, and Lerothodi Leeuw. M. A.' s and M.H.'s research is funded through the NSERC Discovery Grant, Canada Research Chair, Canada Foundation for Innovation, Ontario Innovation Trust, and Western's Academic Development Fund programs. SHARC II is funded through the NSF grant AST 05-40882 to the California Institute of Technology. The development of SHARP was funded by an NSF grant to Northwestern University (AST 02-43156), and its subsequent commissioning was funded by NSF grants to Northwestern University (AST 05-05230) and University of Chicago (AST 05-05124). NR 35 TC 22 Z9 22 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD SEP 10 PY 2009 VL 702 IS 2 BP 1584 EP 1592 DI 10.1088/0004-637X/702/2/1584 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 487BI UT WOS:000269245000064 ER PT J AU Cranmer, SR Matthaeus, WH Breech, BA Kasper, JC AF Cranmer, Steven R. Matthaeus, William H. Breech, Benjamin A. Kasper, Justin C. TI EMPIRICAL CONSTRAINTS ON PROTON AND ELECTRON HEATING IN THE FAST SOLAR WIND SO ASTROPHYSICAL JOURNAL LA English DT Review DE hydrodynamics; MHD; plasmas; solar wind; turbulence; waves ID ANISOTROPIC MAGNETOHYDRODYNAMIC TURBULENCE; 1 AU; ALFVENIC TURBULENCE; LOW-FREQUENCY; HYDROMAGNETIC TURBULENCE; VELOCITY DISTRIBUTIONS; ULYSSES OBSERVATIONS; INTERSTELLAR-MEDIUM; ACCRETION FLOWS; MHD TURBULENCE AB We analyze measured proton and electron temperatures in the high-speed solar wind in order to calculate the separate rates of heat deposition for protons and electrons. When comparing with other regions of the heliosphere, the fast solar wind has the lowest density and the least frequent Coulomb collisions. This makes the fast wind an optimal testing ground for studies of collisionless kinetic processes associated with the dissipation of plasma turbulence. Data from the Helios and Ulysses plasma instruments were collected to determine mean radial trends in the temperatures and the electron heat conduction flux between 0.29 and 5.4 AU. The derived heating rates apply specifically for these mean plasma properties and not for the full range of measured values around the mean. We found that the protons receive about 60% of the total plasma heating in the inner heliosphere, and that this fraction increases to approximately 80% by the orbit of Jupiter. A major factor affecting the uncertainty in this fraction is the uncertainty in the measured radial gradient of the electron heat conduction flux. The empirically derived partitioning of heat between protons and electrons is in rough agreement with theoretical predictions from a model of linear Vlasov wave damping. For a modeled power spectrum consisting only of Alfvenic fluctuations, the best agreement was found for a distribution of wavenumber vectors that evolves toward isotropy as distance increases. C1 [Cranmer, Steven R.; Kasper, Justin C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Matthaeus, William H.] Univ Delaware, Dept Phys & Astron, Bartol Res Inst, Newark, DE 19716 USA. [Breech, Benjamin A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Cranmer, SR (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM scranmer@cfa.harvard.edu RI Kasper, Justin/D-1152-2010 OI Kasper, Justin/0000-0002-7077-930X FU National Aeronautics and Space Administration (NASA) [NNG04GE77G, NNX06AG95G, NNX09AB27G, NNX08AI47G, NNX08AW07G]; NSF [ATM 0752135] FX The authors thank Adriaan van Ballegooijen and Eliot Quataert for valuable discussions. S.R.C.'s work was supported by the National Aeronautics and Space Administration (NASA) under grants NNG04GE77G, NNX06AG95G, and NNX09AB27G to the Smithsonian Astrophysical Observatory. W.H.M.'s research was supported by NSF ATM 0752135 (SHINE) and NASA NNX08AI47G (Heliophysics Theory Program). B.A.B.'s research was supported in part by an appointment to the NASA Postdoctoral Program at Goddard Space Flight Center, administered by Oak Ridge Associated Universities through a contract with NASA. J.C.K.'s research was supported in part by NASA grant NNX08AW07G. NR 117 TC 76 Z9 76 U1 0 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD SEP 10 PY 2009 VL 702 IS 2 BP 1604 EP 1614 DI 10.1088/0004-637X/702/2/1604 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 487BI UT WOS:000269245000066 ER PT J AU Hartman, JM Patruno, A Chakrabarty, D Markwardt, CB Morgan, EH van der Klis, M Wijnands, R AF Hartman, Jacob M. Patruno, Alessandro Chakrabarty, Deepto Markwardt, Craig B. Morgan, Edward H. van der Klis, Michiel Wijnands, Rudy TI A DECADE OF TIMING AN ACCRETION-POWERED MILLISECOND PULSAR: THE CONTINUING SPIN DOWN AND ORBITAL EVOLUTION OF SAX J1808.4-3658 SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: general; stars: individual (SAX J1808.4-3658); stars: neutron; stars: rotation; X-rays: binaries; X-rays: stars ID X-RAY PULSAR; BINARY PSR B1957+20; ACTIVE RADIO PULSAR; OPTICAL COUNTERPART; XMM-NEWTON; OUTBURST; QUIESCENCE; SAX-J1808.4-3658; VARIABILITY; CONSTRAINTS AB The Rossi X-ray Timing Explorer has observed five outbursts from the transient 2.5 ms accretion-powered pulsar SAX J1808.4-3658 during 1998-2008. We present a pulse timing study of the most recent outburst and compare it with the previous timing solutions. The spin frequency of the source continues to decrease at a rate of (-5.5 +/- 1.2) x 10(-18) Hz s(-1), which is consistent with the previously determined spin derivative. The spin down occurs mostly during quiescence, and is most likely due to the magnetic dipole torque from a B = 1.5 x 10(8) G dipolar field at the neutron star surface. We also find that the 2 hr binary orbital period is increasing at a rate of (3.80 +/- 0.06) x 10(-12) s s(-1), also consistent with previous measurements. It remains uncertain whether this orbital change reflects secular evolution or short-term variability. C1 [Hartman, Jacob M.] USN, Div Space Sci, Res Lab, Washington, DC 20375 USA. [Patruno, Alessandro; van der Klis, Michiel; Wijnands, Rudy] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands. [Chakrabarty, Deepto; Morgan, Edward H.] MIT, Dept Phys, Cambridge, MA 02139 USA. [Chakrabarty, Deepto; Morgan, Edward H.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Markwardt, Craig B.] Univ Maryland, Dept Astron, CRESST, College Pk, MD 20742 USA. [Markwardt, Craig B.] NASA, Astrophys Sci Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Hartman, JM (reprint author), USN, Div Space Sci, Res Lab, Washington, DC 20375 USA. EM jacob.hartman@nrl.navy.mil; a.patruno@uva.nl; deepto@space.mit.edu; craigm@milkyway.gsfc.nasa.gov; ehm@space.mit.edu; m.b.m.vanderklis@uva.nl; r.a.d.wijnands@uva.nl FU NASA [NNX07AP93G, NNX08AJ43G]; MIT FX We are grateful to Jean Swank and the RXTE operations team at NASA Goddard Space Flight Center for their help in scheduling these observations. We also thank Tiziana Di Salvo, Luciano Burderi, Duncan Galloway, and Mike Wolff for useful discussions. We thank the referee for useful suggestions. This work was supported in part by NASA grants NNX07AP93G and NNX08AJ43G, awarded to MIT through the RXTE Guest Observer Program and the Astrophysics Data Program. NR 41 TC 47 Z9 47 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD SEP 10 PY 2009 VL 702 IS 2 BP 1673 EP 1678 DI 10.1088/0004-637X/702/2/1673 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 487BI UT WOS:000269245000070 ER PT J AU An, D Ramirez, SV Sellgren, K Arendt, RG Boogert, ACA Schultheis, M Stolovy, SR Cotera, AS Robitaille, TP Smith, HA AF An, Deokkeun Ramirez, Solange V. Sellgren, Kris Arendt, Richard G. Boogert, A. C. Adwin Schultheis, Mathias Stolovy, Susan R. Cotera, Angela S. Robitaille, Thomas P. Smith, Howard A. TI FIRST SPECTROSCOPIC IDENTIFICATION OF MASSIVE YOUNG STELLAR OBJECTS IN THE GALACTIC CENTER SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE infrared: ISM; ISM: molecules; stars: formation ID SPITZER-SPACE-TELESCOPE; 2-DIMENSIONAL RADIATIVE-TRANSFER; SPECTRAL ENERGY-DISTRIBUTIONS; INFRARED ARRAY CAMERA; CARBON-DIOXIDE; MU-M; PROTOSTELLAR ENVELOPES; MOLECULAR CLOUDS; ISO-SWS; STARS AB We report the detection of several molecular gas-phase and ice absorption features in three photometrically selected young stellar object (YSO) candidates in the central 280 pc of the Milky Way. Our spectra, obtained with the Infrared Spectrograph (IRS) onboard the Spitzer Space Telescope, reveal gas-phase absorption from CO2 (15.0 mu m), C2H2 (13.7 mu m), and HCN (14.0 mu m). We attribute this absorption to warm, dense gas in massive YSOs. We also detect strong and broad 15 mu m CO2 ice absorption features, with a remarkable double-peaked structure. The prominent long-wavelength peak is due to CH3OH-rich ice grains, and is similar to those found in other known massive YSOs. Our IRS observations demonstrate the youth of these objects, and provide the first spectroscopic identification of massive YSOs in the Galactic Center. C1 [An, Deokkeun; Boogert, A. C. Adwin] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA. [Ramirez, Solange V.] CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA. [Sellgren, Kris] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Arendt, Richard G.] NASA, CREST, UMBC, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Schultheis, Mathias] Observ Besancon, F-25000 Besancon, France. [Schultheis, Mathias] CNRS, Inst Astrophys Paris, F-75014 Paris, France. [Stolovy, Susan R.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Cotera, Angela S.] SETI Inst, Mountain View, CA 94043 USA. [Robitaille, Thomas P.; Smith, Howard A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP An, D (reprint author), CALTECH, Ctr Infrared Proc & Anal, Mail Stop 100-22, Pasadena, CA 91125 USA. EM deokkeun@ipac.caltech.edu; sellgren@astronomy.ohio-state.edu OI Arendt, Richard/0000-0001-8403-8548; Robitaille, Thomas/0000-0002-8642-1329 FU NASA through an award issued by JPL/Caltech FX Support for this work was provided by NASA through an award issued by JPL/Caltech. This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France. NR 47 TC 8 Z9 8 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD SEP 10 PY 2009 VL 702 IS 2 BP L128 EP L132 DI 10.1088/0004-637X/702/2/L128 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 487BN UT WOS:000269245500007 ER PT J AU Contopoulos, I Christodoulou, DM Kazanas, D Gabuzda, DC AF Contopoulos, Ioannis Christodoulou, Dimitris M. Kazanas, Demosthenes Gabuzda, Denise C. TI THE INVARIANT TWIST OF MAGNETIC FIELDS IN THE RELATIVISTIC JETS OF ACTIVE GALACTIC NUCLEI SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE accretion, accretion disks; galaxies: active; galaxies: jets; galaxies: magnetic fields; magnetic fields ID SCALE ROTATION MEASURES; FARADAY-ROTATION; COSMIC BATTERY; RADIO GALAXIES; QUASAR CORES; ORIGIN; GRADIENTS; 3C-273; 3C-120; VIEW AB The origin of cosmicmagnetic (B) fields remains an open question. It is generally believed that very weak primordial B fields are amplified by dynamo processes, but it appears unlikely that the amplification proceeds fast enough to account for the fields presently observed in galaxies and galaxy clusters. In an alternative scenario, cosmic B fields are generated near the inner edges of accretion disks in active galactic nuclei (AGNs) by azimuthal electric currents due to the difference between the plasma electron and ion velocities that arises when the electrons are retarded by interactions with photons. While dynamo processes show no preference for the polarity of the (presumably random) seed field that they amplify, this alternative mechanism uniquely relates the polarity of the poloidal B field to the angular velocity of the accretion disk, resulting in a unique direction for the toroidal B field induced by disk rotation. Observations of the toroidal fields of 29 AGN jets revealed by parsec-scale Faraday rotation measurements show a clear asymmetry that is consistent with this model, with the probability that this asymmetry came about by chance being less than 1%. This lends support to the hypothesis that the universe is seeded by B fields that are generated in AGNs via this mechanism and subsequently injected into intergalactic space by the jet outflows. C1 [Contopoulos, Ioannis] Acad Athens, Res Ctr Astron, Athens 11527, Greece. [Christodoulou, Dimitris M.] Univ Massachusetts, Dept Math Sci, Lowell, MA 01854 USA. [Kazanas, Demosthenes] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Gabuzda, Denise C.] Natl Univ Ireland Univ Coll Cork, Dept Phys, Cork, Ireland. RP Contopoulos, I (reprint author), Acad Athens, Res Ctr Astron, Athens 11527, Greece. EM icontop@academyofathens.gr; dimitris_christodoulou@uml.edu; demos.kazanas@nasa.gov; gabuzda@physics.ucc.ie NR 37 TC 30 Z9 29 U1 1 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD SEP 10 PY 2009 VL 702 IS 2 BP L148 EP L152 DI 10.1088/0004-637X/702/2/L148 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 487BN UT WOS:000269245500011 ER PT J AU Fragos, T Kalogera, V Willems, B Belczynski, K Fabbiano, G Brassington, NJ Kim, DW Angelini, L Davies, RL Gallagher, JS King, AR Pellegrini, S Trinchieri, G Zepf, SE Zezas, A AF Fragos, T. Kalogera, V. Willems, B. Belczynski, K. Fabbiano, G. Brassington, N. J. Kim, D. -W. Angelini, L. Davies, R. L. Gallagher, J. S. King, A. R. Pellegrini, S. Trinchieri, G. Zepf, S. E. Zezas, A. TI TRANSIENT LOW-MASS X-RAY BINARY POPULATIONS IN ELLIPTICAL GALAXIES NGC 3379 AND NGC 4278 SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE binaries: close; galaxies: elliptical and lenticular, cD; stars: evolution; X-rays: binaries ID CHANDRA MONITORING OBSERVATIONS; ULTRACOMPACT BINARIES; LUMINOSITY FUNCTION; GLOBULAR-CLUSTERS; IRRADIATION; INSTABILITY; EVOLUTION; CATALOG; STARS AB We propose a physically motivated and self-consistent prescription for the modeling of transient neutron star low-mass X-ray binary (LMXB) properties, such as duty cycle (DC), outburst duration, and recurrence time. We apply this prescription to the population synthesis models of field LMXBs presented by Fragos et al., and compare the transient LMXB population to the Chandra X-ray survey of the two elliptical galaxies NGC 3379 and NGC 4278, which revealed several transient sources. We are able to exclude models with a constant DC for all transient systems, while models with a variable DC based on the properties of each system are consistent with the observed transient populations. We predict that the majority of the observed transient sources in these two galaxies are LMXBs with red giant donors. Finally, our comparison suggests that transient LMXBs are very rare in globular clusters (GCs), and thus the number of identified transient LMXBs may be used as a tracer of the relative contribution of field and GC LMXB populations. C1 [Fragos, T.; Kalogera, V.; Willems, B.] Northwestern Univ, Dept Phys & Astron, Evanston, IL 60208 USA. [Belczynski, K.] New Mexico State Univ, Dept Astron, Las Cruces, NM 88003 USA. [Fabbiano, G.; Brassington, N. J.; Kim, D. -W.; Zezas, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Angelini, L.] NASA, High Energy Astrophys Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Davies, R. L.] Univ Oxford, Oxford OX1 3RH, England. [Gallagher, J. S.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. [King, A. R.] Univ Leicester, Leicester LE1 7RH, Leics, England. [Pellegrini, S.] Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy. [Trinchieri, G.] Observ Astron Brera, INAF, I-20121 Milan, Italy. [Zepf, S. E.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. RP Fragos, T (reprint author), Northwestern Univ, Dept Phys & Astron, 2145 Sheridan Rd, Evanston, IL 60208 USA. EM tassosfragos@northwestern.edu; vicky@northwestern.edu; kbelczyn@nmsu.edu; gfabbiano@cfa.harvard.edu; nbrassington@head.cfa.harvard.edu; kim@cfa.harvard.edu; angelini@davide.gsfc.nasa.gov; rld@astro.ox.ac.uk; jsg@astro.wisc.edu; ark@star.le.ac.uk; silvia.pellegrini@unibo.it; ginevra.trinchieri@brera.inaf.it; zepf@pa.msu.edu; azezas@cfa.harvard.edu RI Zezas, Andreas/C-7543-2011; Fragos, Tassos/A-3581-2016 OI Zezas, Andreas/0000-0001-8952-676X; Trinchieri, Ginevra/0000-0002-0227-502X; Fragos, Tassos/0000-0003-1474-1523 FU Northwestern Presidential Fellowship FX T.F. acknowledges support from the Northwestern Presidential Fellowship. NR 23 TC 16 Z9 16 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 SEP 10 PY 2009 VL 702 IS 2 BP L143 EP L147 DI 10.1088/0004-637X/702/2/L143 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 487BN UT WOS:000269245500010 ER PT J AU Griffith, CA Penteado, P Rodriguez, S Le Mouelic, S Baines, KH Buratti, B Clark, R Nicholson, P Jaumann, R Sotin, C AF Griffith, Caitlin A. Penteado, Paulo Rodriguez, Sebastien Le Mouelic, Stephane Baines, Kevin H. Buratti, Bonnie Clark, Roger Nicholson, Phil Jaumann, Ralf Sotin, Christophe TI CHARACTERIZATION OF CLOUDS IN TITAN'S TROPICAL ATMOSPHERE SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE convection; methods: analytical; planets and satellites: individual (Titan); radiative transfer ID TROPOSPHERIC CLOUDS; SOUTH-POLE; SURFACE; CIRCULATION; DESCENT; STORMS; HAZE; RAIN AB Images of Titan's clouds, possible over the past 10 years, indicate primarily discrete convective methane clouds near the south and north poles and an immense stratiform cloud, likely composed of ethane, around the north pole. Here we present spectral images from Cassini's Visual Mapping Infrared Spectrometer that reveal the increasing presence of clouds in Titan's tropical atmosphere. Radiative transfer analyses indicate similarities between summer polar and tropical methane clouds. Like their southern counterparts, tropical clouds consist of particles exceeding 5 mu m. They display discrete structures suggestive of convective cumuli. They prevail at a specific latitude band between 8 degrees-20 degrees S, indicative of a circulation origin and the beginning of a circulation turnover. Yet, unlike the high latitude clouds that often reach 45 km altitude, these discrete tropical clouds, so far, remain capped to altitudes below 26 km. Such low convective clouds are consistent with the highly stable atmospheric conditions measured at the Huygens landing site. Their characteristics suggest that Titan's tropical atmosphere has a dry climate unlike the south polar atmosphere, and despite the numerous washes that carve the tropical landscape. C1 [Griffith, Caitlin A.; Penteado, Paulo] Univ Arizona, Dept Planetary Sci, Tucson, AZ 85719 USA. [Rodriguez, Sebastien] Univ Paris 07, CNRS, Lab AIM, CEA Saclay,DSM,IRFU,SAp, F-75221 Paris 05, France. [Le Mouelic, Stephane] Univ Nantes, CNRS, Lab Planetol & Geodynam, UMR 6112, F-44000 Nantes, France. [Baines, Kevin H.; Buratti, Bonnie; Sotin, Christophe] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Clark, Roger] US Geol Survey, Denver, CO 80225 USA. [Nicholson, Phil] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. RP Griffith, CA (reprint author), Univ Arizona, Dept Planetary Sci, Tucson, AZ 85719 USA. RI Penteado, Paulo/F-9081-2012; Rodriguez, Sebastien/H-5902-2016 OI Penteado, Paulo/0000-0001-6759-2037; Rodriguez, Sebastien/0000-0003-1219-0641 FU NASA's Cassini Program; Brazilian Governments CAPES scholarship FX C.A.G.'s research is funded by NASA's Cassini Program. P.P.'s work is supported by the Brazilian Governments CAPES scholarship and NASA's Cassini Program. NR 35 TC 20 Z9 20 U1 0 U2 5 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 SEP 10 PY 2009 VL 702 IS 2 BP L105 EP L109 DI 10.1088/0004-637X/702/2/L105 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 487BN UT WOS:000269245500002 ER PT J AU Reeves, JN Sambruna, RM Braito, V Eracleous, M AF Reeves, J. N. Sambruna, R. M. Braito, V. Eracleous, Michael TI CHANDRA DETECTION OF A PARSEC SCALE WIND IN THE BROAD-LINE RADIO GALAXY 3C 382 SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE galaxies: active; galaxies: individual (3C 382); X-rays: galaxies ID ACTIVE GALACTIC NUCLEI; SOFT-X-RAY; XMM-NEWTON; EMISSION; ABSORPTION; SPECTRUM; QUASARS; OUTFLOW; IRON; GAS AB We present unambiguous evidence for a parsec scale wind in the broad-line radio galaxy 3C 382, the first radio-loud active galactic nucleus, with R(L) = log(10)(f(5) (GHz)/f(4400)) > 1, whereby an outflow has been measured with X-ray grating spectroscopy. A 118 ks Chandra grating (HETG) observation of 3C 382 has revealed the presence of several high ionization absorption lines in the soft X-ray band, from Fe, Ne, Mg, and Si. The absorption lines are blueshifted with respect to the systemic velocity of 3C 382 by -840 +/- 60 km s(-1) and are resolved by Chandra with a velocity width of sigma = 340 +/- 70 km s(-1). The outflow appears to originate from a single zone of gas of column density N(H) = 1.3 x 10(21) cm(-2) and ionization parameter log(xi/erg cm s(-1)) = 2.45. From the above measurements we calculate that the outflow is observed on parsec scales, within the likely range from 10 to 1000 pc, i.e., consistent with an origin in the narrow-line region. C1 [Reeves, J. N.] Univ Keele, Astrophys Grp, Sch Phys & Geog Sci, Keele ST5 5BG, Staffs, England. [Sambruna, R. M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Braito, V.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Eracleous, Michael] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Eracleous, Michael] Penn State Univ, Ctr Gravitat Wave Phys, University Pk, PA 16802 USA. RP Reeves, JN (reprint author), Univ Keele, Astrophys Grp, Sch Phys & Geog Sci, Keele ST5 5BG, Staffs, England. EM jnr@astro.keele.ac.uk OI Braito, Valentina/0000-0002-2629-4989 FU NASA through the Suzaku and Chandra programs; NSF [AST-0807993] FX This research has made use of data obtained from the High Energy Astrophysics Science Archive Research Center (HEASARC), provided by NASA's Goddard Space Flight Center. R. M. S. acknowledges support from NASA through the Suzaku and Chandra programs. M. E. thanks the NSF for support via grant AST-0807993. We thank Tahir Yaqoob for assistance with the Chandra data analysis. NR 33 TC 16 Z9 16 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 SEP 10 PY 2009 VL 702 IS 2 BP L187 EP L190 DI 10.1088/0004-637X/702/2/L187 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 487BN UT WOS:000269245500019 ER PT J AU Wang, W Ichii, K Hashimoto, H Michaelis, AR Thornton, PE Law, BE Nemani, RR AF Wang, Weile Ichii, Kazuhito Hashimoto, Hirofumi Michaelis, Andrew R. Thornton, Peter E. Law, Beverly E. Nemani, Ramakrishna R. TI A hierarchical analysis of terrestrial ecosystem model Biome-BGC: Equilibrium analysis and model calibration SO ECOLOGICAL MODELLING LA English DT Article DE Terrestrial ecosystem; Biome-BGC; Hierarchical analysis; Equilibrium analysis; Model calibration ID NET PRIMARY PRODUCTIVITY; CARBON STORAGE; REGIONAL APPLICATIONS; NORTHERN WISCONSIN; GENERAL-MODEL; UNITED-STATES; FLUX DATA; FORESTS; CLIMATE; ASSIMILATION AB The increasing complexity of ecosystem models represents a major difficulty in tuning model parameters and analyzing simulated results. To address this problem, this study develops a hierarchical scheme that simplifies the Biome-BGC model into three functionally cascaded tiers and analyzes them sequentially. The first-tier model focuses on leaf-level ecophysiological processes; it simulates evapotranspiration and photosynthesis with prescribed leaf area index (LAI). The restriction on LAI is then lifted in the following two model tiers, which analyze how carbon and nitrogen is cycled at the whole-plant level (the second tier) and in all litter/soil pools (the third tier) to dynamically support the prescribed canopy. in particular, this study analyzes the steady state of these two model tiers by a set of equilibrium equations that are derived from Biome-BGC algorithms and are based on the principle of mass balance. Instead of spinning-up the model for thousands of climate years, these equations are able to estimate carbon/nitrogen stocks and fluxes of the target (steady-state) ecosystem directly from the results obtained by the first-tier model. The model hierarchy is examined with model experiments at four AmeriFlux sites. The results indicate that the proposed scheme can effectively calibrate Biome-BCC to simulate observed fluxes of evapotranspiration and photosynthesis; and the carbon/nitrogen stocks estimated by the equilibrium analysis approach are highly consistent with the results of model simulations. Therefore, the scheme developed in this study may serve as a practical guide to calibrate/analyze Biome-BGC; it also provides an efficient way to solve the problem of model spin-up, especially for applications over large regions. The same methodology may help analyze other similar ecosystem models as well. (C) 2009 Elsevier B.V. All rights reserved. C1 [Wang, Weile] Care of Ramakrishna R Nemani, NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Wang, Weile; Hashimoto, Hirofumi; Michaelis, Andrew R.] Calif State Univ, Seaside, CA USA. [Ichii, Kazuhito] Fukushima Univ, Fac Symbiot Syst Sci, Fukushima, Japan. [Thornton, Peter E.] Oak Ridge Natl Lab, Oak Ridge, TN USA. [Law, Beverly E.] Oregon State Univ, Dept Forest Ecosyst & Soc, Corvallis, OR 97331 USA. RP Wang, W (reprint author), Care of Ramakrishna R Nemani, NASA, Ames Res Ctr, Mail Stop 242-4, Moffett Field, CA 94035 USA. EM weile.wang@gmail.com RI Ichii, Kazuhito/D-2392-2010; Thornton, Peter/B-9145-2012; OI Ichii, Kazuhito/0000-0002-8696-8084; Thornton, Peter/0000-0002-4759-5158; Law, Beverly/0000-0002-1605-1203 NR 52 TC 25 Z9 27 U1 0 U2 23 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0304-3800 EI 1872-7026 J9 ECOL MODEL JI Ecol. Model. PD SEP 10 PY 2009 VL 220 IS 17 BP 2009 EP 2023 DI 10.1016/j.ecolmodel.2009.04.051 PG 15 WC Ecology SC Environmental Sciences & Ecology GA 479LC UT WOS:000268659800007 ER PT J AU Huffman, GJ Adler, RF Bolvin, DT Gu, GJ AF Huffman, George J. Adler, Robert F. Bolvin, David T. Gu, Guojun TI Improving the global precipitation record: GPCP Version 2.1 SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID OUTGOING LONGWAVE RADIATION; DATASET AB The GPCP has developed Version 2.1 of its long-term (1979-present) global Satellite-Gauge (SG) data sets to take advantage of the improved GPCC gauge analysis, which is one key input. As well, the OPI estimates used in the pre-SSM/I era have been rescaled to 20 years of the SSM/I-era SG. The monthly, pentad, and daily GPCP products have been entirely reprocessed, continuing to require that the submonthly estimates sum to the monthly. Version 2.1 is close to Version 2, with the global ocean, land, and total values about 0%, 6%, and 2% higher, respectively. The revised long-term global precipitation rate is 2.68 mm/d. The corresponding tropical (25 degrees N-S) increases are 0%, 7%, and 3%. Long-term linear changes in the data tend to be smaller in Version 2.1, but the statistics are sensitive to the threshold for land/ocean separation and use of the pre-SSM/I part of the record. Citation: Huffman, G. J., R. F. Adler, D. T. Bolvin, and G. Gu (2009), Improving the global precipitation record: GPCP Version 2.1, Geophys. Res. Lett., 36, L17808, doi: 10.1029/2009GL040000. C1 [Huffman, George J.; Adler, Robert F.; Bolvin, David T.; Gu, Guojun] NASA, Goddard Space Flight Ctr, Lab Atmospheres Global Merge Dev Ctr, Global Precipitat Climatol Project, Greenbelt, MD 20771 USA. [Huffman, George J.; Bolvin, David T.] Sci Syst & Applicat Inc, Lanham, MD USA. [Adler, Robert F.; Gu, Guojun] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. RP Huffman, GJ (reprint author), NASA, Goddard Space Flight Ctr, Lab Atmospheres Global Merge Dev Ctr, Global Precipitat Climatol Project, Code 613-1, Greenbelt, MD 20771 USA. EM george.j.huffman@nasa.gov RI Huffman, George/F-4494-2014 OI Huffman, George/0000-0003-3858-8308 NR 10 TC 374 Z9 379 U1 4 U2 65 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 SEP 10 PY 2009 VL 36 AR L17808 DI 10.1029/2009GL040000 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 493RR UT WOS:000269756100006 ER PT J AU Murphy, DM Solomon, S Portmann, RW Rosenlof, KH Forster, PM Wong, T AF Murphy, D. M. Solomon, S. Portmann, R. W. Rosenlof, K. H. Forster, P. M. Wong, T. TI An observationally based energy balance for the Earth since 1950 SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID OCEAN HEAT-CONTENT; SEA-LEVEL RISE; RADIATION BUDGET; CLIMATE SYSTEM; VOLCANIC-ERUPTIONS; DECADAL CHANGES; TEMPERATURE; SENSITIVITY; FUTURE; VARIABILITY AB We examine the Earth's energy balance since 1950, identifying results that can be obtained without using global climate models. Important terms that can be constrained using only measurements and radiative transfer models are ocean heat content, radiative forcing by long-lived trace gases, and radiative forcing from volcanic eruptions. We explicitly consider the emission of energy by a warming Earth by using correlations between surface temperature and satellite radiant flux data and show that this term is already quite significant. About 20% of the integrated positive forcing by greenhouse gases and solar radiation since 1950 has been radiated to space. Only about 10% of the positive forcing (about 1/3 of the net forcing) has gone into heating the Earth, almost all into the oceans. About 20% of the positive forcing has been balanced by volcanic aerosols, and the remaining 50% is mainly attributable to tropospheric aerosols. After accounting for the measured terms, the residual forcing between 1970 and 2000 due to direct and indirect forcing by aerosols as well as semidirect forcing from greenhouse gases and any unknown mechanism can be estimated as -1.1 +/- 0.4 W m(-2) (1 sigma). This is consistent with the Intergovernmental Panel on Climate Change's best estimates but rules out very large negative forcings from aerosol indirect effects. Further, the data imply an increase from the 1950s to the 1980s followed by constant or slightly declining aerosol forcing into the 1990s, consistent with estimates of trends in global sulfate emissions. An apparent increase in residual forcing in the late 1990s is discussed. C1 [Murphy, D. M.; Solomon, S.; Portmann, R. W.; Rosenlof, K. H.] NOAA, Div Chem Sci, Earth Syst Res Lab, Boulder, CO 80303 USA. [Forster, P. M.] Univ Leeds, Sch Earth & Environm, Leeds LS2 9JT, W Yorkshire, England. [Wong, T.] NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Murphy, DM (reprint author), NOAA, Div Chem Sci, Earth Syst Res Lab, 325 Broadway, Boulder, CO 80303 USA. EM daniel.m.murphy@noaa.gov RI Portmann, Robert/C-4903-2009; Murphy, Daniel/J-4357-2012; Rosenlof, Karen/B-5652-2008; Forster, Piers/F-9829-2010; Manager, CSD Publications/B-2789-2015 OI Portmann, Robert/0000-0002-0279-6087; Murphy, Daniel/0000-0002-8091-7235; Rosenlof, Karen/0000-0002-0903-8270; Forster, Piers/0000-0002-6078-0171; FU NOAA; NASA FX This work was supported by NOAA base and climate change funding. T. Wong is supported by the NASA Science Mission Directorate through the CERES Project at the NASA Langley Research Center. We thank a number of people for digital versions of published data, including C. M. Domingues, J. A. Church, M. Ishii, and A. Koehl for ocean heat content; J. M. Gregory for radiative forcing; and T. Zhao for AVHRR optical depth. Sea level files were obtained from the CSIRO web site, stratospheric forcing history was obtained from the GISS web site, and global temperature history was obtained from the Hadley Centre web site. The CERES data are from the NASA Langley Atmospheric Science Data Center. Levitus et al. [2009] data are available from the NOAA Oceanographic Data Center (ftp://ftp. nodc. noaa. gov/pub/data. nodc/woa/DATA_ANALYSIS/3M_HEAT_CONTENT/DATA/basin/yearly/ h22-w0-700m. dat). NCEP Reanalysis data were provided by the NOAA ESRL Physical Sciences Division from their web site (http://www.cdc.noa.gov/). NR 64 TC 108 Z9 113 U1 2 U2 45 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 SEP 9 PY 2009 VL 114 AR D17107 DI 10.1029/2009JD012105 PG 14 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 493RX UT WOS:000269756700002 ER PT J AU Choi, Y Kim, J Eldering, A Osterman, G Yung, YL Gu, Y Liou, KN AF Choi, Yunsoo Kim, Jinwon Eldering, Annmarie Osterman, Gregory Yung, Yuk L. Gu, Yu Liou, K. N. TI Lightning and anthropogenic NOx sources over the United States and the western North Atlantic Ocean: Impact on OLR and radiative effects SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID TROPOSPHERIC CHEMISTRY; OZONE; PARAMETERIZATION; MODEL AB The migration of enhancements in NO2 concentration, outgoing longwave radiation (OLR), and radiative effects associated with the onset of the North American Monsoon in July 2005 has been investigated using satellite data and the Regional Chemical Transport Model (REAM). The satellite data include the tropospheric NO2 columns, tropospheric O-3 profiles, and OLR from OMI, TES and NOAA-16 satellite, respectively, for June and July 2005. The simulated OLR captures the spatial distribution of the remotely sensed OLR fields with relatively small biases (<= 5.7%) and high spatial correlations (R >= 0.88). This study reveals that the lightning-generated NOx exerts a larger, by up to a factor of three, impact on OLR (up to 0.35 Wm(-2)) and radiative effects (up to 0.55 Wm(-2)) by enhancing O-3 in the upper troposphere than anthropogenic NOx that increases O-3 in the lower troposphere, despite the fact that the lightning-generated NOx and O-3 are much smaller than those from the anthropogenic emissions. The radiative effect by lightning-derived upper tropospheric O-3 over the convective outflow regions is affected by the changes in lightning frequency. Thus the changes in convection due to global warming may alter the geographical distribution and magnitude of the radiative effect of lightning-derived O-3, and this paper is a first step in quantifying the current radiative impact. Citation: Choi, Y., J. Kim, A. Eldering, G. Osterman, Y. L. Yung, Y. Gu, and K. N. Liou (2009), Lightning and anthropogenic NOx sources over the United States and the western North Atlantic Ocean: Impact on OLR and radiative effects, Geophys. Res. Lett., 36, L17806, doi:10.1029/2009GL039381. C1 [Choi, Yunsoo; Eldering, Annmarie; Osterman, Gregory] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Kim, Jinwon; Gu, Yu; Liou, K. N.] Univ Calif Los Angeles, Dept Atmospher & Ocean Sci, Los Angeles, CA 90095 USA. [Kim, Jinwon; Gu, Yu; Liou, K. N.] Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA 90095 USA. [Yung, Yuk L.