FN Thomson Reuters Web of Science™ VR 1.0 PT J AU Zhu, WW Stairs, IH Demorest, PB Nice, DJ Ellis, JA Ransom, SM Arzoumanian, Z Crowter, K Dolch, T Ferdman, RD Fonseca, E Gonzalez, ME Jones, G Jones, ML Lam, MT Levin, L McLaughlin, MA Pennucci, T Stovall, K Swiggum, J AF Zhu, W. W. Stairs, I. H. Demorest, P. B. Nice, D. J. Ellis, J. A. Ransom, S. M. Arzoumanian, Z. Crowter, K. Dolch, T. Ferdman, R. D. Fonseca, E. Gonzalez, M. E. Jones, G. Jones, M. L. Lam, M. T. Levin, L. McLaughlin, M. A. Pennucci, T. Stovall, K. Swiggum, J. TI TESTING THEORIES OF GRAVITATION USING 21-YEAR TIMING OF PULSAR BINARY J1713+0747 SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: general; gravitation; parallaxes; pulsars: individual (PSR J1713+0747); stars: neutron ID BLACK-HOLE BINARIES; X-RAY BINARIES; MILLISECOND PULSARS; NEUTRON-STAR; PSR J1713+0747; RADIO PULSARS; EQUIVALENCE PRINCIPLES; RELATIVISTIC GRAVITY; GENERAL-RELATIVITY; MASS-DISTRIBUTION AB We report 21-year timing of one of the most precise pulsars: PSR J1713+0747. Its pulse times of arrival are well modeled by a comprehensive pulsar binary model including its three-dimensional orbit and a noise model that incorporates short-and long-timescale correlated noise such as jitter and red noise. Its timing residuals have weighted root mean square similar to 92 ns. The new data set allows us to update and improve previous measurements of the system properties, including the masses of the neutron star (1.31 +/- 0.11 M-circle dot) and the companion white dwarf (0.286 +/- 0.012 M-circle dot) as well as their parallax distance 1.15 +/- 0.03 kpc. We measured the intrinsic change in orbital period, (P) over dot(b)(Int), is -0.20 +/- 0.17 ps s(-1), which is not distinguishable from zero. This result, combined with the measured (P) over dot(b)(Int) of other pulsars, can place a generic limit on potential changes in the gravitational constant G. We found that (G) over dot/G is consistent with zero [(-0.6 +/- 1.1) x 10(-12) yr(-1), 95% confidence] and changes at least a factor of 31 (99.7% confidence) more slowly than the average expansion rate of the universe. This is the best (G) over dot/G limit from pulsar binary systems. The (P) over dot(b)(Int) of pulsar binaries can also place limits on the putative coupling constant for dipole gravitational radiation kappa(D) = (-0.9 +/- 3.3) 10(-4) (95% confidence). Finally, the nearly circular orbit of this pulsar binary allows us to constrain statistically the strong-field post-Newtonian parameters Delta, which describes the violation of strong equivalence principle, and (alpha) over cap (3), which describes a breaking of both Lorentz invariance in gravitation and conservation of momentum. We found, at 95% confidence, Delta < 0.01 and <(alpha)over cap>(3) < 2 x 10(-20) based on PSR J1713+0747. C1 [Zhu, W. W.; Stairs, I. H.; Crowter, K.; Fonseca, E.; Gonzalez, M. E.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T IZ1, Canada. [Zhu, W. W.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Demorest, P. B.] Natl Radio Astron Observ, Socorro, NM 87801 USA. [Nice, D. J.] Lafayette Coll, Dept Phys, Easton, PA 18042 USA. [Ransom, S. M.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. [Arzoumanian, Z.] NASA Goddard Space Flight Ctr, Ctr Res & Explorat Space Sci & Technol, Greenbelt, MD 20771 USA. [Arzoumanian, Z.] NASA Goddard Space Flight Ctr, X Ray Astrophys Lab, Greenbelt, MD 20771 USA. [Arzoumanian, Z.] Univ Space Res Assoc, Columbia, MD 21046 USA. [Dolch, T.; Lam, M. T.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. [Ferdman, R. D.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Gonzalez, M. E.] Vancouver Coastal Hlth Author, Dept Nucl Med, Vancouver, BC V5Z IM9, Canada. [Jones, G.] Columbia Univ, Dept Phys, New York, NY 10027 USA. [Jones, M. L.; Levin, L.; McLaughlin, M. A.; Swiggum, J.] West Virginia Univ, Dept Phys & Astron, Morgantown, WV 26505 USA. [Levin, L.] Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England. [Pennucci, T.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. [Stovall, K.] Univ New Mexico, Dept Phys & Astron, Albuquerque, NM 87131 USA. RP Zhu, WW (reprint author), Univ British Columbia, Dept Phys & Astron, 6224 Agr Rd, Vancouver, BC V6T IZ1, Canada. EM zhuww@phas.ubc.ca; istairs@phas.ubc.ca OI Ransom, Scott/0000-0001-5799-9714; Nice, David/0000-0002-6709-2566 FU NSERC Discovery Grant and Discovery Accelerator Supplement; Canadian Institute for Advanced Research; NASA through Einstein Fellowship [PF4-150120]; NSF [0923409, 0647820]; National Science Foundation (NSF) PIRE program [0968296]; National Science Foundation [AST-1100968]; Associated Universities, Inc; National Aeronautics and Space Administration FX The authors thank N. Wex, P. C. C. Freire, C. Ng, and J. Cordes for helpful comments and discussions. Pulsar research at UBC is supported by an NSERC Discovery Grant and Discovery Accelerator Supplement, and by the Canadian Institute for Advanced Research. J.A.E. acknowledges support by NASA through Einstein Fellowship grant PF4-150120. Some computational work was performed on the Nemo cluster at UWM supported by NSF grant No. 0923409. Portions of this research were carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. T. Pennucci is a student at the National Radio Astronomy Observatory. The NANOGrav project receives support from the National Science Foundation (NSF) PIRE program award number 0968296. This work was supported by NSF grant 0647820. The Arecibo Observatory is operated by SRI International under a cooperative agreement with the National Science Foundation (AST-1100968), and in alliance with Ana G. Mendez-Universidad Metropolitana, and the Universities Space Research Association. The National Radio Astronomy Observatory (GBT) is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. NR 100 TC 23 Z9 23 U1 1 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD AUG 10 PY 2015 VL 809 IS 1 AR 41 DI 10.1088/0004-637X/809/1/41 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CR9DN UT WOS:000361653500041 ER PT J AU Clark, CJ Pletsch, HJ Wu, J Guillemot, L Ackermann, M Allen, B de Angelis, A Aulbert, C Baldini, L Ballet, J Barbiellini, G Bastieri, D Bellazzini, R Bissaldi, E Bock, O Bonino, R Bottacini, E Brandt, TJ Bregeon, J Bruel, P Buson, S Caliandro, GA Cameron, RA Caragiulo, M Caraveo, PA Cecchi, C Champion, DJ Charles, E Chekhtman, A Chiang, J Chiaro, G Ciprini, S Claus, R Cohen-Tanugi, J Cuellar, A Cutini, S D'Ammando, F Desiante, R Drell, PS Eggenstein, HB Favuzzi, C Fehrmann, H Ferrara, EC Focke, WB Franckowiak, A Fusco, P Gargano, F Gasparrini, D Giglietto, N Giordano, F Glanzman, T Godfrey, G Grenier, IA Grove, JE Guiriec, S Harding, AK Hays, E Hewitt, JW Hill, AB Horan, D Hou, X Jogler, T Johnson, AS Johannesson, G Kramer, M Krauss, F Kuss, M Laffon, H Larsson, S Latronico, L Li, J Li, L Longo, F Loparco, F Lovellette, MN Lubrano, P Machenschalk, B Manfreda, A Marelli, M Mayer, M Mazziotta, MN Michelson, PF Mizuno, T Monzani, ME Morselli, A Moskalenko, IV Murgia, S Nuss, E Ohsugi, T Orienti, M Orlando, E de Palma, F Paneque, D Pesce-Rollins, M Piron, F Pivato, G Raino, S Rando, R Razzano, M Reimer, A Parkinson, PMS Schaal, M Schulz, A Sgro, C Siskind, EJ Spada, F Spandre, G Spinelli, P Suson, DJ Takahashi, H Thayer, JB Tibaldo, L Torne, P Torres, DF Tosti, G Troja, E Vianello, G Wood, KS Wood, M Yassine, M AF Clark, C. J. Pletsch, H. J. Wu, J. Guillemot, L. Ackermann, M. Allen, B. de Angelis, A. Aulbert, C. Baldini, L. Ballet, J. Barbiellini, G. Bastieri, D. Bellazzini, R. Bissaldi, E. Bock, O. Bonino, R. Bottacini, E. Brandt, T. J. Bregeon, J. Bruel, P. Buson, S. Caliandro, G. A. Cameron, R. A. Caragiulo, M. Caraveo, P. A. Cecchi, C. Champion, D. J. Charles, E. Chekhtman, A. Chiang, J. Chiaro, G. Ciprini, S. Claus, R. Cohen-Tanugi, J. Cuellar, A. Cutini, S. D'Ammando, F. Desiante, R. Drell, P. S. Eggenstein, H. B. Favuzzi, C. Fehrmann, H. Ferrara, E. C. Focke, W. B. Franckowiak, A. Fusco, P. Gargano, F. Gasparrini, D. Giglietto, N. Giordano, F. Glanzman, T. Godfrey, G. Grenier, I. A. Grove, J. E. Guiriec, S. Harding, A. K. Hays, E. Hewitt, J. W. Hill, A. B. Horan, D. Hou, X. Jogler, T. Johnson, A. S. Johannesson, G. Kramer, M. Krauss, F. Kuss, M. Laffon, H. Larsson, S. Latronico, L. Li, J. Li, L. Longo, F. Loparco, F. Lovellette, M. N. Lubrano, P. Machenschalk, B. Manfreda, A. Marelli, M. Mayer, M. Mazziotta, M. N. Michelson, P. F. Mizuno, T. Monzani, M. E. Morselli, A. Moskalenko, I. V. Murgia, S. Nuss, E. Ohsugi, T. Orienti, M. Orlando, E. de Palma, F. Paneque, D. Pesce-Rollins, M. Piron, F. Pivato, G. Raino, S. Rando, R. Razzano, M. Reimer, A. Parkinson, P. M. Saz Schaal, M. Schulz, A. Sgro, C. Siskind, E. J. Spada, F. Spandre, G. Spinelli, P. Suson, D. J. Takahashi, H. Thayer, J. B. Tibaldo, L. Torne, P. Torres, D. F. Tosti, G. Troja, E. Vianello, G. Wood, K. S. Wood, M. Yassine, M. TI PSR J1906+0722: AN ELUSIVE GAMMA-RAY PULSAR SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE gamma rays: stars; pulsars: individual (PSR J1906+0722) ID LARGE-AREA TELESCOPE; FERMI UNASSOCIATED SOURCES; REMNANT 3C 397; SOURCE CATALOG; SEARCHES; MULTIWAVELENGTH; DISCOVERY; MODEL; YOUNG AB We report the discovery of PSR J1906+0722, a gamma-ray pulsar detected as part of a blind survey of unidentified Fermi Large Area Telescope (LAT) sources being carried out on the volunteer distributed computing system, Einstein@Home. This newly discovered pulsar previously appeared as the most significant remaining unidentified gamma-ray source without a known association in the second Fermi-LAT source catalog (2FGL) and was among the top 10 most significant unassociated sources in the recent third catalog (3FGL). PSR J1906+0722 is a young, energetic, isolated pulsar, with a spin frequency of 8.9 Hz, a characteristic age of 49 kyr, and spin-down power 1.0 x 10(36) erg s(-1). In 2009 August it suffered one of the largest glitches detected from a gamma-ray pulsar (Delta f/f approximate to 4.5 x 10(-6)). Remaining undetected in dedicated radio follow-up observations, the pulsar is likely radio-quiet. An off-pulse analysis of the gamma-ray flux from the location of PSR J1906+0722 revealed the presence of an additional nearby source, which may be emission from the interaction between a neighboring supernova remnant and a molecular cloud. We discuss possible effects which may have hindered the detection of PSR J1906+0722 in previous searches and describe the methods by which these effects were mitigated in this survey. We also demonstrate the use of advanced timing methods for estimating the positional, spin and glitch parameters of difficult-to-time pulsars such as this. C1 [Clark, C. J.; Pletsch, H. J.; Allen, B.; Aulbert, C.; Bock, O.; Cuellar, A.; Eggenstein, H. B.; Fehrmann, H.; Machenschalk, B.] Max Planck Inst Gravitat Phys, Albert Einstein Inst, D-30167 Hannover, Germany. [Clark, C. J.; Pletsch, H. J.; Allen, B.; Aulbert, C.; Bock, O.; Cuellar, A.; Eggenstein, H. B.; Fehrmann, H.; Machenschalk, B.] Leibniz Univ Hannover, D-30167 Hannover, Germany. [Wu, J.; Champion, D. J.; Kramer, M.; Torne, P.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Guillemot, L.] Univ Orleans, CNRS, Lab Phys & Chim Environm & Espace, F-45071 Orleans 02, France. [Guillemot, L.] Observ Paris, CNRS, INSU, Stn Radioastron Nancay, F-18330 Nancay, France. [Ackermann, M.; Mayer, M.; Schulz, A.] Deutsch Elektronen Synchrotron DESY, D-15738 Zeuthen, Germany. [Allen, B.] Univ Wisconsin, Dept Phys, Milwaukee, WI 53201 USA. [de Angelis, A.] Univ Udine, Dipartimento Fis, I-33100 Udine, Italy. [de Angelis, A.] Ist Nazl Fis Nucl, Sez Trieste, Grp Coll Udine, I-33100 Udine, Italy. [Baldini, L.] Univ Pisa, I-56127 Pisa, Italy. [Baldini, L.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy. [Baldini, L.; Bottacini, E.; Caliandro, G. A.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; Drell, P. S.; Focke, W. B.; Franckowiak, A.; Glanzman, T.; Godfrey, G.; Hill, A. B.; Jogler, T.; Johnson, A. S.; Michelson, P. F.; Monzani, M. E.; Moskalenko, I. V.; Orlando, E.; Paneque, D.; Pesce-Rollins, M.; Reimer, A.; Thayer, J. B.; Tibaldo, L.; Vianello, G.; Wood, M.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Dept Phys, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA. [Baldini, L.; Bottacini, E.; Caliandro, G. A.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; Drell, P. S.; Focke, W. B.; Franckowiak, A.; Glanzman, T.; Godfrey, G.; Hill, A. B.; Jogler, T.; Johnson, A. S.; Michelson, P. F.; Monzani, M. E.; Moskalenko, I. V.; Orlando, E.; Paneque, D.; Pesce-Rollins, M.; Reimer, A.; Thayer, J. B.; Tibaldo, L.; Vianello, G.; Wood, M.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA. [Ballet, J.; Grenier, I. A.] CEA Saclay, Univ Paris Diderot, CNRS, Lab AIM,CEA IRFU,Serv Astrophys, 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.] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy. [Bastieri, D.; Buson, S.; Chiaro, G.; Rando, R.] Univ Padua, Dipartimento Fis & Astron G Galilei, I-35131 Padua, Italy. [Bellazzini, R.; Kuss, M.; Manfreda, A.; Pesce-Rollins, M.; Pivato, G.; Razzano, M.; Sgro, C.; Spada, F.; Spandre, G.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy. [Bissaldi, E.; Caragiulo, M.; Favuzzi, C.; Fusco, P.; Gargano, F.; Giglietto, N.; Giordano, F.; Loparco, F.; Mazziotta, M. N.; de Palma, F.; Raino, S.; Spinelli, P.] Ist Nazl Fis Nucl, Sez Bari, I-70126 Bari, Italy. [Bonino, R.; Desiante, R.; Latronico, L.] Ist Nazl Fis Nucl, Sez Torino, I-10125 Turin, Italy. [Bonino, R.] Univ Turin, Dipartimento Fis Gen Amadeo Avogadro, I-10125 Turin, Italy. [Brandt, T. J.; Ferrara, E. C.; Guiriec, S.; Harding, A. K.; Hays, E.; Troja, E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Bregeon, J.; Cohen-Tanugi, J.; Nuss, E.; Piron, F.; Yassine, M.] Univ Montpellier, CNRS, IN2P3, Lab Univ & Particules Montpellier, F-34059 Montpellier, France. [Bruel, P.; Horan, D.] Ecole Polytech, CNRS, IN2P3, Lab Leprince Ringuet, F-91128 Palaiseau, France. [Caliandro, G. A.] CIFS, I-10133 Turin, Italy. [Caraveo, P. A.; Marelli, M.] INAF Ist Astrofis Spaziale & Fis Cosm, I-20133 Milan, Italy. [Cecchi, C.; Ciprini, S.; Cutini, S.; Gasparrini, D.; Lubrano, P.; Tosti, G.] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy. [Cecchi, C.; Lubrano, P.; Tosti, G.] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy. [Chekhtman, A.] George Mason Univ, Coll Sci, Fairfax, VA 22030 USA. [Ciprini, S.; Cutini, S.; Gasparrini, D.] ASI Sci Data Ctr, I-00133 Rome, Italy. [Ciprini, S.; Cutini, S.; Gasparrini, D.] Osserv Astron Roma, INAF, I-00040 Rome, Italy. [D'Ammando, F.; Orienti, M.] Ist Radioastron, INAF, I-40129 Bologna, Italy. [D'Ammando, F.] Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy. [Desiante, R.] Univ Udine, I-33100 Udine, Italy. [Favuzzi, C.; Fusco, P.; Giglietto, N.; Giordano, F.; Loparco, F.; Raino, S.; Spinelli, P.] Univ Bari, Dipartimento Fis M Merlin, I-70126 Bari, Italy. [Favuzzi, C.; Fusco, P.; Giglietto, N.; Giordano, F.; Loparco, F.; Raino, S.; Spinelli, P.] Politecn Bari, I-70126 Bari, Italy. [Grove, J. E.; Lovellette, M. N.; Wood, K. S.] Naval Res Lab, Div Space Sci, Washington, DC 20375 USA. [Hewitt, J. W.] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA. [Hewitt, J. W.] Univ Maryland Baltimore Cty, Ctr Space Sci & Technol, Baltimore, MD 21250 USA. [Hewitt, J. W.] CRESST, Greenbelt, MD 20771 USA. [Hewitt, J. W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Hill, A. B.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Hou, X.] Chinese Acad Sci, Yunnan Observ, Kunming 650216, Peoples R China. [Hou, X.] Chinese Acad Sci, Key Lab Struct & Evolut Celestial Objects, Kunming 650216, Peoples R China. [Johannesson, G.] Univ Iceland, Inst Sci, IS-107 Reykjavik, Iceland. [Kramer, M.] Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England. [Krauss, F.] Univ Erlangen Nurnberg, Dr Remeis Sternwarte & ECAP, D-96049 Bamberg, Germany. [Krauss, F.] Univ Wurzburg, Inst Theoret Phys & Astrophys, D-97074 Wurzburg, Germany. [Laffon, H.] Univ Bordeaux 1, CNRS, IN2P3, CEN Bordeaux Gradignan, F-33175 Gradignan, France. [Larsson, S.; Li, L.] KTH Royal Inst Technol, Dept Phys, SE-10691 Stockholm, Sweden. [Larsson, S.; Li, L.] Oskar Klein Ctr Cosmoparticle Phys, SE-10691 Stockholm, Sweden. [Li, J.; Torres, D. F.] IEEC CSIC, Inst Space Sci, E-08193 Barcelona, Spain. [Mizuno, T.; Ohsugi, T.] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Higashihiroshima, Hiroshima 7398526, Japan. [Morselli, A.] Ist Nazl Fis Nucl, Sez Roma, I-00133 Rome, Italy. [Murgia, S.] Univ Calif Irvine, Ctr Cosmol, Dept Phys & Astron, Irvine, CA 92697 USA. [de Palma, F.] Univ Telemat Pegaso, Piazza Trieste & Trento, I-80132 Naples, Italy. [Paneque, D.] Max Planck Inst Phys & Astrophys, D-80805 Munich, Germany. [Reimer, A.] Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria. [Reimer, A.] Univ Innsbruck, Inst Theoret Phys, A-6020 Innsbruck, Austria. [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. [Parkinson, P. M. Saz] Univ Hong Kong, Dept Phys, Hong Kong, Hong Kong, Peoples R China. [Schaal, M.] Natl Acad Sci, Natl Res Council Res Associate, Washington, DC 20001 USA. [Siskind, E. J.] NYCB Real Time Comp Inc, Lattingtown, NY 11560 USA. [Suson, D. J.] Purdue Univ Calumet, Dept Chem & Phys, Hammond, IN 46323 USA. [Takahashi, H.] Hiroshima Univ, Dept Phys Sci, Higashihiroshima, Hiroshima 7398526, Japan. [Torres, D. F.] ICREA, Barcelona, Spain. [Troja, E.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA. [Troja, E.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. RP Clark, CJ (reprint author), Max Planck Inst Gravitat Phys, Albert Einstein Inst, D-30167 Hannover, Germany. EM colin.clark@aei.mpg.de RI Morselli, Aldo/G-6769-2011; Johannesson, Gudlaugur/O-8741-2015; Loparco, Francesco/O-8847-2015; Mazziotta, Mario /O-8867-2015; Gargano, Fabio/O-8934-2015; giglietto, nicola/I-8951-2012; Moskalenko, Igor/A-1301-2007; Sgro, Carmelo/K-3395-2016; Bissaldi, Elisabetta/K-7911-2016; Torres, Diego/O-9422-2016; Orlando, E/R-5594-2016; Bonino, Raffaella/S-2367-2016; OI Sgro', Carmelo/0000-0001-5676-6214; SPINELLI, Paolo/0000-0001-6688-8864; Pesce-Rollins, Melissa/0000-0003-1790-8018; Allen, Bruce/0000-0003-4285-6256; orienti, monica/0000-0003-4470-7094; Bonino, Raffaella/0000-0002-4264-1215; Gasparrini, Dario/0000-0002-5064-9495; Baldini, Luca/0000-0002-9785-7726; Hill, Adam/0000-0003-3470-4834; Morselli, Aldo/0000-0002-7704-9553; Johannesson, Gudlaugur/0000-0003-1458-7036; Loparco, Francesco/0000-0002-1173-5673; Mazziotta, Mario /0000-0001-9325-4672; Gargano, Fabio/0000-0002-5055-6395; giglietto, nicola/0000-0002-9021-2888; Moskalenko, Igor/0000-0001-6141-458X; Bissaldi, Elisabetta/0000-0001-9935-8106; Torres, Diego/0000-0002-1522-9065; Caraveo, Patrizia/0000-0003-2478-8018 FU Max-Planck-Gesellschaft (MPG); Deutsche Forschungsgemeinschaft (DFG) [PL 710/1-1] FX This work was supported by the Max-Planck-Gesellschaft (MPG), as well as by the Deutsche Forschungsgemeinschaft (DFG) through an Emmy Noether research grant PL 710/1-1 (PI: Holger J. Pletsch). We are very grateful to all Einstein@Home volunteers who have donated their spare computing time, especially Connor Barry of Lafayette, CO, USA and Rich Johnson of Hayward, CA, USA on whose computers PSR J1906+0722 was first detected. The Fermi-LAT Collaboration acknowledges support for LAT development, operation, and data analysis from NASA and DOE (United States); CEA/Irfu and IN2P3/CNRS (France); ASI and INFN (Italy); MEXT, KEK, and JAXA (Japan); and the K. A. Wallenberg Foundation, the Swedish Research Council, and the National Space Board (Sweden). Science analysis support in the operations phase from INAF (Italy) and CNES (France) is also gratefully acknowledged. NR 28 TC 3 Z9 3 U1 0 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD AUG 10 PY 2015 VL 809 IS 1 AR L2 DI 10.1088/2041-8205/809/1/L2 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO7EJ UT WOS:000359321900002 ER PT J AU Drlica-Wagner, A Albert, A Bechtol, K Wood, M Strigari, L Sanchez-Conde, M Baldini, L Essig, R Cohen-Tanugi, J Anderson, B Bellazzini, R Bloom, ED Caputo, R Cecchi, C Charles, E Chiang, J de Angelis, A Funk, S Fusco, P Gargano, F Giglietto, N Giordano, F Guiriec, S Gustafsson, M Kuss, M Loparco, F Lubrano, P Mirabal, N Mizuno, T Morselli, A Ohsugi, T Orlando, E Persic, M Raino, S Sehgal, N Spada, F Suson, DJ Zaharijas, G Zimmer, S Abbott, T Allam, S Balbinot, E Bauer, AH Benoit-Levy, A Bernstein, RA Bernstein, GM Bertin, E Brooks, D Buckley-Geer, E Burke, DL Rosell, AC Castander, FJ Covarrubias, R D'Andrea, CB da Costa, LN DePoy, DL Desai, S Diehl, HT Cunha, CE Eifler, TF Estrada, J Evrard, AE Neto, AF Fernandez, E Finley, DA Flaugher, B Frieman, J Gaztanaga, E Gerdes, D Gruen, D Gruendl, RA Gutierrez, G Honscheid, K Jain, B James, D Jeltema, T Kent, S Kron, R Kuehn, K Kuropatkin, N Lahav, O Li, TS Luque, E Maia, MAG Makler, M March, M Marshall, J Martini, P Merritt, KW Miller, C Miquel, R Mohr, J Neilsen, E Nord, B Ogando, R Peoples, J Petravick, D Pieres, A Plazas, AA Queiroz, A Romer, AK Roodman, A Rykoff, ES Sako, M Sanchez, E Santiago, B Scarpine, V Schubnell, M Sevilla, I Smith, RC Soares-Santos, M Sobreira, F Suchyta, E Swanson, MEC Tarle, G Thaler, J Thomas, D Tucker, D Walker, AR Wechsler, RH Wester, W Williams, P Yanny, B Zuntz, J AF Drlica-Wagner, A. Albert, A. Bechtol, K. Wood, M. Strigari, L. Sanchez-Conde, M. Baldini, L. Essig, R. Cohen-Tanugi, J. Anderson, B. Bellazzini, R. Bloom, E. D. Caputo, R. Cecchi, C. Charles, E. Chiang, J. de Angelis, A. Funk, S. Fusco, P. Gargano, F. Giglietto, N. Giordano, F. Guiriec, S. Gustafsson, M. Kuss, M. Loparco, F. Lubrano, P. Mirabal, N. Mizuno, T. Morselli, A. Ohsugi, T. Orlando, E. Persic, M. Raino, S. Sehgal, N. Spada, F. Suson, D. J. Zaharijas, G. Zimmer, S. Abbott, T. Allam, S. Balbinot, E. Bauer, A. H. Benoit-Levy, A. Bernstein, R. A. Bernstein, G. M. Bertin, E. Brooks, D. Buckley-Geer, E. Burke, D. L. Carnero Rosell, A. Castander, F. J. Covarrubias, R. D'Andrea, C. B. da Costa, L. N. DePoy, D. L. Desai, S. Diehl, H. T. Cunha, C. E. Eifler, T. F. Estrada, J. Evrard, A. E. Fausti Neto, A. Fernandez, E. Finley, D. A. Flaugher, B. Frieman, J. Gaztanaga, E. Gerdes, D. Gruen, D. Gruendl, R. A. Gutierrez, G. Honscheid, K. Jain, B. James, D. Jeltema, T. Kent, S. Kron, R. Kuehn, K. Kuropatkin, N. Lahav, O. Li, T. S. Luque, E. Maia, M. A. G. Makler, M. March, M. Marshall, J. Martini, P. Merritt, K. W. Miller, C. Miquel, R. Mohr, J. Neilsen, E. Nord, B. Ogando, R. Peoples, J. Petravick, D. Pieres, A. Plazas, A. A. Queiroz, A. Romer, A. K. Roodman, A. Rykoff, E. S. Sako, M. Sanchez, E. Santiago, B. Scarpine, V. Schubnell, M. Sevilla, I. Smith, R. C. Soares-Santos, M. Sobreira, F. Suchyta, E. Swanson, M. E. C. Tarle, G. Thaler, J. Thomas, D. Tucker, D. Walker, A. R. Wechsler, R. H. Wester, W. Williams, P. Yanny, B. Zuntz, J. CA Fermi-LAT Collaboration DES Collaboration TI SEARCH FOR GAMMA-RAY EMISSION FROM DES DWARF SPHEROIDAL GALAXY CANDIDATES WITH FERMI-LAT DATA SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE dark matter; galaxies: dwarf; gamma rays: galaxies; Local Group ID LARGE-AREA TELESCOPE; UNIVERSAL MASS PROFILE; DARK-MATTER; LOCAL GROUP; CONSTRAINTS AB Due to their proximity, high dark-matter (DM) content, and apparent absence of non-thermal processes, Milky Way dwarf spheroidal satellite galaxies (dSphs) are excellent targets for the indirect detection of DM. Recently, eight new dSph candidates were discovered using the first year of data from the Dark Energy Survey (DES). We searched for gamma-ray emission coincident with the positions of these new objects in six years of Fermi Large Area Telescope data. We found no significant excesses of gamma-ray emission. Under the assumption that the DES candidates are dSphs with DM halo properties similar to the known dSphs, we computed individual and combined limits on the velocity-averaged DM annihilation cross section for these new targets. If the estimated DM content of these dSph candidates is confirmed, they will constrain the annihilation cross section to lie below the thermal relic cross section for DM particles with masses less than or similar to 20 GeV annihilating via the b (b) over bar or pi(+)pi(-) channels. C1 [Drlica-Wagner, A.; Allam, S.; Buckley-Geer, E.; Diehl, H. T.; Estrada, J.; Finley, D. A.; Flaugher, B.; Frieman, J.; Gutierrez, G.; Kent, S.; Kuropatkin, N.; Merritt, K. W.; Neilsen, E.; Nord, B.; Peoples, J.; Scarpine, V.; Soares-Santos, M.; Sobreira, F.; Tucker, D.; Wester, W.; Yanny, B.] Fermilab Natl Accelerator Lab, Ctr Particle Astrophys, Batavia, IL 60510 USA. [Albert, A.; Wood, M.; Bloom, E. D.; Charles, E.; Chiang, J.; Funk, S.; Orlando, E.] Stanford Univ, Dept Phys, Kavli Inst Particle Astrophys & Cosmol, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA. [Albert, A.; Wood, M.; Bloom, E. D.; Charles, E.; Chiang, J.; Funk, S.; Orlando, E.