FN Thomson Reuters Web of Science™ VR 1.0 PT J AU Stefanik, RP Torres, G Latham, DW Landsman, W Craig, N Murrett, J AF Stefanik, Robert P. Torres, Guillermo Latham, David W. Landsman, Wayne Craig, Nathaniel Murrett, James TI OBSERVATIONS AND ORBITAL ANALYSIS OF THE GIANT WHITE DWARF BINARY SYSTEM HR 5692 SO ASTRONOMICAL JOURNAL LA English DT Article DE binaries: general; methods: data analysis; stars: individual (HR 5692); techniques: spectroscopic; white dwarfs ID INTERMEDIATE ASTROMETRIC DATA; RADIAL-VELOCITIES; SPECTROSCOPIC BINARIES; BARIUM STARS; S STARS; MASS; CATALOG; EXTINCTION; ISOCHRONES; SIRIUS AB We report spectroscopic observations of the red giant star HR5692, previously known to be a binary system both from other spectroscopic work and from deviations in the astrometric motion detected by the Hipparcos satellite. Earlier International Ultraviolet Explorer (IUE) observations had shown the presence of a hot white dwarf companion to the giant primary. We have combined our radial velocity observations with other existing measurements and with the Hipparcos intermediate astrometric data to determine a complete astrometric-spectroscopic orbital solution, providing the inclination angle for the first time. We also determine an improved parallax for the system of 10.12 +/- 0.67 mas. We derive the physical properties of the primary, and with an estimate of its mass from stellar evolution models (1.84 +/- 0.40M(circle dot)), we infer the mass of the white dwarf companion to be M-WD = 0.59 +/- 0.12M(circle dot). An analysis of an IUE white dwarf spectrum, using our parallax, yields T-eff = 30,400 +/- 780 K, log g = 8.25 +/- 0.15, and a mass M-WD = 0.79 +/- 0.09M(circle dot), in marginal agreement with the dynamical mass. C1 [Stefanik, Robert P.; Torres, Guillermo; Latham, David W.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Landsman, Wayne] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Craig, Nathaniel; Murrett, James] Harvard Univ, Cambridge, MA 02138 USA. RP Stefanik, RP (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM rstefanik@cfa.harvard.edu FU NSF [AST-0708229, AST-1007992]; NASA [NAS5-26555]; NASA Office of Space Science [NNX09AF08G] FX We thank Michael Calkins, Joe Caruso, Gil Esquerdo, and Joe Zajac for obtaining many of the spectroscopic observations used here. We also thank I. Hubeny for his assistance with the TLUSTY code. G. T. acknowledges partial support for this work from NSF grants AST-0708229 and AST-1007992. This research has made use of the SIMBAD database and the VizieR catalog access tool, both operated at CDS, Strasbourg, France, of NASA's Astrophysics Data System Abstract Service, and of data products from the Two Micron All Sky Survey (2MASS), which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by NASA and the NSF. Some of the data presented in this paper were obtained from the Multimission Archive at the Space Telescope Science Institute (MAST). STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. Support for MAST for non-HST data is provided by the NASA Office of Space Science via grant NNX09AF08G and by other grants and contracts. NR 56 TC 4 Z9 4 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD MAY PY 2011 VL 141 IS 5 AR 144 DI 10.1088/0004-6256/141/5/144 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 746JB UT WOS:000289240800003 ER PT J AU Batista, V Gould, A Dieters, S Dong, S Bond, I Beaulieu, JP Maoz, D Monard, B Christie, GW McCormick, J Albrow, MD Horne, K Tsapras, Y Burgdorf, MJ Novati, SC Skottfelt, J Caldwell, J Kozlowski, S Kubas, D Gaudi, BS Han, C Bennett, DP An, J Abe, F Botzler, CS Douchin, D Freeman, M Fukui, A Furusawa, K Hearnshaw, JB Hosaka, S Itow, Y Kamiya, K Kilmartin, PM Korpela, A Lin, W Ling, CH Makita, S Masuda, K Matsubara, Y Miyake, N Muraki, Y Nagaya, M Nishimoto, K Ohnishi, K Okumura, T Perrott, YC Rattenbury, N Saito, T Sullivan, DJ Sumi, T Sweatman, WL Tristram, PJ Von Seggern, E Yock, PCM Brillant, S Calitz, JJ Cassan, A Cole, A Cook, K Coutures, C Prester, DD Donatowicz, J Greenhill, J Hoffman, M Jablonski, F Kane, SR Kains, N Marquette, JB Martin, R Martioli, E Meintjes, P Menzies, J Pedretti, E Pollard, K Sahu, KC Vinter, C Wambsganss, J Watson, R Williams, A Zub, M Allen, W Bolt, G Bos, M Depoy, DL Drummond, J Eastman, JD Gal-Yam, A Gorbikov, E Higgins, D Janczak, J Kaspi, S Lee, CU Mallia, F Maury, A Monard, LAG Moorhouse, D Morgan, N Natusch, T Ofek, EO Park, BG Pogge, RW Polishook, D Santallo, R Shporer, A Spector, O Thornley, G Yee, JC Bozza, V Browne, P Dominik, M Dreizler, S Finet, F Glitrup, M Grundahl, F Harpsoe, K Hessman, FV Hinse, TC Hundertmark, M Jorgensen, UG Liebig, C Maier, G Mancini, L Mathiasen, M Rahvar, S Ricci, D Scarpetta, G Southworth, J Surdej, J Zimmer, F Allan, A Bramich, DM Snodgrass, C Steele, IA Street, RA AF Batista, V. Gould, A. Dieters, S. Dong, S. Bond, I. Beaulieu, J. P. Maoz, D. Monard, B. Christie, G. W. McCormick, J. Albrow, M. D. Horne, K. Tsapras, Y. Burgdorf, M. J. Novati, S. Calchi Skottfelt, J. Caldwell, J. Kozlowski, S. Kubas, D. Gaudi, B. S. Han, C. Bennett, D. P. An, J. Abe, F. Botzler, C. S. Douchin, D. Freeman, M. Fukui, A. Furusawa, K. Hearnshaw, J. B. Hosaka, S. Itow, Y. Kamiya, K. Kilmartin, P. M. Korpela, A. Lin, W. Ling, C. H. Makita, S. Masuda, K. Matsubara, Y. Miyake, N. Muraki, Y. Nagaya, M. Nishimoto, K. Ohnishi, K. Okumura, T. Perrott, Y. C. Rattenbury, N. Saito, To. Sullivan, D. J. Sumi, T. Sweatman, W. L. Tristram, P. J. Von Seggern, E. Yock, P. C. M. Brillant, S. Calitz, J. J. Cassan, A. Cole, A. Cook, K. Coutures, C. Prester, D. Dominis Donatowicz, J. Greenhill, J. Hoffman, M. Jablonski, F. Kane, S. R. Kains, N. Marquette, J. -B. Martin, R. Martioli, E. Meintjes, P. Menzies, J. Pedretti, E. Pollard, K. Sahu, K. C. Vinter, C. Wambsganss, J. Watson, R. Williams, A. Zub, M. Allen, W. Bolt, G. Bos, M. Depoy, D. L. Drummond, J. Eastman, J. D. Gal-Yam, A. Gorbikov, E. Higgins, D. Janczak, J. Kaspi, S. Lee, C. -U. Mallia, F. Maury, A. Monard, L. A. G. Moorhouse, D. Morgan, N. Natusch, T. Ofek, E. O. Park, B. -G. Pogge, R. W. Polishook, D. Santallo, R. Shporer, A. Spector, O. Thornley, G. Yee, J. C. Bozza, V. Browne, P. Dominik, M. Dreizler, S. Finet, F. Glitrup, M. Grundahl, F. Harpsoe, K. Hessman, F. V. Hinse, T. C. Hundertmark, M. Jorgensen, U. G. Liebig, C. Maier, G. Mancini, L. Mathiasen, M. Rahvar, S. Ricci, D. Scarpetta, G. Southworth, J. Surdej, J. Zimmer, F. Allan, A. Bramich, D. M. Snodgrass, C. Steele, I. A. Street, R. A. CA MOA Collaboration PLANET Collaboration FUN Collaboration MiNDSTEp Consortium RoboNet Collaboration TI MOA-2009-BLG-387Lb: a massive planet orbiting an M dwarf SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE gravitational lensing: micro; methods: data analysis; planets and satellites: detection; methods: numerical; instrumentation: adaptive optics; instrumentation: photometers ID GALACTIC BULGE; MICROLENSING EVENT; JUPITER/SATURN ANALOG; GIANT PLANETS; SNOW LINE; STARS; MASSES; PHOTOMETRY; COOL; LUMINOSITY AB Aims. We report the discovery of a planet with a high planet-to-star mass ratio in the microlensing event MOA-2009-BLG-387, which exhibited pronounced deviations over a 12-day interval, one of the longest for any planetary event. The host is an M dwarf, with a mass in the range 0.07 M-circle dot < M-host < 0.49 M-circle dot at 90% confidence. The planet-star mass ratio q = 0.0132 +/- 0.003 has been measured extremely well, so at the best-estimated host mass, the planet mass is m(p) = 2.6 Jupiter masses for the median host mass, M = 0.19 M-circle dot. Methods. The host mass is determined from two "higher order" microlensing parameters. One of these, the angular Einstein radius theta(E) = 0.31 +/- 0.03 mas has been accurately measured, but the other (the microlens parallax pi(E), which is due to the Earth's orbital motion) is highly degenerate with the orbital motion of the planet. We statistically resolve the degeneracy between Earth and planet orbital effects by imposing priors from a Galactic model that specifies the positions and velocities of lenses and sources and a Kepler model of orbits. Results. The 90% confidence intervals for the distance, semi-major axis, and period of the planet are 3.5 kpc < D-L < 7.9 kpc, 1.1 AU < a < 2.7 AU, and 3.8 yr < P < 7.6 yr, respectively. C1 [Batista, V.; Dieters, S.; Beaulieu, J. P.; Albrow, M. D.; Horne, K.; Tsapras, Y.; Caldwell, J.; Kubas, D.; Bennett, D. P.; Bramich, D. M.] Probing Lensing Anomalies NETwork PLANET, Chicago, IL USA. [Dieters, S.; Beaulieu, J. P.; Kubas, D.; Cassan, A.; Marquette, J. -B.] Univ Paris 06, Inst Astrophys Paris, CNRS UMR7095, F-75014 Paris, France. [Gould, A.; Dong, S.; Maoz, D.; Monard, B.; Christie, G. W.; McCormick, J.; Gaudi, B. S.; Han, C.] Microlensing Follow Network FUN, New York, NY USA. [Gould, A.; Kozlowski, S.; Gaudi, B. S.; Eastman, J. D.; Janczak, J.; Morgan, N.; Pogge, R. W.; Yee, J. C.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Dong, S.] Inst Adv Study, Princeton, NJ 08540 USA. [Bond, I.; Bennett, D. P.] MOA, Notre Dame, IN USA. [Bond, I.; Lin, W.; Ling, C. H.; Sweatman, W. L.] Massey Univ, Inst Informat & Math Sci, N Shore Mail Ctr, Auckland, New Zealand. [Maoz, D.; Gorbikov, E.; Kaspi, S.; Polishook, D.; Shporer, A.; Spector, O.] Tel Aviv Univ, Sch Phys & Astron, IL-69978 Tel Aviv, Israel. [Maoz, D.; Gorbikov, E.; Kaspi, S.; Polishook, D.; Shporer, A.; Spector, O.] Tel Aviv Univ, Wise Observ, IL-69978 Tel Aviv, Israel. [Monard, B.; Monard, L. A. G.] Ctr Backyard Astrophys, Bronberg Observ, Pretoria, South Africa. [Christie, G. W.] Auckland Observ, Auckland, New Zealand. [McCormick, J.] Ctr Backyard Astrophys, Farm Cove Observ, Auckland, New Zealand. [Albrow, M. D.; Hearnshaw, J. B.; Pollard, K.] Univ Canterbury, Dept Phys & Astron, Christchurch 8020, New Zealand. [Horne, K.; Tsapras, Y.; Rattenbury, N.; Kains, N.] RoboNet Collaborat, Chicago, IL USA. [Horne, K.; Kains, N.; Pedretti, E.; Browne, P.; Dominik, M.; Liebig, C.] Univ St Andrews, SUPA Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland. [Burgdorf, M. J.; Novati, S. Calchi; Skottfelt, J.; Wambsganss, J.; Snodgrass, C.] Microlensing Network Detect Small Terr Exoplanets, Les Ulis, France. [Skottfelt, J.; Vinter, C.; Harpsoe, K.; Hinse, T. C.; Jorgensen, U. G.; Mathiasen, M.; Zimmer, F.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen O, Denmark. [Jorgensen, U. G.] Univ Copenhagen, Ctr Star & Planet Format, DK-1350 Copenhagen O, Denmark. [Caldwell, J.] McDonald Observ, Ft Davis, TX 79734 USA. [Kubas, D.; Brillant, S.; Snodgrass, C.] European So Observ, Santiago 19, Chile. [Han, C.] Chungbuk Natl Univ, Dept Phys, Inst Basic Sci Res, Chonju 361763, South Korea. [Bennett, D. P.] Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA. [Abe, F.; Fukui, A.; Furusawa, K.; Hosaka, S.; Itow, Y.; Kamiya, K.; Makita, S.; Masuda, K.; Matsubara, Y.; Miyake, N.; Nagaya, M.; Nishimoto, K.; Okumura, T.; Sumi, T.] Nagoya Univ, Solar Terr Environm Lab, Nagoya, Aichi 4648601, Japan. [Botzler, C. S.; Douchin, D.; Freeman, M.; Perrott, Y. C.; Rattenbury, N.; Von Seggern, E.; Yock, P. C. M.] Univ Auckland, Dept Phys, Auckland, New Zealand. [Kilmartin, P. M.; Tristram, P. J.] Mt John Observ, Lake Tekapo 8780, New Zealand. [Korpela, A.; Sullivan, D. J.] Victoria Univ, Sch Chem & Phys Sci, Wellington, New Zealand. [Muraki, Y.] Konan Univ, Dept Phys, Kobe, Hyogo 6588501, Japan. [Ohnishi, K.] Nagano Natl Coll Technol, Nagano 3818550, Japan. [Saito, To.] Tokyo Metropolitan Coll Ind Technol, Tokyo 1168523, Japan. [Calitz, J. J.; Hoffman, M.; Meintjes, P.] Univ Free State, Fac Nat & Agr Sci, Dept Phys, ZA-9300 Bloemfontein, South Africa. [Cole, A.; Greenhill, J.; Watson, R.] Univ Tasmania, Sch Math & Phys, Hobart, Tas 7001, Australia. [Cook, K.] Lawrence Livermore Natl Lab, Inst Geophys & Planetary Phys, Livermore, CA 94551 USA. [Coutures, C.] CEA Saclay, F-91191 Gif Sur Yvette, France. [Prester, D. Dominis] Univ Rijeka, Dept Phys, Rijeka 51000, Croatia. [Donatowicz, J.] Vienna Univ Technol, A-1040 Vienna, Austria. Univ Toulouse, CNRS, LATT, Toulouse, France. [Jablonski, F.; Martioli, E.] Inst Nacl Pesquisas Espaciais, BR-12201 Sao Jose Dos Campos, SP, Brazil. [Kane, S. R.] CALTECH, NASA Exoplanet Sci Inst, Pasadena, CA 91125 USA. [Martin, R.; Williams, A.] Perth Observ, Perth, WA 6076, Australia. [Menzies, J.] S African Astron Observ, ZA-7935 Observatory, South Africa. [Sahu, K. C.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Wambsganss, J.; Zub, M.; Liebig, C.; Maier, G.; Zimmer, F.] Heidelberg Univ, Astron Rechen Inst, Zentrum Astron, D-69120 Heidelberg, Germany. [Zub, M.] Univ Zielona Gora, Inst Astron, PL-65265 Zielona Gora, Poland. [Allen, W.] Vintage Lane Observ, Blenheim, New Zealand. [Bos, M.] Molehill Astron Observ, Auckland, New Zealand. [Depoy, D. L.] Texas A&M Univ, Dept Phys & Astron, College Stn, TX USA. [Drummond, J.] Possum Observ, Patutahi, New Zealand. [Gal-Yam, A.] Weizmann Inst Sci, Dept Particle Phys & Astrophys, IL-76100 Rehovot, Israel. [Higgins, D.] Hunters Hill Observ, Canberra, ACT, Australia. [Gorbikov, E.; Kaspi, S.] Technion Israel Inst Technol, Dept Phys, IL-32000 Haifa, Israel. [Lee, C. -U.; Park, B. -G.] Korea Astron & Space Sci Inst, Taejon 305348, South Korea. [Mallia, F.; Maury, A.] Campo Catino Austral Observ, San Pedro De Atacama, Chile. [Moorhouse, D.; Thornley, G.] Kumeu Observ, Kumeu, New Zealand. [Natusch, T.] AUT Univ, Auckland, New Zealand. [Ofek, E. O.] Palomar Observ, San Diego, CA USA. [Santallo, R.] So Stars Observ, Faaa, Tahiti, Fr Polynesia. [Allan, A.] Univ Exeter, Sch Phys, Exeter EX4 4QL, Devon, England. [Steele, I. A.] Liverpool John Moores Univ, Astrophys Res Inst, Liverpool CH41 1LD, Merseyside, England. [Kains, N.; Bramich, D. M.] European So Observ, D-85748 Garching, Germany. [Burgdorf, M. J.] Univ Stuttgart, Deutsch SOFIA Inst, D-70569 Stuttgart, Germany. [Burgdorf, M. J.] NASA, Ames Res Ctr, SOFIA Sci Ctr, Moffett Field, CA 94035 USA. Univ Manchester, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England. [Snodgrass, C.] Max Planck Inst Solar Syst Res, D-37191 Katlenburg Lindau, Germany. [Tsapras, Y.] Univ London, Astron Unit, Sch Math Sci, London E1 4NS, England. [Tsapras, Y.; Street, R. A.] Las Cumbres Observ Global Telescope Network, Goleta, CA 93117 USA. [Street, R. A.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Novati, S. Calchi; Bozza, V.; Mancini, L.; Scarpetta, G.] Univ Salerno, Dipartimento Fis ER Caianiello, I-84085 Fisciano, SA, Italy. [Novati, S. Calchi; Bozza, V.; Mancini, L.; Scarpetta, G.] IIASS, I-84019 Vietri Sul Mare, SA, Italy. [Novati, S. Calchi; Bozza, V.; Scarpetta, G.] Ist Nazl Fis Nucl, Grp Collegato Salerno, Sez Napoli, Catania, Italy. [Dominik, M.] Royal Soc Univ, London, England. [Dreizler, S.; Hessman, F. V.; Hundertmark, M.] Univ Gottingen, Inst Astrophys, D-37077 Gottingen, Germany. [Finet, F.; Ricci, D.; Surdej, J.] Inst Astrophys & Geophys, B-4000 Liege, Belgium. [Glitrup, M.; Grundahl, F.] Aarhus Univ, Dept Phys & Astron, DK-8000 Aarhus C, Denmark. [Hinse, T. C.] Armagh Observ, Armagh BT61 9DG, North Ireland. [Rahvar, S.] Sharif Univ Technol, Dept Phys, Tehran 111559161, Iran. [Southworth, J.] Keele Univ, Astrophys Grp, Keele ST5 5BG, Staffs, England. [Rahvar, S.] IPM Inst Studies Theoret Phys & Math, Sch Astron, Tehran, Iran. [Mancini, L.] Univ Sannio, Dipartimento Ingn, I-82100 Benevento, Italy. [An, J.] Chinese Acad Sci, Natl Astron Observ, Beijing 100012, Peoples R China. [Williams, A.] Univ Western Australia, Sch Phys, Perth, WA 6009, Australia. RP Batista, V (reprint author), Probing Lensing Anomalies NETwork PLANET, Chicago, IL USA. EM batista@iap.fr; gould@astronomy.ohio-state.edu; dong@ias.edu; i.a.bond@massey.ac.nz; beaulieu@iap.fr; lagmonar@nmisa.org; gwchristie@christie.org.nz; farmcoveobs@xtra.co.nz; Michael.Albrow@canterbury.ac.nz; caldwell@astro.as.utexas.edu; simkoz@astronomy.ohio-state.edu; dkubas@eso.org; gaudi@astronomy.ohio-state.edu; cheongho@astroph.chungbuk.ac.kr; bennett@nd.edu; jinan@nao.cas.cn; abe@stelab.nagoya-u.ac.jp; c.botzler@auckland.ac.nz; afukui@stelab.nagoya-u.ac.jp; furusawa@stelab.nagoya-u.ac.jp; itow@stelab.nagoya-u.ac.jp; kkamiya@stelab.nagoya-u.ac.jp; a.korpela@niwa.co.nz; w.lin@massey.ac.nz; c.h.ling@massey.ac.nz; kmasuda@stelab.nagoya-u.ac.jp; ymatsu@stelab.nagoya-u.ac.jp; nmiyake@stelab.nagoya-u.ac.jp; mnagaya@stelab.nagoya-u.ac.jp; okumurat@stelab.nagoya-u.ac.jp; yper006@auckland.ac.nz; denis.sullivan@vuw.ac.nz; sumi@stelab.nagoya-u.ac.jp; w.sweatman@massey.ac.nz; p.yock@auckland.ac.nz; sbrillan@eso.org; cassan@iap.fr; Andrew.Cole@utas.edu.au; kcook@llnl.gov; coutures@iap.fr; donatowicz@tuwien.ac.at; John.Greenhill@utas.edu.au; HoffmaMJ.SCI@mail.uovs.ac.za; skane@ipac.caltech.edu; nk87@st-andrews.ac.uk; marquett@iap.fr; Ralph.Martin@dec.wa.gov.au; ep41@st-andrews.ac.uk; Andrew.Williams@dec.wa.gov.au; whallen@xtra.co.nz; gbolt@iinet.net.au; molehill@ihug.co.nz; depoy@physics.tamu.edu; john_drummond@xtra.co.nz; jdeast@astronomy.ohio-state.edu; avishay.gal-yam@weizmann.ac.il; dhi67540@bigpond.net.au; leecu@kasi.re.kr; francomallia@campocatinobservatory.org; alain@spaceobs.com; lagmonar@nmisa.org; acrux@orcon.net.nz; nick.morgan@alum.mit.edu; tim.natusch@aut.ac.nz; eran@astro.caltech.edu; bgpark@kasi.re.kr; pogge@astronomy.ohio-state.edu; obs930@southernstars-observatory.org; shporer@wise.tau; odedspec@wise.tau; guy.thornley@gmail.com; jyee@astronomy.ohio-state.edu RI Zimmer, Fabian/M-4765-2014; Hundertmark, Markus/C-6190-2015; Rahvar, Sohrab/A-9350-2008; Gaudi, Bernard/I-7732-2012; Dong, Subo/J-7319-2012; Kane, Stephen/B-4798-2013; Greenhill, John/C-8367-2013; Kozlowski, Szymon/G-4799-2013; 7, INCT/H-6207-2013; Astrofisica, Inct/H-9455-2013; Williams, Andrew/K-2931-2013 OI Cole, Andrew/0000-0003-0303-3855; Ricci, Davide/0000-0002-9790-0552; Snodgrass, Colin/0000-0001-9328-2905; Hundertmark, Markus/0000-0003-0961-5231; Rahvar, Sohrab/0000-0002-7084-5725; Eastman, Jason/0000-0003-3773-5142; Dominik, Martin/0000-0002-3202-0343; Kozlowski, Szymon/0000-0003-4084-880X; Williams, Andrew/0000-0001-9080-0105 FU HOLMES [ANR-06-BLAN-0416]; NSF [AST-0757888, AST-0206189, AST-0708890]; NASA [NNG04GL51G, NAF5-13042, NNX07AL71G]; Polish MNiSW [N20303032/4275, HST-GO-11311]; Korea Science and Engineering Foundation [2009-008561]; Korea Research Foundation [2006-311-C00072]; Korea Astronomy and Space Science Institute (KASI); Deutsche Forschungsgemeinschaft; PPARC/STFC; EU; Dill Faulkes Educational Trust (Faulkes Telescope North); Marsden Fund of NZ; Foundation for Research Science and Technology of NZ; Creative Research Initiative program [2009-008561]; Chinese Academy of Sciences (CAS) [2009Y2AJ7]; [JSPS18253002]; [JSPS20340052]; [JSPS19340058]; [MEXT19015005]; [JSPS18749004] FX V.B. thanks Ohio State University for its hospitality during a six week visit, during which this study was initiated. We acknowledge the following support: Grants HOLMES ANR-06-BLAN-0416 Dave Warren for the Mt Canopus Observatory; NSF AST-0757888 (AG, SD); NASA NNG04GL51G (DD, AG, RP); Polish MNiSW N20303032/4275 (AU); HST-GO-11311 (KS); NSF AST-0206189 and AST-0708890, NASA NAF5-13042 and NNX07AL71G (DPB); Korea Science and Engineering Foundation grant 2009-008561 (CH); Korea Research Foundation grant 2006-311-C00072 (B-GP); Korea Astronomy and Space Science Institute (KASI); Deutsche Forschungsgemeinschaft (CSB); PPARC/STFC, EU FP6 programme "ANGLES" (LW, NJR); PPARC/STFC (RoboNet); Dill Faulkes Educational Trust (Faulkes Telescope North); Grants JSPS18253002, JSPS20340052 and JSPS19340058 (MOA); Marsden Fund of NZ(IAB, PCMY); Foundation for Research Science and Technology of NZ; Creative Research Initiative program (2009-008561) (CH); Grants MEXT19015005 and JSPS18749004 (TS). Work by S. D. was performed under contract with the California Institute of Technology (Caltech) funded by NASA through the Sagan Fellowship Program. J.C.Y. is supported by an NSF Graduate Research Fellowship. This work was supported in part by an allocation of computing time from the Ohio Supercomputer Center. J.A. is supported by the Chinese Academy of Sciences (CAS) Fellowships for Young International Scientist, Grant No.: 2009Y2AJ7. NR 48 TC 41 Z9 41 U1 0 U2 8 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 MAY PY 2011 VL 529 AR A102 DI 10.1051/0004-6361/201016111 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 750OG UT WOS:000289557200110 ER PT J AU Berger, JP Monnier, JD Millan-Gabet, R Renard, S Pedretti, E Traub, W Bechet, C Benisty, M Carleton, N Haguenauer, P Kern, P Labeye, P Longa, F Lacasse, M Malbet, F Perraut, K Ragland, S Schloerb, P Schuller, PA Thiebaut, E AF Berger, J. -P. Monnier, J. D. Millan-Gabet, R. Renard, S. Pedretti, E. Traub, W. Bechet, C. Benisty, M. Carleton, N. Haguenauer, P. Kern, P. Labeye, P. Longa, F. Lacasse, M. Malbet, F. Perraut, K. Ragland, S. Schloerb, P. Schuller, P. A. Thiebaut, E. TI First astronomical unit scale image of the GW Orionis triple system Direct detection of a new stellar companion SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE binaries: general; stars: variables: T Tauri; Herbig Ae/Be; accretion, accretion disks; techniques: interferometric ID INTERFEROMETRY; ACCRETION; EVOLUTION; DISTANCE; NEBULA; TRACKS; STARS; IOTA AB Context. Young and close multiple systems are unique laboratories to probe the initial dynamical interactions between forming stellar systems and their dust and gas environment. Their study is a key building block to understanding the high frequency of main-sequence multiple systems. However, the number of detected spectroscopic young multiple systems that allow dynamical studies is limited. GW Orionis is one such system. It is one of the brightest young T Tauri stars and is surrounded by a massive disk. Aims. Our goal is to probe the GW Orionis multiplicity at angular scales at which we can spatially resolve the orbit. Methods. We used the IOTA/IONIC3 interferometer to probe the environment of GW Orionis with an astronomical unit resolution in 2003, 2004, and 2005. By measuring squared visibilities and closure phases with a good UV coverage we carry out the first image reconstruction of GW Ori from infrared long-baseline interferometry. Results. We obtained the first infrared image of a T Tauri multiple system with astronomical unit resolution. We show that GW Orionis is a triple system, resolve for the first time the previously known inner pair (separation rho similar to 1.4 AU) and reveal a new more distant component (GW Ori C) with a projected separation of similar to 8 AU with direct evidence of motion. Furthermore, the nearly equal (2: 1) H-band flux ratio of the inner components suggests that either GW Ori B is undergoing a preferential accretion event that increases its disk luminosity or that the estimate of the masses has to be revisited in favour of a more equal mass-ratio system that is seen at lower inclination. Conclusions. Accretion disk models of GW Ori will need to be completely reconsidered because of this outer companion C and the unexpected brightness of companion B. C1 [Berger, J. -P.; Haguenauer, P.] European So Observ, Santiago 19, Chile. [Berger, J. -P.; Renard, S.; Kern, P.; Longa, F.; Malbet, F.; Perraut, K.] Univ Grenoble 1, IPAG, CNRS UMR 5571, F-38041 Grenoble, France. [Monnier, J. D.] Univ Michigan, Ann Arbor, MI 48109 USA. [Millan-Gabet, R.] CALTECH, Pasadena, CA 91125 USA. [Pedretti, E.] Univ St Andrews, St Andrews KY16 9AJ, Fife, Scotland. [Traub, W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Benisty, M.] INAF Osservatorio Astrofis Arcetri, I-50125 Florence, Italy. [Carleton, N.; Lacasse, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Labeye, P.] CEA DRT LETI, F-38054 Grenoble, France. [Ragland, S.] WM Keck Observ, Kamuela, HI 96743 USA. [Schloerb, P.] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. [Schuller, P. A.] Univ Paris 11, CNRS UMR 8617, IAS, F-91405 Orsay, France. [Bechet, C.; Thiebaut, E.] CRAL Observ Lyon, F-69561 St Genis Laval, France. RP Berger, JP (reprint author), European So Observ, Alonso de Cordova 3107 Vitacura,Casilla 19001, Santiago 19, Chile. EM jpberger@eso.org RI Bechet, Clementine/A-6828-2017 OI Bechet, Clementine/0000-0002-0885-3644 FU ASHRA; PNPS/INSU; Michelson fellowship program; CNRS; CNES FX This work was supported by ASHRA, PNPS/INSU, and Michelson fellowship program. This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France and getCal software from the NASA Exoplanet Science Institute, Caltech. Bibliographic references were provided by the SAO/NASA Astrophysics Data System. IONIC-3 has been developed by LAOG and CEA-LETI, and funded by the CNRS and CNES. We thank Russel White, Lee Hartmann and S. Meimon for useful discussions. NR 18 TC 4 Z9 4 U1 0 U2 6 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD MAY PY 2011 VL 529 AR L1 DI 10.1051/0004-6361/201016219 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 750OG UT WOS:000289557200002 ER PT J AU Bouwman, J Cuppen, HM Steglich, M Allamandola, LJ Linnartz, H AF Bouwman, J. Cuppen, H. M. Steglich, M. Allamandola, L. J. Linnartz, H. TI Photochemistry of polycyclic aromatic hydrocarbons in cosmic water ice II. Near UV/VIS spectroscopy and ionization rates SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE astrochemistry; molecular processes; methods: laboratory; techniques: spectroscopic; ISM: molecules ID YOUNG STELLAR OBJECTS; H2O INTERSTELLAR ICE; RADICAL CATIONS; OPTICAL SPECTROSCOPY; VIBRATIONAL-SPECTRA; ASTROPHYSICAL ICES; EXCITATION-SPECTRA; FACILE GENERATION; CORONENE CATION; EXCITED-STATES AB Context. Mid-infrared emission features originating from polycyclic aromatic hydrocarbons (PAHs) are observed towards photon dominated regions in space. Towards dense clouds, however, these emission features are quenched. Observations of dense clouds show that many simple volatile molecules are frozen out on interstellar grains, forming thin layers of ice. Recently, observations have shown that more complex non-volatile species, presumably including PAHs, also freeze out and contribute to the ongoing solid-state chemistry. Aims. The study presented here aims at obtaining reaction rate data that characterize PAH photochemistry upon vacuum ultraviolet (VUV) irradiation in an interstellar H(2)O ice analogue to explore the potential impact of PAH:H(2)O ice reactions on overall interstellar ice chemistry. To this end, the experimental results are implemented in a chemical model under simple interstellar cloud conditions. Methods. Time-dependent near-UV/VIS spectroscopy on the VUV photochemistry of anthracene, pyrene, benzo[ghi]perylene and coronene containing interstellar H(2)O ice analogs is performed at 25 and 125 K, using an optical absorption setup. Results. Near-UV/VIS absorption spectra are presented for these four PAHs and their photoproducts including cationic species trapped in H(2)O ice. Oscillator strengths of the cation absorption bands are derived relative to the oscillator strength of the neutral parent PAH. The loss of the parent and growth of PAH photoproducts are measured as a function of VUV dose, yielding solid state reaction constants. The rate constants are used in an exploratory astrochemical model, to assess the importance of PAH:H(2)O ice photoprocessing in UV exposed interstellar environments, compared with the timescales in which PAH molecules are incorporated in interstellar ices. Conclusions. All four PAHs studied here are found to be readily ionized upon VUV photolysis when trapped in H(2)O ice and exhibit similar rates for ionization at astronomically relevant temperatures. Depending on the relative efficiency of H(2)O photodesorption and PAH photoionization in H(2)O ice, the latter may trigger a charge induced aromatic solid state chemistry, in which PAH cations play a central role. C1 [Steglich, M.] Univ Jena, Lab Astrophys Grp, Max Planck Inst Astron, Inst Solid State Phys, D-07743 Jena, Germany. [Allamandola, L. J.] NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA. [Bouwman, J.; Cuppen, H. M.; Linnartz, H.] Leiden Univ, Leiden Observ, Raymond & Beverly Sackler Lab Astrophys, NL-2300 RA Leiden, Netherlands. RP Bouwman, J (reprint author), Univ Calif Berkeley, Dept Chem, Berkeley, CA 94720 USA. EM bouwman@berkeley.edu RI Cuppen, Herma/F-9729-2015; OI Cuppen, Herma/0000-0003-4397-0739; Steglich, Mathias/0000-0001-8206-6588 FU "Stichting voor Fundamenteel Onderzoek der Materie" (FOM); "the Netherlands Research School for Astronomy" (NOVA); NASA's Laboratory; European Community [238258] FX This work is financially supported by "Stichting voor Fundamenteel Onderzoek der Materie" (FOM), "the Netherlands Research School for Astronomy" (NOVA), and NASA's Laboratory Astrophysics and Astrobiology Programs. The research leading to these results has received funding from the [European Community's] Seventh Framework Programme [FP7/2007-2013] under grant agreement no [238258]. The authors would like to thank Ankan Das for his contribution to the data reduction. NR 46 TC 19 Z9 19 U1 3 U2 39 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 MAY PY 2011 VL 529 AR A46 DI 10.1051/0004-6361/201015762 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 750OG UT WOS:000289557200054 ER PT J AU Faure, C Anguita, T Alloin, D Bundy, K Finoguenov, A Leauthaud, A Knobel, C Kneib, JP Jullo, E Ilbert, O Koekemoer, AM Capak, P Scoville, N Tasca, LAM AF Faure, C. Anguita, T. Alloin, D. Bundy, K. Finoguenov, A. Leauthaud, A. Knobel, C. Kneib, J-P Jullo, E. Ilbert, O. Koekemoer, A. M. Capak, P. Scoville, N. Tasca, L. A. M. TI On the evolution of environmental and mass properties of strong lens galaxies in COSMOS SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE gravitational lensing: strong ID DARK-MATTER HALOS; HIGH-DENSITY ENVIRONMENTS; WIDE-FIELD SURVEY; ACS SURVEY; GRAVITATIONAL LENSES; STELLAR MASS; QUANTITATIVE MORPHOLOGY; PHOTOMETRIC REDSHIFTS; INTERNAL STRUCTURE; OPTICAL DEPTHS AB Context. Nearly 100 new strong-lens candidates have been discovered in the COSMOS field. Among these, 20 lens candidates with 0.34 less than or similar to z(lens) <= 1.13 feature multiple images of background sources. Aims. Using the multi-wavelength coverage of the field and its spectroscopic follow-up, we characterize the evolution with redshift of the environment and of the dark-matter (DM) fraction of the lens galaxies. Methods. We present spectroscopic and new photometric redshifts of the strong-lens candidates. The lens environment is characterized in the following way: we account for the projected 10 closest galaxies around each lens and for galaxies with a projected distance less than 1 Mpc at the lens galaxy redshift. In both cases, we perform similar measurements on a control sample of "twin" non-lens early-type galaxies (ETGs). In addition, we identify group members and field galaxies in the X-ray and optical catalogs of galaxy groups and clusters. From those catalogs, we measure the external shear contribution of the groups/clusters surrounding the lens galaxies. The systems are then modeled using a singular isothermal ellipsoid for the lens galaxies plus the external shear produced by the groups/clusters. Results. We observe that the average stellar mass of lens galaxies increases with redshift. In addition, we measure that the environment of lens galaxies is compatible with that of the twins over the whole redshift range tested here. During the lens modeling, we notice that when let free, the external shear points in a direction which is the mean direction of the external shear produced by the groups/clusters and of the closest galaxy to the lens. We also notice that the DM fraction of the lens galaxies measured within the Einstein radius significantly decreases as the redshift increases. Conclusions. Given these observations, we conclude that while the environment of lens galaxies is compatible with that of non-lens ETGS over a wide range of redshifts, their mass properties evolves significantly with redshift: it is still not clear whether this advocates in favor of a stronger lensing bias toward massive objects at high redshift or if it is simply representative of the high proportion of massive and high stellar density galaxies at high redshift. C1 [Faure, C.] Observ Sauverny, Ecole Polytech Fed Lausanne, Astrophys Lab, CH-1290 Versoix, Switzerland. [Anguita, T.] Pontificia Univ Catolica Chile, Dept Astron & Astrofis, Ctr Astroingn, Santiago, Chile. [Anguita, T.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Alloin, D.] Univ Paris Diderot, CNRS, Lab AIM, CEA,DSM,IRFU,SEDI,SAP,Serv Astrophys,CEA Saclay, F-91191 Gif Sur Yvette, France. [Bundy, K.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Finoguenov, A.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Leauthaud, A.] Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. [Leauthaud, A.] Univ Calif Berkeley, Berkeley Ctr Cosmol Phys, Berkeley, CA 94720 USA. [Knobel, C.] ETH, Inst Astron, CH-8093 Zurich, Switzerland. [Kneib, J-P; Ilbert, O.; Tasca, L. A. M.] Univ Aix Marseille 1, CNRS, Lab Astrophys Marseille, F-13388 Marseille 13, France. [Jullo, E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Koekemoer, A. M.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Capak, P.; Scoville, N.] CALTECH, Pasadena, CA 91125 USA. RP Faure, C (reprint author), Observ Sauverny, Ecole Polytech Fed Lausanne, Astrophys Lab, CH-1290 Versoix, Switzerland. RI Kneib, Jean-Paul/A-7919-2015; OI Kneib, Jean-Paul/0000-0002-4616-4989; Koekemoer, Anton/0000-0002-6610-2048 FU CNRS; CEA; SL2S [ANR-06-BLAN-0067]; DESIR [ANR-07-BLAN-0228]; NPP; NASA FX We acknowledge the anonymous referee for providing a detailed and very useful report. We are gratefully indebted to M. Limousin and R. Gavazzi for enlightening discussions. D.A. thanks CNRS and CEA for support and visits to the Geneva observatory, where this work was finalized. J.P.K. thanks for support from CNRS and SL2S ANR-06-BLAN-0067 and DESIR ANR-07-BLAN-0228. E.J. acknowledges the support of the NPP, administered by Oak Ridge Associated Universities through a contract with NASA. NR 68 TC 17 Z9 17 U1 1 U2 4 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD MAY PY 2011 VL 529 AR A72 DI 10.1051/0004-6361/200913498 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 750OG UT WOS:000289557200080 ER PT J AU Guilbert-Lepoutre, A Lasue, J Federico, C Coradini, A Orosei, R Rosenberg, ED AF Guilbert-Lepoutre, A. Lasue, J. Federico, C. Coradini, A. Orosei, R. Rosenberg, E. D. TI New 3D thermal evolution model for icy bodies application to trans-Neptunian objects SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE Kuiper belt: general; diffusion; methods: numerical ID KUIPER-BELT OBJECTS; COMET NUCLEI; SOLAR-SYSTEM; PHASE-TRANSITION; WATER-ICE; CENTAURS; SURFACE; ORIGIN; HEAT; IRRADIATION AB Context. Thermal evolution models have been developed over the years to investigate the evolution of thermal properties based on the transfer of heat fluxes or transport of gas through a porous matrix, among others. Applications of such models to trans-Neptunian objects (TNOs) and Centaurs has shown that these bodies could be strongly differentiated from the point of view of chemistry (i.e. loss of most volatile ices), as well as from physics (e.g. melting of water ice), resulting in stratified internal structures with differentiated cores and potential pristine material close to the surface. In this context, some observational results, such as the detection of crystalline water ice or volatiles, remain puzzling. Aims. In this paper, we would like to present a new fully three-dimensional thermal evolution model. With this model, we aim to improve determination of the temperature distribution inside icy bodies such as TNOs by accounting for lateral heat fluxes, which have been proven to be important for accurate simulations. We also would like to be able to account for heterogeneous boundary conditions at the surface through various albedo properties, for example, that might induce different local temperature distributions. Methods. In a departure from published modeling approaches, the heat diffusion problem and its boundary conditions are represented in terms of real spherical harmonics, increasing the numerical efficiency by roughly an order of magnitude. We then compare this new model and another 3D model recently published to illustrate the advantages and limits of the new model. We try to put some constraints on the presence of crystalline water ice at the surface of TNOs. Results. The results obtained with this new model are in excellent agreement with results obtained by different groups with various models. Small TNOs could remain primitive unless they are formed quickly (less than 2 Myr) or are debris from the disruption of larger bodies. We find that, for large objects with a thermal evolution dominated by the decay of long-lived isotopes (objects with a formation period greater than 2 to 3 Myr), the presence of crystalline water ice would require both a large radius (>300 km) and high density (>1500 kg m(-3)). In particular, objects with intermediate radii and densities would be an interesting transitory population deserving a detailed study of individual fates. C1 [Guilbert-Lepoutre, A.] Observ Paris, Sect Meudon, LESIA, F-92195 Meudon, France. [Guilbert-Lepoutre, A.] Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90095 USA. [Lasue, J.] Los Alamos Natl Lab, ISR 1, Los Alamos, NM 87545 USA. [Lasue, J.] Lunar & Planetary Inst, Houston, TX 77058 USA. [Federico, C.] Univ Perugia, Dipartimento Sci Terra, I-06123 Perugia, Italy. [Coradini, A.] INAF IFSI, I-00133 Rome, Italy. [Orosei, R.] INAF IASF, I-00133 Rome, Italy. [Rosenberg, E. D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Guilbert-Lepoutre, A (reprint author), Observ Paris, Sect Meudon, LESIA, 2 Pl J Janssen, F-92195 Meudon, France. EM aguilbert@ucla.edu FU NASA FX A.G.L. thanks G. Magni, M. T. Capria, M. C. De Sanctis and D. Turini for useful discussions on the model, and D. Jewitt for useful comments on the manuscript. J.L. thanks the LPI contribution 1549. A.G.L. was supported in part by a NASA Herschel grant to David Jewitt. The authors want to thank the anonymous referee for their useful comments that contributed to a major improvement of the manuscript. NR 64 TC 11 Z9 11 U1 0 U2 6 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD MAY PY 2011 VL 529 AR A71 DI 10.1051/0004-6361/201014194 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 750OG UT WOS:000289557200079 ER PT J AU Marshall, JP Lohne, T Montesinos, B Krivov, AV Eiroa, C Absil, O Bryden, G Maldonado, J Mora, A Sanz-Forcada, J Ardila, D Augereau, JC Bayo, A del Burgo, C Danchi, W Ertel, S Fedele, D Fridlund, M Lebreton, J Gonzalez-Garcia, BM Liseau, R Meeus, G Muller, S Pilbratt, GL Roberge, A Stapelfeldt, K Thebault, P White, GJ Wolf, S AF Marshall, J. P. Loehne, T. Montesinos, B. Krivov, A. V. Eiroa, C. Absil, O. Bryden, G. Maldonado, J. Mora, A. Sanz-Forcada, J. Ardila, D. Augereau, J. -Ch. Bayo, A. del Burgo, C. Danchi, W. Ertel, S. Fedele, D. Fridlund, M. Lebreton, J. Gonzalez-Garcia, B. M. Liseau, R. Meeus, G. Mueller, S. Pilbratt, G. L. Roberge, A. Stapelfeldt, K. Thebault, P. White, G. J. Wolf, S. TI A Herschel resolved far-infrared dust ring around HD 207129 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: individual: HD 207129; circumstellar matter; infrared: stars ID MAIN-SEQUENCE STARS; VEGA-TYPE STARS; NEARBY STARS; DEBRIS DISKS; BETA-PICTORIS; Q(1) ERIDANI; PLANET; SEARCH; SPACE; BELT AB Context. Dusty debris discs around main sequence stars are thought to be the result of continuous collisional grinding of planetesimals in the system. The majority of these systems are unresolved and analysis of the dust properties is limited by the lack of information regarding the dust location. Aims. The Herschel DUNES key program is observing 133 nearby, Sun-like stars (<20 pc, FGK spectral type) in a volume limited survey to constrain the absolute incidence of cold dust around these stars by detection of far infrared excess emission at flux levels comparable to the Edgeworth-Kuiper belt (EKB). Methods. We have observed the Sun-like star HD 207129 with Herschel PACS and SPIRE. In all three PACS bands we resolve a ring-like structure consistent with scattered light observations. Using alpha Bootis as a reference point spread function (PSF), we deconvolved the images, clearly resolving the inner gap in the disc at both 70 and 100 mu m. Results. We have resolved the dust-producing planetesimal belt of a debris disc at 100 mu m for the first time. We measure the radial profile and fractional luminosity of the disc, and compare the values to those of discs around stars of similar age and/or spectral type, placing this disc in context of other resolved discs observed by Herschel/DUNES. C1 [Marshall, J. P.; Eiroa, C.; Maldonado, J.; Mora, A.; Fedele, D.; Meeus, G.] Univ Autonoma Madrid, Dept Fis Teor, Fac Ciencias, E-28049 Madrid, Spain. [Loehne, T.; Krivov, A. V.; Mueller, S.] Univ Jena, Inst Astrophys, D-07743 Jena, Germany. [Loehne, T.; Krivov, A. V.; Mueller, S.] Univ Sternwarte, D-07743 Jena, Germany. [Montesinos, B.; Sanz-Forcada, J.] CSIC INTA, CAB, Ctr Astrobiol, Dept Astrofis, Madrid 28691, Spain. [Absil, O.] Univ Liege, Inst Astrophys & Geophys, B-4000 Sart Tilman Par Liege, Belgium. [Bryden, G.; Stapelfeldt, K.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Mora, A.] ESA ESAC Gaia SOC, Madrid 28691, Spain. [Ardila, D.] CALTECH, NASA Herschel Sci Ctr, Pasadena, CA 91125 USA. [Augereau, J. -Ch.; Lebreton, J.] UJF Grenoble 1 CNRS INSU, IPAG, UMR 5274, F-38041 Grenoble, France. [Bayo, A.] European Space Observ, Santiago 19, Chile. [del Burgo, C.] UNINOVA CA3, P-2825149 Caparica, Portugal. [Danchi, W.; Roberge, A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Ertel, S.; Wolf, S.] Univ Kiel, Inst Theoret Phys & Astrophys, D-24098 Kiel, Germany. [Fedele, D.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Fedele, D.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21210 USA. [Fridlund, M.; Pilbratt, G. L.] ESTEC SRE SA, ESA Astrophys & Fundamental Phys Missions Div, NL-2201 AZ Noordwijk, Netherlands. [Gonzalez-Garcia, B. M.] ESAC, INSA, Madrid 28691, Spain. [Liseau, R.] Chalmers, Onsala Space Observ, S-43992 Onsala, Sweden. [Thebault, P.] Observ Paris, LESIA, F-92195 Meudon, France. [White, G. J.] Open Univ, Dept Phys & Astrophys, Milton Keynes MK7 6AA, Bucks, England. [White, G. J.] Rutherford Appleton Lab, Didcot OX11 0QX, Oxon, England. RP Marshall, JP (reprint author), Univ Autonoma Madrid, Dept Fis Teor, Fac Ciencias, E-28049 Madrid, Spain. EM jonathan.marshall@uam.es RI Roberge, Aki/D-2782-2012; Stapelfeldt, Karl/D-2721-2012; Fedele, Davide/L-8688-2013; Sanz-Forcada, Jorge/C-3176-2017; Montesinos, Benjamin/C-3493-2017; OI Roberge, Aki/0000-0002-2989-3725; Fedele, Davide/0000-0001-6156-0034; Sanz-Forcada, Jorge/0000-0002-1600-7835; Montesinos, Benjamin/0000-0002-7982-2095; Marshall, Jonathan/0000-0001-6208-1801 FU Spanish grant [AYA 2008/01727]; DFG [Lo 1715/1-1, Kr 2164/9-1]; CNES-PNP FX We would like to thank the staff at the Herschel Science Centre, discussions with whom added immeasurably to the quality of the data reduction. C. Eiroa, J. Maldonado, J. P. Marshall, and B. Montesinos are partly supported by Spanish grant AYA 2008/01727. T. Lohne, S. Muller and A. Krivov acknowledge support by the DFG, projects Lo 1715/1-1 and Kr 2164/9-1. J.-Ch. Augereau, J. Lebreton and P. Thebault are supported by a CNES-PNP grant. NR 46 TC 28 Z9 28 U1 0 U2 8 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 MAY PY 2011 VL 529 AR A117 DI 10.1051/0004-6361/201116673 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 750OG UT WOS:000289557200125 ER PT J AU Abbasi, R Abdou, Y Abu-Zayyad, T Adams, J Aguilar, JA Ahlers, M Andeen, K Auffenberg, J Bai, X Baker, M Barwick, SW Bay, R Alba, JLB Beattie, K Beatty, JJ Bechet, S Becker, JK Becker, KH Benabderrahmane, ML BenZvi, S Berdermann, J Berghaus, P Berley, D Bernardini, E Bertrand, D Besson, DZ Bissok, M Blaufuss, E Blumenthal, J Boersma, DJ Bohm, C Bose, D Boser, S Botner, O Braun, J Brown, AM Buitink, S Carson, M Chirkin, D Christy, B Clem, J Clevermann, F Cohen, S Colnard, C Cowen, DF D'Agostino, MV Danninger, M Daughhetee, J Davis, JC De Clercq, C Demirors, L Depaepe, O Descamps, F Desiati, P de Vries-Uiterweerd, G DeYoung, T Diaz-Velez, JC Dierckxsens, M Dreyer, J Dumm, JP Ehrlich, R Eisch, J Ellsworth, RW Engdegard, O Euler, S Evenson, PA Fadiran, O Fazely, AR Fedynitch, A Feusels, T Filimonov, K Finley, C Foerster, MM Fox, BD Franckowiak, A Franke, R Gaisser, TK Gallagher, J Geisler, M Gerhardt, L Gladstone, L Glusenkamp, T Goldschmidt, A Goodman, JA Grant, D Griesel, T Gross, A Grullon, S Gurtner, M Ha, C Hallgren, A Halzen, F Han, K Hanson, K Helbing, K Herquet, P Hickford, S Hill, GC Hoffman, KD Homeier, A Hoshina, K Hubert, D Huelsnitz, W Hulss, JP Hulth, PO Hultqvist, K Hussain, S Ishihara, A Jacobsen, J Japaridze, GS Johansson, H Joseph, JM Kampert, KH Kappes, A Karg, T Karle, A Kelley, JL Kemming, N Kenny, P Kiryluk, J Kislat, F Klein, SR Kohne, JH Kohnen, G Kolanoski, H Kopke, L Koskinen, DJ Kowalski, M Kowarik, T Krasberg, M Krings, T Kroll, G Kuehn, K Kuwabara, T Labare, M Lafebre, S Laihem, K Landsman, H Larson, MJ Lauer, R Lehmann, R Lunemann, J Madsen, J Majumdar, P Marotta, A Maruyama, R Mase, K Matis, HS Matusik, M Meagher, K Merck, M Meszaros, P Meures, T Middell, E Milke, N Miller, J Montaruli, T Morse, R Movit, SM Nahnhauer, R Nam, JW Naumann, U Niessen, P Nygren, DR Odrowski, S Olivas, A Olivo, M O'Murchadha, A Ono, M Panknin, S Paul, L de los Heros, CP Petrovic, J Piegsa, A Pieloth, D Porrata, R Posselt, J Price, PB Prikockis, M Przybylski, GT Rawlins, K Redl, P Resconi, E Rhode, W Ribordy, M Rizzo, A Rodrigues, JP Roth, P Rothmaier, F Rott, C Ruhe, T Rutledge, D Ruzybayev, B Ryckbosch, D Sander, HG Santander, M Sarkar, S Schatto, K Schlenstedt, S Schmidt, T Schukraft, A Schultes, A Schulz, O Schunck, M Seckel, D Semburg, B Seo, SH Sestayo, Y Seunarine, S Silvestri, A Singh, K Slipak, A Spiczak, GM Spiering, C Stamatikos, M Stanev, T Stephens, G Stezelberger, T Stokstad, RG Stoyanov, S Strahler, EA Straszheim, T Sullivan, GW Swillens, Q Taavola, H Taboada, I Tamburro, A Tarasova, O Tepe, A Ter-Antonyan, S Tilav, S Toale, PA Toscano, S Tosi, D Turcan, D van Eijndhoven, N Vandenbroucke, J Van Overloop, A van Santen, J Vehring, M Voge, M Voigt, B Walck, C Waldenmaier, T Wallraff, M Walter, M Weaver, C Wendt, C Westerhoff, S Whitehorn, N Wiebe, K Wiebusch, CH Williams, DR Wischnewski, R Wissing, H Wolf, M Woschnagg, K Xu, C Xu, XW Yodh, G Yoshida, S Zarzhitsky, P AF Abbasi, R. Abdou, Y. Abu-Zayyad, T. Adams, J. Aguilar, J. A. Ahlers, M. Andeen, K. Auffenberg, J. Bai, X. Baker, M. Barwick, S. W. Bay, R. Alba, J. L. Bazo Beattie, K. Beatty, J. J. Bechet, S. Becker, J. K. Becker, K-H Benabderrahmane, M. L. BenZvi, S. Berdermann, J. Berghaus, P. Berley, D. Bernardini, E. Bertrand, D. Besson, D. Z. Bissok, M. Blaufuss, E. Blumenthal, J. Boersma, D. J. Bohm, C. Bose, D. Boeser, S. Botner, O. Braun, J. Brown, A. M. Buitink, S. Carson, M. Chirkin, D. Christy, B. Clem, J. Clevermann, F. Cohen, S. Colnard, C. Cowen, D. F. D'Agostino, M. V. Danninger, M. Daughhetee, J. Davis, J. C. De Clercq, C. Demiroers, L. Depaepe, O. Descamps, F. Desiati, P. de Vries-Uiterweerd, G. DeYoung, T. Diaz-Velez, J. C. Dierckxsens, M. Dreyer, J. Dumm, J. P. Ehrlich, R. Eisch, J. Ellsworth, R. W. Engdegard, O. Euler, S. Evenson, P. A. Fadiran, O. Fazely, A. R. Fedynitch, A. Feusels, T. Filimonov, K. Finley, C. Foerster, M. M. Fox, B. D. Franckowiak, A. Franke, R. Gaisser, T. K. Gallagher, J. Geisler, M. Gerhardt, L. Gladstone, L. Gluesenkamp, T. Goldschmidt, A. Goodman, J. A. Grant, D. Griesel, T. Gross, A. Grullon, S. Gurtner, M. Ha, C. Hallgren, A. Halzen, F. Han, K. Hanson, K. Helbing, K. Herquet, P. Hickford, S. Hill, G. C. Hoffman, K. D. Homeier, A. Hoshina, K. Hubert, D. Huelsnitz, W. Huelss, J-P Hulth, P. O. Hultqvist, K. Hussain, S. Ishihara, A. Jacobsen, J. Japaridze, G. S. Johansson, H. Joseph, J. M. Kampert, K-H Kappes, A. Karg, T. Karle, A. Kelley, J. L. Kemming, N. Kenny, P. Kiryluk, J. Kislat, F. Klein, S. R. Koehne, J-H Kohnen, G. Kolanoski, H. Koepke, L. Koskinen, D. J. Kowalski, M. Kowarik, T. Krasberg, M. Krings, T. Kroll, G. Kuehn, K. Kuwabara, T. Labare, M. Lafebre, S. Laihem, K. Landsman, H. Larson, M. J. Lauer, R. Lehmann, R. Luenemann, J. Madsen, J. Majumdar, P. Marotta, A. Maruyama, R. Mase, K. Matis, H. S. Matusik, M. Meagher, K. Merck, M. Meszaros, P. Meures, T. Middell, E. Milke, N. Miller, J. Montaruli, T. Morse, R. Movit, S. M. Nahnhauer, R. Nam, J. W. Naumann, U. Niessen, P. Nygren, D. R. Odrowski, S. Olivas, A. Olivo, M. O'Murchadha, A. Ono, M. Panknin, S. Paul, L. de los Heros, C. Perez Petrovic, J. Piegsa, A. Pieloth, D. Porrata, R. Posselt, J. Price, P. B. Prikockis, M. Przybylski, G. T. Rawlins, K. Redl, P. Resconi, E. Rhode, W. Ribordy, M. Rizzo, A. Rodrigues, J. P. Roth, P. Rothmaier, F. Rott, C. Ruhe, T. Rutledge, D. Ruzybayev, B. Ryckbosch, D. Sander, H-G Santander, M. Sarkar, S. Schatto, K. Schlenstedt, S. Schmidt, T. Schukraft, A. Schultes, A. Schulz, O. Schunck, M. Seckel, D. Semburg, B. Seo, S. H. Sestayo, Y. Seunarine, S. Silvestri, A. Singh, K. Slipak, A. Spiczak, G. M. Spiering, C. Stamatikos, M. Stanev, T. Stephens, G. Stezelberger, T. Stokstad, R. G. Stoyanov, S. Strahler, E. A. Straszheim, T. Sullivan, G. W. Swillens, Q. Taavola, H. Taboada, I. Tamburro, A. Tarasova, O. Tepe, A. Ter-Antonyan, S. Tilav, S. Toale, P. A. Toscano, S. Tosi, D. Turcan, D. van Eijndhoven, N. Vandenbroucke, J. Van Overloop, A. van Santen, J. Vehring, M. Voge, M. Voigt, B. Walck, C. Waldenmaier, T. Wallraff, M. Walter, M. Weaver, Ch. Wendt, C. Westerhoff, S. Whitehorn, N. Wiebe, K. Wiebusch, C. H. Williams, D. R. Wischnewski, R. Wissing, H. Wolf, M. Woschnagg, K. Xu, C. Xu, X. W. Yodh, G. Yoshida, S. Zarzhitsky, P. CA IceCube Collaboration TI TIME-INTEGRATED SEARCHES FOR POINT-LIKE SOURCES OF NEUTRINOS WITH THE 40-STRING IceCube DETECTOR SO ASTROPHYSICAL JOURNAL LA English DT Article DE astroparticle physics; cosmic rays; neutrinos ID HIGH-ENERGY NEUTRINOS; GAMMA-RAY EMISSION; COSMIC-RAYS; GALAXIES; CLUSTERS; TELESCOPES; ASTRONOMY; ASTROPHYSICS; SELECTION; MILAGRO AB We present the results of time-integrated searches for astrophysical neutrino sources in both the northern and southern skies. Data were collected using the partially completed IceCube detector in the 40-string configuration recorded between 2008 April 5 and 2009 May 20, totaling 375.5 days livetime. An unbinned maximum likelihood ratio method is used to search for astrophysical signals. The data sample contains 36,900 events: 14,121 from the northern sky, mostly muons induced by atmospheric neutrinos, and 22,779 from the southern sky, mostly high-energy atmospheric muons. The analysis includes searches for individual point sources and stacked searches for sources in a common class, sometimes including a spatial extent. While this analysis is sensitive to TeV-PeV energy neutrinos in the northern sky, it is primarily sensitive to neutrinos with energy greater than about 1 PeV in the southern sky. No evidence for a signal is found in any of the searches. Limits are set for neutrino fluxes from astrophysical sources over the entire sky and compared to predictions. The sensitivity is at least a factor of two better than previous searches (depending on declination), with 90% confidence level muon neutrino flux upper limits being between E(2)d Phi/dE similar to 2-200 x 10(-12) TeV cm(-2) s(-1) in the northern sky and between 3-700 x 10(-12) TeV cm(-2) s(-1) in the southern sky. The stacked source searches provide the best limits to specific source classes. The full IceCube detector is expected to improve the sensitivity to d Phi/dE proportional to E-2 sources by another factor of two in the first year of operation. C1 [Abbasi, R.; Aguilar, J. A.; Andeen, K.; Baker, M.; BenZvi, S.; Berghaus, P.; Braun, J.; Chirkin, D.; Desiati, P.; Diaz-Velez, J. C.; Dumm, J. P.; Eisch, J.; Gladstone, L.; Grullon, S.; Halzen, F.; Hanson, K.; Hill, G. C.; Hoshina, K.; Jacobsen, J.; Karle, A.; Kelley, J. L.; Krasberg, M.; Landsman, H.; Maruyama, R.; Merck, M.; Montaruli, T.; Morse, R.; O'Murchadha, A.; Rodrigues, J. P.; Santander, M.; Toscano, S.; van Santen, J.; Weaver, Ch.; Wendt, C.; Westerhoff, S.; Whitehorn, N.] Univ Wisconsin, Dept Phys, Madison, WI 53706 USA. [Abdou, Y.; Carson, M.; Descamps, F.; de Vries-Uiterweerd, G.; Feusels, T.; Ryckbosch, D.; Van Overloop, A.] Univ Ghent, Dept Subatom & Radiat Phys, B-9000 Ghent, Belgium. [Abu-Zayyad, T.; Madsen, J.; Spiczak, G. M.; Tamburro, A.] Univ Wisconsin, Dept Phys, River Falls, WI 54022 USA. [Adams, J.; Brown, A. M.; Gross, A.; Han, K.; Hickford, S.] Univ Canterbury, Dept Phys & Astron, Christchurch, New Zealand. [Ahlers, M.; Sarkar, S.] Univ Oxford, Dept Phys, Oxford OX1 3NP, England. [Auffenberg, J.; Becker, K-H; Gurtner, M.; Helbing, K.; Kampert, K-H; Karg, T.; Matusik, M.; Naumann, U.; Posselt, J.; Schultes, A.; Semburg, B.] Univ Wuppertal, Dept Phys, D-42119 Wuppertal, Germany. [Bai, X.; Clem, J.; Evenson, P. A.; Gaisser, T. K.; Hussain, S.; Kuwabara, T.; Niessen, P.; Ruzybayev, B.; Seckel, D.; Stanev, T.; Stoyanov, S.; Tilav, S.; Xu, C.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA. [Bai, X.; Clem, J.; Evenson, P. A.; Gaisser, T. K.; Hussain, S.; Kuwabara, T.; Niessen, P.; Ruzybayev, B.; Seckel, D.; Stanev, T.; Stoyanov, S.; Tilav, S.; Xu, C.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA. [Barwick, S. W.; Nam, J. W.; Silvestri, A.; Yodh, G.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. [Bay, R.; D'Agostino, M. V.; Filimonov, K.; Gerhardt, L.; Kiryluk, J.; Klein, S. R.; Porrata, R.; Price, P. B.; Vandenbroucke, J.; Woschnagg, K.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Alba, J. L. Bazo; Benabderrahmane, M. L.; Berdermann, J.; Bernardini, E.; Franke, R.; Kislat, F.; Lauer, R.; Majumdar, P.; Middell, E.; Nahnhauer, R.; Schlenstedt, S.; Spiering, C.; Tarasova, O.; Tosi, D.; Voigt, B.; Walter, M.; Wischnewski, R.] DESY, D-15735 Zeuthen, Germany. [Beattie, K.; Buitink, S.; Gerhardt, L.; Goldschmidt, A.; Joseph, J. M.; Kiryluk, J.; Klein, S. R.; Matis, H. S.; Nygren, D. R.; Przybylski, G. T.; Stezelberger, T.; Stokstad, R. G.] Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. [Beatty, J. J.; Davis, J. C.; Kuehn, K.; Rott, C.; Stamatikos, M.] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA. [Beatty, J. J.; Davis, J. C.; Kuehn, K.; Rott, C.; Stamatikos, M.] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA. [Beatty, J. J.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Bechet, S.; Bertrand, D.; Dierckxsens, M.; Hanson, K.; Marotta, A.; Petrovic, J.; Swillens, Q.] Univ Libre Brussels, Sci Fac CP230, B-1050 Brussels, Belgium. [Becker, J. K.; Dreyer, J.; Fedynitch, A.; Olivo, M.] Ruhr Univ Bochum, Fak Phys & Astron, D-44780 Bochum, Germany. [Berley, D.; Blaufuss, E.; Christy, B.; Ehrlich, R.; Ellsworth, R. W.; Goodman, J. A.; Hoffman, K. D.; Huelsnitz, W.; Meagher, K.; Olivas, A.; Redl, P.; Roth, P.; Schmidt, T.; Straszheim, T.; Sullivan, G. W.; Turcan, D.; Wissing, H.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA. [Besson, D. Z.; Kenny, P.] Univ Kansas, Dept Phys & Astron, Lawrence, KS 66045 USA. [Bissok, M.; Blumenthal, J.; Boersma, D. J.; Euler, S.; Geisler, M.; Gluesenkamp, T.; Huelss, J-P; Krings, T.; Laihem, K.; Meures, T.; Paul, L.; Schukraft, A.; Schunck, M.; Vehring, M.; Wallraff, M.; Wiebusch, C. H.] Rhein Westfal TH Aachen, Inst Phys 3, D-52056 Aachen, Germany. [Bohm, C.; Danninger, M.; Finley, C.; Hulth, P. O.; Hultqvist, K.; Johansson, H.; Seo, S. H.; Walck, C.] Stockholm Univ, Oskar Klein Ctr, SE-10691 Stockholm, Sweden. [Bohm, C.; Danninger, M.; Finley, C.; Hulth, P. O.; Hultqvist, K.; Johansson, H.; Seo, S. H.; Walck, C.] Stockholm Univ, Deptartment Phys, SE-10691 Stockholm, Sweden. [Bose, D.; De Clercq, C.; Depaepe, O.; Hubert, D.; Labare, M.; Rizzo, A.; Singh, K.; Strahler, E. A.; van Eijndhoven, N.] Vrije Univ Brussel, Dienst ELEM, B-1050 Brussels, Belgium. [Boeser, S.; Franckowiak, A.; Homeier, A.; Kowalski, M.; Panknin, S.] Univ Bonn, Inst Phys, D-53115 Bonn, Germany. [Botner, O.; Engdegard, O.; Hallgren, A.; Miller, J.; Olivo, M.; de los Heros, C. Perez; Taavola, H.] Uppsala Univ, Dept Phys & Astron, S-75120 Uppsala, Sweden. [Clevermann, F.; Koehne, J-H; Milke, N.; Pieloth, D.; Rhode, W.; Ruhe, T.] TU Dortmund Univ, Dept Phys, D-44221 Dortmund, Germany. [Cohen, S.; Demiroers, L.; Ribordy, M.] Ecole Polytech Fed Lausanne, High Energy Phys Lab, CH-1015 Lausanne, Switzerland. [Colnard, C.; Gross, A.; Odrowski, S.; Resconi, E.; Schulz, O.; Sestayo, Y.; Voge, M.; Wolf, M.] Max Planck Inst Kernphys, D-69177 Heidelberg, Germany. [Cowen, D. F.; DeYoung, T.; Foerster, M. M.; Fox, B. D.; Ha, C.; Koskinen, D. J.; Lafebre, S.; Larson, M. J.; Meszaros, P.; Prikockis, M.; Rutledge, D.; Slipak, A.; Stephens, G.; Toale, P. A.] Penn State Univ, Dept Phys, University Pk, PA 16802 USA. [Cowen, D. F.; Meszaros, P.; Movit, S. M.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Daughhetee, J.; Taboada, I.; Tepe, A.] Georgia Inst Technol, Sch Phys, Atlanta, GA 30332 USA. [Daughhetee, J.; Taboada, I.; Tepe, A.] Georgia Inst Technol, Ctr Relativist Astrophys, Atlanta, GA 30332 USA. [Fadiran, O.; Japaridze, G. S.] Clark Atlanta Univ, CTSPS, Atlanta, GA 30314 USA. [Fazely, A. R.; Ter-Antonyan, S.; Xu, X. W.] Southern Univ, Dept Phys, Baton Rouge, LA 70813 USA. [Gallagher, J.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. [Grant, D.] Univ Alberta, Dept Phys, Edmonton, AB T6G 2G7, Canada. [Griesel, T.; Koepke, L.; Kowarik, T.; Kroll, G.; Luenemann, J.; Piegsa, A.; Rothmaier, F.; Sander, H-G; Schatto, K.; Wiebe, K.] Johannes Gutenberg Univ Mainz, Inst Phys, D-55099 Mainz, Germany. [Herquet, P.; Kohnen, G.] Univ Mons, B-7000 Mons, Belgium. [Ishihara, A.; Mase, K.; Ono, M.; Yoshida, S.] Chiba Univ, Dept Phys, Chiba 2638522, Japan. [Kappes, A.; Kemming, N.; Kolanoski, H.; Lehmann, R.; Waldenmaier, T.] Humboldt Univ, Inst Phys, D-12489 Berlin, Germany. [Rawlins, K.] Univ Alaska Anchorage, Dept Phys & Astron, Anchorage, AK 99508 USA. [Seunarine, S.] Univ W Indies, Dept Phys, BB-11000 Bridgetown, Barbados. [Stamatikos, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Williams, D. R.; Zarzhitsky, P.] Univ Alabama, Dept Phys & Astron, Tuscaloosa, AL 35487 USA. RP Abbasi, R (reprint author), Univ Wisconsin, Dept Phys, 1150 Univ Ave, Madison, WI 53706 USA. RI Taavola, Henric/B-4497-2011; Beatty, James/D-9310-2011; Wiebusch, Christopher/G-6490-2012; Kowalski, Marek/G-5546-2012; Tamburro, Alessio/A-5703-2013; Botner, Olga/A-9110-2013; Hallgren, Allan/A-8963-2013; Tjus, Julia/G-8145-2012; Auffenberg, Jan/D-3954-2014; Koskinen, David/G-3236-2014; Aguilar Sanchez, Juan Antonio/H-4467-2015; Maruyama, Reina/A-1064-2013; Sarkar, Subir/G-5978-2011 OI Ter-Antonyan, Samvel/0000-0002-5788-1369; Schukraft, Anne/0000-0002-9112-5479; Perez de los Heros, Carlos/0000-0002-2084-5866; Taavola, Henric/0000-0002-2604-2810; Buitink, Stijn/0000-0002-6177-497X; Hubert, Daan/0000-0002-4365-865X; Benabderrahmane, Mohamed Lotfi/0000-0003-4410-5886; Carson, Michael/0000-0003-0400-7819; Beatty, James/0000-0003-0481-4952; Actis, Oxana/0000-0001-8851-3983; Wiebusch, Christopher/0000-0002-6418-3008; Auffenberg, Jan/0000-0002-1185-9094; Koskinen, David/0000-0002-0514-5917; Aguilar Sanchez, Juan Antonio/0000-0003-2252-9514; Maruyama, Reina/0000-0003-2794-512X; Sarkar, Subir/0000-0002-3542-858X FU U.S. National Science Foundation; U.S. National Science Foundation-Physics Division; University of Wisconsin Alumni Research Foundation; Grid Laboratory Of Wisconsin (GLOW) grid infrastructure at the University of Wisconsin-Madison; Open Science Grid (OSG) grid infrastructure; U.S. Department of Energy; National Energy Research Scientific Computing Center; Louisiana Optical Network Initiative (LONI) grid computing resources; National Science and Engineering Research Council of Canada; Swedish Research Council; Swedish Polar Research Secretariat; Swedish National Infrastructure for Computing (SNIC); Knut and Alice Wallenberg Foundation, Sweden; German Ministry for Education and Research (BMBF); Deutsche Forschungsgemeinschaft (DFG); Research Department of Plasmas with Complex Interactions (Bochum), Germany; Fund for Scientific Research (FNRS-FWO); FWO Odysseus Programme; Flanders Institute to encourage scientific and technological research in industry (IWT); Belgian Federal Science Policy Office (Belspo); University of Oxford, UK; Marsden Fund, New Zealand; Japan Society for Promotion of Science (JSPS); Swiss National Science Foundation (SNSF), Switzerland; EU; Capes Foundation, Ministry of Education of Brazil FX We acknowledge the support from the following agencies: U.S. National Science Foundation-Office of Polar Programs, U.S. National Science Foundation-Physics Division, University of Wisconsin Alumni Research Foundation, the Grid Laboratory Of Wisconsin (GLOW) grid infrastructure at the University of Wisconsin-Madison, the Open Science Grid (OSG) grid infrastructure; U.S. Department of Energy, and National Energy Research Scientific Computing Center, the Louisiana Optical Network Initiative (LONI) grid computing resources; National Science and Engineering Research Council of Canada; Swedish Research Council, Swedish Polar Research Secretariat, Swedish National Infrastructure for Computing (SNIC), and Knut and Alice Wallenberg Foundation, Sweden; German Ministry for Education and Research (BMBF), Deutsche Forschungsgemeinschaft (DFG), Research Department of Plasmas with Complex Interactions (Bochum), Germany; Fund for Scientific Research (FNRS-FWO), FWO Odysseus Programme, Flanders Institute to encourage scientific and technological research in industry (IWT), Belgian Federal Science Policy Office (Belspo); University of Oxford, UK; Marsden Fund, New Zealand; Japan Society for Promotion of Science (JSPS); the Swiss National Science Foundation (SNSF), Switzerland; A. Gross acknowledges support by the EU Marie Curie OIF Program; J. P. Rodrigues acknowledges support by the Capes Foundation, Ministry of Education of Brazil. NR 76 TC 93 Z9 93 U1 1 U2 6 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 MAY 1 PY 2011 VL 732 IS 1 AR 18 DI 10.1088/0004-637X/732/1/18 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 751OD UT WOS:000289626500018 ER PT J AU Ballard, S Christiansen, JL Charbonneau, D Deming, D Holman, MJ A'Hearn, MF Wellnitz, DD Barry, RK Kuchner, MJ Livengood, TA Hewagama, T Sunshine, JM Hampton, DL Lisse, CM Seager, S Veverka, JF AF Ballard, Sarah Christiansen, Jessie L. Charbonneau, David Deming, Drake Holman, Matthew J. A'Hearn, Michael F. Wellnitz, Dennis D. Barry, Richard K. Kuchner, Marc J. Livengood, Timothy A. Hewagama, Tilak Sunshine, Jessica M. Hampton, Don L. Lisse, Carey M. Seager, Sara Veverka, Joseph F. TI A SEARCH FOR ADDITIONAL PLANETS IN FIVE OF THE EXOPLANETARY SYSTEMS STUDIED BY THE NASA EPOXI MISSION SO ASTROPHYSICAL JOURNAL LA English DT Article DE eclipses; planetary systems; techniques: image processing; techniques: photometric ID TRANSIT LIGHT-CURVE; DEEP IMPACT MISSION; GIANT PLANET; KEPLER FIELD; HOT JUPITER; TRES-2; PARAMETERS; STAR; DYNAMICS; HAT-P-7B AB We present time series photometry and constraints on additional planets in five of the exoplanetary systems studied by the EPOCh (Extrasolar Planet Observation and Characterization) component of the NASA EPOXI mission: HAT-P-4, TrES-3, TrES-2, WASP-3, and HAT-P-7. We conduct a search of the high-precision time series for photometric transits of additional planets. We find no candidate transits with significance higher than our detection limit. From Monte Carlo tests of the time series using putative periods from 0.5 days to 7 days, we demonstrate the sensitivity to detect Neptune-sized companions around TrES-2, sub-Saturn-sized companions in the HAT-P-4, TrES-3, and WASP-3 systems, and Saturn-sized companions around HAT-P-7. We investigate in particular our sensitivity to additional transits in the dynamically favorable 3: 2 and 2: 1 exterior resonances with the known exoplanets: if we assume coplanar orbits with the known planets, then companions in these resonances with HAT-P-4b, WASP-3b, and HAT-P-7b would be expected to transit, and we can set lower limits on the radii of companions in these systems. In the nearly grazing exoplanetary systems TrES-3 and TrES-2, additional coplanar planets in these resonances are not expected to transit. However, we place lower limits on the radii of companions that would transit if the orbits were misaligned by 2 degrees.0 and 1 degrees.4 for TrES-3 and TrES-2, respectively. C1 [Ballard, Sarah; Charbonneau, David; Holman, Matthew J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Christiansen, Jessie L.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Deming, Drake; Barry, Richard K.; Kuchner, Marc J.; Livengood, Timothy A.; Hewagama, Tilak] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [A'Hearn, Michael F.; Wellnitz, Dennis D.; Hewagama, Tilak; Sunshine, Jessica M.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Hampton, Don L.] Univ Alaska Fairbanks, Inst Geophys, Fairbanks, AK 99775 USA. [Lisse, Carey M.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Seager, Sara] MIT, Cambridge, MA 02139 USA. [Veverka, Joseph F.] Cornell Univ, Dept Space Sci, Ithaca, NY 14853 USA. RP Ballard, S (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM sballard@cfa.harvard.edu RI Wellnitz, Dennis/B-4080-2012; Hewagama, T/C-8488-2012; Livengood, Timothy/C-8512-2012; Lisse, Carey/B-7772-2016; OI Lisse, Carey/0000-0002-9548-1526; Charbonneau, David/0000-0002-9003-484X FU National Aeronautics and Space Administration [NNX08AB64A, NNX08AD05A] FX Support for this work was provided by the EPOXI Project of the National Aeronautics and Space Administration's Discovery Program via funding to the Goddard Space Flight Center, and to Harvard University via Co-operative Agreement NNX08AB64A, and to the Smithsonian Astrophysical Observatory via Co-operative Agreement NNX08AD05A. NR 33 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 J9 ASTROPHYS J JI Astrophys. J. PD MAY 1 PY 2011 VL 732 IS 1 AR 41 DI 10.1088/0004-637X/732/1/41 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 751OD UT WOS:000289626500041 ER PT J AU Bhat, NDR Cordes, JM Cox, PJ Deneva, JS Hankins, TH Lazio, TJW McLaughlin, MA AF Bhat, N. D. R. Cordes, J. M. Cox, P. J. Deneva, J. S. Hankins, T. H. Lazio, T. J. W. McLaughlin, M. A. TI AN ARECIBO SEARCH FOR PULSARS AND TRANSIENT SOURCES IN M33 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: individual (M33); pulsars: general; pulsars: individual (Crab pulsar, B0045+33, J0628+0909); surveys ID GIANT PULSES; X-RAY; NEUTRON-STARS; CRAB PULSAR; GAMMA-RAY; STATISTICAL PROPERTIES; MILLISECOND PULSARS; RADIO TRANSIENTS; TELESCOPE; GALAXIES AB We report on a systematic and sensitive search for pulsars and transient sources in the nearby spiral galaxy M33, conducted at 1.4 GHz with the Arecibo telescope's seven-beam receiver system, ALFA. Data were searched for both periodic and aperiodic sources, up to 1000 pc cm(-3) in dispersion measure and on timescales from similar to 50 mu s to several seconds. The galaxy was sampled with 12 ALFA pointings, or 84 pixels in total, each of which was searched for 2-3 hr. We describe the observations, search methodologies, and analysis strategies applicable to multibeam systems, and comment on the data quality and statistics of spurious events that arise due to radio frequency interference. While these searches have not led to any conclusive signals of periodic or transient nature that originate in the galaxy, they illustrate some of the underlying challenges and difficulties in such searches and the efficacy of simultaneous multiple beams in the analysis of search output. The implied limits are less than or similar to 5 mu Jy Mpc(2) in luminosity (at 1400 MHz) for periodic sources in M33 with duty cycles less than or similar to 5%. For short-duration transient signals (with pulse widths less than or similar to 100 mu s), the limiting peak flux density is 100 mJy, which would correspond to a 5 sigma detection of bright giant pulses (similar to 20 kJy) from Crab-like pulsars if located at the distance of M33. We discuss the implications of our null results for various source populations within the galaxy and comment on the future prospects to conduct even more sensitive searches with the upcoming next-generation instruments including the Square Kilometer Array and its pathfinders. C1 [Bhat, N. D. R.; Cox, P. J.] Swinburne Univ, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia. [Cordes, J. M.; Deneva, J. S.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. [Hankins, T. H.] New Mexico Inst Min & Technol, Dept Phys, Socorro, NM 87801 USA. [Lazio, T. J. W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Lazio, T. J. W.] SKA Program Dev Off, Manchester M13 9PL, Lancs, England. [McLaughlin, M. A.] W Virginia Univ, Dept Phys, Morgantown, WV 26506 USA. [McLaughlin, M. A.] Natl Radio Astron Observ, Green Bank, WV 24944 USA. RP Bhat, NDR (reprint author), Swinburne Univ, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia. RI Bhat, Ramesh/B-7396-2013; OI Cox, Peter/0000-0002-6157-3430 FU NSF [AST0807151, AST-0607492]; Swinburne University; ANSTO [06/07-O-02]; AAS; Alfred P. Sloan Fellowship; WVEPSCOR FX We thank Arun Venkataraman for his assistance in transport of the large data volume to Swinburne University. This research was supported by NSF grant AST0807151 to Cornell University and an internal grant from Swinburne University. N.D.R.B. acknowledges the support received through the ANSTO travel grant 06/07-O-02 and a research grant from AAS, and thanks Matthew Bailes for continued support and encouragement extended to this project. M.A.M. is supported by an Alfred P. Sloan Fellowship and by WVEPSCOR. T.H.H. acknowledges partial support from NSF grant AST-0607492. We thank Willem van Straten for fruitful discussions and Sarah Burke-Spolaor for software assistance related to event analysis. Part of this research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. We thank the referee, Scott Ransom, for providing comments that helped to improve the clarity of some parts of the paper. The Arecibo Observatory is operated by the National Astronomy and Ionosphere Center under a cooperative agreement to Cornell University. NR 44 TC 7 Z9 7 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 1 PY 2011 VL 732 IS 1 AR 14 DI 10.1088/0004-637X/732/1/14 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 751OD UT WOS:000289626500014 ER PT J AU Brodwin, M Stern, D Vikhlinin, A Stanford, SA Gonzalez, AH Eisenhardt, PR Ashby, MLN Bautz, M Dey, A Forman, WR Gettings, D Hickox, RC Jannuzi, BT Jones, C Mancone, C Miller, ED Moustakas, LA Ruel, J Snyder, G Zeimann, G AF Brodwin, M. Stern, D. Vikhlinin, A. Stanford, S. A. Gonzalez, A. H. Eisenhardt, P. R. Ashby, M. L. N. Bautz, M. Dey, A. Forman, W. R. Gettings, D. Hickox, R. C. Jannuzi, B. T. Jones, C. Mancone, C. Miller, E. D. Moustakas, L. A. Ruel, J. Snyder, G. Zeimann, G. TI X-RAY EMISSION FROM TWO INFRARED-SELECTED GALAXY CLUSTERS AT z > 1.4 IN THE IRAC SHALLOW CLUSTER SURVEY SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: clusters: individual (ISCS J1432.4+3250, ISCS J1438.1+3414); galaxies: distances and redshifts; galaxies: evolution ID DIGITAL SKY SURVEY; WIDE-FIELD SURVEY; VELOCITY DISPERSION; COMA CLUSTER; MASS; TEMPERATURE; LUMINOSITY; TELESCOPE; COSMOLOGY; ROBUST AB We report the X-ray detection of two z > 1.4 infrared-selected galaxy clusters from the IRAC Shallow Cluster Survey (ISCS). We present new data from the Hubble Space Telescope and the W. M. Keck Observatory that spectroscopically confirm cluster ISCS J1432.4+3250 at z = 1.49, the most distant of 18 confirmed z > 1 clusters in the ISCS to date. We also present new spectroscopy for ISCS J1438.1+3414, previously reported at z = 1.41, and measure its dynamical mass. Clusters ISCS J1432.4+3250 and ISCS J1438.1+3414 are detected in 36 ks and 143 ks Chandra exposures at significances of 5.2 sigma and 9.7 sigma, from which we measure total masses of log (M-200,M-LX/M-circle dot) = 14.4 +/- 0.2 and 14.35(-0.11)(+0.14), respectively. The consistency of the X-ray and dynamical properties of these high-redshift clusters further demonstrates that the ISCS is robustly detecting massive clusters to at least z = 1.5. C1 [Brodwin, M.; Vikhlinin, A.; Ashby, M. L. N.; Forman, W. R.; Jones, C.; Snyder, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Stern, D.; Eisenhardt, P. R.; Moustakas, L. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Stanford, S. A.; Zeimann, G.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. [Stanford, S. A.] Lawrence Livermore Natl Lab, Inst Geophys & Planetary Phys, Livermore, CA 94550 USA. [Gonzalez, A. H.; Gettings, D.; Mancone, C.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA. [Bautz, M.; Miller, E. D.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Dey, A.; Jannuzi, B. T.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Hickox, R. C.] Univ Durham, Dept Phys, Durham DH1 3LE, England. [Ruel, J.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Brodwin, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA USA. RP Brodwin, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Moustakas, Leonidas/0000-0003-3030-2360 FU Chandra X-Ray Observatory [SV4-74018, A31]; Smithsonian Astrophysical Observatory; NASA [G09-0150A, NAS 5-26555]; JPL/Caltech; NASA through Space Telescope Science Institute [11597, 11663]; W. M. Keck Foundation; U.S. Department of Energy [W-7405-ENG-48] FX This work is based, in part, on observations obtained with the Chandra X-Ray Observatory under contract SV4-74018, A31 with the Smithsonian Astrophysical Observatory which operates Chandra for NASA. Support for this research was provided by NASA grant G09-0150A. This work is also based, in part, on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech. This work is based, in part, 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. These observations are associated with programs 11597 and 11663. Support for programs 11597 and 11663 were 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. Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. This work makes use of image data from the NOAO Deep Wide-Field Survey (NDWFS) and the Deep Lens Survey (DLS) as distributed by the NOAO Science Archive. NOAO is operated by the Association of Universities for Research in Astronomy (AURA), Inc., under a cooperative agreement with the National Science Foundation.; This paper would not have been possible without the efforts of the Spitzer, Chandra, HST, and Keck support staff. We thank C. Fedeli for helpful discussions on the evolution of the mass function. Support for M. B. was provided by the W. M. Keck Foundation. The work by S. A. S. at LLNL was performed under the auspices of the U.S. Department of Energy under contract No. W-7405-ENG-48. NR 60 TC 45 Z9 45 U1 0 U2 5 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 MAY 1 PY 2011 VL 732 IS 1 AR 33 DI 10.1088/0004-637X/732/1/33 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 751OD UT WOS:000289626500033 ER PT J AU Chaplin, WJ Kjeldsen, H Bedding, TR Christensen-Dalsgaard, J Gilliland, RL Kawaler, SD Appourchaux, T Elsworth, Y Garcia, RA Houdek, G Karoff, C Metcalfe, TS Molenda-Zakowicz, J Monteiro, MJPFG Thompson, MJ Verner, GA Batalha, N Borucki, WJ Brown, TM Bryson, ST Christiansen, JL Clarke, BD Jenkins, JM Klaus, TC Koch, D An, D Ballot, J Basu, S Benomar, O Bonanno, A Broomhall, AM Campante, TL Corsaro, E Creevey, OL Esch, L Gai, N Gaulme, P Hale, SJ Handberg, R Hekker, S Huber, D Mathur, S Mosser, B New, R Pinsonneault, MH Pricopi, D Quirion, PO Regulo, C Roxburgh, IW Salabert, D Stello, D Suran, MD AF Chaplin, W. J. Kjeldsen, H. Bedding, T. R. Christensen-Dalsgaard, J. Gilliland, R. L. Kawaler, S. D. Appourchaux, T. Elsworth, Y. Garcia, R. A. Houdek, G. Karoff, C. Metcalfe, T. S. Molenda-Zakowicz, J. Monteiro, M. J. P. F. G. Thompson, M. J. Verner, G. A. Batalha, N. Borucki, W. J. Brown, T. M. Bryson, S. T. Christiansen, J. L. Clarke, B. D. Jenkins, J. M. Klaus, T. C. Koch, D. An, D. Ballot, J. Basu, S. Benomar, O. Bonanno, A. Broomhall, A. -M. Campante, T. L. Corsaro, E. Creevey, O. L. Esch, L. Gai, N. Gaulme, P. Hale, S. J. Handberg, R. Hekker, S. Huber, D. Mathur, S. Mosser, B. New, R. Pinsonneault, M. H. Pricopi, D. Quirion, P. -O. Regulo, C. Roxburgh, I. W. Salabert, D. Stello, D. Suran, M. D. TI PREDICTING THE DETECTABILITY OF OSCILLATIONS IN SOLAR-TYPE STARS OBSERVED BY KEPLER SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars: interiors; stars: late-type; stars: oscillations ID MAIN-SEQUENCE STARS; THEORETICAL ISOCHRONES; PHOTOMETRIC SYSTEMS; HR DIAGRAM; ASTEROSEISMOLOGY; CONVECTION; MISSION; AMPLITUDES; PARAMETERS; EVOLUTION AB Asteroseismology of solar-type stars has an important part to play in the exoplanet program of the NASA Kepler Mission. Precise and accurate inferences on the stellar properties that are made possible by the seismic data allow very tight constraints to be placed on the exoplanetary systems. Here, we outline how to make an estimate of the detectability of solar-like oscillations in any given Kepler target, using rough estimates of the temperature and radius, and the Kepler apparent magnitude. C1 [Chaplin, W. J.; Elsworth, Y.; Verner, G. A.; Broomhall, A. -M.; Hale, S. J.; Hekker, S.] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. [Kjeldsen, H.; Christensen-Dalsgaard, J.; Karoff, C.; Campante, T. L.; Handberg, R.] Aarhus Univ, Dept Phys & Astron, DK-8000 Aarhus, Denmark. [Bedding, T. R.; Huber, D.; Stello, D.] Univ Sydney, Sch Phys, Sydney Inst Astron SIfA, Sydney, NSW 2006, Australia. [Gilliland, R. L.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Kawaler, S. D.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. [Appourchaux, T.; Benomar, O.; Gaulme, P.] Univ Paris 11, Inst Astrophys Spatiale, CNRS, UMR8617, F-91405 Orsay, France. [Garcia, R. A.] Univ Paris Diderot, IRFU SAp, CNRS, CEA DSM,Lab AIM, F-91191 Gif Sur Yvette, France. [Houdek, G.] Univ Vienna, Inst Astron, A-1180 Vienna, Austria. [Metcalfe, T. S.; Thompson, M. J.; Mathur, S.] Natl Ctr Atmospher Res, High Altitude Observ, Boulder, CO 80307 USA. [Metcalfe, T. S.; Thompson, M. J.; Huber, D.] Natl Ctr Atmospher Res, Div Comp Sci, Boulder, CO 80307 USA. [Molenda-Zakowicz, J.] Univ Wroclaw, Astron Inst, PL-51622 Wroclaw, Poland. [Monteiro, M. J. P. F. G.; Campante, T. L.] Univ Porto, Ctr Astrofis, P-4150762 Oporto, Portugal. [Monteiro, M. J. P. F. G.; Campante, T. L.] Univ Porto, Fac Ciencias, P-4150762 Oporto, Portugal. [Verner, G. A.; Roxburgh, I. W.] Univ London, Astron Unit, London E1 4NS, England. [Christiansen, J. L.; Clarke, B. D.; Jenkins, J. M.] NASA, Ames Res Ctr, SETI Inst, Moffett Field, CA 94035 USA. [Brown, T. M.] Las Cumbres Observ Global Telescope, Goleta, CA 93117 USA. [Klaus, T. C.] NASA, Ames Res Ctr, Orbital Sci Corp, Moffett Field, CA 94035 USA. [An, D.] Ewha Womans Univ, Dept Sci Educ, Seoul 120750, South Korea. [Ballot, J.] Univ Toulouse, CNRS, Inst Rech Astrophys & Planetol, F-31400 Toulouse, France. [Basu, S.; Esch, L.; Gai, N.] Yale Univ, Dept Astron, New Haven, CT 06520 USA. [Bonanno, A.; Corsaro, E.] INAF Osservatorio Astrofis Catania, I-95123 Catania, Italy. [Creevey, O. L.; Regulo, C.; Salabert, D.] Univ La Laguna, Dept Astrofis, E-38206 Tenerife, Spain. [Creevey, O. L.; Regulo, C.; Salabert, D.] Inst Astrofis Canarias, E-38200 Tenerife, Spain. [Gai, N.] Beijing Normal Univ, Beijing 100875, Peoples R China. [Hekker, S.] Univ Amsterdam, Astron Inst, NL-1090 GE Amsterdam, Netherlands. [Mosser, B.] Univ Paris 07, Univ Paris 06, Observ Paris, CNRS,LESIA, F-92195 Meudon, France. [New, R.] Sheffield Hallam Univ, Mat Engn Res Inst, Fac Arts Comp Engn & Sci, Sheffield S1 1WB, S Yorkshire, England. [Pinsonneault, M. H.] Ohio State Univ, Dept Astron, McPherson Lab 4055, Columbus, OH 43210 USA. [Pricopi, D.; Suran, M. D.] Acad Romana, Astron Inst, RO-40557 Bucharest, Romania. [Quirion, P. -O.] Canadian Space Agcy, St Hubert, PQ J3Y 8Y9, Canada. RP Chaplin, WJ (reprint author), Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. RI Ballot, Jerome/G-1019-2010; Monteiro, Mario J.P.F.G./B-4715-2008; Hale, Steven/E-3472-2015; OI Kawaler, Steven/0000-0002-6536-6367; Monteiro, Mario J.P.F.G./0000-0003-0513-8116; Hale, Steven/0000-0002-6402-8382; Bonanno, Alfio/0000-0003-3175-9776; Bedding, Timothy/0000-0001-5943-1460; Metcalfe, Travis/0000-0003-4034-0416; Bedding, Tim/0000-0001-5222-4661; Basu, Sarbani/0000-0002-6163-3472; Garcia, Rafael/0000-0002-8854-3776 FU NASA's Science Mission Directorate; UK Science and Technology Facilities Council (STFC); Netherlands Organisation for Scientific Research (NWO); National Science Foundation; International Space Science Institute (ISSI) FX Funding for this Discovery mission is provided by NASA's Science Mission Directorate. The authors wish to thank the entire Kepler team, without whom these results would not be possible. We also thank all funding councils and agencies that have supported the activities of KASC Working Group 1. W.J.C., Y.E., S.J.H., and G.A.V. acknowledge the support of the UK Science and Technology Facilities Council (STFC). S.H. acknowledges support from the Netherlands Organisation for Scientific Research (NWO). NCAR is supported by the National Science Foundation. We are also grateful for support from the International Space Science Institute (ISSI). NR 43 TC 48 Z9 49 U1 0 U2 5 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 MAY 1 PY 2011 VL 732 IS 1 AR 54 DI 10.1088/0004-637X/732/1/54 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 751OD UT WOS:000289626500054 ER PT J AU Cognard, I Guillemot, L Johnson, TJ Smith, DA Venter, C Harding, AK Wolff, MT Cheung, CC Donato, D Abdo, AA Ballet, J Camilo, F Desvignes, G Dumora, D Ferrara, EC Freire, PCC Grove, JE Johnston, S Keith, M Kramer, M Lyne, AG Michelson, PF Parent, D Ransom, SM Ray, PS Romani, RW Parkinson, PMS Stappers, BW Theureau, G Thompson, DJ Weltevrede, P Wood, KS AF Cognard, I. Guillemot, L. Johnson, T. J. Smith, D. A. Venter, C. Harding, A. K. Wolff, M. T. Cheung, C. C. Donato, D. Abdo, A. A. Ballet, J. Camilo, F. Desvignes, G. Dumora, D. Ferrara, E. C. Freire, P. C. C. Grove, J. E. Johnston, S. Keith, M. Kramer, M. Lyne, A. G. Michelson, P. F. Parent, D. Ransom, S. M. Ray, P. S. Romani, R. W. Parkinson, P. M. Saz Stappers, B. W. Theureau, G. Thompson, D. J. Weltevrede, P. Wood, K. S. TI DISCOVERY OF TWO MILLISECOND PULSARS IN FERMI SOURCES WITH THE NANCAY RADIO TELESCOPE SO ASTROPHYSICAL JOURNAL LA English DT Article DE gamma rays: general; pulsars: general; pulsars: individual (J2017+0603, J2302+4442) ID LARGE-AREA TELESCOPE; GAMMA-RAY PULSARS; LIGHT CURVES; MONTE-CARLO; EMISSION; CATALOG; POPULATION; BINARY; RADIATION; TUCANAE AB We report the discovery of two millisecond pulsars in a search for radio pulsations at the positions of Fermi-Large Area Telescope sources with no previously known counterparts, using the Nancay Radio Telescope. The two millisecond pulsars, PSRs J2017+0603 and J2302+4442, have rotational periods of 2.896 and 5.192 ms and are both in binary systems with low-eccentricity orbits and orbital periods of 2.2 and 125.9 days, respectively, suggesting long recycling processes. Gamma-ray pulsations were subsequently detected for both objects, indicating that they power the associated Fermi sources in which they were found. The gamma-ray light curves and spectral properties are similar to those of previously detected gamma-ray millisecond pulsars. Detailed modeling of the observed radio and gamma-ray light curves shows that the gamma-ray emission seems to originate at high altitudes in their magnetospheres. Additionally, X-ray observations revealed the presence of an X-ray source at the position of PSR J2302+4442, consistent with thermal emission from a neutron star. These discoveries along with the numerous detections of radio-loud millisecond pulsars in gamma rays suggest that many Fermi sources with no known counterpart could be unknown millisecond pulsars. C1 [Cognard, I.; Theureau, G.] Univ Orleans, CNRS, LPC2E, F-45071 Orleans 02, France. [Cognard, I.; Theureau, G.] Observ Paris, CNRS, INSU, Stn Radioastron Nancay, F-18330 Nancay, France. [Guillemot, L.; Freire, P. C. C.; Kramer, M.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Johnson, T. J.; Harding, A. K.; Ferrara, E. C.; Thompson, D. J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Johnson, T. J.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA. [Johnson, T. J.; Donato, D.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Smith, D. A.; Dumora, D.] Univ Bordeaux 1, CNRS, IN2P3, Ctr Etud Nucleaires Bordeaux Gradignan, F-33175 Gradignan, France. [Venter, C.] North West Univ, ZA-2520 Potchefstroom, South Africa. [Wolff, M. T.; Grove, J. E.; Ray, P. S.; Wood, K. S.] USN, Res Lab, Div Space Sci, Washington, DC 20375 USA. [Cheung, C. C.; Abdo, A. A.] Natl Acad Sci, Natl Res Council, Washington, DC 20001 USA. [Donato, D.] CRESST, Greenbelt, MD 20771 USA. [Donato, D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Ballet, J.] Univ Paris Diderot, CNRS, CEA IRFU, Lab AIM,Serv Astrophys,CEA Saclay, F-91191 Gif Sur Yvette, France. [Camilo, F.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Desvignes, G.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Desvignes, G.] Univ Calif Berkeley, Radio Astron Lab, Berkeley, CA 94720 USA. [Johnston, S.; Keith, M.] CSIRO, Australia Telescope Natl Facil, Epping, NSW 1710, Australia. [Kramer, M.; Lyne, A. G.; Stappers, B. W.; Weltevrede, P.] Univ Manchester, Jodrell Bank Ctr Astrophys, Sch Phys & Astron, Manchester M13 9PL, Lancs, England. [Michelson, P. F.; Romani, R. W.] Stanford Univ, WW Hansen Expt Phys Lab, Kavli Inst Particle Astrophys & Cosmol, Dept Phys, Stanford, CA 94305 USA. [Michelson, P. F.; Romani, R. W.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA. [Parent, D.] George Mason Univ, Coll Sci, Fairfax, VA 22030 USA. [Ransom, S. M.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. [Parkinson, P. M. Saz] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Dept Phys, Santa Cruz, CA 95064 USA. [Parkinson, P. M. Saz] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. RP Cognard, I (reprint author), Univ Orleans, CNRS, LPC2E, F-45071 Orleans 02, France. EM icognard@cnrs-orleans.fr; guillemo@mpifr-bonn.mpg.de; tyrel.j.johnson@gmail.com RI Thompson, David/D-2939-2012; Harding, Alice/D-3160-2012; Venter, Christo/E-6884-2011; OI Thompson, David/0000-0001-5217-9135; Venter, Christo/0000-0002-2666-4812; Ransom, Scott/0000-0001-5799-9714; Ray, Paul/0000-0002-5297-5278 FU Science and Technology Facilities Council of the United Kingdom FX The Nancay Radio Observatory is operated by the Paris Observatory, associated with the French Centre National de la Recherche Scientifique. The Green Bank Telescope is operated by the National Radio Astronomy Observatory, a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. The Lovell Telescope is owned and operated by the University of Manchester as part of the Jodrell Bank Centre for Astrophysics with support from the Science and Technology Facilities Council of the United Kingdom. NR 63 TC 46 Z9 46 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 MAY 1 PY 2011 VL 732 IS 1 AR 47 DI 10.1088/0004-637X/732/1/47 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 751OD UT WOS:000289626500047 ER PT J AU Currie, T Sicilia-Aguilar, A AF Currie, Thayne Sicilia-Aguilar, Aurora TI THE TRANSITIONAL PROTOPLANETARY DISK FREQUENCY AS A FUNCTION OF AGE: DISK EVOLUTION IN THE CORONET CLUSTER, TAURUS, AND OTHER 1-8 Myr OLD REGIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE planets and satellites: formation; protoplanetary disks; stars: pre-main sequence ID YOUNG STELLAR OBJECTS; SPECTRAL ENERGY-DISTRIBUTIONS; SPITZER-SPACE-TELESCOPE; MAIN-SEQUENCE STARS; LOW-MASS STARS; 2-DIMENSIONAL RADIATIVE-TRANSFER; ETA CHAMAELEONTIS CLUSTER; CIRCUMSTELLAR DUST DISKS; DEBRIS DISKS; PLANET FORMATION AB We present Spitzer 3.6-24 mu m photometry and spectroscopy for stars in the 1-3 Myr old Coronet Cluster, expanding upon the survey of Sicilia-Aguilar et al. Using sophisticated radiative transfer models, we analyze these new data and those from Sicilia-Aguilar et al. to identify disks with evidence for substantial dust evolution consistent with disk clearing: transitional disks. We then analyze data in Taurus and others young clusters-IC 348, NGC 2362, and eta Cha-to constrain the transitional disk frequency as a function of time. Our analysis confirms previous results finding evidence for two types of transitional disks-those with inner holes and those that are homologously depleted. The percentage of disks in the transitional phase increases from similar to 15%-20% at 1-2 Myr to >= 50% at 5-8 Myr; the mean transitional disk lifetime is closer to similar to 1 Myr than 0.1-0.5 Myr, consistent with previous studies by Currie et al. and Sicilia-Aguilar et al. In the Coronet Cluster and IC 348, transitional disks are more numerous for very low mass M3-M6 stars than for more massive K5-M2 stars, while Taurus lacks a strong spectral-type-dependent frequency. Assuming standard values for the gas-to-dust ratio and other disk properties, the lower limit for the masses of optically thick primordial disks is M-disk approximate to 0.001-0.003 M-star. We find that single color-color diagrams do not by themselves uniquely identify transitional disks or primordial disks. Full spectral energy distribution modeling is required to accurately assess disk evolution for individual sources and inform statistical estimates of the transitional disk population in large samples using mid-IR colors. C1 [Currie, Thayne] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Sicilia-Aguilar, Aurora] Max Planck Inst Astron, D-69117 Heidelberg, Germany. RP Currie, T (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. FU NASA; Deutsche Forschungsgemeinschaft (DFG) [SI-1486/1-1] FX The anonymous referee provided comments and suggestions that greatly improved the organization and content of this paper. We thank Cornelis Dullemond, Thomas Henning, Scott Kenyon, James Muzerolle, Carol Grady, Adam Kraus, and Meredith Hughes for useful conversations and suggestions. We also thank Richard Alexander for providing us with output from his disk evolution models presented in Alexander & Armitage (2009). Finally, we thank Jeroen Bouwman for assistance with our IRS data reduction. T.C. is supported by a NASA Postdoctoral Fellowship; A.S-A. acknowledges support from the Deutsche Forschungsgemeinschaft (DFG) grant SI-1486/1-1. This work made extensive use of the SIMBAD Astronomical Database. NR 122 TC 48 Z9 48 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 MAY 1 PY 2011 VL 732 IS 1 AR 24 DI 10.1088/0004-637X/732/1/24 PG 35 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 751OD UT WOS:000289626500024 ER PT J AU Kashlinsky, A Atrio-Barandela, F Ebeling, H AF Kashlinsky, A. Atrio-Barandela, F. Ebeling, H. TI MEASURING THE DARK FLOW WITH PUBLIC X-RAY CLUSTER DATA SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmic background radiation; cosmology: observations; early universe; inflation; large-scale structure of universe ID SCALE PECULIAR VELOCITIES; LOCAL GROUP; MILKY-WAY; GALAXIES; ANISOTROPY; SAMPLE; SPECTROSCOPY; PHOTOMETRY; CATALOG; SEARCH AB We present new results on the "dark flow" from a measurement of the dipole in the distribution of peculiar velocities of galaxy clusters, applying the methodology proposed and developed by us earlier. Our latest measurement is conducted using new, low-noise 7 yr WMAP data as well as an all-sky sample of X-ray-selected galaxy clusters compiled exclusively from published catalogs. Our analysis of the cosmic microwave background signature of the kinematic Sunyaev-Zel'dovich (SZ) effect finds a statistically significant dipole at the location of galaxy clusters. The residual dipole outside the cluster regions is small, rendering our overall measurement 3s-4s significant. The amplitude of the dipole correlates with cluster properties, being larger for the most X-ray luminous clusters, as required if the signal is produced by the SZ effect. Since it is measured at zero monopole, the dipole cannot be due to the thermal SZ effect. Our results are consistent with those obtained earlier by us from 5 yr WMAP data and using a proprietary cluster catalog. In addition, they are robust to quadrupole removal, demonstrating that quadrupole leakage contributes negligibly to the signal. The lower noise of the 7 yr WMAP also allows us, for the first time, to obtain tentative empirical confirmation of our earlier conjecture that the adopted filtering alters the sign of the kinematic SZ (KSZ) effect for realistic clusters and thus of the deduced direction of the flow. The latter is consistent with our earlier measurement in both the amplitude and direction. Assuming the filtering indeed alters the sign of the KSZ effect from the clusters, the direction agrees well also with the results of independent work using galaxies as tracers at lower distances. We make all maps and cluster templates derived by us from public data available to the scientific community to allow independent tests of our method and findings. C1 [Kashlinsky, A.] Goddard Space Flight Ctr, SSAI, Greenbelt, MD 20771 USA. [Kashlinsky, A.] Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA. [Atrio-Barandela, F.] Univ Salamanca, E-37008 Salamanca, Spain. [Ebeling, H.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. RP Kashlinsky, A (reprint author), Goddard Space Flight Ctr, SSAI, Code 665, Greenbelt, MD 20771 USA. EM alexander.kashlinsky@nasa.gov RI Atrio-Barandela, Fernando/A-7379-2017 OI Atrio-Barandela, Fernando/0000-0002-2130-2513 FU Spanish Ministerio de Educacion y Ciencia/Junta de Castilla y Leon [NNG04G089G/09-ADP09-0050, FIS2009-07238/GR-234/SyEC CSD 2007-00050] FX We acknowledge NASA NNG04G089G/09-ADP09-0050 and FIS2009-07238/GR-234/SyEC CSD 2007-00050 grants from Spanish Ministerio de Educacion y Ciencia/Junta de Castilla y Leon. We thank our collaborators on the SCOUT/"dark flow" project, Dale Kocevski and Alastair Edge, for their numerous valuable contributions to the project. NR 36 TC 34 Z9 35 U1 0 U2 3 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 MAY 1 PY 2011 VL 732 IS 1 AR 1 DI 10.1088/0004-637X/732/1/1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 751OD UT WOS:000289626500001 ER PT J AU Minton, DA Malhotra, R AF Minton, David A. Malhotra, Renu TI SECULAR RESONANCE SWEEPING OF THE MAIN ASTEROID BELT DURING PLANET MIGRATION SO ASTROPHYSICAL JOURNAL LA English DT Article DE celestial mechanics; minor planets, asteroids: general; planets and satellites: dynamical evolution and stability ID LATE HEAVY BOMBARDMENT; SOLAR-SYSTEM; ORBITAL EVOLUTION; KUIPER-BELT; ORIGIN; NEPTUNE; SIMULATIONS; CONSTRAINTS; IMPACTORS; NEBULA AB We calculate the eccentricity excitation of asteroids produced by the sweeping nu(6) secular resonance during the epoch of planetesimal-driven giant planet migration in the early history of the solar system. We derive analytical expressions for the magnitude of the eccentricity change and its dependence on the sweep rate and on planetary parameters; the nu(6) sweeping leads to either an increase or a decrease of eccentricity depending on an asteroid's initial orbit. Based on the slowest rate of nu(6) sweeping that allows a remnant asteroid belt to survive, we derive a lower limit on Saturn's migration speed of similar to 0.15 AU Myr(-1) during the era that the nu(6) resonance swept through the inner asteroid belt (semimajor axis range 2.1-2.8 AU). This rate limit is for Saturn's current eccentricity and scales with the square of its eccentricity; the limit on Saturn's migration rate could be lower if its eccentricity were lower during its migration. Applied to an ensemble of fictitious asteroids, our calculations show that a prior single-peaked distribution of asteroid eccentricities would be transformed into a double-peaked distribution due to the sweeping of the nu(6) resonance. Examination of the orbital data of main belt asteroids reveals that the proper eccentricities of the known bright (H <= 10.8) asteroids may be consistent with a double-peaked distribution. If so, our theoretical analysis then yields two possible solutions for the migration rate of Saturn and for the dynamical states of the pre-migration asteroid belt: a dynamically cold state (single-peaked eccentricity distribution with mean of similar to 0.05) linked with Saturn'smigration speed similar to 4 AU Myr(-1) or a dynamically hot state (single-peaked eccentricity distribution with mean of similar to 0.3) linked with Saturn's migration speed similar to 0.8 AU Myr(-1). C1 [Minton, David A.] SW Res Inst, Boulder, CO 80302 USA. [Minton, David A.] NASA, Lunar Sci Inst, Boulder, CO 80302 USA. [Malhotra, Renu] Univ Arizona, Dept Planetary Sci, Tucson, AZ 85721 USA. RP Minton, DA (reprint author), SW Res Inst, 1050 Walnut St,Suite 300, Boulder, CO 80302 USA. EM daminton@boulder.swri.edu; renu@lpl.arizona.edu OI Malhotra, Renu/0000-0002-1226-3305 FU NSF [AST-0806828]; NASA:NESSF [NNX08AW25H]; NASA NLSI/CLOE [NNA09DB32A] FX The authors thank the anonymous reviewer and the editor Eric Feigelson for useful comments. This research was supported in part by NSF grant no. AST-0806828 and NASA:NESSF grant no. NNX08AW25H. The work of David Minton was additionally partially supported by NASA NLSI/CLOE research grant no. NNA09DB32A NR 42 TC 30 Z9 30 U1 0 U2 8 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAY 1 PY 2011 VL 732 IS 1 AR 53 DI 10.1088/0004-637X/732/1/53 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 751OD UT WOS:000289626500053 ER PT J AU Muchovej, S Leitch, E Carlstrom, JE Culverhouse, T Greer, C Hawkins, D Hennessy, R Joy, M Lamb, J Loh, M Marrone, DP Miller, A Mroczkowski, T Pryke, C Sharp, M Woody, D AF Muchovej, Stephen Leitch, Erik Carlstrom, John E. Culverhouse, Thomas Greer, Chris Hawkins, David Hennessy, Ryan Joy, Marshall Lamb, James Loh, Michael Marrone, Daniel P. Miller, Amber Mroczkowski, Tony Pryke, Clem Sharp, Matthew Woody, David TI COSMOLOGICAL CONSTRAINTS FROM A 31 GHz SKY SURVEY WITH THE SUNYAEV-ZEL'DOVICH ARRAY SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmic background radiation; cosmology: observations; galaxies: clusters: general; large-scale structure of universe; surveys; techniques: interferometric ID SOUTH-POLE TELESCOPE; GALAXY CLUSTERS; POWER SPECTRUM; RADIO-SOURCES; ANISOTROPY; REDSHIFT; PROBE; PARAMETERS; PRECISION; UNIVERSE AB We present the results of an analysis of 4.4 deg(2) selected from a 6.1 deg(2) survey for clusters of galaxies via their Sunyaev-Zel'dovich effect at 31 GHz. From late 2005 to mid 2007, the Sunyaev-Zel'dovich Array observed four fields of roughly 1.5 deg(2) each. One of the fields shows evidence for significant diffuse Galactic emission, and is therefore excised from this analysis. We estimate the cluster detectability for the survey using mock observations of simulations of clusters of galaxies and determine that, at intermediate redshifts (z similar to 0.8), the survey is 50% complete to a limiting mass (M-200 (rho) over bar) of similar to 6.0 x 10(14) M-circle dot, with the mass limit decreasing at higher redshifts. We detect no clusters at a significance greater than five times the rms noise level in the maps, and place an upper limit on sigma(8), the amplitude of mass density fluctuations on a scale of 8 h(-1) Mpc, of 0.84 + 0.04 + 0.04 at 95% confidence, where the first uncertainty reflects an estimate of additional sample variance due to non-Gaussianity in the distribution of clusters and the second reflects calibration and systematic effects. This result is consistent with estimates from other cluster surveys and cosmic microwave background anisotropy experiments. C1 [Muchovej, Stephen; Hawkins, David; Lamb, James; Woody, David] Owens Valley Radio Observ, CALTECH, Big Pine, CA 93513 USA. [Muchovej, Stephen; Mroczkowski, Tony] Columbia Univ, Dept Astron, New York, NY 10027 USA. [Leitch, Erik; Carlstrom, John E.; Culverhouse, Thomas; Greer, Chris; Hennessy, Ryan; Loh, Michael; Marrone, Daniel P.; Pryke, Clem; Sharp, Matthew] Univ Chicago, Dept Astron & Astrophys, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Carlstrom, John E.] Univ Chicago, Dept Phys, Enrico Fermi Inst, Chicago, IL 60637 USA. [Joy, Marshall] NASA, Marshall Space Flight Ctr, Space Sci VP62, Huntsville, AL 35812 USA. [Miller, Amber] Columbia Univ, Columbia Astrophys Lab, Dept Phys, New York, NY 10027 USA. [Mroczkowski, Tony] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. RP Muchovej, S (reprint author), Owens Valley Radio Observ, CALTECH, Big Pine, CA 93513 USA. OI Marrone, Daniel/0000-0002-2367-1080; Mroczkowski, Tony/0000-0003-3816-5372 FU James S. McDonnell Foundation; National Science Foundation [AST-0507545, AST-05-07161]; University of Chicago; NSF Division of Astronomical Sciences [AST-0604982]; NSF Physics Frontier Center [PHY-0114422]; NASA [HST-HF-51259.01] FX We thank John Cartwright, Ben Reddall, and Marcus Runyan for their significant contributions to the construction and commissioning of the SZA instrument. We thank the staff of the Owens Valley Radio Observatory and CARMA for their outstanding support. We thank Bryan Butler and Mark Gurwell for providing the Mars model to which the SZA data are calibrated. We also thank Laurie Shaw and Martin White for providing us with the simulations used in this work. We gratefully acknowledge the James S. McDonnell Foundation, the National Science Foundation, and the University of Chicago for funding to construct the SZA. The operation of the SZA is supported by NSF Division of Astronomical Sciences through grant AST-0604982. Partial support is provided by NSF Physics Frontier Center grant PHY-0114422 to the Kavli Institute of Cosmological Physics at the University of Chicago, and by NSF grants AST-0507545 and AST-05-07161 to Columbia University. A. M. acknowledges support from a Sloan Fellowship, D. P. M. from a Hubble Fellowship under NASA grant HST-HF-51259.01, S. M. from an NSF Astronomy and Astrophysics Fellowship, and C. G., S. M., and M. S. from NSF Graduate Research Fellowships. NR 40 TC 9 Z9 9 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 MAY 1 PY 2011 VL 732 IS 1 AR 28 DI 10.1088/0004-637X/732/1/28 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 751OD UT WOS:000289626500028 ER PT J AU Raichoor, A Mei, S Nakata, F Stanford, SA Holden, BP Rettura, A Huertas-Company, M Postman, M Rosati, P Blakeslee, JP Demarco, R Eisenhardt, P Illingworth, G Jee, MJ Kodama, T Tanaka, M White, RL AF Raichoor, A. Mei, S. Nakata, F. Stanford, S. A. Holden, B. P. Rettura, A. Huertas-Company, M. Postman, M. Rosati, P. Blakeslee, J. P. Demarco, R. Eisenhardt, P. Illingworth, G. Jee, M. J. Kodama, T. Tanaka, M. White, R. L. TI EARLY-TYPE GALAXIES AT z similar to 1.3. II. MASSES AND AGES OF EARLY-TYPE GALAXIES IN DIFFERENT ENVIRONMENTS AND THEIR DEPENDENCE ON STELLAR POPULATION MODEL ASSUMPTIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: clusters: individual (RX J0849+4452, RX J0848+4453); galaxies: elliptical and lenticular, cD; galaxies: evolution; galaxies: formation; galaxies: high-redshift; galaxies: photometry ID HIGH-REDSHIFT GALAXIES; COLOR-MAGNITUDE RELATION; GIANT BRANCH STARS; DIGITAL SKY SURVEY; GOODS-SOUTH FIELD; VLT DEEP SURVEY; TP-AGB STARS; LUMINOSITY FUNCTION; LYNX SUPERCLUSTER; PASSIVE GALAXIES AB We have derived masses and ages for 79 early-type galaxies (ETGs) in different environments at z similar to 1.3 in the Lynx supercluster and in the GOODS/CDF-S field using multi-wavelength (0.6-4.5 mu m; KPNO, Palomar, Keck, Hubble Space Telescope, Spitzer) data sets. At this redshift the contribution of the thermally pulsing asymptotic giant branch (TP-AGB) phase is important for ETGs, and the mass and age estimates depend on the choice of the stellar population model used in the spectral energy distribution fits. We describe in detail the differences among model predictions for a large range of galaxy ages, showing the dependence of these differences on age. Current models still yield large uncertainties. While recent models from Maraston and Charlot & Bruzual offer better modeling of the TP-AGB phase with respect to less recent Bruzual & Charlot models, their predictions do not often match. The modeling of this TP-AGB phase has a significant impact on the derived parameters for galaxies observed at high redshift. Some of our results do not depend on the choice of the model: for all models, the most massive galaxies are the oldest ones, independent of the environment. When using the Maraston and Charlot & Bruzual models, the mass distribution is similar in the clusters and in the groups, whereas in our field sample there is a deficit of massive (M greater than or similar to 10(11) M-circle dot) ETGs. According to those last models, ETGs belonging to the cluster environment host on average older stars with respect to group and field populations. This difference is less significant than the age difference in galaxies of different masses. C1 [Raichoor, A.; Mei, S.; Huertas-Company, M.] Observ Paris, Sect Meudon, GEPI, F-92190 Meudon, France. [Mei, S.; Huertas-Company, M.] Univ Paris Denis Diderot, F-75205 Paris 13, France. [Mei, S.] CALTECH, Pasadena, CA 91125 USA. [Nakata, F.; Kodama, T.] Natl Inst Nat Sci, Natl Astron Observ Japan, Subaru Telescope, Hilo, HI 96720 USA. [Stanford, S. A.; Rettura, A.; Jee, M. J.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. [Stanford, S. A.] Lawrence Livermore Natl Lab, Inst Geophys & Planetary Phys, Livermore, CA 94551 USA. [Holden, B. P.; Illingworth, G.] Univ Calif Santa Cruz, Lick Observ, UCO, Santa Cruz, CA 95065 USA. [Rettura, A.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Postman, M.; White, R. L.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Rosati, P.] European S Observ, D-85748 Garching, Germany. [Blakeslee, J. P.] Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada. [Demarco, R.] Univ Concepcion, Dept Astron, Concepcion, Chile. [Eisenhardt, P.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Kodama, T.] Natl Inst Nat Sci, Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan. [Tanaka, M.] Univ Tokyo, Inst Phys & Math Universe, Kashiwa, Chiba 2778583, Japan. RP Raichoor, A (reprint author), Osserv Astron Brera, Via Brera 28, I-20121 Milan, Italy. EM anand.raichoor@brera.inaf.it OI Blakeslee, John/0000-0002-5213-3548 FU NASA [NAS 5-32865, NAS5-26555]; NASA HST [GO-10574.01-A]; Spitzer [20694]; W. M. Keck Foundation FX ACS was developed under NASA contract NAS 5-32865. This research has been supported by the NASA HST grant GO-10574.01-A, and Spitzer grant for program 20694. The Space Telescope Science Institute is operated by AURA Inc., under NASA contract NAS5-26555. Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. The authors recognize and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. Some data were based on observations obtained at the Gemini Observatory, which is operated by the Association of Universities for Research in Astronomy, Inc., under a cooperative agreement with the NSF on behalf of the Gemini partnership: the National Science Foundation (United States), the Science and Technology Facilities Council (United Kingdom), the National Research Council (Canada), CONlCYT (Chile), the Australian Research Council (Australia), Ministrio da Cincia e Tecnologia (Brazil) and Ministerio de Ciencia, Tecnologa e Innovacin Productiva (Argentina), Gemini Science Program ID: GN-2006A-Q-78. We thank the anonymous referee for constructive comments. We thank Raphael Gobat and Veronica Strazzullo for useful discussions. NR 85 TC 17 Z9 17 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 MAY 1 PY 2011 VL 732 IS 1 AR 12 DI 10.1088/0004-637X/732/1/12 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 751OD UT WOS:000289626500012 ER PT J AU Rigby, JR Wuyts, E Gladders, MD Sharon, K Becker, GD AF Rigby, J. R. Wuyts, E. Gladders, M. D. Sharon, K. Becker, G. D. TI THE PHYSICAL CONDITIONS OF A LENSED STAR-FORMING GALAXY AT z=1.7 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: abundances; galaxies: evolution; galaxies: high-redshift; gravitational lensing: strong ID LYMAN BREAK GALAXY; MASS-METALLICITY RELATION; SIMILAR-TO 2; DIGITAL SKY SURVEY; H-II REGIONS; MS 1512-CB58; HII-REGIONS; ULTRAVIOLET-SPECTRUM; CHEMICAL-COMPOSITION; STELLAR POPULATIONS AB We report rest-frame optical Keck/NIRSPEC spectroscopy of the bright lensed galaxy RCSGA 032727-132609 at z = 1.7037. From precise measurements of the nebular lines, we infer a number of physical properties: redshift, extinction, star formation rate, ionization parameter, electron density, electron temperature, oxygen abundance, and N/O, Ne/O, and Ar/O abundance ratios. The limit on [O III] 4363 angstrom tightly constrains the oxygen abundance via the "direct" or T-e method, for the first time in an average-metallicity galaxy at z similar to 2. We compare this result to several standard "bright-line" O abundance diagnostics, thereby testing these empirically-calibrated diagnostics in situ. Finally, we explore the positions of lensed and unlensed galaxies in standard diagnostic diagrams, and the diversity of ionization conditions and mass-metallicity ratios at z = 2. C1 [Rigby, J. R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Wuyts, E.; Gladders, M. D.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Wuyts, E.; Gladders, M. D.; Sharon, K.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Becker, G. D.] Kavli Inst Cosmol, Cambridge, England. [Rigby, J. R.] Carnegie Inst Sci, Pasadena, CA 91101 USA. RP Rigby, JR (reprint author), NASA, Goddard Space Flight Ctr, Code 665, Greenbelt, MD 20771 USA. EM Jane.R.Rigby@nasa.gov RI Rigby, Jane/D-4588-2012 OI Rigby, Jane/0000-0002-7627-6551 FU Carnegie Fellowship; W.M. Keck Foundation FX We thank the IRTF Spex team for making public their telluric correction routine and their tool to find telluric standard stars, at http://irtfweb.ifa.hawaii.edu/similar to spex/. We thank Kevin Schawinski for code to generate the SDSS contours in Figure 7, which is adapted from Schawinski et al. (2010); we thank Fuyan Bian for code to generate Figure 6, which is adapted from Bian et al. (2010). We thank Andrew Marble for use of his implementation of MPFITFUN (Markwardt 2009) to fit multiple Gaussians. J.R.R. gratefully acknowledges the financial support and intellectual freedom of a Carnegie Fellowship.; Data presented herein were obtained at the W.M. Keck Observatory from telescope time allocated to the National Aeronautics and Space Administration through the agency's scientific partnership with the California Institute of Technology and the University of California. The Observatory was made possible by the generous financial support of the W.M. Keck Foundation. We 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 67 TC 39 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 MAY 1 PY 2011 VL 732 IS 1 AR 59 DI 10.1088/0004-637X/732/1/59 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 751OD UT WOS:000289626500059 ER PT J AU Searles, JM Destree, JD Snow, TP Salama, F York, DG Dahlstrom, J AF Searles, Justin M. Destree, Joshua D. Snow, Theodore P. Salama, Farid York, Donald G. Dahlstrom, Julie TI SEARCHING FOR NAPHTHALENE CATION ABSORPTION IN THE INTERSTELLAR MEDIUM SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: lines and bands; line: profiles; surveys ID ANOMALOUS MICROWAVE EMISSION; PULSED DISCHARGE NOZZLE; RING-DOWN SPECTROSCOPY; BANDS AB Interstellar naphthalene cations (C10H8+) have been proposed by a study to be the carriers of a small number of diffuse interstellar bands (DIBs). Using an archive of high signal-to-noise spectra obtained at the Apache Point Observatory, we used two methods to test the hypothesis. Both methods failed to detect significant absorption at lab wavelengths of interstellar spectra with laboratory spectra. We thereby conclude that C10H8+ is not a DIB carrier in typical reddened sight lines. C1 [Searles, Justin M.; Destree, Joshua D.; Snow, Theodore P.] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA. [Salama, Farid] NASA, Ames Res Ctr, Space Sci & Astrobiol Div, Moffett Field, CA 94035 USA. [York, Donald G.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [York, Donald G.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [Dahlstrom, Julie] Carthage Coll, Kenosha, WI 53140 USA. RP Searles, JM (reprint author), Univ Colorado, Ctr Astrophys & Space Astron, Campus Box 391, Boulder, CO 80309 USA. EM searlesj@colorado.edu; destree@colorado.edu; tsnow@casa.colorado.edu; Farid.Salama@nasa.gov; don@oddjob.uchicago.edu; jdahlstrom1@carthage.edu RI Salama, Farid/A-8787-2009 OI Salama, Farid/0000-0002-6064-4401 FU NASA [NNX08AC14G] FX This research was supported by NASA grant NNX08AC14G. NR 24 TC 12 Z9 12 U1 1 U2 9 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 MAY 1 PY 2011 VL 732 IS 1 AR 50 DI 10.1088/0004-637X/732/1/50 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 751OD UT WOS:000289626500050 ER PT J AU Sehgal, N Trac, H Acquaviva, V Ade, PAR Aguirre, P Amiri, M Appel, JW Barrientos, LF Battistelli, ES Bond, JR Brown, B Burger, B Chervenak, J Das, S Devlin, MJ Dicker, SR Doriese, WB Dunkley, J Dunner, R Essinger-Hileman, T Fisher, RP Fowler, JW Hajian, A Halpern, M Hasselfield, M Hernandez-Monteagudo, C Hilton, GC Hilton, M Hincks, AD Hlozek, R Holtz, D Huffenberger, KM Hughes, DH Hughes, JP Infante, L Irwin, KD Jones, A Juin, JB Klein, J Kosowsky, A Lau, JM Limon, M Lin, YT Lupton, RH Marriage, TA Marsden, D Martocci, K Mauskopf, P Menanteau, F Moodley, K Moseley, H Netterfield, CB Niemack, MD Nolta, MR Page, LA Parker, L Partridge, B Reid, B Sherwin, BD Sievers, J Spergel, DN Staggs, ST Swetz, DS Switzer, ER Thornton, R Tucker, C Warne, R Wollack, E Zhao, Y AF Sehgal, Neelima Trac, Hy Acquaviva, Viviana Ade, Peter A. R. Aguirre, Paula Amiri, Mandana Appel, John W. Felipe Barrientos, L. Battistelli, Elia S. Bond, J. Richard Brown, Ben Burger, Bryce Chervenak, Jay Das, Sudeep Devlin, Mark J. Dicker, Simon R. Doriese, W. Bertrand Dunkley, Joanna Duenner, Rolando Essinger-Hileman, Thomas Fisher, Ryan P. Fowler, Joseph W. Hajian, Amir Halpern, Mark Hasselfield, Matthew Hernandez-Monteagudo, Carlos Hilton, Gene C. Hilton, Matt Hincks, Adam D. Hlozek, Renee Holtz, David Huffenberger, Kevin M. Hughes, David H. Hughes, John P. Infante, Leopoldo Irwin, Kent D. Jones, Andrew Baptiste Juin, Jean Klein, Jeff Kosowsky, Arthur Lau, Judy M. Limon, Michele Lin, Yen-Ting Lupton, Robert H. Marriage, Tobias A. Marsden, Danica Martocci, Krista Mauskopf, Phil Menanteau, Felipe Moodley, Kavilan Moseley, Harvey Netterfield, Calvin B. Niemack, Michael D. Nolta, Michael R. Page, Lyman A. Parker, Lucas Partridge, Bruce Reid, Beth Sherwin, Blake D. Sievers, Jon Spergel, David N. Staggs, Suzanne T. Swetz, Daniel S. Switzer, Eric R. Thornton, Robert Tucker, Carole Warne, Ryan Wollack, Ed Zhao, Yue TI THE ATACAMA COSMOLOGY TELESCOPE: COSMOLOGY FROM GALAXY CLUSTERS DETECTED VIA THE SUNYAEV-ZEL'DOVICH EFFECT SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmic background radiation; cosmology: observations; galaxies: clusters: general ID SOUTH-POLE TELESCOPE; DIGITAL SKY SURVEY; BACKGROUND POWER SPECTRUM; TREE PARTICLE-MESH; X-RAY; RADIO-SOURCES; HYDRODYNAMICAL SIMULATIONS; PECULIAR VELOCITIES; SCALING RELATIONS; CATALOG AB We present constraints on cosmological parameters based on a sample of Sunyaev-Zel'dovich-selected (SZ-selected) galaxy clusters detected in a millimeter-wave survey by the Atacama Cosmology Telescope. The cluster sample used in this analysis consists of nine optically confirmed high-mass clusters comprising the high-significance end of the total cluster sample identified in 455 deg(2) of sky surveyed during 2008 at 148 GHz. We focus on the most massive systems to reduce the degeneracy between unknown cluster astrophysics and cosmology derived from SZ surveys. We describe the scaling relation between cluster mass and SZ signal with a four-parameter fit. Marginalizing over the values of the parameters in this fit with conservative priors gives sigma(8) = 0.851 +/- 0.115 and omega = -1.14 +/- 0.35 for a spatially flat wCDM cosmological model with Wilkinson Microwave Anisotropy Probe (WMAP) seven-year priors on cosmological parameters. This gives a modest improvement in statistical uncertainty over WMAP seven-year constraints alone. Fixing the scaling relation between the cluster mass and SZ signal to a fiducial relation obtained from numerical simulations and calibrated by X-ray observations, we find sigma(8) = 0.821 +/- 0.044 and omega = -1.05 +/- 0.20. These results are consistent with constraints from WMAP7 plus baryon acoustic oscillations plus Type Ia supernova which give sigma(8) = 0.802 +/- 0.038 and omega = -0.98 +/- 0.053. A stacking analysis of the clusters in this sample compared to clusters simulated assuming the fiducial model also shows good agreement. These results suggest that, given the sample of clusters used here, both the astrophysics of massive clusters and the cosmological parameters derived from them are broadly consistent with current models. C1 [Sehgal, Neelima; Lau, Judy M.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA. [Trac, Hy] Carnegie Mellon Univ, Dept Phys, Pittsburgh, PA 15213 USA. [Trac, Hy] Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Acquaviva, Viviana; Das, Sudeep; Dunkley, Joanna; Hajian, Amir; Lin, Yen-Ting; Lupton, Robert H.; Marriage, Tobias A.; Spergel, David N.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Acquaviva, Viviana; Menanteau, Felipe] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. [Ade, Peter A. R.; Mauskopf, Phil; Tucker, Carole] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Aguirre, Paula; Felipe Barrientos, L.; Duenner, Rolando; Infante, Leopoldo; Baptiste Juin, Jean; Lin, Yen-Ting] Pontificia Univ Catolica Chile, Fac Fis, Dept Astron & Astrofis, Santiago 22, Chile. [Amiri, Mandana; Battistelli, Elia S.; Burger, Bryce; Halpern, Mark; Hasselfield, Matthew] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z4, Canada. [Appel, John W.; Das, Sudeep; Dunkley, Joanna; Essinger-Hileman, Thomas; Fisher, Ryan P.; Fowler, Joseph W.; Hajian, Amir; Hincks, Adam D.; Holtz, David; Jones, Andrew; Lau, Judy M.; Limon, Michele; Martocci, Krista; Niemack, Michael D.; Page, Lyman A.; Parker, Lucas; Reid, Beth; Sherwin, Blake D.; Staggs, Suzanne T.; Switzer, Eric R.] Princeton Univ, Joseph Henry Labs Phys, Princeton, NJ 08544 USA. [Battistelli, Elia S.] Univ Roma La Sapienza, Dept Phys, I-00185 Rome, Italy. [Bond, J. Richard; Hajian, Amir; Nolta, Michael R.; Sievers, Jon] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada. [Brown, Ben; Kosowsky, Arthur] Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA. [Chervenak, Jay; Moseley, Harvey; Wollack, Ed; Zhao, Yue] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Das, Sudeep] Univ Calif Berkeley, Berkeley Ctr Cosmol Phys, LBL, Berkeley, CA 94720 USA. [Das, Sudeep] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Devlin, Mark J.; Dicker, Simon R.; Klein, Jeff; Limon, Michele; Marriage, Tobias A.; Swetz, Daniel S.; Thornton, Robert] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. [Doriese, W. Bertrand; Fowler, Joseph W.; Hilton, Gene C.; Irwin, Kent D.; Niemack, Michael D.; Swetz, Daniel S.] NIST, Quantum Devices Grp, Boulder, CO 80305 USA. [Dunkley, Joanna; Hlozek, Renee] Univ Oxford, Dept Astrophys, Oxford OX1 3RH, England. [Hernandez-Monteagudo, Carlos] Max Planck Inst Astrophys, D-85741 Garching, Germany. [Hilton, Matt; Moodley, Kavilan; Warne, Ryan] Univ KwaZulu Natal, Astrophys & Cosmol Res Unit, Sch Math Sci, ZA-4041 Durban, South Africa. [Hilton, Matt; Moodley, Kavilan] Ctr High Performance Comp, Cape Town, South Africa. [Huffenberger, Kevin M.] Univ Miami, Dept Phys, Coral Gables, FL 33124 USA. [Hughes, David H.] INAOE, Puebla, Mexico. [Lau, Judy M.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA. [Limon, Michele] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Lin, Yen-Ting] Univ Tokyo, Inst Phys & Math Universe, Chiba 2778568, Japan. [Marriage, Tobias A.