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. RP Choi, Y (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM yunsoo.choi@jpl.nasa.gov FU Jet Propulsion Laboratory at the California Institute of Technology; NASA; Korean Ministry of Environment [1700-1737-322-210-13] FX We thank all members of the OMI, TES and NOAA16 satellite team for providing the data. Special thanks to anonymous reviewers for helpful comments. This work was funded by the Jet Propulsion Laboratory at the California Institute of Technology, under contract to NASA and University of California Office of President, and Grant No. 1700-1737-322-210-13 from the Korean Ministry of Environment. NR 22 TC 17 Z9 17 U1 1 U2 9 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 SEP 4 PY 2009 VL 36 AR L17806 DI 10.1029/2009GL039381 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 492DT UT WOS:000269635500003 ER PT J AU Landerer, FW Jungclaus, JH Marotzke, J AF Landerer, Felix W. Jungclaus, Johann H. Marotzke, Jochem TI Long-term polar motion excited by ocean thermal expansion SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID GLOBAL SEA-LEVEL; EARTH ROTATION; MODEL; SIGNALS; ENIGMA; ICE AB Ocean warming is commonly considered unable to excite significant long-term trends in polar motion. Here, however, we argue that this assumption needs to be revised. We demonstrate that steric sea level rise leads to a distinct pattern of horizontal mass redistribution within ocean basins and hence to ocean bottom pressure changes that alter Earth's inertia tensor on decadal and longer time scales. Based on Earth system model simulations, we estimate that ocean warming leads to polar motion of 0.15 to 0.20 milliarcseconds per one millimeter of thermal sea level rise. This is equivalent to a polar motion rate of about 0.47 milliarcseconds per year towards 155 degrees W to 160 degrees W for current projections of steric sea level rise during the 21st century. The proposed polar motion signal is therefore not negligible in comparison to other decadal and secular signals, and should be accounted for in the interpretation of polar motion observations. Citation: Landerer, F. W., J. H. Jungclaus, and J. Marotzke (2009), Long-term polar motion excited by ocean thermal expansion, Geophys. Res. Lett., 36, L17603, doi:10.1029/2009GL039692. C1 [Landerer, Felix W.] Max Planck Inst Meteorol, Int Max Planck Res Sch Earth Syst Modelling, D-20146 Hamburg, Germany. RP Landerer, FW (reprint author), CALTECH, Jet Prop Lab, MS 238-600,4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM felix.w.landerer@jpl.nasa.gov OI Landerer, Felix/0000-0003-2678-095X FU Max Planck Society; International Max Planck Research School on Earth System Modelling FX This work was supported by the Max Planck Society and the International Max Planck Research School on Earth System Modelling. The simulations with ECHAM5/MPI-OM were performed at the DKRZ (Deutsches Klimarechenzentrum) in Hamburg, Germany; GFDL-CM2.1 data was downloaded from http://nomads.gfdl.noaa.gov. We thank GFDL for providing their data online, and Richard Gross, Erik Ivins, and the reviewers for their comments. NR 28 TC 1 Z9 1 U1 0 U2 3 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 SEP 4 PY 2009 VL 36 AR L17603 DI 10.1029/2009GL039692 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 492DT UT WOS:000269635500005 ER PT J AU Katzberg, SJ Dunion, J AF Katzberg, Stephen J. Dunion, Jason TI Comparison of reflected GPS wind speed retrievals with dropsondes in tropical cyclones SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID SURFACE; SIGNALS; DROPWINDSONDE AB In an earlier communication, data were presented that demonstrated that quasi-specular, L-Band reflection measurements could be used to infer ocean surface winds. Applying an indirect calibration technique, a mean square slope versus surface wind speed was developed and reported. Retrievals using this calibration showed that the resulting surface wind speeds were comparable with other measurements. This report extends the previous results by presenting direct comparisons between GPS dropwindsonde (dropsonde)-reported wind speeds and the Bi-static GPS wind speed retrievals for data sets acquired in 2008. Editing of the Bi-static GPS data will be discussed that takes into effect overland and inside-the-eye winnowing. Data will be presented with a regression line to determine the comparative relationship. It will be shown that good agreement exists between the reflected Bi-static GPS retrieved winds and those reported by the dropsondes when certain well-defined types of data are excluded. Citation: Katzberg, S. J., and J. Dunion (2009), Comparison of reflected GPS wind speed retrievals with dropsondes in tropical cyclones, Geophys. Res. Lett., 36, L17602, doi: 10.1029/2009GL039512. C1 [Katzberg, Stephen J.] NASA, Langley Res Ctr, Hampton, VA 23681 USA. [Dunion, Jason] NOAA, Atlantic Oceanog & Meteorol Lab, Hurricane Res Div, Miami, FL 33149 USA. RP Katzberg, SJ (reprint author), NASA, Langley Res Ctr, MS 473, Hampton, VA 23681 USA. EM stephen.j.katzberg@nasa.gov RI Dunion, Jason/B-1352-2014 OI Dunion, Jason/0000-0001-7489-0569 NR 11 TC 18 Z9 19 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 SEP 3 PY 2009 VL 36 AR L17602 DI 10.1029/2009GL039512 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 492CY UT WOS:000269633200001 ER PT J AU Grigoriev, AI Williams, RS Comtois, JM Damann, V Tachibana, S Nicogossian, AE Bogomolov, VV Pool, SL Sargsyan, AE Knowingkov, OL Doarn, CR AF Grigoriev, Anatoly I. Williams, Richard S. Comtois, Jean-Marc Damann, Volker Tachibana, Shoichi Nicogossian, Arnauld E. Bogomolov, Valery V. Pool, Sam L. Sargsyan, Ashot E. Knowingkov, Oleg L. Doarn, Charles R. TI Space medicine policy development for the International Space Station SO ACTA ASTRONAUTICA LA English DT Review DE Medical care; Medicine; Multilateral; Multinational; International medical policy; ISS AB Providing medical care capability in a multinational setting in space is a daunting challenge. As the International Space Station (ISS) has taken shape over the last decade the space medicine community of the ISS partners has established a foundation with which to govern medical policy, medial processes, and medical care during the ISS Program. This foundation was predicated on a rich history of bilateral and multilateral cooperation among space faring nations. Three key organizations were established, they include the agency or senior level Multilateral Medical Policy Board (MMPB), the Multilateral Space Medicine Board (MSMB), and the Multilateral Medical Operations Panel (MMOP). All three are staffed by senior medical personnel within each of the partner organizations of the ISS and each has specific roles and responsibilities. These three entities strive to protect the human element of spaceflight through highly effective interaction in a multilingual, multicultural program. This paper reviews the creation of this tripartite approach to the development of medical policy for ISS. (C) 2009 Elsevier Ltd. All rights reserved. C1 [Doarn, Charles R.] Univ Cincinnati, Dept Surg, Cincinnati, OH 45267 USA. [Grigoriev, Anatoly I.; Bogomolov, Valery V.] Inst Biomed Problems IBMP, Moscow, Russia. [Williams, Richard S.; Nicogossian, Arnauld E.; Doarn, Charles R.] NASA Headquarters, Off Chief Hlth & Med, Washington, DC USA. [Comtois, Jean-Marc] Canadian Space Agcy, St Hubert, PQ, Canada. [Damann, Volker] European Space Agcy, European Astronaut Ctr, Cologne, Germany. [Tachibana, Shoichi] Japan Aerosp Explorat Agcy, Tokyo, Japan. [Pool, Sam L.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Nicogossian, Arnauld E.] George Mason Univ, Fairfax, VA 22030 USA. [Sargsyan, Ashot E.] Wyle Integrated Sci & Engn Grp, Houston, TX USA. [Knowingkov, Oleg L.] NASA, Dynamac Corp, Kennedy Space Ctr, FL USA. RP Doarn, CR (reprint author), Univ Cincinnati, Dept Surg, 231 Albert Sabin Way,SRU 1446 ML 0558, Cincinnati, OH 45267 USA. EM charles.doarn@uc.edu NR 12 TC 4 Z9 4 U1 1 U2 11 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 SEP-OCT PY 2009 VL 65 IS 5-6 BP 603 EP 612 DI 10.1016/j.actaastro.2009.03.005 PG 10 WC Engineering, Aerospace SC Engineering GA 468WP UT WOS:000267855400001 ER PT J AU Laskin, RA Marr, JC AF Laskin, Robert A. Marr-, James C., IV TI SIM-PlanetQuest technology: A retrospective view SO ACTA ASTRONAUTICA LA English DT Article AB Optical interferometry will open new vistas for astronomy over the next decade. The Space Interferometry Mission (SIM-PlanetQuest), operating unfettered by the Earth's atmosphere, will offer unprecedented astrometric precision that promises the discovery of Earth-class extra-solar planets as well as a wealth of important astrophysics. Optical interferometers. also present severe technological challenges: laser metrology systems must perform with sub-nanometer precision; mechanical vibrations must be controlled to nanometers requiring orders of magnitude disturbance rejection; a multitude of actuators and sensors must operate flawlessly and in concert. The Jet Propulsion Laboratory, with the support of Lockheed Martin Advanced Technology Center (LM ATC) and Northrop Grumman Space Technology (NGST), has addressed these challenges with a technology development program that is now complete. Technology transfer to the SIM flight team is now well along and the project is proceeding toward Preliminary Design Review (PDR) with a quickening pace. (C) 2009 Published by Elsevier Ltd. C1 [Laskin, Robert A.; Marr-, James C., IV] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. RP Laskin, RA (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. EM Robert.A.Laskin@jpl.nasa.gov; James.C.Marr@jpl.nasa.gov NR 1 TC 0 Z9 0 U1 0 U2 1 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0094-5765 J9 ACTA ASTRONAUT JI Acta Astronaut. PD SEP-OCT PY 2009 VL 65 IS 5-6 BP 624 EP 642 DI 10.1016/j.actaastro.2009.01.043 PG 19 WC Engineering, Aerospace SC Engineering GA 468WP UT WOS:000267855400003 ER PT J AU Iessa, L Asmar, S Tortora, P AF Iessa, Luciano Asmar, Sami Tortora, Paolo TI MORE: An advanced tracking experiment for the exploration of Mercury with the mission BepiColombo SO ACTA ASTRONAUTICA LA English DT Article ID PLANET MERCURY; GRAVITY-FIELD; SPACECRAFT; ROTATION; LINKS AB Precise microwave tracking of interplanetary spacecraft has been a crucial tool in solar system exploration. Range and range rate measurements, the main observable quantities in spacecraft orbit determination and navigation, have been widely used to refine the dynamical model of the solar system and to probe planetary interiors. Thanks to the use of Ka-band and multifrequency radio links, a significant improvement in microwave tracking systems has been demonstrated by the radio science experiments of the Cassini mission to Saturn. The Cassini radio system has been used to carry out the most accurate test of general relativity to date. Further developments in the radio instrumentation have been recently started for the Mercury Orbiter Radio Experiment (MORE), selected for the ESA mission to Mercury, BepiColombo. MORE addresses the mission's scientific goals in geodesy, geophysics and fundamental physics. In addition, MORE will carry out a navigation experiment, aiming to a precise assessment of the orbit determination accuracies attainable with the use of the novel instrumentation. The key instrument is a Ka/Ka band digital transponder enabling a high phase coherence between uplink and downlink carriers and supporting a wideband ranging tone. The onboard instrumentation is complemented by a ground system based upon the simultaneous transmission and reception of multiple frequencies at X- and Ka-band. The new wideband ranging system is designed for an end-to-end accuracy of 20 cm using integration times of a few seconds. Two-way range rate measurements are expected to be accurate to 3 mu m/s, thanks to nearly complete cancellation or calibration of the propagation noise from interplanetary plasma and troposphere. We review the experimental configuration of the experiment and outline its scientific goals and expected results. (C) 2009 Published by Elsevier Ltd. C1 [Iessa, Luciano] Univ Roma La Sapienza, Dipartimento Ingn Aerospaziale & Astronaut, Rome, Italy. [Asmar, Sami] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Tortora, Paolo] Univ Bologna, DIEM Fac Ingn 2, I-40126 Bologna, Italy. RP Iessa, L (reprint author), Univ Roma La Sapienza, Dipartimento Ingn Aerospaziale & Astronaut, Rome, Italy. EM luciano.iess@uniromal.it; sami.asmar@jpl.nasa.gov; paolo.tortora@unibo.it RI Tortora, Paolo/J-6191-2012; OI Tortora, Paolo/0000-0001-9259-7673; IESS, Luciano/0000-0002-6230-5825 NR 24 TC 23 Z9 23 U1 0 U2 3 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 SEP-OCT PY 2009 VL 65 IS 5-6 BP 666 EP 675 DI 10.1016/j.actaastro.2009.01.049 PG 10 WC Engineering, Aerospace SC Engineering GA 468WP UT WOS:000267855400007 ER PT J AU Quadrelli, MB Mettler, E Soloway, D Kelkar, A AF Quadrelli, Marco B. Mettler, Edward Soloway, Don Kelkar, Atul TI Controls structure interaction on the Jupiter Icy Moons Orbiter SO ACTA ASTRONAUTICA LA English DT Article DE Spacecraft dynamics; Flexible spacecraft; Attitude control; Pointing AB The baseline Jupiter Icy Moons Orbiter (JIMO) spacecraft presented challenging controls-structure interactions caused by having to accurately and simultaneously point the existing multiple articulated payloads (high-gain antenna, scan platform) which are mounted on a large flexible base. Sensitivity analyses and simulation studies were carried out using complex finite element models describing the vehicle's dynamics. The results of these studies indicate that: (1) the attitude controller bandwidth (BW) should be less than 0.01 Hz for stable pointing control at the end of a slew with fine thrusters; (2) to achieve a 90 degrees slew maneuver in 2 h the attitude controller BW should be greater than 0.0001 Hz with coarse thrusters; and (3) the first natural frequency of the flexible vehicle should be in the range of I Hz, to avoid potential interactions with other flexible modes. A dissipative controller ensures the stability robustness during large-angle maneuvers of the articulated payloads at high speeds when linearity assumptions are likely to be incorrect and nonlinearity in dynamics may be significant. An advantage of the proposed controller is that the closed-loop stability is not only robust to unmodeled dynamics but also to actuator nonlinearities as expected in the proposed gimbals for JIMO. (C) 2008 Elsevier Ltd. All rights reserved. C1 [Quadrelli, Marco B.; Mettler, Edward] CALTECH, Jet Prop Lab, Guidance & Control Anal Grp, Pasadena, CA 91109 USA. [Soloway, Don] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Kelkar, Atul] Iowa State Univ, Dept Mech & Aerosp Engn, Ames, IA 50011 USA. RP Quadrelli, MB (reprint author), CALTECH, Jet Prop Lab, Guidance & Control Anal Grp, Mail Stop 198-326,4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Marco.B.Quadrelli@jpl.nasa.gov NR 8 TC 0 Z9 0 U1 0 U2 2 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 SEP-OCT PY 2009 VL 65 IS 5-6 BP 766 EP 786 DI 10.1016/j.actaastro.2009.03.013 PG 21 WC Engineering, Aerospace SC Engineering GA 468WP UT WOS:000267855400016 ER PT J AU Russell, MJ AF Russell, Michael J. TI The Alkaline Solution to the Emergence of Life: Energy, Entropy and Early Evolution (vol 55, pg 133, 2007) SO ACTA BIOTHEORETICA LA English DT Correction C1 CALTECH, Jet Prop Lab, Planetary Sci & Life Detect Sect 3220, Pasadena, CA 91109 USA. RP Russell, MJ (reprint author), CALTECH, Jet Prop Lab, Planetary Sci & Life Detect Sect 3220, 4800 Oak Grove Dr,MS 183-601, Pasadena, CA 91109 USA. EM Michael.J.Russell@jpl.nasa.gov NR 1 TC 0 Z9 0 U1 3 U2 6 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0001-5342 J9 ACTA BIOTHEOR JI Acta Biotheor. PD SEP PY 2009 VL 57 IS 3 BP 389 EP 394 DI 10.1007/s10441-007-9026-5 PG 6 WC Mathematical & Computational Biology SC Mathematical & Computational Biology GA 483OE UT WOS:000268976100006 ER PT J AU Willis, P Ries, JC Zelensky, NP Soudarin, L Fagard, H Pavlis, EC Lemoine, FG AF Willis, P. Ries, J. C. Zelensky, N. P. Soudarin, L. Fagard, H. Pavlis, E. C. Lemoine, F. G. TI DPOD2005: An extension of ITRF2005 for Precise Orbit Determination SO ADVANCES IN SPACE RESEARCH LA English DT Article DE DORIS; ITRF2005; Coordinate time series; Arequipa; Gavdos; Precision orbit determination ID TERRESTRIAL REFERENCE FRAME; INTERNATIONAL DORIS SERVICE; TECTONIC PLATE MOTIONS; SEA-LEVEL; SYSTEM; TOPEX/POSEIDON; NETWORK; DEFORMATIONS; KINEMATICS; FAULT AB For Precise Orbit Determination of altimetry missions, we have computed a data set of DORIS station coordinates defined for specific time intervals called DPOD2005. This terrestrial reference set is an extension of ITRF2005. However, it includes all new DORIS stations and is more reliable, as we disregard stations with large velocity formal errors as they could contaminate POD Computations in the near future. About 1/4 of the station coordinates need to be defined as they do not appear in the original ITRF2005 realization. These results were verified with available DORIS and GPS results, as the integrity of DPOD2005 is almost as critical as its accuracy. Besides station coordinates and velocities, we also provide additional information such as periods for which DORIS data should be disregarded for specific DORIS stations, and epochs of coordinate and velocity discontinuities (related to either geophysical events, equipment problem or human intervention). The DPOD model was tested for orbit determination for TOPEX/Poseidon (T/P), Jason-1 and Jason-2. Test results show DPOD2005 offers improvement over the original ITRF2005, improvement that rapidly and significantly increases after 2005. Improvement is also significant for the early T/P cycles indicating improved station velocities in the DPOD2005 model and a more complete station set. Following 2005 the radial accuracy and centering of the ITRF2005-original orbits rapidly degrades due to station loss. (C) 2009 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 [Willis, P.] Inst Geog Natl, Direct Tech, F-94160 St Mande, France. [Willis, P.] Inst Phys Globe, Paris, France. [Ries, J. C.] Univ Texas Austin, Ctr Space Res, Austin, TX 78712 USA. [Zelensky, N. P.] SGT Inc, Greenbelt, MD 20771 USA. [Soudarin, L.] Collecte Localisat Satellites, F-31520 Ramonville St Agne, France. [Fagard, H.] Inst Geog Natl, Serv Geodesie & Nivellement, F-94160 St Mande, France. [Pavlis, E. C.; Lemoine, F. G.] NASA, Goddard Space Flight Ctr, Planetary Geodynam Lab, Greenbelt, MD 20771 USA. [Pavlis, E. C.] Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, Baltimore, MD 21250 USA. RP Willis, P (reprint author), Inst Geog Natl, Direct Tech, 2 Ave Pasteur,BP 68, F-94160 St Mande, France. EM willis@ipgp.jussieu.fr RI Willis, Pascal/A-8046-2008; Lemoine, Frank/D-1215-2013 OI Willis, Pascal/0000-0002-3257-0679; FU Centre National d'Etudes Spatiales (CNES) FX This paper is IPGP contribution number 2496. This work was supported by the Centre National d'Etudes Spatiales (CNES). It is based on observations with DORIS embarked on TOPEX/Poseidon, SPOT-2, SPOT-3, SPOT-4, SPOT-5, ENVISAT, Jason-1 and Jason-2 and satellites. NR 45 TC 40 Z9 42 U1 0 U2 2 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 SEP 1 PY 2009 VL 44 IS 5 BP 535 EP 544 DI 10.1016/j.asr.2009.04.018 PG 10 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA 489LC UT WOS:000269420600001 ER PT J AU Hanada, T Liou, JC Nakajima, T Stansbery, E AF Hanada, T. Liou, J. -C. Nakajima, T. Stansbery, E. TI Outcome of recent satellite impact experiments SO ADVANCES IN SPACE RESEARCH LA English DT Article DE Space debris; Impact fragmentation ID LOW-VELOCITY; BREAKUP MODEL; SPACECRAFT; NASA AB This paper summarizes three micro-satellite impact tests completed in early 2007 through collaboration between Kyushu University and the NASA Orbital Debris Program Office. The previous experiments completed in late 2005 aimed to compare low- and hypervelocity impacts on identical target micro-satellites, whereas the new tests used larger micro-satellites as targets and aimed to investigate the effects of impact directions. Three identical micro-satellites equipped with fully functional electronic devices were prepared as targets. Their dimensions were 20 cm by 20 cm by 20 cm, and the mass of each was approximately 1.3 kg. Aluminum alloy solid spheres, with a diameter of 3 cm and a mass of 39 g, were prepared as projectiles. The impact velocity was approximately 1.7 km/s. The impact tests were carried out using the two-stage light gas gun at the Kyushu Institute of Technology. All target micro-satellites were completely fragmented, but there were noticeable differences among the three sets of fragments due to the different impact directions. More than 1000 fragments from each test were collected, measured, photographed, and documented with material descriptions. Preliminary results of the new data and comparisons with the previous data will be presented in the paper. (C) 2009 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 [Hanada, T.] Kyushu Univ, Dept Aeronaut & Astronaut, Nishi Ku, Fukuoka 8190395, Japan. [Hanada, T.; Nakajima, T.] ISAS JAXA, Sagamihara, Kanagawa 2298510, Japan. [Liou, J. -C.; Stansbery, E.] NASA, JSC, Houston, TX 77058 USA. RP Hanada, T (reprint author), Kyushu Univ, Dept Aeronaut & Astronaut, Nishi Ku, 744 Motooka, Fukuoka 8190395, Japan. EM toshi@aero.kyushu-u.ac.jp NR 17 TC 5 Z9 8 U1 1 U2 5 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 SEP 1 PY 2009 VL 44 IS 5 BP 558 EP 567 DI 10.1016/j.asr.2009.04.016 PG 10 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA 489LC UT WOS:000269420600003 ER PT J AU Echer, E Tsurutani, BT Guarnieri, FL AF Echer, Ezequiel Tsurutani, Bruce T. Guarnieri, Fernando L. TI Solar and interplanetary origins of the November 2004 superstorms SO ADVANCES IN SPACE RESEARCH LA English DT Article DE Geomagnetic storms; Solar flares; CMEs; Shocks; Magnetic clouds ID 1-AU ARRIVAL AB During the first half of November 2004, many solar flares and coronal mass ejections (CMEs) were associated with solar active region (AR) 10696. This paper attempts to identify the solar and interplanetary origins of two superstorms which occurred on 8 and 10 November with peak intensities of Dst = -373 nT and -289 nT, respectively. Southward interplanetary magnetic fields within a magnetic cloud (MC), and a sheath + MC were the causes of these two superstorms, respectively. Two different CME propagation models [Gopalswamy, N., Yashiro, S., Kaiser, M.L. et al. Predicting the 1-AU arrival times of coronal mass ejections. J. Geophys. Res. 106, 29207-29219, 2001; Gopalswamy, N.S., Lara, A., Manoharan, P.K. et al. An empirical model to predict the 1-AU arrival of interplanetary shocks. Adv. Space Res. 36, 2289-2294, 2005] were employed to attempt to identify the solar sources. It is found that the models identify several potential CMEs as possible sources for each of the superstorms. The two Gopalswamy et al. models give the possible sources for the first superstorm as CMEs on 2330 UT 4 November 2004 or on 1454 UT 5 November 2004. For the second superstorm, the possible solar source was a CME that on 0754 UT 5 November 2004 or one that occurred on 1206 UT 5 November 2004. We note that other propagation models sometimes agree and other times disagree with the above results. It is concluded that during high solar/interplanetary activity intervals such as this one, the exact solar source is difficult to identify. More refined propagation models are needed. (C) 2009 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 [Echer, Ezequiel] INPE, Sao Jose Dos Campos, SP, Brazil. [Tsurutani, Bruce T.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Guarnieri, Fernando L.] Univ Vale Paraiba UNIVAP, Sao Jose Dos Campos, SP, Brazil. RP Echer, E (reprint author), INPE, Ave Astronautas 1758,POB 515, Sao Jose Dos Campos, SP, Brazil. EM eecher@dge.inpe.br FU Jet Propulsion Laboratory; California Institute of Technology; CNPq [PQ-300104/2005-7, 470706/2006-6]; FAPESP [2008/05607-2] FX Portions of this research were performed at the Jet Propulsion Laboratory, California Institute of Technology under contract with NASA. E.E. would like to thank CNPq agency (PQ-300104/2005-7 and 470706/2006-6) and F.L.G. and B.T.T. thank to FAPESP (Project 2008/05607-2) for financial supports. We thank SOHO and ACE science teams for make solar and solar wind data available. NR 21 TC 2 Z9 2 U1 0 U2 0 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 SEP 1 PY 2009 VL 44 IS 5 BP 615 EP 620 DI 10.1016/j.asr.2009.05.003 PG 6 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA 489LC UT WOS:000269420600010 ER PT J AU Sietzen, F Weiler, EJ AF Sietzen, Frank Weiler, Edward J. TI Conversations with Edward J. Weiler SO AEROSPACE AMERICA LA English DT Editorial Material C1 [Weiler, Edward J.] Goddard Space Flight Ctr, Greenbelt, MD USA. [Weiler, Edward J.] NASAs Space Sci Enterprise, Washington, DC USA. [Weiler, Edward J.] NASA Headquarters, Astron Search Origins Program, Washington, DC USA. [Weiler, Edward J.] NASA Headquarters, Ultraviolet Visible & Gravitat Astrophys Div, Washington, DC USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU AMER INST AERONAUT ASTRONAUT PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0740-722X J9 AEROSPACE AM JI Aerosp. Am. PD SEP PY 2009 VL 47 IS 8 BP 12 EP 15 PG 4 WC Engineering, Aerospace SC Engineering GA 493MQ UT WOS:000269741400006 ER PT J AU Choi, JI Edwards, JR Baurle, RA AF Choi, Jung-Il Edwards, Jack R. Baurle, Robert A. TI Compressible Boundary-Layer Predictions at High Reynolds Number Using Hybrid LES/RANS Methods SO AIAA JOURNAL LA English DT Article; Proceedings Paper CT AIAA 38th Fluid Dynamics Conference and Exhibit CY JUN 23-26, 2008 CL Seattle, WA SP AIAA ID LARGE-EDDY SIMULATION; DIRECT NUMERICAL-SIMULATION; NAVIER-STOKES SIMULATIONS; PRESSURE-GRADIENT; TURBULENCE STRUCTURE; FLOWS; WALL; ANEMOMETER; CURVATURE; MODELS AB Simulations of compressible boundary-layer How at three different Reynolds numbers (Re-delta = 5.59 x 10(4), 1.78 x 10(5), and 1.58 x 10(6)) are performed using a hybrid large-eddy simulation/Reynolds-averaged Navier-Stokes method. Variations in the recycling/rescaling method, the higher order extension, the choice of primitive variables, the Reynolds-averaged Navier-Stokes to large eddy simulation transition parameters, and the mesh resolution are considered in order to assess the model. The results indicate that the present model can provide good predictions of the mean-flow properties, second-moment statistics, and structural features of the boundary layers considered. Normalized turbulent statistics in the outer layer are found to be independent of Reynolds number, similar to incompressible turbulent boundary layers. C1 [Choi, Jung-Il; Edwards, Jack R.] N Carolina State Univ, Dept Mech & Aerosp Engn, Raleigh, NC 27695 USA. [Baurle, Robert A.] NASA, Hyperson Airbreathing Prop Branch, Langley Res Ctr, Hampton, VA 23681 USA. RP Choi, JI (reprint author), N Carolina State Univ, Dept Mech & Aerosp Engn, Raleigh, NC 27695 USA. EM jungil_choi@ncsu.edu; jredward@ncsu.edu; robert.a.baurle@nasa.gov RI Choi, Jung-il/H-1013-2011 NR 44 TC 13 Z9 14 U1 0 U2 3 PU AMER INST AERONAUTICS ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0001-1452 EI 1533-385X J9 AIAA J JI AIAA J. PD SEP PY 2009 VL 47 IS 9 BP 2179 EP 2193 DI 10.2514/1.41598 PG 15 WC Engineering, Aerospace SC Engineering GA 495NB UT WOS:000269898800017 ER PT J AU Rumsey, CL Greenblatt, D AF Rumsey, Christopher L. Greenblatt, David TI Flow Control Predictions Using Unsteady Reynolds-Averaged Navier-Stokes Modeling: A Parametric Study SO AIAA JOURNAL LA English DT Article ID WALL-MOUNTED HUMP; SEPARATION CONTROL C1 [Rumsey, Christopher L.] NASA, Computat Aerosci Branch, Langley Res Ctr, Hampton, VA 23681 USA. [Greenblatt, David] Technion Israel Inst Technol, Fac Mech Engn, IL-32000 Haifa, Israel. RP Rumsey, CL (reprint author), NASA, Computat Aerosci Branch, Langley Res Ctr, Mail Stop 128, Hampton, VA 23681 USA. NR 15 TC 1 Z9 1 U1 0 U2 1 PU AMER INST AERONAUT ASTRONAUT PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0001-1452 J9 AIAA J JI AIAA J. PD SEP PY 2009 VL 47 IS 9 BP 2259 EP 2262 DI 10.2514/1.41855 PG 4 WC Engineering, Aerospace SC Engineering GA 495NB UT WOS:000269898800025 ER PT J AU Anderes, E Yu, B Jovanovic, V Moroney, C Garay, M Braverman, A Clothiaux, E AF Anderes, E. Yu, B. Jovanovic, V. Moroney, C. Garay, M. Braverman, A. Clothiaux, E. TI MAXIMUM LIKELIHOOD ESTIMATION OF CLOUD HEIGHT FROM MULTI-ANGLE SATELLITE IMAGERY SO ANNALS OF APPLIED STATISTICS LA English DT Article DE Random fields; cloud height estimation; super resolution; multiangle imaging spectroradiometer; depth-of-field; maximum likelihood estimation ID RANDOM FIELD; SUPERRESOLUTION; STRATOCUMULUS; MATRICES; STEREO; SUMS; ROW AB We develop a new estimation technique for recovering depth-of-field from multiple stereo images. Depth-of-field is estimated by determining the shift in image location resulting from different camera viewpoints. When this shift is not divisible by pixel width, the multiple stereo images can be combined to form a super-resolution image. By modeling this super-resolution image as a realization of a random field, one can view the recovery of depth as a likelihood estimation problem. We apply these modeling techniques to the recovery of cloud height from multiple viewing angles provided by the MISR instrument on the Terra Satellite. Our efforts are focused on a two layer cloud ensemble where both layers are relatively planar, the bottom layer is optically thick and textured, and the top layer is optically thin. Our results demonstrate that with relative ease, we get comparable estimates to the M2 stereo matcher which is the same algorithm used in the current MISR standard product (details can be found in [IEEE Transactions oil Geoscience and Remote Sensing 40 (2002) 1547-1559]). Moreover, our techniques provide the possibility of modeling all of the MISR data in a unified way for cloud height estimation. Research is underway to extend this framework for fast, quality global estimates of cloud height. C1 [Anderes, E.] Univ Calif Davis, Dept Stat, Davis, CA 95616 USA. [Jovanovic, V.; Moroney, C.; Braverman, A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Yu, B.] Univ Calif Berkeley, Dept Stat, Berkeley, CA 94720 USA. [Garay, M.] Raytheon Corp, Intelligence & Informat Syst, Pasadena, CA 91109 USA. [Clothiaux, E.] Penn State Univ, Dept Meteorol, University Pk, PA 16802 USA. RP Anderes, E (reprint author), Univ Calif Davis, Dept Stat, 4214 Math Sci Bldg, Davis, CA 95616 USA. EM anderes@stat.ucdavis.edu; binyu@stat.berkeley.edu; veljko.m.jovanovic@jpl.nasa.gov; Catherine.Moroney@jpl.nasa.gov; Michael.Garay@jpl.nasa.gov; Amy.Braverman@jpl.nasa.gov; cloth@essc.psu.edu FU NSF [DMS-05-03227, NSF DMS-06-05165, ARO W911NF-05-1-0104, NSFC-60628102]; JPL Grant [1302389]; ARO; Guggenheim Fellowship in 2006; MSRA FX Supported in part by Grants NSF DMS-06-05165, ARO W911NF-05-1-0104, NSFC-60628102, a Guggenheim Fellowship in 2006 and a grant from MSRA. NR 20 TC 1 Z9 2 U1 0 U2 4 PU INST MATHEMATICAL STATISTICS PI CLEVELAND PA 3163 SOMERSET DR, CLEVELAND, OH 44122 USA SN 1932-6157 J9 ANN APPL STAT JI Ann. Appl. Stat. PD SEP PY 2009 VL 3 IS 3 BP 902 EP 921 DI 10.1214/09-AOAS243 PG 20 WC Statistics & Probability SC Mathematics GA 522EF UT WOS:000271979900002 ER PT J AU Nuevo, M Milam, SN Sandford, SA Elsila, JE Dworkin, JP AF Nuevo, Michel Milam, Stefanie N. Sandford, Scott A. Elsila, Jamie E. Dworkin, Jason P. TI Formation of Uracil from the Ultraviolet Photo-Irradiation of Pyrimidine in Pure H2O Ices SO ASTROBIOLOGY LA English DT Article DE Pyrimidine; Nucleobases; Interstellar ices; Cometary ices; Molecular processes; Prebiotic chemistry ID POLYCYCLIC AROMATIC-HYDROCARBONS; MIDINFRARED LABORATORY SPECTRA; SIDE-GROUP ADDITION; MURCHISON METEORITE; HETEROCYCLIC-COMPOUNDS; AMINO-ACIDS; BUTYLDIMETHYLSILYL DERIVATIVES; INTERSTELLAR-MOLECULES; RADIATION-FIELD; ION-BOMBARDMENT AB The detection of nucleobases in carbonaceous chondrites such as Murchison supports the scenario in which extraterrestrial organic molecules could have contributed to the origin of life on Earth. However, such large molecules have not been observed to date in astrophysical environments, in particular, comets and the interstellar medium (ISM). The physico-chemical conditions under which nucleobases and, more generally, N-heterocycles were formed are unknown, as are their mechanisms of formation. In this work, H2O: pyrimidine ice mixtures were irradiated with UV photons under interstellar/cometary-relevant conditions to study the formation of pyrimidine derivatives, including the nucleobase uracil. Liquid and gas chromatography analyses of the samples produced in our experiments revealed the presence of numerous photoproducts among which 4(3H)-pyrimidone and uracil could be conclusively identified. The photostability of pyrimidine against UV photons was also studied, and we showed that it would survive from the ISM to the solar nebula if formed and preserved in ice mantles on the surface of cold grains. We propose pathways for the formation of 4(3H)-pyrimidone and uracil under astrophysically relevant conditions and discuss the possibility for such molecules to survive from the ISM to their delivery to Earth and other Solar System bodies. C1 [Nuevo, Michel; Milam, Stefanie N.; Sandford, Scott A.] NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA. [Milam, Stefanie N.] SETI Inst, Mountain View, CA USA. [Elsila, Jamie E.; Dworkin, Jason P.] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA. RP Nuevo, M (reprint author), NASA, Ames Res Ctr, Div Space Sci, Mail Stop 245-6, Moffett Field, CA 94035 USA. EM michel.nuevo-1@nasa.gov RI Elsila, Jamie/C-9952-2012; Milam, Stefanie/D-1092-2012; Dworkin, Jason/C-9417-2012 OI Milam, Stefanie/0000-0001-7694-4129; Dworkin, Jason/0000-0002-3961-8997 FU NASA FX This work was supported by NASA grants from the "Astrobiology'' and "Origins of Solar Systems'' programs. M. N., S. N. M., and S. A. S. would also like to acknowledge excellent technical support from R. Walker and thank M. Levit for his contribution to the preparation of the samples and standards for high-performance liquid chromatography analysis. NR 52 TC 47 Z9 47 U1 2 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 SEP PY 2009 VL 9 IS 7 BP 683 EP 695 DI 10.1089/ast.2008.0324 PG 13 WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics; Geology GA 498JE UT WOS:000270134600008 PM 19778279 ER PT J AU Marion, GH Hoflich, P Gerardy, CL Vacca, WD Wheeler, JC Robinson, EL AF Marion, G. H. Hoeflich, P. Gerardy, C. L. Vacca, W. D. Wheeler, J. C. Robinson, E. L. TI A CATALOG OF NEAR-INFRARED SPECTRA FROM TYPE Ia SUPERNOVAE SO ASTRONOMICAL JOURNAL LA English DT Article DE cosmology: observations; infrared: general; line: identification; supernovae: general ID LIGHT-CURVE SHAPES; THERMONUCLEAR SUPERNOVAE; WHITE-DWARFS; SN 1994D; DETONATION; SPECTROPOLARIMETRY; NUCLEOSYNTHESIS; SPECTROGRAPH; CONSTANT; ROTATION AB We present 41 near-infrared (NIR, 0.7-2.5 mu m) spectra from normal Type Ia supernovae (SNe Ia) obtained at epochs ranging from 14 days before to 75 days with respect to the maximum light date in the V band. All data were obtained at the Infrared Telescope Facility using the SpeX instrument. We identify many spectral features, measure the Doppler velocities, and discuss the chemical distribution of explosion products in SNe Ia. We describe procedures for smoothing data, fitting continua, and measuring absorption features to ensure consistency for measurement and analysis. This sample provides the first opportunity to examine and compare a large number of SNe Ia in this wavelength region. NIR data are a rich source of information about explosion products whose signatures are blended or obscured in other spectral regions and NIR observations probe a greater radial depth than optical wavelengths. We analyze similarities and differences in the spectra and we show that the progressive development of spectral features for normal SNe Ia in the NIR is consistent with time. We confirm the presence of O I, Mg II, Ca II, Si II, Fe II, and Co II in these SNe. Possible identifications are made for S I, Si III, Mn II, and Fe III. There is no evidence in these data for H I, He I, C I, or C II. As the explosion products expand and cool, progressively deeper layers are revealed. Thus, a time sequence of spectra examines the chemical structure and provides direct evidence of the physical properties of SNe Ia from the outer layers to deep inside the SN. Measured Doppler velocities indicate that burning products in SNe Ia are distributed in distinct layers with no large-scale mixing. Carbon is not detected in these data, in agreement with previous results with NIR data establishing very low limits on carbon abundance in SNe Ia. Carbon burning products, O and Mg, are plentiful in the outer layers suggesting that the entire progenitor is burned in the explosion. The data provide a resource for investigations of cross-correlations with other data libraries that may further constrain SN Ia physics and improve the effectiveness of SNe Ia as cosmological distance indicators. C1 [Marion, G. H.; Wheeler, J. C.; Robinson, E. L.