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA. [Bechtol, K.; Frieman, J.; Kron, R.; Williams, P.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Strigari, L.] Texas A&M Univ, Dept Phys & Astron, College Stn, TX 77843 USA. [Sanchez-Conde, M.; Zimmer, S.] AlbaNova, Oskar Klein Ctr Cosmoparticle Phys, SE-10691 Stockholm, Sweden. [Sanchez-Conde, M.; Zimmer, S.] Stockholm Univ, Dept Phys, AlbaNova, SE-10691 Stockholm, Sweden. [Baldini, L.] Univ Pisa, I-56127 Pisa, Italy. [Baldini, L.; Bellazzini, R.; Kuss, M.; Spada, F.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy. [Essig, R.] SUNY Stony Brook, CN Yang Inst Theoret Phys, Stony Brook, NY 11794 USA. [Cohen-Tanugi, J.] Univ Montpellier 2, CNRS, IN2P3, Lab Univers & Particules Montpellier, Montpellier, France. [Caputo, R.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Dept Phys, Santa Cruz, CA 95064 USA. [Caputo, R.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Cecchi, C.; Lubrano, P.] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy. [Cecchi, C.; Lubrano, P.] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy. [de Angelis, A.] Univ Udine, Dipartimento Fis, I-33100 Udine, Italy. [de Angelis, A.] Ist Nazl Fis Nucl, Sez Trieste, Grp Collegato Udine, I-33100 Udine, Italy. [Fusco, P.; Giglietto, N.; Giordano, F.; Loparco, F.; Raino, S.] Univ Bari, Dipartimento Fis M Merlin, I-70126 Bari, Italy. [Fusco, P.; Giglietto, N.; Giordano, F.; Loparco, F.; Raino, S.] Politecn Bari, I-70126 Bari, Italy. [Fusco, P.; Gargano, F.; Giglietto, N.; Giordano, F.; Loparco, F.; Raino, S.] Ist Nazl Fis Nucl, Sez Bari, I-70126 Bari, Italy. [Guiriec, S.; Mirabal, N.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Gustafsson, M.] Univ Gottingen, Inst Theoret Phys, Fac Phys, D-37077 Gottingen, Germany. [Mizuno, T.; Ohsugi, T.] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Hiroshima 7398526, Japan. [Morselli, A.] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, I-00133 Rome, Italy. [Persic, M.; Zaharijas, G.] Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy. [Persic, M.] Osserv Astron Trieste, Ist Nazl Astrofis, I-34143 Trieste, Italy. [Sehgal, N.] SUNY Stony Brook, Dept Phys & Astron, Stony Brook, NY 11794 USA. [Suson, D. J.] Purdue Univ Calumet, Dept Chem & Phys, Hammond, IN 46323 USA. [Zaharijas, G.] Univ Trieste, I-34127 Trieste, Italy. [Zaharijas, G.] Univ Nova Gorica, Lab Astroparticle Phys, SI-5000 Nova Gorica, Slovenia. [Abbott, T.; James, D.; Smith, R. C.; Walker, A. R.] Cerro Tololo Interamer Observ, Natl Opt Astron Observ, La Serena, Chile. [Allam, S.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Balbinot, E.] Univ Surrey, Dept Phys, Guildford GU2 7XH, Surrey, England. [Balbinot, E.; Carnero Rosell, A.; da Costa, L. N.; Fausti Neto, A.; Maia, M. A. G.; Ogando, R.; Sobreira, F.] Lab Interinst E Astron LIneA, BR-20921400 Rio De Janeiro, RJ, Brazil. [Bauer, A. H.; Castander, F. J.; Gaztanaga, E.] Fac Ciencies, IEEC CSIC, Inst Ciencies Espai, E-08193 Barcelona, Spain. [Benoit-Levy, A.; Brooks, D.; Lahav, O.] UCL, Dept Phys & Astron, London WC1E 6BT, England. [Bernstein, R. A.] Carnegie Observat, Pasadena, CA 91101 USA. [Bernstein, G. M.; Eifler, T. F.; Jain, B.; March, M.; Sako, M.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. [Bertin, E.] Univ Paris 06, Inst Astrophys Paris, F-75014 Paris, France. [Bertin, E.] CNRS, UMR7095, F-75014 Paris, France. [Burke, D. L.; Roodman, A.; Rykoff, E. S.; Wechsler, R. H.] SLAC Natl Accelerator Lab, Menlo Pk, CA 94025 USA. [Carnero Rosell, A.; da Costa, L. N.; Maia, M. A. G.; Ogando, R.] Observ Nacl, BR-20921400 Rio De Janeiro, RJ, Brazil. [Covarrubias, R.; Gruendl, R. A.; Petravick, D.; Swanson, M. E. C.] Univ Illinois, Natl Ctr Supercomp Applicat, Urbana, IL 61801 USA. [D'Andrea, C. B.; Thomas, D.] Univ Portsmouth, Inst Cosmol & Gravitat, Portsmouth PO1 3FX, Hants, England. [DePoy, D. L.; Li, T. S.; Marshall, J.] Texas A&M Univ, George P & Cynthia Woods Mitchell Inst Fundamenta, College Stn, TX 77843 USA. [DePoy, D. L.; Li, T. S.; Marshall, J.] Texas A&M Univ, Dept Phys & Astron, College Stn, TX 77843 USA. [Desai, S.; Mohr, J.] Excellence Cluster Universe, D-85748 Garching, Germany. [Desai, S.; Mohr, J.] Univ Munich, Dept Phys, D-81679 Munich, Germany. [Cunha, C. E.; Roodman, A.; Wechsler, R. H.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA. [Eifler, T. F.; Plazas, A. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Evrard, A. E.; Gerdes, D.; Miller, C.; Schubnell, M.; Tarle, G.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA. [Fernandez, E.; Miquel, R.] Inst Catalana Recerca & Estudis Avancats, E-08010 Barcelona, Spain. [Fernandez, E.; Miquel, R.] Univ Autonoma Barcelona, Inst Fis Altes Energies, E-08193 Barcelona, Spain. [Gruen, D.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Gruen, D.] Univ Observ Munich, D-81679 Munich, Germany. [Gruendl, R. A.; Sevilla, I.] Univ Illinois, Dept Astron, Urbana, IL 61801 USA. [Honscheid, K.; Martini, P.; Suchyta, E.] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA. [Honscheid, K.; Suchyta, E.] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA. [Jeltema, T.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA. [Jeltema, T.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA. [Kuehn, K.] Australian Astron Observ, N Ryde, NSW 2113, Australia. [Kuehn, K.] Argonne Natl Lab, Lemont, IL 60639 USA. [Luque, E.; Pieres, A.; Queiroz, A.; Santiago, B.] Univ Fed Rio Grande do Sul, Inst Fis, BR-91501970 Porto Alegre, RS, Brazil. [Makler, M.] Ctr Brasileiro Pesquisas Fis, ICRA, BR-22290180 Rio De Janeiro, RJ, Brazil. [Martini, P.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Miller, C.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Plazas, A. A.] Brookhaven Natl Lab, Upton, NY 11973 USA. [Romer, A. K.] Univ Sussex, Ctr Astron, Brighton BN1 9QH, E Sussex, England. [Sanchez, E.; Sevilla, I.] Ctr Invest Energet Medioambientales & Tecnol CIEM, Madrid, Spain. [Thaler, J.] Univ Illinois, Dept Phys, Urbana, IL 61801 USA. [Wechsler, R. H.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA. [Zuntz, J.] Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England. RP Drlica-Wagner, A (reprint author), Fermilab Natl Accelerator Lab, Ctr Particle Astrophys, POB 500, Batavia, IL 60510 USA. EM kadrlica@fnal.gov; aalbert@slac.stanford.edu; bechtol@kicp.uchicago.edu; mdwood@slac.stanford.edu; strigari@physics.tamu.edu RI Balbinot, Eduardo/E-8019-2015; Morselli, Aldo/G-6769-2011; Loparco, Francesco/O-8847-2015; Gargano, Fabio/O-8934-2015; Makler, Martin/G-2639-2012; giglietto, nicola/I-8951-2012; Sanchez, Eusebio/H-5228-2015; Sobreira, Flavia/F-4168-2015; Fernandez, Enrique/L-5387-2014; Orlando, E/R-5594-2016; Gaztanaga, Enrique/L-4894-2014; Funk, Stefan/B-7629-2015; Ogando, Ricardo/A-1747-2010 OI Giordano, Francesco/0000-0002-8651-2394; Balbinot, Eduardo/0000-0002-1322-3153; Zaharijas, Gabrijela/0000-0001-8484-7791; Persic, Massimo/0000-0003-1853-4900; Strigari, Louis/0000-0001-5672-6079; Baldini, Luca/0000-0002-9785-7726; Tucker, Douglas/0000-0001-7211-5729; Morselli, Aldo/0000-0002-7704-9553; Loparco, Francesco/0000-0002-1173-5673; Gargano, Fabio/0000-0002-5055-6395; Makler, Martin/0000-0003-2206-2651; giglietto, nicola/0000-0002-9021-2888; Sanchez, Eusebio/0000-0002-9646-8198; Sobreira, Flavia/0000-0002-7822-0658; Fernandez, Enrique/0000-0002-6405-9488; Gaztanaga, Enrique/0000-0001-9632-0815; Suchyta, Eric/0000-0002-7047-9358; Funk, Stefan/0000-0002-2012-0080; Ogando, Ricardo/0000-0003-2120-1154 FU U.S. Department of Energy; U.S. National Science Foundation; Ministry of Science and Education of Spain; Science and Technology Facilities Council of the United Kingdom; Higher Education Funding Council for England; National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign; Kavli Institute of Cosmological Physics at the University of Chicago; Center for Cosmology and Astro-Particle Physics at the Ohio State University; Mitchell Institute for Fundamental Physics and Astronomy at Texas AM University; Financiadora de Estudos e Projetos; Fundacao Carlos Chagas Filho de Amparo a Pesquisa do Estado do Rio de Janeiro; Conselho Nacional de Desenvolvimento Cientifico e Tecnologico; Ministerio da Ciencia, Tecnologia e Inovacao; Deutsche Forschungsgemeinschaft; National Science Foundation [AST-1138766]; MINECO [AYA2012-39559, ESP2013-48274, FPA2013-47986]; Centro de Excelencia Severo Ochoa [SEV-2012-0234]; European Union; Argonne National Laboratory; University of California at Santa Cruz; University of Cambridge; Centro de Investigaciones Energeticas, Medioambientales y Tecnologicas-Madrid; University of Chicago; University College London; DES-Brazil Consortium; University of Edinburgh; Eidgenossische Technische Hochschule (ETH) Zurich; Fermi National Accelerator Laboratory; University of Illinois at Urbana-Champaign; Institut de Ciencies de l'Espai (IEEC/CSIC); Institut de Fisica d'Altes Energies; Lawrence Berkeley National Laboratory; Ludwig-Maximilians Universitat Munchen; associated Excellence Cluster Universe; University of Michigan; National Optical Astronomy Observatory; University of Nottingham; Ohio State University; University of Pennsylvania; University of Portsmouth; SLAC National Accelerator Laboratory; Stanford University; University of Sussex; Texas AM University; PAPDRJ CAPES/FAPERJ; DOE [DE-AC02-98CH10886]; JPL; National Aeronautics and Space Administration FX The Fermi-LAT Collaboration acknowledges support for LAT development, operation and data analysis from NASA and DOE (United States), CEA/Irfu and IN2P3/CNRS (France), ASI and INFN (Italy), MEXT, KEK, and JAXA (Japan), and the K. A. Wallenberg Foundation, the Swedish Research Council and the National Space Board (Sweden). Science analysis support in the operations phase from INAF (Italy) and CNES (France) is also gratefully acknowledged. Funding for the DES Projects has been provided by the U.S. Department of Energy, the U.S. National Science Foundation, the Ministry of Science and Education of Spain, the Science and Technology Facilities Council of the United Kingdom, the Higher Education Funding Council for England, the National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign, the Kavli Institute of Cosmological Physics at the University of Chicago, the Center for Cosmology and Astro-Particle Physics at the Ohio State University, the Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M University, Financiadora de Estudos e Projetos, Fundacao Carlos Chagas Filho de Amparo a Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Cientifico e Tecnologico and the Ministerio da Ciencia, Tecnologia e Inovacao, the Deutsche Forschungsgemeinschaft and the Collaborating Institutions in the Dark Energy Survey. The DES data management system is supported by the National Science Foundation under Grant Number AST-1138766. The DES participants from Spanish institutions are partially supported by MINECO under grants AYA2012-39559, ESP2013-48274, FPA2013-47986, and Centro de Excelencia Severo Ochoa SEV-2012-0234, some of which include ERDF funds from the European Union. The Collaborating Institutions are Argonne National Laboratory, the University of California at Santa Cruz, the University of Cambridge, Centro de Investigaciones Energeticas, Medioambientales y Tecnologicas-Madrid, the University of Chicago, University College London, the DES-Brazil Consortium, the University of Edinburgh, the Eidgenossische Technische Hochschule (ETH) Zurich, Fermi National Accelerator Laboratory, the University of Illinois at Urbana-Champaign, the Institut de Ciencies de l'Espai (IEEC/CSIC), the Institut de Fisica d'Altes Energies, Lawrence Berkeley National Laboratory, the Ludwig-Maximilians Universitat Munchen and the associated Excellence Cluster Universe, the University of Michigan, the National Optical Astronomy Observatory, the University of Nottingham, the Ohio State University, the University of Pennsylvania, the University of Portsmouth, SLAC National Accelerator Laboratory, Stanford University, the University of Sussex, and Texas A&M University. A.C.R. acknowledges financial support provided by the PAPDRJ CAPES/FAPERJ Fellowship. A.A.P. was supported by DOE grant DE-AC02-98CH10886 and by JPL, run by Caltech under a contract for NASA. This research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. We would like to thank the anonomous referee for many helpful comments. NR 43 TC 43 Z9 43 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 AUG 10 PY 2015 VL 809 IS 1 AR L4 DI 10.1088/2041-8205/809/1/L4 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO7EJ UT WOS:000359321900004 ER PT J AU Zhao, JW Chen, RZ Hartlep, T Kosovichev, AG AF Zhao, Junwei Chen, Ruizhu Hartlep, Thomas Kosovichev, Alexander G. TI DETECTION OF FAST-MOVING WAVES PROPAGATING OUTWARD ALONG SUNSPOTS' RADIAL DIRECTION IN THE PHOTOSPHERE SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE sunspots; Sun: helioseismology; Sun: oscillations ID SOLAR ACOUSTIC-WAVES; RUNNING PENUMBRAL WAVES; OSCILLATIONS; CHROMOSPHERE AB Helioseismic and magnetohydrodynamic waves are abundant in and above sunspots. Through cross-correlating oscillation signals in the photosphere observed by the Solar Dynamics Observatory/Helioseismic and Magnetic Imager, we reconstruct how waves propagate away from virtual wave sources located inside a sunspot. In addition to the usual helioseismic wave, a fast-moving wave is detected traveling along the sunspot's radial direction from the umbra to about 15 Mm beyond the sunspot boundary. The wave has a frequency range of 2.5-4.0 mHz with a phase velocity of 45.3 km s(-1), substantially faster than the typical speeds of Alfven and magnetoacoustic waves in the photosphere. The observed phenomenon is consistent with a scenario of that a magnetoacoustic wave is excited at approximately 5 Mm beneath the sunspot. Its wavefront travels to and sweeps across the photosphere with a speed higher than the local magnetoacoustic speed. The fast-moving wave, if truly excited beneath the sunspot's surface, will help open a new window for studying the internal structure and dynamics of sunspots. C1 [Zhao, Junwei; Chen, Ruizhu] Stanford Univ, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA. [Chen, Ruizhu] Stanford Univ, Dept Phys, Stanford, CA 94305 USA. [Hartlep, Thomas] NASA, BAER Inst, Ames Res Ctr, Moffett Field, CA 94043 USA. [Kosovichev, Alexander G.] New Jersey Inst Technol, Dept Phys, Newark, NJ 07102 USA. RP Zhao, JW (reprint author), Stanford Univ, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA. RI Zhao, Junwei/A-1177-2007; OI Hartlep, Thomas/0000-0002-5062-9507 FU NASA [NAS5-02139] FX SDO is a NASA mission, and the HMI project is supported by NASA contract NAS5-02139 to Stanford University. NR 19 TC 3 Z9 3 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD AUG 10 PY 2015 VL 809 IS 1 AR L15 DI 10.1088/2041-8205/809/1/L15 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO7EJ UT WOS:000359321900015 ER PT J AU Kozorezov, AG Lambert, C Marsili, F Stevens, MJ Verma, VB Stern, JA Horansky, R Dyer, S Duff, S Pappas, DP Lita, A Shaw, MD Mirin, RP Nam, SW AF Kozorezov, A. G. Lambert, C. Marsili, F. Stevens, M. J. Verma, V. B. Stern, J. A. Horansky, R. Dyer, S. Duff, S. Pappas, D. P. Lita, A. Shaw, M. D. Mirin, R. P. Nam, Sae Woo TI Quasiparticle recombination in hotspots in superconducting current-carrying nanowires SO PHYSICAL REVIEW B LA English DT Article ID SINGLE-PHOTON DETECTORS; TRANSITION-EDGE SENSORS; TUNGSTEN-SILICIDE; EFFICIENCY; STRIPS; FILM AB We describe a kinetic model of recombination of nonequilibrium quasiparticles generated by single photon absorption in superconducting current-carrying nanowires. The model is developed to interpret two-photon detection experiments in which a single photon does not possess sufficient energy for breaking superconductivity at a fixed low bias current. We show that quasiparticle self-recombination in relaxing hotspots dominates diffusion expansion effects and explains the observed strong bias current, wavelength, and temperature dependencies of hotspot relaxation in tungsten silicide superconducting nanowire single-photon detectors. C1 [Kozorezov, A. G.; Lambert, C.] Univ Lancaster, Dept Phys, Lancaster, England. [Marsili, F.; Stern, J. A.; Shaw, M. D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Stevens, M. J.; Verma, V. B.; Horansky, R.; Dyer, S.; Duff, S.; Pappas, D. P.; Lita, A.; Mirin, R. P.; Nam, Sae Woo] NIST, Boulder, CO 80305 USA. RP Kozorezov, AG (reprint author), Univ Lancaster, Dept Phys, Lancaster, England. OI Mirin, Richard/0000-0002-4472-4655 FU Engineering and Physical Sciences Research Council FX A.G.K. and C.L. gratefully acknowledge financial support from the Engineering and Physical Sciences Research Council. Part of the research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. NR 39 TC 5 Z9 5 U1 2 U2 13 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1098-0121 EI 1550-235X J9 PHYS REV B JI Phys. Rev. B PD AUG 6 PY 2015 VL 92 IS 6 AR 064504 DI 10.1103/PhysRevB.92.064504 PG 16 WC Physics, Condensed Matter SC Physics GA CO3HD UT WOS:000359046500010 ER PT J AU Jensen, BD Wise, KE Odegard, GM AF Jensen, Benjamin D. Wise, Kristopher E. Odegard, Gregory M. TI The effect of time step, thermostat, and strain rate on ReaxFF simulations of mechanical failure in diamond, graphene, and carbon nanotube SO JOURNAL OF COMPUTATIONAL CHEMISTRY LA English DT Article DE molecular dynamics; SWNT; molecular modeling; fracture; mechanical properties ID REACTIVE FORCE-FIELD; MOLECULAR-DYNAMICS SIMULATIONS; THERMAL-DECOMPOSITION; STRENGTH; OXIDATION; SURFACES; FRACTURE; HYDROCARBONS; TRANSITIONS; VALIDATION AB As the sophistication of reactive force fields for molecular modeling continues to increase, their use and applicability has also expanded, sometimes beyond the scope of their original development. Reax Force Field (ReaxFF), for example, was originally developed to model chemical reactions, but is a promising candidate for modeling fracture because of its ability to treat covalent bond cleavage. Performing reliable simulations of a complex process like fracture, however, requires an understanding of the effects that various modeling parameters have on the behavior of the system. This work assesses the effects of time step size, thermostat algorithm and coupling coefficient, and strain rate on the fracture behavior of three carbon-based materials: graphene, diamond, and a carbon nanotube. It is determined that the simulated stress-strain behavior is relatively independent of the thermostat algorithm, so long as coupling coefficients are kept above a certain threshold. Likewise, the stress-strain response of the materials was also independent of the strain rate, if it is kept below a maximum strain rate. Finally, the mechanical properties of the materials predicted by the Chenoweth C/H/O parameterization for ReaxFF are compared with literature values. Some deficiencies in the Chenoweth C/H/O parameterization for predicting mechanical properties of carbon materials are observed. (c) 2015 Wiley Periodicals, Inc. C1 [Jensen, Benjamin D.; Wise, Kristopher E.] NASA, Langley Res Ctr, Adv Mat & Proc Branch, Hampton, VA 23665 USA. [Jensen, Benjamin D.; Odegard, Gregory M.] Michigan Technol Univ, Dept Mech Engn Engn Mech, Houghton, MI 49931 USA. RP Odegard, GM (reprint author), Michigan Technol Univ, Dept Mech Engn Engn Mech, Houghton, MI 49931 USA. EM gmodegar@mtu.edu RI Jensen, Benjamin/B-1297-2013 OI Jensen, Benjamin/0000-0002-7982-0663 FU NASA under the Revolutionary Technology Challenges Program [NNX09AM50A] FX Contract grant sponsor: NASA under the Revolutionary Technology Challenges Program; Contract grant number: NNX09AM50A NR 61 TC 5 Z9 5 U1 16 U2 53 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0192-8651 EI 1096-987X J9 J COMPUT CHEM JI J. Comput. Chem. PD AUG 5 PY 2015 VL 36 IS 21 BP 1587 EP 1596 DI 10.1002/jcc.23970 PG 10 WC Chemistry, Multidisciplinary SC Chemistry GA CM7SN UT WOS:000357896900003 PM 26096628 ER PT J AU Breon, FM Vermote, E Murphy, EF Franch, B AF Breon, Francois-Marie Vermote, Eric Murphy, Emilie Fedele Franch, Belen TI Measuring the Directional Variations of Land Surface Reflectance From MODIS SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE Bidirectional reflectance distribution function (BRDF); Moderate Resolution Imaging Spectroradiometer (MODIS); surface reflectance ID KERNEL-DRIVEN MODELS; BIDIRECTIONAL REFLECTANCE; ALBEDO RETRIEVAL; BRDF; VARIABILITY; PRODUCTS; AIRBORNE; IMPACT; FIELD; SPOT AB The directional variation of land surface reflectance generates an apparent noise in the time series acquired from satellites with variable observation geometries, which can be corrected through appropriate modeling of the bidirectional reflectance distribution function (BRDF). In a previous paper, we described and validated the VJB method that estimates a target BRDF shape and corrects for directional effects and yet retains the high temporal resolution of the measurement. Here, we analyze its potential to measure the BRDF of targets at the 0.5-km resolution of Moderate Resolution Imaging Spectroradiometer (MODIS). The description of the BRDF in the NASA MCD43A1 product shows very large temporal variations that are unrealistic. However, the reflectance time series, normalized to a standard observation geometry using this modeling, have a similar quality as those derived using VJB. Conversely, the MCD43A1 modeled reflectances for a nonstandard geometry are unrealistically variable. These results indicate that the standard BRDF model inversion used to derive the MCD43A1 product is underconstrained due to the limited directional sampling of the 16-day composite period. The apparent noise in the corrected reflectance time series is significantly larger than the one obtained at lower spatial resolution, and is very much a function of the spatial heterogeneity of the area surrounding the target. These results strongly indicate that the multitemporal MODIS measurement at high spatial resolution (0.5 km) is affected by a change in the effective resolution for off-nadir observation and by inaccurate registration. The resulting noise in the measurements precludes an accurate measurement of the BRDF at such a scale. C1 [Breon, Francois-Marie] CEA CNRS UVSQ, IPSL, Lab Sci Climat & Environm, UMR, F-91191 Gif Sur Yvette, France. [Vermote, Eric] NASA, Goddard Space Flight Ctr, Terr Informat Syst Lab, Greenbelt, MD 20771 USA. [Murphy, Emilie Fedele; Franch, Belen] NASA, Goddard Space Flight Ctr, Terr Informat Syst Lab, Greenbelt, MD 20771 USA. [Murphy, Emilie Fedele; Franch, Belen] Univ Maryland, College Pk, MD 20740 USA. RP Breon, FM (reprint author), CEA CNRS UVSQ, IPSL, Lab Sci Climat & Environm, UMR, F-91191 Gif Sur Yvette, France. EM breon@lsce.ipsl.fr; eric.f.vermote@nasa.gov; emilie.murphy@nasa.gov; befranch@umd.edu RI Breon, Francois-Marie/M-4639-2016 OI Breon, Francois-Marie/0000-0003-2128-739X NR 28 TC 3 Z9 3 U1 1 U2 1 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0196-2892 EI 1558-0644 J9 IEEE T GEOSCI REMOTE JI IEEE Trans. Geosci. Remote Sensing PD AUG PY 2015 VL 53 IS 8 BP 4638 EP 4649 DI 10.1109/TGRS.2015.2405344 PG 12 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA DN3VU UT WOS:000376993000002 ER PT J AU Piles, M McColl, KA Entekhabi, D Das, N Pablos, M AF Piles, Maria McColl, Kaighin A. Entekhabi, Dara Das, Narendra Pablos, Miriam TI Sensitivity of Aquarius Active and Passive Measurements Temporal Covariability to Land Surface Characteristics SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE Active-passive; Aquarius/SAC-D mission; L-band microwave remote sensing; radiometer; scatterometer; Soil Moisture Active Passive (SMAP) mission ID SOIL-MOISTURE; SMAP MISSION; VALIDATION; SCATTERING; HYDROLOGY; DIVERSITY; SALINITY; EMISSION; FIELD AB Active and passive microwave observations over land are affected by surface characteristics in different ways. L-band radar backscatter and radiometer measurements each have distinct advantages and problematic issues when applied to surface soil moisture estimation. Spaceborne radiometry has the advantage of better sensitivity to the geophysical parameter but suffers from coarse spatial resolution given limitations on antenna dimensions. Active sensing has the advantage of higher spatial resolution, but the measurements are, relative to radiometry, more affected by the confounding influences of scattering by vegetation and rough surfaces. Active and passive measurements can potentially span different scales and allow the combining of the relative advantages of the two sensing approaches. This strategy is being implemented in the NASA Soil Moisture Active Passive (SMAP) mission, which relies on the relationship between active and passive measurements to provide 9-km surface soil moisture estimates. The aim of this paper is to study the sensitivity of spaceborne L-band active and passive temporal covariations to land surface characteristics, in preparation for SMAP. A significant linear relationship (with slope beta) is obtained between NASA's Aquarius scatterometer and radiometer observations across major global biomes. The error in beta estimation is found to increase with land cover heterogeneity and to be unaffected by vegetation density (up to moderate densities). Results show that beta estimated with two to eight months of Aquarius measurements (depending on vegetation seasonality) reflect local vegetation cover conditions under surfaces with complex mixture of vegetation, surface roughness, and dielectric constant. C1 [Piles, Maria; Pablos, Miriam] Univ Politecn Cataluna, Dept Teoria Senyal & Comunicac, Remote Sensing Lab, ES-08034 Barcelona, Spain. [Piles, Maria; Pablos, Miriam] UPC, CRAE, IEEC, Barcelona 08034, Spain. [Piles, Maria; Pablos, Miriam] SMOS BEC, Barcelona 08003, Spain. [McColl, Kaighin A.; Entekhabi, Dara] MIT, Dept Civil & Environm Engn, 77 Massachusetts Ave, Cambridge, MA 02139 USA. [Das, Narendra] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. RP Piles, M (reprint author), Univ Politecn Cataluna, Dept Teoria Senyal & Comunicac, Remote Sensing Lab, ES-08034 Barcelona, Spain. EM maria.piles@tsc.upc.edu RI Pablos Hernandez, Miriam/G-2845-2013; OI Pablos Hernandez, Miriam/0000-0003-2694-7107; Piles, Maria/0000-0002-1169-3098 NR 35 TC 7 Z9 7 U1 4 U2 5 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0196-2892 EI 1558-0644 J9 IEEE T GEOSCI REMOTE JI IEEE Trans. Geosci. Remote Sensing PD AUG PY 2015 VL 53 IS 8 BP 4700 EP 4711 DI 10.1109/TGRS.2015.2407611 PG 12 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA DN3VU UT WOS:000376993000007 ER PT J AU Chapman, BD Comer, DC Isla, JA Silverman, H AF Chapman, Bruce D. Comer, Douglas C. Isla, Johny A. Silverman, Helaine TI The Measurement by Airborne Synthetic Aperture Radar (SAR) of Disturbance Within the Nasca World Heritage Site SO CONSERVATION AND MANAGEMENT OF ARCHAEOLOGICAL SITES LA English DT Article DE Nasca; geoglyphs; Synthetic Aperture Radar (SAR); Uninhabited Aerial Vehicle Synthetic Aperture Radar (UAVSAR); remote sensing; World Heritage Sites; archaeology; heritage management; monitoring ID VALLEYS; NAZCA; PERU AB In this paper we report on our use of Synthetic Aperture Radar (SAR) as a means of monitoring the Lines and Geoglyphs of Nasca and Pampas de Jumana World Heritage Site in Peru, where the colossal ground drawings, popularly known as the Nasca Lines, are found. Our research to date indicates that the environment in which the Nasca geoglyphs are found, and the nature of the geoglyphs themselves, are suited perfectly for investigation by SAR. SAR also provides a new and valuable tool for understanding the human activities and natural processes that have damaged the geoglyphs and which, unchecked, will continue to do so in the future. Further, SAR can be used to categorize geoglyphs according to structural differences and similarities in ways that have heretofore not been possible, thereby serving as a basis for a geoglyph catalogue. C1 [Chapman, Bruce D.