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Martocci, Krista; Switzer, Eric R.] Kavli Inst Cosmol Phys, Lab Astrophys & Space Res, Chicago, IL 60637 USA. [Netterfield, Calvin B.] Univ Toronto, Dept Phys, Toronto, ON M5S 1A7, Canada. [Partridge, Bruce] Haverford Coll, Dept Phys & Astron, Haverford, PA 19041 USA. [Reid, Beth] Univ Barcelona, ICC, E-08028 Barcelona, Spain. [Thornton, Robert] W Chester Univ Penn, Dept Phys, W Chester, PA 19383 USA. RP Sehgal, N (reprint author), Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA. RI Klein, Jeffrey/E-3295-2013; Spergel, David/A-4410-2011; Hilton, Matthew James/N-5860-2013; Trac, Hy/N-8838-2014; Wollack, Edward/D-4467-2012; OI Trac, Hy/0000-0001-6778-3861; Wollack, Edward/0000-0002-7567-4451; Huffenberger, Kevin/0000-0001-7109-0099; Menanteau, Felipe/0000-0002-1372-2534; Sievers, Jonathan/0000-0001-6903-5074; /0000-0002-0896-8628; Limon, Michele/0000-0002-5900-2698 FU US National Science Foundation [AST-0408698, PHY-0355328, AST-0707731, PIRE-0507768]; Princeton University; University of Pennsylvania; Canada Foundation for Innovation; Compute Canada; Government of Ontario; Ontario Research Fund-Research Excellence; University of Toronto; U.S. Department of Energy [DE-AC3-76SF00515]; NASA [NNX08AH30G]; Natural Science and Engineering Research Council of Canada (NSERC); NSF Physics Frontier Center [PHY-0114422]; FONDAP Centro de Astrofisica; RCUK; South African National Research Foundation (NRF); Meraka Institute; South African Square Kilometer Array (SKA) Project; CONICYT; MECESUP; Fundacion Andes; Rhodes Trust; Berkeley Center for Cosmological Physics; World Premier International Research Center Initiative, MEXT, Japan; NASA Office of Space Science; [NSFAST-0546035]; [AST-0606975] FX This work was supported by the US National Science Foundation through awards AST-0408698 for the ACT project, and PHY-0355328, AST-0707731, and PIRE-0507768. Funding was also provided by Princeton University and the University of Pennsylvania. The PIRE program made possible exchanges between Chile, South Africa, Spain, and the US that enabled this research program. Computations were performed on the GPC supercomputer at the SciNet HPC Consortium. SciNet is funded by the Canada Foundation for Innovation under the auspices of Compute Canada, the Government of Ontario, Ontario Research Fund-Research Excellence, and the University of Toronto.; N.S. is supported by the U.S. Department of Energy contract to SLAC No. DE-AC3-76SF00515. A. H., T. M., S. D., and V. A. were supported through NASA grant NNX08AH30G. A. H. received additional support from a Natural Science and Engineering Research Council of Canada (NSERC) PGS-D scholarship. A. K. and B. P. were partially supported through NSFAST-0546035 and AST-0606975, respectively, for work on ACT. E. S. acknowledges support by NSF Physics Frontier Center grant PHY-0114422 to the Kavli Institute of Cosmological Physics. H. Q. and L. I. acknowledge partial support from FONDAP Centro de Astrofisica. J.D. received support from an RCUK Fellowship. K. M., M. H., and R. W. received financial support from the South African National Research Foundation (NRF), the Meraka Institute via funding for the South African Centre for High Performance Computing (CHPC), and the South African Square Kilometer Array (SKA) Project. R. D. was supported by CONICYT, MECESUP, and Fundacion Andes. RH acknowledges funding from the Rhodes Trust. S. D. acknowledges support from the Berkeley Center for Cosmological Physics. Y.T.L. acknowledges support from the World Premier International Research Center Initiative, MEXT, Japan. Some of the results in this paper have been derived using the HEALPix package (Gorski et al. 2005). 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. The data will be made public through LAMBDA (http://lambda.gsfc.nasa.gov/) and the ACT Web site (http://www.physics.princeton.edu/act/). NR 87 TC 100 Z9 100 U1 0 U2 8 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAY 1 PY 2011 VL 732 IS 1 AR 44 DI 10.1088/0004-637X/732/1/44 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 751OD UT WOS:000289626500044 ER PT J AU Stacey, WS Heinke, CO Elsner, RF Edmonds, PD Weisskopf, MC Grindlay, JE AF Stacey, W. S. Heinke, C. O. Elsner, R. F. Edmonds, P. D. Weisskopf, M. C. Grindlay, J. E. TI TRANSIENT EXTREMELY SOFT X-RAY EMISSION FROM THE UNUSUALLY BRIGHT CATACLYSMIC VARIABLE IN THE GLOBULAR CLUSTER M3: A NEW CV X-RAY LUMINOSITY RECORD? SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; globular clusters: individual (NGC 5272); novae, cataclysmic variables; white dwarfs; X-rays: binaries ID ABSOLUTE MAGNITUDES; SUPERSOFT SOURCES; ACCRETION DISKS; GALACTIC-CENTER; IA SUPERNOVAE; SKY SURVEY; GK-PERSEI; BINARIES; EVOLUTION; NOVAE AB We observed the accreting white dwarf (WD) 1E1339.8+2837 (1E1339) in the globular cluster M3 in 2003 November, 2004 May, and 2005 January, using the Chandra ACIS-S detector. The source was observed in 1992 to possess traits of a supersoft X-ray source (SSS), with a 0.1-2.4 keV luminosity as large as 2 x 10(35) erg s(-1), after which time the source's luminosity fell by roughly two orders of magnitude, adopting a hard X-ray spectrum more typical of cataclysmic variables (CVs). Our observations confirm 1E1339's hard CV-like spectrum, with photon index Gamma = 1.3 +/- 0.2. We found 1E1339 to be highly variable, with a 0.5-10 keV luminosity ranging from (1.4 +/- 0.3) x 10(34) erg s-1 to 8.5(-4.6)(+4.9) x 10(32) erg s(-1), with 1E1339's maximum luminosity being perhaps the highest yet recorded for hard X-ray emission from a WD. In 2005 January, 1E1339 displayed substantial low-energy emission below similar to 0.3 keV. Although current Chandra responses cannot properly model this emission, its bolometric luminosity appears comparable to or greater than that of the hard spectral component. This raises the possibility that the supersoft X-ray emission seen from 1E1339 in 1992 may have shifted to the far-UV. C1 [Stacey, W. S.; Heinke, C. O.] Univ Alberta, Dept Phys, Edmonton, AB T6G 2G7, Canada. [Elsner, R. F.; Weisskopf, M. C.] NASA, Marshall Space Flight Ctr, Huntsville, AL 35812 USA. [Edmonds, P. D.; Grindlay, J. E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Stacey, WS (reprint author), Univ Alberta, Dept Phys, 11322-89 Ave, Edmonton, AB T6G 2G7, Canada. EM heinke@ualberta.ca OI Heinke, Craig/0000-0003-3944-6109 NR 44 TC 6 Z9 6 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 MAY 1 PY 2011 VL 732 IS 1 AR 46 DI 10.1088/0004-637X/732/1/46 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 751OD UT WOS:000289626500046 ER PT J AU Vacca, WD Sandell, G AF Vacca, William D. Sandell, Goeran TI NEAR-INFRARED SPECTROSCOPY OF TW Hya: A REVISED SPECTRAL TYPE AND COMPARISON WITH MAGNETOSPHERIC ACCRETION MODELS SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars: individual (TW Hya); stars: pre-main sequence; techniques: spectroscopic ID LOW-MASS STARS; RECOMBINATION-LINE-INTENSITIES; MAIN-SEQUENCE STARS; TAURI STARS; HYDRAE ASSOCIATION; DISK ACCRETION; YOUNG STARS; TELESCOPE FACILITY; CIRCUMSTELLAR DISK; HYDROGENIC IONS AB We present high signal-to-noise ratio (S/N), moderate spectral resolution (R similar to 2000-2500) near-infrared (0.8-5.0 mu m) spectroscopy of the nearby T Tauri star TW Hya. By comparing the spectrum and the equivalent widths of several atomic and molecular features with those for stars in the IRTF near-infrared library, we revise the spectral type to M2.5V, which is later than what is usually adopted (K7V). This implies a substantially cooler stellar temperature than previously assumed. Comparison with various pre-main-sequence models suggests that TW Hya is only similar to 3 Myr old, much younger than the usually adopted 8-10 Myr. Analysis of the relative strengths of the H lines seen in the spectrum yields estimates for the temperature and density of the emitting region of T-e >= 7500 K and n(e) similar to 10(12)-10(13) cm(-3). The thickness of the emitting region is 10(2)-10(4) km and the covering fraction is f(*) similar to 0.04. Our derived physical parameter values agree with the predictions of the magnetospheric accretion scenario. The highest S/N H lines have profiles that indicate multiple emission components. We derive an excess spectrum (above that of the M2.5V template) that peaks in the H band. Although our derived veiling values (similar to 0.1) agree with previous estimates, the excess spectrum does not match that of current models in which this flux is generated by an inner optically thin disk. We suggest that the excess flux spectrum instead reflects the differences in atmospheric opacity, gravity, and age between TW Hya and older, higher gravity, field M2.5 dwarfs. C1 [Vacca, William D.; Sandell, Goeran] NASA, SOFIA USRA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Vacca, WD (reprint author), NASA, SOFIA USRA, Ames Res Ctr, Mail Stop 211-3,Bldg N211,Rm 251, Moffett Field, CA 94035 USA. EM wvacca@sofia.usra.edu; gsandell@sofia.usra.edu FU National Aeronautics and Space Administration, Science Mission Directorate [NNX-08AE38A] FX Visiting Astronomer at the Infrared Telescope Facility, which is operated by the University of Hawaii under Cooperative Agreement No. NNX-08AE38A with the National Aeronautics and Space Administration, Science Mission Directorate, Planetary Astronomy Program. NR 79 TC 40 Z9 40 U1 0 U2 3 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 MAY 1 PY 2011 VL 732 IS 1 AR 8 DI 10.1088/0004-637X/732/1/8 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 751OD UT WOS:000289626500008 ER PT J AU Rosenzweig, C Solecki, WD Blake, R Bowman, M Faris, C Gornitz, V Horton, R Jacob, K LeBlanc, A Leichenko, R Linkin, M Major, D O'Grady, M Patrick, L Sussman, E Yohe, G Zimmerman, R AF Rosenzweig, Cynthia Solecki, William D. Blake, Reginald Bowman, Malcolm Faris, Craig Gornitz, Vivien Horton, Radley Jacob, Klaus LeBlanc, Alice Leichenko, Robin Linkin, Megan Major, David O'Grady, Megan Patrick, Lesley Sussman, Edna Yohe, Gary Zimmerman, Rae TI Developing coastal adaptation to climate change in the New York City infrastructure-shed: process, approach, tools, and strategies SO CLIMATIC CHANGE LA English DT Article ID SEA-LEVEL RISE; IMPACTS; BOSTON AB While current rates of sea level rise and associated coastal flooding in the New York City region appear to be manageable by stakeholders responsible for communications, energy, transportation, and water infrastructure, projections for sea level rise and associated flooding in the future, especially those associated with rapid icemelt of the Greenland and West Antarctic Icesheets, may be outside the range of current capacity because extreme events might cause flooding beyond today's planning and preparedness regimes. This paper describes the comprehensive process, approach, and tools for adaptation developed by the New York City Panel on Climate Change (NPCC) in conjunction with the region's stakeholders who manage its critical infrastructure, much of which lies near the coast. It presents the adaptation framework and the sea-level rise and storm projections related to coastal risks developed through the stakeholder process. Climate change adaptation planning in New York City is characterized by a multi-jurisdictional stakeholder-scientist process, state-of-the-art scientific projections and mapping, and development of adaptation strategies based on a risk-management approach. C1 [Rosenzweig, Cynthia] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Solecki, William D.; Patrick, Lesley] CUNY Hunter Coll, New York, NY 10021 USA. [Blake, Reginald] CUNY, New York City Coll Technol, Brooklyn, NY 11210 USA. [Bowman, Malcolm] SUNY Stony Brook, Stony Brook, NY 11794 USA. [Faris, Craig] Accenture, Washington, DC USA. [Gornitz, Vivien; Horton, Radley; Jacob, Klaus; Major, David; O'Grady, Megan] Columbia Univ, New York, NY USA. [Leichenko, Robin] Rutgers State Univ, Piscataway, NJ USA. [Linkin, Megan] Swiss Reinsurance Amer Corp, Armonk, NY USA. [Sussman, Edna] Sussman ADR LLC, New York, NY USA. [Yohe, Gary] Wesleyan Univ, Middletown, CT USA. [Zimmerman, Rae] NYU, New York, NY USA. RP Rosenzweig, C (reprint author), NASA, Goddard Inst Space Studies, New York, NY 10025 USA. EM crosenzweig@giss.nasa.gov; aliceleblanc@verizon.net RI Leichenko, Robin/C-6047-2013 OI Leichenko, Robin/0000-0003-0607-5874 NR 53 TC 54 Z9 54 U1 6 U2 67 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0165-0009 EI 1573-1480 J9 CLIMATIC CHANGE JI Clim. Change PD MAY PY 2011 VL 106 IS 1 SI SI BP 93 EP 127 DI 10.1007/s10584-010-0002-8 PG 35 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA 747CW UT WOS:000289298900006 ER PT J AU Kim, H Liou, MS AF Kim, Hyoungjin Liou, Meng-Sing TI Accurate adaptive level set method and sharpening technique for three dimensional deforming interfaces SO COMPUTERS & FLUIDS LA English DT Article DE Level set; Re-initialization; Interface tracking; Interface sharpening ID INCOMPRESSIBLE 2-PHASE FLOWS; EFFICIENT IMPLEMENTATION; ALGORITHM; SCHEMES AB In this paper, we demonstrate improved accuracy of the level set method for resolving deforming interfaces by proposing two key elements: (1) accurate level set solutions on adapted Cartesian grids by judiciously choosing interpolation polynomials in regions of different grid levels and (2) enhanced re-initialization by an interface sharpening procedure. The level set equation is solved using a fifth order WENO scheme or a second order central differencing scheme depending on availability of uniform stencils at each grid point. Grid adaptation criteria are determined so that the Hamiltonian functions at nodes adjacent to interfaces are always calculated by the fifth order WENO scheme. This selective usage between the fifth order WENO and second order central differencing schemes is confirmed to give more accurate results compared to those in literature for standard test problems. In order to further improve accuracy especially near thin filaments, we suggest an artificial sharpening method, which is in a similar form with the conventional re-initialization method but utilizes sign of curvature instead of sign of the level set function. Consequently, volume loss due to numerical dissipation on thin filaments is remarkably reduced for the test problems. (C) 2010 Elsevier Ltd. All rights reserved. C1 [Kim, Hyoungjin] NASA Glenn Res Ctr, NASA Postdoctoral Program, Cleveland, OH 44135 USA. [Liou, Meng-Sing] NASA Glenn Res Ctr, Aeropropuls Div, Cleveland, OH 44135 USA. RP Kim, H (reprint author), NASA Glenn Res Ctr, Ohio Aerosp Inst, 22800 Cedar Point Rd, Cleveland, OH 44135 USA. EM hyoungjinkim1@gmail.com FU Oak Ridge Associated Universities through a contract with NASA FX This research was supported by an appointment to the NASA Postdoctoral Program at the Glenn Research Center, administered by Oak Ridge Associated Universities through a contract with NASA. NR 20 TC 7 Z9 7 U1 0 U2 6 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0045-7930 EI 1879-0747 J9 COMPUT FLUIDS JI Comput. Fluids PD MAY PY 2011 VL 44 IS 1 BP 111 EP 129 DI 10.1016/j.compfluid.2010.12.020 PG 19 WC Computer Science, Interdisciplinary Applications; Mechanics SC Computer Science; Mechanics GA 747LG UT WOS:000289320700011 ER PT J AU Bryson, S Epshteyn, Y Kurganov, A Petrova, G AF Bryson, Steve Epshteyn, Yekaterina Kurganov, Alexander Petrova, Guergana TI WELL-BALANCED POSITIVITY PRESERVING CENTRAL-UPWIND SCHEME ON TRIANGULAR GRIDS FOR THE SAINT-VENANT SYSTEM SO ESAIM-MATHEMATICAL MODELLING AND NUMERICAL ANALYSIS-MODELISATION MATHEMATIQUE ET ANALYSE NUMERIQUE LA English DT Article DE Hyperbolic systems of conservation and balance laws; semi-discrete central-upwind schemes; Saint-Venant system of shallow water equations ID HYPERBOLIC CONSERVATION-LAWS; SHALLOW-WATER EQUATIONS; FINITE-VOLUME SCHEMES; UNSTRUCTURED GRIDS; SOURCE TERMS; WENO SCHEMES; ORDER; FLOWS; ACCURACY; LIMITERS AB We introduce a new second-order central-upwind scheme for the Saint-Venant system of shallow water equations on triangular grids. We prove that the scheme both preserves "lake at rest" steady states and guarantees the positivity of the computed fluid depth. Moreover, it can be applied to models with discontinuous bottom topography and irregular channel widths. We demonstrate these features of the new scheme, as well as its high resolution and robustness in a number of numerical examples. C1 [Bryson, Steve] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Epshteyn, Yekaterina] Carnegie Mellon Univ, Dept Math Sci, Pittsburgh, PA 15213 USA. [Kurganov, Alexander] Tulane Univ, Dept Math, New Orleans, LA 70118 USA. [Petrova, Guergana] Texas A&M Univ, Dept Math, College Stn, TX 77843 USA. RP Bryson, S (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM Stephen.T.Bryson@nasa.gov; rina10@andrew.cmu.edu; kurganov@math.tulane.edu; gpetrova@math.tamu.edu RI Kurganov, Alexander/H-8789-2013 OI Kurganov, Alexander/0000-0003-0231-986X FU Center for Nonlinear Analysis (CNA) under the NSF [DMS-0635983]; NSF [DMS-0610430, DMS-0810869]; King Abdullah University of Science and Technology (KAUST) [KUS-C1-016-04] FX The research of Y. Epshteyn is based upon work supported by the Center for Nonlinear Analysis (CNA) under the NSF Grant # DMS-0635983. The research of A. Kurganov was supported in part by the NSF Grant # DMS-0610430. The research of G. Petrova was supported in part by the NSF Grant # DMS-0810869 and Award # KUS-C1-016-04, made by King Abdullah University of Science and Technology (KAUST). NR 37 TC 28 Z9 29 U1 0 U2 4 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0764-583X EI 1290-3841 J9 ESAIM-MATH MODEL NUM JI ESAIM-Math. Model. Numer. Anal.-Model. Math. Anal. Numer. PD MAY-JUN PY 2011 VL 45 IS 3 BP 423 EP 446 DI 10.1051/m2an/2010060 PG 24 WC Mathematics, Applied SC Mathematics GA 751MS UT WOS:000289622800002 ER PT J AU Holzmann, GJ Florian, M AF Holzmann, Gerard J. Florian, Mihai TI Model checking with bounded context switching SO FORMAL ASPECTS OF COMPUTING LA English DT Article DE Logic model checking; Depth-first search; Bounded context-switching; Partial order reduction; Bitstate hashing; Software verification AB We discuss the implementation of a bounded context switching algorithm in the Spin model checker. The algorithm allows us to find counter-examples that are often simpler to understand, and that may be more likely to occur in practice. We discuss extensions of the algorithm that allow us to use this new algorithm in combination with most other search modes supported in Spin, including partial order reduction and bitstate hashing. We show that, other than often assumed, the enforcement of a bounded context switching discipline does not decrease but increases the complexity of the model checking procedure. We discuss the performance of the algorithm on a range of applications. C1 [Holzmann, Gerard J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Florian, Mihai] CALTECH, Dept Comp Sci, Pasadena, CA 91109 USA. RP Holzmann, GJ (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,M-S 301-230, Pasadena, CA 91109 USA. EM gerard@spinroot.com NR 14 TC 7 Z9 8 U1 0 U2 0 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0934-5043 EI 1433-299X J9 FORM ASP COMPUT JI Form. Asp. Comput. PD MAY PY 2011 VL 23 IS 3 BP 365 EP 389 DI 10.1007/s00165-010-0160-5 PG 25 WC Computer Science, Software Engineering SC Computer Science GA 750DI UT WOS:000289524500007 ER PT J AU Kay, RB Poulios, D Coyle, DB Stysley, PR Clarke, GB AF Kay, Richard B. Poulios, Demetrios Coyle, Donald Barry Stysley, Paul R. Clarke, Gregory B. TI Derivation of the Frantz-Nodvik Equation for Diode-Side-Pumped Zigzag Slab Laser Amplifiers with Gaussian Laser Mode and Pump Beam Shapes SO IEEE JOURNAL OF QUANTUM ELECTRONICS LA English DT Article DE Laser diode-side-pumping; spatial pump distribution; zigzag slab amplifiers ID Q-SWITCHED LASER AB The theory for Gaussian beam pulse propagation in a zigzag slab amplifier with a Gaussian pump distribution is detailed. Provisions are made for amplification of an input signal with an elliptical Gaussian spatial mode by modifying the time-dependent photon transport equations as described by Eggleston Frantz, and Injeyan. A comparison is made with experimental results of a diode-side-pumped zigzag slab amplifier element amplifying a near-Gaussian beam. C1 [Kay, Richard B.; Poulios, Demetrios; Clarke, Gregory B.] American Univ, Dept Phys, Washington, DC 20016 USA. [Coyle, Donald Barry; Stysley, Paul R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Kay, RB (reprint author), American Univ, Dept Phys, Washington, DC 20016 USA. EM Richard.B.Kay@nasa.gov; poulios@american.edu; Barry.Coyle@nasa.gov; Paul.Stysley@nasa.gov; gc8795a@student.american.edu FU National Aeronautics and Space Administration [NNX08AJ95A]; Laser Physics Group, Department of Physics, American University, Washington D.C., USA FX This work was supported in part by the National Aeronautics and Space Administration Cooperative Research under Agreement NNX08AJ95A with the Laser Physics Group, Department of Physics, American University, Washington D.C., USA. NR 7 TC 1 Z9 1 U1 1 U2 9 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0018-9197 EI 1558-1713 J9 IEEE J QUANTUM ELECT JI IEEE J. Quantum Electron. PD MAY PY 2011 VL 47 IS 5 BP 745 EP 749 DI 10.1109/JQE.2011.2114329 PG 5 WC Engineering, Electrical & Electronic; Optics; Physics, Applied SC Engineering; Optics; Physics GA 749PF UT WOS:000289480100007 ER PT J AU Schuet, S Timucin, D Wheeler, K AF Schuet, Stefan Timucin, Dogan Wheeler, Kevin TI A Model-Based Probabilistic Inversion Framework for Characterizing Wire Fault Detection Using TDR SO IEEE TRANSACTIONS ON INSTRUMENTATION AND MEASUREMENT LA English DT Article; Proceedings Paper CT IEEE International Instrumentation and Measurement Conference CY MAY 03-06, 2010 CL Austin, TX SP IEEE DE Bayesian; fault detection; S-parameters; time-domain reflectometry (TDR); wiring ID DOMAIN REFLECTOMETRY; WIRING FAULTS; LOCATION AB Time-domain reflectometry (TDR) is one of the standard methods for diagnosing faults in electrical wiring and interconnect systems, with a long-standing history focused mainly on hardware development of both high-fidelity systems for laboratory use and portable handheld devices for field deployment. While these devices can easily assess distance to hard faults such as sustained opens or shorts, their ability to assess subtle but important degradation such as chafing remains an open question. This paper presents a unified framework for TDR-based chafing fault detection in lossy coaxial cables by combining an S-parameter-based forward-modeling approach with a probabilistic (Bayesian) inference algorithm. Results are presented for the estimation of nominal and faulty cable parameters from laboratory data. C1 [Schuet, Stefan; Timucin, Dogan; Wheeler, Kevin] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Schuet, S (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM stefan.r.schuet@nasa.gov; kevin.r.wheeler@nasa.gov NR 17 TC 19 Z9 19 U1 0 U2 5 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0018-9456 EI 1557-9662 J9 IEEE T INSTRUM MEAS JI IEEE Trans. Instrum. Meas. PD MAY PY 2011 VL 60 IS 5 BP 1654 EP 1663 DI 10.1109/TIM.2011.2105030 PG 10 WC Engineering, Electrical & Electronic; Instruments & Instrumentation SC Engineering; Instruments & Instrumentation GA 745XH UT WOS:000289204400017 ER PT J AU Bhatia, AK Landi, E AF Bhatia, A. K. Landi, E. TI Atomic data and spectral line intensities for Ni XVII SO ATOMIC DATA AND NUCLEAR DATA TABLES LA English DT Article ID EXTREME-ULTRAVIOLET SPECTRUM; ELECTRON-IMPACT EXCITATION; MG-LIKE IONS; INTERCOMBINATION LINES; RATE COEFFICIENTS; EMISSION-LINES; ENERGY-LEVELS; CA-IX; ISOELECTRONIC SEQUENCE; MAGNESIUM SEQUENCE AB Electron impact collision strengths, energy levels, oscillator strengths, and spontaneous radiative decay rates are calculated for Ni XVII. We include in the calculations the 23 lowest configurations, corresponding to 159 fine-structure levels: 3l3l', 3l4l '', and 3s51", with l,l' = s,p,d, l '' = s,p,d, f, and l''' = s,p,d. Collision strengths are calculated at five incident energies for all transitions at varying energies above the threshold of each transition. One additional energy, very close to the threshold of each transition, has also been included. Calculations have been carried out using the Flexible Atomic Code in the distorted wave approximation. Additional calculations have been performed with the University College London suite of codes for comparison. Excitation rate coefficients are calculated as a function of electron temperature by assuming a Maxwellian electron velocity distribution. Using the excitation rate coefficients and the radiative transition rates of the present work, statistical equilibrium equations for level populations are solved at electron densities covering the range of 10(8) - 10(14) cm(-3) and at an electron temperature of log T(e)(K) = 6.5, corresponding to the maximum abundance of Ni XVII. Spectral line intensities are calculated, and their diagnostic relevance is discussed. This dataset will be made available in the next version of the CHIANTI database. (C) 2010 Published by Elsevier Inc. C1 [Landi, E.] Univ Michigan, Ann Arbor, MI 48109 USA. [Bhatia, A. K.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Landi, E.] USN, Res Lab, Washington, DC 20375 USA. RP Landi, E (reprint author), Univ Michigan, Ann Arbor, MI 48109 USA. EM elandi@umich.edu RI Landi, Enrico/H-4493-2011 FU NASA; [NNH06CD24C]; [NNG04ED07P] FX The work of Enrico Landi is supported by the NNH06CD24C, NNG04ED07P, and other NASA Grants. Calculations were carried out using the Discover computer of the NASA Center for Computation Science. NR 44 TC 5 Z9 6 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 0092-640X J9 ATOM DATA NUCL DATA JI Atom. Data Nucl. Data Tables PD MAY PY 2011 VL 97 IS 3 BP 189 EP 224 DI 10.1016/j.adt.2010.07.001 PG 36 WC Physics, Atomic, Molecular & Chemical; Physics, Nuclear SC Physics GA 747OJ UT WOS:000289329000001 ER PT J AU Norvig, P Aldhous, P AF Norvig, Peter Aldhous, Peter TI Google's data junkie SO NEW SCIENTIST LA English DT Editorial Material C1 [Norvig, Peter] NASA, Ames Res Ctr, Computat Sci Div, Washington, DC 20546 USA. RP Norvig, P (reprint author), NASA, Ames Res Ctr, Computat Sci Div, Washington, DC 20546 USA. NR 0 TC 0 Z9 0 U1 1 U2 6 PU REED BUSINESS INFORMATION LTD PI SUTTON PA QUADRANT HOUSE THE QUADRANT, SUTTON SM2 5AS, SURREY, ENGLAND SN 0262-4079 J9 NEW SCI JI New Sci. PD APR 30 PY 2011 VL 210 IS 2810 BP 26 EP 27 PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 760AX UT WOS:000290294300028 ER PT J AU Huang, JF Hsu, NC Tsay, SC Jeong, MJ Holben, BN Berkoff, TA Welton, EJ AF Huang, Jingfeng Hsu, N. Christina Tsay, Si-Chee Jeong, Myeong-Jae Holben, Brent N. Berkoff, Timothy A. Welton, Ellsworth J. TI Susceptibility of aerosol optical thickness retrievals to thin cirrus contamination during the BASE-ASIA campaign SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID RESOLUTION IMAGING SPECTRORADIOMETER; ACE-ASIA; CLOUD; SATELLITE; AERONET; MODIS; ALGORITHMS; 1.38-MU-M; CHANNELS; IMPACTS AB We used a combination of ground measurements (Aerosol Robotic Network, AERONET; Micro-Pulse Lidar Network, MPLNET) and satellite data (Moderate Resolution Imaging Spectroradiometer, MODIS; Cloud-Aerosol Lidar and Infrared Pathfinder Satellite Observation, CALIPSO) to examine the susceptibility of ground and satellite aerosol retrievals to thin cirrus contamination at Phimai, Thailand (102.56 degrees E, 15.18 degrees N, also known as Pimai), during the Biomass-burning Aerosols in South East-Asia: Smoke Impact Assessment (BASE-ASIA) campaign (February-May 2006). Using the strengths of spaceborne or ground lidars to detect cirrus clouds, we conducted statistical analyses for four different scenarios: MPLNET versus AERONET, MPLNET versus MODIS, CALIPSO versus AERONET, and CALIPSO versus MODIS. Cirrus identifications from MPLNET or CALIPSO were paired up with concurrent aerosol optical thickness (AOT) measurements from AERONET or MODIS. Results from the BASE-ASIA campaign suggest that current operational AERONET and MODIS AOT products are influenced by thin cirrus contamination featuring strong seasonality. Concurrent AERONET and MPLNET observations indicate that additional thin cirrus screening changes AOT monthly means by 5%, with 20% of the AERONET aerosol data at Phimai being cirrus contaminated in boreal spring. From noncirrus cases to cirrus-contaminated cases, AERONET AOT increases along with larger particle sizes. We further evaluated the performance of eight MODIS-derived cirrus screening parameters for their effectiveness on thin cirrus screening: apparent reflectance at 1.38 mu m (R1.38), cirrus reflectance at 0.66 mu m (CR0.66), CR0.66 cirrus flag, reflectance ratio between 1.38 mu m and 0.66 mu m (RR1.38/0.66), reflectance ratio between 1.38 mu m and 1.24 mu m (RR1.38/1.24), brightness temperature difference between 8.6 mu m and 11 mu m (BTD8.6-11), brightness temperature difference between 11 mu m and 12 mu m (BTD11-12), and cloud phase infrared approach. Correlation analysis with the MPLNET cirrus flag indicates that RR1.38/0.66 is slightly preferable for high thin cirrus screening for the AERONET AOT measurements. The quantitative findings from this study suggest particular caution and careful evaluation of thin cirrus contamination in the satellite and ground AOT measurements before they are used for aerosol-related climatic forcing studies. C1 [Huang, Jingfeng; Jeong, Myeong-Jae; Berkoff, Timothy A.] Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA. [Huang, Jingfeng; Hsu, N. Christina; Tsay, Si-Chee; Jeong, Myeong-Jae; Holben, Brent N.; Berkoff, Timothy A.; Welton, Ellsworth J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Huang, JF (reprint author), Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, 5523 Res Pk Dr, Baltimore, MD 21228 USA. EM jfhuang@umbc.edu RI Jeong, Myeong/B-8803-2008; Welton, Ellsworth/A-8362-2012; Huang, Jingfeng/D-7336-2012; Hsu, N. Christina/H-3420-2013; Tsay, Si-Chee/J-1147-2014 OI Huang, Jingfeng/0000-0002-8779-2922; FU NASA EOS FX This work is supported by a grant from the NASA EOS Program, managed by Hal Maring. The authors thank Alexander Smirnov, David Giles, Bo-Cai Gao, Richard A. Hansell, Steve Ou, and Zhien Wang for their constructive comments on the use of in situ and satellite data, analysis methodology, and cirrus climatology. The authors thank three anonymous reviewers for their comments that were valuable to improving the paper. Aqua MODIS L1B and L2 data were obtained from NASA L1 and Atmosphere Archive and Distribution System (LAADS). CALIPSO data were obtained from the NASA Langley Research Center Atmospheric Science Data Center. NR 36 TC 36 Z9 36 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 APR 30 PY 2011 VL 116 AR D08214 DI 10.1029/2010JD014910 PG 12 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 757QT UT WOS:000290103500002 ER PT J AU Seker, I Fung, SF Mathews, JD AF Seker, Ilgin Fung, Shing F. Mathews, John D. TI Relation between magnetospheric state parameters and the occurrence of plasma depletion events in the nighttime midlatitude F region SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID TRAVELING IONOSPHERIC DISTURBANCES; EQUATORIAL SPREAD-F; GEOMAGNETIC-ACTIVITY; RADAR; AIRGLOW; BUBBLES; INSTABILITY; ARECIBO; NETWORK AB Studies using all-sky imagers have revealed the presence of various ionospheric irregularities in the nighttime midlatitude F region. The most prevalent and well known of these are the medium-scale traveling ionospheric disturbances (MSTIDs) that usually occur when the geomagnetic activity is low and midlatitude spread F plumes that are often observed when the geomagnetic activity is high. The inverse and direct relations between geomagnetic activity and the occurrence rate of MSTIDs and midlatitude plumes, respectively, have been observed by several studies using different instruments; however, most of them focus on MSTIDs only and use only Kp to characterize geomagnetic activity. In order to understand the underlying causes of these two relations and to distinguish between MSTIDs and plumes, it is illuminating to better characterize the occurrence of MSTIDs and plumes using multiple magnetospheric state parameters. Here we statistically compare multiple geomagnetic driver and response parameters (such as Kp, AE, Dst, and solar wind parameters) with the occurrence rates of nighttime MSTIDs and plumes observed using an all-sky imager at Arecibo Observatory (AO) between 2003 and 2008. We also present seasonal and annual variations of MSTIDs and plumes at AO. The results not only allow us to better distinguish MSTIDs and plumes, but also to shed further light on the generation mechanism and electrodynamics of these two different phenomena occurring at nighttime in the midlatitude F region. C1 [Seker, Ilgin; Fung, Shing F.] NASA, Goddard Space Flight Ctr, Geospace Phys Lab, Heliophys Sci Div, Greenbelt, MD 20771 USA. [Mathews, John D.] Penn State Univ, Radar Space Sci Lab, Dept Elect Engn, University Pk, PA 16902 USA. RP Seker, I (reprint author), NASA, Goddard Space Flight Ctr, Geospace Phys Lab, Heliophys Sci Div, Code 632, Greenbelt, MD 20771 USA. EM ilgin.seker@nasa.gov RI Fung, Shing/F-5647-2012 FU NASA; NSF [ATM 07-21613] FX This research was supported by an appointment to the NASA Postdoctoral Program at the Goddard Space Flight Center, administered by Oak Ridge Associated Universities through a contract with NASA. The Penn State All-Sky Imager System is supported under NSF grant ATM 07-21613 to Pennsylvania State University. The monthly and annual variation plots have been provided by NASA summer intern Seok Youl Yoon. We thank the reviewers for their constructive comments. NR 32 TC 4 Z9 4 U1 0 U2 3 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 APR 30 PY 2011 VL 116 AR A04323 DI 10.1029/2010JA015521 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 757RH UT WOS:000290104900001 ER PT J AU Davami, K Kang, D Lee, JS Meyyappan, M AF Davami, Keivan Kang, Daegun Lee, Jeong-Soo Meyyappan, M. TI Synthesis of ZnTe nanostructures by vapor-liquid-solid technique (vol 504, pg 62, 2011) SO CHEMICAL PHYSICS LETTERS LA English DT Correction C1 [Davami, Keivan; Kang, Daegun; Lee, Jeong-Soo] Pohang Univ Sci & Technol POSTECH, Div IT Convergence Engn, Pohang, South Korea. [Meyyappan, M.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Lee, JS (reprint author), Pohang Univ Sci & Technol POSTECH, Div IT Convergence Engn, Pohang, South Korea. EM ljs6951@postech.ac.kr; m.meyyappan@nasa.gov NR 1 TC 2 Z9 3 U1 1 U2 10 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0009-2614 J9 CHEM PHYS LETT JI Chem. Phys. Lett. PD APR 29 PY 2011 VL 507 IS 1-3 BP 208 EP 208 DI 10.1016/j.cplett.2011.03.029 PG 1 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 753KP UT WOS:000289772600040 ER PT J AU Sola, F Hurwitz, F Yang, J AF Sola, F. Hurwitz, F. Yang, J. TI A new scanning electron microscopy approach to image aerogels at the nanoscale SO NANOTECHNOLOGY LA English DT Article ID IONIZATION CROSS-SECTIONS; LOW-VACUUM; EMISSION; SILICA; SEM AB A new scanning electron microscopy (SEM) technique to image poor electrically conductive aerogels is presented. The process can be performed by non-expert SEM users. We showed that negative charging effects on aerogels can be minimized significantly by inserting dry nitrogen gas close to the region of interest. The process involves the local recombination of accumulated negative charges with positive ions generated from ionization processes. This new technique made possible the acquisition of images of aerogels with pores down to approximately 3 nm in diameter using a positively biased Everhart-Thornley (ET) detector. C1 [Sola, F.; Hurwitz, F.] NASA, Glenn Res Ctr, Mat & Struct Div, Cleveland, OH 44135 USA. [Yang, J.] Carl Zeiss NTS LLC, Peabody, MA 01960 USA. RP Sola, F (reprint author), NASA, Glenn Res Ctr, Mat & Struct Div, Cleveland, OH 44135 USA. EM francisco.sola-lopez@nasa.gov FU Hypersonic Project in the Fundamental Aeronautics Program FX This work was supported by the Hypersonic Project in the Fundamental Aeronautics Program. NR 24 TC 1 Z9 1 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0957-4484 J9 NANOTECHNOLOGY JI Nanotechnology PD APR 29 PY 2011 VL 22 IS 17 AR 175704 DI 10.1088/0957-4484/22/17/175704 PG 6 WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary; Physics, Applied SC Science & Technology - Other Topics; Materials Science; Physics GA 736QR UT WOS:000288509700017 PM 21411927 ER PT J AU Li, XL Palo, S Kohnert, R AF Li, Xinlin Palo, Scott Kohnert, Rick TI Small Space Weather Research Mission Designed Fully by Students SO SPACE WEATHER-THE INTERNATIONAL JOURNAL OF RESEARCH AND APPLICATIONS LA English DT Editorial Material C1 [Li, Xinlin; Kohnert, Rick] Univ Colorado, LASP, Boulder, CO 80309 USA. [Li, Xinlin; Palo, Scott] Univ Colorado, Dept Aerosp Engn Sci, Boulder, CO 80309 USA. [Li, Xinlin] NASA, RBSP Mission, Washington, DC USA. RP Li, XL (reprint author), Univ Colorado, LASP, Boulder, CO 80309 USA. EM lix@lasp.colorado.edu OI PALO, SCOTT/0000-0002-4729-4929 NR 0 TC 4 Z9 4 U1 0 U2 1 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 1542-7390 J9 SPACE WEATHER JI Space Weather PD APR 28 PY 2011 VL 9 AR S04006 DI 10.1029/2011SW000668 PG 2 WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences GA 757QY UT WOS:000290104000002 ER PT J AU Rastatter, L Kuznetsova, MM Vapirev, A Ridley, A Wiltberger, M Pulkkinen, A Hesse, M Singer, HJ AF Rastaetter, L. Kuznetsova, M. M. Vapirev, A. Ridley, A. Wiltberger, M. Pulkkinen, A. Hesse, M. Singer, H. J. TI Geospace Environment Modeling 2008-2009 Challenge: Geosynchronous magnetic field SO SPACE WEATHER-THE INTERNATIONAL JOURNAL OF RESEARCH AND APPLICATIONS LA English DT Article ID INNER MAGNETOSPHERE; SIMULATION; MAGNETOPAUSE; SUBSTORM; SCHEME; WIND AB In this paper the metrics-based results of the inner magnetospheric magnetic field part of the 2008-2009 GEM Metrics Challenge are reported. The Metrics Challenge asked modelers to submit results for four geomagnetic storm events and five different types of observations that can be modeled by statistical or climatological or physics-based (e. g., MHD) models of the magnetosphere-ionosphere system. We present the results of 12 model settings that were run at the Community Coordinated Modeling Center and at the institutions of various modelers for these events. To measure the performance of each of the models against the observations, we use direct comparisons between the strength of the measured magnetic field (B), the sine of the elevation angle Theta(xz) (tau), and the spectral power of fluctuations for both quantities. We find that model rankings vary widely by type of variable and skill score used. None of the models consistently performs best for all events. We find that empirical models perform well for weak storm events, and physics-based (magnetohydrodynamic) models are better for strong storm events. Within a series of runs of the same model we find that higher resolution may not always improve results unless more physics of the inner magnetosphere, such as the kinetic description of the ring current, is included. C1 [Rastaetter, L.; Kuznetsova, M. M.; Pulkkinen, A.; Hesse, M.] NASA, Community Coordinated Modeling Ctr, Space Weather Lab, Goddard Space Flight Ctr, Greenbelt, MD 20770 USA. [Ridley, A.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. [Singer, H. J.] NOAA, Space Weather Predict Ctr, Natl Ctr Environm Predict, Natl Weather Serv, Boulder, CO 80305 USA. [Wiltberger, M.] Natl Ctr Atmospher Res, High Altitude Observ, Boulder, CO 80307 USA. [Vapirev, A.] Univ New Hampshire, Ctr Space Sci, Durham, NH 03824 USA. [Pulkkinen, A.] Catholic Univ Amer, IACS, Washington, DC 20064 USA. RP Rastatter, L (reprint author), NASA, Community Coordinated Modeling Ctr, Space Weather Lab, Goddard Space Flight Ctr, Code 674, Greenbelt, MD 20770 USA. EM lutz.rastaetter@nasa.gov; maria.m.kuznetsova@nasa.gov; alexander.vapirev@unh.edu; ridley@umich.edu; wiltbemj@ucar.edu; antti.a.pulkkinen@nasa.gov; michael.hesse@nasa.gov; howard.singer@noaa.gov RI Ridley, Aaron/F-3943-2011; Hesse, Michael/D-2031-2012; Rastaetter, Lutz/D-4715-2012; Wiltberger, Michael/B-8781-2008 OI Ridley, Aaron/0000-0001-6933-8534; Rastaetter, Lutz/0000-0002-7343-4147; Wiltberger, Michael/0000-0002-4844-3148 NR 24 TC 17 Z9 17 U1 0 U2 1 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 1542-7390 J9 SPACE WEATHER JI Space Weather PD APR 28 PY 2011 VL 9 AR S04005 DI 10.1029/2010SW000617 PG 15 WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences GA 757QY UT WOS:000290104000001 ER PT J AU Kersten, K Cattell, CA Breneman, A Goetz, K Kellogg, PJ Wygant, JR Wilson, LB Blake, JB Looper, MD Roth, I AF Kersten, K. Cattell, C. A. Breneman, A. Goetz, K. Kellogg, P. J. Wygant, J. R. Wilson, L. B., III Blake, J. B. Looper, M. D. Roth, I. TI Observation of relativistic electron microbursts in conjunction with intense radiation belt whistler-mode waves SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID MAGNETOSPHERIC CHORUS; VLF CHORUS; ASSOCIATION; MISSION; RADIO; SOLAR AB We present multi-satellite observations of large amplitude radiation belt whistler-mode waves and relativistic electron precipitation. On separate occasions during the Wind petal orbits and STEREO phasing orbits, Wind and STEREO recorded intense whistler-mode waves in the outer nightside equatorial radiation belt with peak-to-peak amplitudes exceeding 300 mV/m. During these intervals of intense wave activity, SAMPEX recorded relativistic electron microbursts in near magnetic conjunction with Wind and STEREO. This evidence of microburst precipitation occurring at the same time and at nearly the same magnetic local time and L-shell with a bursty temporal structure similar to that of the observed large amplitude wave packets suggests a causal connection between the two phenomena. Simulation studies corroborate this idea, showing that nonlinear wave-particle interactions may result in rapid energization and scattering on timescales comparable to those of the impulsive relativistic electron precipitation. Citation: Kersten, K., C. A. Cattell, A. Breneman, K. Goetz, P. J. Kellogg, J. R. Wygant, L. B. Wilson III, J. B. Blake, M. D. Looper, and I. Roth (2011), Observation of relativistic electron microbursts in conjunction with intense radiation belt whistler-mode waves, Geophys. Res. Lett., 38, L08107, doi:10.1029/2011GL046810. C1 [Kersten, K.; Cattell, C. A.; Breneman, A.; Goetz, K.; Kellogg, P. J.; Wygant, J. R.] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA. [Blake, J. B.; Looper, M. D.] Aerosp Corp, Dept Space Sci, El Segundo, CA 90245 USA. [Roth, I.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Wilson, L. B., III] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Kersten, K (reprint author), Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA. EM kkersten@physics.umn.edu RI Wilson III, Lynn/D-4425-2012; OI Wilson III, Lynn/0000-0002-4313-1970; Cattell, Cynthia/0000-0002-3805-320X FU NASA STEREO [NNX09AG82G, NNX07AF23G]; NASA, APL [NAS5-01072] FX This work was supported by NASA STEREO grants NNX09AG82G and NNX07AF23G, and by NASA grant NAS5-01072 under contract from APL for the development of RBSP/EFW. Simulation work was carried out using resources of the University of Minnesota Supercomputing Institute with the assistance of Shuxia Zhang. Geosynchronous electron data provided by LANL. DST and AE indices courtesy of WDC for Geomagnetism, Kyoto. NR 24 TC 27 Z9 27 U1 0 U2 4 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD APR 28 PY 2011 VL 38 AR L08107 DI 10.1029/2011GL046810 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 757SR UT WOS:000290108500002 ER PT J AU Schinder, PJ Flasar, FM Marouf, EA French, RG McGhee, CA Kliore, AJ Rappaport, NJ Barbinis, E Fleischman, D Anabtawi, A AF Schinder, P. J. Flasar, F. M. Marouf, E. A. French, R. G. McGhee, C. A. Kliore, A. J. Rappaport, N. J. Barbinis, E. Fleischman, D. Anabtawi, A. TI Saturn's equatorial oscillation: Evidence of descending thermal structure from Cassini radio occultations SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID STRATOSPHERIC TEMPERATURES; MIDDLE ATMOSPHERE; ZONAL WINDS; JUPITER AB A series of near-equatorial radio occultations of Cassini by Saturn occurred in 2005 and again in 2009-2010. Comparison of the temperature-pressure profiles obtained from the two sets of occultations shows evidence of a descending pattern in the stratosphere that is similar to those associated with equatorial oscillations in Earth's middle atmosphere. This is the first time that this descent has been observed in another planetary atmosphere. If absorption of upwardly propagating waves drives the descent, the implied absorbed flux is 0.05 m(2) s(-2), at least as large if not greater than on Earth. Citation: Schinder, P. J., F. M. Flasar, E. A. Marouf, R. G. French, C. A. McGhee, A. J. Kliore, N. J. Rappaport, E. Barbinis, D. Fleischman, and A. Anabtawi (2011), Saturn's equatorial oscillation: Evidence of descending thermal structure from Cassini radio occultations, Geophys. Res. Lett., 38, L08205, doi:10.1029/2011GL047191. C1 [Schinder, P. J.] Cornell Univ, Ctr Radiophys & Space Res, Ithaca, NY 14853 USA. [Kliore, A. J.; Rappaport, N. J.; Barbinis, E.; Fleischman, D.; Anabtawi, A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Flasar, F. M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [French, R. G.; McGhee, C. A.] Wellesley Coll, Dept Astron, Wellesley, MA 02481 USA. [Marouf, E. A.] San Jose State Univ, Dept Elect Engn, San Jose, CA 95192 USA. RP Schinder, PJ (reprint author), Cornell Univ, Ctr Radiophys & Space Res, Ithaca, NY 14853 USA. EM schinder@astro.cornell.edu RI Flasar, F Michael/C-8509-2012; OI Schinder, Paul/0000-0002-4571-7895 NR 17 TC 8 Z9 8 U1 0 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 APR 28 PY 2011 VL 38 AR L08205 DI 10.1029/2011GL047191 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 757SR UT WOS:000290108500007 ER PT J AU Nguyen, AT Menemenlis, D Kwok, R AF Nguyen, An T. Menemenlis, Dimitris Kwok, Ronald TI Arctic ice-ocean simulation with optimized model parameters: Approach and assessment SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS LA English DT Article ID SEA-ICE; FRAM STRAIT; CIRCULATION; REANALYSIS; REPRESENTATION; ASSIMILATION; VARIABILITY; TOPOGRAPHY; THICKNESS; DYNAMICS AB We present an optimized 1992-2008 coupled ice-ocean simulation of the Arctic Ocean. A Green's function approach adjusts a set of parameters for best model-data agreement. Overall, model-data differences are reduced by 45%. The optimized simulation reproduces the negative trends in ice extent in the satellite records. Volume and thickness distributions are comparable to those from the Ice, Cloud, and land Elevation Satellite (2003-2008). The upper cold halocline is consistent with observations in the western Arctic. The freshwater budget of the Arctic Ocean and volume/heat transports of Pacific and Atlantic waters across major passages are comparable with observation-based estimates. We note that the optimized parameters depend on the selected atmospheric forcing. The use of the 25 year Japanese reanalysis results in sea ice albedos that are consistent with field observations. Simulated Pacific Water enters the Bering Strait and flows off the Chukchi Shelf along four distinct channels. This water takes similar to 5-10 years to exit the Arctic Ocean at the Canadian Arctic Archipelago, Nares, or Fram straits. Atlantic Water entering the Fram Strait flows eastward, merges with the St Ana Trough inflow, and splits into two branches at the southwest corner of the Makarov Basin. One branch flows along Lomonosov Ridge back to Fram Strait. The other enters the western Arctic, circulates cyclonically below the halocline, and exits mainly through the Nares and Fram straits. This work utilizes the record of available observations to obtain an Arctic Ocean simulation that is in agreement with observations both within and beyond the optimization period and that can be used for tracer and process studies. C1 [Nguyen, An T.] Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA 90095 USA. [Nguyen, An T.; Menemenlis, Dimitris; Kwok, Ronald] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Nguyen, AT (reprint author), Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA 90095 USA. EM an.t.nguyen@jpl.nasa.gov; dimitris.menemenlis@jpl.nasa.gov; ronald.kwok@jpl.nasa.gov RI Kwok, Ron/A-9762-2008 OI Kwok, Ron/0000-0003-4051-5896 FU ECCO2 project; NASA Advanced Supercomputing (NAS) Division; JPL Supercomputing and Visualization Facility (SVF) FX Sea ice draft data were downloaded from the National Snow and Ice Data Center (NSIDC). This work is funded by the ECCO2 project, a contribution to the NASA Modeling Analysis and Prediction (MAP) program. We gratefully acknowledge computational resources and support from the NASA Advanced Supercomputing (NAS) Division and from the JPL Supercomputing and Visualization Facility (SVF). NR 82 TC 48 Z9 51 U1 0 U2 10 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9275 EI 2169-9291 J9 J GEOPHYS RES-OCEANS JI J. Geophys. Res.-Oceans PD APR 27 PY 2011 VL 116 AR C04025 DI 10.1029/2010JC006573 PG 18 WC Oceanography SC Oceanography GA 757SK UT WOS:000290107800002 ER PT J AU Hand, KP Khurana, KK Chyba, CF AF Hand, K. P. Khurana, K. K. Chyba, C. F. TI Joule heating of the south polar terrain on Enceladus SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID VAPOR PLUMES; PLASMA TORUS; IO; EUROPA; SODIUM; OCEAN; WATER AB We report that Joule heating in Enceladus, resulting from the interaction of Enceladus with Saturn's magnetic field, may account for 150 kW to 52 MW of power through Enceladus. Electric currents passing through subsurface channels of low salinity and just a few kilometers in depth could supply a source of power to the south polar terrain, providing a small but previously unaccounted for contribution to the observed heat flux and plume activity. Studies of the electrical heating of Jupiter's moon Europa have concluded that electricity is a negligible heating source since no connection between the conductive subsurface and Alfven currents has been observed. Here we show that, contrary to results for the Jupiter system, electrical heating may be a source of internal energy for Enceladus, contributing to localized heating, production of water vapor, and the persistence of the "tiger stripes." This contribution is of order 0.001-0.25% of the total observed heat flux, and thus, Joule heating cannot explain the total south polar terrain heat anomaly. The exclusion of salt ions during refreezing serves to enhance volumetric Joule heating and could extend the lifetime of liquid water fractures in the south polar terrain. C1 [Hand, K. P.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Chyba, C. F.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Khurana, K. K.] Univ Calif Los Angeles, Dept Planetary Sci, Los Angeles, CA 90095 USA. RP Hand, KP (reprint author), CALTECH, Jet Prop Lab, MS 183-601,4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Kevin.P.Hand@jpl.nasa.gov FU Jet Propulsion Laboratory, California Institute of Technology; NASA; NASA Astrobiology Institute, Astrobiology of Icy Worlds' team at the Jet Propulsion Laboratory FX K. P. Hand acknowledges support from the Jet Propulsion Laboratory, California Institute of Technology, through a contract with NASA, and support through the NASA Astrobiology Institute, Astrobiology of Icy Worlds' team at the Jet Propulsion Laboratory. NR 35 TC 2 Z9 2 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-PLANET JI J. Geophys. Res.-Planets PD APR 27 PY 2011 VL 116 AR E04010 DI 10.1029/2010JE003776 PG 5 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 757TD UT WOS:000290109700001 ER PT J AU Isaacson, PJ Pieters, CM Besse, S Clark, RN Head, JW Klima, RL Mustard, JF Petro, NE Staid, MI Sunshine, JM Taylor, LA Thaisen, KG Tompkins, S AF Isaacson, Peter J. Pieters, Carle M. Besse, Sebastien Clark, Roger N. Head, James W. Klima, Rachel L. Mustard, John F. Petro, Noah E. Staid, Matthew I. Sunshine, Jessica M. Taylor, Lawrence A. Thaisen, Kevin G. Tompkins, Stefanie TI Remote compositional analysis of lunar olivine-rich lithologies with Moon Mineralogy Mapper (M-3) spectra SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID CLEMENTINE NIR DATA; REFLECTANCE SPECTROSCOPY; OPTICAL-PROPERTIES; CRATER COPERNICUS; MARE BASALTS; SPACE; IRON; SIMULATION; ARISTARCHUS; ASTEROIDS AB A systematic approach for deconvolving remotely sensed lunar olivine-rich visible to near-infrared (VNIR) reflectance spectra with the Modified Gaussian Model (MGM) is evaluated with Chandrayaan-1 Moon Mineralogy Mapper (M-3) spectra. Whereas earlier studies of laboratory reflectance spectra focused only on complications due to chromite inclusions in lunar olivines, we develop a systematic approach for addressing (through continuum removal) the prominent continuum slopes common to remotely sensed reflectance spectra of planetary surfaces. We have validated our continuum removal on a suite of laboratory reflectance spectra. Suites of olivine-dominated reflectance spectra from a small crater near Mare Moscoviense, the Copernicus central peak, Aristarchus, and the crater Marius in the Marius Hills were analyzed. Spectral diversity was detected in visual evaluation of the spectra and was quantified using the MGM. The MGM-derived band positions are used to estimate the olivine's composition in a relative sense. Spectra of olivines from Moscoviense exhibit diversity in their absorption features, and this diversity suggests some variation in olivine Fe/Mg content. Olivines from Copernicus are observed to be spectrally homogeneous and thus are predicted to be more compositionally homogeneous than those at Moscoviense but are of broadly similar composition to the Moscoviense olivines. Olivines from Aristarchus and Marius exhibit clear spectral differences from those at Moscoviense and Copernicus but also exhibit features that suggest contributions from other phases. If the various precautions discussed here are weighed carefully, the methods presented here can be used to make general predictions of absolute olivine composition (Fe/Mg content). C1 [Isaacson, Peter J.; Pieters, Carle M.; Head, James W.; Mustard, John F.] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA. [Besse, Sebastien; Sunshine, Jessica M.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Clark, Roger N.] US Geol Survey, Denver Fed Ctr, Denver, CO 80225 USA. [Klima, Rachel L.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20732 USA. [Petro, Noah E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Staid, Matthew I.] Planetary Sci Inst, Tucson, AZ 85719 USA. [Taylor, Lawrence A.; Thaisen, Kevin G.] Univ Tennessee, Dept Earth & Planetary Sci, Planetary Geosci Inst, Knoxville, TN 37996 USA. [Tompkins, Stefanie] Def Adv Res Projects Agcy, Arlington, VA 22203 USA. RP Isaacson, PJ (reprint author), Brown Univ, Dept Geol Sci, Box 1846, Providence, RI 02912 USA. EM Peter_Isaacson@Brown.edu RI Klima, Rachel/H-9383-2012; Petro, Noah/F-5340-2013; OI Klima, Rachel/0000-0002-9151-6429; Besse, Sebastien/0000-0002-1052-5439 FU NASA [NNM05AB26C]; NASA LSI at Brown University [NNA09DB34A] FX The efforts of the entire M3 engineering, operations, and science teams are gratefully acknowledged. M3 science validation is supported through NASA contract NNM05AB26C. M3 is supported as a NASA Discovery Program mission of opportunity. The M3 team is grateful to ISRO for the opportunity to fly as a guest instrument on Chandrayaan-1. Partial funding for this analysis has also been provided through the NASA LSI at Brown University under contract NNA09DB34A. Careful reviews by Brett Denevi and an anonymous reviewer have improved this manuscript substantially. The views, opinions, and/or findings contained in this paper are those of the authors and should not be interpreted as representing the official views, either expressed or implied, of the Defense Advanced Research Projects Agency or the Department of Defense. NR 59 TC 32 Z9 37 U1 0 U2 13 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 APR 26 PY 2011 VL 116 AR E00G11 DI 10.1029/2010JE003731 PG 17 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 757TA UT WOS:000290109400002 ER PT J AU Phebus, BD Johnson, AV Mar, B Stone, BM Colaprete, A Iraci, LT AF Phebus, Bruce D. Johnson, Alexandria V. Mar, Brendan Stone, Bradley M. Colaprete, Anthony Iraci, Laura T. TI Water ice nucleation characteristics of JSC Mars-1 regolith simulant under simulated Martian atmospheric conditions SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID GENERAL-CIRCULATION MODEL; MINERAL DUST PARTICLES; CLOUD FORMATION; VAPOR; TEMPERATURES; PATHFINDER; SURROGATES; EVOLUTION; CHAMBER; CLIMATE AB Water ice clouds in the Martian atmosphere are governed by parameters such as number density and particle size distribution that in turn affect how they influence the climate. With some of the underlying properties of cloud formation well known only for Earth, extrapolations to Mars are potentially misleading. We report here continued laboratory experiments to identify critical onset conditions for water ice formation under Martian cloud forming temperatures and water partial pressures (155-182 K, 7.6 x 10(-5) to 7.7 x 10(-3) Pa H(2)O). By observing the 3 mu m infrared band to monitor nucleation and growth, we observe significant temperature dependence in the nucleation of ice on JSC Mars-1 regolith simulant, with critical saturation ratios, S(crit), as high as 3.8 at 155 K. At temperatures below similar to 180 K, ice nucleation on JSC Mars-1 requires significant supersaturation, potentially impacting the Martian hydrological cycle. C1 [Phebus, Bruce D.; Johnson, Alexandria V.; Mar, Brendan; Colaprete, Anthony; Iraci, Laura T.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Phebus, Bruce D.; Mar, Brendan; Stone, Bradley M.] San Jose State Univ, Dept Chem, San Jose, CA 95192 USA. [Johnson, Alexandria V.] Michigan Technol Univ, Dept Phys, Houghton, MI 49931 USA. RP Phebus, BD (reprint author), Univ Calif Santa Cruz, Dept Chem & Biochem, 1156 High St, Santa Cruz, CA 95064 USA. EM laura.t.iraci@nasa.gov OI Phebus, Bruce/0000-0003-3489-5546 FU NASA FX Thanks are due to D. Scimeca and E. Quigley for construction of the apparatus. O. Marcu and M. Sanchez made possible the micrographs of the JSC Mars-1 samples. Useful conversations with R. Terrill, A. Maattanen, and M. Trainer are gratefully acknowledged. Funding for this work was provided by the NASA Planetary Atmospheres Program (P. Crane, Program Officer) with additional assistance provided from the NASA Undergraduate Student Research Program (A.V.J). NR 46 TC 5 Z9 5 U1 1 U2 10 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 APR 26 PY 2011 VL 116 AR E04009 DI 10.1029/2010JE003699 PG 8 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 757TA UT WOS:000290109400001 ER PT J AU Staid, MI Pieters, CM Besse, S Boardman, J Dhingra, D Green, R Head, JW Isaacson, P Klima, R Kramer, G Mustard, JM Runyon, C Sunshine, J Taylor, LA AF Staid, M. I. Pieters, C. M. Besse, S. Boardman, J. Dhingra, D. Green, R. Head, J. W. Isaacson, P. Klima, R. Kramer, G. Mustard, J. M. Runyon, C. Sunshine, J. Taylor, L. A. TI The mineralogy of late stage lunar volcanism as observed by the Moon Mineralogy Mapper on Chandrayaan-1 SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID INFRARED SPECTRAL REFLECTANCE; PROCELLARUM KREEP TERRANE; PROSPECTOR GAMMA-RAY; MARE BASALTS; OCEANUS PROCELLARUM; CLEMENTINE MISSION; IRON; OLIVINE; TIO2; SPECTROMETER AB The last major phases of lunar volcanism produced spectrally unique high-titanium basalts on the western nearside of the Moon. The Moon Mineralogy Mapper (M-3) on Chandrayaan-1 has provided detailed measurements of these basalts at spatial and spectral resolutions necessary for mineralogical interpretation and mapping of distinct compositional units. The M-3 imaging spectrometer acquired data in 85 spectral bands from similar to 430 to 3000 nm at 140 to 280 m/pixel in its global mapping mode during the first half of 2009. Reflectance data of several key sites in the western maria were also acquired at higher spatial and spectral resolutions using M-3's target mode, prior to the end of the Chandrayaan-1 mission. These new observations confirm that both fresh craters and mare soils within the western high-Ti basalts display strong 1 mm and weak 2 mm absorptions consistent with olivine-rich basaltic compositions. The inferred abundance of olivine is observed to correlate with stratigraphic sequence across different mare regions and absolute ages. The apparent stratigraphic evolution and Fe-rich compositions of these basalts as a whole suggest an origin from evolved residual melts rather than through the assimilation of more primitive olivine-rich sources. Mare deposits with spectral properties similar to these late stage high-Ti basalts appear to be very limited outside the Procellarum-Imbrium region of the Moon and, where present, appear to occur as small areas of late stage regional volcanism. Detailed analyses of these new data and supporting measurements are in progress to provide further constraints on the mineralogy, olivine abundance, and compositions of these final products of lunar volcanism and the nature and evolution of their source regions. C1 [Staid, M. I.] Planetary Sci Inst, Tucson, AZ 85719 USA. [Pieters, C. M.; Dhingra, D.; Head, J. W.; Isaacson, P.; Mustard, J. M.] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA. [Besse, S.; Sunshine, J.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Boardman, J.] Analyt Imaging & Geophys LLC, Boulder, CO 80305 USA. [Green, R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Klima, R.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20732 USA. [Kramer, G.] Bear Fight Inst, Winthrop, WA 98862 USA. [Runyon, C.] Coll Charleston, Dept Geol, Charleston, SC 29424 USA. [Taylor, L. A.] Univ Tennessee, Dept Earth & Planetary Sci, Knoxville, TN 37996 USA. RP Staid, MI (reprint author), Planetary Sci Inst, 1700 E Ft Lowell,Ste 106, Tucson, AZ 85719 USA. EM staid@psi.edu OI Besse, Sebastien/0000-0002-1052-5439 FU NASA [NNM05AB26C] FX M3 is funded as a mission of opportunity through the NASA Discovery program. The M3 science team and science validation are supported through NASA contract NNM05AB26C. We thank ISRO for the opportunity to fly as a guest instrument on Chandrayaan-1 and gratefully acknowledge their many contributions to the acquisition and return of the M3 data. NR 102 TC 28 Z9 30 U1 3 U2 14 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 APR 26 PY 2011 VL 116 AR E00G10 DI 10.1029/2010JE003735 PG 15 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 757TA UT WOS:000290109400003 ER PT J AU Smith, DM Dwyer, JR Hazelton, BJ Grefenstette, BW Martinez-McKinney, GFM Zhang, ZY Lowell, AW Kelley, NA Splitt, ME Lazarus, SM Ulrich, W Schaal, M Saleh, ZH Cramer, E Rassoul, HK Cummer, SA Lu, G Blakeslee, RJ AF Smith, D. M. Dwyer, J. R. Hazelton, B. J. Grefenstette, B. W. Martinez-McKinney, G. F. M. Zhang, Z. Y. Lowell, A. W. Kelley, N. A. Splitt, M. E. Lazarus, S. M. Ulrich, W. Schaal, M. Saleh, Z. H. Cramer, E. Rassoul, H. K. Cummer, S. A. Lu, G. Blakeslee, R. J. TI The rarity of terrestrial gamma-ray flashes SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID INTRACLOUD LIGHTNING DISCHARGES; RUNAWAY BREAKDOWN; ELECTRIC-FIELDS; X-RAYS; THUNDERSTORMS; INITIATION; BURSTS; AIR AB We report on the first search for Terrestrial Gamma-ray Flashes (TGFs) from altitudes where they are thought to be produced. The Airborne Detector for Energetic Lightning Emissions (ADELE), an array of gamma-ray detectors, was flown near the tops of Florida thunderstorms in August/September 2009. The plane passed within 10 km horizontal distance of 1213 lightning discharges and only once detected a TGF. If these discharges had produced TGFs of the same intensity as those seen from space, every one should have been seen by ADELE. Separate and significant nondetections are established for intracloud lightning, negative cloud-to-ground lightning, and narrow bipolar events. We conclude that TGFs are not a primary triggering mechanism for lightning. We estimate the TGF-to-flash ratio to be on the order of 10(-2) to 10(-3) and show that TGF intensities cannot follow the well-known power-law distribution seen in earthquakes and solar flares, due to our limits on the presence of faint events. Citation: Smith, D. M., et al. (2011), The rarity of terrestrial gamma-ray flashes, Geophys. Res. Lett., 38, L08807, doi: 10.1029/2011GL046875. C1 [Smith, D. M.; Martinez-McKinney, G. F. M.; Zhang, Z. Y.; Kelley, N. A.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA. [Smith, D. M.; Martinez-McKinney, G. F. M.; Zhang, Z. Y.; Kelley, N. A.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA. [Smith, D. M.; Lowell, A. W.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Dwyer, J. R.; Schaal, M.; Saleh, Z. H.; Cramer, E.; Rassoul, H. K.] Florida Inst Technol, Dept Phys & Space Sci, Melbourne, FL 32901 USA. [Hazelton, B. J.] Univ Washington, Dept Phys, Seattle, WA 98195 USA. [Grefenstette, B. W.] CALTECH, Space Radiat Lab, Pasadena, CA 91125 USA. [Splitt, M. E.; Lazarus, S. M.; Ulrich, W.] Florida Inst Technol, Dept Marine & Environm Syst, Melbourne, FL 32901 USA. [Cummer, S. A.; Lu, G.] Duke Univ, Dept Elect & Comp Engn, Durham, NC 27708 USA. [Blakeslee, R. J.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35805 USA. RP Smith, DM (reprint author), Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, 1156 High St, Santa Cruz, CA 95064 USA. EM dsmith@scipp.ucsc.edu RI Lu, Gaopeng/D-9011-2012; Cummer, Steven/A-6118-2008; OI Cummer, Steven/0000-0002-0002-0613; Rassoul, Hamid Kyan Sam/0000-0003-0681-7276; Lazarus, Steven/0000-0002-5918-1059 FU NSF [ATM-0619941, ATM-0846609] FX We thank Allen Schanot, the managing scientist of our field campaign from NCAR/EOL; the other NCAR scientists who filled this role earlier or helped us with GV data: Pavel Romashkin, Jorgen Jensen, and Jeff Stith; and the EOL pilots, engineers, and technicians who provided exemplary support. We also thank Stan Heckman of Weatherbug/AWS, not only for providing sferic data, but for significant personal attention in helping us interpret the data. ADELE was funded by NSF Major Research Instrumentation grant ATM-0619941. Our simulation work was supported by NSF grant ATM-0846609. NR 30 TC 20 Z9 20 U1 1 U2 2 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD APR 22 PY 2011 VL 38 AR L08807 DI 10.1029/2011GL046875 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 754LD UT WOS:000289855200003 ER PT J AU Tosca, MG Randerson, JT Zender, CS Nelson, DL Diner, DJ Logan, JA AF Tosca, M. G. Randerson, J. T. Zender, C. S. Nelson, D. L. Diner, D. J. Logan, J. A. TI Dynamics of fire plumes and smoke clouds associated with peat and deforestation fires in Indonesia SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID FOREST-FIRE; SATELLITE-OBSERVATIONS; MARITIME CONTINENT; EQUATORIAL ASIA; EL-NINO; BIOMASS; EMISSIONS; TRANSPORT; CONVECTION; POLLUTION AB During the dry season, anthropogenic fires in tropical forests and peatlands of equatorial Asia produce regionally expansive smoke clouds that have important effects on atmospheric radiation and air quality. Here we estimated the height of smoke on Borneo and Sumatra and characterized its sensitivity to El Nino and regional drought. We used Multiangle Imaging Spectroradiometer (MISR) satellite data and the MISR Interactive Explorer (MINX) software to estimate the heights of 317 smoke plumes on Borneo and 139 plumes on Sumatra during 2001-2009. In addition, we estimated the altitudes of larger smoke regions (smoke clouds) over Borneo using data from MISR and Cloud-Aerosol Lidar and Infrared Pathfinder Satellite Observation (CALIPSO) products. Most smoke plumes on Borneo (83%) were observed during El Nino years. Annually averaged plume heights on Borneo were significantly higher during El Nino events. Mean MISR-derived plume heights were 709 +/- 14 m on Borneo and 749 +/- 24 m on Sumatra during 2001-2009, with 96% of all plumes confined to within 500 m of the atmospheric boundary layer. Smoke clouds on Borneo were observed at altitudes between 1000 and 2000 m as measured by both MISR and CALIPSO. The difference in height between individual plumes and longer-lived regional smoke clouds may be related to deeper planetary boundary layers and higher-intensity fires later in the afternoon or other atmospheric mixing processes that occur on synoptic time scales. Our measurements and analyses suggested that direct injection of smoke into the free troposphere within fire plumes was not an important mechanism for vertical mixing of aerosols in equatorial Asia. C1 [Tosca, M. G.; Randerson, J. T.; Zender, C. S.] Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA 92697 USA. [Nelson, D. L.; Diner, D. J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Logan, J. A.] Harvard Univ, Sch Engn & Appl Sci, Cambridge, MA 02138 USA. RP Tosca, MG (reprint author), Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA 92697 USA. EM mtosca@uci.edu RI Zender, Charles/D-4485-2012; Tosca, Michael/J-4908-2015 OI Zender, Charles/0000-0003-0129-8024; Tosca, Michael/0000-0003-1301-8341 FU NSF [ATM-0628637, ARC-0714088]; NASA [NNX08AF64G, 08-Earth08F-189, NNX07AR23G] FX The data presented here are publicly available in a database of plume injection heights (http://misr.jpl.nasa.gov/getData/accessData/MisrMinxPlumes/). We thank three anonymous reviewers for critical analysis and insightful comments about the interpretation of our results. We thank Ralph Kahn for advice on comparisons between MISR and CALIPSO altitudes. We are grateful for support from NSF (ATM-0628637) and NASA (NNX08AF64G). M. G. T. received support from a NASA Earth and Space Science Fellowship (08-Earth08F-189). C.S.Z. acknowledges NSF (ARC-0714088) and NASA (NNX07AR23G) support. The MINX plume digitizing tool is publicly available for Apple and PC users and can be downloaded at: http://www.openchannelfoundation.org/projects/MINX. NR 46 TC 44 Z9 44 U1 4 U2 38 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 APR 22 PY 2011 VL 116 AR D08207 DI 10.1029/2010JD015148 PG 14 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 754KJ UT WOS:000289853200004 ER PT J AU Kramer, GY Combe, JP Harnett, EM Hawke, BR Noble, SK Blewett, DT McCord, TB Giguere, TA AF Kramer, Georgiana Y. Combe, Jean-Philippe Harnett, Erika M. Hawke, Bernard Ray Noble, Sarah K. Blewett, David T. McCord, Thomas B. Giguere, Thomas A. TI Characterization of lunar swirls at Mare Ingenii: A model for space weathering at magnetic anomalies SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID SOLAR-WIND; OPTICAL-PROPERTIES; FINEST FRACTION; ION IRRADIATION; CLEMENTINE DATA; IMPACT CRATERS; MOON; SURFACE; MATURITY; MERCURY AB Analysis of spectra from the Clementine ultraviolet-visible and near-infrared cameras of small, immature craters and surface soils both on and adjacent to the lunar swirls at Mare Ingenii has yielded the following conclusions about space weathering at a magnetic anomaly. (1) Despite having spectral characteristics of immaturity, the lunar swirls are not freshly exposed surfaces. (2) The swirl surfaces are regions of retarded weathering, while immediately adjacent regions experience accelerated weathering. (3) Weathering in the off-swirl regions darkens and flattens the spectrum with little to no reddening, which suggests that the production of larger (>40 nm) nanophase iron dominates in these locations as a result of charged particle sorting by the magnetic field. Preliminary analysis of two other lunar swirl regions, Reiner Gamma and Mare Marginis, is consistent with our observations at Mare Ingenii. Our results indicate that sputtering/vapor deposition, implanted solar wind hydrogen, and agglutination share responsibility for creating the range in npFe(0) particle sizes responsible for the spectral effects of space weathering. C1 [Kramer, Georgiana Y.; Combe, Jean-Philippe; McCord, Thomas B.] Bear Fight Inst, Winthrop, WA 98862 USA. [Harnett, Erika M.] Univ Washington, Dept Earth & Space Sci, Seattle, WA 98195 USA. [Hawke, Bernard Ray; Giguere, Thomas A.] Univ Hawaii, Hawaii Inst Geophys & Planetol, Honolulu, HI 96822 USA. [Noble, Sarah K.] NASA, Marshall Space Flight Ctr, Huntsville, AL 35812 USA. [Blewett, David T.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Giguere, Thomas A.] Intergraph Corp, Kapolei, HI 96706 USA. RP Kramer, GY (reprint author), Lunar & Planetary Inst, 3600 Bay Area Blvd, Houston, TX 77058 USA. EM kramer@lpi.usra.edu RI Noble, Sarah/D-7614-2012; Blewett, David/I-4904-2012 OI Blewett, David/0000-0002-9241-6358 NR 117 TC 18 Z9 18 U1 0 U2 10 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 APR 22 PY 2011 VL 116 AR E04008 DI 10.1029/2010JE003669 PG 18 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 754JX UT WOS:000289852000001 ER PT J AU Pieters, CM Besse, S Boardman, J Buratti, B Cheek, L Clark, RN Combe, JP Dhingra, D Goswami, JN Green, RO Head, JW Isaacson, P Klima, R Kramer, G Lundeen, S Malaret, E McCord, T Mustard, J Nettles, J Petro, N Runyon, C Staid, M Sunshine, J Taylor, LA Thaisen, K Tompkins, S Whitten, J AF Pieters, C. M. Besse, S. Boardman, J. Buratti, B. Cheek, L. Clark, R. N. Combe, J. P. Dhingra, D. Goswami, J. N. Green, R. O. Head, J. W. Isaacson, P. Klima, R. Kramer, G. Lundeen, S. Malaret, E. McCord, T. Mustard, J. Nettles, J. Petro, N. Runyon, C. Staid, M. Sunshine, J. Taylor, L. A. Thaisen, K. Tompkins, S. Whitten, J. TI Mg-spinel lithology: A new rock type on the lunar farside SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID REFLECTANCE SPECTROSCOPY; SELENE; IMPACT; CAMERA; FIELD; MOON; GEOTHERMOMETRY; PETROGENESIS; INSTRUMENT; PYROXENES AB High-resolution compositional data from Moon Mineralogy Mapper (M-3) for the Moscoviense region on the lunar farside reveal three unusual, but distinctive, rock types along the inner basin ring. These are designated "OOS" since they are dominated by high concentrations of orthopyroxene, olivine, and Mg-rich spinel, respectively. The OOS occur as small areas, each a few kilometers in size, that are widely separated within the highly feldspathic setting of the basin rim. Although the abundance of plagioclase is not well constrained within the OOS, the mafic mineral content is exceptionally high, and two of the rock types could approach pyroxenite and harzburgite in composition. The third is a new rock type identified on the Moon that is dominated by Mg-rich spinel with no other mafic minerals detectable (<5% pyroxene, olivine). All OOS surfaces are old and undisturbed since basin formation. They are effectively invisible in image data and are only recognized by their distinctive composition identified spectroscopically. The origin of these unusual lithologies appears to be linked to one or more magmatic intrusions into the lower crust, perhaps near the crust-mantle interface. Processes such as fractional crystallization and gravity settling within such intrusions may provide a mechanism for concentrating the mafic components within zones several kilometers in dimension. The OOS are embedded within highly anorthositic material from the lunar crust; they may thus be near contemporaneous with crustal products from the cooling magma ocean. C1 [Pieters, C. M.; Cheek, L.; Dhingra, D.; Head, J. W.; Isaacson, P.; Mustard, J.; Nettles, J.; Whitten, J.] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA. [Besse, S.; Sunshine, J.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Boardman, J.] Analyt Imaging & Geophys LLC, Boulder, CO 80305 USA. [Buratti, B.; Green, R. O.; Lundeen, S.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Clark, R. N.] US Geol Survey, Fed Ctr, Denver, CO 80225 USA. [Combe, J. P.; Kramer, G.; McCord, T.] Bear Fight Inst, Winthrop, WA 98862 USA. [Goswami, J. N.] NAVRANGPURA THALTEJ, ISRO, Phys Res Lab, Ahmadabad 380009, Gujarat, India. [Klima, R.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20732 USA. [Malaret, E.] Appl Coherent Technol Corp, Herndon, VA 22070 USA. [Petro, N.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Runyon, C.] Coll Charleston, Dept Geol, Charleston, SC 29424 USA. [Staid, M.] Planetary Sci Inst, Tucson, AZ 85719 USA. [Taylor, L. A.; Thaisen, K.] Univ Tennessee, Planetary Geosci Inst, Dept Earth & Planetary Sci, Knoxville, TN 37996 USA. [Tompkins, S.] Def Adv Res Projects Agcy, Arlington, VA 22203 USA. RP Pieters, CM (reprint author), Brown Univ, Dept Geol Sci, Box 1846, Providence, RI 02912 USA. EM carle_pieters@Brown.edu RI Klima, Rachel/H-9383-2012; Petro, Noah/F-5340-2013; OI Klima, Rachel/0000-0002-9151-6429; Besse, Sebastien/0000-0002-1052-5439 FU NASA [NNM05AB26C] FX M3 is supported as a NASA Discovery Program mission of opportunity. These science results and science validation is supported through NASA contract NNM05AB26C. The M3 team is honored to have had the opportunity to fly as a guest instrument on Chandrayaan-1, and we are grateful to all the ISRO team that enabled M3 data to be returned. We gratefully acknowledge the valuable input to this project by the Chandrayaan-1 Terrain Mapping Camera team led by K. Kumar and by the public release of SELENE Terrain Camera data and LRO Narrow Angle Camera data. We appreciate the helpful review comments by Brad Jolliff. NR 51 TC 51 Z9 56 U1 1 U2 19 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9097 EI 2169-9100 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD APR 22 PY 2011 VL 116 AR E00G08 DI 10.1029/2010JE003727 PG 14 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 754JX UT WOS:000289852000003 ER PT J AU Ruff, SW Farmer, JD Calvin, WM Herkenhoff, KE Johnson, JR Morris, RV Rice, MS Arvidson, RE Bell, JF Christensen, PR Squyres, SW AF Ruff, Steven W. Farmer, Jack D. Calvin, Wendy M. Herkenhoff, Kenneth E. Johnson, Jeffrey R. Morris, Richard V. Rice, Melissa S. Arvidson, Raymond E. Bell, James F., III Christensen, Philip R. Squyres, Steven W. TI Characteristics, distribution, origin, and significance of opaline silica observed by the Spirit rover in Gusev crater, Mars SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID TAUPO VOLCANIC ZONE; THERMAL EMISSION-SPECTROSCOPY; YELLOWSTONE-NATIONAL-PARK; NEW-ZEALAND; HYDROTHERMAL ALTERATION; PARTICULATE SURFACES; REFLECTANCE SPECTRA; GEOTHERMAL FIELDS; SPRING DEPOSITS; LOW-TEMPERATURE AB The presence of outcrops and soil (regolith) rich in opaline silica (similar to 65-92 wt % SiO2) in association with volcanic materials adjacent to the "Home Plate" feature in Gusev crater is evidence for hydrothermal conditions. The Spirit rover has supplied a diverse set of observations that are used here to better understand the formation of silica and the activity, abundance, and fate of water in the first hydrothermal system to be explored in situ on Mars. We apply spectral, chemical, morphological, textural, and stratigraphic observations to assess whether the silica was produced by acid sulfate leaching of precursor rocks, by precipitation from silica-rich solutions, or by some combination. The apparent lack of S enrichment and the relatively low oxidation state of the Home Plate silica-rich materials appear inconsistent with the originally proposed Hawaiian analog for fumarolic acid sulfate leaching. The stratiform distribution of the silica-rich outcrops and their porous and brecciated microtextures are consistent with sinter produced by silica precipitation. There is no evidence for crystalline quartz phases among the silica occurrences, an indication of the lack of diagenetic maturation following the production of the amorphous opaline phase. C1 [Ruff, Steven W.; Farmer, Jack D.; Christensen, Philip R.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [Calvin, Wendy M.] Univ Nevada, Dept Geol Sci, Reno, NV 89557 USA. [Herkenhoff, Kenneth E.; Johnson, Jeffrey R.] US Geol Survey, Astrogeol Team, Flagstaff, AZ 86001 USA. [Morris, Richard V.] NASA, Johnson Space Ctr, Houston, TX 77058 USA. [Rice, Melissa S.; Bell, James F., III; Squyres, Steven W.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. [Arvidson, Raymond E.] Washington Univ, Dept Planetary Sci, St Louis, MO 63130 USA. RP Ruff, SW (reprint author), Arizona State Univ, Sch Earth & Space Explorat, Moeur Bldg,Rm 131,Box 876305, Tempe, AZ 85287 USA. EM steve.ruff@asu.edu RI Johnson, Jeffrey/F-3972-2015 FU NASA FX This work was funded in part by NASA grants from the Mars Data Analysis and Mars Fundamental Research programs. We thank Patrick Browne and an anonymous reviewer for their thorough and thoughtful reviews of a very lengthy manuscript. Their suggestions have improved the final paper. NR 88 TC 47 Z9 47 U1 3 U2 31 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 APR 22 PY 2011 VL 116 AR E00F23 DI 10.1029/2010JE003767 PG 48 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 754JX UT WOS:000289852000005 ER PT J AU Laurent, P Rodriguez, J Wilms, J Bel, MC Pottschmidt, K Grinberg, V AF Laurent, P. Rodriguez, J. Wilms, J. Bel, M. Cadolle Pottschmidt, K. Grinberg, V. TI Polarized Gamma-Ray Emission from the Galactic Black Hole Cygnus X-1 SO SCIENCE LA English DT Article ID BROAD-BAND SPECTRUM; X-RAY; ACCRETION DISKS; LOW/HARD STATE; RADIATION; JETS; TELESCOPE; IBIS AB Because of their inherently high flux allowing the detection of clear signals, black hole x-ray binaries are interesting candidates for polarization studies, even if no polarization signals have been observed from them before. Such measurements would provide further detailed insight into these sources' emission mechanisms. We measured the polarization of the gamma-ray emission from the black hole binary system Cygnus X-1 with the International Gamma-Ray Astrophysics Laboratory Imager on Board the Integral Satellite (INTEGRAL/IBIS) telescope. Spectral modeling of the data reveals two emission mechanisms: The 250- to 400-keV ( kilo-electron volt) data are consistent with emission dominated by Compton scattering on thermal electrons and are weakly polarized. The second spectral component seen in the 400-keV to 2-MeV band is by contrast strongly polarized, revealing that the MeV emission is probably related to the jet first detected in the radio band. C1 [Laurent, P.] Commissariat Energie Atom & Energies Alternat, Inst Rech Lois Fondamentales Univers CEA IRFU, F-75205 Paris 13, France. [Rodriguez, J.] Univ Paris Diderot, Inst Natl Sci Univers, CEA Saclay, DSM,IRFU,SAp,CEA,Lab AIM,CNRS, F-91191 Gif Sur Yvette, France. [Wilms, J.; Grinberg, V.] Univ Erlangen Nurnberg, Dr Karl Remeis Sternwarte & Erlangen Ctr Astropar, D-96049 Bamberg, Germany. [Bel, M. Cadolle] European Space Astron Ctr, Sci Operat Dept, Int Gamma Ray Astrophys Lab INTEGRAL Sci Operat C, E-28691 Madrid, Spain. [Pottschmidt, K.] CRESST, Greenbelt, MD 20771 USA. [Pottschmidt, K.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Pottschmidt, K.] Univ Maryland Baltimore Cty, Ctr Space Sci & Technol, Baltimore, MD 21250 USA. RP Laurent, P (reprint author), Commissariat Energie Atom & Energies Alternat, Inst Rech Lois Fondamentales Univers CEA IRFU, 10 Rue Alice Domon & Leonie Duquet, F-75205 Paris 13, France. EM plaurent@cea.fr RI Wilms, Joern/C-8116-2013; OI Wilms, Joern/0000-0003-2065-5410; Rodriguez, Jerome/0000-0002-4151-4468 FU European Commission [ITN 215212]; Bundesministerium fur Wirtschaft und Technologie under Deutsches Zentrum fur Luftund Raumfahrt [50 OR 1007]; NASA [NNX08AE84G, NNX08AY24G, NX09AT28G] FX ISGRI has been realized and maintained in flight by CEA-Saclay/IRFU with the support of Centre National d'Etudes Spatiales. Based on observations with INTEGRAL, a European Space Agency (ESA) project with instruments and science data center funded by ESA member states (especially the Principal Investigator countries: Denmark, France, Germany, Italy, Switzerland, and Spain), Czech Republic and Poland, and with the participation of Russia and the United States. We acknowledge partial funding from the European Commission under contract ITN 215212 "Black Hole Universe" and from the Bundesministerium fur Wirtschaft und Technologie under Deutsches Zentrum fur Luftund Raumfahrt grant 50 OR 1007. K. P. acknowledges support by NASA's INTEGRAL Guest Observer grants NNX08AE84G, NNX08AY24G, and NX09AT28G. We thank S. Corbel for useful comments. NR 31 TC 97 Z9 97 U1 1 U2 4 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 APR 22 PY 2011 VL 332 IS 6028 BP 438 EP 439 DI 10.1126/science.1200848 PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 753NG UT WOS:000289784900035 PM 21436402 ER PT J AU Minazzoli, O Chauvineau, B AF Minazzoli, Olivier Chauvineau, Bertrand TI Scalar-tensor propagation of light in the inner solar system including relevant c(-4) contributions for ranging and time transfer SO CLASSICAL AND QUANTUM GRAVITY LA English DT Article ID COSMOLOGICAL CONSTANT; GENERAL-RELATIVITY; SITTER SPACETIMES; GRAVITY-FIELD; CORE; KERR-(ANTI); DYNAMICS; ROTATION; ORBITS; MODES AB In a recent paper (Minazzoli and Chauvineau 2009 Phys. Rev. D 79 084027), motivated by forthcoming space experiments involving propagation of light in the solar system, we have proposed an extension of the IAU metric equations at the c(-4) level in general relativity. However, scalar-tensor theories may induce corrections numerically comparable to the c(-4) general relativistic terms. Accordingly, one first proposes in this paper an extension of Minazzoli and Chauvineau (2009) to the scalar-tensor case. The case of a hierarchized system (such as the solar system) is emphasized. In this case, the relevant metric solution is proposed. Then, the corresponding isotropic geodesic solution relevant for distance measurements and time transfers in the inner solar system is given in explicit form. C1 [Minazzoli, Olivier; Chauvineau, Bertrand] Observ Cote Azur, ARTEMIS CNRS UMR 6162, UNS, F-06304 Nice, France. [Minazzoli, Olivier] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Minazzoli, Olivier] Univ Nice, ICRAnet, F-06103 Nice, France. [Chauvineau, Bertrand] Observ Cote Azur, CASSIOPEE CNRS UMR6202, UNS, F-06304 Nice, France. RP Minazzoli, O (reprint author), Observ Cote Azur, ARTEMIS CNRS UMR 6162, UNS, F-06304 Nice, France. EM olivier.l.minazzoli@jpl.nasa.gov; bertrand.chauvineau@oca.eu OI Minazzoli, Olivier/0000-0002-3151-7593 FU Government of the Principality of Monaco FX OM wants to thank the Government of the Principality of Monaco for their financial support. NR 59 TC 15 Z9 15 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0264-9381 EI 1361-6382 J9 CLASSICAL QUANT GRAV JI Class. Quantum Gravity PD APR 21 PY 2011 VL 28 IS 8 AR 085010 DI 10.1088/0264-9381/28/8/085010 PG 27 WC Astronomy & Astrophysics; Physics, Multidisciplinary; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 752FV UT WOS:000289677400011 ER PT J AU Comiso, JC Kwok, R Martin, S Gordon, AL AF Comiso, Josefino C. Kwok, Ronald Martin, Seelye Gordon, Arnold L. TI Variability and trends in sea ice extent and ice production in the Ross Sea SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS LA English DT Article ID SOUTHERN-OCEAN; CLIMATE-CHANGE; ANNULAR MODE; SHELF; THICKNESS; POLYNYA; SURFACE; WESTERN; FLUX; OSCILLATION AB Salt release during sea ice formation in the Ross Sea coastal regions is regarded as a primary forcing for the regional generation of Antarctic Bottom Water. Passive microwave data from November 1978 through 2008 are used to examine the detailed seasonal and interannual characteristics of the sea ice cover of the Ross Sea and the adjacent Bellingshausen and Amundsen seas. For this period the sea ice extent in the Ross Sea shows the greatest increase of all the Antarctic seas. Variability in the ice cover in these regions is linked to changes in the Southern Annular Mode and secondarily to the Antarctic Circumpolar Wave. Over the Ross Sea shelf, analysis of sea ice drift data from 1992 to 2008 yields a positive rate of increase in the net ice export of about 30,000 km(2) yr(-1). For a characteristic ice thickness of 0.6 m, this yields a volume transport of about 20 km(3) yr(-1), which is almost identical, within error bars, to our estimate of the trend in ice production. The increase in brine rejection in the Ross Shelf Polynya associated with the estimated increase with the ice production, however, is not consistent with the reported Ross Sea salinity decrease. The locally generated sea ice enhancement of Ross Sea salinity may be offset by an increase of relatively low salinity of the water advected into the region from the Amundsen Sea, a consequence of increased precipitation and regional glacial ice melt. C1 [Comiso, Josefino C.] NASA, Cryospher Sci Branch, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Kwok, Ronald] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Martin, Seelye] Univ Washington, Sch Oceanog, Seattle, WA 98195 USA. [Gordon, Arnold L.] Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY 10964 USA. RP Comiso, JC (reprint author), NASA, Cryospher Sci Branch, Goddard Space Flight Ctr, 8800 Greenbelt Rd,Code 614-1, Greenbelt, MD 20771 USA. EM josefino.c.comiso@nasa.gov RI Gordon, Arnold/H-1049-2011; Kwok, Ron/A-9762-2008 OI Gordon, Arnold/0000-0001-6480-6095; Kwok, Ron/0000-0003-4051-5896 FU NASA [NNG04GM69G]; National Science Foundation Office of the Polar Programs [ANT-0538148]; National Science Foundation FX J.C.C. would like to thank Robert Gerstein for programming support in the analysis of SSM/I and AMSR-E data and is grateful to the NASA Cryospheric Sciences Program for funding support. S. M. thanks Robert Drucker for his help with Figure 13 and gratefully acknowledges the support of NASA under contract NNG04GM69G. R. K. performed this work at the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA. A.L.G.'s support is from the National Science Foundation Office of the Polar Programs grant ANT-0538148, Lamont-Doherty contribution number 7397. We all thank the National Snow and Ice Data Center for provision of the SMMR, SSM/I and AMSR-E data. The ECMWF meteorological products are provided by the Data Support Section of the Scientific Computing Division of the National Center for Atmospheric Research (NCAR). NCAR is supported by grants from the National Science Foundation. NR 49 TC 60 Z9 60 U1 2 U2 34 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 APR 21 PY 2011 VL 116 AR C04021 DI 10.1029/2010JC006391 PG 19 WC Oceanography SC Oceanography GA 754JV UT WOS:000289851800002 ER PT J AU Pryor, WR Rymer, AM Mitchell, DG Hill, TW Young, DT Saur, J Jones, GH Jacobsen, S Cowley, SWH Mauk, BH Coates, AJ Gustin, J Grodent, D Gerard, JC Lamy, L Nichols, JD Krimigis, SM Esposito, LW Dougherty, MK Jouchoux, AJ Stewart, AIF McClintock, WE Holsclaw, GM Ajello, JM Colwell, JE Hendrix, AR Crary, FJ Clarke, JT Zhou, XY AF Pryor, Wayne R. Rymer, Abigail M. Mitchell, Donald G. Hill, Thomas W. Young, David T. Saur, Joachim Jones, Geraint H. Jacobsen, Sven Cowley, Stan W. H. Mauk, Barry H. Coates, Andrew J. Gustin, Jacques Grodent, Denis Gerard, Jean-Claude Lamy, Laurent Nichols, Jonathan D. Krimigis, Stamatios M. Esposito, Larry W. Dougherty, Michele K. Jouchoux, Alain J. Stewart, A. Ian F. McClintock, William E. Holsclaw, Gregory M. Ajello, Joseph M. Colwell, Joshua E. Hendrix, Amanda R. Crary, Frank J. Clarke, John T. Zhou, Xiaoyan TI The auroral footprint of Enceladus on Saturn SO NATURE LA English DT Article ID IO FLUX TUBE; CASSINI; ATMOSPHERE; MAGNETOSPHERE; SPECTROMETER; JUPITER; ORIGIN; PLASMA; PLUME AB Although there are substantial differences between the magnetospheres of Jupiter and Saturn, it has been suggested that cryovolcanic activity at Enceladus(1-9) could lead to electrodynamic coupling between Enceladus and Saturn like that which links Jupiter with Io, Europa and Ganymede. Powerful field-aligned electron beams associated with the Io-Jupiter coupling, for example, create an auroral footprint in Jupiter's ionosphere(10,11). Auroral ultraviolet emission associated with Enceladus-Saturn coupling is anticipated to be just a few tenths of a kilorayleigh (ref. 12), about an order of magnitude dimmer than Io's footprint and below the observable threshold, consistent with its non-detection(13). Here we report the detection of magnetic-field-aligned ion and electron beams (offset several moon radii downstream from Enceladus) with sufficient power to stimulate detectable aurora, and the subsequent discovery of Enceladus-associated aurora in a few per cent of the scans of the moon's footprint. The footprint varies in emission magnitude more than can plausibly be explained by changes in magnetospheric parameters-and as such is probably indicative of variable plume activity. C1 [Rymer, Abigail M.; Mitchell, Donald G.; Mauk, Barry H.; Krimigis, Stamatios M.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Pryor, Wayne R.] Cent Arizona Coll, Dept Sci, Coolidge, AZ 85128 USA. [Pryor, Wayne R.] Space Environm Technol, Pacific Palisades, CA 90272 USA. [Hill, Thomas W.] Rice Univ, Dept Phys & Astron, Houston, TX 77005 USA. [Young, David T.; Crary, Frank J.] SW Res Inst, Space Sci & Engn Div, San Antonio, TX 78238 USA. [Saur, Joachim; Jacobsen, Sven] Univ Cologne, Inst Geophys & Meteorol, D-50923 Cologne, Germany. [Jones, Geraint H.; Coates, Andrew J.] Univ Coll London, Mullard Space Sci Lab, Dept Space & Climate Phys, Dorking RH5 6NT, Surrey, England. [Jones, Geraint H.] Univ London Birkbeck Coll, Ctr Planetary Sci, London WC1E 6BT, England. [Cowley, Stan W. H.; Nichols, Jonathan D.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Gustin, Jacques; Grodent, Denis; Gerard, Jean-Claude] Univ Liege, Lab Phys Atmospher & Planetaire, Dept Astrophys Geophys & Oceanog, B-4000 Liege, Belgium. [Lamy, Laurent] Univ Paris Diderot, Univ Pierre & Marie Curie, Lab Etud Spatiales & Instrumentat Astrophys, Observ Paris,Ctr Natl Rech Sci, F-92195 Meudon, France. [Krimigis, Stamatios M.] Acad Athens, Athens 11527, Greece. [Esposito, Larry W.; Jouchoux, Alain J.; Stewart, A. Ian F.; McClintock, William E.; Holsclaw, Gregory M.] Univ Colorado, Lab Atmospher & Space Phys, Boulder, CO 80303 USA. [Dougherty, Michele K.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, London SW7 2AZ, England. [Ajello, Joseph M.; Hendrix, Amanda R.; Zhou, Xiaoyan] Jet Prop Lab, Pasadena, CA 91109 USA. [Colwell, Joshua E.] Univ Cent Florida, Dept Phys, Orlando, FL 32816 USA. [Clarke, John T.] Boston Univ, Dept Astron, Boston, MA 02215 USA. RP Rymer, AM (reprint author), Johns Hopkins Univ, Appl Phys Lab, Johns Hopkins Rd, Laurel, MD 20723 USA. EM abigail.rymer@jhuapl.edu RI Nichols, Jonathan/F-5764-2010; Coates, Andrew/C-2396-2008; Clarke, John/C-8644-2013; Jacobsen, Sven/E-1763-2013; Jones, Geraint/C-1682-2008; Mauk, Barry/E-8420-2017; OI Nichols, Jonathan/0000-0002-8004-6409; Coates, Andrew/0000-0002-6185-3125; Mauk, Barry/0000-0001-9789-3797; Jones, Geraint/0000-0002-5859-1136; GERARD, Jean-Claude/0000-0002-8565-8746 FU NASA/ESA; NASA FX We acknowledge support from the NASA/ESA Cassini Project and NASA's Cassini Data Analysis Program. NR 30 TC 49 Z9 49 U1 0 U2 16 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 APR 21 PY 2011 VL 472 IS 7343 BP 331 EP 333 DI 10.1038/nature09928 PG 3 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 752VW UT WOS:000289724600035 PM 21512570 ER PT J AU Green, JD Evans, NJ Kospal, A van Kempen, TA Herczeg, G Quanz, SP Henning, T Lee, JE Dunham, MM Meeus, G Bouwman, J van Dishoeck, E Chen, JH Gudel, M Skinner, SL Merello, M Pooley, D Rebull, LM Guieu, S AF Green, Joel D. Evans, Neal J., II Kospal, Agnes van Kempen, Tim A. Herczeg, Gregory Quanz, Sascha P. Henning, Thomas Lee, Jeong-Eun Dunham, Michael M. Meeus, Gwendolyn Bouwman, Jeroen van Dishoeck, Ewine Chen, Jo-Hsin Guedel, Manuel Skinner, Stephen L. Merello, Manuel Pooley, David Rebull, Luisa M. Guieu, Sylvain TI DISENTANGLING THE ENVIRONMENT OF THE FU ORIONIS CANDIDATE HBC 722 WITH HERSCHEL SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE ISM: jets and outflows; stars: individual (HBC 722); stars: pre-main sequence; stars: variables: T Tauri, Herbig Ae/Be; submillimeter: ISM ID NORTH-AMERICA; SHARC-II; SUBMILLIMETER; OBJECTS; STARS; EVOLUTION; DISKS; DUST; PROTOSTELLAR; INSTRUMENT AB We analyze the submillimeter emission surrounding the new FU Orionis-type object, HBC 722. We present the first epoch of observations of the active environs of HBC 722, with imaging and spectroscopy from PACS, SPIRE, and HIFI on board the Herschel Space Observatory, as well as CO J = 2-1 and 350 mu m imaging (SHARC-II) with the Caltech Submillimeter Observatory. The primary source of submillimeter continuum emission in the region-2MASS 20581767+4353310-is located 16 '' south-southeast of the optical flaring source while the optical and near-infrared emission is dominated by HBC 722. A bipolar outflow extends over HBC 722; the most likely driver is the submillimeter source. We detect warm (100 K) and hot (246 K) CO emission in the surrounding region, evidence of outflow-driven heating in the vicinity. The region around HBC 722 itself shows little evidence of heating driven by the new outbursting source itself. C1 [Green, Joel D.; Evans, Neal J., II; Merello, Manuel; Pooley, David] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Kospal, Agnes; van Kempen, Tim A.; van Dishoeck, Ewine] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [van Kempen, Tim A.] Joint ALMA Off, Santiago, Chile. [Herczeg, Gregory; van Dishoeck, Ewine] Max Planck Inst Extraterr Phys, D-37075 Garching, Germany. [Quanz, Sascha P.] ETH, Inst Astron, CH-8092 Zurich, Switzerland. [Henning, Thomas; Bouwman, Jeroen] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Lee, Jeong-Eun] Kyung Hee Univ, Dept Astron & Space Sci, Gyeonggi 446701, South Korea. [Dunham, Michael M.] Yale Univ, Dept Astron, New Haven, CT 06511 USA. [Meeus, Gwendolyn] Univ Autonoma Madrid, Dept Fis Teor C XV, E-28049 Madrid, Spain. [Chen, Jo-Hsin] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Guedel, Manuel] Univ Vienna, Dept Astron, A-1010 Vienna, Austria. [Skinner, Stephen L.] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA. [Pooley, David] Eureka Sci, Austin, TX USA. [Rebull, Luisa M.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Guieu, Sylvain] European So Observ, Santiago 19, Chile. RP Green, JD (reprint author), Univ Texas Austin, Dept Astron, RLM 15308, Austin, TX 78712 USA. RI Lee , Jeong-Eun/E-2387-2013; Guedel, Manuel/C-8486-2015; OI Guedel, Manuel/0000-0001-9818-0588; Rebull, Luisa/0000-0001-6381-515X; Herczeg, Gregory/0000-0002-7154-6065 FU Netherlands Organisation for Scientific Research; Ministry of Education, Science and Technology [2010-0008704] FX The authors acknowledge the Herschel Director, G.L. Pilbratt, for the timely approval and execution of this Target of Opportunity program; Amanda Heiderman for providing CSO data; Paul Harvey, Michelle Rascati, and the HSC and NHSC Helpdesk for data processing and analysis assistance, and Colette Salyk and Geoff Blake for helpful discussions. The research of A.K. is supported by the Netherlands Organisation for Scientific Research. The research of J.-E.L. is supported by Basic Science Research Program through the National Research Foundation of Korea (NRF) funded by the Ministry of Education, Science and Technology (no. 2010-0008704). This work is based in part on data obtained as part of the UKIRT Infrared Deep Sky Survey. NR 34 TC 14 Z9 14 U1 1 U2 8 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 APR 20 PY 2011 VL 731 IS 2 AR L25 DI 10.1088/2041-8205/731/2/L25 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 797LB UT WOS:000293128100004 ER PT J AU Brower, LP Williams, EH Fink, LS Slayback, DA Ramirez, MI Garcia, MV Zubieta, RR Weiss, SB Calvert, WH Zuchowski, W AF Brower, Lincoln P. Williams, Ernest H. Fink, Linda S. Slayback, Daniel A. Isabel Ramirez, M. Van Limon Garcia, M. Zubieta, Raul R. Weiss, Stuart B. Calvert, William H. Zuchowski, Willow TI OVERWINTERING CLUSTERS OF THE MONARCH BUTTERFLY COINCIDE WITH THE LEAST HAZARDOUS VERTICAL TEMPERATURES IN THE OYAMEL FOREST SO JOURNAL OF THE LEPIDOPTERISTS SOCIETY LA English DT Article DE Danaus plexippus; conservation; Monarch Butterfly Biosphere Reserve; forest management; microclimate; trunk and bough clustering behavior; vertical temperature distribution; negative effects of forest thinning ID MOUNTAIN CHICKADEES; DANAUS-PLEXIPPUS; SITE SELECTION; MEXICO; MICROCLIMATE; ADVANTAGES; SURVIVAL AB During winter, monarch butterflies form dense colonies in oyamel fir forests on high mountains in central Mexico, where the forest canopy serves both as a blanket, moderating temperature, and an umbrella, shielding the butterflies from rain. In this study we investigated die vertical dimension of the butterflies' use of the oyamel forest: we predicted that clusters form at the heights above ground that provide the greatest protection from freezing. By suspending temperature recorders at eight heights, from ground level up to 22m, we established two vertical transects in the forest. We set one transect in a densely forested area and the other in a thinned area, and we recorded hourly temperatures from Jan 13 through Feb 5, 2006. Intermediate heights in the forest, from 10 to 15m above ground, remained the warmest during the cold night and early morning. We also determined that this temperature distribution matched available records of the vertical distribution of butterflies roosting in branch and trunk clusters. The vertical temperature profiles became uniform during mid-day. Temperature extremes were moderated more dining clear than during cloudy periods and more in the denser than in the thinned forest. Our results illustrate how the monarch butterfly is behaviorally adapted to the three-dimensional complexity of microclimate in the yarned forest. A denser forest provides better protection for the overwintering survival of monarch butterflies than a thinned forest. This research bolsters our other microclimatic studies, all of which point to the urgency of prohibiting logging within the oyamel forest used as wintering habitat by monarch butterflies. C1 [Brower, Lincoln P.; Fink, Linda S.] Sweet Briar Coll, Dept Biol, Sweet Briar, VA 24595 USA. [Williams, Ernest H.] Hamilton Coll, Dept Biol, Clinton, NY 13323 USA. [Slayback, Daniel A.] NASA, Goddard Space Flight Ctr, Sci Syst & Applicat Inc, Biospher Sci Branch, Greenbelt, MD 20771 USA. [Isabel Ramirez, M.] Univ Nacl Autonoma Mexico, Ctr Invest Geog Ambiental, Morelia 58190, Michoacan, Mexico. [Van Limon Garcia, M.] Univ Nacl Autonoma Mexico, Fac Ciencias, Inst Geog, Mexico City 04510, DF, Mexico. [Weiss, Stuart B.] Creekside Ctr Earth Observat, Menlo Pk, CA 94025 USA. RP Brower, LP (reprint author), Sweet Briar Coll, Dept Biol, Sweet Briar, VA 24595 USA. EM brower@sbc.edu RI Slayback, Daniel/E-7465-2011; Ramirez, M. Isabel/D-3010-2012 FU National Science Foundation [14265, DEB-0415340]; Hamilton College; DGAPA-PAPIIT [IN114707] FX We are indebted to Prof. Rudolf Geiger for his pioneering syntheses of microclimate. We thank Jennifer Wiley and Carlos Carrillo Tellez for help in setting the vertical transects. We are grateful to lug. Concepcion Miguel Martinez, former Director of the Monarch Butterfly Biosphere Reserve, for facilitating our access to the study area, and to the Arizmendi family for providing accommodations in Angangueo. We are grateful to Myron Zalucki and Jenny Williams for critiques of the manuscript and to Zach Dietz for extensive advice on statistical analyses. Support during the 1978-1979 overwintering season was provided by National Science Foundation grant 14265 to Amherst College with L.P. Brower as principal investigator, and during 2006 by NSF grant DEB-0415340 to Sweet Briar College with L.P. Brower and L.S. Fink as principal investigators. We are grateful for additional support from the October Hill Foundation, the Monarch Butterfly Sanctuary Foundation, and SCION Natural Science Association, Ernest Williams was supported by the Leonard C. Ferguson and Christian A. Johnson Professorship Funds at Hamilton College. DGAPA-PAPIIT (IN114707) provided financial support to M. Isabel Ramirez. NR 62 TC 1 Z9 2 U1 2 U2 22 PU LEPIDOPTERISTS SOC PI LOS ANGELES PA 900 EXPOSITION BLVD, LOS ANGELES, CA 90007-4057 USA SN 0024-0966 J9 J LEPID SOC JI J. Lepid. Soc. PD APR 20 PY 2011 VL 65 IS 1 BP 27 EP 46 PG 20 WC Entomology SC Entomology GA 758AM UT WOS:000290131800003 ER PT J AU Foley, RJ Andersson, K Bazin, G de Haan, T Ruel, J Ade, PAR Aird, KA Armstrong, R Ashby, MLN Bautz, M Benson, BA Bleem, LE Bonamente, M Brodwin, M Carlstrom, JE Chang, CL Clocchiatti, A Crawford, TM Crites, AT Desai, S Dobbs, MA Dudley, JP Fazio, GG Forman, WR Garmire, G George, EM Gladders, MD Gonzalez, AH Halverson, NW High, FW Holder, GP Holzapfel, WL Hoover, S Hrubes, JD Jones, C Joy, M Keisler, R Knox, L Lee, AT Leitch, EM Lueker, M Luong-Van, D Marrone, DP McMahon, JJ Mehl, J Meyer, SS Mohr, JJ Montroy, TE Murray, SS Padin, S Plagge, T Pryke, C Reichardt, CL Rest, A Ruhl, JE Saliwanchik, BR Saro, A Schaffer, KK Shaw, L Shirokoff, E Song, J Spieler, HG Stalder, B Stanford, SA Staniszewski, Z Stark, AA Story, K Stubbs, CW Vanderlinde, K Vieira, JD Vikhlinin, A Williamson, R Zenteno, A AF Foley, R. J. Andersson, K. Bazin, G. de Haan, T. Ruel, J. Ade, P. A. R. Aird, K. A. Armstrong, R. Ashby, M. L. N. Bautz, M. Benson, B. A. Bleem, L. E. Bonamente, M. Brodwin, M. Carlstrom, J. E. Chang, C. L. Clocchiatti, A. Crawford, T. M. Crites, A. T. Desai, S. Dobbs, M. A. Dudley, J. P. Fazio, G. G. Forman, W. R. Garmire, G. George, E. M. Gladders, M. D. Gonzalez, A. H. Halverson, N. W. High, F. W. Holder, G. P. Holzapfel, W. L. Hoover, S. Hrubes, J. D. Jones, C. Joy, M. Keisler, R. Knox, L. Lee, A. T. Leitch, E. M. Lueker, M. Luong-Van, D. Marrone, D. P. McMahon, J. J. Mehl, J. Meyer, S. S. Mohr, J. J. Montroy, T. E. Murray, S. S. Padin, S. Plagge, T. Pryke, C. Reichardt, C. L. Rest, A. Ruhl, J. E. Saliwanchik, B. R. Saro, A. Schaffer, K. K. Shaw, L. Shirokoff, E. Song, J. Spieler, H. G. Stalder, B. Stanford, S. A. Staniszewski, Z. Stark, A. A. Story, K. Stubbs, C. W. Vanderlinde, K. Vieira, J. D. Vikhlinin, A. Williamson, R. Zenteno, A. TI DISCOVERY AND COSMOLOGICAL IMPLICATIONS OF SPT-CL J2106-5844, THE MOST MASSIVE KNOWN CLUSTER AT z > 1 SO ASTROPHYSICAL JOURNAL LA English DT Article DE early universe; galaxies: clusters: individual (SPT-CL J2106-5844); galaxies: evolution; galaxies: formation; large-scale structure of universe ID SOUTH-POLE TELESCOPE; IRAC SHALLOW SURVEY; GALAXY CLUSTER; X-RAY; SPECTROSCOPIC CONFIRMATION; VELOCITY DISPERSIONS; ENVIRONMENT; EXTRACTION; PRECISION; REDSHIFTS AB Using the South Pole Telescope (SPT), we have discovered the most massive known galaxy cluster at z > 1, SPT-CL J2106-5844. In addition to producing a strong Sunyaev-Zel'dovich (SZ) effect signal, this system is a luminous X-ray source and its numerous constituent galaxies display spatial and color clustering, all indicating the presence of a massive galaxy cluster. Very Large Telescope and Magellan spectroscopy of 18 member galaxies shows that the cluster is at z = 1.132(-0.003)(+0.002). Chandra observations obtained through a combined HRC-ACIS GTO program reveal an X-ray spectrum with an Fe K line redshifted by z = 1.18 +/- 0.03. These redshifts are consistent with the galaxy colors found in optical, near-infrared, and mid-infrared imaging. SPT-CL J2106-5844 displays extreme X-ray properties for a cluster having a core-excluded temperature of T-X = 11.0(-1.9)(+2.6) keV and a luminosity (within r(500)) of L-X(0.5-2.0 keV) = (13.9 +/- 1.0) x 10(44) erg s(-1). The combined mass estimate from measurements of the SZ effect and X-ray data is M-200 = (1.27 +/- 0.21) x 10(15) h(70)(-1) M-circle dot. The discovery of such amassive gravitationally collapsed system at high redshift provides an interesting laboratory for galaxy formation and evolution, and is a probe of extreme perturbations of the primordial matter density field. We discuss the latter, determining that, under the assumption of Lambda CDM cosmology with only Gaussian perturbations, there is only a 7% chance of finding a galaxy cluster similar to SPT-CL J2106-5844 in the 2500 deg(2) SPT survey region and that only one such galaxy cluster is expected in the entire sky. C1 [Foley, R. J.; Ashby, M. L. N.; Brodwin, M.; Fazio, G. G.; Forman, W. R.; Jones, C.; Murray, S. S.; Stalder, B.; Stark, A. A.; Stubbs, C. W.; Vikhlinin, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Andersson, K.; Bazin, G.; Mohr, J. J.; Saro, A.; Zenteno, A.] Univ Munich, Dept Phys, D-81679 Munich, Germany. [Andersson, K.; Bautz, M.] MIT, MIT Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Bazin, G.; Mohr, J. J.; Zenteno, A.] Excellence Cluster Universe, D-85748 Garching, Germany. [de Haan, T.; Dobbs, M. A.; Dudley, J. P.; Holder, G. P.; Shaw, L.; Vanderlinde, K.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Ruel, J.; Rest, A.; Stubbs, C. W.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Ade, P. A. R.] Cardiff Univ, Dept Phys & Astron, Cardiff CF24 3YB, S Glam, Wales. [Armstrong, R.; Desai, S.] Univ Illinois, Natl Ctr Supercomp Applicat, Urbana, IL 61801 USA. [Benson, B. A.; Bleem, L. E.; Carlstrom, J. E.; Chang, C. L.; Crawford, T. M.; Crites, A. T.; Gladders, M. D.; High, F. W.; Hoover, S.; Keisler, R.; Leitch, E. M.; Marrone, D. P.; McMahon, J. J.; Mehl, J.; Meyer, S. S.; Padin, S.; Plagge, T.; Pryke, C.; Schaffer, K. K.; Story, K.; Vieira, J. D.; Williamson, R.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Benson, B. A.; Carlstrom, J. E.; Chang, C. L.; Hoover, S.; McMahon, J. J.; Meyer, S. S.; Pryke, C.; Schaffer, K. K.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [Bleem, L. E.; Carlstrom, J. E.; Keisler, R.; Meyer, S. S.; Story, K.; Vieira, J. D.] Univ Chicago, Dept Phys, Chicago, IL 60637 USA. [Bonamente, M.] Univ Alabama, Dept Phys, Huntsville, AL 35899 USA. [Carlstrom, J. E.; Crawford, T. M.; Crites, A. T.; Gladders, M. D.; High, F. W.; Leitch, E. M.; Mehl, J.; Meyer, S. S.; Padin, S.; Plagge, T.; Pryke, C.; Williamson, R.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Clocchiatti, A.] Pontificia Univ Catolica Chile, Dept Astron & Astrofis, Santiago 22, Chile. [Desai, S.] Univ Illinois, Dept Astron, Urbana, IL 61801 USA. [Garmire, G.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [George, E. M.; Holzapfel, W. L.; Lee, A. T.; Lueker, M.; Reichardt, C. L.; Shirokoff, E.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Gonzalez, A. H.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA. [Halverson, N. W.] Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA. [Halverson, N. W.] Univ Colorado, Dept Phys, Boulder, CO 80309 USA. [Joy, M.] NASA, George C Marshall Space Flight Ctr, VP62, Dept Space Sci, Huntsville, AL 35812 USA. [Knox, L.; Stanford, S. A.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. [Lee, A. T.; Spieler, H. G.] Univ Calif Berkeley, Lawrence Berkeley Lab, Div Phys, Berkeley, CA 94720 USA. [McMahon, J. J.; Song, J.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA. [Mohr, J. J.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Montroy, T. E.; Ruhl, J. E.; Saliwanchik, B. R.; Staniszewski, Z.] Case Western Reserve Univ, Dept Phys, Cleveland, OH 44106 USA. [Padin, S.; Vieira, J. D.] CALTECH, Pasadena, CA 91125 USA. [Rest, A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Shaw, L.] Yale Univ, Dept Phys, New Haven, CT 06520 USA. RP Foley, RJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM rfoley@cfa.harvard.edu RI Stubbs, Christopher/C-2829-2012; Williamson, Ross/H-1734-2015; Holzapfel, William/I-4836-2015; OI Stubbs, Christopher/0000-0003-0347-1724; Williamson, Ross/0000-0002-6945-2975; Aird, Kenneth/0000-0003-1441-9518; Reichardt, Christian/0000-0003-2226-9169; Stark, Antony/0000-0002-2718-9996 FU National Science Foundation [ANT-0638937, PHY-0114422, AST-1009012, AST-1009649, MRI-0723073]; Kavli Foundation; Gordon and Betty Moore Foundation; NASA [12800071, 12800088, NAS8-03060]; JPL/Caltech; Chandra X-ray Observatory Center; NASA Office of Space Science; National Sciences and Engineering Research Council of Canada; Canada Research Chairs program; Canadian Institute for Advanced Research; Excellence Cluster Universe; DFG [TR33]; Clay Fellowship; KICP Fellowship; W.M. Keck Foundation; Pennsylvania State University [2834-MIT-SAO-4018]; Basal CATA PFB [06/09]; FONDAP [15010003]; Alfred P. Sloan Research Fellowship; Smithsonian Institution; Brinson Foundation FX The South Pole Telescope program is supported by the National Science Foundation through grant ANT-0638937. Partial support is also provided by the NSF Physics Frontier Center grant PHY-0114422 to the Kavli Institute of Cosmological Physics at the University of Chicago, the Kavli Foundation, and the Gordon and Betty Moore Foundation. This work is based in part on observations obtained with the Spitzer Space Telescope (PID 60099), 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. Additional data were obtained with the 6.5 m Magellan Telescopes located at the Las Campanas Observatory, Chile. Support for X-ray analysis was provided by NASA through Chandra Project Numbers 12800071 and 12800088 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. Observations from VLT programs 086.A-0741 and 286.A-5021 were included in this work. 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. Galaxy cluster research at Harvard is supported by NSF grant AST-1009012. Galaxy cluster research at SAO is supported in part by NSF grants AST-1009649 and MRI-0723073. The McGill group acknowledges funding from the National Sciences and Engineering Research Council of Canada, Canada Research Chairs program, and the Canadian Institute for Advanced Research. X-ray research at the CfA is supported through NASA Contract NAS 8-03060. The Munich group acknowledges support from the Excellence Cluster Universe and the DFG research program TR33. R.J.F. is supported by a Clay Fellowship. B. A. B. is supported by a KICP Fellowship, support for M. Brodwin was provided by the W.M. Keck Foundation, M. Bautz acknowledges support from contract 2834-MIT-SAO-4018 from the Pennsylvania State University to the Massachusetts Institute of Technology. A.C. acknowledges the support of grants Basal CATA PFB 06/09 and FONDAP No. 15010003. M.D. acknowledges support from an Alfred P. Sloan Research Fellowship, W.F. and C.J. acknowledge support from the Smithsonian Institution, and B.S. acknowledges support from the Brinson Foundation. NR 58 TC 81 Z9 82 U1 1 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 APR 20 PY 2011 VL 731 IS 2 AR 86 DI 10.1088/0004-637X/731/2/86 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 753MM UT WOS:000289779600009 ER PT J AU Garcia, J Kallman, TR Mushotzky, RF AF Garcia, J. Kallman, T. R. Mushotzky, R. F. TI X-RAY REFLECTED SPECTRA FROM ACCRETION DISK MODELS. II. DIAGNOSTIC TOOLS FOR X-RAY OBSERVATIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; atomic processes; black hole physics; line: formation; radiative transfer; X-rays: general ID RESONANT AUGER DESTRUCTION; K-SHELL PHOTOABSORPTION; ACTIVE GALACTIC NUCLEI; COMPTON REFLECTION; SEYFERT-GALAXIES; ATOMIC DATABASE; ALPHA-LINES; COLD MATTER; BLACK-HOLES; IRON AB We present a comprehensive study of the emission spectra from accreting sources. We use our new reflection code to compute the reflected spectra from an accretion disk illuminated by X-rays. This set of models covers different values of ionization parameter, solar iron abundance, and photon index for the illuminating spectrum. These models also include the most complete and recent atomic data for the inner shell of the iron and oxygen isonuclear sequences. We concentrate our analysis on the 2-10 keV energy region and in particular on the iron K-shell emission lines. We show the dependency of the equivalent width (EW) of the Fe K alpha on the ionization parameter. The maximum value of the EW is similar to 800 eV for models with log xi similar to 1.5 and decreases monotonically as xi increases. For lower values of xi, the Fe K alpha EW decreases to a minimum near log xi similar to 0.8. We produce simulated CCD observations based on our reflection models. For low-ionized, reflection-dominated cases, the 2-10 keV energy region shows a very broad, curving continuum that cannot be represented by a simple power law. We show that in addition to the Fe K-shell emission, there are other prominent features such as the Si and S L alpha lines, a blend of Ar VIII-XI lines, and the Ca X K alpha line. In some cases, the S XV blends with the He-like Si radiative recombination continua producing a broad feature that cannot be reproduced by a simple Gaussian profile. This could be used as a signature of reflection. C1 [Garcia, J.] Western Michigan Univ, Dept Phys, Kalamazoo, MI 49008 USA. [Garcia, J.; Kallman, T. R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Mushotzky, R. F.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. RP Garcia, J (reprint author), Western Michigan Univ, Dept Phys, Kalamazoo, MI 49008 USA. EM javier.garcia@wmich.edu; timothy.r.kallman@nasa.gov; richard@astro.umd.edu FU NASA [05-ATP05-18] FX This work was supported by a grant from the NASA astrophysics theory program 05-ATP05-18. This research has made use of NASA's Astrophysics Data System. NR 39 TC 33 Z9 33 U1 0 U2 3 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 APR 20 PY 2011 VL 731 IS 2 AR 131 DI 10.1088/0004-637X/731/2/131 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 753MM UT WOS:000289779600054 ER PT J AU Hickox, RC Myers, AD Brodwin, M Alexander, DM Forman, WR Jones, C Murray, SS Brown, MJI Cool, RJ Kochanek, CS Dey, A Jannuzi, BT Eisenstein, D Assef, RJ Eisenhardt, PR Gorjian, V Stern, D Le Floc'h, E Caldwell, N Goulding, AD Mullaney, JR AF Hickox, Ryan C. Myers, Adam D. Brodwin, Mark Alexander, David M. Forman, William R. Jones, Christine Murray, Stephen S. Brown, Michael J. I. Cool, Richard J. Kochanek, Christopher S. Dey, Arjun Jannuzi, Buell T. Eisenstein, Daniel Assef, Roberto J. Eisenhardt, Peter R. Gorjian, Varoujan Stern, Daniel Le Floc'h, Emeric Caldwell, Nelson Goulding, Andrew D. Mullaney, James R. TI CLUSTERING OF OBSCURED AND UNOBSCURED QUASARS IN THE BOOTES FIELD: PLACING RAPIDLY GROWING BLACK HOLES IN THE COSMIC WEB SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; large-scale structure of universe; quasars: general; surveys ID DIGITAL-SKY-SURVEY; ACTIVE GALACTIC NUCLEI; LUMINOUS RED GALAXIES; DARK-MATTER HALOES; PHOTOMETRICALLY CLASSIFIED QUASARS; SPECTRAL ENERGY-DISTRIBUTIONS; CROSS-CORRELATION FUNCTION; LARGE-SCALE STRUCTURE; IRAC SHALLOW SURVEY; QSO REDSHIFT SURVEY AB We present the first measurement of the spatial clustering of mid-infrared-selected obscured and unobscured quasars, using a sample in the redshift range 0.7 < z < 1.8 selected from the 9 deg(2) Bootes multiwavelength survey. Recently, the Spitzer Space Telescope and X-ray observations have revealed large populations of obscured quasars that have been inferred from models of the X-ray background and supermassive black hole evolution. To date, little is known about obscured quasar clustering, which allows us to measure the masses of their host dark matter halos and explore their role in the cosmic evolution of black holes and galaxies. In this study, we use a sample of 806 mid-infrared-selected quasars and approximate to 250,000 galaxies to calculate the projected quasar-galaxy cross-correlation function w(p) (R). The observed clustering yields characteristic dark matter halo masses of log(M-halo [h(-1) M-circle dot]) = 12.7(-0.6)(+0.4) and 13.3(-0.4)(+0.3) for unobscured quasars (QSO-1s) and obscured quasars (Obs-QSOs), respectively. The results for QSO-1s are in excellent agreement with previous measurements for optically selected quasars, while we conclude that the Obs-QSOs are at least as strongly clustered as the QSO-1s. We test for the effects of photometric redshift errors on the optically faint Obs-QSOs, and find that our method yields a robust lower limit on the clustering; photo-z errors may cause us to underestimate the clustering amplitude of the Obs-QSOs by at most similar to 20%. We compare our results to previous studies, and speculate on physical implications of stronger clustering for obscured quasars. C1 [Hickox, Ryan C.; Alexander, David M.; Goulding, Andrew D.; Mullaney, James R.] Univ Durham, Dept Phys, Durham DH1 3LE, England. [Hickox, Ryan C.; Brodwin, Mark; Forman, William R.; Jones, Christine; Murray, Stephen S.; Eisenstein, Daniel; Caldwell, Nelson; Goulding, Andrew D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Myers, Adam D.] Univ Illinois, Dept Astron, Urbana, IL 61801 USA. [Murray, Stephen S.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Brown, Michael J. I.] Monash Univ, Sch Phys, Clayton, Vic 3800, Australia. [Cool, Richard J.] Princeton Univ Observ, Princeton, NJ 08544 USA. [Kochanek, Christopher S.