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Hoeflich, P.; Gerardy, C. L.] Florida State Univ, Dept Phys, Tallahassee, FL 32306 USA. [Vacca, W. D.] NASA, Ames Res Ctr, SOFIA USRA, Moffett Field, CA 94035 USA. RP Marion, GH (reprint author), Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. NR 38 TC 38 Z9 38 U1 0 U2 2 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 SEP PY 2009 VL 138 IS 3 BP 727 EP 757 DI 10.1088/0004-6256/138/3/727 PG 31 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 490OF UT WOS:000269509700002 ER PT J AU Braito, V Reeves, JN Della Ceca, R Ptak, A Risaliti, G Yaqoob, T AF Braito, V. Reeves, J. N. Della Ceca, R. Ptak, A. Risaliti, G. Yaqoob, T. TI A Suzaku observation of the ULIRG IRAS19254-7245: discerning the AGN component SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE galaxies: active; galaxies: individual: IRAS 19254-7245; galaxies: Seyfert; X-rays: galaxies ID ULTRALUMINOUS INFRARED GALAXIES; ACTIVE GALACTIC NUCLEUS; STAR-FORMATION RATE; X-RAY-SPECTRA; BRIGHT SERENDIPITOUS SURVEY; FORMATION RATE INDICATOR; XMM-NEWTON OBSERVATIONS; 2-10 KEV LUMINOSITY; BLACK-HOLES; STARBURST GALAXIES AB We discuss a long Suzaku observation of IRAS 19254-7245 (also known as the Superantennae), one of the brightest and well studied Ultra Luminous Infrared Galaxies in the local Universe. This long observation provided the first detection of IRAS 19254-7245 above 10 keV, and a measurement of a 15-30 keV flux of similar to 5 x 10(-12) erg cm(-2) s(-1). The detection above 10 keV has allowed us to determine, for the first time, the intrinsic luminosity of the AGN hosted in IRAS 19254-7245, which is strongly absorbed (N-H similar to 3 x 10(24) cm(-2)) and has an intrinsic luminosity (L(2 - 10 keV) similar to 3 x 10(44) erg s(-1)) in the QSO regime. The 2-10 keV spectrum of IRAS 19254-7245 is remarkably hard (Gamma similar to 1.2), and presents a strong iron line (EW similar to 0.7 keV), clearly suggesting that below 10 keV we observe only reprocessed radiation. Since the energy of the Fe K emission is found to be similar to 6.7 keV, consistent with He-like Fe, and its EW is too high to be explained by a starburst-dominated scenario, we suggest that the 2-10 keV emission of IRAS 19254-7245 is dominated by reflection/scattering from highly ionized matter. Within this latter scenario, we found that the photon index of the illuminating source is Gamma = 1.87(-0.28)(+0.11) in excellent agreement with the mean value found for radio quiet unobscured AGN. C1 [Braito, V.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Braito, V.; Reeves, J. N.; Ptak, A.; Yaqoob, T.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Reeves, J. N.] Keele Univ, Sch Phys & Geog Sci, Astrophys Grp, Keele ST5 5BG, Staffs, England. [Della Ceca, R.] INAF Osservatorio Astron Brera, I-20121 Milan, Italy. [Ptak, A.; Yaqoob, T.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Risaliti, G.] INAF Osservatorio Astrofis Arcetri, I-50125 Florence, Italy. [Risaliti, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Braito, V (reprint author), Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. EM bv67@star.le.ac.uk RI Ptak, Andrew/D-3574-2012; XRAY, SUZAKU/A-1808-2009; OI Risaliti, Guido/0000-0002-3556-977X; Della Ceca, Roberto/0000-0001-7551-2252; Braito, Valentina/0000-0002-2629-4989 FU UK STFC research council; ASI (Agenzia Spaziale Italiana) [I/088/06/0]; National Aeronautics and Space Administration through the NASA [NNG04GB78A] FX V. B. acknowledge support from the UK STFC research council. R. D. C. acknowledge financial support from the ASI (Agenzia Spaziale Italiana) grant I/088/06/0. Support for this work was provided by the National Aeronautics and Space Administration through the NASA grant NNG04GB78A. We thank the anonymous referee for his/her useful comments, which have improved this paper. NR 49 TC 13 Z9 13 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 SEP PY 2009 VL 504 IS 1 BP 53 EP 59 DI 10.1051/0004-6361/200811516 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 493HU UT WOS:000269728200006 ER PT J AU Cappi, M Tombesi, F Bianchi, S Dadina, M Giustini, M Malaguti, G Maraschi, L Palumbo, GGC Petrucci, PO Ponti, G Vignali, C Yaqoob, T AF Cappi, M. Tombesi, F. Bianchi, S. Dadina, M. Giustini, M. Malaguti, G. Maraschi, L. Palumbo, G. G. C. Petrucci, P. O. Ponti, G. Vignali, C. Yaqoob, T. TI X-ray evidence for a mildly relativistic and variable outflow in the luminous Seyfert 1 galaxy Mrk 509 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE galaxies: active; X-rays: galaxies; accretion, accretion disks; thechniques: spectroscopic; line: formation; galaxies: Seyfert ID ACTIVE GALACTIC NUCLEI; ACCRETION DISK WINDS; XMM-NEWTON; ABSORPTION-LINES; PHOTOIONIZED GAS; BLACK-HOLE; FE LINE; SPECTRUM; AGN; ABSORBERS AB Context. There is growing evidence for the presence of blueshifted Fe K absorption lines in a number of radio-quiet AGNs and QSOs. These may be fundamental to probe flow dynamics near supermassive black holes. Aims. Here we aim to verify and better characterise the existence of such Fe K absorption at similar to 8-10 keV in the luminous Seyfert 1 galaxy Mrk 509, one of the most promising target for these studies. Methods. We present a comprehensive spectral analysis of the six XMM-Newton observations of the source (for a total of similar to 200 ks), focusing on a detailed and systematic search for absorption features in the high-energy data. Results. We detect several absorption features at rest-frame energies similar to 8-8.5 keV and similar to 9.7 keV. The lines are consistent with being produced by H-like iron K alpha and K beta shell absorptions associated with an outflow with a mildly relativistic velocity of similar to 0.14-0.2 c. The lines are found to be variable in energy and, marginally, in intensity, implying variations in either the column density, geometry and/or ionization structure of the outflow are common. C1 [Cappi, M.; Tombesi, F.; Dadina, M.; Giustini, M.; Malaguti, G.] INAF IASF Bologna, I-40129 Bologna, Italy. [Tombesi, F.; Giustini, M.; Palumbo, G. G. C.; Vignali, C.] Univ Bologna, Dipartmento Astron, I-40127 Bologna, Italy. [Tombesi, F.; Yaqoob, T.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Tombesi, F.; Yaqoob, T.] NASA, Goddard Space Flight Ctr, High Energy Astrophys Lab, Greenbelt, MD 20771 USA. [Bianchi, S.] Univ Roma Tre, Dipartimento Fis, I-00146 Rome, Italy. [Giustini, M.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Maraschi, L.] Osserv Astron Brera, INAF, I-20121 Milan, Italy. [Petrucci, P. O.] Univ Grenoble 1, CNRS, UMR 5571, Lab Astrophys Grenoble, F-38041 Grenoble, France. [Ponti, G.] Univ Paris 07, APC, F-75205 Paris, France. RP Cappi, M (reprint author), INAF IASF Bologna, Via Gobetti 101, I-40129 Bologna, Italy. EM cappi@iasfbo.inaf.it RI Bianchi, Stefano/B-4804-2010; Vignali, Cristian/J-4974-2012; Cappi, Massimo/F-4813-2015; OI Bianchi, Stefano/0000-0002-4622-4240; Vignali, Cristian/0000-0002-8853-9611; Cappi, Massimo/0000-0001-6966-8920; Dadina, Mauro/0000-0002-7858-7564; Malaguti, Giuseppe/0000-0001-9872-3378 FU ASI [ASI/INAF I/023/05/0, I/088/06/0]; ANR [ANR-06-JCJC-0047] FX This paper is based on observations obtained with the XMM-Newton satellite, an ESA funded mission with contributions by ESA Member States and USA. We would like to thank the referee K. Pounds for his constructive suggestions. We thank A. De Rosa for useful discussions. M. C., S. B., M. D. and G. P. acknowledge financial support from ASI under contracts ASI/INAF I/023/05/0 and I/088/06/0. GP aknowledges ANR for support under grant number ANR-06-JCJC-0047. NR 42 TC 41 Z9 41 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 SEP PY 2009 VL 504 IS 2 BP 401 EP 407 DI 10.1051/0004-6361/200912137 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 496PD UT WOS:000269986100009 ER PT J AU Endres, CP Drouin, BJ Pearson, JC Muller, HSP Lewen, F Schlemmer, S Giesen, TF AF Endres, C. P. Drouin, B. J. Pearson, J. C. Mueller, H. S. P. Lewen, F. Schlemmer, S. Giesen, T. F. TI Dimethyl ether: laboratory spectra up to 2.1 THz Torsion-rotational spectra within the vibrational ground state SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE ISM: molecules; molecular data; methods: laboratory; techniques: spectroscopic; radio lines: ISM; submillimeter ID MICROWAVE-SPECTRA; MOLECULAR-SPECTROSCOPY; COLOGNE DATABASE; LINE SURVEY; ORION-KL; SUBMILLIMETER; GHZ; MILLIMETER; PHASE; CDMS AB Dimethyl ether (CH(3)OCH(3)) is one of the largest organic molecules detected in the interstellar medium. As an asymmetric top molecule with two methyl groups which undergo large amplitude motions and a dipole moment of mu = 1.3 D, it conveys a dense spectrum throughout the terahertz region and contributes to the spectral line confusion in astronomical observations at these frequencies. In this paper, we present rotational spectra of dimethyl ether in its ground vibrational states, which have been measured in the laboratory and analyzed covering frequencies up to 2.1 THz. The analysis is based on an effective Hamiltonian for a symmetric two-top rotor and includes experimental data published so far. Frequency predictions are presented up to 2.5 THz for astronomical applications with accuracies better than 1 MHz. C1 [Endres, C. P.; Mueller, H. S. P.; Lewen, F.; Schlemmer, S.; Giesen, T. F.] Univ Cologne, Inst Phys 1, D-50937 Cologne, Germany. [Drouin, B. J.; Pearson, J. C.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Endres, CP (reprint author), Univ Cologne, Inst Phys 1, Zulpicher Str 77, D-50937 Cologne, Germany. EM endres@ph1.uni-koeln.de RI Giesen, Thomas /B-9476-2015; Schlemmer, Stephan/E-2903-2015 OI Giesen, Thomas /0000-0002-2401-0049; Schlemmer, Stephan/0000-0002-1421-7281 FU Deutsche Forschungsgemeinschaft (DFG) [(SFB) 494]; Laboratoire Europeen Associe (LEA) HiRes [GI 319/1-1]; Bundesministerium fur Bildung und Forschung (BMBF); National Aeronautics and Space Administration FX The authors would like to thank P. Groner for his kind support and for valuable discussions. Funding has been provided by the Deutsche Forschungsgemeinschaft (DFG), in Cologne within the Sonderforschungsbereich (SFB) 494 and the Laboratoire Europeen Associe (LEA) HiRes, administered by the DFG via Grant GI 319/1-1. H. S. P. M. has been supported by the Bundesministerium fur Bildung und Forschung (BMBF) administered through Deutsches Zentrum fur Luft- und Raumfahrt (DLR). Portions of this paper present research carried out at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. NR 21 TC 18 Z9 18 U1 2 U2 10 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD SEP PY 2009 VL 504 IS 2 BP 635 EP 640 DI 10.1051/0004-6361/200912409 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 496PD UT WOS:000269986100031 ER PT J AU Stratta, G Pozanenko, A Atteia, JL Klotz, A Basa, S Gendre, B Verrecchia, F Boer, M Cutini, S Henze, M Holland, S Ibrahimov, M Ienna, F Khamitov, I Klose, S Rumyantsev, V Biryukov, V Sharapov, D Vachier, F Arnouts, S Perley, DA AF Stratta, G. Pozanenko, A. Atteia, J. -L. Klotz, A. Basa, S. Gendre, B. Verrecchia, F. Boer, M. Cutini, S. Henze, M. Holland, S. Ibrahimov, M. Ienna, F. Khamitov, I. Klose, S. Rumyantsev, V. Biryukov, V. Sharapov, D. Vachier, F. Arnouts, S. Perley, D. A. TI A multiwavelength study of Swift GRB 060111B constraining the origin of its prompt optical emission SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE gamma rays: bursts; radiation mechanisms: non-thermal; methods: data analysis ID GAMMA-RAY BURST; LIGHT CURVES; LORENTZ FACTOR; HOST GALAXIES; XRT DATA; AFTERGLOW; TELESCOPE; DUST; GRB-021211; ULTRAVIOLET AB Context. The detection of bright optical emission measured with good temporal resolution during the prompt phase of GRB 060111B makes this GRB a rare event that is especially useful for constraining theories of the prompt emission. Aims. For this reason an extended multi-wavelength campaign was performed to further constrain the physical interpretation of the observations. Methods. In this work, we present the results obtained from our multi-wavelength campaign, as well as from the public Swift/BAT, XRT, and UVOT data. Results. We identified the host galaxy at R similar to 25 mag from deep R-band exposures taken 5 months after the trigger. Its featureless spectrum and brightness, as well as the non-detection of any associated supernova 16 days after the trigger, enabled us to constrain the distance scale of GRB 060111B within 0.4 <= z <= 3 in the most conservative case. The host galaxy spectral continuum is best fit with a redshift of z similar to 2, and other independent estimates converge to z similar to 1-2. From the analysis of the early afterglow SED, we find that non-negligible host galaxy dust extinction, in addition to the Galactic one, affects the observed flux in the optical regime. The extinction-corrected optical-to-gamma-ray SED during the prompt emission shows a flux density ratio F-gamma/F-opt = 10(-2)-10(-4) with spectral index beta(gamma,opt) > beta(gamma), strongly suggesting a separate origin of the optical and gamma-ray components. This result is supported by the lack of correlated behavior in the prompt emission light curves observed in the two energy domains. The temporal properties of the prompt optical emission observed during GRB 060111B and their similarities to other rapidly-observed events favor interpretation of this optical light as radiation from the reverse shock. Observations are in good agreement with theoretical expectations for a thick shell limit in slow cooling regime. The expected peak flux is consistent with the observed one corrected for the host extinction, likely indicating that the starting time of the TAROT observations is very near to or coincident with the peak time. The estimated fireball initial Lorentz factor is Gamma >= 260-360 at z = 1-2, similar to the Lorentz factors obtained from other GRBs. GRB 060111B is a rare case of a GRB with both a bright, well-observed optical counterpart and a "canonical" early X-ray light curve, thus providing a good test case of the reverse shock emission mechanism in both energy ranges. C1 [Stratta, G.; Verrecchia, F.; Cutini, S.] ASI Sci Data Ctr, ASDC, I-00044 Frascati, Italy. [Pozanenko, A.] Space Res Inst IKI, Moscow 117910, Russia. [Atteia, J. -L.; Ienna, F.] Univ Toulouse, LATT, CNRS, F-31400 Toulouse, France. [Klotz, A.] Univ Toulouse, CESR, CNRS, F-31028 Toulouse 04, France. [Basa, S.; Gendre, B.; Arnouts, S.] Observ Astron Marseille, LAM, F-13388 Marseille 13, France. [Boer, M.] Observ Haute Provence, F-04870 St Michel lObservatoire, France. [Henze, M.; Klose, S.] Thueringer Landessternwarte Tautenburg, D-07778 Tautenburg, Germany. [Holland, S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Ibrahimov, M.; Sharapov, D.] Ulugh Beg Astron Inst, Tashkent 700052, Uzbekistan. [Khamitov, I.] Akdeniz Univ, TUBITAK Natl Observ, TR-07058 Antalya, Turkey. [Rumyantsev, V.] SRI Crimean Astrophys Observ, UA-98409 Nauchnyi, Crimea, Ukraine. [Biryukov, V.] Moscow MV Lomonosov State Univ, Sternberg Astron Inst, Crimean Lab, UA-98409 Nauchnyi, Crimea, Ukraine. [Vachier, F.] Observ Paris, IMCCE, F-75014 Paris, France. [Arnouts, S.] Canada France Hawaii Telescope Corp, Kamuela, HI 96743 USA. [Perley, D. A.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. RP Stratta, G (reprint author), ASI Sci Data Ctr, ASDC, Via Galileo Galilei, I-00044 Frascati, Italy. EM giulia.stratta@asdc.asi.it RI gendre, bruce/O-2923-2013; Stratta, Maria Giuliana/L-3045-2016; OI gendre, bruce/0000-0002-9077-2025; Stratta, Maria Giuliana/0000-0003-1055-7980; Rumyantsev, Vasilij/0000-0003-1894-7019; Cutini, Sara/0000-0002-1271-2924; Henze, Martin/0000-0001-9985-3406 FU CNES post-doctoral grant FX The authors thank the anonymous referee for his/her useful comments and acknowledge Taka Sakamoto and Scott D. Barthelmy for making BAT data available to the community, and J. S. Bloom for obtaining the Keck data. B. G. is funded by a french CNES post-doctoral grant. NR 79 TC 12 Z9 12 U1 1 U2 3 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 EI 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD SEP PY 2009 VL 503 IS 3 BP 783 EP 795 DI 10.1051/0004-6361/200911981 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 493HJ UT WOS:000269727100014 ER PT J AU Gielen, C Van Winckel, H Matsuura, M Min, M Deroo, P Waters, LBFM Dominik, C AF Gielen, C. Van Winckel, H. Matsuura, M. Min, M. Deroo, P. Waters, L. B. F. M. Dominik, C. TI Analysis of the infrared spectra of the peculiar post-AGB stars EP Lyrae and HD 52961 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: AGB and post-AGB; stars: binaries: general; stars: circumstellar matter; stars: individual: EP Lyrae; stars: individual: HD 52961 ID RV-TAURI STARS; AROMATIC-HYDROCARBON EMISSION; CRYSTALLINE SILICATE DUST; SPITZER-SPACE-TELESCOPE; HERBIG AE/BE STARS; RED-RECTANGLE; CARBON STARS; EVOLVED STARS; CIRCUMSTELLAR ENVELOPES; ABUNDANCE ANALYSES AB Aims. We aim to study in detail the peculiar mineralogy and structure of the circumstellar environment of two binary post-AGB stars, EP Lyr and HD52961. Both stars were selected from a larger sample of evolved disc sources observed with Spitzer and show unique solid-state and gas features in their infrared spectra. Moreover, they show a very small infrared excess in comparison with the other sample stars. Methods. The different dust and gas species are identified on the basis of high-resolution Spitzer-IRS spectra. We fit the full spectrum to constrain grain sizes and temperature distributions in the discs. This, combined with our broad-band spectral energy distribution and interferometric measurements, allows us to study the physical structure of the disc, using a self-consistent 2D radiative-transfer disc model. Results. We find that both stars have strong emission features due to CO2 gas, dominated by (CO2)-C-12-O-16, but with clear (CO2)-C-13-O-16 and even (OCO)-O-16-C-12-O-18 isotopic signatures. Crystalline silicates are apparent in both sources but proved very hard to model. EP Lyr also shows evidence of mixed chemistry, with emission features of the rare class-C PAHs. Whether these PAHs reside in the oxygen-rich disc or in a carbon-rich outflow is still unclear. With the strongly processed silicates, the mixed chemistry and the low C-12/C-13 ratio, EP Lyr resembles some silicate J-type stars, although the depleted photosphere makes nucleosynthetic signatures difficult to probe. We find that the disc environment of both sources is, to a first approximation, well modelled with a passive disc, but additional physics such as grain settling, radial dust distributions, and an outflow component must be included to explain the details of the observed spectral energy distributions in both stars. C1 [Gielen, C.; Van Winckel, H.; Waters, L. B. F. M.] Katholieke Univ Leuven, Inst Sterrenkunde, B-3001 Louvain, Belgium. [Matsuura, M.] UCL, Dept Phys & Astron, Astrophys Grp, London WC1E 6BT, England. [Matsuura, M.] Natl Astron Observ, Div Opt & IR Astron, Tokyo 1818588, Japan. [Min, M.; Waters, L. B. F. M.; Dominik, C.] Univ Amsterdam, Sterrenkundig Inst Anton Pannekoek, NL-1098 Amsterdam, Netherlands. [Deroo, P.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Dominik, C.] Radboud Univ Nijmegen, Dept Astrophys, NL-6500 GL Nijmegen, Netherlands. RP Gielen, C (reprint author), Katholieke Univ Leuven, Inst Sterrenkunde, Celestijnenlaan 200D, B-3001 Louvain, Belgium. EM clio.gielen@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) [0178.02, 0470.07] FX C. G. acknowledges support of the Fund for Scientific Research of Flanders (FWO) under the grant G. 0178.02. and G. 0470.07. NR 91 TC 14 Z9 14 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 SEP PY 2009 VL 503 IS 3 BP 843 EP 854 DI 10.1051/0004-6361/200912060 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 493HJ UT WOS:000269727100020 ER PT J AU Wang, TJ Ofman, L Davila, JM Mariska, JT AF Wang, T. J. Ofman, L. Davila, J. M. Mariska, J. T. TI Hinode/EIS observations of propagating low-frequency slow magnetoacoustic waves in fan-like coronal loops SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE Sun: atmosphere; Sun: corona; Sun: oscillations; Sun: UV radiation; waves ID EUV IMAGING SPECTROMETER; SOLAR CORONA; OSCILLATIONS; SEISMOLOGY; TRACE; SUMER AB Aims. We report the first observation of multiple-periodic propagating disturbances along a fan-like coronal structure simultaneously detected in both intensity and Doppler shift in the Fe XII 195 angstrom line with the EUV Imaging Spectrometer (EIS) onboard Hinode. A new application of coronal seismology is provided based on this observation. Methods. We analyzed the EIS sit-and-stare mode observation of oscillations using the running difference and wavelet techniques. Results. Two harmonics with periods of 12 and 25 min are detected. We measured the Doppler shift amplitude of 1-2 km s(-1), the relative intensity amplitude of 3%-5% and the apparent propagation speed of 100-120 km s(-1). Conclusions. The amplitude relationship between intensity and Doppler shift oscillations provides convincing evidence that these propagating features are a manifestation of slow magnetoacoustic waves. Detection lengths (over which the waves are visible) of the 25 min wave are about 70-90 Mm, much longer than those of the 5 min wave previously detected by TRACE. This difference may be explained by the dependence of damping length on the wave period for thermal conduction. Based on a linear wave theory, we derive an inclination of the magnetic field to the line-of-sight about 59 +/- 8 degrees, a true propagation speed of 128 +/- 25 km s(-1) and a temperature of 0.7 +/- 0.3 MK near the loop's footpoint from our measurements. C1 [Wang, T. J.; Ofman, L.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA. [Wang, T. J.; Ofman, L.; Davila, J. M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Mariska, J. T.] USN, Res Lab, Div Space Sci, Washington, DC 20375 USA. RP Wang, TJ (reprint author), Catholic Univ Amer, Dept Phys, 620 Michigan Ave, Washington, DC 20064 USA. EM wangtj@helio.gsfc.nasa.gov FU NRL [N00173-06-1-G033]; NASA [NNG06GI55G] FX Hinode is a Japanese mission developed and launched by ISAS/JAXA in partnership with NAOJ, NASA, and STFC (UK). Additional operation support is provided by ESA and NSC ( Norway). The authors are grateful to Dr. Harry Warren for his planning of EIS observations. The work of L. O. and T. J. W. was supported by NRL grant N00173-06-1-G033. L. O. was also supported by NASA grant NNG06GI55G. The authors also thank the referee, Dr. Dipankar Banerjee, for his constructive comments and suggestions. NR 22 TC 62 Z9 62 U1 0 U2 2 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD SEP PY 2009 VL 503 IS 3 BP L25 EP U14 DI 10.1051/0004-6361/200912534 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 493HJ UT WOS:000269727100002 ER PT J AU Grasso, D Profumo, S Strong, AW Baldini, L Bellazzini, R Bloom, ED Bregeon, J Di Bernardo, G Gaggero, D Giglietto, N Kamae, T Latronico, L Longo, F Mazziotta, MN Moiseev, AA Morselli, A Ormes, JF Pesce-Rollins, M Pohl, M Razzano, M Sgro, C Spandre, G Stephens, TE AF Grasso, D. Profumo, S. Strong, A. W. Baldini, L. Bellazzini, R. Bloom, E. D. Bregeon, J. Di Bernardo, G. Gaggero, D. Giglietto, N. Kamae, T. Latronico, L. Longo, F. Mazziotta, M. N. Moiseev, A. A. Morselli, A. Ormes, J. F. Pesce-Rollins, M. Pohl, M. Razzano, M. Sgro, C. Spandre, G. Stephens, T. E. TI On possible interpretations of the high energy electron-positron spectrum measured by the Fermi Large Area Telescope SO ASTROPARTICLE PHYSICS LA English DT Article DE Cosmic ray electrons and positrons; Pulsars; Dark-matter; Fermi-LAT ID COSMIC-RAY ELECTRONS; DARK-MATTER; SUPERNOVA-REMNANTS; GAMMA-RAYS; PULSARS; PROPAGATION; ORIGIN; FLIGHT AB The Fermi-LAT experiment recently reported high precision measurements of the spectrum of cosmic-ray electrons-plus-positrons (CRE) between 20 GeV and 1 TeV. The spectrum shows no prominent spectral features, and is significantly harder than that inferred from several previous experiments. Here we discuss several interpretations of the Fermi results based either on a single large scale Galactic CRE component or by invoking additional electron-positron primary sources, e.g. nearby pulsars or particle dark matter annihilation. We show that while the reported Fermi-LAT data alone can be interpreted in terms of a single component scenario, when combined with other complementary experimental results, specifically the CRE spectrum measured by H.E.S.S. and especially the positron fraction reported by PAMELA between 1 and 100 GeV, that class of models fails to provide a consistent interpretation. Rather, we find that several combinations of parameters, involving both the pulsar and dark matter scenarios, allow a consistent description of those results. We also briefly discuss the possibility of discriminating between the pulsar and dark matter interpretations by looking for a possible anisotropy in the CRE flux. (C) 2009 Elsevier B.V. All rights reserved. C1 [Grasso, D.; Baldini, L.; Bellazzini, R.; Bregeon, J.; Di Bernardo, G.; Gaggero, D.; Latronico, L.; Pesce-Rollins, M.; Razzano, M.; Sgro, C.; Spandre, G.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy. [Profumo, S.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA. [Profumo, S.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA. [Strong, A. W.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Bloom, E. D.; Kamae, T.] Stanford Univ, Dept Phys, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA. [Bloom, E. D.; Kamae, T.] Stanford Univ, Natl Accelerator Lab, SLAC, Stanford, CA 94305 USA. [Di Bernardo, G.; Gaggero, D.] Univ Pisa, Dipartimento Fis, I-56127 Pisa, Italy. [Giglietto, N.] M Merlin Univ, Dipartmento Fis, I-70126 Bari, Italy. [Giglietto, N.] Politecn Bari, I-70126 Bari, Italy. [Giglietto, N.; Mazziotta, M. N.] Ist Nazl Fis Nucl, Sez Bari, I-70126 Bari, Italy. [Longo, F.] Univ Trieste, Dipartmento Fis, I-34127 Trieste, Italy. [Moiseev, A. A.] NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA. [Moiseev, A. A.] Univ Maryland, College Pk, MD 20742 USA. [Morselli, A.] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, I-00133 Rome, Italy. [Ormes, J. F.] Univ Denver, Dept Phys & Astron, Denver, CO 80208 USA. [Pohl, M.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. [Stephens, T. E.] NASA, Ames Res Ctr, Univ Space Res Assoc, Moffett Field, CA 94035 USA. RP Grasso, D (reprint author), Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy. EM dario.grasso@pi.infn.it; profumo@scipp.ucsc.edu; aws@mpe.mpg.de RI Baldini, Luca/E-5396-2012; Morselli, Aldo/G-6769-2011; Grasso, Dario/I-2440-2012; giglietto, nicola/I-8951-2012; Mazziotta, Mario /O-8867-2015; Sgro, Carmelo/K-3395-2016; OI Baldini, Luca/0000-0002-9785-7726; Morselli, Aldo/0000-0002-7704-9553; Grasso, Dario/0000-0001-7761-7242; giglietto, nicola/0000-0002-9021-2888; Mazziotta, Mario /0000-0001-9325-4672; Sgro', Carmelo/0000-0001-5676-6214; Stephens, Thomas/0000-0003-3065-6871; Pesce-Rollins, Melissa/0000-0003-1790-8018 FU Italian Space Agency [AMS-02.ASI/AMS-02 n.I/035/07/0]; Dipartimento di Fisica dell'Universita di Padova and UniverseNet EU Network [MRTN-CF-2006-035863]; US DoE [DEFG02-04ER41268, DE-AC02-76-SF00515]; NSF [PHY-0757911] 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 I'Energie Atomique and the Centre National de la Recherche Scientifique/Institut National de Physique Nuclaire et de Physique des Particules in France, the Agenzia Spaziale Italiana and the Istituto Nazionale di Fisica Nucleare in Italy, the Ministry of Education, Culture, Sports, Science and Technology (MEXT), High Energy Accelerator Research Organization (KEK) and Japan Aerospace Exploration Agency (JAXA) in Japan, and the K.A. Wallenberg Foundation, the Swedish Research Council and the Swedish National Space Board in Sweden.; Additional support for science analysis during the operations phase from the following agency is also gratefully acknowledged: the Istituto Nazionale di Astrofisica in Italy.; D.G. is supported by the Italian Space Agency under the Contract AMS-02.ASI/AMS-02 n.I/035/07/0. He also thanks the Dipartimento di Fisica dell'Universita di Padova and UniverseNet EU Network under Contract No. MRTN-CF-2006-035863 for partial financial support. S.P. is partly supported by US DoE Contract DEFG02-04ER41268 and by NSF Grant PHY-0757911. E.D.B. and T.K. are Supported by US DoE Contract DE-AC02-76-SF00515.; We thank the anonymous referee for several useful comments. NR 73 TC 173 Z9 173 U1 0 U2 4 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0927-6505 EI 1873-2852 J9 ASTROPART PHYS JI Astropart Phys. PD SEP PY 2009 VL 32 IS 2 BP 140 EP 151 DI 10.1016/j.astropartphys.2009.07.003 PG 12 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 513RL UT WOS:000271340800008 ER PT J AU Ragland, S Akeson, RL Armandroff, T Colavita, MM Danchi, WC Hillenbrand, LA Millan-Gabet, R Ridgway, ST Traub, WA Vasisht, G Wizinowich, PL AF Ragland, S. Akeson, R. L. Armandroff, T. Colavita, M. M. Danchi, W. C. Hillenbrand, L. A. Millan-Gabet, R. Ridgway, S. T. Traub, W. A. Vasisht, G. Wizinowich, P. L. TI FIRST L-BAND INTERFEROMETRIC OBSERVATIONS OF A YOUNG STELLAR OBJECT: PROBING THE CIRCUMSTELLAR ENVIRONMENT OF MWC 419 SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; instrumentation: interferometers; stars: emission-line, Be; stars: individual (MWC 419); stars: pre-main sequence; techniques: interferometric ID HERBIG-AE/BE STARS; PALOMAR TESTBED INTERFEROMETER; INFRARED-EMISSION; INNER DISK; AE STARS; T-TAURI; SPECTRA; DUST; SPECTROSCOPY; LUMINOSITY AB We present spatially resolved K- and L-band spectra (at spectral resolution R = 230 and R = 60, respectively) of MWC 419, a Herbig Ae/Be star. The data were obtained simultaneously with a new configuration of the 85 m baseline Keck Interferometer. Our observations are sensitive to the radial distribution of temperature in the inner region of the disk of MWC 419. We fit the visibility data with both simple geometric and more physical disk models. The geometric models (uniform disk and Gaussian) show that the apparent size increases linearly with wavelength in the 2-4 mu m wavelength region, suggesting that the disk is extended with a temperature gradient. A model having a power-law temperature gradient with radius simultaneously fits our interferometric measurements and the spectral energy distribution data from the literature. The slope of the power law is close to that expected from an optically thick disk. Our spectrally dispersed interferometric measurements include the Br gamma emission line. The measured disk size at and around Br gamma suggests that emitting hydrogen gas is located inside (or within the inner regions) of the dust disk. C1 [Ragland, S.; Armandroff, T.; Wizinowich, P. L.] WM Keck Observ, Kamuela, HI 96743 USA. [Akeson, R. L.; Millan-Gabet, R.] CALTECH, NExScI, Pasadena, CA 91125 USA. [Colavita, M. M.; Traub, W. A.; Vasisht, G.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Danchi, W. C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Ridgway, S. T.] Natl Opt Astron Observ, Tucson, AZ 85726 USA. RP Ragland, S (reprint author), WM Keck Observ, 65-1120 Mamalahoa Hwy, Kamuela, HI 96743 USA. EM sragland@keck.hawaii.edu FU National Aeronautics and Space Administration (NASA) FX Keck Interferometer is funded by the National Aeronautics and Space Administration (NASA). Observations presented were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and NASA. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. We thank E. Appleby, B. Berkey, A. Booth, A. Cooper, S. Crawford, W. Dahl, C. Felizardo, J. Garcia-Gathright, J. Herstein, R. Ligon, D. Medeiros, D. Morrison, T. Panteleeva, B. Parvin, B. Smith, K. Summers, K. Tsubota, C. Tyau, and E. Wetherell for their contributions to the instrument development, integration, and operations. S. Ragland also thanks M. Hrynevych, M. Kassis, and J. Woillez for useful discussions. We thank the referee for constructive critical comments that helped us to significantly improve the paper. NR 46 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 SEP PY 2009 VL 703 IS 1 BP 22 EP 29 DI 10.1088/0004-637X/703/1/22 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 492AE UT WOS:000269625000003 ER PT J AU Swartz, DA Tennant, AF Soria, R AF Swartz, Douglas A. Tennant, Allyn F. Soria, Roberto TI ULTRALUMINOUS X-RAY SOURCE CORRELATIONS WITH STAR-FORMING REGIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: general; X-rays: galaxies; X-rays: general ID DIGITAL SKY SURVEY; OPTICAL COUNTERPART; DATA RELEASE; RUNAWAY COLLISIONS; SOURCE POPULATION; NEARBY GALAXIES; MASSIVE STARS; CLUSTERS; EVOLUTION; ASSOCIATIONS AB Maps of low-inclination nearby galaxies in Sloan Digitized Sky Survey u - g, g - r, and r - i colors are used to determine whether ultraluminous X-ray sources (ULXs) are predominantly associated with star-forming regions of their host galaxies. An empirical selection criterion is derived from colors of H II regions in M 81 and M 101 that differentiates between the young, blue stellar component and the older disk and bulge population. This criterion is applied to a sample of 58 galaxies of Hubble type S0 and later and verified through an application of Fisher's linear discriminant analysis. It is found that 60% (49%) of ULXs in optically bright environments are within regions blueward of their host galaxy's H II regions compared to only 27% (0%) of a control sample according to the empirical (Fisher) criterion. This is an excess of 3 sigma above the 32% (27%) expected if the ULXs were randomly distributed within their galactic hosts. This indicates a ULX preference for young, less than or similar to 10 Myr, OB associations. However, none of the ULX environments have the morphology and optical brightness suggestive of a massive young super-star cluster though several are in extended or crowded star-forming (blue) environments that may contain clusters unresolved by Sloan imaging. Ten of the 12 ULX candidates with estimated X-ray luminosities in excess of 3 x 10(39) erg s(-1) are equally divided among the group of ULX environments redward of H II regions and the group of optically faint regions. This likely indicates that the brightest ULXs turn on at a time somewhat later than typical of H II regions; say 10-20 Myr after star formation has ended. This would be consistent with the onset of an accretion phase as the donor star ascends the giant branch if the donor is an less than or similar to 20 M(circle dot) star. C1 [Swartz, Douglas A.] NASA, George C Marshall Space Flight Ctr, Univ Space Res Assoc, Huntsville, AL 35812 USA. [Tennant, Allyn F.] NASA, George C Marshall Space Flight Ctr, Space Sci Off, Huntsville, AL 35812 USA. [Soria, Roberto] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. RP Swartz, DA (reprint author), NASA, George C Marshall Space Flight Ctr, Univ Space Res Assoc, VP62, Huntsville, AL 35812 USA. FU Chandra Award [GO6-7081A]; Alfred P. Sloan Foundation; Participating Institutions; National Science Foundation; U.S. Department of Energy; National Aeronautics and Space Administration [NAS8-03060]; Japanese Monbukagakusho; Max Planck Society; Higher Education Funding Council for England FX This work was supported, in part, by Chandra Award GO6-7081A issued by the Chandra X-ray Observatory Center which is operated by the Smithsonian Astrophysical Observatory for and on behalf of NASA under contract NAS8-03060. This work has made extensive use of DR6 of the Sloan Digitized Sky Survey. Funding for the SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, the U.S. Department of Energy, the National Aeronautics and Space Administration, the Japanese Monbukagakusho, the Max Planck Society, and the Higher Education Funding Council for England. NR 47 TC 43 Z9 44 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 SEP PY 2009 VL 703 IS 1 BP 159 EP 168 DI 10.1088/0004-637X/703/1/159 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 492AE UT WOS:000269625000018 ER PT J AU Sajina, A Spoon, H Yan, L Imanishi, M Fadda, D Elitzur, M AF Sajina, Anna Spoon, Henrik Yan, Lin Imanishi, Masatoshi Fadda, Dario Elitzur, Moshe TI DETECTIONS OF WATER ICE, HYDROCARBONS, AND 3.3 mu m PAH IN z similar to 2 ULIRGs SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: high-redshift; galaxies: ISM; infrared: galaxies; quasars: absorption lines ID ULTRALUMINOUS INFRARED GALAXIES; SPITZER MIDINFRARED SPECTROSCOPY; ACTIVE GALACTIC NUCLEI; LUMINOUS GALAXIES; SPACE-TELESCOPE; INTERSTELLAR ICE; STAR-FORMATION; QUASARS; SPECTRA; SAMPLE AB We present the first detections of the 3 mu m water ice and 3.4 mu m amorphous hydrocarbon (HAC) absorption features in z similar to 2 ULIRGs. These are based on deep rest-frame 2-8 mu m Spitzer Infrared Spectrograph spectra of 11 sources selected for their appreciable silicate absorption. The HAC-to-silicate ratio for our z similar to 2 sources is typically higher by a factor of 2-5 than that observed in the Milky Way. This HAC "excess" suggests compact nuclei with steep temperature gradients as opposed to predominantly host obscuration. Beside the above molecular absorption features, we detect the 3.3 mu m polycyclic aromatic hydrocarbon (PAH) emission feature in one of our sources with three more individual spectra showing evidence for it. Stacking analysis suggests that water ice, hydrocarbons, and PAH are likely present in the bulk of this sample even when not individually detected. The most unexpected result of our study is the lack of clear detections of the 4.67 mu m CO gas absorption feature. Only three of the sources show tentative signs of this feature at significantly lower levels than has been observed in local ULIRGs. Overall we find that the closest local analogs to our sources, in terms of 3-4 mu m color, HAC-to-silicate and ice-to-silicate ratios, as well as low PAH equivalent widths, are sources dominated by deeply obscured nuclei. Such sources form only a small fraction of ULIRGs locally and are commonly believed to be dominated by buried active galactic nuclei (AGNs). Our sample suggests that, in an absolute number, such buried AGNs are at least an order of magnitude more common at z similar to 2 than today. The presence of PAH suggests that significant levels of star formation are present even if the obscured AGNs typically dominate the power budget. C1 [Sajina, Anna] Haverford Coll, Dept Phys & Astron, Haverford, PA 19041 USA. [Spoon, Henrik] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. [Yan, Lin] CALTECH, IPAC, Pasadena, CA 91125 USA. [Imanishi, Masatoshi] Natl Astron Observ, Mitaka, Tokyo 1818588, Japan. [Fadda, Dario] CALTECH, NASA, Herschel Space Telescope Ctr, Pasadena, CA 91125 USA. [Elitzur, Moshe] Univ Kentucky, Dept Phys & Astron, Lexington, KY 40506 USA. RP Sajina, A (reprint author), Haverford Coll, Dept Phys & Astron, Haverford, PA 19041 USA. FU NASA FX We thank the anonymous referee for their thoughtful comments, which have improved this paper. We also wish to thank Brian Siana and Kalliopi Dasyra for helpful discussions. 