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Isla, Johny A.] Minist Culture, Lima, Peru. [Silverman, Helaine] Univ Illinois, Dept Anthropol, Champaign, IL USA. RP Chapman, BD (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. EM Bruce.D.Chapman@jpl.nasa.gov NR 21 TC 0 Z9 0 U1 3 U2 3 PU ROUTLEDGE JOURNALS, TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXFORDSHIRE, ENGLAND SN 1350-5033 EI 1753-5522 J9 CONSERV MANAGE ARCHA JI Conserv. Manag. Archaeol. Sites PD AUG PY 2015 VL 17 IS 3 BP 270 EP 286 DI 10.1080/13505033.2015.1129801 PG 17 WC Archaeology SC Archaeology GA DK4TC UT WOS:000374911500006 ER PT J AU Autsavapromporn, N Plante, I Liu, CH Konishi, T Usami, N Funayama, T Uchihori, Y Hei, TK Azzam, EI Yamada, S Murakami, T Suzuki, M AF Autsavapromporn, Narongchai Plante, Ianik Liu, Cuihua Konishi, Teruaki Usami, Noriko Funayama, Tomoo Uchihori, Yukio Hei, Tom K. Azzam, Edouard I. Yamada, Sirikan Murakami, Takeshi Suzuki, Masao TI Bystander effect and genomic instability in human cells and their progeny after irradiation with X rays, protons or carbon ions: role of gap junction communication SO CANCER RESEARCH LA English DT Meeting Abstract CT 106th Annual Meeting of the American-Association-for-Cancer-Research (AACR) CY APR 18-22, 2015 CL Philadelphia, PA SP Amer Assoc Canc Res C1 [Autsavapromporn, Narongchai; Yamada, Sirikan] Chiang Mai Univ, Chiang Mai 50000, Thailand. [Plante, Ianik] NASA, Johnson Space Ctr, Houston, TX USA. [Liu, Cuihua; Konishi, Teruaki; Uchihori, Yukio; Murakami, Takeshi; Suzuki, Masao] Natl Inst Radiol Sci, Chiba 260, Japan. [Usami, Noriko] High Energy Accelerator Res Org, Ibaraki, Japan. [Funayama, Tomoo] Japan Atom Energy Agcy, Gunma, Japan. [Hei, Tom K.] Columbia Univ, New York, NY USA. [Azzam, Edouard I.] Rutgers State Univ, Newark, NJ 07102 USA. NR 0 TC 0 Z9 0 U1 1 U2 1 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 AUG 1 PY 2015 VL 75 SU 15 MA 1815 DI 10.1158/1538-7445.AM2015-1815 PG 2 WC Oncology SC Oncology GA DF8AH UT WOS:000371578503300 ER PT J AU Bautista, MA Fivet, V Ballance, C Quinet, P Ferland, G Mendoza, C Kallman, TR AF Bautista, Manuel A. Fivet, Vanessa Ballance, Connor Quinet, Pascal Ferland, Gary Mendoza, Claudio Kallman, Timothy R. TI ATOMIC DATA AND SPECTRAL MODEL FOR Fe II SO ASTROPHYSICAL JOURNAL LA English DT Article DE atomic data; atomic processes; ISM: abundances; line: formation; stars: massive; stars: variables: T Tauri, Herbig Ae/Be ID ELECTRON-IMPACT EXCITATION; IRON-PROJECT; TRANSITION-PROBABILITIES; FORBIDDEN TRANSITIONS; COLLISION STRENGTHS; R-MATRIX; QUASARS; BREIT; LINES; EMISSION AB We present extensive calculations of radiative transition rates and electron impact collision strengths for Fe II. The data sets involve 52 levels from the 3d(7), 3d(6)4s, and 3d(5)4s(2) configurations. Computations of A-values are carried out with a combination of state-of-the-art multiconfiguration approaches, namely the relativistic Hartree-Fock, Thomas-Fermi-Dirac potential, and Dirac-Fock methods, while the R-matrix plus intermediate coupling frame transformation, Breit-Pauli R-matrix, and Dirac R-matrix packages are used to obtain collision strengths. We examine the advantages and shortcomings of each of these methods, and estimate rate uncertainties from the resulting data dispersion. We proceed to construct excitation balance spectral models, and compare the predictions from each data set with observed spectra from various astronomical objects. We are thus able to establish benchmarks in the spectral modeling of [Fe II] emission in the IR and optical regions as well as in the UV Fe II absorption spectra. Finally, we provide diagnostic line ratios and line emissivities for emission spectroscopy as well as column densities for absorption spectroscopy. All atomic data and models are available online and through the AtomPy atomic data curation environment. C1 [Bautista, Manuel A.; Fivet, Vanessa] Western Michigan Univ, Dept Phys, Kalamazoo, MI 49008 USA. [Ballance, Connor] Auburn Univ, Dept Phys, Auburn, AL 36849 USA. [Quinet, Pascal] Univ Mons UMONS, Astrophys & Spect, B-7000 Mons, Belgium. [Ferland, Gary] Univ Kentucky, Dept Phys & Astron, Lexinton, KY 40506 USA. [Mendoza, Claudio] Inst Venezolano Invest Cient, Ctr Fis, Caracas 1020, Venezuela. [Kallman, Timothy R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Bautista, MA (reprint author), Western Michigan Univ, Dept Phys, Kalamazoo, MI 49008 USA. EM manuel.bautista@wmich.edu OI Mendoza, Claudio/0000-0002-2854-4806; Ferland, Gary/0000-0003-4503-6333 FU NASA Astronomy and Physics Research and Analysis Program [NNX09AB99G]; Space Telescope Science Institute [GO-11745] FX We acknowledge support from the NASA Astronomy and Physics Research and Analysis Program (Award NNX09AB99G) and the Space Telescope Science Institute (Project GO-11745). V.F. is currently a postdoctoral researcher of the Return Grant Program of the Belgian Scientific Policy (BELSPO). P.Q. is Research Director of the Belgian National Fund for Scientific Research F.R.S.-FNRS. NR 40 TC 8 Z9 8 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD AUG 1 PY 2015 VL 808 IS 2 AR 174 DI 10.1088/0004-637X/808/2/174 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DF0BA UT WOS:000371002400070 ER PT J AU Bennett, DP Bhattacharya, A Anderson, J Bond, IA Anderson, N Barry, R Batista, V Beaulieu, JP Depoy, DL Dong, SB Gaudi, BS Gilbert, E Gould, A Pfeifle, R Pogge, RW Suzuki, D Terry, S Udalski, A AF Bennett, D. P. Bhattacharya, A. Anderson, J. Bond, I. A. Anderson, N. Barry, R. Batista, V. Beaulieu, J. -P. DePoy, D. L. Dong, Subo Gaudi, B. S. Gilbert, E. Gould, A. Pfeifle, R. Pogge, R. W. Suzuki, D. Terry, S. Udalski, A. TI CONFIRMATION OF THE PLANETARY MICROLENSING SIGNAL AND STAR AND PLANET MASS DETERMINATIONS FOR EVENT OGLE-2005-BLG-169 SO ASTROPHYSICAL JOURNAL LA English DT Article DE gravitational lensing: micro; planetary systems ID GALACTIC BULGE; SNOW LINE; OGLE-III; JUPITER/SATURN ANALOG; LUMINOSITY-RELATION; IMAGE SUBTRACTION; MAIN-SEQUENCE; GIANT PLANETS; SYSTEMS; EXTINCTION AB We present Hubble Space Telescope (HST) Wide Field Camera 3 (WFC3) observations of the source and lens stars for planetary microlensing event OGLE-2005-BLG-169, which confirm the relative proper motion prediction due to the planetary light curve signal observed for this event. This (and the companion Keck result) provide the first confirmation of a planetary microlensing signal, for which the deviation was only 2%. The follow-up observations determine the flux of the planetary host star in multiple passbands and remove light curve model ambiguity caused by sparse sampling of part of the light curve. This leads to a precise determination of the properties of the OGLE-2005-BLG-169Lb planetary system. Combining the constraints from the microlensing light curve with the photometry and astrometry of the HST/WFC3 data, we find star and planet masses of M-* = 0.69 +/- 0.02M(circle dot) and m(p) = 14.1 +/- 0.9M(circle dot). The planetary microlens system is located toward the Galactic bulge at a distance of D-L = 4.1 +/- 0.4 kpc and the projected star-planet separation is a(perpendicular to) = 3.5 +/- 0.3 AU, corresponding to a semimajor axis of a 4.0(-0.6)(+2.2) AU. C1 [Bennett, D. P.; Bhattacharya, A.; Suzuki, D.] Univ Notre Dame, Dept Phys, 225 Nieuwland Sci Hall, Notre Dame, IN 46556 USA. [Anderson, J.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Bond, I. A.] Massey Univ, Inst Nat & Math Sci, Auckland 0745, New Zealand. [Anderson, N.; Barry, R.; Gilbert, E.; Pfeifle, R.; Terry, S.] NASA, Goddard Space Flight Ctr, Lab Exoplanets & Stellar Astrophys, Greenbelt, MD 20815 USA. [Batista, V.; Beaulieu, J. -P.] Univ Paris 06, CNRS, UMR 7095, Inst Astrophys Paris, F-75014 Paris, France. [DePoy, D. L.] Texas A&M Univ, Dept Phys, College Stn, TX 77843 USA. [Dong, Subo] Peking Univ, Kavli Inst Astron & Astrophys, Beijing 100871, Peoples R China. [Gaudi, B. S.; Gould, A.; Pogge, R. W.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Udalski, A.] Univ Warsaw Observ, PL-00478 Warsaw, Poland. RP Bennett, DP (reprint author), Univ Notre Dame, Dept Phys, 225 Nieuwland Sci Hall, Notre Dame, IN 46556 USA. EM bennett@nd.edu FU NASA [NAS 5-26555, NNX12AB99G]; NASA from the STScI; NSF [AST 110347]; Chinese Academy of Sciences [XDB09000000]; European Research Council under the European Community/ERC [246678]; [12541]; [13417]; [NASA-NNX12AF54G] FX Based on observations made with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute (STScI), 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 # 12541 and 13417. D. P. B., A. B., and D. S. were supported by NASA through grants from the STScI and grant NASA-NNX12AF54G. A. G. and B. S. G. were supported by NSF grant AST 110347 and by NASA grant NNX12AB99G. S. D. is supported by the Strategic Priority Research Program-The Emergence of Cosmological Structures of the Chinese Academy of Sciences (grant No. XDB09000000). The OGLE project has received funding from the European Research Council under the European Community's Seventh Framework Programme (FP7/2007-2013)/ERC grant agreement no. 246678 to AU. NR 56 TC 19 Z9 19 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD AUG 1 PY 2015 VL 808 IS 2 AR 169 DI 10.1088/0004-637X/808/2/169 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DF0BA UT WOS:000371002400064 ER PT J AU Civano, F Hickox, RC Puccetti, S Comastri, A Mullaney, JR Zappacosta, L LaMassa, SM Aird, J Alexander, DM Ballantyne, DR Bauer, FE Brandt, WN Boggs, SE Christensen, FE Craig, WW Del-Moro, A Elvis, M Forster, K Gandhi, P Grefenstette, BW Hailey, CJ Harrison, FA Lansbury, GB Luo, B Madsen, K Saez, C Stern, D Treister, E Urry, MC Wik, DR Zhang, W AF Civano, F. Hickox, R. C. Puccetti, S. Comastri, A. Mullaney, J. R. Zappacosta, L. LaMassa, S. M. Aird, J. Alexander, D. M. Ballantyne, D. R. Bauer, F. E. Brandt, W. N. Boggs, S. E. Christensen, F. E. Craig, W. W. Del-Moro, A. Elvis, M. Forster, K. Gandhi, P. Grefenstette, B. W. Hailey, C. J. Harrison, F. A. Lansbury, G. B. Luo, B. Madsen, K. Saez, C. Stern, D. Treister, E. Urry, M. C. Wik, D. R. Zhang, W. TI THE NuSTAR EXTRAGALACTIC SURVEYS: OVERVIEW AND CATALOG FROM THE COSMOS FIELD SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: nuclei; X-rays: general ID ACTIVE GALACTIC NUCLEI; X-RAY LUMINOSITY; MEDIUM-SENSITIVITY SURVEY; POINT-SOURCE CATALOG; CHANDRA DEEP SURVEY; COMPTON-THICK AGN; SWIFT-BAT SURVEY; ALL-SKY SURVEY; XMM-NEWTON; HELLAS2XMM SURVEY AB To provide the census of the sources contributing to the X-ray background peak above 10 keV, Nuclear Spectroscopic Telescope Array (NuSTAR) is performing extragalactic surveys using a three-tier "wedding cake" approach. We present the NuSTAR survey of the COSMOS field, the medium sensitivity, and medium area tier, covering 1.7 deg(2) and overlapping with both Chandra and XMM-Newton data. This survey consists of 121 observations for a total exposure of similar to 3 Ms. To fully exploit these data, we developed a new detection strategy, carefully tested through extensive simulations. The survey sensitivity at 20% completeness is 5.9, 2.9, and 6.4 x 10(-14) erg cm(-2) s(-1) in the 3-24, 3-8, and 8-24 keV bands, respectively. By combining detections in 3 bands, we have a sample of 91 NuSTAR sources with 10(42)-10(45.5) erg s(-1) luminosities and redshift z = 0.04-2.5. Thirty-two sources are detected in the 8-24 keV band with fluxes similar to 100 times fainter than sources detected by Swift-BAT. Of the 91 detections, all but 4 are associated with a Chandra and/or XMM-Newton point-like counterpart. One source is associated with an extended lower energy X-ray source. We present the X-ray (hardness ratio and luminosity) and optical-to-X-ray properties. The observed fraction of candidate Compton-thick active galactic nuclei measured from the hardness ratio is between 13%-20%. We discuss the spectral properties of NuSTAR J100259+0220.6 (ID 330) at z = 0.044, with the highest hardness ratio in the entire sample. The measured column density exceeds 10(24) cm(-2), implying the source is Compton-thick. This source was not previously recognized as such without the >10 keV data. C1 [Civano, F.; LaMassa, S. M.; Urry, M. C.] Yale Ctr Astron & Astrophys, 260 Whitney Ave, New Haven, CT 06520 USA. [Civano, F.; Hickox, R. C.] Dartmouth Coll, Dept Phys & Astron, Wilder Lab 6127, Hanover, NH 03755 USA. [Civano, F.; Elvis, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Puccetti, S.] ASDC ASI, I-00133 Rome, Italy. [Comastri, A.] INAF Osservatorio Astron Bologna, I-40127 Bologna, Italy. [Mullaney, J. R.] Univ Sheffield, Dept Phys & Astron, Sheffield S3 7RH, S Yorkshire, England. [Zappacosta, L.] INAF Osservatorio Astron Roma, I-00040 Monte Porzio Catone, RM, Italy. [Aird, J.; Alexander, D. M.; Del-Moro, A.; Gandhi, P.; Lansbury, G. B.] Univ Durham, Dept Phys, Durham DH1 3LE, England. [Aird, J.] Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England. [Ballantyne, D. R.] Georgia Inst Technol, Sch Phys, Ctr Relativist Astrophys, Atlanta, GA 30332 USA. [Bauer, F. E.; Luo, B.; Saez, C.] Pontificia Univ Catolica Chile, Inst Astrofis, Fac Fis, Santiago 22, Chile. [Bauer, F. E.; Luo, B.] Millennium Inst Astrophys, Santiago, Chile. [Bauer, F. E.] Space Sci Inst, Boulder, CO 80301 USA. [Brandt, W. N.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Brandt, W. N.] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA. [Brandt, W. N.] Penn State Univ, Dept Phys, University Pk, PA 16802 USA. [Boggs, S. E.; Craig, W. W.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Christensen, F. E.] Tech Univ Denmark, DTU Space Natl Space Inst, DK-2800 Lyngby, Denmark. [Craig, W. W.] Lawrence Livermore Natl Lab, Livermore, CA USA. [Forster, K.; Grefenstette, B. W.; Harrison, F. A.; Madsen, K.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Gandhi, P.] Univ Southampton, Sch Phys Astron, Southampton SO17 1BJ, Hants, England. [Hailey, C. J.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Stern, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Treister, E.] Univ Concepcion, Dept Astron, Concepcion, Chile. [Wik, D. R.; Zhang, W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Civano, F (reprint author), Yale Ctr Astron & Astrophys, 260 Whitney Ave, New Haven, CT 06520 USA. RI Boggs, Steven/E-4170-2015; OI Boggs, Steven/0000-0001-9567-4224; Puccetti, Simonetta/0000-0002-2734-7835; Comastri, Andrea/0000-0003-3451-9970; Ballantyne, David/0000-0001-8128-6976; Urry, Meg/0000-0002-0745-9792 FU National Aeronautics and Space Administration; NASA [11-ADAP110218, GO3-14150C]; Science and Technology Facilities Council [ST/I001573/1]; NSF [AST 1008067]; NuSTAR grant [44A-1092750]; NASA ADP grant [NNX10AC99G]; V. M. Willaman Endowment; CONICYT-Chile [Basal-CATA PFB-06/2007]; FONDECYT [1141218, 1120061]; "EMBIGGEN" Anillo [ACT1101]; Ministry of Economy, Development, and Tourism's Millennium Science Initiative [IC120009]; Center of Excellence in Astrophysics and Associated Technologies; ASI/INAF [I/037/12/0] FX We thank the anonymous referee for interesting comments and A. Goulding and M. Rose for useful discussions. This work made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NUSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). We acknowledge support from the NASA grants 11-ADAP110218 and GO3-14150C (FC); from the Science and Technology Facilities Council ST/I001573/1 (ADM, DMA); NSF award AST 1008067 (DRB); NuSTAR grant 44A-1092750, NASA ADP grant NNX10AC99G, and the V. M. Willaman Endowment (WNB, BL); CONICYT-Chile grants Basal-CATA PFB-06/2007 (FEB), FONDECYT 1141218 (FEB), and "EMBIGGEN" Anillo ACT1101 (FEB, ET); the Ministry of Economy, Development, and Tourism's Millennium Science Initiative through grant IC120009, awarded to The Millennium Institute of Astrophysics, MAS (FEB); the Center of Excellence in Astrophysics and Associated Technologies (PFB 06) and by the FONDECYT regular grant 1120061 (ET); financial support under ASI/INAF contract I/037/12/0 (LZ). NR 96 TC 10 Z9 10 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD AUG 1 PY 2015 VL 808 IS 2 AR 185 DI 10.1088/0004-637X/808/2/185 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DF0BA UT WOS:000371002400081 ER PT J AU Coley, JB Corbet, RHD Krimm, HA AF Coley, Joel B. Corbet, Robin H. D. Krimm, Hans A. TI PROBING THE MASSES AND RADII OF DONOR STARS IN ECLIPSING X-RAY BINARIES WITH THE SWIFT BURST ALERT TELESCOPE SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars: individual (IGR J16393-4643, IGR J16418-4532, IGR J16479-4514, IGR J18027-2016, XTE J1855-026); stars: neutron ID TRANSIENT IGR J16479-4514; PULSAR XTE J1855-026; GALACTIC-O-STARS; XMM-NEWTON; MULTIWAVELENGTH OBSERVATIONS; SUPERGIANT SYSTEM; DUST SCATTERING; COMPANION STAR; WIND-ACCRETION; CENTAURUS X-3 AB Physical parameters of both the mass donor and compact object can be constrained in X-ray binaries with well-defined eclipses, as our survey of wind-fed supergiant X-ray binaries IGR J16393-4643, IGR J16418-4532, IGR J16479-4514, IGR J18027-2016, and XTE J1855-026 reveals. Using the orbital period and Kepler's third law, we express the eclipse half-angle in terms of radius, inclination angle, and the sum of the masses. Pulse-timing and radial velocity curves can give masses of both the donor and compact object as in the case of the "double-lined" binaries IGR J18027-2016 and XTE J1855-026. The eclipse half angles are 15-2+3, 31.7(-0.8)(+0.7), 32 +/- 2,34 +/- 2, and 33.6 +/- 0.7 degrees for IGR J16393-4643, IGR J16418-4532, IGR J16479-4514, IGR J18027-2016, and XTE 1855-026, respectively. In wind-fed systems, the primary not exceeding the Roche-lobe size provides an upper limit on system parameters. In IGR J16393-4643, spectral types of B0 V or B0-5 III are found to be consistent with the eclipse duration and Roche-lobe, but the previously proposed donor stars in IGR J16418-4532 and IGR J16479-4514 were found to be inconsistent with the Roche-lobe size. Stars with spectral types O7.5 I and earlier are possible. For IGR J18027-2016, the mass and radius of the donor star lie between 18.6-19.4 M-circle dot and 17.4-19.5 R-circle dot. We constrain the neutron star mass between 1.37 and 1.43 M-circle dot. We find the mass and radius of the donor star in XTE J1855-026 to lie between 19.6-20.2 M-circle dot and 21.5-23.0 R-circle dot. The neutron star mass was constrained to 1.77-1.82 M-circle dot. Eclipse profiles are asymmetric in IGR J18027-2016 and XTE J1855-026, which we attribute to accretion wakes. C1 [Coley, Joel B.; Corbet, Robin H. D.] Univ Maryland Baltimore Cty, Baltimore, MD 21228 USA. [Coley, Joel B.; Corbet, Robin H. D.; Krimm, Hans A.] NASA, Xray Astrophys Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Krimm, Hans A.] Univ Space Res Assoc, Columbia, MD 21046 USA. RP Coley, JB (reprint author), Univ Maryland Baltimore Cty, Baltimore, MD 21228 USA. EM jcoley1@umbc.edu OI Coley, Joel/0000-0001-7532-8359 FU NASA [14-ADAP14-0167] FX We thank the anonymous referee for useful comments and are also thankful for support from NASA 14-ADAP14-0167. NR 85 TC 3 Z9 3 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD AUG 1 PY 2015 VL 808 IS 2 AR 140 DI 10.1088/0004-637X/808/2/140 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DF0BA UT WOS:000371002400035 ER PT J AU de Martino, I Genova-Santos, R Atrio-Barandela, F Ebeling, H Kashlinsky, A Kocevski, D Martins, CJAP AF de Martino, I. Genova-Santos, R. Atrio-Barandela, F. Ebeling, H. Kashlinsky, A. Kocevski, D. Martins, C. J. A. P. TI CONSTRAINING THE REDSHIFT EVOLUTION OF THE COSMIC MICROWAVE BACKGROUND BLACKBODY TEMPERATURE WITH PLANCK DATA SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmic background radiation; cosmology: observations; cosmology: theory ID BRIGHTEST CLUSTER SAMPLE; RELATIVISTIC CORRECTIONS; RADIATION TEMPERATURE; GALAXIES; POLE; VELOCITY; UNIVERSE; CATALOG; REGION AB We constrain the deviation of adiabatic evolution of the universe using the data on the cosmic microwave background (CMB) temperature anisotropies measured by the Planck satellite and a sample of 481 X-ray selected clusters with spectroscopically measured redshifts. To avoid antenna beam effects, we bring all of the maps to the same resolution. We use a CMB template to subtract the cosmological signal while preserving the Thermal Sunyaev-Zeldovich (TSZ) anisotropies; next, we remove galactic foreground emissions around each cluster and we mask out all known point sources. If the CMB blackbody temperature scales with redshift as T(z) = T-0(1 + z)(1-alpha), we constrain deviations of adiabatic evolution to be alpha = -0.007 +/- 0.013, consistent with the temperature-redshift relation of the standard cosmological model. This result could suffer from a potential bias da associated with the CMB template. We quantify it to be vertical bar delta alpha vertical bar <= 0.02, with the same sign as the measured value of a. Our result is free from those biases associated with using TSZ selected clusters; it represents the best constraint to date of the temperature-redshift relation of the Big Bang model using only CMB data, confirming previous results. C1 [de Martino, I.; Atrio-Barandela, F.] Univ Salamanca, Fis Teor, E-37008 Salamanca, Spain. [Genova-Santos, R.] Inst Astrofis Canarias, E-38200 San Cristobal la Laguna, Spain. [Ebeling, H.