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Dey, Arjun; Jannuzi, Buell T.] Natl Opt Astron Observ, Tucson, AZ 85726 USA. [Eisenstein, Daniel] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Assef, Roberto J.; Eisenhardt, Peter R.; Gorjian, Varoujan; Stern, Daniel] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Le Floc'h, Emeric; Mullaney, James R.] Univ Paris Diderot, Lab AIM Paris Saclay, CEA DSM Irfu CNRS, CE Saclay, F-91191 Gif Sur Yvette, France. RP Hickox, RC (reprint author), Univ Durham, Dept Phys, South Rd, Durham DH1 3LE, England. EM ryan.hickox@durham.ac.uk RI Brown, Michael/B-1181-2015; OI Brown, Michael/0000-0002-1207-9137; Alexander, David/0000-0002-5896-6313; Forman, William/0000-0002-9478-1682 FU NOAO; STFC; SAO; NASA [NNX08AJ28G] FX We thank our colleagues on the NDWFS, AGES, SDWFS, and XBootes teams. We thank the anonymous referee for helpful comments that improved the paper, and Philip Hopkins and Peder Norberg for productive discussions. The NOAO Deep Wide-field Survey, and the research of A.D. and B.T.J. are supported by NOAO, which is operated by the Association of Universities for Research in Astronomy (AURA), Inc. under a cooperative agreement with the National Science Foundation. This paper would not have been possible without the efforts of the Chandra, Spitzer, KPNO, and MMT support staff. Optical spectroscopy discussed in this paper was obtained at the MMT Observatory, a joint facility of the Smithsonian Institution and the University of Arizona. The first Spitzer MIPS survey of the Bootes region was obtained using GTO time provided by the Spitzer Infrared Spectrograph Team (PI: James Houck) and by M. Rieke. We thank the collaborators in that work for access to the 24 micron catalog generated from those data. R.C.H. was supported by an STFC Postdoctoral Fellowship and an SAO Postdoctoral Fellowship, and A.D.M. was generously funded by the NASA ADAP program under grant NNX08AJ28G. D.M.A. is grateful to the Royal Society and Philip Leverhulme Prize for their generous support. R.J.A. was supported by the NASA Postdoctoral Program, administered by Oak Ridge Associated Universities through a contract with NASA. NR 134 TC 52 Z9 52 U1 0 U2 5 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 APR 20 PY 2011 VL 731 IS 2 AR 117 DI 10.1088/0004-637X/731/2/117 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 753MM UT WOS:000289779600040 ER PT J AU Kamenetzky, J Glenn, J Maloney, PR Aguirre, JE Bock, JJ Bradford, CM Earle, L Inami, H Matsuhara, H Murphy, EJ Naylor, BJ Nguyen, HT Zmuidzinas, J AF Kamenetzky, J. Glenn, J. Maloney, P. R. Aguirre, J. E. Bock, J. J. Bradford, C. M. Earle, L. Inami, H. Matsuhara, H. Murphy, E. J. Naylor, B. J. Nguyen, H. T. Zmuidzinas, J. TI THE DENSE MOLECULAR GAS IN THE CIRCUMNUCLEAR DISK OF NGC 1068 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: individual (NGC 1068); galaxies: ISM; galaxies: Seyfert; ISM: molecules ID ACTIVE GALACTIC NUCLEUS; STAR-FORMATION; GALAXY NUCLEI; NGC-1068; EMISSION; HCN; CO; SPECTROSCOPY; CHEMISTRY; LINE AB We present a 190-307 GHz broadband spectrum obtained with Z-Spec of NGC 1068 with new measurements of molecular rotational transitions. After combining our measurementswith those previously published and considering the specific geometry of this Seyfert 2 galaxy, we conduct amulti-species Bayesian likelihood analysis of the density, temperature, and relative molecular abundances of HCN, HNC, CS, and HCO+. We find that these molecules trace warm (T > 100 K) gas of H-2 number densities 10(4.2)-10(4.9) cm(-3). Our models also place strong constraints on the column densities and relative abundances of these molecules, as well as on the total mass in the circumnuclear disk. Using the uniform calibration afforded by the broad Z-Spec bandpass, we compare our line ratios to X-ray-dominated region (XDR) and photon-dominated region models. The majority of our line ratios are consistent with the XDR models at the densities indicated by the likelihood analysis, lending substantial support to the emerging interpretation that the energetics in the circumnuclear disk of NGC 1068 are dominated by accretion onto an active galactic nucleus. C1 [Kamenetzky, J.; Glenn, J.; Maloney, P. R.; Earle, L.] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80303 USA. [Aguirre, J. E.] Univ Penn, Dept Phys, Philadelphia, PA 19104 USA. [Bock, J. J.; Bradford, C. M.; Naylor, B. J.; Nguyen, H. T.; Zmuidzinas, J.] NASA, Jet Prop Lab, Pasadena, CA 91109 USA. [Earle, L.] Natl Renewable Energy Lab, Golden, CO 80401 USA. [Inami, H.; Matsuhara, H.] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2298510, Japan. [Murphy, E. J.] Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA. RP Kamenetzky, J (reprint author), Univ Colorado, Ctr Astrophys & Space Astron, 389-UCB, Boulder, CO 80303 USA. OI Kamenetzky, Julia/0000-0001-7877-7942 FU NASA [NAGS-11911, NAGS-12788]; NSF [AST-0239270, AST-087990]; Research Corporation Award [RI0928]; Caltech Millikan fellowship; JPL Director's fellowship; NRAO FX We thank the anonymous referee for a thorough and constructive report, and we also express our gratitude to the staff at the Caltech Submillimeter Observatory. We acknowledge the following grants and fellowships in support of this work: NASA SARA grants NAGS-11911 and NAGS-12788, an NSF Career grant AST-0239270, and a Research Corporation Award RI0928 to J.G.; a Caltech Millikan fellowship and JPL Director's fellowship to C.M.B.; an NRAO Jansky fellowship and NSF grant AST-087990 to J.E.A.; a NASA GSRP fellowship to L.E.; and an NSF GRFP fellowship to J.K. NR 46 TC 23 Z9 23 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 20 PY 2011 VL 731 IS 2 AR 83 DI 10.1088/0004-637X/731/2/83 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 753MM UT WOS:000289779600006 ER PT J AU Linker, JA Lionello, R Mikic, Z Titov, VS Antiochos, SK AF Linker, Jon A. Lionello, Roberto Mikic, Zoran Titov, Viacheslav S. Antiochos, Spiro K. TI THE EVOLUTION OF OPEN MAGNETIC FLUX DRIVEN BY PHOTOSPHERIC DYNAMICS SO ASTROPHYSICAL JOURNAL LA English DT Article DE magnetohydrodynamics (MHD); Sun: corona; Sun: magnetic topology; solar wind ID SLOW SOLAR-WIND; WHOLE SUN MONTH; CORONAL MASS EJECTIONS; DIFFERENTIAL ROTATION; MAGNETOHYDRODYNAMIC SIMULATIONS; FIELD STRENGTH; MHD MODEL; HOLES; INTERPLANETARY; SPEED AB The coronal magnetic field is of paramount importance in solar and heliospheric physics. Two profoundly different views of the coronal magnetic field have emerged. In quasi-steady models, the predominant source of open magnetic field is in coronal holes. In contrast, in the interchange model, the open magnetic flux is conserved, and the coronal magnetic field can only respond to the photospheric evolution via interchange reconnection. In this view, the open magnetic flux diffuses through the closed, streamer belt fields, and substantial open flux is present in the streamer belt during solar minimum. However, Antiochos and coworkers, in the form of a conjecture, argued that truly isolated open flux cannot exist in a configuration with one heliospheric current sheet-it will connect via narrow corridors to the polar coronal hole of the same polarity. This contradicts the requirements of the interchange model. We have performed an MHD simulation of the solar corona up to 20 R-circle dot to test both the interchange model and the Antiochos conjecture. We use a synoptic map for Carrington rotation 1913 as the boundary condition for the model, with two small bipoles introduced into the region where a positive polarity extended coronal hole forms. We introduce flows at the photospheric boundary surface to see if open flux associated with the bipoles can be moved into the closed-field region. Interchange reconnection does occur in response to these motions. However, we find that the open magnetic flux cannot be simply injected into closed-field regions-the flux eventually closes down and disconnected flux is created. Flux either opens or closes, as required, to maintain topologically distinct open- and closed-field regions, with no indiscriminate mixing of the two. The early evolution conforms to the Antiochos conjecture in that a narrow corridor of open flux connects the portion of the coronal hole that is nearly detached by one of the bipoles. In the later evolution, a detached coronal hole forms, in apparent violation of the Antiochos conjecture. Further investigation reveals that this detached coronal hole is actually linked to the extended coronal hole by a separatrix footprint on the photosphere of zero width. Therefore, the essential idea of the conjecture is preserved, if we modify it to state that coronal holes in the same polarity region are always linked, either by finite width corridors or separatrix footprints. The implications of these results for interchange reconnection and the sources of the slow solar wind are briefly discussed. C1 [Linker, Jon A.; Lionello, Roberto; Mikic, Zoran; Titov, Viacheslav S.] Predict Sci Inc, San Diego, CA 92121 USA. [Antiochos, Spiro K.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Linker, JA (reprint author), Predict Sci Inc, 9990 Mesa Rim Rd,Suite 170, San Diego, CA 92121 USA. EM linkerj@predsci.com; lionel@predsci.com; mikicz@predsci.com; titovv@predsci.com; spiro.antiochos@nasa.gov RI Antiochos, Spiro/D-4668-2012 OI Antiochos, Spiro/0000-0003-0176-4312 FU NASA; NSF; AFOSR; Center for Integrated Space Weather Modeling (an NSF Science and Technology Center) FX This work was supported by NASA's Heliophysics Theory, LWS, and Guest Investigator programs, the LWS Strategic Capabilities Program (NASA, NSF, and AFOSR), and the Center for Integrated Space Weather Modeling (an NSF Science and Technology Center). Computational resources were provided by the NSF supported Texas Advanced Computing Center (TACC) in Austin and the NASA Advanced Supercomputing Division (NAS) at Ames Research Center. This work was initiated and greatly benefitted from discussions in the LWS TR&T focus team on the solar and heliospheric magnetic field. NR 77 TC 22 Z9 23 U1 0 U2 8 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD APR 20 PY 2011 VL 731 IS 2 AR 110 DI 10.1088/0004-637X/731/2/110 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 753MM UT WOS:000289779600033 ER PT J AU Marriage, TA Juin, JB Lin, YT Marsden, D Nolta, MR Partridge, B Ade, PAR Aguirre, P Amiri, M Appel, JW Barrientos, LF Battistelli, ES Bond, JR Brown, B Burger, B Chervenak, J Das, S Devlin, MJ Dicker, SR Doriese, WB Dunkley, J Dunner, R Essinger-Hileman, T Fisher, RP Fowler, JW Hajian, A Halpern, M Hasselfield, M Hernandez-Monteagudo, C Hilton, GC Hilton, M Hincks, AD Hlozek, R Huffenberger, KM Hughes, DH Hughes, JP Infante, L Irwin, KD Kaul, M Klein, J Kosowsky, A Lau, JM Limon, M Lupton, RH Martocci, K Mauskopf, P Menanteau, F Moodley, K Moseley, H Netterfield, CB Niemack, MD Page, LA Parker, L Quintana, H Reid, B Sehgal, N Sherwin, BD Sievers, J Spergel, DN Staggs, ST Swetz, DS Switzer, ER Thornton, R Trac, H Tucker, C Warne, R Wilson, G Wollack, E Zhao, Y AF Marriage, Tobias A. Baptiste Juin, Jean Lin, Yen-Ting Marsden, Danica Nolta, Michael R. Partridge, Bruce Ade, Peter A. R. Aguirre, Paula Amiri, Mandana Appel, John William Felipe Barrientos, L. Battistelli, Elia S. Bond, John R. Brown, Ben Burger, Bryce Chervenak, Jay Das, Sudeep Devlin, Mark J. Dicker, Simon R. Doriese, W. Bertrand Dunkley, Joanna Duenner, Rolando Essinger-Hileman, Thomas Fisher, Ryan P. Fowler, Joseph W. Hajian, Amir Halpern, Mark Hasselfield, Matthew Hernandez-Monteagudo, Carlos Hilton, Gene C. Hilton, Matt Hincks, Adam D. Hlozek, Renee Huffenberger, Kevin M. Handel Hughes, David Hughes, John P. Infante, Leopoldo Irwin, Kent D. Kaul, Madhuri Klein, Jeff Kosowsky, Arthur Lau, Judy M. Limon, Michele Lupton, Robert H. Martocci, Krista Mauskopf, Phil Menanteau, Felipe Moodley, Kavilan Moseley, Harvey Netterfield, Calvin B. Niemack, Michael D. Page, Lyman A. Parker, Lucas Quintana, Hernan Reid, Beth Sehgal, Neelima Sherwin, Blake D. Sievers, Jon Spergel, David N. Staggs, Suzanne T. Swetz, Daniel S. Switzer, Eric R. Thornton, Robert Trac, Hy Tucker, Carole Warne, Ryan Wilson, Grant Wollack, Ed Zhao, Yue TI THE ATACAMA COSMOLOGY TELESCOPE: EXTRAGALACTIC SOURCES AT 148 GHz IN THE 2008 SURVEY SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmic background radiation; galaxies: active; radio continuum: galaxies; surveys ID SOUTH-POLE TELESCOPE; ZELDOVICH POWER SPECTRUM; GALAXY CLUSTERS; SOURCE CATALOG; RADIO-SOURCES; SOURCE COUNTS; SKY SURVEY; ANISOTROPY; FIELD; SZ AB We report on extragalactic sources detected in a 455 deg(2) map of the southern sky made with data at a frequency of 148 GHz from the Atacama Cosmology Telescope (ACT) 2008 observing season. We provide a catalog of 157 sources with flux densities spanning two orders of magnitude: from 15 mJy to 1500 mJy. Comparison to other catalogs shows that 98% of the ACT detections correspond to sources detected at lower radio frequencies. Three of the sources appear to be associated with the brightest cluster galaxies of low-redshift X-ray-selected galaxy clusters. Estimates of the radio to millimeter-wave spectral indices and differential counts of the sources further bolster the hypothesis that they are nearly all radio sources, and that their emission is not dominated by re-emission from warm dust. In a bright (> 50 mJy) 148 GHz selected sample with complete cross-identifications from the Australia Telescope 20 GHz survey, we observe an average steepening of the spectra between 5, 20, and 148 GHz with median spectral indices of alpha(5-20) = -0.07 +/- 0.06, alpha(20-148) = -0.39 +/- 0.04, and alpha(5-148) = -0.20 +/- 0.03. When the measured spectral indices are taken into account, the 148 GHz differential source counts are consistent with previous measurements at 30 GHz in the context of a source count model dominated by radio sources. Extrapolating with an appropriately rescaled model for the radio source counts, the Poisson contribution to the spatial power spectrum from synchrotron-dominated sources with flux density less than 20 mJy is C-Sync = (2.8 +/- 0.3) x 10(-6) mu K-2. C1 [Marriage, Tobias A.; Lin, Yen-Ting; Das, Sudeep; Dunkley, Joanna; Hajian, Amir; Lupton, Robert H.; Spergel, David N.; Trac, Hy] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Baptiste Juin, Jean; Lin, Yen-Ting; Aguirre, Paula; Felipe Barrientos, L.; Duenner, Rolando; Infante, Leopoldo; Quintana, Hernan] Pontificia Univ Catolica Chile, Fac Fis, Dept Astron & Astrofis, Santiago 22, Chile. [Lin, Yen-Ting] Univ Tokyo, Inst Phys & Math Universe, Chiba 2778568, Japan. [Marsden, Danica; Devlin, Mark J.; Dicker, Simon R.; Kaul, Madhuri; Klein, Jeff; Limon, Michele; Swetz, Daniel S.; Thornton, Robert] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. [Nolta, Michael R.; Bond, John R.; Hajian, Amir; Sievers, Jon] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada. [Partridge, Bruce] Haverford Coll, Dept Phys & Astron, Haverford, PA 19041 USA. [Ade, Peter A. R.; Mauskopf, Phil; Tucker, Carole] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Amiri, Mandana; Battistelli, Elia S.; Burger, Bryce; Halpern, Mark; Hasselfield, Matthew] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z4, Canada. [Appel, John William; Das, Sudeep; Dunkley, Joanna; Essinger-Hileman, Thomas; Fisher, Ryan P.; Fowler, Joseph W.; Hajian, Amir; Hincks, Adam D.; Lau, Judy M.; Limon, Michele; Martocci, Krista; Niemack, Michael D.; Page, Lyman A.; Parker, Lucas; Reid, Beth; Sherwin, Blake D.; Staggs, Suzanne T.; Switzer, Eric R.; Zhao, Yue] Princeton Univ, Joseph Henry Labs Phys, Princeton, NJ 08544 USA. [Battistelli, Elia S.] Univ Roma La Sapienza, Dept Phys, I-00185 Rome, Italy. [Brown, Ben; Kosowsky, Arthur] Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA. [Chervenak, Jay; Moseley, Harvey; Wollack, Ed] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Das, Sudeep] Univ Calif Berkeley, LBL, Berkeley Ctr Cosmol Phys, Berkeley, CA 94720 USA. [Das, Sudeep] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Doriese, W. Bertrand; Hilton, Gene C.; Irwin, Kent D.; Niemack, Michael D.; Swetz, Daniel S.] NIST Quantum Devices Grp, Boulder, CO 80305 USA. [Dunkley, Joanna; Hlozek, Renee] Univ Oxford, Dept Astrophys, Oxford OX1 3RH, England. [Hernandez-Monteagudo, Carlos] Max Planck Inst Astrophys, D-85741 Garching, Germany. [Hilton, Matt; Moodley, Kavilan; Warne, Ryan] Univ KwaZulu Natal, Sch Math Sci, Astrophys & Cosmol Res Unit, ZA-4041 Durban, South Africa. [Hilton, Matt; Moodley, Kavilan] Ctr High Performance Comp, Cape Town, South Africa. [Huffenberger, Kevin M.] Univ Miami, Dept Phys, Coral Gables, FL 33124 USA. [Handel Hughes, David] INAOE, Puebla, Mexico. [Hughes, John P.; Menanteau, Felipe] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. [Lau, Judy M.; Sehgal, Neelima] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA. [Lau, Judy M.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA. [Limon, Michele] Columbia Astrophys Lab, New York, NY 10027 USA. [Martocci, Krista; Switzer, Eric R.] Lab Astrophys & Space Res, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Netterfield, Calvin B.] Univ Toronto, Dept Phys, Toronto, ON M5S 1A7, Canada. [Reid, Beth] Univ Barcelona, ICC, E-08028 Barcelona, Spain. [Reid, Beth] Univ Barcelona, ICREA, E-08028 Barcelona, Spain. [Thornton, Robert] W Chester Univ, Dept Phys, W Chester, PA 19383 USA. [Trac, Hy] Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Wilson, Grant] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. RP Marriage, TA (reprint author), Princeton Univ, Dept Astrophys Sci, Peyton Hall, Princeton, NJ 08544 USA. RI Klein, Jeffrey/E-3295-2013; Spergel, David/A-4410-2011; Hilton, Matthew James/N-5860-2013; Trac, Hy/N-8838-2014; Wollack, Edward/D-4467-2012; OI Limon, Michele/0000-0002-5900-2698; Trac, Hy/0000-0001-6778-3861; Wollack, Edward/0000-0002-7567-4451; Huffenberger, Kevin/0000-0001-7109-0099; Menanteau, Felipe/0000-0002-1372-2534; Sievers, Jonathan/0000-0001-6903-5074 FU U.S. National Science Foundation [AST-0408698, PHY-0355328, AST-0707731, PIRE-0507768]; Princeton University; University of Pennsylvania; Canada Foundation for Innovation under the auspices of Compute Canada; Government of Ontario; Ontario Research Fund-Research Excellence; University of Toronto; NASA [NNX08AH30G]; FONDECYT [3085031]; Natural Science and Engineering Research Council of Canada (NSERC); NSF [AST-0546035, AST-0606975]; FONDAP Centro de Astrofisica; U.S. Department of Energy [DE-AC3-76SF00515]; CONICYT; MECESUP; Fundacion Andes; Rhodes Trust; NSF Physics Frontier Center [PHY-0114422]; World Premier International Research Center Initiative, MEXT, Japan FX This work was supported by the U.S. National Science Foundation through awards AST-0408698 for the ACT project, and PHY-0355328, AST-0707731, and PIRE-0507768. Funding was also provided by Princeton University and the University of Pennsylvania. The PIRE program made possible exchanges between Chile, South Africa, Spain, and the US that enabled this research program. Computations were performed on the GPC supercomputer at the SciNet HPC Consortium. SciNet is funded by: the Canada Foundation for Innovation under the auspices of Compute Canada; the Government of Ontario; Ontario Research Fund-Research Excellence; and the University of Toronto.; T.M. was supported through NASA grant NNX08AH30G. J.B.J. was supported by the FONDECYT grant 3085031. A. D. H. received additional support from a Natural Science and Engineering Research Council of Canada (NSERC) PGS-D scholarship. A. K. and B. P. were partially supported through NSF AST-0546035 and AST-0606975, respectively, for work on ACT. H. Q. and L. I. acknowledge partial support from FONDAP Centro de Astrofisica. N.S. is supported by the U.S. Department of Energy contract to SLAC no. DE-AC3-76SF00515. R. D. was supported by CONICYT, MECESUP, and Fundacion Andes. R. H. was supported by the Rhodes Trust. E. S. acknowledges support by NSF Physics Frontier Center grant PHY-0114422 to the Kavli Institute of Cosmological Physics. Y.T.L. acknowledges support from the World Premier International Research Center Initiative, MEXT, Japan. The ACT data will be made public through LAMBDA (http://lambda.gsfc.nasa.gov/) and the ACT Web site (http://www.physics.princeton.edu/act/). NR 48 TC 54 Z9 54 U1 0 U2 7 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 APR 20 PY 2011 VL 731 IS 2 AR 100 DI 10.1088/0004-637X/731/2/100 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 753MM UT WOS:000289779600023 ER PT J AU Mullan, B Konstantopoulos, S Kepley, AA Lee, KH Charlton, JC Knierman, K Bastian, N Chandar, R Durrell, PR Elmegreen, D English, J Gallagher, SC Gronwall, C Hibbard, JE Hunsberger, S Johnson, KE Maybhate, A Palma, C Trancho, G Vacca, WD AF Mullan, B. Konstantopoulos, S. Kepley, A. A. Lee, K. H. Charlton, J. C. Knierman, K. Bastian, N. Chandar, R. Durrell, P. R. Elmegreen, D. English, J. Gallagher, S. C. Gronwall, C. Hibbard, J. E. Hunsberger, S. Johnson, K. E. Maybhate, A. Palma, C. Trancho, G. Vacca, W. D. TI STAR CLUSTERS IN THE TIDAL TAILS OF INTERACTING GALAXIES: CLUSTER POPULATIONS ACROSS A VARIETY OF TAIL ENVIRONMENTS SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: interactions; galaxies: photometry; galaxies: star clusters: general ID YOUNG GLOBULAR-CLUSTERS; SPACE-TELESCOPE OBSERVATIONS; INITIAL MASS FUNCTION; DWARF GALAXIES; STELLAR POPULATIONS; LUMINOSITY FUNCTION; SPIRAL GALAXIES; PHOTOMETRIC EVOLUTION; SPATIAL-DISTRIBUTION; ANTENNAE GALAXIES AB We have searched for compact stellar structures within 17 tidal tails in 13 different interacting galaxies using F606W- and F814W-band images from the Wide Field Planetary Camera 2 on the Hubble Space Telescope. The sample of tidal tails includes a diverse population of optical properties, merging galaxy mass ratios, Hi content, and ages. Combining our tail sample with Knierman et al., we find evidence of star clusters formed in situ with M-V < -8.5 and V - I < 2.0 in 10 of 23 tidal tails; we are able to identify cluster candidates to M-V = -6.5 in the closest tails. Three tails offer clear examples of "beads on a string" star formation morphology in V - I color maps. Two tails present both tidal dwarf galaxy candidates and cluster candidates. Statistical diagnostics indicate that clusters in tidal tails may be drawn from the same power-law luminosity functions (with logarithmic slopes approximate to-2 to -2.5) found in quiescent spiral galaxies and interiors of interacting systems. We find that the tail regions with the largest number of observable clusters are relatively young (less than or similar to 250 Myr old) and bright (V less than or similar to 24 mag arcsec(-2)), probably attributed to the strong bursts of star formation in interacting systems soon after periapse. Otherwise, we find no statistical difference between cluster-rich and cluster-poor tails in terms of many observable characteristics, though this analysis suffers from complex, unresolved gas dynamics and projection effects. C1 [Mullan, B.; Konstantopoulos, S.; Lee, K. H.; Charlton, J. C.; Gronwall, C.; Hunsberger, S.; Palma, C.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16803 USA. [Kepley, A. A.; Johnson, K. E.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. [Kepley, A. A.; Hibbard, J. E.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. [Knierman, K.] Arizona State Univ, Bateman Phys Sci Ctr, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [Bastian, N.] Univ Exeter, Sch Phys, Exeter EX4 4QL, Devon, England. [Chandar, R.] Univ Toledo, Dept Phys & Astron, Toledo, OH 43606 USA. [Durrell, P. R.] Youngstown State Univ, Dept Phys & Astron, Youngstown, OH 44555 USA. [Elmegreen, D.] Vassar Coll, Dept Phys & Astron, Poughkeepsie, NY 12604 USA. [English, J.] Univ Manitoba, Dept Phys & Astron, Winnipeg, MB R3T 2N2, Canada. [Gallagher, S. C.] Univ Western Ontario, Dept Phys & Astron, London, ON N6A 3K7, Canada. [Maybhate, A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Trancho, G.] Gemini Observ, La Serena, Chile. [Vacca, W. D.] NASA Ames Res Ctr, Univ Space Res Assoc, Stratospher Observ Infrared Astron, Stanford, CA 94305 USA. RP Mullan, B (reprint author), Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16803 USA. EM mullan@astro.psu.edu OI Konstantopoulos, Iraklis/0000-0003-2177-0146 FU Space Telescope Science Institute [HST-GO-11134.05-A] FX We wish to thank Barbel Koribalski for sharing Hi data and helpful comments for NGC 6872. This project was supported by a grant from the Space Telescope Science Institute (grant No. HST-GO-11134.05-A). NR 113 TC 27 Z9 27 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 20 PY 2011 VL 731 IS 2 AR 93 DI 10.1088/0004-637X/731/2/93 PG 25 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 753MM UT WOS:000289779600016 ER PT J AU Sandell, G Weintraub, DA Hamidouche, M AF Sandell, Goeran Weintraub, David A. Hamidouche, Murad TI A SUB-MILLIMETER MAPPING SURVEY OF HERBIG AeBe STARS (vol 26, pg 727, 2011) SO ASTROPHYSICAL JOURNAL LA English DT Correction C1 [Sandell, Goeran; Hamidouche, Murad] NASA, SOFIA USRA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Weintraub, David A.] Vanderbilt Univ, Dept Phys & Astron, Nashville, TN 37235 USA. RP Sandell, G (reprint author), NASA, SOFIA USRA, Ames Res Ctr, Mail Stop N211-3,Bldg N211,Rm 249, Moffett Field, CA 94035 USA. NR 1 TC 1 Z9 1 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 APR 20 PY 2011 VL 731 IS 2 AR 133 DI 10.1088/0004-637X/731/2/133 PG 1 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 753MM UT WOS:000289779600056 ER PT J AU Su, Y Holman, GD Dennis, BR AF Su, Yang Holman, Gordon D. Dennis, Brian R. TI EVIDENCE FOR THE FULL HARD X-RAY SPECTRAL SIGNATURE OF NONUNIFORM IONIZATION IN A SOLAR FLARE SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun: chromosphere; Sun: flares; Sun: X-rays, gamma rays ID THERMAL ELECTRONS; REVERSE-CURRENT; BREMSSTRAHLUNG; TARGET; ENERGY; RHESSI; EXPLANATION; BURSTS; BEAMS AB The hard X-ray (HXR) emission from solar flares is observed primarily from the footpoints of flare magnetic loops, where nonthermal electrons are understood to emit thick-target bremsstrahlung as they stream from the fully ionized hot corona to the denser, cooler, and partially ionized chromosphere. The change in the plasma ionization along the path of the electrons should result in a characteristic upward break and corresponding flattening of the X-ray spectrum with increasing energy at lower energies, and a downward break at higher energies. Due to the presence of thermal emission, the upward break usually cannot be observed. We report the first evidence for both breaks in spectra measured with the Reuven Ramaty High Energy Solar Spectroscopic Imager (RHESSI) during the GOES X1.2 class flare that happened on 2002 October 31. The RHESSI X-ray spectral analysis shows both the breakup at similar to 49 keV and the breakdown at similar to 134 keV at the HXR peak time. The time evolution of both breaks also agrees with the nonuniform ionization (NUI) model. Other possible explanations for the breaks are considered, but the NUI model provides the simplest explanation for the spectral shape and its time evolution. We find that the average column density of the fully ionized plasma changed from 2 x 10(19) cm(-2) in the rise phase to 7 x 10(21) cm(-2) after the peak. This indicates that plasma in the target was heated and became ionized during the flare, in agreement with heating by the nonthermal electrons and chromospheric evaporation expected in the collisional thick-target model. C1 [Su, Yang] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA. [Su, Yang; Holman, Gordon D.; Dennis, Brian R.] NASA, Goddard Space Flight Ctr, Solar Phys Lab, Greenbelt, MD 20771 USA. [Su, Yang] Chinese Acad Sci, Purple Mt Observ, Key Lab Dark Matter & Space Astron, Nanjing 210008, Peoples R China. RP Su, Y (reprint author), Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA. EM yang.su@nasa.gov; gordon.d.holman@nasa.gov RI Dennis, Brian/C-9511-2012; Holman, Gordon/C-9548-2012; Su, Yang/J-5381-2014 FU NSF [ATM-0725135]; NASA [NNX06AE64G]; National Natural Science Foundation of China [10773031, 10833007, 11078025]; Ministry of Science and Technology of China [MSTC 2011CB811402]; RHESSI FX We thank the RHESSI PI team for the excellence and easy availability of the data and the analysis software. Yang Su thanks Dr. Linhui Sui and Dr. Jeffrey W. Brosius for providing the research opportunity, Qingrong Chen and the referee for the valuable discussions and comments. Yang Su also acknowledges NSF support through ATM-0725135 and NASA support through grant NNX06AE64G. This work was supported in part by the National Natural Science Foundation of China (grant nos. 10773031, 10833007, 11078025), the Ministry of Science and Technology of China (MSTC 2011CB811402), the RHESSI Project, and a NASA HGI (Heliophysics Guest Investigator) grant. NR 25 TC 10 Z9 11 U1 1 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 APR 20 PY 2011 VL 731 IS 2 AR 106 DI 10.1088/0004-637X/731/2/106 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 753MM UT WOS:000289779600029 ER PT J AU Titov, VS Mikic, Z Linker, JA Lionello, R Antiochos, SK AF Titov, V. S. Mikic, Z. Linker, J. A. Lionello, R. Antiochos, S. K. TI MAGNETIC TOPOLOGY OF CORONAL HOLE LINKAGES SO ASTROPHYSICAL JOURNAL LA English DT Article DE solar wind; Sun: corona; Sun: coronal mass ejections (CMEs); Sun: magnetic topology ID QUASI-SEPARATRIX LAYERS; SLOW SOLAR-WIND; MASS EJECTIONS; NULL POINTS; ACTIVE REGIONS; RECONNECTION; FIELDS; MODEL; DYNAMICS; OUTFLOWS AB In recent work, Antiochos and coworkers argued that the boundary between the open and closed field regions on the Sun can be extremely complex with narrow corridors of open flux connecting seemingly disconnected coronal holes from the main polar holes and that these corridors may be the sources of the slow solar wind. We examine, in detail, the topology of such magnetic configurations using an analytical source surface model that allows for analysis of the field with arbitrary resolution. Our analysis reveals three new important results. First, a coronal hole boundary can join stably to the separatrix boundary of a parasitic polarity region. Second, a single parasitic polarity region can produce multiple null points in the corona and, more important, separator lines connecting these points. It is known that such topologies are extremely favorable for magnetic reconnection, because they allow this process to occur over the entire length of the separators rather than being confined to a small region around the nulls. Finally, the coronal holes are not connected by an open-field corridor of finite width, but instead are linked by a singular line that coincides with the separatrix footprint of the parasitic polarity. We investigate how the topological features described above evolve in response to the motion of the parasitic polarity region. The implications of our results for the sources of the slow solar wind and for coronal and heliospheric observations are discussed. C1 [Titov, V. S.; Mikic, Z.; Linker, J. A.; Lionello, R.] Predict Sci Inc, San Diego, CA 92121 USA. [Antiochos, S. K.] NASA GSFC, Greenbelt, MD 20771 USA. RP Titov, VS (reprint author), Predict Sci Inc, 9990 Mesa Rim Rd,Suite 170, San Diego, CA 92121 USA. EM titovv@predsci.com; mikicz@predsci.com; linkerj@predsci.com; lionel@predsci.com; spiro.antiochos@nasa.gov RI Antiochos, Spiro/D-4668-2012 OI Antiochos, Spiro/0000-0003-0176-4312 FU NASA; Center for Integrated Space Weather Modeling (an NSF Science and Technology Center) FX We thank the referee for a careful review of our paper, which helped us to significantly improve the presentation of our results. The contribution of V.S.T., Z.M., J.R.L., and R.L. was supported by NASA's Heliophysics Theory, Living With a Star, and SR&T programs, and the Center for Integrated Space Weather Modeling (an NSF Science and Technology Center). The contribution by S.K.A. was supported by the NASA HTP, TR&T, and SR&T programs. NR 34 TC 38 Z9 38 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 APR 20 PY 2011 VL 731 IS 2 AR 111 DI 10.1088/0004-637X/731/2/111 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 753MM UT WOS:000289779600034 ER PT J AU Toma, K Sakamoto, T Meszaros, P AF Toma, Kenji Sakamoto, Takanori Meszaros, Peter TI POPULATION III GAMMA-RAY BURST AFTERGLOWS: CONSTRAINTS ON STELLAR MASSES AND EXTERNAL MEDIUM DENSITIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE black hole physics; dark ages, reionization, first stars; gamma-ray burst: general; radio continuum: general; stars: Population III; surveys; X-rays: bursts ID HIGH-REDSHIFT; BLACK-HOLES; COSMIC REIONIZATION; FERMI OBSERVATIONS; RELATIVISTIC JETS; RADIO AFTERGLOWS; MAGNETIC-FIELDS; MASSIVE STARS; NEUTRON-STARS; 1ST STAR AB Population (Pop.) III stars are theoretically expected to be prominent around redshifts z similar to 20, consisting of mainly very massive stars with M-* greater than or similar to 100 M-circle dot, though there is no direct observational evidence for these objects. They may produce collapsar gamma-ray bursts (GRBs), with jets driven by magnetohydrodynamic processes, whose total isotropic-equivalent energy could be as high as E-iso greater than or similar to 10(57) erg over a cosmological-rest-frame duration of t(d) greater than or similar to 10(4) s, depending on the progenitor mass. Here, we calculate the afterglow spectra of such Pop. III GRBs based on the standard external shock model and show that they will be detectable with the Swift Burst Alert Telescope (BAT)/XRT and Fermi Large Area Telescope (LAT) instruments. We find that in some cases a spectral break due to electron-positron pair creation will be observable in the LAT energy range, which can put constraints on the ambient density of the pre-collapse Pop. III star. Thus, high-redshift GRB afterglow observations could be unique and powerful probes of the properties of Pop. III stars and their environments. We examine the trigger threshold of the BAT instrument in detail, focusing on the image trigger system, and show that the prompt emission of Pop. III GRBs could also be detected by BAT. Finally we briefly show that the late-time radio afterglows of Pop. III GRBs for typical parameters, despite the large distances, can be very bright: similar or equal to 140 mJy at 1 GHz, which may lead to a constraint on the Pop. III GRB rate from the current radio survey data, and similar or equal to 2.4 mJy at 70 MHz, which implies that Pop. III GRB radio afterglows could be interesting background source candidates for 21 cm absorption line detections. C1 [Toma, Kenji; Meszaros, Peter] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Toma, Kenji; Meszaros, Peter] Penn State Univ, Ctr Particle Astrophys, University Pk, PA 16802 USA. [Sakamoto, Takanori] NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA. [Sakamoto, Takanori] Univ Maryland, Joint Ctr Astrophys, Baltimore, MD 21250 USA. [Meszaros, Peter] Penn State Univ, Dept Phys, University Pk, PA 16802 USA. RP Toma, K (reprint author), Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA. EM toma@astro.psu.edu; takanori@milkyway.gsfc.nasa.gov; nnp@astro.psu.edu FU NASA [NNX09AT72G, NNX08AL40G]; NSF [PHY-0757155] FX We thank D. N. Burrows, A. D. Falcone, D. B. Fox, A. Gal-Yam, S. Gao, K. Murase, S. Naoz, and the anonymous referee for useful comments. We acknowledge NASA NNX09AT72G, NASA NNX08AL40G, and NSF PHY-0757155 for partial support. NR 91 TC 47 Z9 47 U1 0 U2 3 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 APR 20 PY 2011 VL 731 IS 2 AR 127 DI 10.1088/0004-637X/731/2/127 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 753MM UT WOS:000289779600050 ER PT J AU Antiochos, SK Mikic, Z Titov, VS Lionello, R Linker, JA AF Antiochos, S. K. Mikic, Z. Titov, V. S. Lionello, R. Linker, J. A. TI A MODEL FOR THE SOURCES OF THE SLOW SOLAR WIND SO ASTROPHYSICAL JOURNAL LA English DT Article DE solar wind; Sun: corona; Sun: magnetic topology ID HELIOSPHERIC PLASMA SHEET; OPEN MAGNETIC-FLUX; WHOLE SUN MONTH; CORONAL STREAMERS; PHOTOSPHERIC NETWORK; RECONNECTION; DYNAMICS; FIELDS; INTERPLANETARY; ACCELERATION AB Models for the origin of the slow solar wind must account for two seemingly contradictory observations: the slow wind has the composition of the closed-field corona, implying that it originates from the continuous opening and closing of flux at the boundary between open and closed field. On the other hand, the slow wind also has large angular width, up to similar to 60 degrees, suggesting that its source extends far from the open-closed boundary. We propose a model that can explain both observations. The key idea is that the source of the slow wind at the Sun is a network of narrow (possibly singular) open-field corridors that map to a web of separatrices and quasi-separatrix layers in the heliosphere. We compute analytically the topology of an open-field corridor and show that it produces a quasi-separatrix layer in the heliosphere that extends to angles far from the heliospheric current sheet. We then use an MHD code and MDI/SOHO observations of the photospheric magnetic field to calculate numerically, with high spatial resolution, the quasi-steady solar wind, and magnetic field for a time period preceding the 2008 August 1 total solar eclipse. Our numerical results imply that, at least for this time period, a web of separatrices (which we term an S-web) forms with sufficient density and extent in the heliosphere to account for the observed properties of the slow wind. We discuss the implications of our S-web model for the structure and dynamics of the corona and heliosphere and propose further tests of the model. C1 [Antiochos, S. K.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Mikic, Z.; Titov, V. S.; Lionello, R.; Linker, J. A.] Predict Sci Inc, San Diego, CA 92121 USA. RP Antiochos, SK (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM spiro.antiochos@nasa.gov RI Antiochos, Spiro/D-4668-2012 OI Antiochos, Spiro/0000-0003-0176-4312 FU NASA FX This work has been supported by the NASA TR&T, SR&T, and HTP programs. The work has benefited greatly from the authors' participation in the NASA TR&T focused science team on the solar-heliospheric magnetic field. S.K.A. thanks J. Karpen for invaluable scientific discussions and help with the graphics. NR 66 TC 71 Z9 71 U1 2 U2 12 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD APR 20 PY 2011 VL 731 IS 2 AR 112 DI 10.1088/0004-637X/731/2/112 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 753MM UT WOS:000289779600035 ER PT J AU Kondo, Y Matsui, H Moteki, N Sahu, L Takegawa, N Kajino, M Zhao, Y Cubison, MJ Jimenez, JL Vay, S Diskin, GS Anderson, B Wisthaler, A Mikoviny, T Fuelberg, HE Blake, DR Huey, G Weinheimer, AJ Knapp, DJ Brune, WH AF Kondo, Y. Matsui, H. Moteki, N. Sahu, L. Takegawa, N. Kajino, M. Zhao, Y. Cubison, M. J. Jimenez, J. L. Vay, S. Diskin, G. S. Anderson, B. Wisthaler, A. Mikoviny, T. Fuelberg, H. E. Blake, D. R. Huey, G. Weinheimer, A. J. Knapp, D. J. Brune, W. H. TI Emissions of black carbon, organic, and inorganic aerosols from biomass burning in North America and Asia in 2008 SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID TRANSFORM INFRARED-SPECTROSCOPY; IONIZATION MASS-SPECTROMETRY; LASER-INDUCED INCANDESCENCE; CENTRAL MEXICAN PLATEAU; LIGHT-ABSORPTION; TRACE GASES; AIRCRAFT MEASUREMENTS; GLOBAL PRECIPITATION; PHYSICAL-PROPERTIES; FIRE EMISSIONS AB Reliable assessment of the impact of aerosols emitted from boreal forest fires on the Arctic climate necessitates improved understanding of emissions and the microphysical properties of carbonaceous (black carbon (BC) and organic aerosols (OA)) and inorganic aerosols. The size distributions of BC were measured by an SP2 based on the laser-induced incandescence technique on board the DC-8 aircraft during the NASA ARCTAS campaign. Aircraft sampling was made in fresh plumes strongly impacted by wildfires in North America (Canada and California) in summer 2008 and in those transported from Asia (Siberia in Russia and Kazakhstan) in spring 2008. We extracted biomass burning plumes using particle and tracer (CO, CH3CN, and CH2Cl2) data. OA constituted the dominant fraction of aerosols mass in the submicron range. The large majority of the emitted particles did not contain BC. We related the combustion phase of the fire as represented by the modified combustion efficiency (MCE) to the emission ratios between BC and other species. In particular, we derived the average emission ratios of BC/CO = 2.3 +/- 2.2 and 8.5 +/- 5.4 ng m(-3)/ppbv for BB in North America and Asia, respectively. The difference in the BC/CO emission ratios is likely due to the difference in MCE. The count median diameters and geometric standard deviations of the lognormal size distribution of BC in the BB plumes were 136-141 nm and 1.32-1.36, respectively, and depended little on MCE. These BC particles were thickly coated, with shell/core ratios of 1.3-1.6. These parameters can be used directly for improving model estimates of the impact of BB in the Arctic. C1 [Kondo, Y.; Matsui, H.; Moteki, N.; Sahu, L.; Takegawa, N.; Kajino, M.] Univ Tokyo, Res Ctr Adv Sci & Technol, Meguro Ku, Tokyo 1538904, Japan. [Vay, S.; Diskin, G. S.; Anderson, B.] NASA, Langley Res Ctr, Hampton, VA 23681 USA. [Blake, D. R.] Univ Calif Irvine, Dept Chem, Irvine, CA 92697 USA. [Brune, W. H.] Penn State Univ, Dept Meteorol, University Pk, PA 16802 USA. [Cubison, M. J.; Jimenez, J. L.] Univ Colorado, Dept Chem & Biochem, Boulder, CO 80309 USA. [Fuelberg, H. E.] Florida State Univ, Dept Meteorol, Tallahassee, FL 32306 USA. [Huey, G.] Georgia Inst Technol, Sch Earth & Atmospher Sci, Atlanta, GA 30332 USA. [Weinheimer, A. J.; Knapp, D. J.] Natl Ctr Atmospher Res, Div Atmospher Chem, Boulder, CO 80305 USA. [Wisthaler, A.; Mikoviny, T.] Univ Innsbruck, Inst Ion Phys & Appl Phys, A-6020 Innsbruck, Austria. [Zhao, Y.] Univ Calif Davis, Air Qual Res Ctr, Davis, CA 95616 USA. [Cubison, M. J.; Jimenez, J. L.] Univ Colorado, CIRES, Boulder, CO 80309 USA. RP Kondo, Y (reprint author), Univ Tokyo, Res Ctr Adv Sci & Technol, Meguro Ku, 4-6-1 Komaba, Tokyo 1538904, Japan. EM y.kondo@atmos.rcast.u-tokyo.ac.jp; matsui@atmos.rcast.u-tokyo.ac.jp; moteki@atmos.rcast.u-tokyo.ac.jp; lokesh@prl.res.in; takegawa@atmos.rcast.u-tokyo.ac.jp; kajino@mri-jma.go.jp; yjzhao@ucdavis.edu; michael.cubison@colorado.edu; jose.jimenez@colorado.edu; stephanie.a.vay@nasa.gov; glenn.s.diskin@nasa.gov; b.e.anderson@larc.nasa.gov; armin.wisthaler@uibk.ac.at; tomas.mikoviny@uibk.ac.at; fuelberg@met.fsu.edu; drblake@uci.edu; greg.huey@eas.gatech.edu; wein@ucar.edu; david@ucar.edu; brune@meteo.psu.edu RI Jimenez, Jose/A-5294-2008; Kajino, Mizuo/B-5645-2012; Kondo, Yutaka/D-1459-2012 OI Jimenez, Jose/0000-0001-6203-1847; FU NASA [USP-SMD-08-009, NNX08D39G]; Ministry of Education, Culture, Sports, Science, and Technology (MEXT); Japan Science and Technology Agency (JST); Japanese Ministry of the Environment [B-083] FX The ARCTAS mission was supported by NASA. We are indebted to all the ARCTAS participants for their cooperation and support. Special thanks are due to the flight and ground crews of the NASA DC-8 aircraft. P.O. Wennberg provided the SO2 data used for the present study. We thank M. Osuka for his assistance with the field measurements. R. Yokelson provided very useful comments on the manuscript. The meteorological data were supplied by the European Centre for Medium-Range Weather Forecasts (ECWMF). This work was supported in part by the Ministry of Education, Culture, Sports, Science, and Technology (MEXT); the Strategic International Cooperative Program of the Japan Science and Technology Agency (JST); and the Global Environment Research Fund of the Japanese Ministry of the Environment (B-083). Y.Z. was supported in part by the NASA Tropospheric Chemistry Program (USP-SMD-08-009). M.J.C. and J.L.J. acknowledge NASA grant NNX08D39G. CH3CN measurements were supported by the Austrian Research Promotion Agency (FFG-ALR) and the Tiroler Zukunftstiftung, operated with the help and support of M. Graus, A. Hansel, and T. D. Maerk. NR 112 TC 69 Z9 69 U1 6 U2 55 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 APR 19 PY 2011 VL 116 AR D08204 DI 10.1029/2010JD015152 PG 25 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 754KE UT WOS:000289852700009 ER PT J AU Ajello, JM Mangina, RS Strickland, DJ Dziczek, D AF Ajello, Joseph M. Mangina, Rao S. Strickland, Douglas J. Dziczek, Dariusz TI Laboratory studies of UV emissions from proton impact on N-2: The Lyman-Birge-Hopfield band system for aurora analysis SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID LOW-ENERGY H; RESOLUTION ELECTRON-IMPACT; TRANSPORT-THEORETIC MODEL; HYDROGEN ATOM AURORA; CROSS-SECTIONS; ALPHA EMISSION; DISSOCIATIVE EXCITATION; STATISTICAL-MODEL; N=3 STATES; ULTRAVIOLET AB We have measured the emission cross sections of the Lyman-Birge-Hopfield (LBH) a (1)Pi(g) - X (1)Sigma(+)(g) band system and several atomic nitrogen (N I) multiplets (1200, 1243, 1493 angstrom) by H+ (proton) impact on N-2 over an impact energy range of 1-7 keV. The peak proton-impact-induced emission cross section of the LBH band system (1260-2500 angstrom) was measured to be 5.05 +/- 1.52 x 10 (17) cm(2) at 7 keV. To the best of our knowledge, the present LBH emission cross sections are reported for the first time in the far ultraviolet (FUV) wavelength range of 1100-1600 angstrom. The proton energy range in this study, when coupled with previously published 10-100 keV proton excited emissions of N I multiplets, provides a wide energy range of emission cross sections for proton energy loss transport codes. This energy range includes the peak cross section and the energy range for Born scaling. The reported measurements lead to an important component of monoenergetic yields for proton FUV auroral emission. Such yields, based on emission cross sections and transport modeling, allowed for convenient comparison of emission efficiencies between proton and electron aurora. In addition, we have measured the H Ly alpha, LBH, and N I multiplet emission cross sections for H-2(+) and H-3(+) ion impact on N-2 at 5 keV and found that the magnitude of H Ly a emission cross section, sigma(em)(Ly alpha), follows in the order of impact ion mass H-3(+) > H-2(+) > H+. C1 [Ajello, Joseph M.; Mangina, Rao S.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Strickland, Douglas J.] Computat Phys Inc, Springfield, VA 22151 USA. [Dziczek, Dariusz] Nicolaus Copernicus Univ, Inst Phys, PL-97100 Torun, Poland. RP Ajello, JM (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM joseph.m.ajello@jpl.nasa.gov RI Dziczek, Dariusz/G-3620-2014 FU NASA; National Science Foundation Office [0850396]; Astronomy and Physics Research and Analysis Program; Cassini Data Analysis Program; Space Physics Program Offices 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 Geospace and Planetary Atmospheres programs, the National Science Foundation Office under grant 0850396, the Astronomy and Physics Research and Analysis Program, the Cassini Data Analysis Program and Space Physics Program Offices. We thank Lars Wahlin for helping establish operation of the Colutron ion source at JPL and Ronald Cummings for his technician support. We have benefited from discussions with B. Van Zyl of the University of Denver. NR 68 TC 6 Z9 6 U1 1 U2 4 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD APR 19 PY 2011 VL 116 AR A00K03 DI 10.1029/2010JA016103 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 754KX UT WOS:000289854600005 ER PT J AU Ruzmaikin, A Feynman, J Stoev, SA AF Ruzmaikin, A. Feynman, J. Stoev, S. A. TI Distribution and clustering of fast coronal mass ejections SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID ACTIVE REGIONS; ACCELERATION; PATTERNS AB The purpose of this paper is to investigate the statistical properties of high-speed coronal mass ejections (fast CMEs), which play a major role in Space Weather. We study the cumulative distribution of the initial CME speeds applying a new, advanced statistical method based on the scaling properties of averages of maximal speeds selected in time intervals of fixed sizes. This method allows us for the first time to obtain a systematic statistical description of the fast CME speeds. Using this method, we identify a self-similar (power law) high-speed portion of the spectrum of the speed maxima in the range of speeds from about 700 km/s to 2000 km/s. This self-similar range of the speed distribution provides a meaningful definition of "the fast" CMEs and indicates that these CMEs are produced by a process that is the same across the range of scales. The investigation of the temporal behavior of the fast CME events indicates that the time intervals between fast CMEs are not independent, i.e., fast CMEs arrive in clusters. We characterize the fast CMEs clustering by the exponent theta called the extremal index, which is the inverse of the averaged number of CMEs per cluster. An independent correlation analysis of the tail of the CME distribution confirms and further quantifies the temporal dependence among the fast CME events. To illustrate the predictive capabilities of the method, we identify clusters in the time series of CMEs with speeds greater than 1000 km/s and calculate their statistical characteristics such as the size and duration of the clusters. The method used in this paper can be applied to many other extreme geophysical events. C1 [Ruzmaikin, A.; Feynman, J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Stoev, S. A.] Univ Michigan, Dept Stat, Ann Arbor, MI 48109 USA. RP Ruzmaikin, A (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM alexander.ruzmaikin@jpl.nasa.gov; joan.feynman@jpl.nasa.gov; sstoev@umich.edu FU Jet Propulsion Laboratory of the California Institute of Technology under National Aeronautics and Space Administration; NSF [DMS-0806094] FX We are grateful to anonymous reviewers for helpful critical comments. This work was supported in part by the Jet Propulsion Laboratory of the California Institute of Technology, under a contract with the National Aeronautics and Space Administration. S. Stoev was partially supported by the NSF grant DMS-0806094. NR 25 TC 6 Z9 6 U1 0 U2 7 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 APR 19 PY 2011 VL 116 AR A04220 DI 10.1029/2010JA016247 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 754KX UT WOS:000289854600009 ER PT J AU Nunes, DC Smrekar, SE Fisher, B Plaut, JJ Holt, JW Head, JW Kadish, SJ Phillips, RJ AF Nunes, Daniel Cahn Smrekar, Suzanne E. Fisher, Brian Plaut, Jeffrey J. Holt, John W. Head, James W. Kadish, Seth J. Phillips, Roger J. TI Shallow Radar (SHARAD), pedestal craters, and the lost Martian layers: Initial assessments SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID SOUTH POLAR-REGION; MEDUSAE FOSSAE FORMATION; IMPACT CRATERS; WIND EROSION; GROUND ICE; NORTHERN-HEMISPHERE; CLIMATE-CHANGE; MARS; DEPOSITS; SURFACE AB Since their discovery, Martian pedestal craters have been interpreted as remnants of layers that were once regionally extensive but have since been mostly removed. Pedestals span from subkilometer to hundreds of kilometers, but their thickness is less than similar to 500 m. Except for a small equatorial concentration in the Medusae Fossae Formation, the nearly exclusive occurrence of pedestal craters in the middle and high latitudes of Mars has led to the suspicion that the lost units bore a significant fraction of volatiles, such as water ice. Recent morphological characterizations of pedestal deposits have further supported this view. Here we employ radar soundings obtained by the Shallow Radar (SHARAD) to investigate the volumes of a subset of the pedestal population, in concert with high-resolution imagery to assist our interpretations. From the analysis of 97 pedestal craters we find that large pedestals (diameter > 30 km) are relatively transparent to radar in their majority, with SHARAD being able to detect the base of the pedestal deposits, and possess an average dielectric permittivity of 4 +/- 0.5. In one of the cases of large pedestals in Malea Planum, layering is detected both in SHARAD data and in high-resolution imagery of the pedestal margins. We find that clutter is a major issue in the analysis of radar soundings for smaller pedestals, and tentative detection of the basal reflection occurs in only a few of the cases examined. These detections yield a higher average permittivity of similar to 6. The permittivity value derived for the larger pedestals, for which a basal reflection is unambiguous, is higher than that of pure water ice but lower than that of most silicate materials. A mixture of ice and silicates or an ice-free porous silicate matrix can explain a permittivity of similar to 4, and radar alone cannot resolve this nonuniqueness. Data from the Compact Reconnaissance Imaging Spectrometer (CRISM) tentatively confirms a mafic component in at least one pedestal in Malea Planum. Interpretation of SHARAD results can support either a mixture of ice and silicates or a porous silicate. The former is compatible with a model where nonpolar ice is periodically deposited in the midlatitudes as a result of obliquity variations. The latter is compatible with ash deposits, at least in where pedestals appear in volcanic centers such as Malea Planum. C1 [Nunes, Daniel Cahn; Smrekar, Suzanne E.; Plaut, Jeffrey J.] CALTECH, Jet Prop Lab, Pasadena, CA 91101 USA. [Fisher, Brian] Brown Univ, Div Engn, Providence, RI 02912 USA. [Holt, John W.] Univ Texas Austin, Inst Geophys, Austin, TX 78758 USA. [Head, James W.; Kadish, Seth J.] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA. [Phillips, Roger J.] SW Res Inst, Boulder, CO 80302 USA. RP Nunes, DC (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,M-S 183-301, Pasadena, CA 91101 USA. EM Daniel.Nunes@jpl.nasa.gov FU Caltech; Mars Reconnaissance Orbiter program office; National Aeronautics and Space Administration FX We would like to acknowledge Stefania Mattei and her team at the SHARAD Operations Center for their continued dedication to provide the best quality data set possible, grazie mille a voi. We would also like to thank Eldar Noe Dobrea for discussions regarding CRISM data. Caltech's Summer Undergraduate Research Fellowship supported B. Fisher and the initial thrust of this work. D. Nunes would like to thank the support from Caltech Postdoctoral Scholar Program and the Mars Reconnaissance Orbiter program office. The authors would like to acknowledge reviews by Nadine Barlow and James Skinner, which helped improve the quality of this manuscript. 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 81 TC 9 Z9 9 U1 0 U2 4 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 APR 19 PY 2011 VL 116 AR E04006 DI 10.1029/2010JE003690 PG 20 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 754JR UT WOS:000289851400002 ER PT J AU Kurtz, NT Markus, T Farrell, SL Worthen, DL Boisvert, LN AF Kurtz, N. T. Markus, T. Farrell, S. L. Worthen, D. L. Boisvert, L. N. TI Observations of recent Arctic sea ice volume loss and its impact on ocean-atmosphere energy exchange and ice production SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS LA English DT Article ID MODEL; FLUX; AMPLIFICATION; THICKNESS; CLIMATE; BALANCE; SHEBA; SNOW AB Using recently developed techniques we estimate snow and sea ice thickness distributions for the Arctic basin through the combination of freeboard data from the Ice, Cloud, and land Elevation Satellite (ICESat) and a snow depth model. These data are used with meteorological data and a thermodynamic sea ice model to calculate ocean-atmosphere heat exchange and ice volume production during the 2003-2008 fall and winter seasons. The calculated heat fluxes and ice growth rates are in agreement with previous observations over multiyear ice. In this study, we calculate heat fluxes and ice growth rates for the full distribution of ice thicknesses covering the Arctic basin and determine the impact of ice thickness change on the calculated values. Thinning of the sea ice is observed which greatly increases the 2005-2007 fall period ocean-atmosphere heat fluxes compared to those observed in 2003. Although there was also a decline in sea ice thickness for the winter periods, the winter time heat flux was found to be less impacted by the observed changes in ice thickness. A large increase in the net Arctic ocean-atmosphere heat output is also observed in the fall periods due to changes in the areal coverage of sea ice. The anomalously low sea ice coverage in 2007 led to a net ocean-atmosphere heat output approximately 3 times greater than was observed in previous years and suggests that sea ice losses are now playing a role in increasing surface air temperatures in the Arctic. C1 [Kurtz, N. T.] Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, Baltimore, MD 21228 USA. [Kurtz, N. T.; Markus, T.; Farrell, S. L.; Worthen, D. L.; Boisvert, L. N.] NASA, Goddard Space Flight Ctr, Hydrospher & Biospher Sci Lab, Greenbelt, MD 20771 USA. [Farrell, S. L.] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, Cooperat Inst Climate Studies, College Pk, MD 20742 USA. [Worthen, D. L.] RS Informat Syst, Mclean, VA USA. [Boisvert, L. N.] Univ Maryland, Dept Atmospher & Ocean Sci, College Pk, MD 20742 USA. RP Kurtz, NT (reprint author), Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, Baltimore, MD 21228 USA. EM nathan.t.kurtz@nasa.gov RI Farrell, Sinead/F-5586-2010; Markus, Thorsten/D-5365-2012 OI Farrell, Sinead/0000-0003-3222-2751; FU National Science Foundation (NSF) FX The authors would like to thank two anonymous reviewers for their invaluable suggestions, which helped in improving the manuscript. The ECMWF data for this study are from the Research Data Archive (RDA), which is maintained by the Computational and Information Systems Laboratory (CISL) at the National Center for Atmospheric Research (NCAR). NCAR is sponsored by the National Science Foundation (NSF). The original data are available from the RDA (http://dss.ucar.edu) in data set number ds627.0. We also acknowledge NSIDC for providing the AMSR-E and ICESat data used in this study (http://nsidc.org/). NR 47 TC 27 Z9 29 U1 1 U2 10 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9275 EI 2169-9291 J9 J GEOPHYS RES-OCEANS JI J. Geophys. Res.-Oceans PD APR 16 PY 2011 VL 116 AR C04015 DI 10.1029/2010JC006235 PG 19 WC Oceanography SC Oceanography GA 751VY UT WOS:000289647000001 ER PT J AU Ashley, JW Golombek, MP Christensen, PR Squyres, SW McCoy, TJ Schroder, C Fleischer, I Johnson, JR Herkenhoff, KE Parker, TJ AF Ashley, J. W. Golombek, M. P. Christensen, P. R. Squyres, S. W. McCoy, T. J. Schroeder, C. Fleischer, I. Johnson, J. R. Herkenhoff, K. E. Parker, T. J. TI Evidence for mechanical and chemical alteration of iron-nickel meteorites on Mars: Process insights for Meridiani Planum SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID ANTARCTIC METEORITES; ORDINARY CHONDRITES; CARBONACEOUS CHONDRITES; GALACTIC EVOLUTION; BURNS FORMATION; GROUND ICE; ORIGIN; SURFACE; OXIDATION; SILICON AB The weathering of meteorites found on Mars involves chemical and physical processes that can provide clues to climate conditions at the location of their discovery. Beginning on sol 1961, the Opportunity rover encountered three large iron meteorites within a few hundred meters of each other. In order of discovery, these rocks have been assigned the unofficial names Block Island, Shelter Island, and Mackinac Island. Each rock presents a unique but complimentary set of features that increase our understanding of weathering processes at Meridiani Planum. Significant morphologic characteristics interpretable as weathering features include (1) a large pit in Block Island, lined with delicate iron protrusions suggestive of inclusion removal by corrosive interaction; (2) differentially eroded kamacite and taenite lamellae in Block Island and Shelter Island, providing relative timing through crosscutting relationships with deposition of (3) an iron oxide-rich dark coating; (4) regmaglypted surfaces testifying to regions of minimal surface modification, with other regions in the same meteorites exhibiting (5) large-scale, cavernous weathering (in Shelter Island and Mackinac Island). We conclude that the current size of the rocks is approximate to their original postfall contours. Their morphology thus likely results from a combination of atmospheric interaction and postfall weathering effects. Among our specific findings is evidence supporting (1) at least one possible episode of aqueous acidic exposure for Block Island; (2) ripple migration over portions of the meteorites; (3) a minimum of two separate episodes of wind abrasion; alternating with (4) at least one episode of coating-forming chemical alteration, most likely at subzero temperatures. C1 [Ashley, J. W.; Christensen, P. R.] Arizona State Univ, Sch Earth & Space Explorat, Mars Space Flight Facil, Tempe, AZ 85287 USA. [Golombek, M. P.; Parker, T. J.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Squyres, S. W.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. [McCoy, T. J.] Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, Washington, DC 20560 USA. [Schroeder, C.] Univ Tubingen, Ctr Appl Geosci, Tubingen, Germany. [Fleischer, I.] Johannes Gutenberg Univ Mainz, Inst Anorgan & Analyt Chem, Mainz, Germany. [Johnson, J. R.; Herkenhoff, K. E.] US Geol Survey, Astrogeol Sci Ctr, Flagstaff, AZ 86001 USA. RP Ashley, JW (reprint author), Arizona State Univ, Sch Earth & Space Explorat, Mars Space Flight Facil, Tempe, AZ 85287 USA. RI Schroder, Christian/B-3870-2009; Johnson, Jeffrey/F-3972-2015 OI Schroder, Christian/0000-0002-7935-6039; FU NASA [NNX06-AD83H] FX We would like to express our sincerest thanks to our two anonymous reviewers. Jonathan Hill and Eliana McCartney were supportive in the acquisition of data products. Marc Fries was helpful in preliminary discussions. Ella Mae Lee and Bonnie Redding from the USGS team are thanked for assembling the MI mosaics for this paper. Laurence Garvie of Arizona State University's Center for Meteorite Studies is acknowledged for access to meteorite collections and discussions. For the MIPL geometric model of Block Island, we thank Nick Ruoff for tiepointing and localization, Oleg Pariser for meshing, Kris Capraro for masking off bad areas, Zareh Gorjian and Mike Stetson for cleaning up the model and determining the volume, and Bob Deen for overseeing the effort. Funding was provided in part through NASA Graduate Student Researchers Program grant NNX06-AD83H. NR 112 TC 10 Z9 10 U1 2 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 APR 16 PY 2011 VL 116 AR E00F20 DI 10.1029/2010JE003672 PG 22 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 751WA UT WOS:000289647200001 ER PT J AU Thaisen, KG Head, JW Taylor, LA Kramer, GY Isaacson, P Nettles, J Petro, N Pieters, CM AF Thaisen, Kevin G. Head, James W. Taylor, Lawrence A. Kramer, Georgiana Y. Isaacson, Peter Nettles, Jeff Petro, Noah Pieters, Carle M. TI Geology of the Moscoviense Basin SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID PEAK-RING FORMATION; MULTIRING BASINS; IMPACT CRATERS; LUNAR; MOON; EVOLUTION; VOLCANISM; MISSION; SELENE; CHICXULUB AB The Moscoviense Basin, on the northern portion of the lunar farside, displays topography with a partial peak ring, in addition to rings that are offset to the southeast. These rings do not follow the typical concentric ring spacing that is recognized with other basins, suggesting that they may have formed as a result of an oblique impact or perhaps multiple impacts. In addition to the unusual ring spacing present, the Moscoviense Basin contains diverse mare basalt units covering the basin floor and a few highland mafic exposures within its rings. New analysis of previously mapped mare units suggests that the oldest mare unit is the remnant of the impact melt sheet. The Moscoviense Basin provides a glimpse into the lunar highlands terrain and an opportunity to explore the geologic context of initial lunar crustal development and modification. C1 [Thaisen, Kevin G.; Taylor, Lawrence A.] Univ Tennessee, Dept Earth & Planetary Sci, Planetary Geosci Inst, Knoxville, TN 37996 USA. [Head, James W.; Isaacson, Peter; Nettles, Jeff; Pieters, Carle M.] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA. [Kramer, Georgiana Y.] Bear Fight Inst, Winthrop, WA 98862 USA. [Petro, Noah] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Kramer, Georgiana Y.] Lunar & Planetary Inst, Houston, TX 77058 USA. RP Thaisen, KG (reprint author), Univ Tennessee, Dept Earth & Planetary Sci, Planetary Geosci Inst, 1412 Circle Dr, Knoxville, TN 37996 USA. EM kthaisen@utk.edu RI Petro, Noah/F-5340-2013 FU NASA [NNM05AB26C] FX M3 is supported as a NASA Discovery Program mission of opportunity. The science results and science validation is supported through NASA contract NNM05AB26C. The M3 team is honored to have had the opportunity to fly as a guest instrument on Chandrayaan-1 and is grateful to all the ISRO team that enabled M3 data to be returned. We gratefully acknowledge the valuable input to this project by the public release of SELENE Terrain Camera data and LRO Laser Altimeter data. NR 66 TC 6 Z9 6 U1 1 U2 5 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 APR 16 PY 2011 VL 116 AR E00G07 DI 10.1029/2010JE003732 PG 14 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 751WA UT WOS:000289647200002 ER PT J AU Grange, ML Nemchin, AA Timms, N Pidgeon, RT Meyer, C AF Grange, M. L. Nemchin, A. A. Timms, N. Pidgeon, R. T. Meyer, C. TI Complex magmatic and impact history prior to 4.1 Ga recorded in zircon from Apollo 17 South Massif aphanitic breccia 73235 SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Article ID URANIUM-LEAD AGES; PLASTIC-DEFORMATION; MELT BRECCIAS; LUNAR; STATION-2; BOULDER-1; MANTLE; CHEMISTRY; EVOLUTION; HIGHLANDS AB Sample 73235 is one of several aphanitic impact melt breccias collected by the Apollo 17 mission at stations 2 and 3 on the slopes of the South Massif. This study presents a detailed investigation of internal structures and U-Pb ages of large zircon grains from this breccia sample. New data combined with the results of previous studies of zircon grains from the same location indicate that most zircon clasts in breccias from stations 2 and 3 formed during multiple magmatic events between 4.37 and 4.31 Ga, although the oldest zircon crystallized at about 4.42 Ga and the youngest at 4.21 Ga. In addition, zircons from the aphanitic breccias record several impact events prior to the similar to 3.9 Ga Late Heavy Bombardment. The results indicate that the zircons probably crystallized at different locations within the Procellarum KREEEP Terrane and were later excavated and modified by several impacts and delivered to the same locality within separate ejecta blankets. This locality became a source of material that formed the aphanitic impact melt breccias of the South Massif during a similar to 3.9 Ga impact. However, the zircons, showing old impact features, are not modified by this similar to 3.9 Ga impact event suggesting that (i) this common source area was located at the periphery of excavation cavity, and (ii) the > 3.9 Ga ages recorded by the zircon grains could date large (basin-forming) events as significant as major later (similar to 3.9 Ga) collisions such as Imbrium and Serenitatis. (C) 2011 Elsevier Ltd. All rights reserved. C1 [Grange, M. L.; Nemchin, A. A.; Timms, N.; Pidgeon, R. T.] Curtin Univ, Western Australian Sch Mines, Dept Appl Geol, Perth, WA 6845, Australia. [Nemchin, A. A.] Univ Munster, Inst Mineral, D-48149 Munster, Germany. [Meyer, C.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. RP Grange, ML (reprint author), Curtin Univ, Western Australian Sch Mines, Dept Appl Geol, GPO Box U1987, Perth, WA 6845, Australia. EM m.grange@curtin.edu.au RI Grange, Marion/B-1449-2013; OI Timms, Nicholas/0000-0003-2997-4303; Grange, Marion/0000-0001-6405-8795 FU Curtin Internal Research Grant; DFG FX We want to thank the NASA, and especially the crew of Apollo 17 as none of the samples will be available for the study without their hard work. We are also grateful to Marc Norman, Liu Dunyi and Odette James for their constructive comments that helped improve the paper. M. G. and N.T. acknowledge funding from a Curtin Internal Research Grant. Rob Hart is thanked for his assistance with scanning electron microscopy. A.N. research at Munster University is currently supported by DFG. NR 57 TC 22 Z9 22 U1 1 U2 6 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 APR 15 PY 2011 VL 75 IS 8 BP 2213 EP 2232 DI 10.1016/j.gca.2011.01.036 PG 20 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 796EJ UT WOS:000293033100014 ER PT J AU Danielson, S Eisner, L Weingartner, T Aagaard, K AF Danielson, S. Eisner, L. Weingartner, T. Aagaard, K. TI Thermal and haline variability over the central Bering Sea shelf: Seasonal and interannual perspectives SO CONTINENTAL SHELF RESEARCH LA English DT Article DE Bering Sea; Seasonal variability; Interannual variability; Temperature; Salinity; Ekman transport ID ALASKA COASTAL CURRENT; ARCTIC-OCEAN; ALEUTIAN LOW; FRESH-WATER; HEAT FLUXES; ICE; CIRCULATION; ECOSYSTEM; PATTERNS; PACIFIC AB We examine multi-year conductivity-temperature-depth (CTD) data to better understand temperature and salinity variability over the central Bering Sea shelf. Particular consideration is given to observations made annually from 2002 to 2007 between August and October, although other seasons and years are also considered. Vertical and horizontal correlation maps show that near-surface and near-bottom salinity anomalies tend to fluctuate in phase across the central shelf, but that temperature anomalies are vertically coherent only in the weakly or unstratified inner-shelf waters. We formulate heat content (HC) and freshwater content (FWC) budgets based on the CTD observations, direct estimates of external fluxes (surface heat fluxes, ice melt, precipitation (P), evaporation (E) and river discharge), and indirect estimates of advective contributions. Ice melt, P - E, river discharge, and along-isobath advection are sufficient to account for the mean spring-to-fall increase in FWC, while summer surface heat fluxes are primarily responsible for the mean seasonal increase in HC, although interannual variability in the HC at the end of summer appears related to variability in the along-isobath advection during the summer months. On the other hand, FWC anomalies at the end of summer are significantly correlated with the mean wind direction and cross-isobath Ekman transport averaged over the previous winter. Consistent with the latter finding, salinities exhibit a weak but significant inverse correlation between the coastal and mid-shelf waters. The cross-shelf transport likely has significant effect on nutrient fluxes and other processes important to the functioning of the shelf ecosystem. Both the summer and winter advection fields appear to result from the seasonal mean position and strength of the Aleutian Low. We find that interannual thermal and haline variability over the central Bering Sea shelf are largely uncoupled. (C) 2010 Elsevier Ltd. All rights reserved. C1 [Danielson, S.; Weingartner, T.] Univ Alaska Fairbanks, Inst Marine Sci, Sch Fisheries & Ocean Sci, Fairbanks, AK 99775 USA. [Eisner, L.] Natl Marine Fisheries Serv, NOAA, Alaska Fisheries Sci Ctr, Ted Stevens Marine Res Inst, Juneau, AK USA. [Aagaard, K.] Univ Washington, Appl Phys Lab, Polar Sci Ctr, Seattle, WA 98105 USA. RP Danielson, S (reprint author), Univ Alaska Fairbanks, Inst Marine Sci, Sch Fisheries & Ocean Sci, Rm 114,ONeill Bldg, Fairbanks, AK 99775 USA. EM seth@ims.uaf.edu FU BASIS scientists at NOAA/AFSC; NOAA/PMEL; NSF [HLY-07-01, HLY-08-03, KN195-10, ARC-0732428, ARC-0732771]; Arctic-Yukon-Kuskokwim Sustainable Salmon Initiative; Bering Sea Fisherman's Association; NOAA; National Marine Fisheries Service; North Pacific Research Board [NPMRI 12130]; Arctic Yukon Kuskokwim Sustainable Salmon Initiative [1195952] FX This manuscript would not have been possible without the cross-institutional and cross-disciplinary collaboration that has been fostered through the BASIS and BEST programs. We particularly thank Ed Farley and the rest of the BASIS scientists at NOAA/AFSC for their support. Many thanks to Kristin Cieciel for survey logistics, oceanographic data collection, CTD data processing, and database maintenance; John Pohl and Alex Andrews for oceanographic data collection; Jennifer Lanksbury for database design and maintenance; Rolf Gradinger, Katrin Iken, and Bodil Bluhm for sharing their ice station data; and Phyllis Stabeno for sharing M2 mooring data and BEST CTD data, both collected with the support of the NOAA/PMEL Eco-FOCI program. We thank he dedicated crews of the F/V Sea Storm, F/V NW Explorer, R/V Oscar Dyson, R/V Knorr, R/V Point Sur, and the USCGC Healy for the many successful BASIS and BEST cruises. We thank the BEST program scientists and field crews for the LID data collections and processing. Data from NSF sponsored BEST cruises HLY-07-01, HLY-08-03, and KN195-10 were taken under the direction of chief scientist R. Sambrotto, Lamont-Doherty Earth Observatory, Palisades, NY; data from cruise HLY-08-02 were taken under the direction of chief scientist Carin Ashjian, Woods Hole Oceanographic Institute, Woods Hole, MA; and data from cruise HLY-09-01 were taken under the direction of chief scientist Lee Cooper, University of Maryland Center for Environmental Science, Solomons, MD. The manuscript was improved with valuable comments from two anonymous reviewers. BASIS oceanographic data collection was funded by the Arctic-Yukon-Kuskokwim Sustainable Salmon Initiative, the Bering Sea Fisherman's Association, NOAA Fisheries and the Environment (FATE) program, and the National Marine Fisheries Service. Drifter data were collected under funding from the North Pacific Research Board, Grant NPMRI 12130, and the Arctic Yukon Kuskokwim Sustainable Salmon Initiative, Grant ADN #1195952. This manuscript is listed as BEST/BSIERP Publication #6. K. Aagaard was supported by NSF Grant ARC-0732428. S. Danielson and T. Weingartner received financial support from the Bering Sea Fisherman's Association Grant AC-299 and NSF Grant ARC-0732771. NR 79 TC 34 Z9 35 U1 0 U2 12 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0278-4343 J9 CONT SHELF RES JI Cont. Shelf Res. PD APR 15 PY 2011 VL 31 IS 6 BP 539 EP 554 DI 10.1016/j.csr.2010.12.010 PG 16 WC Oceanography SC Oceanography GA 765ZE UT WOS:000290747100003 ER PT J AU Righter, K King, C Danielson, L Pando, K Lee, CT AF Righter, K. King, C. Danielson, L. Pando, K. Lee, C. T. TI Experimental determination of the metal/silicate partition coefficient of Germanium: Implications for core and mantle differentiation SO EARTH AND PLANETARY SCIENCE LETTERS LA English DT Article DE Germanium; Core formation; Siderophile; Mantle; Differentiation ID SILICATE MELT COMPOSITION; SIDEROPHILE ELEMENTS; IRON-METEORITES; HIGH-PRESSURE; MAGMA OCEAN; ISOTOPIC VARIATIONS; BASALTIC GLASSES; HIGH-TEMPERATURE; OXYGEN FUGACITY; TRACE-ELEMENTS AB Germanium is a moderately siderophile, and volatile element that exhibits a depletion in Earth's mantle and other planetary and asteroidal basalts (relative to chondritic values). Attempts to explain these depletions have not been satisfactory, but there have also been too few experimental studies to constrain the chemical behavior of Ge. Experimental data have been challenging due to difficulties in analyzing the low (1 to 100 ppm) concentrations of Ge in silicate melts. In this study we examine the role of temperature and silicate melt composition in controlling the value of D(Ge) metal/silicate, by carrying out new experiments at high temperature and pressure. The experimental glasses were analyzed using laser-ablation ICP-MS, which can detect levels of Ge much lower than possible with the electron microprobe. Our new results show that D(Ge) metal/silicate decreases with increasing temperature over the range from 1500 to 1900 degrees C. Additionally, changing silicate melt composition from basalt to peridotite causes a small increase in D(Ge) metal/silicate, compared to the decrease observed in previous studies across a different range of melt composition. These results, combined with previous studies at higher pressures and with S-bearing metallic liquids, show that there are high PT conditions at which the Ge concentration Earth's primitive upper mantle can be explained through metal-silicate equilibrium in a magma ocean stage, where equilibration took place at 40 (+/- 4) GPa and 3200 (+/- 200) degrees C. Additionally, estimated Ge contents of the lunar, Martian and HED parent body mantles can be explained by magma ocean conditions in all of these bodies early in the solar system. These calculations all take into account both the volatile and siderophile nature of Ge. Published by Elsevier B.V. C1 [Righter, K.; Danielson, L.; Pando, K.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [King, C.] Univ Arizona, Dept Geosci, Tucson, AZ 85721 USA. [King, C.] Lunar & Planetary Inst, Houston, TX 77058 USA. [Lee, C. T.] Rice Univ, Dept Earth Sci, Houston, TX 77005 USA. RP Righter, K (reprint author), NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. EM kevin.righter-1@nasa.gov RI Lee, Cin-Ty/A-5469-2008 FU Lunar and Planetary Institute (LPI); RTOP; Packard Fellowship FX C. King was supported by a summer internship at the Lunar and Planetary Institute (LPI). The research was supported by an RTOP to K. Righter and a Packard Fellowship to C.-T. Lee. V. LeRoux provided assistance with the LA-ICP-MS analysis, as did A. Peslier and L Le on the electron microprobe at JSC. The manuscript benefitted from the journal reviews of D. Walker and an anonymous reviewer. NR 77 TC 16 Z9 16 U1 2 U2 19 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 APR 15 PY 2011 VL 304 IS 3-4 BP 379 EP 388 DI 10.1016/j.epsl.2011.02.015 PG 10 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 767EV UT WOS:000290839000009 ER PT J AU Simon, JI Young, ED AF Simon, Justin I. Young, Edward D. TI Resetting, errorchrons and the meaning of canonical CAI initial Al-26/Al-27 values SO EARTH AND PLANETARY SCIENCE LETTERS LA English DT Article DE solar nebula; chronology; 26Al; open system resetting; isochrons; CAIs ID AL-RICH INCLUSIONS; EARLY SOLAR-SYSTEM; MAGNESIUM ISOTOPE HETEROGENEITY; REFRACTORY INCLUSIONS; SELF-DIFFUSION; ALLENDE; NEBULA; MG; FRACTIONATION; EVAPORATION AB The difference between the precise MC-ICPMS analyses of bulk calcium-aluminum-rich inclusion (CAI) fragments (e.g., Jacobsen et al., 2008) and supra-canonical values obtained by micro-analytical techniques, e.g., laser ablation MC-ICPMS (Young et al., 2005) and SIMS (Taylor et al., 2005), at face value seems to be problematic and therefore leads many to dismiss claims of the solar system (Al-26/Al-22)(o) greater than similar to 5 x 10(-5) as spurious. Here we use mass balance calculations to quantify the importance of open system isotopic exchange during CAI evolution and show that in situ supra-canonical, in-situ canonical, and bulk canonical measurements can all exist for an individual CAI. The calculations describe mechanisms of isotopic exchange that may have occurred early (100's ka) and late (similar to 1.5 Ma) in the solar nebula and much later (> 10's Ma) on parent body planetesimals. A range of possible modal mineralogies is modeled in order to populate the compositional space defined by in situ and bulk CAI measurements. In support of these simulated data we. describe in situ measurements of Al-27/Mg-24, Mg-25/Mg-24, and Mg-26/Mg-24 obtained by IA-MC-ICPMS comprising core-to-rim traverses across three CV3 CAls. The CAls exhibit distinctive Mg isotopic zoning profiles and varying abundances of daughter products of the short-lived nuclide Al-26 that are consistent with varying amounts of open system isotope exchange. Published by Elsevier B.V. C1 [Simon, Justin I.] NASA, Lyndon B Johnson Space Ctr, Astromat Res Off KR111, Houston, TX 77058 USA. [Young, Edward D.] Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90095 USA. [Young, Edward D.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90095 USA. RP Simon, JI (reprint author), NASA, Lyndon B Johnson Space Ctr, Astromat Res Off KR111, Houston, TX 77058 USA. EM Justin.I.Simon@NASA.gov RI Simon, Justin/D-7015-2011 FU NASA; NASA Astrobiology Institute; National Science Foundation (USA); NASA Johnson Space Cente FX Discussions with K. McKeegan, A. Davis, M. Ito, Q. Yin, B. Jacobsen, S. Jacobsen, I. Hutcheon, A. Galy, and O. Lovera are greatly appreciated. As are input and sample material provided by S. Russell. Critical and helpful reviews by A. Davis and T. Fagan improve the clarity of the manuscript. This work was supported by grants from the NASA Cosmochemistry program, the NASA Astrobiology Institute, and the National Science Foundation (USA). J. Simon acknowledges support from NASA Johnson Space Center and wishes to thank D. DePaolo and P. Renne for their support of his postdoctoral research over which time some of the ideas and calculations for this contribution originated. NR 60 TC 8 Z9 8 U1 1 U2 6 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 APR 15 PY 2011 VL 304 IS 3-4 BP 468 EP 482 DI 10.1016/j.epsl.2011.02.023 PG 15 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 767EV UT WOS:000290839000017 ER PT J AU Sakamoto, T Barbier, L Barthelmy, SD Cummings, JR Fenimore, EE Gehrels, N Krimm, HA Markwardt, CB Palmer, DM Parsons, AM Sato, G Stamatikos, M Tueller, J AF Sakamoto, T. Barbier, L. Barthelmy, S. D. Cummings, J. R. Fenimore, E. E. Gehrels, N. Krimm, H. A. Markwardt, C. B. Palmer, D. M. Parsons, A. M. Sato, G. Stamatikos, M. Tueller, J. TI Probing the nature of short swift bursts via deep INTEGRAL monitoring of GRB 050925 SO ADVANCES IN SPACE RESEARCH LA English DT Article DE Gamma-ray; Burst ID GAMMA-RAY BURSTS; SGR-1900+14; SGR-1806-20; DISCOVERY; EMISSION; HETE-2; FLARE AB We present results from Swift, XMM-Newton, and deep INTEGRAL monitoring in the region of GRB 050925. This short Swift burst is a candidate for a newly discovered soft gamma-ray repeater (SGR) with the following observational burst properties: (1) galactic plane (b = -0.1 degrees) localization, (2) 150 ms duration, and (3) a blackbody rather than a simple power-law spectral shape (with a significance level of 97%). We found two possible X-ray counterparts of GRB 050925 by comparing the X-ray images from Swift XRT and XMM-Newton. Both X-ray sources show the transient behavior with a power-law decay index shallower than -1. We found no hard X-ray emission nor any additional burst from the location of GRB 050925 in similar to 5 ms of INTEGRAL data. We discuss about the three BATSE short bursts which might be associated with GRB 050925, based on their location and the duration. Assuming GRB 050925 is associated with the H-11 regions (W 58) at the galactic longitude of l = 70 degrees, we also discuss the source frame properties of GRB 050925. (C) 2010 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 [Sakamoto, T.; Cummings, J. R.; Krimm, H. A.; Markwardt, C. B.] CRESST, Greenbelt, MD 20771 USA. [Sakamoto, T.; Barbier, L.; Barthelmy, S. D.; Cummings, J. R.; Gehrels, N.; Krimm, H. A.; Markwardt, C. B.; Parsons, A. M.; Tueller, J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Sakamoto, T.; Cummings, J. R.] Univ Maryland, Joint Ctr Astrophys, Baltimore, MD 21250 USA. [Fenimore, E. E.; Palmer, D. M.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA. [Krimm, H. A.] Univ Space Res Assoc, Columbia, MD 21044 USA. [Markwardt, C. B.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Sato, G.] JAXA, Inst Space & Astronaut Sci, Kanagawa 2298510, Japan. [Stamatikos, M.] Oak Ridge Associated Univ, Oak Ridge, TN 37831 USA. RP Sakamoto, T (reprint author), CRESST, Greenbelt, MD 20771 USA. EM Taka.Sakamoto@nasa.gov RI Barthelmy, Scott/D-2943-2012; Gehrels, Neil/D-2971-2012; Tueller, Jack/D-5334-2012; Parsons, Ann/I-6604-2012 NR 23 TC 3 Z9 3 U1 0 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 APR 15 PY 2011 VL 47 IS 8 BP 1346 EP 1352 DI 10.1016/j.asr.2010.08.004 PG 7 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA 758CE UT WOS:000290136700011 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 Vachier, F Arnouts, S Perley, D 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. Vachier, F. Arnouts, S. Perley, D. TI The origin of the prompt optical emission in GRB 060111B SO ADVANCES IN SPACE RESEARCH LA English DT Article DE Gamma-ray burst; Non-thermal radiation ID GAMMA-RAY BURSTS AB The detection of a bright optical emission measured with good temporal resolution during the prompt phase makes ORB 060111B a rare event that is especially useful for constraining theories of the prompt optical emission. Comparing this burst with other GRBs with evidence of optical peaks, we find that the optical peak epoch (t(p)) is anti-correlated with the high energy burst energetic assuming an isotropic energy release (E-iso) in agreement with Liang et al. (2009), and that the steeper is the post-peak afterglow decay, the less is the agreement with the correlation. GRB 060111B is among the tatters and it does not match the correlation. The Cannonball scenario is also discussed and we find that this model cannot be excluded for GRB 060111B. (C) 2010 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 [Stratta, G.; Gendre, B.; Verrecchia, F.; Cutini, S.] ASI Sci Data Ctr, ASDC, I-00044 Frascati, Italy. [Pozanenko, A.] Space Res Inst IKI, Moscow 117997, Russia. [Atteia, J. L.; Ienna, F.] Univ Toulouse, LATT, CNRS, F-31400 Toulouse, France. [Klotz, A.] Univ Toulouse, CESR, CNRS, UMR 5187, F-31028 Toulouse, France. [Basa, S.] LAM OAM, F-13388 Marseille, France. [Boer, M.] Observ Haute Provence, OHP, F-04870 St Michel Lobservatoire, France. [Henze, M.; Klose, S.] Thueringer Landessternwarte, D-07778 Tautenburg, Germany. [Holland, S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Ibrahimov, M.] Ulugh Beg Astron Inst, Tashkent 100052, Uzbekistan. [Khamitov, I.] Akdeniz Univ Yerleskesi, TUBITAK Natl Observ, TR-07058 Antalya, Turkey. [Rumyantsev, V.] SRI Crimean Astrophys Observ, Sci Res Inst, 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-92190 Paris, France. [Arnouts, S.] Canada France Hawaii Telescope Corp, Kamuela, HI 96743 USA. [Perley, D.] 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 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; Verrecchia, Francesco/0000-0003-3455-5082; Rumyantsev, Vasilij/0000-0003-1894-7019; Cutini, Sara/0000-0002-1271-2924; Henze, Martin/0000-0001-9985-3406 NR 9 TC 1 Z9 1 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 APR 15 PY 2011 VL 47 IS 8 BP 1413 EP 1415 DI 10.1016/j.asr.2010.06.014 PG 3 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA 758CE UT WOS:000290136700020 ER PT J AU Nishikawa, KI Niemiec, J Medvedev, M Zhang, B Hardee, P Nordlund, A Frederiksen, J Mizuno, Y Sol, H Pohl, M Hartmann, DH Oka, M Fishman, GJ AF Nishikawa, K. -I. Niemiec, J. Medvedev, M. Zhang, B. Hardee, P. Nordlund, A. Frederiksen, J. Mizuno, Y. Sol, H. Pohl, M. Hartmann, D. H. Oka, M. Fishman, G. J. TI Radiation from relativistic shocks in turbulent magnetic fields SO ADVANCES IN SPACE RESEARCH LA English DT Article DE Acceleration of particles; Radiation; Jets; Gamma rays bursts; Magnetic fields; Plasmas ID GAMMA-RAY BURSTS; PARTICLE-ACCELERATION; COLLISIONLESS SHOCKS; WEIBEL INSTABILITY; PROMPT EMISSION; FIREBALL MODEL; AFTERGLOWS; SIMULATIONS; GENERATION; EVOLUTION AB Using our new 3-D relativistic particle-in-cell (PIC) code parallelized with MPI, we investigated long-term particle acceleration associated with a relativistic electron positron jet propagating in an unmagnetized ambient electron positron plasma. The simulations were performed using a much longer simulation system than our previous simulations in order to investigate the full nonlinear stage of the Weibel instability and its particle acceleration mechanism. Cold jet electrons are thermalized and ambient electrons are accelerated in the resulting shocks. Acceleration of ambient electrons leads to a maximum ambient electron density three times larger than the original value as predicted by hydrodynamic shock compression. In the jet (reverse) shock behind the bow (forward) shock the strongest electromagnetic fields are generated. These fields may lead to time dependent afterglow emission. In order to calculate radiation from first principles that goes beyond the standard synchrotron model used in astrophysical objects we have used PIC simulations. Initially we calculated radiation from electrons propagating in a uniform parallel magnetic field to verify the technique. We then used the technique to calculate emission from electrons in a small simulation system. From these simulations we obtained spectra which are consistent with those generated from electrons propagating in turbulent magnetic fields with red noise. This turbulent magnetic field is similar to the magnetic field generated at an early nonlinear stage of the Weibel instability. A fully developed shock within a larger simulation system may generate a jitter/synchrotron spectrum. (C) 2011 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 [Nishikawa, K. -I.; Mizuno, Y.] Natl Space Sci & Technol Ctr, Huntsville, AL 35805 USA. [Niemiec, J.] Inst Nucl Phys PAN, PL-31342 Krakow, Poland. [Medvedev, M.] Univ Kansas, Dept Phys & Astron, Lawrence, KS 66045 USA. [Zhang, B.] Univ Nevada, Dept Phys, Las Vegas, NV 89154 USA. [Hardee, P.] Univ Alabama, Dept Phys & Astron, Tuscaloosa, AL 35487 USA. [Nordlund, A.; Frederiksen, J.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark. [Sol, H.] Observ Paris, LUTH, F-92195 Meudon, France. [Pohl, M.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. [Hartmann, D. H.] Clemson Univ, Dept Phys & Astron, Clemson, SC 29634 USA. [Oka, M.] Univ Calif Berkeley, ISpace Sci Lab, Berkeley, CA 94720 USA. [Fishman, G. J.] NASA MSFC, Huntsville, AL 35805 USA. RP Nishikawa, KI (reprint author), Natl Space Sci & Technol Ctr, Huntsville, AL 35805 USA. EM ken-ichi.nishikawa-l@nasa.gov RI Nordlund, Aake/M-4528-2014; Frederiksen, Jacob Trier/P-6757-2015; Mizuno, Yosuke/D-5656-2017 OI Nordlund, Aake/0000-0002-2219-0541; Frederiksen, Jacob Trier/0000-0002-3560-0044; Mizuno, Yosuke/0000-0002-8131-6730 FU MNiSW [1 P03D 003 29, N N203 393034]; Foundation for Polish Science; EEA Financial Mechanism; National Science Foundation NSF [PHY05-51164]; Danish Natural Science Research Council; [NSF-AST-0506719]; [AST-0506666]; [AST-0908040]; [AST-0908010]; [NASA-NNG05G-K73G]; [NNX07AJ88G]; [NNX08AG83G]; [NNX 08AL39G]; [NNX09AD16G] FX This work is supported by NSF-AST-0506719, AST-0506666, AST-0908040, AST-0908010, NASA-NNG05G-K73G, NNX07AJ88G, NNX08AG83G, NNX 08AL39G, and NNX09AD16G. JN was supported by MNiSW research projects 1 P03D 003 29 and N N203 393034, and The Foundation for Polish Science through the HOMING program, which is supported through the EEA Financial Mechanism. Simulations were performed at the Columbia facility at the NASA Advanced Supercomputing (NAS) and IBM p690 (Copper) at the National Center for Supercomputing Applications (NCSA) which is supported by the NSF. Part of this work was done while K.-I. N. was visiting the Niels Bohr Institute. Support from the Danish Natural Science Research Council is gratefully acknowledged. This report was finalized during the program "Particle Acceleration in Astrophysical Plasmas" at the Kavli Institute for Theoretical Physics which is supported by the National Science Foundation under Grant No. PHY05-51164. NR 48 TC 16 Z9 16 U1 0 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 APR 15 PY 2011 VL 47 IS 8 BP 1434 EP 1440 DI 10.1016/j.asr.2011.01.032 PG 7 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA 758CE UT WOS:000290136700024 ER PT J AU Sakamoto, T Wallace, CA Donato, D Gehrels, N Okajima, T Ukwatta, TN AF Sakamoto, T. Wallace, C. A. Donato, D. Gehrels, N. Okajima, T. Ukwatta, T. N. TI Goddard Robotic Telescope - Optical follow-up of GRBs and coordinated observations of AGNs SO ADVANCES IN SPACE RESEARCH LA English DT Article DE Gamma ray; Burst; AGN; Optical ID GAMMA-RAY BURSTS; PROMPT; NUCLEI AB Since it is not possible to predict when a Gamma-Ray Burst (GRB) will occur or when Active Galactic Nucleus (AGN) flaring activity starts, follow-up/monitoring ground telescopes must be located as uniformly as possible all over the world in order to collect data simultaneously with Fermi and Swift detections. However, there is a distinct gap in follow-up coverage of telescopes in the eastern U.S. region based on the operations of Swift. Motivated by this fact, we have constructed a 14 '' fully automated optical robotic telescope, Goddard Robotic Telescope (GRT), at the Goddard Geophysical and Astronomical Observatory. The aims of our robotic telescope are (1) to follow-up Swift/Fermi GRBs and (2) to perform the coordinated optical observations of Fermi Large Area Telescope (LAT) AGN. Our telescope system consists of off-the-shelf hardware. With the focal reducer, we are able to match the field of view of Swift narrow instruments (20' x 20'). We started scientific observations in mid-November 2008 and GRT has been fully remotely operated since August 2009. The 3 sigma upper limit in a 30s exposure in the R filter is similar to 15.4 mag; however, we can reach to similar to 18 mag in a 600 s exposures. Due to the weather condition at the telescope site, our observing efficiency is 30-40% on average. (c) 2010 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 [Sakamoto, T.; Donato, D.] CRESST, Greenbelt, MD 20771 USA. [Sakamoto, T.; Donato, D.; Gehrels, N.; Okajima, T.; Ukwatta, T. N.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Sakamoto, T.] Univ Maryland Baltimore Cty, Joint Ctr Astrophys, Baltimore, MD 21250 USA. [Wallace, C. A.] Florida Gulf Coast Univ, Ft Myers, FL 33965 USA. [Donato, D.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Okajima, T.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Ukwatta, T. N.] George Washington Univ, Dept Phys, Washington, DC 20052 USA. RP Sakamoto, T (reprint author), CRESST, Greenbelt, MD 20771 USA. EM Taka.Sakamoto@nasa.gov RI Gehrels, Neil/D-2971-2012 NR 11 TC 1 Z9 1 U1 0 U2 2 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0273-1177 J9 ADV SPACE RES JI Adv. Space Res. PD APR 15 PY 2011 VL 47 IS 8 BP 1444 EP 1450 DI 10.1016/j.asr.2010.10.018 PG 7 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA 758CE UT WOS:000290136700026 ER PT J AU Mawet, D Serabyn, E Wallace, JK Pueyo, L AF Mawet, Dimitri Serabyn, Eugene Wallace, J. Kent Pueyo, Laurent TI Improved high-contrast imaging with on-axis telescopes using a multistage vortex coronagraph SO OPTICS LETTERS LA English DT Article AB The vortex coronagraph is one of the most promising coronagraphs for high-contrast imaging because of its simplicity, small inner working angle, high throughput, and clear off-axis discovery space. However, as with most coronagraphs, centrally obscured on-axis telescopes degrade contrast. Based on the remarkable ability of vortex coronagraphs to move light between the interior and exterior of pupils, we propose a method based on multiple vortices, that without sacrificing throughput, reduces the residual light leakage to (a/A)(n), with n >= 4, and a and A being the radii of the central obscuration and primary mirror, respectively. This method thus enables high contrasts to be reached even with an on-axis telescope. (c) 2011 Optical Society of America C1 [Mawet, Dimitri; Serabyn, Eugene; Wallace, J. Kent; Pueyo, Laurent] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Pueyo, Laurent] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Pueyo, Laurent] Johns Hopkins Univ, Baltimore, MD 21218 USA. RP Mawet, D (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM dmawet@eso.org FU National Aeronautics and Space Administration; Carl Sagan Fellowship Program FX This work was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. L. Pueyo acknowledge support from the Carl Sagan Fellowship Program. NR 11 TC 36 Z9 37 U1 0 U2 4 PU OPTICAL SOC AMER PI WASHINGTON PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA SN 0146-9592 J9 OPT LETT JI Opt. Lett. PD APR 15 PY 2011 VL 36 IS 8 BP 1506 EP 1508 PG 3 WC Optics SC Optics GA 756SH UT WOS:000290034500067 PM 21499405 ER PT J AU Volz, MP Mazuruk, K AF Volz, M. P. Mazuruk, K. TI Existence and shapes of menisci in detached Bridgman growth SO JOURNAL OF CRYSTAL GROWTH LA English DT Article DE Bridgman technique; Detached growth; Microgravity conditions; Growth from melt; Semiconducting germanium ID GERMANIUM SINGLE-CRYSTALS; CRUCIBLE CONTACT; SOLIDIFICATION; MELTS; MICROGRAVITY; DEPENDENCE; ANGLE AB In detached Bridgman growth, the crystal radius is less than the crucible radius and a meniscus bridges the gap between the crystal and crucible wall. Existence of detached growth depends upon the contact angle of the melt with the crucible wall, the growth angle of the solidifying crystal, the pressure differential across the meniscus, and the Bond number. The Young-Laplace capillary equation is used to calculate the crystal radii of detached states as a function of the pressure differential across the meniscus. Both terrestrial and microgravity conditions are considered. A variety of solution states is found, and multiple solutions with different crystal radii can exist for a given value of the pressure differential. The meniscus shapes for the detached states vary from simply convex or concave to shapes with numerous inflections. An approximate solution to the Young-Laplace equation for small Bond numbers is derived. Published by Elsevier B.V. C1 [Volz, M. P.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. [Mazuruk, K.] Univ Alabama, Huntsville, AL 35899 USA. RP Volz, MP (reprint author), NASA, George C Marshall Space Flight Ctr, EM31, Huntsville, AL 35812 USA. EM Martin.Volz@nasa.gov FU NASA International Space Station FX The authors gratefully acknowledge support from the NASA International Space Station Research Project. NR 27 TC 7 Z9 7 U1 2 U2 5 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0022-0248 J9 J CRYST GROWTH JI J. Cryst. Growth PD APR 15 PY 2011 VL 321 IS 1 BP 29 EP 35 DI 10.1016/j.jcrysgro.2011.02.035 PG 7 WC Crystallography; Materials Science, Multidisciplinary; Physics, Applied SC Crystallography; Materials Science; Physics GA 757BC UT WOS:000290057900006 ER PT J AU Schultz, JK Becker, BL Johanos, TC Lopez, JU Kashinsky, L AF Schultz, Jennifer K. Becker, Brenda L. Johanos, Thea C. Lopez, Jessica U. Kashinsky, Lizabeth TI Dizygotic twinning in the Hawaiian monk seal SO JOURNAL OF MAMMALOGY LA English DT Article DE fecundity; maternal investment; microsatellite; multiple maternity; Monachus schauinslandi ID ZEALAND FUR-SEAL; MONACHUS-SCHAUINSLANDI; FOSTERING BEHAVIOR; REPRODUCTIVE-CYCLE; HALICHOERUS-GRYPUS; ELEPHANT SEALS; GREY SEALS; SURVIVAL; PUP AB Twinning is extremely rare in pinnipeds. Instances in which a female is observed simultaneously nursing 2 pups may represent alloparenting, or nonfilial nursing, a relatively common trait in pinnipeds. We explored the incidence of twinning in the Hawaiian monk seal (Monachus schauinslandi). We observed 7 sets of putative twins (i.e., an isolated female nursing 2 newborn pups) of 4,965 total births recorded between 1983 and 2008 (minimum twinning rate = 0.1%). Genetic specimens from the mother and both pups were available only for 5 of the 7 sets. Microsatellite genotyping revealed all of these to be dizygotic twins, with low probability of false assignment (P < 0.001). On average, Hawaiian monk seal twins were less likely to survive to weaning than singletons born in the same year and on the same island (P = 0.008). Those that weaned were smaller in size (i.e., axillary girths 1-4 SDs lower than singletons). In the critically endangered Hawaiian monk seal twinning appears to be a rare trait that results in overall lower survival rates but also offers a small opportunity for stock enhancement. C1 [Schultz, Jennifer K.] Univ Hawaii Manoa, Sch Ocean & Earth Sci & Technol, Hawaii Inst Marine Biol, Kaneohe, HI 96744 USA. [Becker, Brenda L.; Johanos, Thea C.; Lopez, Jessica U.; Kashinsky, Lizabeth] Natl Marine Fisheries Serv, Pacific Isl Fisheries Sci Ctr, Honolulu, HI 96814 USA. RP Schultz, JK (reprint author), Univ Hawaii Manoa, Sch Ocean & Earth Sci & Technol, Hawaii Inst Marine Biol, POB 1346, Kaneohe, HI 96744 USA. EM jschultz@hawaii.edu FU Marine Mammal Commission [GS00M04PDM0027]; Northwestern Hawaiian Islands Coral Reef Ecosystem Reserve; Environmental Protection Agency STAR; National Science Foundation [0549514] FX We thank the numerous seasonal field crews for their efforts in the collection of data, particularly S. Canja, S. Farry, J. Henderson, J. Klavitter, L. Laniawe, R. Marshall, A. Dietrich, E. Green, J. Jones, J. Palmer, and M. Vekasy. Drs. R. Braun and A. Aguirre conducted necropsies on several of the dead twins. We thank F. Parrish, C. Littnan, J. Baker, T. Wurth, and A. Harting for comments on the manuscript. For logistical support we thank the Papahanaumokuakea Marine National Monument, United States Fish and Wildlife Service, and the captain, officers, and crew of the National Oceanic and Atmospheric Administration ships Townsend Cromwell and Oscar Elton Sette. This research was performed under the following National Marine Fisheries Service Scientific Research and Enhancement permits: 413, 482, 489, 889, 848-1335, and 848-1695. Funding was provided by the Marine Mammal Commission (research grant GS00M04PDM0027) and the Northwestern Hawaiian Islands Coral Reef Ecosystem Reserve. JKS was supported by Environmental Protection Agency STAR and National Science Foundation IGERT fellowships (award 0549514; principal investigator B. A. Wilcox). This is contribution 1416 from the Hawai'i Institute of Marine Biology and contribution 8033 from the School of Ocean and Earth Science and Technology at the University of Hawai'i. NR 36 TC 2 Z9 2 U1 0 U2 11 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 0022-2372 EI 1545-1542 J9 J MAMMAL JI J. Mammal. PD APR 15 PY 2011 VL 92 IS 2 BP 336 EP 341 DI 10.1644/10-MAMM-A-275.1 PG 6 WC Zoology SC Zoology GA 754PV UT WOS:000289869700008 ER PT J AU Masek, JG Cohen, WB Leckie, D Wulder, MA Vargas, R de Jong, B Healey, S Law, B Birdsey, R Houghton, RA Mildrexler, D Goward, S Smith, WB AF Masek, Jeffrey G. Cohen, Warren B. Leckie, Donald Wulder, Michael A. Vargas, Rodrigo de Jong, Ben Healey, Sean Law, Beverly Birdsey, Richard Houghton, R. A. Mildrexler, David Goward, Samuel Smith, W. Brad TI Recent rates of forest harvest and conversion in North America SO JOURNAL OF GEOPHYSICAL RESEARCH-BIOGEOSCIENCES LA English DT Article ID LAND-USE CHANGE; REMOTELY-SENSED DATA; UNITED-STATES; CARBON STORAGE; PONDEROSA PINE; WOOD PRODUCTS; COVER LOSS; MANAGEMENT-PRACTICES; PACIFIC-NORTHWEST; TROPICAL FORESTS AB Incorporating ecological disturbance into biogeochemical models is critical for estimating current and future carbon stocks and fluxes. In particular, anthropogenic disturbances, such as forest conversion and wood harvest, strongly affect forest carbon dynamics within North America. This paper summarizes recent (2000-2008) rates of extraction, including both conversion and harvest, derived from national forest inventories for North America (the United States, Canada, and Mexico). During the 2000s, 6.1 million ha/yr were affected by harvest, another 1.0 million ha/yr were converted to other land uses through gross deforestation, and 0.4 million ha/yr were degraded. Thus about 1.0% of North America's forests experienced some form of anthropogenic disturbance each year. However, due to harvest recovery, afforestation, and reforestation, the total forest area on the continent has been roughly stable during the decade. On average, about 110 m(3) of roundwood volume was extracted per hectare harvested across the continent. Patterns of extraction vary among the three countries, with U.S. and Canadian activity dominated by partial and clear-cut harvest, respectively, and activity in Mexico dominated by conversion (deforestation) for agriculture. Temporal trends in harvest and clearing may be affected by economic variables, technology, and forest policy decisions. While overall rates of extraction appear fairly stable in all three countries since the 1980s, harvest within the United States has shifted toward the southern United States and away from the Pacific Northwest. C1 [Masek, Jeffrey G.] NASA, Goddard Space Flight Ctr, Biospher Sci Branch, Greenbelt, MD 20771 USA. [Birdsey, Richard] US Forest Serv, No Global Change Res Program, Newtown Sq, PA 19073 USA. [Cohen, Warren B.] US Forest Serv, Pacific NW Res Stn, Corvallis, OR 97331 USA. [de Jong, Ben] El Colegio Frontera Sur, Tabasco 86280, Mexico. [Goward, Samuel] Univ Maryland, Dept Geog, College Pk, MD 20742 USA. [Healey, Sean] US Forest Serv, Rocky Mt Res Stn, Ogden, UT 84401 USA. [Houghton, R. A.] Woods Hole Res Ctr, Falmouth, MA 02543 USA. [Law, Beverly] Oregon State Univ, Coll Forestry, Corvallis, OR 97331 USA. [Leckie, Donald; Wulder, Michael A.] Canadian Forest Serv, Pacific Forestry Ctr, Victoria, BC V8Z 1M5, Canada. [Mildrexler, David] Univ Montana, Numer Terradynam Simulat Grp, Missoula, MT 59812 USA. [Smith, W. Brad] US Forest Serv, Arlington, VA 22209 USA. [Vargas, Rodrigo] Ctr Invest Cient & Educ Super Ensenada, Dept Biol Conservac, Ensenada 22830, Baja California, Mexico. RP Masek, JG (reprint author), NASA, Goddard Space Flight Ctr, Biospher Sci Branch, Greenbelt, MD 20771 USA. EM jeffrey.g.masek@nasa.gov RI Masek, Jeffrey/D-7673-2012; Trejo, Yesenia/D-9257-2012; Wulder, Michael/J-5597-2016; Vargas, Rodrigo/C-4720-2008; Law, Beverly/G-3882-2010 OI Wulder, Michael/0000-0002-6942-1896; Vargas, Rodrigo/0000-0001-6829-5333; Law, Beverly/0000-0002-1605-1203 FU NASA; U.S. Forest Service; Canadian Forest Service; ECOSUR; Office of Science (BER) U.S. Department of Energy [DE-FG02-04ER63911] FX This work was prepared as part of the North American Carbon Program (NACP) and CarbonNA activities, with support from the NASA Terrestrial Ecology Program, the U.S. Forest Service, the Canadian Forest Service, and ECOSUR. B.E.L. acknowledges the Office of Science (BER) U.S. Department of Energy (award DE-FG02-04ER63911) for support of AmeriFlux synthesis. NR 120 TC 33 Z9 33 U1 2 U2 41 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-BIOGEO JI J. Geophys. Res.-Biogeosci. PD APR 15 PY 2011 VL 116 AR G00K03 DI 10.1029/2010JG001471 PG 22 WC Environmental Sciences; Geosciences, Multidisciplinary SC Environmental Sciences & Ecology; Geology GA 751WL UT WOS:000289648300002 ER PT J AU Goodrich, JP Varner, RK Frolking, S Duncan, BN Crill, PM AF Goodrich, Jordan P. Varner, Ruth K. Frolking, Steve Duncan, Bryan N. Crill, Patrick M. TI High-frequency measurements of methane ebullition over a growing season at a temperate peatland site SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID ART. NO. GB1003; ATMOSPHERIC METHANE; NATURAL WETLANDS; VASCULAR PLANTS; WATER-TABLE; EXCHANGE; EMISSIONS; BIOGEOCHEMISTRY; DYNAMICS; CLIMATE AB Bubbles can contribute a significant fraction of methane emissions from wetlands; however the range of reported fractions is very large and accurate characterization of this pathway has proven difficult. Here we show that continuous automated flux chambers combined with an integrated cavity output spectroscopy (ICOS) instrument allow us to quantify both CH4 ebullition rate and magnitude. For a temperate poor fen in 2009, ebullition rate varied on hourly to seasonal time scales. A diel pattern in ebullition was identified with peak release occurring between 20:00 and 06:00 local time, though steady fluxes (i.e., those with a linear increase in chamber headspace CH4 concentration) did not exhibit diel variability. Seasonal mean ebullition rates peaked at 843.5 +/- 384.2 events m(-2) d(-1) during the summer, with a mean magnitude of 0.19 mg CH4 released in each event. Citation: Goodrich, J. P., R. K. Varner, S. Frolking, B. N. Duncan, and P. M. Crill (2011), High-frequency measurements of methane ebullition over a growing season at a temperate peatland site, Geophys. Res. Lett., 38, L07404, doi: 10.1029/2011GL046915. C1 [Goodrich, Jordan P.; Varner, Ruth K.; Frolking, Steve] Univ New Hampshire, Complex Syst Res Ctr, Durham, NH 03824 USA. [Duncan, Bryan N.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Crill, Patrick M.] Stockholm Univ, Dept Geol Sci, SE-10691 Stockholm, Sweden. RP Goodrich, JP (reprint author), Univ New Hampshire, Complex Syst Res Ctr, 8 Coll Rd, Durham, NH 03824 USA. EM jpd2@unh.edu RI Varner, Ruth/E-5371-2011; Duncan, Bryan/A-5962-2011; OI Varner, Ruth/0000-0002-3571-6629; Crill, Patrick/0000-0003-1110-3059 FU U.S. Department of Energy's Office of Science (BER) through the Northeastern Regional Center of the National Institute for Climate Change Research and the Research; University of New Hampshire; NASA GSFC FX This research was supported in part by the U.S. Department of Energy's Office of Science (BER) through the Northeastern Regional Center of the National Institute for Climate Change Research and the Research and Discover program by the University of New Hampshire and NASA GSFC. Special thanks to Eduardo Miranda and Michael Keller for their contributions to the success of this project. NR 25 TC 22 Z9 22 U1 3 U2 36 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 APR 15 PY 2011 VL 38 AR L07404 DI 10.1029/2011GL046915 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 751XA UT WOS:000289649800003 ER PT J AU Vernier, JP Thomason, LW Kar, J AF Vernier, J. -P. Thomason, L. W. Kar, J. TI CALIPSO detection of an Asian tropopause aerosol layer SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID TIBETAN PLATEAU; STRATOSPHERIC AEROSOL; MONSOON ANTICYCLONE; WATER-VAPOR; TROPOSPHERE; TRANSPORT; POLLUTION; SUMMER; SIMULATION; EXCHANGE AB The first four years of the CALIPSO lidar measurements have revealed the existence of an aerosol layer at the tropopause level associated with the Asian monsoon season in June, July and August. This Asian Tropopause Aerosol Layer (ATAL) extends geographically from Eastern Mediterranean (down to North Africa) to Western China (down to Thailand), and vertically from 13 to 18 km. The Scattering Ratio inferred from CALIPSO shows values between 1.10-1.15 on average with associated depolarization ratio of less than 5%. The Gaussian distribution of the points indicates that the mean value is statistically driven by an enhancement of the background aerosol level and not by episodic events such as a volcanic eruption or cloud contamination. Further satellite observations of aerosols and gases as well as field campaigns are urgently needed to characterize this layer, which is likely to be a significant source of non-volcanic aerosols for the global upper troposphere with a potential impact on its radiative and chemical balance. Citation: Vernier, J.-P., L. W. Thomason, and J. Kar (2011), CALIPSO detection of an Asian tropopause aerosol layer, Geophys. Res. Lett., 38, L07804, doi: 10.1029/2010GL046614. C1 [Vernier, J. -P.; Thomason, L. W.] NASA, Langley Res Ctr, Hampton, VA 23681 USA. [Kar, J.] Sci Syst & Applicat Inc, Hampton, VA 23666 USA. RP Vernier, JP (reprint author), NASA, Langley Res Ctr, Mail Stop 475, Hampton, VA 23681 USA. EM jean-paul.vernier@nasa.gov NR 30 TC 54 Z9 54 U1 5 U2 29 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 APR 15 PY 2011 VL 38 AR L07804 DI 10.1029/2010GL046614 PG 6 WC Geosciences, Multidisciplinary SC Geology GA 751XA UT WOS:000289649800001 ER PT J AU Jones, L Dolinsky, V Haykowsky, M Patterson, I Jones, L Allen, J Scott, J Rogan, K Khouri, M Hornsby, W Young, M Peppercorn, J Kimmick, G Dyck, J AF Jones, Lee Dolinsky, Vernon Haykowsky, Mark Patterson, Ian Jones, Lee Allen, Jason Scott, Jessica Rogan, Kyle Khouri, Michael Hornsby, Whitney Young, Martin Peppercorn, Jeffrey Kimmick, Gretchen Dyck, Jason TI Effects of aerobic training to improve cardiovascular function and prevent cardiac remodeling after cytotoxic therapy in early breast cancer SO CANCER RESEARCH LA English DT Meeting Abstract C1 [Jones, Lee; Jones, Lee; Allen, Jason; Khouri, Michael; Hornsby, Whitney; Peppercorn, Jeffrey; Kimmick, Gretchen] Duke Univ, Med Ctr, Durham, NC USA. [Dolinsky, Vernon; Haykowsky, Mark; Patterson, Ian; Rogan, Kyle; Dyck, Jason] Univ Alberta, Edmonton, AB, Canada. [Scott, Jessica] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Young, Martin] Univ Alabama Birmingham, Birmingham, AL USA. NR 0 TC 2 Z9 2 U1 0 U2 0 PU AMER ASSOC CANCER RESEARCH PI PHILADELPHIA PA 615 CHESTNUT ST, 17TH FLOOR, PHILADELPHIA, PA 19106-4404 USA SN 0008-5472 EI 1538-7445 J9 CANCER RES JI Cancer Res. PD APR 15 PY 2011 VL 71 SU 8 MA 5024 DI 10.1158/1538-7445.AM2011-5024 PG 2 WC Oncology SC Oncology GA V43SO UT WOS:000209701302473 ER PT J AU Wang, ML Hada, M Pluth, J Anderson, J O'Neill, P Cucinotta, F AF Wang, Minli Hada, Megumi Pluth, Janice Anderson, Jennifer O'Neill, Peter Cucinotta, Francis TI Ionizing radiation can enhance TGF beta induced EMT: Investigation of signatures of cross-talk with the ATM pathway SO CANCER RESEARCH LA English DT Meeting Abstract C1 [Wang, Minli; Hada, Megumi] USRA NASA, Houston, TX USA. [Pluth, Janice] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. [Anderson, Jennifer; O'Neill, Peter] Univ Oxford, Gray Inst Radiat Oncol & Biol, Oxford, England. [Cucinotta, Francis] NASA Johnson Space Ctr, Houston, TX USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU AMER ASSOC CANCER RESEARCH PI PHILADELPHIA PA 615 CHESTNUT ST, 17TH FLOOR, PHILADELPHIA, PA 19106-4404 USA SN 0008-5472 EI 1538-7445 J9 CANCER RES JI Cancer Res. PD APR 15 PY 2011 VL 71 SU 8 MA LB-50 DI 10.1158/1538-7445.AM2011-LB-50 PG 2 WC Oncology SC Oncology GA V43SO UT WOS:000209701303357 ER PT J AU Chen, J Zhu, XL Vogelmann, JE Gao, F Jin, SM AF Chen, Jin Zhu, Xiaolin Vogelmann, James E. Gao, Feng Jin, Suming TI A simple and effective method for filling gaps in Landsat ETM plus SLC-off images SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE Landsat ETM; SLC-off; Gap filling ID CONTERMINOUS UNITED-STATES; COVER; MODIS; CALIBRATION; SENSORS; TM AB The scan-line corrector (SIC) of the Landsat 7 Enhanced Thematic Mapper Plus (ETM+) sensor failed in 2003, resulting in about 22% of the pixels per scene not being scanned. The SLC failure has seriously limited the scientific applications of ETM+ data. While there have been a number of methods developed to fill in the data gaps, each method has shortcomings, especially for heterogeneous landscapes. Based on the assumption that the same-class neighboring pixels around the un-scanned pixels have similar spectral characteristics, and that these neighboring and un-scanned pixels exhibit similar patterns of spectral differences between dates, we developed a simple and effective method to interpolate the values of the pixels within the gaps. We refer to this method as the Neighborhood Similar Pixel Interpolator (NSPI). Simulated and actual SIC-off ETM+ images were used to assess the performance of the NSPI. Results indicate that NSPI can restore the value of un-scanned pixels very accurately, and that it works especially well in heterogeneous regions. In addition, it can work well even if there is a relatively long time interval or significant spectral changes between the input and target image. The filled images appear reasonably spatially continuous without obvious striping patterns. Supervised classification using the maximum likelihood algorithm was done on both gap-filled simulated SIC-off data and the original "gap free" data set, and it was found that classification results, including accuracies, were very comparable. This indicates that gap-filled products generated by NSPI will have relevance to the user community for various land cover applications. In addition, the simple principle and high computational efficiency of NSPI will enable processing large volumes of SIC-off ETM+ data. Published by Elsevier Inc. C1 [Vogelmann, James E.; Jin, Suming] USGS Earth Resources Observat & Sci EROS Ctr, ASRC Res & Technol Solut ARTS, Sioux Falls, SD 57198 USA. [Chen, Jin; Zhu, Xiaolin] Beijing Normal Univ, State Key Lab Earth Surface Proc & Resource Ecol, Beijing 100875, Peoples R China. [Zhu, Xiaolin] Ohio State Univ, Dept Geog, Columbus, OH 43210 USA. [Gao, Feng] NASA, Goddard Space Flight Ctr, Biospher Sci Branch, Greenbelt, MD 20771 USA. [Gao, Feng] Earth Resources Technol Inc, Laurel, MD 20707 USA. RP Vogelmann, JE (reprint author), USGS Earth Resources Observat & Sci EROS Ctr, ASRC Res & Technol Solut ARTS, Sioux Falls, SD 57198 USA. EM vogel@usgs.gov RI Chen, Jin/A-6417-2011; li, dongsheng/B-2285-2012; Zhu, Xiaolin/K-8175-2012; Chen, Jin/I-7666-2016; Chen, Lijun/Q-5012-2016; OI Chen, Jin/0000-0002-6497-4141; Zhu, Xiaolin/0000-0001-6967-786X; Vogelmann, James/0000-0002-0804-5823 FU Ministry of Science and Technology of China [2009AA12004]; USGS Landsat Science Team FX This study was supported by 863 project (2009AA12004) from Ministry of Science and Technology of China. We would also like to acknowledge the support from the USGS Landsat Science Team. We thank Tom Maiersperger, Kurtis Nelson and an anonymous reviewer for helpful comments on the manuscript. NR 20 TC 112 Z9 122 U1 8 U2 51 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 APR 15 PY 2011 VL 115 IS 4 BP 1053 EP 1064 DI 10.1016/j.rse.2010.12.010 PG 12 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA 728UE UT WOS:000287899200010 ER PT J AU Jones, MO Jones, LA Kimball, JS McDonald, KC AF Jones, Matthew O. Jones, Lucas A. Kimball, John S. McDonald, Kyle C. TI Satellite passive microwave remote sensing for monitoring global land surface phenology SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE AMSR-E; MODIS; Phenology; Optical depth; Vegetation index; NDVI; EVI; LAI; Growing season ID POLARIZATION DIFFERENCE INDEX; OPTICAL DEPTH RETRIEVAL; SOIL-MOISTURE; AMSR-E; VEGETATION INDEXES; SPRING PHENOLOGY; FOREST CANOPY; LEAF-AREA; EMISSION; BIOMASS AB Vegetation phenology characterizes seasonal life-cycle events that influence the carbon cycle and land-atmosphere water and energy exchange. We analyzed global phenology cycles over a six year record (2003-2008) using satellite passive microwave remote sensing based Vegetation Optical Depth (VOD) retrievals derived from daily time series brightness temperature (T-b) measurements from the Advanced Microwave Scanning Radiometer on EOS (AMSR-E) and other ancillary data inputs. The VOD parameter derives vegetation canopy attenuation at a given microwave frequency (18.7 GHz) and varies with canopy height, density, structure and water content. An error sensitivity analysis indicates that the retrieval algorithm can resolve the VOD seasonal cycle over a majority of global vegetated land areas. The VOD results corresponded favorably (p < 0.01) with vegetation indices (VIs) and leaf area index (lid) information from satellite optical-infrared (MODIS) remote sensing, and phenology cycles determined from a simple bioclimatic growing season index (GSI) for over 82% of the global domain. Lower biomass land cover classes (e.g. savannas) show the highest correlations (R=0.66), with reduced correspondence at higher biomass levels (0.03 < R < 0.51) and higher correlations for homogeneous land cover areas (0.41 < R < 0.83). The VOD results display a unique end-of-season signal relative to VI and LAI series, and may reflect microwave sensitivity to the timing of vegetation biomass depletion (e.g. leaf abscission) and associated changes in canopy water content (e.g. dormancy preparation). The VOD parameter is independent of and synergistic with optical-infrared remote sensing based vegetation metrics, and contributes to a more comprehensive view of land surface phenology. (C) 2011 Elsevier Inc. All rights reserved. C1 [Jones, Matthew O.; Jones, Lucas A.; Kimball, John S.] Univ Montana, Flathead Lake Biol Stn, Polson, MT 59860 USA. [Jones, Matthew O.; Jones, Lucas A.; Kimball, John S.] Univ Montana, Numer Terradynam Simulat Grp, Missoula, MT 59812 USA. [McDonald, Kyle C.