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 50 TC 12 Z9 11 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD SEP PY 2009 VL 703 IS 1 BP 270 EP 284 DI 10.1088/0004-637X/703/1/270 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 492AE UT WOS:000269625000026 ER PT J AU Dye, S Ade, PAR Bock, JJ Chapin, EL Devlin, MJ Dunlop, JS Eales, SA Griffin, M Gundersen, JO Halpern, M Hargrave, PC Hughes, DH Klein, J Magnelli, B Marsden, G Mauskopf, P Moncelsi, L Netterfield, CB Olmi, L Pascale, E Patanchon, G Rex, M Scott, D Semisch, C Targett, T Thomas, N Truch, MDP Tucker, C Tucker, GS Viero, MP Wiebe, DV AF Dye, Simon Ade, Peter A. R. Bock, James J. Chapin, Edward L. Devlin, Mark J. Dunlop, James S. Eales, Stephen A. Griffin, Matthew Gundersen, Joshua O. Halpern, Mark Hargrave, Peter C. Hughes, David H. Klein, Jeff Magnelli, Benjamin Marsden, Gaelen Mauskopf, Philip Moncelsi, Lorenzo Netterfield, Calvin B. Olmi, Luca Pascale, Enzo Patanchon, Guillaume Rex, Marie Scott, Douglas Semisch, Christopher Targett, Tom Thomas, Nicholas Truch, Matthew D. P. Tucker, Carole Tucker, Gregory S. Viero, Marco P. Wiebe, Donald V. TI RADIO AND MID-INFRARED IDENTIFICATION OF BLAST SOURCE COUNTERPARTS IN THE CHANDRA DEEP FIELD SOUTH SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology: observations; galaxies: high-redshift; infrared: galaxies; submillimeter; surveys ID DEGREE EXTRAGALACTIC SURVEY; APERTURE SUBMILLIMETER TELESCOPE; UNIVERSE GALAXY SURVEY; HIGH-REDSHIFT; PHOTOMETRIC REDSHIFTS; STAR-FORMATION; NUMBER COUNTS; SCUBA; HALF; LUMINOSITY AB We have identified radio and/or mid-infrared counterparts to 198 out of 350 sources detected at >= 5 sigma over similar to 9 deg(2) centered on the Chandra Deep Field South by the Balloon-borne Large Aperture Submillimeter Telescope (BLAST) at 250, 350, and 500 mu m. We have matched 114 of these counterparts to optical sources with previously derived photometric redshifts and fitted spectral energy distributions to the BLAST fluxes and fluxes at 70 and 160 mu m acquired with the Spitzer Space Telescope. In this way, we have constrained dust temperatures, total far-infrared/submillimeter luminosities, and star formation rates for each source. Our findings show that, on average, the BLAST sources lie at significantly lower redshifts and have significantly lower rest-frame dust temperatures compared to submillimeter sources detected in surveys conducted at 850 mu m. We demonstrate that an apparent increase in dust temperature with redshift in our sample arises as a result of selection effects. Finally, we provide the full multiwavelength catalog of >= 5 sigma BLAST sources contained within the complete similar to 9 deg(2) survey area. C1 [Dye, Simon; Ade, Peter A. R.; Eales, Stephen A.; Griffin, Matthew; Hargrave, Peter C.; Mauskopf, Philip; Moncelsi, Lorenzo; Pascale, Enzo; Tucker, Carole] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Bock, James J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Chapin, Edward L.; Halpern, Mark; Marsden, Gaelen; Scott, Douglas; Targett, Tom; Wiebe, Donald V.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. [Devlin, Mark J.; Klein, Jeff; Rex, Marie; Semisch, Christopher; Truch, Matthew D. P.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. [Dunlop, James S.] Univ Edinburgh, Royal Observ, Astron Inst, Edinburgh EH9 3HJ, Midlothian, Scotland. [Gundersen, Joshua O.; Thomas, Nicholas] Univ Miami, Dept Phys, Coral Gables, FL 33146 USA. [Hughes, David H.] INAOE, Puebla 72000, Mexico. [Magnelli, Benjamin] Univ Paris Diderot, Lab AIM, CEA, DSM,CNRS,IRFU,Serv Astrophys,CEA Saclay, F-91191 Gif Sur Yvette, France. [Netterfield, Calvin B.; Viero, Marco P.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada. [Netterfield, Calvin B.] Univ Toronto, Dept Phys, Toronto, ON M5S 1A7, Canada. [Olmi, Luca] Univ Puerto Rico, Dept Phys, UPR Stn, San Juan, PR 00936 USA. [Olmi, Luca] Osserv Astrofis Arcetri, INAF, I-50125 Florence, Italy. [Patanchon, Guillaume] Univ Paris Diderot, Lab APC, F-75205 Paris, France. [Tucker, Gregory S.] Brown Univ, Dept Phys, Providence, RI 02912 USA. RP Dye, S (reprint author), Cardiff Univ, Sch Phys & Astron, Queens Bldg, Cardiff CF24 3AA, S Glam, Wales. RI Klein, Jeffrey/E-3295-2013; OI Olmi, Luca/0000-0002-1162-7947; Scott, Douglas/0000-0002-6878-9840; Dye, Simon/0000-0002-1318-8343 FU Natural Sciences and Engineering Research Council (NSERC) of Canada; NASA; UK Science and Technology Facilities Council (STFC) FX Natural Sciences and Engineering Research Council (NSERC) of Canada. This work is based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. S. D. is supported by the UK Science and Technology Facilities Council (STFC). We thank Guilane Lagache for advice on implementation of her galaxy evolution models. NR 48 TC 37 Z9 37 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 SEP PY 2009 VL 703 IS 1 BP 285 EP 299 DI 10.1088/0004-637X/703/1/285 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 492AE UT WOS:000269625000027 ER PT J AU Burlaga, LF Ness, NF AF Burlaga, L. F. Ness, N. F. TI COMPRESSIBLE "TURBULENCE" OBSERVED IN THE HELIOSHEATH BY VOYAGER 2 SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; solar wind; Sun: magnetic fields; turbulence ID WIND TERMINATION SHOCK; SOLAR-WIND; MAGNETIC-FIELD; FLUCTUATIONS; PLASMA; DISTRIBUTIONS; TEMPERATURE; STATISTICS; UPSTREAM; REGION AB This paper describes the multiscale structure of the compressible "turbulence" observed in the high-resolution (48 s) observations of the magnetic field strength B made by Voyager 2 (V2) in the heliosheath behind the termination shock from 2007 DOY 245.0-300.8 and in a unipolar region from 2008 DOY 2.9-75.6. The magnetic field strength is highly variable on scales from 48 s to several hours in both intervals. The distributions of daily averages and 48 s averages of B are lognormal in the post-termination shock (TS) region and Gaussian in the unipolar region, respectively. The amplitudes of the fluctuations were greater in the post-TS region than in the unipolar region, at scales less than several hours. The multiscale structure of the increments of B is described by the q-Gaussian distribution of nonextensive statistical mechanics on all scales from 48 s to 3.4 hr in the unipolar region and from 48 s to 6.8 hr in the post-TS region, respectively. The amplitudes of the fluctuations of increments of B are larger in the post-TS region than in the unipolar region at all scales. The probability density functions of the increments of B are non-Gaussian at all scales in the unipolar region, but they are Gaussian at the largest scales in the post-TS region. Time series of the magnitude and direction of B show that the fluctuations are highly compressive. The small-scale fluctuations are a mixture of coherent structures (semi-deterministic structures) and random structures, which vary significantly from day to day. Several types of coherent structures were identified in both regions. C1 [Burlaga, L. F.] NASA, Goddard Space Flight Ctr, Geospace Phys Lab, Greenbelt, MD 20771 USA. [Ness, N. F.] Catholic Univ Amer, Inst Astrophys & Computat Sci, Washington, DC 20064 USA. RP Burlaga, LF (reprint author), NASA, Goddard Space Flight Ctr, Geospace Phys Lab, Code 673, Greenbelt, MD 20771 USA. EM Leonard.F.Burlaga@NASA.gov; nfnudel@yahoo.com FU NASA [NNX07AW09G] FX The data in this paper are from the magnetic field experiment on Voyager 2. N. F. N. was partially supported by NASA grant NNX07AW09G to the Catholic University of America. McClanahan and S. Kramer carried out the processing of the data. The "0-offset tables" were computed by D. Berdichevsky. The speeds quoted in this paper were derived from the plasma instrument on V2 and provided online by J. Richardson. NR 46 TC 46 Z9 47 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 SEP PY 2009 VL 703 IS 1 BP 311 EP 324 DI 10.1088/0004-637X/703/1/311 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 492AE UT WOS:000269625000029 ER PT J AU Rex, M Ade, PAR Aretxaga, I Bock, JJ Chapin, EL Devlin, MJ Dicker, SR Griffin, M Gundersen, JO Halpern, M Hargrave, PC Hughes, DH Klein, J Marsden, G Martin, PG Mauskopf, P Montana, A Netterfield, CB Olmi, L Pascale, E Patanchon, G Scott, D Semisch, C Thomas, N Truch, MDP Tucker, C Tucker, GS Viero, MP Wiebe, DV AF Rex, Marie Ade, Peter A. R. Aretxaga, Itziar Bock, James J. Chapin, Edward L. Devlin, Mark J. Dicker, Simon R. Griffin, Matthew Gundersen, Joshua O. Halpern, Mark Hargrave, Peter C. Hughes, David H. Klein, Jeff Marsden, Gaelen Martin, Peter G. Mauskopf, Philip Montana, Alfredo Netterfield, Calvin B. Olmi, Luca Pascale, Enzo Patanchon, Guillaume Scott, Douglas Semisch, Christopher Thomas, Nicholas Truch, Matthew D. P. Tucker, Carole Tucker, Gregory S. Viero, Marco P. Wiebe, Donald V. TI A BRIGHT SUBMILLIMETER SOURCE IN THE BULLET CLUSTER (1E0657-56) FIELD DETECTED WITH BLAST SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: clusters: individual (1E0657-56); submillimeter ID DEGREE EXTRAGALACTIC SURVEY; STAR-FORMING GALAXIES; NUMBER COUNTS; HIGH-REDSHIFT; PHOTOMETRIC REDSHIFTS; INFRARED GALAXY; DARK-MATTER; 1E 0657-56; MAPS; HALF AB We present the 250, 350, and 500 mu m detection of bright submillimeter emission in the direction of the Bullet Cluster measured by the Balloon-borne Large-Aperture Submillimeter Telescope (BLAST). The 500 mu m centroid is coincident with an AzTEC 1.1 mm point-source detection at a position close to the peak lensing magnification produced by the cluster. However, the 250 mu m and 350 mu m centroids are elongated and shifted toward the south with a differential shift between bands that cannot be explained by pointing uncertainties. We therefore conclude that the BLAST detection is likely contaminated by emission from foreground galaxies associated with the Bullet Cluster. The submillimeter redshift estimate based on 250-1100 mu m photometry at the position of the AzTEC source is z(phot) = 2.9(-0.3)(+0.6), consistent with the infrared color redshift estimation of the most likely Infrared Array Camera counterpart. These flux densities indicate an apparent far-infrared (FIR) luminosity of L-FIR = 2 x 10(13) L-circle dot. When the amplification due to the gravitational lensing of the cluster is removed, the intrinsic FIR luminosity of the source is found to be L-FIR <= 10(12) L-circle dot, consistent with typical luminous infrared galaxies. C1 [Rex, Marie; Devlin, Mark J.; Dicker, Simon R.; Klein, Jeff; Semisch, Christopher; Truch, Matthew D. P.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. [Ade, Peter A. R.; Griffin, Matthew; Hargrave, Peter C.; Mauskopf, Philip; Pascale, Enzo; Tucker, Carole] Cardiff Univ, Dept Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Aretxaga, Itziar; Hughes, David H.; Montana, Alfredo] INAOE, Puebla 72000, Mexico. [Bock, James J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Bock, James J.] CALTECH, Pasadena, CA 91125 USA. [Chapin, Edward L.; Halpern, Mark; Marsden, Gaelen; Scott, Douglas; Wiebe, Donald V.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. [Gundersen, Joshua O.; Thomas, Nicholas] Univ Miami, Dept Phys, Carol Gables, FL 33146 USA. [Martin, Peter G.] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada. [Martin, Peter G.; Netterfield, Calvin B.; Viero, Marco P.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada. [Netterfield, Calvin B.; Wiebe, Donald V.] Univ Toronto, Dept Phys, Toronto, ON M5S 1A7, Canada. [Olmi, Luca] Ist Radioastron, I-50125 Florence, Italy. [Olmi, Luca] Univ Puerto Rico, Dept Phys, UPR Stn, San Juan, PR 00936 USA. [Patanchon, Guillaume] Lab APC, F-75205 Paris, France. [Tucker, Gregory S.] Brown Univ, Dept Phys, Providence, RI 02912 USA. RP Rex, M (reprint author), Univ Penn, Dept Phys & Astron, 209 S 33rd St, Philadelphia, PA 19104 USA. EM madamson@physics.upenn.edu RI Klein, Jeffrey/E-3295-2013; OI Olmi, Luca/0000-0002-1162-7947; Scott, Douglas/0000-0002-6878-9840 FU NASA [NAG5-12785, NAG5-13301, NNGO-6GI11G]; NSF; Canadian Space Agency; Natural Sciences and Engineering Research Council (NSERC) of Canada; UK Science and Technology Facilities Council (STFC) FX We acknowledge the support of NASA through grant NAG5-12785, NAG5-13301, and NNGO-6GI11G, the NSF Office of Polar Programs, the Canadian Space Agency, the Natural Sciences and Engineering Research Council (NSERC) of Canada, and the UK Science and Technology Facilities Council (STFC). We thank Tony Mroczkowski for his help with the SZE simulations. This research has been enabled by the use of West-Grid computing resources. This research also made use of the SIMBAD database, observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA, and SAOImage DS9, developed by Smithsonian Astrophysical Observatory. NR 41 TC 11 Z9 11 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 SEP PY 2009 VL 703 IS 1 BP 348 EP 353 DI 10.1088/0004-637X/703/1/348 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 492AE UT WOS:000269625000032 ER PT J AU Willacy, K Woods, PM AF Willacy, K. Woods, P. M. TI DEUTERIUM CHEMISTRY IN PROTOPLANETARY DISKS. II. THE INNER 30 AU SO ASTROPHYSICAL JOURNAL LA English DT Review DE astrochemistry; circumstellar matter; ISM: abundances; ISM: molecules; solar system: formation; stars: formation; stars: pre-main sequence ID DENSE INTERSTELLAR CLOUDS; WEAKLY MAGNETIZED DISKS; GLOBAL BAROCLINIC INSTABILITY; LOCAL SHEAR INSTABILITY; INTER-STELLAR CLOUDS; GAS-PHASE CHEMISTRY; T-TAURI DISKS; ACCRETION DISKS; IONIZATION FRACTION; PROTOSTELLAR DISKS AB We present the results of models of the chemistry, including deuterium, in the inner regions of protostellar disks. We find good agreement with recent gas-phase observations of several (non-deuterated) species. We also compare our results with observations of comets and find that in the absence of other processing, e. g., in the accretion shock at the surface of the disk, or by mixing in the disk, the calculated D/H ratios in ices are higher than measured and reflect the D/H ratio set in the molecular cloud phase. Our models give quite different abundances and molecular distributions to other inner disk models because of the differences in physical conditions in the model disk. This emphasizes how changes in the assumptions about the density and temperature distribution can radically affect the results of chemical models. C1 [Willacy, K.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Woods, P. M.] Univ Manchester, Jodrell Bank, Ctr Astrophys, Sch Phys & Astron, Manchester M13 9PL, Lancs, England. RP Willacy, K (reprint author), CALTECH, Jet Prop Lab, MS 169-506, Pasadena, CA 91109 USA. EM Karen.Willacy@jpl.nasa.gov; Paul.Woods@manchester.ac.uk RI Woods, Paul/E-6926-2011 OI Woods, Paul/0000-0003-4340-3590 FU National Aeronautics and Space Administration FX This research was conducted at the Jet Propulsion Laboratory, California Institute of Technology under contract with the National Aeronautics and Space Administration. Partial support was provided to K. W. by a grant from the NASA TPF Foundation Science program. A portion of this research was carried out while P. M. W. was supported by an appointment to the NASA Postdoctoral Program at JPL, administered by ORAU through a contract with NASA. We also wish to acknowledge the helpful comments of Bockelee-Morvan concerning the measurements of the D/H ratio in cometary water. NR 129 TC 55 Z9 55 U1 0 U2 11 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 SEP PY 2009 VL 703 IS 1 BP 479 EP 499 DI 10.1088/0004-637X/703/1/479 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 492AE UT WOS:000269625000041 ER PT J AU Fischer, CF Tachiev, G Rubin, RH Rodriguez, M AF Fischer, C. Froese Tachiev, G. Rubin, R. H. Rodriguez, M. TI ANALYSIS OF BREIT-PAULI TRANSITION PROBABILITIES FOR LINES IN O III SO ASTROPHYSICAL JOURNAL LA English DT Article DE atomic data; atomic processes ID TELESCOPE ECHELLE SPECTROPHOTOMETRY; OSCILLATOR-STRENGTHS; BOWEN FLUORESCENCE; ORION-NEBULA; CROSS-SECTIONS; ENERGY-LEVELS; ATOMIC DATA; SPECTROSCOPY; LIFETIME; OXYGEN AB Accurate atomic data are essential for understanding the properties of both O III lines produced by the Bowen fluorescence mechanism and [O III] forbidden lines observed in numerous gaseous nebulae. Improved Breit-Pauli transition probabilities have been published for the carbon sequence. Included were revised data for O III. The present paper analyzes the accuracy of the data specifically for O III by comparison with other theory as well as some recent experiments and observations. For the electric dipole transition probabilities, good agreement is found for allowed Bowen fluorescence lines between predictions of intensity ratios with observed data. For forbidden transitions, the Breit-Pauli magnetic dipole transition operator requires corrections that often are neglected. Good agreement is found when these transition probabilities are computed with multiconfiguration Dirac-Hartree-Fock methods. C1 [Fischer, C. Froese] Natl Inst Stand & Technol, Gaithersburg, MD 20899 USA. [Tachiev, G.] Florida Int Univ, Miami, FL 33199 USA. [Rubin, R. H.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Rubin, R. H.] Orion Enterprises, Moffett Field, CA 94035 USA. [Rubin, R. H.] Peking Univ, Kavli Inst Astron & Astrophys, Beijing 100871, Peoples R China. [Rodriguez, M.] Inst Nacl Astrofis Opt & Electr, Puebla 72000, Mexico. RP Fischer, CF (reprint author), Natl Inst Stand & Technol, Gaithersburg, MD 20899 USA. EM charlotte.fischer@nist.gov FU NASA [HST-AR-10973.01-A, NAS5-26555]; Mexican CONACYT [50359-F] FX We are grateful to Xiao-wei Liu for providing some past history regarding the observations and theory pertaining to the lambdaair = 4931 angstrom line. We thank NASA Ames summer students Julia Fang and Patrick Maher for their help measuring the HST/STIS spectral lines. Partial support for this publication was provided by NASA through Program number HST-AR-10973.01-A (PI RR) from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, under NASA contract NAS5-26555. M. R. acknowledges support from Mexican CONACYT project 50359-F. NR 36 TC 3 Z9 3 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 SEP PY 2009 VL 703 IS 1 BP 500 EP 506 DI 10.1088/0004-637X/703/1/500 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 492AE UT WOS:000269625000042 ER PT J AU Rozo, E Rykoff, ES Koester, BP McKay, T Hao, JG Evrard, A Wechsler, RH Hansen, S Sheldon, E Johnston, D Becker, M Annis, J Bleem, L Scranton, R AF Rozo, Eduardo Rykoff, Eli S. Koester, Benjamin P. McKay, Timothy Hao, Jiangang Evrard, August Wechsler, Risa H. Hansen, Sarah Sheldon, Erin Johnston, David Becker, Matthew Annis, James Bleem, Lindsey Scranton, Ryan TI IMPROVEMENT OF THE RICHNESS ESTIMATES OF maxBCG CLUSTERS SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology: observations; methods: data analysis ID DIGITAL SKY SURVEY; FLUX-LIMITED SAMPLE; X-RAY LUMINOSITY; SPECTROSCOPIC TARGET SELECTION; NEAR-INFRARED PROPERTIES; ADAPTIVE MATCHED-FILTER; GALAXY CLUSTERS; MASS FUNCTION; VELOCITY DISPERSION; MAGNITUDE RELATION AB Minimizing the scatter between cluster mass and accessible observables is an important goal for cluster cosmology. In this work, we introduce a new matched filter richness estimator, and test its performance using the maxBCG cluster catalog. Our new estimator significantly reduces the variance in the L(X)-richness relation, from sigma(ln) (2)(LX) = (0.86 +/- 0.02)(2) to sigma(ln) (2)(LX) = (0.69 +/- 0.02)(2). Relative to the maxBCG richness estimate, it also removes the strong redshift dependence of the L(X)-richness scaling relations, and is significantly more robust to photometric and redshift errors. These improvements are largely due to the better treatment of galaxy color data. We also demonstrate the scatter in the L(X)-richness relation depends on the aperture used to estimate cluster richness, and introduce a novel approach for optimizing said aperture which can easily be generalized to other mass tracers. C1 [Rozo, Eduardo] Ohio State Univ, CCAPP, Columbus, OH 43210 USA. [Rykoff, Eli S.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Koester, Benjamin P.; Hansen, Sarah; Becker, Matthew; Bleem, Lindsey] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Koester, Benjamin P.; Hansen, Sarah; Becker, Matthew] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [McKay, Timothy; Hao, Jiangang; Evrard, August] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA. [McKay, Timothy; Evrard, August] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [McKay, Timothy; Evrard, August] Michigan Ctr Theoret Phys, Ann Arbor, MI 48109 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. [Sheldon, Erin] NYU, Dept Phys, Ctr Cosmol & Particle Phys, New York, NY 10003 USA. [Johnston, David] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Annis, James] Fermilab Natl Accelerator Lab, Batavia, IL 60510 USA. [Scranton, Ryan] Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA. RP Rozo, E (reprint author), Ohio State Univ, CCAPP, Columbus, OH 43210 USA. RI Hao, Jiangang/G-3954-2011; McKay, Timothy/C-1501-2009; OI McKay, Timothy/0000-0001-9036-6150; Becker, Matthew/0000-0001-7774-2246; Evrard, August/0000-0002-4876-956X; Hao, Jiangang/0000-0003-0502-7571 FU U. S. Department of Energy [DE-AC02-76SF00515, DE-FG02-95ER40899]; Terman Fellowship; NSF [AST 0807304, AST-0708150]; Alfred P. Sloan Foundation; National Aeronautics and Space Administration; Japanese Monbukagakusho; Max Planck Society FX Funding for the creation and distribution of the SDSS Archive has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Aeronautics and Space Administration, the National Science Foundation, the U. S. Department of Energy, the Japanese Monbukagakusho, and the Max Planck Society. The SDSS Web site is http://www.sdss.org/. NR 97 TC 45 Z9 45 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 SEP PY 2009 VL 703 IS 1 BP 601 EP 613 DI 10.1088/0004-637X/703/1/601 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 492AE UT WOS:000269625000048 ER PT J AU Cherchneff, I Dwek, E AF Cherchneff, Isabelle Dwek, Eli TI THE CHEMISTRY OF POPULATION III SUPERNOVA EJECTA. I. FORMATION OF MOLECULES IN THE EARLY UNIVERSE SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrochemistry; early universe; molecular processes; supernovae: general ID CARBON-MONOXIDE; RADIATIVE ASSOCIATION; SN 1987A; DUST FORMATION; STAR-FORMATION; LIGHT-CURVE; RICH EJECTA; SHOCK-TUBE; 1ST STARS; MU-M AB We study the formation and destruction of molecules in the ejecta of Population III supernovae (SNe) using a chemical kinetic approach to follow the evolution of molecular abundances from day 100 to day 1000 after explosion. The chemical species included in the study range from simple diatomic molecules to more complex dust precursor species. All relevant molecule formation and destruction processes that are unique to the SN environment are considered. Our work focuses on zero-metallicity progenitors with masses of 20, 170, and 270 M-circle dot, and we study the effect of different levels of heavy element mixing and the inward diffusion of hydrogen and helium on the ejecta chemistry. We show that the ejecta chemistry does not reach a steady state within the relevant timespan (similar to 3 yr) for molecule formation, thus invalidating previous results relying on this assumption. The primary species formed in the harsh SN environment are O-2, CO, SiS, and SO. The SiO, formed as early as 200 days after explosion, is rapidly depleted by the formation of silica molecular precursors in the ejecta. The rapid conversion of CO to C-2 and its thermal fractionation at temperatures above 5000 K allow for the formation of carbon chains in the oxygen-rich zone of the unmixed models, providing an important pathway for the formation of carbon dust in hot environments where the C/O ratio is less than 1. We show that the fully mixed ejecta of a 170 M-circle dot progenitor synthesizes 11.3 M-circle dot of molecules, whereas 20 M-circle dot and 270 M-circle dot progenitors produce 0.78 M-circle dot and 3.2 M-circle dot of molecules, respectively. The admixing of 10% of hydrogen into the fully mixed ejecta of the 170 M-circle dot progenitor increases its molecular yield to similar to 47 M-circle dot. The unmixed ejecta of a 170 M-circle dot progenitor SN without hydrogen penetration synthesizes similar to 37 M-circle dot of molecules, whereas its 20 M-circle dot counterpart produces similar to 1.2 M-circle dot. This smaller efficiency at forming molecules is due to the large fraction of He+ in the outer mass zone of the ejecta. Finally, we discuss the cosmological implication of molecule formation by Pop III SNe in the early universe. C1 [Cherchneff, Isabelle] Univ Basel, Dept Phys, CH-4056 Basel, Switzerland. [Dwek, Eli] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA. RP Cherchneff, I (reprint author), Univ Basel, Dept Phys, CH-4056 Basel, Switzerland. EM isabelle.cherchneff@unibas.ch; eli.dwek@nasa.gov RI Dwek, Eli/C-3995-2012 FU Swiss National Science Foundation FX I. C. acknowledges support from the Swiss National Science Foundation through a Maria Heim-Vogtlin fellowship. NR 76 TC 50 Z9 50 U1 0 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD SEP PY 2009 VL 703 IS 1 BP 642 EP 661 DI 10.1088/0004-637X/703/1/642 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 492AE UT WOS:000269625000052 ER PT J AU Pineda, JL Ott, J Klein, U Wong, T Muller, E Hughes, A AF Pineda, Jorge L. Ott, Juergen Klein, Ulrich Wong, Tony Muller, Erik Hughes, Annie TI THE INFLUENCE OF FAR-ULTRAVIOLET RADIATION ON THE PROPERTIES OF MOLECULAR CLOUDS IN THE 30 DOR REGION OF THE LARGE MAGELLANIC CLOUD SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: ISM; ISM: molecules; ISM: structure; Magellanic Clouds ID CO-TO-H-2 CONVERSION FACTOR; SEST KEY PROGRAM; PHOTON-DOMINATED REGIONS; COMPLETE CO SURVEY; STAR-FORMATION; IRREGULAR GALAXIES; LOW-METALLICITY; MASS-SPECTRA; PHOTODISSOCIATION REGIONS; SPITZER SURVEY AB We present a complete (12)CO J = 1 -> 0 map of the prominent molecular ridge in the Large Magellanic Cloud (LMC) obtained with the 22 m ATNF Mopra Telescope. The region stretches southward by similar to 2 degrees. ( or 1.7 kpc) from 30 Doradus, the most vigorous star-forming region in the Local Group. The location of this molecular ridge is unique insofar as it allows us to study the properties of molecular gas as a function of the ambient radiation field in a low-metallicity environment. We find that the physical properties of CO-emitting clumps within the molecular ridge do not vary with the strength of the far-ultraviolet radiation field. Since the peak CO brightness of the clumps shows no correlation with the radiation field strength, the observed constant value for CO-to-H(2) conversion factor along the ridge seems to require an increase in the kinetic temperature of the molecular gas that is offset by a decrease in the angular filling factor of the CO emission. We find that the difference between the CO-to-H(2) conversion factor in the molecular ridge and the outer Milky Way is smaller than has been reported by previous studies of the CO emission: applying the same cloud identification and analysis methods to our CO observations of the LMC molecular ridge and CO data from the outer Galaxy survey by Dame et al., we find that the average CO-to-H(2) conversion factor in the molecular ridge is X(CO) similar or equal to (3.9 +/- 2.5) x 10(20) cm(-2) ( K km s(-1))(-1), approximately twice the value that we determine for the outer Galaxy clouds. The mass spectrum and the scaling relations between the properties of the CO clumps in the molecular ridge are similar, but not identical, to those that have been established for Galactic molecular clouds. C1 [Pineda, Jorge L.; Klein, Ulrich] Univ Bonn, Argelander Inst Astron, D-53121 Bonn, Germany. [Ott, Juergen] Natl Radio Astron Observ, Socorro, NM 87801 USA. [Wong, Tony] Univ New S Wales, Sch Phys, Sydney, NSW 2052, Australia. [Muller, Erik] Nagoya Univ, Dept Astrophys, Chikusa Ku, Nagoya, Aichi 4648602, Japan. [Hughes, Annie] Swinburne Univ Technol, Ctr Supercomp & Astrophys, Hawthorn, Vic 3122, Australia. [Ott, Juergen] CALTECH, Pasadena, CA 91125 USA. [Wong, Tony; Muller, Erik; Hughes, Annie] CSIRO, Australia Telescope Natl Facil, Epping, NSW 1710, Australia. RP Pineda, JL (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Jorge.Pineda@jpl.nasa.gov FU Deutsche Forschungs Gemeinschaft (DFG) [SFB 494] FX This work was supported by the Deutsche Forschungs Gemeinschaft (DFG) via Grant SFB 494. We thank Frank Israel for providing the SEST data set used to check the calibration of our data, Thomas Dame for providing the 2nd Quadrant data set, and Erik Rosolowsky for helping us with CLOUDPROPS, used to check our GAUSSCLUMPS decomposition, and with the error-in-variables procedure. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. We made use of the NASA/IPAC/IRAS/HiRES data reduction facilities. This research has made use of NASA's Astrophysics Data System Abstract Service. NR 87 TC 22 Z9 22 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP PY 2009 VL 703 IS 1 BP 736 EP 751 DI 10.1088/0004-637X/703/1/736 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 492AE UT WOS:000269625000060 ER PT J AU Lister, TA Anderson, DR Gillon, M Hebb, L Smalley, BS Triaud, AHMJ Cameron, AC Wilson, DM West, RG Bentley, SJ Christian, DJ Enoch, R Haswell, CA Hellier, C Horne, K Irwin, J Joshi, YC Kane, SR Mayor, M Maxted, PFL Norton, AJ Parley, N Pepe, F Pollacco, D Queloz, D Ryans, R Segransan, D Skillen, I Street, RA Todd, I Udry, S Wheatley, PJ AF Lister, T. A. Anderson, D. R. Gillon, M. Hebb, L. Smalley, B. S. Triaud, A. H. M. J. Cameron, A. Collier Wilson, D. M. West, R. G. Bentley, S. J. Christian, D. J. Enoch, R. Haswell, C. A. Hellier, C. Horne, K. Irwin, J. Joshi, Y. C. Kane, S. R. Mayor, M. Maxted, P. F. L. Norton, A. J. Parley, N. Pepe, F. Pollacco, D. Queloz, D. Ryans, R. Segransan, D. Skillen, I. Street, R. A. Todd, I. Udry, S. Wheatley, P. J. TI WASP-16b: A NEW JUPITER-LIKE PLANET TRANSITING A SOUTHERN SOLAR ANALOG SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems; stars: abundances; stars: individual (WASP-16b) ID MASS STARS; TELESCOPE; SUPERWASP; CANDIDATES; PHOTOMETRY; PROJECT; SEARCH; MODELS AB We report the discovery from WASP-South of a new Jupiter-like extrasolar planet, WASP-16b, which transits its solar analog host star every 3.12 days. Analysis of the transit photometry and radial velocity spectroscopic data leads to a planet with R(p) = 1.008 +/- 0.071 R(Jup) and M(p) = 0.855 +/- 0.059 M(Jup), orbiting a host star with R(*) = 0.946 +/- 0.054 R(circle dot) and M(*) = 1.022 +/- 0.101M(circle dot). Comparison of the high resolution stellar spectrum with synthetic spectra and stellar evolution models indicates the host star is a near-solar metallicity ([Fe/H] = 0.01 +/- 0.10) solar analog (T(eff) = 5700 +/- 150 K and log g = 4.5 +/- 0.2) of intermediate age (tau = 2.3(-2.2)(+5.8) Gyr). C1 [Lister, T. A.; Street, R. A.] Las Cumbres Observ, Goleta, CA 93117 USA. [Anderson, D. R.; Smalley, B. S.; Wilson, D. M.; Bentley, S. J.; Hellier, C.; Maxted, P. F. L.] Univ Keele, Astrophys Grp, Keele ST5 5BG, Staffs, England. [Gillon, M.; Triaud, A. H. M. J.; Mayor, M.; Pepe, F.; Queloz, D.; Segransan, D.; Udry, S.] Univ Geneva, Observ Geneva, CH-1290 Sauverny, Switzerland. [Gillon, M.] Univ Liege, Inst Astrophys & Geophys, Liege 1, Belgium. [Hebb, L.; Cameron, A. Collier; Enoch, R.; Horne, K.; Parley, N.] Univ St Andrews, Sch Phys & Astron, SUPA, St Andrews KY16 9SS, Fife, Scotland. [Wilson, D. M.] Univ Kent, Sch Phys Sci, Ctr Astrophys & Planetary Sci, Canterbury CT2 7NH, Kent, England. [West, R. G.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Christian, D. J.; Joshi, Y. C.; Pollacco, D.; Ryans, R.; Todd, I.] Queens Univ Belfast, Sch Math & Phys, Astrophys Res Ctr, Belfast BT7 1NN, Antrim, North Ireland. [Christian, D. J.] Calif State Univ Northridge, Northridge, CA 91330 USA. [Enoch, R.; Haswell, C. A.; Norton, A. J.; Parley, N.] Open Univ, Dept Phys & Astron, Milton Keynes MK7 6AA, Bucks, England. [Irwin, J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kane, S. R.] CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA. [Skillen, I.] Isaac Newton Grp Telescopes, E-38700 Tenerife, Spain. [Wheatley, P. J.] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. RP Lister, TA (reprint author), Las Cumbres Observ, 6740 Cortona Dr,Suite 102, Goleta, CA 93117 USA. EM tlister@lcogt.net RI Kane, Stephen/B-4798-2013; OI Norton, Andrew/0000-0001-7619-8269; Cameron, Andrew/0000-0002-8863-7828; Triaud, Amaury/0000-0002-5510-8751; Christian, Damian/0000-0003-1746-3020; Wheatley, Peter/0000-0003-1452-2240 FU South African Astronomical Observatory; consortium universities; UK's Science and Technology Facilities Council FX The WASP Consortium comprises the Universities of Keele, Leicester, St. Andrews, the Queen's University Belfast, the Open University, and the Isaac Newton Group. WASP-South is hosted by the South African Astronomical Observatory, and we are grateful for their support and assistance. Funding for WASP comes from the consortium universities and from the UK's Science and Technology Facilities Council. NR 22 TC 22 Z9 22 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 SEP PY 2009 VL 703 IS 1 BP 752 EP 756 DI 10.1088/0004-637X/703/1/752 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 492AE UT WOS:000269625000061 ER PT J AU Kim, DW Fabbiano, G Brassington, NJ Fragos, T Kalogera, V Zezas, A Jordan, A Sivakoff, GR Kundu, A Zepf, SE Angelini, L Davies, RL Gallagher, JS Juett, AM King, AR Pellegrini, S Sarazin, CL Trinchieri, G AF Kim, D. -W. Fabbiano, G. Brassington, N. J. Fragos, T. Kalogera, V. Zezas, A. Jordan, A. Sivakoff, G. R. Kundu, A. Zepf, S. E. Angelini, L. Davies, R. L. Gallagher, J. S. Juett, A. M. King, A. R. Pellegrini, S. Sarazin, C. L. Trinchieri, G. TI COMPARING GC AND FIELD LMXBs IN ELLIPTICAL GALAXIES WITH DEEP CHANDRA AND HUBBLE DATA SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: elliptical and lenticular, cD; galaxies: individual (NGC 3379, NGC 4278, NGC 4697); X-rays: binaries; X-rays: galaxies ID X-RAY BINARIES; GLOBULAR-CLUSTER CONNECTION; MULTIWAVELENGTH PROJECT; LUMINOSITY FUNCTION; BLACK-HOLE; ULTRACOMPACT BINARIES; SOURCE CATALOG; POINT SOURCES; CENTAURUS-A; NGC 3379 AB We present a statistical study of the low-mass X-ray binary (LMXB) populations of three nearby, old elliptical galaxies: NGC 3379, NGC 4278, and NGC 4697. With a cumulative similar to 1 Ms Chandra ACIS observing time, we detect 90-170 LMXBs within the D(25) ellipse of each galaxy. Cross-correlating Chandra X-ray sources and HST optical sources, we identify 75 globular cluster (GC) LMXBs and 112 field LMXBs with L(X) > 10(36) erg s(-1) ( detections of these populations are 90% complete down to luminosities in the range of 6 x 10(36) to 1.5 x 10(37) erg s(-1)). At the higher luminosities explored in previous studies, the statistics of this sample are consistent with the properties of GC-LMXBs reported in the literature. In the low-luminosity range allowed by our deeper data (L(X) < 5 x 10(37) erg s(-1)), we find a significant relative lack of GC-LMXBs, when compared with field sources. Using the co-added sample from the three galaxies, we find that the incompleteness-corrected X-ray luminosity functions (XLFs) of GC and field LMXBs differ at similar to 4 sigma significance at L(X) < 5 x 10(37) erg s(-1). As previously reported, these XLFs are consistent at higher luminosities. The presently available theoretical models for LMXB formation and evolution in clusters are not sophisticated enough to provide a definite explanation for the shape of the observed GC-LMXB XLF. Our observations may indicate a potential predominance of GC-LMXBs with donors evolved beyond the main sequence, when compared to current models, but their efficient formation requires relatively high initial binary fractions in clusters. The field LMXB XLF can be fitted with either a single power-law model plus a localized excess at a luminosity of (5-6) x 10(37) erg s(-1), or a broken power law with a similar low-luminosity break. This XLF may be explained with NS-red-giant LMXBs, contributing to similar to 15% of total LMXBs population at similar to 5 x 10(37) erg s(-1). The difference in the GC and field XLFs is consistent with different origins and/or evolutionary paths between the two LMXB populations, although a fraction of the field sources are likely to have originated in GCs. C1 [Kim, D. -W.; Fabbiano, G.; Brassington, N. J.; Zezas, A.; Jordan, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Fragos, T.; Kalogera, V.] Northwestern Univ, Dept Phys & Astron, Evanston, IL 60208 USA. [Jordan, A.] Pontificia Univ Catolica Chile, Dept Astron & Astrofis, Santiago 22, Chile. [Sivakoff, G. R.; Sarazin, C. L.