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Kashlinsky, A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Kashlinsky, A.] NASA, SSAI, Observat Cosmol Lab, Greenbelt, MD 20771 USA. [Kocevski, D.] Univ Kentucky, Lexington, KY 40508 USA. [Martins, C. J. A. P.] Univ Porto, Ctr Astrofis, P-4150762 Oporto, Portugal. [Martins, C. J. A. P.] CAUP, Inst Astrofis & Ciencias Espaco, P-4150762 Oporto, Portugal. RP de Martino, I (reprint author), Univ Salamanca, Fis Teor, E-37008 Salamanca, Spain. EM ivan.demartino1983@gmail.com; ricardo.genova@iac.es; atrio@usal.es; ebeling@ifa.hawaii.edu; Alexander.Kashlinsky@nasa.gov; kocevski@pa.uky.edu; Carlos.Martins@astro.up.pt RI Atrio-Barandela, Fernando/A-7379-2017; OI Atrio-Barandela, Fernando/0000-0002-2130-2513; de Martino, Ivan/0000-0001-5948-9689 FU FCT/MICINN [AIC10-D-000443]; Ministerio de Educacion y Ciencia, Spain [FIS2012-30926]; FCT, Portugal [PTDC/FIS/111725/2009]; FCT [IF/00064/2012]; FCT/MCTES (Portugal); POPH/FSE (EC) FX We thank the referee for his/her comments that helped to improve the manuscript. This work was done in the context of the FCT/MICINN cooperation grant "Cosmology and Fundamental Physics with the Sunyaev-Zel'dovich Effect" AIC10-D-000443, with additional support from projects FIS2012-30926 from the Ministerio de Educacion y Ciencia, Spain and PTDC/FIS/111725/2009 from FCT, Portugal. C.M. is also supported by a FCT Research Professorship, contract reference IF/00064/2012, funded by FCT/MCTES (Portugal) and POPH/FSE (EC). NR 52 TC 9 Z9 9 U1 1 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD AUG 1 PY 2015 VL 808 IS 2 AR 128 DI 10.1088/0004-637X/808/2/128 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DF0BA UT WOS:000371002400023 ER PT J AU Furst, F Nowak, MA Tomsick, JA Miller, JM Corbel, S Bachetti, M Boggs, SE Christensen, FE Craig, WW Fabian, AC Gandhi, P Grinberg, V Hailey, CJ Harrison, FA Kara, E Kennea, JA Madsen, KK Pottschmidt, K Stern, D Walton, DJ Wilms, J Zhang, WW AF Fuerst, F. Nowak, M. A. Tomsick, J. A. Miller, J. M. Corbel, S. Bachetti, M. Boggs, S. E. Christensen, F. E. Craig, W. W. Fabian, A. C. Gandhi, P. Grinberg, V. Hailey, C. J. Harrison, F. A. Kara, E. Kennea, J. A. Madsen, K. K. Pottschmidt, K. Stern, D. Walton, D. J. Wilms, J. Zhang, W. W. TI THE COMPLEX ACCRETION GEOMETRY OF GX 339-4 AS SEEN BY NuSTAR AND SWIFT SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; stars: black holes; X-rays: binaries; X-rays: individual (GX 339-4) ID BLACK-HOLE SPIN; X-RAY REFLECTION; ADVECTION-DOMINATED ACCRETION; HARD STATE; LOW/HARD STATE; CANDIDATE GX-339-4; EMISSION; BINARIES; SPECTROSCOPY; DISC AB We present spectral analyses of five Nuclear Spectroscopic Telescope Array and Swift observations of GX 339-4 taken during a failed outburst during the summer of 2013. These observations cover Eddington luminosity fractions in the range approximate to 0.9%-6%. Throughout this outburst GX 339-4 stayed in the hard state and all five observations show similar X-ray spectra, with a hard power law with a photon index near 1.6, and significant contribution from reflection. Using simple reflection models we find unrealistically high iron abundances. Allowing for different photon indices for the continuum incident on the reflector relative to the underlying observed continuum results in a statistically better fit and reduced iron abundances. With a photon index around 1.3, the input power law on the reflector is significantly harder than that which is directly observed. We study the influence of different emissivity profiles and geometries and consistently find an improvement when using separate photon indices. The inferred inner accretion disk radius is strongly model dependent, but we do not find evidence for a truncation radius larger than 100 r(g) in any model. The data do not allow independent spin constraints, but the results are consistent with the literature (i.e., a > 0). Our best-fit models indicate an inclination angle in the range 40 degrees-60 degrees, consistent with limits on the orbital inclination but higher than reported in the literature using standard reflection models. The iron line around 6.4 keV is clearly broadened, and we detect a superimposed narrow core as well. This core originates from a fluorescent region outside the influence of the strong gravity of the black hole. Additionally, we discuss possible geometries. C1 [Fuerst, F.; Harrison, F. A.; Madsen, K. K.; Walton, D. J.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Nowak, M. A.; Grinberg, V.] MIT, Kavli Inst Astrophys, Cambridge, MA 02139 USA. [Tomsick, J. A.; Boggs, S. E.; Craig, W. W.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Miller, J. M.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Corbel, S.] Univ Paris Diderot, Lab AIM, CEA IRFU CNRS INSU, CEA DSM IRFU SAp, F-91191 Gif Sur Yvette, France. [Corbel, S.] Univ Orleans, OSUC, Stn Radioastron Nancay, Observ Paris,CNRS INSU,USR 704, F-18330 Nancay, France. [Bachetti, M.] Univ Toulouse, UPS OMP, IRAP, Toulouse, France. [Bachetti, M.] CNRS, Inst Rech Astrophys & Planetol, F-31028 Toulouse 4, France. [Bachetti, M.] Osservatorio Astron Cagliari, INAF, I-09047 Selargius, CA, Italy. [Christensen, F. E.] Tech Univ Denmark, Natl Space Inst, DTU Space, DK-2800 Lyngby, Denmark. [Craig, W. W.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA. [Fabian, A. C.; Kara, E.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Gandhi, P.] Univ Durham, Dept Phys, Durham DH1 3LE, England. [Gandhi, P.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Hailey, C. J.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Kennea, J. A.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Pottschmidt, K.; Zhang, W. W.] UMBC, CRESST, Greenbelt, MD 20771 USA. [Pottschmidt, K.; Zhang, W. W.] NASA GSFC, Greenbelt, MD 20771 USA. [Pottschmidt, K.] NASA Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Stern, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Wilms, J.] Univ Erlangen Nurnberg, Dr Karl Remeis Sternwarte, D-96049 Bamberg, Germany. [Wilms, J.] Univ Erlangen Nurnberg, ECAP, D-96049 Bamberg, Germany. RP Furst, F (reprint author), CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. RI Wilms, Joern/C-8116-2013; Boggs, Steven/E-4170-2015; OI Wilms, Joern/0000-0003-2065-5410; Boggs, Steven/0000-0001-9567-4224; Bachetti, Matteo/0000-0002-4576-9337 FU NASA [NNG08FD60C, NNX13AJ81G, NNX14AC56G]; National Aeronautics and Space Administration; ANR "CHAOS" [ANR-12-BS05-0009] FX We thank the anonymous referee for very constructive and helpful comments. This work was supported under NASA Contract No. NNG08FD60C and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software, and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS), jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). J.A.T. acknowledges partial support from NASA Swift Guest Investigator grants NNX13AJ81G and NNX14AC56G. S.C. acknowledges funding support from the ANR "CHAOS" (ANR-12-BS05-0009). We would like to thank John E. Davis for the slxfig module, which was used to produce all figures in this work. NR 66 TC 12 Z9 12 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD AUG 1 PY 2015 VL 808 IS 2 AR 122 DI 10.1088/0004-637X/808/2/122 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DF0BA UT WOS:000371002400017 ER PT J AU Jang-Condell, H Chen, CH Mittal, T Manoj, P Watson, D Lisse, CM Nesvold, E Kuchner, M AF Jang-Condell, Hannah Chen, Christine H. Mittal, Tushar Manoj, P. Watson, Dan Lisse, Carey M. Nesvold, Erika Kuchner, Marc TI SPITZER IRS SPECTRA OF DEBRIS DISKS IN THE SCORPIUS-CENTAURUS OB ASSOCIATION SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; open clusters and associations: individual (Upper Scorpius, Lower Centaurus-Crux, Upper Centaurus-Lupus); planet-disk interactions ID T-TAURI STARS; PRIMORDIAL BINARY POPULATION; TERRESTRIAL PLANET FORMATION; INTERMEDIATE-MASS STARS; CIRCUMSTELLAR DUST DISK; MAIN-SEQUENCE STARS; CIRCLE-DOT STARS; BETA-PICTORIS; YOUNG STARS; HR 8799 AB We analyze spectra obtained with the Spitzer Infrared Spectrograph (IRS) of 110 B-, A-, F-, and G-type stars with optically thin infrared excess in the Scorpius-Centaurus OB association. The ages of these stars range from 11 to 17 Myr. We fit the infrared excesses observed in these sources by Spitzer IRS and the Multiband Imaging Photometer for Spitzer (MIPS) to simple dust models according to Mie theory. We find that nearly all of the objects in our study can be fit by one or two belts of dust. Dust around lower mass stars appears to be closer in than around higher mass stars, particularly for the warm dust component in the two-belt systems, suggesting a mass-dependent evolution of debris disks around young stars. For those objects with stellar companions, all dust distances are consistent with truncation of the debris disk by the binary companion. The gaps between several of the two-belt systems can place limits on the planets that might lie between the belts, potentially constraining the mass and locations of planets that may be forming around these stars. C1 [Jang-Condell, Hannah] Univ Wyoming, Dept Phys & Astron, Laramie, WY 82071 USA. [Chen, Christine H.; Mittal, Tushar; Lisse, Carey M.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Mittal, Tushar] Univ Calif Berkeley, Dept Earth & Planetary Sci, Berkeley, CA 94720 USA. [Manoj, P.] Tata Inst Fundamental Res, Dept Astron & Astrophys, Bombay 400005, Maharashtra, India. [Watson, Dan] Univ Rochester, Dept Phys & Astron, Rochester, NY 14627 USA. [Lisse, Carey M.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Nesvold, Erika; Kuchner, Marc] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA. [Nesvold, Erika] Univ Maryland Baltimore Cty, Baltimore, MD 21250 USA. RP Jang-Condell, H (reprint author), Univ Wyoming, Dept Phys & Astron, Laramie, WY 82071 USA. RI Lisse, Carey/B-7772-2016; OI Lisse, Carey/0000-0002-9548-1526; Jang-Condell, Hannah/0000-0002-7639-1322 FU NASA; NASA by JPL/Caltech; NASA [NNX12AD43G] FX This work is based on observations made with the Spitzer Space Telescope, which is operated by JPL/Caltech under a contract with NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech. H.J.-C. acknowledges support from NASA grant NNX12AD43G. NR 86 TC 7 Z9 7 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD AUG 1 PY 2015 VL 808 IS 2 AR 167 DI 10.1088/0004-637X/808/2/167 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DF0BA UT WOS:000371002400062 ER PT J AU Kuntz, KD Collado-Vega, YM Collier, MR Connor, HK Cravens, TE Koutroumpa, D Porter, FS Robertson, IP Sibeck, DG Snowden, SL Thomas, NE Walsh, BM AF Kuntz, K. D. Collado-Vega, Y. M. Collier, M. R. Connor, H. K. Cravens, T. E. Koutroumpa, D. Porter, F. S. Robertson, I. P. Sibeck, D. G. Snowden, S. L. Thomas, N. E. Walsh, B. M. TI THE SOLAR WIND CHARGE-EXCHANGE PRODUCTION FACTOR FOR HYDROGEN SO ASTROPHYSICAL JOURNAL LA English DT Article DE X-rays: diffuse background ID X-RAY-EMISSION; LOCAL INTERSTELLAR-MEDIUM; XMM-NEWTON OBSERVATIONS; HIGH-ALTITUDE; HOT BUBBLE; O VII; MAGNETOSPHERE; IONIZATION; PARAMETERS; HELIUM AB The mean production factor, or broadband averaged cross-section, for solar wind charge-exchange (SWCX) with hydrogen producing emission in the ROSAT 1/4 keV (R12) band is (3.8 +/- 0.2) x 10(-20) count degree(-2) cm(4). The production factor is expected to be temporally variable, and that variation is roughly 15%. These values are derived from a comparison of the long-term (background) enhancements in the ROSAT All-Sky Survey with magnetohysdrodynamic simulations of the magnetosheath. This value is 1.8-4.5 times higher than values derived from limited atomic data, suggesting that those values may be missing a large number of faint lines. This production factor is important for deriving the exact amount of 1/4 keV band flux that is due to the Local Hot Bubble, for planning future observations in the 1/4 keV band, and for evaluating proposals for remote sensing of the magnetosheath. The same method cannot be applied to the 3/4 keV band as that band, being composed primarily of the oxygen lines, is far more sensitive to the detailed abundances and ionization balance in the solar wind. We also show, incidentally, that recent efforts to correlate XMM-Newton observing geometry with magnetosheath SWCX emission in the oxygen lines have been, quite literally, misguided. Simulations of the inner heliosphere show that broader efforts to correlate heliospheric SWCX with local solar wind parameters are unlikely to produce useful results. C1 [Kuntz, K. D.] Johns Hopkins Univ, Henry A Rowland Dept Phys & Astron, 3400 N Charles St, Baltimore, MD 21218 USA. [Collado-Vega, Y. M.; Collier, M. R.; Connor, H. K.; Porter, F. S.; Sibeck, D. G.; Snowden, S. L.; Thomas, N. E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Cravens, T. E.; Robertson, I. P.] Univ Kansas, Dept Phys & Astron, Lawrence, KS 66045 USA. [Koutroumpa, D.] Univ Versailles St Quentin Yvelines, LATMOS IPSL CNRS, Guyancourt, France. [Walsh, B. M.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. RP Kuntz, KD (reprint author), Johns Hopkins Univ, Henry A Rowland Dept Phys & Astron, 3400 N Charles St, Baltimore, MD 21218 USA. EM kuntz@pha.jhu.edu RI Porter, Frederick/D-3501-2012; Collier, Michael/I-4864-2013; OI Porter, Frederick/0000-0002-6374-1119; Collier, Michael/0000-0001-9658-6605; Walsh, Brian/0000-0001-7426-5413 FU National Aeronautics and Space Administration ADAP grant [06-ADP06-32]; NASA through Science Mission Directorate's Planetary Science Division [LSSO06-0032]; XMM-Newton Guest Observer Facility FX The initial studies that led to this work funded K.D.K. and M.R.C. through National Aeronautics and Space Administration ADAP grant 06-ADP06-32. M.R.C. was partially funded by NASA under grant LSSO06-0032 issued through the Science Mission Directorate's Planetary Science Division. K.D.K. was funded in part through the XMM-Newton Guest Observer Facility. K.D.K. would also like to thank the Chemical Heritage Foundation for the hospitality of their reading room for the creation of the first draft of this work. Part of this work was performed while the primary author and many of the coauthors were attending the International Space Science Institute (ISSI) workshop on solar wind charge-exchange in 2013 October in Bern, Switzerland. Many of the coauthors also attended the ISSI workshop on solar wind charge-exchange in 2013 January. We are deeply grateful to ISSI for these very productive workshops. Our thanks also to the Community Coordinated Modeling Center at Goddard Space Flight Center for producing the extended ENLIL run, and for providing the large number of BATS-R-US runs used for this work. The BATS-R-US and ENLIL simulation results were provided by the CCMC through their public "Runs on Request" system (http://ccmc.gsfc.nasa.gov). The CCMC is a multi-agency partnership between NASA, AFMC, AFOSR, AFRL, AFWA, NOAA, NSF and ONR. Even with the large number of authors, a study of this type does not occur in a vacuum. We would like to thank all those who, through discussion, argument, and spirited altercations, helped make this a better paper. Finally, we would like to thank the referee for prompting a number of clarifications, improvements, and additions. NR 72 TC 6 Z9 6 U1 2 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 AUG 1 PY 2015 VL 808 IS 2 AR 143 DI 10.1088/0004-637X/808/2/143 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DF0BA UT WOS:000371002400038 ER PT J AU Mullaney, JR Del-Moro, A Aird, J Alexander, DM Civano, FM Hickox, RC Lansbury, GB Ajello, M Assef, R Ballantyne, DR Balokovic, M Bauer, FE Brandt, WN Boggs, SE Brightman, M Christensen, FE Comastri, A Craig, WW Elvis, M Forster, K Gandhi, P Grefenstette, BW Hailey, CJ Harrison, FA Koss, M LaMassa, SM Luo, B Madsen, KK Puccetti, S Saez, C Stern, D Treister, E Urry, CM Wik, DR Zappacosta, L Zhang, W AF Mullaney, J. R. Del-Moro, A. Aird, J. Alexander, D. M. Civano, F. M. Hickox, R. C. Lansbury, G. B. Ajello, M. Assef, R. Ballantyne, D. R. Balokovic, M. Bauer, F. E. Brandt, W. N. Boggs, S. E. Brightman, M. Christensen, F. E. Comastri, A. Craig, W. W. Elvis, M. Forster, K. Gandhi, P. Grefenstette, B. W. Hailey, C. J. Harrison, F. A. Koss, M. LaMassa, S. M. Luo, B. Madsen, K. K. Puccetti, S. Saez, C. Stern, D. Treister, E. Urry, C. M. Wik, D. R. Zappacosta, L. Zhang, W. TI THE NuSTAR EXTRAGALACTIC SURVEYS: INITIAL RESULTS AND CATALOG FROM THE EXTENDED CHANDRA DEEP FIELD SOUTH SO ASTROPHYSICAL JOURNAL LA English DT Article DE astronomical databases: miscellaneous; galaxies: active; galaxies: evolution; X-rays: galaxies; X-rays: general ID ACTIVE GALACTIC NUCLEI; POINT-SOURCE CATALOG; HARD X-RAYS; MS SOURCE CATALOGS; SWIFT-BAT SURVEY; NUMBER COUNTS; BACKGROUND SPECTRUM; LUMINOSITY FUNCTION; SPACE DENSITY; BLACK-HOLES AB We present the initial results and the source catalog from the Nuclear Spectroscopic Telescope Array (NuSTAR) survey of the Extended Chandra Deep Field South (hereafter, ECDFS)-currently the deepest contiguous component of the NuSTAR extragalactic survey program. The survey covers the full approximate to 30' x 30' area of this field to a maximum depth of approximate to 360 ks (approximate to 220 ks when corrected for vignetting at 3-24 keV), reaching sensitivity limits of approximate to 1.3 x 10(-14) erg s(-1) cm(-2) (3-8 keV), approximate to 3.4 x 10(-14) erg s(-1) cm(-2) (8-24 keV), and approximate to 3.0 x 10(-14) erg s(-1) cm(-2) (3-24 keV). A total of 54 sources are detected over the full field, although five of these are found to lie below our significance threshold once contaminating flux from neighboring (i.e., blended) sources is taken into account. Of the remaining 49 that are significant, 19 are detected in the 8-24 keV band. The 8-24 to 3-8 keV band ratios of the 12 sources that are detected in both bands span the range 0.39-1.7, corresponding to a photon index range of Gamma approximate to 0.5-2.3, with a median photon index of (Gamma) over bar = 1.70 +/- 0.52. The redshifts of the 49 sources in our main sample span the range z = 0.21-2.7, and their rest-frame 10-40 keV luminosities (derived from the observed 8-24 keV fluxes) span the range L10-40 keV (0.7-300) 10 erg s(-1), sampling below the "knee" of the X-ray luminosity function out to z similar to 0.8-1. Finally, we identify one NuSTAR source that has neither a Chandra nor an XMM-Newton counterpart, but that shows evidence of nuclear activity at infrared wavelengths and thus may represent a genuine, new X-ray source detected by NuSTAR in the ECDFS. C1 [Mullaney, J. R.; Del-Moro, A.; Aird, J.; Alexander, D. M.; Lansbury, G. B.; Gandhi, P.] Univ Durham, Dept Phys, Ctr Extragalact Astron, South Rd, Durham DH1 3LE, England. [Mullaney, J. R.] Univ Sheffield, Dept Phys & Astron, Sheffield S3 7RH, S Yorkshire, England. [Aird, J.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Civano, F. M.; LaMassa, S. M.; Urry, C. M.] Yale Ctr Astron & Astrophys, New Haven, CT 06520 USA. [Civano, F. M.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Civano, F. M.; Hickox, R. C.] Dartmouth Coll, Dept Phys & Astron, Wilder Lab 6127, Hanover, NH 03755 USA. [Ajello, M.; Boggs, S. E.; Craig, W. W.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Assef, R.] Univ Diego Portales, Nucleo Astron, Fac Ingn, Santiago, Chile. [Ballantyne, D. R.] Georgia Inst Technol, Sch Phys, Ctr Relativist Astrophys, Atlanta, GA 30332 USA. [Balokovic, M.; Brightman, M.; Forster, K.; Grefenstette, B. W.; Harrison, F. A.; Madsen, K. K.] CALTECH, Cahill Ctr Astrophys, Pasadena, CA 91125 USA. [Bauer, F. E.] Pontificia Univ Catolica Chile, Fac Fis, Inst Astrofis, Santiago 22, Chile. [Bauer, F. E.] Millennium Inst Astrophys, Santiago, Chile. [Bauer, F. E.] Space Sci Inst, Boulder, CO 80301 USA. [Brandt, W. N.; Luo, B.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA. [Brandt, W. N.; Luo, B.] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA. [Brandt, W. N.] Penn State Univ, Dept Phys, University Pk, PA 16802 USA. [Christensen, F. E.] Tech Univ Denmark, Natl Space Inst, DTU Space, DK-2800 Lyngby, Denmark. [Comastri, A.] INAF Osservatorio Astron Bologna, I-40127 Bologna, Italy. [Elvis, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Gandhi, P.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Hailey, C. J.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Koss, M.] Swiss Fed Inst Technol, Dept Phys, Inst Astron, CH-8093 Zurich, Switzerland. [Puccetti, S.] ASDC ASI, I-00133 Rome, Italy. [Puccetti, S.; Zappacosta, L.] INAF, Osservatorio Astron Roma, I-00040 Monte Porzio Catone, Rome, Italy. [Saez, C.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Stern, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Treister, E.] Univ Concepcion, Dept Astron, Concepcion, Chile. [Wik, D. R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Wik, D. R.] Johns Hopkins Univ, Baltimore, MD 21218 USA. [Zhang, W.] West Virginia Wesleyan Coll, Phys & Engn Dept, Buckhannon, WV 26201 USA. RP Mullaney, JR (reprint author), Univ Durham, Dept Phys, Ctr Extragalact Astron, South Rd, Durham DH1 3LE, England. RI Boggs, Steven/E-4170-2015; OI Boggs, Steven/0000-0001-9567-4224; Puccetti, Simonetta/0000-0002-2734-7835; Koss, Michael/0000-0002-7998-9581; Comastri, Andrea/0000-0003-3451-9970; Ballantyne, David/0000-0001-8128-6976; Urry, Meg/0000-0002-0745-9792; Lansbury, George/0000-0002-5328-9827 FU National Aeronautics and Space Administration; Science and Technology Facilities Council [ST/I001573/1]; Institute of Advanced Study, Durham University; ERC; NASA [11-ADAP11-0218, GO3-14150C]; NSF [AST 1008067]; NuSTAR [44A-1092750]; NASA ADP [NNX10AC99G]; V. M. Willaman Endowment; CONICYT-Chile [Basal-CATA PFB-06/2007]; FONDECYT [1141218, 1120061]; "EMBIGGEN" Anillo [ACT1101]; Ministry of Economy, Development, and Tourism's Millennium Science Initiative [IC120009]; Center of Excellence in Astrophysics and Associated Technologies [PFB 06]; ASI/INAF [I/037/12/0 011/13]; NASA Headquarters under the NASA Earth and Space Science Fellowship Program [NNX14AQ07H] FX We thank the anonymous referee for their careful reading of the manuscript and comments that improved the clarity of the text. This work made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software, and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NUSTARDAS), jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). A.D.M. and D.M.A. gratefully acknowledge financial support from the Science and Technology Facilities Council (ST/I001573/1). J.A. acknowledges support from a COFUND Junior Research Fellowship from the Institute of Advanced Study, Durham University, and ERC Advanced Grant FEEDBACK at the University of Cambridge. F.M.C. acknowledges support from NASA grants 11-ADAP11-0218 and GO3-14150C. D.R.B. is supported in part by NSF award AST 1008067. W.N.B. and B.L. thank NuSTAR grant 44A-1092750, NASA ADP grant NNX10AC99G, and the V. M. Willaman Endowment. We acknowledge support from CONICYT-Chile grants Basal-CATA PFB-06/2007 (FEB), FONDECYT 1141218 (FEB) and 1120061 (ET), and "EMBIGGEN" Anillo ACT1101 (FEB, ET); and the Ministry of Economy, Development, and Tourism's Millennium Science Initiative through grant IC120009, awarded to The Millennium Institute of Astrophysics, MAS (FEB). Support for the work of E.T. was also provided by the Center of Excellence in Astrophysics and Associated Technologies (PFB 06). A.C., S.P., and L.Z. acknowledge support from the ASI/INAF grant I/037/12/0 011/13. A.C. acknowledges the Caltech Kingsley visitor program. M.B. acknowledges support from NASA Headquarters under the NASA Earth and Space Science Fellowship Program, grant NNX14AQ07H. NR 79 TC 7 Z9 7 U1 1 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD AUG 1 PY 2015 VL 808 IS 2 AR 184 DI 10.1088/0004-637X/808/2/184 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DF0BA UT WOS:000371002400080 ER PT J AU Reynolds, CS Lohfink, AM Ogle, PM Harrison, FA Madsen, KK Fabian, AC Wik, DR Madejski, G Ballantyne, DR Boggs, SE Christensen, FE Craig, WW Fuerst, F Hailey, CJ Lanz, L Miller, JM Saez, C Stern, D Walton, DJ Zhang, W AF Reynolds, Christopher S. Lohfink, Anne M. Ogle, Patrick M. Harrison, Fiona A. Madsen, Kristin K. Fabian, Andrew C. Wik, Daniel R. Madejski, Grzegorz Ballantyne, David R. Boggs, Steven E. Christensen, Finn E. Craig, William W. Fuerst, Felix Hailey, Charles J. Lanz, Lauranne Miller, Jon M. Saez, Cristian Stern, Daniel Walton, Dominic J. Zhang, William TI NuSTAR OBSERVATIONS OF THE POWERFUL RADIO-GALAXY CYGNUS A SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; galaxies: clusters: intracluster medium; galaxies: jets; X-rays: individual (Cygnus A) ID ACTIVE GALACTIC NUCLEI; HOLE ACCRETION DISKS; X-RAY OBSERVATIONS; BLACK-HOLE; WINDS; REFLECTION; EMISSION; FEEDBACK; SPECTRA; ENERGY AB We present NuSTAR observations of the powerful radio galaxy Cygnus A, focusing on the central absorbed active galactic nucleus (AGN). Cygnus A is embedded in a cool-core galaxy cluster, and hence we also examine archival XMM-Newton data to facilitate the decomposition of the spectrum into the AGN and intracluster medium components. NuSTAR gives a source-dominated spectrum of the AGN out to >70 keV. In gross terms, the NuSTAR spectrum of the AGN has the form of a power law (Gamma similar to 1.6-1.7) absorbed by a neutral column density of N-H similar to 1.6 10(23) cm(-2). However, we also detect curvature in the hard (>10 keV) spectrum resulting from reflection by Compton-thick matter out of our line of sight to the X-ray source. Compton reflection, possibly from the outer accretion disk or obscuring torus, is required even permitting a high-energy cut off in the continuum source; the limit on the cut-off energy is E-cut > 111 keV(90% confidence). Interestingly, the absorbed power law plus reflection model leaves residuals suggesting the absorption/emission from a fast (15,000-26,000 km s(-1)), high column-density (N-W > 3 x 10(23) cm(-2)), highly ionized (xi similar to 2500 erg cm s(-1)) wind. A second, even faster ionized wind component is also suggested by these data. We show that the ionized wind likely carries a significant mass and momentum flux, and may carry sufficient kinetic energy to exercise feedback on the host galaxy. If confirmed, the simultaneous presence of a strong wind and powerful jets in Cygnus A demonstrates that feedback from radio-jets and sub-relativistic winds are not mutually exclusive phases of AGN activity but can occur simultaneously. C1 [Reynolds, Christopher S.; Saez, Cristian] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Reynolds, Christopher S.] Joint Space Sci Inst JSI, College Pk, MD 20742 USA. [Lohfink, Anne M.; Fabian, Andrew C.] Inst Astron, Cambridge CB3 OHA, England. [Ogle, Patrick M.; Lanz, Lauranne] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA. [Harrison, Fiona A.; Madsen, Kristin K.; Fuerst, Felix; Walton, Dominic J.