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Jones, MO (reprint author), Univ Montana, Numer Terradynam Simulat Grp, CHCB 424,32 Campus Dr, Missoula, MT 59812 USA. EM matt.jones@ntsg.umt.edu FU NASA FX This study was carried out with funding from the NASA Terrestrial Ecology program. The AMSR-E Tb data and MODIS land cover in EASE grid format were provided by the National Snow and Ice Data Center (NSIDC). Other MODIS data were provided by the EOS data gateway, and NNR meteorological data were provided by the NOAA/OAR/ESRL PSD, Boulder, Colorado, USA (http://www.cdc.noaa.gov). The independent emissivity database was provided by Jean-Luc Moncet and Pan Liang of Atmospheric and Environmental Research, Inc., (http://www.aer.com/scienceResearch/mwrs/emis.html). The AMSR-E global VOD database and associated biophysical retrievals from this study are available through the UMT online data archives (ftp://ftp.ntsg.umt.edu/pub/data) and the NSIDC (http://nsidc.org/data/nsidc-0451.html). This work was performed at the University of Montana (UMT) and at the Jet Propulsion Laboratory, California Institute of Technology, under contract to the National Aeronautics and Space Administration. NR 59 TC 79 Z9 81 U1 5 U2 60 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 APR 15 PY 2011 VL 115 IS 4 BP 1102 EP 1114 DI 10.1016/j.rse.2010.12.015 PG 13 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA 728UE UT WOS:000287899200014 ER PT J AU Klima, RL Pieters, CM Boardman, JW Green, RO Head, JW Isaacson, PJ Mustard, JF Nettles, JW Petro, NE Staid, MI Sunshine, JM Taylor, LA Tompkins, S AF Klima, Rachel L. Pieters, Carle M. Boardman, Joseph W. Green, Robert O. Head, James W., III Isaacson, Peter J. Mustard, John F. Nettles, Jeff W. Petro, Noah E. Staid, Matthew I. Sunshine, Jessica M. Taylor, Lawrence A. Tompkins, Stefanie TI New insights into lunar petrology: Distribution and composition of prominent low-Ca pyroxene exposures as observed by the Moon Mineralogy Mapper (M-3) SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID MODIFIED GAUSSIAN MODEL; ORDER-DISORDER; MARE VOLCANISM; EVOLUTION; SPECTRA; ANORTHOSITES; SPECTROSCOPY; BULLIALDUS; HISTORY; SURFACE AB Lunar geochemical groups such as Mg suite, ferroan anorthosite, and alkali suite rocks are difficult to distinguish from orbit because they are defined by both modal mineralogy and elemental composition of their constituent minerals. While modal mineralogy can be modeled, only specific minerals or elements can be directly detected. At near-infrared (NIR) wavelengths, pyroxenes are among the most spectrally distinctive minerals, and their absorption bands are sensitive to structure and composition. Pyroxenes thus provide important clues to distinguish these geochemical groups and to understand lunar crustal evolution. Using Moon Mineralogy Mapper data, we search for lithologies dominated by strong low-calcium pyroxene (LCP) signatures. We compare the NIR absorptions of 20 LCPs to a suite of synthetic pyroxenes to determine which lunar pyroxenes appear magnesian enough to be candidate Mg suite norites. We detail three prominent regions of LCP (1) in South Pole-Aitken Basin (SPA), (2) south of Mare Frigoris, and (3) north of Mare Frigoris. The absorption band positions suggest that the LCPs north of Mare Frigoris and those in SPA are compositionally similar to one another and of similar to Mg50-75, implying that the mafic material excavated by the SPA impact was relatively iron-rich. Modified Gaussian modeling results suggest that the Apollo basin may have tapped different composition material than is exposed in much of SPA. The LCPs located in the highlands south of Mare Frigoris exhibit absorption bands at short wavelengths consistent with Mg > similar to 80. The coincidence of these Mg-rich LCPs with the thorium measured by Lunar Prospector make them good candidates for KREEP-related Mg suite pyroxenes. C1 [Klima, Rachel L.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20732 USA. [Pieters, Carle M.; Head, James W., III; Isaacson, Peter J.; Mustard, John F.; Nettles, Jeff W.] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA. [Boardman, Joseph W.] Analyt Imaging & Geophys LLC, Boulder, CO 80305 USA. [Green, Robert O.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Petro, Noah E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Staid, Matthew I.] Planetary Sci Inst, Tucson, AZ 85719 USA. [Sunshine, Jessica M.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Taylor, Lawrence A.] Univ Tennessee, Planetary Geosci Inst, Dept Earth & Planetary Sci, Knoxville, TN 37996 USA. [Tompkins, Stefanie] Def Adv Res Projects Agcy, Arlington, VA 22203 USA. RP Klima, RL (reprint author), Johns Hopkins Univ, Appl Phys Lab, 11100 Johns Hopkins Rd, Laurel, MD 20732 USA. EM rachel.klima@jhuapl.edu RI Klima, Rachel/H-9383-2012; Petro, Noah/F-5340-2013 OI Klima, Rachel/0000-0002-9151-6429; FU NASA [NNM05AB26C]; NASA LSI at the Applied Physics Lab [NNA09D-B31A] FX We are grateful to Joshua Cahill for a thorough and helpful review that greatly improved our manuscript. The M3 instrument was funded as a mission of opportunity through the NASA Discovery program. M3 science validation is supported through NASA contract NNM05AB26C. Partial funding for this analysis has also been provided through NASA LSI at the Applied Physics Lab under contract NNA09D-B31A. We are extremely grateful to ISRO for the opportunity to fly as a guest instrument on Chandrayaan-1. The views, opinions, and/or findings contained in this paper are those of the authors and should not be interpreted as representing the official views, either expressed or implied, of the Defense Advanced Research Projects Agency or the Department of Defense. NR 50 TC 25 Z9 25 U1 0 U2 5 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 APR 14 PY 2011 VL 116 AR E00G06 DI 10.1029/2010JE003719 PG 13 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 751VV UT WOS:000289646700002 ER PT J AU Verronen, PT Rodger, CJ Clilverd, MA Wang, SH AF Verronen, Pekka T. Rodger, Craig J. Clilverd, Mark A. Wang, Shuhui TI First evidence of mesospheric hydroxyl response to electron precipitation from the radiation belts SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID SOLAR PROTON EVENT; NORTHERN-HEMISPHERE; ATMOSPHERE; SATELLITE; NOX AB Utilizing observations from the Medium Energy Proton and Electron Detector (MEPED) on board the Polar Orbiting Environmental Satellite (POES) and the Microwave Limb Sounder (MLS) on board the Aura satellite, we demonstrate that there is a strong link between 100-300 keV loss cone electron count rates observed in the outer radiation belt and nighttime OH concentrations in the middle mesosphere at 71-78 km altitude. In theory, this can be expected because the ionization caused by energetic electron precipitation (EEP) leads to odd hydrogen (HOx) production through ionic reactions. However, this is the first time that OH production due to EEP has been observed. We consider daily mean data from 2 months, March 2005 and April 2006, which were selected because of (1) relatively high count rates of radiation belt electrons observed and (2) the absence of solar proton events that could mask the EEP effects. The results show that at 55-65 degrees magnetic latitude (equivalent to McIlwain L shells 3.0-5.6) increases in electron count rates by 2 orders of magnitude are accompanied by increases in nighttime OH concentration of 100%. There is a high correlation between MEPED and MLS data such that 56-87% of the OH variation can be explained by changes in EEP. Because the relation between MEPED count rate observations and the flux of electrons actually entering the atmosphere is not trivial, we discuss the possibility of using OH observations to obtain an estimate of EEP forcing that could be used in atmospheric modeling. C1 [Verronen, Pekka T.] Finnish Meteorol Inst, FI-00101 Helsinki, Finland. [Rodger, Craig J.] Univ Otago, Dept Phys, Dunedin, New Zealand. [Clilverd, Mark A.] British Antarctic Survey, Cambridge CB3 0ET, England. [Wang, Shuhui] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Verronen, PT (reprint author), Finnish Meteorol Inst, POB 503, FI-00101 Helsinki, Finland. EM pekka.verronen@fmi.fi; crodger@physics.otago.ac.nz; macl@bas.ac.uk; shuhui.wang@jpl.nasa.gov RI Verronen, Pekka/G-6658-2014; Rodger, Craig/A-1501-2011 OI Verronen, Pekka/0000-0002-3479-9071; Rodger, Craig/0000-0002-6770-2707 FU Academy of Finland [136225/SPOC, 123275/THERMES]; National Aeronautics and Space Administration FX P. T. V. would like to thank Marko Laine for valuable discussions. The work of P. T. V. was supported by the Academy of Finland through projects 136225/SPOC (Significance of Energetic Electron Precipitation to Odd Hydrogen, Ozone, and Climate) and 123275/THERMES (Thermosphere and Mesosphere Affecting the Stratosphere). Research at the Jet Propulsion Laboratory, California Institute of Technology, is performed under contract with the National Aeronautics and Space Administration. POES data were provided by NOAA National Geophysical Data Center. MLS/Aura data were provided by the NASA Goddard Earth Sciences Data and Information Service Center (GES DISC). NR 27 TC 35 Z9 35 U1 0 U2 5 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 APR 14 PY 2011 VL 116 AR D07307 DI 10.1029/2010JD014965 PG 12 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 751WI UT WOS:000289648000003 ER PT J AU Hale, AS Tamppari, LK Bass, DS Smith, MD AF Hale, A. Snyder Tamppari, L. K. Bass, D. S. Smith, M. D. TI Martian water ice clouds: A view from Mars Global Surveyor Thermal Emission Spectrometer SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID INTERANNUAL VARIABILITY; MGS TES; VIKING; APHELION; ATMOSPHERE; BEHAVIOR; CLIMATE; MISSION; ALBEDO; MAPPER AB We have used the Mars Global Surveyor Thermal Emission Spectrometer (MGS TES) data to map water ice clouds in the Martian atmosphere in the latitude range -60 to +60 over a period of three Martian years. We have used the same method we have previously used on Viking Infrared Thermal Mapper data in order to allow direct comparison of the cloud behavior in the Viking and MGS eras and confirmed the validity of this method by comparing it to MGS TES standard retrievals. We note that the large-scale behavior of water ice clouds is remarkably consistent, both between the Viking and the MGS eras as well as between years observed by MGS. We also compare our results to water ice absorption-only optical depths derived from TES data and show that correlation is best for type 2 water ice clouds. C1 [Hale, A. Snyder; Tamppari, L. K.; Bass, D. S.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Smith, M. D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Hale, AS (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM amy.s.hale@jpl.nasa.gov RI Smith, Michael/C-8875-2012 FU NASA FX The authors would like to thank Charles Thompson for invaluable help in developing our IDL code and David Paige for the surface model and access to the source code used to generate it. The authors would like to thank Alexey Pankine for assistance with estimating the range of appropriate cloud temperatures within the TES data set; they would also like to thank Terry Z. Martin and Deborah Bass for many helpful discussions and Ashwin Vasavada for his comments on a draft version of this paper. This work was carried out at JPL/CIT under a grant from the NASA Mars Data Analysis Program. We would also like to thank Sasha Rodin and an anonymous reviewer for their helpful comments and critique, which have greatly improved this manuscript. NR 29 TC 1 Z9 1 U1 0 U2 4 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9097 EI 2169-9100 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD APR 13 PY 2011 VL 116 AR E04004 DI 10.1029/2009JE003449 PG 14 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 751VT UT WOS:000289646500001 ER PT J AU Heavens, NG Richardson, MI Kleinbohl, A Kass, DM McCleese, DJ Abdou, W Benson, JL Schofield, JT Shirley, JH Wolkenberg, PM AF Heavens, N. G. Richardson, M. I. Kleinboehl, A. Kass, D. M. McCleese, D. J. Abdou, W. Benson, J. L. Schofield, J. T. Shirley, J. H. Wolkenberg, P. M. TI The vertical distribution of dust in the Martian atmosphere during northern spring and summer: Observations by the Mars Climate Sounder and analysis of zonal average vertical dust profiles SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID GENERAL-CIRCULATION MODEL; WATER ICE CLOUDS; MIDDLE ATMOSPHERE; ORBITER CAMERA; INTERANNUAL VARIABILITY; INFRARED MEASUREMENTS; THERMAL STRUCTURE; POLAR WARMINGS; PARTICLE SIZES; MGS TES AB The vertical distribution of dust in Mars's atmosphere is a critical and poorly known input in atmospheric physical and chemical models and a source of insight into the lifting and transport of dust and general vertical mixing in the atmosphere. We investigate vertical profiles of dust opacity retrieved from limb observations by Mars Climate Sounder during the relatively dust-clear Martian northern summer of 2006-2007 (L-s = 111 degrees-177 degrees of Mars year (MY) 28) and Martian northern spring and summer of 2007-2008 (L-s = 0 degrees-180 degrees of MY 29). To represent local maxima in inferred mass mixing ratio in these profiles, we develop an empirical alternative to the classic "Conrath profile" for representing the vertical distribution of dust in the Martian atmosphere. We then assess the magnitude and variability of atmospheric dust loading, the depth of dust penetration during these seasons, and the impact of the observed vertical dust distribution on the radiative forcing of the circulation. During most of northern spring and summer, the dust mass mixing ratio in the tropics has a maximum at 15-25 km above the local surface (the high-altitude tropical dust maximum (HATDM)). The HATDM appears to have increased significantly in magnitude and altitude during middle to late northern summer of MY 29. The HATDM gradually decayed during late summer of MY 28. Interannual variability in the dust distribution during middle to late northern summer may be connected with known interannual variability in tropical dust storm activity. C1 [Richardson, M. I.] Ashima Res, Pasadena, CA 91106 USA. [Heavens, N. G.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91109 USA. [Kleinboehl, A.; Kass, D. M.; McCleese, D. J.; Abdou, W.; Benson, J. L.; Schofield, J. T.; Shirley, J. H.; Wolkenberg, P. M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Heavens, NG (reprint author), Cornell Univ, Dept Earth & Atmospher Sci, 1118 Bradfield Hall, Ithaca, NY 14853 USA. EM heavens@cornell.edu OI Heavens, Nicholas/0000-0001-7654-503X FU National Aeronautics and Space Administration FX We thank Aymeric Spiga and an anonymous reviewer for extremely thorough and helpful reviews. The authors also would like to thank Tim McConnochie and Todd Clancy for useful discussions. This work was funded by and performed in part at the Jet Propulsion Laboratory, California Institute of Technology under contract with the National Aeronautics and Space Administration as part of the Mars Reconnaissance Orbiter project. NR 64 TC 32 Z9 32 U1 0 U2 15 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9097 EI 2169-9100 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD APR 13 PY 2011 VL 116 AR E04003 DI 10.1029/2010JE003691 PG 23 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 751VT UT WOS:000289646500002 ER PT J AU Hwang, KJ Goldstein, ML Lee, E Pickett, JS AF Hwang, K. -J. Goldstein, M. L. Lee, E. Pickett, J. S. TI Cluster observations of multiple dipolarization fronts SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID PROTON-BEAM GENERATION; WHISTLER WAVES; MAGNETIC RECONNECTION; CURRENT DISRUPTION; EARTH; MAGNETOSPHERE; INSTABILITY; MOTION; FLOWS; SHEET AB We present Cluster observations of a series of dipolarization fronts (DF 1 to 6) at the central current sheet in Earth's magnetotail. The velocities of fast earthward flow following behind each DF 1-3 are comparable to the Alfven velocity, indicating that the flow bursts might have been generated by bursty reconnection that occurred tailward of the spacecraft. Based on multispacecraft timing analysis, DF normals are found to propagate mainly earthward at 160-335 km/s with a thickness of 900-1500 km, which corresponds to the ion inertial length or gyroradius scale. Each DF is followed by significant fluctuations in the x and y components of the magnetic field whose peaks are found 1-2 min after the DF passage. These (B-x, B-y) fluctuations propagate dawnward (mainly) and earthward. Strongly enhanced field-aligned beams are observed coincidently with (B-x, B-y) fluctuations, while an enhancement of cross-tail currents is associated with the DFs. From the observed pressure imbalance and flux tube entropy changes between the two regions separated by the DF, we speculate that interchange instability destabilizes the DFs and causes the deformation of the midtail magnetic topology. This process generates significant field-aligned currents and might power the auroral brightening in the ionosphere. However, this event is associated with neither the main substorm auroral breakup nor the poleward expansion, which might indicate that the observed multiple DFs have been dissipated before they reach the inner plasma sheet boundary. C1 [Hwang, K. -J.; Goldstein, M. L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Lee, E.] Kyung Hee Univ, Dept Astron & Space Sci, Yongin 446701, Kyung Ki, South Korea. [Pickett, J. S.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. [Hwang, K. -J.] Univ Maryland Baltimore Cty, Goddard Earth & Sci Technol Ctr, Baltimore, MD 21228 USA. RP Hwang, KJ (reprint author), NASA, Goddard Space Flight Ctr, Code 661, Greenbelt, MD 20771 USA. EM kyoung-joo.hwang@nasa.gov; melvyn.l.goldstein@nasa.gov; eslee@khu.ac.kr; pickett@uiowa.edu RI Goldstein, Melvyn/B-1724-2008; Lee, Ensang/E-2356-2013; NASA MMS, Science Team/J-5393-2013 OI NASA MMS, Science Team/0000-0002-9504-5214 FU NASA's MMS/IDS and Cluster missions at the Goddard Space Flight Center; UMBC/GEST FX This study was supported by NASA's MMS/IDS and Cluster missions at the Goddard Space Flight Center and by UMBC/GEST. We acknowledges all Cluster instrument teams, including PEACE, CIS, FGM, EFW, RAPID, WHISPER, and WIDEBAND staffs and the Cluster Active Archive (http://caa.estec.esa.int/caa). The authors acknowledge the referee correcting the estimation of the foot point of the Cluster location using the T96 model and both referee advising in using the interchange-instability criterion. K.-J. Hwang thanks Miho Saito for helpful discussions. NR 57 TC 36 Z9 36 U1 0 U2 11 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 APR 13 PY 2011 VL 116 AR A00I32 DI 10.1029/2010JA015742 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 751VG UT WOS:000289645200002 ER PT J AU Lau, KM Kim, KM AF Lau, K. M. Kim, K. M. TI Comment on '"Elevated heat pump' hypothesis for the aerosol-monsoon hydroclimate link: 'Grounded' in observations?" by S. Nigam and M. Bollasina SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Editorial Material ID BLACK CARBON AEROSOLS; ASIAN SUMMER MONSOON; INDIAN MONSOON C1 [Lau, K. M.] NASA, Atmospheres Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Kim, K. M.] Univ Maryland Baltimore Cty, Goddard Earth Sci Technol Ctr, Baltimore, MD 21250 USA. RP Lau, KM (reprint author), NASA, Atmospheres Lab, Goddard Space Flight Ctr, Code 613, Greenbelt, MD 20771 USA. EM william.k.lau@nasa.gov RI Kim, Kyu-Myong/G-5398-2014; Lau, William /E-1510-2012 OI Lau, William /0000-0002-3587-3691 NR 11 TC 16 Z9 17 U1 1 U2 4 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 APR 12 PY 2011 VL 116 AR D07203 DI 10.1029/2010JD014800 PG 4 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 751WG UT WOS:000289647800001 ER PT J AU Jenet, FA Armstrong, JW Tinto, M AF Jenet, Fredrick A. Armstrong, J. W. Tinto, Massimo TI Pulsar timing sensitivity to very-low-frequency gravitational waves SO PHYSICAL REVIEW D LA English DT Article ID BLACK-HOLE BINARIES; UPPER LIMITS; RADIATION; COALESCENCE; PRECISION; MODEL AB We compute the sensitivity, constrained by instrumental, propagation, and other fundamental noises, of pulsar timing to very-low-frequency gravitational waves (GWs). Reaching predicted GW signal strengths will require suppression of time-of-arrival fluctuations caused by interstellar plasma turbulence and a reduction of white rms timing noise to less than or similar to 100 ns. Assuming negligible intrinsic pulsar rotational noise, perfect time transfer from time standard to observatory, and stable pulse profiles, the resulting single-pulsar signal-to-noise ratio 1 sensitivity is limited by terrestrial time standards at h(rms) similar to 2 x 10(-16) [f/(1 cycle/year)] -1/2 for f < 3 x 10(-8) Hz, where f is the Fourier frequency and a bandwidth of 1 cycle/(10 years) is assumed. Since this sensitivity is comparable to predicted GW signal levels, a reliable detection will require substantial signal-to-noise ratio improvement via pulsar timing array. C1 [Jenet, Fredrick A.] Univ Texas Brownsville, Ctr Gravitat Wave Astron, Brownsville, TX 78520 USA. [Armstrong, J. W.; Tinto, Massimo] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Jenet, FA (reprint author), Univ Texas Brownsville, Ctr Gravitat Wave Astron, Brownsville, TX 78520 USA. EM merlyn@phys.utb.edu; john.w.armstrong@jpl.nasa.gov; massimo.tinto@jpl.nasa.gov FU U.S. National Science Foundation (AST) [0545837]; National Aeronautics and Space Administration; internal Research and Technology Development program FX We thank F. B. Estabrook for discussions on gravitational wave sensitivity and W. A. Coles for comments on an early draft of this paper. F. A. J.'s contribution was funded by a grant from the U.S. National Science Foundation (AST #0545837). For J. W. A. and M. T., this research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration and funded through the internal Research and Technology Development program. NR 32 TC 8 Z9 8 U1 0 U2 1 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1550-7998 EI 1550-2368 J9 PHYS REV D JI Phys. Rev. D PD APR 11 PY 2011 VL 83 IS 8 AR 081301 DI 10.1103/PhysRevD.83.081301 PG 4 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 747WZ UT WOS:000289353200001 ER PT J AU Garcia, J Ramirez, JM Kallman, TR Witthoeft, M Bautista, MA Mendoza, C Palmeri, P Quinet, P AF Garcia, J. Ramirez, J. M. Kallman, T. R. Witthoeft, M. Bautista, M. A. Mendoza, C. Palmeri, P. Quinet, P. TI MODELING THE OXYGEN K ABSORPTION IN THE INTERSTELLAR MEDIUM: AN XMM-NEWTON VIEW OF Sco X-1 SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE atomic data; atomic processes; dust, extinction; line: formation; X-rays: general ID X-RAY SPECTROSCOPY; FINE-STRUCTURE; ATOMIC OXYGEN; SCORPIUS X-1; EDGE; IRON; PHOTOABSORPTION; MCG-6-30-15; SPECTRUM; DUST AB We investigate the X-ray absorption structure of oxygen in the interstellar medium by analyzing XMM-Newton observations of the low-mass X-ray binary Sco X-1. Simple models based on the O I atomic photoabsorption cross section from different sources are used to fit the data and evaluate the impact of the atomic data on the interpretation of the observations. We show that relatively small differences in the atomic calculations can yield spurious results, and that the most complete and accurate set of atomic cross sections successfully reproduce the observed data in the 21.0-24.5 angstrom wavelength region of the spectrum. Our fits indicate that the absorption is mainly due to neutral gas with an ionization parameter of xi = 10(-4) erg cm s(-1) and an oxygen column density of N-O approximate to (8-10) x 10(17) cm(-2). The models are able to reproduce both the K edge and the K alpha absorption line from O I which are the two main features in this region. We find no conclusive evidence for absorption by anything other than atomic oxygen. C1 [Garcia, J.; Bautista, M. A.] Western Michigan Univ, Dept Phys, Kalamazoo, MI 49008 USA. [Garcia, J.; Kallman, T. R.; Witthoeft, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Ramirez, J. M.] Inst Astrophys, D-14482 Potsdam, Germany. [Mendoza, C.] IVIC, Ctr Fis, Caracas 1020, Venezuela. [Palmeri, P.; Quinet, P.] Univ Mons, B-7000 Mons, Belgium. [Quinet, P.] Univ Liege, IPNAS, B-4000 Liege, Belgium. RP Garcia, J (reprint author), Western Michigan Univ, Dept Phys, Kalamazoo, MI 49008 USA. EM javier.garcia@wmich.edu; jramirez@aip.de; timothy.r.kallman@nasa.gov; michael.c.witthoeft@nasa.gov; manuel.bautista@wmich.edu; claudio@ivic.gob.ve; palmeri@umh.ac.be; quinet@umh.ac.be FU NASA [05-ATP05-18] FX We thank Tom Gorczyca for providing the MCK98 and GMC00 calculations. This work was supported by a grant from the NASA astrophysics theory program 05-ATP05-18. This research has made extensive use of the NASA Astrophysics Data System. NR 32 TC 11 Z9 11 U1 1 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 APR 10 PY 2011 VL 731 IS 1 AR L15 DI 10.1088/2041-8205/731/1/L15 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 797KQ UT WOS:000293126600015 ER PT J AU Miller, JM Maitra, D Cackett, EM Bhattacharyya, S Strohmayer, TE AF Miller, Jon M. Maitra, Dipankar Cackett, Edward M. Bhattacharyya, Sudip Strohmayer, Tod E. TI A FAST X-RAY DISK WIND IN THE TRANSIENT PULSAR IGR J17480-2446 IN TERZAN 5 SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE accretion, accretion disks; globular clusters: individual (Terzan 5); pulsars: individual (IGR J17480-2446); stars: neutron ID ACCRETION DISKS; NEUTRON-STAR; MILLISECOND PULSAR; SAX J1808.4-3658; CHANDRA; LINES; SPECTROSCOPY; BINARIES; DISCOVERY; EMISSION AB Accretion disk winds are revealed in Chandra gratings spectra of black holes. The winds are hot and highly ionized (typically composed of He-like and H-like charge states) and show modest blueshifts. Similar line spectra are sometimes seen in "dipping" low-mass X-ray binaries (LMXBs), which are likely viewed edge-on; however, that absorption is tied to structures in the outer disk, and blueshifts are not typically observed. Here, we report the detection of blueshifted He-like Fe XXV (3100 +/- 400 km s(-1)) and H-like Fe XXVI (1000 +/- 200 km s(-1)) absorption lines in a Chandra/HETG spectrum of the transient pulsar and LMXB IGR J17480-2446 in Terzan 5. These features indicate a disk wind with at least superficial similarities to those observed in stellar-mass black holes. The wind does not vary strongly with numerous weak X-ray bursts or flares. A broad Fe K emission line is detected in the spectrum, and fits with different line models suggest that the inner accretion disk in this system may be truncated. If the stellar magnetic field truncates the disk, a field strength of B = (0.7-4.0) x 10(9) G is implied, which is in line with estimates based on X-ray timing techniques. We discuss our findings in the context of accretion flows onto neutron stars and stellar-mass black holes. C1 [Miller, Jon M.; Maitra, Dipankar] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Cackett, Edward M.] Univ Cambridge, Inst Astron, Cambridge CB3 OHA, England. [Bhattacharyya, Sudip] Tata Inst Fundamental Res, Dept Astron & Astrophys, Mumbai 400005, Maharashtra, India. [Strohmayer, Tod E.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. RP Miller, JM (reprint author), Univ Michigan, Dept Astron, 500 Church St, Ann Arbor, MI 48109 USA. EM jonmm@umich.edu FU Chandra Guest Observer program FX We thank Harvey Tananbaum, Belinda Wilkes, and Andrea Prestwich for executing this observation. We acknowledge David Pooley and Jeroen Homan for helping to coordinate different observations of IGR J17480-2446. We thank Tim Kallman and Cole Miller for helpful discussions. Finally, we thank the anonymous referee for a helpful review. J.M.M. acknowledges support from the Chandra Guest Observer program. NR 40 TC 35 Z9 35 U1 0 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD APR 10 PY 2011 VL 731 IS 1 AR L7 DI 10.1088/2041-8205/731/1/L7 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 797KQ UT WOS:000293126600007 ER PT J AU Moore, RL Sterling, AC Cirtain, JW Falconer, DA AF Moore, Ronald L. Sterling, Alphonse C. Cirtain, Jonathan W. Falconer, David A. TI SOLAR X-RAY JETS, TYPE-II SPICULES, GRANULE-SIZE EMERGING BIPOLES, AND THE GENESIS OF THE HELIOSPHERE SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE Sun: activity; Sun: chromosphere; Sun: corona; Sun: heliosphere; Sun: magnetic topology; Sun: surface magnetism ID HORIZONTAL MAGNETIC-FIELDS; QUIET-SUN INTERNETWORK; CORONAL JETS; ENERGY-FLOW; CHROMOSPHERE; TELESCOPE; MODEL; NETWORK; REGIONS; WAVES AB From Hinode observations of solar X-ray jets, Type-II spicules, and granule-size emerging bipolar magnetic fields in quiet regions and coronal holes, we advocate a scenario for powering coronal heating and the solar wind. In this scenario, Type-II spicules and Alfven waves are generated by the granule-size emerging bipoles (EBs) in the manner of the generation of X-ray jets by larger magnetic bipoles. From observations and this scenario, we estimate that Type-II spicules and their co-generated Alfven waves carry into the corona an area-average flux of mechanical energy of similar to 7 x 10(5) erg cm(-2) s(-1). This is enough to power the corona and solar wind in quiet regions and coronal holes, and therefore indicates that the granule-size EBs are the main engines that generate and sustain the entire heliosphere. C1 [Moore, Ronald L.; Sterling, Alphonse C.; Cirtain, Jonathan W.; Falconer, David A.] NASA, George C Marshall Space Flight Ctr, Space Sci Off, VP62, Huntsville, AL 35812 USA. [Falconer, David A.] Univ Alabama, Dept Phys, Huntsville, AL 35899 USA. [Falconer, David A.] Univ Alabama, Ctr Space Plasma & Aeron Res, Huntsville, AL 35899 USA. RP Moore, RL (reprint author), NASA, George C Marshall Space Flight Ctr, Space Sci Off, VP62, Huntsville, AL 35812 USA. EM ron.moore@nasa.gov FU NASA's Science Mission Directorate FX This work was funded by NASA's Science Mission Directorate through the Heliophysics Guest Investigators Program, the Hinode Project, and the Living With a Star Targeted Research and Technology Program. NR 43 TC 31 Z9 31 U1 0 U2 9 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 APR 10 PY 2011 VL 731 IS 1 AR L18 DI 10.1088/2041-8205/731/1/L18 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 797KQ UT WOS:000293126600018 ER PT J AU Sterling, AC Moore, RL Freeland, SL AF Sterling, Alphonse C. Moore, Ronald L. Freeland, Samuel L. TI INSIGHTS INTO FILAMENT ERUPTION ONSET FROM SOLAR DYNAMICS OBSERVATORY OBSERVATIONS SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE Sun: activity; Sun: filaments, prominences; Sun: flares; Sun: UV radiation ID CORONAL MASS EJECTIONS; UNSTABLE FLUX ROPES; EMERGING FLUX; MAGNETIC-FLUX; SLOW-RISE; FLARES; INITIATION; HINODE; RECONNECTION; CANCELLATION AB We examine the buildup to and onset of an active region filament confined eruption of 2010 May 12, using EUV imaging data from the Solar Dynamics Observatory (SDO) Atmospheric Imaging Array and line-of-sight magnetic data from the SDO Helioseismic and Magnetic Imager. Over the hour preceding eruption the filament undergoes a slow rise averaging similar to 3 km s(-1), with a step-like trajectory. Accompanying a final rise step similar to 20 minutes prior to eruption is a transient preflare brightening, occurring on loops rooted near the site where magnetic field had canceled over the previous 20 hr. Flow-type motions of the filament are relatively smooth with speeds similar to 50 km s(-1) prior to the preflare brightening and appear more helical, with speeds similar to 50-100 km s(-1), after that brightening. After a final plateau in the filament's rise, its rapid eruption begins, and concurrently an outer shell "cocoon" of the filament material increases in emission in hot EUV lines, consistent with heating in a newly formed magnetic flux rope. The main flare brightenings start similar to 5 minutes after eruption onset. The main flare arcade begins between the legs of an envelope-arcade loop that is nearly orthogonal to the filament, suggesting that the flare results from reconnection among the legs of that loop. This progress of events is broadly consistent with flux cancellation leading to formation of a helical flux rope that subsequently erupts due to onset of a magnetic instability and/or runaway tether cutting. C1 [Sterling, Alphonse C.; Moore, Ronald L.] NASA, George C Marshall Space Flight Ctr, Space Sci Off, VP62, Huntsville, AL 35812 USA. [Freeland, Samuel L.] Lockheed Martin Solar & Astrophys Lab, Dept ADBS, Palo Alto, CA 94304 USA. RP Sterling, AC (reprint author), JAXA, Inst Space & Astronaut Sci, Hinode Grp, 3-1-1 Yoshinodai, Sagamihara, Kanagawa 2298510, Japan. EM alphonse.sterling@nasa.gov; ron.moore@nasa.gov FU NASA's Office of Space Science FX We thank G. L. Slater for valuable assistance with the AIA data. SDO is a mission for NASA's Living With a Star (LWS) Program. A. C. S. and R. L. M. were supported by funding from NASA's Office of Space Science through the Solar Physics Supporting Research and Technology Program, the Sun-Earth Connection Guest Investigator Program, and the Living With a Star Targeted Research & Technology Program. NR 50 TC 28 Z9 28 U1 1 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD APR 10 PY 2011 VL 731 IS 1 AR L3 DI 10.1088/2041-8205/731/1/L3 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 797KQ UT WOS:000293126600003 ER PT J AU Abdo, AA Ackermann, M Ajello, M Baldini, L Ballet, J Barbiellini, G Bastieri, D Bechtol, K Bellazzini, R Berenji, B Blandford, RD Bonamente, E Borgland, AW Bouvier, A Bregeon, J Brez, A Brigida, M Bruel, P Buehler, R Buson, S Caliandro, GA Cameron, RA Caraveo, PA Carrigan, S Casandjian, JM Cavazzuti, E Cecchi, C Celik, O Charles, E Chekhtman, A Cheung, CC Chiang, J Ciprini, S Claus, R Cohen-Tanugi, J Conrad, J Costamante, L Cutini, S Davis, DS Dermer, CD de Palma, F Digel, SW Silva, EDE Drell, PS Dubois, R Dumora, D Favuzzi, C Fegan, SJ Fortin, P Frailis, M Fuhrmann, L Fukazawa, Y Funk, S Fusco, P Gargano, F Gasparrini, D Gehrels, N Germani, S Giglietto, N Giommi, P Giordano, F Giroletti, M Glanzman, T Godfrey, G Grenier, IA Grove, JE Guillemot, L Guiriec, S Hadasch, D Hayashida, M Hays, E Horan, D Hughes, RE Itoh, R Johannesson, G Johnson, AS Johnson, TJ Johnson, WN Kamae, T Katagiri, H Kataoka, J Knodlseder, J Kuss, M Lande, J Latronico, L Lee, SH Longo, F Loparco, F Lott, B Lovellette, MN Lubrano, P Makeev, A Mazziotta, MN McEnery, JE Mehault, J Michelson, PF Mizuno, T Moiseev, AA Monte, C Monzani, ME Morselli, A Moskalenko, IV Murgia, S Nakamori, T Naumann-Godo, M Nestoras, I Nolan, PL Norris, JP Nuss, E Ohsugi, T Okumura, A Omodei, N Orlando, E Ormes, JF Ozaki, M Paneque, D Panetta, JH Parent, D Pelassa, V Pepe, M Pesce-Rollins, M Piron, F Porter, TA Raino, S Rando, R Razzano, M Reimer, A Reimer, O Reyes, LC Ripken, J Ritz, S Romani, RW Roth, M Sadrozinski, HFW Sanchez, D Sander, A Scargle, JD Sgro, C Shaw, MS Smith, PD Spandre, G Spinelli, P Strickman, MS Suson, DJ Takahashi, H Tanaka, T Thayer, JB Thayer, JG Thompson, DJ Tibaldo, L Torres, DF Tosti, G Tramacere, A Usher, TL Vandenbroucke, J Vasileiou, V Vilchez, N Vitale, V Waite, AP Wang, P Winer, BL Wood, KS Yang, Z Ylinen, T Ziegler, M Acciari, VA Aliu, E Arlen, T Aune, T Beilicke, M Benbow, W Bottcher, M Boltuch, D Bradbury, SM Buckley, JH Bugaev, V Byrum, K Cannon, A Cesarini, A Christiansen, JL Ciupik, L Cui, W Perez, ID Dickherber, R Errando, M Falcone, A Finley, JP Finnegan, G Fortson, L Furniss, A Galante, N Gall, D Gillanders, GH Godambe, S Grube, J Guenette, R Gyuk, G Hanna, D Holder, J Hui, CM Humensky, TB Imran, A Kaaret, P Karlsson, N Kertzman, M Kieda, D Konopelko, A Krawczynski, H Krennrich, F Lang, MJ LeBohec, S Maier, G McArthur, S McCann, A McCutcheon, M Moriarty, P Mukherjee, R Ong, RA Otte, AN Pandel, D Perkins, JS Pichel, A Pohl, M Quinn, J Ragan, K Reynolds, PT Roache, E Rose, HJ Schroedter, M Sembroski, GH Senturk, GD Smith, AW Steele, D Swordy, SP Tesic, G Theiling, M Thibadeau, S Varlotta, A Vassiliev, VV Vincent, S Wakely, SP Ward, JE Weekes, TC Weinstein, A Weisgarber, T Williams, DA Wissel, S Wood, M Villata, M Raiteri, CM Gurwell, MA Larionov, VM Kurtanidze, OM Aller, MF Lahteenmaki, A Chen, WP Berduygin, A Agudo, I Aller, HD Arkharov, AA Bach, U Bachev, R Beltrame, P Benitez, E Buemi, CS Dashti, J Calcidese, P Capezzali, D Carosati, D Da Rio, D Di Paola, A Diltz, C Dolci, M Dultzin, D Forne, E Gomez, JL Hagen-Thorn, VA Halkola, A Heidt, J Hiriart, D Hovatta, T Hsiao, HY Jorstad, SG Kimeridze, GN Konstantinova, TS Kopatskaya, EN Koptelova, E Leto, P Ligustri, R Lindfors, E Lopez, JM Marscher, AP Mommert, M Mujica, R Nikolashvili, MG Nilsson, K Palma, N Pasanen, M Roca-Sogorb, M Ros, JA Roustazadeh, P Sadun, AC Saino, J Sigua, LA Sillanaa, A Sorcia, M Takalo, LO Tornikoski, M Trigilio, C Turchetti, R Umana, G Belloni, T Blake, CH Bloom, JS Angelakis, E Fumagalli, M Hauser, M Prochaska, JX Riquelme, D Sievers, A Starr, DL Tagliaferri, G Ungerechts, H Wagner, S Zensus, JA AF Abdo, A. A. Ackermann, M. Ajello, M. Baldini, L. Ballet, J. Barbiellini, G. Bastieri, D. Bechtol, K. Bellazzini, R. Berenji, B. Blandford, R. D. Bonamente, E. Borgland, A. W. Bouvier, A. Bregeon, J. Brez, A. Brigida, M. Bruel, P. Buehler, R. Buson, S. Caliandro, G. A. Cameron, R. A. Caraveo, P. A. Carrigan, S. Casandjian, J. M. Cavazzuti, E. Cecchi, C. Celik, Oe. Charles, E. Chekhtman, A. Cheung, C. C. Chiang, J. Ciprini, S. Claus, R. Cohen-Tanugi, J. Conrad, J. Costamante, L. Cutini, S. Davis, D. S. Dermer, C. D. de Palma, F. Digel, S. W. do Couto e Silva, E. Drell, P. S. Dubois, R. Dumora, D. Favuzzi, C. Fegan, S. J. Fortin, P. Frailis, M. Fuhrmann, L. Fukazawa, Y. Funk, S. Fusco, P. Gargano, F. Gasparrini, D. Gehrels, N. Germani, S. Giglietto, N. Giommi, P. Giordano, F. Giroletti, M. Glanzman, T. Godfrey, G. Grenier, I. A. Grove, J. E. Guillemot, L. Guiriec, S. Hadasch, D. Hayashida, M. Hays, E. Horan, D. Hughes, R. E. Itoh, R. Johannesson, G. Johnson, A. S. Johnson, T. J. Johnson, W. N. Kamae, T. Katagiri, H. Kataoka, J. Knoedlseder, J. Kuss, M. Lande, J. Latronico, L. Lee, S. -H. Longo, F. Loparco, F. Lott, B. Lovellette, M. N. Lubrano, P. Makeev, A. Mazziotta, M. N. McEnery, J. E. Mehault, J. Michelson, P. F. Mizuno, T. Moiseev, A. A. Monte, C. Monzani, M. E. Morselli, A. Moskalenko, I. V. Murgia, S. Nakamori, T. Naumann-Godo, M. Nestoras, I. 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. Pelassa, V. Pepe, M. Pesce-Rollins, M. Piron, F. Porter, T. A. Raino, S. Rando, R. Razzano, M. Reimer, A. Reimer, O. Reyes, L. C. Ripken, J. Ritz, S. Romani, R. W. Roth, M. Sadrozinski, H. F. -W. Sanchez, D. Sander, A. Scargle, J. D. Sgro, C. Shaw, M. S. Smith, P. D. Spandre, G. Spinelli, P. Strickman, M. S. Suson, D. J. Takahashi, H. Tanaka, T. Thayer, J. B. Thayer, J. G. Thompson, D. J. Tibaldo, L. Torres, D. F. Tosti, G. Tramacere, A. Usher, T. L. Vandenbroucke, J. Vasileiou, V. Vilchez, N. Vitale, V. Waite, A. P. Wang, P. Winer, B. L. Wood, K. S. Yang, Z. Ylinen, T. Ziegler, M. Acciari, V. A. Aliu, E. Arlen, T. Aune, T. Beilicke, M. Benbow, W. Boettcher, M. Boltuch, D. Bradbury, S. M. Buckley, J. H. Bugaev, V. Byrum, K. Cannon, A. Cesarini, A. Christiansen, J. L. Ciupik, L. Cui, W. de la Calle Perez, I. Dickherber, R. Errando, M. Falcone, A. Finley, J. P. Finnegan, G. Fortson, L. Furniss, A. Galante, N. Gall, D. Gillanders, G. H. Godambe, S. Grube, J. Guenette, R. Gyuk, G. Hanna, D. Holder, J. Hui, C. M. Humensky, T. B. Imran, A. Kaaret, P. Karlsson, N. Kertzman, M. Kieda, D. Konopelko, A. Krawczynski, H. Krennrich, F. Lang, M. J. LeBohec, S. Maier, G. McArthur, S. McCann, A. McCutcheon, M. Moriarty, P. Mukherjee, R. Ong, R. A. Otte, A. N. Pandel, D. Perkins, J. S. Pichel, A. Pohl, M. Quinn, J. Ragan, K. Reynolds, P. T. Roache, E. Rose, H. J. Schroedter, M. Sembroski, G. H. Senturk, G. Demet Smith, A. W. Steele, D. Swordy, S. P. Tesic, G. Theiling, M. Thibadeau, S. Varlotta, A. Vassiliev, V. V. Vincent, S. Wakely, S. P. Ward, J. E. Weekes, T. C. Weinstein, A. Weisgarber, T. Williams, D. A. Wissel, S. Wood, M. Villata, M. Raiteri, C. M. Gurwell, M. A. Larionov, V. M. Kurtanidze, O. M. Aller, M. F. Laehteenmaeki, A. Chen, W. P. Berduygin, A. Agudo, I. Aller, H. D. Arkharov, A. A. Bach, U. Bachev, R. Beltrame, P. Benitez, E. Buemi, C. S. Dashti, J. Calcidese, P. Capezzali, D. Carosati, D. Da Rio, D. Di Paola, A. Diltz, C. Dolci, M. Dultzin, D. Forne, E. Gomez, J. L. Hagen-Thorn, V. A. Halkola, A. Heidt, J. Hiriart, D. Hovatta, T. Hsiao, H. -Y. Jorstad, S. G. Kimeridze, G. N. Konstantinova, T. S. Kopatskaya, E. N. Koptelova, E. Leto, P. Ligustri, R. Lindfors, E. Lopez, J. M. Marscher, A. P. Mommert, M. Mujica, R. Nikolashvili, M. G. Nilsson, K. Palma, N. Pasanen, M. Roca-Sogorb, M. Ros, J. A. Roustazadeh, P. Sadun, A. C. Saino, J. Sigua, L. A. Sillanaa, A. Sorcia, M. Takalo, L. O. Tornikoski, M. Trigilio, C. Turchetti, R. Umana, G. Belloni, T. Blake, C. H. Bloom, J. S. Angelakis, E. Fumagalli, M. Hauser, M. Prochaska, J. X. Riquelme, D. Sievers, A. Starr, D. L. Tagliaferri, G. Ungerechts, H. Wagner, S. Zensus, J. A. CA Fermi-LAT Collaboration VERITAS Collaboration GASP-WEBT Consortium TI MULTI-WAVELENGTH OBSERVATIONS OF THE FLARING GAMMA-RAY BLAZAR 3C 66A IN 2008 OCTOBER (vol 726, pg 43, 2011) SO ASTROPHYSICAL JOURNAL LA English DT Correction C1 [Abdo, A. A.; Chekhtman, A.; Cheung, C. C.; Dermer, C. D.; Grove, J. E.; Johnson, W. N.; Lovellette, M. N.; Makeev, A.; Parent, D.; Strickman, M. S.; Wood, K. S.] USN, Res Lab, Div Space Sci, Washington, DC 20375 USA. [Abdo, A. A.; Cheung, C. C.] Natl Acad Sci, Washington, DC 20001 USA. [Ackermann, M.; Ajello, M.; Bechtol, K.; Berenji, B.; Blandford, R. D.; Borgland, A. W.; Bouvier, A.; Buehler, R.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; Costamante, L.; Digel, S. W.; do Couto e Silva, E.; Drell, P. S.; Dubois, R.; Funk, S.; Glanzman, T.; Godfrey, G.; Hayashida, M.; Johannesson, G.; Johnson, A. S.; Kamae, T.; Lande, J.; Lee, S. -H.; Michelson, P. F.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Nolan, P. L.; Omodei, N.; Paneque, D.; Panetta, J. H.; Porter, T. A.; Reimer, A.; Reimer, O.; Romani, R. W.; Shaw, M. S.; Tanaka, T.; Thayer, J. B.; Thayer, J. G.; Tramacere, A.; Usher, T. L.; Vandenbroucke, J.; Waite, A. P.; Wang, P.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA. [Abdo, A. A.; Ackermann, M.; Ajello, M.; Bechtol, K.; Berenji, B.; Blandford, R. D.; Borgland, A. W.; Bouvier, A.; Brez, A.; Buehler, R.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; Costamante, L.; Digel, S. W.; do Couto e Silva, E.; Drell, P. S.; Dubois, R.; Funk, S.; Glanzman, T.; Godfrey, G.; Hayashida, M.; Johannesson, G.; Johnson, A. S.; Kamae, T.; Lande, J.; Lee, S. -H.; Michelson, P. F.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Nolan, P. L.; Omodei, N.; Paneque, D.; Panetta, J. H.; Porter, T. A.; Reimer, A.; Reimer, O.; Romani, R. W.; Shaw, M. S.; Tanaka, T.; Thayer, J. B.; Thayer, J. G.; Tramacere, A.; Usher, T. L.; Vandenbroucke, J.; Waite, A. P.; Wang, P.] Stanford Univ, WW Hansen Expt Phys Lab, Kavli Inst Particle Astrophys & Cosmol, Dept Phys, Stanford, CA 94305 USA. [Baldini, L.; Bellazzini, R.; Bregeon, J.; Brez, A.; Kuss, M.; Latronico, L.; 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.; Naumann-Godo, M.; Tibaldo, L.] Univ Paris Diderot, Serv Astrophys, CEA Saclay, Lab AIM,CEA IRFU,CNRS, F-91191 Gif Sur Yvette, France. [Barbiellini, G.; Longo, F.] Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy. [Barbiellini, G.; Longo, F.] Univ Trieste, Dipartimento Fis, I-34127 Trieste, Italy. [Bastieri, D.; Buson, S.; Rando, R.; Tibaldo, L.] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy. [Bastieri, D.; Buson, S.; Carrigan, S.; Rando, R.; Tibaldo, L.] Univ Padua, Dipartimento Fis G Galilei, I-35131 Padua, Italy. [Bonamente, E.; Cecchi, C.; 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.; 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.; de Palma, F.; Favuzzi, C.; Fusco, P.; Gargano, F.; Giglietto, N.; Giordano, F.; Loparco, F.; Mazziotta, M. N.; Monte, C.; Raino, S.; Spinelli, P.] Ist Nazl Fis Nucl, Sez Bari, I-70126 Bari, Italy. [Bruel, P.; Fegan, S. J.; Fortin, P.; Horan, D.; Sanchez, D.] Ecole Polytech, CNRS, IN2P3, Lab Leprince Ringuet, F-91128 Palaiseau, France. [Caliandro, G. A.; Hadasch, D.; Torres, D. F.] Inst Ciencies Espai IEEC CSIC, Barcelona 08193, Spain. [Caraveo, P. A.] INAF Ist Astrofis Spaziale & Fis Cosm, I-20133 Milan, Italy. [Cavazzuti, E.; Cutini, S.; Gasparrini, D.; Giommi, P.] Sci Data Ctr, ASI, I-00044 Rome, Italy. [Celik, Oe.; Davis, D. S.; Gehrels, N.; Hays, E.; Johnson, T. J.; McEnery, J. E.; Moiseev, A. A.; Thompson, D. J.; Vasileiou, V.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Celik, Oe.; Moiseev, A. A.; Vasileiou, V.] CRESST, Greenbelt, MD 20771 USA. [Celik, Oe.; Davis, D. S.; Vasileiou, V.] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA. [Celik, Oe.; Davis, D. S.; Vasileiou, V.] Univ Maryland Baltimore Cty, Ctr Space Sci & Technol, Baltimore, MD 21250 USA. [Chekhtman, A.; Makeev, A.; Parent, D.] George Mason Univ, Fairfax, VA 22030 USA. [Cohen-Tanugi, J.; Mehault, J.; Nuss, E.; Pelassa, V.; Piron, F.] Univ Montpellier 2, CNRS, IN2P3, Lab Phys Theor & Astroparticules, Montpellier, France. [Conrad, J.; Ripken, J.; Yang, Z.] Stockholm Univ, Dept Phys, SE-10691 Stockholm, Sweden. [Conrad, J.; Ripken, J.; Yang, Z.; Ylinen, T.] Oskar Klein Ctr Cosmoparticle Phys, SE-10691 Stockholm, Sweden. [Dumora, D.; Guillemot, L.; Lott, B.] CEN Bordeaux Gradignan, CNRS, IN2P3, UMR 5797, F-33175 Gradignan, France. [Dumora, D.; Guillemot, L.; Lott, B.] Univ Bordeaux, CEN Bordeaux Gradignan, UMR 5797, F-33175 Gradignan, France. [Frailis, M.] Univ Udine, Dipartimento Fis, I-33100 Udine, Italy. [Frailis, M.] Ist Nazl Fis Nucl, Sez Trieste, Grp Collegato Udine, I-33100 Udine, Italy. [Frailis, M.] Ist Nazl Astrofis, Osservatorio Astron Trieste, I-34143 Trieste, Italy. [Fuhrmann, L.; Guillemot, L.; Nestoras, I.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Fukazawa, Y.; Itoh, R.; Katagiri, H.; Mizuno, T.] Hiroshima Univ, Dept Phys Sci, Hiroshima 7398526, Japan. [Giroletti, M.] INAF Ist Radioastron, I-40129 Bologna, Italy. [Guiriec, S.] Univ Alabama Huntsville, CSPAR, Huntsville, AL 35899 USA. [Hughes, R. E.; Sander, A.; Smith, P. D.; Winer, B. L.] Ohio State Univ, Dept Phys, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA. [Johnson, T. J.; McEnery, J. E.; Moiseev, A. A.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA. [Johnson, T. J.; McEnery, J. E.; Moiseev, A. A.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Kataoka, J.; Nakamori, T.] Waseda Univ, Res Inst Sci & Engn, Shinjuku Ku, Tokyo 1698555, Japan. [Knoedlseder, J.; Vilchez, N.] UPS, CNRS, Ctr Etud Spatiale Rayonnements, F-31028 Toulouse 4, France. [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. [Ohsugi, T.; Takahashi, H.] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Hiroshima 7398526, Japan. [Okumura, A.; Ozaki, M.] JAXA, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2298510, Japan. [Orlando, E.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Reimer, A.; Reimer, O.] Leopold Franzens Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria. [Reimer, A.; Reimer, O.] Leopold Franzens Univ Innsbruck, Inst Theoret Phys, A-6020 Innsbruck, Austria. [Reyes, L. C.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Ritz, S.; Sadrozinski, H. F. -W.; Ziegler, M.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Dept Phys, Santa Cruz, CA 95064 USA. [Ritz, S.; Sadrozinski, H. F. -W.; Ziegler, M.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Roth, M.] Univ Washington, Dept Phys, Seattle, WA 98195 USA. [Scargle, J. D.] NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA. [Suson, D. J.] Purdue Univ Calumet, Dept Chem & Phys, Hammond, IN 46323 USA. [Torres, D. F.] ICREA, Barcelona, Spain. [Tramacere, A.] CIFS, I-10133 Turin, Italy. [Tramacere, A.] INTEGRAL Sci Data Ctr, CH-1290 Versoix, Switzerland. [Vitale, V.] Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy. [Ylinen, T.] Royal Inst Technol KTH, Dept Phys, SE-10691 Stockholm, Sweden. [Ylinen, T.] Univ Kalmar, Sch Pure & Appl Nat Sci, SE-39182 Kalmar, Sweden. [Acciari, V. A.; Benbow, W.; Galante, N.; Perkins, J. S.; Roache, E.; Theiling, M.; Weekes, T. C.] Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA. [Aliu, E.; Errando, M.; Mukherjee, R.] Columbia Univ, Dept Phys & Astron, Barnard Coll, New York, NY 10027 USA. [Arlen, T.; Ong, R. A.; Vassiliev, V. V.; Weinstein, A.; Wood, M.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Aune, T.; Furniss, A.; Otte, A. N.; Williams, D. A.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA. [Aune, T.; Furniss, A.; Otte, A. N.; Williams, D. A.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA. [Beilicke, M.; Buckley, J. H.; Bugaev, V.; Dickherber, R.; Krawczynski, H.; McArthur, S.; Thibadeau, S.] Washington Univ, Dept Phys, St Louis, MO 63130 USA. [Boettcher, M.] Ohio Univ, Inst Astrophys, Dept Phys & Astron, Athens, OH 45701 USA. [Boltuch, D.; Holder, J.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA. [Boltuch, D.; Holder, J.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA. [Bradbury, S. M.; Rose, H. J.] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England. [Byrum, K.; Smith, A. W.] Argonne Natl Lab, Argonne, IL 60439 USA. [Cannon, A.; Quinn, J.; Ward, J. E.] Univ Coll Dublin, Sch Phys, Dublin 4, Ireland. [Cesarini, A.; Gillanders, G. H.; Lang, M. J.] Natl Univ Ireland Galway, Sch Phys, Galway, Ireland. [Christiansen, J. L.] Calif Polytech State Univ San Luis Obispo, Dept Phys, San Luis Obispo, CA 94307 USA. [Ciupik, L.; Fortson, L.; Grube, J.; Gyuk, G.; Karlsson, N.; Steele, D.] Adler Planetarium & Astron Museum, Dept Astron, Chicago, IL 60605 USA. [Cui, W.; Finley, J. P.; Gall, D.; Sembroski, G. H.; Varlotta, A.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. [de la Calle Perez, I.] Satellite Tracking Stn, European Space Astron Ctr INSA ESAC, ESA, E-28080 Madrid, Spain. [Falcone, A.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA. [Finnegan, G.; Godambe, S.; Hui, C. M.; Kieda, D.; LeBohec, S.; Vincent, S.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA. [Guenette, R.; Hanna, D.; Maier, G.; McCann, A.; McCutcheon, M.; Ragan, K.; Tesic, G.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Humensky, T. B.; Swordy, S. P.; Wakely, S. P.; Weisgarber, T.; Wissel, S.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [Imran, A.; Krennrich, F.; Pohl, M.; Schroedter, M.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. [Kaaret, P.; Pandel, D.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. [Kertzman, M.] Depauw Univ, Dept Phys & Astron, Greencastle, IN 46135 USA. [Konopelko, A.] Pittsburg State Univ, Dept Phys, Pittsburg, KS 66762 USA. [Moriarty, P.] Galway Mayo Inst Technol, Dept Life & Phys Sci, Galway, Ireland. [Pichel, A.] Inst Astron & Fis Espacio, RA-1428 Buenos Aires, DF, Argentina. [Reynolds, P. T.] Cork Inst Technol, Dept Appl Phys & Instrumentat, Cork, Ireland. [Senturk, G. Demet] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Villata, M.; Raiteri, C. M.] Osserv Astron Torino, INAF, Turin, Italy. [Gurwell, M. A.] Harvard Smithsonian Ctr Astrophys, Boston, MA USA. [Larionov, V. M.; Hagen-Thorn, V. A.; Konstantinova, T. S.; Kopatskaya, E. N.] St Petersburg State Univ, Astron Inst, St Petersburg, Russia. [Larionov, V. M.; Hagen-Thorn, V. A.] Isaac Newton Inst Chile, St Petersburg Branch, St Petersburg, Russia. [Kurtanidze, O. M.; Kimeridze, G. N.; Nikolashvili, M. G.; Sigua, L. A.] Abastumani Observ, GE-0301 Mt Kanobili, Abastumani, Rep of Georgia. [Aller, M. F.; Aller, H. D.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Laehteenmaeki, A.; Hovatta, T.; Tornikoski, M.] Aalto Univ, Metsahovi Radio Observ, Helsinki, Finland. [Chen, W. P.; Hsiao, H. -Y.; Koptelova, E.] Natl Cent Univ, Inst Astron, Taipei, Taiwan. [Berduygin, A.; Halkola, A.; Lindfors, E.; Pasanen, M.; Saino, J.; Sillanaa, A.; Takalo, L. O.] Univ Turku, Tuorla Observ, Dept Phys & Astron, SF-20500 Turku, Finland. [Agudo, I.; Gomez, J. L.; Roca-Sogorb, M.] CSIC, Inst Astrofis Andalucia, Madrid, Spain. [Bachev, R.] Bulgarian Acad Sci, Inst Astron, BG-1040 Sofia, Bulgaria. [Benitez, E.; Dultzin, D.; Sorcia, M.] Univ Nacl Autonoma Mexico, Inst Astron, Mexico City 04510, DF, Mexico. [Buemi, C. S.; Leto, P.; Trigilio, C.; Umana, G.] Osserv Astrofis Catania, INAF, Catania, Italy. [Dashti, J.; Diltz, C.; Palma, N.; Roustazadeh, P.] Ohio Univ, Inst Astrophys, Dept Phys & Astron, Athens, OH 45701 USA. [Calcidese, P.] Osservatorio Astron Reg Autonoma Aosta, Aosta, Italy. [Di Paola, A.] Osserv Astron Roma, INAF, Rome, Italy. [Dolci, M.] Osservatorio Astron Collurania Teramo, INAF, Teramo, Italy. [Forne, E.; Ros, J. A.] Agrupacio Astron Sabadell, Sabadell, Spain. [Heidt, J.; Mommert, M.] Landessternwarte Heidelberg, ZAH, D-69117 Heidelberg, Germany. [Hiriart, D.; Lopez, J. M.] Univ Nacl Autonoma Mexico, Inst Astron, Ensenada 22800, Baja California, Mexico. [Jorstad, S. G.; Marscher, A. P.] Boston Univ, Inst Astrophys Res, Boston, MA 02215 USA. [Mommert, M.] Inst Planetary Res, DLR, D-12489 Berlin, Germany. [Mujica, R.] INAOE, Puebla 72000, Mexico. [Nilsson, K.] Univ Turku, Finnish Ctr Astron ESO FINCA, FI-21500 Piikkio, Finland. [Sadun, A. C.] Univ Colorado, Dept Phys, Denver, CO 80202 USA. [Belloni, T.; Tagliaferri, G.] INAF Osservatorio Astron Brera, I-23807 Merate, Italy. [Blake, C. H.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Bloom, J. S.; Starr, D. L.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Angelakis, E.; Zensus, J. A.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Fumagalli, M.; Prochaska, J. X.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Hauser, M.; Wagner, S.] Heidelberg Univ, D-69117 Heidelberg, Germany. [Prochaska, J. X.] Univ Calif Santa Cruz, UCO Lick Observ, Santa Cruz, CA 95064 USA. [Riquelme, D.; Sievers, A.; Ungerechts, H.] Inst Radio Astron Millimetr, Granada 18012, Spain. [Conrad, J.] Royal Swedish Acad Sci, Stockholm, Sweden. RP Abdo, AA (reprint author), USN, Res Lab, Div Space Sci, Washington, DC 20375 USA. EM lreyes@kicp.uchicago.edu RI Lahteenmaki, Anne/L-5987-2013; Hays, Elizabeth/D-3257-2012; Johnson, Neil/G-3309-2014; Kurtanidze, Omar/J-6237-2014; Agudo, Ivan/G-1701-2015; Jorstad, Svetlana/H-6913-2013; Grishina, Tatiana/H-6873-2013; Hagen-Thorn, Vladimir/H-3983-2013; Loparco, Francesco/O-8847-2015; Gargano, Fabio/O-8934-2015; Johannesson, Gudlaugur/O-8741-2015; Moskalenko, Igor/A-1301-2007; Mazziotta, Mario /O-8867-2015; Thompson, David/D-2939-2012; Gehrels, Neil/D-2971-2012; McEnery, Julie/D-6612-2012; Baldini, Luca/E-5396-2012; lubrano, pasquale/F-7269-2012; Kuss, Michael/H-8959-2012; giglietto, nicola/I-8951-2012; Morselli, Aldo/G-6769-2011; Reimer, Olaf/A-3117-2013; Tosti, Gino/E-9976-2013; Larionov, Valeri/H-1349-2013; Kopatskaya, Evgenia/H-4720-2013; Ozaki, Masanobu/K-1165-2013; Rando, Riccardo/M-7179-2013; Sgro, Carmelo/K-3395-2016; Torres, Diego/O-9422-2016; Orlando, E/R-5594-2016; Funk, Stefan/B-7629-2015 OI Agudo, Ivan/0000-0002-3777-6182; Jorstad, Svetlana/0000-0001-9522-5453; Grishina, Tatiana/0000-0002-3953-6676; Hagen-Thorn, Vladimir/0000-0002-6431-8590; Loparco, Francesco/0000-0002-1173-5673; Gargano, Fabio/0000-0002-5055-6395; Johannesson, Gudlaugur/0000-0003-1458-7036; Moskalenko, Igor/0000-0001-6141-458X; Mazziotta, Mario /0000-0001-9325-4672; Thompson, David/0000-0001-5217-9135; lubrano, pasquale/0000-0003-0221-4806; giglietto, nicola/0000-0002-9021-2888; Morselli, Aldo/0000-0002-7704-9553; Reimer, Olaf/0000-0001-6953-1385; Larionov, Valeri/0000-0002-4640-4356; Kopatskaya, Evgenia/0000-0001-9518-337X; Torres, Diego/0000-0002-1522-9065; Funk, Stefan/0000-0002-2012-0080 NR 2 TC 3 Z9 3 U1 0 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 APR 10 PY 2011 VL 731 IS 1 AR 77 DI 10.1088/0004-637X/731/1/77 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 753KR UT WOS:000289772800077 ER PT J AU Bell, TA Willacy, K Phillips, TG Allen, M Lis, DC AF Bell, T. A. Willacy, K. Phillips, T. G. Allen, M. Lis, D. C. TI THE INFLUENCE OF DEUTERATION AND TURBULENT DIFFUSION ON THE OBSERVED D/H RATIO SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrochemistry; diffusion; ISM: abundances; ISM: clouds; ISM: molecules; turbulence ID ULTRAVIOLET-SPECTROSCOPIC-EXPLORER; PRE-PROTOSTELLAR COLLAPSE; DENSE INTERSTELLAR CORES; DEUTERIUM FRACTIONATION; MOLECULAR CLOUDS; PRESTELLAR CORES; CO DEPLETION; GALACTIC DISK; 1ST DETECTION; DARK CLOUDS AB The influence of turbulent mixing on the chemistry of the interstellar medium (ISM) has so far received little attention. Previous studies of this effect have suggested that it might play an important role in mixing the various phases of the ISM. In this paper, we examine the potential effects of turbulent diffusion on the deuterium chemistry within molecular clouds. We find that such mixing acts to reduce the efficiency of deuteration in these clouds by increasing the ionization fraction and reducing freeze-out of heavy molecules. This leads to lower abundances for many deuterated species. We also examine the influence of turbulent mixing on the transition from atomic hydrogen to H-2 and from atomic deuterium to HD near the cloud edge. We find that including turbulent diffusion in our models serves to push these transitions deeper into the cloud and helps maintain a higher atomic fraction throughout the cloud envelope. Based on these findings, we propose a new process to account for the significant scatter in the observed atomic D/H ratio for galactic sightlines extending beyond the Local Bubble. Although several mechanisms have been put forward to explain this scatter, they are unable to fully account for the range in D/H values. We suggest a scenario in which turbulent mixing of atomic and molecular gas at the edges of molecular clouds causes the observed atomic D/H ratio to vary by a factor of similar to 2. C1 [Bell, T. A.; Phillips, T. G.; Lis, D. C.] CALTECH, Dept Astron, Pasadena, CA 91125 USA. [Willacy, K.; Allen, M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Bell, TA (reprint author), CALTECH, Dept Astron, 1200 E Calif Blvd, Pasadena, CA 91125 USA. EM tab@caltech.edu FU National Science Foundation [AST-0838261]; National Aeronautics and Space Administration FX We thank W. D. Langer for helpful discussions and the referee for constructive comments which helped to improve an earlier draft of this paper. This research has been supported by the National Science Foundation grant AST-0838261 to the Caltech Submillimeter Observatory. Part of this research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. NR 78 TC 6 Z9 6 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 APR 10 PY 2011 VL 731 IS 1 AR 48 DI 10.1088/0004-637X/731/1/48 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 753KR UT WOS:000289772800048 ER PT J AU Chiar, JE Pendleton, YJ Allamandola, LJ Boogert, ACA Ennico, K Greene, TP Geballe, TR Keane, JV Lada, CJ Mason, RE Roellig, TL Sandford, SA Tielens, AGGM Werner, MW Whittet, DCB Decin, L Eriksson, K AF Chiar, J. E. Pendleton, Y. J. Allamandola, L. J. Boogert, A. C. A. Ennico, K. Greene, T. P. Geballe, T. R. Keane, J. V. Lada, C. J. Mason, R. E. Roellig, T. L. Sandford, S. A. Tielens, A. G. G. M. Werner, M. W. Whittet, D. C. B. Decin, L. Eriksson, K. TI ICES IN THE QUIESCENT IC 5146 DENSE CLOUD SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrochemistry; dust, extinction; infrared: ISM; ISM: individual objects (IC 5146); ISM: molecules ID TAURUS DARK CLOUDS; SPITZER-SPACE-TELESCOPE; YOUNG STELLAR OBJECTS; DIFFUSE INTERSTELLAR-MEDIUM; SOLID CARBON-MONOXIDE; 3 MICRON SPECTRA; INFRARED-SPECTROSCOPY; MOLECULAR-CLOUD; ABSORPTION FEATURES; ABSOLUTE CALIBRATION AB This paper presents spectra in the 2 to 20 mu m range of quiescent cloud material located in the IC 5146 cloud complex. The spectra were obtained with NASA's Infrared Telescope Facility SpeX instrument and the Spitzer Space Telescope's Infrared Spectrometer. We use these spectra to investigate dust and ice absorption features in pristine regions of the cloud that are unaltered by embedded stars. We find that the H2O-ice threshold extinction is 4.03 +/- 0.05 mag. Once foreground extinction is taken into account, however, the threshold drops to 3.2 mag, equivalent to that found for the Taurus dark cloud, generally assumed to be the touchstone quiescent cloud against which all other dense cloud and embedded young stellar object observations are compared. Substructure in the trough of the silicate band for two sources is attributed to CH3OH and NH3 in the ices, present at the similar to 2% and similar to 5% levels, respectively, relative to H2O-ice. The correlation of the silicate feature with the E(J-K) color excess is found to follow a much shallower slope relative to lines of sight that probe diffuse clouds, supporting the previous results by Chiar et al. C1 [Chiar, J. E.] Carl Sagan Ctr, SETI Inst, Mountain View, CA 94035 USA. [Pendleton, Y. J.; Allamandola, L. J.; Ennico, K.; Greene, T. P.; Roellig, T. L.; Sandford, S. A.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Boogert, A. C. A.] CALTECH, IPAC, NASA, Herschel Sci Ctr, Pasadena, CA 91125 USA. [Geballe, T. R.; Mason, R. E.] No Operat Ctr, Gemini Observ, Hilo, HI 96720 USA. [Keane, J. V.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Lada, C. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Tielens, A. G. G. M.] Leiden Observ, NL-2300 RA Leiden, Netherlands. [Werner, M. W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Whittet, D. C. B.] Rensselaer Polytech Inst, New York Ctr Astrobiol, Dept Phys Appl Phys & Astron, Troy, NY 12180 USA. [Decin, L.] Katholieke Univ Leuven, Inst Sterrenkunde, B-3001 Louvain, Belgium. [Eriksson, K.] Uppsala Univ, Dept Phys & Astron, S-75120 Uppsala, Sweden. RP Chiar, JE (reprint author), Carl Sagan Ctr, SETI Inst, 189 Bernardo Ave, Mountain View, CA 94035 USA. EM jchiar@seti.org RI Ennico, Kimberly/L-9606-2014; OI Whittet, Douglas/0000-0001-8539-3891 FU NASA [NNX07AK38G]; NASA's Astrobiology [811073.02.12.03]; Laboratory Astrophysics [09-APRA09-0019]; NASA Astrobiology Institute [NNA09DA80A]; Gemini Observatory; National Science Foundation 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 a contract with NASA. Support for this work was provided to J.E.C. by NASA through an award issued by JPL/Caltech and to Y.J.P., L.J.A., K. E., T. P. G., T. L. R., and S. A. S. by NASA. L.J.A. gratefully acknowledges support from NASA's Astrobiology (grant 811073.02.12.03) and Laboratory Astrophysics (grant 09-APRA09-0019) programs. D. C. B. W. is grateful to the NASA Exobiology and Evolutionary Biology Program (grant NNX07AK38G) and the NASA Astrobiology Institute (grant NNA09DA80A) for financial support. R. E. M. and T. R. G. are supported by the Gemini Observatory, which is operated by the Association of Universities for Research in Astronomy, Inc., on behalf of the international Gemini partnership of Argentina, Australia, Brazil, Canada, Chile, the United Kingdom, and the United States of America. The work is also based in part on observations made at 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, and Planetary Astronomy Program. 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 79 TC 30 Z9 30 U1 0 U2 9 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 APR 10 PY 2011 VL 731 IS 1 AR 9 DI 10.1088/0004-637X/731/1/9 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 753KR UT WOS:000289772800009 ER PT J AU Cowan, NB Robinson, T Livengood, TA Deming, D Agol, E A'Hearn, MF Charbonneau, D Lisse, CM Meadows, VS Seager, S Shields, AL Wellnitz, DD AF Cowan, Nicolas B. Robinson, Tyler Livengood, Timothy A. Deming, Drake Agol, Eric A'Hearn, Michael F. Charbonneau, David Lisse, Carey M. Meadows, Victoria S. Seager, Sara Shields, Aomawa L. Wellnitz, Dennis D. TI ROTATIONAL VARIABILITY OF EARTH'S POLAR REGIONS: IMPLICATIONS FOR DETECTING SNOWBALL PLANETS SO ASTROPHYSICAL JOURNAL LA English DT Article DE methods: analytical; methods: numerical; methods: observational; planets and satellites: individual (Earth); techniques: photometric ID GENERAL-CIRCULATION MODEL; EXTRASOLAR PLANETS; LIGHT-CURVES; PHOTOMETRIC VARIABILITY; EXOPLANETS; ALBEDO; OCEAN; SPECTRUM; CLIMATE; SURFACE AB We have obtained the first time-resolved, disk-integrated observations of Earth's poles with the Deep Impact spacecraft as part of the EPOXI mission of opportunity. These data mimic what we will see when we point next-generation space telescopes at nearby exoplanets. We use principal component analysis (PCA) and rotational light curve inversion to characterize color inhomogeneities and map their spatial distribution from these unusual vantage points, as a complement to the equatorial views presented by Cowan et al. in 2009. We also perform the same PCA on a suite of simulated rotational multi-band light curves from NASA's Virtual Planetary Laboratory three-dimensional spectral Earth model. This numerical experiment allows us to understand what sorts of surface features PCA can robustly identify. We find that the EPOXI polar observations have similar broadband colors as the equatorial Earth, but with 20%-30% greater apparent albedo. This is because the polar observations are most sensitive to mid-latitudes, which tend to be more cloudy than the equatorial latitudes emphasized by the original EPOXI Earth observations. The cloudiness of the mid-latitudes also manifests itself in the form of increased variability at short wavelengths in the polar observations and as a dominant gray eigencolor in the south polar observation. We construct a simple reflectance model for a snowball Earth. By construction, our model has a higher Bond albedo than the modern Earth; its surface albedo is so high that Rayleigh scattering does not noticeably affect its spectrum. The rotational color variations occur at short wavelengths due to the large contrast between glacier ice and bare land in those wavebands. Thus, we find that both the broadband colors and diurnal color variations of such a planet would be easily distinguishable from the modern-day Earth, regardless of viewing angle. C1 [Cowan, Nicolas B.] Northwestern Univ, Evanston, IL 60208 USA. [Robinson, Tyler; Agol, Eric; Meadows, Victoria S.; Shields, Aomawa L.] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Robinson, Tyler; Agol, Eric; Meadows, Victoria S.; Shields, Aomawa L.] Univ Washington, Astrobiol Program, Seattle, WA 98195 USA. [Livengood, Timothy A.; Deming, Drake] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [A'Hearn, Michael F.; Wellnitz, Dennis D.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Charbonneau, David] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Lisse, Carey M.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Seager, Sara] MIT, Dept Earth Atmospher & Planetary Sci, Dept Phys, Cambridge, MA 02139 USA. RP Cowan, NB (reprint author), Northwestern Univ, 2131 Tech Dr, Evanston, IL 60208 USA. EM n-cowan@northwestern.edu RI Wellnitz, Dennis/B-4080-2012; Livengood, Timothy/C-8512-2012; Agol, Eric/B-8775-2013; Lisse, Carey/B-7772-2016; OI Agol, Eric/0000-0002-0802-9145; Lisse, Carey/0000-0002-9548-1526; Charbonneau, David/0000-0002-9003-484X FU NASA; National Science Foundation FX This work was supported by the NASA Discovery Program. We thank D. S. Abbot and R. T. Pierrehumbert for providing us with cloud maps of snowball Earth. N.B.C. acknowledges many useful discussions with S. G. Warren about snowball Earth, and thanks W. Sullivan for encouraging him to complete his astrobiology research rotation. E.A. is supported by a National Science Foundation Career Grant. NR 53 TC 22 Z9 22 U1 2 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 APR 10 PY 2011 VL 731 IS 1 AR 76 DI 10.1088/0004-637X/731/1/76 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 753KR UT WOS:000289772800076 ER PT J AU Hong, S Calzetti, D Dopita, MA Blair, WP Whitmore, BC Balick, B Bond, HE Carollo, M Disney, MJ Frogel, JA Hall, D Holtzman, JA Kimble, RA McCarthy, PJ O'Connell, RW Paresce, F Saha, A Silk, JI Trauger, JT Walker, AR Windhorst, RA Young, ET Mutchler, M AF Hong, Sungryong Calzetti, Daniela Dopita, Michael A. Blair, William P. Whitmore, Bradley C. Balick, Bruce Bond, Howard E. Carollo, Marcella Disney, Michael J. Frogel, Jay A. Hall, Donald Holtzman, Jon A. Kimble, Randy A. McCarthy, Patrick J. O'Connell, Robert W. Paresce, Francesco Saha, Abhijit Silk, Joseph I. Trauger, John T. Walker, Alistair R. Windhorst, Rogier A. Young, Erick T. Mutchler, Max TI LARGE-SCALE SHOCK-IONIZED AND PHOTOIONIZED GAS IN M83: THE IMPACT OF STAR FORMATION SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: interactions; galaxies: ISM; galaxies: starburst; ISM: structure ID HUBBLE-SPACE-TELESCOPE; II ESI SPECTRA; FIELD CAMERA 3; STARBURST GALAXIES; HII-REGIONS; INTERSTELLAR-MEDIUM; GASEOUS OUTFLOWS; YOUNG CLUSTERS; MODELS; SPECTROSCOPY AB We investigate the ionization structure of the nebular gas in M83 using the line diagnostic diagram, [O III](5007 angstrom)/H beta versus [S II](6716 angstrom+6731 angstrom)/H alpha, with the newly available narrowband images from the Wide Field Camera 3 (WFC3) of the Hubble Space Telescope (HST). We produce the diagnostic diagram on a pixel-by-pixel (0 ''.2 x 0 ''.2) basis and compare it with several photo- and shock-ionization models. We select four regions from the center to the outer spiral arm and compare them in the diagnostic diagram. For the photoionized gas, we observe a gradual increase of the log ([O III]/H beta) ratios from the center to the spiral arm, consistent with the metallicity gradient, as the H II regions go from super-solar abundance to roughly solar abundance from the center out. Using the diagnostic diagram, we separate the photoionized from the shock-ionized component of the gas. We find that the shock-ionized H alpha emission ranges from similar to 2% to about 15%-33% of the total, depending on the separation criteria used. An interesting feature in the diagnostic diagram is a horizontal distribution around log ([O III]/H beta) approximate to 0. This feature is well fit by a shock-ionization model with 2.0 Z(circle dot) metallicity and shock velocities in the range of 250350 km s(-1). A low-velocity shock component, <200 km s(-1), is also detected and is spatially located at the boundary between the outer ring and the spiral arm. The low-velocity shock component can be due to (1) supernova remnants located nearby, (2) dynamical interaction between the outer ring and the spiral arm, and (3) abnormal line ratios from extreme local dust extinction. The current data do not enable us to distinguish among those three possible interpretations. Our main conclusion is that, even at the HST resolution, the shocked gas represents a small fraction of the total ionized gas emission at less than 33% of the total. However, it accounts for virtually all of the mechanical energy produced by the central starburst in M83. C1 [Hong, Sungryong; Calzetti, Daniela] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. [Dopita, Michael A.] Australian Natl Univ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia. [Blair, William P.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Whitmore, Bradley C.; Bond, Howard E.; Mutchler, Max] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Balick, Bruce] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Carollo, Marcella] ETH, Dept Phys, CH-8093 Zurich, Switzerland. [Disney, Michael J.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Frogel, Jay A.] Assoc Univ Res Astron, Washington, DC 20005 USA. [Hall, Donald] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Holtzman, Jon A.] New Mexico State Univ, Dept Astron, Las Cruces, NM 88003 USA. [Kimble, Randy A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [McCarthy, Patrick J.] Observ Carnegie Inst Washington, Pasadena, CA 91101 USA. [O'Connell, Robert W.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. [Paresce, Francesco] INAF, Ist Astrofis Spaziale & Fis Cosm, I-40129 Bologna, Italy. [Saha, Abhijit] Natl Opt Astron Observ, Tucson, AZ 85726 USA. [Silk, Joseph I.] Univ Oxford, Dept Phys, Oxford OX1 3PU, England. [Trauger, John T.] NASA, Jet Prop Lab, Pasadena, CA 91109 USA. [Walker, Alistair R.] Cerro Tololo Interamer Observ, La Serena, Chile. [Windhorst, Rogier A.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [Young, Erick T.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Hong, S (reprint author), Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. EM wpb@pha.jhu.edu RI Dopita, Michael/P-5413-2014; OI Dopita, Michael/0000-0003-0922-4986; silk, joe/0000-0002-1566-8148 FU NASA [NAS5-26555] FX We are grateful to an anonymous referee for comments that have improved this paper. This paper is based on observations taken with the NASA/ESA Hubble Space Telescope obtained at the Space Telescope Science Institute, which is operated by AURA, Inc., under NASA contract NAS5-26555. It uses Early Release Science observations made by the WFC3 Science Oversight Committee. We are grateful to the Director of STScI for awarding Director's Discretionary Time for this program. NR 40 TC 6 Z9 6 U1 0 U2 3 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 APR 10 PY 2011 VL 731 IS 1 AR 45 DI 10.1088/0004-637X/731/1/45 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 753KR UT WOS:000289772800045 ER PT J AU Jia, JJ Ptak, A Heckman, TM Overzier, RA Hornschemeier, A LaMassa, SM AF Jia, Jianjun Ptak, Andrew Heckman, Timothy M. Overzier, Roderik A. Hornschemeier, Ann LaMassa, Stephanie M. TI EVIDENCE FOR BLACK HOLE GROWTH IN LOCAL ANALOGS TO LYMAN BREAK GALAXIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: starburst; quasars: general; X-rays: galaxies ID ACTIVE GALACTIC NUCLEI; STAR-FORMATION RATE; ULTRALUMINOUS INFRARED GALAXIES; ULTRAVIOLET-LUMINOUS GALAXIES; TYPE-2 SEYFERT-GALAXIES; X-RAY OBSERVATIONS; PARAMETER-ESTIMATION; INTERSTELLAR-MEDIUM; FORMING GALAXIES; FAR-ULTRAVIOLET AB We have used XMM-Newton to observe six Lyman break analogs (LBAs): members of the rare population of local galaxies that have properties that are very similar to distant Lyman break galaxies. Our six targets were specifically selected because they have optical emission-line properties that are intermediate between starbursts and Type 2 (obscured) active galactic nuclei (AGNs). Our new X-ray data provide an important diagnostic of the presence of an AGN. We find X-ray luminosities of order 10(42) erg s(-1) and ratios of X-ray to far-IR luminosities that are higher than values in pure starburst galaxies by factors ranging from similar to 3 to 30. This strongly suggests the presence of an AGN in at least some of the galaxies. The ratios of the luminosities of the hard (2-10 keV) X-ray to [O III]lambda 5007 emission line are low by about an order of magnitude compared with Type 1 AGN, but are consistent with the broad range seen in Type 2 AGN. Either the AGN hard X-rays are significantly obscured or the [O III] emission is dominated by the starburst. We searched for an iron emission line at similar to 6.4 keV, which is a key feature of obscured AGNs, but only detected emission at the similar to 2 sigma level. Finally, we find that the ratios of the mid-infrared (24 mu m) continuum to [O III]lambda 5007 luminosities in these LBAs are higher than the values for Type 2 AGN by an average of 0.8 dex. Combining all these clues, we conclude that an AGN is likely to be present, but that the bolometric luminosity is produced primarily by an intense starburst. If these black holes are radiating at the Eddington limit, their masses would lie in the range of 10(5)-10(6) M circle dot. These objects may offer ideal local laboratories to investigate the processes by which black holes grew in the early universe. C1 [Jia, Jianjun; Heckman, Timothy M.; LaMassa, Stephanie M.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Ptak, Andrew; Hornschemeier, Ann] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Overzier, Roderik A.] Max Planck Inst Astrophys, D-85748 Garching, Germany. RP Jia, JJ (reprint author), Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. FU NASA [NNX08AZ0G] FX We are very grateful to the anonymous referee for helpful comments that have improved the manuscript. We also thank Marat Gilfanov for discussion. This work is supported by NASA grant NNX08AZ0G. NR 46 TC 17 Z9 17 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 10 PY 2011 VL 731 IS 1 AR 55 DI 10.1088/0004-637X/731/1/55 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 753KR UT WOS:000289772800055 ER PT J AU Krughoff, KS Connolly, AJ Frieman, J SubbaRao, M Kilper, G Schneider, DP AF Krughoff, K. Simon Connolly, Andrew J. Frieman, Joshua SubbaRao, Mark Kilper, Gary Schneider, Donald P. TI SPECTROSCOPIC DETERMINATION OF THE LOW-REDSHIFT TYPE Ia SUPERNOVA RATE FROM THE SLOAN DIGITAL SKY SURVEY SO ASTROPHYSICAL JOURNAL LA English DT Article DE methods: statistical; supernovae: general; techniques: spectroscopic ID DELAY-TIME DISTRIBUTION; SURVEY IMAGING DATA; STAR-FORMATION; DATA RELEASE; SPECTRAL CLASSIFICATION; ULTRAVIOLET EXTINCTION; LEGACY SURVEY; LIGHT CURVES; DEEP SURVEY; PROGENITORS AB Supernova rates (SNRs) are directly coupled to high-mass stellar birth and evolution. As such, they are one of the few direct measures of the history of cosmic stellar evolution. In this paper, we describe a probabilistic technique for identifying supernovae within spectroscopic samples of galaxies. We present a study of 52 Type Ia supernovae ranging in age from -14 days to +40 days extracted from a parent sample of similar to 350,000 spectra from the SDSS DR5. We find an SNR of 0.472(-0.039)(+0.048) (Systematic)(-0.071)(+0.081)(Statistical)SNu at a redshift of < z > = 0.1. This value is higher than other values at low redshift at the 1 sigma level, but is consistent at the 3 sigma level. In this paper, we demonstrate the potential for the described approach to detect supernovae in future spectroscopic surveys. C1 [Krughoff, K. Simon; Connolly, Andrew J.] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Frieman, Joshua] Fermilab Natl Accelerator Lab, Batavia, IL 60510 USA. [Frieman, Joshua] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Frieman, Joshua; SubbaRao, Mark] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [SubbaRao, Mark] Adler Planetarium & Astron Museum, Chicago, IL 60605 USA. [Kilper, Gary] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Schneider, Donald P.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 408A, University Pk, PA 16802 USA. RP Krughoff, KS (reprint author), Univ Washington, Dept Astron, Box 351580, Seattle, WA 98195 USA. FU NSF [AST-0851007]; DOE [DE-FG02-87ER40315]; Alfred P. Sloan Foundation; National Science Foundation; U.S. Department of Energy; National Aeronautics and Space Administration; Japanese Monbukagakusho; Max Planck Society; Higher Education Funding Council for England; American Museum of Natural History; Astrophysical Institute Potsdam,; University of Basel; University of Cambridge; Case Western Reserve University; University of Chicago; Drexel University; Fermilab; Institute for Advanced Study; Japan Participation Group; Johns Hopkins University; Joint Institute for Nuclear Astrophysics; Kavli Institute for Particle Astrophysics and Cosmology; Korean Scientist Group; Chinese Academy of Sciences (LAMOST); Los Alamos National Laboratory; Max-Planck-Institute for Astronomy (MPIA); Max-Planck-Institute for Astrophysics (MPA); New Mexico State University; Ohio State University; University of Pittsburgh; University of Portsmouth; Princeton University; United States Naval Observatory; University of Washington FX The authors wish to thank the reviewer for many excellent points that served to greatly improve the quality of the analysis. K. S. K. and A.J.C. acknowledge partial support from NSF grant AST-0851007 and DOE grant DE-FG02-87ER40315. Funding for the SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, the U.S. Department of Energy, the National Aeronautics and Space Administration, the Japanese Monbukagakusho, the Max Planck Society, and the Higher Education Funding Council for England. The SDSS Web Site is http://www.sdss.org/.; The SDSS is managed by the Astrophysical Research Consortium for the Participating Institutions. The Participating Institutions are the American Museum of Natural History, Astrophysical Institute Potsdam, University of Basel, University of Cambridge, Case Western Reserve University, University of Chicago, Drexel University, Fermilab, the Institute for Advanced Study, the Japan Participation Group, Johns Hopkins University, the Joint Institute for Nuclear Astrophysics, the Kavli Institute for Particle Astrophysics and Cosmology, the Korean Scientist Group, the Chinese Academy of Sciences (LAMOST), Los Alamos National Laboratory, the Max-Planck-Institute for Astronomy (MPIA), the Max-Planck-Institute for Astrophysics (MPA), New Mexico State University, Ohio State University, University of Pittsburgh, University of Portsmouth, Princeton University, the United States Naval Observatory, and the University of Washington. NR 75 TC 9 Z9 9 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 APR 10 PY 2011 VL 731 IS 1 AR 42 DI 10.1088/0004-637X/731/1/42 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 753KR UT WOS:000289772800042 ER PT J AU Mainzer, A Bauer, J Grav, T Masiero, J Cutri, RM Dailey, J Eisenhardt, P McMillan, RS Wright, E Walker, R Jedicke, R Spahr, T Tholen, D Alles, R Beck, R Brandenburg, H Conrow, T Evans, T Fowler, J Jarrett, T Marsh, K Masci, F McCallon, H Wheelock, S Wittman, M Wyatt, P DeBaun, E Elliott, G Elsbury, D Gautier, T Gomillion, S Leisawitz, D Maleszewski, C Micheli, M Wilkins, A AF Mainzer, A. Bauer, J. Grav, T. Masiero, J. Cutri, R. M. Dailey, J. Eisenhardt, P. McMillan, R. S. Wright, E. Walker, R. Jedicke, R. Spahr, T. Tholen, D. Alles, R. Beck, R. Brandenburg, H. Conrow, T. Evans, T. Fowler, J. Jarrett, T. Marsh, K. Masci, F. McCallon, H. Wheelock, S. Wittman, M. Wyatt, P. DeBaun, E. Elliott, G. Elsbury, D. Gautier, T. Gomillion, S. Leisawitz, D. Maleszewski, C. Micheli, M. Wilkins, A. TI PRELIMINARY RESULTS FROM NEOWISE: AN ENHANCEMENT TO THE WIDE-FIELD INFRARED SURVEY EXPLORER FOR SOLAR SYSTEM SCIENCE SO ASTROPHYSICAL JOURNAL LA English DT Article DE catalogs; comets: general; minor planets, asteroids: general; surveys ID NEAR-EARTH ASTEROIDS; JOVIAN TROJAN ASTEROIDS; DUST TRAILS; SIZE DISTRIBUTIONS; PERIOD COMETS; OORT CLOUD; ORIGIN; MISSION; OBJECTS; IRAS AB The Wide-field Infrared Survey Explorer (WISE) has surveyed the entire sky at four infrared wavelengths with greatly improved sensitivity and spatial resolution compared to its predecessors, the Infrared Astronomical Satellite and the Cosmic Background Explorer. NASA's Planetary Science Division has funded an enhancement to the WISE data processing system called "NEOWISE" that allows detection and archiving of moving objects found in the WISE data. NEOWISE has mined the WISE images for a wide array of small bodies in our solar system, including near-Earth objects (NEOs), Main Belt asteroids, comets, Trojans, and Centaurs. By the end of survey operations in 2011 February, NEOWISE identified over 157,000 asteroids, including more than 500 NEOs and similar to 120 comets. The NEOWISE data set will enable a panoply of new scientific investigations. C1 [Mainzer, A.; Bauer, J.; Masiero, J.; Eisenhardt, P.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Bauer, J.; Cutri, R. M.; Dailey, J.; Alles, R.; Beck, R.; Brandenburg, H.; Conrow, T.; Evans, T.; Fowler, J.; Jarrett, T.; Marsh, K.; Masci, F.; McCallon, H.; Wheelock, S.; Wittman, M.; Wyatt, P.] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA. [Grav, T.] Johns Hopkins Univ, Dept Astron, Baltimore, MD USA. [McMillan, R. S.; Maleszewski, C.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Wright, E.] UCLA Astron, Los Angeles, CA 90095 USA. [Walker, R.] Monterey Inst Res Astron, Monterey, CA USA. [Jedicke, R.; Tholen, D.; Elliott, G.; Micheli, M.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Spahr, T.] Harvard Smithsonian Ctr Astrophys, Minor Planet Ctr, Cambridge, MA 02138 USA. [DeBaun, E.] Dartmouth Coll, Hanover, NH 03755 USA. [Elsbury, D.] Notre Dame High Sch, Sherman Oaks, CA 91423 USA. [Gautier, T.] Flintridge Preparatory Sch, La Canada Flintridge, CA 91101 USA. [Gomillion, S.] Embry Riddle Aeronaut Univ, Daytona Beach, FL 32114 USA. [Leisawitz, D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Wilkins, A.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. RP Mainzer, A (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM amainzer@jpl.nasa.gov OI Masiero, Joseph/0000-0003-2638-720X; Micheli, Marco/0000-0001-7895-8209 FU National Aeronautics and Space Administration; Planetary Science Division of the National Aeronautics and Space Administration FX This publication makes use of data products from WISE, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration. This publication also makes use of data products from NEOWISE, which is a project of the Jet Propulsion Laboratory/California Institute of Technology, funded by the Planetary Science Division of the National Aeronautics and Space Administration. We gratefully acknowledge the extraordinary services specific to NEOWISE contributed by the International Astronomical Union's Minor Planet Center, operated by the Harvard-Smithsonian Center for Astrophysics, and the Central Bureau for Astronomical Telegrams, operated by Harvard University. We appreciate the contributions of the referee, J. Emery, which greatly improved the manuscript. We also thank the worldwide community of dedicated amateur and professional astronomers devoted to minor planet follow-up observations. This research has made use of the NASA/IPAC Infrared Science Archive, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. We thank the Auton Lab of Carnegie Mellon University for use of their libraries, and the PanSTARRS project for MOPS. NR 80 TC 138 Z9 138 U1 1 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 APR 10 PY 2011 VL 731 IS 1 AR 53 DI 10.1088/0004-637X/731/1/53 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 753KR UT WOS:000289772800053 ER PT J AU Schwadron, NA Allegrini, F Bzowski, M Christian, ER Crew, GB Dayeh, M DeMajistre, R Frisch, P Funsten, HO Fuselier, SA Goodrich, K Gruntman, M Janzen, P Kucharek, H Livadiotis, G McComas, DJ Moebius, E Prested, C Reisenfeld, D Reno, M Roelof, E Siegel, J Vanderspek, R AF Schwadron, N. A. Allegrini, F. Bzowski, M. Christian, E. R. Crew, G. B. Dayeh, M. DeMajistre, R. Frisch, P. Funsten, H. O. Fuselier, S. A. Goodrich, K. Gruntman, M. Janzen, P. Kucharek, H. Livadiotis, G. McComas, D. J. Moebius, E. Prested, C. Reisenfeld, D. Reno, M. Roelof, E. Siegel, J. Vanderspek, R. TI SEPARATION OF THE INTERSTELLAR BOUNDARY EXPLORER RIBBON FROM GLOBALLY DISTRIBUTED ENERGETIC NEUTRAL ATOM FLUX SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: general; magnetohydrodynamics (MHD); plasmas; shock waves; solar wind; Sun: heliosphere ID SOLAR-WIND; TERMINATION SHOCK; MAGNETIC-FIELD; OUTER HELIOSPHERE; IBEX RIBBON; PICKUP IONS; ENA FLUX; HELIOSHEATH; MECHANISM; GENERATION AB The Interstellar Boundary Explorer (IBEX) observes a remarkable feature, the IBEX ribbon, which has energetic neutral atom (ENA) flux over a narrow region similar to 20 degrees. wide, a factor of 2-3 higher than the more globally distributed ENA flux. Here, we separate ENA emissions in the ribbon from the distributed flux by applying a transparency mask over the ribbon and regions of high emissions, and then solve for the distributed flux using an interpolation scheme. Our analysis shows that the energy spectrum and spatial distribution of the ribbon are distinct from the surrounding globally distributed flux. The ribbon energy spectrum shows a knee between similar to 1 and 4 keV, and the angular distribution is approximately independent of energy. In contrast, the distributed flux does not show a clear knee and more closely conforms to a power law over much of the sky. Consistent with previous analyses, the slope of the power law steepens from the nose to tail, suggesting a weaker termination shock toward the tail as compared to the nose. The knee in the energy spectrum of the ribbon suggests that its source plasma population is generated via a distinct physical process. Both the slope in the energy distribution of the distributed flux and the knee in the energy distribution of the ribbon are ordered by latitude. The heliotail may be identified in maps of globally distributed flux as a broad region of low flux centered similar to 44 degrees W of the interstellar downwind direction, suggesting heliotail deflection by the interstellar magnetic field. C1 [Schwadron, N. A.; Kucharek, H.; Moebius, E.] Univ New Hampshire, Ctr Space Sci, Durham, NH 03824 USA. [Schwadron, N. A.; Allegrini, F.; Dayeh, M.; Livadiotis, G.; McComas, D. J.; Reno, M.] SW Res Inst, San Antonio, TX 78228 USA. [Allegrini, F.; McComas, D. J.] Univ Texas San Antonio, Dept Phys, San Antonio, TX 78249 USA. [Bzowski, M.] Polish Acad Sci, Space Res Ctr, PL-00716 Warsaw, Poland. [Christian, E. R.; Vanderspek, R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Crew, G. B.; Roelof, E.] MIT, Cambridge, MA 02139 USA. [DeMajistre, R.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Frisch, P.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Funsten, H. O.; Goodrich, K.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA. [Fuselier, S. A.] Lockheed Martin Adv Technol Ctr, Palo Alto, CA 94304 USA. [Gruntman, M.] Univ So Calif, Dept Astronaut Engn, Los Angeles, CA 90089 USA. [Janzen, P.; Reisenfeld, D.] Univ Montana, Dept Phys, Missoula, MT 59812 USA. [Prested, C.; Siegel, J.] Boston Univ, Dept Astron, Boston, MA 02215 USA. RP Schwadron, NA (reprint author), Univ New Hampshire, Ctr Space Sci, Durham, NH 03824 USA. EM n.schwadron@unh.edu; fallegrini@swri.edu; bzowski@cbk.waw.pl; eric.r.christian@nasa.gov; gbc@space.mit.edu; maldayeh@swri.edu; Bob.DeMajistre@jhuapl.edu; frisch@oddjob.uchicago.edu; hfunsten@lanl.gov; stephen.a.fuselier@lmco.com; kgoodri@lanl.gov; mikeg@usc.edu; paul.janzen@umontana.edu; harald.kucharek@unh.edu; george.livadiotis@swri.org; dmccomas@swri.org; eberhard.moebius@unh.edu; cprested@bu.edu; dan.reisenfeld@umontana.edu; mreno@swri.edu; Edmond.Roelof@jhuapl.edu; jacob707@gmail.com RI Christian, Eric/D-4974-2012; Funsten, Herbert/A-5702-2015; Reisenfeld, Daniel/F-7614-2015; Gruntman, Mike/A-5426-2008; OI Christian, Eric/0000-0003-2134-3937; Funsten, Herbert/0000-0002-6817-1039; Gruntman, Mike/0000-0002-0830-010X; Moebius, Eberhard/0000-0002-2745-6978 FU NASA; Polish Ministry for Science and Higher Education [NS-1260-11-09] FX We are deeply indebted to all of the outstanding people who have made the IBEX mission possible. This work was carried out as a part of the IBEX project, with support from NASA's Explorer Program and Polish Ministry for Science and Higher Education (grant NS-1260-11-09). NR 40 TC 80 Z9 82 U1 0 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 APR 10 PY 2011 VL 731 IS 1 AR 56 DI 10.1088/0004-637X/731/1/56 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 753KR UT WOS:000289772800056 ER PT J AU Spezzi, L Beccari, G De Marchi, G Young, ET Paresce, F Dopita, MA Andersen, M Panagia, N Balick, B Bond, HE Calzetti, D Carollo, CM Disney, MJ Frogel, JA Hall, DNB Holtzman, JA Kimble, RA McCarthy, PJ O'Connell, RW Ryan, RE Saha, A Silk, JI Trauger, JT Walker, AR Whitmore, BC Windhorst, RA AF Spezzi, Loredana Beccari, Giacomo De Marchi, Guido Young, Erick T. Paresce, Francesco Dopita, Michael A. Andersen, Morten Panagia, Nino Balick, Bruce Bond, Howard E. Calzetti, Daniela Carollo, C. Marcella Disney, Michael J. Frogel, Jay A. Hall, Donald N. B. Holtzman, Jon A. Kimble, Randy A. McCarthy, Patrick J. O'Connell, Robert W. Ryan, Russell E., Jr. Saha, Abhijit Silk, Joseph I. Trauger, John T. Walker, Alistair R. Whitmore, Bradley C. Windhorst, Rogier A. TI DETECTION OF BROWN DWARF LIKE OBJECTS IN THE CORE OF NGC 3603 SO ASTROPHYSICAL JOURNAL LA English DT Article DE brown dwarfs; instrumentation: photometers; open clusters and associations: individual (NCG 3603); stars: pre-main sequence; techniques: photometric ID INITIAL MASS FUNCTION; NEAR-INFRARED SPECTRA; STAR-FORMING REGION; GIANT BRANCH STARS; EVOLUTIONARY MODELS; ORBITAL PERIOD; TAURUS-AURIGA; YOUNG CLUSTER; HII-REGIONS; SKY SURVEY AB We used near-infrared data obtained with the Wide Field Camera 3 on the Hubble Space Telescope to identify objects having the colors of brown dwarfs (BDs) in the field of the massive galactic cluster NGC 3603. These are identified through a combination of narrow-and medium-band filters which span the J and H bands and are particularly sensitive to the presence of the 1.3-1.5 mu m H2O molecular band unique to BDs. We provide a calibration of the relationship between effective temperature and color for both field stars and BDs. This photometric method provides effective temperatures for BDs to an accuracy of +/-350K relative to spectroscopic techniques. This accuracy is shown to be not significantly affected by either stellar surface gravity or uncertainties in the interstellar extinction. We identify nine objects having effective temperatures between 1700 and 2200 K, typical of BDs, observed J-band magnitudes in the range 19.5-21.5, and that are strongly clustered toward the luminous core of NGC 3603. However, if these are located at the distance of the cluster, they are far too luminous to be normal BDs. We argue that it is unlikely that these objects are either artifacts of our data set, normal field BDs/M-type giants, or extragalactic contaminants and, therefore, might represent a new class of stars having the effective temperatures of BDs but with luminosities of more massive stars. We explore the interesting scenario in which these objects would be normal stars that have recently tidally ingested a hot Jupiter, the remnants of which are providing a short-lived extended photosphere to the central star. In this case, we would expect them to show the signature of fast rotation. C1 [Spezzi, Loredana; Beccari, Giacomo; De Marchi, Guido; Andersen, Morten] European Space Agcy ESTEC, NL-2200 AG Noordwijk, Netherlands. [Young, Erick T.] NASA, SOFIA Sci Ctr, Ames Res Ctr, Moffett Field, CA 94035 USA. [Paresce, Francesco] Ist Fis Spaziale & Fis Cosm Bologna, I-40129 Bologna, Italy. [Dopita, Michael A.] Australian Natl Univ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia. [Panagia, Nino; Bond, Howard E.; Whitmore, Bradley C.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Balick, Bruce] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Calzetti, Daniela] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. [Carollo, C. Marcella] ETH, Dept Phys, CH-8093 Zurich, Switzerland. [Disney, Michael J.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Frogel, Jay A.] Assoc Univ Res Astron, Washington, DC 20005 USA. [Hall, Donald N. B.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Holtzman, Jon A.] New Mexico State Univ, Dept Astron, Las Cruces, NM 88003 USA. [Kimble, Randy A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [McCarthy, Patrick J.] Observ Carnegie Inst Washington, Pasadena, CA 91101 USA. [O'Connell, Robert W.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. [Ryan, Russell E., Jr.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. [Saha, Abhijit] Natl Opt Astron Observ, Tucson, AZ 85726 USA. [Silk, Joseph I.] Univ Oxford, Dept Phys, Oxford OX1 3PU, England. [Trauger, John T.] NASA, Jet Prop Lab, Pasadena, CA 91109 USA. [Walker, Alistair R.] Natl Opt Astron Observ, Cerro Tololo Inter Amer Observ, La Serena, Chile. [Windhorst, Rogier A.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. RP Spezzi, L (reprint author), European Space Agcy ESTEC, POB 299, NL-2200 AG Noordwijk, Netherlands. EM lspezzi@rssd.esa.int RI Dopita, Michael/P-5413-2014; OI Dopita, Michael/0000-0003-0922-4986; silk, joe/0000-0002-1566-8148 FU Australian Research Council (ARC) [DP0984657, DP0664434] FX This paper is based on Early Release Science observations made by the WFC3 Scientific Oversight Committee. We are grateful to the Director of the Space Telescope Science Institute for awarding Director's Discretionary Time for this program. We thank B. Burningham for providing unpublished spectra of brown dwarfs, X. Pang and A. Pasquali for providing unpublished information on reddening effects in NGC 3603, and the anonymous referee for his careful reading and useful comments/suggestions. M. A. D. acknowledges the support of the Australian Research Council (ARC) through Discovery projects DP0984657 and DP0664434. We also acknowledge extensive use of the SIMBAD database, operated at CDS Strasbourg, the SpeX Prism Spectral Libraries, maintained by A. Burgasser, and the Multimission Archive at the Space Telescope Science Institute. NR 87 TC 2 Z9 2 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 APR 10 PY 2011 VL 731 IS 1 AR 1 DI 10.1088/0004-637X/731/1/1 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 753KR UT WOS:000289772800001 ER PT J AU Zhu, L Martins, JV Remer, LA AF Zhu, L. Martins, J. V. Remer, L. A. TI Biomass burning aerosol absorption measurements with MODIS using the critical reflectance method SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID REMOTE-SENSING OBSERVATIONS; BLACK CARBON AEROSOLS; MINERAL DUST TYPES; LIGHT-ABSORPTION; HYDROLOGICAL CYCLE; OPTICAL-PROPERTIES; SOUTHERN AFRICA; SKY RADIANCE; CLIMATE; SATELLITE AB This research uses the critical reflectance technique, a space-based remote sensing method, to measure the spatial distribution of aerosol absorption properties over land. Choosing two regions dominated by biomass burning aerosols, a series of sensitivity studies were undertaken to analyze the potential limitations of this method for the type of aerosol to be encountered in the selected study areas, and to show that the retrieved results are relatively insensitive to uncertainties in the assumptions used in the retrieval of smoke aerosol. The critical reflectance technique is then applied to Moderate Resolution Imaging Spectrometer (MODIS) data to retrieve the spectral aerosol single-scattering albedo (SSA) in South African and South American biomass burning events. The retrieved results were validated with collocated Aerosol Robotic Network (AERONET) retrievals. Approximately 67% of the comparisons show a difference between MODIS and AERONET smaller than 0.03, the magnitude of the AERONET uncertainty. The overlap of the two retrievals increases to 88%, allowing for measurement variance in the MODIS retrievals, as well. The ensemble average of MODIS-derived SSA for the Amazon forest station is 0.92 at 670 nm, and 0.84-0.89 for the southern African savanna stations. The critical reflectance technique allows evaluation of the spatial variability of SSA and shows that SSA in South America exhibits higher spatial variation than in South Africa. The accuracy of the retrieved aerosol SSA from MODIS data indicates that this product can help to better understand how aerosols affect the regional and global climate. C1 [Zhu, L.; Martins, J. V.] Univ Maryland Baltimore Cty, Dept Phys, Joint Ctr Earth Syst Technol, Baltimore, MD 21250 USA. [Remer, L. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Zhu, L (reprint author), Univ Maryland Baltimore Cty, Dept Phys, Joint Ctr Earth Syst Technol, 1000 Hilltop Circle, Baltimore, MD 21250 USA. EM zhuli1@umbc.edu; martins@umbc.edu; Lorraine.A.Remer@nasa.gov FU NASA [NNX08AJ78G] FX We would like to thank NASA for funding this project under grant NNX08AJ78G. We also would like to thank the MODIS and AERONET teams for their excellent work on the instrument development, maintenance, and calibration. We thank their effort on data quality control and for providing data to the public, as well. Thanks also go to Kelley Wells, Alexandre Correia, Tom Eck, Tianle Yuan, Ralph Kahn, and the anonymous reviewers for their constructive comments and suggestions. NR 54 TC 12 Z9 12 U1 0 U2 10 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 APR 9 PY 2011 VL 116 AR D07202 DI 10.1029/2010JD015187 PG 15 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 747ZO UT WOS:000289360000002 ER PT J AU Kramer, GY Besse, S Nettles, J Combe, JP Clark, RN Pieters, CM Staid, M Malaret, E Boardman, J Green, RO Head, JW McCord, TB AF Kramer, Georgiana Y. Besse, Sebastien Nettles, Jeffrey Combe, Jean-Philippe Clark, Roger N. Pieters, Carle M. Staid, Matthew Malaret, Erik Boardman, Joseph Green, Robert O. Head, James W., III McCord, Thomas B. TI Newer views of the Moon: Comparing spectra from Clementine and the Moon Mineralogy Mapper SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID ABSOLUTE CALIBRATION; MARE SOILS; REFLECTANCE; TRANSPORT; CRATERS; SURFACE AB The Moon Mineralogy Mapper (M-3) provided the first global hyperspectral data of the lunar surface in 85 bands from 460 to 2980 nm. The Clementine mission provided the first global multispectral maps the lunar surface in 11 spectral bands across the ultraviolet-visible (UV-VIS) and near-infrared (NIR). In an effort to understand how M-3 improves our ability to analyze and interpret lunar data, we compare M-3 spectra with those from Clementine's UV-VIS and NIR cameras. The Clementine mission provided the first global multispectral maps the lunar surface in 11 spectral bands across the UV-VIS and NIR. We have found that M-3 reflectance values are lower across all wavelengths compared with albedos from both of Clementine's UV-VIS and NIR cameras. M-3 spectra show the Moon to be redder, that is, have a steeper continuum slope, than indicated by Clementine. The 1 mu m absorption band depths may be comparable between the instruments, but Clementine data consistently exhibit shallower 2 mu m band depths than M-3. Absorption band minimums are difficult to compare due to the significantly different spectral resolutions. C1 [Kramer, Georgiana Y.; Combe, Jean-Philippe; McCord, Thomas B.] Bear Fight Inst, Winthrop, WA 98862 USA. [Besse, Sebastien] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Nettles, Jeffrey; Pieters, Carle M.; Head, James W., III] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA. [Clark, Roger N.] US Geol Survey, Fed Ctr, Denver, CO 80225 USA. [Staid, Matthew] Planetary Sci Inst, Napa Valley, CA USA. [Malaret, Erik] Appl Coherent Technol, Herndon, VA 20170 USA. [Boardman, Joseph] Analyt Imaging & Geophys LLC, Boulder, CO 80305 USA. [Green, Robert O.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Kramer, GY (reprint author), Bear Fight Inst, 22 Fiddlers Rd,Box 667, Winthrop, WA 98862 USA. EM kramer@lpi.usra.edu OI Besse, Sebastien/0000-0002-1052-5439 NR 34 TC 8 Z9 8 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-PLANET JI J. Geophys. Res.-Planets PD APR 9 PY 2011 VL 116 AR E00G04 DI 10.1029/2010JE003728 PG 11 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 748AD UT WOS:000289361500001 ER PT J AU Xu, LA Samanta, A Costa, MH Ganguly, S Nemani, RR Myneni, RB AF Xu, Liang Samanta, Arindam Costa, Marcos H. Ganguly, Sangram Nemani, Ramakrishna R. Myneni, Ranga B. TI Widespread decline in greenness of Amazonian vegetation due to the 2010 drought SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID RAIN-FORESTS; CLIMATE; INFORMATION; SATELLITE; BIOMASS; DIEBACK; INDEXES; GROWTH; MODEL AB During this decade, the Amazon region has suffered two severe droughts in the short span of five years - 2005 and 2010. Studies on the 2005 drought present a complex, and sometimes contradictory, picture of how these forests have responded to the drought. Now, on the heels of the 2005 drought, comes an even stronger drought in 2010, as indicated by record low river levels in the 109 years of bookkeeping. How has the vegetation in this region responded to this record-breaking drought? Here we report widespread, severe and persistent declines in vegetation greenness, a proxy for photosynthetic carbon fixation, in the Amazon region during the 2010 drought based on analysis of satellite measurements. The 2010 drought, as measured by rainfall deficit, affected an area 1.65 times larger than the 2005 drought - nearly 5 million km(2) of vegetated area in Amazonia. The decline in greenness during the 2010 drought spanned an area that was four times greater (2.4 million km(2)) and more severe than in 2005. Notably, 51% of all drought-stricken forests showed greenness declines in 2010 (1.68 million km(2)) compared to only 14% in 2005 (0.32 million km(2)). These declines in 2010 persisted following the end of the dry season drought and return of rainfall to normal levels, unlike in 2005. Overall, the widespread loss of photosynthetic capacity of Amazonian vegetation due to the 2010 drought may represent a significant perturbation to the global carbon cycle. Citation: Xu, L., A. Samanta, M. H. Costa, S. Ganguly, R. R. Nemani, and R. B. Myneni (2011), Widespread decline in greenness of Amazonian vegetation due to the 2010 drought, Geophys. Res. Lett., 38, L07402, doi:10.1029/2011GL046824. C1 [Xu, Liang; Samanta, Arindam; Myneni, Ranga B.] Boston Univ, Dept Geog & Environm, Boston, MA 02215 USA. [Samanta, Arindam] Atmospher & Environm Res Inc, Lexington, MA 02421 USA. [Costa, Marcos H.] Univ Fed Vicosa, Dept Agr & Environm Engn, BR-36570000 Vicosa, MG, Brazil. [Ganguly, Sangram] NASA, Ames Res Ctr, Bay Area Environm Res Inst, Moffett Field, CA 94035 USA. [Nemani, Ramakrishna R.] NASA, Ames Res Ctr, Biospher Sci Branch, Moffett Field, CA 94035 USA. RP Xu, LA (reprint author), Boston Univ, Dept Geog & Environm, Boston, MA 02215 USA. EM arindam.sam@gmail.com RI Xu, Liang/D-1247-2013; ganguly, sangram/B-5108-2010; Myneni, Ranga/F-5129-2012 FU NASA FX We acknowledge funding from Earth science and Advanced Information Systems Technology programs at NASA. This research was performed using NASA Earth Exchange. NEX combines state-of-the-art supercomputing, Earth system modeling, remote sensing data from NASA and other agencies, and a scientific social networking platform to deliver a complete work environment in which users can explore and analyze large Earth science data sets, run modeling codes, collaborate on new or existing projects, and share results within and/or among communities. Arindam Samanta and Liang Xu contributed equally to this work. NR 27 TC 72 Z9 74 U1 2 U2 37 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD APR 8 PY 2011 VL 38 AR L07402 DI 10.1029/2011GL046824 PG 4 WC Geosciences, Multidisciplinary SC Geology GA 747YM UT WOS:000289357200001 ER PT J AU Pi, XQ Freeman, A Chapman, B Rosen, P Li, ZH AF Pi, Xiaoqing Freeman, Anthony Chapman, Bruce Rosen, Paul Li, Zhenhong TI Imaging ionospheric inhomogeneities using spaceborne synthetic aperture radar SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID LATITUDE; CALIBRATION AB We present a technique and results of 2-D imaging of Faraday rotation and total electron content using spaceborne L band polarimetric synthetic aperture radar (PolSAR). The results are obtained by processing PolSAR data collected using the Phased Array type L-band Synthetic Aperture Radar (PALSAR) on board the Advanced Land Observation Satellite. Distinguished ionospheric inhomogeneities are captured in 2-D images from space with relatively high resolutions of hundreds of meters to a couple of kilometers in auroral-, middle-, and low-latitude regions. The observed phenomena include aurora-associated ionospheric enhancement arcs, the middle- latitude trough, traveling ionospheric disturbances, and plasma bubbles, as well as ionospheric irregularities. These demonstrate a new capability of spaceborne synthetic aperture radar that will not only provide measurements to correction of ionospheric effects in Earth science imagery but also significantly benefit ionospheric studies. C1 [Pi, Xiaoqing; Freeman, Anthony; Chapman, Bruce; Rosen, Paul] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Li, Zhenhong] Univ Glasgow, Dept Geog & Earth Sci, Glasgow G12 8QQ, Lanark, Scotland. RP Pi, XQ (reprint author), CALTECH, Jet Prop Lab, M-S 138-308,4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM xiaoqing.pi@jpl.nasa.gov RI NCEO, COMET+`/A-3443-2013; Li, Zhenhong/F-8705-2010 OI Li, Zhenhong/0000-0002-8054-7449 FU NASA FX The authors thank the Japanese Aerospace and Exploration Agency, the Earth Observation Research Center of Japan, and Masanobu Shimada for providing PALSAR data for this study, and the Alaska Satellite Facility for processing and distributing PALSAR data. The authors also thank the International GNSS Service (IGS) for organizing the IGS GPS networking and archiving, as well as distributing the GPS data that are used in this study, and the Geographical Survey Institute of Japan and Akinori Saito at Kyoto University for providing the GEONET GPS TEC data for this study. The research performed at the Jet Propulsion Laboratory, California Institute of Technology, is under a contract with NASA. NR 24 TC 18 Z9 18 U1 0 U2 2 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD APR 8 PY 2011 VL 116 AR A04303 DI 10.1029/2010JA016267 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 747YR UT WOS:000289357700002 ER PT J AU Beck, PG Bedding, TR Mosser, B Stello, D Garcia, RA Kallinger, T Hekker, S Elsworth, Y Frandsen, S Carrier, F De Ridder, J Aerts, C White, TR Huber, D Dupret, MA Montalban, J Miglio, A Noels, A Chaplin, WJ Kjeldsen, H Christensen-Dalsgaard, J Gilliland, RL Brown, TM Kawaler, SD Mathur, S Jenkins, JM AF Beck, P. G. Bedding, T. R. Mosser, B. Stello, D. Garcia, R. A. Kallinger, T. Hekker, S. Elsworth, Y. Frandsen, S. Carrier, F. De Ridder, J. Aerts, C. White, T. R. Huber, D. Dupret, M-A Montalban, J. Miglio, A. Noels, A. Chaplin, W. J. Kjeldsen, H. Christensen-Dalsgaard, J. Gilliland, R. L. Brown, T. M. Kawaler, S. D. Mathur, S. Jenkins, J. M. TI Kepler Detected Gravity-Mode Period Spacings in a Red Giant Star SO SCIENCE LA English DT Article C1 [Beck, P. G.; Carrier, F.; De Ridder, J.; Aerts, C.] Katholieke Univ Leuven, Inst Sterrenkunde, B-3001 Louvain, Belgium. [Bedding, T. R.; Stello, D.; White, T. R.; Huber, D.] Univ Sydney, Sch Phys, Sydney Inst Astron, Sydney, NSW 2006, Australia. [Mosser, B.] Univ Paris 07, Univ Paris 06, Lab Etud Spatiales & Instrumentat Astrophys, Observ Paris,CNRS, F-92195 Meudon, France. [Garcia, R. A.] Univ Paris Diderot, Lab Astrophys Instrumentat & Modelisat, Inst Rech Lois Fondamentales Univers, Serv Astrophys,Direct Sci Mat,CEA,CNRS,Ctr Saclay, F-91191 Gif Sur Yvette, France. [Kallinger, T.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. [Hekker, S.; Elsworth, Y.; Chaplin, W. J.] Univ Birmingham, Birmingham B15 2TT, W Midlands, England. [Hekker, S.; Frandsen, S.] Univ Amsterdam, Astron Inst, NL-1090 GE Amsterdam, Netherlands. [Kjeldsen, H.; Christensen-Dalsgaard, J.] Aarhus Univ, Dept Phys & Astron, DK-8000 Aarhus C, Denmark. [Aerts, C.] Radboud Univ Nijmegen, Dept Astrophys, Inst Math Astrophys & Particle Phys, NL-6500 GL Nijmegen, Netherlands. [Dupret, M-A; Montalban, J.; Miglio, A.; Noels, A.] Univ Liege, Inst Astrophys & Geophys, B-4000 Liege, Belgium. [Gilliland, R. L.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Brown, T. M.] Las Cumbres Observ Global Telescope, Goleta, CA 93117 USA. [Kawaler, S. D.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. [Mathur, S.] Natl Ctr Atmospher Res, High Altitude Observ, Boulder, CO 80307 USA. [Jenkins, J. M.] NASA, Ames Res Ctr, SETI Inst, Moffett Field, CA 94035 USA. RP Beck, PG (reprint author), Katholieke Univ Leuven, Inst Sterrenkunde, B-3001 Louvain, Belgium. EM paul.beck@ster.kuleuven.be OI Kallinger, Thomas/0000-0003-3627-2561; Bedding, Timothy/0000-0001-5943-1460; Bedding, Tim/0000-0001-5222-4661; Garcia, Rafael/0000-0002-8854-3776; Kawaler, Steven/0000-0002-6536-6367 FU NASA's Science Mission Directorate; European Community, European Research Council [227224] FX We acknowledge the work of the team behind Kepler. Funding for the Kepler mission is provided by NASA's Science Mission Directorate. We received funding from the European Community's 7th Framework Programme, European Research Council grant no. 227224 (PROSPERITY). All authors thank their national funding agencies. NR 4 TC 118 Z9 118 U1 2 U2 7 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 APR 8 PY 2011 VL 332 IS 6026 BP 205 EP 205 DI 10.1126/science.1201939 PG 1 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 746MM UT WOS:000289251100041 PM 21415318 ER PT J AU Chaplin, WJ Kjeldsen, H Christensen-Dalsgaard, J Basu, S Miglio, A Appourchaux, T Bedding, TR Elsworth, Y Garcia, RA Gilliland, RL Girardi, L Houdek, G Karoff, C Kawaler, SD Metcalfe, TS Molenda-Zakowicz, J Monteiro, MJPFG Thompson, MJ Verner, GA Ballot, J Bonanno, A Brandao, IM Broomhall, AM Bruntt, H Campante, TL Corsaro, E Creevey, OL Dogan, G Esch, L Gai, N Gaulme, P Hale, SJ Handberg, R Hekker, S Huber, D Jimenez, A Mathur, S Mazumdar, A Mosser, B New, R Pinsonneault, MH Pricopi, D Quirion, PO Regulo, C Salabert, D Serenelli, AM Aguirre, VS Sousa, SG Stello, D Stevens, IR Suran, MD Uytterhoeven, K White, TR Borucki, WJ Brown, TM Jenkins, JM Kinemuchi, K Van Cleve, J Klaus, TC AF Chaplin, W. J. Kjeldsen, H. Christensen-Dalsgaard, J. Basu, S. Miglio, A. Appourchaux, T. Bedding, T. R. Elsworth, Y. Garcia, R. A. Gilliland, R. L. Girardi, L. Houdek, G. Karoff, C. Kawaler, S. D. Metcalfe, T. S. Molenda-Zakowicz, J. Monteiro, M. J. P. F. G. Thompson, M. J. Verner, G. A. Ballot, J. Bonanno, A. Brandao, I. M. Broomhall, A-M Bruntt, H. Campante, T. L. Corsaro, E. Creevey, O. L. Dogan, G. Esch, L. Gai, N. Gaulme, P. Hale, S. J. Handberg, R. Hekker, S. Huber, D. Jimenez, A. Mathur, S. Mazumdar, A. Mosser, B. New, R. Pinsonneault, M. H. Pricopi, D. Quirion, P-O Regulo, C. Salabert, D. Serenelli, A. M. Aguirre, V. Silva Sousa, S. G. Stello, D. Stevens, I. R. Suran, M. D. Uytterhoeven, K. White, T. R. Borucki, W. J. Brown, T. M. Jenkins, J. M. Kinemuchi, K. Van Cleve, J. Klaus, T. C. TI Ensemble Asteroseismology of Solar-Type Stars with the NASA Kepler Mission SO SCIENCE LA English DT Article ID SUN-LIKE STAR; RED GIANTS; OSCILLATIONS; COROT; AMPLITUDES; ISOCHRONES; RADIUS; CYCLE; DEEP AB In addition to its search for extrasolar planets, the NASA Kepler mission provides exquisite data on stellar oscillations. We report the detections of oscillations in 500 solar-type stars in the Kepler field of view, an ensemble that is large enough to allow statistical studies of intrinsic stellar properties (such as mass, radius, and age) and to test theories of stellar evolution. We find that the distribution of observed masses of these stars shows intriguing differences to predictions from models of synthetic stellar populations in the Galaxy. C1 [Chaplin, W. J.; Miglio, A.; Elsworth, Y.; Verner, G. A.; Broomhall, A-M; Hale, S. J.; Hekker, S.; Stevens, I. R.] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. [Kjeldsen, H.; Christensen-Dalsgaard, J.; Karoff, C.; Bruntt, H.; Campante, T. L.; Dogan, G.; Handberg, R.] Aarhus Univ, Dept Phys & Astron, DK-8000 Aarhus C, Denmark. [Basu, S.; Esch, L.; Gai, N.] Yale Univ, Dept Astron, New Haven, CT 06520 USA. [Miglio, A.] Univ Liege, Dept Astrophys Geophys & Oceanog, B-4000 Liege 1, Belgium. [Appourchaux, T.; Gaulme, P.] Univ Paris 11, CNRS, UMR8617, Inst Astrophys Spatiale, F-91405 Orsay, France. [Bedding, T. R.; Huber, D.; Stello, D.; White, T. R.] Univ Sydney, Sch Phys, Sydney Inst Astron, Sydney, NSW 2006, Australia. [Garcia, R. A.; Uytterhoeven, K.] Univ Paris Diderot, Inst Rech Lois Fondamentales Univers, Lab Astrophys Instrumentat & Modelisat, Direct Sci Mat,CEA,CNRS,Serv Astrophys,Ctr Saclay, F-91191 Gif Sur Yvette, France. [Gilliland, R. L.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Girardi, L.] Ist Nazl Astrofis INAF, Osservatorio Astron Padova, I-35122 Padua, Italy. [Houdek, G.] Univ Vienna, Inst Astron, A-1180 Vienna, Austria. [Kawaler, S. D.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. [Metcalfe, T. S.; Thompson, M. J.; Mathur, S.] Natl Ctr Atmospher Res, High Altitude Observ, Boulder, CO 80307 USA. [Molenda-Zakowicz, J.] Univ Wroclaw, Astron Inst, PL-51622 Wroclaw, Poland. [Monteiro, M. J. P. F. G.; Brandao, I. M.; Campante, T. L.; Sousa, S. G.] Univ Porto, Ctr Astrofis, P-4150762 Oporto, Portugal. [Monteiro, M. J. P. F. G.; Brandao, I. M.; Campante, T. L.; Sousa, S. G.] Univ Porto, Fac Ciencias, P-4150762 Oporto, Portugal. [Verner, G. A.] Univ London, Astron Unit, London E1 4NS, England. [Ballot, J.] Univ Toulouse, CNRS, Inst Rech Astrophys & Planetol, F-31400 Toulouse, France. [Bonanno, A.; Corsaro, E.] INAF Osservatorio Astrofis Catania, I-95123 Catania, Italy. [Creevey, O. L.; Jimenez, A.; Regulo, C.; Salabert, D.] Univ La Laguna, Dept Astrofis, E-38206 Tenerife, Spain. [Creevey, O. L.; Jimenez, A.; Regulo, C.; Salabert, D.] Inst Astrofis Canarias, E-38200 Tenerife, Spain. [Gai, N.] Dezhou Univ, Dept Phys, Dezhou 253023, Peoples R China. [Hekker, S.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1090 GE Amsterdam, Netherlands. [Mazumdar, A.] Homi Bhabha Ctr Sci Educ, Bombay 400088, Maharashtra, India. [Mosser, B.] Univ Paris 07, Univ Paris 06, Lab Etud Spatiales & Instrumentat Astrophys, Observ Paris,CNRS, F-92195 Meudon, France. [New, R.] Sheffield Hallam Univ, Fac Arts Comp Engn & Sci, Mat Engn Res Inst, Sheffield S1 1WB, S Yorkshire, England. [Pinsonneault, M. H.] Ohio State Univ, Dept Astron, McPherson Lab 4055, Columbus, OH 43210 USA. [Pricopi, D.; Suran, M. D.] Acad Romana, Astron Inst, RO-40557 Bucharest, Romania. [Quirion, P-O] Canadian Space Agcy, St Hubert, PQ J3Y 8Y9, Canada. [Serenelli, A. M.] Fac Ciencies, Inst Estudis Espacials Catalunya, Inst Ciencias Espacio, Bellaterra 08193, Spain. [Aguirre, V. Silva] Max Planck Inst Astrophys, D-85741 Garching, Germany. [Borucki, W. J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Brown, T. M.] Las Cumbres Observ Global Telescope, Goleta, CA 93117 USA. [Jenkins, J. M.; Van Cleve, J.] NASA, Ames Res Ctr, SETI Inst, Moffett Field, CA 94035 USA. [Kinemuchi, K.] NASA, Ames Res Ctr, Bay Area Environm Res Inst, Moffett Field, CA 94035 USA. [Klaus, T. C.] NASA, Ames Res Ctr, Orbital Sci Corp, Moffett Field, CA 94035 USA. RP Chaplin, WJ (reprint author), Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. EM w.j.chaplin@bham.ac.uk RI Ballot, Jerome/G-1019-2010; PRICOPI, Dumitru/C-4358-2011; Mazumdar, Anwesh/B-1588-2012; Sousa, Sergio/I-7466-2013; Brandao, Isa/M-5172-2013; Monteiro, Mario J.P.F.G./B-4715-2008; Basu, Sarbani/B-8015-2014; Hale, Steven/E-3472-2015 OI Bedding, Timothy/0000-0001-5943-1460; Metcalfe, Travis/0000-0003-4034-0416; Karoff, Christoffer/0000-0003-2009-7965; Bedding, Tim/0000-0001-5222-4661; Garcia, Rafael/0000-0002-8854-3776; Serenelli, Aldo/0000-0001-6359-2769; Handberg, Rasmus/0000-0001-8725-4502; Kawaler, Steven/0000-0002-6536-6367; Mazumdar, Anwesh/0000-0003-2409-2942; Bonanno, Alfio/0000-0003-3175-9776; Sousa, Sergio/0000-0001-9047-2965; Brandao, Isa/0000-0002-1153-0942; Monteiro, Mario J.P.F.G./0000-0003-0513-8116; Basu, Sarbani/0000-0002-6163-3472; Hale, Steven/0000-0002-6402-8382 FU NASA's Science Mission Directorate FX Kepler is a NASA discovery class mission, which was launched in March 2009 and whose funding is provided by NASA's Science Mission Directorate. The authors thank the entire Kepler team, without whom these results would not be possible. The asteroseismology program of Kepler is being conducted by the Kepler Asteroseismic Science Consortium. NR 32 TC 174 Z9 175 U1 2 U2 27 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 APR 8 PY 2011 VL 332 IS 6026 BP 213 EP 216 DI 10.1126/science.1201827 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 746MM UT WOS:000289251100044 PM 21474754 ER PT J AU Derekas, A Kiss, LL Borkovits, T Huber, D Lehmann, H Southworth, J Bedding, TR Balam, D Hartmann, M Hrudkova, M Ireland, MJ Kovacs, J Mezo, G Moor, A Niemczura, E Sarty, GE Szabo, GM Szabo, R Telting, JH Tkachenko, A Uytterhoeven, K Benko, JM Bryson, ST Maestro, V Simon, AE Stello, D Schaefer, G Aerts, C ten Brummelaar, TA De Cat, P McAlister, HA Maceroni, C Merand, A Still, M Sturmann, J Sturmann, L Turner, N Tuthill, PG Christensen-Dalsgaard, J Gilliland, RL Kjeldsen, H Quintana, EV Tenenbaum, P Twicken, JD AF Derekas, A. Kiss, L. L. Borkovits, T. Huber, D. Lehmann, H. Southworth, J. Bedding, T. R. Balam, D. Hartmann, M. Hrudkova, M. Ireland, M. J. Kovacs, J. Mezo, Gy. Moor, A. Niemczura, E. Sarty, G. E. Szabo, Gy. M. Szabo, R. Telting, J. H. Tkachenko, A. Uytterhoeven, K. Benko, J. M. Bryson, S. T. Maestro, V. Simon, A. E. Stello, D. Schaefer, G. Aerts, C. ten Brummelaar, T. A. De Cat, P. McAlister, H. A. Maceroni, C. Merand, A. Still, M. Sturmann, J. Sturmann, L. Turner, N. Tuthill, P. G. Christensen-Dalsgaard, J. Gilliland, R. L. Kjeldsen, H. Quintana, E. V. Tenenbaum, P. Twicken, J. D. TI HD 181068: A Red Giant in a Triply Eclipsing Compact Hierarchical Triple System SO SCIENCE LA English DT Article ID STARS; BINARIES; SCIENCE AB Hierarchical triple systems comprise a close binary and a more distant component. They are important for testing theories of star formation and of stellar evolution in the presence of nearby companions. We obtained 218 days of Kepler photometry of HD 181068 (magnitude of 7.1), supplemented by ground-based spectroscopy and interferometry, which show it to be a hierarchical triple with two types of mutual eclipses. The primary is a red giant that is in a 45-day orbit with a pair of red dwarfs in a close 0.9-day orbit. The red giant shows evidence for tidally induced oscillations that are driven by the orbital motion of the close pair. HD 181068 is an ideal target for studies of dynamical evolution and testing tidal friction theories in hierarchical triple systems. C1 [Derekas, A.] Eotvos Lorand Univ, Dept Astron, Budapest, Hungary. [Derekas, A.; Kiss, L. L.; Mezo, Gy.; Moor, A.; Szabo, Gy. M.; Szabo, R.; Benko, J. M.; Simon, A. E.] Hungarian Acad Sci, Konkoly Observ Budapest, H-1525 Budapest, Hungary. [Kiss, L. L.; Huber, D.; Bedding, T. R.; Ireland, M. J.; Maestro, V.; Stello, D.; Tuthill, P. G.] Univ Sydney, Sch Phys, Sydney Inst Astron, Sydney, NSW 2006, Australia. [Borkovits, T.] Baja Astron Observ, H-6500 Baja, Hungary. [Borkovits, T.] Eotvos Jozsef Coll, H-6500 Baja, Hungary. [Lehmann, H.; Hartmann, M.; Hrudkova, M.; Tkachenko, A.] Thuringer Landessternwarte TLS Tautenburg, Karl Schwarzschild Observ, D-07778 Tautenburg, Germany. [Southworth, J.] Univ Keele, Astrophys Grp, Newcastle Under Lyme ST5 5BG, Staffs, England. [Balam, D.] Dominion Astrophys Observ, Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada. [Kovacs, J.] Eotvos Lorand Univ, Gothard Observ, H-9704 Szombathely, Hungary. [Niemczura, E.] Univ Wroclaw, Astron Inst, PL-51622 Wroclaw, Poland. [Sarty, G. E.] Univ Saskatchewan, Dept Phys & Engn Phys, Saskatoon, SK S7N 5A5, Canada. [Telting, J. H.] Nord Opt Telescope, Santa Cruz De La Palma 38700, Spain. [Uytterhoeven, K.] Univ Paris Diderot, Lab Astrophys Instrumentat & Modelisat, Inst Rech Lois Fondamentales Univers, Direct Sci Mat,CEA,CNRS,Serv Astrophys, F-91191 Gif Sur Yvette, France. [Uytterhoeven, K.] Kiepenheuer Inst Sonnenphys, D-79104 Freiburg, Germany. [Bryson, S. T.; Still, M.