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. [Kundu, A.; Zepf, S. E.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. [Angelini, L.; Juett, A. M.] NASA, Goddard Space Flight Ctr, High Energy Astrophys Lab, Greenbelt, MD 20771 USA. [Davies, R. L.] Univ Oxford, Oxford, England. [Gallagher, J. S.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. [King, A. R.] Univ Leicester, Leicester LE1 7RH, Leics, England. [Pellegrini, S.] Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy. [Trinchieri, G.] Osserv Astron Brera, INAF, I-20121 Milan, Italy. RP Kim, DW (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM kim@cfa.harvard.edu; gfabbiano@cfa.harvard.edu; vicky@northwestern.edu; azezas@cfa.harvard.edu; ajordan@astro.puc.cl; grs8g@virginia.edu; zepf@pa.msu.edu; angelini@davide.gsfc.nasa.gov; rld@astro.ox.ac.uk; jsg@astro.wisc.edu; Adrienne.M.Juett@nasa.gov; ark@star.le.ac.uk; silvia.pellegrini@unibo.it; cls7i@virginia.edu; ginevra.trinchieri@brera.inaf.it RI Sivakoff, Gregory/G-9602-2011; Zezas, Andreas/C-7543-2011; Fragos, Tassos/A-3581-2016; OI Sivakoff, Gregory/0000-0001-6682-916X; Zezas, Andreas/0000-0001-8952-676X; Trinchieri, Ginevra/0000-0002-0227-502X; Fragos, Tassos/0000-0003-1474-1523; Jordan, Andres/0000-0002-5389-3944 FU CXC CIAO; CALDB; Chandra GO [G06-7079A, G06-7079B, GO7-8078X, GO7-8089A, GO8-9085X]; NASA [NAS8-03060, NAG5-13056]; Northwestern University; Hubble [HST-GO-10597.03-A, HST-GO-10582.02-A, HST-GO-10835.01-A]; Kavli Institute for Theoretical Physics; National Science Foundation [PHY05-51164] FX We thank Chris Deloye, Natalia Ivanova, and Fred Rasio for very useful discussions. The data analysis was supported by the CXC CIAO software and CALDB. We have used the NASA NED and ADS facilities, and have extracted archival data from the Chandra archives. This work was supported by the Chandra GO grant G06-7079A ( PI: Fabbiano) and subcontract G06-7079B ( PI: Kalogera). We acknowledge partial support from NASA contract NAS8-03060 ( CXC). D.-W.K. acknowledges support from Chandra archival research grant AR6-7008X, and A.Z. from NASA LTSA grant NAG5-13056. T. F. acknowledges support by a Northwestern University Presidential Fellowship. G. S., C. S., and A.J. were supported in part by Hubble grants HST-GO-10597.03-A, HST-GO-10582.02-A, and HST-GO-10835.01-A, and Chandra grants GO7-8078X, GO7-8089A, and GO8-9085X. G. F., T. F., and V. K. also acknowledge support by the Kavli Institute for Theoretical Physics at UCSB where part of this work was completed. This research was supported in part by the National Science Foundation under Grant PHY05-51164. NR 74 TC 45 Z9 45 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 SEP PY 2009 VL 703 IS 1 BP 829 EP 844 DI 10.1088/0004-637X/703/1/829 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 492AE UT WOS:000269625000067 ER PT J AU Hwang, U Laming, JM AF Hwang, Una Laming, J. Martin TI THE CIRCUMSTELLAR MEDIUM OF CASSIOPEIA A INFERRED FROM THE OUTER EJECTA KNOT PROPERTIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; supernova remnants; X-rays: individual (Cassiopeia A) ID SUPERNOVA REMNANT CASSIOPEIA; CORE-COLLAPSE SUPERNOVAE; X-RAY; SHOCK BREAKOUT; A SUPERNOVA; MASSIVE STARS; ACCELERATED ELECTRONS; EMISSION; PROGENITORS; EXPLOSION AB We investigate the effect of the circumstellar medium density profile on the X-ray emission from outer ejecta knots in the Cassiopeia A supernova remnant using the 1 Ms Chandra observation. The spectra of a number of radial series of ejecta knots at various positions around the remnant are analyzed using techniques similar to those devised in previous papers. We can obtain a reasonable match to our data for a circumstellar density profile proportional to r(-2) as would arise from the steady dense wind of a red supergiant, but the agreement is improved if we introduce a small (0.2-0.3 pc) central cavity around the progenitor into our models. Such a profile might arise if the progenitor emitted a fast tenuous stellar wind for a short period immediately prior to explosion. We review other lines of evidence supporting this conclusion. The spectra also indicate the widespread presence of Fe-enriched plasma that was presumably formed by complete Si burning during the explosion, possibly via alpha-rich freezeout. This component is typically associated with hotter and more highly ionized gas than the bulk of the O- and Si-rich ejecta. C1 [Hwang, Una] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Hwang, Una] Johns Hopkins Univ, Baltimore, MD 21218 USA. [Laming, J. Martin] USN, Res Lab, Div Space Sci, Washington, DC 20375 USA. RP Hwang, U (reprint author), NASA, Goddard Space Flight Ctr, Code 662, Greenbelt, MD 20771 USA. EM Una.Hwang-1@nasa.gov FU NASA LTSA [NNG06GB89G]; Office of Naval Research FX U. H. and J.M.L. acknowledge support through NASA LTSA grant NNG06GB89G. J. M. L. was also supported by basic research funds of the Office of Naval Research. We thank Roger Chevalier and the anonymous referee for helpful comments on the paper. NR 47 TC 17 Z9 17 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 SEP PY 2009 VL 703 IS 1 BP 883 EP 893 DI 10.1088/0004-637X/703/1/883 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 492AE UT WOS:000269625000071 ER PT J AU Giodini, S Pierini, D Finoguenov, A Pratt, GW Boehringer, H Leauthaud, A Guzzo, L Aussel, H Bolzonella, M Capak, P Elvis, M Hasinger, G Ilbert, O Kartaltepe, JS Koekemoer, AM Lilly, SJ Massey, R McCracken, HJ Rhodes, J Salvato, M Sanders, DB Scoville, NZ Sasaki, S Smolcic, V Taniguchi, Y Thompson, D AF Giodini, S. Pierini, D. Finoguenov, A. Pratt, G. W. Boehringer, H. Leauthaud, A. Guzzo, L. Aussel, H. Bolzonella, M. Capak, P. Elvis, M. Hasinger, G. Ilbert, O. Kartaltepe, J. S. Koekemoer, A. M. Lilly, S. J. Massey, R. McCracken, H. J. Rhodes, J. Salvato, M. Sanders, D. B. Scoville, N. Z. Sasaki, S. Smolcic, V. Taniguchi, Y. Thompson, D. CA COSMOS Collaboration TI STELLAR AND TOTAL BARYON MASS FRACTIONS IN GROUPS AND CLUSTERS SINCE REDSHIFT 1 SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmological parameters; cosmology: observations; diffuse radiation; galaxies: clusters: general; galaxies: stellar content; X-rays: galaxies: clusters ID EVOLUTION SURVEY COSMOS; NEARBY GALAXY CLUSTERS; X-RAY LUMINOSITY; DIFFUSE OPTICAL LIGHT; DIGITAL SKY SURVEY; WIDE-FIELD SURVEY; COLD DARK-MATTER; M-T RELATION; STAR-FORMATION; XMM-NEWTON AB We investigate if the discrepancy between estimates of the total baryon mass fraction obtained from observations of the cosmic microwave background (CMB) and of galaxy groups/clusters persists when a large sample of groups is considered. To this purpose, 91 candidate X-ray groups/poor clusters at redshift 0.1 <= z <= 1 are selected from the COSMOS 2 deg(2) survey, based only on their X-ray luminosity and extent. This sample is complemented by 27 nearby clusters with a robust, analogous determination of the total and stellar mass inside R(500). The total sample of 118 groups and clusters with z <= 1 spans a range in M(500) of similar to 10(13)-10(15) M(circle dot). We find that the stellar mass fraction associated with galaxies at R(500) decreases with increasing total mass as M(500)(-0.37+/-0.04), independent of redshift. Estimating the total gas mass fraction from a recently derived, high-quality scaling relation, the total baryon mass fraction (f(500)(stars+gas) = f(500)(stars) + f(500)(gas)) is found to increase by similar to 25%, when M(500) increases from < M > = 5 x 10(13) M(circle dot) to < M > = 7 x 10(14)M(circle dot). After consideration of a plausible contribution due to intracluster light (11%-22% of the total stellar mass) and gas depletion through the hierarchical assembly process (10% of the gas mass), the estimated values of the total baryon mass fraction are still lower than the latest CMB measure of the same quantity (WMAP5), at a significance level of 3.3 sigma for groups of < M > = 5 x 10(13) M(circle dot). The discrepancy decreases toward higher total masses, such that it is 1 sigma at < M > = 7 x 10(14) M(circle dot). We discuss this result in terms of nongravitational processes such as feedback and filamentary heating. C1 [Giodini, S.; Pierini, D.; Finoguenov, A.; Pratt, G. W.; Boehringer, H.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Finoguenov, A.] Univ Maryland, Baltimore, MD 21250 USA. [Leauthaud, A.] Univ Calif Berkeley, LBNL, Berkeley, CA 94720 USA. [Leauthaud, A.] Univ Calif Berkeley, Berkeley Ctr Cosmol Phys, Berkeley, CA 94720 USA. [Guzzo, L.] INAF, Osservatorio Astron Brera, I-23807 Merate, LC, Italy. [Aussel, H.] Univ Paris 07, AIM Unite Mixte Rech, CEA, CNRS,UMR N158, Paris, France. [Bolzonella, M.] INAF, Bologna Astron Observ, I-40127 Bologna, Italy. [Capak, P.; Scoville, N. Z.] Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Capak, P.; Massey, R.; Rhodes, J.; Salvato, M.; Smolcic, V.; Thompson, D.] CALTECH, Pasadena, CA 91125 USA. [Elvis, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Hasinger, G.] Max Planck Inst Plasma Phys, D-85748 Garching, Germany. [Ilbert, O.; Kartaltepe, J. S.; Sanders, D. B.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Koekemoer, A. M.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Lilly, S. J.] ETH, Inst Astron, Dept Phys, CH-8093 Zurich, Switzerland. [McCracken, H. J.] Univ Paris 06, Inst Astrophys, UMR 7095, CNRS, F-75014 Paris, France. [Rhodes, J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Sasaki, S.] Tohoku Univ, Astron Inst, Grad Sch Sci, Aoba Ku, Sendai, Miyagi 9808578, Japan. [Sasaki, S.] Ehime Univ, Dept Phys, Grad Sch Sci & Engn, Matsuyama, Ehime 7908577, Japan. [Taniguchi, Y.] Ehime Univ, Res Ctr Space & Cosm Evolut, Matsuyama, Ehime 7908577, Japan. [Thompson, D.] Univ Arizona, Large Binocular Telescope Observ, Tucson, AZ 85721 USA. RP Giodini, S (reprint author), Max Planck Inst Extraterr Phys, Giessenbachstr, D-85748 Garching, Germany. RI Bolzonella, Micol/O-9495-2015; OI Bolzonella, Micol/0000-0003-3278-4607; Koekemoer, Anton/0000-0002-6610-2048 NR 84 TC 177 Z9 177 U1 0 U2 7 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 SEP PY 2009 VL 703 IS 1 BP 982 EP 993 DI 10.1088/0004-637X/703/1/982 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 492AE UT WOS:000269625000081 ER PT J AU Gliozzi, M Papadakis, IE Eracleous, M Sambruna, RM Ballantyne, DR Braito, V Reeves, JN AF Gliozzi, Mario Papadakis, Iossif E. Eracleous, Michael Sambruna, Rita M. Ballantyne, David R. Braito, Valentina Reeves, James N. TI SHORT-TERM VARIABILITY AND POWER SPECTRAL DENSITY ANALYSIS OF THE RADIO-LOUD ACTIVE GALACTIC NUCLEUS 3C 390.3 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: nuclei; X-rays: galaxies ID RAY-TIMING-EXPLORER; BALMER EMISSION-LINES; PHOTON IMAGING CAMERA; XMM-NEWTON VIEW; X-RAY; SEYFERT-1 GALAXIES; SIMULTANEOUS RXTE; LONG; ACCRETION; 4C+74.26 AB We investigate the short-term variability properties and the power spectral density (PSD) of the broad-line radio galaxy (BLRG) 3C 390.3 using observations made by XMM-Newton, RXTE, and Suzaku on several occasions between 2004 October and 2006 December. The main aim of this work is to derive model-independent constraints on the origin of the X-ray emission and on the nature of the central engine in 3C 390.3. On timescales of the order of few hours, probed by uninterrupted XMM-Newton light curves, the flux of 3C 390.3 is consistent with being constant in all energy bands. On longer timescales, probed by the 2-day RXTE and Suzaku observations, the flux variability becomes significant. The latter observation confirms that the spectral variability behavior of 3C 390.3 is consistent with the spectral evolution observed in (radio-quiet) Seyfert galaxies: the spectrum softens as the source brightens. The correlated variability between soft and hard X-rays, observed during the Suzaku exposure and between the two XMM-Newton pointings, taken 1 week apart, argues against scenarios characterized by the presence of two distinct variable components in the 0.5-10 keV X-ray band. A detailed PSD analysis carried out over five decades in frequency suggests the presence of a break at T(br) = 43(-25)(+34) days at a 92% confidence level. This is the second tentative detection of a PSD break in a radio-loud, non-jet dominated active galactic nucleus (AGN), after the BLRG 3C 120, and appears to be in general agreement with the relation between T(br), M(BH), and L(bol), followed by Seyfert galaxies. Our results indicate that the X-ray variability properties of 3C 390.3 are broadly consistent with those of radio-quiet AGN, suggesting that the X-ray emission mechanism in 3C 390.3 is similar to that of nearby Seyfert galaxies without any significant contribution from a jet component. C1 [Gliozzi, Mario] George Mason Univ, Fairfax, VA 22030 USA. [Papadakis, Iossif E.] Univ Crete, Dept Phys, Khania, Greece. [Papadakis, Iossif E.] Fdn Res & Technol, IESL, Iraklion 71110, Greece. [Eracleous, Michael] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Sambruna, Rita M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Ballantyne, David R.] Georgia Inst Technol, Ctr Relativist Astrophys, Sch Phys, Atlanta, GA 30032 USA. [Braito, Valentina] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Reeves, James N.] Univ Keele, Astrophys Grp, Sch Phys & Geog Sci, Keele ST5 5BG, Staffs, England. [Eracleous, Michael] Penn State Univ, Ctr Gravitat Wave Phys, University Pk, PA 16802 USA. RP Gliozzi, M (reprint author), George Mason Univ, 4400 Univ Dr, Fairfax, VA 22030 USA. RI Papadakis, Iossif/C-3235-2011; XRAY, SUZAKU/A-1808-2009; OI Braito, Valentina/0000-0002-2629-4989 FU NASA; EU [MTKD-CT-2006-039965] FX We acknowledge support from NASA through the Suzaku and XMM-Newton programs. I. E. P. acknowledges support by the EU grant MTKD-CT-2006-039965. NR 47 TC 4 Z9 4 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 SEP PY 2009 VL 703 IS 1 BP 1021 EP 1029 DI 10.1088/0004-637X/703/1/1021 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 492AE UT WOS:000269625000084 ER PT J AU Weber, AS Hodyss, R Johnson, PV Willacy, K Kanik, I AF Weber, Amanda S. Hodyss, Robert Johnson, Paul V. Willacy, Karen Kanik, Isik TI HYDROGEN-DEUTERIUM EXCHANGE IN PHOTOLYZED METHANE-WATER ICES SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrochemistry; ISM: molecules; methods: laboratory; molecular processes; radiation mechanisms: non-thermal ID DEUTERATED MOLECULES; SOLID METHANOL; B2 HYAKUTAKE; RATIO; HYDROCARBONS; ENRICHMENT; ABUNDANCE; CHEMISTRY; ANALOGS; COMETS AB Previous work has concluded that H-D exchange occurs readily in polycyclic aromatic hydrocarbons frozen in deuterated water (D(2)O) irradiated with ultraviolet light. Here, we examine H-D exchange in methane-water ices following exposure to ultraviolet radiation and analyze the products formed as a result. We find that H-D exchange also occurs in methane-water ices by means of ultraviolet photolysis. Exchange proceeds through a radical mechanism that implies that almost all organic species will undergo significant H-D exchange with the matrix in water ices exposed to ultraviolet radiation. Given sufficient energetic processing of the ice, the H/D ratio of an ice matrix may be transferred to the organic species in the ice. C1 [Weber, Amanda S.; Hodyss, Robert; Johnson, Paul V.; Willacy, Karen; Kanik, Isik] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Weber, AS (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Robert.P.Hodyss@jpl.nasa.gov RI Johnson, Paul/D-4001-2009 OI Johnson, Paul/0000-0002-0186-8456 FU NASA FX This researchwas carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration and funded through the internal Research and Technology Development program. A. S. W. was sponsored by the NASA's Undergraduate Student Research Program. We also thank an anonymous reviewer whose comments greatly improved this manuscript. NR 26 TC 8 Z9 8 U1 0 U2 7 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 SEP PY 2009 VL 703 IS 1 BP 1030 EP 1033 DI 10.1088/0004-637X/703/1/1030 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 492AE UT WOS:000269625000085 ER PT J AU Stephens, DC Leggett, SK Cushing, MC Marley, MS Saumon, D Geballe, TR Golimowski, DA Fan, XH Noll, KS AF Stephens, D. C. Leggett, S. K. Cushing, Michael C. Marley, Mark S. Saumon, D. Geballe, T. R. Golimowski, David A. Fan, Xiaohui Noll, K. S. TI THE 0.8-14.5 mu m SPECTRA OF MID-L TO MID-T DWARFS: DIAGNOSTICS OF EFFECTIVE TEMPERATURE, GRAIN SEDIMENTATION, GAS TRANSPORT, AND SURFACE GRAVITY SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars: individual (2MASS J00361617+1821104, 2MASS J05591914-1404488, 2MASS J08251968+2115521, 2MASS J09083803+5032088, 2MASS J15074769-1627386, 2MASS J22244381-0158521, 2MASS J22443167+2043433, 2MASS J22541892+3123498, DENIS-P J025503.3-470049, SDSS J000013.54+255418.6, SDSS J075840.32+324723.3, SDSS J080531.83+481233.1, SDSS J085758.44+570851.4, SDSS J105213.50+442255.6AB, SDSS J111009.99+011613.0, SDSS J115553.85+055957.5, SDSS J120747.17+024424.8, SDSS J125453.90-012247.5, SDSS J133148.88-011652.5, SDSS J151643.00+305344.3, SDSS J152039.82+354619.8); stars: low-mass, brown dwarfs ID SPITZER-SPACE-TELESCOPE; DIGITAL SKY SURVEY; LOW-MASS STARS; FIELD L-DWARFS; EXTRASOLAR GIANT PLANETS; COLOR-MAGNITUDE DIAGRAMS; INFRARED ARRAY CAMERA; EXOPLANET HOST STAR; BROWN DWARFS; L/T TRANSITION AB We present new 5.2-14.5 mu m low-resolution spectra of 14 mid-L to mid-T dwarfs. We also present new 3.0-4.1 mu m spectra for five of these dwarfs. These data are supplemented by existing red and near-infrared spectra (similar to 0.6-2.5 mu m), as well as red through mid-infrared spectroscopy of seven other L and T dwarfs presented by Cushing et al. We compare these spectra to those generated from the model atmospheres of Saumon & Marley. The models reproduce the observed spectra well, except in the case of one very red L3.5 dwarf, 2MASS J22244381-0158521. The broad wavelength coverage allows us to constrain almost independently the four parameters used to describe these photospheres in our models: effective temperature (T(eff)), surface gravity, grain sedimentation efficiency (f(sed)), and vertical gas transport efficiency (K(zz)). The CH(4) bands centered at 2.2, 3.3, and 7.65 mu m and the CO band at 2.3 mu m are sensitive to K(zz), and indicates that chemical mixing is important in all L and T dwarf atmospheres. The sample of L3.5 to T5.5 dwarfs spans the range 1800 K greater than or similar to T(eff) greater than or similar to 1000 K, with an L-T transition (spectral types L7 to T4) that lies between 1400 and 1100 K for dwarfs with typical near-infrared colors; bluer and redder dwarfs can be 100 K warmer or cooler, respectively, when using infrared spectral types. When using optical spectral types, the bluer dwarfs have more typical T(eff) values as they tend to have earlier optical spectral types. In this model analysis, f(sed) increases rapidly between types T0 and T4, indicating that increased sedimentation can explain the rapid disappearance of clouds at this stage of brown dwarf evolution. There is a suggestion that the transition to dust-free atmospheres happens at lower temperatures for lower gravity dwarfs. C1 [Stephens, D. C.] Brigham Young Univ, Dept Phys & Astron, Provo, UT 84602 USA. [Leggett, S. K.; Geballe, T. R.] No Operat Ctr, Gemini Observ, Hilo, HI 96720 USA. [Cushing, Michael C.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Marley, Mark S.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Saumon, D.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA. [Golimowski, David A.; Noll, K. S.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Fan, Xiaohui] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. RP Stephens, DC (reprint author), Brigham Young Univ, Dept Phys & Astron, N486 ESC, Provo, UT 84602 USA. EM denise_stephens@byu.edu RI Noll, Keith/C-8447-2012; Marley, Mark/I-4704-2013 FU Spitzer Cycle 1 and 2 Guest Observer Programs [3431, 20514]; Gemini Observatory; Spitzer Cycle 3 Theory; NASA [NAG5-13127]; National Science Foundation; SIMBAD database FX This work is based on observations made with the Spitzer Space Telescope and the Gemini North Observatory through programs GN-2005A-Q-23 and GN-2006B-Q-37. Spitzer is operated by the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. Gemini Observatory is operated by the Association of Universities for Research in Astronomy, Inc., under a cooperative agreement with the NSF on behalf of the Gemini partnership: the National Science Foundation (United States), the Science and Technology Facilities Council (United Kingdom), the National Research Council (Canada), CONICYT (Chile), the Australian Research Council (Australia), Ministerio da Ciencia e Technologia (Brazil), and Ministerio da Ciencia Tecnologia e Innovacion Productiva (Argentina). This work has been supported in part by funds from the Spitzer Cycle 1 and 2 Guest Observer Programs 3431 and 20514 granted through the California Institute of Technology. S.K.L.'s and T.R.G.'s research is supported by Gemini Observatory. D.S.'s contribution was supported by a Spitzer Cycle 3 Theory grant. D.C.S.'s acquisition and reduction of Gemini data was funded by NASA Grant NAG5-13127. This publication makes 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, and funded by the National Aeronautics and Space Administration and the National Science Foundation, the SIMBAD database, operated at CDS, Strasbourg, France, and NASA's Astrophysics Data System Bibliographic Services. NR 99 TC 168 Z9 168 U1 1 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 SEP 1 PY 2009 VL 702 IS 1 BP 154 EP 170 DI 10.1088/0004-637X/702/1/154 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 487BD UT WOS:000269244500013 ER PT J AU Frankel, M Beiersdorfer, P Brown, GV Gu, MF Kelley, RL Kilbourne, CA Porter, FS AF Frankel, M. Beiersdorfer, P. Brown, G. V. Gu, M. F. Kelley, R. L. Kilbourne, C. A. Porter, F. S. TI X-RAY SIGNATURE OF CHARGE EXCHANGE IN L-SHELL SULFUR IONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE atomic data; atomic processes; line: formation; line: identification; planets and satellites: individual (Jupiter); X-rays: individual (Jupiter, laboratory) ID SOLAR-WIND IONS; CROSS-SECTIONS; XMM-NEWTON; HE-LIKE; SPECTRA; ENERGY; COLLISIONS; TRAP; EBIT; MICROCALORIMETER AB The X-ray signature of L-shell charge exchange in sulfur was studied in the laboratory. A comparison of the charge exchange (CX) spectra with those obtained under electron-impact excitation showed marked differences. In the CX spectra, an enhancement was observed in the transitions from levels with high principal quantum numbers, n = 4, 5, 6 -> n = 2 in comparison with the n = 3 -> n = 2 transitions that dominate the direct excitation spectra. An even greater enhancement was recorded in the transitions from the levels of electron capture to the ground states: n = 7, 8, 9 -> n = 2. The spectra mainly consist of emission from S XIV, but lower charge states such as S XIII, S XII, and S xi also contribute. The results have been compared with observations made by the Chandra and XMM-Newton X-ray Observatories of Jupiter's polar regions. The enhancement we noticed in transitions from the high-n levels is not seen in the Chandra spectra. C1 [Frankel, M.; Beiersdorfer, P.; Brown, G. V.; Gu, M. F.] Univ Calif Berkeley, Lawrence Berkeley Lab, Berkeley, CA 94720 USA. [Beiersdorfer, P.; Gu, M. F.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Kelley, R. L.; Kilbourne, C. A.; Porter, F. S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Frankel, M (reprint author), Univ Calif Berkeley, Lawrence Berkeley Lab, Berkeley, CA 94720 USA. EM frankel4@llnl.gov; beiersdorfer1@llnl.gov RI Porter, Frederick/D-3501-2012; Kelley, Richard/K-4474-2012 OI Porter, Frederick/0000-0002-6374-1119; FU U.S. Department of Energy [DE-AC52-07NA27344]; NASA [NNG06GB11G]; Laboratory Directed Research and Development Program [06-ERD-010] FX Work at LLNL was performed under the auspices of the U.S. Department of Energy by Lawrence Livermore National Laboratory under Contract DE-AC52-07NA27344 and was in part supported by NASA, including through grant NNG06GB11G from the Planetary Atmospheres Program to UC Berkeley and through support from the Astronomy and Physics Research and Analysis Program received by LLNL, SAO, and GSFC. Part of the work was funded by the Laboratory Directed Research and Development Program at LLNL under project tracking number 06-ERD-010.r M. F. would like to thank Prof. Tomas Brage as well as Dr. P.O. Zetterberg and Dr. Carl-Erik Magnusson at Lund University, Lund, Sweden, for their continued support during her stay at Livermore. The authors wish to thank Joel Clementson, Daniel Thorn, and Ed Magee for their technical support and advice. NR 41 TC 5 Z9 5 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 SEP 1 PY 2009 VL 702 IS 1 BP 171 EP 177 DI 10.1088/0004-637X/702/1/171 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 487BD UT WOS:000269244500014 ER PT J AU Yusef-Zadeh, F Hewitt, JW Arendt, RG Whitney, B Rieke, G Wardle, M Hinz, JL Stolovy, S Lang, CC Burton, MG Ramirez, S AF Yusef-Zadeh, F. Hewitt, J. W. Arendt, R. G. Whitney, B. Rieke, G. Wardle, M. Hinz, J. L. Stolovy, S. Lang, C. C. Burton, M. G. Ramirez, S. TI STAR FORMATION IN THE CENTRAL 400 PC OF THE MILKY WAY: EVIDENCE FOR A POPULATION OF MASSIVE YOUNG STELLAR OBJECTS SO ASTROPHYSICAL JOURNAL LA English DT Review DE galaxies: starburst; Galaxy: center; ISM: clouds; masers; stars: formation ID GALACTIC-CENTER REGION; INFRARED-DARK CLOUDS; 2-DIMENSIONAL RADIATIVE-TRANSFER; SPECTRAL ENERGY-DISTRIBUTIONS; MIDCOURSE-SPACE-EXPERIMENT; CENTER MOLECULAR CLOUDS; GIANT BRANCH STARS; 1612 MHZ SURVEY; 70 MU-M; METHANOL MASERS AB The central kpc of the Milky Way might be expected to differ significantly from the rest of the Galaxy with regard to gasdynamics and the formation of young stellar objects (YSOs). We probe this possibility with mid-infrared observations obtained with Infrared Array Camera and Multiband Imaging Photometer on Spitzer and with Midcourse Space Experiment. We use color-color diagrams and spectral energy distribution (SED) fits to explore the nature of YSO candidates (including objects with 4.5 mu m excesses possibly due to molecular emission). There is an asymmetry in the distribution of the candidate YSOs, which tend to be found at negative Galactic longitudes; this behavior contrasts with that of the molecular gas, approximately 2/3 of which is at positive longitudes. The small-scale height of these objects suggests that they are within the Galactic center region and are dynamically young. They lie between two layers of infrared dark clouds and may have originated from these clouds. We identify new sites for this recent star formation by comparing the mid-IR, radio, submillimeter, and methanol maser data. The methanol masers appear to be associated with young, embedded YSOs characterized by 4.5 mu m excesses. We use the SEDs of these sources to estimate their physical characteristics; their masses appear to range from similar to 10 to similar to 20 M-circle dot. Within the central 400 x 50 pc (vertical bar l vertical bar < 1 degrees.3 and vertical bar b vertical bar < 10') the star formation rate (SFR) based on the identification of Stage I evolutionary phase of YSO candidates is about 0.14 M-circle dot yr(-1). Given that the majority of the sources in the population of YSOs are classified as Stage I objects, we suggest that a recent burst of star formation took place within the last 10(5) yr. This suggestion is also consistent with estimates of SFRs within the last similar to 10(7) yr showing a peak around 10(5) yr ago. Lastly, we find that the Schmidt-Kennicutt Law applies well in the central 400 pc of the Galaxy. This implies that star formation does not appear to be dramatically affected by the extreme physical conditions in the Galactic center region. C1 [Yusef-Zadeh, F.; Hewitt, J. W.] Northwestern Univ, Dept Phys & Astron, Evanston, IL 60208 USA. [Arendt, R. G.] NASA, Goddard Space Flight Ctr, Sci Syst & Applicat Inc, Greenbelt, MD 20771 USA. [Arendt, R. G.] Univ Maryland, GSFC, Greenbelt, MD 20771 USA. [Whitney, B.] Space Sci Inst, Boulder, CO 80301 USA. [Rieke, G.; Hinz, J. L.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Wardle, M.] Macquarie Univ, Dept Phys & Engn, Sydney, NSW 2109, Australia. [Stolovy, S.; Ramirez, S.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Lang, C. C.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52245 USA. [Burton, M. G.] Univ New S Wales, Sch Phys, Sydney, NSW 2052, Australia. RP Yusef-Zadeh, F (reprint author), Northwestern Univ, Dept Phys & Astron, Evanston, IL 60208 USA. EM zadeh@northwestern.edu OI Burton, Michael/0000-0001-7289-1998; Wardle, Mark/0000-0002-1737-0871; Arendt, Richard/0000-0001-8403-8548 NR 122 TC 76 Z9 76 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 SEP 1 PY 2009 VL 702 IS 1 BP 178 EP 225 DI 10.1088/0004-637X/702/1/178 PG 48 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 487BD UT WOS:000269244500015 ER PT J AU Debes, JH Weinberger, AJ Kuchner, MJ AF Debes, John H. Weinberger, Alycia J. Kuchner, Marc J. TI INTERSTELLAR MEDIUM SCULPTING OF THE HD 32297 DEBRIS DISK SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; methods: N-body simulations; stars: individual (HD 3229, HD 15115, HD 61005) ID STAR AU-MICROSCOPII; CIRCUMSTELLAR DISK; SPACE-TELESCOPE; BETA-PICTORIS; SOLAR-SYSTEM; CORONAGRAPHIC OBSERVATIONS; DUSTY DEBRIS; MASS STARS; HD-32297; DISCOVERY AB We detect the HD 32297 debris disk in scattered light at 1.6 and 2.05 mu m. We use these new observations together with a previous scattered light image of the disk at 1.1 mu m to examine the structure and scattering efficiency of the disk as a function of wavelength. In addition to surface brightness asymmetries and a warped morphology beyond similar to 1 ''.5 for one lobe of the disk, we find that there exists an asymmetry in the spectral features of the grains between the northeastern and southwestern lobes. The mostly neutral color of the disk lobes implies roughly 1 mu m-sized grains are responsible for the scattering. We find that the asymmetries in color and morphology can plausibly be explained by HD 32297's motion into a dense interstellar medium cloud at a relative velocity of 15 km s(-1). We model the interaction of dust grains with H I gas in the cloud. We argue that supersonic ballistic drag can explain the morphology of the debris disks of HD 32297, HD 15115, and HD 61005. C1 [Debes, John H.; Kuchner, Marc J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Weinberger, Alycia J.] Carnegie Inst Washington, Dept Terr Magnetism, Washington, DC 20015 USA. RP Debes, JH (reprint author), NASA, Goddard Space Flight Ctr, Code 667, Greenbelt, MD 20771 USA. RI Kuchner, Marc/E-2288-2012; OI Weinberger, Alycia/0000-0001-6654-7859 FU NASA [10857]; NASA Astrobiology Institute FX The authors thank Dean Hines and Glenn Schneider for kindly providing an image of HD 61005 and useful discussions on both HD 61005 and HD 32297. We also thank Carey Lisse for pointing out that stellar winds can affect dust/gas interactions and Chris Stark for a careful reading of the manuscript. This research is based on observations with the NASA/ESA Hubble Space Telescope which is operated by the AURA, under NASA contract NAS 5-26555. These observations are associated with programs GO No. 10177, No. 10527, and No. 10857. Support for program No. 10857 was provided by NASA through a grant from STScI. This research was supported by an appointment of JD to the NASA Postdoctoral Program at the Goddard Space Flight Center, administered by Oak Ridge Associated Universities through a contract with NASA. A.J.W. and M.J.K. also acknowledge support from the NASA Astrobiology Institute. NR 41 TC 39 Z9 39 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 SEP 1 PY 2009 VL 702 IS 1 BP 318 EP 326 DI 10.1088/0004-637X/702/1/318 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 487BD UT WOS:000269244500024 ER PT J AU Rykoff, ES Aharonian, F Akerlof, CW Ashley, MCB Barthelmy, SD Flewelling, HA Gehrels, N Gogus, E Guver, T Kiziloglu, U Krimm, HA McKay, TA Ozel, M Phillips, A Quimby, RM Rowell, G Rujopakarn, W Schaefer, BE Smith, DA Vestrand, WT Wheeler, JC Wren, J Yuan, F Yost, SA AF Rykoff, E. S. Aharonian, F. Akerlof, C. W. Ashley, M. C. B. Barthelmy, S. D. Flewelling, H. A. Gehrels, N. Gogus, E. Guver, T. Kiziloglu, Ue. Krimm, H. A. McKay, T. A. Ozel, M. Phillips, A. Quimby, R. M. Rowell, G. Rujopakarn, W. Schaefer, B. E. Smith, D. A. Vestrand, W. T. Wheeler, J. C. Wren, J. Yuan, F. Yost, S. A. TI LOOKING INTO THE FIREBALL: ROTSE-III AND SWIFT OBSERVATIONS OF EARLY GAMMA-RAY BURST AFTERGLOWS SO ASTROPHYSICAL JOURNAL LA English DT Review DE gamma rays: bursts ID EARLY OPTICAL AFTERGLOW; HOST GALAXIES; LIGHT CURVES; THEORETICAL IMPLICATIONS; SPECTRAL EVOLUTION; GRB OBSERVATIONS; PROMPT EMISSION; DUST EXTINCTION; XRT DATA; FLARES AB We report on a complete set of early optical afterglows of gamma-ray bursts (GRBs) obtained with the Robotic Optical Transient Search Experiment (ROTSE-III) telescope network from 2005 March through 2007 June. This set is comprised of 12 afterglows with early optical and Swift/X-Ray Telescope observations, with a median ROTSE-III response time of 45 s after the start of gamma-ray emission (8 s after the GCN notice time). These afterglows span 4 orders of magnitude in optical luminosity, and the contemporaneous X-ray detections allow multi-wavelength spectral analysis. Excluding X-ray flares, the broadband synchrotron spectra show that the optical and X-ray emission originate in a common region, consistent with predictions of the external forward shock in the fireball model. However, the fireball model is inadequate to predict the temporal decay indices of the early afterglows, even after accounting for possible long-duration continuous energy injection. We find that the optical afterglow is a clean tracer of the forward shock, and we use the peak time of the forward shock to estimate the initial bulk Lorentz factor of the GRB outflow, and find 100 less than or similar to Gamma(0) less than or similar to 1000, consistent with expectations. C1 [Rykoff, E. S.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Aharonian, F.] Max Planck Inst Kernphys, D-69117 Heidelberg, Germany. [Akerlof, C. W.; Flewelling, H. A.; McKay, T. A.; Yuan, F.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA. [Ashley, M. C. B.; Phillips, A.] Univ New S Wales, Sch Phys, Dept Astrophys & Opt, Sydney, NSW 2052, Australia. [Barthelmy, S. D.; Gehrels, N.; Krimm, H. A.] NASA, Goddard Space Flight Ctr, High Energy Astrophys Lab, Greenbelt, MD 20771 USA. [Gogus, E.] Sabanci Univ, Fac Sci & Engn, TR-34956 Istanbul, Turkey. [Guver, T.] Univ Arizona, Dept Astron, Tucson, AZ 85721 USA. [Kiziloglu, Ue.] Middle E Tech Univ, TR-06531 Ankara, Turkey. [Krimm, H. A.] Univ Space Res Assoc, Columbia, MD 21044 USA. [Ozel, M.] Cag Univ, Fac Arts & Sci, Yenise Tarsus Mersin, Turkey. [Quimby, R. M.] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA. [Rowell, G.] Univ Adelaide, Sch Chem & Phys, Adelaide, SA 5005, Australia. [Rujopakarn, W.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Schaefer, B. E.] Louisiana State Univ, Dept Phys & Astron, Baton Rouge, LA 70803 USA. [Smith, D. A.] Guilford Coll, Greensboro, NC 27410 USA. [Vestrand, W. T.; Wren, J.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA. [Wheeler, J. C.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Yost, S. A.] St Johns Univ, Coll St Benedict, Dept Phys, Collegeville, MN 56321 USA. RP Rykoff, ES (reprint author), Univ Calif Santa Barbara, Dept Phys, 2233B Broida Hall, Santa Barbara, CA 93106 USA. EM erykoff@physics.ucsb.edu RI Guver, Tolga/C-1408-2011; Barthelmy, Scott/D-2943-2012; Gehrels, Neil/D-2971-2012; Rujopakarn, Wiphu/E-7849-2012; McKay, Timothy/C-1501-2009; Guver, Tolga/B-1039-2014; OI McKay, Timothy/0000-0001-9036-6150; Guver, Tolga/0000-0002-3531-9842; Rujopakarn, Wiphu/0000-0002-0303-499X; Flewelling, Heather/0000-0002-1050-4056; Rowell, Gavin/0000-0002-9516-1581 FU NASA [NNG-04WC41G, NNG-06GI90G, NNX-07AF02G]; NSF [AST-0407061, PHY-0801007, AST-0335588, AST-0707769]; Australian Research Council's Discovery Projects; University of New South Wales; University of Texas; University of Michigan; Michigan Space Grant Consortium FX E. S. R. thanks the TABASGO foundation. This work has been supported by NASA grant NNG-04WC41G, NSF grants AST-0407061 and PHY-0801007, the Australian Research Council's Discovery Projects funding scheme, the University of New South Wales, the University of Texas, and the University of Michigan. H. A. F. has been supported by NSF grant AST-0335588 and by the Michigan Space Grant Consortium. F. Y. has been supported under NASA Swift Guest Investigator grants NNG-06GI90G and NNX-07AF02G. J.C.W. is supported in part by NSF grant AST-0707769. Special thanks to David Doss at McDonald Observatory, Toni Hanke at the H. E. S. S. site, and Tuncay Ozisik at TUG. NR 115 TC 65 Z9 66 U1 0 U2 11 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD SEP 1 PY 2009 VL 702 IS 1 BP 489 EP 505 DI 10.1088/0004-637X/702/1/489 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 487BD UT WOS:000269244500040 ER PT J AU Dib, R Kaspi, VM Gavriil, FP AF Dib, Rim Kaspi, Victoria M. Gavriil, Fotis P. TI ROSSI X-RAY TIMING EXPLORER MONITORING OF THE ANOMALOUS X-RAY PULSAR 1E 1048.1-5937: LONG-TERM VARIABILITY AND THE 2007 MARCH EVENT SO ASTROPHYSICAL JOURNAL LA English DT Article DE pulsars: individual (1E 1048.1-5937); stars: neutron; X-rays: stars ID SOFT GAMMA-REPEATERS; MAGNETIZED NEUTRON-STARS; 1RXS J170849.0-400910; INFRARED COUNTERPART; TRANSIENT MAGNETAR; XTE J1810-197; 1E-1048.1-5937; EMISSION; GLITCHES; BURSTS AB After three years of no unusual activity, Anomalous X-ray Pulsar 1E 1048.1-5937 reactivated in 2007 March. We report on the detection of a large glitch (Delta nu/nu = 1.63(2) x 10(-5)) on 2007 March 26 (MJD 54185.9), contemporaneous with the onset of a pulsed-flux flare, the third flare observed from this source in 10 years of monitoring with the Rossi X-ray Timing Explorer (RXTE). Additionally, we report on a detailed study of the evolution of the timing properties, the pulsed flux, and the pulse profile of this source as measured by RXTE from 1996 July to 2008 January. In our timing study, we attempted phase-coherent timing of all available observations. We show that in 2001 a timing anomaly of uncertain nature occurred near the rise of the first pulsed flux flare; we show that a likely glitch (Delta nu/nu = 2.91(9) x 10(-6)) occurred in 2002, near the rise of the second flare, and we present a detailed description of the variations in the spin down. In our pulsed flux study, we compare the decays of the three flares and discuss changes in the hardness ratio. In our pulse profile study, we show that the profile exhibited large variations near the peak of the first two flares, and several small short-term profile variations during the most recent flare. Finally, we report on the discovery of a small burst 27 days after the peak of the last flare, the fourth burst discovered from this source. We discuss the relationships between the observed properties in the framework of the magnetar model. C1 [Dib, Rim; Kaspi, Victoria M.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Gavriil, Fotis P.] NASA, Goddard Space Flight Ctr, Ctr Res & Explorat Space Sci & Technol, Greenbelt, MD 20771 USA. [Gavriil, Fotis P.] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA. RP Dib, R (reprint author), McGill Univ, Dept Phys, 3600 Univ St, Montreal, PQ H3A 2T8, Canada. FU NSERC Discovery Grant [Rgpin 228738-08]; FQRNT Centre; CIFAR; Canada Research Chairs Program; Lorne Trottier Chair in Astrophysics and Cosmology FX We thank A. Cumming and D. Eichler for useful discussions. Support was provided to V. M. K. by NSERC Discovery Grant Rgpin 228738-08, an FQRNT Centre Grant, CIFAR, the Canada Research Chairs Program, and the Lorne Trottier Chair in Astrophysics and Cosmology. NR 46 TC 48 Z9 48 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 SEP 1 PY 2009 VL 702 IS 1 BP 614 EP 630 DI 10.1088/0004-637X/702/1/614 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 487BD UT WOS:000269244500049 ER PT J AU Von Braun, K Kane, SR Ciardi, DR AF Von Braun, Kaspar Kane, Stephen R. Ciardi, David R. TI OBSERVATIONAL WINDOW FUNCTIONS IN PLANET TRANSIT SURVEYS SO ASTROPHYSICAL JOURNAL LA English DT Article DE eclipses; methods: statistical; planetary systems; surveys; techniques: photometric; time ID TREND FILTERING ALGORITHM; ASTRONOMICAL TIME-SERIES; EXTRASOLAR PLANETS; HIPPARCOS PHOTOMETRY; ORBITAL ECCENTRICITY; PERIOD DISTRIBUTION; LIGHT CURVES; SEARCH; VARIABILITY; PROJECT AB The probability that an existing planetary transit is detectable in one's data is sensitively dependent upon the window function of the observations. We quantitatively characterize and provide visualizations of the dependence of this probability as a function of orbital period upon several observing strategy and astrophysical parameters, such as length of observing run, observing cadence, length of night, transit duration and depth, and the minimum number of sampled transits. The ability to detect a transit is directly related to the intrinsic noise of the observations. In our simulations of observational window functions, we explicitly address noncorrelated (Gaussian or white) noise and correlated (red) noise and discuss how these two noise components affect transit detectability in fundamentally different manners, especially for long periods and/or small transit depths. We furthermore discuss the consequence of competing effects on transit detectability, elaborate on measures of observing strategies, and examine the projected efficiency of different transit survey scenarios with respect to certain regions of parameter space. C1 [Von Braun, Kaspar; Kane, Stephen R.; Ciardi, David R.] CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA. RP Von Braun, K (reprint author), CALTECH, NASA, Exoplanet Sci Inst, MC 100-22, Pasadena, CA 91125 USA. EM kaspar@ipac.caltech.edu; skane@ipac.caltech.edu; ciardi@ipac.caltech.edu RI Kane, Stephen/B-4798-2013; OI Ciardi, David/0000-0002-5741-3047 NR 45 TC 19 Z9 19 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 SEP 1 PY 2009 VL 702 IS 1 BP 779 EP 790 DI 10.1088/0004-637X/702/1/779 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 487BD UT WOS:000269244500064 ER PT J AU Meegan, C Lichti, G Bhat, PN Bissaldi, E Briggs, MS Connaughton, V Diehl, R Fishman, G Greiner, J Hoover, AS van der Horst, AJ Von Kienlin, A Kippen, RM Kouveliotou, C McBreen, S Paciesas, WS Preece, R Steinle, H Wallace, MS Wilson, RB Wilson-Hodge, C AF Meegan, Charles Lichti, Giselher Bhat, P. N. Bissaldi, Elisabetta Briggs, Michael S. Connaughton, Valerie Diehl, Roland Fishman, Gerald Greiner, Jochen Hoover, Andrew S. van der Horst, Alexander J. Von Kienlin, Andreas Kippen, R. Marc Kouveliotou, Chryssa McBreen, Sheila Paciesas, W. S. Preece, Robert Steinle, Helmut Wallace, Mark S. Wilson, Robert B. Wilson-Hodge, Colleen TI THE FERMI GAMMA-RAY BURST MONITOR SO ASTROPHYSICAL JOURNAL LA English DT Article DE gamma rays: bursts; instrumentation: detectors ID HIGH-ENERGY; HIGH-REDSHIFT; BATSE; DETECTORS AB The Gamma-Ray Burst Monitor (GBM) will significantly augment the science return from the Fermi Observatory in the study of gamma-ray bursts (GRBs). The primary objective of GBM is to extend the energy range over which bursts are observed downward from the energy range of the Large Area Telescope (LAT) on Fermi into the hard X-ray range where extensive previous data sets exist. A secondary objective is to compute burst locations onboard to allow re-orienting the spacecraft so that the LAT can observe delayed emission from bright bursts. GBM uses an array of 12 sodium iodide scintillators and two bismuth germanate scintillators to detect gamma rays from similar to 8 keV to similar to 40 MeV over the full unocculted sky. The onboard trigger threshold is similar to 0.7 photons cm(-2) s(-1) (50-300 keV, 1 s peak). GBM generates onboard triggers for similar to 250 GRBs per year. C1 [Meegan, Charles] Univ Space Res Assoc, NSSTC, Huntsville, AL 35805 USA. [Lichti, Giselher; Bissaldi, Elisabetta; Diehl, Roland; Greiner, Jochen; Von Kienlin, Andreas; Steinle, Helmut] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Bhat, P. N.; Briggs, Michael S.; Connaughton, Valerie; Paciesas, W. S.; Preece, Robert; Wilson, Robert B.] Univ Alabama, NSSTC, Huntsville, AL 35805 USA. [Fishman, Gerald; Kouveliotou, Chryssa; Wilson-Hodge, Colleen] NASA, Space Sci Off, George C Marshall Space Flight Ctr, VP62, Huntsville, AL 35812 USA. [Hoover, Andrew S.; Kippen, R. Marc; Wallace, Mark S.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA. [McBreen, Sheila] Natl Univ Ireland Univ Coll Dublin, Dublin 4, Ireland. RP Meegan, C (reprint author), Univ Space Res Assoc, NSSTC, 320 Sparkman Dr, Huntsville, AL 35805 USA. RI Bissaldi, Elisabetta/K-7911-2016; OI Bissaldi, Elisabetta/0000-0001-9935-8106; Preece, Robert/0000-0003-1626-7335; McBreen, Sheila/0000-0002-1477-618X NR 31 TC 369 Z9 371 U1 0 U2 11 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 SEP 1 PY 2009 VL 702 IS 1 BP 791 EP 804 DI 10.1088/0004-637X/702/1/791 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 487BD UT WOS:000269244500065 ER PT J AU Comerford, JM Griffith, RL Gerke, BF Cooper, MC Newman, JA Davis, M Stern, D AF Comerford, Julia M. Griffith, Roger L. Gerke, Brian F. Cooper, Michael C. Newman, Jeffrey A. Davis, Marc Stern, Daniel TI 1.75 h(-1) kpc SEPARATION DUAL ACTIVE GALACTIC NUCLEI AT z=0.36 IN THE COSMOS FIELD SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE galaxies: active; galaxies: individual (COSMOS J100043.15+020637.2); galaxies: interactions; galaxies: nuclei ID SUPERMASSIVE BLACK-HOLES; DIGITAL SKY SURVEY; SPACE-TELESCOPE; HOST GALAXIES; REDSHIFT SURVEY; DISCOVERY; EMISSION; SYSTEM; CLASSIFICATION; SELECTION AB We present strong evidence for dual active galactic nuclei (AGNs) in the z = 0.36 galaxy COSMOS J100043.15+020637.2. COSMOS Hubble Space Telescope (HST) imaging of the galaxy shows a tidal tail, indicating that the galaxy recently underwent a merger, as well as two bright point sources near the galaxy's center. The luminosities of these sources (derived from the HST image) and their emission line flux ratios (derived from Keck/DEIMOS slit spectroscopy) suggest that both are AGNs and not star-forming regions or supernovae. Observations from zCOSMOS, the Sloan Digital Sky Survey, XMM-Newton, Spitzer, and the Very Large Array fortify the evidence for AGN activity. With HST imaging we measure a projected spatial offset between the two AGNs of 1.75 +/- 0.03 h(-1) kpc, and with DEIMOS we measure a 150 +/- 40 km s(-1) line-of-sight velocity offset between the two AGNs. Combined, these observations provide substantial evidence that COSMOS J100043.15+020637.2 is a merger-remnant galaxy with dual AGNs. C1 [Comerford, Julia M.; Davis, Marc] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Griffith, Roger L.; Stern, Daniel] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Gerke, Brian F.] Stanford Linear Accelerator Ctr, Kavli Inst Particle Astrophys & Cosmol, Menlo Pk, CA 94724 USA. [Cooper, Michael C.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Newman, Jeffrey A.] Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA. [Davis, Marc] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. RP Comerford, JM (reprint author), Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA. NR 45 TC 69 Z9 69 U1 0 U2 2 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 SEP 1 PY 2009 VL 702 IS 1 BP L82 EP L86 DI 10.1088/0004-637X/702/1/L82 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 484NR UT WOS:000269053200018 ER PT J AU Groeneboom, NE Eriksen, HK Gorski, K Huey, G Jewell, J Wandelt, B AF Groeneboom, N. E. Eriksen, H. K. Gorski, K. Huey, G. Jewell, J. Wandelt, B. TI BAYESIAN ANALYSIS OF WHITE NOISE LEVELS IN THE FIVE-YEAR WMAP DATA SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE cosmic microwave background; cosmology: observations; methods: numerical ID INFLATIONARY UNIVERSE SCENARIO; POWER SPECTRUM ESTIMATION; SKY MAPS; ANISOTROPY; EMISSION; FLATNESS; HORIZON; ARRAY AB We develop a new Bayesian method for estimating white noise levels in CMB sky maps, and apply this algorithm to the five-year Wilkinson Microwave Anisotropy Probe (WMAP) data. We assume that the amplitude of the noise rms is scaled by a constant value, a, relative to a pre-specified noise level. We then derive the corresponding conditional density, P(alpha vertical bar s, C(l), d), which is subsequently integrated into a general CMB Gibbs sampler. We first verify our code by analyzing simulated data sets, and then apply the framework to the WMAP data. For the foreground-reduced five-year WMAP sky maps and the nominal noise levels initially provided in the five-year data release, we find that the posterior means typically range between alpha = 1.005 +/- 0.001 and alpha = 1.010 +/- 0.001 depending on differencing assembly, indicating that the noise level of these maps are biased low by 0.5%-1.0%. The same problem is not observed for the uncorrected WMAP sky maps. After the preprint version of this letter appeared on astro-ph., the WMAP team has corrected the values presented on their web page, noting that the initially provided values were in fact estimates from the three-year data release, not from the five-year estimates. However, internally in their five-year analysis the correct noise values were used, and no cosmological results are therefore compromised by this error. Thus, our method has already been demonstrated in practice to be both useful and accurate. C1 [Groeneboom, N. E.; Eriksen, H. K.] Univ Oslo, Inst Theoret Astrophys, N-0315 Oslo, Norway. [Gorski, K.; Huey, G.; Jewell, J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Wandelt, B.] Univ Illinois, Dept Phys & Astron, Urbana, IL 61801 USA. RP Groeneboom, NE (reprint author), Univ Oslo, Inst Theoret Astrophys, POB 1029 Blindern, N-0315 Oslo, Norway. EM nicolaag@astro.uio.no OI WANDELT, Benjamin/0000-0002-5854-8269 FU Research Council of Norway; NASA FX The authors thank Joanna Dunkley for useful comments and for pointing out the issue of incorrect noise levels on LAMBDA. N. E. G. and H. K. E. acknowledge financial support from the Research Council of Norway. The computations presented in this Letter were carried out on Titan, a cluster owned and maintained by the University of Oslo and NOTUR. We acknowledge the use of the HEALPix (see footnote 5) software (Gorski et al. 2005) and analysis package for deriving the results in this Letter. 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 30 TC 7 Z9 7 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 SEP 1 PY 2009 VL 702 IS 1 BP L87 EP L90 DI 10.1088/0004-637X/702/1/L87 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 484NR UT WOS:000269053200019 ER PT J AU Mawet, D Serabyn, E Stapelfeldt, K Crepp, J AF Mawet, D. Serabyn, E. Stapelfeldt, K. Crepp, J. TI IMAGING THE DEBRIS DISK OF HD 32297 WITH A PHASE-MASK CORONAGRAPH AT HIGH STREHL RATIO SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE circumstellar matter; infrared: stars; instrumentation: adaptive optics; planetary systems: protoplanetary disks; stars: individual (HD 32297) ID OPTICAL-IMAGES; HD-32297; DUST; APERTURE; STARS AB We present the first K(s)-band image of the scattered light from HD 32297's debris disk. HD 32297 is an A5 star known to possess a nearly edge-on disk with a high fractional luminosity L(d)/L(star) approximate to 0.003 in the infrared. Our image was obtained using phase-mask coronagraphy on the 1.6 m well-corrected subaperture on the 5 m Palomar Hale telescope, and reaches an inner working angle of 400 mas. We confirm the previously reported disk asymmetry and central hole. The gray J-K(s) disk color appears similar on the two sides of the disk, which would demand a minimum grain size of at least a few microns, larger than thermal arguments suggest. One possible explanation is a planetesimal clump in a resonant orbit with an outward migrating giant planet, located at larger radii than the warm dust emitting at longer wavelengths. Our observations also clearly demonstrate the benefits of operating in the extreme adaptive optics regime with a coronagraph able to reach a very small inner working angle. C1 [Mawet, D.; Serabyn, E.; Stapelfeldt, K.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Crepp, J.] CALTECH, Dept Astron, Opt Observ, Pasadena, CA 91125 USA. RP Mawet, D (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Dimitri.Mawet@jpl.nasa.gov RI Stapelfeldt, Karl/D-2721-2012 NR 20 TC 21 Z9 21 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 SEP 1 PY 2009 VL 702 IS 1 BP L47 EP L50 DI 10.1088/0004-637X/702/1/L47 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 484NR UT WOS:000269053200011 ER PT J AU Savcheva, A Cirtain, JW DeLuca, EE Golub, L AF Savcheva, A. Cirtain, J. W. DeLuca, E. E. Golub, L. TI DOES A POLAR CORONAL HOLE'S FLUX EMERGENCE FOLLOW A HALE-LIKE LAW? SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE Sun: corona; Sun: magnetic fields; Sun: X-rays, gamma rays ID X-RAY TELESCOPE; HINODE MISSION; JETS; REGIONS; XRT AB Recent increases in spatial and temporal resolution for solar telescopes sensitive to EUV and X-ray radiation have revealed the prevalence of transient jet events in polar coronal holes. Using data collected by the X-Ray Telescope on Hinode, Savcheva et al. confirmed the observation, made first by the Soft X-ray Telescope on Yohkoh, that some jets exhibit a motion transverse to the jet outflow direction. The velocity of this transverse motion is, on average, 10 km s(-1). The direction of the transverse motion, in combination with the standard reconnection model for jet production (e. g., Shibata et al.), reflects the magnetic polarity orientation of the ephemeral active region at the base of the jet. From this signature, we find that during the present minimum phase of the solar cycle the jet-base ephemeral active regions in the polar coronal holes had a preferred east-west direction, and that this direction reversed during the cycle's progression through minimum. In late 2006 and early 2007, the preferred direction was that of the active regions of the coming sunspot cycle (cycle 24), but in late 2008 and early 2009 the preferred direction has been that of the active regions of sunspot cycle 25. These findings are consistent with the observations of Wilson et al. suggesting that each cycle of solar activity begins at polar latitudes soon after the onset of the previous cycle. C1 [Savcheva, A.; DeLuca, E. E.; Golub, L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Cirtain, J. W.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. RP Savcheva, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,Mail Stop 58, Cambridge, MA 02138 USA. EM asavcheva@cfa.harvard.edu RI DeLuca, Edward/L-7534-2013 OI DeLuca, Edward/0000-0001-7416-2895 FU NASA [NNM07AB07C] FX Hinode is a Japanese mission developed, launched, and operated by ISAS/JAXA in partnership with NAOJ, NASA, and STFC ( UK). Additional operational support is provided by ESA, NSC (Norway). This work was supported by NASA contract NNM07AB07C to SAO. We thank Dibyendu Nandi, Piet Martens, Andres Munoz-Jeramillo, Ron Moore, and Julie Stern for helpful discussions. We thank the referee for very useful comments and suggestions that greatly helped to make this Letter better. NR 18 TC 16 Z9 16 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD SEP 1 PY 2009 VL 702 IS 1 BP L32 EP L36 DI 10.1088/0004-637X/702/1/L32 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 484NR UT WOS:000269053200008 ER PT J AU Veneziani, M Amblard, A Cooray, A Piacentini, F Pietrobon, D Serra, P Ade, PAR Bock, JJ Bond, JR Borrill, J Boscaleri, A Cabella, P Contaldi, CR Crill, BP de Bernardis, P De Gasperis, G de Oliveira-Costa, A De Troia, G Di Stefano, G Ganga, KM Hivon, E Jones, WC Kisner, TS Lange, AE MacTavish, CJ Masi, S Mauskopf, PD Melchiorri, A Montroy, TE Natoli, P Netterfield, CB Pascale, E Polenta, G Ricciardi, S Romeo, G Ruhl, JE Santini, P Tegmark, M Vittorio, N AF Veneziani, M. Amblard, A. Cooray, A. Piacentini, F. Pietrobon, D. Serra, P. Ade, P. A. R. Bock, J. J. Bond, J. R. Borrill, J. Boscaleri, A. Cabella, P. Contaldi, C. R. Crill, B. P. de Bernardis, P. De Gasperis, G. de Oliveira-Costa, A. De Troia, G. Di Stefano, G. Ganga, K. M. Hivon, E. Jones, W. C. Kisner, T. S. Lange, A. E. MacTavish, C. J. Masi, S. Mauskopf, P. D. Melchiorri, A. Montroy, T. E. Natoli, P. Netterfield, C. B. Pascale, E. Polenta, G. Ricciardi, S. Romeo, G. Ruhl, J. E. Santini, P. Tegmark, M. Vittorio, N. TI SUBDEGREE SUNYAEV-ZEL'DOVICH SIGNAL FROM MULTIFREQUENCY BOOMERANG OBSERVATIONS SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE cosmic microwave background; cosmological parameters; cosmology: observations; large-scale structure of universe ID MICROWAVE BACKGROUND-RADIATION; POWER SPECTRUM; ANISOTROPY POWER; 2003 FLIGHT; MAPS; CLUSTERS; FLUCTUATIONS; TEMPERATURE; PLANCK AB The Sunyaev-Zel'dovich (SZ) effect is the inverse Compton-scattering of cosmic microwave background (CMB) photons by hot electrons in the intervening gas throughout the universe. The effect has a distinct spectral signature that allows its separation from other signals in multifrequency CMB data sets. Using CMB anisotropies measured at three frequencies by the BOOMERanG 2003 flight we constrain SZ fluctuations in the 10 arcmin to 1 deg angular range. Propagating errors and potential systematic effects through simulations, we obtain an overall upper limit of 15.3 mu K (2 sigma) for rms SZ fluctuations in a broad bin between multipoles of 250 and 1200 at the Rayleigh-Jeans (RJ) end of the spectrum. The resulting upper limit on the local universe normalization of the density perturbations with BOOMERanG SZ data alone is sigma(SZ)(8) < 1.14 at the 95% confidence level. When combined with other CMB anisotropy and SZ measurements, we find sigma(SZ)(8) < 0.92 (95% c. l.). C1 [Veneziani, M.; Amblard, A.; Cooray, A.; Serra, P.] Univ Calif Irvine, Ctr Cosmol, Irvine, CA 92697 USA. [Veneziani, M.; Piacentini, F.; de Bernardis, P.; Masi, S.; Melchiorri, A.; Polenta, G.; Ricciardi, S.; Santini, P.] Univ Roma La Sapienza, Dipartimento Fis, I-00185 Rome, Italy. [Veneziani, M.; Ganga, K. M.] Univ Paris Diderot, APC, F-75013 Paris, France. [Pietrobon, D.; Cabella, P.; De Gasperis, G.; De Troia, G.; Natoli, P.; Vittorio, N.] Univ Roma Tor Vergata, Dipartimento Fis, I-00173 Rome, Italy. [Pietrobon, D.] Univ Portsmouth, Inst Cosmol & Gravitat, Portsmouth PO1 2UP, Hants, England. [Ade, P. A. R.; Mauskopf, P. D.] Cardiff Univ, Dept Phys & Astron, Cardiff, S Glam, Wales. [Bock, J. J.; Crill, B. P.; Lange, A. E.] Jet Prop Lab, Pasadena, CA 91109 USA. [Bock, J. J.; Crill, B. P.] CALTECH, Pasadena, CA 91125 USA. [Bond, J. R.] Univ Toronto, CITA, Toronto, ON M5S 3H8, Canada. [Borrill, J.] LBNL, Computat Res Div, Berkeley, CA 94720 USA. [Boscaleri, A.] IFAC CNR, I-50127 Florence, Italy. [Contaldi, C. R.] Univ London Imperial Coll Sci Technol & Med, Theoret Phys Grp, London, England. [de Oliveira-Costa, A.; Tegmark, M.] MIT, Dept Phys, Cambridge, MA 02139 USA. [De Troia, G.; Romeo, G.] Ist Nazl Geofis & Vulcanol, I-00143 Rome, Italy. [Hivon, E.] Inst Astrophys, F-75014 Paris, France. [Jones, W. C.] Princeton Univ, Dept Phys, Princeton, NJ 08544 USA. [Kisner, T. S.; Montroy, T. E.; Ruhl, J. E.] Case Western Reserve Univ, Cleveland, OH 44106 USA. [MacTavish, C. J.] Univ London Imperial Coll Sci Technol & Med, Astrophys Grp, London, England. [Netterfield, C. B.; Pascale, E.] Univ Toronto, Dept Phys, Toronto, ON, Canada. [Polenta, G.] ESRIN, ASI Sci Data Ctr, I-00044 Frascati, Italy. [Polenta, G.] INAF, Osservatorio Astron Roma, Monte Porzio Catone, Italy. [Ricciardi, S.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. RP Veneziani, M (reprint author), Univ Calif Irvine, Ctr Cosmol, Irvine, CA 92697 USA. EM marcella.veneziani@roma1.infn.it; amblard@uci.edu RI de Gasperis, Giancarlo/C-8534-2012; Serra, Paolo/G-9678-2014; amblard, alexandre/L-7694-2014; Piacentini, Francesco/E-7234-2010; OI Melchiorri, Alessandro/0000-0001-5326-6003; Hivon, Eric/0000-0003-1880-2733; de Gasperis, Giancarlo/0000-0003-2899-2171; Santini, Paola/0000-0002-9334-8705; Serra, Paolo/0000-0002-7609-3931; Ricciardi, Sara/0000-0002-3807-4043; amblard, alexandre/0000-0002-2212-5395; Piacentini, Francesco/0000-0002-5444-9327; Masi, Silvia/0000-0001-5105-1439; de Bernardis, Paolo/0000-0001-6547-6446; ROMEO, Giovanni/0000-0002-5535-7803; Polenta, Gianluca/0000-0003-4067-9196 FU NSF [AST-0645427]; Italian Space Agency [I/087/06/0, I/016/07/0]; Programma Nazionale Ricerche in Antartide FX We gratefully acknowledge support from NSF CAREER AST-0645427 at UCI. We also acknowledge support from the Italian Space Agency (contracts I/087/06/0 and I/016/07/0), and from Programma Nazionale Ricerche in Antartide. The authors acknowledge the use of the Planck Sky Model, developed by theComponent SeparationWorking Group (WG2) of the Planck Collaboration. NR 34 TC 8 Z9 8 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD SEP 1 PY 2009 VL 702 IS 1 BP L61 EP L65 DI 10.1088/0004-637X/702/1/L61 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 484NR UT WOS:000269053200014 ER PT J AU Brauer, CS Pearson, JC Drouin, BJ Yu, SS AF Brauer, Carolyn S. Pearson, John C. Drouin, Brian J. Yu, Shanshan TI NEW GROUND-STATE MEASUREMENTS OF ETHYL CYANIDE SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE catalogs; line: identification; methods: laboratory; molecular data; techniques: spectroscopic ID HOT MOLECULAR CORES; PROPIONITRILE C2H5CN; VIBRATIONAL-SPECTRA; ROTATION; SUBMILLIMETER; CHEMISTRY; ORION AB The spectrum of ethyl cyanide, or propionitrile (CH(3)CH(2)CN), has been repeatedly observed in the interstellar medium with large column densities and surprisingly high temperatures in hot core sources. The construction of new, more sensitive, observatories accessing higher frequencies such as Herschel, ALMA, and SOFIA have made it important to extend the laboratory data for ethyl cyanide to coincide with the capabilities of the new instruments. We report extensions of the laboratory measurements of the rotational spectrum of ethyl cyanide in its ground vibrational state to 1.6 THz. A global analysis of the ground state, which includes all of the previous data and 3356 newly assigned transitions, has been fitted to within experimental error to J = 132, K = 36, using both Watson A-reduced and Watson S-reduced Hamiltonians. C1 [Brauer, Carolyn S.; Pearson, John C.; Drouin, Brian J.; Yu, Shanshan] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Brauer, CS (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Carolyn.S.Brauer@jpl.nasa.gov RI Yu, Shanshan/D-8733-2016 FU NASA Herschel Science Center Laboratory Astrophysics Program FX Portions of research described in this paper were carried out at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. Support for this work, part of the NASA Herschel Science Center Laboratory Astrophysics Program, was provided by NASA. NR 23 TC 12 Z9 12 U1 1 U2 9 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 SEP PY 2009 VL 184 IS 1 BP 133 EP 137 DI 10.1088/0067-0049/184/1/133 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 492AF UT WOS:000269625100005 ER PT J AU Brown, TM Smith, E Ferguson, HC Guhathakurta, P Kalirai, JS Kimble, RA Renzini, A Rich, RM Sweigart, AV VandenBerg, DA AF Brown, Thomas M. Smith, Ed Ferguson, Henry C. Guhathakurta, Puragra Kalirai, Jason S. Kimble, Randy A. Renzini, Alvio Rich, R. Michael Sweigart, Allen V. VandenBerg, Don A. TI DEEP OPTICAL PHOTOMETRY OF SIX FIELDS IN THE ANDROMEDA GALAXY SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE galaxies: evolution; galaxies: individual (M31); galaxies: stellar content ID STAR-FORMATION HISTORY; MAIN-SEQUENCE PHOTOMETRY; MINOR AXIS; OUTER DISK; M31; HALO; STREAM; KPC AB Using the Advanced Camera for Surveys on the Hubble Space Telescope, we have obtained deep optical images reaching well below the oldest main-sequence turnoff in six fields of the Andromeda Galaxy. The fields fall at four positions on the southeast minor axis, one position in the giant stellar stream, and one position on the northeast major axis. These data were obtained as part of three large observing programs designed to probe the star formation history of the stellar population in various structures of the galaxy. In this paper, we present the images, catalogs, and artificial star tests for these observing programs as a supplement to the analyses published previously. These high-level science products are also archived at the Multimission Archive at the Space Telescope Science Institute. C1 [Brown, Thomas M.; Smith, Ed; Ferguson, Henry C.; Kalirai, Jason S.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Guhathakurta, Puragra] Univ Calif Santa Cruz, Univ Calif Observ, Lick Observ, Santa Cruz, CA 95064 USA. [Kimble, Randy A.; Sweigart, Allen V.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Renzini, Alvio] Osserv Astron Padova, I-35122 Padua, Italy. [Rich, R. Michael] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [VandenBerg, Don A.] Univ Victoria, Dept Phys & Astron, Victoria, BC V8W 3P6, Canada. RP Brown, TM (reprint author), Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA. EM tbrown@stsci.edu; edsmith@stsci.edu; ferguson@stsci.edu; raja@ucolick.org; jkalirai@stsci.edu; randy.a.kimble@nasa.gov; alvio.renzini@oapd.inaf.it; rmr@astro.ucla.edu; allen.v.sweigart@nasa.gov; vandenbe@uvic.ca RI Kimble, Randy/D-5317-2012 FU NASA [GO-9453, GO-10265, GO-10816, NAS5-26555]; Space Telescope Science Institute; NSF [AST-0307966, AST-0507483, AST-0607852]; HST programs; [NSF-AST-0307931] FX Support for Programs GO-9453, GO-10265, and GO-10816 was provided by NASA through a grant from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555. P. Royle and S. Meyett were enormously helpful in the scheduling and execution of these Large HST programs. P. G. and J. S. K. acknowledge support from NASA grants associated with these HST programs and from the following NSF grants to UCSC: AST-0307966, AST-0507483, and AST-0607852. R. M. R. acknowledges support from grants associated with these HST programs and also NSF-AST-0307931. We are grateful to P. Stetson for his DAOPHOT code. NR 13 TC 14 Z9 14 U1 0 U2 1 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 SEP PY 2009 VL 184 IS 1 BP 152 EP 157 DI 10.1088/0067-0049/184/1/152 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 492AF UT WOS:000269625100007 ER PT J AU Li, H Faruque, F Williams, W Al-Hamdan, M Luvall, J Crosson, W Rickman, D Limaye, A AF Li, Hui Faruque, Fazlay Williams, Worth Al-Hamdan, Mohammad Luvall, Jeffrey Crosson, William Rickman, Douglas Limaye, Ashutosh TI Optimal temporal scale for the correlation of AOD and ground measurements of PM2.5 in a real-time air quality estimation system SO ATMOSPHERIC ENVIRONMENT LA English DT Article DE Aerosol optical depth (AOD); PM2.5; Air quality; Temporal scale; Remote sensing; Real-time system ID AEROSOL OPTICAL DEPTH; PARTICULATE MATTER; SATELLITE DATA; MODIS; POLLUTION; PRODUCTS; EVENTS AB Aerosol optical depth (AOD), an indirect estimate of particulate matter using satellite observations, has shown great promise in improving estimates of PM2.5 (particulate matter with aerodynamic diameter less than or equal to 2.5 mu m) surface. Currently, few studies have been conducted to explore the optimal way to apply AOD data to improve the model accuracy of PM2.5 in a real-time air quality system. We believe that two major aspects may be worthy of consideration in that area: 1) an approach that integrates satellite measurements with ground measurements in the estimates of pollutants and 2) identification of an optimal temporal scale to calculate the correlation of ACD and ground measurements. This paper is focused on the second aspect, identifying the optimal temporal scale to correlate AOD with PM2.5. Five following different temporal scales were chosen to evaluate their impact on the model performance: 1) within the last 3 days, 2) within the last 10 days, 3) within the last 30 days, 4) within the last 90 days, and 5) the time period with the highest correlation in a year. The model performance is evaluated for its accuracy, bias, and errors based on the following selected statistics: the Mean Bias, the Normalized Mean Bias, the Root Mean Square Error, Normalized Mean Error, and the index of Agreement. This research shows that the model with the temporal scale: within the last 30 days, displays the best model performance in a southern multi-state area centered in Mississippi using 2004 and 2005 data sets. (C) 2009 Elsevier Ltd. All rights reserved. C1 [Li, Hui; Faruque, Fazlay; Williams, Worth] Univ Mississippi, Med Ctr, Jackson, MS 39216 USA. [Al-Hamdan, Mohammad; Crosson, William; Limaye, Ashutosh] NASA, George C Marshall Space Flight Ctr, Univ Space Res Assoc, Huntsville, AL 35805 USA. [Luvall, Jeffrey; Rickman, Douglas] NASA, George C Marshall Space Flight Ctr, Earth Sci Off, Huntsville, AL 35805 USA. RP Li, H (reprint author), Univ Mississippi, Med Ctr, 2500 N State St, Jackson, MS 39216 USA. EM hli@dor.umsmed.edu OI Rickman, Doug/0000-0003-3409-2882 FU NASA's Stennis Space Center (SSC) through Mississippi Research Consortium (MRC) [USM-MRCSSC-12162005-68D/NNS06AA68D] FX This work was partially funded by the NASA's Stennis Space Center (SSC) through Mississippi Research Consortium (MRC) (grant#: USM-MRCSSC-12162005-68D/NNS06AA68D). NR 20 TC 5 Z9 5 U1 0 U2 14 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1352-2310 J9 ATMOS ENVIRON JI Atmos. Environ. PD SEP PY 2009 VL 43 IS 28 BP 4303 EP 4310 DI 10.1016/j.atmosenv.2009.06.004 PG 8 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA 485BM UT WOS:000269095400007 ER PT J AU Zeng, LL Shi, P Liu, WT Wang, DX AF Zeng, Lili Shi, Ping Liu, W. Timothy Wang, Dongxiao TI Evaluation of a satellite-derived latent heat flux product in the South China Sea: A comparison with moored buoy data and various products SO ATMOSPHERIC RESEARCH LA English DT Article; Proceedings Paper CT Special Session on Ocean-Atmosphere Coupling held at the 24th IUGG CY JUL 02-12, 2007 CL Perugia, ITALY SP IUGG DE Latent heat flux; South China Sea; TMI; Seasonal variations ID GLOBAL OCEANS; BULK PARAMETERIZATION; SURFACE TEMPERATURE; DATA SETS; HUMIDITY; ALGORITHM AB Latent heat flux in the South China Sea (SCS) mainly based on the Tropical Rain Measuring Mission Microwave Imager (TMI) is compared with the Objectively Analyzed air-sea heat Fluxes (OAFlux), the Goddard Satellite-Based Surface Turbulent Fluxes, version 2 (GSSTF2), the Japanese Ocean Flux Data Sets with use of Remote Sensing Observations (J-OFURO), the European Centre for Medium-Range Weather Forecasts (ECMWF), the National Centers for Environmental Prediction/Department of Energy reanalysis 2 (NCEP2), and International Comprehensive Ocean-Atmosphere Data Set data (ICOADS). These products did not all compare well to in situ data. It is found that TMI latent heat flux and OAFlux approximately reproduce the time variations of buoy data. However, ECMWF and ICOADS were found that had moderate