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Wik, Daniel R.; Zhang, William] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Madejski, Grzegorz] SLAC Natl Accelerator Lab, Kavli Inst Particle Astrophys & Cosmol, Menlo Pk, CA 94025 USA. [Ballantyne, David R.] Georgia Inst Technol, Sch Phys, Ctr Relativist Astrophys, Atlanta, GA 30332 USA. [Boggs, Steven E.; Craig, William W.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Christensen, Finn E.] Tech Univ Denmark, Natl Space Inst, DTU Space, DK-2800 Lyngby, Denmark. [Craig, William W.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA. [Hailey, Charles J.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Miller, Jon M.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Stern, Daniel] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Reynolds, CS (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA. EM chris@astro.umd.edu RI Boggs, Steven/E-4170-2015; OI Boggs, Steven/0000-0001-9567-4224; Lanz, Lauranne/0000-0002-3249-8224; Reynolds, Christopher/0000-0002-1510-4860; Madsen, Kristin/0000-0003-1252-4891 FU NASA [NNX14AF86G, NNG08FD60C]; National Aeronautics and Space Administration FX We thank the anonymous referee for their thorough and constructive comments that improved the quality of the manuscript. The authors also thank Francesco Tombesi for stimulating conversations throughout the course of this work. C.S.R. thanks NASA for support under grant NNX14AF86G. Our analysis makes use of the XSPEC_EMCEE package developed and distributed by Jeremy Sanders. This work was supported under NASA Contract No. NNG08FD60C, and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). NR 49 TC 8 Z9 8 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD AUG 1 PY 2015 VL 808 IS 2 AR 154 DI 10.1088/0004-637X/808/2/154 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DF0BA UT WOS:000371002400049 ER PT J AU Seifina, E Titarchuk, L Shrader, C Shaposhnikov, N AF Seifina, Elena Titarchuk, Lev Shrader, Chris Shaposhnikov, Nikolai TI BEPPOSAX AND RXTE SPECTRAL STUDY OF THE LOW-MASS X-RAY BINARY 4U 1705-44: SPECTRAL HARDENING DURING THE BANANA BRANCH SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; black hole physics; radiation mechanisms: non-thermal; stars: individual (4U 1705-44); X-rays: binaries ID QUASI-PERIODIC OSCILLATIONS; COLOR-COLOR DIAGRAM; SOURCE GX 340+0; SCORPIUS X-1; NEUTRON-STAR; ASTRONOMY SATELLITE; XTE J1701-462; ON-BOARD; PROPORTIONAL COUNTER; TIMING EXPLORER AB We analyze the X-ray spectra of the atoll. 4U 1705-44 when the source undergoes the island-banana state transition. We use the RXTE and BeppoSAX observations for this analysis. We demonstrate that the broadband energy spectral distributions for all evolutinary states can be fitted by a model. consisting of two Comptonized components. One arises from the seed photons coming from a neutron star (NS) atmosphere at a temperature kT(s1) less than or similar to 1.5 keV (herein Comptb1), and a second results. from the seed photons of T-s2 similar to 1.1-1.3 keV coming from the disk (herein Comptb2). We found that we needed to add a low-temperature blackbody and an iron-line (Gaussian) component to the model in order to obtain high-quality fits. The data analysis using this model indicates that the power-law photon index Gamma(1) of our model is always about 2, independently of the spectral state. Another parameter, Gamma(2), demonstrates a two-phase behavior depending on the spectral state. Gamma(2) is quasi-constant at Gamma(2) similar to 2 when the electron temperature kT(e)((2)) < keV, and Gamma(2) is less than 2, in the range of 1.3 2 < Gamma(2) <, when kT(e)((2)) > 80 keV. This phase is similar to that previously found in the Z-source Sco X-1. We interpret the decreasing index phase using a model in which a super-Eddington radiation pressure from the NS causes an expansion of the Compton cloud similar to that found previously in Sco X-1 during the Flaring branch. C1 [Seifina, Elena] Moscow MV Lomonosov State Univ, Sternberg Astron Inst, Univ Prospect 13, Moscow 119992, Russia. [Titarchuk, Lev] Univ Ferrara, Dipartimento Fis, I-44122 Ferrara, Italy. [Titarchuk, Lev] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20770 USA. [Shrader, Chris] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Shrader, Chris] Univ Space Res Assoc, Columbia, MD 21044 USA. [Shaposhnikov, Nikolai] Univ Maryland, CRESST, Dept Astron, College Pk, MD 20742 USA. [Shaposhnikov, Nikolai] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Seifina, E (reprint author), Moscow MV Lomonosov State Univ, Sternberg Astron Inst, Univ Prospect 13, Moscow 119992, Russia. EM seif@sai.msu.ru; titarchuk@fe.infn.it; Chris.R.Shrader@nasa.gov; nikolai.v.shaposhnikov@nasa.gov OI Titarchuk, Lev/0000-0002-9998-7591 FU NASA [NNX13AF39G] FX We recognize the contribution of the referee who has thoroughly checked the paper's context. N.S. also acknowledges the support of this research by NASA under grant NNX13AF39G. NR 57 TC 4 Z9 4 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD AUG 1 PY 2015 VL 808 IS 2 AR 142 DI 10.1088/0004-637X/808/2/142 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DF0BA UT WOS:000371002400037 ER PT J AU Stark, CC Roberge, A Mandell, A Clampin, M Domagal-Goldman, SD McElwain, MW Stapelfeldt, KR AF Stark, Christopher C. Roberge, Aki Mandell, Avi Clampin, Mark Domagal-Goldman, Shawn D. McElwain, Michael W. Stapelfeldt, Karl R. TI LOWER LIMITS ON APERTURE SIZE FOR AN EXOEARTH DETECTING CORONAGRAPHIC MISSION SO ASTROPHYSICAL JOURNAL LA English DT Article DE methods: numerical; planetary systems; telescopes ID KEPLER PLANET CANDIDATES; MAIN-SEQUENCE STARS; SOLAR-TYPE STARS; EARTH; POPULATION; COMPLETENESS; SEARCH; MASS AB The yield of Earth-like planets will likely be a primary science metric for future space-based missions that will drive telescope aperture size. Maximizing the exoEarth candidate yield is therefore critical to minimizing the required aperture. Here we describe a method for exoEarth candidate yield maximization that simultaneously optimizes, for the first time, the targets chosen for observation, the number of visits to each target, the delay time between visits, and the exposure time of every observation. This code calculates both the detection time and multi-wavelength spectral characterization time required for planets. We also refine the astrophysical assumptions used as inputs to these calculations, relying on published estimates of planetary occurrence rates as well as theoretical and observational constraints on terrestrial planet sizes and classical habitable zones. Given these astrophysical assumptions, optimistic telescope and instrument assumptions, and our new completeness code that produces the highest yields to date, we suggest lower limits on the aperture size required to detect and characterize a statistically motivated sample of exoEarths. C1 [Stark, Christopher C.] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA. [Roberge, Aki; Mandell, Avi; Clampin, Mark; Domagal-Goldman, Shawn D.; McElwain, Michael W.; Stapelfeldt, Karl R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Stark, CC (reprint author), Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA. EM cstark@stsci.edu RI Roberge, Aki/D-2782-2012; OI Roberge, Aki/0000-0002-2989-3725; Domagal-Goldman, Shawn/0000-0003-0354-9325 FU NASA; GSFC's internal research and development fund FX This research was 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. S.D.D.G., A.M., and A.R. acknowledge support by GSFC's internal research and development fund. NR 26 TC 19 Z9 19 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD AUG 1 PY 2015 VL 808 IS 2 AR 149 DI 10.1088/0004-637X/808/2/149 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DF0BA UT WOS:000371002400044 ER PT J AU Stovall, K Ray, PS Blythe, J Dowell, J Eftekhari, T Garcia, A Lazio, TJW McCrackan, M Schinzel, FK Taylor, GB AF Stovall, K. Ray, P. S. Blythe, J. Dowell, J. Eftekhari, T. Garcia, A. Lazio, T. J. W. McCrackan, M. Schinzel, F. K. Taylor, G. B. TI PULSAR OBSERVATIONS USING THE FIRST STATION OF THE LONG WAVELENGTH ARRAY AND THE LWA PULSAR DATA ARCHIVE SO ASTROPHYSICAL JOURNAL LA English DT Article DE pulsars: general ID GIGAHERTZ-PEAKED SPECTRA; LOW-FREQUENCY; DISPERSION MEASURE; PROFILE EVOLUTION; EMPIRICAL-THEORY; RADIO TELESCOPE; GIANT PULSES; MHZ; EMISSION; LIMITS AB We present initial pulsar results from the first station of the Long Wavelength Array (LWA1) obtained during the commissioning period of LWA1 and in early science results. We present detections of periodic emission from 44 previously known pulsars, including 3 millisecond pulsars. The effects of the interstellar medium (ISM) on pulsar emission are significantly enhanced at the low frequencies of the LWA1 band (10-88 MHz), making LWA1 a very sensitive instrument for characterizing changes in the dispersion measure (DM) and other effects from the ISM. Pulsars also often have significant evolution in their pulse profile at low frequency and a break in their spectral index. We report DM measurements for 44 pulsars, mean flux density measurements for 36 pulsars, and multi-frequency component spacing and widths for 15 pulsars with more than one profile component. For 27 pulsars, we report spectral index measurements within our frequency range. We also introduce the LWA1 Pulsar Data Archive, which stores reduced data products from LWA1 pulsar observations. Reduced data products for the observations presented here can be found in the archive. Reduced data products from future LWA1 pulsar observations will also be made available through the archive. C1 [Stovall, K.; Dowell, J.; Eftekhari, T.; McCrackan, M.; Schinzel, F. K.; Taylor, G. B.] Univ New Mexico, Dept Phys & Astron, Albuquerque, NM 87131 USA. [Ray, P. S.; Blythe, J.] Naval Res Lab, Div Space Sci, Washington, DC 20375 USA. [Garcia, A.] Univ Texas Brownsville, Ctr Adv Radio Astron, Brownsville, TX 78520 USA. [Lazio, T. J. W.] CALTECH, Jet Prop Lab, Pasadena, CA 91106 USA. RP Stovall, K (reprint author), Univ New Mexico, Dept Phys & Astron, Albuquerque, NM 87131 USA. EM stovall.kevin@gmail.com OI Ray, Paul/0000-0002-5297-5278; Schinzel, Frank/0000-0001-6672-128X; Eftekhari, Tarraneh/0000-0003-0307-9984 FU Office of Naval Research [N00014-07-C-0147]; National Science Foundation [AST-1139963, AST-1139974]; National Aeronautics and Space Administration FX Construction of the LWA has been supported by the Office of Naval Research under Contract N00014-07-C-0147. Support for operations and continuing development of the LWA1 is provided by the National Science Foundation under grants AST-1139963 and AST-1139974 of the University Radio Observatory program. Basic research on pulsars at NRL is supported by the Chief of Naval Research (CNR). 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. The authors thank an anonymous referee for useful comments. NR 57 TC 8 Z9 8 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD AUG 1 PY 2015 VL 808 IS 2 AR 156 DI 10.1088/0004-637X/808/2/156 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DF0BA UT WOS:000371002400051 ER PT J AU Leinonen, J Szyrmer, W AF Leinonen, Jussi Szyrmer, Wanda TI Radar signatures of snowflake riming: A modeling study SO EARTH AND SPACE SCIENCE LA English DT Article ID MELTING LAYER; ICE CRYSTALS; SNOW GROWTH; CLIMATE MODEL; LIQUID WATER; CLOUDS; PARTICLES; PHASE; AGGREGATE; SATELLITE AB The capability to detect the state of snowflake riming reliably from remote measurements would greatly expand the understanding of its global role in cloud-precipitation processes. To investigate the ability of multifrequency radars to detect riming, a three-dimensional model of snowflake growth was used to generate simulated aggregate and crystal snowflakes with various degrees of riming. Three different growth scenarios, representing different temporal relationships between aggregation and riming, were formulated. The discrete dipole approximation was then used to compute the radar backscattering properties of the snowflakes at frequencies of 9.7, 13.6, 35.6, and 94 GHz. In two of the three growth scenarios, the rimed snowflakes exhibit large differences between the backscattering cross sections of the detailed three-dimensional models and the equivalent homogeneous spheroidal models, similarly to earlier results for unrimed snowflakes. When three frequencies are used simultaneously, riming appears to be detectable in a robust manner across all three scenarios. In spite of the differences in backscattering cross sections, the triple-frequency signatures of heavily rimed particles resemble those of the homogeneous spheroids, thus explaining earlier observational results that were compatible with such spheroids. C1 [Leinonen, Jussi] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Szyrmer, Wanda] McGill Univ, Dept Atmospher & Ocean Sci, Montreal, PQ, Canada. RP Leinonen, J (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA USA. EM jussi.s.leinonen@jpl.nasa.gov OI Leinonen, Jussi/0000-0002-6560-6316 NR 59 TC 5 Z9 5 U1 1 U2 4 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2333-5084 J9 Earth Space Sci JI Earth Space Sci. PD AUG PY 2015 VL 2 IS 8 BP 346 EP 358 DI 10.1002/2015EA000102 PG 13 WC Geosciences, Multidisciplinary SC Geology GA DE6NK UT WOS:000370750400002 PM 27981073 ER PT J AU Mannucci, AJ Tsurutani, BT Verkhoglyadova, OP Meng, X AF Mannucci, A. J. Tsurutani, B. T. Verkhoglyadova, O. P. Meng, X. TI On scientific inference in geophysics and the use of numerical simulations for scientific investigations SO EARTH AND SPACE SCIENCE LA English DT Article ID MODELS; TEMPERATURE; IONOSPHERE AB Scientific knowledge is acquired in geophysics generally without the benefit of controlled experiments. In this paper, we discuss how scientific inference based on observations occurs in geophysical contexts. We develop a specific approach that uses approximate simultaneity of proposed cause and effect phenomena to infer causality. The approach applies equally well to effect phenomena that follow the cause with a known time delay. We find that, in general, establishing a causal relationship between two phenomena based on simultaneity requires knowledge of how often simultaneity of these phenomena occurs in the absence of causality. We then extend the discussion to using numerical simulations in the scientific inference process. Numerical simulations of physical processes, because they can simulate the values of observations, are often used to infer what physical processes are occurring in nature. We discuss agreement between model output and observations as a basis for inferring the physical processes underlying the observations. We find that an important factor to consider, which we here call the "confusion factor," is how often it may occur that insufficient model representations of the physical processes nevertheless lead to agreement between model computations and observations. We suggest that models of intermediate or low complexity may have a significant role to play when using geophysical simulations to reach scientific conclusions. C1 [Mannucci, A. J.; Tsurutani, B. T.; Verkhoglyadova, O. P.; Meng, X.] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Mannucci, AJ (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA USA. EM anthony.j.mannucci@jpl.nasa.gov NR 16 TC 1 Z9 1 U1 0 U2 0 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2333-5084 J9 Earth Space Sci JI Earth Space Sci. PD AUG PY 2015 VL 2 IS 8 BP 359 EP 367 DI 10.1002/2015EA000108 PG 9 WC Geosciences, Multidisciplinary SC Geology GA DE6NK UT WOS:000370750400003 ER PT J AU Bounoua, L Zhang, P Mostovoy, G Thome, K Masek, J Imhoff, M Shepherd, M Quattrochi, D Santanello, J Silva, J Wolfe, R Toure, AM AF Bounoua, Lahouari Zhang, Ping Mostovoy, Georgy Thome, Kurtis Masek, Jeffrey Imhoff, Marc Shepherd, Marshall Quattrochi, Dale Santanello, Joseph Silva, Julie Wolfe, Robert Toure, Ally Mounirou TI Impact of urbanization on US surface climate SO ENVIRONMENTAL RESEARCH LETTERS LA English DT Article DE urbanization; modeling; urban heat island; surface runoff; urban carbon ID URBAN HEAT ISLANDS; NET PRIMARY PRODUCTIVITY; UNITED-STATES; PARAMETERIZATION SIB2; ATMOSPHERIC GCMS; SATELLITE DATA; LAND; ENERGY; EMISSIONS; MODIS AB We combine Landsat and MODIS data in a land model to assess the impact of urbanization on US surface climate. For cities built within forests, daytime urban land surface temperature (LST) is much higher than that of vegetated lands. For example, in Washington DC and Atlanta, daytime mean temperature differences between impervious and vegetated lands reach 3.3 and 2.0 degrees C, respectively. Conversely, for cities built within arid lands, such as Phoenix, urban areas are 2.2 degrees C cooler than surrounding shrubs. We find that the choice and amount of tree species in urban settings play a commanding role in modulating cities' LST. At continental and monthly scales, impervious surfaces are 1.9 degrees C +/- 0.6 degrees C warmer than surroundings during summer and expel 12% of incoming precipitation as surface runoff compared to 3.2% over vegetation. We also show that the carbon lost to urbanization represents 1.8% of the continental total, a striking number considering urbanization occupies only 1.1% of the US land. With a small areal extent, urbanization has significant effects on surface energy, water and carbon budgets and reveals an uneven impact on surface climate that should inform upon policy options for improving urban growth including heat mitigation and carbon sequestration. C1 [Bounoua, Lahouari; Zhang, Ping; Mostovoy, Georgy; Thome, Kurtis; Masek, Jeffrey; Toure, Ally Mounirou] NASA, Goddard Space Flight Ctr, Biospher Sci Lab, Greenbelt, MD 20771 USA. [Zhang, Ping; Mostovoy, Georgy; Imhoff, Marc] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. [Shepherd, Marshall] Univ Georgia, Dept Geog, Athens, GA 30602 USA. [Quattrochi, Dale] MSFC, Marshal Space Flight Ctr, Huntsville, AL USA. [Santanello, Joseph] NASA, Goddard Space Flight Ctr, Hydrol Sci Lab, Greenbelt, MD 20771 USA. [Silva, Julie] Univ Maryland, Dept Geog Sci, College Pk, MD 20742 USA. [Wolfe, Robert] NASA, Goddard Space Flight Ctr, Terr Informat Syst Lab, Greenbelt, MD 20771 USA. [Zhang, Ping; Toure, Ally Mounirou] Sci Syst Applicat Inc, Lanham, MD USA. RP Bounoua, L (reprint author), NASA, Goddard Space Flight Ctr, Biospher Sci Lab, Greenbelt, MD 20771 USA. EM Lahouari.Bounoua@nasa.gov RI Masek, Jeffrey/D-7673-2012; Wolfe, Robert/E-1485-2012; Santanello, Joseph/D-4438-2012 OI Wolfe, Robert/0000-0002-0915-1855; Santanello, Joseph/0000-0002-0807-6590 FU NASA Interdisciplinary Research in Earth Science [NNH09ZDA001N-IDS] FX This work is funded by the NASA Interdisciplinary Research in Earth Science NNH09ZDA001N-IDS (2012). Garik Gutman, program manager. NR 40 TC 12 Z9 12 U1 10 U2 29 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 1748-9326 J9 ENVIRON RES LETT JI Environ. Res. Lett. PD AUG PY 2015 VL 10 IS 8 AR 084010 DI 10.1088/1748-9326/10/8/084010 PG 9 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA CZ3JD UT WOS:000366999400011 ER PT J AU Engelbrecht, F Adegoke, J Bopape, MJ Naidoo, M Garland, R Thatcher, M McGregor, J Katzfey, J Werner, M Ichoku, C Gatebe, C AF Engelbrecht, Francois Adegoke, Jimmy Bopape, Mary-Jane Naidoo, Mogesh Garland, Rebecca Thatcher, Marcus McGregor, John Katzfey, Jack Werner, Micha Ichoku, Charles Gatebe, Charles TI Projections of rapidly rising surface temperatures over Africa under low mitigation SO ENVIRONMENTAL RESEARCH LETTERS LA English DT Article DE climate change; African temperatures; regional climate model projections; heat-waves; high fire-danger days; drought index; actionable messages for adaptation ID CUBIC ATMOSPHERIC MODEL; SOUTHERN AFRICA; CLIMATE; FIRE; PRECIPITATION; SIMULATIONS; PATTERNS; SAVANNA; MONSOON; WORLD AB An analysis of observed trends in African annual-average near-surface temperatures over the last five decades reveals drastic increases, particularly over parts of the subtropics and central tropical Africa. Over these regions, temperatures have been rising at more than twice the global rate of temperature increase. An ensemble of high-resolution downscalings, obtained using a single regional climate model forced with the sea-surface temperatures and sea-ice fields of an ensemble of global circulation model (GCM) simulations, is shown to realistically represent the relatively strong temperature increases observed in subtropical southern and northern Africa. The amplitudes of warming are generally underestimated, however. Further warming is projected to occur during the 21st century, with plausible increases of 4-6 degrees Cover the subtropics and 3-5 degrees Cover the tropics by the end of the century relative to present-day climate under the A2 (a low mitigation) scenario of the Special Report on Emission Scenarios. High impact climate events such as heat-wave days and high fire-danger days are consistently projected to increase drastically in their frequency of occurrence. General decreases in soil-moisture availability are projected, even for regions where increases in rainfall are plausible, due to enhanced levels of evaporation. The regional dowscalings presented here, and recent GCM projections obtained for Africa, indicate that African annual-averaged temperatures may plausibly rise at about 1.5 times the global rate of temperature increase in the subtropics, and at a somewhat lower rate in the tropics. These projected increases although drastic, may be conservative given the model underestimations of observed temperature trends. The relatively strong rate of warming over Africa, in combination with the associated increases in extreme temperature events, may be key factors to consider when interpreting the suitability of global mitigation targets in terms of African climate change and climate change adaptation in Africa. C1 [Engelbrecht, Francois; Bopape, Mary-Jane; Naidoo, Mogesh; Garland, Rebecca] Council Sci & Ind Res Nat Resources & Environm, Climate Studies Modelling & Environm Hlth, ZA-0001 Pretoria, South Africa. [Engelbrecht, Francois] Univ Witwatersrand, Sch Geog Archaeol & Environm Studies, ZA-2000 Johannesburg, South Africa. [Adegoke, Jimmy] Univ Missouri, Dept Geosci, Kansas City, MO 64110 USA. [Garland, Rebecca] North West Univ, Unit Environm Sci & Management, Climatol Res Grp, Potchefstroom, South Africa. [Thatcher, Marcus; McGregor, John; Katzfey, Jack] Commonwealth Sci & Ind Res Org, Oceans & Atmosphere Flagship, Melbourne, Vic, Australia. [Werner, Micha] UNESCO IHE Inst Water Educ, Dept Water Engn, Delft, Netherlands. [Werner, Micha] Operat Water Management, Deltares, Rotterdam, Netherlands. [Ichoku, Charles; Gatebe, Charles] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Gatebe, Charles] Univ Space Res Assoc, Columbia, MD USA. RP Engelbrecht, F (reprint author), Council Sci & Ind Res Nat Resources & Environm, Climate Studies Modelling & Environm Hlth, ZA-0001 Pretoria, South Africa. EM fengelbrecht@csir.co.za RI Ichoku, Charles/E-1857-2012; Gatebe, Charles/G-7094-2011 OI Ichoku, Charles/0000-0003-3244-4549; Gatebe, Charles/0000-0001-9261-2239 