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Schaefer, G.; ten Brummelaar, T. A.; McAlister, H. A.; Sturmann, J.; Sturmann, L.; Turner, N.] Georgia State Univ, Ctr High Angular Resolut Astron, Atlanta, GA 30302 USA. [Aerts, C.] Katholieke Univ Leuven, Inst Sterrenkunde, B-3001 Louvain, Belgium. [Aerts, C.] Radboud Univ Nijmegen, Dept Astrophys, IMAPP, NL-6500 GL Nijmegen, Netherlands. [De Cat, P.] Royal Observ Belgium, B-1180 Brussels, Belgium. [Maceroni, C.] Osserv Astron Roma, Ist Nazl Astrofis INAF, I-00040 Monteporzio C, Italy. [Merand, A.] European So Observ, Santiago 19, Chile. [Christensen-Dalsgaard, J.; Kjeldsen, H.] Aarhus Univ, Dept Phys & Astron, DK-8000 Aarhus C, Denmark. [Gilliland, R. L.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Quintana, E. V.; Tenenbaum, P.; Twicken, J. D.] SETI Inst, Moffett Field, CA 94035 USA. RP Derekas, A (reprint author), Eotvos Lorand Univ, Dept Astron, Budapest, Hungary. EM derekas@konkoly.hu RI Szabo, Gyula/A-8310-2012; Derekas, Aliz/G-2091-2016; OI Derekas, Aliz/0000-0002-6526-9444; Sarty, Gordon/0000-0001-5516-7869; Benko, Jozsef/0000-0003-3851-6603; Bedding, Timothy/0000-0001-5943-1460; Szabo, Robert/0000-0002-3258-1909; Bedding, Tim/0000-0001-5222-4661 FU NASA's Science Mission Directorate; Hungarian Scientific Research Fund (OTKA) [K76816, K83790, MB08C 81013]; Hungarian Academy of Sciences; Magyary Zoltan Higher Educational Public Foundation; American Astronomical Society; NSF [AST09-08253]; W. M. Keck Foundation; NASA Exoplanet Science Center; Deutsche Forschungsgemeinschaft [HA 3279/5-1]; European Research Council (ERC) under the European Community [227224] FX A.D. is a Magyary Zoltan Postdoctoral Research Fellow. Funding for this Discovery mission is provided by NASA's Science Mission Directorate. The authors gratefully acknowledge the entire Kepler team, whose outstanding efforts have made these results possible. This project has been supported by Hungarian Scientific Research Fund (OTKA) grants K76816, K83790, and MB08C 81013; the "Lendulet" Program of the Hungarian Academy of Sciences; and the Magyary Zoltan Higher Educational Public Foundation. The DAO observations were supported by an American Astronomical Society Small Research Grant. The CHARA Array is owned by Georgia State University. Additional funding for the CHARA Array is provided by NSF under grant AST09-08253, the W. M. Keck Foundation, and the NASA Exoplanet Science Center. TLS observations were done as a part of the Deutsche Forschungsgemeinschaft grant HA 3279/5-1. For her research, C. A. received funding from the European Research Council (ERC) under the European Community's Seventh Framework Programme (FP7/2007-2013)/ERC grant agreement no. 227224 (Prosperity). NR 19 TC 51 Z9 51 U1 1 U2 4 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 APR 8 PY 2011 VL 332 IS 6026 BP 216 EP 218 DI 10.1126/science.1201762 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 746MM UT WOS:000289251100045 PM 21474755 ER PT J AU Lin, RQ Kuang, WJ AF Lin, Ray-Qing Kuang, Weijia TI A fully nonlinear, dynamically consistent numerical model for solid-body ship motion. I. Ship motion with fixed heading SO PROCEEDINGS OF THE ROYAL SOCIETY A-MATHEMATICAL PHYSICAL AND ENGINEERING SCIENCES LA English DT Article DE ship motion; nonlinearity; hydrodynamics; solid body; numerical model ID WAVES AB In this paper, we describe the details of our numerical model for simulating ship solid-body motion in a given environment. In this model, the fully nonlinear dynamical equations governing the time-varying solid-body ship motion under the forces arising from ship-wave interactions are solved with given initial conditions. The net force and moment (torque) on the ship body are directly calculated via integration of the hydrodynamic pressure over the wetted surface and the buoyancy effect from the underwater volume of the actual ship hull with a hybrid finite-difference/finite-element method. Neither empirical nor free parametrization is introduced in this model, i.e. no a priori experimental data are needed for modelling. This model is benchmarked with many experiments of various ship hulls for heave, roll and pitch motion. In addition to the benchmark cases, numerical experiments are also carried out for strongly nonlinear ship motion with a fixed heading. These new cases demonstrate clearly the importance of nonlinearities in ship motion modelling. C1 [Lin, Ray-Qing] NSWCCD, Carderock Div, Bethesda, MD USA. [Kuang, Weijia] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Lin, RQ (reprint author), NSWCCD, Carderock Div, Bethesda, MD USA. EM ray.lin@navy.mil RI Kuang, Weijia/K-5141-2012 OI Kuang, Weijia/0000-0001-7786-6425 FU David Taylor Model Basin, Carderock Division; NASA ESIP; MFRP FX R.L. is supported by ILIR programme from the David Taylor Model Basin, Carderock Division. W. K. is supported by NASA ESIP and MFRP. We thank T. Applebee and J. Gorski of the David Taylor Model Basin, Hydromechanics Department for their help on this work. NR 26 TC 5 Z9 5 U1 0 U2 1 PU ROYAL SOC PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 1364-5021 J9 P ROY SOC A-MATH PHY JI Proc. R. Soc. A-Math. Phys. Eng. Sci. PD APR 8 PY 2011 VL 467 IS 2128 BP 911 EP 927 DI 10.1098/rspa.2010.0310 PG 17 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 726OX UT WOS:000287735600001 ER PT J AU Qu, TD Gao, S Fukumori, I AF Qu, Tangdong Gao, Shan Fukumori, Ichiro TI What governs the North Atlantic salinity maximum in a global GCM? SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID SEA-SURFACE SALINITY; TROPICAL ATLANTIC; MIXED-LAYER; OCEAN; MODEL; TRENDS; CLIMATOLOGY; VARIABILITY AB Taking advantage of the rapid advance in ocean modeling, this study investigates the sea surface salinity maximum in the North Atlantic, using results from a model of the Consortium for Estimating the Circulation and Climate of the Ocean (ECCO). Salinity budget terms were computed at the model's integration time step and archived as monthly averages. The simulated mixed layer salinity budget provides the first quantitative evidence for the ocean's role in governing the sea surface salinity maximum in the North Atlantic. Our analysis reveals that ocean dynamics explains about half of the sea surface salinity variance, being of equal importance as surface forcing. The sea surface salinity maximum varies both seasonally and interannually, as a consequence of interplay among surface flux, advection, and vertical entrainment. Contribution from eddies and small-scale processes is relatively weak but not negligible. These results may provide useful hints for the design and interpretation of future observations in the region. Citation: Qu, T., S. Gao, and I. Fukumori (2011), What governs the North Atlantic salinity maximum in a global GCM?, Geophys. Res. Lett., 38, L07602, doi:10.1029/2011GL046757. C1 [Qu, Tangdong] Univ Hawaii Manoa, SOEST, Int Pacific Res Ctr, Honolulu, HI 96822 USA. [Gao, Shan] Chinese Acad Sci, Inst Oceanol, Qingdao 266071, Shandong, Peoples R China. [Fukumori, Ichiro] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Qu, TD (reprint author), Univ Hawaii Manoa, SOEST, Int Pacific Res Ctr, 1680 East West Rd, Honolulu, HI 96822 USA. EM tangdong@hawaii.edu RI Gao, Shan/H-7959-2013 OI Gao, Shan/0000-0003-4510-5028 FU NASA; JAMSTEC; NOAA; National Science Foundation of China [40876011] FX This research was supported by NASA as part of the Aquarius Science Team investigation. Additional support for T. Qu was provided by JAMSTEC, NASA, and NOAA through their sponsorship of research activities at the IPRC. S. Gao was supported by the National Science Foundation of China through grant 40876011. The authors are grateful to F. Bingham, L. Yu, A. Gordon, P. Hacker, and E. Lindstrom for valuable discussions and to two anonymous reviewers for thoughtful comments on the manuscript. SOEST contribution 8104 and IPRC contribution IPRC-763. NR 28 TC 28 Z9 29 U1 1 U2 8 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 APR 7 PY 2011 VL 38 AR L07602 DI 10.1029/2011GL046757 PG 6 WC Geosciences, Multidisciplinary SC Geology GA 747YK UT WOS:000289357000001 ER PT J AU Martini, M Allen, DJ Pickering, KE Stenchikov, GL Richter, A Hyer, EJ Loughner, CP AF Martini, Matus Allen, Dale J. Pickering, Kenneth E. Stenchikov, Georgiy L. Richter, Andreas Hyer, Edward J. Loughner, Christopher P. TI The impact of North American anthropogenic emissions and lightning on long-range transport of trace gases and their export from the continent during summers 2002 and 2004 SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID TROPOSPHERIC OZONE PRODUCTION; OPTICAL TRANSIENT DETECTOR; REGIONAL AIR-POLLUTION; EASTERN UNITED-STATES; VERTICAL-DISTRIBUTION; GENERATED NOX; SURFACE OZONE; SCALE-MODEL; STERAO-A; CHEMISTRY AB We analyze the contribution of North American (NA) lightning and anthropogenic emissions to ozone concentrations, radiative forcing, and export fluxes from North America during summers 2002 and 2004 using the University of Maryland Chemical Transport Model (UMD-CTM) driven by GEOS-4 reanalysis. Reduced power plant emissions (NOx SIP Call) and cooler temperatures in 2004 compared to 2002 resulted in lower ambient ozone concentrations over the eastern United States. Lightning flash rates in early summer 2004 were 50% higher than 2002 over the United States. Over the North Atlantic, changes in ozone column between early summer 2002 and 2004 due to changes in lightning and meteorology exceeded the change due to emission reductions by a factor of 7. Late summer changes in lightning had a much smaller impact on ozone columns. In summer 2004, net downward radiative flux at the tropopause due to ozone produced from anthropogenic emissions ranged from 0.15 to 0.30 W m(-2) across the North Atlantic, while that due to ozone produced from lightning NO emissions ranged from 0.20 to 0.50 W m(-2). Enhanced lofting of polluted air followed by stronger westerly winds led to more net export of NOx, NOy, and ozone in early summer 2004 than 2002 despite reduced anthropogenic emissions. Ozone export fluxes across the eastern NA boundary due to anthropogenic emissions were factors of 1.6 and 2 larger than those due to lightning in 2004 and 2002, respectively. Doubling the NA lightning NO source increased downwind ozone enhancements due to lightning NO emissions by one third. C1 [Martini, Matus; Allen, Dale J.; Loughner, Christopher P.] Univ Maryland, Dept Atmospher & Ocean Sci, College Pk, MD 20742 USA. [Hyer, Edward J.] USN, UCAR Visiting Scientist Program, Res Lab, Monterey, CA 93943 USA. [Pickering, Kenneth E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Richter, Andreas] Univ Bremen, Inst Environm Phys, D-28359 Bremen, Germany. [Stenchikov, Georgiy L.] Rutgers State Univ, Dept Environm Sci, New Brunswick, NJ 08901 USA. [Stenchikov, Georgiy L.] King Abdullah Univ Sci & Technol, Thuwal, Saudi Arabia. RP Martini, M (reprint author), Univ Maryland, Dept Atmospher & Ocean Sci, College Pk, MD 20742 USA. EM martini@atmos.umd.edu RI Hyer, Edward/E-7734-2011; Pickering, Kenneth/E-6274-2012; Georgiy, Stenchikov/J-8569-2013; Richter, Andreas/C-4971-2008; Allen, Dale/F-7168-2010; OI Hyer, Edward/0000-0001-8636-2026; Loughner, Christopher/0000-0002-3833-2014; Richter, Andreas/0000-0003-3339-212X; Allen, Dale/0000-0003-3305-9669; Stenchikov, Georgiy Lvovich/0000-0001-9033-4925; Martini, Matus/0000-0003-0459-4988 FU NASA [NNG04GD32G, NNG06GE01G, NNG06GB52G] FX This work was funded under NASA grants NNG04GD32G and NNG06GE01G (Interdisciplinary Science Investigation) and under NASA grant NNG06GB52G from the Tropospheric Chemistry Program. Model simulations have been conducted at NCCS at NASA Goddard Space Flight Center. We thank the INTEX-A science team for the aircraft measurements and Anne Thompson for IONS measurements. The NLDN data were collected by Vaisala, Inc., and archived by NASA Marshall Space Flight Center. OTD/LIS data were processed by NASA Marshall. We thank Owen Cooper for the IC/CG ratios prepared by Dennis Boccippio. We thank Arlene Fiore and two anonymous reviewers for their helpful comments. We also thank Ross Salawitch and Amanda Evans for their revisions and comments. NR 90 TC 6 Z9 6 U1 1 U2 17 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD APR 7 PY 2011 VL 116 AR D07305 DI 10.1029/2010JD014305 PG 22 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 747ZN UT WOS:000289359900001 ER PT J AU Abbasi, R Abdou, Y Abu-Zayyad, T Adams, J Aguilar, JA Ahlers, M Andeen, K Auffenberg, J Bai, X Baker, M Barwick, SW Bay, R Alba, JLB Beattie, K Beatty, JJ Bechet, S Becker, JK Becker, KH Benabderrahmane, ML BenZvi, S Berdermann, J Berghaus, P Berley, D Bernardini, E Bertrand, D Besson, DZ Bindig, D Bissok, M Blaufuss, E Blumenthal, J Boersma, DJ Bohm, C Bose, D Boser, S Botner, O Braun, J Brown, AM Buitink, S Carson, M Chirkin, D Christy, B Clem, J Clevermann, F Cohen, S Colnard, C Cowen, DF D'Agostino, MV Danninger, M Daughhetee, J Davis, JC De Clercq, C Demirors, L Depaepe, O Descamps, F Desiati, P de Vries-Uiterweerd, G DeYoung, T Diaz-Velez, JC Dierckxsens, M Dreyer, J Dumm, JP Ehrlich, R Eisch, J Ellsworth, RW Engdegard, O Euler, S Evenson, PA Fadiran, O Fazely, AR Fedynitch, A Feusels, T Filimonov, K Finley, C Fischer-Wasels, T Foerster, MM Fox, BD Franckowiak, A Franke, R Gaisser, TK Gallagher, J Geisler, M Gerhardt, L Gladstone, L Glusenkamp, T Goldschmidt, A Goodman, JA Grant, D Griesel, T Gross, A Grullon, S Gurtner, M Ha, C Hallgren, A Halzen, F Han, K Hanson, K Heinen, D Helbing, K Herquet, P Hickford, S Hill, GC Hoffman, KD Homeier, A Hoshina, K Hubert, D Huelsnitz, W Hulss, JP Hulth, PO Hultqvist, K Hussain, S Ishihara, A Jacobsen, J Japaridze, GS Johansson, H Joseph, JM Kampert, KH Kappes, A Karg, T Karle, A Kelley, JL Kemming, N Kenny, P Kiryluk, J Kislat, F Klein, SR Kohne, JH Kohnen, G Kolanoski, H Kopke, L Kopper, S Koskinen, DJ Kowalski, M Kowarik, T Krasberg, M Krings, T Kroll, G Kuehn, K Kuwabara, T Labare, M Lafebre, S Laihem, K Landsman, H Larson, MJ Lauer, R Lehmann, R Lunemann, J Madsen, J Majumdar, P Marotta, A Maruyama, R Mase, K Matis, HS Meagher, K Merck, M Meszaros, P Meures, T Middell, E Milke, N Miller, J Montaruli, T Morse, R Movit, SM Nahnhauer, R Nam, JW Naumann, U Niessen, P Nygren, DR Odrowski, S Olivas, A Olivo, M O'Murchadha, A Ono, M Panknin, S Paul, L de los Heros, CP Petrovic, J Piegsa, A Pieloth, D Porrata, R Posselt, J Price, PB Prikockis, M Przybylski, GT Rawlins, K Redl, P Resconi, E Rhode, W Ribordy, M Rizzo, A Rodrigues, JP Roth, P Rothmaier, F Rott, C Ruhe, T Rutledge, D Ruzybayev, B Ryckbosch, D Sander, HG Santander, M Sarkar, S Schatto, K Schmidt, T Schoenwald, A Schukraft, A Schultes, A Schulz, O Schunck, M Seckel, D Semburg, B Seo, SH Sestayo, Y Seunarine, S Silvestri, A Slipak, A Spiczak, GM Spiering, C Stamatikos, M Stanev, T Stephens, G Stezelberger, T Stokstad, RG Stoyanov, S Strahler, EA Straszheim, T Sullivan, GW Swillens, Q Taavola, H Taboada, I Tamburro, A Tarasova, O Tepe, A Ter-Antonyan, S Tilav, S Toale, PA Toscano, S Tosi, D Turcan, D van Eijndhoven, N Vandenbroucke, J Van Overloop, A van Santen, J Vehring, M Voge, M Voigt, B Walck, C Waldenmaier, T Wallraff, M Walter, M Weaver, C Wendt, C Westerhoff, S Whitehorn, N Wiebe, K Wiebusch, CH Williams, DR Wischnewski, R Wissing, H Wolf, M Woschnagg, K Xu, C Xu, XW Yodh, G Yoshida, S Zarzhitsky, P AF Abbasi, R. Abdou, Y. Abu-Zayyad, T. Adams, J. Aguilar, J. A. Ahlers, M. Andeen, K. Auffenberg, J. Bai, X. Baker, M. Barwick, S. W. Bay, R. Alba, J. L. Bazo Beattie, K. Beatty, J. J. Bechet, S. Becker, J. K. Becker, K. -H. Benabderrahmane, M. L. BenZvi, S. Berdermann, J. Berghaus, P. Berley, D. Bernardini, E. Bertrand, D. Besson, D. Z. Bindig, D. Bissok, M. Blaufuss, E. Blumenthal, J. Boersma, D. J. Bohm, C. Bose, D. Boeser, S. Botner, O. Braun, J. Brown, A. M. Buitink, S. Carson, M. Chirkin, D. Christy, B. Clem, J. Clevermann, F. Cohen, S. Colnard, C. Cowen, D. F. D'Agostino, M. V. Danninger, M. Daughhetee, J. Davis, J. C. De Clercq, C. Demiroers, L. Depaepe, O. Descamps, F. Desiati, P. de Vries-Uiterweerd, G. DeYoung, T. Diaz-Velez, J. C. Dierckxsens, M. Dreyer, J. Dumm, J. P. Ehrlich, R. Eisch, J. Ellsworth, R. W. Engdegard, O. Euler, S. Evenson, P. A. Fadiran, O. Fazely, A. R. Fedynitch, A. Feusels, T. Filimonov, K. Finley, C. Fischer-Wasels, T. Foerster, M. M. Fox, B. D. Franckowiak, A. Franke, R. Gaisser, T. K. Gallagher, J. Geisler, M. Gerhardt, L. Gladstone, L. Gluesenkamp, T. Goldschmidt, A. Goodman, J. A. Grant, D. Griesel, T. Gross, A. Grullon, S. Gurtner, M. Ha, C. Hallgren, A. Halzen, F. Han, K. Hanson, K. Heinen, D. Helbing, K. Herquet, P. Hickford, S. Hill, G. C. Hoffman, K. D. Homeier, A. Hoshina, K. Hubert, D. Huelsnitz, W. Huelss, J. -P. Hulth, P. O. Hultqvist, K. Hussain, S. Ishihara, A. Jacobsen, J. Japaridze, G. S. Johansson, H. Joseph, J. M. Kampert, K. -H. Kappes, A. Karg, T. Karle, A. Kelley, J. L. Kemming, N. Kenny, P. Kiryluk, J. Kislat, F. Klein, S. R. Koehne, J. -H. Kohnen, G. Kolanoski, H. Koepke, L. Kopper, S. Koskinen, D. J. Kowalski, M. Kowarik, T. Krasberg, M. Krings, T. Kroll, G. Kuehn, K. Kuwabara, T. Labare, M. Lafebre, S. Laihem, K. Landsman, H. Larson, M. J. Lauer, R. Lehmann, R. Luenemann, J. Madsen, J. Majumdar, P. Marotta, A. Maruyama, R. Mase, K. Matis, H. S. Meagher, K. Merck, M. Meszaros, P. Meures, T. Middell, E. Milke, N. Miller, J. Montaruli, T. Morse, R. Movit, S. M. Nahnhauer, R. Nam, J. W. Naumann, U. Niessen, P. Nygren, D. R. Odrowski, S. Olivas, A. Olivo, M. O'Murchadha, A. Ono, M. Panknin, S. Paul, L. de los Heros, C. Perez Petrovic, J. Piegsa, A. Pieloth, D. Porrata, R. Posselt, J. Price, P. B. Prikockis, M. Przybylski, G. T. Rawlins, K. Redl, P. Resconi, E. Rhode, W. Ribordy, M. Rizzo, A. Rodrigues, J. P. Roth, P. Rothmaier, F. Rott, C. Ruhe, T. Rutledge, D. Ruzybayev, B. Ryckbosch, D. Sander, H. -G. Santander, M. Sarkar, S. Schatto, K. Schmidt, T. Schoenwald, A. Schukraft, A. Schultes, A. Schulz, O. Schunck, M. Seckel, D. Semburg, B. Seo, S. H. Sestayo, Y. Seunarine, S. Silvestri, A. Slipak, A. Spiczak, G. M. Spiering, C. Stamatikos, M. Stanev, T. Stephens, G. Stezelberger, T. Stokstad, R. G. Stoyanov, S. Strahler, E. A. Straszheim, T. Sullivan, G. W. Swillens, Q. Taavola, H. Taboada, I. Tamburro, A. Tarasova, O. Tepe, A. Ter-Antonyan, S. Tilav, S. Toale, P. A. Toscano, S. Tosi, D. Turcan, D. van Eijndhoven, N. Vandenbroucke, J. Van Overloop, A. van Santen, J. Vehring, M. Voge, M. Voigt, B. Walck, C. Waldenmaier, T. Wallraff, M. Walter, M. Weaver, C. Wendt, C. Westerhoff, S. Whitehorn, N. Wiebe, K. Wiebusch, C. H. Williams, D. R. Wischnewski, R. Wissing, H. Wolf, M. Woschnagg, K. Xu, C. Xu, X. W. Yodh, G. Yoshida, S. Zarzhitsky, P. TI Limits on Neutrino Emission from Gamma-Ray Bursts with the 40 String IceCube Detector SO PHYSICAL REVIEW LETTERS LA English DT Article ID HIGH-ENERGY NEUTRINOS; MUON NEUTRINOS; SEARCH; AMANDA AB IceCube has become the first neutrino telescope with a sensitivity below the TeV neutrino flux predicted from gamma-ray bursts if gamma-ray bursts are responsible for the observed cosmic-ray flux above 10(18) eV. Two separate analyses using the half-complete IceCube detector, one a dedicated search for neutrinos from p gamma interactions in the prompt phase of the gamma-ray burst fireball and the other a generic search for any neutrino emission from these sources over a wide range of energies and emission times, produced no evidence for neutrino emission, excluding prevailing models at 90% confidence. C1 [Berley, D.; Blaufuss, E.; Christy, B.; Ehrlich, R.; Ellsworth, R. W.; Goodman, J. A.; Hoffman, K. D.; Huelsnitz, W.; Meagher, K.; Olivas, A.; Redl, P.; Roth, P.; Schmidt, T.; Straszheim, T.; Sullivan, G. W.; Turcan, D.; Wissing, H.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA. [Bissok, M.; Blumenthal, J.; Boersma, D. J.; Euler, S.; Geisler, M.; Gluesenkamp, T.; Heinen, D.; Huelss, J. -P.; Krings, T.; Laihem, K.; Meures, T.; Paul, L.; Schukraft, A.; Schunck, M.; Vehring, M.; Wallraff, M.; Wiebusch, C. H.] Rhein Westfal TH Aachen, Inst Phys 3, D-52056 Aachen, Germany. [Williams, D. R.; Zarzhitsky, P.] Univ Alabama, Dept Phys & Astron, Tuscaloosa, AL 35487 USA. [Rawlins, K.] Univ Alaska Anchorage, Dept Phys & Astron, Anchorage, AK 99508 USA. [Fadiran, O.; Japaridze, G. S.] Clark Atlanta Univ, CTSPS, Atlanta, GA 30314 USA. [Daughhetee, J.; Taboada, I.; Tepe, A.] Georgia Inst Technol, Sch Phys, Atlanta, GA 30332 USA. [Daughhetee, J.; Taboada, I.; Tepe, A.] Georgia Inst Technol, Ctr Relativist Astrophys, Atlanta, GA 30332 USA. [Fazely, A. R.; Ter-Antonyan, S.; Xu, X. W.] So Univ, Dept Phys, Baton Rouge, LA 70813 USA. [Bay, R.; D'Agostino, M. V.; Filimonov, K.; Gerhardt, L.; Kiryluk, J.; Klein, S. R.; Porrata, R.; Price, P. B.; Vandenbroucke, J.; Woschnagg, K.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Beattie, K.; Buitink, S.; Gerhardt, L.; Goldschmidt, A.; Joseph, J. M.; Kiryluk, J.; Klein, S. R.; Matis, H. S.; Nygren, D. R.; Przybylski, G. T.; Stezelberger, T.; Stokstad, R. G.] Univ Calif Berkeley, Lawrence Berkeley Lab, Berkeley, CA 94720 USA. [Kappes, A.; Kemming, N.; Kolanoski, H.; Lehmann, R.; Waldenmaier, T.] Humboldt Univ, Inst Phys, D-12489 Berlin, Germany. [Becker, J. K.; Dreyer, J.; Fedynitch, A.; Olivo, M.] Ruhr Univ Bochum, Fak Phys & Astron, D-44780 Bochum, Germany. [Boeser, S.; Franckowiak, A.; Homeier, A.; Kowalski, M.; Panknin, S.] Univ Bonn, Inst Phys, D-53115 Bonn, Germany. [Seunarine, S.] Univ W Indies, Dept Phys, BB-11000 Bridgetown, Barbados. [Bechet, S.; Bertrand, D.; Dierckxsens, M.; Hanson, K.; Marotta, A.; Petrovic, J.; Swillens, Q.] Univ Libre Brussels, Fac Sci, B-1050 Brussels, Belgium. [Bose, D.; De Clercq, C.; Depaepe, O.; Hubert, D.; Labare, M.; Rizzo, A.; Strahler, E. A.; van Eijndhoven, N.] Vrije Univ Brussel, Dienst ELEM, B-1050 Brussels, Belgium. [Ishihara, A.; Mase, K.; Ono, M.; Yoshida, S.] Chiba Univ, Dept Phys, Chiba 2638522, Japan. [Adams, J.; Brown, A. M.; Gross, A.; Han, K.; Hickford, S.] Univ Canterbury, Dept Phys & Astron, Christchurch 1, New Zealand. [Beatty, J. J.; Davis, J. C.; Kuehn, K.; Rott, C.; Stamatikos, M.] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA. [Beatty, J. J.; Davis, J. C.; Kuehn, K.; Rott, C.; Stamatikos, M.] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA. [Beatty, J. J.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Clevermann, F.; Koehne, J. -H.; Milke, N.; Pieloth, D.; Rhode, W.; Ruhe, T.] TU Dortmund Univ, Dept Phys, D-44221 Dortmund, Germany. [Grant, D.] Univ Alberta, Dept Phys, Edmonton, AB T6G 2G7, Canada. [Abdou, Y.; Carson, M.; Descamps, F.; de Vries-Uiterweerd, G.; Feusels, T.; Ryckbosch, D.; Van Overloop, A.] Univ Ghent, Dept Subatom & Radiat Phys, B-9000 Ghent, Belgium. [Colnard, C.; Gross, A.; Odrowski, S.; Resconi, E.; Schulz, O.; Sestayo, Y.; Voge, M.; Wolf, M.] Max Planck Inst Kernphys, D-69177 Heidelberg, Germany. [Barwick, S. W.; Nam, J. W.; Silvestri, A.; Yodh, G.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. [Cohen, S.; Demiroers, L.; Ribordy, M.] Ecole Polytech Fed Lausanne, High Energy Phys Lab, CH-1015 Lausanne, Switzerland. [Besson, D. Z.; Kenny, P.] Univ Kansas, Dept Phys & Astron, Lawrence, KS 66045 USA. [Gallagher, J.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. [Abbasi, R.; Aguilar, J. A.; Andeen, K.; Baker, M.; BenZvi, S.; Berghaus, P.; Braun, J.; Chirkin, D.; Desiati, P.; Diaz-Velez, J. C.; Dumm, J. P.; Eisch, J.; Gladstone, L.; Grullon, S.; Halzen, F.; Hanson, K.; Hill, G. C.; Hoshina, K.; Jacobsen, J.; Karle, A.; Kelley, J. L.; Krasberg, M.; Landsman, H.; Maruyama, R.; Merck, M.; Montaruli, T.; Morse, R.; O'Murchadha, A.; Rodrigues, J. P.; Santander, M.; Toscano, S.; van Santen, J.; Weaver, C.; Wendt, C.; Westerhoff, S.; Whitehorn, N.] Univ Wisconsin, Dept Phys, Madison, WI 53706 USA. [Griesel, T.; Koepke, L.; Kowarik, T.; Kroll, G.; Luenemann, J.; Piegsa, A.; Rothmaier, F.; Sander, H. -G.; Schatto, K.; Wiebe, K.] Johannes Gutenberg Univ Mainz, Inst Phys, D-55099 Mainz, Germany. [Herquet, P.; Kohnen, G.] Univ Mons, B-7000 Mons, Belgium. [Bai, X.; Clem, J.; Evenson, P. A.; Gaisser, T. K.; Hussain, S.; Kuwabara, T.; Niessen, P.; Ruzybayev, B.; Seckel, D.; Stanev, T.; Stoyanov, S.; Tilav, S.; Xu, C.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA. [Bai, X.; Clem, J.; Evenson, P. A.; Gaisser, T. K.; Hussain, S.; Kuwabara, T.; Niessen, P.; Ruzybayev, B.; Seckel, D.; Stanev, T.; Stoyanov, S.; Tilav, S.; Xu, C.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA. [Ahlers, M.; Sarkar, S.] Univ Oxford, Dept Phys, Oxford OX1 3NP, England. [Abu-Zayyad, T.; Madsen, J.; Spiczak, G. M.; Tamburro, A.] Univ Wisconsin, Dept Phys, River Falls, WI 54022 USA. [Bohm, C.; Danninger, M.; Finley, C.; Hulth, P. O.; Hultqvist, K.; Johansson, H.; Seo, S. H.; Walck, C.] Stockholm Univ, Oskar Klein Ctr, SE-10691 Stockholm, Sweden. [Bohm, C.; Danninger, M.; Finley, C.; Hulth, P. O.; Hultqvist, K.; Johansson, H.; Seo, S. H.; Walck, C.] Stockholm Univ, Dept Phys, SE-10691 Stockholm, Sweden. [Cowen, D. F.; Meszaros, P.; Movit, S. M.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Cowen, D. F.; DeYoung, T.; Foerster, M. M.; Fox, B. D.; Ha, C.; Koskinen, D. J.; Lafebre, S.; Larson, M. J.; Meszaros, P.; Prikockis, M.; Rutledge, D.; Slipak, A.; Stephens, G.; Toale, P. A.] Penn State Univ, Dept Phys, University Pk, PA 16802 USA. [Botner, O.; Engdegard, O.; Hallgren, A.; Miller, J.; Olivo, M.; de los Heros, C. Perez; Taavola, H.] Uppsala Univ, Dept Phys & Astron, S-75120 Uppsala, Sweden. [Auffenberg, J.; Becker, K. -H.; Bindig, D.; Fischer-Wasels, T.; Gurtner, M.; Helbing, K.; Kampert, K. -H.; Karg, T.; Kopper, S.; Naumann, U.; Posselt, J.; Schultes, A.; Semburg, B.] Univ Wuppertal, Dept Phys, D-42119 Wuppertal, Germany. [Alba, J. L. Bazo; Benabderrahmane, M. L.; Berdermann, J.; Bernardini, E.; Franke, R.; Kislat, F.; Lauer, R.; Majumdar, P.; Middell, E.; Nahnhauer, R.; Schoenwald, A.; Spiering, C.; Tarasova, O.; Tosi, D.; Voigt, B.; Walter, M.; Wischnewski, R.] DESY, D-15735 Zeuthen, Germany. [Montaruli, T.] Univ Bari, I-70126 Bari, Italy. [Montaruli, T.] Sezione Ist Nazl Fis Nucl, Dipartimento Fis, I-70126 Bari, Italy. [Stamatikos, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Meagher, K (reprint author), Univ Maryland, Dept Phys, College Pk, MD 20742 USA. RI Tamburro, Alessio/A-5703-2013; Botner, Olga/A-9110-2013; Hallgren, Allan/A-8963-2013; Tjus, Julia/G-8145-2012; Auffenberg, Jan/D-3954-2014; Koskinen, David/G-3236-2014; Aguilar Sanchez, Juan Antonio/H-4467-2015; Maruyama, Reina/A-1064-2013; Sarkar, Subir/G-5978-2011; Beatty, James/D-9310-2011; Wiebusch, Christopher/G-6490-2012; Kowalski, Marek/G-5546-2012; Taavola, Henric/B-4497-2011; OI Auffenberg, Jan/0000-0002-1185-9094; Koskinen, David/0000-0002-0514-5917; Aguilar Sanchez, Juan Antonio/0000-0003-2252-9514; Maruyama, Reina/0000-0003-2794-512X; Sarkar, Subir/0000-0002-3542-858X; Beatty, James/0000-0003-0481-4952; Actis, Oxana/0000-0001-8851-3983; Wiebusch, Christopher/0000-0002-6418-3008; Ter-Antonyan, Samvel/0000-0002-5788-1369; Schukraft, Anne/0000-0002-9112-5479; Perez de los Heros, Carlos/0000-0002-2084-5866; Taavola, Henric/0000-0002-2604-2810; Buitink, Stijn/0000-0002-6177-497X; Carson, Michael/0000-0003-0400-7819; Hubert, Daan/0000-0002-4365-865X; Benabderrahmane, Mohamed Lotfi/0000-0003-4410-5886 FU U.S. NSF-Office of Polar Programs; U.S. NSF-Physics Division; University of Wisconsin Alumni Research Foundation; GLOW and OSG grids; U.S. DOE; NERSCC; LONI grid; NSERC, Canada; Swedish Research Council; Swedish Polar Research Secretariat; SNIC; K. and A. Wallenberg Foundation, Sweden; German Ministry for Education and Research; Deutsche Forschungsgemeinschaft; FSR; FWO Odysseus; IWT; BELSPO, Belgium; Marsden Fund, New Zealand; JSPS, Japan; SNSF, Switzerland; EU; Capes Foundation, Brazil; NSF GRFP FX We acknowledge support from the following agencies: U.S. NSF-Office of Polar Programs, U.S. NSF-Physics Division, University of Wisconsin Alumni Research Foundation, the GLOW and OSG grids; U.S. DOE, NERSCC, the LONI grid; NSERC, Canada; Swedish Research Council, Swedish Polar Research Secretariat, SNIC, K. and A. Wallenberg Foundation, Sweden; German Ministry for Education and Research, Deutsche Forschungsgemeinschaft; FSR, FWO Odysseus, IWT, BELSPO, Belgium; Marsden Fund, New Zealand; JSPS, Japan; SNSF, Switzerland. A. Gross is supported by the EU Marie Curie OIF Program, J. P. R. by the Capes Foundation, Brazil, and N. W. by the NSF GRFP. NR 18 TC 74 Z9 76 U1 1 U2 9 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 APR 7 PY 2011 VL 106 IS 14 AR 141101 DI 10.1103/PhysRevLett.106.141101 PG 5 WC Physics, Multidisciplinary SC Physics GA 747XY UT WOS:000289355800002 PM 21561178 ER PT J AU Falconer, D Barghouty, AF Khazanov, I Moore, R AF Falconer, David Barghouty, Abdulnasser F. Khazanov, Igor Moore, Ron TI A tool for empirical forecasting of major flares, coronal mass ejections, and solar particle events from a proxy of active-region free magnetic energy SO SPACE WEATHER-THE INTERNATIONAL JOURNAL OF RESEARCH AND APPLICATIONS LA English DT Article ID VECTOR MAGNETOGRAMS; FIELD; NONPOTENTIALITY; PRODUCTIVITY; HELIOSPHERE; PREDICTION; TIME AB This paper describes a new forecasting tool developed for and currently being tested by NASA's Space Radiation Analysis Group (SRAG) at Johnson Space Center, which is responsible for the monitoring and forecasting of radiation exposure levels of astronauts. The new software tool is designed for the empirical forecasting of M- and X-class flares, coronal mass ejections, and solar energetic particle events. For each type of event, the algorithm is based on the empirical relationship between the event rate and a proxy of the active region's free magnetic energy. Each empirical relationship is determined from a data set of similar to 40,000 active-region magnetograms from similar to 1300 active regions observed by SOHO/Michelson Doppler Imager (MDI) that have known histories of flare, coronal mass ejection, and solar energetic particle event production. The new tool automatically extracts each strong-field magnetic area from an MDI full-disk magnetogram, identifies each as a NOAA active region, and measures the proxy of the active region's free magnetic energy from the extracted magnetogram. For each active region, the empirical relationship is then used to convert the free-magnetic-energy proxy into an expected event rate. The expected event rate in turn can be readily converted into the probability that the active region will produce such an event in a given forward time window. Descriptions of the data sets, algorithm, and software in addition to sample applications and a validation test are presented. Further development and transition of the new tool in anticipation of SDO/HMI are briefly discussed. C1 [Falconer, David; Barghouty, Abdulnasser F.; Moore, Ron] NASA, Space Sci Off, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. [Falconer, David; Khazanov, Igor] Univ Alabama, Ctr Space Plasma & Aeron Res, Huntsville, AL 35899 USA. [Falconer, David] Univ Alabama, Dept Phys, Huntsville, AL 35899 USA. RP Falconer, D (reprint author), NASA, Space Sci Off, George C Marshall Space Flight Ctr, Mail Code VP62, Huntsville, AL 35812 USA. EM david.a.falconer@nasa.gov FU NASA's Office of Chief Engineer Technical Excellence Initiative; NASA Heliophysics Division; NSF's Division of Atmospheric Sciences; AFOSR FX The development of this tool was supported by funding from NASA's Office of Chief Engineer Technical Excellence Initiative. The science that went into development of this tool was supported by funding from the NASA Heliophysics Division, from NSF's Division of Atmospheric Sciences, and from AFOSR'S MURI Program. We wish to acknowledge the use of both Chris Balch flare/CME data sets and the CME catalog generated and maintained at the CDAW Data Center by NASA and The Catholic University of America in cooperation with the Naval Research Laboratory. The paper has also been improved by comments of the two anonymous referees. NR 25 TC 26 Z9 26 U1 0 U2 2 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 1542-7390 J9 SPACE WEATHER JI Space Weather PD APR 7 PY 2011 VL 9 AR S04003 DI 10.1029/2009SW000537 PG 12 WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences GA 747ZV UT WOS:000289360700001 ER PT J AU Wei, CY Pohorile, A AF Wei, Chenyu Pohorile, Andrew TI Permeation of Nucleosides through Lipid Bilayers SO JOURNAL OF PHYSICAL CHEMISTRY B LA English DT Article ID FREE-ENERGY CALCULATIONS; RNA WORLD; SIMULATION; LIPOSOMES; MEMBRANE; SPECTROSCOPY; COMPONENTS; DYNAMICS; VESICLES; MODELS AB Elucidating mechanisms that facilitate primordial synthesis of information polymers is central to understanding the origins of life. One such mechanism might have been the recently discovered diastereoselectivity of membranes favoring uptake of ribose (Sacerdote, M. G.; Szostak, J. W. Proc. Natl. Acad. Sci. U.S.A. 2005, 102, 6004), which might have promoted its preferential incorporation into nucleic acids. To determine whether the same mechanism was available if nucleosides rather than sugars were supplied to ancestral cells, we carry out molecular dynamics simulations of their permeation through a lipid bilayer. We find that the free energy barriers to permeation of ribo-adenosine and arabino-adenosine through the 1-palmitoyl-2-oleoyl-sn-glycero-3-phosphatidylcholine membrane are quite similar, equal to 10.0 and 10.4 kcal/mol, respectively. The corresponding permeability coefficients are also similar, equal to 9.1 x 10(-7) and 5.3 x 10(-7) cm/s. The 10-fold increase in permeability of membranes to ribose over its diastereomers is not preserved for nucleosides because in contrast to free aldopentoses they exist in the furanose rather than pyranose form. This change eliminates the possibility of forming a network of favorable, intramolecular interactions between exocyclic, hydroxyl groups that stabilizes ribose, but not its diastereomers, inside membranes. Thus, uptake of nutrients provided selective advantage to primordial RNA only if the species absorbed through cell walls were sugars rather than nucleosides. C1 [Wei, Chenyu; Pohorile, Andrew] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Wei, Chenyu; Pohorile, Andrew] Univ Calif San Francisco, Dept Pharmaceut Chem, San Francisco, CA 94143 USA. RP Wei, CY (reprint author), NASA, Ames Res Ctr, Mail Stop 229-1, Moffett Field, CA 94035 USA. EM Chenyu.Wei@nasa.gov; Andrew.Pohor-ille@nasa.gov FU NASA Exobiology Program FX This work was supported by the NASA Exobiology Program. NASA Advanced Supercomputing (NAS) Division provided computational resources needed to carry out this study. NR 53 TC 19 Z9 19 U1 1 U2 67 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 1520-6106 J9 J PHYS CHEM B JI J. Phys. Chem. B PD APR 7 PY 2011 VL 115 IS 13 BP 3681 EP 3688 DI 10.1021/jp112104r PG 8 WC Chemistry, Physical SC Chemistry GA 741SU UT WOS:000288885700044 PM 21405137 ER PT J AU Choi, YJ Lu, J Sohn, HY Fang, ZZ Kim, C Bowman, RC Hwang, SJ AF Choi, Young Joon Lu, Jun Sohn, Hong Yong Fang, Zhigang Zak Kim, Chul Bowman, Robert C., Jr. Hwang, Son-Jong TI Reaction Mechanisms in the Li3AlH6/LiBH4 and Al/LiBH4 Systems for Reversible Hydrogen Storage. Part 2: Solid-State NMR Studies SO JOURNAL OF PHYSICAL CHEMISTRY C LA English DT Article ID MAS NMR; LIBH4; AL-27; ALUMINUM; HYDRIDE; AL; BOROHYDRIDES; POWDER; MG; TI AB In Part 1, the promising hydrogen storage properties of the combined systems of Li3AlH6/LiBH4 and Al/LiBH4, exhibiting the favorable formation of AlB2 during dehydrogenation, were presented based on TGA and XRD analyses. The present Part 2 describes the characterization of the intermediate and final products of the dehydrogenation and rehydrogenation of the above systems by multinuclear solid-state NMR characterization. This work has also verified that the presence of Al resulted in the re-formation of LiBH4 occurring at a much lower temperature and H-2 pressure, under which conditions the dehydrogenation product from LiBH4 alone does not show any degree of rehydrogenation. NMR studies mainly identified various reaction intermediates for LiBH4 dehydrogenation/rehydrotrnation reactions. Unlike the XRD studies, the AlB2 formation, in particular, could not be unambiguously confirmed by NMR. Al-27 NMR showed that aluminum was mainly involved in various Li-Al alloy formations. The catalytic role of Al in the LiBH4 hydrogen storage reactivity could be achieved by a reversible cycle of the Al + LiH <-> LiAl + 1/2H(2) reaction. C1 [Choi, Young Joon; Lu, Jun; Sohn, Hong Yong; Fang, Zhigang Zak] Univ Utah, Dept Met Engn, Salt Lake City, UT 84112 USA. [Kim, Chul; Hwang, Son-Jong] CALTECH, Div Chem & Chem Engn, Pasadena, CA 91125 USA. [Bowman, Robert C., Jr.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Sohn, HY (reprint author), Univ Utah, Dept Met Engn, 135 S 1460 E Room, Salt Lake City, UT 84112 USA. EM h.y.sohn@utah.edu; sonjong@cheme.caltech.edu FU U.S. Department of Energy (DOE), Office of Energy Efficiency and Renewable Energy [DE-FC36-05GO15069, DE-Al-01-05EE11105]; National Science Foundation (NSF) [9724240, DMR-520565] FX This research was supported by the U.S. Department of Energy (DOE), Office of Energy Efficiency and Renewable Energy, through the Hydrogen, Fuel Cells & Infrastructure Technologies Program under Contract Numbers DE-FC36-05GO15069 (U. Utah) and DE-AI-01-05EE11105 (Jet Propulsion Lab). The NMR facility at Caltech was supported by the National Science Foundation (NSF) under Grant Number 9724240 and partially supported by the MRSEC Program of the NSF under Award Number DMR-520565. NR 25 TC 24 Z9 24 U1 1 U2 29 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 1932-7447 J9 J PHYS CHEM C JI J. Phys. Chem. C PD APR 7 PY 2011 VL 115 IS 13 BP 6048 EP 6056 DI 10.1021/jp109113f PG 9 WC Chemistry, Physical; Nanoscience & Nanotechnology; Materials Science, Multidisciplinary SC Chemistry; Science & Technology - Other Topics; Materials Science GA 741SW UT WOS:000288885900105 ER PT J AU Bushnell, D Garneau, M Logsdon, JM Sagdeev, R Lu, E Mountain, M Stephenson, N AF Bushnell, Dennis Garneau, Marc Logsdon, John M. Sagdeev, Roald Lu, Ed Mountain, Matt Stephenson, Neal TI NASA: what now? SO NATURE LA English DT Editorial Material C1 [Bushnell, Dennis] NASA, Langley Res Ctr, Washington, DC 20546 USA. [Logsdon, John M.] George Washington Univ, Washington, DC 20052 USA. [Sagdeev, Roald] Russian Space Res Inst, Moscow, Russia. [Mountain, Matt] NASA, Space Telescope Sci Inst, Washington, DC USA. RP Bushnell, D (reprint author), NASA, Langley Res Ctr, Washington, DC 20546 USA. NR 0 TC 1 Z9 1 U1 0 U2 3 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD APR 7 PY 2011 VL 472 IS 7341 BP 27 EP 29 PG 3 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 745VV UT WOS:000289199400016 PM 21475173 ER PT J AU Buratti, BJ Hicks, MD Nettles, J Staid, M Pieters, CM Sunshine, J Boardman, J Stone, TC AF Buratti, B. J. Hicks, M. D. Nettles, J. Staid, M. Pieters, C. M. Sunshine, J. Boardman, J. Stone, T. C. TI A wavelength-dependent visible and infrared spectrophotometric function for the Moon based on ROLO data SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID BIDIRECTIONAL REFLECTANCE SPECTROSCOPY; SATELLITES; PHOTOMETRY; CLEMENTINE AB The USGS's Robotic Lunar Observatory (ROLO) dedicated ground-based lunar calibration project obtained photometric observations of the Moon over the spectral range attainable from Earth (0.347-2.39 mu m) and over solar phase angles of 1.55 degrees-97 degrees. From these observations, we derived empirical lunar surface solar phase functions for both the highlands and maria that can be used for a wide range of applications. The functions can be used to correct for the effects of viewing geometry to produce lunar mosaics, spectra, and quick-look products for future lunar missions and ground-based observations. Our methodology can be used for a wide range of objects for which multiply scattered radiation is not significant, including all but the very brightest asteroids and moons. C1 [Buratti, B. J.; Hicks, M. D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Nettles, J.; Pieters, C. M.] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA. [Staid, M.] Planetary Sci Inst, Tucson, AZ 85719 USA. [Sunshine, J.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Boardman, J.] Analyt Imaging & Geophys, Boulder, CO 80303 USA. [Stone, T. C.] USGS, Flagstaff, AZ 86001 USA. RP Buratti, BJ (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,MS 183-401, Pasadena, CA 91109 USA. EM bonnie.j.buratti@jpl.nasa.gov FU National Aeronautics and Space Administration FX This research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under contract to the National Aeronautics and Space Administration. We thank Deborah Domingue for a detailed review. NR 24 TC 10 Z9 10 U1 2 U2 7 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 APR 5 PY 2011 VL 116 AR E00G03 DI 10.1029/2010JE003724 PG 8 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 748AA UT WOS:000289361200001 ER PT J AU Parker, ET Cleaves, HJ Dworkin, JP Glavin, DP Callahan, M Aubrey, A Lazcano, A Bada, JL AF Parker, Eric T. Cleaves, Henderson J. Dworkin, Jason P. Glavin, Daniel P. Callahan, Michael Aubrey, Andrew Lazcano, Antonio Bada, Jeffrey L. TI Primordial synthesis of amines and amino acids in a 1958 Miller H2S-rich spark discharge experiment SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE prebiotic chemistry; volcano plume chemistry; carbonaceous chondrites ID EARLY EARTH ATMOSPHERE; LIQUID-CHROMATOGRAPHY; NITROGEN-FIXATION; PRIMITIVE EARTH; LIFE; CHEMISTRY; ERUPTIONS; SULFUR; ORIGIN; OCEAN AB Archived samples from a previously unreported 1958 Stanley Miller electric discharge experiment containing hydrogen sulfide (H2S) were recently discovered and analyzed using high-performance liquid chromatography and time-of-flight mass spectrometry. We report here the detection and quantification of primary amine-containing compounds in the original sample residues, which were produced via spark discharge using a gaseous mixture of H2S, CH4, NH3, and CO2. A total of 23 amino acids and 4 amines, including 7 organosulfur compounds, were detected in these samples. The major amino acids with chiral centers are racemic within the accuracy of the measurements, indicating that they are not contaminants introduced during sample storage. This experiment marks the first synthesis of sulfur amino acids from spark discharge experiments designed to imitate primordial environments. The relative yield of some amino acids, in particular the isomers of aminobutyric acid, are the highest ever found in a spark discharge experiment. The simulated primordial conditions used by Miller may serve as a model for early volcanic plume chemistry and provide insight to the possible roles such plumes may have played in abiotic organic synthesis. Additionally, the overall abundances of the synthesized amino acids in the presence of H2S are very similar to the abundances found in some carbonaceous meteorites, suggesting that H2S may have played an important role in prebiotic reactions in early solar system environments. C1 [Parker, Eric T.; Bada, Jeffrey L.] Univ Calif San Diego, Scripps Inst Oceanog, Geosci Res Div, La Jolla, CA 92093 USA. [Cleaves, Henderson J.] Carnegie Inst Sci, Geophys Lab, Washington, DC 20015 USA. [Dworkin, Jason P.; Glavin, Daniel P.; Callahan, Michael] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA. [Aubrey, Andrew] CALTECH, Jet Prop Lab, NASA, Pasadena, CA 91109 USA. [Lazcano, Antonio] Univ Nacl Autonoma Mexico, Fac Ciencias, Mexico City 04510, DF, Mexico. RP Bada, JL (reprint author), Univ Calif San Diego, Scripps Inst Oceanog, Geosci Res Div, 8615 Kennel Way, La Jolla, CA 92093 USA. EM jbada@ucsd.edu RI Callahan, Michael/D-3630-2012; Glavin, Daniel/D-6194-2012; Dworkin, Jason/C-9417-2012; OI Glavin, Daniel/0000-0001-7779-7765; Dworkin, Jason/0000-0002-3961-8997; Cleaves, Henderson/0000-0003-4101-0654 FU National Aeronautics and Space Administration Astrobiology Institute; Goddard Center for Astrobiology; National Aeronautics and Space Administration; National Science Foundation [CHE-1004570] FX Stanley L. Miller passed away on May 20, 2007. Because his research ushered in the era of experimental studies on the origin of life, we dedicate this work to his memory. We thank Jamie Elsila for GC-MS analyses of these residues and Facundo Fernandez and the reviewers for helpful comments. We deeply appreciate the Mandeville Special Collections in the University of California, San Diego Geisel Library for assistance with archiving and retrieving Miller's original laboratory notebooks. We are grateful for funding support from the National Aeronautics and Space Administration Astrobiology Institute and the Goddard Center for Astrobiology. M. C. and H.J.C. acknowledge support from the National Aeronautics and Space Administration Postdoctoral Program administered by Oak Ridge Associated Universities. Assistance with data analysis and figure preparation (A. A.) was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. J.L.B. and H.J.C. are also affiliated with the Center for Chemical Evolution at the Georgia Institute of Technology, which is jointly supported by the National Science Foundation and the National Aeronautics and Space Administration Astrobiology Program, under the National Science Foundation Grant CHE-1004570. NR 39 TC 64 Z9 69 U1 10 U2 70 PU NATL ACAD SCIENCES PI WASHINGTON PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA SN 0027-8424 J9 P NATL ACAD SCI USA JI Proc. Natl. Acad. Sci. U. S. A. PD APR 5 PY 2011 VL 108 IS 14 BP 5526 EP 5531 DI 10.1073/pnas.1019191108 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 746RT UT WOS:000289265300013 PM 21422282 ER PT J AU Kobrick, RL Klaus, DM Street, KW AF Kobrick, Ryan L. Klaus, David M. Street, Kenneth W. TI Standardization of a volumetric displacement measurement for two-body abrasion scratch test data analysis SO WEAR LA English DT Article DE Two-body abrasion; Scratch testing; Lunar dust; Surface topography; Profilometry; Surface analysis ID PARALLEL GROOVES; GENERATION; SURFACES AB A limitation has been identified in the existing test standards used for making controlled, two-body abrasion scratch measurements (ASTM Standard G 171) based solely on the width of the resultant score on the surface of the material. A new, more robust method is proposed to complement the current two-body scratch test standard for analyzing a surface scratch that takes into account the full three-dimensional (3D) profile of the displaced material. To accomplish this, a set of four volume displacement metrics are systematically defined by normalizing the overall surface profile to statistically denote the area of relevance, termed the 'Zone of Interaction' (ZOI). From this baseline, depth of the trough and height of the ploughed material are factored into the overall deformation assessment. A complete set of roughness parameters are calculated on the fresh surface and resulting abraded surface to aid in shape change characterization of the material. Proof of concept data were collected and analyzed to demonstrate the performance of this proposed methodology. This technique takes advantage of advanced imaging capabilities that now allow resolution of the scratched surface to be quantified in greater detail than was previously achievable. A quantified understanding of fundamental particle-material interaction is critical to anticipating how well components can withstand prolonged use in highly abrasive environments, specifically for our intended applications on the surface of the moon and other planets or asteroids, as well as in similarly demanding, harsh terrestrial settings. (C) 2011 Elsevier B.V. All rights reserved. C1 [Kobrick, Ryan L.; Klaus, David M.] Univ Colorado, Boulder, CO 80309 USA. [Street, Kenneth W.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Kobrick, RL (reprint author), Univ Colorado, 429 UCB, Boulder, CO 80309 USA. EM Kobrick@Colorado.edu; Klaus@Colorado.edu; Kenneth.W.Street@nasa.gov FU NASA [NNX07AR55H]; NASA Glenn Research Center FX This research was supported by a NASA Graduate Student Researchers Program (GSRP) grant (NNX07AR55H) provided by the Dust Management Project, under the Exploration Technology Development Program. MATLAB assistance was provided by Kevin Higdon, Ph.D. Candidate (UCB) and Bradley W. Cheetham, Ph.D. Student (UCB). SEM work was conducted by Prof. Sayed M. Khalil (Sohag University, Egypt) at the Nanomaterials Characterization Facility, UCB. Test equipment and support were provided by NASA Glenn Research Center. Additional support was provided by BioServe Space Technologies (UCB) and the Achievement Rewards for College Scientists (ARCS) Foundation, Inc. NR 15 TC 4 Z9 4 U1 0 U2 2 PU ELSEVIER SCIENCE SA PI LAUSANNE PA PO BOX 564, 1001 LAUSANNE, SWITZERLAND SN 0043-1648 J9 WEAR JI Wear PD APR 4 PY 2011 VL 270 IS 9-10 BP 650 EP 657 DI 10.1016/j.wear.2011.01.026 PG 8 WC Engineering, Mechanical; Materials Science, Multidisciplinary SC Engineering; Materials Science GA 758AS UT WOS:000290132500013 ER PT J AU Leer, K Goetz, W Chan, MA Gorevan, S Hansen, MF Jensen, CL Kletetschka, G Kusack, A Madsen, MB AF Leer, Kristoffer Goetz, Walter Chan, Marjorie A. Gorevan, Steven Hansen, Mikkel Fougt Jensen, Christian Lundmand Kletetschka, Gunther Kusack, Alastair Madsen, Morten Bo TI RAT magnet experiment on the Mars Exploration Rovers: Spirit and Opportunity beyond sol 500 SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID MERIDIANI-PLANUM; DIAGENETIC HEMATITE; BURNS FORMATION; SOUTHERN UTAH; FLUID-FLOW; USA AB The Rock Abrasion Tool (RAT) magnet experiment on the Mars Exploration Rovers was designed to collect dust from rocks ground by the RAT of the two rovers on the surface of Mars. The dust collected on the magnets is now a mixture of dust from many grindings. Here the new data from the experiment are presented. The findings from Mars are furthermore compared to simulation experiments performed on Earth. New experiments with analog rocks that mainly contain hematite indicate the likely presence of a stronger magnetic phase besides hematite in the outcrop rock formations found on Meridiani Planum, a phase which was hitherto not detected by other measurements (such as Mossbauer) on these rocks. C1 [Leer, Kristoffer; Jensen, Christian Lundmand; Madsen, Morten Bo] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark. [Goetz, Walter] Max Planck Inst Solar Syst Res, D-37191 Katlenburg Lindau, Germany. [Chan, Marjorie A.] Univ Utah, Dept Geol & Geophys, Salt Lake City, UT 84112 USA. [Gorevan, Steven; Kusack, Alastair] Honeybee Robot, New York, NY 10001 USA. [Hansen, Mikkel Fougt] Tech Univ Denmark, Dept Micro & Nanotechnol, DK-2800 Lyngby, Denmark. [Kletetschka, Gunther] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA. [Kletetschka, Gunther] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Kletetschka, Gunther] Acad Sci Czech Republic, Inst Geol, Prague, Czech Republic. RP Leer, K (reprint author), Univ Copenhagen, Niels Bohr Inst, Blegdamsvej 17, DK-2100 Copenhagen, Denmark. EM kleer@kleer.dk RI Kletetschka, Gunther/C-9996-2011; Hansen, Mikkel/A-3024-2012; Madsen, Morten/D-2082-2011 OI Kletetschka, Gunther/0000-0002-0645-9037; Hansen, Mikkel/0000-0003-3333-2856; Madsen, Morten/0000-0001-8909-5111 FU Danish Science Agency; Thomas B. Thrige's foundation; Danish Electronics, Light, and Acoustics (DELTA) in Horsholm, Denmark; Honeybee Robotics, New York FX Danish participation in the MER missions was supported by the Danish Science Agency, by Thomas B. Thrige's foundation, and by Danish Electronics, Light, and Acoustics (DELTA) in Horsholm, Denmark. Honeybee Robotics, New York, has been a very important player, and we thank Honeybee for helping with simulation experiments. Tonci Balic-Zunic and Anna Katerinopoulou from Institute of Geography and Geology, University of Copenhagen, have been most helpful in acquisition and interpretation of X-ray data. Furthermore, Mandy Bacon from the Niels Bohr Institute, University of Copenhagen, has supported this project. We are indebted to the scientists and engineers of the MER team for their continuous support which made these experiments possible. NR 25 TC 2 Z9 2 U1 0 U2 18 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 APR 2 PY 2011 VL 116 AR E00F18 DI 10.1029/2010JE003667 PG 8 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 744HH UT WOS:000289085000001 ER PT J AU Anderson, RL Lo, MW AF Anderson, Rodney L. Lo, Martin W. TI A Dynamical Systems Analysis of Resonant Flybys: Ballistic Case SO JOURNAL OF THE ASTRONAUTICAL SCIENCES LA English DT Article ID TRAJECTORY DESIGN; ORBITS; COMETS AB In this analysis, resonant flybys were explored within the context of the circular restricted three-body problem using dynamical systems theory. The first step in this process involved the construction of a flyby trajectory continuously transiting between 3:4 and 5:6 resonances in the Jupiter-Europa circular restricted three-body problem. An examination of this trajectory revealed that it followed the invariant manifolds of resonant orbits during these transitions. It was discovered that these transitions occurred for specific energies where the invariant manifolds of the 3:4 and 5:6 resonant orbits were closely related. The potential of the information obtained from this analysis for use in mission design was demonstrated by developing resonance transition trajectories using resonant orbit homoclinic and heteroclinic connections. C1 [Anderson, Rodney L.] Univ Colorado, Colorado Ctr Astrodynam Res, Boulder, CO 80309 USA. [Lo, Martin W.] CALTECH, Jet Prop Lab, High Capabil Comp & Modeling Grp, Pasadena, CA 91109 USA. RP Anderson, RL (reprint author), Univ Colorado, Colorado Ctr Astrodynam Res, Boulder, CO 80309 USA. OI Anderson, Rodney/0000-0001-5336-2775 FU National Aeronautics and Space Administration; Jupiter Icy Moons Orbiter mission design tool development task; JPL Institutional Computing and Information Services; NASA Offices of Earth Science, Aeronautics, and Space Science FX The authors would like to thank Dr. George Born for his support of the research and Dr. Bob Easton for his helpful discussions. This work was conducted for the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. It was funded in part by the Jupiter Icy Moons Orbiter mission design tool development task. The supercomputer used in this investigation was provided by funding from JPL Institutional Computing and Information Services and the NASA Offices of Earth Science, Aeronautics, and Space Science. NR 38 TC 10 Z9 10 U1 2 U2 4 PU AMER ASTRONAUTICAL SOC PI SPRINGFIELD PA 6352 ROLLING MILL PLACE SUITE 102, SPRINGFIELD, VA 22152 USA SN 0021-9142 J9 J ASTRONAUT SCI JI J. Astronaut. Sci. PD APR-JUN PY 2011 VL 58 IS 2 BP 167 EP 194 PG 28 WC Engineering, Aerospace SC Engineering GA 881CE UT WOS:000299457300002 ER PT J AU Koshak, WJ Solakewicz, RJ AF Koshak, W. J. Solakewicz, R. J. TI Retrieving the Fraction of Ground Flashes from Satellite Lightning Imager Data Using CONUS-Based Optical Statistics SO JOURNAL OF ATMOSPHERIC AND OCEANIC TECHNOLOGY LA English DT Article AB A retrieval method is introduced for estimating the fraction of ground flashes in a set of N flashes observed from either a low earth-orbiting or geostationary satellite lightning imager. The methodology exploits the fact that mean optical characteristics of ground and cloud flashes differ, and hence a properly posed equation set for mean conditions of a set of N observed flashes can be mathematically inverted to estimate the ground flash fraction (and hence the cloud flash-to-ground flash ratio). Explicit analytic expressions for the retrieval errors are derived, and numerical tests of the retrieval method are provided to quantify retrieval accuracy. It has been found that the retrieval method works best when only one optimum optical parameter is used (the single-characteristic solution approach) rather than a mixture of optical parameters (the multiple-characteristic solution approach); that is, the suboptimum optical parameters in the mix degrade retrieval accuracy. Since the retrieval method uses conterminous United States (CONUS)-averaged values of the lightning optical measurements, retrieval errors tend to be smallest in geographical regions whose specific mean lightning optical measurements are closest to the CONUS mean values. The rms ground flash fraction retrieval errors for 52 widely distributed regions across CON US ranged from as low as 0.061 to 0.111, depending on the true ground flash fraction sought. C1 [Koshak, W. J.] NASA Marshall Space Flight Ctr, Earth Sci Off, Huntsville, AL 35805 USA. [Solakewicz, R. J.] Chicago State Univ, Chicago, IL USA. RP Koshak, WJ (reprint author), NASA Marshall Space Flight Ctr, Earth Sci Off, VP61,Robert Cramer Res Hall,320 Sparkman Dr, Huntsville, AL 35805 USA. EM william.koshak@nasa.gov FU NOAA/NESDIS/STAR GOES-R Risk Reduction Program [NA07AA-NEG0284]; NASA FX This research has been supported by the NOAA/NESDIS/STAR GOES-R Risk Reduction Program under Space Act Agreement No. NA07AA-NEG0284 (Ms. Ingrid Guch, Chief, NOAA/NESDIS/STAR Cooperative Research Programs Division, Dr. Mark De Maria Chief, NOAA/NESDIS Regional and Mesoscale Meteorology Branch, and Dr. Steven J. Goodman, Senior (Chief) Scientist, GOES-R System Program), and by the Lightning Imaging Sensor (LIS) project (Program Manager, Ramesh Kakar, NASA Headquarters) as part of the NASA Earth Science Enterprise (ESE) Earth Observing system (EOS) project. We would also like to express our thanks to the NASA Postdoctoral Program (NPP) under which co-author Dr. Richard Solakiewicz served during a portion of this research effort. NR 4 TC 6 Z9 6 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 APR PY 2011 VL 28 IS 4 BP 459 EP 473 DI 10.1175/2010JTECHA1408.1 PG 15 WC Engineering, Ocean; Meteorology & Atmospheric Sciences SC Engineering; Meteorology & Atmospheric Sciences GA 757AZ UT WOS:000290057600002 ER PT J AU Koshak, WJ AF Koshak, W. J. TI A Mixed Exponential Distribution Model for Retrieving Ground Flash Fraction from Satellite Lightning Imager Data SO JOURNAL OF ATMOSPHERIC AND OCEANIC TECHNOLOGY LA English DT Article AB A Bayesian inversion method is introduced for retrieving the fraction of ground flashes in a set of flashes observed from a (low earth orbiting or geostationary) satellite lightning imager. The method employs a constrained mixed exponential distribution model to describe the lightning optical measurements. Because the method also retrieves certain population statistics of ground and cloud flash optical properties, the method can be applied to an arbitrary geographical region, including those regions where the lightning optical statistics either are not known or are difficult to obtain. The approach is tested by performing simulated retrievals, and retrieval error statistics are provided. A first-attempt retrieval of the global geographical distribution of ground flash fraction is obtained using the 5-yr Optical Transient Detector (OTD) dataset; the spatially averaged ground flash fraction over the global-scale domain studied was 0.151 with a standard deviation of 0.081. The ability to retrieve ground flash fraction has important benefits to the atmospheric chemistry community. For example, using the method to partition the existing OTD/Lightning Imaging Sensor (LIS) satellite global lightning climatology into separate ground and cloud flash climatologies would improve estimates of regional and global lightning nitrogen oxides (NO(x)) production; this, in turn, would improve both regional air quality and global chemistry/climate model predictions. C1 NASA Marshall Space Flight Ctr, Earth Sci Off, Huntsville, AL 35805 USA. RP Koshak, WJ (reprint author), NASA Marshall Space Flight Ctr, Earth Sci Off, 320 Sparkman Dr,VP61,Robert Cramer Res Hall, Huntsville, AL 35805 USA. EM william.koshak@nasa.gov FU NOAA/NESDIS/STAR GOES-R Risk Reduction Program [NA07AA-NEG0284]; NASA Earth Science Enterprise (ESE) Earth Observing System (EOS) FX This research has been supported by the NOAA/NESDIS/STAR GOES-R Risk Reduction Program under Space Act Agreement NA07AA-NEG0284 [Ms. Ingrid Guch, Chief, NOAA/NESDIS/STAR Cooperative Research Programs Division; Dr. Mark De Maria, Chief, NOAA/NESDIS Regional and Mesoscale Meteorology Branch; and Dr. Steven J. Goodman, Senior (Chief) Scientist, GOES-R System Program], and by the Lightning Imaging Sensor (US) project (Program Manager, Ramesh Kakar, NASA Headquarters) as part of the NASA Earth Science Enterprise (ESE) Earth Observing System (EOS) project. The author also thanks Dr. Richard Solakiewicz for his comments on a draft version of this manuscript, and Dr. Harold Peterson (NASA Postdoctoral Program) for his clerical help in finding some of the references cited here. NR 14 TC 5 Z9 5 U1 0 U2 4 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 APR PY 2011 VL 28 IS 4 BP 475 EP 492 DI 10.1175/2010JTECHA1438.1 PG 18 WC Engineering, Ocean; Meteorology & Atmospheric Sciences SC Engineering; Meteorology & Atmospheric Sciences GA 757AZ UT WOS:000290057600003 ER PT J AU Shindell, D Faluvegi, G Walsh, M Anenberg, SC Van Dingenen, R Muller, NZ Austin, J Koch, D Milly, G AF Shindell, Drew Faluvegi, Greg Walsh, Michael Anenberg, Susan C. Van Dingenen, Rita Muller, Nicholas Z. Austin, Jeff Koch, Dorothy Milly, George TI Climate, health, agricultural and economic impacts of tighter vehicle-emission standards SO NATURE CLIMATE CHANGE LA English DT Article ID AIR-POLLUTION; OZONE; STRATEGIES; MORTALITY; BENEFITS; SECTORS; ROAD AB Non-CO2 air pollutants from motor vehicles have traditionally been controlled to protect air quality and health, but also affect climate. We use global composition-climate modelling to examine the integrated impacts of adopting stringent European on-road vehicle-emission standards for these pollutants in 2015 in many developing countries. Relative to no extra controls, the tight standards lead to annual benefits in 2030 and beyond of 120,000-280,000 avoided premature air pollution-related deaths, 6.1-19.7 million metric tons of avoided ozone-related yield losses of major food crops, $1.50.6-2.4 trillion avoided health damage and $US1.1-4.3 billion avoided agricultural damage, and mitigation of 0.20 (+0.14/-0.17)degrees C of Northern Hemisphere extratropical warming during 2040-2070. Tighter vehicle-emission standards are thus extremely likely to mitigate short-term climate change in most cases, in addition to providing large improvements in human health and food security. These standards will not reduce CO2 emissions, however, which is required to mitigate long-term climate change. C1 [Shindell, Drew; Faluvegi, Greg; Koch, Dorothy; Milly, George] Columbia Univ, NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Shindell, Drew; Faluvegi, Greg; Koch, Dorothy; Milly, George] Columbia Univ, Columbia Earth Inst, New York, NY 10025 USA. [Walsh, Michael] Int Council Clean Transportat, San Francisco, CA 94104 USA. [Anenberg, Susan C.] US EPA, Res Triangle Pk, NC 27711 USA. [Anenberg, Susan C.] Univ N Carolina, Dept Environm Sci & Engn, Chapel Hill, NC 27599 USA. [Van Dingenen, Rita] Inst Environm & Sustainabil, European Commiss, Joint Res Ctr, I-21027 Ispra, Italy. [Muller, Nicholas Z.] Middlebury Coll, Dept Econ, Middlebury, VT 05753 USA. [Austin, Jeff] Calif Air Resources Board, Sacramento, CA 95814 USA. RP Shindell, D (reprint author), Columbia Univ, NASA, Goddard Inst Space Studies, New York, NY 10025 USA. EM drew.t.shindell@nasa.gov RI Shindell, Drew/D-4636-2012 FU NASA; ClimateWorks Foundation; California Air Resources Board FX We thank the NASA Applied Sciences program, the ClimateWorks Foundation and the California Air Resources Board for supporting this work. We also thank T. Bond for gridding the emissions, M. Brauer for providing the PM2.5-measurement database, J. West for assistance with the population projection, B. Croes and D. Luo at GARB for their assistance and the UNEP/WMO Integrated Assessment of Black Carbon and Tropospheric Ozone team for discussions. Conclusions expressed in this article are the authors and do not necessarily represent those of their employers. NR 38 TC 42 Z9 42 U1 3 U2 34 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 1758-678X EI 1758-6798 J9 NAT CLIM CHANGE JI Nat. Clim. Chang. PD APR PY 2011 VL 1 IS 1 BP 59 EP 66 DI 10.1038/NCLIMATE1066 PG 8 WC Environmental Sciences; Environmental Studies; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA 805HS UT WOS:000293718100025 ER PT J AU Johnson, PV Hodyss, R Tang, KQ Brinckerhoff, WB Smith, RD AF Johnson, Paul V. Hodyss, Robert Tang, Keqi Brinckerhoff, William B. Smith, Richard D. TI The laser ablation ion funnel: Sampling for in situ mass spectrometry on Mars SO PLANETARY AND SPACE SCIENCE LA English DT Article DE Ion funnel; Laser ablation; Mars; Mass spectrometry ID INTERFACE; PRESSURE; PERFORMANCE; TRANSPORT; DESIGN; SPACE AB A considerable investment has been made by NASA and other space agencies to develop instrumentation suitable for in situ analytical investigation of extra terrestrial bodies including various mass spectrometers (time-of-flight, quadrupole ion trap, quadrupole mass filters, etc.). However, the front-end sample handling that is needed to collect and prepare samples for interrogation by such instrumentation remains underdeveloped. Here we describe a novel approach tailored to the exploration of Mars where ions are created in the ambient atmosphere via laser ablation and then efficiently transported into a mass spectrometer for in situ analysis using an electrodynamic ion funnel. This concept would enable elemental and isotopic analysis of geological samples with the analysis of desorbed organic material a possibility as well. Such an instrument would be suitable for inclusion on all potential missions currently being considered such as the Mid-Range Rover, the Astrobiology Field Laboratory, and Mars Sample Return (i.e., as a sample pre-selection triage instrument), among others. (C) 2011 Elsevier Ltd. All rights reserved. C1 [Johnson, Paul V.; Hodyss, Robert] CALTECH, Jet Prop Lab, Pasadena, CA 91101 USA. [Tang, Keqi; Smith, Richard D.] Pacific NW Natl Lab, Environm Mol Sci Lab, Richland, WA 99352 USA. [Tang, Keqi; Smith, Richard D.] Pacific NW Natl Lab, Div Biol Sci, Richland, WA 99352 USA. [Brinckerhoff, William B.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Johnson, PV (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91101 USA. EM Paul.V.Johnson@jpl.nasa.gov RI Smith, Richard/J-3664-2012; Brinckerhoff, William/F-3453-2012; Johnson, Paul/D-4001-2009 OI Smith, Richard/0000-0002-2381-2349; Brinckerhoff, William/0000-0001-5121-2634; Johnson, Paul/0000-0002-0186-8456 FU National Aeronautics and Space Administration (NASA); DOE [DE-AC05-76RLO 1830]; NASA; JPL 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) and at the Environmental Molecular Sciences Laboratory, a US DOE national scientific user facility located at the Pacific Northwest National Laboratory (PNNL) in Richland, Washington. PNNL is a multiprogram national laboratory operated by Battelle for the DOE under Contract no. DE-AC05-76RLO 1830. Funding from NASA's Planetary Instrument Definition and Development program and the JPL Director's Research and Development Fund is gratefully acknowledged. NR 27 TC 4 Z9 4 U1 5 U2 27 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 APR PY 2011 VL 59 IS 5-6 BP 387 EP 393 DI 10.1016/j.pss.2011.01.004 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 737PT UT WOS:000288581400003 ER PT J AU Cordiner, MA Charnley, SB Buckle, JV Walsh, C Millar, TJ AF Cordiner, M. A. Charnley, S. B. Buckle, J. V. Walsh, C. Millar, T. J. TI DISCOVERY OF INTERSTELLAR ANIONS IN CEPHEUS AND AURIGA SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE astrochemistry; ISM: abundances; ISM: clouds; ISM: molecules; stars: formation ID MASS PROTOSTAR IRAS-04368+2557; CARBON-CHAIN MOLECULES; STAR-FORMING REGIONS; GAS GRAIN PROCESSES; DARK CLOUDS; ASTRONOMICAL IDENTIFICATION; INITIAL CONDITIONS; CHEMICAL-MODELS; DENSE CORES; L1527 AB We report the detection of microwave emission lines from the hydrocarbon anion C6H- and its parent neutral C6H in the star-forming region L1251A (in Cepheus), and the pre-stellar core L1512 (in Auriga). The carbon-chain-bearing species C4H, HC3N, HC5N, HC7N, and C3S are also detected in large abundances. The observations of L1251A constitute the first detections of anions and long-chain polyynes and cyanopolyynes (with more than five carbon atoms) in the Cepheus Flare star-forming region, and the first detection of anions in the vicinity of a protostar outside of the Taurus molecular cloud complex, indicating a possible wider importance for anions in the chemistry of star formation. Rotational excitation temperatures have been derived from the HC3N hyperfine structure lines and are found to be 6.2 K for L1251A and 8.7 K for L1512. The anion-to-neutral ratios are 3.6% and 4.1%, respectively, which are within the range of values previously observed in the interstellar medium, and suggest a relative uniformity in the processes governing anion abundances in different dense interstellar clouds. This research contributes toward the growing body of evidence that carbon chain anions are relatively abundant in interstellar clouds throughout the Galaxy, but especially in the regions of relatively high density and high depletion surrounding pre-stellar cores and young, embedded protostars. C1 [Cordiner, M. A.; Charnley, S. B.] NASA, Goddard Space Flight Ctr, Astrochem Lab, Greenbelt, MD 20771 USA. [Cordiner, M. A.; Charnley, S. B.] NASA, Goddard Space Flight Ctr, Goddard Ctr Astrobiol, Greenbelt, MD 20771 USA. [Buckle, J. V.] Univ Cambridge, Cavendish Astrophys Grp, Cambridge CB3 0HE, England. [Buckle, J. V.] Univ Cambridge, Kavli Inst Cosmol, Inst Astron, Cambridge CB3 0HE, England. [Walsh, C.; Millar, T. J.] Queens Univ Belfast, Astrophys Res Ctr, Sch Math & Phys, Belfast BT7 1NN, Antrim, North Ireland. RP Cordiner, MA (reprint author), NASA, Goddard Space Flight Ctr, Astrochem Lab, Code 691,8800 Greenbelt Rd, Greenbelt, MD 20771 USA. EM martin.cordiner@nasa.gov RI Charnley, Steven/C-9538-2012; OI Millar, Tom/0000-0001-5178-3656 FU NASA; Goddard Center for Astrobiology; STFC FX This research was supported by the NASA Exobiology Program and the Goddard Center for Astrobiology. Astrophysics at QUB is supported by a grant from STFC. NR 50 TC 26 Z9 26 U1 1 U2 10 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 APR 1 PY 2011 VL 730 IS 2 AR L18 DI 10.1088/2041-8205/730/2/L18 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 797KK UT WOS:000293125600006 ER PT J AU Gilli, R Su, J Norman, C Vignali, C Comastri, A Tozzi, P Rosati, P Stiavelli, M Brandt, WN Xue, YQ Luo, B Castellano, M Fontana, A Fiore, F Mainieri, V Ptak, A AF Gilli, R. Su, J. Norman, C. Vignali, C. Comastri, A. Tozzi, P. Rosati, P. Stiavelli, M. Brandt, W. N. Xue, Y. Q. Luo, B. Castellano, M. Fontana, A. Fiore, F. Mainieri, V. Ptak, A. TI A COMPTON-THICK ACTIVE GALACTIC NUCLEUS AT z similar to 5 IN THE 4 Ms CHANDRA DEEP FIELD SOUTH SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE galaxies: active; galaxies: high-redshift; X-rays: galaxies ID STAR-FORMATION RATE; BLACK-HOLES; SUBMILLIMETER GALAXY; INFRARED GALAXIES; HELLAS2XMM SURVEY; SOURCE CATALOGS; SPACE DENSITY; OBSCURED AGN; STELLAR MASS; RAY AB We report the discovery of a Compton-thick active galactic nucleus (AGN) at z = 4.76 in the 4 Ms Chandra Deep Field South. This object was selected as a V-band dropout in HST/ACS images and previously recognized as an AGN from optical spectroscopy. The 4Ms Chandra observations show a significant (similar to 4.2 sigma) X-ray detection at the V-band dropout position. The X-ray source displays a hardness ratio of HR = 0.23 +/- 0.24, which, for a source at z similar to 5, is highly suggestive of Compton-thick absorption. The source X-ray spectrum is seen above the background level in the energy range of similar to 0.9-4 keV, i.e., in the rest-frame energy range of similar to 5-23 keV. When fixing the photon index to Gamma = 1.8, the measured column density is N-H = 1.4(-0.5)(+0.9) x 10(24) cm(-2), which is Compton thick. To our knowledge, this is the most distant heavily obscured AGN, confirmed by X-ray spectral analysis, discovered so far. The intrinsic (de-absorbed), rest-frame luminosity in the 2-10 keV band is similar to 2.5 x 10(44) erg s(-1), which places this object among type-2 quasars. The spectral energy distribution shows that massive star formation is associated with obscured black hole (BH) accretion. This system may have then been caught during a major coeval episode of BH and stellar mass assembly at early times. The measure of the number density of heavily obscured AGN at high redshifts will be crucial to reconstructing the BH/galaxy evolution history from the beginning. C1 [Gilli, R.; Comastri, A.] INAF Osservatorio Astron Bologna, I-40127 Bologna, Italy. [Su, J.; Norman, C.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Norman, C.; Stiavelli, M.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Vignali, C.] Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy. [Tozzi, P.] INAF Osservatorio Astron Trieste, I-34131 Trieste, Italy. [Rosati, P.; Mainieri, V.] European So Observ, D-85748 Garching, Germany. [Brandt, W. N.; Xue, Y. Q.; Luo, B.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Brandt, W. N.; Xue, Y. Q.; Luo, B.] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA. [Castellano, M.; Fontana, A.; Fiore, F.] INAF Osservatorio Astron Roma, I-00040 Monte Porzio Catone, Italy. [Ptak, A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Gilli, R (reprint author), INAF Osservatorio Astron Bologna, Via Ranzani 1, I-40127 Bologna, Italy. EM roberto.gilli@oabo.inaf.it RI Vignali, Cristian/J-4974-2012; Brandt, William/N-2844-2015; Comastri, Andrea/O-9543-2015; Gilli, Roberto/P-1110-2015; OI Vignali, Cristian/0000-0002-8853-9611; Brandt, William/0000-0002-0167-2453; Comastri, Andrea/0000-0003-3451-9970; Gilli, Roberto/0000-0001-8121-6177; Castellano, Marco/0000-0001-9875-8263; fontana, adriano/0000-0003-3820-2823; Fiore, Fabrizio/0000-0002-4031-4157 FU Italian Space Agency (ASI) under the ASI-INAF [I/009/10/0, I/088/06/0]; NASA [SP1-12007A, NNX10AC99G]; Chandra archival grant [SP89004X]; DFG cluster of excellence Origin and Structure of the Universe FX We acknowledge the following supporting agencies and grants: Italian Space Agency (ASI) under the ASI-INAF contracts I/009/10/0 and I/088/06/0 (R. G., C. V., A. C.); NASA through CXC grant SP1-12007A and ADP grant NNX10AC99G (W.N.B., Y.Q.X., B. L.); Chandra archival grant SP89004X (A. P., R. G.); DFG cluster of excellence Origin and Structure of the Universe (P. R.). We thank the referee for a constructive report and N. Miller and M. Mignoli for useful discussions. R. G. gratefully acknowledges hospitality by the Johns Hopkins University where this work started. NR 51 TC 31 Z9 31 U1 0 U2 9 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 APR 1 PY 2011 VL 730 IS 2 AR L28 DI 10.1088/2041-8205/730/2/L28 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 797KK UT WOS:000293125600016 ER PT J AU Morales, FY Rieke, GH Werner, MW Bryden, G Stapelfeldt, KR Su, KYL AF Morales, Farisa Y. Rieke, G. H. Werner, M. W. Bryden, G. Stapelfeldt, K. R. Su, K. Y. L. TI COMMON WARM DUST TEMPERATURES AROUND MAIN-SEQUENCE STARS SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE circumstellar matter; infrared: stars; interplanetary medium ID SPITZER-SPACE-TELESCOPE; SUN-LIKE STARS; TURBULENT PROTOPLANETARY DISKS; DEBRIS DISKS; SNOW LINE; ASTEROID BELT; HR 8799; EMISSION; POPULATION; COLLISIONS AB We compare the properties of warm dust emission from a sample of main-sequence A-type stars (B8-A7) to those of dust around solar-type stars (F5-K0) with similar Spitzer Space Telescope Infrared Spectrograph/MIPS data and similar ages. Both samples include stars with sources with infrared spectral energy distributions that show evidence of multiple components. Over the range of stellar types considered, we obtain nearly the same characteristic dust temperatures (similar to 190 K and similar to 60 K for the inner and outer dust components, respectively)-slightly above the ice evaporation temperature for the inner belts. The warm inner dust temperature is readily explained if populations of small grains are being released by sublimation of ice from icy planetesimals. Evaporation of low-eccentricity icy bodies at similar to 150 K can deposit particles into an inner/warm belt, where the small grains are heated to T-dust similar to 190 K. Alternatively, enhanced collisional processing of an asteroid belt-like system of parent planetesimals just interior to the snow line may account for the observed uniformity in dust temperature. The similarity in temperature of the warmer dust across our B8-K0 stellar sample strongly suggests that dust-producing planetesimals are not found at similar radial locations around all stars, but that dust production is favored at a characteristic temperature horizon. C1 [Morales, Farisa Y.; Werner, M. W.; Bryden, G.; Stapelfeldt, K. R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Morales, Farisa Y.] Univ So Calif, Dept Phys & Astron, Los Angeles, CA 90089 USA. [Rieke, G. H.; Su, K. Y. L.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Bryden, G.] CALTECH, NExScI, NASA Exoplanet Sci Inst, Pasadena, CA 91125 USA. RP Morales, FY (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Farisa@jpl.nasa.gov RI Stapelfeldt, Karl/D-2721-2012; OI Su, Kate/0000-0002-3532-5580 FU NASA [1407] FX We thank Paul Weissman and Neal Turner (JPL) for their helpful comments and stimulating discussions, and the referee for the careful reading and detailed comments. This work is based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under NASA contract 1407. NR 40 TC 59 Z9 59 U1 0 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD APR 1 PY 2011 VL 730 IS 2 AR L29 DI 10.1088/0004-637X/730/2/L29 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 797KK UT WOS:000293125600017 ER PT J AU Raga, AC Noriega-Crespo, A Lora, V Stapelfeldt, KR Carey, SJ AF Raga, A. C. Noriega-Crespo, A. Lora, V. Stapelfeldt, K. R. Carey, S. J. TI THE JET/COUNTERJET INFRARED SYMMETRY OF HH 34 AND THE SIZE OF THE JET FORMATION REGION SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE circumstellar matter; Herbig-Haro objects; infrared: ISM; ISM: individual objects (HH 34); ISM: jets and outflows; stars: formation ID SPITZER-SPACE-TELESCOPE; BOW SHOCK; HH-34 JET; IMAGES; KINEMATICS; EVOLUTION; EMISSION; OUTFLOWS; COMPLEX; SYSTEM AB We present new Spitzer IRAC images of the HH 34 outflow. These are the first images that detect both the knots along the southern jet and the northern counterjet (the counterjet knots were only detected previously in a long-slit spectrum). This result removes the problem of the apparent coexistence of a large-scale symmetry (at distances of up to similar to 1 pc) and a complete lack of symmetry close to the source (at distances of similar to 10(17) cm) for this outflow. We present a quantitative evaluation of the newly found symmetry between the HH 34 jet and counterjet, and show that the observed degree of symmetry implies that the jet production region has a characteristic size < 2.8 AU. This is the strongest constraint yet derived for the size of the region in which HH jets are produced. C1 [Raga, A. C.] Univ Nacl Autonoma Mexico, Inst Ciencias Nucl, Mexico City 04510, DF, Mexico. [Noriega-Crespo, A.; Carey, S. J.] CALTECH, SPITZER Sci Ctr, Pasadena, CA 91125 USA. [Lora, V.] Univ Heidelberg, Astron Rechen Inst Zentrum Astron, D-69120 Heidelberg, Germany. [Stapelfeldt, K. R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Raga, AC (reprint author), Univ Nacl Autonoma Mexico, Inst Ciencias Nucl, Ap 70-543, Mexico City 04510, DF, Mexico. FU NASA [1407]; CONACyT [61547, 101356, 101975] 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. The work of A. R. and V. L. was supported by the CONACyT grants 61547, 101356, and 101975. NR 30 TC 11 Z9 11 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD APR 1 PY 2011 VL 730 IS 2 AR L17 DI 10.1088/2041-8205/730/2/L17 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 797KK UT WOS:000293125600005 ER PT J AU Halkides, D Lee, T AF Halkides, Daria Lee, Tong TI Mechanisms controlling seasonal mixed layer temperature and salinity in the Southwestern Tropical Indian Ocean SO DYNAMICS OF ATMOSPHERES AND OCEANS LA English DT Article DE Indian Ocean; Thermocline ridge; Mixed layer budgets ID SHALLOW-WATER SIMULATIONS; SEA-LEVEL VARIATIONS; INTERANNUAL VARIABILITY; INTRASEASONAL VARIABILITY; STATISTICAL PREDICTION; INDONESIAN THROUGHFLOW; CIRCULATION MODEL; SURFACE CURRENTS; HEAT-TRANSPORT; PACIFIC-OCEAN AB We use a heat-and salt-conserving ocean state estimation product to study the seasonal cycles of the mixed layer (ML) temperature (MLT) and salinity (MIS) balances over the southwestern tropical Indian Ocean (SWTIO) thermocline ridge (STR; 50 degrees-75 degrees E, 12 degrees-5 degrees S). For seasonal MLT, surface heat flux and ocean processes are both important. They tend to re-enforce each other during peak cooling (May-June) and warming (November) periods, but not during transition periods. The dominant ocean process is wind-driven vertical mixing. It is modulated by the variable strength of the monsoon winds (which affect the vertical diffusivity), and to a lesser extent by variability of thermocline depth (which influences the vertical stratification across the ML base). For example, thermocline shoaling in April-July alters the vertical stratification near the ML base; thus, when the monsoon winds heighten (June-September) and the vertical diffusivity increases (deepening the ML base), relatively cool subsurface water is near the ML base and easily incorporated into the ML by vertical mixing. However, vertical advection as a direct response to thermocline shoaling has little affect on MLT. This explains why MLT and thermocline depth are not positively correlated here on the seasonal timescale (as they are on the interannual timescale). Meridional advection associated with Ekman transport driven by the monsoon winds plays a secondary role. Seasonal MLS, however, is dominated by meridional advection. Vertical process effects on MLS are small, due to a weak salinity gradient near the ML base throughout the year. (C) 2011 Elsevier B.V. All rights reserved. C1 [Halkides, Daria] Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA 90024 USA. [Halkides, Daria; Lee, Tong] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Halkides, D (reprint author), Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA 90024 USA. EM halkides@jpl.nasa.gov FU NASA; PO.DAAC (http://podaac.jpl.nasa.gov) FX This research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA. Support by PO.DAAC (http://podaac.jpl.nasa.gov) is acknowledged. The 1992-2002 mean ocean dynamic topography data was obtained from Nikolai Maximenko (IPRC) and Peter Niiler (SIO; http://apdrc.soest.hawaii.edu/projects/DOT/index.html). NR 64 TC 11 Z9 12 U1 1 U2 20 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0377-0265 J9 DYNAM ATMOS OCEANS JI Dyn. Atmos. Oceans PD APR PY 2011 VL 51 IS 3 BP 77 EP 93 DI 10.1016/j.dynatmoce.2011.03.002 PG 17 WC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences; Oceanography SC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences; Oceanography GA 795AV UT WOS:000292944800002 ER PT J AU Hagler, P Johnson, RW Chen, LY AF Hagler, Ping Johnson, R. Wayne Chen, Liang-Yu TI SiC Die Attach Metallurgy and Processes for Applications up to 500 degrees C SO IEEE TRANSACTIONS ON COMPONENTS PACKAGING AND MANUFACTURING TECHNOLOGY LA English DT Article DE Die attach; die metallization; high temperature; liquid transient phase bonding ID LOW-TEMPERATURE AB The challenges of packaging SiC-based electronics for high-temperature applications include their high operating temperatures, wide thermal cycle ranges, and, sometimes, high currents and high voltages. As a result, the selection of metallurgy for high-temperature SiC die attach is crucial to a successful package design, which involves chip metallization, substrate metallization, and die attach alloy. This paper examines off-eutectic Au-Sn as the die attach alloy with a PtAu thick film metallization on AlN substrates. A pure Au thick film layer was printed over the PtAu thick film layer. AlN substrates metalized with refractory MoMn and electroplated Ni/Au were also used. Two different die attach approaches have been investigated, using Sn-Au-Sn off-eutectic thick foil and limited-volume eutectic AuSn (80/20 wt.%) preform. The SiC backside metallizations evaluated were Ti/TaSi(2)/Pt/Au and Cr/NiCr/Au. Die shear tests were performed after aging at 500 degrees C and after thermal cycling. The shear test results and failure surface analysis are discussed. C1 [Hagler, Ping] Auburn Univ, Dept Elect & Comp Engn, Auburn, AL 36849 USA. [Johnson, R. Wayne] Auburn Univ, Dept Elect & Commun Engn, Auburn, AL 36849 USA. [Chen, Liang-Yu] NASA, Glenn Res Ctr, Ohio Aerosp Inst, Cleveland, OH 44135 USA. RP Hagler, P (reprint author), Missile Def Agcy, Dept Def, Washington, DC 20301 USA. EM ping.hagler@hotmail.com; john-son@eng.auburn.edu; liangyu.chen-1@nasa.gov FU National Aeronautics and Space Administration (NASA) [NNC07ZA11A] FX This work was supported in part by the Integrated Vehicle Health Management Project of National Aeronautics and Space Administration (NASA) Aviation Safety Program under the NASA Research Announcement Grant NNC07ZA11A monitored by G. W. Hunter at the NASA Glenn Research Center. Recommended for publication by Associate Editor I. Fidan upon evaluation of reviewers' comments. NR 14 TC 11 Z9 11 U1 0 U2 12 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 2156-3950 J9 IEEE T COMP PACK MAN JI IEEE Trans. Compon. Pack. Manuf. Technol. PD APR PY 2011 VL 1 IS 4 BP 630 EP 639 DI 10.1109/TCPMT.2011.2106160 PG 10 WC Engineering, Manufacturing; Engineering, Electrical & Electronic; Materials Science, Multidisciplinary SC Engineering; Materials Science GA 793MP UT WOS:000292827500019 ER PT J AU Sun, J Choi, KK Jhabvala, MD Jhabvala, C AF Sun, Jason Choi, Kwong-Kit Jhabvala, Merzy D. Jhabvala, Christine TI Advanced substrate thinning process for GaAs-based devices SO JOURNAL OF MICRO-NANOLITHOGRAPHY MEMS AND MOEMS LA English DT Article DE inductively coupled plasma selective etching; corrugated quantum well infrared photodetector focal plane arrays; GaAs substrate thinning ID ALGAAS; ETCH; PLASMAS; LAYERS; DAMAGE AB We developed an optimized substrate removal process for GaAs-based opto-electronic devices by establishing a reliable two-step process. In this process, the substrate is first thinned by mechanical lapping and then followed by selective high density plasma etching. The adopted inductively coupled plasma etching, having an optimized boron trichloride (BCl3)/sulfur hexafluoride (SF6)/argon composition, shows a nearly infinite etching selectivity for the GaAs substrate over the aluminum gallium arsenide (AlxGa1-xAs) etch-stop layer. The surface of the die is perfectly smooth and mirror-like after processing. In addition to its simplicity, the process is also highly reproducible and shows no damage to the underlying detector material. (C) 2011 Society of Photo-Optical Instrumentation Engineers (SPIE). [DOI:10.1117/1.3580755] C1 [Sun, Jason; Choi, Kwong-Kit] USA, Res Lab, Adelphi, MD 20783 USA. [Jhabvala, Merzy D.; Jhabvala, Christine] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Sun, J (reprint author), USA, Res Lab, Adelphi, MD 20783 USA. EM jason.sun@arl.army.mil RI Choi, Kwong-Kit/K-9205-2013 NR 11 TC 5 Z9 5 U1 0 U2 3 PU SPIE-SOC PHOTO-OPTICAL INSTRUMENTATION ENGINEERS PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98225 USA SN 1932-5150 J9 J MICRO-NANOLITH MEM JI J. Micro-Nanolithogr. MEMS MOEMS PD APR-JUN PY 2011 VL 10 IS 2 AR 023004 DI 10.1117/1.3580755 PG 4 WC Engineering, Electrical & Electronic; Nanoscience & Nanotechnology; Materials Science, Multidisciplinary; Optics SC Engineering; Science & Technology - Other Topics; Materials Science; Optics GA 787JU UT WOS:000292373200006 ER PT J AU Wahlgren, GM AF Wahlgren, Glenn M. TI Atomic data for stellar astrophysics: from the UV to the IR SO CANADIAN JOURNAL OF PHYSICS LA English DT Article; Proceedings Paper CT 10th International Colloquium on AtomicSpectroscopy and Oscillator Strengths for Astrophysical andLaboratory Plasmas (ASOS) CY AUG 03-07, 2010 CL Berkeley, CA ID CHEMICALLY PECULIAR STAR; FINE-STRUCTURE LINES; TRANSITION-PROBABILITIES; OSCILLATOR-STRENGTHS; ENERGY-LEVELS; WAVELENGTH DETERMINATIONS; SPECTRAL CLASSIFICATION; RADIATIVE LIFETIMES; EMISSION-LINES; COOL STARS AB The study of stars and stellar evolution relies heavily on the analysis of stellar spectra. The need for atomic line data from the ultraviolet (UV) to the infrared (IR) regions is greater now than ever. In the past twenty years, the time since the launch of the Hubble Space Telescope, great progress has been made in acquiring atomic data for UV transitions. The optical wavelength region, now expanded by progress in detector technology, continues to provide motivation for new atomic data. In addition, investments in new instrumentation for ground-based and space observatories has lead to the availability of high-quality spectra at IR wavelengths, where the need for atomic data is most critical. In this review, examples are provided of the progress made in generating atomic data for stellar studies, with a look to the future for addressing the accuracy and completeness of atomic data for anticipated needs. C1 [Wahlgren, Glenn M.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA. [Wahlgren, Glenn M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Wahlgren, GM (reprint author), NASA, Goddard Space Flight Ctr, Code 667, Greenbelt, MD 20771 USA. EM glenn.m.wahlgren@nasa.gov FU NASA [NNG06GJ29G] FX The author acknowledges support from NASA grant NNG06GJ29G. NR 66 TC 3 Z9 3 U1 1 U2 4 PU CANADIAN SCIENCE PUBLISHING, NRC RESEARCH PRESS PI OTTAWA PA 65 AURIGA DR, SUITE 203, OTTAWA, ON K2E 7W6, CANADA SN 0008-4204 EI 1208-6045 J9 CAN J PHYS JI Can. J. Phys. PD APR PY 2011 VL 89 IS 4 BP 345 EP 356 DI 10.1139/P10-125 PG 12 WC Physics, Multidisciplinary SC Physics GA 775QA UT WOS:000291475700005 ER PT J AU Sterling, NC Witthoeft, MC Esteves, DA Bilodeau, RC Kilcoyne, ALD Red, EC Phaneuf, RA Alna'Washi, G Aguilar, A AF Sterling, N. C. Witthoeft, M. C. Esteves, D. A. Bilodeau, R. C. Kilcoyne, A. L. D. Red, E. C. Phaneuf, R. A. Alna'Washi, G. Aguilar, A. TI New atomic data for trans-iron elements and their application to abundance determinations in planetary nebulae SO CANADIAN JOURNAL OF PHYSICS LA English DT Article; Proceedings Paper CT 10th International Colloquium on AtomicSpectroscopy and Oscillator Strengths for Astrophysical andLaboratory Plasmas (ASOS) CY AUG 03-07, 2010 CL Berkeley, CA ID GIANT BRANCH STARS; NEUTRON-CAPTURE ELEMENTS; EFFECTIVE COLLISION STRENGTHS; S-PROCESS; CHARGE-TRANSFER; DIELECTRONIC RECOMBINATION; FORBIDDEN TRANSITIONS; CROSS-SECTIONS; MASSIVE STARS; CONFIGURATIONS AB Investigations of neutron(n)-capture element nucleosynthesis and chemical evolution have largely been based on stellar spectroscopy. However, the recent detection of these elements in several planetary nebulae (PNe) indicates that nebular spectroscopy is a promising new tool for such studies. In PNe, n-capture element abundance determinations reveal details of s-process nucleosynthesis and convective mixing in evolved low-mass stars, as well as the chemical evolution of elements that cannot be detected in stellar spectra. Only one or two ions of a given trans-iron element can typically be detected in individual nebulae. Elemental abundance determinations thus require corrections for the abundances of unobserved ions. Such corrections rely on the availability of atomic data for processes that control the ionization equilibrium of nebulae (e. g., photoionization cross sections and rate coefficients for various recombination processes). Until recently, these data were unknown for virtually all n-capture element ions. For the first six ions of Se, Kr, and Xe - the three most widely detected n-capture elements in PNe we are calculating photoionization cross sections and radiative and dielectronic recombination rate coefficients using the multi-configuration Breit-Pauli atomic structure code AUTOSTRUCTURE. Charge transfer rate coefficients are being determined with a multichannel Landau-Zener code. To calibrate these calculations, we have measured absolute photoionization cross sections of Se and Xe ions at the Advanced Light Source synchrotron radiation facility. These atomic data can be incorporated into photoionization codes, which we will use to derive ionization corrections (hence abundances) for Se, Kr, and Xe in ionized nebulae. Using Monte Carlo simulations, we will investigate the effects of atomic data uncertainties on the derived abundances, illuminating the systems and atomic processes that require further analysis. These results are critical for honing nebular spectroscopy into a more effective tool for investigating the production and chemical evolution of trans-iron elements in the Universe. C1 [Sterling, N. C.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. [Witthoeft, M. C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Esteves, D. A.; Phaneuf, R. A.; Alna'Washi, G.] Univ Nevada, Dept Phys, Reno, NV 89557 USA. [Bilodeau, R. C.] Western Michigan Univ, Dept Phys, Kalamazoo, MI 49008 USA. [Kilcoyne, A. L. D.; Red, E. C.; Aguilar, A.] Univ Calif Berkeley, Lawrence Berkeley Lab, Berkeley, CA 94720 USA. RP Sterling, NC (reprint author), Michigan State Univ, Dept Phys & Astron, 3248 Biomed Phys Sci, E Lansing, MI 48824 USA. EM sterling@pa.msu.edu RI Kilcoyne, David/I-1465-2013; OI Bilodeau, Rene/0000-0001-8607-2328 FU Office of Science, Office of Basic Energy Sciences, of the US Department of Energy [DE-AC02-05CH11231, DE-AC03-76SF-00098, DE-FG02-03ER15424]; National Science Foundation [AST-0901432]; NASA [06-APRA206-0049]; NASA Goddard Space Flight Center [NNX08AJ96G] FX We acknowledge support by the Director, Office of Science, Office of Basic Energy Sciences, of the US Department of Energy under contracts DE-AC02-05CH11231, DE-AC03-76SF-00098, and grant DE-FG02-03ER15424. N. C. Sterling acknowledges support from an National Science Foundation Astronomy and Astrophysics Postdoctoral Fellowship under award AST-0901432 and from NASA grant 06-APRA206-0049. D. Esteves acknowledges support from grant NNX08AJ96G with NASA Goddard Space Flight Center and the Doctoral Fellowship Program at the Advanced Light Source. We thank N. R. Badnell for many enlightening discussions regarding AUTOSTRUCTURE, and P. Stancil for helpful discussions and providing a code for our CT calculations. NR 57 TC 7 Z9 7 U1 0 U2 7 PU CANADIAN SCIENCE PUBLISHING, NRC RESEARCH PRESS PI OTTAWA PA 65 AURIGA DR, SUITE 203, OTTAWA, ON K2E 7W6, CANADA SN 0008-4204 EI 1208-6045 J9 CAN J PHYS JI Can. J. Phys. PD APR PY 2011 VL 89 IS 4 BP 379 EP 385 DI 10.1139/P10-105 PG 7 WC Physics, Multidisciplinary SC Physics GA 775QA UT WOS:000291475700009 ER PT J AU Forth, KE Fiedler, MJ Paloski, WH AF Forth, Katharine E. Fiedler, Matthew J. Paloski, William H. TI Estimating functional stability boundaries for bipedal stance SO GAIT & POSTURE LA English DT Article DE Balance control; Stability limits; Falls; Time-to-boundary; Stability margin ID TIME; POSTUROGRAPHY; CONTACT; LIMITS; AGE AB We propose a technique to estimate functional limits of stability (LOS) during bipedal stance using a controlled, low speed, voluntary leaning protocol requiring feet to remain in contact with the ground. LOS are estimated from ellipses fit to center-of-mass position data obtained during the leaning protocol. The LOS of nine healthy subjects were found to be 20-59% closer to the center of stance than the more frequently used anatomical boundaries and were reduced by closing the eyes. We conclude that functional stability boundaries should be used when the outcome measure is related to fall risk. Published by Elsevier B.V. C1 [Paloski, William H.] Univ Houston, Ctr Neuromotor & Biomech Res, Houston, TX 77204 USA. [Forth, Katharine E.] Univ Space Res Assoc, Houston, TX USA. [Fiedler, Matthew J.] Wyle Integrated Sci & Engn Grp, Houston, TX USA. [Paloski, William H.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. RP Paloski, WH (reprint author), Univ Houston, Ctr Neuromotor & Biomech Res, 3855 Holman St,Garrison 104, Houston, TX 77204 USA. EM whpaloski@uh.edu NR 10 TC 6 Z9 6 U1 0 U2 7 PU ELSEVIER IRELAND LTD PI CLARE PA ELSEVIER HOUSE, BROOKVALE PLAZA, EAST PARK SHANNON, CO, CLARE, 00000, IRELAND SN 0966-6362 J9 GAIT POSTURE JI Gait Posture PD APR PY 2011 VL 33 IS 4 BP 715 EP 717 DI 10.1016/j.gaitpost.2010.12.024 PG 3 WC Neurosciences; Orthopedics; Sport Sciences SC Neurosciences & Neurology; Orthopedics; Sport Sciences GA 771EI UT WOS:000291139600036 PM 21277211 ER PT J AU Barker, HW Jerg, MP Wehr, T Kato, S Donovan, DP Hogan, RJ AF Barker, H. W. Jerg, M. P. Wehr, T. Kato, S. Donovan, D. P. Hogan, R. J. TI A 3D cloud-construction algorithm for the EarthCARE satellite mission SO QUARTERLY JOURNAL OF THE ROYAL METEOROLOGICAL SOCIETY LA English DT Article DE cloud; radiative transfer; satellite; EarthCARE ID ANGULAR-DISTRIBUTION MODELS; RADIATIVE FLUX ESTIMATION; ENERGY SYSTEM INSTRUMENT; ACCURATE PARAMETERIZATION; OPTICAL-PROPERTIES; UNRESOLVED CLOUDS; TERRA SATELLITE; CLIMATE MODELS; CIRRUS CLOUDS; WATER CLOUDS AB This article presents and assesses an algorithm that constructs 3D distributions of cloud from passive satellite imagery and collocated 2D nadir profiles of cloud properties inferred synergistically from lidar, cloud radar and imager data. It effectively widens the active-passive retrieved cross-section (RXS) of cloud properties, thereby enabling computation of radiative fluxes and radiances that can be compared with measured values in an attempt to perform radiative closure experiments that aim to assess the RXS. For this introductory study, A-train data were used to verify the scene-construction algorithm and only 1D radiative transfer calculations were performed. The construction algorithm fills off-RXS recipient pixels by computing sums of squared differences (a cost function F) between their spectral radiances and those of potential donor pixels/columns on the RXS. Of the RXS pixels with F lower than a certain value, the one with the smallest Euclidean distance to the recipient pixel is designated as the donor, and its retrieved cloud properties and other attributes such as 1D radiative heating rates are consigned to the recipient. It is shown that both the RXS itself and Moderate Resolution Imaging Spectroradiometer (MODIS) imagery can be reconstructed extremely well using just visible and thermal infrared channels. Suitable donors usually lie within 10 km of the recipient. RXSs and their associated radiative heating profiles are reconstructed best for extensive planar clouds and less reliably for broken convective clouds. Domain-average 1D broadband radiative fluxes at the top of the atmosphere (TOA) for (21 km) 2 domains constructed from MODIS, CloudSat and Cloud-Aerosol Lidar and Infrared Pathfinder Satellite Observations (CALIPSO) data agree well with coincidental values derived from Clouds and the Earth's Radiant Energy System (CERES) radiances: differences between modelled and measured reflected shortwave fluxes are within +/- 10 Wm(-2) for similar to 35% of the several hundred domains constructed for eight orbits. Correspondingly, for outgoing longwave radiation similar to 65% are within +/- 10 W m(-2). Copyright (C) 2011 Royal Meteorological Society and Crown in the right of Canada. C1 [Barker, H. W.] Environm Canada, Cloud Phys & Severe Weather Res Sect ARMP, Toronto, ON M3H 5T4, Canada. [Wehr, T.] European Space Agcy, NL-2200 AG Noordwijk, Netherlands. [Kato, S.] NASA, Langley Res Ctr, Hampton, VA 23665 USA. [Donovan, D. P.] KNMI, De Bilt, Netherlands. [Hogan, R. J.] Univ Reading, Reading, Berks, England. RP Barker, HW (reprint author), Environm Canada, Cloud Phys & Severe Weather Res Sect ARMP, 4905 Dufferin St, Toronto, ON M3H 5T4, Canada. EM howard.barker@ec.gc.ca RI Hogan, Robin/M-6549-2016 OI Hogan, Robin/0000-0002-3180-5157 FU European Space Agency FX This study was supported by a contract issued to Environment Canada by the European Space Agency under the EarthCARE component of its Living Planet Programme. NR 36 TC 24 Z9 24 U1 0 U2 12 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-9009 J9 Q J ROY METEOR SOC JI Q. J. R. Meteorol. Soc. PD APR PY 2011 VL 137 IS 657 BP 1042 EP 1058 DI 10.1002/qj.824 PN B PG 17 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 777CU UT WOS:000291592800016 ER PT J AU Liu, Z Ostrenga, D Leptoukh, G AF Liu, Zhong Ostrenga, Dana Leptoukh, Gregory TI ONLINE VISUALIZATION AND ANALYSIS OF GLOBAL HALF-HOURLY INFRARED SATELLITE DATA SO BULLETIN OF THE AMERICAN METEOROLOGICAL SOCIETY LA English DT Article C1 [Liu, Zhong] George Mason Univ, CSISS, Fairfax, VA 22030 USA. [Liu, Zhong; Ostrenga, Dana; Leptoukh, Gregory] NASA, Goddard Space Flight Ctr, NASA Goddard Earth Sci GES, Data & Informat Serv Ctr DISC, Greenbelt, MD 20771 USA. [Ostrenga, Dana] ADNET Syst, Rockville, MD USA. RP Liu, Z (reprint author), George Mason Univ, CSISS, 4400 Univ Dr,MSN 6E1, Fairfax, VA 22030 USA. EM Zhong.Liu@nasa.gov NR 3 TC 1 Z9 1 U1 0 U2 2 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 APR PY 2011 VL 92 IS 4 BP 429 EP 432 DI 10.1175/2010BAMS2976.1 PG 4 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 773QT UT WOS:000291323900002 ER PT J AU Gorchakov, GI Sviridenkov, MA Semoutnikova, EG Chubarova, NY Holben, BN Smirnov, AV Emilenko, AS Isakov, AA Kopeikin, VM Karpov, AV Lezina, EA Zadorozhnaya, OS AF Gorchakov, G. I. Sviridenkov, M. A. Semoutnikova, E. G. Chubarova, N. Y. Holben, B. N. Smirnov, A. V. Emilenko, A. S. Isakov, A. A. Kopeikin, V. M. Karpov, A. V. Lezina, E. A. Zadorozhnaya, O. S. TI Optical and microphysical parameters of the aerosol in the smoky atmosphere of the Moscow region in 2010 SO DOKLADY EARTH SCIENCES LA English DT Article ID SURFACE AEROSOL; FIRES C1 [Gorchakov, G. I.; Sviridenkov, M. A.; Emilenko, A. S.; Isakov, A. A.; Kopeikin, V. M.; Karpov, A. V.] Russian Acad Sci, Oboukhov Inst Atmospher Phys, Moscow 109017, Russia. [Semoutnikova, E. G.; Lezina, E. A.; Zadorozhnaya, O. S.] Mosekomonitoring, Moscow 119019, Russia. [Chubarova, N. Y.] Moscow MV Lomonosov State Univ, Moscow 119899, Russia. [Holben, B. N.; Smirnov, A. V.] NASA, Goddard Space Flight Ctr, Biospher Sci Branch, Greenbelt, MD 20771 USA. RP Gorchakov, GI (reprint author), Russian Acad Sci, Oboukhov Inst Atmospher Phys, Pyzhevskii Per 3, Moscow 109017, Russia. EM gengor@ifaran.ru RI Smirnov, Alexander/C-2121-2009 OI Smirnov, Alexander/0000-0002-8208-1304 FU Russian Foundation for Basic Research [10-05-01019] FX This work was supported in part by the Russian Foundation for Basic Research (project no. 10-05-01019). NR 14 TC 17 Z9 17 U1 0 U2 3 PU MAIK NAUKA/INTERPERIODICA/SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013-1578 USA SN 1028-334X J9 DOKL EARTH SCI JI Dokl. Earth Sci. PD APR PY 2011 VL 437 IS 2 BP 513 EP 517 DI 10.1134/S1028334X11040131 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 763PH UT WOS:000290571700016 ER PT J AU Bhagwat, MJ AF Bhagwat, Mahendra J. TI Effect of Blade Number on Induced Power in Hover SO JOURNAL OF THE AMERICAN HELICOPTER SOCIETY LA English DT Article AB Hover performance is thought to be primarily affected by rotor solidity, and it has been suggested that the blade number does not have any effect on performance while comparing rotors with the same solidity. Vortex theory inherently includes the blade number effect but does not account for chord or solidity. For example, Goldstein's classical theory for lightly loaded propellers shows the effect of blade number (independent from blade chord or solidity) on optimum loading and induced power. Simpler analytical formulations, while less accurate, are more useful for understanding these effects. This paper employs combined blade element momentum theory augmented with a finite blade number or "tip loss" effect, using Prandtl's approximation to Goldstein's theory to study induced power in hover. An examination of induced flow effects resulting from finite blade number suggests, contrary to conventional wisdom, that blade number, and not just solidity, has a primary influence on the induced power in hover. Blade aspect ratio or mean nondimensional chord, the other constituent in solidity, appears to have a much smaller and secondary influence. This paper further addresses similarity considerations that can be applied to understand induced power trends. C1 USA, Res Dev & Engn Command, Aeroflightdynam Directorate AMRDEC, Ames Res Ctr, Moffett Field, CA USA. RP Bhagwat, MJ (reprint author), USA, Res Dev & Engn Command, Aeroflightdynam Directorate AMRDEC, Ames Res Ctr, Moffett Field, CA USA. EM mahendra.bhagwat@us.army.mil NR 14 TC 1 Z9 1 U1 0 U2 1 PU AMER HELICOPTER SOC INC PI ALEXANDRIA PA 217 N WASHINGTON ST, ALEXANDRIA, VA 22314 USA SN 0002-8711 J9 J AM HELICOPTER SOC JI J. Am. Helicopter Soc. PD APR PY 2011 VL 56 IS 2 AR 022002 DI 10.4050/JAHS.56.022002 PG 8 WC Engineering, Aerospace SC Engineering GA 761RF UT WOS:000290415000002 ER PT J AU Datta, A Johnson, W AF Datta, Anubhav Johnson, Wayne TI Three-Dimensional Finite Element Formulation and Scalable Domain Decomposition for High-Fidelity Rotor Dynamic Analysis SO JOURNAL OF THE AMERICAN HELICOPTER SOCIETY LA English DT Article ID ELLIPTIC PROBLEMS; SUBSTRUCTURING METHODS; PRECONDITIONERS; CONSTRUCTION; CONSTRAINTS; FETI AB This paper implements and analyzes a dual-primal iterative substructuring method that is parallel and scalable for the solution of a three-dimensional finite element based dynamic analysis of helicopter rotor blades. The analysis is developed using isoparametric hexahedral brick finite elements. Particular emphasis is placed on the formulation of the inertial terms that are unique to rotary wing dynamics. The scalability of the solution method is studied using two prototype problems one for steady hover (symmetric) and one for transient forward flight (nonsymmetric)-both carried out on up to 48 processors with each substructure on a separate processor. In both hover and forward flight, a linear speedup is observed with number of processors, up to the point of substructure optimality. Substructure optimality and the linear speedup range are shown to depend both on the problem size as well as a corner-based global coarse problem selection. An increase in problem size extends the linear speedup range up to a new substructure optimality. A smaller coarse problem selection extends optimality to a greater number of processors. The key conclusion is that a three-dimensional finite element analysis of a helicopter rotor can be carried out in a fully parallel and scalable manner. The careful selection of substructure corner nodes that are used to construct the global coarse problem is key to extending linear speedup to as high a processor number as possible, thus minimizing the solution time for a given problem size. C1 [Datta, Anubhav] NASA, Ames Res Ctr, Sci & Technol Corp, USA,Aeroflightdynam Directorate, Moffett Field, CA 94035 USA. [Johnson, Wayne] NASA, Ames Res Ctr, Aeromech Branch, Moffett Field, CA 94035 USA. RP Datta, A (reprint author), NASA, Ames Res Ctr, Sci & Technol Corp, USA,Aeroflightdynam Directorate, Moffett Field, CA 94035 USA. EM datta@merlin.arc.nasa.gov FU U.S. Department of Defense HPC Modernization Program Office FX Material presented in this paper is a product of the CREATE-AV Element of the Computational Research and Engineering for Acquisition Tools and Environments (CREATE) Program sponsored by the U.S. Department of Defense HPC Modernization Program Office. This research is conducted at the U. S. Army Aeroflightdynamics Directorate as part of the HPC Institute of Advanced Rotorcraft Modeling and Simulation (HI-ARMS) led by Dr. Roger Strawn. NR 35 TC 0 Z9 0 U1 0 U2 3 PU AMER HELICOPTER SOC INC PI ALEXANDRIA PA 217 N WASHINGTON ST, ALEXANDRIA, VA 22314 USA SN 0002-8711 J9 J AM HELICOPTER SOC JI J. Am. Helicopter Soc. PD APR PY 2011 VL 56 IS 2 AR 022003 DI 10.4050/JAHS.56.022003 PG 14 WC Engineering, Aerospace SC Engineering GA 761RF UT WOS:000290415000003 ER PT J AU Taroyan, Y Erdelyi, R Bradshaw, SJ AF Taroyan, Y. Erdelyi, R. Bradshaw, S. J. TI Observational Signatures of Impulsively Heated Coronal Loops: Power-Law Distribution of Energies SO SOLAR PHYSICS LA English DT Article DE Heating, coronal; Flares, microflares and nanoflares; Spectral line, intensity and diagnostics ID SOLAR; NANOFLARES; OSCILLATIONS; STATISTICS; HINODE; FLARES; WAVES AB It has been established that small scale heating events, known as nanoflares, are important for solar coronal heating if the power-law distribution of their energies has a slope alpha steeper than -2 (alpha < -2). Forward modeling of impulsively heated coronal loops with a set of prescribed power-law indices alpha is performed. The power-law distribution is incorporated into the governing equations of motion through an impulsive heating term. The results are converted into synthetic Hinode/EIS observations in the 40 '' imaging mode, using a selection of spectral lines formed at various temperatures. It is shown that the intensities of the emission lines and their standard deviations are sensitive to changes in alpha. A method based on a combination of observations and forward modeling is proposed for determining whether the heating in a particular case is due to small or large scale events. The method is extended and applied to a loop structure that consists of multiple strands. C1 [Taroyan, Y.] Aberystwyth Univ, Inst Math & Phys, Aberystwyth, Dyfed, Wales. [Erdelyi, R.] Univ Sheffield, Dept Appl Math, SP2RC, Sheffield, S Yorkshire, England. [Bradshaw, S. J.] Rice Univ, Dept Phys & Astron, Houston, TX USA. [Bradshaw, S. J.] NASA, Goddard Space Flight Ctr, Solar Phys Lab, Greenbelt, MD 20771 USA. RP Taroyan, Y (reprint author), Aberystwyth Univ, Inst Math & Phys, Aberystwyth, Dyfed, Wales. EM yot@aber.ac.uk; Robertus@sheffield.ac.uk; stephen.bradshaw@nasa.gov FU NSF, Hungary [K67746] FX R.E. acknowledges NSF, Hungary (OTKA, ref. no. K67746) and M. Keray for patient encouragement. NR 30 TC 5 Z9 5 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 APR PY 2011 VL 269 IS 2 BP 295 EP 307 DI 10.1007/s11207-010-9702-5 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 762DE UT WOS:000290451700005 ER PT J AU Xu, YS Fu, LL AF Xu, Yongsheng Fu, Lee-Lueng TI Global Variability of the Wavenumber Spectrum of Oceanic Mesoscale Turbulence SO JOURNAL OF PHYSICAL OCEANOGRAPHY LA English DT Article ID GEOSTROPHIC TURBULENCE; ENERGY; ALTIMETER; FLOW; TOPEX/POSEIDON; SIMULATIONS; INSTABILITY; EDDIES; SCALES AB The wavenumber spectra of sea surface height from satellite altimeter observations have revealed complex spatial variability that cannot be explained by a universal theory of mesoscale turbulence. Near the edge of the core regions of high eddy energy, agreement is observed with the prediction of the surface quasigeostrophic (SQG) turbulence theory, which has fundamental differences from that of the traditional quasigeostrophic (QG) turbulence theory. In the core regions of high eddy energy, the spectra are consistent with frontogenesis that is not fully accounted for by the SQG theory. However, the observations in the vast ocean interior of low eddy energy exhibit substantial differences from the predictions of existing theories of oceanic mesoscale turbulence. The spectra in these regions may reflect the ocean's response to short-scale atmospheric forcing and air sea interaction. The observations presented in this paper serve as a test bed for new theories and ocean general circulation models. C1 [Xu, Yongsheng; Fu, Lee-Lueng] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Xu, YS (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM yongsheng.xu@jpl.nasa.gov FU National Aeronautics and Space Administration; Jason-1; OSTM/Jason-2 FX The research presented in the paper was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. Support from the Jason-1 and OSTM/Jason-2 projects is acknowledged. The authors thank Raffaele Ferrari, James McWilliams, Dudley Chelton, and Patrice Klein for their comments. NR 25 TC 34 Z9 34 U1 0 U2 8 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 APR PY 2011 VL 41 IS 4 BP 802 EP 809 DI 10.1175/2010JPO4558.1 PG 8 WC Oceanography SC Oceanography GA 757AV UT WOS:000290057200009 ER PT J AU Hesse, M Birn, J Zenitani, S AF Hesse, Michael Birn, Joachim Zenitani, Seiji TI Magnetic reconnection in a compressible MHD plasma SO PHYSICS OF PLASMAS LA English DT Article ID PARALLEL ELECTRIC-FIELDS AB Using steady-state resistive MHD, magnetic reconnection is reinvestigated for conditions of high resistivity/low magnetic Reynolds number, when the thickness of the diffusion region is no longer small compared to its length. Implicit expressions for the reconnection rate and other reconnection parameters are derived based on the requirements of mass, momentum, and energy conservation. These expressions are solved via simple iterative procedures. Implications specifically for low Reynolds number/high resistivity are being discussed. (C) 2011 American Institute of Physics. [doi:10.1063/1.3581077] C1 [Hesse, Michael; Zenitani, Seiji] NASA, Space Weather Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Birn, Joachim] Los Alamos Natl Lab, Los Alamos, NM 87545 USA. RP Hesse, M (reprint author), NASA, Space Weather Lab, Goddard Space Flight Ctr, Code 674, Greenbelt, MD 20771 USA. 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's MMS mission; ROSES program; JSPS FX The authors gratefully acknowledge the support by NASA's MMS mission and ROSES program. One of us (S.Z.) gratefully acknowledges the support from JSPS Fellowship for Research Abroad. NR 24 TC 7 Z9 7 U1 0 U2 2 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 APR PY 2011 VL 18 IS 4 AR 042104 DI 10.1063/1.3581077 PG 10 WC Physics, Fluids & Plasmas SC Physics GA 757TI UT WOS:000290110200006 ER PT J AU Jacquot, BC Monacos, SP Hoenk, ME Greer, F Jones, TJ Nikzad, S AF Jacquot, Blake C. Monacos, Steve P. Hoenk, Michael E. Greer, Frank Jones, Todd J. Nikzad, Shouleh TI A system and methodologies for absolute quantum efficiency measurements from the vacuum ultraviolet through the near infrared SO REVIEW OF SCIENTIFIC INSTRUMENTS LA English DT Article ID CHARGE-COUPLED-DEVICE; DELTA-DOPED CCDS; SILICON PHOTODIODES; UV; DETECTORS; PRESSURE; GROWTH; NM AB In this paper we present our system design and methodology for making absolute quantum efficiency (QE) measurements through the vacuum ultraviolet (VUV) and verify the system with delta-doped silicon CCDs. Delta-doped detectors provide an excellent platform to validate measurements through the VUV due to their enhanced UV response. The requirements for measuring QE through the VUV are more strenuous than measurements in the near UV and necessitate, among other things, the use of a vacuum monochromator, good dewar chamber vacuum to prevent on-chip condensation, and more stringent handling requirements. (C) 2011 American Institute of Physics. [doi:10.1063/1.3574220] C1 [Jacquot, Blake C.; Monacos, Steve P.; Hoenk, Michael E.; Greer, Frank; Jones, Todd J.; Nikzad, Shouleh] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Jacquot, BC (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM bcj7@cornell.edu; snikzad@jpl.nasa.gov FU National Aeronautics and Space Administration FX We gratefully acknowledge Patrick Morrissey for discussions on quantum yield and Tom Elliott for support of Cassini devices. We thank Dr. Geoffrey James for information and great discussions related to the measurement system as well as generous equipment contributions. We also thank the reviewer of this manuscript for extensive and thoughtful comments that improved the quality of this paper. The research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. NR 21 TC 9 Z9 9 U1 0 U2 4 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 0034-6748 J9 REV SCI INSTRUM JI Rev. Sci. Instrum. PD APR PY 2011 VL 82 IS 4 AR 043102 DI 10.1063/1.3574220 PG 10 WC Instruments & Instrumentation; Physics, Applied SC Instruments & Instrumentation; Physics GA 756YU UT WOS:000290051500002 PM 21528990 ER PT J AU Wang, RH Burleigh, SC Parikh, P Lin, CJ Sun, B AF Wang, Ruhai Burleigh, Scott C. Parikh, Paavan Lin, Che-Jen (Jerry) Sun, Bo TI Licklider Transmission Protocol (LTP)-Based DTN for Cislunar Communications SO IEEE-ACM TRANSACTIONS ON NETWORKING LA English DT Article DE Bundle Protocol (BP); delay-tolerant networking (DTN); interplanetary Internet (IPN); Licklider Transmission Protocol convergence layer (LTPCL); satellite communications; Transmission Control Protocol convergence layer (TCPCL) ID INTERPLANETARY INTERNET; TRANSPORT PROTOCOL; SATELLITE NETWORKS; CONGESTION CONTROL; SPACE-INTERNET; PERFORMANCE; ARCHITECTURE; TCP/IP; LINKS AB Delay/disruption-tolerant networking (DTN) technology offers a new solution to highly stressed communications in space environments, especially those with long link delay and frequent link disruptions in deep-space missions. To date, little work has been done in evaluating the performance of the available "convergence layer" protocols of DTN, especially the Licklider Transmission Protocol (LTP), when they are applied to an interplanetary Internet (IPN). In this paper, we present an experimental evaluation of the Bundle Protocol (BP) running over various "convergence layer" protocols in a simulated cislunar communications environment characterized by varying degrees of signal propagation delay and data loss. We focus on the LTP convergence layer (LTPCL) adapter running on top of UDP/IP (i.e., BP/LTPCL/UDP/IP). The performance of BP/LTPCL/UDP/IP in realistic file transfers over a PC-based network test bed is compared to that of two other DTN protocol stack options, BP/TCPCL/TCP/IP and BP/UDPCL/UDP/IP. A statistical method of t-test is also used for analysis of the experimental results. The experiment results show that LTPCL has a significant performance advantage over Transmission Control Protocol convergence layer (TCPCL) for link delays longer than 4000 ms regardless of the bit error rate (BER). For a very lossy channel with a BER of around 10(-5), LTPCL has a significant goodput advantage over TCPCL at all the link delay levels studied, with an advantage of around 3000 B/s for delays longer than 1500 ms. LTPCL has a consistently significant goodput advantage over UDPCL, around 2500-3000 B/s, at all levels of link delays and BERs. C1 [Wang, Ruhai] Soochow Univ, Sch Elect & Informat Engn, Suzhou 215006, Peoples R China. [Wang, Ruhai; Parikh, Paavan] Lamar Univ, Phillip M Drayer Dept Elect Engn, Beaumont, TX 77710 USA. [Burleigh, Scott C.