systematic errors with respect to in situ data. All products qualitatively reveal a similar pattern in climatological fields. Although the satellite-derived products are quite similar, TMI latent heat is smaller than those of OAFlux, GSSTF2 and J-OFURO in the northern SCS. The difference between TMI latent heat and ICOADS is large, and the temporal correlation is extremely low in the entire basin except the Luson Strait. This is owned to that the ICOADS hardly reproduces accurate variability in the data-sparse regions. Also the temporal cross-correlation coefficients of between TMI latent heat and ECMWF or NCEP2 are considerably lower in the central SCS, may be affected by the lack of ship observations of ECMWF and NCEP2 there. The present study also compares meridional structures of the zonal averaged latent heat. The TMI latent heat and OAFlux overestimate the other two satellite-derived products during summer, whereas in winter, the TMI latent heat underestimates the other products in the northern regions. Though the examination of the influence of input variables, we note that the underestimation of TMI latent heat flux than other three satellite derived products in the northern region is mainly caused by larger near-surface air humidity there. While, large sea surface saturation humidity contributes to larger ECMWF latent heat flux. On the other hand, lager latent heat flux of NCEP2 in central parts and ICOADS in eastern bands is possibly mainly caused by the difference in winds. (C) 2008 Elsevier B.V. All rights reserved. C1 [Zeng, Lili; Shi, Ping; Wang, Dongxiao] Chinese Acad Sci, S China Sea Inst Oceanol, Key Lab Trop Marine Environm Dynam, Guangzhou 510301, Guangdong, Peoples R China. [Liu, W. Timothy] CALTECH, Jet Prop Lab 300 323, Pasadena, CA 91109 USA. RP Wang, DX (reprint author), Chinese Acad Sci, S China Sea Inst Oceanol, Key Lab Trop Marine Environm Dynam, 164 W Xingang Rd, Guangzhou 510301, Guangdong, Peoples R China. EM dxwang@scsio.ac.cn RI Zeng, Lily/N-7980-2013; WANG, DongXiao/B-4445-2012 NR 28 TC 21 Z9 28 U1 2 U2 11 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 SEP PY 2009 VL 94 IS 1 BP 91 EP 105 DI 10.1016/j.atmosres.2008.12.007 PG 15 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 496HR UT WOS:000269961500010 ER PT J AU Welch, RB Hoover, M Southward, EF AF Welch, Robert B. Hoover, Merrit Southward, Elissa F. TI Cognitive Performance During Prismatic Displacement as a Partial Analogue of "Space Fog" SO AVIATION SPACE AND ENVIRONMENTAL MEDICINE LA English DT Article DE microgravity; adaptation; space fog; cognitive performance ID PARABOLIC FLIGHT; ARM MOVEMENTS; ADAPTATION; EXPOSURE; COORDINATION; ATTENTION; MISSION; REARRANGEMENT; ENVIRONMENTS; SPACEFLIGHT AB WELCH RB, HOOVER M, SOUTHWARD EF. Cognitive performance during prismatic displacement as a partial analogue of "space fog." Aviat Space Environ Med 2009; 80:771-80. Background: The fact that microgravity adaptation and recovery from the cognitive deficit of "space fog" follow approximately the same time Course raises the possibility that they are related to one another. Two experiments tested this hypothesis. Methods: Because microgravity adaptation is unique to outer space, we investigated the Earth-based analogue of adapting to prismatic displacement. Participants' goal was to overcome the disruptive effects of this optical distortion oil the speed and accuracy with which they negotiated an outdoor "slalom course." The experimental group had the additional assignment of performing a cognitive task. In Experiment 1, the task was making serial Subtractions of 7 from an initial starting number, while in Experiment 2 it was to repeat back a sequence of high- and low-pitched tones. Results: in neither experiment did adaptation influence cognitive performance or vice versa. That is, the improvement of slalom-walking performance attributable to prism adaptation was the same with or without a concurrent cognitive task and cognitive task performance was unaffected by exposure to prismatic displacement. Instead, the experiments revealed that both prism exposure and cognitive task performance reduced participants' walking speed. Conclusions: These results Suggest that the pace of astronauts' visual-motor behavior in space will be slowed by both microgravity and the cognitive tasks they must perform. They also bolster the use of prism adaptation as all inexpensive, ground-based means of studying microgravity adaptation. C1 [Welch, Robert B.] NASA, Ames Res Ctr, Human Syst Integrat Div, Moffett Field, CA 94035 USA. [Hoover, Merrit; Southward, Elissa F.] Univ Calif Santa Cruz, Dept Psychol, Santa Cruz, CA 95064 USA. RP Welch, RB (reprint author), NASA, Ames Res Ctr, Human Syst Integrat Div, Mail Stop 262-2, Moffett Field, CA 94035 USA. EM robert.b.welch@nasa.gov FU National Aeronautics and Space Administration FX This research was supported by the Space Human Factors Engineering/Human Research Program of the National Aeronautics and Space Administration. The authors wish to thank Drs. Jacob Bloomberg, Malcolm M. Cohen, and Gordon M. Redding for their comments on an earlier draft of this Manuscript, and to Dr. Martine Godfroy for statistical and other assistance. NR 34 TC 4 Z9 4 U1 1 U2 3 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 SEP PY 2009 VL 80 IS 9 BP 771 EP 780 DI 10.3357/ASEM.2415.2009 PG 10 WC Public, Environmental & Occupational Health; Medicine, General & Internal; Sport Sciences SC Public, Environmental & Occupational Health; General & Internal Medicine; Sport Sciences GA 488FD UT WOS:000269333700001 PM 19750873 ER PT J AU Rosenzweig, C Solecki, WD Parshall, L Lynn, B Cox, J Goldberg, R Hodges, S Gaffin, S Slosberg, RB Savio, P Dunstan, F Watson, M AF Rosenzweig, Cynthia Solecki, William D. Parshall, Lily Lynn, Barry Cox, Jennifer Goldberg, Richard Hodges, Sara Gaffin, Stuart Slosberg, Ronald B. Savio, Peter Dunstan, Frank Watson, Mark TI MITIGATING NEW YORK CITY'S HEAT ISLAND Integrating Stakeholder Perspectives and Scientific Evaluation SO BULLETIN OF THE AMERICAN METEOROLOGICAL SOCIETY LA English DT Article ID SPECTRAL MIXTURE ANALYSIS; SURFACE-HYDROLOGY MODEL; AIR-QUALITY; METROPOLITAN-AREA; URBAN VEGETATION; MESOSCALE MODEL; IMPACTS; CLIMATE; SYSTEM; IMPLEMENTATION C1 [Rosenzweig, Cynthia] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Solecki, William D.; Cox, Jennifer; Hodges, Sara] CUNY Hunter Coll, Dept Geog, New York, NY 10021 USA. [Parshall, Lily; Lynn, Barry; Goldberg, Richard; Gaffin, Stuart] Columbia Univ, Ctr Climate Syst Res, New York, NY USA. [Slosberg, Ronald B.] L & S Energy Serv, Clifton Pk, NY USA. [Savio, Peter; Watson, Mark] New York State Energy Res & Dev Author, Albany, NY USA. [Dunstan, Frank] New York State Dept Environm Conservat, Albany, NY USA. RP Rosenzweig, C (reprint author), NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA. EM crosenzweig@giss.nasa.gov FU NYSERDA; New York State Department of Environmental Conservation (NYSDEC) FX The project was sponsored by NYSERDA and the New York State Department of Environmental Conservation (NYSDEC). The research team met regularly with NYSERDA and NYSDEC to refine research questions and receive feedback on research approaches, and with a steering group from local and national government agencies including NYC Department of Parks and Recreation, NYC Department of Design and Construction, and U. S. Environmental Protection Agency (EPA) Region II], nongovernmental organizations (e. g., Sustainable Energy Partnerships and Environmental Energy Alliance of New York), and private utilities (e. g., Con Edison). NR 52 TC 37 Z9 39 U1 5 U2 22 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 SEP PY 2009 VL 90 IS 9 BP 1297 EP 1312 DI 10.1175/2009BAMS2308.1 PG 16 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 509AH UT WOS:000270982600003 ER PT J AU Nayagam, V Balasubramaniam, R Williams, FA AF Nayagam, Vedha Balasubramaniam, R. Williams, Forman A. TI Diffusion flames over a melting polymer disk in von karman swirling flows SO COMBUSTION AND FLAME LA English DT Article DE Polymer combustion; Diffusion flame ID EXTINCTION; COUNTERFLOW; COMBUSTION; FUEL AB A laminar diffusion flame that is established over a spinning, thermoplastic, polymer fuel disk in a quiescent, oxidizing environment under microgravity is analyzed theoretically. The conservation equations for the polymer melt layer coupled to the gas-phase equations are solved numerically using similarity transformations. The polymer melting Fate, the thickness of the melt layer, and the fraction of melted fuel that is burned in the gas-phase are predicted as functions of the ambient conditions and polymer property values. In these Calculations the melt viscosity is assumed to vary with temperature in an Arrhenius form. Results are presented for polymethylmethacrylate (PMMA) disks burning in air at atmospheric pressure and compared against earlier experimental results. (C) 2009 The Combustion Institute. Published by Elsevier Inc. All rights reserved. C1 [Nayagam, Vedha; Balasubramaniam, R.] NASA Glenn Res Ctr, Natl Ctr Space Explorat Res, Cleveland, OH 44135 USA. [Williams, Forman A.] Univ Calif San Diego, Dept Mech & Aerosp Engn, La Jolla, CA 92093 USA. RP Nayagam, V (reprint author), NASA Glenn Res Ctr, Natl Ctr Space Explorat Res, Cleveland, OH 44135 USA. EM v.nayagam@grc.nasa.gov FU NASA FX This work was Supported by the Fire Prevention, Detection, and Suppression Project at the NASA Glenn Research Center and directed Dr. Gary Ruff. NR 22 TC 2 Z9 2 U1 0 U2 2 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0010-2180 J9 COMBUST FLAME JI Combust. Flame PD SEP PY 2009 VL 156 IS 9 BP 1698 EP 1704 DI 10.1016/j.combustflame.2009.06.009 PG 7 WC Thermodynamics; Energy & Fuels; Engineering, Multidisciplinary; Engineering, Chemical; Engineering, Mechanical SC Thermodynamics; Energy & Fuels; Engineering GA 487SR UT WOS:000269296500002 ER PT J AU d'Humieres, D Krafczyk, M Luo, LS Rubinstein, R AF d'Humieres, Dominique Krafczyk, Manfred Luo, Li-Shi Rubinstein, Robert TI Dedication to Pierre Lallemand on the occasion of his retirement SO COMPUTERS & MATHEMATICS WITH APPLICATIONS LA English DT Biographical-Item C1 [Luo, Li-Shi] Old Dominion Univ, Dept Math & Stat, Norfolk, VA 23529 USA. [Luo, Li-Shi] Old Dominion Univ, Ctr Computat Sci, Norfolk, VA 23529 USA. [d'Humieres, Dominique] Ecole Normale Super, Phys Stat Lab, F-75231 Paris, France. [Krafczyk, Manfred] Tech Univ Carolo Wilhelmina Braunschweig, Inst Rechnergestutzte Modellierung Bauingenieurwe, D-38106 Braunschweig, Germany. [Rubinstein, Robert] NASA, Langley Res Ctr, Computat Aerosci Branch, Hampton, VA 23681 USA. RP Luo, LS (reprint author), Old Dominion Univ, Dept Math & Stat, Norfolk, VA 23529 USA. EM dominiq@lps.ens.fr; kraft@irmb.tu-bs.de; lluo@odu.edu; r.rubinstein@nasa.gov NR 2 TC 0 Z9 0 U1 0 U2 2 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0898-1221 J9 COMPUT MATH APPL JI Comput. Math. Appl. PD SEP PY 2009 VL 58 IS 5 BP 821 EP 822 DI 10.1016/j.camwa.2009.02.007 PG 2 WC Mathematics, Applied SC Mathematics GA 488ED UT WOS:000269331000002 ER PT J AU Coustenis, A Lunine, J Lebreton, JP Matson, D Erd, C Reh, K Beauchamp, P Lorenz, R Waite, H Sotin, C Gurvits, L Hirtzig, M AF Coustenis, Athena Lunine, Jonathan Lebreton, Jean-Pierre Matson, Dennis Erd, Christian Reh, Kim Beauchamp, Patricia Lorenz, Ralph Waite, Hunter Sotin, Christophe Gurvits, Leonid Hirtzig, Mathieu TI Earth-Based Support for the Titan Saturn System Mission SO EARTH MOON AND PLANETS LA English DT Article; Proceedings Paper CT Workshop on Future Ground-based Solar System Research - Synergies with Space Probes and Space Telescope CY SEP 08-12, 2008 CL Portoferraio, ITALY SP INAF, Arcetri ESO DE Titan; Space mission; Probes; Balloons; Montgolfiere; Lander AB The Titan Saturn System Mission (TSSM) concept is composed of a TSSM orbiter provided by NASA that would carry two Titan in situ elements provided by ESA: the montgolfiSre and the probe/lake lander. One overarching goal of TSSM is to explore in situ the atmosphere and surface of Titan. The mission has been prioritized as the second Outer Planets Flagship Mission, the first one being the Europa Jupiter System Mission (EJSM). TSSM would launch around 2023-2025 arriving at Saturn 9 years later followed by a 4-year science mission in the Saturn system. Following delivery of the in situ elements to Titan, the TSSM orbiter would explore the Saturn system via a 2-year tour that includes Enceladus and Titan flybys before entering into a dedicated orbit around Titan. The Titan montgolfiSre aerial vehicle under consideration will circumnavigate Titan at a latitude of similar to 20A degrees and at altitudes of similar to 10 km for a minimum of 6 months. The probe/lake lander will descend through Titan's atmosphere and land on the liquid surface of Kraken Mare (similar to 75A degrees north latitude). As for any planetary space science mission, and based on the Cassini-Huygens experience, Earth-based observations will be synergistic and enable scientific optimization of the return of such a mission. Some specific examples of how this can be achieved (through VLBI and Doppler tracking, continuous monitoring of atmospheric and surface features, and Direct-to-Earth transmission) are described in this paper. C1 [Coustenis, Athena; Hirtzig, Mathieu] Observ Paris, LESIA, F-92195 Meudon, France. [Lunine, Jonathan] Univ Arizona, Dept Planetary Sci, Tucson, AZ 85721 USA. [Lebreton, Jean-Pierre; Erd, Christian] ESA, Estec, SRE SM, NL-2201 AZ Noordwijk, Netherlands. [Matson, Dennis; Reh, Kim; Beauchamp, Patricia; Sotin, Christophe] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Lorenz, Ralph] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Waite, Hunter] SW Res Inst, San Antonio, TX USA. [Gurvits, Leonid] Joint Inst VLBI Europe, NL-7990 AA Dwingeloo, Netherlands. RP Coustenis, A (reprint author), Observ Paris, LESIA, 5,Pl J Janssen, F-92195 Meudon, France. EM Athena.coustenis@obspm.fr; jlunine@lpl.arizona.edu; jean-pierre.lebreton@esa.int; dmatson@jpl.nasa.gov; kim.r.reh@jpl.nasa.gov; patricia.m.beauchamp@jpl.nasa.gov; Ralph.lorenz@jhuapl.edu; hwaite@swri.edu; csotin@jpl.nasa.gov; lgurvits@jive.nl RI Lorenz, Ralph/B-8759-2016 OI Lorenz, Ralph/0000-0001-8528-4644 NR 7 TC 4 Z9 4 U1 0 U2 7 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0167-9295 J9 EARTH MOON PLANETS JI Earth Moon Planets PD SEP PY 2009 VL 105 IS 2-4 BP 135 EP 142 DI 10.1007/s11038-009-9308-9 PG 8 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Geology GA 480ZP UT WOS:000268776300012 ER PT J AU Orton, GS AF Orton, Glenn S. TI Ground-Based Observational Support for Spacecraft Exploration of the Outer Planets SO EARTH MOON AND PLANETS LA English DT Article; Proceedings Paper CT Workshop on Future Ground-based Solar System Research - Synergies with Space Probes and Space Telescope CY SEP 08-12, 2008 CL Portoferraio, ITALY SP INAF, Arcetri ESO DE Infrared; Outer planets; Atmospheres; Cassini; JUNO ID PROBE ENTRY SITE; STRATOSPHERIC TEMPERATURES; HOT-SPOTS; JUPITER; OSCILLATION; POLARIMETRY; PHOTOMETRY; LATITUDE; SATURN; CLOUD AB This report presents both a retrospective of ground-based support for spacecraft missions to the outer solar system and a perspective of support for future missions. Past support is reviewed in a series of case studies involving the author. The most basic support is essential, providing the mission with information without which the planned science would not have been accomplished. Another is critical, without which science would have been returned, but missing a key element in its understanding. Some observations are enabling by accomplishing one aspect of an experiment which would otherwise not have been possible. Other observations provide a perspective of the planet as a whole which is not available to instruments with narrow fields of view and limited spatial coverage, sometimes motivating a re-prioritizing of experiment objectives. Ground-based support is also capable of providing spectral coverage not present in the complement of spacecraft instruments. Earth-based observations also have the capability of filling in gaps of spacecraft coverage of atmospheric phenomena, as well as providing surveillance of longer-term behavior than the coverage available to the mission. Future missions benefiting from ground-based support would include the Juno mission to Jupiter in the next decade, a flagship-class mission to the Jupiter or to the Saturn systems currently under consideration, and possible intermediate-class missions which might be proposed in NASA's New Frontiers category. One of the principal benefits of future 30 m-class giant telescopes would be to improve the spatial resolution of maps of temperature and composition which are derived from observations of thermal emission at mid-infrared and longer wavelengths. In many situations, this spatial resolution is competitive with those of the relevant instruments on the spacecraft themselves. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Orton, GS (reprint author), CALTECH, Jet Prop Lab, MS 169-237,4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM go@scn.jpl.nasa.gov NR 25 TC 2 Z9 2 U1 3 U2 4 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0167-9295 J9 EARTH MOON PLANETS JI Earth Moon Planets PD SEP PY 2009 VL 105 IS 2-4 BP 143 EP 152 DI 10.1007/s11038-009-9295-x PG 10 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Geology GA 480ZP UT WOS:000268776300013 ER PT J AU Mark, S Reynolds-May, MF AF Mark, Saralyn Reynolds-May, Margaret F. TI IMPACT OF SEX AND GENDER IN ENDOCRINOLOGY AND IMPLICATIONS FOR CLINICAL PRACTICE SO ENDOCRINE PRACTICE LA English DT Editorial Material ID THYROID-DYSFUNCTION; ANTIBODIES; PREVALENCE; HEALTH; MEN C1 [Mark, Saralyn] NASA, Off Chief Hlth & Med Officer, Washington, DC 20546 USA. [Mark, Saralyn; Reynolds-May, Margaret F.] Yale Univ, Sch Med, New Haven, CT USA. RP Mark, S (reprint author), NASA, Off Chief Hlth & Med Officer, Headquarters 5H35,300 E St SW, Washington, DC 20546 USA. EM smark@hq.nasa.gov NR 20 TC 0 Z9 0 U1 1 U2 2 PU AMER ASSOC CLIN ENDOCRINOL PI JACKSONVILLE PA 1000 RIVERSIDE AVE, STE 205, JACKSONVILLE, FL 32204 USA SN 1530-891X J9 ENDOCR PRACT JI Endocr. Pract. PD SEP-OCT PY 2009 VL 15 IS 6 BP 587 EP 589 DI 10.4158/EP09094.CO PG 3 WC Endocrinology & Metabolism SC Endocrinology & Metabolism GA 520EP UT WOS:000271823300011 PM 19491066 ER PT J AU Garonna, I Fazey, I Brown, ME Pettorelli, N AF Garonna, Irene Fazey, Ioan Brown, Molly E. Pettorelli, Nathalie TI Rapid primary productivity changes in one of the last coastal rainforests: the case of Kahua, Solomon Islands SO ENVIRONMENTAL CONSERVATION LA English DT Article DE MODIS (moderate-resolution imaging spectro-radiometer); NDVI (normalized difference vegetation index); primary productivity; Solomon Islands; tropical forests ID AVHRR DATA; TROPICAL FORESTS; SATELLITE DATA; SOUTH-AMERICA; VEGETATION; CLIMATE; ENVIRONMENT; ADAPTATION; COVER; NDVI AB The growth of human populations has many direct and indirect impacts on tropical forest ecosystems both locally and globally. This is particularly true in the Solon-ion Islands, where coastal rainforest cover still remains, but where climate change and a growing human Population is putting increasing pressure on ecosystems. This study assessed recent primary productivity changes in the Kahua region (Makira, Solomon Islands) using remote sensing data (normalized difference vegetation index, NDVI). In this area, there has been no commercial logging and there is no existing information about the state of the forests. Results indicate that primary productivity has been decreasing in recent years, and that the recent changes arc more marked near vi I]ages. Multiple factors may explain the reported pattern in primary productivity. The study highlights the need to (1) assess how accurately remote sensing data-based results match field data on the ground; (2) identify, the relative contribution of the climatic, socioeconomic and political drivers of such changes; and (3) evaluate how primary productivity changes affect biodiversity level, ecosystem functioning and human livelihoods. C1 [Garonna, Irene; Pettorelli, Nathalie] Zool Soc London, Inst Zool, London NW1 4RY, England. [Fazey, Ioan] Univ St Andrews, Sch Geog & Geosci, St Andrews KY16 9AL, Fife, Scotland. [Brown, Molly E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Pettorelli, N (reprint author), Zool Soc London, Inst Zool, Regents Pk, London NW1 4RY, England. EM Nathalie.Pettorelli@ioz.ac.uk RI Brown, Molly/E-2724-2010; Brown, Molly/M-5146-2013 OI Brown, Molly/0000-0001-7384-3314; Brown, Molly/0000-0001-7384-3314 NR 49 TC 19 Z9 19 U1 0 U2 6 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 0376-8929 J9 ENVIRON CONSERV JI Environ. Conserv. PD SEP PY 2009 VL 36 IS 3 BP 253 EP 260 DI 10.1017/S0376892909990208 PG 8 WC Biodiversity Conservation; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 573GQ UT WOS:000275897300010 ER PT J AU House, CH Orphan, VJ Turk, KA Thomas, B Pernthaler, A Vrentas, JM Joye, SB AF House, Christopher H. Orphan, Victoria J. Turk, Kendra A. Thomas, Burt Pernthaler, Annelie Vrentas, Jennifer M. Joye, Samantha B. TI Extensive carbon isotopic heterogeneity among methane seep microbiota SO ENVIRONMENTAL MICROBIOLOGY LA English DT Article ID ANOXIC MARINE-SEDIMENTS; MEXICO COLD SEEPS; EEL RIVER-BASIN; ANAEROBIC OXIDATION; SULFATE REDUCTION; BLACK-SEA; COMMUNITIES; ARCHAEA; METHANOGENESIS; CONSORTIUM AB P>To assess and study the heterogeneity of delta(13)C values for seep microorganisms of the Eel River Basin, we studied two principally different sample sets: sediments from push cores and artificial surfaces colonized over a 14 month in situ incubation. In a single sediment core, the delta(13)C compositions of methane seep-associated microorganisms were measured and the relative activity of several metabolisms was determined using radiotracers. We observed a large range of archaeal delta(13)C values (> 50 parts per thousand) in this microbial community. The delta(13)C of ANME-1 rods ranged from -24 parts per thousand to -87 parts per thousand. The delta(13)C of ANME-2 sarcina ranged from -18 parts per thousand to -75 parts per thousand. Initial measurements of shell aggregates were as heavy as -19.5 parts per thousand with none observed to be lighter than -57 parts per thousand. Subsequent measurements on shell aggregates trended lighter reaching values as (13)C-depleted as -73 parts per thousand. The observed isotopic trends found for mixed aggregates were similar to those found for shell aggregates in that the initial measurements were often enriched and the subsequent analyses were more (13)C-depleted (with values as light as -56 parts per thousand). The isotopic heterogeneity and trends observed within taxonomic groups suggest that ANME-1 and ANME-2 sarcina are capable of both methanogenesis and methanotrophy. In situ microbial growth was investigated by incubating a series of slides and silicon (Si) wafers for 14 months in seep sediment. The experiment showed ubiquitous growth of bacterial filaments (mean delta(13)C = -38 +/- 3 parts per thousand), suggesting that this bacterial morphotype was capable of rapid colonization and growth. C1 [House, Christopher H.; Thomas, Burt; Vrentas, Jennifer M.] Penn State Univ, Dept Geosci, University Pk, PA 16802 USA. [House, Christopher H.; Thomas, Burt; Vrentas, Jennifer M.] Penn State Univ, Penn State Astrobiol Res Ctr, University Pk, PA 16802 USA. [Orphan, Victoria J.; Turk, Kendra A.; Pernthaler, Annelie] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Joye, Samantha B.] Univ Georgia, Dept Marine Sci, Athens, GA 30602 USA. RP House, CH (reprint author), NASA, Ames Res Ctr, Mail Stop 239-4, Moffett Field, CA 94035 USA. EM chouse@geosc.psu.edu RI Orphan, Victoria/K-1002-2014; UCLA, SIMS/A-1459-2011; OI Orphan, Victoria/0000-0002-5374-6178; Thomas, Burt/0000-0002-2228-6770; Joye, Samantha/0000-0003-1610-451X FU Penn State Astrobiology Research Center; NOAA-NURP [UAF 05-0132]; National Science Foundation [MCB-0348492, OCE-0085549]; ACS-PRF; National Science Foundation Instrumentation and Facilities Program; Moore Foundation; NSF (IGERT) [DGE-9972759] FX We thank Zhidan Zhang and Tsegereda Embaye for laboratory assistance, and the captain and crew of the R/V Western Flyer and ROV Tiburon for their tireless efforts during the field expedition. We also thank Katherine H. Freeman for the opportunity to measure the delta13C isotopic composition of our Escherichia coli cells by EA-CF-IRMS in the PSU Isotope Biogeochemistry Laboratory. This work was funded by the Penn State Astrobiology Research Center (through the National Astrobiology Institute), NOAA-NURP (UAF 05-0132), the National Science Foundation (MCB-0348492 and OCE-0085549), and the ACS-PRF. The UCLA ion Microprobe is partially supported by a grant from the National Science Foundation Instrumentation and Facilities Program. Also, the ion microprobe work in this paper was supported by a grant from the Moore Foundation. Graduate support (B.T.) for this project was provided by the Penn State Biogeochemical Research Initiative for Education funded by NSF (IGERT) Grant DGE-9972759. NR 33 TC 23 Z9 24 U1 0 U2 16 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1462-2912 J9 ENVIRON MICROBIOL JI Environ. Microbiol. PD SEP PY 2009 VL 11 IS 9 BP 2207 EP 2215 DI 10.1111/j.1462-2920.2009.01934.x PG 9 WC Microbiology SC Microbiology GA 490WV UT WOS:000269539700004 PM 19508338 ER PT J AU Anenberg, SC West, JJ Fiore, AM Jaffe, DA Prather, MJ Bergmann, D Cuvelier, K Dentener, FJ Duncan, BN Gauss, M Hess, P Jonson, JE Lupu, A MacKenzie, IA Marmer, E Park, RJ Sanderson, MG Schultz, M Shindell, DT Szopa, S Vivanco, MG Wild, O Zang, G AF Anenberg, Susan Casper West, J. Jason Fiore, Arlene M. Jaffe, Daniel A. Prather, Michael J. Bergmann, Daniel Cuvelier, Kees Dentener, Frank J. Duncan, Bryan N. Gauss, Michael Hess, Peter Jonson, Jan Eiof Lupu, Alexandru MacKenzie, Ian A. Marmer, Elina Park, Rokjin J. Sanderson, Michael G. Schultz, Martin Shindell, Drew T. Szopa, Sophie Garcia Vivanco, Marta Wild, Oliver Zang, Guang TI Intercontinental Impacts of Ozone Pollution on Human Mortality SO ENVIRONMENTAL SCIENCE & TECHNOLOGY LA English DT Article ID TROPOSPHERIC OZONE; HEALTH-BENEFITS; AIR-POLLUTION; METAANALYSIS; EMISSIONS AB Ozone exposure is associated with negative health impacts, including premature mortality. Observations and modeling studies demonstrate that emissions from one continent influence ozone air quality over other continents. We estimate the premature mortalities avoided from surface ozone decreases obtained via combined 20% reductions of anthropogenic nitrogen oxide, nonmethane volatile organic compound, and carbon monoxide emissions in North America (NA), East Asia (EA), South Asia (SA), and Europe (EU). We use estimates of ozone responses to these emission changes from several atmospheric chemical transport models combined with a health impact function. Foreign emission reductions contribute approximately 30%, 30%, 20%, and > 50% of the mortalities avoided by reducing precursor emissions in all regions together in NA, EA, SA, and EU, respectively. Reducing emissions in NA and EU avoids more mortalities outside the source region than within, owing in part to larger populations in foreign regions. Lowering the global methane abundance by 20% reduces mortality most in SA,followed by EU, EA, and NA. For some source-receptor pairs, there is greater uncertainty in our estimated avoided mortalities associated with the modeled ozone responses to emission changes than with the health impact function parameters. C1 [Anenberg, Susan Casper; West, J. Jason] Univ N Carolina, Chapel Hill, NC 27515 USA. [Fiore, Arlene M.] NOAA, Geophys Fluid Dynam Lab, Princeton, NJ USA. [Jaffe, Daniel A.] Univ Washington Bothell, Bothell, WA USA. [Prather, Michael J.] Univ Calif Irvine, Irvine, CA USA. [Bergmann, Daniel] Lawrence Livermore Natl Lab, Div Atmospher Sci, Livermore, CA USA. [Cuvelier, Kees; Dentener, Frank J.] Commiss European Communities, DG Joint Res Ctr, Inst Environm & Sustainability, Ispra, Italy. [Gauss, Michael; Sanderson, Michael G.] Univ Oslo, Dept Geosci, N-0316 Oslo, Norway. [Gauss, Michael; Jonson, Jan Eiof; Szopa, Sophie] Norwegian Meteorol Inst, Oslo, Norway. [Hess, Peter] Natl Ctr Atmospher Res, Boulder, CO 80307 USA. [Hess, Peter] Cornell Univ, Ithaca, NY USA. [Lupu, Alexandru] York Univ, Ctr Res Earth & Space Sci, N York, ON M3J 1P3, Canada. [MacKenzie, Ian A.] Univ Edinburgh, Sch Geosci, Edinburgh EH8 9YL, Midlothian, Scotland. [Park, Rokjin J.] Harvard Univ, Atmospher Chem Modeling Grp, Cambridge, MA 02138 USA. [Sanderson, Michael G.] Hadley Ctr, Met Off, Exeter, Devon, England. [Schultz, Martin] Forschungszentrum Julich, ICG 2, Julich, Germany. [Shindell, Drew T.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Shindell, Drew T.] Columbia Univ, New York, NY USA. [Szopa, Sophie] UVSQ, CNRS, CEA, Lab Sci Climat & Environm,IPSL, Gif Sur Yvette, France. [Garcia Vivanco, Marta] CIEMAT, E-28040 Madrid, Spain. [Wild, Oliver] Univ Lancaster, Lancaster Environm Ctr, Lancaster LA1 4YW, England. [Zang, Guang] Univ Cambridge, Dept Chem, Natl Ctr Atmospher Sci, Cambridge CB2 1TN, England. RP West, JJ (reprint author), Univ N Carolina, Chapel Hill, NC 27515 USA. EM jasonwest@unc.edu RI Wild, Oliver/A-4909-2009; Szopa, Sophie/F-8984-2010; Lupu, Alexandru/D-3689-2009; Bergmann, Daniel/F-9801-2011; Vivanco, Marta/L-9816-2014; West, Jason/J-2322-2015; Park, Rokjin/I-5055-2012; Hess, Peter/M-3145-2015; Shindell, Drew/D-4636-2012; Duncan, Bryan/A-5962-2011; Schultz, Martin/I-9512-2012; mackenzie, ian/E-9320-2013 OI Wild, Oliver/0000-0002-6227-7035; Szopa, Sophie/0000-0002-8641-1737; Lupu, Alexandru/0000-0002-4520-5523; Bergmann, Daniel/0000-0003-4357-6301; Vivanco, Marta/0000-0002-5828-1859; West, Jason/0000-0001-5652-4987; Park, Rokjin/0000-0001-8922-0234; Hess, Peter/0000-0003-2439-3796; Schultz, Martin/0000-0003-3455-774X; FU Merck Foundation; University of North Carolina Junior Faculty Development Award; Canadian Foundation for Climate and Atmospheric Sciences; Ontario Ministry of the Environment; Canadian Foundation for Innovation; Ontario Innovation Trust; Research Settlement Fund; NERC [NE/D012538/1]; Defra [AQ0409]; DECC/Defra [GA01101]; MOD [CBC/2B/0417-Annex C5] FX This work was Supported by the Merck Foundation and a University of North Carolina Junior Faculty Development Award. Model Simulations were performed under the UN ECE Task Force oil Hemispheric Transport of Air Pollution. A.L. acknowledges financial support from the Canadian Foundation for Climate and Atmospheric Sciences, the Ontario Ministry of the Environment, the Canadian Foundation for Innovation and the Ontario Innovation Trust. R.J.P. was partly supported by Research Settlement Fund for the new faculty of SNU. I.A.M. acknowledges funding from NERC (NE/D012538/1). M.G.S. was supported by Defra (AQ0409), DECC/Defra (GA01101), and MOD (CBC/2B/0417-Annex C5). NR 25 TC 39 Z9 40 U1 5 U2 28 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 SEP 1 PY 2009 VL 43 IS 17 BP 6482 EP 6487 DI 10.1021/es900518z PG 6 WC Engineering, Environmental; Environmental Sciences SC Engineering; Environmental Sciences & Ecology GA 487GB UT WOS:000269258000012 PM 19764205 ER PT J AU Maier, GO Simenstad, CA AF Maier, Greer O. Simenstad, Charles A. TI The Role of Marsh-Derived Macrodetritus to the Food Webs of Juvenile Chinook Salmon in a Large Altered Estuary SO ESTUARIES AND COASTS LA English DT Article DE Detritus; Food webs; Isotopes; Juvenile Chinook; Columbia River estuary ID COLUMBIA RIVER ESTUARY; STABLE-ISOTOPE RATIOS; ORGANIC-MATTER FLOW; SALT-MARSH; CARBON ISOTOPES; ONCORHYNCHUS-TSHAWYTSCHA; SPARTINA-ALTERNIFLORA; BENTHIC MICROALGAE; BRITISH-COLUMBIA; GROWTH-RATE AB The goal of this study was to determine the food web pathways supporting juvenile Chinook (Oncorhynchus tshawytscha) salmon in the Columbia River estuary through multiple stable isotope analysis (delta(13)C, delta(15)N, delta(34)S). Using this method, we distinguished the role of various organic matter sources in Chinook food webs and interpreted the dynamics of their use both spatially and temporally within the estuary. Our results indicate that subyearling Chinook are associated with fluvial, anthropogenic, estuarine, and marine organic matter sources, with hatchery food and vascular plant detritus being the most dominant sources in juvenile Chinook food webs. Although freshwater phytoplankton is involved in many food web pathways to subyearling Chinook, increased phytoplankton production from the impounded river has not replaced the loss of autochthonous marsh production to fish. Our results indicate that large-scale ecosystem alteration may have decreased the availability and quality of food webs in the estuary and potentially diminished the ability of the Columbia to support Chinook salmon. C1 [Maier, Greer O.; Simenstad, Charles A.] Univ Washington, Sch Aquat & Fishery Sci, Seattle, WA 98195 USA. RP Maier, GO (reprint author), Natl Marine Fisheries Serv, NOAA, 1829 S Oregon St, Yreka, CA 96097 USA. EM greer.anderson@noaa.gov; simenstd@u.washington.edu FU Bonneville Power Administration; University of Washington FX The authors of this paper are grateful to a number of people for their contribution to this work: firstly, Dan Bottom, Mary Bhuthimethee, Lance Campbell, Ed Casillas, Kurt Fresh, Susan Hinton, George McCabe, Regan McNatt, Curtis Roegner, Lia Stamatiou, David Teel, and Jen Zamon for their help collecting fish. Jen Burke, Mary Austill Lott, and Daniel Shindler from the University of Washington provided continuous support and guidance. They would also like to thank Fred Prahl at Oregon State University for his assistance during laboratory and data analysis. Lastly, Peter Bisson and Jim Lichatowich helped in reviewing this paper and financial support was provided by Bonneville Power Administration and the University of Washington. NR 66 TC 15 Z9 15 U1 0 U2 23 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 1559-2723 J9 ESTUAR COAST JI Estuaries Coasts PD SEP PY 2009 VL 32 IS 5 BP 984 EP 998 DI 10.1007/s12237-009-9197-1 PG 15 WC Environmental Sciences; Marine & Freshwater Biology SC Environmental Sciences & Ecology; Marine & Freshwater Biology GA 482PP UT WOS:000268901500013 ER PT J AU Funk, CC Brown, ME AF Funk, Chris C. Brown, Molly E. TI Declining global per capita agricultural production and warming oceans threaten food security SO FOOD SECURITY LA English DT Article DE Global food security; Food availability; Agricultural production; Agricultural development; Climate change; Drought; Population growth ID CLIMATE-CHANGE; AFRICA AB Despite accelerating globalization, most people still eat food that is grown locally. Developing countries with weak purchasing power tend to import as little food as possible from global markets, suffering consumption deficits during times of high prices or production declines. Local agricultural production, therefore, is critical to both food security and economic development among the rural poor. The level of local agricultural production, in turn, will be determined by the amount and quality of arable land, the amount and quality of agricultural inputs (fertilizer, seeds, pesticides, etc.), as well as farm-related technology, practices and policies. This paper discusses several emerging threats to global and regional food security, including declining yield gains that are failing to keep up with population increases, and warming in the tropical Indian Ocean and its impact on rainfall. If yields continue to grow more slowly than per capita harvested area, parts of Africa, Asia and Central and Southern America will experience substantial declines in per capita cereal production. Global per capita cereal production will potentially decline by 14% between 2008 and 2030. Climate change is likely to further affect food production, particularly in regions that have very low yields due to lack of technology. Drought, caused by anthropogenic warming in the Indian and Pacific Oceans, may also reduce 21st century food availability in some countries by disrupting moisture transports and bringing down dry air over crop growing areas. The impacts of these circulation changes over Asia remain uncertain. For Africa, however, Indian Ocean warming appears to have already reduced rainfall during the main growing season along the eastern edge of tropical Africa, from southern Somalia to northern parts