FU European Commission Seventh Framework Programme 'FP7' through the report of EU-FP7 project DEWFORA-Improved Drought Early Warning and FORecasting to strengthen preparedness and adaptation to droughts in Africa [265454]; CSIR Parliamentary Grant [EECM066]; Thematic Area 2 of the Applied Centre for Climate and Earth System Studies (ACCESS) in South Africa; National Aeronautics and Space Administration (NASA) under its Research Opportunities in Space and Earth Sciences (ROSES) Interdisciplinary Studies (IDS) Programme; Office of Science, US Department of Energy FX The research received funding support from the European Commission Seventh Framework Programme 'FP7' through the report of EU-FP7 project DEWFORA-Improved Drought Early Warning and FORecasting to strengthen preparedness and adaptation to droughts in Africa, Grant No. 265454, a CSIR Parliamentary Grant EECM066, Thematic Area 2 of the Applied Centre for Climate and Earth System Studies (ACCESS) in South Africa and the National Aeronautics and Space Administration (NASA) under its Research Opportunities in Space and Earth Sciences (ROSES)-2009 Interdisciplinary Studies (IDS) Programme. All regional projections were performed on the computer clusters of the Centre for High Performance Computing (CHPC) in South Africa. Christien Engelbrecht and Neville Sweijd are thanked for their constructive comments on the manuscript. Moreover, comments from three anonymous reviewers have helped to improve the paper. We acknowledge the modelling groups, the Program for Climate Model Diagnosis and Intercomparison (PCMDI) and the World Climate Research Programme's (WCRP's) Working Group on Coupled Modelling (WGCM) for their roles in making available the WCRP CMIP3 multi-model dataset (with regards to the GCM projections downscaled in this paper). Support of this dataset is provided by the Office of Science, US Department of Energy. NR 64 TC 5 Z9 6 U1 2 U2 10 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 1748-9326 J9 ENVIRON RES LETT JI Environ. Res. Lett. PD AUG PY 2015 VL 10 IS 8 AR 085004 DI 10.1088/1748-9326/10/8/085004 PG 16 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA CZ3JD UT WOS:000366999400031 ER PT J AU Xu, L Saatchi, SS Yang, Y Myneni, RB Frankenberg, C Chowdhury, D Bi, J AF Xu, Liang Saatchi, Sassan S. Yang, Yan Myneni, Ranga B. Frankenberg, Christian Chowdhury, Diya Bi, Jian TI Satellite observation of tropical forest seasonality: spatial patterns of carbon exchange in Amazonia SO ENVIRONMENTAL RESEARCH LETTERS LA English DT Article DE vegetation seasonality; amazonia; tropical forest; remote sensing; pheno-region; GPP; fluorescence ID FUTURE CLIMATE; RAIN-FORESTS; DRY-SEASON; PRODUCTIVITY; DYNAMICS; MODIS; TEMPERATURE; SENSITIVITY; VALIDATION; ECOSYSTEMS AB Determining the seasonality of terrestrial carbon exchange with the atmosphere remains a challenge in tropical forests because of the heterogeneity of ecosystem and climate. The magnitude and spatial variability of this flux are unknown, particularly in Amazonia where empirical upscaling approaches from spatially sparse in situ measurements and simulations from process-based models have been challenged in recent scientific literature. Here, we use satellite proxy observations of canopy structure, skin temperature, water content, and optical properties over a period of 10 years (2000-2009) to constrain and quantify the spatial pattern and seasonality of carbon exchange of Amazonian forests. We identify nine regions through an optimized cluster approach with distinct leaf phenology synchronized with either water or light availability and corresponding seasonal cycles of gross primary production (GPP), covering more than 600 million ha of remaining old growth forests of Amazonia. We find South and Southwestern regions show strong seasonality of GPP with a peak in the wet season; while from Central Western to Northeastern Amazonia cover three regions with rising GPP in the dry season. The remaining four regions have significant but weak seasonality. These patterns agree with satellite florescence observations, a better proxy for photosynthetic activity. Our results suggest that only one-third of the patterns can be explained by the spatial autocorrelation caused by intra-annual variability of climate over Amazonia. The remaining two thirds of variations are due to biogeography of the Amazon basin driven by forest composition, structure, and nutrients. These patterns, for the first time, provide a complex picture of seasonal changes of tropical forests related to photosynthesis and influenced by water, light, and stomatal responses of trees that can improve modeling of regional carbon cycle and future prediction of impacts of climate change. C1 [Xu, Liang; Saatchi, Sassan S.; Yang, Yan; Chowdhury, Diya] Univ Calif Los Angeles, Inst Environm & Sustainabil, Los Angeles, CA 90095 USA. [Saatchi, Sassan S.; Frankenberg, Christian] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Yang, Yan; Myneni, Ranga B.; Bi, Jian] Boston Univ, Dept Earth & Environm, Boston, MA 02215 USA. RP Xu, L (reprint author), Univ Calif Los Angeles, Inst Environm & Sustainabil, Los Angeles, CA 90095 USA. EM xuliang@ucla.edu; saatchi@jpl.nasa.gov RI Myneni, Ranga/F-5129-2012; Frankenberg, Christian/A-2944-2013 OI Frankenberg, Christian/0000-0002-0546-5857 FU NASA FX This work was funded by NASA Earth Science Division. We thank NSIDC, BYU, NASA MODIS Project, NASA GSFC, and CERES science team for making their data available. The authors thank C J Tucker and J E Pinzon for providing the newer version of AVHRR NDVI. We also thank M Jung for the upscaled GPP data set available at the MPI-BGC data portal. NR 57 TC 4 Z9 4 U1 3 U2 18 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 1748-9326 J9 ENVIRON RES LETT JI Environ. Res. Lett. PD AUG PY 2015 VL 10 IS 8 AR 084005 DI 10.1088/1748-9326/10/8/084005 PG 10 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA CZ3JD UT WOS:000366999400006 ER PT J AU Roedel, H Plata, IR Lepech, M Loftus, D AF Roedel, Henning Plata, Isamar Rosa Lepech, Michael Loftus, David TI Sustainability Assessment of Protein-Soil Composite Materials for Limited Resource Environments SO JOURNAL OF RENEWABLE MATERIALS LA English DT Article DE Biocomposite; sustainability; protein; concrete ID BOVINE AB This article presents the sustainability assessment of a novel biocomposite material that is under investigation by NASA for use in construction in limited resource environments. The composite consists of soil particles solidified by a protein binding agent. Preliminary compressive strength data suggests the biocomposite could be used for numerous construction applications. To assess the biocomposite's potential for use in sustainable construction, a comparative process-based life cycle assessment between biocomposite and concrete pavers was performed to analyze the life cycle primary energy and IMPACT 2002+ points of both types of pavers. Results show that the concrete pavers outperform the biocomposite pavers in initial impact. However, biocomposite pavers can be more favorable when binder reclamation and reuse scenarios are taken into account at end-of-life. Based on these results, recommendations include switching to a mixture of lower grade proteins to reduce the biocomposite impact as well as further laboratory investigations into recycling scenarios. C1 [Roedel, Henning; Plata, Isamar Rosa; Lepech, Michael] Stanford Univ, Dept Civil & Environm Engn, Stanford, CA 94305 USA. [Loftus, David] NASA, Ames Res Ctr, Div Space Biosci, Moffett Field, CA 94035 USA. RP Lepech, M (reprint author), Stanford Univ, Dept Civil & Environm Engn, 450 Serra Mall, Stanford, CA 94305 USA. EM mlepech@stanford.edu FU Center Investment Fund, NASA Ames Research Center; Game Changing Development Program, Science and Technology Mission Directorate, NASA; California Home Builders Association Scholarship; Division of Space Biosciences, NASA Ames Research Center; Stanford Graduate Fellowship Program; National Science Foundation Graduate Research Fellowship Program; Department of Civil and Environmental Engineering, Stanford University FX The authors would like to gratefully acknowledge funding support from the Center Investment Fund, NASA Ames Research Center; the Game Changing Development Program, Science and Technology Mission Directorate, NASA; the California Home Builders Association Scholarship (to H.R.); the Division of Space Biosciences, NASA Ames Research Center; the Stanford Graduate Fellowship Program; the National Science Foundation Graduate Research Fellowship Program; and, the Department of Civil and Environmental Engineering, Stanford University. We gratefully acknowledge programmatic and management support from the following individuals: Dr. Pete Warden, Dr. David Bergner, Dr. Mark Kliss, Sid Sun, and Laura Lewis, all at NASA Ames Research Center. We gratefully acknowledge helpful discussions with the Synthetic Biology Team at NASA Ames Research Center, especially with Dr. Lynn J. Rothschild, Dr. Rocco L. Mancinelli, and Dr. John Hogan. We gratefully acknowledge the UCSC Materials Analysis for Collaborative Science facility at NASA Ames Research Center and the help of Dr. Mike Oye, Joseph Varelas, and Dr. Jessica Koehne. We gratefully acknowledge the technical contributions of Jon Rask (NASA Ames Research Center), Peggy Moriarty (Stanford University), Daniel Z. Fischer (Dartmouth College), Capt. Patrick J. Sullivan (Stanford University), Mark Solorio (Stanford University), Sarah Woogen (Stanford University), Chase Young (Stanford University), and Sophie Zhang (Stanford University). NR 30 TC 0 Z9 0 U1 0 U2 0 PU SCRIVENER PUBLISHING PI BEVERLY PA 100 CUMMINGS CENTER, SUITE 541J, BEVERLY, MA 01915-6106 USA SN 2164-6325 EI 2164-6341 J9 J RENEW MATER JI J. Renew. Mater. PD AUG PY 2015 VL 3 IS 3 SI SI BP 183 EP 194 DI 10.7569/JRM.2015.634107 PG 12 WC GREEN & SUSTAINABLE SCIENCE & TECHNOLOGY; Materials Science, Composites; Polymer Science SC Science & Technology - Other Topics; Materials Science; Polymer Science GA CX4KT UT WOS:000365669800004 ER PT J AU Thompson, DJ AF Thompson, David J. TI Space detectors for gamma rays (100 MeV-100 GeV): From EGRET to Fermi LAT SO COMPTES RENDUS PHYSIQUE LA English DT Article DE Gamma rays; Detectors; Space ID LARGE-AREA TELESCOPE; COS-B; PAIR PRODUCTION; CRAB-NEBULA; CALIBRATION; RADIATION; EMISSION; CATALOG; PULSAR; POLARIMETRY AB The design of spaceborne high-energy (E > 100 MeV) gamma-ray detectors depends on two principal factors: (1) the basic physics of detecting and measuring the properties of the gamma rays; and (2) the constraints of operating such a detector in space for an extended period. Improvements in technology have enabled major advances in detector performance, as illustrated by two successful instruments, EGRET on the Compton Gamma Ray Observatory and LAT on the Fermi Gamma-ray Space Telescope. (C) 2015 Academie des sciences. Published by Elsevier Masson SAS. All rights reserved. C1 [Thompson, David J.] NASA Goddard Space Flight Ctr, Astroparticle Phys Lab, Greenbelt, MD 20771 USA. RP Thompson, DJ (reprint author), NASA Goddard Space Flight Ctr, Astroparticle Phys Lab, Greenbelt, MD 20771 USA. EM David.J.Thompson@nasa.gov NR 46 TC 8 Z9 8 U1 0 U2 0 PU ELSEVIER FRANCE-EDITIONS SCIENTIFIQUES MEDICALES ELSEVIER PI PARIS PA 23 RUE LINOIS, 75724 PARIS, FRANCE SN 1631-0705 EI 1878-1535 J9 CR PHYS JI C. R. Phys. PD AUG-SEP PY 2015 VL 16 IS 6-7 BP 600 EP 609 DI 10.1016/j.crhy.2015.07.002 PG 10 WC Astronomy & Astrophysics; Physics, Multidisciplinary SC Astronomy & Astrophysics; Physics GA CW8JE UT WOS:000365244800002 ER PT J AU Grenier, IA Harding, AK AF Grenier, Isabelle A. Harding, Alice K. TI Gamma-ray pulsars: A gold mine SO COMPTES RENDUS PHYSIQUE LA English DT Article DE Pulsar; Neutron star; Magnetosphere; Gamma rays; Acceleration ID HIGH-ENERGY EMISSION; FERMI/LARGE AREA TELESCOPE; RAPIDLY SPINNING PULSARS; BINARY PSR J1023+0038; POLAR-CAP CASCADE; OUTER-GAP MODEL; CRAB-NEBULA; MILLISECOND PULSAR; X-RAY; LIGHT CURVES AB The most energetic neutron stars, powered by their rotation, are capable of producing pulsed radiation from the radio up to gamma rays with nearly TeV energies. These pulsars are part of the universe of energetic and powerful particle accelerators, using their uniquely fast rotation and formidable magnetic fields to accelerate particles to ultra-relativistic speed. The extreme properties of these stars provide an excellent testing ground, beyond Earth experience, for nuclear, gravitational, and quantum-electrodynamical physics. A wealth of gamma-ray pulsars has recently been discovered with the Fermi Gamma-Ray Space Telescope. The energetic gamma rays enable us to probe the magnetospheres of neutron stars and particle acceleration in this exotic environment. We review the latest developments in this field, beginning with a brief overview of the properties and mysteries of rotation-powered pulsars, and then discussing gamma-ray observations and magnetospheric models in more detail. (C) 2015 Academie des sciences. Published by Elsevier Masson SAS. All rights reserved. C1 [Grenier, Isabelle A.] Univ Paris Diderot, CNRS, CEA IRFU, Lab AIM Paris Saclay, F-91191 Gif Sur Yvette, France. [Harding, Alice K.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Grenier, IA (reprint author), Univ Paris Diderot, CNRS, CEA IRFU, Lab AIM Paris Saclay, F-91191 Gif Sur Yvette, France. EM isabelle.grenier@cea.fr; Alice.K.Harding@nasa.gov FU Institut Universitaire de France; NASA Astrophysics Theory Program FX We thank the pulsar timing and search consortia for their key support of the Fermi-LAT pulsar analyses and we thank the Fermi-LAT pulsar team and the pulsar theory group at NASA GSFC for many inspiring discussions. I.G. acknowledges research support from the Institut Universitaire de France. AKH acknowledges support from the NASA Astrophysics Theory Program. NR 186 TC 10 Z9 10 U1 0 U2 4 PU ELSEVIER FRANCE-EDITIONS SCIENTIFIQUES MEDICALES ELSEVIER PI PARIS PA 23 RUE LINOIS, 75724 PARIS, FRANCE SN 1631-0705 EI 1878-1535 J9 CR PHYS JI C. R. Phys. PD AUG-SEP PY 2015 VL 16 IS 6-7 BP 641 EP 660 DI 10.1016/j.crhy.2015.08.013 PG 20 WC Astronomy & Astrophysics; Physics, Multidisciplinary SC Astronomy & Astrophysics; Physics GA CW8JE UT WOS:000365244800005 ER PT J AU Raccanelli, A Dore, O Dalal, N AF Raccanelli, Alvise Dore, Olivier Dalal, Neal TI Optimization of spectroscopic surveys for testing non-Gaussianity SO JOURNAL OF COSMOLOGY AND ASTROPARTICLE PHYSICS LA English DT Article DE redshift surveys; inflation; cosmological parameters from LSS; physics of the early universe ID REDSHIFT-SPACE DISTORTIONS; PRIMORDIAL NON-GAUSSIANITY; DISTANCE SCALE; GALAXY SURVEYS; COSMOLOGY; GROWTH; INFLATION; GRAVITY; LAMBDA AB We investigate optimization strategies to measure primordial non-Gaussianity with future spectroscopic surveys. We forecast measurements coming from the 3D galaxy power spectrum and compute constraints on primordial non-Gaussianity parameters f(NL), and nNG. After studying the dependence on those parameters upon survey specifications such as redshift range, area, number density, we assume a reference mock survey and investigate the trade-off between number density and area surveyed. We then define the observational requirements to reach the detection of f(NL) of order 1. Our results show that power spectrum constraints on non-Gaussianity from future spectroscopic surveys can improve on current CMB limits, but the multi-tracer technique and higher order correlations will be needed in order to reach an even better precision in the measurements of the non-Gaussianity parameter f(NL). C1 [Raccanelli, Alvise; Dore, Olivier] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Raccanelli, Alvise; Dore, Olivier] CALTECH, Pasadena, CA 91125 USA. [Dalal, Neal] Univ Illinois, Dept Astron, Urbana, IL 61801 USA. RP Raccanelli, A (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM alvise@caltech.edu; Olivier.P.Dore@jpl.nasa.gov; dalaln@illinois.edu OI Raccanelli, Alvise/0000-0001-6726-0438 NR 74 TC 1 Z9 1 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 1475-7516 J9 J COSMOL ASTROPART P JI J. Cosmol. Astropart. Phys. PD AUG PY 2015 IS 8 AR 034 DI 10.1088/1475-7516/2015/08/034 PG 17 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA CW5OT UT WOS:000365046600034 ER PT J AU Lee, JH Han, JW Yu, CG Park, JT AF Lee, Jae Hoon Han, Jin-Woo Yu, Chong Gun Park, Jong Tae TI Effect of source and drain asymmetry on hot carrier degradation in vertical nanowire MOSFETs SO MICROELECTRONICS RELIABILITY LA English DT Article; Proceedings Paper CT 26th European Symposium on Reliability of Electron Devices, Failure Physics and Analysis CY OCT 05-19, 2015 CL Toulouse, FRANCE DE Vertical MOSFET; Hot carrier degradation; Asymmetry source/drain ID FIELD-EFFECT TRANSISTORS; GATE; RELIABILITY; PERFORMANCE; CMOS AB Effects of source and drain (S/D) asymmetry on hot carrier degradation in vertical nanowire MOSFETs have been investigated with different nanowire radiuses. The S/D asymmetry causes different degree of hot carrier degradations between forward and reverse stresses. The actual stress voltage applied to the channel as a result of parasitic resistance and gate to junction overlap length is attributed to the cause of the asymmetric degradation. The narrower nanowire also suffers from worse hot carrier effects due to current crowding and geometric effects. (C) 2015 Elsevier Ltd. All rights reserved. C1 [Lee, Jae Hoon; Yu, Chong Gun; Park, Jong Tae] Incheon Natl Univ, Dept Elect Engn, Inchon 406772, South Korea. [Han, Jin-Woo] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Park, JT (reprint author), Incheon Natl Univ, Dept Elect Engn, 119 Acad Ro, Inchon 406772, South Korea. EM jtpark@incheon.ac.kr FU Incheon National University Research Grant FX This work was supported by the Incheon National University Research Grant in 2015. NR 15 TC 1 Z9 1 U1 5 U2 8 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0026-2714 J9 MICROELECTRON RELIAB JI Microelectron. Reliab. PD AUG-SEP PY 2015 VL 55 IS 9-10 BP 1456 EP 1459 DI 10.1016/j.microrel.2015.06.062 PG 4 WC Engineering, Electrical & Electronic; Nanoscience & Nanotechnology; Physics, Applied SC Engineering; Science & Technology - Other Topics; Physics GA CV4SI UT WOS:000364256400036 ER PT J AU Parazoo, NC Barnes, E Worden, J Harper, AB Bowman, KB Frankenberg, C Wolf, S Litvak, M Keenan, TF AF Parazoo, Nicholas C. Barnes, Elizabeth Worden, John Harper, Anna B. Bowman, Kevin B. Frankenberg, Christian Wolf, Sebastian Litvak, Marcy Keenan, Trevor F. TI Influence of ENSO and the NAO on terrestrial carbon uptake in the Texas-northern Mexico region SO GLOBAL BIOGEOCHEMICAL CYCLES LA English DT Article ID ENVIRONMENT SIMULATOR JULES; GROSS PRIMARY PRODUCTION; LAND-SURFACE SCHEME; STOMATAL CONDUCTANCE; CLIMATE VARIABILITY; MODEL DESCRIPTION; DROUGHT; PHOTOSYNTHESIS; DIOXIDE; WATER AB Climate extremes such as drought and heat waves can cause substantial reductions in terrestrial carbon uptake. Advancing projections of the carbon uptake response to future climate extremes depends on (1) identifying mechanistic links between the carbon cycle and atmospheric drivers, (2) detecting and attributing uptake changes, and (3) evaluating models of land response and atmospheric forcing. Here, we combine model simulations, remote sensing products, and ground observations to investigate the impact of climate variability on carbon uptake in the Texas-northern Mexico region. Specifically, we (1) examine the relationship between drought, carbon uptake, and variability of El Nino-Southern Oscillation (ENSO) and the North Atlantic Oscillation (NAO) using the Joint UK Land-Environment Simulator (JULES) biosphere simulations from 1950-2012, (2) quantify changes in carbon uptake during record drought conditions in 2011, and (3) evaluate JULES carbon uptake and soil moisture in 2011 using observations from remote sensing and a network of flux towers in the region. Long-term simulations reveal systematic decreases in regional-scale carbon uptake during negative phases of ENSO and NAO, including amplified reductions of gross primary production (GPP) (-0.42+/-0.18 Pg C yr(-1)) and net ecosystem production (NEP) (-0.14 +/- 0.11 Pg C yr(-1)) during strong La Nina years. The 2011 megadrought caused some of the largest declines of GPP (-0.50 Pg C yr(-1)) and NEP (-0.23 Pg C yr(-1)) in our simulations. In 2011, consistent declines were found in observations, including high correlation of GPP and surface soil moisture (r = 0.82 +/- 0.23, p = 0.012) in remote sensing-based products. These results suggest a large-scale response of carbon uptake to ENSO and NAO, and highlight a need to improve model predictions of ENSO and NAO in order to improve predictions of future impacts on the carbon cycle and the associated feedbacks to climate change. C1 [Parazoo, Nicholas C.; Worden, John; Bowman, Kevin B.; Frankenberg, Christian] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Parazoo, Nicholas C.; Bowman, Kevin B.] Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA USA. [Barnes, Elizabeth] Colorado State Univ, Dept Atmospher Sci, Ft Collins, CO 80523 USA. [Harper, Anna B.] Univ Exeter, Dept Math & Phys Sci, Exeter, Devon, England. [Wolf, Sebastian] Univ Calif Berkeley, Dept Environm Sci Policy & Management, Berkeley, CA 94720 USA. [Wolf, Sebastian] ETH, Inst Agr Sci, Zurich, Switzerland. [Litvak, Marcy] Univ New Mexico, Dept Biol, Albuquerque, NM 87131 USA. [Keenan, Trevor F.] Macquarie Univ, Dept Biol Sci, Sydney, NSW 2109, Australia. RP Parazoo, NC (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. EM Nicholas.C.Parazoo@jpl.nasa.gov RI Wolf, Sebastian/B-4580-2010; Barnes, Elizabeth/O-1790-2014; Keenan, Trevor/B-2744-2010; Frankenberg, Christian/A-2944-2013 OI Wolf, Sebastian/0000-0001-7717-6993; Barnes, Elizabeth/0000-0003-4284-9320; Keenan, Trevor/0000-0002-3347-0258; Frankenberg, Christian/0000-0002-0546-5857 FU Marie Curie International Outgoing Fellowship; Macquarie University Research Fellowship; NASA ROSES Program; NASA Atmospheric CO2 Observations from Space (ACOS) program [NNX10AT42G] FX CRU-NCEP climate information is obtained from ftp://nacp.ornl.gov/synthesis/2009/frescati/model_driver/cru_ncep/analys is/readme.htm. ENSO and NAO indices are obtained at NOAA CPC (http://www.cpc.ncep.noaa.gov/products/analysis_monitoring/ensostuff/ens oyears.shtml). JULES model output and CRU-NCEP data are provided by A. Harper (A.Harper@exeter.ac.uk). SMOS data are available for data access at http://catds.ifremer.fr/Products/Products-access. Chlorophyll fluorescence data were provided by C. Frankenberg (Christian. Frankenberg@jpl.nasa.gov). MPI-BGC data set was provided by M. Jung (martin.jung@bgc-jena.mpg.de). MODIS MOD17 GPP data are available at http://www.ntsg.umt.edu/project/mod17. GRACE land data are available at http://grace.jpl.nasa.gov. Flux tower data are collected/processed by M. Litvak (marcy.litvak@gmail.com) and gap-filled/partitioned by S. Wolf (sewolf@berkeley.edu). We acknowledge all MODIS land product science team members for providing an invaluable public data set. The improved MOD17 GPP data were provided by the Numerical Terradynamic Simulation Group at the University of Montana. We thank the Global Carbon Project and TRENDY modelers for contributing model output. We also give special thanks to S. Sitch and P. Friedlingstein for organizing TRENDY. GRACE land data processing algorithms were provided by S. Swenson and supported by the NASA MEaSUREs Program. SMOS data were obtained from the Centre Aval de Traitement des Donnees SMOS (CATDS), operated for the Centre National d'Etudes Spatiales (CNES, France) by IFREMER (Brest, France). S. Wolf acknowledges support from a Marie Curie International Outgoing Fellowship. T.F. Keenan acknowledges support from a Macquarie University Research Fellowship. M. Litvak acknowledges support from NASA ROSES Program. We give special thanks to A. Mialon for providing assistance in the processing and interpretation of the SMOS data set. This research was funded by the NASA Atmospheric CO2 Observations from Space (ACOS) program (grant NNX10AT42G) and carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA (C) 2014. NR 67 TC 4 Z9 4 U1 7 U2 28 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0886-6236 EI 1944-9224 J9 GLOBAL BIOGEOCHEM CY JI Glob. Biogeochem. Cycle PD AUG PY 2015 VL 29 IS 8 BP 1247 EP 1265 DI 10.1002/2015GB005125 PG 19 WC Environmental Sciences; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Geology; Meteorology & Atmospheric Sciences GA CU7FP UT WOS:000363702400010 ER PT J AU Eke, VR Bower, KE Diserens, S Ryder, M Yeomans, PEL Teodoro, LFA Elphic, RC Feldman, WC Hermalyn, B Lavelle, CM Lawrence, DJ AF Eke, V. R. Bower, K. E. Diserens, S. Ryder, M. Yeomans, P. E. L. Teodoro, L. F. A. Elphic, R. C. Feldman, W. C. Hermalyn, B. Lavelle, C. M. Lawrence, D. J. TI The effect of craters on the lunar neutron flux SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID SPATIAL-DISTRIBUTION; EPITHERMAL NEUTRONS; WATER ICE; MOON; PROSPECTOR; DETECTOR; LEAKAGE; POLES; PLUME AB The variation of remotely sensed neutron count rates is measured as a function of cratercentric distance using data from the Lunar Prospector Neutron Spectrometer. The count rate, stacked over many craters, peaks over the crater center, has a minimum near the crater rim, and at larger distances, it increases to a mean value that is up to 1% lower than the mean count rate observed over the crater. A simple model is presented, based upon an analytical topographical profile for the stacked craters fitted to data from the Lunar Orbiter Laser Altimeter. The effect of topography coupled with neutron beaming from the surface largely reproduces the observed count rate profiles. However, a model that better fits the observations can be found by including the additional freedom to increase the neutron emissivity of the crater area by similar to 0.35% relative to the unperturbed surface. It is unclear what might give rise to this effect, but it may relate to additional surface roughness in the vicinities of craters. The amplitude of the crater-related signal in the neutron count rate is small, but not too small to demand consideration when inferring water-equivalent hydrogen (WEH) weight percentages in polar permanently shaded regions (PSRs). If the small crater-wide count rate excess is concentrated into a much smaller PSR, then it can lead to a large bias in the inferred WEH weight percentage. For instance, it may increase the inferred WEH for Cabeus crater at the Moon's south pole from similar to 1% to similar to 4%. C1 [Eke, V. R.; Bower, K. E.; Diserens, S.; Ryder, M.; Yeomans, P. E. L.] Univ Durham, Sci Labs, Dept Phys, Inst Computat Cosmol, Durham DH1 3LE, England. [Teodoro, L. F. A.] NASA Ames Res Ctr, Space Sci & Astrobiol Div, Planetary Syst Branch, BAER, Moffett Field, CA USA. [Elphic, R. C.] NASA Ames Res Ctr, Space Sci & Astrobiol Div, Planetary Syst Branch, Moffett Field, CA USA. [Feldman, W. C.] Planetary Sci Inst, Tucson, AZ USA. [Hermalyn, B.] Univ Hawaii Manoa, NASA Astrobiol Inst, Inst Astron, Honolulu, HI 96822 USA. [Lavelle, C. M.; Lawrence, D. J.