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Lin, Che-Jen (Jerry)] Lamar Univ, Dept Civil Engn, Beaumont, TX 77710 USA. [Sun, Bo] Lamar Univ, Dept Comp Sci, Beaumont, TX 77710 USA. RP Wang, RH (reprint author), Soochow Univ, Sch Elect & Informat Engn, Suzhou 215006, Peoples R China. EM rwang@lamar.edu; scott.c.burleigh@jpl.nasa.gov; pparikh@lamar.edu; jerry.lin@lamar.edu; bo.sun@lamar.edu RI yu, yan/C-2322-2012; Lin, Che-Jen/K-1808-2013 OI Lin, Che-Jen/0000-0001-5990-3093 FU National Aeronautics and Space Administration; National Natural Science Foundation of China (NSFC) [61032003] FX Manuscript received March 03, 2009; revised March 02, 2010 and July 06, 2010; accepted July 17, 2010; approved by IEEE/ACM TRANSACTIONS ON NETWORKING Editor M. Liu. Date of publication December 17, 2010; date of current version April 15, 2011. The research described in this paper was performed in part at the Jet Propulsion Laboratory, California Institute of Technology, Pasadena, under a contract with the National Aeronautics and Space Administration, supported in part by the National Natural Science Foundation of China (NSFC) under Grant 61032003. NR 51 TC 32 Z9 34 U1 2 U2 14 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1063-6692 J9 IEEE ACM T NETWORK JI IEEE-ACM Trans. Netw. PD APR PY 2011 VL 19 IS 2 BP 359 EP 368 DI 10.1109/TNET.2010.2060733 PG 10 WC Computer Science, Hardware & Architecture; Computer Science, Theory & Methods; Engineering, Electrical & Electronic; Telecommunications SC Computer Science; Engineering; Telecommunications GA 754HM UT WOS:000289845700005 ER PT J AU Moayeri, N Mapar, J Tompkins, S Pahlavan, K AF Moayeri, Nader Mapar, Jalal Tompkins, Stefanie Pahlavan, Kaveh TI EMERGING OPPORTUNITIES FOR LOCALIZATION AND TRACKING SO IEEE WIRELESS COMMUNICATIONS LA English DT Editorial Material C1 [Moayeri, Nader] NIST, Gaithersburg, MD 20899 USA. [Moayeri, Nader] Hewlett Packard Labs, Imaging Technol Dept, Palo Alto, CA USA. [Moayeri, Nader] Rutgers State Univ, Dept Elect & Comp Engn, Piscataway, NJ 08855 USA. [Mapar, Jalal] SAIC, RDT&E, Mclean, VA USA. [Tompkins, Stefanie] NASA, Washington, DC 20546 USA. [Pahlavan, Kaveh] Worcester Polytech Inst, Ctr Wireless Informat Network Studies, Worcester, MA USA. RP Moayeri, N (reprint author), NIST, Gaithersburg, MD 20899 USA. EM nader.moayeri@nist.gov; Jalal.Mapar@dhs.gov; Stefanie.Tompkins@darpa.mil; kavehpahlavan@gmail.com NR 0 TC 9 Z9 9 U1 0 U2 2 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1536-1284 J9 IEEE WIREL COMMUN JI IEEE Wirel. Commun. PD APR PY 2011 VL 18 IS 2 BP 8 EP 9 PG 2 WC Computer Science, Hardware & Architecture; Computer Science, Information Systems; Engineering, Electrical & Electronic; Telecommunications SC Computer Science; Engineering; Telecommunications GA 753PI UT WOS:000289791500004 ER PT J AU Fridlind, AM Ackerman, AS AF Fridlind, Ann M. Ackerman, Andrew S. TI Estimating the Sensitivity of Radiative Impacts of Shallow, Broken Marine Clouds to Boundary Layer Aerosol Size Distribution Parameter Uncertainties for Evaluation of Satellite Retrieval Requirements SO JOURNAL OF ATMOSPHERIC AND OCEANIC TECHNOLOGY LA English DT Article ID TRADE-WIND CUMULI; CLIMATE; CONVECTION; SIMULATIONS; CONSEQUENCES; MODELS; ALBEDO AB A proposed objective of the planned Aerosol-Cloud-Ecosystem (ACE) satellite mission is to provide constraints on climate model representation of aerosol effects on clouds by retrieving profiles of aerosol number concentration, effective variance, and effective radius over the 0.1-1-mu m radius range under humidified ambient conditions with 500-m vertical resolution and uncertainties of 100%, 50%. and 10%, respectively. Shallow, broken marine clouds provide an example of conditions where boundary layer aerosol properties would be retrieved in clear-sky gaps. To quantify the degree of constraint that proposed retrievals might provide on cloud radiative forcing (CRF) simulated by climate models under such conditions, dry aerosol size distribution parameters are independently varied here in large-eddy simulations of three well-established modeling case studies. Using the rudimentary available aerosol specifications, it is found that relative changes of total dry aerosol properties in simulations can be used as a proxy for relative changes of ambient aerosol properties targeted by ACE retrievals. The sensitivity of simulated daytime shortwave CRF to the proposed uncertainty in retrieved aerosol number concentration is -15 W m(-2) in the overcast limit, roughly a factor of 2 smaller than a simple analytic estimate owing primarily to aerosol-induced reductions in simulated liquid water path across this particular set of case studies. The CRF sensitivity to proposed uncertainties in retrieved aerosol effective variance and effective radius is typically far smaller, with no corresponding analytic estimate. Generalization of the results obtained here using only three case studies would require statistical analysis of relevant meteorological and aerosol observations and quantification of observational and model uncertainties and biases. C1 [Fridlind, Ann M.; Ackerman, Andrew S.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. RP Fridlind, AM (reprint author), NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA. EM ann.fridlind@nasa.gov RI Ackerman, Andrew/D-4433-2012; Fridlind, Ann/E-1495-2012 OI Ackerman, Andrew/0000-0003-0254-6253; FU NASA; NASA Advanced Supercomputing Division FX Financial and computational support was provided by the NASA Radiation Sciences Program and the NASA Advanced Supercomputing Division. We thank three anonymous reviewers and the authors of NASA's ACE white papers for useful comments. We thank Alexander Avramov for contributions to model analysis. NR 30 TC 4 Z9 4 U1 0 U2 2 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 APR PY 2011 VL 28 IS 4 BP 530 EP 538 DI 10.1175/2010JTECHA1520.1 PG 9 WC Engineering, Ocean; Meteorology & Atmospheric Sciences SC Engineering; Meteorology & Atmospheric Sciences GA 757AZ UT WOS:000290057600006 ER PT J AU Wagner, D Papastamatiou, YP Kosaki, RK Gleason, KA McFall, GB Boland, RC Pyle, RL Toonen, RJ AF Wagner, Daniel Papastamatiou, Yannis P. Kosaki, Randall K. Gleason, Kelly A. McFall, Greg B. Boland, Raymond C. Pyle, Richard L. Toonen, Robert J. TI New Records of Commercially Valuable Black Corals (Cnidaria: Antipatharia) from the Northwestern Hawaiian Islands at Mesophotic Depths SO PACIFIC SCIENCE LA English DT Article ID ANTHOZOA ANTIPATHARIA; CARIJOA-RIISEI; ZOOGEOGRAPHY; SYSTEMATICS; ACROPORA AB Mesophotic coral reef ecosystems are notoriously undersurveyed worldwide and particularly in remote locations like the Northwestern Hawaiian Islands (NWHI). A total of 37 mixed-gas technical dives were performed to depths of 80 m across the NWHI to survey for the presence of the invasive octocoral Carijoa sp., the invasive red alga Acanthophora spicifera, and conspicuous megabenthic fauna such as black corals. The two invasive species were not recorded from any of the surveys, but two commercially valuable black coral species, Antipathes griggi and Myriopathes ulex, were found, representing substantial range expansions for these species. Antipathes griggi was recorded from the islands of Necker and Laysan in 58-70 m, and Myriopathes ulex was recorded from Necker Island and Pearl and Hermes Atoll in 58-70 in. Despite over 30 yr of research in the NWHI, these black coral species had remained undetected. The new records of these conspicuous marine species highlight the utility of deep-diving technologies in surveying the largest part of the depth range of coral reef ecosystems (40-150 m), which remains largely unexplored. C1 [Wagner, Daniel; Toonen, Robert J.] Hawaii Inst Marine Biol, Kaneohe, HI 96744 USA. [Papastamatiou, Yannis P.] Univ Florida, Florida Museum Nat Hist, Gainesville, FL 32611 USA. [Kosaki, Randall K.; Gleason, Kelly A.] NOAA Papahanaumokuakea Marine Natl Monument, Honolulu, HI 96825 USA. [McFall, Greg B.] NOAA, Natl Marine Sanctuary Program, Savannah, GA 31411 USA. [Boland, Raymond C.] Natl Marine Fisheries Serv, Pacific Isl Fisheries Sci Ctr, Honolulu, HI 96822 USA. [Pyle, Richard L.] Bernice P Bishop Museum, Honolulu, HI 96817 USA. RP Wagner, D (reprint author), Hawaii Inst Marine Biol, Kaneohe, HI 96744 USA. EM wagnerda@hawaii.edu RI Toonen, Rob/K-2891-2012 OI Toonen, Rob/0000-0001-6339-4340 FU Western Pacific Fisheries Management Council to the University of Hawai'i through the NOAA [NA07N-MF4410114]; NSF [OCE-0623678]; NMSP MOA [2005-008/66882] FX This work was funded in part by the Western Pacific Fisheries Management Council to the University of Hawai'i through the NOAA Coral Reef Conservation Giant Program under award number NA07N-MF4410114, NSF OCE-0623678, and NMSP MOA#2005-008/66882. This is HIMR contribution 1395 and SOEST 7986. Manuscript accepted 30 July 2010. NR 43 TC 8 Z9 10 U1 0 U2 6 PU UNIV HAWAII PRESS PI HONOLULU PA 2840 KOLOWALU ST, HONOLULU, HI 96822 USA SN 0030-8870 J9 PAC SCI JI Pac. Sci. PD APR PY 2011 VL 65 IS 2 BP 249 EP 255 DI 10.2984/65.2.249 PG 7 WC Marine & Freshwater Biology; Zoology SC Marine & Freshwater Biology; Zoology GA 753WV UT WOS:000289811900008 ER PT J AU Grav, T Jedicke, R Denneau, L Chesley, S Holman, MJ Spahr, TB AF Grav, Tommy Jedicke, Robert Denneau, Larry Chesley, Steve Holman, Matthew J. Spahr, Timothy B. TI The Pan-STARRS Synthetic Solar System Model: A Tool for Testing and Efficiency Determination of the Moving Object Processing System SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article ID JOVIAN TROJAN ASTEROIDS; JUPITER-FAMILY COMETS; LONG-PERIOD COMETS; NEAR-EARTH OBJECTS; KUIPER-BELT; SIZE DISTRIBUTION; MAGNITUDE DISTRIBUTION; POPULATION; CENTAURS; ORIGIN AB We present here the Pan-STARRS Moving Object Processing System (MOPS) Synthetic Solar System Model (S3M), the first-ever attempt at building a comprehensive flux-limited model of the major small-body populations in the solar system. The goal of the S3M is to provide a valuable tool in the design and testing of the MOPS software, and will be used in the monitoring of the upcoming Pan-STARRS 1 all-sky survey, which started science operations during late spring of 2010. The model is composed of synthetic populations of near-Earth objects (NEOs with a subpopulation of Earth impactors), the main-belt asteroids (MBAs), Jovian Trojans, Centaurs, trans-Neptunian objects (classical, resonant, and scattered trans-Neptunian objects [TNOs]), Jupiter-family comets (JECs), long-period comets (LPCs), and interstellar comets. The model reasonably reproduces the true populations to a minimum of V = 24.5, corresponding to approximately the expected limiting magnitude for Pan-STARRS's ability to detect moving objects. The NEO synthetic population has been extended to H < 25 (corresponding to objects of about 50 m in diameter), allowing for close flybys of the Earth to be modeled. C1 [Grav, Tommy] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Jedicke, Robert; Denneau, Larry] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Chesley, Steve] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Holman, Matthew J.; Spahr, Timothy B.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA USA. RP Grav, T (reprint author), Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. EM tgrav@pha.jhu.edu; jedicke@ifa.hawaii.edu; denneau@ifa.hawaii.edu; steve.chesley@jpl.nasa.gov; mholman@cfa.harvard.edu; tspahr@cfa.harvard.cdu FU US Air Force Research Laboratory (Albuquerque, New Mexico) [F29601-02-1-0268] FX 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 US Air Force Research Laboratory (Albuquerque, New Mexico) through grant number F29601-02-1-0268. This work was conducted in part at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. NR 70 TC 24 Z9 24 U1 0 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 APR PY 2011 VL 123 IS 902 BP 423 EP 447 PG 25 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 757YM UT WOS:000290124900005 ER PT J AU Vilozny, B Actis, P Seger, RA Pourmand, N AF Vilozny, Boaz Actis, Paolo Seger, R. Adam Pourmand, Nader TI Dynamic Control of Nanoprecipitation in a Nanopipette SO ACS NANO LA English DT Article DE nanoprecipitation; nanopipette; nanopore; ion current rectification; current oscillations ID POTENTIAL BIOMEDICAL APPLICATIONS; CONICAL NANOPORE SENSOR; CURRENT RECTIFICATION; NANOPARTICLES; OSCILLATIONS; ZINC AB Studying the earliest, stages of precipitation at the nanoscale is technically challenging but quite valuable as such phenomena reflect important processes such as crystallization and biomineralization. Using a quartz nanopipette as a nanoreactor, we induced precipitation of an insoluble salt to generate oscillating current blockades. The reversible process can be used to measure both kinetics of precipitation and relative size of the resulting nanoparticles. Counter ions for the highly water-Insoluble salt zinc phosphate were separated by the pore of a nanopipette and a potential applied to cause ion migration to the Interface. By analyzing the kinetics of pore blockage, two distinct mechanisms were identified: a slower process due to precipitation from solution, and a faster process attributed to voltage-driven migration of a trapped precipitate. We discuss the potential of these techniques in studying precipitation dynamics, trapping particles within a nanoreactor, and electrical sensors based on nanoprecipitation. C1 [Vilozny, Boaz; Actis, Paolo; Seger, R. Adam; Pourmand, Nader] Univ Calif Santa Cruz, Dept Biomol Engn, Santa Cruz, CA 95064 USA. [Vilozny, Boaz; Actis, Paolo; Seger, R. Adam; Pourmand, Nader] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Vilozny, Boaz; Actis, Paolo; Seger, R. Adam; Pourmand, Nader] UC Santa Cruz, Adv Studies Labs, Moffett Field, CA 94035 USA. [Actis, Paolo] Texas So Univ, Dept Biol, Houston, TX 77004 USA. RP Pourmand, N (reprint author), Univ Calif Santa Cruz, Dept Biomol Engn, 1156 High St, Santa Cruz, CA 95064 USA. EM pourmand@soe.ucsc.edu RI babakinejad, babak/G-2674-2012; Actis, Paolo/A-7694-2012 FU National Aeronautics and Space Administration [NNX10AQ16A, NNX08BA47A]; National Institutes of Health [P01-HG000205] FX This work was supported in part by grants from the National Aeronautics and Space Administration Cooperative Agreements NNX10AQ16A and NNX08BA47A, and the National Institutes of Health [P01-HG000205]. NR 32 TC 12 Z9 12 U1 8 U2 55 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 1936-0851 J9 ACS NANO JI ACS Nano PD APR PY 2011 VL 5 IS 4 BP 3191 EP 3197 DI 10.1021/nn200320b PG 7 WC Chemistry, Multidisciplinary; Chemistry, Physical; Nanoscience & Nanotechnology; Materials Science, Multidisciplinary SC Chemistry; Science & Technology - Other Topics; Materials Science GA 753CJ UT WOS:000289742100090 PM 21413733 ER PT J AU Schubert, WW Beaudet, RA AF Schubert, Wayne W. Beaudet, Robert A. TI Determination of Lethality Rate Constants and D-Values for Heat-Resistant Bacillus Spores ATCC 29669 Exposed to Dry Heat from 125 degrees C to 200 degrees C SO ASTROBIOLOGY LA English DT Article DE Bacillus; Spores; Planetary protection; Dry heat microbial reduction; ATCC 29669; D-value ID AIRBORNE BACTERIAL-SPORES; SUBTILIS VAR NIGER; THERMAL-RESISTANCE; SPACECRAFT; DEATH; MICROORGANISMS; INACTIVATION; KINETICS; CURVES; SYSTEM AB Exposing flight hardware to dry heat is a NASA-approved sterilization method for reducing microbial bioburden on spacecraft. The existing NASA specification only allows heating the flight hardware between 104 degrees C and 125 degrees C to reduce the number of viable microbes and bacterial spores. Also, the NASA specifications only allow a four log reduction by dry heat microbial reduction because very heat-resistant spores are presumed to exist in a diverse population (0.1%). The goal of this research was to obtain data at higher temperatures than 125 degrees C for one of the most heat-resistant microorganisms discovered in a spacecraft assembly area. These data support expanding the NASA specifications to temperatures higher than 125 degrees C and relaxing the four log reduction specification. Small stainless steel vessels with spores of the Bacillus strain ATCC 29669 were exposed to constant temperatures between 125 degrees C and 200 degrees C under both dry and ambient room humidity for set time durations. After exposures, the thermal spore exposure vessels were cooled and the remaining spores recovered and plated out. Survivor ratios, lethality rate constants, and D-values were determined at each temperature. The D-values for the spores exposed under dry humidity conditions were always found to be shorter than those under ambient humidity. The temperature dependence of the lethality rate constants was obtained by assuming that they obeyed Arrhenius behavior. The results are compared to those of B. atrophaeus ATCC 9372. In all cases, the D-values of ATCC 29669 are between 20 and 50 times longer than those of B. atrophaeus ATCC 9372. C1 [Schubert, Wayne W.; Beaudet, Robert A.] CALTECH, Jet Prop Lab, Biotechnol & Planetary Protect Grp, Pasadena, CA 91109 USA. RP Schubert, WW (reprint author), CALTECH, Jet Prop Lab, Biotechnol & Planetary Protect Grp, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Wayne.W.Schubert@jpl.nasa.gov FU National Aeronautics and Space Administration; Jet Propulsion Laboratory Mars Program Office FX The research described in this paper was carried out by the Jet Propulsion Laboratory (JPL), California Institute of Technology, under a contract with the National Aeronautics and Space Administration. Funding for this work was provided by the Jet Propulsion Laboratory Mars Program Office, and we thank the Mars Program Planetary Protection Manager Dr. Karen Buxbaum for her support of this task. We thank Dr. Michael J. Kempf for his extensive work on developing the methods used in this study. We also thank Dr. J. Andy Spry from the Biotechnology and Planetary Protection Group at JPL, J. Rudy Puleo at Kennedy Space Center, and Dr. Terry Foster (TVF, Inc., The Woodlands, TX), for their helpful comments and discussions. A new technology report (JPL, NTR-47399) was submitted describing the use of these heat-resistant spores of this bacterial strain. NR 27 TC 3 Z9 4 U1 0 U2 8 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 APR PY 2011 VL 11 IS 3 BP 213 EP 223 DI 10.1089/ast.2010.0502 PG 11 WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics; Geology GA 752GE UT WOS:000289678500005 PM 21417744 ER PT J AU Philip, GK Freeland, SJ AF Philip, Gayle K. Freeland, Stephen J. TI Did Evolution Select a Nonrandom "Alphabet" of Amino Acids? SO ASTROBIOLOGY LA English DT Article DE Astrobiology; Evolution; Molecular biology; Modeling studies ID GENETIC-CODE; GENOMICS AB The last universal common ancestor of contemporary biology (LUCA) used a precise set of 20 amino acids as a standard alphabet with which to build genetically encoded protein polymers. Considerable evidence indicates that some of these amino acids were present through nonbiological syntheses prior to the origin of life, while the rest evolved as inventions of early metabolism. However, the same evidence indicates that many alternatives were also available, which highlights the question: what factors led biological evolution on our planet to define its standard alphabet? One possibility is that natural selection favored a set of amino acids that exhibits clear, nonrandom properties-a set of especially useful building blocks. However, previous analysis that tested whether the standard alphabet comprises amino acids with unusually high variance in size, charge, and hydrophobicity (properties that govern what protein structures and functions can be constructed) failed to clearly distinguish evolution's choice from a sample of randomly chosen alternatives. Here, we demonstrate unambiguous support for a refined hypothesis: that an optimal set of amino acids would spread evenly across a broad range of values for each fundamental property. Specifically, we show that the standard set of 20 amino acids represents the possible spectra of size, charge, and hydrophobicity more broadly and more evenly than can be explained by chance alone. C1 [Philip, Gayle K.; Freeland, Stephen J.] Univ Hawaii, NASA Astrobiol Inst, Honolulu, HI 96822 USA. RP Freeland, SJ (reprint author), Univ Hawaii, NASA Astrobiol Inst, Honolulu, HI 96822 USA. EM freeland@ifa.hawaii.edu OI Philip, Gayle/0000-0002-2671-5093 FU National Aeronautics and Space Administration through the NASA Astrobiology Institute [NNA09DA77A] FX We acknowledge the access provided to the computational facilities of the Bioinformatics research unit at NUI Maynooth. This research was supported by the National Aeronautics and Space Administration through the NASA Astrobiology Institute under Cooperative Agreement No. NNA09DA77A issued through the Office of Space Science. NR 21 TC 13 Z9 13 U1 1 U2 18 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 APR PY 2011 VL 11 IS 3 BP 235 EP 240 DI 10.1089/ast.2010.0567 PG 6 WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics; Geology GA 752GE UT WOS:000289678500007 PM 21434765 ER PT J AU Thompson, AM Oltmans, SJ Tarasick, DW von der Gathen, P Smit, HGJ Witte, JC AF Thompson, Anne M. Oltmans, Samuel J. Tarasick, David. W. von der Gathen, Peter Smit, Herman G. J. Witte, Jacquelyn C. TI Strategic ozone sounding networks: Review of design and accomplishments SO ATMOSPHERIC ENVIRONMENT LA English DT Review DE Ozone; Ozonesondes; TTL; Stratosphere-troposphere exchange; Tropospheric ozone; Tropics; Ozone depleticn ID TROPICAL TROPOSPHERIC OZONE; MAPPING SPECTROMETER TOMS; DATA ASSIMILATION SYSTEM; WAVE INDUCED LAMINAE; IN-SITU MEASUREMENTS; ARCTIC POLAR VORTEX; STRATOSPHERIC OZONE; LOSS RATES; CHEMICAL DEPLETION; SEASONAL EVOLUTION AB Ozone soundings are used to integrate models, satellite, aircraft and ground-based measurements for better interpretation of ozone variability, including atmospheric losses (predominantly in the stratosphere) and pollution (troposphere). A well-designed network of ozonesonde stations gives information with high vertical and horizontal resolution on a number of dynamical and chemical processes, allowing us to answer questions not possible with aircraft campaigns or current satellite technology. Strategic ozonesonde networks are discussed for high, mid- and low latitude studies. The Match sounding network was designed specifically to follow ozone depletion within the polar vortex: the standard sites are at middle to high northern hemisphere latitudes and typically operate from December through mid-March. Three mid-latitude strategic networks (the IONS series) operated over North America in July-August 2004, March-May and August 2006, and April and June-July-2008. These were designed to address questions about tropospheric ozone budgets and sources, including stratosphere-troposphere transport, and to validate satellite instruments and models. A global network focusing on processes in the equatorial zone, SHADOZ (Southern Hemisphere Additional Ozonesondes), has operated since 1998 in partnership with NOAA, NASA and the Meteorological Services of host countries. Examples of important findings from these networks are described. (C) 2010 Elsevier Ltd. All rights reserved. C1 [Thompson, Anne M.] Penn State Univ, Dept Meteorol, University Pk, PA 16802 USA. [Oltmans, Samuel J.] NOAA, Global Monitoring Div, Environm Syst Res Lab, Boulder, CO 80305 USA. [Tarasick, David. W.] Environm Canada, Air Qual Res Div, Downsview, ON M3H 5T4, Canada. [von der Gathen, Peter] Alfred Wegener Inst Polar & Marine Res, D-14473 Potsdam, Germany. [Smit, Herman G. J.] FZ Juelich, Inst Chem & Dynam Geosphere Troposphere ICG 2, D-52428 Julich, Germany. [Witte, Jacquelyn C.] NASA, SSAI, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Thompson, AM (reprint author), Penn State Univ, Dept Meteorol, 503 Walker Bldg, University Pk, PA 16802 USA. EM amt16@psu.edu; samuel.j.oltmans@noaa.gov; david.tarasick@ec.gc.ca; peter.von.der.gathen@awi.de; h.smit@fz-juelich.de; Jacquelyn.witte@nasa.gov RI von der Gathen, Peter/B-8515-2009; Smit, Herman/J-2397-2012; Thompson, Anne /C-3649-2014; OI von der Gathen, Peter/0000-0001-7409-1556; Smit, Herman/0000-0002-2268-4189; Thompson, Anne /0000-0002-7829-0920; Tarasick, David/0000-0001-9869-0692 NR 159 TC 28 Z9 29 U1 4 U2 27 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 APR PY 2011 VL 45 IS 13 BP 2145 EP 2163 DI 10.1016/j.atmosenv.2010.05.002 PG 19 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA 753ZG UT WOS:000289819200001 ER PT J AU Voulgarakis, A Hadjinicolaou, P Pyle, JA AF Voulgarakis, A. Hadjinicolaou, P. Pyle, J. A. TI Increases in global tropospheric ozone following an El Nino event: examining stratospheric ozone variability as a potential driver SO ATMOSPHERIC SCIENCE LETTERS LA English DT Article DE El Nino; STE; tropospheric ozone; stratospheric ozone ID SOUTHERN-OSCILLATION; EXCHANGE; CLOUDS; SIMULATIONS; PHOTOLYSIS; TRANSPORT; PACIFIC; CLIMATE; BUDGET; MODEL AB The stratosphere can strongly influence the interannual variability of tropospheric ozone. It has been discussed previously that tropospheric ozone can increase following an El Nino event, due to enhanced stratosphere/troposphere exchange (STE) of ozone. Here, we run a chemical-transport model for 5 years, covering a period including a strong El Nino event (1997-1998), and find that variability of ozone in the stratosphere is an almost negligible driver of modelled post-El Nino increases of ozone STE and tropospheric ozone abundances. Changes in the dynamics, affecting the cross-tropopause air-mass flux, may be far more important in driving these anomalies. Copyright. (C) 2011 Royal Meteorological Society C1 [Voulgarakis, A.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Voulgarakis, A.] Columbia Univ, Ctr Climate Syst Res, New York, NY USA. [Voulgarakis, A.; Pyle, J. A.] Univ Cambridge, NCAS Climate, Ctr Atmospher Sci, Dept Chem, Cambridge CB2 1TN, England. [Hadjinicolaou, P.] Cyprus Inst, Energy Environm & Water Res Ctr, Nicosia, Cyprus. RP Voulgarakis, A (reprint author), NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA. EM avoulgarakis@giss.nasa.gov RI Hadjinicolaou, Panos/H-1729-2016 OI Hadjinicolaou, Panos/0000-0003-1170-2182 FU NERC; NCAS (UK); IKY (Greece) FX The authors thank NERC and NCAS (UK) for funding the research presented here. A. V. thanks IKY (Greece) for financial support and P. Braesicke for useful discussions on the experimental set-up. We also thank G. D. Carver for his help with model development and P. Berrisford for providing ECMWF data. NR 30 TC 19 Z9 20 U1 3 U2 18 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1530-261X J9 ATMOS SCI LETT JI Atmos. Sci. Lett. PD APR-JUN PY 2011 VL 12 IS 2 BP 228 EP 232 DI 10.1002/asl.318 PG 5 WC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences SC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences GA 751WU UT WOS:000289649200012 ER PT J AU Sherrit, S Bao, XQ Jones, CM Aldrich, JB Blodget, CJ Moore, JD Carson, JW Goullioud, R AF Sherrit, Stewart Bao, Xiaoqi Jones, Christopher M. Aldrich, Jack B. Blodget, Chad J. Moore, James D. Carson, John W. Goullioud, Renaud TI Piezoelectric Multilayer Actuator Life Test SO IEEE TRANSACTIONS ON ULTRASONICS FERROELECTRICS AND FREQUENCY CONTROL LA English DT Article AB Potential NASA optical missions such as the Space Interferometer Mission require actuators for precision positioning to accuracies of the order of nanometers. Commercially available multilayer piezoelectric stack actuators are being considered for driving these precision mirror positioning mechanisms. These mechanisms have potential mission operational requirements that exceed 5 years for one mission life. To test the feasibility of using these commercial actuators for these applications and to determine their reliability and the redundancy requirements, a life test study was undertaken. The nominal actuator requirements for the most critical actuators on the Space Interferometry Mission (SIM) in terms of number of cycles was estimated from the Modulation Optics Mechanism (MOM) and Pathlength control Optics Mechanism (POM) and these requirements were used to define the study. At a nominal drive frequency of 250 Hz, one mission life is calculated to be 40 billion cycles. In this study, a set of commercial PZT stacks configured in a potential flight actuator configuration (pre-stressed to 18 MPa and bonded in flexures) were tested for up to 100 billion cycles. Each test flexure allowed for two sets of primary and redundant stacks to be mechanically connected in series. The tests were controlled using an automated software control and data acquisition system that set up the test parameters and monitored the waveform of the stack electrical current and voltage. The samples were driven between 0 and 20 V at 2000 Hz to accelerate the life test and mimic the voltage amplitude that is expected to be applied to the stacks during operation. During the life test, 10 primary stacks were driven and 10 redundant stacks, mechanically in series with the driven stacks, were open-circuited. The stroke determined from a strain gauge, the temperature and humidity in the chamber, and the temperature of each individual stack were recorded. Other properties of the stacks, including the displacement from a capacitance gap sensor and impedance spectra were measured at specific intervals. The average degradation in the stroke over the life test was found to be small (<3%) for the primary stacks and <4% for the redundant stacks. It was noted that about half of the stroke reduction occurred within the first 10 billion cycles. At the end of the life test, it was found that the actuator could recover about half of the lost stroke by applying a dc voltage of 100 V at room temperature. The data up to 100 billion cycles for these tests and the analysis of the experimental results are presented in this paper. C1 [Sherrit, Stewart; Jones, Christopher M.; Aldrich, Jack B.] CALTECH, Jet Prop Lab, Adv Technol Grp, Pasadena, CA 91125 USA. [Bao, Xiaoqi] CALTECH, Jet Prop Lab, Adv Actuators Team, Pasadena, CA USA. RP Sherrit, S (reprint author), CALTECH, Jet Prop Lab, Adv Technol Grp, Pasadena, CA 91125 USA. EM ssherrit@jpl.nasa.gov FU National Aeronautics Space Agency (NASA) FX Research reported in this manuscript was conducted at the Jet Propulsion Laboratory (JPL), California Institute of Technology, under a contract with National Aeronautics Space Agency (NASA). Reference herein to any specific commercial product, process, or service by trade name, trademark, manufacturer, or otherwise, does not constitute or imply its endorsement by the United States Government or the Jet Propulsion Laboratory, California Institute of Technology. NR 12 TC 2 Z9 4 U1 2 U2 21 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0885-3010 J9 IEEE T ULTRASON FERR JI IEEE Trans. Ultrason. Ferroelectr. Freq. Control PD APR PY 2011 VL 58 IS 4 BP 820 EP 828 DI 10.1109/TUFFC.2011.1874 PG 9 WC Acoustics; Engineering, Electrical & Electronic SC Acoustics; Engineering GA 754EB UT WOS:000289834500016 PM 21507759 ER PT J AU Liu, KC Chattopadhyay, A Bednarcyk, B Arnold, SM AF Liu, Kuang C. Chattopadhyay, Aditi Bednarcyk, Brett Arnold, Steven M. TI Efficient Multiscale Modeling Framework for Triaxially Braided Composites using Generalized Method of Cells SO JOURNAL OF AEROSPACE ENGINEERING LA English DT Article DE Micromechanics; Polymer matrix composites; Multiscale modeling; Triaxially braided composites; Generalized method of cells; Repeating unit cell; Homogenization; Localization ID TEXTILE COMPOSITES; COMPRESSIVE RESPONSE; MECHANICAL-BEHAVIOR; STRENGTH; FAILURE; PREDICTION; DESIGN AB In this paper, a framework for a three-scale analysis, beginning at the constituent response and propagating to the braid repeating unit cell (RUC) level, is presented. At each scale in the analysis, the response of the appropriate RUC is represented by homogenized effective properties determined from the generalized method of cells micromechanics theory. Two different macroscale RUC architectures are considered, one for eventual finite-element implementation and the other for material design, and their differences are compared. Model validation is presented through comparison to both experimental data and detailed finite-element simulations. Results show good correlation within range of experimental scatter and the finite-element simulation. Results are also presented for parametric studies varying both the overall fiber volume fraction and braid angle. These studies are compared to predictions from classical lamination theory for reference. Finally, the multiscale analysis framework is used to predict the onset of failure in a transversely loaded triaxially braided composite. The predicted transverse failure initiation stress value shows excellent correlation and provides the bound for which linear elastic constitutive models are acceptable for implementation. DOI: 10.1061/(ASCE)AS.1943-5525.0000009. (C) 2011 American Society of Civil Engineers. C1 [Liu, Kuang C.; Chattopadhyay, Aditi] Arizona State Univ, Sch Engn Matter Transport & Energy, Tempe, AZ 85287 USA. [Bednarcyk, Brett; Arnold, Steven M.] NASA, Mech & Life Predict Branch, Struct & Mat Div, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Liu, KC (reprint author), Arizona State Univ, Sch Engn Matter Transport & Energy, Tempe, AZ 85287 USA. NR 20 TC 19 Z9 20 U1 2 U2 15 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 APR PY 2011 VL 24 IS 2 BP 162 EP 169 DI 10.1061/(ASCE)AS.1943-5525.0000009 PG 8 WC Engineering, Aerospace; Engineering, Civil SC Engineering GA 752KU UT WOS:000289690900005 ER PT J AU Li, XT Binienda, WK Goldberg, RK AF Li, Xuetao Binienda, Wieslaw K. Goldberg, Robert K. TI Finite-Element Model for Failure Study of Two-Dimensional Triaxially Braided Composite SO JOURNAL OF AEROSPACE ENGINEERING LA English DT Article DE Two-dimensional triaxially braided composite; Unit cell; Progressive degradation; Cohesive; Debonding; Straight-sided specimen test ID FRACTURE-TOUGHNESS; PROGRESSIVE DAMAGE; DELAMINATION; IMPACT AB A new three-dimensional finite-element model of two-dimensional, triaxially braided composites is presented in this paper. This mesoscale modeling technique is used to examine and predict the deformation and damage observed in tests of straight-sided specimens. A unit cell-based approach is used to consider the braiding architecture and the mechanical properties of the fiber tows, the matrix, and the fiber tow-matrix interface. A 0 degrees/ +/- 60 braiding configuration has been investigated by conducting static finite-element analyses. Failure initiation and progressive degradation has been simulated in the fiber tows by using the Hashin failure criteria and a damage evolution law. The fiber tow-matrix interface was modeled by using a cohesive zone approach to capture any fiber-matrix debonding. By comparing the analytical results with those obtained experimentally, the applicability of the developed model was assessed and the failure process was investigated. DOI: 10.1061/(ASCE)AS.1943-5525.0000029. (C) 2011 American Society of Civil Engineers. C1 [Li, Xuetao; Binienda, Wieslaw K.] Univ Akron, Akron, OH 44325 USA. [Goldberg, Robert K.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Li, XT (reprint author), Univ Akron, Akron, OH 44325 USA. EM xl17@zips.uakron.edu; wbinienda@uakron.edu; Robert.K.Goldberg@nasa.gov NR 26 TC 13 Z9 13 U1 1 U2 10 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 APR PY 2011 VL 24 IS 2 BP 170 EP 180 DI 10.1061/(ASCE)AS.1943-5525.0000029 PG 11 WC Engineering, Aerospace; Engineering, Civil SC Engineering GA 752KU UT WOS:000289690900006 ER PT J AU Keckhut, P Randel, WJ Claud, C Leblanc, T Steinbrecht, W Funatsu, BM Bencherif, H McDermid, IS Hauchecorne, A Long, C Lin, R Baumgarten, G AF Keckhut, P. Randel, W. J. Claud, C. Leblanc, T. Steinbrecht, W. Funatsu, B. M. Bencherif, H. McDermid, I. S. Hauchecorne, A. Long, C. Lin, R. Baumgarten, G. TI An evaluation of uncertainties in monitoring middle atmosphere temperatures with the ground-based lidar network in support of space observations SO JOURNAL OF ATMOSPHERIC AND SOLAR-TERRESTRIAL PHYSICS LA English DT Article DE Middle atmosphere temperature; Lidar; Satellite; Uncertainties ID RESOLUTION DOPPLER IMAGER; LONG-TERM CHANGES; STRATOSPHERIC OZONE; THERMAL TIDES; PART I; TRENDS; CLIMATOLOGY; ROCKETSONDES; VARIABILITY; MESOSPHERE AB The capability of the longest lidar data sets to monitor long-term temperature changes have been evaluated through comparisons with the successive Stratospheric Sounder Units (SSU) onboard NOAA satellites. Cross-consistency investigations between SSU and the lidar network can be considered as a first attempt to demonstrate how the synergistic use of space and ground-based instruments could provide reliable monitoring of the temperature of the middle atmosphere. The breakdown of the temperature cooling trend, and the following flattening observed in the satellite temperature series, is qualitatively confirmed by the lidars. However, there are still large differences that can either be due to SSU continuity (orbit drifts or weighting function modifications) or lidar operation changes (time of measurements, accuracy, sampling, etc.). SSU vertical weighting functions have been taken into account for comparisons. Some discontinuity events cannot be explained by the SSU weighting function drifts due to CO(2). For the upper channels of SSU (peaking around 50 km), the results are probably sensitive to the mesospheric part of the lidar profiles that can explain some discontinuities. Tropical lidar stations show clear inter-annual differences with the SSU channels covering the lowest altitude range that needs further investigations to understand if the origin is instrumental or geophysical. An attempt to derive non-linear trends with combinations of linear, hockey stick, and quadratic functions has been made. While the quadratic term is not highly significant, this approach allows the derivation of a better quantification of the linear trend terms. (C) 2011 Elsevier Ltd. All rights reserved. C1 [Keckhut, P.; Funatsu, B. M.; Hauchecorne, A.] Univ Versailles St Quentin 11, Lab Atmospheres, UMR 8190, Inst Pierre Simon Laplace, F-78280 Verrieres Le Buisson, France. [Randel, W. J.] Natl Ctr Atmospher Res, Boulder, CO 80307 USA. [Claud, C.; Funatsu, B. M.] Ecole Polytech, Meteorol Dynam Lab, UMR 8539, Inst Pierre Simon Laplace, F-91128 Palaiseau, France. [Leblanc, T.; McDermid, I. S.] CALTECH, Jet Prop Lab, Wrightwood, CA USA. [Steinbrecht, W.] Meteorol Observ, Hohenpeissenberg, Germany. [Bencherif, H.] Univ La Reunion, Lab Atmosphere & Cyclones, UMR 8105, St Denis, France. [Long, C.; Lin, R.] NOAA, Predict Ctr, NCEP, Natl Weather Serv, Camp Springs, MD USA. [Baumgarten, G.] Leibniz Inst Atmospher Phys, Kuhlungsborn, Germany. RP Keckhut, P (reprint author), Univ Versailles St Quentin 11, Lab Atmospheres, UMR 8190, Inst Pierre Simon Laplace, Blvd Alembert, F-78280 Verrieres Le Buisson, France. EM Keckhut@latmos.ipsl.fr RI Steinbrecht, Wolfgang/G-6113-2010; Hauchecorne, Alain/A-8489-2013; Randel, William/K-3267-2016; OI Steinbrecht, Wolfgang/0000-0003-0680-6729; Randel, William/0000-0002-5999-7162; Claud, Chantal/0000-0001-7613-9525; Hauchecorne, Alain/0000-0001-9888-6994; Baumgarten, Gerd/0000-0002-6727-284X FU COST Action [ES0702]; European Commission [FP6-2005-Global-4-036677] FX This work was initiated through the SPARC Stratospheric Temperature Trend Assessment group lead by Dr. W. Randel (http://www.atmosp.physics.utoronto.ca/SPARC/initiatives NEW2005Detection.html) and was partly supported by the European Commission through the Global Earth Observation and Monitoring (GEOmon-http://www.geomon.eu/) Integrated Project under the 6th Framework Program (Contract no. FP6-2005-Global-4-036677). It is also part of the COST Action ES0702: European Ground-Based Observations of Essential Variables for Climate and Operational Meteorology (EG-CLIMET). NR 52 TC 18 Z9 18 U1 0 U2 6 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 APR PY 2011 VL 73 IS 5-6 BP 627 EP 642 DI 10.1016/j.jastp.2011.01.003 PG 16 WC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences SC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences GA 741UC UT WOS:000288889600008 ER PT J AU Gopalswamy, N Davila, JM St Cyr, OC Sittler, EC Auchere, F Duvall, TL Hoeksema, JT Maksimovic, M MacDowall, RJ Szabo, A Collier, MR AF Gopalswamy, N. Davila, J. M. St Cyr, O. C. Sittler, E. C. Auchere, F. Duvall, T. L., Jr. Hoeksema, J. T. Maksimovic, M. MacDowall, R. J. Szabo, A. Collier, M. R. TI Earth-Affecting Solar Causes Observatory (EASCO): A potential International Living with a Star Mission from Sun-Earth L5 SO JOURNAL OF ATMOSPHERIC AND SOLAR-TERRESTRIAL PHYSICS LA English DT Article; Proceedings Paper CT Meeting on International Living With a Star (ILWS) CY OCT 04-09, 2009 CL Ubatuba, BRAZIL DE Coronal mass ejections; Earth-Sun L5; Corotating interaction regions; Geomagnetic storms; Solar energetic particles ID CORONAL MASS EJECTIONS; II RADIO-BURSTS; GEOMAGNETIC STORMS; SPACE AB This paper describes the scientific rationale for an L5 mission and a partial list of key scientific instruments the mission should carry. The L5 vantage point provides an unprecedented view of the solar disturbances and their solar sources that can greatly advance the science behind space weather. A coronagraph and a heliospheric imager at L5 will be able to view CMEs broadsided, so space speed of the Earth-directed CMEs can be measured accurately and their radial structure discerned. In addition, an inner coronal imager and a magnetograph from L5 can give advance information on active regions and coronal holes that will soon rotate on to the solar disk. Radio remote sensing at low frequencies can provide information on shock-driving CMEs, the most dangerous of all CMEs. Coordinated helioseismic measurements from the Sun-Earth line and L5 provide information on the physical conditions at the base of the convection zone, where solar magnetism originates. Finally, in situ measurements at L5 can provide information on the large-scale solar wind structures (corotating interaction regions (CIRs)) heading towards Earth that potentially result in adverse space weather. Published by Elsevier Ltd. C1 [Gopalswamy, N.; Davila, J. M.; St Cyr, O. C.; Sittler, E. C.; Duvall, T. L., Jr.; MacDowall, R. J.; Szabo, A.; Collier, M. R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA. [Auchere, F.] Inst Astrophys Spatiale, Orsay, France. [Hoeksema, J. T.] Stanford Univ, Stanford, CA 94305 USA. [Maksimovic, M.] Observ Paris, Meudon, France. RP Gopalswamy, N (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD USA. EM nat.gopalswamy@nasa.gov RI Duvall, Thomas/C-9998-2012; MacDowall, Robert/D-2773-2012; Gopalswamy, Nat/D-3659-2012; Collier, Michael/I-4864-2013; OI Collier, Michael/0000-0001-9658-6605; Auchere, Frederic/0000-0003-0972-7022 NR 21 TC 18 Z9 18 U1 0 U2 5 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 APR PY 2011 VL 73 IS 5-6 BP 658 EP 663 DI 10.1016/j.jastp.2011.01.013 PG 6 WC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences SC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences GA 741UC UT WOS:000288889600011 ER PT J AU Tsurutani, BT Lakhina, GS Verkhoglyadova, OP Gonzalez, WD Echer, E Guarnieri, FL AF Tsurutani, B. T. Lakhina, G. S. Verkhoglyadova, O. P. Gonzalez, W. D. Echer, E. Guarnieri, F. L. TI A review of interplanetary discontinuities and their geomagnetic effects (vol 73, pg 5, 2011) SO JOURNAL OF ATMOSPHERIC AND SOLAR-TERRESTRIAL PHYSICS LA English DT Correction C1 [Tsurutani, B. T.; Verkhoglyadova, O. P.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Lakhina, G. S.] Indian Inst Geomagnetism, Navi Mumbai, India. [Verkhoglyadova, O. P.] Univ Alabama, CSPAR, Huntsville, AL 35899 USA. [Gonzalez, W. D.; Echer, E.] Inst Nacl Pesquisas Espaciais, BR-12201 Sao Jose Dos Campos, SP, Brazil. [Guarnieri, F. L.] Univ Vale do Paraiba, Sao Jose Dos Campos, SP, Brazil. RP Tsurutani, BT (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. EM bruce.tsurutani@jpl.nasa.gov RI Lakhina, Gurbax /C-9295-2012; Tecnologias espaciai, Inct/I-2415-2013 NR 3 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 1364-6826 J9 J ATMOS SOL-TERR PHY JI J. Atmos. Sol.-Terr. Phys. PD APR PY 2011 VL 73 IS 5-6 BP 709 EP 709 DI 10.1016/j.jastp.2011.01.007 PG 1 WC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences SC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences GA 741UC UT WOS:000288889600017 ER PT J AU Lyver, JW Blaisten-Barojas, E AF Lyver, John W. Blaisten-Barojas, Estela TI Lattice Thermal Conductivity in SiC Nanotubes, Nanowires and Nanofilaments: A Molecular Dynamics Study SO JOURNAL OF COMPUTATIONAL AND THEORETICAL NANOSCIENCE LA English DT Article DE Thermal Conductivity; Non-Equilibrium Molecular Dynamics; Silicon Carbide; SiC Nanowires; SiC Nanotubes; SiC Nanofilaments ID FINITE-TEMPERATURE PROPERTIES; SILICON-CARBIDE; HEAT-FLOW; SIMULATIONS; TRANSPORT; CRYSTALS; WALL AB This paper presents results a non-equilibrium Molecular Dynamics approach to determine the lattice thermal conductivity of nanowires, nanotubes, and nanofilaments of silicon carbide. The nanostructures are modeled with the classical potential proposed in J Appl. Phys. 101, 103515 (2007). These nanostructures display very low lattice thermal conductivity, about 50 times smaller than bulk SiC. Among the studied nanostructures, the 3C [(1) over bar 00] nanowires have the highest thermal conductivity, and the (5, 5) nanotubes display the lowest. Dependence on temperature of the lattice thermal conductivity exhibits an inverse power relationship only for nanowires 3C [(1) over bar 00], 2H [110] and the (4, 0), (2, 2) nanotubes. All other structures have thermal conductivities decreasing more gently as a function of increasing temperature, except for nanowires 3C and nanotubes (5, 5) where the thermal conductivity is almost constant as a function of temperature. C1 [Lyver, John W.; Blaisten-Barojas, Estela] George Mason Univ, Computat Mat Sci Ctr, Fairfax, VA 22030 USA. [Lyver, John W.; Blaisten-Barojas, Estela] George Mason Univ, Sch Phys Astron & Computat Sci, Fairfax, VA 22030 USA. [Lyver, John W.] NASA, Off Safety & Mission Assurance, Washington, DC 20546 USA. RP Blaisten-Barojas, E (reprint author), George Mason Univ, Computat Mat Sci Ctr, MS 6A2, Fairfax, VA 22030 USA. FU National Science Foundation [CHE-0626111] FX This work was supported in part by the National Science Foundation, grant CHE-0626111. NR 32 TC 7 Z9 7 U1 0 U2 8 PU AMER SCIENTIFIC PUBLISHERS PI STEVENSON RANCH PA 25650 NORTH LEWIS WAY, STEVENSON RANCH, CA 91381-1439 USA SN 1546-1955 J9 J COMPUT THEOR NANOS JI J. Comput. Theor. Nanosci. PD APR PY 2011 VL 8 IS 4 BP 529 EP 534 DI 10.1166/jctn.2011.1718 PG 6 WC Chemistry, Multidisciplinary; Nanoscience & Nanotechnology; Materials Science, Multidisciplinary; Physics, Applied; Physics, Condensed Matter SC Chemistry; Science & Technology - Other Topics; Materials Science; Physics GA 752NH UT WOS:000289698200002 ER PT J AU Palof, KJ Heifetz, J Gharrett, AJ AF Palof, Katie J. Heifetz, Jonathan Gharrett, Anthony J. TI Geographic structure in Alaskan Pacific ocean perch (Sebastes alutus) indicates limited lifetime dispersal SO MARINE BIOLOGY LA English DT Article ID EFFECTIVE POPULATION-SIZE; MULTILOCUS GENOTYPE DATA; QUEEN-CHARLOTTE SOUND; ROCKFISH SEBASTES; GENE FLOW; MICROSATELLITE LOCI; F-STATISTICS; LINKAGE DISEQUILIBRIUM; PAIRWISE RELATEDNESS; ALLELE FREQUENCIES AB Prevailing oceanographic processes, pelagic larvae, adult mobility, and large populations of many marine species often leads to the assumption of wide-ranging populations. Applying this assumption to more localized populations can lead to inappropriate conservation measures. The Pacific ocean perch (Sebastes alutus, POP) is economically and ecologically valuable, but little is known about its population structure and life history in Alaskan waters. Fourteen microsatellite loci were used to characterize geographic structure and connectivity of POP collections (1999-2005) sampled along the continental shelf break from Dixon Entrance to the Bering Sea. Despite opportunities for dispersal, there was significant, geographically related genetic structure (F(ST) = 0.0123, P < 10(-5)). Adults appear to belong to neighborhoods at geographic scales less than 400 km, and possibly as small as 70 km, which indicates limited dispersal throughout their lives. The population structure observed has a finer geographic scale than current management, which suggests that measures for POP fisheries conservation should be revisited. C1 [Palof, Katie J.; Gharrett, Anthony J.] Univ Alaska Fairbanks, Div Fisheries, Sch Fisheries & Ocean Sci, Juneau, AK 99801 USA. [Heifetz, Jonathan] Natl Marine Fisheries Serv, Auke Bay Labs, Alaska Fisheries Sci Ctr, NOAA, Juneau, AK 99801 USA. RP Palof, KJ (reprint author), Univ Alaska Fairbanks, Div Fisheries, Sch Fisheries & Ocean Sci, 17101 Point Lena Loop Rd, Juneau, AK 99801 USA. EM kjpalof@alaska.edu FU Alaska Sea Grant College Program; Cooperative Institute for Artic Research (CIFAR); NOAA Fisheries-Auke Bay Laboratories; Rasmuson Fisheries Research Center; Pollock Conservation Cooperative Research Center (PCCRC); School of Fisheries and Ocean Sciences, University of Alaska Fairbanks, AK FX We thank R. Waples and L. Hauser for their helpful comments and review. We thank N. Hillgruber for serving on the graduate committee and for her helpful comments. We thank Alaska Fisheries Science Center, NOAA Fisheries personnel who took tissue samples for this study during trawl surveys. This research was supported by: Alaska Sea Grant College Program, Cooperative Institute for Artic Research (CIFAR), NOAA Fisheries-Auke Bay Laboratories, Rasmuson Fisheries Research Center, and the Pollock Conservation Cooperative Research Center (PCCRC), School of Fisheries and Ocean Sciences, University of Alaska Fairbanks, AK. This work represents, in part, the master's work of K. Palof at the University of Alaska Fairbanks. NR 82 TC 13 Z9 13 U1 0 U2 10 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0025-3162 J9 MAR BIOL JI Mar. Biol. PD APR PY 2011 VL 158 IS 4 BP 779 EP 792 DI 10.1007/s00227-010-1606-2 PG 14 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 750IF UT WOS:000289539100007 ER PT J AU Hochhalter, JD Littlewood, DJ Veilleux, MG Bozek, JE Maniatty, AM Rollett, AD Ingraffea, AR AF Hochhalter, J. D. Littlewood, D. J. Veilleux, M. G. Bozek, J. E. Maniatty, A. M. Rollett, A. D. Ingraffea, A. R. TI A geometric approach to modeling microstructurally small fatigue crack formation: III. Development of a semi-empirical model for nucleation SO MODELLING AND SIMULATION IN MATERIALS SCIENCE AND ENGINEERING LA English DT Article ID POLYCRYSTAL PLASTICITY; ALUMINUM-ALLOY; CYCLE FATIGUE; GROWTH; DISLOCATION AB It has been observed during fatigue cracking of AA 7075-T651 that a small percentage of Al(7)Cu(2)Fe particles crack during manufacturing or very early in their life. Some of the cracked particles eventually nucleate cracks into the surrounding microstructure, and among these the number of cycles required for nucleation varies widely. It is important to comprehend the mechanics underpinning the observed variation so that the subsequent propagation stage can be accurately modeled. To this end, finite element models of replicated grain and particle geometry are used to compute mechanical fields near monitored cracked particles using an elastic-viscoplastic crystal plasticity model that captures the effect of the orientation of the grains near each monitored particle. Nonlocal, slip-based metrics are used to study the localization and cyclic accumulation of slip near the cracked particles providing mechanics-based insight into the actuation of the nucleation event. A high slip localization and cyclic accumulation rate are found to be a necessary, but not sufficient, condition for nucleation from cracked particles. A sufficient local driving stress must also be present, which is strongly dependent on the local microstructure and accumulated slip. Furthermore, the simulation results elucidate a quantitative relationship between the slip accumulated during fatigue loading and a consequential reduction of the critical local driving stress for nucleation, providing a physical basis for the fatigue damage concept. The observed nucleation direction is orthogonal to the computed local maximum tangential stress direction, as expected for this alloy. The main result is a semi-empirical model for the number of cycles required for nucleation, which is dependent on the maximum tangential stress and cyclic slip-accumulation rate near a cracked particle. C1 [Hochhalter, J. D.] NASA, Durabil & Damage Tolerance Branch, Langley Res Ctr, Hampton, VA 23681 USA. [Littlewood, D. J.] Sandia Natl Labs, Albuquerque, NM 87185 USA. [Veilleux, M. G.; Bozek, J. E.; Ingraffea, A. R.] Cornell Univ, Cornell Fracture Grp, Ithaca, NY 14853 USA. [Maniatty, A. M.] Rensselaer Polytech Inst, Troy, NY 12180 USA. [Rollett, A. D.] Carnegie Mellon Univ, Dept Mat Sci & Engn, Pittsburgh, PA 15213 USA. RP Hochhalter, JD (reprint author), NASA, Durabil & Damage Tolerance Branch, Langley Res Ctr, MS 188E, Hampton, VA 23681 USA. EM Jacob.D.Hochhalter@nasa.gov RI Rollett, Anthony/A-4096-2012 OI Rollett, Anthony/0000-0003-4445-2191 FU Defense Advanced Research Projects Agency (DARPA) [HR0011-04-C-0003]; NASA [ARMD-NNX07AB69A]; NASA Advanced Supercomputing Division at Ames Research Center FX Dr Gerd Heber developed the parallel finite element code that was used for the finite element simulations presented here. The measurements of microstructural geometry were made by Robert Christ Jr and Dr Elias Anagnostou at the Northrop Grumman Corporation. This work is partially sponsored by the Defense Advanced Research Projects Agency (DARPA) under contract HR0011-04-C-0003. Dr Leo Christodoulou is the DARPA Program Manager. This work is also partially funded by NASA under contract ARMD-NNX07AB69A. Dr Ed Glaessgen is the National Aeronautics and Space Administration (NASA) Contract Monitor. Resources supporting this work were provided by the NASA High-End Computing Program through the NASA Advanced Supercomputing Division at Ames Research Center. The views, opinions, and/or findings contained in this paper are those of the authors and should not be interpreted as representing the official views or policies, either expressed or implied, of the Defense Advanced Research Projects Agency or the Department of Defense. NR 23 TC 11 Z9 11 U1 1 U2 10 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0965-0393 J9 MODEL SIMUL MATER SC JI Model. Simul. Mater. Sci. Eng. PD APR PY 2011 VL 19 IS 3 AR 035008 DI 10.1088/0965-0393/19/3/035008 PG 27 WC Materials Science, Multidisciplinary; Physics, Applied SC Materials Science; Physics GA 753MG UT WOS:000289778700008 ER PT J AU Guo, Q Cole, S Lacey, CG Baugh, CM Frenk, CS Norberg, P Auld, R Baldry, IK Bamford, SP Bourne, N Buttiglione, ES Cava, A Cooray, A Croom, S Dariush, A De Zotti, G Driver, S Dunne, L Dye, S Eales, S Fritz, J Hopkins, A Hopwood, R Ibar, E Ivison, RJ Jarvis, M Jones, DH Kelvin, L Liske, J Loveday, J Maddox, SJ Parkinson, H Pascale, E Peacock, JA Pohlen, M Prescott, M Rigby, EE Robotham, A Rodighiero, G Sharp, R Smith, DJB Temi, P van Kampen, E AF Guo, Qi Cole, Shaun Lacey, Cedric G. Baugh, Carlton M. Frenk, Carlos S. Norberg, Peder Auld, R. Baldry, I. K. Bamford, S. P. Bourne, N. Buttiglione, E. S. Cava, A. Cooray, A. Croom, S. Dariush, A. De Zotti, G. Driver, S. Dunne, L. Dye, S. Eales, S. Fritz, J. Hopkins, A. Hopwood, R. Ibar, E. Ivison, R. J. Jarvis, M. Jones, D. H. Kelvin, L. Liske, J. Loveday, J. Maddox, S. J. Parkinson, H. Pascale, E. Peacock, J. A. Pohlen, M. Prescott, M. Rigby, E. E. Robotham, A. Rodighiero, G. Sharp, R. Smith, D. J. B. Temi, P. van Kampen, E. TI Which haloes host Herschel-ATLAS galaxies in the local Universe? SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: haloes; dark matter; infrared: galaxies ID STAR-FORMATION HISTORY; LOW-REDSHIFT UNIVERSE; MASS ASSEMBLY GAMA; DARK-MATTER; LUMINOSITY FUNCTION; FORMING GALAXIES; FORMATION RATES; NUMBER; SPIRE; BIAS AB We measure the projected cross-correlation between low-redshift (z < 0.5) far-infrared selected galaxies in the science demonstration phase (SDP) field of the Herschel-ATLAS (H-ATLAS) survey and optically selected galaxies from the Galaxy and Mass Assembly (GAMA) redshift survey. In order to obtain robust correlation functions, we restrict the analysis to a subset of 969 out of 6900 H-ATLAS galaxies, which have reliable optical counterparts with r < 19.4 mag and well-determined spectroscopic redshifts. The overlap region between the two surveys is 12.6 deg2; the matched sample has a median redshift of z approximate to 0.2. The cross-correlation of GAMA and H-ATLAS galaxies within this region can be fitted by a power law, with correlation length r(0) approximate to 4.63 +/- 0.51 Mpc. Comparing with the corresponding autocorrelation function of GAMA galaxies within the SDP field yields a relative bias (averaged over 2-8 Mpc) of H-ATLAS and GAMA galaxies of b(H)/b(G) approximate to 0.6. Combined with clustering measurements from previous optical studies, this indicates that most of the low-redshift H-ATLAS sources are hosted by haloes with masses comparable to that of the Milky Way. The correlation function appears to depend on the 250-mu m luminosity, L-250, with bright (median luminosity nu L-250 similar to 1.6 x 1010 L-circle dot) objects being somewhat more strongly clustered than faint (nu L-250 similar to 4.0 x 109 L-circle dot) objects. This implies that galaxies with higher dust-obscured star formation rates are hosted by more massive haloes. C1 [Norberg, Peder; Parkinson, H.; Peacock, J. A.] Univ Edinburgh, Inst Astron, SUPA, Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland. [Auld, R.; Dariush, A.; Dye, S.; Eales, S.; Pascale, E.; Pohlen, M.; Smith, D. J. B.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, Wales. [Baldry, I. K.; Prescott, M.] Liverpool John Moores Univ, Astrophys Res Inst, Birkenhead CH41 1LD, Merseyside, England. [Bamford, S. P.; Bourne, N.; Dunne, L.; Maddox, S. J.; Rigby, E. E.] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England. [Buttiglione, E. S.; De Zotti, G.; Rodighiero, G.] Osserv Astron Padova, INAF, I-35122 Padua, Italy. [Cava, A.] Inst Astrofis Canarias IAC, Tenerife, Spain. [Cooray, A.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. [Croom, S.] Univ Sydney, Sydney Inst Astron, Sch Phys, Sydney, NSW 2006, Australia. [De Zotti, G.] SISSA, I-34136 Trieste, Italy. [Driver, S.; Kelvin, L.; Robotham, A.] Univ St Andrews, Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland. [Fritz, J.] Univ Ghent, Sterrenkundig Observatorium, B-9000 Ghent, Belgium. [Hopkins, A.; Jones, D. H.; Sharp, R.] Australian Astron Observ, Epping, NSW 1710, Australia. [Hopwood, R.] Open Univ, Dept Phys & Astron, Milton Keynes MK7 6AA, Bucks, England. [Ibar, E.; Ivison, R. J.] Royal Observ, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland. [Jarvis, M.] Univ Hertfordshire, Sci & Technol Res Inst, Ctr Astrophys, Hatfield AL10 9AB, Herts, England. [Liske, J.; van Kampen, E.] European So Observ, D-85748 Garching, Germany. [Temi, P.] NASA, Astrophys Branch, Ames Res Ctr, Moffett Field, CA 94035 USA. [Loveday, J.] Univ Sussex, Ctr Astron, Brighton BN1 9QH, E Sussex, England. [Guo, Qi; Cole, Shaun; Lacey, Cedric G.; Baugh, Carlton M.; Frenk, Carlos S.] Univ Durham, Dept Phys, Inst Computat Cosmol, Durham DH1 3LE, England. [Cava, A.] Dept Astrofis La Laguna ULL, Tenerife, Spain. RP Guo, Q (reprint author), Univ Durham, Dept Phys, Inst Computat Cosmol, South Rd, Durham DH1 3LE, England. EM qi.guo@durham.ac.uk RI Baugh, Carlton/A-8482-2012; Robotham, Aaron/H-5733-2014; Driver, Simon/H-9115-2014; Ivison, R./G-4450-2011; Bamford, Steven/E-8702-2010; Cava, Antonio/C-5274-2017; OI Rodighiero, Giulia/0000-0002-9415-2296; Liske, Jochen/0000-0001-7542-2927; Baldry, Ivan/0000-0003-0719-9385; Dye, Simon/0000-0002-1318-8343; Smith, Daniel/0000-0001-9708-253X; Baugh, Carlton/0000-0002-9935-9755; Robotham, Aaron/0000-0003-0429-3579; Driver, Simon/0000-0001-9491-7327; Ivison, R./0000-0001-5118-1313; Bamford, Steven/0000-0001-7821-7195; Cava, Antonio/0000-0002-4821-1275; Maddox, Stephen/0000-0001-5549-195X FU Royal Society; Leverhulme Research Fellowship; Science and Technology Facilities Council; NASA through JPL FX CSF acknowledges a Royal Society Wolfson Research Merit award. SC acknowledges the support of the Leverhulme Research Fellowship. This work was supported in part by a rolling grant from the Science and Technology Facilities Council to the ICC. The H-ATLAS survey is being carried with ESA's Herschel Space Observatory, which is equipped with instruments provided by European-led Principal Investigator consortia, with important participation from the NASA, USA. Authors acknowledge support provided by the NASA through JPL. The GAMA is a joint European-Australian spectroscopic campaign using the Anglo-Australian Telescope. The GAMA input catalogue is based on data from the SDSS and the UKIRT Infrared Deep Sky Survey. Complementary imaging of the GAMA regions is being obtained by a number of independent surveys, including GALEX MIS, VST KIDS, VISTA VIKING, WISE, H-ATLAS, GMRT and ASKAP, providing UV to radio coverage. PN acknowledges the support of a Royal Society University Research Fellowship. We thank Douglas Scott for a critical reading of our manuscript. NR 34 TC 13 Z9 13 U1 1 U2 4 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD APR PY 2011 VL 412 IS 4 BP 2277 EP 2285 DI 10.1111/j.1365-2966.2010.18051.x PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 747BR UT WOS:000289295800012 ER PT J AU De Sanctis, MC Ammannito, E Migliorini, A Lazzaro, D Capria, MT McFadden, L AF De Sanctis, Maria Cristina Ammannito, Eleonora Migliorini, Alessandra Lazzaro, Daniela Capria, Maria Teresa McFadden, Lucy TI Mineralogical characterization of some V-type asteroids, in support of the NASA Dawn mission star SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE minor planets; asteroids general; minor planets; asteroids: individual: 4 Vesta ID EUCRITE PARENT BODY; MAIN-BELT; BASALTIC ASTEROIDS; 4 VESTA; REFLECTANCE SPECTRA; PYROXENE MIXTURES; SOLAR-SYSTEM; DIOGENITES; SPECTROSCOPY; METEORITES AB We present new reflectance spectra of 12 V-type asteroids obtained at the 3.6 m Telescopio Nazionale Galileo (TNG) covering the spectral range 0.7 to 2.5 mu m. This spectral range, encompassing the 1 and 2 mu m, pyroxene features, allows a precise mineralogical characterization of the asteroids. The spectra of these asteroids are examined and compared to spectra for the Howardite, Eucrite and Diogenite (HED) meteorites, of which Vesta is believed to be the parent body. The observed objects were selected from different dynamical populations with the aim to verify if there exist spectral parameters that can shed light on the origin of the objects. A reassessment of data previously published has also been performed using a new methodology. We derive spectral parameters from NIR spectra to infer mineralogical information of the observed asteroids. The V-type asteroids here discussed show mainly orthopyroxene mineralogy although some of them seem to have a mineralogical composition containing cations that are smaller than Mg cations. Most of the observed Vestoids show a low abundance of Ca (< 10 per cent Wo). This result implies that no one of the Vestoids studied consists of just eucritic material, but they must additionally have a diogenitic component. However, we must remember that the ground-based data are subject to larger errors than the laboratory data used as reference spectra for interpretation. Finally, we note that the intermediate belt asteroid (21238) 1995WV7 has spectral parameters quite different from the observed V-type objects of the inner belt, so it could be a basaltic asteroid not related to Vesta. This mineralogical analysis of asteroids related to Vesta is done in support of NASA's Dawn mission, which will enter into orbit around Vesta in the summer of 2011. This work extends the scientific context of the mission to include processes contributing to the nature of smaller V-type asteroids that may be related to Vesta. C1 [De Sanctis, Maria Cristina; Migliorini, Alessandra; Capria, Maria Teresa] Ist Astrofis Spaziale & Fis Cosm, Area Ric Tor Vergata, I-00133 Rome, Italy. [Ammannito, Eleonora] Ist Fis Spazio Interplanetario, Area Ric Tor Vergata, I-00133 Rome, Italy. [Lazzaro, Daniela] Observ Nacl, BR-20921400 Rio De Janeiro, Brazil. [McFadden, Lucy] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP De Sanctis, MC (reprint author), Ist Astrofis Spaziale & Fis Cosm, Area Ric Tor Vergata, Via Fosso Cavaliere 100, I-00133 Rome, Italy. EM mariacristina.desanctis@iasf-roma.inaf.it RI 7, INCT/H-6207-2013; Astrofisica, Inct/H-9455-2013; McFadden, Lucy-Ann/I-4902-2013; De Sanctis, Maria Cristina/G-5232-2013; Lazzaro, Daniela/I-3509-2012; OI McFadden, Lucy-Ann/0000-0002-0537-9975; De Sanctis, Maria Cristina/0000-0002-3463-4437; Lazzaro, Daniela/0000-0002-4470-6043; Migliorini, Alessandra/0000-0001-7386-9215; capria, maria teresa/0000-0002-9814-9588 FU ASI FX This work has been supported by an ASI grant, whose support is gratefully acknowledged. NR 65 TC 17 Z9 17 U1 1 U2 4 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD APR PY 2011 VL 412 IS 4 BP 2318 EP 2332 DI 10.1111/j.1365-2966.2010.18058.x PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 747BR UT WOS:000289295800015 ER PT J AU Dudek, JC AF Dudek, Julianne C. TI Modeling Vortex Generators in a Navier-Stokes Code SO AIAA JOURNAL LA English DT Article; Proceedings Paper CT 48th AIAA Aerospace Sciences Meeting and Exhibit Including the New Horizons Forum and Aerospace Exposition CY JAN 04-08, 2010 CL Orlando, FL SP AIAA, Vinnova, Maritime Competence Ctr Lighthouse, Swedish Armed Forces, Swedish Def Mat Agcy, NASA Langley Res Ctr, NASA Dryden Flight Res Ctr AB A source-term model that simulates the effects of vortex generators was implemented into the Wind-US Navier- Stokes code. The source term added to the Navier-Stokes equations simulates the lift force that would result from a vane-type vortex generator in the flowfield. The implementation is user-friendly, requiring the user to specify only three quantities for each desired vortex generator: the range of grid points over which the force is to be applied and the planform area and angle of incidence of the physical vane. The model behavior was evaluated for subsonic flow in a rectangular duct with a single vane vortex generator, subsonic flow in an S-duct with 22 corotating vortex generators, and supersonic flow in a rectangular duct with a counter-rotating vortex-generator pair. The model was also used to successfully simulate microramps in supersonic flow by treating each microramp as a pair of vanes with opposite angles of incidence. The validation results indicate that the source-term vortex-generator model provides a useful tool for screening vortex-generator configurations and gives comparable results to solutions computed using gridded vanes. C1 NASA John H Glenn Res Ctr Lewis Field, Inlet & Nozzle Branch, Cleveland, OH 44135 USA. RP Dudek, JC (reprint author), NASA John H Glenn Res Ctr Lewis Field, Inlet & Nozzle Branch, 21000 Brookpk Rd, Cleveland, OH 44135 USA. NR 16 TC 7 Z9 7 U1 1 U2 6 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 APR PY 2011 VL 49 IS 4 BP 748 EP 759 DI 10.2514/1.J050683 PG 12 WC Engineering, Aerospace SC Engineering GA 745SI UT WOS:000289185800007 ER PT J AU Diskin, B Thomas, JL AF Diskin, Boris Thomas, James L. TI Comparison of Node-Centered and Cell-Centered Unstructured Finite Volume Discretizations: Inviscid Fluxes SO AIAA JOURNAL LA English DT Article; Proceedings Paper CT 48th AIAA Aerospace Sciences Meeting/New Horizons Forum and Aerospace Exposition CY JAN 04-08, 2010 CL Orlando, FL SP AIAA ID SOLVERS AB Nominally second-order cell-centered and node-centered approaches are compared for unstructured finite volume discretization of inviscid fluxes in two dimensions. Three classes of grids are considered: isotropic grids in a rectangular geometry, anisotropic grids typical of adapted grids, and anisotropic grids over a curved surface typical of advancing-layer grids. The classes contain regular and irregular grids, including mixed-element grids and grids with random perturbations of nodes. Complexity, accuracy, and convergence of defect-correction iterations are studied. Deficiencies of specific schemes, such as instability, accuracy degradation, and/or poor convergence of defect-correction iterations, have been observed in computations and confirmed in analysis. All schemes may produce large relative gradient-reconstruction errors on grids with perturbed nodes. On advancing-layer grids, a local approximate-mapping technique based on the distance function restores gradient-reconstruction accuracy and fast convergence of defect-correction iterations. Among the considered scheme, the best cell-centered and node-centered schemes, which are low-complexity, stable, robust, and uniformly second-order-accurate, are recommended. C1 [Diskin, Boris] Natl Inst Aerosp, Hampton, VA 23681 USA. [Diskin, Boris] Univ Virginia, Dept Mech & Aerosp Engn, Charlottesville, VA 22904 USA. [Thomas, James L.] NASA, Langley Res Ctr, AeroSci Branch, Hampton, VA 23681 USA. RP Diskin, B (reprint author), Natl Inst Aerosp, 100 Explorat Way, Hampton, VA 23681 USA. EM bdiskin@nianet.org; james.l.thomas@nasa.gov NR 21 TC 7 Z9 9 U1 0 U2 4 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 APR PY 2011 VL 49 IS 4 BP 836 EP 854 DI 10.2514/1.J050897 PG 19 WC Engineering, Aerospace SC Engineering GA 745SI UT WOS:000289185800014 ER PT J AU Samanta, A Appelo, D Colonius, T Nott, J Hall, J AF Samanta, Arnab Appeloe, Daniel Colonius, Tim Nott, Julian Hall, Jeffrey TI Comment on "Computational Modeling and Experiments of Natural Convection for a Titan Montgolfiere" Reply SO AIAA JOURNAL LA English DT Editorial Material ID SPHERES C1 [Samanta, Arnab; Colonius, Tim] CALTECH, Div Engn & Appl Sci, Pasadena, CA 91125 USA. [Nott, Julian] Nott Technol LLC, Santa Barbara, CA 93101 USA. [Hall, Jeffrey] CALTECH, Jet Prop Lab, Pasadena, CA 91011 USA. RP Samanta, A (reprint author), CALTECH, Div Engn & Appl Sci, Pasadena, CA 91125 USA. NR 7 TC 1 Z9 1 U1 0 U2 2 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 APR PY 2011 VL 49 IS 4 BP 877 EP 878 DI 10.2514/1.J050961 PG 2 WC Engineering, Aerospace SC Engineering GA 745SI UT WOS:000289185800019 ER PT J AU Barnes, NP Amzajerdian, F Reichle, DJ Carrion, WA Busch, GE Leisher, P AF Barnes, N. P. Amzajerdian, F. Reichle, D. J. Carrion, W. A. Busch, G. E. Leisher, P. TI Diode pumped Ho:YAG and Ho:LuAG lasers, Q-switching and second harmonic generation SO APPLIED PHYSICS B-LASERS AND OPTICS LA English DT Article ID HO-YAG LASER; TM-YLF LASER; ROOM-TEMPERATURE; OPERATION; EMISSION AB Direct diode pumped Ho:YAG generated laser pulses at 2.12 mu m with an optical to optical slope efficiency of 0.24. Ho:YAG and Ho:LuAG laser rods were evaluated with both wide and narrow bandwidth pump diodes. The laser wavelength varies with the level of pumping and optical design. This variation was found to be predictable. Second harmonic at 1.06 mu m was produced in a 6.0 mm long BBO crystal. C1 [Barnes, N. P.; Amzajerdian, F.; Reichle, D. J.] NASA, Langley Res Ctr, Hampton, VA 23681 USA. [Carrion, W. A.; Busch, G. E.] Coherent Applicat Inc, Hampton, VA 23681 USA. [Leisher, P.] nLight, Vancouver, WA 98665 USA. RP Barnes, NP (reprint author), NASA, Langley Res Ctr, Hampton, VA 23681 USA. EM norman.p.barnes@nasa.gov NR 22 TC 16 Z9 16 U1 5 U2 29 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0946-2171 EI 1432-0649 J9 APPL PHYS B-LASERS O JI Appl. Phys. B-Lasers Opt. PD APR PY 2011 VL 103 IS 1 BP 57 EP 66 DI 10.1007/s00340-010-4195-3 PG 10 WC Optics; Physics, Applied SC Optics; Physics GA 750OY UT WOS:000289559000011 ER PT J AU Cao, H Russell, CT Christensen, UR Dougherty, MK Burton, ME AF Cao, Hao Russell, Christopher T. Christensen, Ulrich R. Dougherty, Michele K. Burton, Marcia E. TI Saturn's very axisymmetric magnetic field: No detectable secular variation or tilt SO EARTH AND PLANETARY SCIENCE LETTERS LA English DT Article DE Saturn; magnetic dynamo; interior structure ID ROTATION PERIOD; PLANETS; DYNAMO; MODEL AB Saturn is the only planet in the solar system whose observed magnetic field is highly axisymmetric. At least a small deviation from perfect symmetry is required for a dynamo-generated magnetic field. Analyzing more than six years of magnetometer data obtained by Cassini close to the planet, we show that Saturn's observed field is much more axisymmetric than previously thought. We invert the magnetometer observations that were obtained in the "current-free" inner magnetosphere for an internal model, varying the assumed unknown rotation rate of Saturn's deep interior. No unambiguous non-axially symmetric magnetic moment is detected, with a new upper bound on the dipole tilt of 0.06 degrees. An axisymmetric internal model with Schmidt-normalized spherical harmonic coefficients g10 = 21,191 +/- 24 nT, g20 = 1586 +/- 7 nT. g30 = 2374 +/- 47 nT is derived from these measurements, the upper bounds on the axial degree 4 and 5 terms are 720 nT and 3200 nT respectively. The secular variation for the last 30 years is within the probable error of each term from degree 1 to 3, and the upper bounds are an order of magnitude smaller than in similar terrestrial terms for degrees 1 and 2. Differentially rotating conducting stable layers above Saturn's dynamo region have been proposed to symmetrize the magnetic field (Stevenson, 1982). The new upper bound on the dipole tilt implies that this stable layer must have a thickness L >= 4000 km, and this thickness is consistent with our weak secular variation observations. (C) 2011 Elsevier B.V. All rights reserved. C1 [Cao, Hao; Russell, Christopher T.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90095 USA. [Christensen, Ulrich R.] Max Planck Inst Solar Syst Res, D-37191 Katlenburg Lindau, Germany. [Dougherty, Michele K.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, London SW7 2AZ, England. [Burton, Marcia E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Cao, H (reprint author), 595 Charles E Young Dr E,6862 Slichter Hall, Los Angeles, CA 90095 USA. EM haocao@ucla.edu RI Cao, Hao/B-5689-2012; OI Russell, Christopher/0000-0003-1639-8298 FU National Aeronautics and Space Administration [1236948] FX This work at UCLA is supported by the National Aeronautics and Space Administration under JPL contract 1236948. We thank the two reviewers for their valuable comments and suggestions, which greatly improved this paper. NR 30 TC 18 Z9 18 U1 0 U2 4 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 APR 1 PY 2011 VL 304 IS 1-2 BP 22 EP 28 DI 10.1016/j.epsl.2011.02.035 PG 7 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 748KB UT WOS:000289388400003 ER PT J AU Righter, K AF Righter, K. TI Prediction of metal-silicate partition coefficients for siderophile elements: An update and assessment of PT conditions for metal-silicate equilibrium during accretion of the Earth SO EARTH AND PLANETARY SCIENCE LETTERS LA English DT Article DE mantle; siderophile; core formation; accretion; magma ocean ID TERRESTRIAL MAGMA OCEAN; CORE FORMATION; OXYGEN FUGACITY; HIGH-PRESSURE; OXIDATION-STATE; LOWER-MANTLE; MELT COMPOSITION; EXPERIMENTAL CONSTRAINTS; CHEMICAL-COMPOSITION; TEMPERATURE AB Experimental studies of the partitioning of siderophile elements between metallic and silicate liquids have provided fundamental constraints on the early history and differentiation conditions of the Earth. With many new studies even in the last 20 yr, several models have emerged from the results, including low pressure equilibrium, high pressure equilibrium, and combined high and low pressure multi-stage models. The reasons silicate melt composition, pressure effects on silicate melt structure, different methods for calculating metal activity coefficients, and the role of deep mantle phases - for the multitude of resulting models have not been specifically addressed before, yet are critical in evaluating the more likely and realistic models. The four reasons - leading to the divergence of results will be discussed and evaluated. The behavior of the moderately siderophile elements Ni and Co will be compared using several approaches, each of which results in the same conclusion for Ni and Co. This consistency will eliminate the supposition that one or the other approaches gives a more accurate answer for element partitioning. Newly updated expressions for 11 elements are then derived and presented and applied to the early Earth to evaluate the idea of a late stage equilibration between a core forming metal and silicate melt (or magma ocean). It is possible to explain all 11 elements at conditions of 27-33 GPa, 3300-3600 K, Delta IW = -1, for peridotite and a metallic liquid containing 10% of a light element. The main difference between the current result and several other recent modeling efforts is that Mn, V, and Cr are hosted in deep mantle phases as well as the core. The other elements - Ni, Co, Mo, W. P, Cu, Ga, and Pd - are hosted in core, and detailed modeling here shows the importance of accounting for oxygen fugacity, silicate and metallic liquid compositions, as well as temperature and pressure. The idea of late stage metal-silicate equilibrium at a restricted pressure and temperature range leaving a chemical finger print on the upper mantle remains viable. Published by Elsevier B.V. C1 NASA Johnson Space Ctr, Mailcode KT, Houston, TX 77058 USA. RP Righter, K (reprint author), NASA Johnson Space Ctr, Mailcode KT, Houston, TX 77058 USA. EM kevin.righter-1@nasa.gov FU RTOP from the NASA FX B. Wood provided the Metalcalc code for calculating activity coefficients for trace elements in metallic liquids. K. Leung and B. Fessler provided computing assistance at the Lunar and Planetary Institute. Discussions with L. Danielson, M. Humayun, A. Campbell, and G. Shofner have been influential in the presentation of this work. Journal reviews of L. Burkemper and two anonymous reviewers, as well as the comments of R. Carlson, led to significant improvements in the presentation of this work. Research is supported by an RTOP to KR from the NASA Cosmochemistry program. NR 86 TC 62 Z9 63 U1 4 U2 35 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 APR 1 PY 2011 VL 304 IS 1-2 BP 158 EP 167 DI 10.1016/j.epsl.2011.01.028 PG 10 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 748KB UT WOS:000289388400017 ER PT J AU Russell, MJ Lecakes, GD Mandayam, S Jensen, S AF Russell, Michael J. Lecakes, George D., Jr. Mandayam, Shreekanth Jensen, Scott TI The "Intelligent" Valve: A Diagnostic Framework for Integrated System-Health Management of a Rocket-Engine Test Stand SO IEEE TRANSACTIONS ON INSTRUMENTATION AND MEASUREMENT LA English DT Article DE Automated test and diagnostic systems; human-computer interface; virtual measurement systems ID SENSOR VALIDATION AB Valves play a critical role in rocket-engine test stands because they are essential for the cryogen transport mechanisms that are vital to test operations. Sensors that are placed on valves monitor the pressure, temperature, flow rate, valve position, and any other features that are required for diagnosing their functionality. Integrated system-health management (ISHM) algorithms have been used to identify and evaluate anomalous operating conditions of systems and subsystems (e. g., valves and valve components) on complex structures, such as rocket test stands. In order for such algorithms to be useful, there is a need to develop realistic models for the most common and problem-prone elements. Furthermore, the user needs to be provided with efficient tools to explore the nature of the anomaly and its possible effects on the element, as well as its relationship to the overall system state. This paper presents the development of an intelligent-valve framework that is capable of tracking and visualizing events of the large linear actuator valve (LLAV) in order to detect anomalous conditions. The framework employs a combination of technologies, including a dynamic data exchange data-transfer protocol, autoassociative neural networks, empirical and physical models, and virtual-reality environments. The diagnostic procedure that is developed has the ability to be integrated into existing ISHM systems and can be used for assessing the integrity of rocket-engine test-stand components. C1 [Russell, Michael J.; Lecakes, George D., Jr.; Mandayam, Shreekanth] Rowan Univ, Elect & Comp Engn Dept, Glassboro, NJ 08028 USA. [Jensen, Scott] Natl Aeronaut & Space Adm, Stennis Space Ctr, MS 39529 USA. RP Russell, MJ (reprint author), Rowan Univ, Elect & Comp Engn Dept, Glassboro, NJ 08028 USA. EM shreek@rowan.edu FU National Aeronautics and Space Administration (NASA) Stennis Space Center [NNX08BA19A]; NASA [NNX08AV98H, NNX07AO92H] FX Manuscript received May 27, 2010; revised August 13, 2010; accepted October 5, 2010. Date of publication January 17, 2011; date of current version March 8, 2011. This work was supported in part by the National Aeronautics and Space Administration (NASA) Stennis Space Center under Grant/Cooperative Agreement-NNX08BA19A and in part by the NASA Graduate Student Researchers Program under Grants/Cooperative Agreements-NNX08AV98H and NNX07AO92H. The Associate Editor coordinating the review process for this paper was Dr. John Sheppard. NR 23 TC 4 Z9 4 U1 1 U2 8 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0018-9456 EI 1557-9662 J9 IEEE T INSTRUM MEAS JI IEEE Trans. Instrum. Meas. PD APR PY 2011 VL 60 IS 4 BP 1489 EP 1497 DI 10.1109/TIM.2010.2101350 PG 9 WC Engineering, Electrical & Electronic; Instruments & Instrumentation SC Engineering; Instruments & Instrumentation GA 746AJ UT WOS:000289212900040 ER PT J AU Goossens, S Matsumoto, K Liu, Q Kikuchi, F Sato, K Hanada, H Ishihara, Y Noda, H Kawano, N Namiki, N Iwata, T Lemoine, FG Rowlands, DD Harada, Y Chen, M AF Goossens, S. Matsumoto, K. Liu, Q. Kikuchi, F. Sato, K. Hanada, H. Ishihara, Y. Noda, H. Kawano, N. Namiki, N. Iwata, T. Lemoine, F. G. Rowlands, D. D. Harada, Y. Chen, M. TI Lunar gravity field determination using SELENE same-beam differential VLBI tracking data SO JOURNAL OF GEODESY LA English DT Article DE Lunar gravity; Differential VLBI; Orbit determination; Gravity field determination ID BASE-LINE-INTERFEROMETRY; ORBIT DETERMINATION; PROSPECTOR; MISSION; KAGUYA; VENUS; MOON; SIMULATION; SATELLITES; SELENODESY AB A lunar gravity field model up to degree and order 100 in spherical harmonics, named SGM100i, has been determined from SELENE and historical tracking data, with an emphasis on using same-beam S-band differential VLBI data obtained in the SELENE mission between January 2008 and February 2009. Orbit consistency throughout the entire mission period of SELENE as determined from orbit overlaps for the two sub-satellites of SELENE involved in the VLBI tracking improved consistently from several hundreds of metres to several tens of metres by including differential VLBI data. Through orbits that are better determined, the gravity field model is also improved by including these data. Orbit determination performance for the new model shows improvements over earlier 100th degree and order models, especially for edge-on orbits over the deep far side. Lunar Prospector orbit determination shows an improvement of orbit consistency from 1-day predictions for 2-day arcs of 6 m in a total sense, with most improvement in the along and cross-track directions. Data fit for the types and satellites involved is also improved. Formal errors for the lower degrees are smaller, and the new model also shows increased correlations with topography over the far side. The estimated value for the lunar GM for this model equals 4902.80080 +/- 0.0009 km(3)/s(2) (10 sigma). The lunar degree 2 potential Love number k(2) was also estimated, and has a value of 0.0255 +/- 0.0016 (10 sigma as well). C1 [Goossens, S.; Matsumoto, K.; Kikuchi, F.; Sato, K.; Hanada, H.; Ishihara, Y.; Noda, H.] Natl Astron Observ Japan, RISE Project, Oshu, Iwate 0230861, Japan. [Liu, Q.; Kawano, N.; Harada, Y.; Chen, M.] Shanghai Astron Observ, Shanghai, Peoples R China. [Namiki, N.] Chiba Inst Technol, Planetary Explorat Res Ctr, Chiba, Japan. [Iwata, T.] Japan Aerosp Explorat Agcy, Kanagawa, Japan. [Lemoine, F. G.; Rowlands, D. D.] NASA, Goddard Space Flight Ctr, Planetary Geodynam Lab, Solar Syst Explorat Div, Greenbelt, MD 20771 USA. RP Goossens, S (reprint author), Natl Astron Observ Japan, RISE Project, 2-12 Hoshigaoka, Oshu, Iwate 0230861, Japan. EM sander@miz.nao.ac.jp RI Rowlands, David/D-2751-2012; Ishihara, Yoshiaki/A-8499-2011; Lemoine, Frank/D-1215-2013; he, shuyi/K-2082-2014; Goossens, Sander/K-2526-2015; OI Goossens, Sander/0000-0002-7707-1128; Ishihara, Yoshiaki/0000-0002-0375-6300 FU Japan Society for the Promotion of Science [20244073] FX We would like to express our appreciation to the engineers of NEC/Toshiba Space Systems Ltd. (NTS), Nippon Antenna Co. Ltd., and Nippi Corporation who developed the on-board instruments and the sub-satellites. We would also like to thank the entire staff of the SELENE project, especially the flight directors for both Rstar and Vstar who supervised the tracking of these two sub-satellites. We would especially like to thank all the colleagues at RISE Project, Mizusawa, who helped with the VLBI observations and data correlation. We thank Alex Konopliv (JPL) and two other anonymous reviewers for their comments that helped to improve this paper. VLBI tracking data files and the new model are available through the SELENE Data archive website at http://www.soac.selene.isas.jaxa.jp/archive/. The models are also available through the RISE Data archive website at http://www.miz.nao.ac.jp/rise-pub/en. All figures were drawn using the free software package GMT (Wessel and Smith 1991). Localised spherical harmonic analyses were performed using the freely available software archive SHTOOLS (available at http://www.ipgp.fr/similar to wieczor/SHTOOLS/SHTOOLS.html). This work was supported by Grant-in-Aid for Scientific Research (A) (No. 20244073) from the Japan Society for the Promotion of Science. Finally, we like to mention that the gravity experiments of SELENE would not have been possible without the expertise of Fumio Fuke, an engineer of NTS, who sadly passed away 2 months after the launch of the mission. NR 53 TC 34 Z9 43 U1 0 U2 6 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0949-7714 EI 1432-1394 J9 J GEODESY JI J. Geodesy PD APR PY 2011 VL 85 IS 4 BP 205 EP 228 DI 10.1007/s00190-010-0430-2 PG 24 WC Geochemistry & Geophysics; Remote Sensing SC Geochemistry & Geophysics; Remote Sensing GA 748GI UT WOS:000289377600002 ER PT J AU Waterbury, LD Galindo, D Villanueva, L Nguyen, C Patel, M Borbridge, L Attar, M Schiffman, RM Hollander, DA AF Waterbury, L. David Galindo, Danielle Villanueva, Linda Cathy Nguyen Patel, Milan Borbridge, Lisa Attar, Mayssa Schiffman, Rhett M. Hollander, David A. TI Ocular Penetration and Anti-inflammatory Activity of Ketorolac 0.45% and Bromfenac 0.09% Against Lipopolysaccharide-Induced Inflammation SO JOURNAL OF OCULAR PHARMACOLOGY AND THERAPEUTICS LA English DT Article ID PROSTAGLANDIN E-2; CATARACT-SURGERY; VISCOUS VEHICLE; ANIMAL-MODELS; TROMETHAMINE; 0.4-PERCENT; ABSORPTION; FORMULATIONS; INHIBITION; EFFICACY AB Purpose: Anti-inflammatory activity of topical nonsteroidal anti-inflammatory drugs is mediated by suppression of cyclooxygenase (COX) isoenzymes. This study compared ocular penetration and inflammation suppression of topical ketorolac 0.45% and bromfenac 0.09% ophthalmic solutions in a rabbit model. Methods: At hour 0, 36 rabbits received ketorolac 0.45%, bromfenac 0.09%, or an artificial tear 3 times once every 20 min. Half of the rabbits in each group then received intravenous injections of lipopolysaccharide (LPS) and fluorescein isothiocyanate (FITC)-dextran at hour 1, and the other half at hour 10. Aqueous and iris-ciliary body (ICB) samples were collected in the former group at hour 2 (peak) and in the latter group at hour 11 (trough) An additional group of 6 animals received only FITC-dextran, and samples were collected 1 h later. Peak and trough nonsteroidal anti-inflammatory drug concentrations were compared with previously determined half-maximal inhibitory concentrations (IC(50)) for COX isoenzymes. Results: Peak and trough aqueous and ICB concentrations of ketorolac were at least 7-fold or greater than those of bromfenac. At peak levels, both ketorolac 0.45% and bromfenac 0.09% significantly inhibited LPS-induced aqueous prostaglandin E(2) and FITC-dextran elevation (P < 0.01). At trough, both study drugs significantly inhibited LPS-induced aqueous prostaglandin E(2) elevation (P < 0.05), but only ketorolac 0.45% significantly reduced LPS-induced aqueous FITC-dextran elevation (P < 0.01). Aqueous and ICB ketorolac concentrations exceeded its IC(50) for COX-1 and COX-2 at peak and trough. Aqueous and ICB bromfenac levels exceeded its IC(50) for COX-2 at peak and trough, but not for COX-1 at trough aqueous levels and peak and trough ICB levels. Conclusions: Both ketorolac 0.45% and bromfenac 0.09% effectively suppressed inflammation at peak. At trough, only ketorolac 0.45% effectively suppressed inflammation as measured by FITC-dextran leakage. The difference in inflammation suppression may be due to differences in tissue concentrations and/or greater COX-1 suppression by ketorolac 0.45%. C1 [Waterbury, L. David] Raven Biosolut LLC, San Carlos, CA 94070 USA. [Galindo, Danielle; Cathy Nguyen] NASA, Ames Res Ctr, Lifesource Biomed LLC, Moffett Field, CA 94035 USA. [Villanueva, Linda; Patel, Milan; Borbridge, Lisa; Attar, Mayssa; Schiffman, Rhett M.; Hollander, David A.] Allergan Pharmaceut Inc, Irvine, CA 92715 USA. RP Waterbury, LD (reprint author), Raven Biosolut LLC, POB 7001, San Carlos, CA 94070 USA. EM david_waterbury@yahoo.com FU Allergan, Inc., Irvine, CA; Allergan, Inc. FX This study was funded by Allergan, Inc., Irvine, CA. L. David Waterbury received research support from Allergan, Inc. D. Galindo and C. Nguyen have no financial and/or conflicting interests to disclose. L. Villanueva, M. Patel, L. Borbridge, M. Attar, R. M. Schiffman, and D. A. Hollander are employees of Allergan, Inc. NR 32 TC 6 Z9 6 U1 0 U2 0 PU MARY ANN LIEBERT INC PI NEW ROCHELLE PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA SN 1080-7683 J9 J OCUL PHARMACOL TH JI J. Ocular Pharmacol. Ther. PD APR PY 2011 VL 27 IS 2 BP 173 EP 178 DI 10.1089/jop.2010.0135 PG 6 WC Ophthalmology; Pharmacology & Pharmacy SC Ophthalmology; Pharmacology & Pharmacy GA 751NF UT WOS:000289624100010 PM 21351868 ER PT J AU Hurwitz, MM Newman, PA Oman, LD Molod, AM AF Hurwitz, M. M. Newman, P. A. Oman, L. D. Molod, A. M. TI Response of the Antarctic Stratosphere to Two Types of El Nino Events SO JOURNAL OF THE ATMOSPHERIC SCIENCES LA English DT Article ID CHEMISTRY-CLIMATE MODELS; SEA-SURFACE TEMPERATURE; NORTHERN WINTER; OSCILLATION; REANALYSIS; ENSEMBLE AB This study is the first to identify a robust El Nino-Southern Oscillation (ENSO) signal in the Antarctic stratosphere. El Nino events between 1979 and 2009 are classified as either conventional "cold tongue" events (positive SST anomalies in the Nino-3 region) or "warm pool" events (positive SST anomalies in the Nino-4 region). The 40-yr ECMWF Re-Analysis (ERA-40), NCEP, and Modern Era Retrospective-Analysis for Research and Applications (MERRA) meteorological reanalyses are used to show that the Southern Hemisphere stratosphere responds differently to these two types of El Nino events. Consistent with previous studies, cold tongue events do not impact temperatures in the Antarctic stratosphere. During warm pool El Nino events, the poleward extension and increased strength of the South Pacific convergence zone favor an enhancement of planetary wave activity during September-November. On average, these conditions lead to higher polar stratospheric temperatures and a weakening of the Antarctic polar jet in November and December, as compared with neutral ENSO years. The phase of the quasi-biennial oscillation (QBO) modulates the stratospheric response to warm pool El Nino events; the strongest planetary wave driving events are coincident with the easterly phase of the QBO. C1 [Hurwitz, M. M.] NASA, NASA Postdoctoral Program, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Molod, A. M.] Univ Maryland, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21201 USA. RP Hurwitz, MM (reprint author), NASA, NASA Postdoctoral Program, Goddard Space Flight Ctr, Code 613-3, Greenbelt, MD 20771 USA. EM margaret.m.hurwitz@nasa.gov RI Newman, Paul/D-6208-2012; Oman, Luke/C-2778-2009 OI Newman, Paul/0000-0003-1139-2508; Oman, Luke/0000-0002-5487-2598 FU NASA FX MMH is supported by an appointment to the NASA Postdoctoral Program at Goddard Space Flight Center, administered by Oak Ridge Associated Universities through a contract with NASA. The authors thank NASA's MAP program for funding. NR 34 TC 18 Z9 18 U1 0 U2 9 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0022-4928 EI 1520-0469 J9 J ATMOS SCI JI J. Atmos. Sci. PD APR PY 2011 VL 68 IS 4 BP 812 EP 822 DI 10.1175/2011JAS3606.1 PG 11 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 749TC UT WOS:000289491800010 ER PT J AU Azua-Bustos, A Gonzalez-Silva, C Mancilla, RA Salas, L Gomez-Silva, B McKay, CP Vicuna, R AF Azua-Bustos, Armando Gonzalez-Silva, Carlos Mancilla, Rodrigo A. Salas, Loreto Gomez-Silva, Benito McKay, Christopher P. Vicuna, Rafael TI Hypolithic Cyanobacteria Supported Mainly by Fog in the Coastal Range of the Atacama Desert SO MICROBIAL ECOLOGY LA English DT Article ID 16S RIBOSOMAL-RNA; EXTRACELLULAR POLYSACCHARIDE; ENVIRONMENTAL GRADIENTS; NORTHERN CHILE; HYPERARID CORE; SAND MULCHES; PCR PRIMERS; CHINA HOT; WATER; COMMUNITY AB The Atacama Desert is one of the driest places on Earth, with an arid core highly adverse to the development of hypolithic cyanobacteria. Previous work has shown that when rain levels fall below similar to 1 mm per year, colonization of suitable quartz stones falls to virtually zero. Here, we report that along the coast in these arid regions, complex associations of cyanobacteria, archaea, and heterotrophic bacteria inhabit the undersides of translucent quartz stones. Colonization rates in these areas, which receive virtually no rain but mainly fog, are significantly higher than those reported inland in the hyperarid zone at the same latitude. Here, hypolithic colonization rates can be up to 80%, with all quartz rocks over 20 g being colonized. This finding strongly suggests that hypolithic microbial communities thriving in the seaward face of the Coastal Range can survive with fog as the main regular source of moisture. A model is advanced where the development of the hypolithic communities under quartz stones relies on a positive feedback between fog availability and the higher thermal conductivity of the quartz rocks, which results in lower daytime temperatures at the quartz-soil interface microenvironment. C1 [Azua-Bustos, Armando; Mancilla, Rodrigo A.; Salas, Loreto; Vicuna, Rafael] Pontificia Univ Catolica Chile, Fac Ciencias Biol, Dept Mol Genet & Microbiol, Santiago, Chile. [Gonzalez-Silva, Carlos] Univ Arturo Prat, Ctr Invest Medio Ambiente CENIMA, Iquique, Chile. [McKay, Christopher P.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Azua-Bustos, Armando; Vicuna, Rafael] MIFAB, Santiago, Chile. [Gomez-Silva, Benito] Univ Antofagasta, Fac Ciencias Salud, Dept Biomed, Antofagasta, Chile. RP Azua-Bustos, A (reprint author), Pontificia Univ Catolica Chile, Fac Ciencias Biol, Dept Mol Genet & Microbiol, Alameda 340, Santiago, Chile. EM ajazua@uc.cl RI mancilla, rodrigo/C-8380-2011; azua-bustos, armando/P-8787-2016 FU Millennium Institute of Fundamental and Applied Biology, MIFAB (Chile) FX This work was supported by the Millennium Institute of Fundamental and Applied Biology, MIFAB (Chile). We also thank Alejandro Munizaga and Ximena Verges for the technical support with microscopy methods. NR 55 TC 33 Z9 33 U1 5 U2 30 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0095-3628 EI 1432-184X J9 MICROB ECOL JI Microb. Ecol. PD APR PY 2011 VL 61 IS 3 BP 568 EP 581 DI 10.1007/s00248-010-9784-5 PG 14 WC Ecology; Marine & Freshwater Biology; Microbiology SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Microbiology GA 747BK UT WOS:000289295100009 PM 21188376 ER PT J AU Zhu, DH Vaishampayan, PA Venkateswaran, K Fox, GE AF Zhu, Dianhui Vaishampayan, Parag A. Venkateswaran, Kasthuri Fox, George E. TI STITCH: Algorithm to Splice, Trim, Identify, Track, and Capture the Uniqueness of 16S rRNAs Sequence Pairs Using Public or In-house Database SO MICROBIAL ECOLOGY LA English DT Article ID FOR-BIOTECHNOLOGY-INFORMATION; POLYMERASE-CHAIN-REACTION; PCR; AMPLIFICATION; IDENTIFICATION; FIDELITY; ARB; DNA; RESOURCES; BACTERIA AB A comparison of variable regions within the 16S rRNA gene is widely used to characterize relationships between bacteria and to identify phylogenetic affiliation of unknown bacteria. In environmental studies, polymerase chain reaction amplification of 16S rRNA followed by cloning and sequencing of numerous individual clones is an extensively used molecular method for elucidating microbial diversity. The sequencing process typically utilizes a forward and reverse primer pair to produce two partial reads (similar to 700 to 800 base pairs each) that overlap and in total cover a large region of the full 16S rRNA sequence (similar to 1.5 k base). In a typical application, this approach rapidly generates very large numbers of 16S rRNA datasets that can overwhelm manual processing efforts leading to both delays and errors. In particular, the approach presents two computational challenges: (1) the assembly of a composite sequence from the two partial reads and (2) the subsequent appropriate identification of the organism represented by the newly sequenced clones. Herein, we describe a software package, search, trim, identify, track, and capture the uniqueness of 16S rRNAs using public and in-house database (STITCH), which offers automated sequence pair splicing and genetic identification, thus simplifying the computationally intensive analysis of large sequencing libraries. The STITCH software is freely accessible over the Internet at: http://prion.bchs.uh.edu/stitch/. C1 [Vaishampayan, Parag A.; Venkateswaran, Kasthuri] CALTECH, Jet Prop Lab, Biotechnol & Planetary Protect Grp, Pasadena, CA 91109 USA. [Zhu, Dianhui; Fox, George E.] Univ Houston, Dept Biol & Biochem, Houston, TX 77204 USA. RP Vaishampayan, PA (reprint author), CALTECH, Jet Prop Lab, Biotechnol & Planetary Protect Grp, M-S 89-102,4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM vaishamp@jpl.nasa.gov NR 40 TC 2 Z9 2 U1 0 U2 2 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0095-3628 EI 1432-184X J9 MICROB ECOL JI Microb. Ecol. PD APR PY 2011 VL 61 IS 3 BP 669 EP 675 DI 10.1007/s00248-010-9779-2 PG 7 WC Ecology; Marine & Freshwater Biology; Microbiology SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Microbiology GA 747BK UT WOS:000289295100018 PM 21113709 ER PT J AU Shahzad, MMK Mangala, LS Han, HD Lu, CH Bottsford-Miller, J Nishimura, M Mora, EM Lee, JW Stone, RL Pecot, CV Thanapprapasr, D Roh, JW Gaur, P Nair, MP Park, YY Sabnis, N Deavers, MT Lee, JS Ellis, LM Lopez-Berestein, G McConathy, WJ Prokai, L Lacko, AG Sood, AK AF Shahzad, Mian M. K. Mangala, Lingegowda S. Han, Hee Dong Lu, Chunhua Bottsford-Miller, Justin Nishimura, Masato Mora, Edna M. Lee, Jeong-Won Stone, Rebecca L. Pecot, Chad V. Thanapprapasr, Duangmani Roh, Ju-Won Gaur, Puja Nair, Maya P. Park, Yun-Yong Sabnis, Nirupama Deavers, Michael T. Lee, Ju-Seog Ellis, Lee M. Lopez-Berestein, Gabriel McConathy, Walter J. Prokai, Laszlo Lacko, Andras G. Sood, Anil K. TI Targeted Delivery of Small Interfering RNA Using Reconstituted High-Density Lipoprotein Nanoparticles SO NEOPLASIA LA English DT Article ID FOCAL ADHESION KINASE; ENDOTHELIAL GROWTH-FACTOR; OVARIAN-CARCINOMA; SCAVENGER RECEPTOR; TUMOR ANGIOGENESIS; CANCER-CELLS; SR-BI; CONSTITUTIVE ACTIVATION; ANTICANCER DRUGS; STAT3 AB RNA interference holds tremendous potential as a therapeutic approach, especially in the treatment of malignant tumors. However, efficient and biocompatible delivery methods are needed for systemic delivery of small interfering RNA (siRNA). To maintain a high level of growth, tumor cells scavenge high-density lipoprotein (HDL) particles by overexpressing its receptor: scavenger receptor type B1 (SR-B1). In this study, we exploited this cellular characteristic to achieve efficient siRNA delivery and established a novel formulation of siRNA by incorporating it into reconstituted HDL (rHDL) nanoparticles. Here, we demonstrate that rHDL nanoparticles facilitate highly efficient systemic delivery of siRNA in vivo, mediated by the SR-B1. Moreover, in therapeutic proof-of-concept studies, these nanoparticles were effective in silencing the expression of two proteins that are key to cancer growth and metastasis (signal transducer and activator of transcription 3 and focal adhesion kinase) in orthotopic mouse models of ovarian and colorectal cancer. These data indicate that an rHDL nanoparticle is a novel and highly efficient siRNA carrier, and therefore, this novel technology could serve as the foundation for new cancer therapeutic approaches. C1 [Shahzad, Mian M. K.; Han, Hee Dong; Lu, Chunhua; Bottsford-Miller, Justin; Nishimura, Masato; Lee, Jeong-Won; Stone, Rebecca L.; Thanapprapasr, Duangmani; Roh, Ju-Won; Sood, Anil K.] Univ Texas MD Anderson Canc Ctr, Dept Gynecol Oncol, Houston, TX 77030 USA. [Shahzad, Mian M. K.] Univ Wisconsin, Dept Obstet & Gynecol, Div Gynecol Oncol, Sch Med & Publ Hlth, Madison, WI 53706 USA. [Mangala, Lingegowda S.] Univ Space Res Assoc, Dept Radiat Biophys, NASA Johnson Space Ctr, Houston, TX USA. [Mora, Edna M.; Gaur, Puja; Ellis, Lee M.] Univ Texas MD Anderson Canc Ctr, Dept Surg Oncol, Houston, TX 77030 USA. [Mora, Edna M.] Univ Puerto Rico, Ctr Comprehens Canc, San Juan, PR 00936 USA. [Mora, Edna M.] Univ Puerto Rico, Sch Med, San Juan, PR 00936 USA. [Lee, Jeong-Won] Sungkyunkwan Univ, Sch Med, Samsung Med Ctr, Dept Obstet & Gynecol, Seoul, South Korea. [Pecot, Chad V.] Univ Texas MD Anderson Canc Ctr, Dept Canc Med, Houston, TX 77030 USA. [Nair, Maya P.; Sabnis, Nirupama; Prokai, Laszlo; Lacko, Andras G.] Univ N Texas, HSC, Dept Mol Biol & Immunol, Ft Worth, TX USA. [Park, Yun-Yong; Lee, Ju-Seog] Univ Texas MD Anderson Canc Ctr, Dept Syst Biol, Houston, TX 77030 USA. [Deavers, Michael T.] Univ Texas MD Anderson Canc Ctr, Dept Pathol, Houston, TX 77030 USA. [Ellis, Lee M.; Lopez-Berestein, Gabriel; Sood, Anil K.] Univ Texas MD Anderson Canc Ctr, Dept Canc Biol, Houston, TX 77030 USA. [Lopez-Berestein, Gabriel] Univ Texas MD Anderson Canc Ctr, Dept Expt Therapeut, Houston, TX 77030 USA. [Lopez-Berestein, Gabriel; Sood, Anil K.] Univ Texas MD Anderson Canc Ctr, Ctr RNA Interference & Noncoding RNA, Houston, TX 77030 USA. [McConathy, Walter J.] Texas Tech Univ, HSC, Dept Internal Med, Ft Worth, TX USA. RP Sood, AK (reprint author), Univ Texas MD Anderson Canc Ctr, Dept Gynecol Oncol, 1155 Herman Pressler,Unit 1362, Houston, TX 77030 USA. EM asood@mdanderson.org RI lee, jw/O-6237-2014; OI Prokai, Laszlo/0000-0002-4559-3458 FU GCF; National Institutes of Health [HD050128, CA109298, CA110793, CA128797, RC2GM092599, U54 CA151668]; NCI [CA 101642, CA 009614]; Department of Defense [OC073399, OC093146, BC085265]; Ovarian Cancer Research Fund, Inc; Zarrow Foundation; Marcus Foundation; University of Texas MD Anderson Cancer Center SPORE in Ovarian Cancer [P50 CA083639]; Betty Ann Asche Murray Distinguished Professorship; Deborah Gonzalez Women's Health Fellowship Award; Puerto Rico Comprehensive Cancer Center; University of North Texas Health Science Center FX This research was supported by the GCF Molly-Cade ovarian cancer research grant, grants from the National Institutes of Health (Baylor WRHR Scholarship grant: HD050128; CA109298, CA110793, CA128797, RC2GM092599, U54 CA151668), NCI (T32 training grants CA 101642, CA 009614), Department of Defense (OC073399, OC093146, BC085265), a Program Project Development Grant from the Ovarian Cancer Research Fund, Inc, the Zarrow Foundation, The Marcus Foundation, the University of Texas MD Anderson Cancer Center SPORE in Ovarian Cancer (P50 CA083639), the Betty Ann Asche Murray Distinguished Professorship, Deborah Gonzalez Women's Health Fellowship Award, the Puerto Rico Comprehensive Cancer Center, Cowtown Cruisin' for the Cure, and a HER grant from the University of North Texas Health Science Center. NR 64 TC 82 Z9 89 U1 8 U2 51 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 1476-5586 J9 NEOPLASIA JI Neoplasia PD APR PY 2011 VL 13 IS 4 BP 309 EP U142 DI 10.1593/neo.101372 PG 17 WC Oncology SC Oncology GA 750FB UT WOS:000289529400002 PM 21472135 ER PT J AU Halkides, D Lee, T Kida, S AF Halkides, Daria Lee, Tong Kida, Shinichiro TI Mechanisms controlling the seasonal mixed-layer temperature and salinity of the Indonesian seas SO OCEAN DYNAMICS LA English DT Article DE Indonesian seas; Mixed layer; Seasonal heat budget; Seasonal salinity budget; ECCO; Ocean-state estimation ID MARITIME CONTINENT; CIRCULATION MODEL; UPPER OCEAN; PACIFIC; THROUGHFLOW; PARAMETERIZATION; VARIABILITY; SENSITIVITY; REGION; GCM AB We examine the seasonal mixed-layer temperature (MLT) and salinity (MLS) budgets in the Banda-Arafura Seas region (120-138A degrees E, 8-3A degrees S) using an ECCO ocean-state estimation product. MLT in these seas is relatively high during November-May (austral spring through fall) and relatively low during June-September (austral winter and the period associated with the Asian summer monsoon). Surface heat flux makes the largest contribution to the seasonal MLT tendency, with significant reinforcement by subsurface processes, especially turbulent vertical mixing. Temperature declines (the MLT tendency is negative) in May-August when seasonal insolation is smallest and local winds are strong due to the southeast monsoon, which causes surface heat loss and cooling by vertical processes. In particular, Ekman suction induced by local wind stress curl raises the thermocline in the Arafura Sea, bringing cooler subsurface water closer to the base of the mixed layer where it is subsequently incorporated into the mixed layer through turbulent vertical mixing; this has a cooling effect. The MLT budget also has a small, but non-negligible, semi-annual component since insolation increases and winds weaken during the spring and fall monsoon transitions near the equator. This causes warming via solar heating, reduced surface heat loss, and weakened turbulent mixing compared to austral winter and, to a lesser extent, compared to austral summer. Seasonal MLS is dominated by ocean processes rather than by local freshwater flux. The contributions by horizontal advection and subsurface processes have comparable magnitudes. The results suggest that ocean dynamics play a significant part in determining both seasonal MLT and MLS in the region, such that coupled model studies of the region should use a full ocean model rather than a slab ocean mixed-layer model. C1 [Halkides, Daria] Univ Calif Los Angeles, JIFRESSE, Los Angeles, CA 90095 USA. [Lee, Tong] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Kida, Shinichiro] Japan Agcy Marine Earth Sci & Technol, Earth Simulator Ctr, Yokohama, Kanagawa, Japan. RP Halkides, D (reprint author), Univ Calif Los Angeles, JIFRESSE, Los Angeles, CA 90095 USA. EM halkides@jpl.nasa.gov RI Kida, Shinichiro/E-9137-2014 OI Kida, Shinichiro/0000-0002-9471-4316 FU NASA; PO.DAAC; KAKENHI [21840066] FX This research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA. Support by PO.DAAC (http://podaac.jpl.nasa.gov) is acknowledged. S. Kida was supported by KAKENHI (21840066). NR 40 TC 6 Z9 6 U1 0 U2 11 PU SPRINGER HEIDELBERG PI HEIDELBERG PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY SN 1616-7341 EI 1616-7228 J9 OCEAN DYNAM JI Ocean Dyn. PD APR PY 2011 VL 61 IS 4 BP 481 EP 495 DI 10.1007/s10236-010-0374-3 PG 15 WC Oceanography SC Oceanography GA 750ES UT WOS:000289528400007 ER PT J AU Kwok, R Untersteiner, N AF Kwok, Ronald Untersteiner, Norbert TI The thinning of Arctic sea ice SO PHYSICS TODAY LA English DT Article ID MODEL C1 [Kwok, Ronald] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Untersteiner, Norbert] Univ Washington, Seattle, WA 98195 USA. RP Kwok, R (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. RI Kwok, Ron/A-9762-2008 OI Kwok, Ron/0000-0003-4051-5896 NR 14 TC 66 Z9 69 U1 1 U2 23 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 EI 1945-0699 J9 PHYS TODAY JI Phys. Today PD APR PY 2011 VL 64 IS 4 BP 36 EP 41 PG 6 WC Physics, Multidisciplinary SC Physics GA 748NS UT WOS:000289397900015 ER PT J AU Gopalswamy, N AF Gopalswamy, Nat TI Mukul Ranjan Kundu obituary SO PHYSICS TODAY LA English DT Biographical-Item C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Gopalswamy, N (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RI Gopalswamy, Nat/D-3659-2012; OI Gopalswamy, Nat/0000-0001-5894-9954 NR 1 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 EI 1945-0699 J9 PHYS TODAY JI Phys. Today PD APR PY 2011 VL 64 IS 4 BP 71 EP 71 PG 1 WC Physics, Multidisciplinary SC Physics GA 748NS UT WOS:000289397900019 ER PT J AU Jimenez-Escalona, JC Granados, HD Realmuto, VJ AF Carlos Jimenez-Escalona, Jose Delgado Granados, Hugo Realmuto, Vincent J. TI Use of MODIS images to study eruptive clouds from Volcan de Fuego de Colima (Mexico) and applications on volcano monitoring SO GEOFISICA INTERNACIONAL LA English DT Article DE remote sensing; volcanic emission; MODIS; satellite image; Colima volcano; volcanic cloud ID ASH CLOUDS; DE-COLIMA; EMISSIONS AB Volcano monitoring using satellite images may provide periodic information on gas emission fluctuations such as SO(2) emissions related to the processes occurring inside volcanoes. This study analyses a period of 36 days (May 10 to June 15, 2005) of processing 113 MODIS images for the detection of SO(2). Within this period it was also possible to detect and quantify 8 of 15 explosive events reported by the Washington VAAC. With the satellite images as tools for monitoring the volcanic emissions, it was possible to determine three cases related to volcanic ashes: 1) follow up of volcanic ash and gases transported by wind, 2) calculation of ash-cloud residence time in the atmosphere, 3) effects of shearing winds during the ascent of an ash plume. Regarding the continuous monitoring of passive emissions of SO(2), there is a relationship among explosive events and increasing peaks of SO(2) emission suggesting a difference of approximately 2 days between the two events that may anticipate the type of behavior of the volcano. C1 [Carlos Jimenez-Escalona, Jose; Delgado Granados, Hugo] Univ Nacl Autonoma Mexico, Inst Geofis, Mexico City 04510, DF, Mexico. [Carlos Jimenez-Escalona, Jose] Inst Politecn Nacl, ESIME U Ticoman, Mexico City 07340, DF, Mexico. [Realmuto, Vincent J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Jimenez-Escalona, JC (reprint author), Univ Nacl Autonoma Mexico, Inst Geofis, Ciudad Univ, Mexico City 04510, DF, Mexico. EM jjimeneze@ipn.mx RI Delgado Granados, Hugo/J-3056-2013; OI Delgado Granados, Hugo/0000-0001-5263-7968; Jimenez_Escalona, Jose Carlos/0000-0001-9309-5245 FU EHaz program FX The first author is grateful to William I. Rose for his assistance while in Michigan Tech for learning remote sensing methods, This research was partially funded by the EHaz program. NR 29 TC 2 Z9 2 U1 1 U2 4 PU INST GEOPHYSICS UNAM PI MEXICO PA APDO POSTAL 22-118, DEL TLALPAN, MEXICO, 14000 D F, MEXICO SN 0016-7169 J9 GEOFIS INT JI Geofis. Int. PD APR-JUN PY 2011 VL 50 IS 2 BP 199 EP 210 PG 12 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 746BU UT WOS:000289217400006 ER PT J AU Zahnle, K Freedman, RS Catling, DC AF Zahnle, Kevin Freedman, Richard S. Catling, David C. TI Is there methane on Mars? SO ICARUS LA English DT Article DE Atmospheres, Chemistry; Mars, Atmosphere; Spectroscopy; Photochemistry ID MARTIAN DUST DEVILS; ATMOSPHERIC CHEMISTRY; NOBLE-GASES; OXIDANT ENHANCEMENT; PHOTOCHEMICAL DATA; CARBON-MONOXIDE; H2O PHOTOLYSIS; ISOTOPIC CO2; ORIGIN; LIFE AB There have been several reports of methane on Mars at the 10-60 ppbv level. Most suggest that methane is both seasonally and latitudinally variable. Here we review why variable methane on Mars is physically and chemically implausible, and then we critically review the published reports. There is no known mechanism for destroying methane chemically on Mars. But if there is one, methane oxidation would deplete the O-2 in Mars's atmosphere in less than 10,000 years unless balanced by an equally large unknown source of oxidizing power. Physical sequestration does not raise these questions, but adsorption in the regolith or condensation in clathrates ignore competition for adsorption sites or are inconsistent with clathrate stability, respectively. Furthermore, any mechanism that relies on methane's van der Waals' attraction is inconsistent with the continued presence of Xe in the atmosphere at the 60 ppbv level. We then use the HITRAN database and transmission calculations to identify and characterize the absorption lines that would be present on Earth or Mars at the wavelengths of the published observations. These reveal strong competing telluric absorption that is most problematic at just those wavelengths where methane's signature seems most clearly seen from Earth. The competing telluric lines must be removed with models. The best case for martian methane was made for the (CH4)-C-12 nu(3) R0 and R1 lines seen in blueshift when Mars was approaching Earth in early 2003 (Mumma, M.J., Villanueva, G.L., Novak, RE., Hewagama, T., Bonev, B.P., DiSanti, MA., Mandell, A.M., Smith, M.D. [2009]. Science 323, 1041-1045). For these the Doppler shift moves the two martian lines into near coincidence with telluric (CH4)-C-13 nu(3) R1 and R2 lines that are 10-50x stronger than the inferred martian lines. By contrast, the (CH4)-C-12 nu(3) R0 and R1 lines when observed in redshift do not contend with telluric (CH4)-C-13. For these lines, Mumma et al.'s observations and analyses are consistent with an upper limit on the order of 3 ppbv. Published by Elsevier Inc. C1 [Zahnle, Kevin; Freedman, Richard S.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Catling, David C.] Univ Washington, Dept Earth & Space Sci, Seattle, WA 98195 USA. RP Zahnle, K (reprint author), NASA, Ames Res Ctr, MS 245-3, Moffett Field, CA 94035 USA. EM Kevin.J.Zahnle@NASA.gov RI Catling, David/D-2082-2009; OI Catling, David/0000-0001-5646-120X FU NASA FX We thank Todd Clancy, Francois Forget, Colin Goldblatt, Tom Greene, Robert Haberle, Jim Lyons, Chris McKay, and Victoria Meadows for helpful comments, comprehensive discussions, several corrections, and key insights. We especially thank Michael Mumma and Geronimo Villanueva for their openness and the considerable help and encouragement they have given us in all aspects of this work. We also thank Paul Wennberg, Mike Mumma and an anonymous reviewer for careful reviews correcting and improving the manuscript. This work was supported by NASA's Exobiology Program. NR 61 TC 72 Z9 75 U1 5 U2 35 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 APR PY 2011 VL 212 IS 2 BP 493 EP 503 DI 10.1016/j.icarus.2010.11.027 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 745PM UT WOS:000289178100005 ER PT J AU Davila, AF Gross, C Marzo, GA Fairen, AG Kneissl, T McKay, CP Dohm, JM AF Davila, Alfonso F. Gross, Christoph Marzo, Giuseppe A. Fairen, Alberto G. Kneissl, Thomas McKay, Christopher P. Dohm, James M. TI A large sedimentary basin in the Terra Sirenum region of the southern highlands of Mars SO ICARUS LA English DT Article DE Evaporites; Basin; Highlands; Noachian; Water ID ATACAMA DESERT; AQUEOUS ENVIRONMENTS; IMPACT CRATERS; EVAPORITES; CHILE; PHYLLOSILICATES; EVOLUTION; MINERALS; CLIMATE; MISSION AB Different lines of evidence point to hydrological cycling in the martian past. The extent, duration, and magnitude of this cycling remains unclear, as well as the magnitude of aqueous processes on the surface. Here, we provide geomorphic and mineralogic evidence of a large inter-crater sedimentary basin located in the Terra Sirenum region, which was once covered by a body of liquid water with an areal extent of at least 30,000 km(2) and a depth of approximately 200 m. The topographic basin, which is modified by a number of large impact craters, is partly controlled by ancient impact and tectonic structures. As a result of evaporation of the large body of water, salt flats formed in the lowest topographic reaches of the basin. Hydrated phyllosilicates occur in close proximity to the salt flats and in the ejecta and rim materials of small impact craters with stratigraphic relations that suggest that they underlie the evaporite deposits. Crater statistics place the maximum age of aqueous activity during the Late Noachian epoch. The relatively pristine mineral deposits in the basin have a high potential to yield information of the geochemistry and water activity during the ancient Noachian Period when conditions were seemingly more conducive to life. (C) 2010 Elsevier Inc. All rights reserved. C1 [Davila, Alfonso F.; Marzo, Giuseppe A.; Fairen, Alberto G.; McKay, Christopher P.] NASA, Ames Res Ctr, Space Sci & Astrobiol Div, Moffett Field, CA 94035 USA. [Davila, Alfonso F.; Fairen, Alberto G.] SETI Inst, Carl Sagan Ctr Study Life Universe, Mountain View, CA 94043 USA. [Gross, Christoph; Kneissl, Thomas] Free Univ Berlin, Inst Geol Sci Planetary Sci & Remote Sensing, D-12249 Berlin, Germany. [Marzo, Giuseppe A.] Bay Area Environm Res Inst, Sonoma, CA 95476 USA. [Dohm, James M.] Univ Arizona, Dept Hydrol & Water Resources, Tucson, AZ 85719 USA. RP Davila, AF (reprint author), NASA, Ames Res Ctr, Space Sci & Astrobiol Div, Moffett Field, CA 94035 USA. EM adavila@seti.org RI Davila, Alfonso/A-2198-2013; Dohm, James/A-3831-2014; Marzo, Giuseppe/A-9765-2015 OI Davila, Alfonso/0000-0002-0977-9909; FU Helmholtz Association through the research alliance "Planetary Evolution and Life" FX We wish to thank the comments and suggestions of two anonymous reviewers, which greatly improved the manuscript. Research by C.G. and T.K. was supported by the Helmholtz Association through the research alliance "Planetary Evolution and Life". NR 56 TC 10 Z9 10 U1 1 U2 6 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD APR PY 2011 VL 212 IS 2 BP 579 EP 589 DI 10.1016/j.icarus.2010.12.023 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 745PM UT WOS:000289178100011 ER PT J AU Busch, MW Ostro, SJ Benner, LAM Brozovic, M Giorgini, JD Jao, JS Scheeres, DJ Magri, C Nolan, MC Howell, ES Taylor, PA Margot, JL Brisken, W AF Busch, Michael W. Ostro, Steven J. Benner, Lance A. M. Brozovic, Marina Giorgini, Jon D. Jao, Joseph S. Scheeres, Daniel J. Magri, Christopher Nolan, Michael C. Howell, Ellen S. Taylor, Patrick A. Margot, Jean-Luc Brisken, Walter TI Radar observations and the shape of near-Earth ASTEROID 2008 EV5 SO ICARUS LA English DT Article DE Asteroids; Asteroids, Surfaces; Asteroids, Dynamics; Radar observations ID BINARY ASTEROIDS; 2867 STEINS; 1999 KW4; YORP; POPULATION; YARKOVSKY; REGOLITH; HAYABUSA; SPINS AB We observed the near-Earth ASTEROID 2008 EV5 with the Arecibo and Goldstone planetary radars and the Very Long Baseline Array during December 2008. EV5 rotates retrograde and its overall shape is a 400 +/- 50 m oblate spheroid. The most prominent surface feature is a ridge parallel to the asteroid's equator that is broken by a concavity about 150 m in diameter. Otherwise the asteroid's surface is notably smooth on decameter scales. EV5's radar and optical albedos are consistent with either rocky or stony-iron composition. The equatorial ridge is similar to structure seen on the rubble-pile near-Earth asteroid (66391) 1999 KW4 and is consistent with YORP spin-up reconfiguring the asteroid in the past. We interpret the concavity as an impact crater. Shaking during the impact and later regolith redistribution may have erased smaller features, explaining the general lack of decameter-scale surface structure. (C) 2011 Elsevier Inc. All rights reserved. C1 [Busch, Michael W.; Margot, Jean-Luc] Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90095 USA. [Ostro, Steven J.; Benner, Lance A. M.; Brozovic, Marina; Giorgini, Jon D.; Jao, Joseph S.