of the Republic of South Africa. Through a combination of quantitative modeling of food balances and an examination of climate change, this study presents an analysis of emerging threats to global food security. C1 [Funk, Chris C.] Univ Calif Santa Barbara, US Geol Survey, Earth Resources Observat & Sci EROS Ctr, Dept Geog, Santa Barbara, CA 96105 USA. [Brown, Molly E.] NASA, Goddard Space Flight Ctr, Biospher Sci Branch, Greenbelt, MD 20771 USA. RP Funk, CC (reprint author), Univ Calif Santa Barbara, US Geol Survey, Earth Resources Observat & Sci EROS Ctr, Dept Geog, Ellison Hall, Santa Barbara, CA 96105 USA. EM cfunk@usgs.gov RI Brown, Molly/M-5146-2013 OI Brown, Molly/0000-0001-7384-3314 FU US Agency for International Development Famine Early Warning System Network; NASA Precipitation Monitoring Mission [NNX07AG26G]; NASA [NN-H-04-Z-YO-010-C] FX The authors would like to sincerely thank our anonymous reviewers, as well as colleagues from the USGS who graciously supplied their comments. Without their efforts this paper would be much less coherent. We would also like to express our gratitude to the UN Food and Agricultural Organization and the Program for Climate Model Diagnostics and Intercomparison for providing, respectively, access to the agriculture and climate modeling data used in this study. This research has been supported by funding from the US Agency for International Development Famine Early Warning System Network, the NASA Precipitation Monitoring Mission (grant NNX07AG26G), and a NASA decision support project (Cooperative Agreement Notice NN-H-04-Z-YO-010-C). NR 26 TC 61 Z9 63 U1 4 U2 51 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 1876-4517 EI 1876-4525 J9 FOOD SECUR JI Food Secur. PD SEP PY 2009 VL 1 IS 3 BP 271 EP 289 DI 10.1007/s12571-009-0026-y PG 19 WC Food Science & Technology SC Food Science & Technology GA 675WE UT WOS:000283870600005 ER PT J AU Krot, AN Amelin, Y Bland, P Ciesla, FJ Connelly, J Davis, AM Huss, GR Hutcheon, ID Makide, K Nagashima, K Nyquist, LE Russell, SS Scott, ERD Thrane, K Yurimoto, H Yin, QZ AF Krot, A. N. Amelin, Y. Bland, P. Ciesla, F. J. Connelly, J. Davis, A. M. Huss, G. R. Hutcheon, I. D. Makide, K. Nagashima, K. Nyquist, L. E. Russell, S. S. Scott, E. R. D. Thrane, K. Yurimoto, H. Yin, Q. -Z. TI Origin and chronology of chondritic components: A review SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Review ID EARLY SOLAR-SYSTEM; ALUMINUM-RICH INCLUSIONS; SHORT-LIVED BE-10; OXYGEN ISOTOPIC COMPOSITIONS; IN-SITU DECAY; CH CARBONACEOUS CHONDRITES; REDUCED-CV CHONDRITES; ZONED METAL GRAINS; REFRACTORY INCLUSIONS; CHONDRULE FORMATION AB Mineralogical observations, chemical and oxygen-isotope compositions, absolute (207)Pb-(206)Pb ages and short-lived isotope systematics ((7)Be-(7)Li, (10)Be-(10)B, (26)Al-(26)Mg, (36)Cl-(36)S, (41)Ca-(41)K, (53)Mn-(53)Cr, (60)Fe-(60)Ni, (182) Hf-(182)W) of refractory inclusions [Ca,Al-rich inclusions (CAIs) and amoeboid olivine aggregates (AOAs)], chondrules and matrices from primitive (unmetamorphosed) chondrites are reviewed in an attempt to test (i) the x-wind model vs. the shock-wave model of the origin of chondritic components and (ii) irradiation vs. stellar origin of short-lived radionuclides. The data reviewed are consistent with an external, stellar origin for most short-lived radionuclides ((7)Be, (10)Be, and (36)Cl are important exceptions) and a shock-wave model for chondrule formation, and provide a sound basis for early Solar System chronology. They are inconsistent with the x-wind model for the origin of chondritic components and a local, irradiation origin of (26)Al, (41)Ca, and (53)Mn. (10)Be is heterogeneously distributed among CAIs, indicating its formation by local irradiation and precluding its use for the early solar system chronology. (41)Ca-(41)K, and (60)Fe-(60)Ni systematics are important for understanding the astrophysical setting of Solar System formation and origin of short-lived radionuclides, but so far have limited implications for the chronology of chondritic components. The chronological significance of oxygen-isotope compositions of chondritic components is limited. The following general picture of formation of chondritic components is inferred. CAIs and AOAs were the first solids formed in the solar nebula similar to 4567-4568 Myr ago, possibly within a period of <0.1 Myr, when the Sun was an infalling (class 0) and evolved (class 1) protostar. They formed during multiple transient heating events in nebular region(s) with high ambient temperature (at or above condensation temperature of forsterite), either throughout the inner protoplanetary disk (1-4 AU) or in a localized region near the proto-Sun (<0.1 AU), and were subsequently dispersed throughout the disk. Most CAIs and AOAs formed in the presence of an (16)O-rich (Delta(17)O similar to -24 +/- 2 parts per thousand) nebular gas. The (26)Al-poor [((26)Al/(27)Al)(0) < 1 x 10(-5)], (16)O-rich (Delta(17)O similar to -24 +/- 2 parts per thousand) CAIs - FUN (fractionation and unidentified nuclear effects) CAIs in CV chondrites, platy hibonite crystals (PLACs) in CM chondrites, pyroxene-hibonite spherules in CM and CO chondrites, and the majority of grossite- and hibonite-rich CAIs in CH chondrites-may have formed prior to injection and/or homogenization of (26)Al in the early Solar System. A small number of igneous CAIs in ordinary, enstatite and carbonaceous chondrites, and virtually all CAIs in CB chondrites are (16)O-depleted (Delta(17)O > - 10 parts per thousand) and have ((26)Al/(27)Al)(0) similar to those in chondrules (<1 x 10(-5)). These CAIs probably experienced melting during chondrule formation. Chondrules and most of the fine-grained matrix materials in primitive chondrites formed 1-4 Myr after CAIs, when the Sun was a classical (class II) and weak-lined T Turi star (class III). These chondritic components formed during multiple transient heating events in regions with low ambient temperature (<1000 K) throughout the inner protoplanetary disk in the presence of (16)O-poor (Delta(17)O > -5 parts per thousand) nebular gas. The majority of chondrules within a chondrite group may have formed over a much shorter period of time (<0.5-1 Myr). Mineralogical and isotopic observations indicate that CAIs were present in the regions where chondrules formed and accreted (1-4 AU), indicating that CAIs were present in the disk as free-floating objects for at least 4 Myr. Many CAIs, however, were largely unaffected by chondrule melting, suggesting that chondrule-forming events experienced by a nebular region could have been small in scale and limited in number. Chondrules and metal grains in CB chondrites formed during a single-stage, highly-energetic event similar to 4563 Myr ago, possibly from a gas-melt plume produced by collision between planetary embryos. (C) 2009 Elsevier Ltd. All rights reserved. C1 [Krot, A. N.; Huss, G. R.; Makide, K.; Nagashima, K.; Scott, E. R. D.] Univ Hawaii Manoa, Sch Ocean & Earth Sci & Technol, Hawaii Inst Geophys & Planetol, Honolulu, HI 96822 USA. [Amelin, Y.] Australian Natl Univ, Inst Plant Sci, Canberra, ACT 0200, Australia. [Amelin, Y.] Australian Natl Univ, Res Sch Earth Sci, Canberra, ACT 0200, Australia. [Bland, P.] Univ London Imperial Coll Sci Technol & Med, Dept Earth Sci & Engn, Impacts & Astromat Res Ctr, London SW7 2AZ, England. [Ciesla, F. J.] Univ Chicago, Dept Geophys Sci, Chicago, IL 60637 USA. [Connelly, J.] Univ Copenhagen, Geol Museum, DK-1350 Copenhagen, Denmark. [Connelly, J.] Univ Texas Austin, Jackson Sch Geosci, Austin, TX 78712 USA. [Hutcheon, I. D.] Lawrence Livermore Natl Lab, Glenn T Seaborg Inst, Livermore, CA 94451 USA. [Nyquist, L. E.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Russell, S. S.] Nat Hist Museum, Dept Mineral, London SW7 5BD, England. [Yurimoto, H.] Hokkaido Univ, Div Earth & Planetary Sci, Sapporo, Hokkaido 0600810, Japan. [Yin, Q. -Z.] Univ Calif Davis, Dept Geol, Davis, CA 95616 USA. RP Krot, AN (reprint author), Univ Hawaii Manoa, Sch Ocean & Earth Sci & Technol, Hawaii Inst Geophys & Planetol, Honolulu, HI 96822 USA. EM sasha@higp.hawaii.edu RI Yin, Qing-Zhu/B-8198-2009; Connelly, James /O-7996-2015; OI Yin, Qing-Zhu/0000-0002-4445-5096; Davis, Andrew/0000-0001-7955-6236 FU NASA [NNX07AI81G, NNG05GG48G, NAG5-10523, NAG5-11591]; Department of Energy by LLNL [W-7405-ENG-48]; NSF Instrumentation and Facilities FX We thank Alan Boss, Marc Chaussidon, Gregory Herzog and anonymous reviewer for critical comments and suggestions which helped to improve the manuscript. This work was supported by NASA Grants NNX07AI81G (A.N. Krot, PI), NNG05GG48G (G.R. Huss, PI), NAG5-10523 (I.D. Hutcheon, PI), and NAG5-11591 (K. Keil, PI), and was performed under the auspices of the Department of Energy by LLNL under Contract W-7405-ENG-48. The UCLA ion microprobe laboratory is partially supported by a grant from the NSF Instrumentation and Facilities program. This is Hawai'i Institute of Geophysics and Planetology publication 1796 and School of Ocean and Earth Science and Technology publication 7726. NR 247 TC 89 Z9 91 U1 9 U2 50 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 SEP 1 PY 2009 VL 73 IS 17 BP 4963 EP 4997 DI 10.1016/j.gca.2008.09.039 PG 35 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 484LX UT WOS:000269047700004 ER PT J AU Nyquist, LE Kleine, T Shih, CY Reese, YD AF Nyquist, L. E. Kleine, T. Shih, C. -Y. Reese, Y. D. TI The distribution of short-lived radioisotopes in the early solar system and the chronology of asteroid accretion, differentiation, and secondary mineralization SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Article ID EQUILIBRATED ORDINARY CHONDRITES; CHROMIUM ISOTOPE SYSTEMATICS; ANGRITE PARENT BODY; U-PB SYSTEMATICS; MN-53-CR-53 SYSTEMATICS; CORE FORMATION; HALF-LIFE; FERROMAGNESIAN CHONDRULES; CARBONACEOUS CHONDRITES; INITIAL AL-26/AL-27 AB We evaluate initial ((26)Al/(27)Al)(0), ((53)Mn/(55)Mn)(0), and ((182)Hf/(180)Hf)(I), ratios, together with (207)Pb/(206)Pb ages for igneous differentiated meteorites and chondrulles from ordinary chondrites for consistency with radioactive decay of the parent nuclides within a common, closed isotopic system, i.e., the early solar nebula. The relative initial isotopic abundances of (26)Al, (53)Mn, and (182)Hf in differentiated meteorites and chondrules are consistent with decay from common solar system initial values, here denoted by I(Al)(SS), I(Mn)(SS), and I(Hf)(SS), respectively. I(Mn)(SS) and I(Hf)(SS) = 9.1 +/- 1.7 x 10(-6) and 1.07 +/- 0.08 x 10(-4), respectively, correspond to "canonical" I(Al)(SS) = 5.1 x 10(-5). I(Hf)(SS) so determined is consistent with I(Hf)(SS) = 9.72 +/- 0.44 x 10(-5) directly determined from an internal Hf-W isochron for CAI minerals. I(Mn)(SS) is within error of the lowest value directly measured for CAIs. We suggest that erratically higher values measured for CAIs in carbonaceous chondrites may reflect proton irradiation of unaccreted CAIs by the early Sun after other asteroids destined for melting by (26)Al decay had already accreted. The (53)Mn incorporated within such asteroids would have been shielded from further "local" spallogenic contributions from within the solar system. The relative initial isotopic abundances of the short-lived nuclides are less consistent with the (207)Pb/(206)Pb ages of the corresponding materials than with one another. The best consistency of short- and long-lived chronometers is obtained for ((182)Hf/(180)Hf)(I), and the (201)Pb/(206)Pb ages of angrites. ((182)Hf/(180)Hf)(I), decreases with decreasing (207)Pb/(206)Pb ages at the rate expected from the 8.90 +/- 0.09 Ma half-life of (182)Hf. The model solar system age thus determined is T(SS,Hf-W) = 4568.3 +/- 0.7 Ma. ((26)Al/(27)Al)(I) and ((53)Mn/(55)Mn)(I) are less consistent with (207)Pb/(206)Pb ages of the corresponding meteorites, but yield T(SS,Mn-Cr) = 4568.2 +/- 0.5 Ma relative to I(Al)(SS) = 5.1 x 10(-5) and a (207)Pb/(206)Pb age of 4558.55 +/- 0.15 Ma for the LEW86010 angrite. The Mn-Cr method with I(Mn)(SS) = 9.1 +/- 1.7 x 10(-6) is useful for dating accretion (if identified with chondrule formation), primary igneous events, and secondary mineralization on asteroid parent bodies. All of these events appear to have occurred approximately contemporaneously on different asteroid parent bodies. For I(Mn)(SS) = 9.1 +/- 1.7 x 10(-6), parent body differentiation is found to extend at least to similar to 5 Ma post-T(SS), i.e., until differentiation of the angrite parent body similar to 4563.5 Ma ago, or similar to 4564.5 Ma ago using the directly measured (201)Pb/(206)Pb ages of the D'Orbigny-clan angrites. The similar to 1 Ma difference is characteristic of a remaining inconsistency for the D'Orbigny-clan between the Al-Mg and Mn-Cr chronometers on one hand, and the (207)Pb/(206)Pb chronometer on the other. Differentiatio of the IIIAB iron meteorite and ureilite parent bodies probably occurred slightly later than for the angrite parent body, and at nearly the same time as one another as shown by the Mn-Cr ages of IIIAB irons and ureilites, respectively. The latest recorded episodes of secondary mineralization are for carbonates on the CI carbonaceous chondrite parent body and fayalites on the CV carbonaceous chondrite parent body, both extending to similar to 10 Ma post-T(SS). Published by Elsevier Ltd. C1 [Nyquist, L. E.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Kleine, T.] ETH, Inst Isotope Geochem & Mineral Resources, CH-8092 Zurich, Switzerland. [Shih, C. -Y.] ESCG Jacobs Sverdrup, Houston, TX 77258 USA. [Reese, Y. D.] ESCG Muniz Engn, Houston, TX 77058 USA. RP Nyquist, LE (reprint author), NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. EM laurence.e.nyquist@nasa.gov FU NASA RTOP [344-31]; Swiss National Science foundation FX L.N. acknowledges the generosity of the organizing committee of the Workshop on the Chronology of Meteorites and the Early Solar System for inviting his participation in the workshop from which this paper results. Thanks are due especially to Sasha Krot for suggesting the topic to be reviewed, and to Ed Scott for hosting a delightful post-conference field trip to the Kilauea volcano. Noriko Kita provided ureilite data for the conference abstract and also for this paper, and encouragement for the writing of both. Comments by I. Leya and an anonymous reviewer as well as discussions with D. Papanastassiou were very helpful. Associate Editor G. Herzog's oversight and attention to detail hopefully has resulted in clearer discussion of the ideas presented here. I. Leya's sharing of the results of unpublished calculations for proton irradiation models (not presented here) is especially appreciated. Financial support was provided by NASA RTOP 344-31 and the Swiss National Science foundation. NR 86 TC 69 Z9 73 U1 3 U2 29 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 SEP 1 PY 2009 VL 73 IS 17 BP 5115 EP 5136 DI 10.1016/j.gca.2008.12.031 PG 22 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 484LX UT WOS:000269047700010 ER PT J AU Amelin, Y Connelly, J Zartman, RE Chen, JH Gopel, C Neymark, LA AF Amelin, Y. Connelly, J. Zartman, R. E. Chen, J. H. Goepel, C. Neymark, L. A. TI Modern U-Pb chronometry of meteorites: Advancing to higher time resolution reveals new problems SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Article ID EARLY SOLAR-SYSTEM; MN-53-CR-53 SYSTEMATICS; CARBONACEOUS CHONDRITE; COOLING HISTORY; CORE FORMATION; PARENT BODY; AGE; ACCRETION; ALLENDE; LEAD AB In this paper, we evaluate the factors that influence the accuracy of lead (Pb)-isotopic ages of meteorites, and may possibly be responsible for inconsistencies between Pb-isotopic and extinct nuclide timescales of the early Solar System: instrumental mass fractionation and other possible analytical sources of error, presence of more than one component of non-radiogenic Pb, migration of ancient radiogenic Pb by diffusion and other mechanisms, possible heterogeneity of the isotopic composition of uranium (U), uncertainties in the decay constants of uranium isotopes, possible presence of "freshly synthesized" actinides with short half-life (e.g. (234)U) in the early Solar System, possible initial disequilibrium in the uranium decay chains, and potential fractionation of radiogenic Pb isotopes and U isotopes caused by alpha-recoil and subsequent laboratory treatment. We review the use of (232)Th/(238)U values to assist in making accurate interpretations of the U-Pb ages of meteorite components. We discuss recently published U-Pb dates of calcium-aluminum-rich inclusions (CAIs), and their apparent disagreement with the extinct nuclide dates, in the context of capability and common pitfalls in modern meteorite chronology. Finally, we discuss the requirements of meteorites that are intended to be used as the reference points in building a consistent time scale of the early Solar System, based on the combined use of the U-Pb system and extinct nuclide chronometers. (C) 2009 Elsevier Ltd. All rights reserved. C1 [Amelin, Y.] Australian Natl Univ, Planetary Sci Inst, Canberra, ACT 0200, Australia. [Amelin, Y.] Australian Natl Univ, Res Sch Earth Sci, Canberra, ACT 0200, Australia. [Connelly, J.] Univ Texas Austin, Jackson Sch Geosci, Austin, TX 78712 USA. [Connelly, J.] Geol Museum, Copenhagen, Denmark. [Zartman, R. E.] MIT, EAPS, Cambridge, MA 02139 USA. [Chen, J. H.] CALTECH, Jet Prop Lab, Div Sci, Pasadena, CA 91109 USA. [Goepel, C.] IPGP, Lab Geochim & Cosmochim, F-75252 Paris 05, France. [Neymark, L. A.] US Geol Survey, Denver, CO 80225 USA. RP Amelin, Y (reprint author), Australian Natl Univ, Planetary Sci Inst, GPO Box 4, Canberra, ACT 0200, Australia. EM yuri.amelin@anu.edu.au; connelly@mail.utexas.edu; rzartman@mit.edu; James.H.Chen@jpl.nasa.gov; gopel@ipgp.jussieu.fr; lneymark@usgs.gov RI Connelly, James /O-7996-2015 NR 65 TC 26 Z9 29 U1 1 U2 12 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 SEP 1 PY 2009 VL 73 IS 17 BP 5212 EP 5223 DI 10.1016/j.gca.2009.01.040 PG 12 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 484LX UT WOS:000269047700015 ER PT J AU Witte, JC Schoeberl, MR Douglass, AR Gleason, JF Krotkov, NA Gille, JC Pickering, KE Livesey, N AF Witte, J. C. Schoeberl, M. R. Douglass, A. R. Gleason, J. F. Krotkov, N. A. Gille, J. C. Pickering, K. E. Livesey, N. TI Satellite observations of changes in air quality during the 2008 Beijing Olympics and Paralympics SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID INSTRUMENT; ALGORITHM; RETRIEVAL; CHINA AB For the August-September 2008 Olympic and the Paralympic Games held in Beijing, China, strict controls on pollutant emissions and motor vehicle traffic were imposed on Beijing and neighboring provinces to the South to improve the air quality in and around the city. Satellite measurements over Beijing between July and September showed 43% reductions of tropospheric column nitrogen dioxide, compared to the past three years. When neighboring provinces to the south are included in our analyses, satellite measurements show boundary layer sulfur dioxide reductions of 13% and carbon monoxide reductions of 12% at 700 hPa. Thus, based on satellites observations alone, noticeable reductions in these pollutant tracers were measured during both games. Citation: Witte, J. C., M. R. Schoeberl, A. R. Douglass, J. F. Gleason, N. A. Krotkov, J. C. Gille, K. E. Pickering, and N. Livesey (2009), Satellite observations of changes in air quality during the 2008 Beijing Olympics and Paralympics, Geophys. Res. Lett., 36, L17803, doi:10.1029/2009GL039236. C1 [Witte, J. C.] Sci Syst & Applicat Inc, Lanham, MD 20703 USA. [Schoeberl, M. R.; Douglass, A. R.; Gleason, J. F.; Pickering, K. E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Krotkov, N. A.] Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Catonsville, MD 21228 USA. [Gille, J. C.] Natl Ctr Atmospher Res, Boulder, CO 80307 USA. [Livesey, N.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Witte, JC (reprint author), Sci Syst & Applicat Inc, 10210 Greenbelt Rd,Suite 600, Lanham, MD 20703 USA. EM witte@gavial.gsfc.nasa.gov RI Gleason, James/E-1421-2012; Douglass, Anne/D-4655-2012; Pickering, Kenneth/E-6274-2012; Krotkov, Nickolay/E-1541-2012 OI Krotkov, Nickolay/0000-0001-6170-6750 FU NASA FX This work is supported by NASA's Atmospheric Chemistry, Modeling and Analysis and Applied Sciences Air Quality Programs. Work performed at the Jet Propulsion Laboratory, California Institute of Technology was under contract to the National Aeronautics and Space Administration. The OMI instrument is managed by The Netherlands Agency for Aerospace Programs and Royal Netherlands Meteorological Institute. We wish to thank Matthew Beckley for graphics assistance on Figure 1. NR 17 TC 61 Z9 67 U1 1 U2 25 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 SEP 1 PY 2009 VL 36 AR L17803 DI 10.1029/2009GL039236 PG 6 WC Geosciences, Multidisciplinary SC Geology GA 492CX UT WOS:000269633100003 ER PT J AU Fast, KE Kostiuk, T Lefevre, F Hewagama, T Livengood, TA Delgado, JD Annen, J Sonnabend, G AF Fast, Kelly E. Kostiuk, Theodor Lefevre, Franck Hewagama, Tilak Livengood, Timothy A. Delgado, Juan D. Annen, John Sonnabend, Guido TI Comparison of HIPWAC and Mars Express SPICAM observations of ozone on Mars 2006-2008 and variation from 1993 IRHS observations SO ICARUS LA English DT Article DE Mars, Atmosphere; Infrared observations; Photochemistry; Spectroscopy; Abundances, Atmospheres ID WATER-VAPOR; ATMOSPHERE; SPECTRA; ABUNDANCE; CHEMISTRY; APHELION; ORBITER; DAYGLOW; SPACE AB Ozone is a tracer of photochemistry in the atmosphere of Mars and an observable used to test predictions of photochemical models. We present a comparison of retrieved ozone abundances on Mars using ground-based infrared heterodyne measurements by NASA Goddard Space Flight Center's Heterodyne Instrument for Planetary Wind And Composition (HIPWAC) and space-based Mars Express Spectroscopy for the Investigation of the Characteristics of the Atmosphere of Mars (SPICAM) ultraviolet measurements. Ozone retrievals from simultaneous measurements in February 2008 were very consistent (0.8 mu m-atm), as were measurements made close in time (ranging from <1 to >8 mu m-atm) during this period and during opportunities in October 2006 and February 2007. The consistency of retrievals from the two different observational techniques supports combining the measurements for testing photochemistry-coupled general circulation models and for investigating variability over the long-term between spacecraft missions. Quantitative comparison with ground-based measurements by NASA/GSFC's Infrared Heterodyne Spectrometer (IRHS) in 1993 reveals 2-4 times more ozone at low latitudes than in 2008 at the same season, and such variability was not evident over the shorter period of the Mars Express mission. This variability may be due to cloud activity. Published by Elsevier Inc. C1 [Fast, Kelly E.; Kostiuk, Theodor; Annen, John] NASA, Goddard Space Flight Ctr, Planetary Syst Lab, Greenbelt, MD 20771 USA. [Lefevre, Franck] Univ Paris 06, CNRS, LATMOS, F-75005 Paris, France. [Hewagama, Tilak; Livengood, Timothy A.; Delgado, Juan D.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Sonnabend, Guido] Univ Cologne, LPhys Inst, D-50937 Cologne, Germany. RP Fast, KE (reprint author), NASA, Goddard Space Flight Ctr, Planetary Syst Lab, Code 693, Greenbelt, MD 20771 USA. EM Kelly.E.Fast@nasa.gov RI Hewagama, T/C-8488-2012; Livengood, Timothy/C-8512-2012; Kostiuk, Theodor/A-3077-2014 FU NASA FX The authors thank Dr. Alan Tokunaga and the staff of the NASA Infrared Telescope Facility for their support of HIPWAC observations of Mars, and Dr. Michael D. Smith for informative discussion. This work was supported by the NASA Planetary Astronomy Program. NR 30 TC 6 Z9 6 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 SEP PY 2009 VL 203 IS 1 BP 20 EP 27 DI 10.1016/j.icarus.2009.05.005 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 599HV UT WOS:000277902900003 ER PT J AU Stepinski, TF Mendenhall, MP Bue, BD AF Stepinski, Tomasz F. Mendenhall, Michael P. Bue, Brian D. TI Machine cataloging of impact craters on Mars SO ICARUS LA English DT Article DE Cratering; Mars, Surface ID ORBITER LASER ALTIMETER; AUTOMATIC RECOGNITION; SUBSURFACE VOLATILES; CHRONOLOGY; SURFACE; DISTRIBUTIONS; REGIONS AB This study presents an automated system for cataloging impact craters using the MOLA 128 pixels/degree digital elevation model of Mars. Craters are detected by a two-step algorithm that first identifies round and symmetric topographic depressions as crater candidates and then selects craters using a machine-learning technique. The system is robust with respect to surface types; craters are identified with similar accuracy from all different types of martian surfaces without adjusting input parameters. By using a large training set in its final selection step, the system produces virtually no false detections. Finally, the system provides a seamless integration of crater detection with its characterization. Of particular interest is the ability of our algorithm to calculate crater depths. The system is described and its application is demonstrated on eight large sites representing all major types of martian surfaces. An evaluation of its performance and prospects for its utilization for global surveys are given by means of detailed comparison of obtained results to the manually-derived Catalog of Large Martian Impact Craters. We use the results from the test sites to construct local depth-diameter relationships based on a large number of craters. In general, obtained relationships are in agreement with what was inferred on the basis of manual measurements. However, we have found that, in Terra Cimmeria, the depth/diameter ratio has an abrupt decrease at similar to 38 degrees S regardless of crater size. If shallowing of craters is attributed to presence of sub-surface ice, a sudden change in its spatial distribution is suggested by our findings. (C) 2009 Elsevier Inc. All rights reserved. C1 [Stepinski, Tomasz F.] Lunar & Planetary Inst, Houston, TX 77058 USA. [Mendenhall, Michael P.] CALTECH, Dept Phys, Pasadena, CA 91125 USA. [Bue, Brian D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Stepinski, TF (reprint author), Lunar & Planetary Inst, 3600 Bay Area Blvd, Houston, TX 77058 USA. EM tom@lpi.usra.edu FU National Science Foundation [IIS-0430208]; NASA [NNG06GE57G, CAN-NCC5-679] FX This work was supported by National Science Foundation under Grant IIS-0430208 and by NASA under Grant NNG06GE57G. The presented research was conducted at the Lunar and Planetary Institute, which is operated by the USRA under Contract CAN-NCC5-679 with NASA, This is LPI Contribution No. 1345. NR 50 TC 28 Z9 28 U1 0 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 SEP PY 2009 VL 203 IS 1 BP 77 EP 87 DI 10.1016/j.icarus.2009.04.026 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 599HV UT WOS:000277902900010 ER PT J AU Guerlet, S Fouchet, T Bezard, B Simon-Miller, AA Flasar, FM AF Guerlet, Sandrine Fouchet, Thierry Bezard, Bruno Simon-Miller, Amy A. Flasar, F. Michael TI Vertical and meridional distribution of ethane, acetylene and propane in Saturn's stratosphere from CIRS/Cassini limb observations SO ICARUS LA English DT Article DE Saturn; Infrared observations; Atmospheres; Composition ID ROTOTRANSLATIONAL ABSORPTION-SPECTRA; ISO-SWS OBSERVATIONS; TEMPERATURE STRUCTURE; THERMAL STRUCTURE; OUTER PLANETS; ATMOSPHERE; C2H6; PHOTOCHEMISTRY; PAIRS; CASSINI/CIRS AB Measuring the spatial distribution of chemical compounds in Saturn's stratosphere is critical to better understand the planet's photochemistry and dynamics. Here we present an analysis of infrared spectra in the range 600-1400 cm(-1) acquired in limb geometry by the Cassini spacecraft between March 2005 and January 2008. We first determine the vertical temperature profiles from 3 to 0.01 hPa, at latitudes ranging from 70 degrees N to 80 degrees S. We infer a similar meridional temperature gradient at 1-2 hPa as in recent previous studies [Fletcher, L.N., Irwin, P.G.J., Teanby, N.A., Orton, CS., Parrish, P.D., de Kok, R., Howett, C., Calcutt, S.B., Bowles, N., Taylor, F.W., 2007. Icarus 189, 457-478: Howett, C.J.A., Irwin, P.G.J., Teanby, N.A., Simon-Miller, A., Calcutt, S.B., Fletcher, L.N., de Kok, R., 2007. Icarus 190, 556-572]. We then retrieve the vertical profiles of C2H6 and C2H2 from 3 to 0.01 hPa and of C3H8 around 1 hPa. At 1 hPa, the meridional variation of C2H2 is found to follow the yearly averaged solar insolation, except for a strong equatorial mole fraction of 8 x 10(-7), nearly two times higher than expected. This enhancement in abundance can be explained by the descent of hydrocarbon-rich air, with a vertical wind speed at the equator of 0.25 +/- 0.1 mm/s at 1 hPa and 0.4 +/- 0.15 mm/s at 0.1 hPa. The ethane distribution is relatively uniform at 1 hPa, with only a moderate 25% increase from 35 degrees S to 80 degrees S. Propane is found to increase from north to south by a factor of 1.9, suggesting that its lifetime may be shorter than Saturn's year at 1 hPa. At high altitudes (1 Pa), C2H2 and C2H6 abundances depart significantly from the photochemical model predictions of Moses and Greathouse [Moses, J.I., Greathouse, T.K., 2005. J. Geophys. Res. 110, 9007], except at high southern latitudes (62, 70 and 80 degrees S) and near the equator. The observed abundances are found strongly depleted in the 20-40 degrees S region and enhanced in the 20-30 degrees N region, the latter coinciding with the ring's shadow. We favor a dynamical explanation for these anomalies. (C) 2009 Elsevier Inc. All rights reserved. C1 [Guerlet, Sandrine; Fouchet, Thierry; Bezard, Bruno] Observ Paris, LESIA, F-92195 Meudon, France. [Simon-Miller, Amy A.; Flasar, F. Michael] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Guerlet, S (reprint author), Observ Paris, LESIA, F-92195 Meudon, France. EM Sandrine.Guerlet@obspm.fr RI Flasar, F Michael/C-8509-2012; Simon, Amy/C-8020-2012; Fouchet, Thierry/C-6374-2017 OI Simon, Amy/0000-0003-4641-6186; Fouchet, Thierry/0000-0001-9040-8285 FU Centre National d'Etudes Spatiales (CNES); Programme National de Planetologie (PNP/INSU) FX We would like to thank the many people in the CIRS investigation team involved in planning the observational sequences and calibration of the data. We also thank Julianne Moses for providing model outputs for comparison to our results. This research was supported by the Centre National d'Etudes Spatiales (CNES) and the Programme National de Planetologie (PNP/INSU). NR 49 TC 33 Z9 33 U1 0 U2 1 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD SEP PY 2009 VL 203 IS 1 BP 214 EP 232 DI 10.1016/j.icarus.2009.04.002 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 599HV UT WOS:000277902900022 ER PT J AU Roman, MT West, RA Banfield, DJ Gierasch, PJ Achterberg, RK Nixon, CA Thomas, PC AF Roman, Michael T. West, Robert A. Banfield, Donald J. Gierasch, Peter J. Achterberg, Richard K. Nixon, Conor A. Thomas, Peter C. TI Determining a tilt in Titan's north-south albedo asymmetry from Cassini images SO ICARUS LA English DT Article DE Titan; Atmospheres, dynamics; Atmospheres; structure ID COMPOSITE INFRARED SPECTROMETER; IMAGING SCIENCE; SATURN; TEMPERATURES; DYNAMICS; WINDS AB Analysis of Titan's hemispheric brightness asymmetry from mapped Cassini images reveals an axis of symmetry that is tilted with respect to the rotational axis of the solid body. Twenty images taken from 2004 through 2007 show a mean axial offset of 3.8 +/- 0.9 degrees relative to the solid body's pole, directed 79 +/- 24 degrees to the west of the sub-solar longitude. These values are consistent with recent measurements of an implied atmospheric spin axis determined from isothermal mapping by [Achterberg, R.K., Conrath, B.J., Gierasch, P.J., Flasar, F.M., Nixon, C.A., 2008. Icarus 197, 549-555]. (C) 2009 Elsevier Inc. All Fights reserved. C1 [Roman, Michael T.; Banfield, Donald J.; Gierasch, Peter J.; Thomas, Peter C.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. [West, Robert A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Achterberg, Richard K.; Nixon, Conor A.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. RP Roman, MT (reprint author), Cornell Univ, Dept Astron, 311 Spaces Sci Bldg, Ithaca, NY 14853 USA. EM mtroman@astro.cornell.edu RI Nixon, Conor/A-8531-2009; OI Nixon, Conor/0000-0001-9540-9121; Banfield, Don/0000-0003-2664-0164 FU NASA FX The authors acknowledge the support of the NASA Cassini project during the period in which this work was conducted. NR 14 TC 12 Z9 12 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 SEP PY 2009 VL 203 IS 1 BP 242 EP 249 DI 10.1016/j.icarus.2009.04.021 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 599HV UT WOS:000277902900025 ER PT J AU Loyola, DGR Hilsenrath, E Reid, JS Braathen, G AF Loyola, Diego G. R. Hilsenrath, Ernest Reid, Jeffrey S. Braathen, Geir TI Introduction to the Issue on Fostering Applications of Earth Observations of the Atmosphere SO IEEE JOURNAL OF SELECTED TOPICS IN APPLIED EARTH OBSERVATIONS AND REMOTE SENSING LA English DT Editorial Material C1 [Loyola, Diego G. R.] German Aerosp Ctr, Remote Sensing Technol Inst, D-82234 Oberpfaffenhofen, Wessling, Germany. [Hilsenrath, Ernest] NASA Headquarters, Div Earth Sci, Washington, DC 20546 USA. [Reid, Jeffrey S.] USN, Res Lab, Marine Meteorol Div, Monterey, CA 93943 USA. [Braathen, Geir] World Meteorol Org, Environm Div, CH-1211 Geneva 2, Switzerland. RP Loyola, DGR (reprint author), German Aerosp Ctr, Remote Sensing Technol Inst, D-82234 Oberpfaffenhofen, Wessling, Germany. EM diego.loyola@dlr.de; ernest.hilsenrath@nasa.gov; jeffrey.reid@nrlmry.navy.mil; gbraathen@wmo.int OI Loyola R., Diego G./0000-0002-8547-9350 NR 0 TC 0 Z9 0 U1 0 U2 4 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 1939-1404 J9 IEEE J-STARS JI IEEE J. Sel. Top. Appl. Earth Observ. Remote Sens. PD SEP PY 2009 VL 2 IS 3 BP 142 EP 143 DI 10.1109/JSTARS.2009.2035021 PG 2 WC Engineering, Electrical & Electronic; Geography, Physical; Remote Sensing; Imaging Science & Photographic Technology SC Engineering; Physical Geography; Remote Sensing; Imaging Science & Photographic Technology GA 515BN UT WOS:000271441400001 ER PT J AU Shu, YS Kyung, M Lee, WM Song, BS Pain, B AF Shu, Yun-Shiang Kyung, MoonJung Lee, Wei-Ming Song, Bang-Sup Pain, Bedabrata TI A 10 similar to 15-bit 60-MS/s Floating-Point ADC With Digital Gain and Offset Calibration SO IEEE JOURNAL OF SOLID-STATE CIRCUITS LA English DT Article DE Background calibration; chopping; digital calibration; floating-point ADC; gain and offset calibration; pseudo-random noise (PN) dithering; self-calibration; variable-gain amplifier ID A/D CONVERTER; BACKGROUND CALIBRATION; DYNAMIC-RANGE AB Floating-point analog-to-digital converter (FADC) utilizes an up-front variable-gain amplifier (VGA) to enhance its low-level resolution. Although it is a single-path system, varying gain by switching circuit elements in and out modulates the gain and offset as in the multi-path time-interleaved ADC. For high-speed operation at all gain settings, a constant-bandwidth switched-capacitor VGA is implemented with variable-bandwidth opamps, and its gain and offset are digitally calibrated in background using signal-dependent pseudo-random noise (PN) dithering and chopping techniques. A three-stage VGA adjusts its gain instantly from x 1 to x 32 depending on the sampled input level, and improves the INL of a 10-bit ADC from 24 to 0.9 least significant bits (LSBs) at a 15-bit level for the low-level input. The resulting 10 similar to 15-bit 60-MS/s ADC needs no input sample-and-hold (S/H) stage, and achieves a system noise of -80 dBFS with a gain set to x 32. A prototype chip in 0.18-mu m CMOS occupies an active area of 3.0 x 2.0 mm(2), and consumes 300 mW at 1.8 V including digital calibration logic. C1 [Shu, Yun-Shiang] Univ Calif San Diego, San Diego, CA 92103 USA. [Kyung, MoonJung; Lee, Wei-Ming; Song, Bang-Sup] Univ Calif San Diego, La Jolla, CA 92093 USA. [Pain, Bedabrata] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Shu, YS (reprint author), Ralink Technol Corp, Taipei, Taiwan. EM song@ece.ucsd.edu NR 18 TC 7 Z9 7 U1 0 U2 2 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 0018-9200 J9 IEEE J SOLID-ST CIRC JI IEEE J. Solid-State Circuit PD SEP PY 2009 VL 44 IS 9 BP 2356 EP 2365 DI 10.1109/JSSC.2009.2022993 PG 10 WC Engineering, Electrical & Electronic SC Engineering GA 489AC UT WOS:000269390700009 ER EF