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA. RP Eke, VR (reprint author), Univ Durham, Sci Labs, Dept Phys, Inst Computat Cosmol, Durham DH1 3LE, England. EM v.r.eke@durham.ac.uk RI Lawrence, David/E-7463-2015 OI Lawrence, David/0000-0002-7696-6667 FU Science and Technology Facilities Council [ST/L00075X/1] FX The LOLA, LPNS, and LEND data can be accessed via the Geosciences Node of NASA's Planetary Data System at http://pds-geosciences.wustl.edu. V.R.E. was supported by the Science and Technology Facilities Council[ST/L00075X/1]. NR 32 TC 3 Z9 3 U1 0 U2 1 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9097 EI 2169-9100 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD AUG PY 2015 VL 120 IS 8 BP 1377 EP 1395 DI 10.1002/2015JE004856 PG 19 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA CU9XB UT WOS:000363899100001 ER PT J AU Borlina, CS Ehlmann, BL Kite, ES AF Borlina, Caue S. Ehlmann, Bethany L. Kite, Edwin S. TI Modeling the thermal and physical evolution of Mount Sharp's sedimentary rocks, Gale Crater, Mars: Implications for diagenesis on the MSL Curiosity rover traverse SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID CLAY-MINERALS; YELLOWKNIFE BAY; ORIGIN; WATER; HISTORY; SULFATE AB Gale Crater, the Mars Science Laboratory (MSL) landing site, contains a central mound, named Aeolis Mons (informally Mount Sharp) that preserves 5 km of sedimentary stratigraphy. Formation scenarios include (1) complete filling of Gale Crater followed by partial sediment removal or (2) building of a central deposit with morphology controlled by slope winds and only incomplete sedimentary fill. Here we model temperature-time paths for both scenarios, compare results with analyses provided by MSL Curiosity, and provide scenario-dependent predictions of temperatures of diagenesis along Curiosity's future traverse. The effects of variable sediment thermal conductivity and historical heat flows are also discussed. Modeled erosion and deposition rates are 5-37 mu m/yr, consistent with previously published estimates from other Mars locations. The occurrence and spatial patterns of diagenesis depend on sedimentation scenario and surface paleotemperature. For (1) temperatures experienced by sediments decrease monotonically along the traverse and up Mount Sharp stratigraphy, whereas for (2) temperatures increase along the traverse reaching maximum temperatures higher up in Mount Sharp's lower units. If early Mars surface temperatures were similar to modern Mars (mean: -50 degrees C), only select locations under select scenarios permit diagenetic fluids. In contrast, if early Mars surface temperatures averaged 0 degrees C or brines had lowered freezing points, diagenesis is predicted in most locations with temperatures < 225 degrees C. Comparing our predictions with future MSL results on diagenetic textures, secondary mineral assemblages, and their spatial variability will constrain past heat flow, Mount Sharp's formation processes, the availability of liquid water on early Mars, and sediment organic preservation potential. C1 [Borlina, Caue S.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. [Borlina, Caue S.; Ehlmann, Bethany L.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Ehlmann, Bethany L.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Kite, Edwin S.] Univ Chicago, Dept Geophys Sci, Chicago, IL 60637 USA. RP Borlina, CS (reprint author), Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. EM caue@umich.edu FU MSL Participating Scientist grant; Princeton University Harry Hess fellowship FX The data for this paper are available at NASA's PDS Geoscience Node. This work was partially funded by an MSL Participating Scientist grant to B.L.E. The Caltech Summer Undergraduate Research Fellowship program provided programmatic support to C.S.B. E.S.K. acknowledges support from a Princeton University Harry Hess fellowship. NR 57 TC 6 Z9 6 U1 3 U2 20 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9097 EI 2169-9100 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD AUG PY 2015 VL 120 IS 8 BP 1396 EP 1414 DI 10.1002/2015JE004799 PG 19 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA CU9XB UT WOS:000363899100002 ER PT J AU Miller, KE Kotrc, B Summons, RE Belmahdi, I Buch, A Eigenbrode, JL Freissinet, C Glavin, DP Szopa, C AF Miller, Kristen E. Kotrc, Benjamin Summons, Roger E. Belmahdi, Imene Buch, Arnaud Eigenbrode, Jennifer L. Freissinet, Caroline Glavin, Daniel P. Szopa, Cyril TI Evaluation of the Tenax trap in the Sample Analysis at Mars instrument suite on the Curiosity rover as a potential hydrocarbon source for chlorinated organics detected in Gale Crater SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID MAGNESIUM PERCHLORATE; THERMAL-DECOMPOSITION AB The Sample Analysis at Mars (SAM) instrument suite aboard Curiosity has detected chlorinated organic compounds in Martian sediment samples. The chlorine in these molecules is thought to derive from oxychlorine salts in Martian sediments, but the carbon source remains under investigation. To constrain possible carbon sources, we investigated how the composition and concentration of oxychlorine phases in solid samples affect organic molecules released from the Tenax traps on board SAM. We created Mars analogue soils by spiking olivine sand with calcium perchlorate, magnesium perchlorate, or ferric iron chloride and analyzed the volatiles generated during pyrolysis-gas chromatography-mass spectrometry using commercial instruments operated under SAM-like conditions, with and without a Tenax trap. Benzoic acid, phthalic anhydride, high molecular weight aromatics, and chlorobenzenes are produced from the trap in response to volatiles released during Cl salt pyrolysis. Changes in composition or concentration of oxychlorine phases between samples could thus potentially produce an increase in chlorobenzene, as observed between samples from Rocknest and Cumberland. However, in our experiments benzoic acid, phthalic anhydride, and chlorobenzenes increase in proportion with the amount of HCl sent to the trap, while in Cumberland samples the chlorobenzene increase showed no corresponding increase in HCl. Based on our experiments, the Tenax trap is a possible source of the traces of chlorobenzene observed at Rocknest, John Klein, and Confidence Hills. The order-of-magnitude higher chlorobenzene abundances observed at Cumberland cannot be attributed to the Tenax trap. Furthermore, we found no evidence of significant trap degradation after hundreds of experiments with Cl salt-containing analogue soils. C1 [Miller, Kristen E.; Kotrc, Benjamin; Summons, Roger E.] MIT, Cambridge, MA 02139 USA. [Belmahdi, Imene; Buch, Arnaud] Lab Genie Procedes & Mat, Chatenay Malabry, France. [Eigenbrode, Jennifer L.; Freissinet, Caroline; Glavin, Daniel P.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Szopa, Cyril] Atmospheres Lab, Milieux, Observat Spatiales, Paris 05, France. RP Summons, RE (reprint author), MIT, 77 Massachusetts Ave, Cambridge, MA 02139 USA. EM rsummons@mit.edu RI Glavin, Daniel/D-6194-2012; szopa, cyril/C-6865-2015 OI Glavin, Daniel/0000-0001-7779-7765; szopa, cyril/0000-0002-0090-4056 FU NASA ROSES MSL Participating Scientist Program; NASA Astrobiology Institute [NNA13AA90A] FX This work was supported by the NASA ROSES MSL Participating Scientist Program through a grant to R.E.S. We thank MSL and SAM science teams for their helpful input. B. Kotrc received additional support from the NASA Astrobiology Institute (NNA13AA90A). Data used for the results of this paper are available upon request from the corresponding author. We thank Mildred Martin for the technical assistance in the work conducted at GSFC. NR 16 TC 3 Z9 3 U1 11 U2 23 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9097 EI 2169-9100 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD AUG PY 2015 VL 120 IS 8 BP 1446 EP 1459 DI 10.1002/2015JE004825 PG 14 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA CU9XB UT WOS:000363899100005 ER PT J AU Liu, L Sletten, RS Hagedorn, B Hallet, B Mckay, CP Stone, JO AF Liu, Lu Sletten, Ronald S. Hagedorn, Birgit Hallet, Bernard Mckay, Christopher P. Stone, John O. TI An enhanced model of the contemporary and long-term (200ka) sublimation of the massive subsurface ice in Beacon Valley, Antarctica SO JOURNAL OF GEOPHYSICAL RESEARCH-EARTH SURFACE LA English DT Article ID MCMURDO DRY VALLEYS; SOUTHERN VICTORIA LAND; MIOCENE GLACIER ICE; GROUND ICE; WATER-VAPOR; MARS; STABILITY; PERMAFROST; REGION; SHEET AB A massive ice body buried under several decimeters of dry regolith in Beacon Valley, Antarctica, is believed to be more than 1 Ma old and perhaps over 8.1 Ma; however, vapor diffusion models suggest that subsurface ice in this region is not stable under current climate conditions. To better understand the controls on sublimation rates and stability of this massive ice, we have modeled vapor diffusion using 12 years of climate and soil temperature data from 1999 to 2011, including field measurements of episodic snow cover and snowmelt events that have not been represented in previous models of ground ice sublimation. The model is then extended to reconstruct the sublimation history over the last 200 ka using paleotemperatures estimated from ice core data from nearby Taylor Dome and a relationship between atmospheric temperature and humidity derived from our meteorological records. The model quantifies the impact of episodic snow events; they account for a nearly 30% reduction in the massive ice loss. The sublimation rate of ground ice averages 0.11 mm a(-1) between 1999 and 2011 in Beacon Valley. Parameterized with past environmental conditions and assuming the same regolith thickness, the modeled sublimation rate of ground ice in Beacon Valley averages 0.09 mm a(-1) for the last 200 ka, comparable to the long-term average rate estimated independently from various studies based on cosmogenic isotopes. This study provides a realistic estimate of the long-term sublimation history and supports the inference that the buried ice in Beacon Valley is older than 1 Ma. C1 [Liu, Lu; Sletten, Ronald S.; Hallet, Bernard; Stone, John O.] Univ Washington, Dept Earth & Space Sci, Seattle, WA 98195 USA. [Hagedorn, Birgit] Univ Alaska Anchorage, Environm & Nat Resources Inst, Anchorage, AK USA. [Mckay, Christopher P.] NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA. RP Liu, L (reprint author), Univ Washington, Dept Earth & Space Sci, Seattle, WA 98195 USA. EM liul99@uw.edu FU National Science Foundation [0541054, 0636998, 1341680]; NASA Mars Science Laboratory via Malin Space Science Systems; Kenneth C. Robbins Graduate Fellowship; Joseph A. Endowed Vance Fellowship; Howard A. Coombs Scholarship FX This material is based upon work supported by the National Science Foundation under grants 0541054, 0636998, and 1341680 and NASA Mars Science Laboratory awarded via Malin Space Science Systems. Funding was also provided by Kenneth C. Robbins Graduate Fellowship, Joseph A. Endowed Vance Fellowship, and the Howard A. Coombs Scholarship. Data supporting this paper are available at http://gcmd.nasa.gov/r/d/[GCMD] UW_Dry_Valley_Datalogging or by contacting the corresponding author at liul99@uw.edu. We thank the Editors and reviewers for their comprehensive and insightful reviews. We are grateful to Antarctic Support Services, PHI, and our colleagues in Christchurch for superb logistical support in the Dry Valleys. NR 60 TC 1 Z9 1 U1 2 U2 4 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9003 EI 2169-9011 J9 J GEOPHYS RES-EARTH JI J. Geophys. Res.-Earth Surf. PD AUG PY 2015 VL 120 IS 8 BP 1596 EP 1610 DI 10.1002/2014JF003415 PG 15 WC Geosciences, Multidisciplinary SC Geology GA CU3YZ UT WOS:000363464000009 ER PT J AU Mallick, K Boegh, E Trebs, I Alfieri, JG Kustas, WP Prueger, JH Niyogi, D Das, N Drewry, DT Hoffmann, L Jarvis, AJ AF Mallick, Kaniska Boegh, Eva Trebs, Ivonne Alfieri, Joseph G. Kustas, William P. Prueger, John H. Niyogi, Dev Das, Narendra Drewry, Darren T. Hoffmann, Lucien Jarvis, Andrew J. TI Reintroducing radiometric surface temperature into the Penman-Monteith formulation SO WATER RESOURCES RESEARCH LA English DT Article ID CONVECTIVE BOUNDARY-LAYER; BEAREX08 FIELD CAMPAIGN; ENERGY-BALANCE FLUXES; SENSIBLE HEAT-FLUX; STOMATAL CONDUCTANCE; SOIL-MOISTURE; LAND-SURFACE; EVAPOTRANSPIRATION ALGORITHM; REGIONAL EVAPORATION; CANOPY TEMPERATURE AB Here we demonstrate a novel method to physically integrate radiometric surface temperature (T-R) into the Penman-Monteith (PM) formulation for estimating the terrestrial sensible and latent heat fluxes (H and lambda E) in the framework of a modified Surface Temperature Initiated Closure (STIC). It combines T-R data with standard energy balance closure models for deriving a hybrid scheme that does not require parameterization of the surface (or stomatal) and aerodynamic conductances (g(S) and g(B)). STIC is formed by the simultaneous solution of four state equations and it uses T-R as an additional data source for retrieving the "near surface'' moisture availability (M) and the Priestley-Taylor coefficient (alpha). The performance of STIC is tested using high-temporal resolution T-R observations collected from different international surface energy flux experiments in conjunction with corresponding net radiation (R-N), ground heat flux (G), air temperature (T-A), and relative humidity (R-H) measurements. A comparison of the STIC outputs with the eddy covariance measurements of lambda E and H revealed RMSDs of 7-16% and 40-74% in half-hourly lambda E and H estimates. These statistics were 5-13% and 10-44% in daily lambda E and H. The errors and uncertainties in both surface fluxes are comparable to the models that typically use land surface parameterizations for determining the unobserved components (g(S) and g(B)) of the surface energy balance models. However, the scheme is simpler, has the capabilities for generating spatially explicit surface energy fluxes and independent of submodels for boundary layer developments. C1 [Mallick, Kaniska; Trebs, Ivonne; Hoffmann, Lucien] Luxembourg Inst Sci & Technol, Dept Environm Res & Innovat, Belvaux, Luxembourg. [Boegh, Eva] Roskilde Univ, Dept Environm Social & Spatial Change, Roskilde, Denmark. [Alfieri, Joseph G.; Kustas, William P.] USDA ARS, Hydrol & Remote Sensing Lab, Beltsville, MD USA. [Prueger, John H.] USDA ARS, Natl Lab Agr & Environm, Ames, IA USA. [Niyogi, Dev] Purdue Univ, Dept Agron, W Lafayette, IN 47907 USA. [Niyogi, Dev] Purdue Univ, Dept Earth & Atmospher & Planetary Sci, W Lafayette, IN 47907 USA. [Das, Narendra; Drewry, Darren T.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Jarvis, Andrew J.] Univ Lancaster, Lancaster Environm Ctr, Lancaster, England. RP Mallick, K (reprint author), Luxembourg Inst Sci & Technol, Dept Environm Res & Innovat, Belvaux, Luxembourg. EM kaniska.mallick@gmail.com RI Trebs, Ivonne/L-9125-2013 FU NERC [NEE0191531]; Space Applications Centre, ISRO; Luxembourg Institute of Science and Technology FX The SMEX02 data for this paper are available at National Snow and Ice Data Centre (NSIDC), University of Colorado, Boulder (http://nsidc.org/data/amsr_validation/soil_moisture/smex02/) (Data set name: Meteorological, SMEX02 SMACEX Tower Meteorological/Flux Data: Iowa). The SAFARI data are available through Oak Ridge National Laboratory Distributed Active Archive Center (ftp://daac.ornl.gov/data/safari2k), Oak Ridge, Tennessee, US. FIFE data sets are available from Alan Betts (through http://alanbetts.com/research/). MERRA data are available through http://disc.sci.gsfc.nasa.gov/daac-bin/DataHoldings.pl. The TVDI data of Mallick et al. [2009] was a part of the project "Energy Water Balance Monitoring from Geostationary Platform for Agricultural Applications" funded by Space Applications Centre, ISRO. The research was conducted at the Luxembourg Institute of Science and Technology (previously Centre de Recherche Public-Gabriel Lippmann) under internally funded REMOD project. K.M. and A.J. was earlier supported by NERC grant (NEE0191531) during the initial development of the work. All the copyrights of 2015 are reserved. The authors declare no conflict of interest. USDA is an equal opportunity provider and employer. NR 82 TC 3 Z9 3 U1 2 U2 11 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0043-1397 EI 1944-7973 J9 WATER RESOUR RES JI Water Resour. Res. PD AUG PY 2015 VL 51 IS 8 BP 6214 EP 6243 DI 10.1002/2014WR016106 PG 30 WC Environmental Sciences; Limnology; Water Resources SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Water Resources GA CU3CZ UT WOS:000363402800020 ER PT J AU Sumata, H Kwok, R Gerdes, R Kauker, F Karcher, M AF Sumata, Hiroshi Kwok, Ronald Gerdes, Ruediger Kauker, Frank Karcher, Michael TI Uncertainty of Arctic summer ice drift assessed by high-resolution SAR data SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS LA English DT Article ID OCEAN-SEA-ICE; DATA ASSIMILATION; VOLUME PRODUCTION; MOTION; DEFORMATION; MODEL; TRACKING; SYSTEM; BUOY; OPTIMIZATION AB Time-space varying uncertainty maps of monthly mean Arctic summer ice drift are presented. To assess the error statistics of two low-resolution Eulerian ice drift products, we use high-resolution Lagrangian ice motion derived from synthetic aperture radar (SAR) imagery. The Lagrangian trajectories from the SAR data are converted to an Eulerian format to serve as reference for the error assessment of the Eulerian products. The statistical error associated with the conversion is suppressed to an acceptable level by applying a threshold for averaging. By using the SAR ice drift as a reference, we formulate the uncertainty of monthly mean ice drift as an empirical function of drift speed and ice concentration. The empirical functions are applied to derive uncertainty maps of Arctic ice drift fields. The estimated uncertainty maps reasonably capture an increase of uncertainty with the progress of summer melting season. The uncertainties range from 1.0 to 2.0 cm s(-1), which indicates that the low-resolution Eulerian products for summer seasons are of practical use for climate studies, model validation, and data assimilation, if their uncertainties are appropriately taken into account. C1 [Sumata, Hiroshi; Gerdes, Ruediger; Kauker, Frank; Karcher, Michael] Alfred Wegener Inst Polar & Marine Res, Sea Ice Phys, Bremerhaven, Germany. [Kwok, Ronald] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Gerdes, Ruediger] Jacobs Univ Bremen, D-28759 Bremen, Germany. [Kauker, Frank; Karcher, Michael] Ocean Atmosphere Syst, Hamburg, Germany. RP Sumata, H (reprint author), Alfred Wegener Inst Polar & Marine Res, Sea Ice Phys, Bremerhaven, Germany. EM hiroshi.sumata@awi.de RI Kwok, Ron/A-9762-2008 OI Kwok, Ron/0000-0003-4051-5896 FU Helmholtz Climate Initiative REKLIM (Regional Climate Change); Helmholtz Association of German research centers (HGF); European Commission [265863]; German Federal Ministry of Education and Research (BMBF) [0F0651 D]; NASA's MEaSUREs program FX Funding by the Helmholtz Climate Initiative REKLIM (Regional Climate Change), a joint research project of the Helmholtz Association of German research centers (HGF) is gratefully acknowledged. This work has partly been supported by the European Commission as part of the FP7 project ACCESS-Arctic Climate Change, Economy and Society (Project 265863). We also would like to express our gratitude toward the German Federal Ministry of Education and Research (BMBF) for the support of the project "RACE-Regional Atlantic Circulation and Global Change" (0F0651 D). The authors express their gratitude for all the data provider; The RGPS ice motion data available at JPL (http://rkwok.jpl.nasa.gov/radarsat/lagrangian.html) are produced with funding from NASA's MEaSUREs program. The Polar Pathfinder Daily 25 km EASE-Grid Sea Ice Motion vectors, Version 2, were provided from NSIDC (http://nsidc.org/data/nsidc-0116.html/), KIMURA ice drift data were provided by N. Kimura at the University of Tokyo, the ice concentration data were provided by OSI SAF (OSI-409: ftp://osisaf.met.no/preprocessed/ice/conc/v1/). The GFD-DENNOU library was used to draw the figures. The authors thank the anonymous reviewer for the constructive reviews. We also thank R. Ricker for his technical assistance and M. Thoma for a fruitful discussion. NR 60 TC 7 Z9 7 U1 2 U2 9 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 AUG PY 2015 VL 120 IS 8 BP 5285 EP 5301 DI 10.1002/2015JC010810 PG 17 WC Oceanography SC Oceanography GA CT2SI UT WOS:000362653600001 ER PT J AU Frank, D Foster, D Sou, IM Calantoni, J AF Frank, Donya Foster, Diane Sou, In Mei Calantoni, Joseph TI Incipient motion of surf zone sediments SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS LA English DT Article ID MIXED-SIZE SEDIMENT; OSCILLATORY FLOWS; BOUNDARY-LAYER; SHEAR-STRESS; WAVES; TRANSPORT AB Incipient motion experiments were conducted with natural gravel, acetate beads, and coarse-gravel-sized electronic grains called Smart Sediment Grains in a Small-Oscillatory Flow Tunnel. Measurements of fluid velocity were made using Particle Image Velocimetry. The strength of the fluid shear stresses and the pressure gradients were examined for a range of oscillatory flow conditions at the onset of motion of the sediment particles to determine which mechanism had induced particle motion. The three sediment types utilized in these experiments facilitated an assessment of the effects of sediment grain size diameter, shape, and density on incipient motion. Results suggested that the onset of sediment motion was dominated by the pressure gradients for flows with small orbital excursion amplitudes, by the shear stresses for flows with large orbital excursion amplitudes and by the combined effects for intermediate flows. The denser, angular gravel required greater free-stream accelerations to trigger sediment motion than the spherical, less dense acetate beads, and Smart Sediment Grains. A combined parameter for incipient motion that accounts for the simultaneous effects of both shear stresses and pressure gradients while depending on the static coefficient of friction and the packing concentration of the mobile bed layer was evaluated for accuracy using a range of sediment types. The results suggested that the combined parameter may be a better indicator of sediment mobilization under oscillatory flows than the typically assumed shear stress criterion. C1 [Frank, Donya] Univ New