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Scheeres, Daniel J.] Univ Colorado, Dept Aerosp Engn Sci, Boulder, CO 80309 USA. [Magri, Christopher] Univ Maine, Farmington, ME 04938 USA. [Nolan, Michael C.; Howell, Ellen S.; Taylor, Patrick A.] Arecibo Observ, Arecibo, PR 00612 USA. [Margot, Jean-Luc] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Brisken, Walter] Natl Radio Astron Observ, Socorro, NM 87801 USA. RP Busch, MW (reprint author), Univ Calif Los Angeles, Dept Earth & Space Sci, 595 Charles Young Dr E, Los Angeles, CA 90095 USA. EM mbusch@ess.ucla.edu RI Margot, Jean-Luc/A-6154-2012; Nolan, Michael/H-4980-2012 OI Margot, Jean-Luc/0000-0001-9798-1797; Nolan, Michael/0000-0001-8316-0680 FU National Science Foundation; National Aeronautics and Space Administration (NASA); Hertz Foundation FX The Goldstone Solar System Radar, Arecibo Observatory, and NRAO Socorro 8: Green Bank staff helped to obtain the data presented here. We thank A. Galad, B.W. Koehn, M.D. Hicks, and V. Reddy for providing EV5's rotation period and spectral type from their optical and infrared observations in advance of publication. The Arecibo Observatory is part of the National Astronomy and Ionosphere Center, which is operated by Cornell University under a cooperative agreement with the National Science Foundation. The NRAO is run by Associated Universities, Inc. for the National Science Foundation. Some of this work was performed at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration (NASA). This paper is based in part on work funded by NASA under the Science Mission Directorate Research and Analysis Programs. M.W. Busch was supported by the Hertz Foundation. Our observations of EV5 are dedicated to the memory of Steven Ostro. NR 46 TC 25 Z9 26 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 APR PY 2011 VL 212 IS 2 BP 649 EP 660 DI 10.1016/j.icarus.2011.01.013 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 745PM UT WOS:000289178100017 ER PT J AU Hendrix, AR Cassidy, TA Johnson, RE Paranicas, C Carlson, RW AF Hendrix, Amanda R. Cassidy, Timothy A. Johnson, Robert E. Paranicas, Chris Carlson, Robert W. TI Europa's disk-resolved ultraviolet spectra: Relationships with plasma flux and surface terrains SO ICARUS LA English DT Article DE Europa; Ices, UV spectroscopy; Jupiter, Satellites; Ultraviolet observations; Satellites, Composition ID ICY GALILEAN SATELLITES; MAGNETOSPHERIC ION-BOMBARDMENT; SULFURIC-ACID; WATER ICE; PHOTOMETRY; SPECTROMETER; IMPLANTATION; RADIOLYSIS; HYDRATE; ALBEDO AB The full set of high-resolution observations from the Galileo Ultraviolet Spectrometer (UVS) is analyzed to look for spectral trends across the surface of Europa. We provide the first disk-resolved map of the 280 nm SO(2) absorption feature and investigate its relationship with sulfur and electron flux distributions as well as with surface features and relative surface ages. Our results have implications for exogenic and endogenic sources. The large-scale pattern in SO(2) absorption band depth is again shown to be similar to the pattern of sulfur ion implantation, but with strong variations in band depth based on terrain. In particular, the young chaos units show stronger SO(2) absorption bands than expected from the average pattern of sulfur ion flux, suggesting a local source of SO(2) in those regions, or diapiric heating that leads to a sulfur-rich lag deposit. While the SO(2) absorption feature is confined to the trailing hemisphere, the near UV albedo (300-310 nm) has a global pattern with a minimum at the center of the trailing hemisphere and a maximum at the center of the leading hemisphere. The global nature of the albedo pattern is suggestive of an exogenic source, and several possibilities are discussed. Like the SO(2) absorption, the near UV albedo also has local variations that depend on terrain type and age. (C) 2011 Elsevier Inc. All rights reserved. C1 [Hendrix, Amanda R.; Cassidy, Timothy A.; Carlson, Robert W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Johnson, Robert E.] Univ Virginia, Charlottesville, VA 22904 USA. [Paranicas, Chris] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. RP Hendrix, AR (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM arh@jpl.nasa.gov RI Paranicas, Christopher/B-1470-2016 OI Paranicas, Christopher/0000-0002-4391-8255 FU Jupiter System Data Analysis Program; Planetary Geology and Geophysics Program; National Aeronautics and Space Administration FX This paper has benefited from good conversations with John Cooper, Gary Hansen, Karl Hibbitts and Bob Nelson, Karen Simmons and Charles Barth. Charles Hord was the PI of the Galileo UVS. This work was supported by the Jupiter System Data Analysis Program and the Planetary Geology and Geophysics Program. 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 46 TC 14 Z9 14 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 J9 ICARUS JI Icarus PD APR PY 2011 VL 212 IS 2 BP 736 EP 743 DI 10.1016/j.icarus.2011.01.023 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 745PM UT WOS:000289178100025 ER PT J AU Williams, DA Radebaugh, J Lopes, RMC Stofan, E AF Williams, David A. Radebaugh, Jani Lopes, Rosaly M. C. Stofan, Ellen TI Geomorphologic mapping of the Menrva region of Titan using Cassini RADAR data SO ICARUS LA English DT Article DE Radar observations; Geological processes ID DIELECTRIC-PROPERTIES; RADIOMETRY DATA; ICY SATELLITES; SURFACE; MAPPER; SAR; DIVERSITY; DUNES AB We made a detailed geomorphologic map of the Menrva region of Titan, using Cassini RADAR data as our map base. Using similar techniques and approaches that were applied to mapping Magellan radar images of Venus, and earlier, more generalized Titan maps, we were able to define and characterize 10 radar morphologic units, along with inferred dunes and fluvial channels, from the RADAR data. Structural features, such as scarps, ridges, and lineaments were also identified. Using principles of superposition, cross-cutting, and embayment relations we created a sequence of map units for this region. We interpret Menrva to be a 440 km wide degraded impact basin, in agreement with earlier studies by Elachi et al. (Elachi, C. et al. [2006]. Nature 441, 709-713) and Wood et al. (Wood, C.A., Lorenz, R., Kirk, R., Lopes, R., Mitchell, K., Stofan, E., and the Cassini RADAR Team [2010]. Icarus 206, 334-344), and identify it as the oldest feature in the map region. Exogenic processes including hydrocarbon fluid channelization forming the Elivagar Flumina channel network and dune fields resulting from aeolian activity are the current geologic processes dominating our map area, and these processes have contributed to the erosion of the crater's ejecta field. There is evidence of multiple episodes of channel formation, erosion and burial by aeolian deposits, as observed elsewhere on Titan by e.g., Barnes et al. (Barnes, J.W. et al. [2005]. Icarus 195,400-414). Channel outflow regions have morphologies suggestive of streams formed by flash floods, and dune fields are small and restricted rather than forming large dune seas, consistent with a desert-like environment for this region with low supply of hydrocarbon particles, also consistent with other studies by e.g.. Lorenz et al. (Lorenz, R.D. et al. [2008a]. Planet. Space Sci. 56, 1132-1144). There is no evidence of cryovolcanism or non-impact-related tectonic activity in the Menrva region, although this region is too small to infer anything about the roles of these processes elsewhere on Titan. This work suggests detailed geomorphologic mapping can confidently be applied to Cassini RADAR data, and we suggest that more extensive mapping should be done using RADAR, ISS, and VIMS data geographically distributed across Titan to assess its usefulness for a future combined RADAR-ISS-VIMS-based global geologic map. (C) 2011 Elsevier Inc. All rights reserved. C1 [Williams, David A.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [Radebaugh, Jani] Brigham Young Univ, Dept Geol Sci, Provo, UT 84602 USA. [Lopes, Rosaly M. C.] CALTECH, Jet Prop Lab, CALTECH, Pasadena, CA 91109 USA. [Stofan, Ellen] Proxemy Res Inc, Rectortown, VA 20140 USA. RP Williams, DA (reprint author), Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. EM david.williams@asu.edu RI Lopes, Rosaly/D-1608-2016 OI Lopes, Rosaly/0000-0002-7928-3167 NR 50 TC 8 Z9 8 U1 1 U2 6 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 J9 ICARUS JI Icarus PD APR PY 2011 VL 212 IS 2 BP 744 EP 750 DI 10.1016/j.icarus.2011.01.014 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 745PM UT WOS:000289178100026 ER PT J AU Anderson, CM Samuelson, RE AF Anderson, Carrie M. Samuelson, Robert E. TI Titan's aerosol and stratospheric ice opacities between 18 and 500 mu m: Vertical and spectral characteristics from Cassini CIRS SO ICARUS LA English DT Article DE Titan; Radiative transfer; Ices ID ROTOTRANSLATIONAL ABSORPTION-SPECTRA; COMPOSITE INFRARED SPECTROMETER; SPECTROSCOPIC DATABASE; CONDENSATE CLOUDS; THERMAL EMISSION; UPPER-ATMOSPHERE; JOVIAN PLANETS; PAIRS; TEMPERATURES; MODEL AB Vertical distributions and spectral characteristics of Titan's photochemical aerosol and stratospheric ices are determined between 20 and 560 cm(-1) (500-18 mu m) from the Cassini Composite Infrared Spectrometer (CIRS). Results are obtained for latitudes of 15 degrees N, 15 degrees S, and 58 degrees S. where accurate temperature profiles can be independently determined. In addition, estimates of aerosol and ice abundances at 62 degrees N relative to those at 15 degrees S are derived. Aerosol abundances are comparable at the two latitudes, but stratospheric ices are similar to 3 times more abundant at 62 degrees N than at 15 degrees S. Generally, nitrile ice clouds (probably HCN and HC3N), as inferred from a composite emission feature at similar to 160 cm(-1), appear to be located over a narrow altitude range in the stratosphere centered at similar to 90 km. Although most abundant at high northern latitudes, these nitrile ice clouds extend down through low latitudes and into mid southern latitudes, at least as far as 58 degrees S. There is some evidence of a second ice cloud layer at similar to 60 km altitude at 58 degrees S associated with an emission feature at similar to 80 cm(-1). We speculate that the identify of this cloud may be due to C2H6 ice, which in the vapor phase is the most abundant hydrocarbon (next to CH4) in the stratosphere of Titan. Unlike the highly restricted range of altitudes (50-100 km) associated with organic condensate clouds, Titan's photochemical aerosol appears to be well-mixed from the surface to the top of the stratosphere near an altitude of 300 km, and the spectral shape does not appear to change between 15 degrees N and 58 degrees S latitude. The ratio of aerosol-to-gas scale heights range from 1.3-2.4 at about 160 km to 1.1-1.4 at 300 km, although there is considerable variability with latitude. The aerosol exhibits a very broad emission feature peaking at similar to 140 cm-1. Due to its extreme breadth and low wavenumber, we speculate that this feature may be caused by low-energy vibrations of two-dimensional lattice structures of large molecules. Examples of such molecules include polycyclic aromatic hydrocarbons (PAHs) and nitrogenated aromatics. Finally, volume extinction coefficients N chi(E) derived from 15 degrees S CIRS data at a wavelength of lambda = 62.5 mu m are compared with those derived from the 10 degrees S Huygens Descent Imager/Spectral Radiometer (DISR) data at 1.583 mu m. This comparison yields volume extinction coefficient ratios N chi(E)(1.583 mu m)/N chi(E)(62.5 mu m) of roughly 70 and 20, respectively, for Titan's aerosol and stratospheric ices. The inferred particle cross-section ratios chi(E)(1.583 mu m)/chi(E)(62.5 mu m) appear to be consistent with sub-micron size aerosol particles, and effective radii of only a few microns for stratospheric ice cloud particles. Published by Elsevier Inc. C1 [Anderson, Carrie M.] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA. [Samuelson, Robert E.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. RP Anderson, CM (reprint author), NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA. EM carrie.m.anderson@nasa.gov RI Anderson, Carrie/C-8097-2012 FU Cassini project; NASA; NSF FX We would like to extend our thanks to Lyn Doose for providing the tabulated Huygens DISR aerosol volume extinction coefficients at 1.583 mu m. We also thank Marla Moore for providing laboratory absorption coefficients for HCN and HC3N ice mixtures. Thanks to Richard Achterberg for providing CIRS Titan temperature structures. C.M.A. was supported in part by the Cassini project and the NASA Cassini Data Analysis Program. R.E.S. was supported in part by the Cassini project and the NSF Planetary Astronomy Program. NR 62 TC 44 Z9 45 U1 2 U2 19 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD APR PY 2011 VL 212 IS 2 BP 762 EP 778 DI 10.1016/j.icarus.2011.01.024 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 745PM UT WOS:000289178100028 ER PT J AU Moore, JM Pappalardo, RT AF Moore, Jeffrey M. Pappalardo, Robert T. TI Titan: An exogenic world? SO ICARUS LA English DT Article DE Saturn, satellites; Titan; Titan, atmosphere; Titan, hydrology; Titan, surface ID HUYGENS LANDING SITE; CASSINI RADAR OBSERVATIONS; SATURNS MOON TITAN; GALILEAN SATELLITES; INTERNAL STRUCTURE; MERCURIAN VOLCANISM; AMMONIUM-SULFATE; ICY SATELLITES; DARK TERRAIN; EARLY MARS AB All landforms on Titan that are unambiguously identifiable can be explained by exogenic processes (aeolian, fluvial, impact cratering, and mass wasting). Previous suggestions of endogenically produced cryovolcanic constructs and flows have, without exception, lacked conclusive diagnostic evidence. The modification of sparse recognizable impact craters (themselves exogenic) can be explained by aeolian and fluvial erosion. Tectonic activity could be driven by global thermal evolution or external forcing, rather than by active interior processes. A lack of cryovolcanism would be consistent with geophysical inferences of a relatively quiescent interior: incomplete differentiation, only minor tidal heating, and possibly a lack of internal convection today. Titan might be most akin to Callisto with weather: an endogenically relatively inactive world with a cool interior. We do not aim to disprove the existence of any and all endogenic activity at Titan, nor to provide definitive alternative hypotheses for all landforms, but instead to inject a necessary level of caution into the discussion. The hypothesis of Titan as a predominantly exogenic world can be tested through additional Cassini observations and analyses of putative cryovolcanic features, geophysical and thermal modeling of Titan's interior evolution, modeling of icy satellite landscape evolution that is shaped by exogenic processes alone, and consideration of possible means for supplying Titan's atmospheric constituents that do not rely on cryovolcanism. Published by Elsevier Inc. C1 [Moore, Jeffrey M.] NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA. [Pappalardo, Robert T.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Moore, JM (reprint author), NASA, Ames Res Ctr, Div Space Sci, M-S 245-3, Moffett Field, CA 94035 USA. EM jeff.moore@nasa.gov; robert.pappalardo@jpl.nasa.gov FU Outer Planets Research Program; Cassini Project; National Aeronautics and Space Administration FX We thank Amy Barr, Bruce Bills, Geoff Collins, Ken Edgett, Alan Howard, Krishan Khurana, Randy Kirk, Bill McKinnon, Giuseppe Mitri, Francis Nimmo, Conor Nixon, Flora Paganelli, Paul Schenk, Larry Soderblom, Christophe Sotin, Don Wilhelms, and Kevin Zahnle for valuable reviews and discussions on various aspects of this research. We are especially grateful for the formal reviews of Jani Radebaugh, Ellen Stofan, and an anonymous reviewer collectively whose comments substantially improved this report. We acknowledge Snowpacalypse 2010 for making the long-awaited completion of this paper possible. Funding for this work was provided by an Outer Planets Research Program grant (JMM) and the Cassini Project (RTP). The portion of this work performed by RTP was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. NR 159 TC 37 Z9 37 U1 3 U2 30 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 APR PY 2011 VL 212 IS 2 BP 790 EP 806 DI 10.1016/j.icarus.2011.01.019 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 745PM UT WOS:000289178100030 ER PT J AU Buratti, BJ Bauer, JM Hicks, MD Hillier, JK Verbiscer, A Hammel, H Schmidt, B Cobb, B Herbert, B Garsky, M Ward, J Foust, J AF Buratti, B. J. Bauer, J. M. Hicks, M. D. Hillier, J. K. Verbiscer, A. Hammel, H. Schmidt, B. Cobb, B. Herbert, B. Garsky, M. Ward, J. Foust, J. TI Photometry of Triton 1992-2004: Surface volatile transport and discovery of a remarkable opposition surge SO ICARUS LA English DT Article DE Triton; Satellites, Surfaces; Satellites, Atmospheres ID BIDIRECTIONAL REFLECTANCE SPECTROSCOPY; DISK-INTEGRATED PHOTOMETRY; OUTER PLANET SATELLITES; HUBBLE-SPACE-TELESCOPE; COHERENT BACKSCATTER; URANIAN SATELLITES; RADIATIVE-TRANSFER; LIGHT-CURVE; VARIABILITY; BRIGHTNESS AB Triton, the large satellite of Neptune, was imaged by the Voyager 2 spacecraft in 1989 with dark plumes originating in its volatile-rich south polar region. Southern summer solstice, a time when seasonal volatile transport should be at a maximum, occurred in 2001. Ground-based observations of Triton's rotational light curve obtained from Table Mountain Observatory in 2000-2004 reveal volatile transport on its surface. When compared with a static frost model constructed from Voyager images, the light curve shows an increase in total amplitude. An earlier light curve obtained in 1992 from Mauna Kea Observatory is consistent with the static frost model. This movement of volatiles on the surface agrees with recent imaging results from the Hubble Space Telescope (Bauer, J.M., Buratti, B.J., Li, J.-Y., Mosher, J.A., Hicks, M.D., Schmidt, BE., Goguen, J.D. [2010]. Astrophys. J. 723, L49-L52). The changes in the light curve can be explained by the transport of nitrogen frost on the surface or by the uncovering of bedrock of less volatile methane. We also find that Triton exhibits a large opposition surge at solar phase angles less than 0.1 degrees. This surge cannot be entirely explained by the effects of coherent backscatter. (C) 2011 Elsevier Inc. All rights reserved. C1 [Buratti, B. J.; Bauer, J. M.; Hicks, M. D.; Schmidt, B.; Cobb, B.; Herbert, B.; Garsky, M.; Ward, J.; Foust, J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Hillier, J. K.] Grays Harbor Coll, Aberdeen, WA 98520 USA. [Verbiscer, A.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. [Hammel, H.] Space Sci Inst, Boulder, CO 80301 USA. RP Buratti, BJ (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Bonnie.Buratti@jpl.nasa.gov OI Schmidt, Britney/0000-0001-7376-8510 FU National Aeronautics and Space Administration; Planetary Geology and Geophysics Undergraduate Research Program FX This research was carried out at the Jet Propulsion Laboratory, California Institute of Technology under contract to the National Aeronautics and Space Administration. We thank NASA's Planetary Astronomy and Planetary Geology and Geophysics Programs for support. The students were sponsored by NASA's Undergraduate Student Research Program, New York Space Grant, and the Planetary Geology and Geophysics Undergraduate Research Program. Copyright 2010 all rights reserved. NR 59 TC 9 Z9 9 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 APR PY 2011 VL 212 IS 2 BP 835 EP 846 DI 10.1016/j.icarus.2011.01.012 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 745PM UT WOS:000289178100033 ER PT J AU Firoz, KA Moon, YJ Cho, KS Hwang, J Park, YD Kudela, K Dorman, LI AF Firoz, K. A. Moon, Y. -J. Cho, K. -S. Hwang, J. Park, Y. D. Kudela, K. Dorman, L. I. TI On the relationship between ground level enhancement and solar flare SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID X-RAY FLARES; PROTON EVENTS; ENERGETIC PARTICLES; NEUTRON-MONITORS; UPPER LIMIT; INDEX; TIMES; SOLAR-CYCLE-23; EMISSION; CYCLES AB We made an effort to understand the associations and relationships between ground level enhancement (GLE) events and solar flares for the time period of 1986-2006. Our results show that, on average, the GLE event-associated solar flare (similar to 0.2 x 10(-4) W/m(2)) is much stronger than the non-GLE-associated solar flare (similar to 0.3 x 10(-5) W/m(2)). The findings have also been supported by the solar flare indices that, on average, the GLE event-associated solar flare index (similar to 35.01) is much higher than the non-GLE-associated solar flare index (similar to 4.88). However, this association does not seem to precisely imply that GLEs can occur because of a solar flare, so we examined cross correlations between GLE events and simultaneous solar flares. We found that most (similar to 78%) of the highest correlations (r > 0.8) took place during an X class flare. There is no clear indication that the more the time lag, the less or more is the correlation or vice versa. Overall, 50% of the high correlations took place at higher time lag (>= 65 min), and similar to 36% of the high correlations took place at lower time lag (<= 40 min), while the rest (similar to 14%) of the correlations were abruptly high and low at medium time lag (> 40 and < 65 min). On the basis of the results of cross correlations, we suggest that the intensive portions of solar flares should be responsible for causing GLEs and that the direct proportionality of the time-integrated intensive portion of a flare with the impulsive phase of a GLE event seems to be the main property for comprehending the mechanism. C1 [Firoz, K. A.; Cho, K. -S.; Hwang, J.; Park, Y. D.] Korea Astron & Space Sci Inst, Solar & Space Weather Res Grp, Taejon 305348, South Korea. [Moon, Y. -J.] Kyung Hee Univ, Sch Space Res, Yongin 446701, Gyeonggi Do, South Korea. [Moon, Y. -J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Kudela, K.] Slovak Acad Sci, Inst Expt Phys, Kosice 04001, Slovakia. [Dorman, L. I.] Russian Acad Sci, Cosm Ray Dept, Moscow 142190, Russia. RP Firoz, KA (reprint author), Korea Astron & Space Sci Inst, Solar & Space Weather Res Grp, Taejon 305348, South Korea. EM kazifiroz2002@gmail.com RI Moon, Yong-Jae/E-1711-2013 FU Development of Korean Space Weather Center of Korea Astronomy and Space Science Institute (KASI); KASI; VEGA [2/0081/10]; NASA [NNX10AL50A]; Ministry of Education, Science and Technology [R31-10016]; Korean government (MOEHRD) [20090071744, 20100014501] FX This work has been financed by the Development of Korean Space Weather Center of Korea Astronomy and Space Science Institute (KASI) and KASI basic research funds. K. Kudela wishes to acknowledge VEGA Project 2/0081/10. Data of the space satellites of GOES of NGDC, NOAA, and NASA and data of the neutron monitor at Oulu have been studied. We would like to express our gratitude to Sung-Hong Park KASI and Dmitry Prokhorov of KASI for important discussions. The authors are indebted to the anonymous reviewers for their constructive comments and suggestions that indeed helped to develop this paper. The authors also recall two important discussions with Sung-Hong Park and Dmitry Prokhorov of KASI. Y.-J. Moon is supported by NASA grant (NNX10AL50A); by the WCU Program (R31-10016) through the National Research Foundation of the Republic of Korea funded by the Ministry of Education, Science and Technology; and by the Korea Research Foundation grant (20090071744 and 20100014501) funded by the Korean government (MOEHRD, Basic Research Promotion Fund). NR 54 TC 9 Z9 9 U1 0 U2 1 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD APR 1 PY 2011 VL 116 AR A04101 DI 10.1029/2010JA016171 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 744HD UT WOS:000289084600004 ER PT J AU Ukwatta, TN Dhuga, KS Morris, DC MacLachlan, G Parke, WC Maximon, LC Eskandarian, A Gehrels, N Norris, JP Shenoy, A AF Ukwatta, T. N. Dhuga, K. S. Morris, D. C. MacLachlan, G. Parke, W. C. Maximon, L. C. Eskandarian, A. Gehrels, N. Norris, J. P. Shenoy, A. TI A new frequency-luminosity relation for long gamma-ray bursts? SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE gamma-ray burst: general ID ALERT TELESCOPE; PEAK LUMINOSITY; VARIABILITY; SPECTRA; ESTIMATOR; MISSION; SAMPLE; BAT AB We have studied power density spectra (PDS) of 206 long gamma-ray bursts. We fitted the PDS with a simple power law and extracted the exponent of the power law (alpha) and the noise-crossing threshold frequency (f(th)). We find that the distribution of the extracted alpha peaks around -1.4 and that of f(th) around 1 Hz. In addition, based on a subset of 58 bursts with known redshifts, we show that the redshift-corrected threshold frequency is positively correlated with the isotropic peak luminosity. The correlation coefficient is 0.57 +/- 0.03. C1 [Ukwatta, T. N.; Dhuga, K. S.; Morris, D. C.; MacLachlan, G.; Parke, W. C.; Maximon, L. C.; Eskandarian, A.; Shenoy, A.] George Washington Univ, Dept Phys, Washington, DC 20052 USA. [Ukwatta, T. N.; Morris, D. C.; Gehrels, N.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Norris, J. P.] Univ Denver, Dept Phys & Astron, Denver, CO 80208 USA. RP Ukwatta, TN (reprint author), George Washington Univ, Dept Phys, Washington, DC 20052 USA. EM tilan.ukwatta@gmail.com RI Gehrels, Neil/D-2971-2012 FU NASA [NNX08AR44A] FX We thank the anonymous referee for comments and suggestions that significantly improved the paper. We also thank T. Sakamoto and C. Guidorzi for useful discussions. The NASA grant NNX08AR44A provided partial support for this work and is gratefully acknowledged. NR 22 TC 3 Z9 3 U1 0 U2 0 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD APR PY 2011 VL 412 IS 2 BP 875 EP 882 DI 10.1111/j.1365-2966.2010.17944.x PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 737DV UT WOS:000288549900010 ER PT J AU Rowe, B Silk, J AF Rowe, Barnaby Silk, Joseph TI The Sunyaev-Zel'dovich effect due to hyperstarburst galaxy winds SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE shock waves; galaxies: high-redshift; intergalactic medium; galaxies: starburst ID MOLECULAR GAS; GALACTIC WINDS; HIGH-REDSHIFT; HOST GALAXY; RELATIVISTIC CORRECTIONS; ULTRALUMINOUS GALAXIES; SUBMILLIMETER GALAXIES; DISTANT QUASARS; BIG-BANG; APEX-SZ AB We construct a simple, spherical blast wave model to estimate the pressure structure of the intergalactic medium surrounding hyperstarburst galaxies, and argue that the effects of interaction with star-forming galaxy winds may be approximated at early times by an adiabatically expanding, self-similar 'bubble' as described by Weaver et al. and Ostriker & McKee. This model is used to make observational predictions for the thermal Sunyaev-Zel'dovich effect in the shocked bubble plasma. Radiative cooling losses are explored, and it is found that bremsstrahlung will limit the epoch of adiabatic expansion to 107- 108 yr: comparable to total hyperstarburst lifetimes. Prospects for making a first Sunyaev-Zel'dovich detection of galaxy wind bubbles using the Atacama Large Millimeter Array are examined for a number of active hyperstarburst sources in the literature. C1 [Rowe, Barnaby] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Rowe, Barnaby] Univ Paris 06, Inst Astrophys Paris, CNRS, UMR7095, F-75014 Paris, France. [Silk, Joseph] Univ Oxford, Dept Phys, Oxford OX1 4LN, England. RP Rowe, B (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM barnaby.t.rowe@jpl.nasa.gov OI silk, joe/0000-0002-1566-8148; Rowe, Barnaby/0000-0002-7042-9174 FU European Union [MRTN-CT-2006-036133] FX The authors would like to thank Richard Bielby, Arthur Kosowsky, Vivienne Wild and the anonymous referee for useful comments and suggestions. BR has been supported in part by the Dark Universe through Extragalactic Lensing (DUEL) European Union FP6 Research Training Network (MRTN-CT-2006-036133). NR 59 TC 0 Z9 0 U1 0 U2 0 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD APR PY 2011 VL 412 IS 2 BP 905 EP 910 DI 10.1111/j.1365-2966.2010.17953.x PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 737DV UT WOS:000288549900013 ER PT J AU Bracco, A Cooray, A Veneziani, M Amblard, A Serra, P Wardlow, J Thompson, MA White, G Auld, R Baes, M Bertoldi, F Buttiglione, S Cava, A Clements, DL Dariush, A De Zotti, G Dunne, L Dye, S Eales, S Fritz, J Gomez, H Hopwood, R Ibar, I Ivison, RJ Jarvis, M Lagache, G Lee, MG Leeuw, L Maddox, S Michalowski, M Pearson, C Pohlen, M Rigby, E Rodighiero, G Smith, DJB Temi, P Vaccari, M van der Werf, P AF Bracco, A. Cooray, A. Veneziani, M. Amblard, A. Serra, P. Wardlow, J. Thompson, M. A. White, G. Auld, R. Baes, M. Bertoldi, F. Buttiglione, S. Cava, A. Clements, D. L. Dariush, A. De Zotti, G. Dunne, L. Dye, S. Eales, S. Fritz, J. Gomez, H. Hopwood, R. Ibar, I. Ivison, R. J. Jarvis, M. Lagache, G. Lee, M. G. Leeuw, L. Maddox, S. Michalowski, M. Pearson, C. Pohlen, M. Rigby, E. Rodighiero, G. Smith, D. J. B. Temi, P. Vaccari, M. van der Werf, P. TI Herschel-ATLAS: statistical properties of Galactic cirrus in the GAMA-9 Hour Science Demonstration Phase Field SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE methods: statistical; ISM: structure; infrared: ISM ID TEMPERATURE-DEPENDENCE; SPECTRAL INDEX; ABSORPTION-COEFFICIENT; SPIRE INSTRUMENT; NUMBER COUNTS; DUST EMISSION; MICRONS; NOISE; GRAINS; CORES AB We study the spectral energy distribution (SED) and the power spectrum of Galactic cirrus emission observed in the 14 deg2 Science Demonstration Phase field of the Herschel-ATLAS using Herschel and IRAS data from 100 to 500 mu m. We compare the Spectral and Photometric Imaging Receiver (SPIRE) 250, 350 and 500 mu m maps with IRAS 100-mu m emission, binned in 6-arcmin pixels. We assume a modified blackbody SED with dust emissivity parameter beta (F proportional to lambda-beta) and a single dust temperature T-d, and find that the dust temperature and emissivity index varies over the science demonstration field as and 1 < beta < 4. The latter values are somewhat higher than the range of beta often quoted in the literature (1 < beta < 2). We estimate the mean values of these parameters to be T-d = 19.0 +/- 2.4 K and beta = 1.4 +/- 0.4. In regions of bright cirrus emission, we find that the dust has similar temperatures with , and similar values of beta, ranging from 1.4 +/- 0.5 to 1.9 +/- 0.5. We show that T-d and beta associated with diffuse cirrus emission are anti-correlated and can be described by the relationship: beta(T-d) = NT alpha(d) with [N = 116 +/- 38, alpha = -1.4 +/- 0.1]. The strong correlation found in this analysis is not just limited to high-density clumps of cirrus emission as seen in previous studies, but is also seen in diffuse cirrus in low-density regions. To provide an independent measure of T-d and beta, we obtain the angular power spectrum of the cirrus emission in the IRAS and SPIRE maps, which is consistent with a power spectrum of the form P(k) = P-0(k/k(0))gamma, where gamma = 2.6 +/- 0.2 for scales of 50-200 arcmin in the SPIRE maps. The cirrus rms fluctuation amplitude at angular scales of 100 arcmin is consistent with a modified blackbody SED with and beta = 1.3 +/- 0.2, in agreement with the values obtained above. C1 [Bracco, A.; Cooray, A.; Veneziani, M.; Amblard, A.; Serra, P.; Wardlow, J.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. [Cooray, A.] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA. [Veneziani, M.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Thompson, M. A.; Jarvis, M.] Univ Hertfordshire, Ctr Astrophys Res, Sci & Technol Res Inst, Hatfield AL10 9AB, Herts, England. [White, G.; Hopwood, R.; Pearson, C.] Open Univ, Dept Phys & Astron, Milton Keynes MK7 6AA, Bucks, England. [White, G.] Rutherford Appleton Lab, Space Sci & Technol Div, Chilton OX11 0NL, Oxon, England. [Auld, R.; Dariush, A.; Dye, S.; Eales, S.; Gomez, H.; Pohlen, M.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Baes, M.; Fritz, J.] Univ Ghent, Sterrenkundig Observatorium, B-9000 Ghent, Belgium. [Bertoldi, F.] INAF Osservatorio Astron Padova, I-35122 Padua, Italy. [Buttiglione, S.; De Zotti, G.] Univ Bonn, Argelander Inst Astron, D-53121 Bonn, Germany. [Cava, A.] Univ La Laguna, Inst Astrofis Canarias, E-38205 San Cristobal la Laguna, Spain. [Cava, A.] Univ La Laguna, Dept Astrofis, E-38205 San Cristobal la Laguna, Spain. [Clements, D. L.] Univ London Imperial Coll Sci Technol & Med, Astrophys Grp, Dept Phys, London SW7 2AZ, England. [De Zotti, G.] SISSA, I-34136 Trieste, Italy. [Dunne, L.; Maddox, S.; Rigby, E.; Smith, D. J. B.] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England. [Ibar, I.; Ivison, R. J.] Royal Observ, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland. [Ivison, R. J.; Michalowski, M.; van der Werf, P.] Univ Edinburgh, Royal Observ, SUPA, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland. [Lagache, G.] Univ Paris 11, Lab IAS, UMR8617, F-91405 Orsay, France. [Lagache, G.] CNRS, F-91405 Orsay, France. [Lee, M. G.] Seoul Natl Univ, Dept Phys & Astron, Seoul 151742, South Korea. [Leeuw, L.] SETI Inst, Mountain View, CA 94043 USA. [Pearson, C.] Rutherford Appleton Lab, Space Sci & Technol Dept, Chilton OX11 0QX, Oxon, England. [Pearson, C.] Univ Lethbridge, Inst Space Imaging Sci, Lethbridge, AB T1K 3M4, Canada. [Rodighiero, G.; Vaccari, M.] Univ Padua, Dept Astron, Padua, Italy. [Temi, P.] NASA, Ames Res Ctr, Astrophys Branch, Moffett Field, CA 94035 USA. [van der Werf, P.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. RP Bracco, A (reprint author), Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. EM acooray@uci.edu RI Baes, Maarten/I-6985-2013; Serra, Paolo/G-9678-2014; amblard, alexandre/L-7694-2014; Wardlow, Julie/C-9903-2015; Ivison, R./G-4450-2011; Vaccari, Mattia/R-3431-2016; Cava, Antonio/C-5274-2017; OI Dye, Simon/0000-0002-1318-8343; Baes, Maarten/0000-0002-3930-2757; Serra, Paolo/0000-0002-7609-3931; amblard, alexandre/0000-0002-2212-5395; Wardlow, Julie/0000-0003-2376-8971; Ivison, R./0000-0001-5118-1313; Vaccari, Mattia/0000-0002-6748-0577; Cava, Antonio/0000-0002-4821-1275; Maddox, Stephen/0000-0001-5549-195X; Smith, Daniel/0000-0001-9708-253X; Rodighiero, Giulia/0000-0002-9415-2296 FU NASA FX The Herschel-ATLAS is a project with Herschel, which is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA. The H-ATLAS website is http://www.h-atlas.org/. AA, AB, AC and PS acknowledge support from NASA funds for US participants in Herschel through JPL. NR 51 TC 31 Z9 31 U1 0 U2 1 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD APR PY 2011 VL 412 IS 2 BP 1151 EP 1161 DI 10.1111/j.1365-2966.2010.17971.x PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 737DV UT WOS:000288549900034 ER PT J AU Braglia, FG Ade, PAR Bock, JJ Chapin, EL Devlin, MJ Edge, A Griffin, M Gundersen, JO Halpern, M Hargrave, PC Hughes, DH Klein, J Marsden, G Mauskopf, P Moncelsi, L Netterfield, CB Ngo, H Olmi, L Pascale, E Patanchon, G Pimbblet, KA Rex, M Scott, D Semisch, C Thomas, N Truch, MDP Tucker, C Tucker, GS Valiante, E Viero, MP Wiebe, DV AF Braglia, Filiberto G. Ade, Peter A. R. Bock, James J. Chapin, Edward L. Devlin, Mark J. Edge, Alastair Griffin, Matthew Gundersen, Joshua O. Halpern, Mark Hargrave, Peter C. Hughes, David H. Klein, Jeff Marsden, Gaelen Mauskopf, Philip Moncelsi, Lorenzo Netterfield, Calvin B. Ngo, Henry Olmi, Luca Pascale, Enzo Patanchon, Guillaume Pimbblet, Kevin A. Rex, Marie Scott, Douglas Semisch, Christopher Thomas, Nicholas Truch, Matthew D. P. Tucker, Carole Tucker, Gregory S. Valiante, Elisabetta Viero, Marco P. Wiebe, Donald V. TI Submillimetre observations of galaxy clusters with the BLAST: the star formation activity in Abell 3112 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: clusters: general; galaxies: clusters: individual: A3112; galaxies: evolution; galaxies: star formation; infrared: galaxies; submillimetre: galaxies ID FAR-INFRARED EMISSION; STARBURST GALAXIES; INTRACLUSTER DUST; GALACTIC NUCLEI; REDSHIFT SURVEY; HOST GALAXIES; RICH CLUSTERS; TO 0.3; EVOLUTION; FIELD AB We present observations at 250, 350 and 500 mu m of the nearby galaxy cluster Abell 3112 (z = 0.075) carried out with the Balloon-borne Large Aperture Submillimeter Telescope. Five cluster members are individually detected as bright submillimetre (submm) sources. Their far-infrared spectral energy distributions and optical colours identify them as normal star-forming galaxies of high mass, with globally evolved stellar populations. They all have (B - R) colours of 1.38 +/- 0.08, transitional between the blue, active population and the red, evolved galaxies that dominate the cluster core. We stack to estimate the mean submm emission from all cluster members, which is determined to be 16.6 +/- 2.5, 6.1 +/- 1.9 and 1.5 +/- 1.3 mJy at 250, 350 and 500 mu m, respectively. Stacking analyses of the submm emission of cluster members reveal trends in the mean far-infrared luminosity with respect to clustercentric radius and K-S-band magnitude. We find that a large fraction of submm emission comes from the boundary of the inner, virialized region of the cluster, at clustercentric distances around R-500. Stacking also shows that the bulk of the submm emission arises in intermediate-mass galaxies with K-S magnitude similar to 1 mag fainter than the giant ellipticals. The results and constraints obtained in this work will provide a useful reference for the forthcoming surveys to be conducted on galaxy clusters by Herschel. C1 [Braglia, Filiberto G.; Chapin, Edward L.; Halpern, Mark; Marsden, Gaelen; Ngo, Henry; Scott, Douglas; Valiante, Elisabetta; Wiebe, Donald V.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. [Ade, Peter A. R.; Griffin, Matthew; Hargrave, Peter C.; Mauskopf, Philip; Moncelsi, Lorenzo; Pascale, Enzo; Tucker, Gregory S.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Bock, James J.] Jet Prop Lab, Pasadena, CA 91109 USA. [Devlin, Mark J.; Klein, Jeff; Semisch, Christopher; Truch, Matthew D. P.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. [Edge, Alastair] Univ Durham, Dept Phys, Durham DH1 3LE, England. [Gundersen, Joshua O.; Thomas, Nicholas] Univ Miami, Dept Phys, Coral Gables, FL 33146 USA. [Hughes, David H.] INAOE, Puebla 72000, Mexico. [Netterfield, Calvin B.] 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, Phys Dept, UPR Stn, Rio Piedras, PR 00931 USA. [Olmi, Luca] INAF Osservatorio Astrofis Arcetri, I-50125 Florence, Italy. [Patanchon, Guillaume] Univ Paris Diderot, Lab APC, F-75205 Paris, France. [Pimbblet, Kevin A.] Monash Univ, Sch Phys, Clayton, Vic 3800, Australia. [Rex, Marie] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Tucker, Carole] Brown Univ, Dept Phys, Providence, RI 02912 USA. [Viero, Marco P.] CALTECH, Pasadena, CA 91125 USA. RP Braglia, FG (reprint author), Univ British Columbia, Dept Phys & Astron, 6224 Agr Rd, Vancouver, BC V6T 1Z1, Canada. EM fbraglia@phas.ubc.ca RI Klein, Jeffrey/E-3295-2013; OI Olmi, Luca/0000-0002-1162-7947; Scott, Douglas/0000-0002-6878-9840; Edge, Alastair/0000-0002-3398-6916; Ngo, Henry/0000-0001-5172-4859 FU National Aeronautics and Space Administration (NASA) [NAG5-12785, NAG5-13301, NNGO-6GI11G]; NSF Office of Polar Programs; Canadian Space Agency; Natural Sciences and Engineering Research Council (NSERC) of Canada; UK Science and Technology Facilities Council (STFC); National Science Foundation FX We acknowledge the support of the National Aeronautics and Space Administration (NASA) through grant numbers 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). This research has been enabled by the use of WestGrid computing resources. FGB acknowledges Daniele Pierini for helpful discussions and the anonymous referee for their suggestions. This work is partly based on observations made at the Australian Astronomical Observatory with the Anglo-Australian Telescope. This research has made use of the NED, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the NASA. This publication makes use of 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 the NASA and the National Science Foundation. 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 the NASA. NR 73 TC 9 Z9 9 U1 0 U2 5 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 APR PY 2011 VL 412 IS 2 BP 1187 EP 1202 DI 10.1111/j.1365-2966.2010.17973.x PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 737DV UT WOS:000288549900037 ER PT J AU Leaman, J Li, WD Chornock, R Filippenko, AV AF Leaman, Jesse Li, Weidong Chornock, Ryan Filippenko, Alexei V. TI Nearby supernova rates from the Lick Observatory Supernova Search - I. The methods and data base SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Review DE surveys; supernovae: general; galaxies: evolution ID CORE-COLLAPSE SUPERNOVAE; AUTOMATIC IMAGING TELESCOPE; HUBBLE-SPACE-TELESCOPE; GAMMA-RAY BURSTS; IA SUPERNOVAE; HOST GALAXIES; RELATIVE FREQUENCIES; STAR-FORMATION; HIGH-REDSHIFT; MASSIVE STAR AB This is the first paper of a series in which we present new measurements of the observed rates of supernovae (SNe) in the local Universe, determined from the Lick Observatory Supernova Search. We have obtained 2.3 million observations of 14 882 sample galaxies over an interval of 11 years (1998 March to 2008 December). We considered 1036 SNe detected in our sample and used an optimal subsample of 726 SNe (274 Type Ia SNe, 116 Type Ibc SNe and Type II 324 SNe) to determine our SN rates. This is the largest and most homogeneous set of nearby SNe ever assembled for this purpose, and ours is the first local SN rate analysis based on CCD imaging and modern image-subtraction techniques. In this paper, we lay the foundation of the study. We derive the recipe for the control-time calculation for SNe with a known luminosity function and provide details on the construction of the galaxy and SN samples used in the calculations. Compared with a complete volume-limited galaxy sample, our sample has a deficit of low-luminosity galaxies but still provides enough statistics for a reliable rate calculation. There is a strong Malmquist bias, so the average size (luminosity or mass) of the galaxies increases monotonically with distance, and this trend is used to showcase a correlation between SN rates and galaxy sizes. Very few core-collapse SNe are found in early-type galaxies, providing strong constraints on the amount of recent star formation within these galaxies. The small average observation interval (similar to 9 d) of our survey ensures that our control-time calculations can tolerate a reasonable amount of uncertainty in the luminosity functions of SNe. We perform Monte Carlo simulations to determine the limiting magnitude of each image and the SN detection efficiency as a function of galaxy Hubble type. The limiting magnitude and the detection efficiency, together with the luminosity function derived from a complete sample of very nearby SNe in Paper II, will be used to calculate the control time and the SN rates in Paper III. C1 [Leaman, Jesse; Li, Weidong; Chornock, Ryan; Filippenko, Alexei V.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Leaman, Jesse] NASA, Ames Res Ctr, Mountain View, CA 94043 USA. [Chornock, Ryan] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Leaman, J (reprint author), Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA. EM jleaman@astro.berkeley.edu; wli@astro.berkeley.edu; rchornock@cfa.harvard.edu; alex@astro.berkeley.edu FU US National Science Foundation (NSF) [AST-0607485, AST-0908886]; TABASGO Foundation; US Department of Energy [DE-FC02-06ER41453, DE-FG02-08ER41563]; Sun Microsystems, Inc.; Hewlett-Packard Company; AutoScope Corporation; Lick Observatory; NSF; University of California; Sylvia & Jim Katzman Foundation; Richard and Rhoda Goldman Fund; NASA FX The LOSS, conducted by AVF's group, has been supported by many grants from the US National Science Foundation (NSF; most recently AST-0607485 and AST-0908886), the TABASGO Foundation, US Department of Energy SciDAC grant DE-FC02-06ER41453 and US Department of Energy grant DE-FG02-08ER41563. The KAIT and its ongoing operation were made possible by donations from Sun Microsystems, Inc., the Hewlett-Packard Company, AutoScope Corporation, Lick Observatory, the NSF, the University of California, the Sylvia & Jim Katzman Foundation, the Richard and Rhoda Goldman Fund and the TABASGO Foundation. We particularly thank Russell M. Genet, who made the KAIT possible with his initial special gift; former Lick Director Joseph S. Miller, who allowed the KAIT to be placed at the Lick Observatory and provided staff support; and the TABASGO Foundation, without which this work would not have been completed. JL is grateful for a fellowship from the NASA Postdoctoral Program. We made use of the NED, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA. We acknowledge the use of the HyperLeda data base (http://leda.univ-lyon1. fr). NR 123 TC 72 Z9 72 U1 0 U2 1 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD APR PY 2011 VL 412 IS 3 BP 1419 EP 1440 DI 10.1111/j.1365-2966.2011.18158.x PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 745IM UT WOS:000289159100002 ER PT J AU Li, WD Leaman, J Chornock, R Filippenko, AV Poznanski, D Ganeshalingam, M Wang, XF Modjaz, M Jha, S Foley, RJ Smith, N AF Li, Weidong Leaman, Jesse Chornock, Ryan Filippenko, Alexei V. Poznanski, Dovi Ganeshalingam, Mohan Wang, Xiaofeng Modjaz, Maryam Jha, Saurabh Foley, Ryan J. Smith, Nathan TI Nearby supernova rates from the Lick Observatory Supernova Search - II. The observed luminosity functions and fractions of supernovae in a complete sample SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Review DE supernovae: general ID CORE-COLLAPSE SUPERNOVAE; GAMMA-RAY BURST; IA SUPERNOVAE; LIGHT CURVES; HOST GALAXIES; INFRARED OBSERVATIONS; RELATIVE FREQUENCIES; PHYSICAL-PROPERTIES; UBVRI PHOTOMETRY; SHOCK BREAKOUT AB This is the second paper of a series in which we present new measurements of the observed rates of supernovae (SNe) in the local Universe, determined from the Lick Observatory Supernova Search (LOSS). In this paper, a complete SN sample is constructed, and the observed (uncorrected for host-galaxy extinction) luminosity functions (LFs) of SNe are derived. These LFs solve two issues that have plagued previous rate calculations for nearby SNe: the luminosity distribution of SNe and the host-galaxy extinction. We select a volume-limited sample of 175 SNe, collect photometry for every object and fit a family of light curves to constrain the peak magnitudes and light-curve shapes. The volume-limited LFs show that they are not well represented by a Gaussian distribution. There are notable differences in the LFs for galaxies of different Hubble types (especially for SNe Ia). We derive the observed fractions for the different subclasses in a complete SN sample, and find significant fractions of SNe II-L (10 per cent), IIb (12 per cent) and IIn (9 per cent) in the SN II sample. Furthermore, we derive the LFs and the observed fractions of different SN subclasses in a magnitude-limited survey with different observation intervals, and find that the LFs are enhanced at the high-luminosity end and appear more 'standard' with smaller scatter, and that the LFs and fractions of SNe do not change significantly when the observation interval is shorter than 10 d. We also discuss the LFs in different galaxy sizes and inclinations, and for different SN subclasses. Some notable results are that there is not a strong correlation between the SN LFs and the host-galaxy size, but there might be a preference for SNe IIn to occur in small, late-type spiral galaxies. The LFs in different inclination bins do not provide strong evidence for extreme extinction in highly inclined galaxies, though the sample is still small. The LFs of different SN subclasses show significant differences. We also find that SNe Ibc and IIb come from more luminous galaxies than SNe II-P, while SNe IIn come from less luminous galaxies, suggesting a possible metallicity effect. The limitations and applications of our LFs are also discussed. C1 [Li, Weidong; Leaman, Jesse; Chornock, Ryan; Filippenko, Alexei V.; Poznanski, Dovi; Ganeshalingam, Mohan; Wang, Xiaofeng; Modjaz, Maryam; Jha, Saurabh; Foley, Ryan J.; Smith, Nathan] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Leaman, Jesse] NASA, Ames Res Ctr, Mountain View, CA 94043 USA. [Chornock, Ryan; Foley, Ryan J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Poznanski, Dovi] Univ Calif Berkeley, Lawrence Berkeley Lab, Computat Cosmol Ctr, Berkeley, CA 94720 USA. [Wang, Xiaofeng] Texas A&M Univ, Dept Phys, College Stn, TX 77843 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. [Modjaz, Maryam] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Jha, Saurabh] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. [Smith, Nathan] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. RP Li, WD (reprint author), Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA. EM wli@astro.berkeley.edu RI Wang, Xiaofeng/J-5390-2015 FU US National Science Foundation (NSF) [AST-0607485, AST-0908886]; TABASGO Foundation; US Department of Energy [DE-FC02-06ER41453, DE-FG02-08ER41563]; Sun Microsystems, Inc.; Hewlett-Packard Company; AutoScope Corporation; Lick Observatory; NSF [AST-0205808, AST-0606772]; University of California; Sylvia & Jim Katzman Foundation; Richard and Rhoda Goldman Fund; NASA; Einstein Fellowship; NSFC [10673007, 11073013]; China-973 Program [2009CB824800]; Miller Institute for Basic Research in Science (UC Berkeley) FX We thank the referee, Enrico Cappellaro, for useful comments and suggestions which improved the paper. We are grateful to the many students, postdocs and other collaborators who have contributed to the Katzman Automatic Imaging Telescope and the Lick Observatory Supernova Search over the past two decades, and to discussions concerning the determination of supernova rates - especially Jack Borde, Frank Serduke, Jeffrey Silverman, Thea Steele and Richard R. Treffers. We thank the Lick Observatory staff for their assistance with the operation of KAIT. LOSS, conducted by AVF's group, has been supported by many grants from the US National Science Foundation (NSF; most recently AST-0607485 and AST-0908886), the TABASGO Foundation, US Department of Energy SciDAC grant DE-FC02-06ER41453 and US Department of Energy grant DE-FG02-08ER41563. KAIT and its ongoing operation were made possible by donations from Sun Microsystems, Inc., the Hewlett-Packard Company, AutoScope Corporation, Lick Observatory, the NSF, the University of California, the Sylvia & Jim Katzman Foundation, the Richard and Rhoda Goldman Fund and the TABASGO Foundation. We give particular thanks to Russell M. Genet, who made KAIT possible with his initial special gift; former Lick Director Joseph S. Miller, who allowed KAIT to be placed at Lick Observatory and provided staff support; and the TABASGO Foundation, without which this work would not have been completed. JL is grateful for a fellowship from the NASA Postdoctoral Program. DP is supported by an Einstein Fellowship. XW acknowledges NSFC grants (10673007, 11073013) and the China-973 Program 2009CB824800. MM acknowledges NSF grants AST-0205808 and AST-0606772, as well as the Miller Institute for Basic Research in Science (UC Berkeley), for support during the time over which part of this work was conducted. We made use of the NASA/IPAC Extragalactic Data base (NED), which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA. We acknowledge use of the HyperLeda data base (http://leda.univ-lyon1.fr). NR 133 TC 277 Z9 279 U1 0 U2 5 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD APR PY 2011 VL 412 IS 3 BP 1441 EP 1472 DI 10.1111/j.1365-2966.2011.18160.x PG 32 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 745IM UT WOS:000289159100003 ER PT J AU Li, WD Chornock, R Leaman, J Filippenko, AV Poznanski, D Wang, XF Ganeshalingam, M Mannucci, F AF Li, Weidong Chornock, Ryan Leaman, Jesse Filippenko, Alexei V. Poznanski, Dovi Wang, Xiaofeng Ganeshalingam, Mohan Mannucci, Filippo TI Nearby supernova rates from the Lick Observatory Supernova Search - III. The rate-size relation, and the rates as a function of galaxy Hubble type and colour SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE supernovae: general ID CORE-COLLAPSE SUPERNOVAE; AEGIS FIELD GALAXIES; IA SUPERNOVAE; STAR-FORMATION; MASSIVE STARS; LEGACY SURVEY; HIGH-REDSHIFT; PROGENITORS; POPULATIONS; LUMINOSITY AB This is the third paper of a series in which we present new measurements of the observed rates of supernovae (SNe) in the local Universe, determined from the Lick Observatory Supernova Search (LOSS). We have considered a sample of similar to 1000 SNe and used an optimal subsample of 726 SNe (274 SNe Ia, 116 SNe Ibc and 324 SNe II) to determine our rates. We study the trend of the rates as a function of a few quantities available for our galaxy sample, such as luminosity in the B and K bands, stellar mass and morphological class. We discuss different choices (SN samples, input SN luminosity functions, inclination correction factors) and their effect on the rates and their uncertainties. A comparison between our SN rates and the published measurements shows that they are consistent with each other to within the uncertainties when the rate calculations are done in the same manner. Nevertheless, our data demonstrate that the rates cannot be adequately described by a single parameter using either galaxy Hubble types or B - K colours. A secondary parameter in galaxy 'size', expressed by luminosity or stellar mass, is needed to adequately describe the rates in the rate-size relation: the galaxies of smaller sizes have higher SN rates per unit mass or per unit luminosity. The trends of the SN rates in galaxies of different Hubble types and colours are discussed. We examine possible causes for the rate-size relation. Physically, such a relation for the core-collapse SNe is probably linked to the correlation between the specific star-formation rate and the galaxy sizes, but it is not clear whether the same link can be established for SNe Ia. We discuss the two-component ('tardy' and 'prompt') model for SN Ia rates, and find that the SN Ia rates in young stellar populations might have a strong correlation with the core-collapse SN rates. We derive volumetric rates for the different SN types [e.g. for SNe Ia, a rate of (0.301 +/- 0.062) x 10-4 SN Mpc-3 yr-1 at redshift 0] and compare them to the measurements at different redshifts. Finally, we estimate the SN rate for the Milky Way Galaxy to be 2.84 +/- 0.60 SNe per century (with a systematic uncertainty of a factor of similar to 2), consistent with published SN rates based on several different techniques. C1 [Li, Weidong; Chornock, Ryan; Leaman, Jesse; Filippenko, Alexei V.; Poznanski, Dovi; Wang, Xiaofeng; Ganeshalingam, Mohan] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Chornock, Ryan] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Leaman, Jesse] NASA, Ames Res Ctr, Mountain View, CA 94043 USA. [Poznanski, Dovi] Univ Calif Berkeley, Lawrence Berkeley Lab, Computat Cosmol Ctr, Berkeley, CA 94720 USA. [Wang, Xiaofeng] Texas A&M Univ, Dept Phys, College Stn, TX 77843 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. [Mannucci, Filippo] INAF Osservatorio Astrofis Arcetri, I-50125 Florence, Italy. RP Li, WD (reprint author), Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA. EM wli@astro.berkeley.edu RI Wang, Xiaofeng/J-5390-2015; OI mannucci, filippo/0000-0002-4803-2381 FU US National Science Foundation (NSF) [AST-0607485, AST-0908886]; TABASGO Foundation; US Department of Energy [DE-FC02-06ER41453, DE-FG02-08ER41563]; Sun Microsystems, Inc.; Hewlett-Packard Company; AutoScope Corporation; Lick Observatory; NSF; University of California; Sylvia & Jim Katzman Foundation; Richard and Rhoda Goldman Fund; NASA; Einstein Fellowship; NSFC [10673007, 11073013]; China-973 Program [2009CB824800] FX The LOSS, conducted by AVF's group, has been supported by many grants from the US National Science Foundation (NSF; most recently AST-0607485 and AST-0908886), the TABASGO Foundation, US Department of Energy SciDAC grant DE-FC02-06ER41453 and US Department of Energy grant DE-FG02-08ER41563. The KAIT and its ongoing operation were made possible by donations from Sun Microsystems, Inc., the Hewlett-Packard Company, AutoScope Corporation, Lick Observatory, the NSF, the University of California, the Sylvia & Jim Katzman Foundation, the Richard and Rhoda Goldman Fund and the TABASGO Foundation. We give particular thanks to Russell M. Genet, who made the KAIT possible with his initial special gift; former Lick Director Joseph S. Miller, who allowed the KAIT to be placed at Lick Observatory and provided staff support; and the TABASGO Foundation, without which this work would not have been completed. JL is grateful for a fellowship from the NASA Postdoctoral Program. DP is supported by an Einstein Fellowship. XW acknowledges NSFC grants (10673007, 11073013) and the China-973 Program 2009CB824800. We made use of the NASA/IPAC Extragalactic Data base (NED), which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA. We acknowledge use of the HyperLeda data base (http://leda.univlyon1.fr). NR 58 TC 199 Z9 202 U1 1 U2 9 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD APR PY 2011 VL 412 IS 3 BP 1473 EP 1507 DI 10.1111/j.1365-2966.2011.18162.x PG 35 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 745IM UT WOS:000289159100004 ER PT J AU Starling, RLC Evans, PA Read, AM Saxton, RD Esquej, P Krimm, H O'Brien, PT Osborne, JP Mateos, S Warwick, R Wiersema, K AF Starling, R. L. C. Evans, P. A. Read, A. M. Saxton, R. D. Esquej, P. Krimm, H. O'Brien, P. T. Osborne, J. P. Mateos, S. Warwick, R. Wiersema, K. TI Swift follow-up of unidentified X-ray sources in the XMM-Newton Slew Survey SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE surveys; X-rays: general ID NORTH ECLIPTIC POLE; CHANDRA DEEP SURVEY; SKY SURVEY; ULTRAVIOLET/OPTICAL TELESCOPE; SPECTRAL PROPERTIES; SOURCE CATALOG; FIELD; BAT; CALIBRATION; MISSION AB We present deep Swift follow-up observations of a sample of 94 unidentified X-ray sources from the XMM-Newton Slew Survey. The X-ray Telescope (XRT) on-board Swift detected 29 per cent of the sample sources; the flux limits for undetected sources suggest the bulk of the Slew Survey sources are drawn from one or more transient populations. We report revised X-ray positions for the XRT-detected sources, with typical uncertainties of 2.9 arcsec, reducing the number of catalogued optical matches to just a single source in most cases. We characterize the sources detected by Swift through their X-ray spectra and variability and via Ultraviolet-Optical Telescope photometry and using catalogued near-infrared, optical and radio observations of potential counterparts. Six sources can be associated with known objects and eight sources may be associated with unidentified ROSAT sources within the 3 Sigma error radii of our revised X-ray positions. We find 10 of the 30 XRT- and/or Burst Alert Telescope (BAT)-detected sources are clearly stellar in nature, including one periodic variable star and two high proper motion stars. For 11 sources we propose an active galactic nucleus (AGN) classification, among which four are detected in hard X-rays and three have redshifts spanning z = 0.2-0.9 obtained from the literature or from optical spectroscopy presented here. A further three sources are suspected AGN and one is a candidate Galactic hard X-ray flash, while five sources remain unclassified. The 67 Slew Survey sources we do not detect with Swift XRT or BAT are studied via their characteristics in the Slew Survey observations and by comparison with the XRT- and BAT-detected population. We suggest that these are mostly if not all extragalactic, though unlikely to be highly absorbed sources in the X-rays such as Compton thick AGN. A large number of these are highly variable soft X-ray (0.2-2 keV) sources and a smaller number are highly variable hard (2-12 keV) sources. A small fraction of mainly hard-band Slew Survey detections may be spurious. This follow-up programme brings us a step further to completing the identifications of a substantial sample of XMM-Newton Slew Survey sources, important for understanding the nature of the transient sky and allowing flux-limited samples to be constructed. C1 [Starling, R. L. C.; Evans, P. A.; Read, A. M.; Esquej, P.; O'Brien, P. T.; Osborne, J. P.; Mateos, S.; Warwick, R.; Wiersema, K.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Saxton, R. D.] ESAC, XMM Newton SOC, Madrid 28691, Spain. [Krimm, H.] Univ Space Res Assoc, Columbia, MD 20144 USA. [Krimm, H.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Starling, RLC (reprint author), Univ Leicester, Dept Phys & Astron, Univ Rd, Leicester LE1 7RH, Leics, England. EM rlcs1@star.le.ac.uk RI Mateos, Silvia/F-9524-2016 OI Mateos, Silvia/0000-0002-1375-2389 FU STFC; National Aeronautics and Space Administration; National Science Foundation FX RLCS, PAE, AMR, PE and JPO acknowledge financial support from STFC. We thank the Swift team for performing these observations. We acknowledge useful discussions with S. Farrell and M. Goad and the anonymous referee for a constructive critique. This work made use of data supplied by the UK Swift Science Data Centre at the University of Leicester. This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. Based on observations obtained at the ESO NTT telescope (programme 084.A-0828). NR 58 TC 5 Z9 5 U1 0 U2 0 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD APR PY 2011 VL 412 IS 3 BP 1853 EP 1869 DI 10.1111/j.1365-2966.2010.18024.x PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 745IM UT WOS:000289159100034 ER PT J AU Zdziarski, AA Pooley, GG Skinner, GK AF Zdziarski, Andrzej A. Pooley, Guy G. Skinner, Gerald K. TI The doubling of the superorbital period of Cyg X-1 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion, accretion discs; stars: individual: Cyg X-1; stars: individual: HDE 226868; radio continuum: stars; X-rays: binaries; X-rays: stars ID ALL-SKY MONITOR; WARPED ACCRETION DISCS; RAY TIMING EXPLORER; HDE 226868/CYG X-1; X-RAY; ORBITAL MODULATION; RADIO-EMISSION; TERM VARIABILITY; SPACED DATA; CYG-X-1 AB We study properties of the superorbital modulation of the X-ray emission of Cyg X-1. We find that it has had a stable period of similar to 300 d in soft and hard X-rays and in radio since 2005 until at least 2010, which is about double the previously seen period. This new period, seen in the hard spectral state only, is detected not only in the light curves but also in soft X-ray hardness ratios and in the amplitude of the orbital modulation. On the other hand, the spectral slope in hard X-rays, greater than or similar to 20 keV, averaged over superorbital bins is constant, and the soft and hard X-rays and the radio emission change in phase. This shows that the superorbital variability consists of changing the normalization of an intrinsic spectrum of a constant shape and of changes of the absorbing column density with the phase. The maximum column density is achieved at the superorbital minimum. The amplitude changes are likely to be caused by a changing viewing angle of an anisotropic emitter, most likely a precessing accretion disc. The constant shape of the intrinsic spectrum shows that this modulation is not caused by a changing accretion rate. The modulated absorbing column density shows the presence of a bulge at the disc edge, as proposed previously. We also find the change of the superorbital period from similar to 150 to similar to 300 d to be associated with almost unchanged average X-ray fluxes, making the period change difficult to explain in the framework of disc-irradiation models. Finally, we find no correlation of the X-ray and radio properties with the reported detections in the GeV and TeV gamma-ray range. C1 [Zdziarski, Andrzej A.] Ctr Astron M Kopernika, PL-00716 Warsaw, Poland. [Pooley, Guy G.] Univ Cambridge, Cavendish Lab, Cambridge CB3 0HE, England. [Skinner, Gerald K.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Skinner, Gerald K.] CRESST, Astroparticle Phys Lab, Greenbelt, MD 20771 USA. [Skinner, Gerald K.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. RP Zdziarski, AA (reprint author), Ctr Astron M Kopernika, Bartycka 18, PL-00716 Warsaw, Poland. EM aaz@camk.edu.pl FU Polish MNiSW [NN203065933, 362/1/N-INTEGRAL/2008/09/0]; STFC FX We thank A. Ogorzalek and L. Wen for help with calculating the rescaled periodograms, H. Krimm and P. Lubinski for help with the BAT data, G. Dubus for discussion of radiation induced precession and the referee for valuable suggestions. This research has been supported in part by the Polish MNiSW grants NN203065933 and 362/1/N-INTEGRAL/2008/09/0. The AMI Arrays are operated by the University of Cambridge and supported by the STFC. We acknowledge the use of data obtained through the HEASARC online service provided by NASA/GSFC. NR 53 TC 11 Z9 11 U1 0 U2 0 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD APR PY 2011 VL 412 IS 3 BP 1985 EP 1992 DI 10.1111/j.1365-2966.2010.18034.x PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 745IM UT WOS:000289159100044 ER PT J AU Brown, ME Osgood, DE Carriquiry, MA AF Brown, Molly E. Osgood, Daniel E. Carriquiry, Miguel A. TI Science-based insurance SO NATURE GEOSCIENCE LA English DT Editorial Material C1 [Brown, Molly E.] NASA, Goddard Space Flight Ctr, Biospher Sci Branch, Greenbelt, MD 20771 USA. [Osgood, Daniel E.] Columbia Univ, Int Climate Res Inst Climate & Soc, Palisades, NY 10964 USA. [Carriquiry, Miguel A.] Iowa State Univ, Ames, IA 50011 USA. RP Brown, ME (reprint author), NASA, Goddard Space Flight Ctr, Biospher Sci Branch, Code 614-4, Greenbelt, MD 20771 USA. EM molly.brown@nasa.gov RI Brown, Molly/M-5146-2013; Brown, Molly/E-2724-2010 OI Brown, Molly/0000-0001-7384-3314; Brown, Molly/0000-0001-7384-3314 NR 7 TC 10 Z9 10 U1 1 U2 10 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 APR PY 2011 VL 4 IS 4 BP 213 EP 214 DI 10.1038/ngeo1117 PG 2 WC Geosciences, Multidisciplinary SC Geology GA 744AL UT WOS:000289063900006 ER PT J AU Cuzzi, J AF Cuzzi, Jeff TI EARLY SOLAR SYSTEM Gathering dust SO NATURE GEOSCIENCE LA English DT News Item ID CHONDRULES; ACCRETION C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Cuzzi, J (reprint author), NASA, Ames Res Ctr, Mail Stop 245-3, Moffett Field, CA 94035 USA. EM Jeffrey.Cuzzi@nasa.gov NR 6 TC 0 Z9 0 U1 1 U2 2 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 APR PY 2011 VL 4 IS 4 BP 219 EP 220 DI 10.1038/ngeo1112 PG 2 WC Geosciences, Multidisciplinary SC Geology GA 744AL UT WOS:000289063900009 ER PT J AU Alim, MA Batra, AK Aggarwal, MD Currie, JR AF Alim, Mohammad A. Batra, A. K. Aggarwal, M. D. Currie, James R. TI Immittance response of the SnO2-Bi2O3 based thick-films SO PHYSICA B-CONDENSED MATTER LA English DT Article DE Tin oxide; Binary oxides; Bismuth oxide; Impedance; Immittance ID POLYCRYSTALLINE SOLID ELECTROLYTES; ZINC-OXIDE; SENSING PROPERTIES; GRAIN-BOUNDARIES; VARISTORS; IMPEDANCE; BEHAVIOR; MICROSTRUCTURE; CONDUCTIVITY; SPECTROSCOPY AB The SnO2-Bi2O3 based thick-film polycrystalline material is fabricated on alumina substrate via screen-printing technique. This material system is evaluated at various temperatures (35 degrees C <= T <= 100 degrees C) using ac small-signal (immittance) measurements in the frequency range 10 Hz <= f <= 10(6) Hz. The simplistic analytical scenario for the immittance data employed the Cole-Cole empirical equation in conjunction with the estimation of the inspected input parameters. This is an alternate approach compared to the complex nonlinear least squares (CNLS) fitting procedure, and purely based on the appearance of the semicircular relaxation in the complex plane. It is found that the constituting components of the semicircular relaxation in the impedance plane are thermally activated indicating complexity in the grain boundary contributions despite the Debye and non-Debye relaxation responses. The possible degree of uniformity or non-uniformity in the grain boundary activity associated with its capacitance term observed via the Debye or non-Debye semicircular relaxation in the impedance (Z*) plane has been postulated. (C) 2011 Elsevier B.V. All rights reserved. C1 [Alim, Mohammad A.] Alabama A&M Univ, Dept Elect Engn, Huntsville, AL 35762 USA. [Batra, A. K.; Aggarwal, M. D.] Alabama A&M Univ, Dept Phys, Normal, AL 35762 USA. [Currie, James R.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. RP Alim, MA (reprint author), Alabama A&M Univ, Dept Elect Engn, POB 297, Huntsville, AL 35762 USA. EM mohammad.alim@aamu.edu FU NSF RISE [0927644] FX The authors gratefully acknowledge the support of the present work through NSF RISE grant no. 0927644. Thanks to Mr. G. Sharp for fabrication of the sample holder and heater assembly. NR 40 TC 1 Z9 1 U1 1 U2 17 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0921-4526 J9 PHYSICA B JI Physica B PD APR 1 PY 2011 VL 406 IS 8 BP 1445 EP 1452 DI 10.1016/j.physb.2011.01.046 PG 8 WC Physics, Condensed Matter SC Physics GA 743ZL UT WOS:000289060100018 ER PT J AU Aihara, H Prieto, CA An, D Anderson, SF Aubourg, E Balbinot, E Beers, TC Berlind, AA Bickerton, SJ Bizyaev, D Blanton, MR Bochanski, JJ Bolton, AS Bovy, J Brandt, WN Brinkmann, J Brown, PJ Brownstein, JR Busca, NG Campbell, H Carr, MA Chen, YM Chiappini, C Comparat, J Connolly, N Cortes, M Croft, RAC Cuesta, AJ da Costa, LN Davenport, JRA Dawson, K Dhital, S Ealet, A Ebelke, GL Edmondson, EM Eisenstein, DJ Escoffier, S Esposito, M Evans, ML Fan, XH Castella, BF Font-Ribera, A Frinchaboy, PM Ge, JA Gillespie, BA Gilmore, G Hernandez, JIG Gott, JR Gould, A Grebel, EK Gunn, JE Hamilton, JC Harding, P Harris, DW Hawley, SL Hearty, FR Ho, S Hogg, DW Holtzman, JA Honscheid, K Inada, N Ivans, II Jiang, LH Johnson, JA Jordan, C Jordan, WP Kazin, EA Kirkby, D Klaene, MA Knapp, GR Kneib, JP Kochanek, CS Koesterke, L Kollmeier, JA Kron, RG Lampeitl, H Lang, D Le Goff, JM Lee, YS Lin, YT Long, DC Loomis, CP Lucatello, S Lundgren, B Lupton, RH Ma, ZB MacDonald, N Mahadevan, S Maia, MAG Makler, M Malanushenko, E Malanushenko, V Mandelbaum, R Maraston, C Margala, D Masters, KL McBride, CK McGehee, PM McGreer, ID Menard, B Miralda-Escude, J Morrison, HL Mullally, F Muna, D Munn, JA Murayama, H Myers, AD Naugle, T Neto, AF Nguyen, DC Nichol, RC O'Connell, RW Ogando, RLC Olmstead, MD Oravetz, DJ Padmanabhan, N Palanque-Delabrouille, N Pan, K Pandey, P Paris, I Percival, WJ Petitjean, P Pfaffenberger, R Pforr, J Phleps, S Pichon, C Pieri, MM Prada, F Price-Whelan, AM Raddick, MJ Ramos, BHF Reyle, C Rich, J Richards, GT Rix, HW Robin, AC Rocha-Pinto, HJ Rockosi, CM Roe, NA Rollinde, E Ross, AJ Ross, NP Rossetto, BM Sanchez, AG Sayres, C Schlegel, DJ Schlesinger, KJ Schmidt, SJ Schneider, DP Sheldon, E Shu, YP Simmerer, J Simmons, AE Sivarani, T Snedden, SA Sobeck, JS Steinmetz, M Strauss, MA Szalay, AS Tanaka, M Thakar, AR Thomas, D Tinker, JL Tofflemire, BM Tojeiro, R Tremonti, CA Vandenberg, J Magana, MV Verde, L Vogt, NP Wake, DA Wang, J Weaver, BA Weinberg, DH White, M White, SDM Yanny, B Yasuda, N Yeche, C Zehavi, I AF Aihara, Hiroaki Allende Prieto, Carlos An, Deokkeun Anderson, Scott F. Aubourg, Eric Balbinot, Eduardo Beers, Timothy C. Berlind, Andreas A. Bickerton, Steven J. Bizyaev, Dmitry Blanton, Michael R. Bochanski, John J. Bolton, Adam S. Bovy, Jo Brandt, W. N. Brinkmann, J. Brown, Peter J. Brownstein, Joel R. Busca, Nicolas G. Campbell, Heather Carr, Michael A. Chen, Yanmei Chiappini, Cristina Comparat, Johan Connolly, Natalia Cortes, Marina Croft, Rupert A. C. Cuesta, Antonio J. da Costa, Luiz N. Davenport, James R. A. Dawson, Kyle Dhital, Saurav Ealet, Anne Ebelke, Garrett L. Edmondson, Edward M. Eisenstein, Daniel J. Escoffier, Stephanie Esposito, Massimiliano Evans, Michael L. Fan, Xiaohui Femenia Castella, Bruno Font-Ribera, Andreu Frinchaboy, Peter M. Ge, Jian Gillespie, Bruce A. Gilmore, G. Gonzalez Hernandez, Jonay I. Gott, J. Richard Gould, Andrew Grebel, Eva K. Gunn, James E. Hamilton, Jean-Christophe Harding, Paul Harris, David W. Hawley, Suzanne L. Hearty, Frederick R. Ho, Shirley Hogg, David W. Holtzman, Jon A. Honscheid, Klaus Inada, Naohisa Ivans, Inese I. Jiang, Linhua Johnson, Jennifer A. Jordan, Cathy Jordan, Wendell P. Kazin, Eyal A. Kirkby, David Klaene, Mark A. Knapp, G. R. Kneib, Jean-Paul Kochanek, C. S. Koesterke, Lars Kollmeier, Juna A. Kron, Richard G. Lampeitl, Hubert Lang, Dustin Le Goff, Jean-Marc Lee, Young Sun Lin, Yen-Ting Long, Daniel C. Loomis, Craig P. Lucatello, Sara Lundgren, Britt Lupton, Robert H. Ma, Zhibo MacDonald, Nicholas Mahadevan, Suvrath Maia, Marcio A. G. Makler, Martin Malanushenko, Elena Malanushenko, Viktor Mandelbaum, Rachel Maraston, Claudia Margala, Daniel Masters, Karen L. McBride, Cameron K. McGehee, Peregrine M. McGreer, Ian D. Menard, Brice Miralda-Escude, Jordi Morrison, Heather L. Mullally, F. Muna, Demitri Munn, Jeffrey A. Murayama, Hitoshi Myers, Adam D. Naugle, Tracy Neto, Angelo Fausti Duy Cuong Nguyen Nichol, Robert C. O'Connell, Robert W. Ogando, Ricardo L. C. Olmstead, Matthew D. Oravetz, Daniel J. Padmanabhan, Nikhil Palanque-Delabrouille, Nathalie Pan, Kaike Pandey, Parul Paris, Isabelle Percival, Will J. Petitjean, Patrick Pfaffenberger, Robert Pforr, Janine Phleps, Stefanie Pichon, Christophe Pieri, Matthew M. Prada, Francisco Price-Whelan, Adrian M. Raddick, M. Jordan Ramos, Beatriz H. F. Reyle, Celine Rich, James Richards, Gordon T. Rix, Hans-Walter Robin, Annie C. Rocha-Pinto, Helio J. Rockosi, Constance M. Roe, Natalie A. Rollinde, Emmanuel Ross, Ashley J. Ross, Nicholas P. Rossetto, Bruno M. Sanchez, Ariel G. Sayres, Conor Schlegel, David J. Schlesinger, Katharine J. Schmidt, Sarah J. Schneider, Donald P. Sheldon, Erin Shu, Yiping Simmerer, Jennifer Simmons, Audrey E. Sivarani, Thirupathi Snedden, Stephanie A. Sobeck, Jennifer S. Steinmetz, Matthias Strauss, Michael A. Szalay, Alexander S. Tanaka, Masayuki Thakar, Aniruddha R. Thomas, Daniel Tinker, Jeremy L. Tofflemire, Benjamin M. Tojeiro, Rita Tremonti, Christy A. Vandenberg, Jan Magana, M. Vargas Verde, Licia Vogt, Nicole P. Wake, David A. Wang, Ji Weaver, Benjamin A. Weinberg, David H. White, Martin White, Simon D. M. Yanny, Brian Yasuda, Naoki Yeche, Christophe Zehavi, Idit TI THE EIGHTH DATA RELEASE OF THE SLOAN DIGITAL SKY SURVEY: FIRST DATA FROM SDSS-III SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE atlases; catalogs; surveys ID SPECTROSCOPIC TARGET SELECTION; STAR-FORMING GALAXIES; 7TH DATA RELEASE; OPEN CLUSTERS; WHITE-DWARFS; USNO-B; SEGUE; RESOLUTION; TELESCOPE; CATALOG AB The Sloan Digital Sky Survey (SDSS) started a new phase in 2008 August, with new instrumentation and new surveys focused on Galactic structure and chemical evolution, measurements of the baryon oscillation feature in the clustering of galaxies and the quasar Ly alpha forest, and a radial velocity search for planets around similar to 8000 stars. This paper describes the first data release of SDSS-III (and the eighth counting from the beginning of the SDSS). The release includes five-band imaging of roughly 5200 deg(2) in the southern Galactic cap, bringing the total footprint of the SDSS imaging to 14,555 deg(2), or over a third of the Celestial Sphere. All the imaging data have been reprocessed with an improved sky-subtraction algorithm and a final, self-consistent photometric recalibration and flat-field determination. This release also includes all data from the second phase of the Sloan Extension for Galactic Understanding and Exploration (SEGUE-2), consisting of spectroscopy of approximately 118,000 stars at both high and low Galactic latitudes. All the more than half a million stellar spectra obtained with the SDSS spectrograph have been reprocessed through an improved stellar parameter pipeline, which has better determination of metallicity for high-metallicity stars. C1 [Bickerton, Steven J.; Carr, Michael A.; Gott, J. Richard; Gunn, James E.; Knapp, G. R.; Lang, Dustin; Loomis, Craig P.; Lupton, Robert H.; Mandelbaum, Rachel; Mullally, F.; Strauss, Michael A.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Aihara, Hiroaki; Lin, Yen-Ting; Menard, Brice; Murayama, Hitoshi; Tanaka, Masayuki; Yasuda, Naoki] Univ Tokyo, Inst Phys & Math Universe, Kashiwa, Chiba 2778583, Japan. [Allende Prieto, Carlos; Esposito, Massimiliano; Femenia Castella, Bruno; Gonzalez Hernandez, Jonay I.] Inst Astrofis Canarias, E-38205 Tenerife, Spain. [Allende Prieto, Carlos; Esposito, Massimiliano; Femenia Castella, Bruno] Univ La Laguna, Dept Astrofis, E-38206 Tenerife, Spain. [An, Deokkeun] Ewha Womans Univ, Dept Sci Educ, Seoul 120750, South Korea. [Anderson, Scott F.; Davenport, James R. A.; Evans, Michael L.; Hawley, Suzanne L.; Sayres, Conor; Schmidt, Sarah J.; Tofflemire, Benjamin M.] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Aubourg, Eric; Hamilton, Jean-Christophe; Magana, M. Vargas] Univ Paris Diderot, Astroparticule & Cosmol APC, F-75205 Paris 13, France. [Aubourg, Eric; Le Goff, Jean-Marc; Palanque-Delabrouille, Nathalie; Rich, James; Yeche, Christophe] CEA, Ctr Saclay, Irfu SPP, F-91191 Gif Sur Yvette, France. [Balbinot, Eduardo; Neto, Angelo Fausti] Univ Fed Rio Grande do Sul, Inst Fis, BR-91501970 Porto Alegre, RS, Brazil. [Balbinot, Eduardo; Chiappini, Cristina; da Costa, Luiz N.; Maia, Marcio A. G.; Makler, Martin; Neto, Angelo Fausti; Ogando, Ricardo L. C.; Ramos, Beatriz H. F.; Rocha-Pinto, Helio J.; Rossetto, Bruno M.] Lab Interinst E Astron LIneA, BR-20921400 Rio De Janeiro, Brazil. [Beers, Timothy C.; Lee, Young Sun] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. [Beers, Timothy C.; Lee, Young Sun] Michigan State Univ, Joint Inst Nucl Astrophys, E Lansing, MI 48824 USA. [Berlind, Andreas A.; Dhital, Saurav; McBride, Cameron K.] Vanderbilt Univ, Dept Phys & Astron, Nashville, TN 37235 USA. [Bizyaev, Dmitry; Brinkmann, J.; Ebelke, Garrett L.; Gillespie, Bruce A.; Jordan, Cathy; Jordan, Wendell P.; Klaene, Mark A.; Long, Daniel C.; Malanushenko, Elena; Malanushenko, Viktor; Naugle, Tracy; Oravetz, Daniel J.; Pan, Kaike; Simmons, Audrey E.; Snedden, Stephanie A.] Apache Point Observ, Sunspot, NM 88349 USA. [Blanton, Michael R.; Bovy, Jo; Hogg, David W.; Kazin, Eyal A.; Muna, Demitri; Price-Whelan, Adrian M.; Tinker, Jeremy L.; Weaver, Benjamin A.] NYU, Ctr Cosmol & Particle Phys, New York, NY 10003 USA. [Bochanski, John J.; Brandt, W. N.; Mahadevan, Suvrath; Schneider, Donald P.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA. [Bolton, Adam S.; Brown, Peter J.; Brownstein, Joel R.; Dawson, Kyle; Harris, David W.; Ivans, Inese I.; Olmstead, Matthew D.; Pandey, Parul; Shu, Yiping; Simmerer, Jennifer] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA. [Brandt, W. N.] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA. [Campbell, Heather; Edmondson, Edward M.; Lampeitl, Hubert; Maraston, Claudia; Masters, Karen L.; Nichol, Robert C.; Percival, Will J.; Pforr, Janine; Ross, Ashley J.; Thomas, Daniel; Tojeiro, Rita] Univ Portsmouth, Inst Cosmol & Gravitat, Portsmouth PO1 3FX, Hants, England. [Chen, Yanmei; Tremonti, Christy A.] Univ Wisconsin, Dept Astron, Madison, WI 53703 USA. [Chiappini, Cristina; Steinmetz, Matthias] Astrophys Inst Potsdam, D-14482 Potsdam, Germany. [Chiappini, Cristina] Ist Nazl Astrofis, I-34143 Trieste, Italy. [Comparat, Johan; Kneib, Jean-Paul] Univ Aix Marseille 1, CNRS, Lab Astrophys Marseille, F-13388 Marseille 13, France. [Connolly, Natalia] Hamilton Coll, Dept Phys, Clinton, NY 13323 USA. [Cortes, Marina; Ho, Shirley; Roe, Natalie A.; Ross, Nicholas P.; Schlegel, David J.] Univ Calif Berkeley, Lawrence Berkeley Lab, Berkeley, CA 94720 USA. [Croft, Rupert A. C.] Carnegie Mellon Univ, Bruce & Astrid McWilliams Ctr Cosmol, Pittsburgh, PA 15213 USA. [Cuesta, Antonio J.; Lundgren, Britt; Padmanabhan, Nikhil; Wake, David A.] Yale Univ, Yale Ctr Astron & Astrophys, New Haven, CT 06520 USA. [da Costa, Luiz N.; Maia, Marcio A. G.; Ogando, Ricardo L. C.; Ramos, Beatriz H. F.] Observ Nacl, BR-20921400 Rio De Janeiro, Brazil. [Ealet, Anne; Escoffier, Stephanie] Aix Marseille Univ, CNRS, IN2P3, Ctr Phys Particules Marseille, Marseille, France. [Ebelke, Garrett L.; Holtzman, Jon A.; Jordan, Wendell P.; Pfaffenberger, Robert; Vogt, Nicole P.] New Mexico State Univ, Dept Astron, Las Cruces, NM 88003 USA. [Eisenstein, Daniel J.; Fan, Xiaohui; Jiang, Linhua; McGreer, Ian D.; Szalay, Alexander S.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Eisenstein, Daniel J.] Harvard Coll Observ, Cambridge, MA 02138 USA. [Font-Ribera, Andreu] CSIC, IEEC, Inst Ciencies Espai, E-08193 Barcelona, Spain. [Frinchaboy, Peter M.] Texas Christian Univ, Dept Phys & Astron, Ft Worth, TX 76129 USA. [Ge, Jian; Duy Cuong Nguyen; Wang, Ji] Univ Florida, Dept Astron, Bryant Space Sci Ctr, Gainesville, FL 32611 USA. [Gilmore, G.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Gould, Andrew; Johnson, Jennifer A.; Kochanek, C. S.; Pieri, Matthew M.; Schlesinger, Katharine J.; Weinberg, David H.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Grebel, Eva K.; Sivarani, Thirupathi] Univ Heidelberg, Zentrum Astron, Astron Rechen Inst, D-69120 Heidelberg, Germany. [Harding, Paul; Ma, Zhibo; Morrison, Heather L.; Zehavi, Idit] Case Western Reserve Univ, Dept Astron, Cleveland, OH 44106 USA. [Hearty, Frederick R.; O'Connell, Robert W.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. [Honscheid, Klaus] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA. [Inada, Naohisa] Univ Tokyo, Grad Sch Sci, Res Ctr Early Universe, Bunkyo Ku, Tokyo 1130033, Japan. [Kirkby, David; Margala, Daniel] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. [Koesterke, Lars] Univ Texas Austin, Texas Adv Comp Ctr, Austin, TX 78758 USA. [Kollmeier, Juna A.] Observ Carnegie Inst Washington, Pasadena, CA 91101 USA. [Kron, Richard G.; Yanny, Brian] Fermilab Natl Accelerator Lab, Batavia, IL 60510 USA. [Kron, Richard G.; Sobeck, Jennifer S.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Lin, Yen-Ting] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan. [Lucatello, Sara] INAF, Osservatorio Astrono Padova, I-35122 Padua, Italy. [Mahadevan, Suvrath; Schneider, Donald P.] Penn State Univ, Ctr Exoplanets & Habitable Worlds, Davey Lab 525, University Pk, PA 16802 USA. [Makler, Martin] ICRA, Ctr Brasileiro Pesquisas Fis, BR-22290180 Rio De Janeiro, Brazil. [McGehee, Peregrine M.] CALTECH, IPAC, Pasadena, CA 91125 USA. [Menard, Brice] Univ Toronto, CITA, Toronto, ON M5S 3H8, Canada. [Menard, Brice; Raddick, M. Jordan; Szalay, Alexander S.; Thakar, Aniruddha R.; Vandenberg, Jan] Johns Hopkins Univ, Dept Phys & Astron, Ctr Astrophys Sci, Baltimore, MD 21218 USA. [Miralda-Escude, Jordi; Verde, Licia] Inst Catalana Recerca & Estudis Avancats, Barcelona, Spain. [Miralda-Escude, Jordi; Verde, Licia] Univ Barcelona, IEEC, Inst Ciencies Cosmos, E-08028 Barcelona, Spain. [Mullally, F.] NASA, Ames Res Ctr, SETI Inst, Moffett Field, CA 94035 USA. [Munn, Jeffrey A.] USN Observ, Flagstaff Stn, Flagstaff, AZ 86001 USA. [Myers, Adam D.] Univ Illinois, Dept Astron, Urbana, IL 61801 USA. [Paris, Isabelle; Petitjean, Patrick; Pichon, Christophe; Rollinde, Emmanuel] Univ Paris 06, Inst Astrophys Paris, CNRS, UMR7095, F-75014 Paris, France. [Phleps, Stefanie; Sanchez, Ariel G.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Pieri, Matthew M.] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA. [Prada, Francisco] CSIC, Inst Astrofis Andalucia, E-18008 Granada, Spain. [Reyle, Celine; Robin, Annie C.] Univ Franche Comte, Observ Besancon, Inst Utinam, F-25010 Besancon, France. [Richards, Gordon T.] Drexel Univ, Dept Phys, Philadelphia, PA 19104 USA. [Rix, Hans-Walter] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Rocha-Pinto, Helio J.; Rossetto, Bruno M.] Univ Fed Rio de Janeiro, Observ Valongo, BR-20080090 Rio De Janeiro, Brazil. [Rockosi, Constance M.] Univ Calif Santa Cruz, UCO Lick Observ, Santa Cruz, CA 95064 USA. [Sheldon, Erin] Bldg 510 Brookhaven Natl Lab Upton, Upton, NY 11973 USA. [Sivarani, Thirupathi] Indian Inst Astrophys, Bangalore 560034, Karnataka, India. [White, Martin] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [White, Simon D. M.] Max Planck Inst Astrophys, D-85748 Garching, Germany. RP Strauss, MA (reprint author), Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. RI Ho, Shirley/P-3682-2014; Balbinot, Eduardo/E-8019-2015; Padmanabhan, Nikhil/A-2094-2012; Roe, Natalie/A-8798-2012; Yasuda, Naoki/A-4355-2011; Aihara, Hiroaki/F-3854-2010; Kneib, Jean-Paul/A-7919-2015; Murayama, Hitoshi/A-4286-2011; Le Goff, Jean-Marc/E-7629-2013; Tecnologias espaciai, Inct/I-2415-2013; Gonzalez Hernandez, Jonay I./L-3556-2014; Ogando, Ricardo/A-1747-2010; Mandelbaum, Rachel/N-8955-2014; Pforr, Janine/J-3967-2015; Makler, Martin/G-2639-2012; White, Martin/I-3880-2015; Brandt, William/N-2844-2015; Rocha-Pinto, Helio/C-2719-2008; Jiang, Linhua/H-5485-2016; Croft, Rupert/N-8707-2014; OI Ho, Shirley/0000-0002-1068-160X; Balbinot, Eduardo/0000-0002-1322-3153; Aihara, Hiroaki/0000-0002-1907-5964; Kneib, Jean-Paul/0000-0002-4616-4989; Gonzalez Hernandez, Jonay I./0000-0002-0264-7356; Ogando, Ricardo/0000-0003-2120-1154; Mandelbaum, Rachel/0000-0003-2271-1527; Cortes, Marina/0000-0003-0485-3767; Schmidt, Sarah/0000-0002-7224-7702; Cuesta Vazquez, Antonio Jose/0000-0002-4153-9470; Bovy, Jo/0000-0001-6855-442X; Verde, Licia/0000-0003-2601-8770; /0000-0002-1891-3794; Masters, Karen/0000-0003-0846-9578; Hogg, David/0000-0003-2866-9403; Davenport, James/0000-0002-0637-835X; Pforr, Janine/0000-0002-3414-8391; Makler, Martin/0000-0003-2206-2651; White, Martin/0000-0001-9912-5070; Brandt, William/0000-0002-0167-2453; Jiang, Linhua/0000-0003-4176-6486; Croft, Rupert/0000-0003-0697-2583; Kirkby, David/0000-0002-8828-5463; Miralda-Escude, Jordi/0000-0002-2316-8370; Escoffier, Stephanie/0000-0002-2847-7498 FU Alfred P. Sloan Foundation; National Science Foundation; US Department of Energy; University of Arizona; Brazilian Participation Group; Brookhaven National Laboratory; University of Cambridge; University of Florida; French Participation Group; German Participation Group; Instituto de Astrofisica de Canarias; Michigan State/Notre Dame/JINA Participation Group; Johns Hopkins University; Lawrence Berkeley National Laboratory; Max Planck Institute for Astrophysics; New Mexico State University; New York University; Ohio State University; Pennsylvania State University; University of Portsmouth; Princeton University; Spanish Participation Group; University of Tokyo; University of Utah; Vanderbilt University; University of Virginia; University of Washington; Yale University FX We thank the referee, Andrew West, for comments that improved the paper. Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the US Department of Energy. The SDSS-III Web site is http://www.sdss3.org/.; SDSS-III is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS-III Collaboration including the University of Arizona, the Brazilian Participation Group, Brookhaven National Laboratory, University of Cambridge, University of Florida, the French Participation Group, the German Participation Group, the Instituto de Astrofisica de Canarias, the Michigan State/Notre Dame/JINA Participation Group, Johns Hopkins University, Lawrence Berkeley National Laboratory, Max Planck Institute for Astrophysics, New Mexico State University, New York University, Ohio State University, Pennsylvania State University, University of Portsmouth, Princeton University, the Spanish Participation Group, University of Tokyo, University of Utah, Vanderbilt University, University of Virginia, University of Washington, and Yale University. NR 86 TC 725 Z9 731 U1 6 U2 53 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD APR PY 2011 VL 193 IS 2 AR 29 DI 10.1088/0067-0049/193/2/29 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 743ZG UT WOS:000289059200007 ER PT J AU Rebull, LM Guieu, S Stauffer, JR Hillenbrand, LA Noriega-Crespo, A Stapelfeldt, KR Carey, SJ Carpenter, JM Cole, DM Padgett, DL Strom, SE Wolff, SC AF Rebull, L. M. Guieu, S. Stauffer, J. R. Hillenbrand, L. A. Noriega-Crespo, A. Stapelfeldt, K. R. Carey, S. J. Carpenter, J. M. Cole, D. M. Padgett, D. L. Strom, S. E. Wolff, S. C. TI THE NORTH AMERICAN AND PELICAN NEBULAE. II. MIPS OBSERVATIONS AND ANALYSIS SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE circumstellar matter; infrared: ISM; infrared: stars; ISM: clouds; ISM: individual objects (NGC 7000, IC 5070, LDN 935); stars: formation; stars: pre-main sequence ID SPITZER C2D SURVEY; MULTIBAND IMAGING PHOTOMETER; YOUNG STELLAR OBJECTS; OPEN CLUSTER NGC-6996; STAR-FORMING REGIONS; EMISSION-LINE STARS; ARRAY CAMERA IRAC; W-80 DARK CLOUD; ALL-SKY SURVEY; T-TAURI STARS AB We present observations of similar to 7 deg(2) of the North American and Pelican Nebulae region at 24, 70, and 160 mu m with the Spitzer Space Telescope Multiband Imaging Photometer for Spitzer (MIPS). We incorporate the MIPS observations with earlier Spitzer Infrared Array Camera (IRAC) observations, as well as archival near-infrared (IR) and optical data. We use the MIPS data to identify 1286 young stellar object (YSO) candidates. IRAC data alone can identify 806 more YSO candidates, for a total of 2076 YSO candidates. Prior to the Spitzer observations, there were only similar to 200 YSOs known in this region. Three subregions within the complex are highlighted as clusters: the Gulf of Mexico, the Pelican, and the Pelican's Hat. The Gulf of Mexico cluster is subject to the highest extinction (A(V) at least similar to 30) and has the widest range of infrared colors of the three clusters, including the largest excesses and by far the most point-source detections at 70 mu m. Just 3% of the cluster members were previously identified; we have redefined this cluster as about 10-100 times larger (in projected area) than was previously realized. C1 [Rebull, L. M.; Stauffer, J. R.; Noriega-Crespo, A.; Carey, S. J.; Padgett, D. L.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Guieu, S.] European So Observ, Santiago 19, Chile. [Hillenbrand, L. A.; Carpenter, J. M.] CALTECH, Dept Astron, Pasadena, CA 91125 USA. [Stapelfeldt, K. R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Cole, D. M.] Raytheon Co, Pasadena, CA USA. [Strom, S. E.; Wolff, S. C.] Natl Opt Astron Observ, Tucson, AZ USA. RP Rebull, LM (reprint author), CALTECH, Spitzer Sci Ctr, M-S 220-6,1200 E Calif Blvd, Pasadena, CA 91125 USA. EM luisa.rebull@jpl.nasa.gov OI Rebull, Luisa/0000-0001-6381-515X FU National Aeronautics and Space Administration; National Science Foundation; U.S. Government [NAG W-2166] FX This research has made use of NASA's Astrophysics Data System (ADS) Abstract Service, and of the SIMBAD database, operated at CDS, Strasbourg, France. This research has made use of data products from the Two Micron All-Sky Survey (2MASS), which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center, funded by the National Aeronautics and Space Administration and the National Science Foundation. These data were served by the NASA/IPAC Infrared Science Archive, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. This research has made use of the Digitized Sky Surveys, which were produced at the Space Telescope Science Institute under U.S. Government grant NAG W-2166. The images of these surveys are based on photographic data obtained using the Oschin Schmidt Telescope on Palomar Mountain and the UK Schmidt Telescope. The plates were processed into the present compressed digital form with the permission of these institutions. This paper makes use of data obtained as part of the INT Photometric Ha Survey of the Northern Galactic Plane (IPHAS) carried out at the Isaac Newton Telescope (INT). The INT is operated on the island of La Palma by the Isaac Newton Group in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias. All IPHAS data, processed by the Cambridge Astronomical Survey Unit, were obtained via the database and image access provided by Astrogrid. NR 86 TC 25 Z9 25 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD APR PY 2011 VL 193 IS 2 AR 25 DI 10.1088/0067-0049/193/2/25 PG 28 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 743ZG UT WOS:000289059200003 ER PT J AU Tullmann, R Gaetz, TJ Plucinsky, PP Kuntz, KD Williams, BF Pietsch, W Haberl, F Long, KS Blair, WP Sasaki, M Winkler, PF Challis, P Pannuti, TG Edgar, RJ Helfand, DJ Hughes, JP Kirshner, RP Mazeh, T Shporer, A AF Tuellmann, R. Gaetz, T. J. Plucinsky, P. P. Kuntz, K. D. Williams, B. F. Pietsch, W. Haberl, F. Long, K. S. Blair, W. P. Sasaki, M. Winkler, P. F. Challis, P. Pannuti, T. G. Edgar, R. J. Helfand, D. J. Hughes, J. P. Kirshner, R. P. Mazeh, T. Shporer, A. TI THE CHANDRA ACIS SURVEY OF M33 (ChASeM33): THE FINAL SOURCE CATALOG SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE binaries: general; galaxies: individual (M33); ISM: supernova remnants; surveys; X-rays: galaxies ID X-RAY SOURCES; STAR-FORMATION RATE; XMM-NEWTON SURVEY; LUMINOSITY FUNCTION; SPIRAL GALAXIES; MILKY-WAY; SUPERNOVA-REMNANTS; PHOTOMETRIC SURVEY; POINT SOURCES; SOURCE LIST AB This study presents the final source catalog of the Chandra ACIS Survey of M33 (ChASeM33). With a total exposure time of 1.4 Ms, ChASeM33 covers similar to 70% of the D-25 isophote (R approximate to 4.0 kpc) of M33 and provides the deepest, most complete, and detailed look at a spiral galaxy in X-rays. The source catalog includes 662 sources, reaches a limiting unabsorbed luminosity of similar to 2.4x10(34) erg s(-1) in the 0.35-8.0 keV energy band, and contains source positions, source net counts, fluxes and significances in several energy bands, and information on source variability. The analysis challenges posed by ChASeM33 and the techniques adopted to address these challenges are discussed. To constrain the nature of the detected X-ray source, hardness ratios were constructed and spectra were fit for 254 sources, follow-up MMT spectra of 116 sources were acquired, and cross-correlations with previous X-ray catalogs and other multi-wavelength data were generated. Based on this effort, 183 of the 662 ChASeM33 sources could be identified. Finally, the luminosity function (LF) for the detected point sources as well as the one for the X-ray binaries (XRBs) in M33 is presented. The LFs in the soft band (0.5-2.0 keV) and the hard band (2.0-8.0 keV) have a limiting luminosity at the 90% completeness limit of 4.0 x 10(34) erg s(-1) and 1.6 x 10(35) erg s(-1)(for D = 817 kpc), respectively, which is significantly lower than what was reported by previous XRB population studies in galaxies more distant than M33. The resulting distribution is consistent with a dominant population of high-mass XRBs as would be expected for M33. C1 [Tuellmann, R.; Gaetz, T. J.; Plucinsky, P. P.; Challis, P.; Edgar, R. J.; Kirshner, R. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kuntz, K. D.; Blair, W. P.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Kuntz, K. D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Williams, B. F.] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Pietsch, W.; Haberl, F.] Max Planck Inst Extraterr Phys, D-85741 Garching, Germany. [Long, K. S.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Sasaki, M.] Univ Tubingen, Inst Astron & Astrophys, Tubingen, Germany. [Winkler, P. F.] Middlebury Coll, Dept Phys, Middlebury, VT 05753 USA. [Pannuti, T. G.] Morehead State Univ, Ctr Space Sci, Morehead, KY 40351 USA. [Helfand, D. J.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Hughes, J. P.] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. [Mazeh, T.] Tel Aviv Univ, Raymond & Beverly Sackler Fac Exact Sci, Sch Phys & Astron, IL-69978 Tel Aviv, Israel. [Shporer, A.] Las Cumbres Observ Global Telescope Network, Santa Barbara, CA 93117 USA. [Shporer, A.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. RP Tullmann, R (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM rtuellmann@cfa.harvard.edu RI Sasaki, Manami/P-3045-2016; OI Sasaki, Manami/0000-0001-5302-1866; Haberl, Frank/0000-0002-0107-5237 FU National Aeronautics and Space Administration [G06-7073A]; National Aeronautics Space and Administration [NAS8-03060] FX Support for this work was provided by the National Aeronautics and Space Administration through Chandra Award Number G06-7073A issued by the Chandra X-ray Observatory Center, which is operated by the Smithsonian Astrophysical Observatory and on behalf of the National Aeronautics Space and Administration under contract NAS8-03060. R.T., P.P.P., T.J.G., and R.J.E. acknowledge support under NASA contract NAS8-03060. This work has made use of SAOImage DS9, developed by the Smithsonian Astrophysical Observatory (Joye & Mandel 2003), the XSPEC spectral fitting package (Arnaud 1996), the FUNTOOLS utilities package, the HEASARC FTOOLS package, the CIAO (Chandra Interactive Analysis of Observations) package, and ACIS Extract, the source extraction and characterization tool developed and maintained by Pat Broos. Sincere thanks to Pat Broos for answering our questions regarding AE and for maintaining this important tool and to David Thilker for kindly providing the Hi map of M33. We also acknowledge the heroic effort of the anonymous referee for a careful reading of the manuscript and several comments that helped to improve the paper. NR 68 TC 16 Z9 16 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD APR PY 2011 VL 193 IS 2 AR 31 DI 10.1088/0067-0049/193/2/31 PG 26 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 743ZG UT WOS:000289059200009 ER PT J AU Windhorst, RA Cohen, SH Hathi, NP McCarthy, PJ Ryan, RE Yan, HJ Baldry, IK Driver, SP Frogel, JA Hill, DT Kelvin, LS Koekemoer, AM Mechtley, M O'Connell, RW Robotham, ASG Rutkowski, MJ Seibert, M Straughn, AN Tuffs, RJ Balick, B Bond, HE Bushouse, H Calzetti, D Crockett, M Disney, MJ Dopita, MA Hall, DNB Holtzman, JA Kaviraj, S Kimble, RA MacKenty, JW Mutchler, M Paresce, F Saha, A Silk, JI Trauger, JT Walker, AR Whitmore, BC Young, ET AF Windhorst, Rogier A. Cohen, Seth H. Hathi, Nimish P. McCarthy, Patrick J. Ryan, Russell E., Jr. Yan, Haojing Baldry, Ivan K. Driver, Simon P. Frogel, Jay A. Hill, David T. Kelvin, Lee S. Koekemoer, Anton M. Mechtley, Matt O'Connell, Robert W. Robotham, Aaron S. G. Rutkowski, Michael J. Seibert, Mark Straughn, Amber N. Tuffs, Richard J. Balick, Bruce Bond, Howard E. Bushouse, Howard Calzetti, Daniela Crockett, Mark Disney, Michael J. Dopita, Michael A. Hall, Donald N. B. Holtzman, Jon A. Kaviraj, Sugata Kimble, Randy A. MacKenty, John W. Mutchler, Max Paresce, Francesco Saha, Abihit Silk, Joseph I. Trauger, John T. Walker, Alistair R. Whitmore, Bradley C. Young, Erick T. TI THE HUBBLE SPACE TELESCOPE WIDE FIELD CAMERA 3 EARLY RELEASE SCIENCE DATA: PANCHROMATIC FAINT OBJECT COUNTS FOR 0.2-2 mu m WAVELENGTH SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE Galaxy: stellar content; infrared: galaxies; instrumentation: high angular resolution; ultraviolet: galaxies ID ULTRA-DEEP-FIELD; EMISSION-LINE GALAXIES; STAR-FORMATION HISTORY; LYMAN BREAK GALAXIES; GOODS-SOUTH FIELD; HIGH-REDSHIFT GALAXIES; EXTREMELY RED OBJECTS; NORTH GALACTIC POLE; MASS ASSEMBLY GAMA; TO 7 GALAXIES AB We describe the Hubble Space Telescope (HST) Wide Field Camera 3 (WFC3) Early Release Science (ERS) observations in the Great Observatories Origins Deep Survey (GOODS) South field. The new WFC3 ERS data provide calibrated, drizzled mosaics in the UV filters F225W, F275W, and F336W, as well as in the near-IR filters F098M (Y-s), F125W (J), and F160W (H) with 1-2 HST orbits per filter. Together with the existing HST Advanced Camera for Surveys (ACS) GOODS-South mosaics in the BViz filters, these panchromatic 10-band ERS data cover 40-50 arcmin(2) at 0.2-1.7 mu m in wavelength at 0 ''.07-0 ''.15 FWHM resolution and 0 ''.090 Multidrizzled pixels to depths of AB similar or equal to 26.0-27.0 mag (5 sigma) for point sources, and AB similar or equal to 25.5-26.5 mag for compact galaxies. In this paper, we describe (1) the scientific rationale, and the data taking plus reduction procedures of the panchromatic 10-band ERS mosaics, (2) the procedure of generating object catalogs across the 10 different ERS filters, and the specific star-galaxy separation techniques used, and (3) the reliability and completeness of the object catalogs from the WFC3 ERS mosaics. The excellent 0 ''.07-0 ''.15 FWHM resolution of HST/WFC3 and ACS makes star-galaxy separation straightforward over a factor of 10 in wavelength to AB similar or equal to 25-26 mag from the UV to the near-IR, respectively. Our main results are: (1) proper motion of faint ERS stars is detected over 6 years at 3.06 +/- 0.66 mas year(-1) (4.6 sigma), consistent with Galactic structure models; (2) both the Galactic star counts and the galaxy counts show mild but significant trends of decreasing count slopes from the mid-UV to the near-IR over a factor of 10 in wavelength; (3) combining the 10-band ERS counts with the panchromatic Galaxy and Mass Assembly survey counts at the bright end (10 mag less than or similar to AB less than or similar to 20 mag) and the Hubble Ultra Deep Field counts in the BVizY(s)JH filters at the faint end (24 mag less than or similar to AB less than or similar to 30 mag) yields galaxy counts that are well measured over the entire flux range 10 mag less than or similar to AB less than or similar to 30 mag for 0.2-2 mu m in wavelength; (4) simple luminosity+density evolution models can fit the galaxy counts over this entire flux range. However, no single model can explain the counts over this entire flux range in all 10 filters simultaneously. More sophisticated models of galaxy assembly are needed to reproduce the overall constraints provided by the current panchromatic galaxy counts for 10 mag less than or similar to AB less than or similar to 30 mag over a factor of 10 in wavelength. C1 [Windhorst, Rogier A.; Cohen, Seth H.; Mechtley, Matt; Rutkowski, Michael J.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [Hathi, Nimish P.] Univ Calif Riverside, Dept Phys & Astron, Riverside, CA 92521 USA. [McCarthy, Patrick J.; Seibert, Mark] Observ Carnegie Inst Washington, Pasadena, CA 91101 USA. [Ryan, Russell E., Jr.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. [Yan, Haojing] Ohio State Univ, Ctr Cosmol & AstroParticle Phys, Columbus, OH 43210 USA. [Baldry, Ivan K.] Liverpool John Moores Univ, Astrophys Res Inst, Birkenhead CH41 1LD, Merseyside, England. [Driver, Simon P.; Hill, David T.; Kelvin, Lee S.; Robotham, Aaron S. G.] Univ St Andrews, Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland. [Frogel, Jay A.] Assoc Univ Res Astron, Washington, DC 20005 USA. [Koekemoer, Anton M.; Bond, Howard E.; Bushouse, Howard; MacKenty, John W.; Mutchler, Max; Whitmore, Bradley C.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [O'Connell, Robert W.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. [Straughn, Amber N.; Kimble, Randy A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Tuffs, Richard J.] Max Planck Inst Nucl Phys MPIK, D-69117 Heidelberg, Germany. [Balick, Bruce] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Calzetti, Daniela; Silk, Joseph I.] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. [Crockett, Mark; Kaviraj, Sugata] Univ Oxford, Dept Phys, Oxford OX1 3PU, England. [Disney, Michael J.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Dopita, Michael A.] Australian Natl Univ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia. [Hall, Donald N. B.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Holtzman, Jon A.] New Mexico State Univ, Dept Astron, Las Cruces, NM 88003 USA. [Paresce, Francesco] INAF IASF Bologna, I-40129 Bologna, Italy. [Saha, Abihit] Natl Opt Astron Observ, Tucson, AZ 85726 USA. [Trauger, John T.] NASA, Jet Prop Lab, Pasadena, CA 91109 USA. [Walker, Alistair R.] Cerro Tololo Interamer Observ, La Serena, Chile. [Young, Erick T.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Windhorst, RA (reprint author), Arizona State Univ, Sch Earth & Space Explorat, POB 871404, Tempe, AZ 85287 USA. EM Rogier.Windhorst@asu.edu RI Robotham, Aaron/H-5733-2014; Dopita, Michael/P-5413-2014; Driver, Simon/H-9115-2014; Hathi, Nimish/J-7092-2014; OI Robotham, Aaron/0000-0003-0429-3579; Dopita, Michael/0000-0003-0922-4986; Driver, Simon/0000-0001-9491-7327; Hathi, Nimish/0000-0001-6145-5090; Mechtley, Matt/0000-0001-6462-6190; Koekemoer, Anton/0000-0002-6610-2048 FU NASA through Space Telescope Science Institute [11359, GO-11359, NAS 5-26555]; NASA JWST, GSFC [NAG5-12460]; Center for Cosmology and AstroParticle Physics (CCAPP) at The Ohio State University FX Support for HST program 11359 was provided by NASA through grant GO-11359 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. R.A.W. also acknowledges support from NASA JWST Interdisciplinary Scientist grant NAG5-12460 from GSFC. H.Y. is supported by the long-term fellowship program of the Center for Cosmology and AstroParticle Physics (CCAPP) at The Ohio State University. NR 131 TC 137 Z9 137 U1 1 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD APR PY 2011 VL 193 IS 2 AR 27 DI 10.1088/0067-0049/193/2/27 PG 33 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 743ZG UT WOS:000289059200005 ER PT J AU Kim, HS Han, HD Armaiz-Pena, GN Stone, RL Nam, EJ Lee, JW Shahzad, MMK Nick, AM Lee, SJ Roh, JW Nishimura, M Mangala, LS Bottsford-Miller, J Gallick, GE Lopez-Berestein, G Sood, AK AF Kim, Hye-Sun Han, Hee Dong Armaiz-Pena, Guillermo N. Stone, Rebecca L. Nam, Eun Ji Lee, Jeong-Won Shahzad, Mian M. K. Nick, Alpa M. Lee, Sun Joo Roh, Ju-Won Nishimura, Masato Mangala, Lingegowda S. Bottsford-Miller, Justin Gallick, Gary E. Lopez-Berestein, Gabriel Sood, Anil K. TI Functional Roles of Src and Fgr in Ovarian Carcinoma SO CLINICAL CANCER RESEARCH LA English DT Article ID FAMILY KINASES; CHITOSAN HYDROGEL; TYROSINE KINASE; CANCER CELLS; GENE AMPLIFICATIONS; SIGNAL-TRANSDUCTION; PROSTATE-CANCER; MACROPHAGES; INHIBITION; EXPRESSION AB Purpose: Src is an attractive target because it is overexpressed in a number of malignancies, including ovarian cancer. However, the effect of Src silencing on other Src family kinases (SFKs) is not known. We hypothesized that other SFK members could compensate for the lack of Src activity. Experimental Design: Cell viability after either Src or Fgr silencing was examined in ovarian cancer cell lines by MTT assay. Expression of SFKs after Src silencing in ovarian cancer cells was examined by real-time reverse transcriptase (RT)-PCR. Therapeutic effect of in vivo Src and/or Fgr silencing was examined using siRNA incorporated into chitosan nanoparticles (siRNA/CH-NP). Microvessel density, cell proliferation, and apoptosis markers were determined by immunohistochemical staining in ovarian tumor tissues. Results: Src silencing enhanced cytotoxicity of docetaxel in both SKOV3ip1 and HeyA8 cells. In addition, Src silencing using siRNA/CH-NP in combination with docetaxel resulted in significant inhibition of tumor growth compared with control siRNA/CH-NP (81.8% reduction in SKOV3ip1, P = 0.017; 84.3% reduction in HeyA8, P < 0.005). These effects were mediated by decreased tumor cell proliferation and angiogenesis, and increased tumor cell apoptosis. Next, we assessed the effects of Src silencing on other SFK members in ovarian cancer cell lines. Src silencing resulted in significantly increased Fgr levels. Dual Src and Fgr silencing in vitro resulted in increased apoptosis that was mediated by increased caspase and AKT activity. In addition, dual silencing of Src and Fgr in vivo using siRNA/CH-NP resulted in the greatest reduction in tumor growth compared with silencing of either Src or Fgr alone in the HeyA8 model (68.8%, P < 0.05). Conclusions: This study demonstrates that, in addition to Src, Fgr plays a biologically significant role in ovarian cancer growth and might represent an important target. Clin Cancer Res; 17(7); 1713-21. (C) 2011 AACR. C1 [Kim, Hye-Sun; Han, Hee Dong; Armaiz-Pena, Guillermo N.; Stone, Rebecca L.; Nam, Eun Ji; Lee, Jeong-Won; Shahzad, Mian M. K.; Nick, Alpa M.; Lee, Sun Joo; Roh, Ju-Won; Nishimura, Masato; Mangala, Lingegowda S.; Bottsford-Miller, Justin; Sood, Anil K.] Univ Texas MD Anderson Canc Ctr, Dept Gynecol Oncol, Houston, TX 77030 USA. [Gallick, Gary E.] Univ Texas MD Anderson Canc Ctr, Dept Genitourinary Med Oncol, Houston, TX 77030 USA. [Lopez-Berestein, Gabriel] Univ Texas MD Anderson Canc Ctr, Dept Expt Therapeut, Houston, TX 77030 USA. [Lopez-Berestein, Gabriel; Sood, Anil K.] Univ Texas MD Anderson Canc Ctr, Dept Canc Biol, Houston, TX 77030 USA. [Han, Hee Dong; Lopez-Berestein, Gabriel; Sood, Anil K.] Univ Texas MD Anderson Canc Ctr, Ctr RNA Interference & Noncoding RNA, Houston, TX 77030 USA. [Mangala, Lingegowda S.] NASA, Lyndon B Johnson Space Ctr, Dept Radiat Biophys, Univ Space Res Assoc, Houston, TX 77058 USA. [Shahzad, Mian M. K.] Univ Wisconsin, Dept Obstet & Gynecol, Div Gynecol Oncol, Madison, WI 53706 USA. [Shahzad, Mian M. K.] Univ Wisconsin, UW Carbone Canc Ctr, Madison, WI USA. [Kim, Hye-Sun] Kwandong Univ, Coll Med, Womens Healthcare Ctr, Goyang, South Korea. [Nam, Eun Ji] Yonsei Univ, Womens Canc Clin, Dept Obstet & Gynecol, Coll Med, Seoul 120749, South Korea. [Lee, Jeong-Won] Sungkyunkwan Univ, Dept Obstet & Gynecol, Samsung Med Ctr, Sch Med, Seoul, South Korea. [Lee, Sun Joo] Konkuk Univ, Dept Obstet & Gynecol, Konkuk Univ Hosp, Sch Med, Seoul, South Korea. [Roh, Ju-Won] Dongguk Univ, Ilsan Hosp, Dept Obstet & Gynecol, Goyang, South Korea. RP Sood, AK (reprint author), Univ Texas MD Anderson Canc Ctr, Dept Gynecol Oncol, 1155 Herman Pressler,Unit 1352, Houston, TX 77030 USA. EM asood@mdanderson.org RI lee, jw/O-6237-2014; OI Armaiz-Pena, Guillermo N/0000-0002-9081-5339 FU NIH [CA 110793, 109298, CA 128797, RC2 GM 092599, U54 CA151668]; DOD [OC-073399, W81 XWH-10-1-0158, BC 085265]; Ovarian Cancer Research Fund, Inc.; U.T.M.D. Anderson Cancer Center SPORE [P50CA083639]; Zarrow Foundation; Marcus Foundation; NCI-DHHS-NIH [T32 CA101642]; Baylor WRHR [HD050128]; GCF Molly-Cade FX Portions of this work were supported by NIH grants (CA 110793, 109298, CA 128797, and RC2 GM 092599, U54 CA151668), DOD (OC-073399, W81 XWH-10-1-0158, BC 085265), the Ovarian Cancer Research Fund, Inc. (Program Project Development Grant), U.T.M.D. Anderson Cancer Center SPORE (P50CA083639), the Zarrow Foundation, the Marcus Foundation, the Betty Anne Asche Murray Distinguished Professorship, and the Laura and John Arnold Foundation. AMN, JBM, and RS are supported by NCI-DHHS-NIH T32 Training Grant (T32 CA101642). MMS was supported by the Baylor WRHR grant (HD050128) and the GCF Molly-Cade ovarian cancer research grant. NR 30 TC 35 Z9 38 U1 0 U2 11 PU AMER ASSOC CANCER RESEARCH PI PHILADELPHIA PA 615 CHESTNUT ST, 17TH FLOOR, PHILADELPHIA, PA 19106-4404 USA SN 1078-0432 J9 CLIN CANCER RES JI Clin. Cancer Res. PD APR 1 PY 2011 VL 17 IS 7 BP 1713 EP 1721 DI 10.1158/1078-0432.CCR-10-2081 PG 9 WC Oncology SC Oncology GA 743XY UT WOS:000289054100009 PM 21300758 ER PT J AU Mulavara, AP Fiedler, MJ Kofman, IS Wood, SJ Serrador, JM Peters, B Cohen, HS Reschke, MF Bloomberg, JJ AF Mulavara, Ajitkumar P. Fiedler, Matthew J. Kofman, Igor S. Wood, Scott J. Serrador, Jorge M. Peters, Brian Cohen, Helen S. Reschke, Millard F. Bloomberg, Jacob J. TI Improving balance function using vestibular stochastic resonance: optimizing stimulus characteristics SO EXPERIMENTAL BRAIN RESEARCH LA English DT Article DE Stochastic resonance; Balance; Vestibular stimulation; Electrical stimulation ID HUMAN POSTURAL CONTROL; SENSORIMOTOR INTEGRATION; TACTILE SENSATION; NOISE; STIMULATION; SYSTEM; MECHANORECEPTORS; SWAY; RESPONSES AB Stochastic resonance (SR) is a phenomenon whereby the response of a non-linear system to a weak periodic input signal is optimized by the presence of a particular non-zero level of noise. Stochastic resonance using imperceptible stochastic vestibular electrical stimulation, when applied to normal young and elderly subjects, has been shown to significantly improve ocular stabilization reflexes in response to whole-body tilt; improved balance performance during postural disturbances and optimize covariance between the weak input periodic signals introduced via venous blood pressure receptors and the heart rate responses. In our study, 15 subjects stood on a compliant surface with their eyes closed. They were given low-amplitude binaural bipolar stochastic electrical stimulation of the vestibular organs in two frequency ranges of 1-2 and 0-30 Hz over the amplitude range of 0 to +/- 700 mu A. Subjects were instructed to maintain an upright stance during 43-s trials, which consisted of baseline (zero amplitude) and stimulation (non-zero amplitude) periods. Measures of stability of the head and trunk using inertial motion unit sensors attached to these segments and the whole body using a force plate were measured and quantified in the mediolateral plane. Using a multivariate optimization criterion, our results show that the low levels of vestibular stimulation given to the vestibular organs improved balance performance in normal healthy subjects in the range of 5-26% consistent with the stochastic resonance phenomenon. In our study, 8 of 15 and 10 of 15 subjects were responsive for the 1-2- and 0-30-Hz stimulus signals, respectively. The improvement in balance performance did not differ significantly between the stimulations in the two frequency ranges. The amplitude of optimal stimulus for improving balance performance was predominantly in the range of +/- 100 to +/- 400 mu A. A device based on SR stimulation of the vestibular system might be useful as either a training modality to enhance adaptability or skill acquisition, or as a miniature patch-type stimulator that may be worn by people with disabilities due to aging or disease to improve posture and locomotion function. C1 [Mulavara, Ajitkumar P.; Wood, Scott J.] Univ Space Res Assoc, Houston, TX 77058 USA. [Fiedler, Matthew J.; Kofman, Igor S.; Peters, Brian] Wyle Integrated Sci & Engn Grp, Houston, TX USA. [Serrador, Jorge M.] NJ Healthcare Syst, Dept Vet Affairs, E Orange, NJ USA. [Cohen, Helen S.] Baylor Coll Med, Houston, TX 77030 USA. [Reschke, Millard F.; Bloomberg, Jacob J.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. RP Mulavara, AP (reprint author), Univ Space Res Assoc, 2101 NASA Pkwy,Mail Code SK-B272, Houston, TX 77058 USA. EM ajitkumar.p.mulavara@nasa.gov FU National Space Biomedical Research Institute through NASA [NCC 9-58 (SA02001)] FX This study was supported in part by a grant from the National Space Biomedical Research Institute through NASA NCC 9-58 (SA02001) to Ajitkumar Mulavara (PI). We would like to thank Erin Heap, Keena Acock, and Elizabeth Fisher for their help with data analysis and data collection and Hamish MacDougal and John Holden for their help with design and building the vestibular stimulation system. We would also like to thank all the subjects who participated voluntarily in the experiments. NR 47 TC 23 Z9 25 U1 1 U2 22 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0014-4819 EI 1432-1106 J9 EXP BRAIN RES JI Exp. Brain Res. PD APR PY 2011 VL 210 IS 2 BP 303 EP 312 DI 10.1007/s00221-011-2633-z PG 10 WC Neurosciences SC Neurosciences & Neurology GA 742QJ UT WOS:000288959200014 PM 21442221 ER PT J AU Zwart, SR Mehta, SK Ploutz-Snyder, R Liourbeau, Y Locke, JP Pierson, DL Smith, SM AF Zwart, Sara R. Mehta, Satish K. Ploutz-Snyder, Robert Liourbeau, YaVonne Locke, James P. Pierson, Duane L. Smith, Scott M. TI Response to Vitamin D Supplementation during Antarctic Winter Is Related to BMI, and Supplementation Can Mitigate Epstein-Barr Virus Reactivation SO JOURNAL OF NUTRITION LA English DT Article ID SPACE-FLIGHT; CALCIUM-METABOLISM; HEALTH; ASTRONAUTS; DISEASE; SPACEFLIGHT; PERSPECTIVE; IMMUNITY; STATION; CANCER AB Maintaining vitamin D status without sunlight exposure is difficult without supplementation. This study was designed to better understand interrelatiorships between periodic vitamin D supplementation and immune function n Antarctic workers. The effect of 2 oral dosing regimens of vitamin D supplementation on vitamin D status and markers of immune function was evaluated in people in Antarctica with no UV light exposure for 6 mo. Participants were given a 2000-IU (50 mu g) daily (n = 15) or 10.000 IU (250 mu g) weekly (n = 14) vitamin D supplement for 6 mo during a winter in Antarctica. Biological samples were collected at baseline and at 3 and 6 mo. Vitamin D intake, markers of vitamin D and bone metabolism. and latent virus reactivation were determined. After 6 mo, the serum 25-hydroxyvitamin D concentration (mean SD) increased from 56 +/- 17 to 79 +/- 16 mmol/L and from 52 = 10 to 60 +/- 9 nmol/1 in the 2000-IU/d and 10,000-IU/wk groups, respectively (main effect over time, P < 0.001). Participants with a greater BMI (participant BMI range = 19-43 g/m(2)) had a smaller increase in 25-hyd-oxyvitamin D after 6 mo supplementation (P < 0.05). Participants with high serum cortisol and higher serum 25-hydroxyvitamin D were less likely to shed Epstein Barr virus in saliva (P < 0.05). The aoses given raised vitamn D status in participants not exposed to sunlight for 6 mo, and the efficacy was influenced by baseline vitamin D status and BMI. The data also provide evidence trial vitamin D, interacting with stress, can reduce risk of latent virus reactivation during the winter in Antarctica. J. Nutr, 141: 692-697, 2011. C1 [Locke, James P.; Pierson, Duane L.; Smith, Scott M.] NASA, Johnson Space Ctr, Space Life Sci Directorate, Houston, TX 77058 USA. [Zwart, Sara R.; Ploutz-Snyder, Robert] Univ Space Res Assoc, Houston, TX 77058 USA. [Mehta, Satish K.; Liourbeau, YaVonne] Enterprise Advisory Serv Inc, Houston, TX 77058 USA. RP Smith, SM (reprint author), NASA, Johnson Space Ctr, Space Life Sci Directorate, Houston, TX 77058 USA. EM scott.m.smith@nasa.gov FU NASA; National Science Foundation FX Supported by The NASA Human Research Program Human Health and Countermeasures Element and made possible by the National Science Foundation NR 27 TC 28 Z9 28 U1 0 U2 5 PU AMER SOC NUTRITIONAL SCIENCE PI BETHESDA PA 9650 ROCKVILLE PIKE, RM L-2407A, BETHESDA, MD 20814 USA SN 0022-3166 J9 J NUTR JI J. Nutr. PD APR PY 2011 VL 141 IS 4 BP 692 EP 697 DI 10.3945/jn.110.134742 PG 6 WC Nutrition & Dietetics SC Nutrition & Dietetics GA 741PU UT WOS:000288876800023 PM 21539011 ER PT J AU Ashour-Abdalla, M El-Alaoui, M Goldstein, ML Zhou, M Schriver, D Richard, R Walker, R Kivelson, MG Hwang, KJ AF Ashour-Abdalla, Maha El-Alaoui, Mostafa Goldstein, Melvyn L. Zhou, Meng Schriver, David Richard, Robert Walker, Raymond Kivelson, Margaret G. Hwang, Kyoung-Joo TI Observations and simulations of non-local acceleration of electrons in magnetotail magnetic reconnection events SO NATURE PHYSICS LA English DT Article ID SUBSTORM ONSET; PARTICLE-ACCELERATION; THEMIS; MOTION; FIELDS AB Magnetic reconnection in magnetized plasmas represents a change in magnetic field topology and is associated with a concomitant energization of charged particles that results from a conversion of magnetic energy into particle energy. In Earth's magnetosphere this process is associated with the entry of the solar wind into the magnetosphere and with the initiation of auroral substorms. Using data from the THEMIS mission, together with global and test particle simulations, we demonstrate that electrons are energized in two distinct regions: a low-energy population (less than or equal to a few kiloelectronvolts) that arises in a diffusion region where particles are demagnetized and the magnetic topology changes, and a high-energy component (approaching 100 keV) that results from betatron acceleration within dipolarization fronts that sweep towards the inner magnetosphere far from the diffusion region. Thus, the observed particle energization is associated with both magnetic reconnection and with betatron acceleration associated with macroscopic flows. C1 [Ashour-Abdalla, Maha; El-Alaoui, Mostafa; Schriver, David; Richard, Robert; Walker, Raymond; Kivelson, Margaret G.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90095 USA. [Goldstein, Melvyn L.; Hwang, Kyoung-Joo] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Zhou, Meng] Nanchang Univ, Inst Space Sci & Technol, Nanchang 330031, Peoples R China. [Kivelson, Margaret G.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. [Hwang, Kyoung-Joo] Univ Maryland Baltimore Cty, Catonsville, MD 21250 USA. RP Ashour-Abdalla, M (reprint author), Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90095 USA. EM mabdalla@igpp.ucla.edu RI Goldstein, Melvyn/B-1724-2008; Kivelson, Margaret/I-9019-2012; NASA MMS, Science Team/J-5393-2013 OI Kivelson, Margaret/0000-0003-3859-8581; NASA MMS, Science Team/0000-0002-9504-5214 FU NASA [NNX08AO48G, NAS5-02099, UCB NAS 5-02099] FX We thank H. Kohne for help with programming and display of the data and simulation results. Research at UCLA was supported by NASA grant NNX08AO48G. We acknowledge NASA contract NAS5-02099 and V. Angelopoulos for use of data from the THEMIS Mission, specifically, C. W. Carlson and J. P. McFadden for the use of ESA data, D. Larson and R. P. Lin for the use of SST data, K. H. Glassmeier, U. Auster and W. Baumjohann for the use of FGM data, J. W. Bonnell and F. S. Mozer for the use of EFI data, and A. Roux and O. LeContel for the use of SCM data. K-J.H. and M. L. G. were supported, in part, by NASA's Magnetospheric Multiscale and Cluster missions at the Goddard Space Flight Center. M. G. K. was supported, in part, by NASA Grant UCB NAS 5-02099. The computing was carried out on NASA's Columbia Supercomputer. NR 39 TC 81 Z9 82 U1 0 U2 8 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 1745-2473 J9 NAT PHYS JI Nat. Phys. PD APR PY 2011 VL 7 IS 4 BP 360 EP 365 DI 10.1038/NPHYS1903 PG 6 WC Physics, Multidisciplinary SC Physics GA 744DZ UT WOS:000289076000025 ER PT J AU Vorotnikov, VS Smith, CW Farrugia, CJ Meredith, CJ Hu, QA Szabo, A Skoug, RM Cohen, CMS Davis, AJ Yumoto, K AF Vorotnikov, Vasiliy S. Smith, Charles W. Farrugia, Charles J. Meredith, Calum J. Hu, Qiang Szabo, Adam Skoug, Ruth M. Cohen, Christina M. S. Davis, Andrew J. Yumoto, Kiyohumi TI Use of single-component wind speed in Rankine-Hugoniot analysis of interplanetary shocks SO SPACE WEATHER-THE INTERNATIONAL JOURNAL OF RESEARCH AND APPLICATIONS LA English DT Article ID SOLAR-WIND AB We have extended and deployed a routine designed to run independently on the Web providing real-time analysis of interplanetary shock observations from L(1). The program accesses real-time magnetic field, solar wind speed, and proton density data from the Advanced Composition Explorer (ACE) spacecraft, searches for interplanetary shocks, analyzes shocks according to the Rankine-Hugoniot (R-H) jump conditions, and provides shock solutions on the Web for space weather applications. Because the ACE real-time data stream contains the wind speed but not the three-component wind velocity, we describe modifications to the R-H analysis that use the scalar wind speed and show successful results for analyses of strong interplanetary shocks at 1 AU. We compare the three-component and one-component solutions and find the greatest disagreement between the two rests in estimations of the shock speed rather than the shock propagation direction. Uncertainties in magnetic quantities such as magnetic compression and shock normal angle relative to the upstream magnetic field show large uncertainties in both analyses when performed using an automated routine whereas analyses of the shock normal alone do not. The automated data point selection scheme, together with the natural variability of the magnetic field, is inferred to be a problem in a few instances for this and other reasons. For a broad range of interplanetary shocks that arrive 30 to 60 min after passing L(1), this method will provide 15 to 45 min of advanced warning prior to the shock's collision with the Earth's magnetopause. The shock, in turn, provides advance warning of the approaching driver gas. C1 [Vorotnikov, Vasiliy S.] Univ New Hampshire, Dept Chem Engn, Durham, NH 03824 USA. [Cohen, Christina M. S.; Davis, Andrew J.] CALTECH, Space Radiat Lab, Pasadena, CA 91125 USA. [Smith, Charles W.; Farrugia, Charles J.] Univ New Hampshire, Ctr Space Sci, Inst Study Earth Oceans & Space, Dept Phys, Durham, NH 03824 USA. [Hu, Qiang] Univ Alabama, CSPAR, Huntsville, AL 35805 USA. [Meredith, Calum J.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Skoug, Ruth M.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA. [Szabo, Adam] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Yumoto, Kiyohumi] Kyushu Univ, Space Environm Res Ctr, Fukuoka 8128581, Japan. RP Vorotnikov, VS (reprint author), Univ New Hampshire, Dept Chem Engn, Durham, NH 03824 USA. EM vasya@udel.edu; charles.smith@unh.edu; charlie.farrugia@unh.edu; cjm49@leicester.ac.uk; qh0001@uah.edu; adam.szabo@nasa.gov; rskoug@lanl.gov; cohen@srl.caltech.edu; ad@srl.caltech.edu; yumoto@serc.kyushu-u.ac.jp FU NASA [NNG04GMO5G, NAG5-12492]; Caltech [44A-1062037]; U.S. Department of Energy FX Funding for this work was provided by NASA grants NNG04GMO5G and NAG5-12492 and Caltech subcontract 44A-1062037 in support of the ACE/MAG experiment. Support at LANL was provided under the auspices of the U.S. Department of Energy, with financial support from the NASA ACE program. We thank the Solar-Terrestrial Laboratory at Nagoya University for providing the 210MM magnetic observations and the IMAGE ground-based magnetometer team for providing data used in this study. V. S. V. was an undergraduate senior at UNH pursuing a chemical engineering major in renewable energy when this work was performed. He is now a graduate student in the Center for Renewable Energy at the University of Delaware. C.J.M. was a visiting undergraduate at UNH at the time this work was completed. NR 14 TC 5 Z9 5 U1 0 U2 5 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 1542-7390 J9 SPACE WEATHER JI Space Weather PD APR 1 PY 2011 VL 9 AR S04001 DI 10.1029/2010SW000631 PG 9 WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences GA 744KS UT WOS:000289093900001 ER PT J AU Ari-Gur, P Sariel, J Stanford, MK DellaCorte, C Abel, PB AF Ari-Gur, P. Sariel, J. Stanford, M. K. DellaCorte, C. Abel, P. B. TI Phase identification of hard precipitates in PS304 coatings SO SURFACE ENGINEERING LA English DT Article DE PS304; Tribological coatings; X-ray diffraction ID TEMPERATURE; STRENGTH AB This paper presents the details of the detection of an unexpected (enigmatic) phase resulting from heat treatment of a tribocoating labelled PS304. This coating, consisting of chromium oxide powder in a Ni-Cr base powder and lubricated by silver metal and fluorides of barium and calcium, provides a plasma sprayed lubricious multitemperature wear and oxidation resistant surface layer for challenging wear applications. Primarily based on X-ray diffraction structural analysis, a chromium disilicide compound has been identified to form as a result of the heat treatment of the coating. A source of the significant strengthening of the coating by the heat treatment process is explained on the basis of the formation of the disilicide compound and its properties. The strengthening effect of fugitive silicon present in such trace levels is recognised for the first time as having a potential for use in many tribocoating systems as a cost effective and efficient strengthening approach. C1 [Ari-Gur, P.] Western Michigan Univ, Dept Mech & Aeronaut Engn, Kalamazoo, MI 49008 USA. [Sariel, J.] Nucl Res Ctr, Beer Sheva, Israel. [Stanford, M. K.; DellaCorte, C.; Abel, P. B.] NASA, Glenn Res Ctr, Cleveland, OH USA. RP Ari-Gur, P (reprint author), Western Michigan Univ, Dept Mech & Aeronaut Engn, Kalamazoo, MI 49008 USA. EM pnina.ari-gur@wmich.edu NR 8 TC 1 Z9 1 U1 1 U2 7 PU MANEY PUBLISHING PI LEEDS PA STE 1C, JOSEPHS WELL, HANOVER WALK, LEEDS LS3 1AB, W YORKS, ENGLAND SN 0267-0844 J9 SURF ENG JI Surf. Eng. PD APR PY 2011 VL 27 IS 3 BP 196 EP 198 DI 10.1179/026708410X12683118611301 PG 3 WC Materials Science, Coatings & Films SC Materials Science GA 744GF UT WOS:000289082200009 ER PT J AU Pinel, SI Signer, HR Zaretsky, EV AF Pinel, Stanley I. Signer, Hans R. Zaretsky, Erwin V. TI Comparison Between Oil-Mist and Oil-Jet Lubrication of High-Speed, Small-Bore, Angular-Contact Ball Bearing SO TRIBOLOGY & LUBRICATION TECHNOLOGY LA English DT Article DE Rolling-Element Bearings; Ball Bearings; Life Prediction; Lubrication; Oil-Jet Lubrication; Air-Oil Mist Lubrication AB Parametric tests were conducted with an optimized 35-mm-bore-angular-contact ball bearing on a high-speed, high-temperature bearing tester Results from both air-oil mist lubrication and oil-jet lubrication systems used to lubricate the bearing were compared to speeds of 2.5Y10(6) DN. The maximum obtainable speed with air-oil mist lubrication is 2.5Y10(6) DN. Lower bearing temperatures and higher power losses are obtained with oil-jet lubrication than with air-oil mist lubrication Bearing power loss is a direct function of oil flow to the bearing and independent of oil delivery system. For a given oil-flow rate, bearing temperature and power loss increase with increases in speed. Bearing life is an inverse function of temperature, the difference in temperature between the individual bearing ring components, and the resultant elastohydrodynamic (EHD)film thicknesses. Bearing life is independent of the oil delivery system except as it affects temperature. Cage slip increased with increases in speed. Cage slip as high as 7 percent was measured and was generally higher with air-oil mist lubrication than with oil-jet lubrication. C1 [Pinel, Stanley I.] Pinel Engn, Fullerton, CA 92821 USA. [Signer, Hans R.] Signer Tech Serv, Fullerton, CA USA. [Zaretsky, Erwin V.] NASA, Glenn Res Ctr, Cleveland, OH USA. RP Pinel, SI (reprint author), Pinel Engn, Fullerton, CA 92821 USA. NR 13 TC 0 Z9 0 U1 1 U2 3 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 APR PY 2011 VL 67 IS 4 BP 32 EP 41 PG 10 WC Engineering, Mechanical SC Engineering GA 744WL UT WOS:000289125800010 ER PT J AU Levit, C Marshall, W AF Levit, Creon Marshall, William TI Improved orbit predictions using two-line elements SO ADVANCES IN SPACE RESEARCH LA English DT Article DE Space debris; Conjunction analysis; Orbit prediction ID ACCURACY ASSESSMENT; SYSTEM; SATELLITES; PRECISION; CATALOG; LEO AB The density of orbital space debris constitutes an increasing environmental challenge. There are two ways to alleviate the problem: debris mitigation and debris removal. This paper addresses collision avoidance, a key aspect of debris mitigation. We describe a method that contributes to achieving a requisite increase in orbit prediction accuracy for objects in the publicly available two-line element (TLE) catalog. Batch least-squares differential correction is applied to the TLEs. Using a high-precision numerical propagator, we fit an orbit to state vectors derived from successive TLEs. We then propagate the fitted orbit further forward in time. These predictions are validated against precision ephemeris data derived from the international laser ranging service (ILRS) for several satellites, including objects in the congested sun-synchronous orbital region. The method leads to a predicted range error that increases at a typical rate of 100 m per day, approximately a 10-fold improvement oyer individual TLE's propagated with their associated analytic propagator (SGP4). Corresponding improvements for debris trajectories could potentially provide conjunction analysis sufficiently accurate for an operationally viable collision avoidance system based on TLEs only. We discuss additional optimization and the computational requirements for applying all-on-all conjunction analysis to the whole TLE catalog, present and near future. Finally, we outline a scheme for debris debris collision avoidance that may become practicable given these developments. Published by Elsevier Ltd. on behalf of COSPAR. C1 [Levit, Creon; Marshall, William] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Marshall, William] Univ Space Res Assoc, Moffett Field, CA 94035 USA. RP Levit, C (reprint author), NASA, Ames Res Ctr, MS202-3, Moffett Field, CA 94035 USA. EM creon.levit@nasa.gov NR 27 TC 14 Z9 23 U1 3 U2 20 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 APR 1 PY 2011 VL 47 IS 7 BP 1107 EP 1115 DI 10.1016/j.asr.2010.10.017 PG 9 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA 741PS UT WOS:000288876600001 ER PT J AU Yang, WW Ponce, A AF Yang, Wan-Wan Ponce, Adrian TI Validation of a Clostridium Endospore Viability Assay and Analysis of Greenland Ices and Atacama Desert Soils SO APPLIED AND ENVIRONMENTAL MICROBIOLOGY LA English DT Article ID GLACIER ICE; BACILLUS-SUBTILIS; BACTERIAL-SPORES; D-ALANINE; MICROORGANISMS; GERMINATION; CORE; ENVIRONMENTS; LIFE; DECONTAMINATION AB A microscopy-based endospore viability assay (micro-EVA) capable of enumerating germinable Clostridium endospores (GCEs) in less than 30 min has been validated and employed to determine GCE concentrations in Greenland ices and Atacama Desert soils. Inoculation onto agarose doped with Tb(3+) and D-alanine triggers Clostridium spore germination and the concomitant release of similar to 10(8) molecules of dipicolinic acid (DPA) per endospore, which, under pulsed UV excitation, enables enumeration of resultant green Tb(3+)-DPA luminescent spots as GCEs with time-gated luminescence microscopy. The intensity time courses of the luminescent spots were characteristic of stage I Clostridium spore germination dynamics. Micro-EVA was validated against traditional CFU cultivation from 0 to 1,000 total endospores/ml (i.e., phase-bright bodies/ml), yielding 56.4% +/- 1.5% GCEs and 43.0% +/- 1.0% CFU. We also show that D-alanine serves as a Clostridium-specific germinant (three species tested) that inhibits Bacillus germination of spores (five species tested) in that endospore concentration regime. Finally, GCE concentrations in Greenland ice cores and Atacama Desert soils were determined with micro-EVA, yielding 1 to 2 GCEs/ml of Greenland ice (versus <1 CFU/ml after 6 months of incubation) and 66 to 157 GCEs/g of Atacama Desert soil (versus 40 CFU/g soil). C1 [Ponce, Adrian] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Ponce, A (reprint author), CALTECH, Jet Prop Lab, M-S 183-301,4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM ponce@caltech.edu FU DHS Science and Technology Directorate; NASA Astrobiology Institute; Planetary Protection FX We are grateful to the DHS Science and Technology Directorate, NASA Astrobiology Institute, and Planetary Protection for funding. NR 44 TC 8 Z9 8 U1 0 U2 5 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 APR PY 2011 VL 77 IS 7 BP 2352 EP 2358 DI 10.1128/AEM.01966-10 PG 7 WC Biotechnology & Applied Microbiology; Microbiology SC Biotechnology & Applied Microbiology; Microbiology GA 741HT UT WOS:000288855500020 PM 21296951 ER PT J AU Bonfils, X Gillon, M Forveille, T Delfosse, X Deming, D Demory, BO Lovis, C Mayor, M Neves, V Perrier, C Santos, NC Seager, S Udry, S Boisse, I Bonnefoy, M AF Bonfils, X. Gillon, M. Forveille, T. Delfosse, X. Deming, D. Demory, B. -O. Lovis, C. Mayor, M. Neves, V. Perrier, C. Santos, N. C. Seager, S. Udry, S. Boisse, I. Bonnefoy, M. TI A short-period super-Earth orbiting the M2.5 dwarf GJ 3634 Detection with HARPS velocimetry and transit search with Spitzer photometry SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE techniques: radial velocities; stars: late-type; planetary systems ID EXTRA-SOLAR PLANETS; LOW-MASS STARS; MAIN-SEQUENCE; DETECTABILITY; METALLICITY; NEPTUNE; CATALOG AB We report on the detection of GJ 3634b, a super-Earth of mass m sin i = 7.0(-0.8)(+0.9) M(circle plus) and period P = 2.64561 +/- 0.00066 day. Its host star is a M2.5 dwarf, has a mass of 0.45 +/- 0.05 M(circle dot), a radius of 0.43 +/- 0.03 R(circle dot) and lies 19.8 +/- 0.6 pc away from our Sun. The planet is detected after a radial-velocity campaign using the ESO/Harps spectrograph. GJ 3634b had an a priori geometric probability to undergo transit of similar to 7% and, if telluric in composition, a non-grazing transit would produce a photometric dip of less than or similar to 0.1%. We therefore followed-up upon the RV detection with photometric observations using the 4.5-mu m band of the IRAC imager onboard Spitzer. Our six-hour long light curve excludes that a transit occurs for 2 sigma of the probable transit window, decreasing the probability that GJ 3634b undergoes transit to similar to 0.5%. C1 [Bonfils, X.; Forveille, T.; Delfosse, X.; Neves, V.; Perrier, C.; Bonnefoy, M.] UJF Grenoble 1, CNRS, INSU, IPAG,UMR 5274, F-38041 Grenoble, France. [Bonfils, X.; Gillon, M.; Lovis, C.; Mayor, M.; Udry, S.] Univ Geneva, Observ Geneva, CH-1290 Sauverny, Switzerland. [Gillon, M.] Univ Liege, Inst Astrophys & Geophys, B-4000 Liege, Belgium. [Deming, D.] NASA, Goddard Space Flight Ctr, Planetary Syst Branch, Greenbelt, MD 20771 USA. [Demory, B. -O.; Seager, S.] MIT, Dept Phys, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA. [Neves, V.; Santos, N. C.; Boisse, I.] Univ Porto, Ctr Astrofis, P-4150762 Oporto, Portugal. [Santos, N. C.] Univ Porto, Fac Ciencias, Dept Fis & Astron, P-4150762 Oporto, Portugal. RP Bonfils, X (reprint author), UJF Grenoble 1, CNRS, INSU, IPAG,UMR 5274, F-38041 Grenoble, France. EM Xavier.Bonfils@obs.ujf-grenoble.fr RI Santos, Nuno/E-9957-2011; OI Santos, Nuno/0000-0003-4422-2919; Bonfils, Xavier/0000-0001-9003-8894 FU European Research Council/European Community; Fundacao para a Ciencia e a Tecnologia (FCT), Portugal [PTDC/CTE-AST/098528/2008, PTDC/CTE-AST/098604/2008, SFRH/BD/60688/2009]; POPH/FSE (EC) FX We thank the anonymous referee for his careful reading and suggestions. M. G. is FNRS Research Associate. N.C.S., V.N. and I. B. acknowedge the support by the European Research Council/European Community under the FP7 through a Starting Grant, as well as in the form of grants reference PTDC/CTE-AST/098528/2008, PTDC/CTE-AST/098604/2008 and SFRH/BD/60688/2009, funded by Fundacao para a Ciencia e a Tecnologia (FCT), Portugal. NCS would further like to thank the support from FCT through a Ciencia 2007 contract funded by FCT/MCTES (Portugal) and POPH/FSE (EC). NR 40 TC 16 Z9 16 U1 0 U2 3 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD APR PY 2011 VL 528 AR A111 DI 10.1051/0004-6361/201015981 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 737BD UT WOS:000288541600151 ER PT J AU Canuto, VM AF Canuto, V. M. TI Stellar mixing V. Overshooting SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE turbulence; diffusion; convection; hydrodynamics; methods: analytical; stars: rotation ID SOLAR CONVECTION ZONE; INTERNAL-ROTATION; MERIDIONAL FLOW; STARS; TURBULENCE; EXTENT AB Helio-seismological data suggest an overshooting (OV) extent of 0.07 H-p (H-p is the pressure scale height), while theoretical predictions from both models and numerical simulations yield values that are an order of magnitude higher. The reason identified by the authors of numerical simulations is the limited range of physical parameters allowed by the numerical simulations compared to the true solar values; specifically, the simulations are still too viscous. In the case of theoretical models, we discuss limitations that at present cannot be solved. For these reasons, we propose and work out a different methodology, which has in principle the following advantages. First, there is no longer a need to model the flux of turbulent kinetic energy, which has been a stumbling block for many years and whose modeling has introduced uncertainties that are difficult to control. Second, we account for processes not included before: shear (differential rotation), meridional currents, gravitational energy, stable-unstable stratification, and double diffusion. C1 [Canuto, V. M.] Goddard Inst Space Studies, NASA, New York, NY 10025 USA. [Canuto, V. M.] Columbia Univ, Dept Appl Phys & Appl Math, New York, NY 10027 USA. RP Canuto, VM (reprint author), Goddard Inst Space Studies, NASA, New York, NY 10025 USA. EM vmc13@columbia.edu NR 24 TC 7 Z9 7 U1 0 U2 4 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD APR PY 2011 VL 528 AR A80 DI 10.1051/0004-6361/201014450 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 737BD UT WOS:000288541600024 ER PT J AU Canuto, VM AF Canuto, V. M. TI Stellar Mixing IV. The angular momentum problem SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE turbulence; diffusion; convection; hydrodynamics; methods: analytical; stars: rotation ID INTERNAL GRAVITY-WAVES; REYNOLDS STRESS MODEL; LOW-MASS STARS; TURBULENT CONVECTION; DIFFERENTIAL ROTATION; SOLAR INTERIOR; MAIN-SEQUENCE; TRANSPORT; FORMALISM; FLOWS AB We present a formalism that provides the Reynolds stresses needed to solve the angular momentum equation. The traditional Reynolds stress model assumes that the only contribution comes from shear (a down-gradient flux), but this leads to an extraction of angular momentum from the interior that is far too small compared to what is required to explain the helio seismological data. An illustrative solution of the new Reynolds stress equations shows that the presence of vorticity in a stably stratified regime, such as the one in the radiative zone, contributes a new term to the angular momentum equation that has an up-gradient flux like the one provided by the IGW model (internal gravity waves). The time scale entailed by such a term may be of the same order of 10(7) yrs produced by the IGW model. It would be instructive to solve the new angular momentum equation together with the formalism developed in Paper III to study not only the solar angular momentum distribution vs. helio data, but also the evolution of elements such as (7)Li and (4)He. These results would allow a more quantitative assessment of the overall model. The complete model yields Reynolds stresses that include differential rotation, unstable/stable stratification, double diffusion, radiative losses (arbitrary Peclet number), and meridional currents. C1 [Canuto, V. M.] Goddard Inst Space Studies, NASA, New York, NY 10025 USA. [Canuto, V. M.] Columbia Univ, Dept Appl Phys & Appl Math, New York, NY 10027 USA. RP Canuto, VM (reprint author), Goddard Inst Space Studies, NASA, New York, NY 10025 USA. EM vmc13@columbia.edu NR 28 TC 5 Z9 5 U1 0 U2 5 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 APR PY 2011 VL 528 AR A79 DI 10.1051/0004-6361/201014449 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 737BD UT WOS:000288541600023 ER PT J AU Canuto, VM AF Canuto, V. M. TI Stellar mixing III. The case of a passive tracer SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE diffusion; instabilities; turbulence; stars: interiors; convection; methods: analytical ID DIFFUSION-PROCESSES; RELEASE EXPERIMENT; SALT FINGERS; STARS; PYCNOCLINE; TURBULENCE; ROTATION AB In Papers I-II, we derived the expressions for the turbulent diffusivities of momentum, temperature T, and mean molecular weight mu. Since the scalar T-mu fields are active tracers (by influencing the density and thus the velocity field), whereas passive tracers such as(7)Li are carried along by the flow without influencing it, it would be unjustified to use the diffusivities of the T-mu fields to represent the diffusivity of passive tracers. In this paper, we present the first derivation of a passive tracer diffusivity. Some key results are: a) In the general 3D case, the passive tracer diffusivity is a tensor given in algebraic form; b) the diffusivity tensor depends on shear, vorticity, T, and mu-gradients, thus including double diffusion and differential rotation; c) in the 1D version of the model, the passive tracer diffusivity is a scalar denoted by K-c; d) in doubly stable regimes, del(mu) > 0, del - del(ad) < 0, K-c is nearly the same as those of the T-mu fields; e) in semi-convection regimes, del(mu) > 0, del - del(ad) > 0, K-c is larger than that of the mu-field; f) in salt fingers regimes del(mu) < 0, del - del(ad) < 0, K-c is smaller than that of the mu-field; and finally, g) in the only case we know of a direct measurement of a passive tracer diffusivity, the oceanographic North Atlantic Tracer Release Experiment (NATRE), the model reproduces the data quite closely. C1 [Canuto, V. M.] Goddard Inst Space Studies, NASA, New York, NY 10025 USA. [Canuto, V. M.] Columbia Univ, Dept Appl Phys & Appl Math, New York, NY 10027 USA. RP Canuto, VM (reprint author), Goddard Inst Space Studies, NASA, New York, NY 10025 USA. EM vmc13@columbia.edu NR 16 TC 4 Z9 4 U1 0 U2 4 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD APR PY 2011 VL 528 AR A78 DI 10.1051/0004-6361/201015372 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 737BD UT WOS:000288541600022 ER PT J AU Canuto, VM AF Canuto, V. M. TI Stellar mixing I. Formalism SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE turbulence; diffusion; convection; hydrodynamics; methods: analytical; stars: rotation ID TURBULENCE CLOSURE-MODEL; STABLY STRATIFIED FLOWS; LOW-MASS STARS; BOUNDARY-LAYER; DIFFERENTIAL ROTATION; RICHARDSON-NUMBER; SURFACE; CONVECTION; HEAT; STABILITY AB In this paper we use the Reynolds stress models (RSM) to derive algebraic expressions for the following variables: a) heat fluxes; b) mu fluxes; and c) momentum fluxes. These relations, which are fully 3D, include: 1) stable and unstable stratification, represented by the Brunt-Vaisala frequency, N-2 = -gH(p)(-1)(del - del(ad))(1 - R-mu); 2) double diffusion, salt-fingers, and semi-convection, represented by the density ratio R-mu = del(mu)(del - del(ad))(-1); 3) shear (differential rotation), represented by the mean squared shear Sigma(2) or by the Richardson number, Ri = N-2 Sigma(-2); 4) radiative losses represented by a Peclet number, Pe; 5) a complete analytical solution of the 1D version of the model. In general, the model requires the solution of two differential equations for the eddy kinetic energy K and its rate of dissipation, e. In the local and stationary cases, when production equals dissipation, the model equations are all algebraic. C1 [Canuto, V. M.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Canuto, V. M.] Columbia Univ, Dept Appl Phys & Appl Math, New York, NY 10027 USA. RP Canuto, VM (reprint author), NASA, Goddard Inst Space Studies, New York, NY 10025 USA. EM vmc13@columbia.edu NR 48 TC 14 Z9 14 U1 0 U2 4 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD APR PY 2011 VL 528 AR A76 DI 10.1051/0004-6361/201014447 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 737BD UT WOS:000288541600020 ER PT J AU Canuto, VM AF Canuto, V. M. TI Stellar mixing II. Double diffusion processes SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE turbulence; diffusion; convection; hydrodynamics; methods: analytical; stars: rotation ID LOW-MASS STARS; THERMOHALINE CONVECTION; RGB-STARS; ROTATION; BLUE; PYCNOCLINE; TURBULENCE; SEQUENCE; FINGERS; TRACER AB In this paper, salt-fingers (also called thermohaline convection) and semi-convection are treated under the name of double-diffusion (DD). We present and discuss the solutions of the RSM(Reynolds stress models) equations that provide the momentum, heat, mu fluxes, and their corresponding diffusivities denoted by K-m,K-h,K-mu. Such fluxes are given by a set of linear, algebraic equations that depend on the following variables: mean velocity gradient (differential rotation), temperature gradients (for both stable and unstable regimes), and mu-gradients (DD). Some key results are as follows. Salt-fingers. When shear is strong and DD is inefficient, heat and mu diffusivities are identical. Second, when shear is weak K-mu > K-h and the difference can be sizeable O(10) meaning that heat and mu diffusivities must therefore be treated as different. Third, for strong-to-moderate shears and for R-mu less than 0.8, both heat and mu diffusivities are practically independent of R-mu. Fourth, the latter result favors parameterizations of the type K-h,K-mu similar to CR mu 0 suggested by some authors. Our results, however, show that C is not a constant but a linear function of the Reynolds number Re = epsilon(nu N-2)(-1) defined in terms of the kinematic viscosity nu, the Brunt-Vaisala frequency N, and the rate of energy input into the system, epsilon. Fifth, we suggest that epsilon is an essential ingredient that has been missing in all diffusivity models, but which ought to be present because without a source of energy, turbulence dies out and so does the turbulent mixing (for example, the turbulent kinetic energy is proportional to the power 2/3 of epsilon). Moreover, since different stellar environments have different epsilon, its presence is necessary for differentiating mixing regimes in different stars. Semi-convection. In this case the destabilizing effect is the T-gradient, and when shear is weak, K-h > K-mu. Since the model is symmetric under the change R-mu to R-mu(-1), most of the results obtained in the previous case can be translated to this case. C1 [Canuto, V. M.] Goddard Inst Space Studies, NASA, New York, NY 10025 USA. [Canuto, V. M.] Columbia Univ, Dept Appl Phys & Appl Math, New York, NY 10027 USA. RP Canuto, VM (reprint author), Goddard Inst Space Studies, NASA, New York, NY 10025 USA. EM vmc13@columbia.edu NR 27 TC 8 Z9 8 U1 0 U2 3 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD APR PY 2011 VL 528 AR A77 DI 10.1051/0004-6361/201014448 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 737BD UT WOS:000288541600021 ER PT J AU Giroletti, M Paragi, Z Bignall, H Doi, A Foschini, L Gabanyi, KE Reynolds, C Blanchard, J Campbell, RM Colomer, F Hong, X Kadler, M Kino, M van Langevelde, HJ Nagai, H Phillips, C Sekido, M Szomoru, A Tzioumis, AK AF Giroletti, M. Paragi, Z. Bignall, H. Doi, A. Foschini, L. Gabanyi, K. E. Reynolds, C. Blanchard, J. Campbell, R. M. Colomer, F. Hong, X. Kadler, M. Kino, M. van Langevelde, H. J. Nagai, H. Phillips, C. Sekido, M. Szomoru, A. Tzioumis, A. K. TI Global e-VLBI observations of the gamma-ray narrow line Seyfert 1 PMN J0948+0022 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE galaxies: active; galaxies: Seyfert; galaxies: jets; instrumentation: high angular resolution; instrumentation: interferometers ID ACTIVE GALACTIC NUCLEI; LARGE-AREA TELESCOPE; RADIO-LOUD; RELATIVISTIC JET; QUASAR; EMISSION; DISCOVERY; GALAXIES AB Context. There is growing evidence of relativistic jets in radio-loud narrow-line Seyfert 1 (RL-NLS1) galaxies. Aims. We constrain the observational properties of the radio emission in the first RL-NLS1 galaxy ever detected in gamma-rays, PMN J0948+0022, i.e., its flux density and structure in both total intensity and polarization, its compactness, and variability. Methods. We performed three real-time e-VLBI observations of PMN J0948+0022 at 22 GHz, using a global array including telescopes in Europe, East Asia, and Australia. These are the first e-VLBI science observations ever carried out with a global array, reaching a maximum baseline length of 12 458 km. The observations were part of a large multiwavelength campaign in 2009. Results. The source is detected at all three epochs. The structure is dominated by a bright component, more compact than 55 mu as, with a fainter component at a position angle theta similar to 35 degrees. Relativistic beaming is required by the observed brightness temperature of 3.4 x 10(11) K. Polarization is detected at a level of about 1%. Conclusions. The parameters derived by the VLBI observations, in addition to the broad-band properties, confirm that PMN J0948+0022 is similar to flat spectrum radio quasars. Global e-VLBI is a reliable and promising technique for future studies. C1 [Giroletti, M.] INAF Ist Radioastron, I-40129 Bologna, Italy. [Paragi, Z.; Campbell, R. M.; van Langevelde, H. J.; Szomoru, A.] Joint Inst VLBI Europe, NL-7990 AA Dwingeloo, Netherlands. [Paragi, Z.; Gabanyi, K. E.] MTA Res Grp Phys Geodesy & Geodynam, H-1521 Budapest, Hungary. [Bignall, H.; Reynolds, C.] Curtin Univ, ICRAR Curtin Inst Radio Astron, Perth, WA 6845, Australia. [Doi, A.; Nagai, H.] JAXA, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2298510, Japan. [Foschini, L.] INAF Osservatorio Astron Brera, I-23807 Merate, Italy. [Gabanyi, K. E.] FOMI Satellite Geodet Observ, H-1592 Budapest, Hungary. [Blanchard, J.] Univ Tasmania, Dept Phys, Hobart, Tas 7001, Australia. [Colomer, F.] Observ Astron Nacl, Madrid 28014, Spain. [Hong, X.] Shanghai Astron Observ, Shanghai 200030, Peoples R China. [Kadler, M.] Univ Erlangen Nurnberg, Dr Remeis Sternwarte & ECAP, D-96049 Bamberg, Germany. [Kadler, M.] NASA, Goddard Space Flight Ctr, Ctr Res & Explorat Space Sci & Technol, Greenbelt, MD 20771 USA. [Kadler, M.] Univ Space Res Assoc, Columbia, MD 21044 USA. [Kino, M.] Natl Astron Observ Japan, Tokyo 1818588, Japan. [van Langevelde, H. J.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Phillips, C.; Tzioumis, A. K.] CSIRO Astron & Space Sci, Epping, NSW 1710, Australia. [Sekido, M.] NIICT, Kashima Space Res Ctr, Kashima, Ibaraki 314, Japan. RP Giroletti, M (reprint author), INAF Ist Radioastron, Via Gobetti 101, I-40129 Bologna, Italy. EM giroletti@ira.inaf.it RI Foschini, Luigi/H-3833-2012; Reynolds, Cormac/B-5635-2013; Bignall, Hayley/B-2867-2013; OI van Langevelde, Huib Jan/0000-0002-0230-5946; Foschini, Luigi/0000-0001-8678-0324; Reynolds, Cormac/0000-0002-8978-0626; Bignall, Hayley/0000-0001-6247-3071; Giroletti, Marcello/0000-0002-8657-8852; Kadler, Matthias/0000-0001-5606-6154 FU European Community [227290]; Italian Ministry of Foreign Affairs, Japan; Italian Ministry of Foreign Affairs, Italy; Communication Network Developments project "EXPReS" [02662]; Commonwealth of Australia FX The authors are grateful to Richard Dodson and Daniele Dallacasa for useful discussions on the polarization calibration, and to Uwe Bach for providing calibration data from the 100-m telescope of the MPIfR (Max-Planck-Institut fur Radioastronomie) at Effelsberg. This activity is supported by the European Community Framework Programme 7, Advanced Radio Astronomy in Europe, grant agreement No. 227290 and by the Italian Ministry of Foreign Affairs within the Scientific and Technology Cooperation Agreement between Japan and Italy. e-VLBI developments in Europe are supported by the EC DG-INFSO funded Communication Network Developments project "EXPReS", Contract No. 02662 (http://www.expres-eu.org/). The European VLBI Network (http://www.evlbi.org/) is a joint facility of European, Chinese, South African and other radio astronomy institutes funded by their national research councils. The Long Baseline Array is part of the Australia Telescope National Facility which is funded by the Commonwealth of Australia for operation as a National Facility managed by CSIRO. NR 27 TC 22 Z9 22 U1 0 U2 3 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD APR PY 2011 VL 528 AR L11 DI 10.1051/0004-6361/201116639 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 737BD UT WOS:000288541600011 ER PT J AU Gruber, D Kruhler, T Foley, S Nardini, M Burlon, D Rau, A Bissaldi, E von Kienlin, A McBreen, S Greiner, J Bhat, PN Briggs, MS Burgess, JM Chaplin, VL Connaughton, V Diehl, R Fishman, GJ Gibby, MH Giles, MM Goldstein, A Guiriec, S van der Horst, AJ Kippen, RM Kouveliotou, C Lin, L Meegan, CA Paciesas, WS Preece, RD Tierney, D Wilson-Hodge, C AF Gruber, D. Kruehler, T. Foley, S. Nardini, M. Burlon, D. Rau, A. Bissaldi, E. von Kienlin, A. McBreen, S. Greiner, J. Bhat, P. N. Briggs, M. S. Burgess, J. M. Chaplin, V. L. Connaughton, V. Diehl, R. Fishman, G. J. Gibby, M. H. Giles, M. M. Goldstein, A. Guiriec, S. van der Horst, A. J. Kippen, R. M. Kouveliotou, C. Lin, L. Meegan, C. A. Paciesas, W. S. Preece, R. D. Tierney, D. Wilson-Hodge, C. TI Fermi/GBM observations of the ultra-long GRB 091024 A burst with an optical flash SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE gamma-ray burst: general; gamma-ray burst: individual: GRB 091024 ID GAMMA-RAY-BURSTS; PROBE WMAP OBSERVATIONS; LAG-LUMINOSITY RELATION; LIGHT CURVES; PEAK LUMINOSITY; COSMOLOGICAL PARAMETERS; SPECTRAL EVOLUTION; BATSE OBSERVATIONS; AFTERGLOW; BRIGHT AB Aims. In this paper we examine gamma-ray and optical data of GRB 091024, a gamma-ray burst (GRB) with an extremely long duration of T-90 approximate to 1020 s, as observed with the Fermi Gamma-ray Burst Monitor (GBM). Methods. We present spectral analysis of all three distinct emission episodes using data from Fermi/GBM. Because of the long nature of this event, many ground-based optical telescopes slewed to its location within a few minutes and thus were able to observe the GRB during its active period. We compare the optical and gamma-ray light curves. Furthermore, we estimate a lower limit on the bulk Lorentz factor from the variability and spectrum of the GBM light curve and compare it with that obtained from the peak time of the forward shock of the optical afterglow. Results. From the spectral analysis we note that, despite its unusually long duration, this burst is similar to other long GRBs, i.e. there is spectral evolution (both the peak energy and the spectral index vary with time) and spectral lags are measured. We find that the optical light curve is highly anti-correlated to the prompt gamma-ray emission, with the optical emission reaching the maximum during an epoch of quiescence in the prompt emission. We interpret this behavior as the reverse shock (optical flash), expected in the internal-external shock model of GRB emission but observed only in a handful of GRBs so far. The lower limit on the initial Lorentz factor deduced from the variability time scale (Gamma(min) = 195(-110)(+ 90)) is consistent within the error to the one obtained using the peak time of the forward shock (Gamma(0) = 120) and is also consistent with Lorentz factors of other long GRBs. C1 [Gruber, D.; Kruehler, T.; Foley, S.; Nardini, M.; Burlon, D.; Rau, A.; Bissaldi, E.; von Kienlin, A.; Greiner, J.; Diehl, R.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Kruehler, T.] Tech Univ Munich, D-85748 Garching, Germany. [McBreen, S.; Tierney, D.] Univ Coll Dublin, Dublin 4, Ireland. [Bhat, P. N.; Briggs, M. S.; Burgess, J. M.; Chaplin, V. L.; Connaughton, V.; Goldstein, A.; Guiriec, S.; van der Horst, A. J.; Paciesas, W. S.; Preece, R. D.] Univ Alabama, NSSTC, Huntsville, AL 35805 USA. [Fishman, G. J.; Kouveliotou, C.; Wilson-Hodge, C.] NASA, George C Marshall Space Flight Ctr, Space Sci Off, Huntsville, AL 35812 USA. [Gibby, M. H.; Giles, M. M.] Jacobs Technol Inc, Huntsville, AL USA. [Kippen, R. M.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA. [Meegan, C. A.] Univ Space Res Assoc, NSSTC, Huntsville, AL 35805 USA. RP Gruber, D (reprint author), Max Planck Inst Extraterr Phys, Giessenbachstr,Postfach 1312, D-85748 Garching, Germany. EM dgruber@mpe.mpg.de RI Bissaldi, Elisabetta/K-7911-2016; OI Bissaldi, Elisabetta/0000-0001-9935-8106; Preece, Robert/0000-0003-1626-7335; Burgess, James/0000-0003-3345-9515; Kruehler, Thomas/0000-0002-8682-2384 FU German Bundesministerium fur Wirtschaft und Technologie (BMWi) via the Deutsches Zentrum fur Luft- und Raumfahrt (DLR) [50 QV 0301, 50 OG 0502]; Irish Research Council for Science, Engineering and Technology; Marie Curie Actions FX The GBM project is supported by the German Bundesministerium fur Wirtschaft und Technologie (BMWi) via the Deutsches Zentrum fur Luft- und Raumfahrt (DLR) under the contract numbers 50 QV 0301 and 50 OG 0502. S.F. acknowledges the support of the Irish Research Council for Science, Engineering and Technology, cofunded by Marie Curie Actions under FP7. NR 65 TC 25 Z9 25 U1 0 U2 4 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD APR PY 2011 VL 528 AR A15 DI 10.1051/0004-6361/201015891 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 737BD UT WOS:000288541600041 ER PT J AU Liuzzo, E Falomo, R Treves, A Donato, D Sambruna, M Arcidiacono, C Giovannini, G Farinato, J Moretti, A Ragazzoni, R Diolaiti, E Lombini, M Brast, R Donaldson, R Kolb, J Marchetti, E Tordo, S AF Liuzzo, E. Falomo, R. Treves, A. Donato, D. Sambruna, M. Arcidiacono, C. Giovannini, G. Farinato, J. Moretti, A. Ragazzoni, R. Diolaiti, E. Lombini, M. Brast, R. Donaldson, R. Kolb, J. Marchetti, E. Tordo, S. TI The jet of the BL Lacertae object PKS 2201+044: MAD near-IR adaptive optics observations and comparison with optical, radio and X-ray data SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE BL Lacertae objects: individual: PKS 2201+044; instrumentation: adaptive optics ID HUBBLE-SPACE-TELESCOPE; ACTIVE GALACTIC NUCLEI; M87 JET; HOST GALAXIES; EMISSION; CHANDRA; 3C-273; VARIABILITY; CANDIDATES; MORPHOLOGY AB Context. Relativistic jets are a common feature of radio loud active galactic nuclei. Multifrequency observations are a unique tool to constrain their physics. Aims. We report on a detailed study of the properties of the jet of the nearby BL Lac object PKS 2201+044, one of the rare cases where the jet is detected from radio to X-rays. Methods. We use new adaptive optics near-IR observations of the source, obtained with the ESO multi-conjugated adaptive optics demonstrator (MAD) at the Very Large Telescope. These observations acquired in Ground-Layer Adaptive Optics mode are combined with images previously achieved by HST, VLA and Chandra to perform a morphological and photometric study of the jet. Results. We find a noticeable similarity in the morphology of the jet at radio, near-IR and optical wavelengths. We construct the spectral shape of the main knot of jet that appears dominated by synchrotron radiation. Conclusions. On the basis of the jet morphology and the weak lines spectrum we suggest that PKS 2201+044 belongs to the class of radio sources intermediate between FRIs and FRIIs. C1 [Liuzzo, E.; Giovannini, G.; Brast, R.] INAF, Ist Radioastron, I-40129 Bologna, Italy. [Liuzzo, E.; Giovannini, G.] Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy. [Falomo, R.; Arcidiacono, C.; Farinato, J.; Moretti, A.; Ragazzoni, R.] INAF, Osservatorio Astron Padova, I-35122 Padua, Italy. [Treves, A.] Univ Insubria Como, INAF, Varese, Italy. [Treves, A.] Ist Nazl Fis Nucl, Milan, Italy. [Donato, D.; Sambruna, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Lombini, M.] INAF, Osservatorio Astron Bologna, I-40127 Bologna, Italy. [Donaldson, R.; Kolb, J.; Marchetti, E.; Tordo, S.] European So Observ, D-85748 Garching, Germany. RP Liuzzo, E (reprint author), INAF, Ist Radioastron, Via Gobetti 101, I-40129 Bologna, Italy. EM liuzzo@ira.inaf.it RI Moretti, Alessia/I-8361-2012; OI Farinato, Jacopo/0000-0002-5840-8362; Giovannini, Gabriele/0000-0003-4916-6362; lombini, matteo/0000-0002-5920-2139; Ragazzoni, Roberto/0000-0002-7697-5555; Falomo, Renato/0000-0003-4137-6541; Arcidiacono, Carmelo/0000-0003-0142-8108; Moretti, Alessia/0000-0002-1688-482X FU European Union; Valle D'Aosta Region; Italian Minister; National Aeronautics and Space Administration FX We wish to thank Teddy Cheung for his work on radio data reduction. This work was supported by contributions of European Union, Valle D'Aosta Region and the Italian Minister for Work and Welfare. This research has made use of the NASA/IPAC Extragalactic Data Base (NED), which is operated by the JPL, California Institute of Technology, under contract with the National Aeronautics and Space Administration. NR 44 TC 2 Z9 2 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 APR PY 2011 VL 528 AR A34 DI 10.1051/0004-6361/201015570 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 737BD UT WOS:000288541600046 ER PT J AU Puccetti, S Capalbi, M Giommi, P Perri, M Stratta, G Angelini, L Burrows, DN Campana, S Chincarini, G Cusumano, G Gehrels, N Moretti, A Nousek, J Osborne, JP Tagliaferri, G AF Puccetti, S. Capalbi, M. Giommi, P. Perri, M. Stratta, G. Angelini, L. Burrows, D. N. Campana, S. Chincarini, G. Cusumano, G. Gehrels, N. Moretti, A. Nousek, J. Osborne, J. P. Tagliaferri, G. TI The Swift serendipitous survey in deep XRT GRB fields (SwiftFT) I. The X-ray catalog and number counts SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE X-rays: general; surveys; catalogs; galaxies: active ID N-LOG S; CHANDRA MULTIWAVELENGTH PROJECT; POINT-SOURCE CATALOGS; MS SOURCE CATALOGS; LOCKMAN-HOLE; COSMOS FIELD; HELLAS2XMM SURVEY; NORTH SURVEY; SOUTH SURVEY; EVOLUTION AB Aims. An accurate census of the active galactic nuclei (AGN) is a key step in investigating the nature of the correlation between the growth and evolution of super massive black holes and galaxy evolution. X-ray surveys provide one of the most efficient ways of selecting AGN. Methods. We searched for X-ray serendipitous sources in over 370 Swift-XRT fields centered on gamma ray bursts detected between 2004 and 2008 and observed with total exposures ranging from 10 ks to over 1 Ms. This defines the Swift Serendipitous Survey in deep XRT GRB fields, which is quite broad compared to existing surveys (similar to 33 square degrees) and medium depth, with a faintest flux limit of 7.2 x 10(-16) erg cm(-2) s(-1) in the 0.5 to 2 keV energy range (4.8 x 10(-15) erg cm(-2) s(-1) at 50% completeness). The survey has a high degree of uniformity thanks to the stable point spread function and small vignetting correction factors of the XRT, moreover is completely random on the sky as GRBs explode in totally unrelated parts of the sky. Results. In this paper we present the sample and the X-ray number counts of the high Galactic-latitude sample, estimated with high statistics over a wide flux range (i.e., 7.2x10(-1)6 divided by similar to 5x10(-13) erg cm(-2) s(-1) in the 0.5-2 keV band and 3.4x10(-15)similar to divided by 6x10(-13) erg cm(-2) s(-1) in the 2-10 keV band). We detect 9387 point-like sources with a detection Poisson probability threshold of <= 2x10(-5), in at least one of the three energy bands considered (i.e. 0.3-3 keV, 2-10 keV, and 0.3-10 keV), for the total sample, while 7071 point-like sources are found at high Galactic-latitudes (i.e. |b|>= 20 deg). The large number of detected sources resulting from the combination of large area and deep flux limits make this survey a new important tool for investigating the evolution of AGN. In particular, the large area permits finding rare high-luminosity objects like QSO2, which are poorly sampled by other surveys, adding precious information for the luminosity function bright end. The high Galactic-latitude log N-log S relation is well determined over all the flux coverage, and it is nicely consistent with previous results at 1 sigma confidence level. By the hard X-ray color analysis, we find that the Swift Serendipitous Survey in deep XRT GRB fields samples relatively unobscured and mildly obscured AGN, with a fraction of obscured sources of similar to 37% (similar to 15%) in the 2-10 (0.3-3 keV) band. C1 [Puccetti, S.; Capalbi, M.; Giommi, P.; Perri, M.; Stratta, G.] ASI Sci Data Ctr, I-00044 Frascati, Italy. [Angelini, L.; Gehrels, N.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Burrows, D. N.; Nousek, J.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Campana, S.; Chincarini, G.; Moretti, A.; Tagliaferri, G.] Osserv Astron Brera, INAF, I-23807 Merate, LC, Italy. [Chincarini, G.] Univ Milano Bicocca, Dipartimento Fis, I-20126 Milan, Italy. [Cusumano, G.] Ist Astrofis Spaziale & Fis Cosm Palermo, INAF, I-90146 Palermo, Italy. [Osborne, J. P.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. RP Puccetti, S (reprint author), ASI Sci Data Ctr, Via Galileo Galilei, I-00044 Frascati, Italy. EM puccetti@asdc.asi.it RI Gehrels, Neil/D-2971-2012; Stratta, Maria Giuliana/L-3045-2016; OI Stratta, Maria Giuliana/0000-0003-1055-7980; Campana, Sergio/0000-0001-6278-1576; giommi, paolo/0000-0002-2265-5003; Cusumano, Giancarlo/0000-0002-8151-1990; moretti, alberto/0000-0002-9770-0315; Puccetti, Simonetta/0000-0002-2734-7835; Perri, Matteo/0000-0003-3613-4409; Tagliaferri, Gianpiero/0000-0003-0121-0723 FU STFC FX S.P. acknowledges F. Fiore for the useful discussions. J.P.O. acknowledges the support of the STFC. We acknowledge the anonymous referee for his comments, that helped improving the quality of the manuscript. NR 49 TC 19 Z9 19 U1 0 U2 3 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD APR PY 2011 VL 528 AR A122 DI 10.1051/0004-6361/201015560 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 737BD UT WOS:000288541600167 ER PT J AU Ricci, D Poels, J Elyiv, A Finet, F Sprimont, PG Anguita, T Bozza, V Browne, P Burgdorf, M Novati, SC Dominik, M Dreizler, S Glitrup, M Grundahl, F Harpsoe, K Hessman, F Hinse, TC Hornstrup, A Hundertmark, M Jorgensen, UG Liebig, C Maier, G Mancini, L Masi, G Mathiasen, M Rahvar, S Scarpetta, G Skottfelt, J Snodgrass, C Southworth, J Teuber, J Thone, CC Wambsganss, J Zimmer, F Zub, M Surdej, J AF Ricci, D. Poels, J. Elyiv, A. Finet, F. Sprimont, P. G. Anguita, T. Bozza, V. Browne, P. Burgdorf, M. Novati, S. Calchi Dominik, M. Dreizler, S. Glitrup, M. Grundahl, F. Harpsoe, K. Hessman, F. Hinse, T. C. Hornstrup, A. Hundertmark, M. Jorgensen, U. G. Liebig, C. Maier, G. Mancini, L. Masi, G. Mathiasen, M. Rahvar, S. Scarpetta, G. Skottfelt, J. Snodgrass, C. Southworth, J. Teuber, J. Thone, C. C. Wambsganss, J. Zimmer, F. Zub, M. Surdej, J. TI Flux and color variations of the quadruply imaged quasar HE 0435-1223 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE quasars: general; gravitational lensing: weak; techniques: photometric ID GRAVITATIONAL LENS; TIME-DELAY; GALAXY; QSO; HE-0435-1223; VARIABILITY; Q2237+0305 AB Aims. We present VRi photometric observations of the quadruply imaged quasar HE0435-1223, carried out with the Danish 1.54 m telescope at the La Silla Observatory. Our aim was to monitor and study the magnitudes and colors of each lensed component as a function of time. Methods. We monitored the object during two seasons (2008 and 2009) in the VRi spectral bands, and reduced the data with two independent techniques: difference imaging and point spread function (PSF) fitting. Results. Between these two seasons, our results show an evident decrease in flux by approximate to 0.2-0.4 magnitudes of the four lensed components in the three filters. We also found a significant increase (approximate to 0.05-0.015) in their V - R and R - i color indices. Conclusions. These flux and color variations are very likely caused by intrinsic variations of the quasar between the observed epochs. Microlensing effects probably also affect the brightest "A" lensed component. C1 [Ricci, D.; Poels, J.; Elyiv, A.; Finet, F.; Sprimont, P. G.; Surdej, J.] Univ Liege, Dept Astrophys Geophys & Oceanog, B-4000 Liege 1, Belgium. [Elyiv, A.] Ukrainian Acad Sci, Main Astron Observ, UA-03680 Kiev, Ukraine. [Anguita, T.] Pontificia Univ Catolica Chile, Dept Astron & Astrofis, Ctr Astro Ingn, Santiago, Chile. [Anguita, T.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Bozza, V.; Novati, S. Calchi; Mancini, L.; Scarpetta, G.] Univ Salerno, Dipartimento Fis ER Caianiello, I-84085 Fisciano, SA, Italy. [Bozza, V.; Scarpetta, G.] Inst Nazl Fis Nucl, Sez Napoli, Milan, Italy. [Browne, P.; Dominik, M.; Liebig, C.] Univ St Andrews, Sch Phys & Astron, SUPA, St Andrews KY16 9SS, Fife, Scotland. [Burgdorf, M.] Univ Stuttgart, Deutsch SOFIA Inst, D-70569 Stuttgart, Germany. [Novati, S. Calchi; Mancini, L.] IIASS, Vietri Sul Mare, SA, Italy. [Dreizler, S.; Hessman, F.; Hundertmark, M.] Univ Gottingen, Inst Astrophys, D-37077 Gottingen, Germany. [Glitrup, M.; Grundahl, F.] Aarhus Univ, Dept Phys & Astron, DK-8000 Aarhus C, Denmark. [Harpsoe, K.; Hinse, T. C.; Jorgensen, U. G.; Mathiasen, M.; Skottfelt, J.; Teuber, J.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen O, Denmark. [Hinse, T. C.] KASI Korea Astron & Space Sci Inst, Taejon 305348, South Korea. [Hornstrup, A.] Tech Univ Denmark, Natl Space Inst, DK-2800 Lyngby, Denmark. [Liebig, C.; Maier, G.; Wambsganss, J.; Zimmer, F.; Zub, M.] Univ Heidelberg, Astron Rechen Inst, Zentrum Astron, D-69120 Heidelberg, Germany. [Mancini, L.] Univ Sannio, Dipartimento Ingn, I-82100 Benevento, Italy. [Masi, G.] Ctr Backyard Astrophys, Bellatrix Astron Observ, Ceccano, FR, Italy. [Rahvar, S.] Sharif Univ Technol, Dept Phys, Tehran, Iran. [Snodgrass, C.] European So Observ, Santiago 19, Chile. [Snodgrass, C.] Max Planck Inst Solar Syst Res, D-37191 Katlenburg Lindau, Germany. [Southworth, J.] Univ Keele, Astrophys Grp, Newcastle Under Lyme ST5 5BG, England. [Thone, C. C.] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen, Denmark. [Thone, C. C.] INAF, Osservatorio Astron Brera, I-23807 Merate, Italy. [Burgdorf, M.] NASA, Ames Res Ctr, SOFIA Sci Ctr, Moffett Field, CA 94035 USA. [Harpsoe, K.; Jorgensen, U. G.] Geol Museum, Ctr Star & Planet Format, DK-1350 Copenhagen, Denmark. RP Ricci, D (reprint author), Univ Liege, Dept Astrophys Geophys & Oceanog, Bat B5C, B-4000 Liege 1, Belgium. EM ricci@astro.ulg.ac.be RI Zimmer, Fabian/M-4765-2014; Hundertmark, Markus/C-6190-2015; Rahvar, Sohrab/A-9350-2008; OI Hundertmark, Markus/0000-0003-0961-5231; Rahvar, Sohrab/0000-0002-7084-5725; Dominik, Martin/0000-0002-3202-0343; Thone, Christina/0000-0002-7978-7648; Ricci, Davide/0000-0002-9790-0552; Snodgrass, Colin/0000-0001-9328-2905 FU ARC - Action de recherche concertee (Communaute Francaise de Belgique - Academie Wallonie-Europe); Belgian Federal Science Policy Office; Department of Culture, Arts & Leisure (DCAL), Northern Ireland, UK FX The research was supported by ARC - Action de recherche concertee (Communaute Francaise de Belgique - Academie Wallonie-Europe). A.E. is the beneficiary of a fellowship granted by the Belgian Federal Science Policy Office. Astronomical research at Armagh Observatory is funded by the Department of Culture, Arts & Leisure (DCAL), Northern Ireland, UK. Operation of the Danish 1.54 m telescope is supported by the Danish National Science Research Council (FNU). We wish to thank the anonymous referee for the remarks and the suggestions. NR 27 TC 9 Z9 9 U1 0 U2 4 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD APR PY 2011 VL 528 AR A42 DI 10.1051/0004-6361/201016188 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 737BD UT WOS:000288541600048 ER PT J AU Abdo, AA Ackermann, M Ajello, M Antolini, E Baldini, L Ballet, J Barbiellini, G Bastieri, D Bechtol, K Bellazzini, R Berenji, B Blandford, RD Bonamente, E Borgland, AW Bregeon, J Brez, A Brigida, M Bruel, P Buehler, R Buson, S Caliandro, GA Cameron, RA Cannon, A Caraveo, PA Carrigan, S Casandjian, JM Cecchi, C Celik, O Charles, E Chekhtman, A Cheung, CC Chiang, J Ciprini, S Claus, R Cohen-Tanugi, J Conrad, J Costamante, L Cutini, S Dermer, CD de Palma, F Donato, D Silva, EDE Drell, PS Dubois, R Escande, L Favuzzi, C Fegan, SJ Finke, J Focke, WB Fortin, P Frailis, M Fukazawa, Y Funk, S Fusco, P Gargano, F Gasparrini, D Gehrels, N Germani, S Giglietto, N Giordano, F Giroletti, M Glanzman, T Godfrey, G Grenier, IA Guiriec, S Hadasch, D Hayashida, M Hays, E Hughes, RE Itoh, R Johannesson, G Johnson, AS Johnson, WN Kamae, T Katagiri, H Kataoka, J Knodlseder, J Kuss, M Lande, J Larsson, S Latronico, L Lee, SH Garde, ML Longo, F Loparco, F Lott, B Lovellette, MN Lubrano, P Makeev, A Mazziotta, MN McEnery, JE Mehault, J Michelson, PF Mizuno, T Monte, C Monzani, ME Morselli, A Moskalenko, IV Murgia, S Nakamori, T Naumann-Godo, M Nishino, 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 Pelassa, V Pepe, M Pesce-Rollins, M Piron, F Porter, TA Raino, S Rando, R Razzano, M Reimer, A Reimer, O Ritz, S Roth, M Sadrozinski, HFW Sanchez, D Sander, A Schinzel, FK Sgro, C Siskind, EJ Smith, PD Sokolovsky, KV Spandre, G Spinelli, P Strickman, MS Suson, DJ Takahashi, H Tanaka, T Thayer, JB Thayer, JG Thompson, DJ Tibaldo, L Torres, DF Tosti, G Tramacere, A Uehara, T Usher, TL Vandenbroucke, J Vasileiou, V Vilchez, N Vitale, V Waite, AP Wallace, E Wang, P Winer, BL Wood, KS Yang, Z Ylinen, T Ziegler, M Berdyugin, A Boettcher, M Carraminana, A Carrasco, L de la Fuente, E Diltz, C Hovatta, T Kadenius, V Kovalev, YY Lahteenmaki, A Lindfors, E Marscher, AP Nilsson, K Pereira, D Reinthal, R Roustazadeh, P Savolainen, T Sillanpaa, A Takalo, LO Tornikoski, M AF Abdo, A. A. Ackermann, M. Ajello, M. Antolini, E. Baldini, L. Ballet, J. Barbiellini, G. Bastieri, D. Bechtol, K. Bellazzini, R. Berenji, B. Blandford, R. D. Bonamente, E. Borgland, A. W. Bregeon, J. Brez, A. Brigida, M. Bruel, P. Buehler, R. Buson, S. Caliandro, G. A. Cameron, R. A. Cannon, A. Caraveo, P. A. Carrigan, S. Casandjian, J. M. Cecchi, C. Celik, Oe Charles, E. Chekhtman, A. Cheung, C. C. Chiang, J. Ciprini, S. Claus, R. Cohen-Tanugi, J. Conrad, J. Costamante, L. Cutini, S. Dermer, C. D. de Palma, F. Donato, D. do Couto e Silva, E. Drell, P. S. Dubois, R. Escande, L. Favuzzi, C. Fegan, S. J. Finke, J. Focke, W. B. Fortin, P. Frailis, M. Fukazawa, Y. Funk, S. Fusco, P. Gargano, F. Gasparrini, D. Gehrels, N. Germani, S. Giglietto, N. Giordano, F. Giroletti, M. Glanzman, T. Godfrey, G. Grenier, I. A. Guiriec, S. Hadasch, D. Hayashida, M. Hays, E. Hughes, R. E. Itoh, R. Johannesson, G. Johnson, A. S. Johnson, W. N. Kamae, T. Katagiri, H. Kataoka, J. Knoedlseder, J. Kuss, M. Lande, J. Larsson, S. Latronico, L. Lee, S. -H. Garde, M. Llena Longo, F. Loparco, F. Lott, B. Lovellette, M. N. Lubrano, P. Makeev, A. Mazziotta, M. N. McEnery, J. E. Mehault, J. Michelson, P. F. Mizuno, T. Monte, C. Monzani, M. E. Morselli, A. Moskalenko, I. V. Murgia, S. Nakamori, T. Naumann-Godo, M. Nishino, 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. Pelassa, V. Pepe, M. Pesce-Rollins, M. Piron, F. Porter, T. A. Raino, S. Rando, R. Razzano, M. Reimer, A. Reimer, O. Ritz, S. Roth, M. Sadrozinski, H. F. -W. Sanchez, D. Sander, A. Schinzel, F. K. Sgro, C. Siskind, E. J. Smith, P. D. Sokolovsky, K. V. Spandre, G. Spinelli, P. Strickman, M. S. Suson, D. J. Takahashi, H. Tanaka, T. Thayer, J. B. Thayer, J. G. Thompson, D. J. Tibaldo, L. Torres, D. F. Tosti, G. Tramacere, A. Uehara, T. Usher, T. L. Vandenbroucke, J. Vasileiou, V. Vilchez, N. Vitale, V. Waite, A. P. Wallace, E. Wang, P. Winer, B. L. Wood, K. S. Yang, Z. Ylinen, T. Ziegler, M. Berdyugin, A. Boettcher, M. Carraminana, A. Carrasco, L. de la Fuente, E. Diltz, C. Hovatta, T. Kadenius, V. Kovalev, Y. Y. Lahteenmaki, A. Lindfors, E. Marscher, A. P. Nilsson, K. Pereira, D. Reinthal, R. Roustazadeh, P. Savolainen, T. Sillanpaa, A. Takalo, L. O. Tornikoski, M. TI THE FIRST FERMI MULTIFREQUENCY CAMPAIGN ON BL LACERTAE: CHARACTERIZING THE LOW-ACTIVITY STATE OF THE EPONYMOUS BLAZAR SO ASTROPHYSICAL JOURNAL LA English DT Article DE BL Lacertae objects: general; BL Lacertae objects: individual (BL Lacertae); galaxies: jets; gamma rays: galaxies; radiation mechanisms: non-thermal; X-rays: galaxies ID LARGE-AREA TELESCOPE; RAY LIGHT CURVES; GAMMA-RAY; MULTIWAVELENGTH OBSERVATIONS; SPECTRAL VARIABILITY; GALACTIC NUCLEI; WEBT CAMPAIGNS; 1997 OUTBURST; OCTOBER 2007; EGRET DATA AB We report on observations of BL Lacertae during the first 18 months of Fermi LAT science operations and present results from a 48 day multifrequency coordinated campaign from 2008 August 19 to 2008 October 7. The radio to gamma-ray behavior of BL Lac is unveiled during a low-activity state thanks to the coordinated observations of radio-band (Metsahovi and VLBA), near-IR/optical (Tuorla, Steward, OAGH, and MDM), and X-ray (RXTE and Swift) observatories. No variability was resolved in gamma rays during the campaign, and the brightness level was 15 times lower than the level of the 1997 EGRET outburst. Moderate and uncorrelated variability has been detected in UV and X-rays. The X-ray spectrum is found to be concave, indicating the transition region between the low- and high-energy components of the spectral energy distribution (SED). VLBA observation detected a synchrotron spectrum self-absorption turnover in the innermost part of the radio jet appearing to be elongated and inhomogeneous, and constrained the average magnetic field there to be less than 3 G. Over the following months, BL Lac appeared variable in gamma rays, showing flares (in 2009 April and 2010 January). There is no evidence for the correlation of gamma rays with the optical flux monitored from the ground in 18 months. The SED may be described by a single-zone or a two-zone synchrotron self-Compton (SSC) model, but a hybrid SSC plus external radiation Compton model seems to be preferred based on the observed variability and the fact that it provides a fit closest to equipartition. C1 [Antolini, E.; Bonamente, E.; Cecchi, C.; Ciprini, S.; Germani, S.; Lubrano, P.; Pepe, M.; Tosti, G.] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy. [Abdo, A. A.; Chekhtman, A.; Cheung, C. C.; Dermer, C. D.; Finke, J.; Johnson, W. N.; Lovellette, M. N.; Makeev, A.; Parent, D.; Strickman, M. S.; Wood, K. S.] USN, Div Space Sci, Res Lab, Washington, DC 20375 USA. [Abdo, A. A.; Cheung, C. C.; Finke, J.] Natl Acad Sci, Natl Res Council Res Associate, Washington, DC 20001 USA. [Ackermann, M.; Ajello, M.; Bechtol, K.; Berenji, B.; Blandford, R. D.; Borgland, A. W.; Buehler, R.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; Costamante, L.; do Couto e Silva, E.; Drell, P. S.; Dubois, R.; Focke, W. B.; Funk, S.; Glanzman, T.; Godfrey, G.; Hayashida, M.; Johnson, A. S.; Kamae, T.; Lande, J.; Lee, S. -H.; Michelson, P. F.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Nolan, P. L.; Omodei, N.; Paneque, D.; Panetta, J. H.; Porter, T. A.; Reimer, A.; Reimer, O.; Tanaka, T.; Thayer, J. B.; Thayer, J. G.; Tramacere, A.; Usher, T. L.; Vandenbroucke, J.; Waite, A. P.; Wang, P.] Stanford Univ, Dept Phys, Kavli Inst Particle Astrophys & Cosmol, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA. [Ackermann, M.; Ajello, M.; Bechtol, K.; Berenji, B.; Blandford, R. D.; Borgland, A. W.; Buehler, R.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; Costamante, L.; do Couto e Silva, E.; Drell, P. S.; Dubois, R.; Focke, W. B.; Funk, S.; Glanzman, T.; Godfrey, G.; Hayashida, M.; Johnson, A. S.; Kamae, T.; Lande, J.; Lee, S. -H.; Michelson, P. F.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Nolan, P. L.; Omodei, N.; Paneque, D.; Panetta, J. H.; Porter, T. A.; Reimer, A.; Reimer, O.; Tanaka, T.; Thayer, J. B.; Thayer, J. G.; Tramacere, A.; Usher, T. L.; Vandenbroucke, J.; Waite, A. P.; Wang, P.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA. [Antolini, E.; Bonamente, E.; Cecchi, C.; Germani, S.; Lubrano, P.; Pepe, M.; Tosti, G.] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy. [Baldini, L.; Bellazzini, R.; Bregeon, J.; Brez, A.; Kuss, M.; Latronico, L.; 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.; Naumann-Godo, M.; Tibaldo, L.] Univ Paris Diderot, CEA Saclay, Serv Astrophys, Lab AIM,CEA IRFU,CNRS, F-91191 Gif Sur Yvette, France. [Barbiellini, G.; Longo, F.] Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy. [Barbiellini, G.; Longo, F.] Univ Trieste, Dipartimento Fis, I-34127 Trieste, Italy. [Bastieri, D.; Buson, S.; Rando, R.; Tibaldo, L.] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy. [Bastieri, D.; Buson, S.; Carrigan, S.; Rando, R.; Tibaldo, L.] Univ Padua, Dipartimento Fis G Galilei, I-35131 Padua, Italy. [Brigida, M.; 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.; de Palma, F.; Favuzzi, C.; Fusco, P.; Gargano, F.; Giglietto, N.; Giordano, F.; Loparco, F.; Mazziotta, M. N.; Monte, C.; Raino, S.; Spinelli, P.] Ist Nazl Fis Nucl, Sez Bari, I-70126 Bari, Italy. [Bruel, P.; Fegan, S. J.; Fortin, P.; Sanchez, D.] Ecole Polytech, CNRS, IN2P3, Lab Leprince Ringuet, F-91128 Palaiseau, France. [Caliandro, G. A.; Hadasch, D.; Torres, D. F.] Inst Ciencies Espai IEEC CSIC, Barcelona 08193, Spain. [Cannon, A.; Celik, Oe; Gehrels, N.; Hays, E.; McEnery, J. E.; Thompson, D. J.; Pereira, D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Cannon, A.] Univ Coll Dublin, Dublin 4, Ireland. [Caraveo, P. A.] INAF Ist Astrofis Spaziale & Fis Cosm, I-20133 Milan, Italy. [Celik, Oe; Donato, D.; Vasileiou, V.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Celik, Oe; Donato, D.; Vasileiou, V.] CRESST, Greenbelt, MD 20771 USA. [Celik, Oe; Vasileiou, V.] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA. [Celik, Oe; Vasileiou, V.] Univ Maryland Baltimore Cty, Ctr Space Sci & Technol, Baltimore, MD 21250 USA. [Chekhtman, A.; Makeev, A.; Parent, D.] George Mason Univ, Fairfax, VA 22030 USA. [Cohen-Tanugi, J.; Mehault, J.; Nuss, E.; Pelassa, V.; Piron, F.] Univ Montpellier 2, Lab Phys Theor & Astroparticules, CNRS, IN2P3, Montpellier, France. [Conrad, J.; Larsson, S.; Garde, M. Llena; Yang, Z.] Stockholm Univ, Dept Phys, SE-10691 Stockholm, Sweden. [Conrad, J.; Larsson, S.; Garde, M. Llena; Yang, Z.; Ylinen, T.] Oskar Klein Ctr Cosmoparticle Phys, SE-10691 Stockholm, Sweden. [Cutini, S.; Gasparrini, D.] Agenzia Spaziale Italiana ASI Sci Data Ctr, I-00044 Rome, Italy. [Donato, D.; McEnery, J. E.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA. [Donato, D.; McEnery, J. E.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Escande, L.; Lott, B.] Univ Bordeaux 1, CNRS, IN2P3, Ctr Etud Nucl Bordeaux Gradignan, F-33175 Gradignan, France. [Frailis, M.] Univ Udine, Dipartimento Fis, I-33100 Udine, Italy. [Frailis, M.] Ist Nazl Fis Nucl, Sez Trieste, Grp Collegato Udine, I-33100 Udine, Italy. [Frailis, M.] Ist Nazl Astrofis, Osservatorio Astron Trieste, I-34143 Trieste, Italy. [Fukazawa, Y.; Itoh, R.; Katagiri, H.; Mizuno, T.; Nishino, S.; Uehara, T.] Hiroshima Univ, Dept Phys Sci, Hiroshima 7398526, Japan. [Giroletti, M.] INAF Ist Radioastron, I-40129 Bologna, Italy. [Guiriec, S.] Univ Alabama, Ctr Space Plasma & Aeron Res, Huntsville, AL 35899 USA. [Hughes, R. E.; Sander, A.; Smith, P. D.; Winer, B. L.] Ohio State Univ, Dept Phys, Ctr Cosmol & Astro Particle Phys, Columbus, OH 43210 USA. [Johannesson, G.] Univ Iceland, Inst Sci, IS-107 Reykjavik, Iceland. [Kataoka, J.; Nakamori, T.] Waseda Univ, Res Inst Sci & Engn, Shinjuku Ku, Tokyo 1698555, Japan. [Knoedlseder, J.; Vilchez, N.] CNRS UPS, Ctr Etud Spatiale Rayonnements, F-30128 Toulouse 4, France. [Larsson, S.] Stockholm Univ, Dept Astron, SE-10691 Stockholm, Sweden. [Dermer, C. D.; 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. [Ohsugi, T.; Takahashi, H.] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Hiroshima 7398526, Japan. [Okumura, A.; Ozaki, M.] JAXA, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2298510, Japan. [Orlando, E.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Reimer, A.; Reimer, O.] Leopold Franzens Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria. [Reimer, A.; Reimer, O.] Leopold Franzens Univ Innsbruck, Inst Theoret Phys, A-6020 Innsbruck, Austria. [Ritz, S.; Sadrozinski, H. F. -W.; Ziegler, M.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA. [Ritz, S.; Sadrozinski, H. F. -W.; Ziegler, M.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Roth, M.; Wallace, E.] Univ Washington, Dept Phys, Seattle, WA 98195 USA. [Schinzel, F. K.; Sokolovsky, K. V.; Kovalev, Y. Y.; Savolainen, T.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Siskind, E. J.] NYCB Real Time Comp Inc, Lattingtown, NY 11560 USA. [Sokolovsky, K. V.; Kovalev, Y. Y.] PN Lebedev Phys Inst, Ctr Astro Space, Moscow 117810, Russia. [Suson, D. J.] Purdue Univ Calumet, Dept Chem & Phys, Hammond, IN 46323 USA. [Torres, D. F.] ICREA, Barcelona, Spain. [Tramacere, A.] CIFS, I-10133 Turin, Italy. [Tramacere, A.] INTEGRAL Sci Data Ctr, CH-1290 Versoix, Switzerland. [Vitale, V.] Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy. [Ylinen, T.] Royal Inst Technol KTH, Dept Phys, SE-10691 Stockholm, Sweden. [Ylinen, T.] Univ Kalmar, Sch Pure & Appl Nat Sci, SE-39182 Kalmar, Sweden. [Berdyugin, A.; Kadenius, V.; Lindfors, E.; Reinthal, R.; Sillanpaa, A.; Takalo, L. O.] Univ Turku, Tuorla Observ, FI-21500 Piikkio, Finland. [Boettcher, M.; Diltz, C.; Roustazadeh, P.] Ohio Univ, Dept Phys & Astron, Athens, OH 45701 USA. [Carraminana, A.; Carrasco, L.] Inst Nacl Astrofis Opt & Electr, Puebla 72840, Mexico. [de la Fuente, E.] Univ Guadalajara, CUCEI, Inst Astron & Meteorol, Guadalajara 44130, Jalisco, Mexico. [Hovatta, T.; Lahteenmaki, A.; Tornikoski, M.] Aalto Univ Metsahovi Radio Observ, FIN-02540 Kylmala, Finland. [Marscher, A. P.] Boston Univ, Inst Astrophys Res, Boston, MA 02215 USA. [Nilsson, K.] Univ Turku, Finnish Ctr Astron ESO FINCA, FI-21500 Piikkio, Finland. RP Ciprini, S (reprint author), Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy. EM elisa.antolini@tiscali.it; stefano.ciprini@pg.infn.it; davide.donato-1@nasa.gov; ksokolov@mpifr.de; gino.tosti@pg.infn.it RI Johnson, Neil/G-3309-2014; Kovalev, Yuri/J-5671-2013; Funk, Stefan/B-7629-2015; Sokolovsky, Kirill/D-2246-2015; 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; Orlando, E/R-5594-2016; Thompson, David/D-2939-2012; 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; Kuss, Michael/H-8959-2012; giglietto, nicola/I-8951-2012; Reimer, Olaf/A-3117-2013; Tosti, Gino/E-9976-2013; Ozaki, Masanobu/K-1165-2013; Rando, Riccardo/M-7179-2013; Lahteenmaki, Anne/L-5987-2013; Hays, Elizabeth/D-3257-2012; OI Kovalev, Yuri/0000-0001-9303-3263; Funk, Stefan/0000-0002-2012-0080; Sokolovsky, Kirill/0000-0001-5991-6863; 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; Frailis, Marco/0000-0002-7400-2135; 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; 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; Caraveo, Patrizia/0000-0003-2478-8018; Sgro', Carmelo/0000-0001-5676-6214; Savolainen, Tuomas/0000-0001-6214-1085; Rando, Riccardo/0000-0001-6992-818X; Bastieri, Denis/0000-0002-6954-8862; Omodei, Nicola/0000-0002-5448-7577; Pesce-Rollins, Melissa/0000-0003-1790-8018; Giroletti, Marcello/0000-0002-8657-8852 FU ASI-INAF [I/047/8/0]; Associated Universities, Inc.; Academy of Finland [212656, 210338]; NASA [NNX08AW56G, NNX09AU10G] FX S.C. acknowledges funding by ASI-INAF grant No. I/047/8/0 related to Fermi on-orbit activities.; This work includes observations obtained with the NASA Swift gamma-ray burst Explorer. Swift is a MIDEX Gamma Ray Burst mission led by NASA with participation of Italy and the UK. This work includes observations obtained with NASA Rossi XTE satellite. The ASM/RXTE teams at MIT and at the RXTE Science Operation Facility and Guest Observer Facility at NASA's GSFC are gratefully thanked. This work includes observations obtained with the Very Long Baseline Array, USA (project code BK150). The National Radio Astronomy Observatory (NRAO VLBA) is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. This work includes observations obtained with the 14 m Metsahovi Radio Observatory, a separate research institute of the Helsinki University of Technology. The Metsahovi team acknowledges the support from the Academy of Finland to our observing projects (numbers 212656, 210338, and others). This work includes observations obtained through the Tuorla Blazar Monitoring Program, carried out with the KVA telescope on La Palma, Canary Islands, and the 1 m telescope at Tuorla. Tuorla Observatory is a division of the Department of Physics and Astronomy at the University of Turku, Finland. This work includes observations obtained through the optical monitoring of BL Lac and other blazars using the 2.3 m Bok and 1.54 m Kuiper telescopes of Steward Observatory that is supported by NASA/Fermi Guest Investigator grants NNX08AW56G and NNX09AU10G. This work includes observations obtained with the 2.1 m telescope of the OAGH (Observatorio Astrofisico Guillermo Haro), in the state of Sonora, Mexico, operated by the Instituto Nacional de Astrofisica, Optica y Electronica (INAOE), Mexico. This work includes observations obtained with the 1.3 m McGraw-Hill Telescope of the Michigan-Dartmouth-MIT (MDM) observatory, operated by University of Michigan, Dartmouth College, Ohio State University, Ohio University, Columbia University, in Arizona, USA. NR 70 TC 27 Z9 27 U1 5 U2 17 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 APR 1 PY 2011 VL 730 IS 2 AR 101 DI 10.1088/0004-637X/730/2/101 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 735TR UT WOS:000288441900041 ER PT J AU Cook, AM Whittet, DCB Shenoy, SS Gerakines, PA White, DW Chiar, JE AF Cook, A. M. Whittet, D. C. B. Shenoy, S. S. Gerakines, P. A. White, D. W. Chiar, J. E. TI THE THERMAL EVOLUTION OF ICES IN THE ENVIRONMENTS OF NEWLY FORMED STARS: THE CO2 DIAGNOSTIC SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrochemistry; dust, extinction; evolution; infrared: ISM; ISM: molecules; stars: pre-main sequence ID SPITZER SPECTROSCOPIC SURVEY; YOUNG STELLAR OBJECTS; SOLID CARBON-DIOXIDE; TAURUS DARK CLOUDS; INFRARED-SPECTROSCOPY; MOLECULAR CLOUD; GRAIN MANTLES; INTERSTELLAR EXTINCTION; BACKGROUND STARS; SPACE-TELESCOPE AB Archival data from the Infrared Spectrometer of the Spitzer Space Telescope are used to study the 15 mu m absorption feature of solid CO2 toward 28 young stellar objects (YSOs) of approximately solar mass. Fits to the absorption profile using laboratory spectra enable categorization according to the degree of thermal processing of the ice matrix that contains the CO2. The majority of YSOs in our sample (20 out of 28) are found to be consistent with a combination of polar (H2O-rich) and nonpolar (CO-rich) ices at low temperature; the remainder exhibit profile structure consistent with partial crystallization as the result of significant heating. Ice-phase column densities of CO2 are determined and compared with those of other species. Lines of sight with crystallization signatures in their spectra are found to be systematically deficient in solid-phase CO, as expected if CO is being sublimated in regions where the ices are heated to crystallization temperatures. Significant variation is found in the CO2 abundance with respect to both H2O (the dominant ice constituent) and total dust column (quantified by the extinction, AV). YSOs in our sample display typically higher CO2 concentrations (independent of evidence for thermal processing) in comparison to quiescent regions of the prototypical cold molecular cloud. This suggests that enhanced CO2 production is driven by photochemical reactions in proximity to some YSOs, and that photoprocessing and thermal processing may occur independently. C1 [Cook, A. M.; Whittet, D. C. B.] Rensselaer Polytech Inst, New York Ctr Astrobiol, Troy, NY 12180 USA. [Cook, A. M.; Whittet, D. C. B.] Rensselaer Polytech Inst, Dept Phys Appl Phys & Astron, Troy, NY 12180 USA. [Shenoy, S. S.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Gerakines, P. A.; White, D. W.] Univ Alabama Birmingham, Dept Phys, Birmingham, AL 35294 USA. [Chiar, J. E.] SETI Inst, Mountain View, CA 94043 USA. RP Cook, AM (reprint author), NASA, Ames Res Ctr, Mail Stop 245-6, Moffett Field, CA 94035 USA. RI Gerakines, Perry/D-2226-2012; Gerakines, Perry/B-9705-2009; OI Gerakines, Perry/0000-0002-9667-5904; Whittet, Douglas/0000-0001-8539-3891 FU Spitzer [1264149, 1290823]; NASA [NNX07AK38G]; NASA Astrobiology Institute [NNA09DA80A]; NASA New York FX This work is based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. Financial support for this research was provided by the Spitzer General Observer and Archival Research Programs (JPL/Caltech Support Agreements nos. 1264149 and 1290823), the NASA Exobiology and Evolutionary Biology program (grant NNX07AK38G), the NASA Astrobiology Institute (grant NNA09DA80A), and the NASA New York Space Grant Consortium. We are grateful to an anonymous referee for helpful comments. NR 51 TC 15 Z9 15 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 APR 1 PY 2011 VL 730 IS 2 AR 124 DI 10.1088/0004-637X/730/2/124 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 735TR UT WOS:000288441900064 ER PT J AU Efremova, BV Bianchi, L Thilker, DA Neill, JD Burgarella, D Wyder, TK Madore, BF Rey, SC Barlow, TA Conrow, T Forster, K Friedman, PG Martin, DC Morrissey, P Neff, SG Schiminovich, D Seibert, M Small, T AF Efremova, Boryana V. Bianchi, Luciana Thilker, David A. Neill, James D. Burgarella, Denis Wyder, Ted K. Madore, Barry F. Rey, Soo-Chang Barlow, Tom A. Conrow, Tim Forster, Karl Friedman, Peter G. Martin, D. Christopher Morrissey, Patrick Neff, Susan G. Schiminovich, David Seibert, Mark Small, Todd TI THE RECENT STAR FORMATION IN NGC 6822: AN ULTRAVIOLET STUDY SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: individual (NGC 6822); galaxies: stellar content; Local Group; stars: formation; ultraviolet: stars ID HUBBLE-SPACE-TELESCOPE; H-II REGIONS; CURRENTLY FORMING STARS; INITIAL MASS FUNCTION; EMISSION-LINE STARS; GALAXY NGC-6822; MAGELLANIC-CLOUD; DUST ATTENUATION; DWARF GALAXIES; LMC CLUSTERS AB We characterize the star formation in the low-metallicity galaxy NGC 6822 over the past few hundred million years, using GALEX far-UV (FUV, 1344-1786 angstrom) and near-UV (NUV, 1771-2831 angstrom) imaging, and ground-based H alpha imaging. From the GALEX FUV image, we define 77 star-forming (SF) regions with area > 860 pc(2), and surface brightness less than or similar to 26.8 mag (AB) arcsec(-2), within 0 degrees.2 (1.7 kpc) of the center of the galaxy. We estimate the extinction by interstellar dust in each SF region from resolved photometry of the hot stars it contains: E(B - V) ranges from the minimum foreground value of 0.22 mag up to 0.66 +/- 0.21 mag. The integrated FUV and NUV photometry, compared with stellar population models, yields ages of the SF complexes up to a few hundred Myr, and masses from 2 x 10(2) M-circle dot to 1.5 x 10(6) M-circle dot. The derived ages and masses strongly depend on the assumed type of interstellar selective extinction, which we find to vary across the galaxy. The total mass of the FUV-defined SF regions translates into an average star formation rate (SFR) of 1.4 x 10(-2) M-circle dot yr(-1) over the past 100 Myr, and SFR = 1.0 x 10(-2) M-circle dot yr(-1) in the most recent 10 Myr. The latter is in agreement with the value that we derive from the H alpha luminosity, SFR = 0.008 M-circle dot yr(-1). The SFR in the most recent epoch becomes higher if we add the SFR = 0.02 M-circle dot yr(-1) inferred from far-IR measurements, which trace star formation still embedded in dust (age less than or similar to a few Myr). C1 [Efremova, Boryana V.; Bianchi, Luciana; Thilker, David A.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Neill, James D.; Wyder, Ted K.; Barlow, Tom A.; Conrow, Tim; Forster, Karl; Friedman, Peter G.; Martin, D. Christopher; Morrissey, Patrick; Small, Todd] CALTECH, Pasadena, CA 91125 USA. [Burgarella, Denis] Lab Astrophys Marseille, F-13376 Marseille 12, France. [Madore, Barry F.; Seibert, Mark] Observ Carnegie Inst Washington, Pasadena, CA 91101 USA. [Rey, Soo-Chang] Chungnam Natl Univ, Dept Astron & Space Sci, Taejon 305764, South Korea. [Rey, Soo-Chang; Neff, Susan G.] NASA, Goddard Space Flight Ctr, Lab Astron & Solar Phys, Greenbelt, MD 20771 USA. [Schiminovich, David] Columbia Univ, Dept Astron, New York, NY 10027 USA. RP Efremova, BV (reprint author), Johns Hopkins Univ, Dept Phys & Astron, 3400 N Charles St, Baltimore, MD 21218 USA. EM boryana@pha.jhu.edu; bianchi@pha.jhu.edu FU NASA [NAS5-26555]; NASA Office of Space Science [NAG5-7584]; NRF of Korea FX The GALEX data presented in this paper were obtained from the Multimission Archive at the Space Telescope Science Institute (MAST). STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. Support for MAST for non-HST data is provided by the NASA Office of Space Science via grant NAG5-7584 and by other grants and contracts. GALEX (The Galaxy Evolution Explorer) is a NASA Small Explorer, launched in 2003 April. We gratefully acknowledge NASA's support for construction, operation, and science analysis of the GALEX mission, developed in cooperation with the Centre National d'Etudes Spatiales of France and the Korean Ministry of Science and Technology. The H alpha image used in this paper was obtained by Massey et al. (2007a) as part of the Survey of Local Group Galaxies Currently Forming Stars and downloaded from http://www.archive.noao.edu/nsa/. S.-C.R. is supported by the NRF of Korea to the Center for Galaxy Evolution Research. NR 56 TC 14 Z9 14 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 1 PY 2011 VL 730 IS 2 AR 88 DI 10.1088/0004-637X/730/2/88 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 735TR UT WOS:000288441900028 ER PT J AU Gruesbeck, JR Lepri, ST Zurbuchen, TH Antiochos, SK AF Gruesbeck, Jacob R. Lepri, Susan T. Zurbuchen, Thomas H. Antiochos, Spiro K. TI CONSTRAINTS ON CORONAL MASS EJECTION EVOLUTION FROM IN SITU OBSERVATIONS OF IONIC CHARGE STATES SO ASTROPHYSICAL JOURNAL LA English DT Article DE atomic processes; plasmas; solar wind; Sun: coronal mass ejections (CMEs) ID ADVANCED COMPOSITION EXPLORER; SOLAR-WIND; PARTICLE-ACCELERATION; MAGNETIC-FIELD; FLARE; TEMPERATURE; SIGNATURES; PLASMA; MODEL; LASCO AB We present a novel procedure for deriving the physical properties of coronal mass ejections (CMEs) in the corona. Our methodology uses in situ measurements of ionic charge states of C, O, Si, and Fe in the heliosphere and interprets them in the context of a model for the early evolution of interplanetary CME (ICME) plasma, between 2 and 5R(circle dot). We find that the data are best fit by an evolution that consists of an initial heating of the plasma, followed by an expansion that ultimately results in cooling. The heating profile is consistent with a compression of coronal plasma due to flare reconnection jets and an expansion cooling due to the ejection, as expected from the standard CME/flare model. The observed frozen-in ionic charge states reflect this time history and, therefore, provide important constraints for the heating and expansion timescales, as well as the maximum temperature the CME plasma is heated to during its eruption. Furthermore, our analysis places severe limits on the possible density of CME plasma in the corona. We discuss the implications of our results for CME models and for future analysis of ICME plasma composition. C1 [Gruesbeck, Jacob R.; Lepri, Susan T.; Zurbuchen, Thomas H.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. [Antiochos, Spiro K.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Gruesbeck, JR (reprint author), Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. EM jagruesb@umich.edu RI Antiochos, Spiro/D-4668-2012; Lepri, Susan/I-8611-2012 OI Antiochos, Spiro/0000-0003-0176-4312; FU NASA [NNX08AI11G, NNX07AB99G, NNX08AM64G]; GSRP FX This work used the SOHO/LASCO CME catalog developed by NASA, NRL, and the Catholic University of America. SOHO is a project of international cooperation between ESA and NASA. This work was performed, in part, with support from NASA grants NNX08AI11G, NNX07AB99G, and NNX08AM64G, as well as the GSRP program. T.H.Z. acknowledges the hospitality of the International Space Science Institute, where much of this work was performed. S.K.A. was supported, in part by the NASA HTP and TR&T Programs. The authors thank Eric Christian for helpful discussions and comments on the manuscript. The authors thank Katherine Baldwin and Jim Raines for their early work, which was a foundation for this study. NR 54 TC 26 Z9 26 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 APR 1 PY 2011 VL 730 IS 2 AR 103 DI 10.1088/0004-637X/730/2/103 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 735TR UT WOS:000288441900043 ER PT J AU Kasliwal, MM Kulkarni, SR Arcavi, I Quimby, RM Ofek, EO Nugent, P Jacobsen, J Gal-Yam, A Green, Y Yaron, O Fox, DB Howell, JL Cenko, SB Kleiser, I Bloom, JS Miller, A Li, WD Filippenko, AV Starr, D Poznanski, D Law, NM Helou, G Frail, DA Neill, JD Forster, K Martin, DC Tendulkar, SP Gehrels, N Kennea, J Sullivan, M Bildsten, L Dekany, R Rahmer, G Hale, D Smith, R Zolkower, J Velur, V Walters, R Henning, J Bui, K McKenna, D Blake, C AF Kasliwal, Mansi M. Kulkarni, Shri R. Arcavi, Iair Quimby, Robert M. Ofek, Eran O. Nugent, Peter Jacobsen, Janet Gal-Yam, Avishay Green, Yoav Yaron, Ofer Fox, Derek B. Howell, Jacob L. Cenko, S. Bradley Kleiser, Io Bloom, Joshua S. Miller, Adam Li, Weidong Filippenko, Alexei V. Starr, Dan Poznanski, Dovi Law, Nicholas M. Helou, George Frail, Dale A. Neill, James D. Forster, Karl Martin, D. Christopher Tendulkar, Shriharsh P. Gehrels, Neil Kennea, Jamie Sullivan, Mark Bildsten, Lars Dekany, Richard Rahmer, Gustavo Hale, David Smith, Roger Zolkower, Jeff Velur, Viswa Walters, Richard Henning, John Bui, Kahnh McKenna, Dan Blake, Cullen TI PTF 10fqs: A LUMINOUS RED NOVA IN THE SPIRAL GALAXY MESSIER 99 SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars: AGB and post-AGB; stars: mass-loss; supernovae: general; supernovae: individual (PTF 10fqs); surveys ID OBSERVATORY SUPERNOVA SEARCH; SN 2008S; OPTICAL TRANSIENT; NEARBY GALAXIES; NGC 300; TELESCOPE; EVOLUTION; EMISSION; SPITZER; PERFORMANCE AB The Palomar Transient Factory (PTF) is systematically charting the optical transient and variable sky. A primary science driver of PTF is building a complete inventory of transients in the local universe (distance less than 200 Mpc). Here, we report the discovery of PTF 10fqs, a transient in the luminosity "gap" between novae and supernovae. Located on a spiral arm of Messier 99, PTF 10fqs has a peak luminosity of M-r = -12.3, red color (g - r = 1.0), and is slowly evolving (decayed by 1 mag in 68 days). It has a spectrum dominated by intermediate-width Ha (approximate to 930 km s(-1)) and narrow calcium emission lines. The explosion signature (the light curve and spectra) is overall similar to that of M85 OT2006-1, SN 2008S, and NGC 300 OT. The origin of these events is shrouded in mystery and controversy (and in some cases, in dust). PTF 10fqs shows some evidence of a broad feature (around 8600 angstrom) that may suggest very large velocities (approximate to 10,000 km s(-1)) in this explosion. Ongoing surveys can be expected to find a few such events per year. Sensitive spectroscopy, infrared monitoring, and statistics (e.g., disk versus bulge) will eventually make it possible for astronomers to unravel the nature of these mysterious explosions. C1 [Kasliwal, Mansi M.; Kulkarni, Shri R.; Quimby, Robert M.; Ofek, Eran O.; Neill, James D.; Forster, Karl; Martin, D. Christopher; Tendulkar, Shriharsh P.] CALTECH, Cahill Ctr Astrophys, Pasadena, CA 91125 USA. [Arcavi, Iair; Gal-Yam, Avishay; Green, Yoav; Yaron, Ofer] Weizmann Inst Sci, Benoziyo Ctr Astrophys, Fac Phys, IL-76100 Rehovot, Israel. [Nugent, Peter; Jacobsen, Janet; Poznanski, Dovi] Univ Calif Berkeley, Lawrence Berkeley Lab, Computat Cosmol Ctr, Berkeley, CA 94720 USA. [Fox, Derek B.; Howell, Jacob L.] Penn State Univ, Eberly Coll Sci, University Pk, PA 16802 USA. [Cenko, S. Bradley; Kleiser, Io; Bloom, Joshua S.; Miller, Adam; Li, Weidong; Filippenko, Alexei V.; Starr, Dan; Poznanski, Dovi] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Law, Nicholas M.] Univ Toronto, Dunlap Inst Astron & Astrophys, Toronto, ON M5S 3H4, Canada. [Helou, George] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA. [Frail, Dale A.] Natl Radio Astron Observ, Array Operat Ctr, Socorro, NM 87801 USA. [Gehrels, Neil] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Kennea, Jamie] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Sullivan, Mark] Univ Oxford, Dept Phys, Oxford OX1 3RH, England. [Bildsten, Lars] Univ Calif Santa Barbara, Kavli Inst Theoret Phys, Santa Barbara, CA 93106 USA. [Bildsten, Lars] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Dekany, Richard; Rahmer, Gustavo; Hale, David; Smith, Roger; Zolkower, Jeff; Velur, Viswa; Walters, Richard; Henning, John; Bui, Kahnh; McKenna, Dan] CALTECH, Caltech Opt Observ, Pasadena, CA 91125 USA. [Blake, Cullen] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. RP Kasliwal, MM (reprint author), CALTECH, Cahill Ctr Astrophys, Pasadena, CA 91125 USA. RI Gehrels, Neil/D-2971-2012; Green, Yoav/L-5874-2015; OI Green, Yoav/0000-0002-0809-6575; Sullivan, Mark/0000-0001-9053-4820 FU Gordon and Betty Moore Foundation; Israel Science Foundation; US-Israel Binational Science Foundation; Weizmann-UK; Marie Curie IRG fellowship; Peter and Patricia Gruber Award; Benoziyo Center for Astrophysics; Yeda-Sela center at the Weizmann Institute; National Science Foundation (NSF) [AST-0908886, PHY 05-51164, AST07-07633]; Sylvia & Jim Katzman Foundation; Richard & Rhoda Goldman Fund; Gary and Cynthia Bengier; TABASGO Foundation; NASA through Spitzer [1322321]; Space Telescope Science Institute [AR-11248]; NASA [NAS 5-26555]; DOE; Einstein fellowship; Harvard University; University of Virginia; Associated Universities, Inc. FX M.M.K. thanks the Gordon and Betty Moore Foundation for a Hale Fellowship in support of graduate study. The Weizmann Institute PTF participation is supported in part by the Israel Science Foundation via grants to A.G.Y. The Weizmann-Caltech collaborative PTF effort is supported by the US-Israel Binational Science Foundation. A.G.Y. and M. S. are jointly supported by the "making connections" Weizmann-UK program. A.G.Y. further acknowledges support by a Marie Curie IRG fellowship and the Peter and Patricia Gruber Award, as well as funding by the Benoziyo Center for Astrophysics and the Yeda-Sela center at the Weizmann Institute. A.V.F.'s group and KAIT are supported by National Science Foundation (NSF) grant AST-0908886, the Sylvia & Jim Katzman Foundation, the Richard & Rhoda Goldman Fund, Gary and Cynthia Bengier, and the TABASGO Foundation; additional funding was provided by NASA through Spitzer grant 1322321, as well as HST grant AR-11248 from the Space Telescope Science Institute, which is operated by Associated Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. J.S.B. and his group are partially funded by a DOE SciDAC grant. E.O.O. and D. P. are supported by the Einstein fellowship. L. B. is supported by the National Science Foundation under grants PHY 05-51164 and AST07-07633.; The Hobby-Eberly Telescope (HET) is a joint project of the University of Texas at Austin, the Pennsylvania State University, Stanford University, Ludwig-Maximillians-Universitat Munchen, and Georg-August-Universitat Gottingen. The HET is named in honor of its principal benefactors, William P. Hobby and Robert E. Eberly. The Marcario LRS is named for Mike Marcario of High Lonesome Optics, who fabricated several optics for the instrument but died before its completion; it is a joint project of the Hobby-Eberly Telescope partnership and the Instituto de Astronomia de la Universidad Nacional Autonoma de Mexico. GALEX (Galaxy Evolution Explorer) 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. PAIRITEL is operated by the Smithsonian Astrophysical Observatory (SAO) and was made possible by a grant from the Harvard University Milton Fund, the camera loan from the University of Virginia, and the continued support of the SAO and UC Berkeley. The Expanded Very Large Array is operated by the National Radio Astronomy Observatory, a facility of the NSF operated under cooperative agreement by Associated Universities, Inc. NR 53 TC 25 Z9 26 U1 0 U2 10 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 APR 1 PY 2011 VL 730 IS 2 AR 134 DI 10.1088/0004-637X/730/2/134 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 735TR UT WOS:000288441900074 ER PT J AU Livingstone, MA Ng, CY Kaspi, VM Gavriil, FP Gotthelf, EV AF Livingstone, Margaret A. Ng, C. -Y. Kaspi, Victoria M. Gavriil, Fotis P. Gotthelf, E. V. TI POST-OUTBURST OBSERVATIONS OF THE MAGNETICALLY ACTIVE PULSAR J1846-0258. A NEW BRAKING INDEX, INCREASED TIMING NOISE, AND RADIATIVE RECOVERY SO ASTROPHYSICAL JOURNAL LA English DT Article DE pulsars: general; pulsars: individual (PSR J1846-0258); supernovae: individual (Kes 75); X-rays: stars ID PROPORTIONAL COUNTER ARRAY; ROTATION-POWERED PULSAR; REMNANT KESTEVEN 75; X-RAY PULSARS; SPIN-DOWN; PSR J1846-0258; MAGNETAR SGR-1806-20; NEUTRON-STARS; VELA PULSAR; WIND NEBULA AB The similar to 800 year old pulsar J1846-0258 is a unique transition object between rotation-powered pulsars and magnetars: though behaving like a rotation-powered pulsar most of the time, in 2006 it exhibited a distinctly magnetar-like outburst accompanied by a large glitch. Here, we present X-ray timing observations taken with the Rossi X-ray Timing Explorer over a 2.2 year period after the X-ray outburst and glitch had recovered. We observe that the braking index of the pulsar, previously measured to be n = 2.65 +/- 0.01, is now n = 2.16 +/- 0.13, a decrease of 18% +/- 5%. We also note a persistent increase in the timing noise relative to the pre-outburst level. Despite the timing changes, a 2009 Chandra X-ray Observatory observation shows that the X-ray flux and spectrum of the pulsar and its wind nebula are consistent with the quiescent levels observed in 2000. C1 [Livingstone, Margaret A.; Ng, C. -Y.; Kaspi, Victoria M.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Gavriil, Fotis P.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Gavriil, Fotis P.] Univ Maryland Baltimore Cty, Ctr Res & Explorat Space Sci & Technol, Baltimore, MD 21250 USA. [Gotthelf, E. V.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. RP Livingstone, MA (reprint author), McGill Univ, Dept Phys, Rutherford Phys Bldg, Montreal, PQ H3A 2T8, Canada. EM maggie@physics.mcgill.ca RI Ng, Chi Yung/A-7639-2013 OI Ng, Chi Yung/0000-0002-5847-2612 FU NSERC [228738-03]; FQRNT; CIFAR FX We thank A. Beloborodov, A. Melatos, and an anonymous referee for comments that improved the manuscript. This research made use of data obtained from the High Energy Astrophysics Science Archive Research Center Online Service, provided by the NASA-Goddard Space Flight Center. C.Y.N. is a CRAQ postdoctoral fellow. V.M.K. holds the Lorne Trottier Chair in Astrophysics and Cosmology and a Canada Research Chair in Observational Astrophysics. Funding for this work was provided by NSERC Discovery Grant Rgpin 228738-03, FQRNT, and CIFAR. NR 50 TC 33 Z9 34 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 APR 1 PY 2011 VL 730 IS 2 AR 66 DI 10.1088/0004-637X/730/2/66 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 735TR UT WOS:000288441900006 ER PT J AU Roy, A Ade, PAR Bock, JJ Brunt, CM Chapin, EL Devlin, MJ Dicker, SR France, K Gibb, AG Griffin, M Gundersen, JO Halpern, M Hargrave, PC Hughes, DH Klein, J Marsden, G Martin, PG Mauskopf, P Netterfield, CB Olmi, L Patanchon, G Rex, M Scott, D Semisch, C Truch, MDP Tucker, C Tucker, GS Viero, MP Wiebe, DV AF Roy, Arabindo Ade, Peter A. R. Bock, James J. Brunt, Christopher M. Chapin, Edward L. Devlin, Mark J. Dicker, Simon R. France, Kevin Gibb, Andrew G. Griffin, Matthew Gundersen, Joshua O. Halpern, Mark Hargrave, Peter C. Hughes, David H. Klein, Jeff Marsden, Gaelen Martin, Peter G. Mauskopf, Philip Netterfield, Calvin B. Olmi, Luca Patanchon, Guillaume Rex, Marie Scott, Douglas Semisch, Christopher Truch, Matthew D. P. Tucker, Carole Tucker, Gregory S. Viero, Marco P. Wiebe, Donald V. TI DECONVOLUTION OF IMAGES FROM BLAST 2005: INSIGHT INTO THE K3-50 AND IC 5146 STAR-FORMING REGIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars: formation; submillimeter: general; techniques: image processing ID DARK CLOUD COMPLEX; APERTURE-SUBMILLIMETER-TELESCOPE; GALACTIC PLANE SURVEY; BLIND DECONVOLUTION; SUPERNOVA REMNANT; MOLECULAR CLOUDS; MAXIMUM-ENTROPY; LUCY ALGORITHM; CO OUTFLOWS; RESTORATION AB We present an implementation of the iterative flux-conserving Lucy-Richardson (L-R) deconvolution method of image restoration for maps produced by the Balloon-borne Large Aperture Submillimeter Telescope (BLAST). Compared to the direct Fourier transform method of deconvolution, the L-R operation restores images with better-controlled background noise and increases source detectability. Intermediate iterated images are useful for studying extended diffuse structures, while the later iterations truly enhance point sources to near the designed diffraction limit of the telescope. The L-R method of deconvolution is efficient in resolving compact sources in crowded regions while simultaneously conserving their respective flux densities. We have analyzed its performance and convergence extensively through simulations and cross-correlations of the deconvolved images with available high-resolution maps. We present new science results from two BLAST surveys, in the Galactic regions K3-50 and IC 5146, further demonstrating the benefits of performing this deconvolution. We have resolved three clumps within a radius of 4.'5 inside the star-forming molecular cloud containing K3-50. Combining the well-resolved dust emission map with available multi-wavelength data, we have constrained the spectral energy distributions (SEDs) of five clumps to obtain masses (M), bolometric luminosities (L), and dust temperatures (T). The L-M diagram has been used as a diagnostic tool to estimate the evolutionary stages of the clumps. There are close relationships between dust continuum emission and both 21 cm radio continuum and (CO)-C-12 molecular line emission. The restored extended large-scale structures in the Northern Streamer of IC 5146 have a strong spatial correlation with both SCUBA and high-resolution extinction images. A dust temperature of 12 K has been obtained for the central filament. We report physical properties of ten compact sources, including six associated protostars, by fitting SEDs to multi-wavelength data. All of these compact sources are still quite cold (typical temperature below similar to 16 K) and are above the critical Bonner-Ebert mass. They have associated low-power young stellar objects. Further evidence for starless clumps has also been found in the IC 5146 region. C1 [Roy, Arabindo; Netterfield, Calvin B.; Viero, Marco P.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada. [Ade, Peter A. R.; Griffin, Matthew; Hargrave, Peter C.; Mauskopf, Philip; Tucker, Carole] Cardiff Univ, Dept Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Bock, James J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Bock, James J.; Viero, Marco P.] CALTECH, Pasadena, CA 91125 USA. [Brunt, Christopher M.] Univ Exeter, Sch Phys, Exeter EX4 4QL, Devon, England. [Chapin, Edward L.; Gibb, Andrew G.; Halpern, Mark; Marsden, Gaelen; Scott, Douglas; Wiebe, Donald V.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. [Devlin, Mark J.; Dicker, Simon R.; Klein, Jeff; Rex, Marie; Semisch, Christopher; Truch, Matthew D. P.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. [France, Kevin] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA. [Gundersen, Joshua O.] Univ Miami, Dept Phys, Carol Gables, FL 33146 USA. [Hughes, David H.] INAOE, Puebla, Mexico. [Martin, Peter G.] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, 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] Ist Radioastron, I-50125 Florence, Italy. [Patanchon, Guillaume] Lab APC, F-75205 Paris, France. [Tucker, Gregory S.] Brown Univ, Dept Phys, Providence, RI 02912 USA. RP Roy, A (reprint author), Univ Toronto, Dept Astron & Astrophys, 50 St George St, Toronto, ON M5S 3H4, Canada. EM aroy@cita.utoronto.ca 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]; Canadian Space Agency (CSA); UK Particle Physics & Astronomy Research Council (PPARC); Canada's Natural Sciences and Engineering Research Council (NSERC) FX The BLAST collaboration acknowledges the support of NASA through grant numbers NAG5-12785, NAG5-13301, and NNGO-6GI11G, the Canadian Space Agency (CSA), the UK Particle Physics & Astronomy Research Council (PPARC), and Canada's Natural Sciences and Engineering Research Council (NSERC). We also thank the Columbia Scientific Balloon Facility (CSBF) staff for their outstanding work. NR 53 TC 5 Z9 5 U1 0 U2 9 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD APR 1 PY 2011 VL 730 IS 2 AR 142 DI 10.1088/0004-637X/730/2/142 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 735TR UT WOS:000288441900082 ER PT J AU Savage, SL McKenzie, DE AF Savage, Sabrina L. McKenzie, David E. TI QUANTITATIVE EXAMINATION OF A LARGE SAMPLE OF SUPRA-ARCADE DOWNFLOWS IN ERUPTIVE SOLAR FLARES SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun: corona; Sun: coronal mass ejections (CMEs); Sun: flares; Sun: magnetic topology; Sun: UV radiation; Sun: X-rays, gamma rays ID CORONAL MASS EJECTION; FIELD LINE SHRINKAGE; CURRENT SHEET; MAGNETIC-FIELDS; RECONNECTION; EMISSIONS; MOTIONS; HINODE; MODEL AB Sunward-flowing voids above post-coronal mass ejection flare arcades were first discovered using the soft X-ray telescope aboard Yohkoh and have since been observed with TRACE (extreme ultraviolet (EUV)), SOHO/LASCO (white light), SOHO/SUMER (EUV spectra), and Hinode/XRT (soft X-rays). Supra-arcade downflow (SAD) observations suggest that they are the cross-sections of thin flux tubes retracting from a reconnection site high in the corona. Supra-arcade downflowing loops (SADLs) have also been observed under similar circumstances and are theorized to be SADs viewed from a perpendicular angle. Although previous studies have focused on dark flows because they are easier to detect and complementary spectral data analysis reveals their magnetic nature, the signal intensity of the flows actually ranges from dark to bright. This implies that newly reconnected coronal loops can contain a range of hot plasma density. Previous studies have presented detailed SAD observations for a small number of flares. In this paper, we present a substantial SADs and SADLs flare catalog. We have applied semiautomatic detection software to several of these events to detect and track individual downflows thereby providing statistically significant samples of parameters such as velocity, acceleration, area, magnetic flux, shrinkage energy, and reconnection rate. We discuss these measurements (particularly the unexpected result of the speeds being an order of magnitude slower than the assumed Alfven speed), how they were obtained, and potential impact on reconnection models. C1 [Savage, Sabrina L.] Oak Ridge Associated Univ, NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Savage, Sabrina L.; McKenzie, David E.] Montana State Univ, Dept Phys, Bozeman, MT 59717 USA. RP Savage, SL (reprint author), Oak Ridge Associated Univ, NASA, Goddard Space Flight Ctr, 8800 Greenbelt Rd,Code 671, Greenbelt, MD 20771 USA. FU NASA [NNM07AB07C]; Harvard-Smithsonian Astrophysical Observatory FX This work was supported by NASA under contract NNM07AB07C with the Harvard-Smithsonian Astrophysical Observatory. The authors thank Drs. D. Longcope, C. Kankelborg, J. Qiu, A. Des Jardins, and the anonymous referee for constructive conversations and comments. Hinode is a Japanese mission developed and launched by ISAS/JAXA, with NAOJ as domestic partner and NASA and STFC (UK) as international partners. It is operated by these agencies in cooperation with ESA and NSC (Norway). Yohkoh data are provided courtesy of the NASA-supported Yohkoh Legacy Archive at Montana State University. NR 18 TC 36 Z9 37 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 APR 1 PY 2011 VL 730 IS 2 AR 98 DI 10.1088/0004-637X/730/2/98 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 735TR UT WOS:000288441900038 ER PT J AU Singal, J Fixsen, DJ Kogut, A Levin, S Limon, M Lubin, P Mirel, P Seiffert, M Villela, T Wollack, E Wuensche, CA AF Singal, J. Fixsen, D. J. Kogut, A. Levin, S. Limon, M. Lubin, P. Mirel, P. Seiffert, M. Villela, T. Wollack, E. Wuensche, C. A. TI THE ARCADE 2 INSTRUMENT SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmic background radiation; instrumentation: detectors; radio continuum: galaxies ID TEMPERATURE; GHZ; CALIBRATOR; RADIATION; DESIGN; COBE AB The second generation Absolute Radiometer for Cosmology, Astrophysics, and Diffuse Emission (ARCADE 2) instrument is a balloon-borne experiment to measure the radiometric temperature of the cosmic microwave background and Galactic and extragalactic emission at six frequencies from 3 to 90 GHz. ARCADE 2 utilizes a double-nulled design where emission from the sky is compared to that from an external cryogenic full-aperture blackbody calibrator by cryogenic switching radiometers containing internal blackbody reference loads. In order to further minimize sources of systematic error, ARCADE 2 features a cold fully open aperture with all radiometrically active components maintained at near 2.7 K without windows or other warm objects, achieved through a novel thermal design. We discuss the design and performance of the ARCADE 2 instrument in its 2005 and 2006 flights. C1 [Singal, J.] SLAC Natl Accelerator Lab, Kavli Inst Particle Astrophys & Cosmol, Menlo Pk, CA 94025 USA. [Singal, J.] Stanford Univ, Menlo Pk, CA 94025 USA. [Fixsen, D. J.] Univ Maryland, Dept Phys, NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Levin, S.; Seiffert, M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Limon, M.] Columbia Univ, Dept Phys, New York, NY 10027 USA. [Lubin, P.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Villela, T.; Wuensche, C. A.] Inst Nacl Pesquisas Espaciais, Div Astrophys, BR-12245970 Sao Jose Dos Campos, SP, Brazil. RP Singal, J (reprint author), SLAC Natl Accelerator Lab, Kavli Inst Particle Astrophys & Cosmol, Menlo Pk, CA 94025 USA. EM jsingal@stanford.edu RI Tecnologias espaciai, Inct/I-2415-2013; Wollack, Edward/D-4467-2012; OI Wollack, Edward/0000-0002-7567-4451; Limon, Michele/0000-0002-5900-2698 FU NASA's Science Mission Directorate; National Aeronautics and Space Administration; CNPq [466184/00-0, 305219-2004-9, 303637/2007-2-FA, 307433/2004-8-FA] FX We thank the staff at CSBF for launch support. We thank Victor Kulesh for contributions to the ground software, and Adam Bushmaker, Jane Cornett, Paul Cursey, Sarah Fixsen, Luke Lowe, and Alexandre Rischard for their work on the project. We thank the Cryogenics Branch at GSFC for supporting the ARCADE 2 design and thermometer calibration, Todd Gaier for the 90 GHz amplifiers, and Custom Microwave, Bechdon, Inc., Flight Fab, and JMD for fabrication of components. This research has been supported by NASA's Science Mission Directorate under the Astronomy and Physics Research and Analysis suborbital program. The research described in this paper was performed in part at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. T. V. acknowledges support from CNPq grants 466184/00-0, 305219-2004-9, and 303637/2007-2-FA, and the technical support from Luiz Reitano. C.A.W. acknowledges support from CNPq grant 307433/2004-8-FA. NR 15 TC 16 Z9 16 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 APR 1 PY 2011 VL 730 IS 2 AR 138 DI 10.1088/0004-637X/730/2/138 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 735TR UT WOS:000288441900078 ER PT J AU Jeon, HS Cho, S Kwak, YS Chung, JK Park, JU Lee, DK Kuzmicz-Cieslak, M AF Jeon, H. S. Cho, S. Kwak, Y. S. Chung, J. K. Park, J. U. Lee, D. K. Kuzmicz-Cieslak, M. TI Mass density of the upper atmosphere derived from Starlette's Precise Orbit Determination with Satellite Laser Ranging SO ASTROPHYSICS AND SPACE SCIENCE LA English DT Article DE Mass density; Starlette; Precise Orbit Determination; Satellite Laser Ranging; MSIS models; Geomagnetic activity ID ACCELEROMETER DATA; MAGNETIC STORMS; NEUTRAL DENSITY; SOLAR; CHAMP; MODEL AB The atmospheric mass density of the upper atmosphere from the spherical Starlette satellite's Precise Orbit Determination is first derived with Satellite Laser Ranging measurements at 815 to 1115 km during strong solar and geomagnetic activities. Starlette's orbit is determined using the improved orbit determination techniques combining optimum parameters with a precise empirical drag application to a gravity field. MSIS-86 and NRLMSISE-00 atmospheric density models are compared with the Starlette drag-derived atmospheric density of the upper atmosphere. It is found that the variation in the Starlette's drag coefficient above 800 km corresponds well with the level of geomagnetic activity. This represents that the satellite orbit is mainly perturbed by the Joule heating from geomagnetic activity at the upper atmosphere. This result concludes that MSIS empirical models strongly underestimate the mass density of the upper atmosphere as compared to the Starlette drag-derived atmospheric density during the geomagnetic storms. We suggest that the atmospheric density models should be analyzed with higher altitude acceleration data for a better understanding of long-term solar and geomagnetic effects. C1 [Jeon, H. S.] Univ Sci & Technol, Taejon 305333, South Korea. [Jeon, H. S.; Cho, S.; Kwak, Y. S.; Chung, J. K.; Park, J. U.] Korea Astron & Space Sci Inst, Div Space Sci, Taejon 305348, South Korea. [Jeon, H. S.; Lee, D. K.] Korean Air Force Headquarters, Gyeryong 321919, Chungnam, South Korea. [Kuzmicz-Cieslak, M.] UMBC & NASA Goddard 698, NASA, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21250 USA. RP Jeon, HS (reprint author), Univ Sci & Technol, Taejon 305333, South Korea. EM ewmann@kasi.re.kr FU NASA Goddard Earth Science and Technology Center (GEST); Goddard Space Flight Center, Greenbelt FX This work was supported by the NASA Goddard Earth Science and Technology Center (GEST) from the Goddard Space Flight Center, Greenbelt. The authors thank the International Laser Ranging Service (ILRS) stations and data centers for the high quality global SLR observations. The author appreciates Dr. K.A. Firoz, Mr. J.H. Baek, and Ms. W.K. Lee in KASI for generous assistances. We are grateful to honorable reviewers for their valuable comments and suggestions that indeed developed the quality of this study. NR 30 TC 2 Z9 2 U1 0 U2 8 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0004-640X J9 ASTROPHYS SPACE SCI JI Astrophys. Space Sci. PD APR PY 2011 VL 332 IS 2 BP 341 EP 351 DI 10.1007/s10509-010-0528-2 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 732UP UT WOS:000288215500014 ER PT J AU Sakowski, C Starc, V Smith, SM Schlegel, TT AF Sakowski, Chris Starc, Vito Smith, Scott M. Schlegel, Todd T. TI Sedentary Long-Duration Head-Down Bed Rest and ECG Repolarization Heterogeneity SO AVIATION SPACE AND ENVIRONMENTAL MEDICINE LA English DT Article DE electrocardiogram; QRS-T angle; QT variability; T-wave complexity; spatial ventricular gradient ID QRS-T ANGLE; LEFT-VENTRICULAR HYPERTROPHY; CORONARY-ARTERY-DISEASE; QT-INTERVAL VARIABILITY; PREDICTS CARDIAC DEATH; TORSADES-DE-POINTES; NUTRITIONAL-STATUS; WAVE ALTERNANS; SPACE-FLIGHT; ELECTROCARDIOGRAPHY AB SAKOWSKI C, STARC V, SMITH SM, SCHLEGEL TT. Sedentary long-duration head-down bed rest and ECG repolarization heterogeneity. Aviat Space Environ Med 2011; 82:416-23. Background: We studied the effects of 90 d of 6 degrees head-down bed rest (HDBR) on cardiac autonomic and advanced electrocardiographic (ECG) function, especially on repolarization heterogeneity as assessed by beat-to-beat QT interval variability (QTV), T-wave complexity, and 3-dimensional ECG. Based on prior observations of lengthening of the QTc interval during long-duration spaceflight, we hypothesized that abnormalities in ECG repolarization would also occur during long-duration HDBR. Methods: During controlled breathing, 5-min supine high-fidelity 12-lead ECGs were obtained from 20 healthy subjects (14 men and 6 women) together with measurements of plasma volume and electrolytes at 5 points in time: within 10 d before; 28-30, 60, and 90 d into; and 3-5 d after HDBR. Results: By repeated measures ANOVA, 90 d of sedentary HDBR significantly increased the QTV index (from 1.87 +/- 0.33 to - 1.53 +/- 0.39 units), the index of unexplained QTV (from 0.61 +/- 0.48 to 1.21 +/- 0.40 units), the T-wave complexity intradipolar ratio (from 0.344 +/- 0.260 to 2.04 +/- 4.01%), and the spatial QRS-T angle (from 49.1 +/- 23.8 to 58.7 +/- 31.0 degrees), and significantly decreased the spatial ventricular gradient (from 91.3 +/- 26.5 to 59.1 +/- 23.0 mV . ms(-1)). These changes resolved in part by 3-5 d after resumption of ambulation, but unlike concomitant changes in the QTc interval itself and in heart rate variability, they did not significantly relate to changes in electrolytes or plasma volume. Conclusions: Sedentary, long-duration HDBR reversibly increases ECG repolarization heterogeneity and by inference ventricular arrhythmic risk. C1 [Smith, Scott M.; Schlegel, Todd T.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Sakowski, Chris] Univ Texas Med Branch, Galveston, TX USA. [Starc, Vito] Univ Ljubljana, Fac Med, Inst Physiol, Ljubljana, Slovenia. RP Schlegel, TT (reprint author), NASA, Lyndon B Johnson Space Ctr, Mail Code SK272, Houston, TX 77058 USA. EM todd.t.schlegel@nasa.gov FU UTMB; USA-Slovenia Cooperation in Science and Technology; Johnson Space Center; Human Test Subject Facility FX This research was supported by the UTMB Medical Student Summer Research Program (CS); the USA-Slovenia Cooperation in Science and Technology (VS, TTS); and the Johnson Space Center Flight Analogs Project (DSM, SMS, TTS) and Human Test Subject Facility (TTS). NR 45 TC 6 Z9 7 U1 0 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 APR PY 2011 VL 82 IS 4 BP 416 EP 423 DI 10.3357/ASEM.2945.2011 PG 8 WC Public, Environmental & Occupational Health; Medicine, General & Internal; Sport Sciences SC Public, Environmental & Occupational Health; General & Internal Medicine; Sport Sciences GA 740YC UT WOS:000288829300002 PM 21485399 ER PT J AU Sulkowski, CM Gilkey, KM Lewandowski, BE Samorezov, S Myers, JG AF Sulkowski, Christina M. Gilkey, Kelly M. Lewandowski, Beth E. Samorezov, Sergey Myers, Jerry G., Jr. TI An Extravehicular Suit Impact Load Attenuation Study to Improve Astronaut Bone Fracture Prediction SO AVIATION SPACE AND ENVIRONMENTAL MEDICINE LA English DT Article DE non-conformal fit; side fall; impact load to hip; space exploration missions; bone mineral density ID LONG-DURATION SPACEFLIGHT; FORCE ATTENUATION; HIP; FALL AB SULKOWSKI CM, GILKEY KM, LEWANDOWSKI BE, SAMOREZOV S, MYERS JR JG. An extravehicular suit impact load attenuation study to improve astronaut bone fracture prediction. Aviat Space Environ Med 2011; 82:455-62. Introduction: Understanding the contributions to the risk of bone fracture during spaceflight is essential for mission success. Methods: A pressurized extravehicular activity (EVA) suit analogue test bed was developed, impact load attenuation data were obtained, and the load at the hip of an astronaut who falls to the side during an EVA was characterized. Offset (representing the gap between the EVA suit and the astronaut's body), impact load magnitude, and EVA suit operating pressure were factors varied in the study. The attenuation data were incorporated into a probabilistic model of bone fracture risk during spaceflight, replacing the previous load attenuation value that was based on commercial hip protector data. Results: Load attenuation was more dependent on offset than on pressurization or load magnitude, especially at small offset values. Load attenuation factors for offsets between 0.1-1.5 cm were 0.69 +/- 0.15, 0.49 +/- 0.22, and 0.35 +/- 0.18 for mean impact forces of 4827, 6400, and 8467 N, respectively. Load attenuation factors for offsets of 2.8-5.3 cm were 0.93 +/- 0.2, 0.94 +/- 0.1, and 0.84 +/- 0.5 for the same mean impact forces. The mean and 95(th) percentile bone fracture risk index predictions were each reduced by 65-83%. The mean and 9.5(th) percentile bone fracture probability predictions were both reduced approximately 20-50%. Discussion: The reduction in uncertainty and improved confidence in bone fracture predictions increased the fidelity and credibility of the fracture risk model and its benefit to mission design and in-flight operational decisions. C1 [Gilkey, Kelly M.; Lewandowski, Beth E.; Myers, Jerry G., Jr.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. [Sulkowski, Christina M.] Univ Akron, Akron, OH 44325 USA. [Samorezov, Sergey] Lerner Res Inst, Cleveland Clin, Cleveland, OH 44106 USA. RP Lewandowski, BE (reprint author), NASA, Glenn Res Ctr, 21000 Brookpk Rd,MS 110-3, Cleveland, OH 44135 USA. EM beth.e.lewandowski@nasa.gov FU NASA Johnson Space Center (JSC) Human Research Program (HRP) Office and the NASA JSC EVA Project Office; National Space Biomedical Research Institute; Baylor College of Medicine; NASA FX The authors of this study acknowledge the NASA Johnson Space Center (JSC) Human Research Program (HRP) Office and the NASA JSC EVA Project Office for their support of this investigation, especially Shane McFarland for his professional consultation on the EVA suit. NASA Glenn Research Center HRP personnel, DeVon Griffin and Gail Perusek, are appreciated for their supporting role as project managers and technical reviewers. The investigation team expresses gratitude to Jim King, Dan Gedeon, and Harkirat Sohi for their technical assistance with the test operations. The National Space Biomedical Research Institute, Baylor College of Medicine, and NASA LERCIP programs are also thanked for their support. NR 16 TC 1 Z9 2 U1 2 U2 7 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 APR PY 2011 VL 82 IS 4 BP 455 EP 462 DI 10.3357/ASEM.2855.2011 PG 8 WC Public, Environmental & Occupational Health; Medicine, General & Internal; Sport Sciences SC Public, Environmental & Occupational Health; General & Internal Medicine; Sport Sciences GA 740YC UT WOS:000288829300007 PM 21485404 ER PT J AU Peters, BT Miller, CA Brady, RA Richards, JT Mulavara, AP Bloomberg, JJ AF Peters, Brian T. Miller, Chris A. Brady, Rachel A. Richards, Jason T. Mulavara, Ajitkumar P. Bloomberg, Jacob J. TI Dynamic Visual Acuity During Walking After Long-Duration Spaceflight SO AVIATION SPACE AND ENVIRONMENTAL MEDICINE LA English DT Article DE spaceflight; human locomotion; dynamic visual acuity; vestibulo-ocular reflex; adaptation ID VESTIBULAR HYPOFUNCTION; RESPONSES; RECOVERY AB PETERS BT, MILLER CA, BRADY RA, RICHARDS JT, MULAVARA AP, BLOOMBERG JJ. Dynamic visual acuity during walking after long-duration spaceflight. Aviat Space Environ Med 2011; 82:463-6. Astronauts experience alterations in gaze control as a result of adaptive changes in eye-head coordination produced by micro-gravity exposure. This may lead to potential changes in postflight visual acuity during head and body motion. Methods: We gathered dynamic visual acuity (DVA) data from 14 astronauts and cosmonauts after long-duration (similar to 6 mo) stays in space. Walking was used to induce self-motion and visual acuity was determined by sequentially presenting Landolt ring optotypes on a computer display placed 4 m in front of subjects. Acuity assessments were made while seated (static condition) and walking (dynamic condition) at 6.4 km . 1171 on a motorized treadmill. In each condition, a psychophysical threshold detection algorithm minimized the required number of optotype presentations by maximizing the amount displayed around the subject's acuity threshold. The difference between static and dynamic acuity measures provided a metric of change in the subjects' ability to maintain gaze fixation on the visual target while walking. Results: A decrement in postflight visual acuity during walking was found. A mean dynamic acuity decrement of approximately 0.75 eye-chart lines was observed 1 d after returning from space. The population mean showed a consistent improvement in DVA performance during the first postflight week. Discussion: The recovery curves for individual subjects did not necessarily follow a pattern of continuous improvement with each passing day. When adjusted for previous long-duration flight experience, the population mean showed an unexpected DVA reduction in the re-adaptation curve that is similar to recovery patterns observed in prism adaptation studies. C1 [Peters, Brian T.; Miller, Chris A.; Brady, Rachel A.; Richards, Jason T.] Wyle Integrated Sci & Engn Grp, Houston, TX 77058 USA. [Mulavara, Ajitkumar P.] Univ Space Res Assoc, Houston, TX USA. [Bloomberg, Jacob J.] NASA, Lyndon B Johnson Space Ctr, Neurosci Labs, Houston, TX 77058 USA. RP Peters, BT (reprint author), Wyle Integrated Sci & Engn Grp, Houston, TX 77058 USA. EM brian.peters-1@nasa.gov FU NASA [E120]; National Space Biomedical Research Institute through NASA [NCC 9-58] FX This work was supported by NASA (Experiment E120) and the National Space Biomedical Research Institute through NASA NCC 9-58. NR 15 TC 8 Z9 10 U1 1 U2 10 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 APR PY 2011 VL 82 IS 4 BP 463 EP 466 DI 10.3357/ASEM.2928.2011 PG 4 WC Public, Environmental & Occupational Health; Medicine, General & Internal; Sport Sciences SC Public, Environmental & Occupational Health; General & Internal Medicine; Sport Sciences GA 740YC UT WOS:000288829300008 PM 21485405 ER PT J AU Thornton, WE AF Thornton, William E. TI A Rationale for Space Motion Sickness SO AVIATION SPACE AND ENVIRONMENTAL MEDICINE LA English DT Editorial Material DE motion sickness ID INNERVATING OTOLITH ORGANS; SQUIRREL-MONKEY; PHYSIOLOGY AB THORNTON WE. A rationale for space motion sickness. Aviat Space Environ Med 2011; 82:467-8. Space motion sickness (SMS) still remains a problematic nuisance for a majority of fliers during their first 1 to 3 clays in space and is an enigma to all concerned after almost half a century of spaceflight and extensive ground and in-flight studies. There is no known etiology consistent with observed signs and symptoms, and attempts to produce pre- and in-flight countermeasures have largely failed. Some medications for motion sickness (MS) have been partially effective, but must be used with caution due to their side effects. A hypothesis regarding SMS that is consistent with current knowledge of vestibular physiology and with observed and measured phenomena during SMS is presented. C1 NASA, Boerne, TX 78015 USA. RP Thornton, WE (reprint author), NASA, 7640 Pimlico Lane, Boerne, TX 78015 USA. EM jwthornt@msn.com NR 10 TC 4 Z9 5 U1 0 U2 5 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 APR PY 2011 VL 82 IS 4 BP 467 EP 468 DI 10.3357/ASEM.2907.2011 PG 2 WC Public, Environmental & Occupational Health; Medicine, General &