Hampshire, Formerly Ctr Ocean Engn, Durham, NH 03824 USA. [Frank, Donya; Sou, In Mei; Calantoni, Joseph] Stennis Space Ctr, Marine Geosci Div, Naval Res Lab, Stennis Space Ctr, MS USA. [Foster, Diane] Univ New Hampshire, Dept Mech Engn, Durham, NH 03824 USA. RP Frank, D (reprint author), Univ New Hampshire, Formerly Ctr Ocean Engn, Durham, NH 03824 USA. EM donya.frank.ctr.jm@nrlssc.navy.mil FU National Science Foundation [CBET-0933409, CBET-0933694, CMMI-1135026]; University of New Hampshire Graduate School; Office of Naval Research; National Research Council Research Associateship Program at the Naval Research Laboratory FX This work was sponsored (in part) by the National Science Foundation under grants CBET-0933409, CBET-0933694 and CMMI-1135026. Any opinions, findings, and conclusions or recommendations expressed in this material are those of the authors and do not necessarily reflect the views of the National Science Foundation. Donya Frank was partially supported by a Dissertation Year Fellowship from the University of New Hampshire Graduate School, and this work was conducted as a part of her PhD studies. In Mei Sou was supported as a postdoctoral fellow through the National Research Council Research Associateship Program at the Naval Research Laboratory. Joseph Calantoni was supported under base funding to the Naval Research Laboratory from the Office of Naval Research. The authors would like to acknowledge Pai Chou and his research teams at the University of California Irvine and National Tsing Hua University, Taiwan, for the development of the SSG electronics. The authors would also like to thank NRL staff members Timothy Kooney, Julian Simeonov, and David Dobson, as well as UNH graduate student Emily Carlson for their assistance with data collection and processing during the experiment. The data used to produce these results were collected with Particle Image Velocimetry techniques, which produce very large data sets and require several days to process with proprietary software. The authors would be willing to collaborate on an individual basis but are unable to make the data publicly available at this time. NR 33 TC 0 Z9 0 U1 3 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 AUG PY 2015 VL 120 IS 8 BP 5710 EP 5734 DI 10.1002/2014JC010424 PG 25 WC Oceanography SC Oceanography GA CT2SI UT WOS:000362653600025 ER PT J AU Okura, Y Plazas, AA May, M Tamagawa, T AF Okura, Y. Plazas, A. A. May, M. Tamagawa, T. TI Spurious shear induced by the tree rings of the LSST CCDs SO JOURNAL OF INSTRUMENTATION LA English DT Article DE Image processing; Photon detectors for UV, visible and IR photons (solid-state) (PIN diodes, APDs, Si-PMTs, G-APDs, CCDs, EBCCDs, EMCCDs etc) ID WEAK LENSING SURVEYS; DARK ENERGY SURVEY; CALIBRATION AB We present an analysis of the impact of the tree rings seen in the candidate sensors of the Large Synoptic Survey Telescope (LSST) on galaxy-shape measurements. The tree rings are a consequence of transverse electric fields caused by circularly symmetric impurity gradients in the silicon of the sensors. They effectively modify the pixel area and shift the photogenerated charge around, displacing the observed photon positions. The displacement distribution generates distortions that cause spurious shears correlated with the tree-rings patterns, potentially biasing cosmic shear measurements. In this paper we quantify the amplitude of the spurious shear caused by the tree rings on the LSST candidate sensors, and calculate its 2-point correlation function. We find that 2-point correlation function of the spurious shear on an area equivalent to the LSST field of view is order of about 10 13, providing a negligible contribution to the 2-point correlation of the cosmic shear signal. Additional work is underway, and the final results and analysis will be published elsewhere (Okura et al. (2015), in prep.) C1 [Okura, Y.; Tamagawa, T.] RIKEN, Wako, Saitama 3510198, Japan. [Okura, Y.] Brookhaven Natl Lab, Dept Phys, RIKEN BNL Res Ctr, Upton, NY 11792 USA. [Plazas, A. A.; May, M.] Brookhaven Natl Lab, Dept Phys, Upton, NY 11792 USA. [Plazas, A. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Okura, Y (reprint author), RIKEN, 2-1 Hirosawa, Wako, Saitama 3510198, Japan. EM yuki.okura@riken.jp FU U.S. Department of Energy [DE-AC02-98CH10886, DE-SC0012704]; JPL; NASA FX We thank G. Bernstein and P. O'Connor for useful comments and discussions. This work was supported in part by the U.S. Department of Energy under Contract No. DE-AC02-98CH10886 and Contract No. DE-SC0012704. AAP is also supported by JPL, which is run under a contract for NASA by Caltech. NR 14 TC 1 Z9 1 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 1748-0221 J9 J INSTRUM JI J. Instrum. PD AUG PY 2015 VL 10 AR C08010 DI 10.1088/1748-0221/10/08/C08010 PG 10 WC Instruments & Instrumentation SC Instruments & Instrumentation GA CS8ZP UT WOS:000362378700010 ER PT J AU Haines, BJ Bar-Sever, YE Bertiger, WI Desai, SD Harvey, N Sibois, AE Weiss, JP AF Haines, Bruce J. Bar-Sever, Yoaz E. Bertiger, Willy I. Desai, Shailen D. Harvey, Nate Sibois, Aurore E. Weiss, Jan P. TI Realizing a terrestrial reference frame using the Global Positioning System SO JOURNAL OF GEOPHYSICAL RESEARCH-SOLID EARTH LA English DT Article DE reference frames; GPS; geocenter motion ID PHASE CENTER VARIATIONS; SATELLITE ANTENNA; ORBIT DETERMINATION; GPS MEASUREMENTS; EARTH; MODEL; ACCURACY; IGS; TOPEX/POSEIDON; CALIBRATION AB We describe a terrestrial reference frame (TRF) realization based on Global Positioning System (GPS) data alone. Our approach rests on a highly dynamic, long-arc (9 day) estimation strategy and on GPS satellite antenna calibrations derived from Gravity Recovery and Climate Experiment and TOPEX/Poseidon low Earth orbit receiver GPS data. Based on nearly 17 years of data (1997-2013), our solution for scale rate agrees with International Terrestrial Reference Frame (ITRF)2008 to 0.03 ppbyr(-1), and our solution for 3-D origin rate agrees with ITRF2008 to 0.4 mmyr(-1). Absolute scale differs by 1.1ppb (7 mm at the Earth's surface) and 3-D origin by 8 mm. These differences lie within estimated error levels for the contemporary TRF. C1 [Haines, Bruce J.; Bar-Sever, Yoaz E.; Bertiger, Willy I.; Desai, Shailen D.; Harvey, Nate; Sibois, Aurore E.; Weiss, Jan P.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. RP Haines, BJ (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. EM Bruce.J.Haines@jpl.nasa.gov RI Sibois, Aurore/I-6415-2016 OI Sibois, Aurore/0000-0003-1212-3940 FU National Aeronautics and Space Administration FX The work described in this paper was performed at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. We thank our JPL colleagues Charles Dunn and Larry Young for providing the calibrations from the JPL outdoor test range for both the TOPEX/Poseidon and TurboRogue antennas, George Purcell for providing the anechoic calibrations for the GRACE antennas, and Sung Byun for producing the simulated multipath estimates for GRACE. We are grateful for fruitful discussions with our JPL collaborators, especially Da Kuang, Mike Heflin, and Xiaoping Wu, the latter of whom kindly provided estimates of annual geocenter motion from his inverse method. We also thank Gerhard Wubbena and Martin Schmitz of geo++ for providing data from the robotic field calibration of the GPS Block IIA antenna assembly. We are grateful to Zuheir Altamimi and an anonymous reviewer for their valuable comments on this manuscript. The GPS tracking data from both ground stations and low Earth orbiters are available from http://cddis.gsfc.nasa.gov, while the JPL products for the GPS constellation are available at ftp://sideshow.jpl.nasa.gov/pub/JPL_GPS_Products. High-level data products underlying all the plots in the paper are available on request from author B.H. NR 123 TC 2 Z9 2 U1 2 U2 9 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9313 EI 2169-9356 J9 J GEOPHYS RES-SOL EA JI J. Geophys. Res.-Solid Earth PD AUG PY 2015 VL 120 IS 8 BP 5911 EP 5939 DI 10.1002/2015JB012225 PG 29 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA CS6WN UT WOS:000362224100027 ER PT J AU Posch, JL Engebretson, MJ Olson, CN Thaller, SA Breneman, AW Wygant, JR Boardsen, SA Kletzing, CA Smith, CW Reeves, GD AF Posch, J. L. Engebretson, M. J. Olson, C. N. Thaller, S. A. Breneman, A. W. Wygant, J. R. Boardsen, S. A. Kletzing, C. A. Smith, C. W. Reeves, G. D. TI Low-harmonic magnetosonic waves observed by the Van Allen Probes SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article DE magnetosonic waves; equatorial noise; waves in plasmas; inner magnetosphere ID EQUATORIAL NOISE; CLUSTER SPACECRAFT; MAGNETIC EQUATOR; ULF WAVES; MAGNETOSPHERE; DISTRIBUTIONS; EXCITATION; PULSATIONS; FREQUENCY; PROTON AB Purely compressional electromagnetic waves (fast magnetosonic waves), generated at multiple harmonics of the local proton gyrofrequency, have been observed by various types of satellite instruments (fluxgate and search coil magnetometers and electric field sensors), but most recent studies have used data from search coil sensors, and many have been restricted to high harmonics. We report here on a survey of low-harmonic waves, based on electric and magnetic field data from the Electric Fields and Waves double probe and Electric and Magnetic Field Instrument Suite and Integrated Science fluxgate magnetometer instruments, respectively, on the Van Allen Probes spacecraft during its first full precession through all local times, from 1 October 2012 to 13 July 2014. These waves were observed both inside and outside the plasmapause (PP), at L shells from 2.4 to similar to 6 (the spacecraft apogee), and in regions with plasma number densities ranging from 10 to >1000cm(-3). Consistent with earlier studies, wave occurrence was sharply peaked near the magnetic equator. Waves appeared at all local times but were more common from noon to dusk, and often occurred within 3h after substorm injections. Outside the PP occurrence maximized broadly across noon, and inside the PP occurrence maximized in the dusk sector, in an extended plasmasphere. We confirm recent ray-tracing studies showing wave refraction and/or reflection at PP-like boundaries. Comparison with waveform receiver data indicates that in some cases these low-harmonic magnetosonic wave events occurred independently of higher-harmonic waves; this indicates the importance of including this population in future studies of radiation belt dynamics. C1 [Posch, J. L.; Engebretson, M. J.; Olson, C. N.] Augsburg Coll, Dept Phys, Minneapolis, MN 55454 USA. [Thaller, S. A.; Breneman, A. W.; Wygant, J. R.] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA. [Boardsen, S. A.] Univ Maryland, Goddard Planetary Heliophys Inst, Baltimore, MD 21201 USA. [Boardsen, S. A.] NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Greenbelt, MD 20771 USA. [Kletzing, C. A.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. [Smith, C. W.] Univ New Hampshire, Ctr Space Sci, Durham, NH 03824 USA. [Reeves, G. D.] Los Alamos Natl Lab, Space Sci & Applicat Grp, Los Alamos, NM USA. RP Posch, JL (reprint author), Augsburg Coll, Dept Phys, Minneapolis, MN 55454 USA. EM posch@augsburg.edu RI Reeves, Geoffrey/E-8101-2011; OI Reeves, Geoffrey/0000-0002-7985-8098; Kletzing, Craig/0000-0002-4136-3348 FU NSF [AGS-1202267, PLR-1341493]; NASA [NAS5-01072] FX We thank both referees for suggestions that greatly improved this manuscript. We thank Augsburg undergraduates Joseph Perrin and Sadie Tetrick for their help in identifying wave events, and Eun-Hwa Kim and Jay Johnson of Princeton University, Richard Horne of the British Antarctic Survey, and Brian Anderson of JHU/APL for their helpful discussions. We acknowledge the use of NASA/GSFC's Space Physics Data Facility's OMNIWeb and CDAWeb data. The EMFISIS data from the Van Allen Probes is available at http://emfisis.physics.uiowa.edu/. The Van Allen Probes EFW data is available at: http://www.space.umn.edu/missions/rbspefw-home-university-of-minnesota/. Research at Augsburg College was supported by NSF grants AGS-1202267 and PLR-1341493, and research at the University of Minnesota, University of Iowa, University of New Hampshire, and Los Alamos National Laboratory was supported by NASA prime contract NAS5-01072 to the Johns Hopkins University Applied Physics Laboratory NR 35 TC 11 Z9 11 U1 0 U2 3 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD AUG PY 2015 VL 120 IS 8 BP 6230 EP 6257 DI 10.1002/2015JA021179 PG 28 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CS5NP UT WOS:000362125300015 ER PT J AU Yue, C Wang, CP Nishimura, Y Murphy, KR Xing, XY Lyons, L Henderson, M Angelopoulos, V Lui, ATY Nagai, T AF Yue, Chao Wang, Chih-Ping Nishimura, Yukitoshi Murphy, Kyle R. Xing, Xiaoyan Lyons, Larry Henderson, Michael Angelopoulos, Vassilis Lui, A. T. Y. Nagai, Tsugunobu TI Empirical modeling of 3-D force-balanced plasma and magnetic field structures during substorm growth phase SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article DE force-balanced magnetic field modeling; substorm growth phase modeling; field-aligned current; ballooning instability; substorm onset location ID BALLOONING INSTABILITY; MAGNETOMETER DATA; CURRENT SHEET; ONSET; PRESSURE; CURRENTS; MAGNETOSPHERE; SCATTERING; EXPANSION; TAIL AB Accurate evaluation of the physical processes during the substorm growth phase, including formation of field-aligned currents (FACs), isotropization by current sheet scattering, instabilities, and ionosphere-magnetosphere connection, relies on knowing the realistic three-dimensional (3-D) magnetic field configuration, which cannot be reliably provided by current available empirical models. We have established a 3-D substorm growth phase magnetic field model, which is uniquely constructed from empirical plasma sheet pressures under the constraint of force balance. We investigated the evolution of model pressure and magnetic field responding to increasing energy loading and their configurations under different solar wind dynamic pressure (P-SW) and sunspot number. Our model reproduces the typical growth phase evolution signatures: plasma pressure increases, magnetic field lines become more stretched, current sheet becomes thinner, and the Region 2 FACs are enhanced. The model magnetic fields agree quantitatively well with observed fields. The magnetic field is substantially more stretched under higher P-SW, while the dependence on sunspot number is nonlinear and less substantial. By applying our modeling to a substorm event, we found that (1) the equatorward movement of proton aurora during the growth phase is mainly due to continuous stretching of magnetic field lines, (2) the ballooning instability is more favorable during late growth phase around midnight tail where there is a localized plasma beta peak, and (3) the equatorial mapping of the breakup auroral arc is at X similar to-14 R-E near midnight, coinciding with the location of the maximum growth rate for the ballooning instability. C1 [Yue, Chao; Wang, Chih-Ping; Nishimura, Yukitoshi; Xing, Xiaoyan; Lyons, Larry] Univ Calif Los Angeles, Dept Atmospher & Ocean Sci, Los Angeles, CA 90095 USA. [Murphy, Kyle R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Henderson, Michael] Los Alamos Natl Lab, Space Sci & Applicat, Los Alamos, NM USA. [Angelopoulos, Vassilis] Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90024 USA. [Lui, A. T. Y.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA. [Nagai, Tsugunobu] Tokyo Inst Technol, Earth & Planetary Sci, Tokyo 152, Japan. RP Yue, C (reprint author), Univ Calif Los Angeles, Dept Atmospher & Ocean Sci, Los Angeles, CA 90095 USA. EM yuechao@atmos.ucla.edu RI Yue, Chao/C-2535-2015; OI Yue, Chao/0000-0001-9720-5210; Henderson, Michael/0000-0003-4975-9029 FU NASA [NNX11AJ12G, NNX08A135G]; NSF [ATM-1003595]; IGPPS Program at Los Alamos National Laboratory FX The work by C. Yue, C.-P. Wang, and L.R. Lyons at UCLA has been supported by NASA grants NNX11AJ12G and NNX08A135G, NSF grant ATM-1003595, and IGPPS Program at Los Alamos National Laboratory. We also acknowledge James Weygand (University of California, Los Angeles, USA) for the very helpful discussion of the observed FACs. All THEMIS data are from THEMIS official website (http://themis.ssl.berkeley.edu/data_files.shtml). All Geotail data are from the Institute of Space and Astronautical Science (ISAS)/Japan Aerospace Exploration Agency through the Data Archives and Transmission System of ISAS (http://www.darts.isas.jaxa.jp/). NR 46 TC 1 Z9 1 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 AUG PY 2015 VL 120 IS 8 BP 6496 EP 6513 DI 10.1002/2015JA021226 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CS5NP UT WOS:000362125300033 ER PT J AU Dixon, P MacDonald, EA Funsten, HO Glocer, A Grande, M Kletzing, C Larsen, BA Reeves, G Skoug, RM Spence, H Thomsen, MF AF Dixon, P. MacDonald, E. A. Funsten, H. O. Glocer, A. Grande, M. Kletzing, C. Larsen, B. A. Reeves, G. Skoug, R. M. Spence, H. Thomsen, M. F. TI Multipoint observations of the open-closed field line boundary as observed by the Van Allen Probes and geostationary satellites during the 14 November 2012 geomagnetic storm SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article DE Magnetosphere; Lobes; Open; closed field line boundary; Modelling ID POLAR-CAP BOUNDARY; GEOSYNCHRONOUS ORBIT; ENERGETIC PARTICLES; MORNING SECTOR; PLASMA; DYNAMICS; MODEL; LOBE; MAGNETOSPHERE; IONOSPHERE AB The twin Van Allen Probes spacecraft witnessed a series of lobe encounters between 0200 and 0515 UT on 14 November 2012. Although lobe entry had been observed previously by other spacecraft, the two Van Allen Probe spacecraft allow us to observe the motion of the boundary for the first time. Moreover, this event is unique in that it consists of a series of six quasi-periodic lobe entries. The events occurred on the dawn flank between 4 and 6.6 local time and at altitudes between 5.6 and 6.2 RE. During the events Dst dropped to less than -100nT with the IMF being strongly southward (B-z=-15nT) and eastward (B-y=20 nT). Observations by LANL-GEO spacecraft at geosynchronous orbit also show lobe encounters on the dawn and dusk flanks. The two spacecraft configuration provides strong evidence that these periodic entries into the lobe are the result of local expansions of the OCB propagating from the tail and passing over the Van Allen Probes. Examination of pitch angle binned data from the HOPE instrument shows spatially large, accelerated ion structures occurring near simultaneously at both spacecraft, with the presence of oxygen indicating that they have an ionospheric source. The outflows are dispersed in energy and are detected when the spacecraft are on both open and closed field lines. These events provide a chance to examine the global magnetic field topology in detail, as well as smaller-scale spatial and temporal characteristics of the OCB, allowing us to constrain the position of the open/closed field line boundary and compare it to a global MHD model using a novel method. This technique shows that the model can reproduce a periodic approach and retreat of the OCB from the spacecraft but can overestimate its distance by as much as 3 R-E. The model appears to simulate the dynamic processes that cause the spacecraft to encounter the lobe but incorrectly maps the overall topology of the magnetosphere during these extreme conditions. C1 [Dixon, P.; Grande, M.] Aberystwyth Univ, Dept Phys, Aberystwyth, Dyfed, Wales. [MacDonald, E. A.; Glocer, A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Funsten, H. O.; Larsen, B. A.; Reeves, G.; Skoug, R. M.; Thomsen, M. F.] Los Alamos Natl Lab, Los Alamos, NM USA. [Kletzing, C.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. [Spence, H.] Univ New Hampshire, Dept Phys, Durham, NH 03824 USA. RP Dixon, P (reprint author), Aberystwyth Univ, Dept Phys, Aberystwyth, Dyfed, Wales. EM pjd9@aber.ac.uk RI Reeves, Geoffrey/E-8101-2011; Grande, Manuel/C-2242-2013; OI Reeves, Geoffrey/0000-0002-7985-8098; Grande, Manuel/0000-0002-2233-2618; Kletzing, Craig/0000-0002-4136-3348; Funsten, Herbert/0000-0002-6817-1039 FU NASA; Science and Technology Funding Council (STFC), UK FX ACE and OMNI teams provided solar wind data through the Space Physics Data Facility of NASA Goddard Space Flight Center. The SYM-H indices are provided by Kyoto University World Data Center for Geomagnetism. The authors would like to acknowledge useful discussions with S. Zou, K.-J. Hwang, and J. Fennell. This work was supported by the NASA Van Allen Probes RBSP-ECT project. Work at Los Alamos was performed under the auspices of the U.S. Department of Energy. Part of the research in this paper was supported by NASA Van Allen Probes mission funding. The work of P. Dixon was supported by a studentship from the Science and Technology Funding Council (STFC), UK. HOPE data are available from the RBSP-ECT website (http://www.rbsp-ect.lanl.gov/science/DataDirectories.php) with the following data sets used in this work: Differential plasma fluxes-rbspb_re-l02_ect-hope-sci-L2_20121114_v4.0.0.cdf, rbspb_rel02_ect-hope-sci-L2_20121114_v4.0.0.cdf; pitch angle binned fluxes-rbspa_rel02_ect-hope-PA-L3_20121114_v5.0.0.cdf, rbspb_rel02_ect-hope-PA-L3_20121114_v5.0.0.cdf; spacecraft ephemeris data-rbspa_def_MagEphem_TS04D_20121113_v2.1.0.txt, rbspa_def_MagEphem_TS04D_20121113_v2.1.0.txt. EMFISIS data are available from http://emfisis.physics.uiowa.edu/data/index with the rbsp-a_magnetometer_4sec-gsm_emfi-sis-L3_20121114_v1.3.2.cdf and rbspb_magnetometer_4sec-gsm_emfisis-L3_20121114_v1.3.2.cdf data sets used in this work. Data from the SOPA instrument on the LANL-GEO spacecraft are available on request from Geoff Reeves, LANL, US-reeves@lanl.gov. For CRCM + BATS-R-US data used in this work, contact Alex Glocer-alex.glocer-1@nasa.gov. NR 41 TC 2 Z9 2 U1 0 U2 3 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD AUG PY 2015 VL 120 IS 8 BP 6596 EP 6613 DI 10.1002/2014JA020883 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CS5NP UT WOS:000362125300040 ER PT J AU Gershman, DJ Dorelli, JC F-Vinas, A Pollock, CJ AF Gershman, Daniel J. Dorelli, John C. F-Vinas, Adolfo Pollock, Craig J. TI The calculation of moment uncertainties from velocity distribution functions with random errors SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article DE particle instrumentation; plasma moments; velocity distribution function; random errors ID IN-FLIGHT CALIBRATION; CLUSTER; MAGNETOSHEATH; SPECTROMETER; INSTRUMENT; SATELLITE; ELECTRONS; PLASMAS; PEACE AB Instrumentation that detects individual plasma particles is susceptible to random counting errors. These errors propagate into the calculations of moments of measured particle velocity distribution functions. Although rules of thumb exist for the effects of random errors on the calculation of lower order moments (e.g., density, velocity, and temperature) of Maxwell-Boltzmann distributions, they do not generally apply to nonthermal distributions or to higher-order moments. To date, such errors have only been estimated using brute force Monte Carlo techniques, i.e., repeated (similar to 50) samplings of distribution functions. Here we present a mathematical formalism for analytically obtaining uncertainty estimates of plasma moments due to random errors either measured in situ by instruments or synthesized by particle simulations. Our uncertainty estimates precisely match the statistical variation of simulated plasma moments and carry the computational cost equivalent of only similar to 15 Monte Carlo samplings. In addition, we provide the means to calculate a covariance matrix that can be reported along with typical plasma moments. This matrix enables the propagation of statistical errors into arbitrary coordinate systems or functions of plasma moments without the need to reanalyze full distribution functions. Our methodology, which is applied to electron data from Plasma Electron and Current Experiment on the Cluster spacecraft as an example, is relevant to both existing and future data sets and requires only instrument-measured counts and phase space densities reported for a set of calibrated energy-angle targets. C1 [Gershman, Daniel J.; Dorelli, John C.; F-Vinas, Adolfo; Pollock, Craig J.] NASA, Goddard Space Flight Ctr, Geospace Phys Lab, Greenbelt, MD 20771 USA. RP Gershman, DJ (reprint author), NASA, Goddard Space Flight Ctr, Geospace Phys Lab, Greenbelt, MD 20771 USA. EM daniel.j.gershman@nasa.gov FU Magnetospheric Multiscale Mission [WBS 943396.05.03.02.10.01] FX The high-resolution electron data used in this work were obtained from Mullard Space Science Laboratory. Cluster/PEACE data were obtained from the open data repository via the UDF software data analysis package, and the magnetic field data were obtained from the Cluster/FGM prime parameters. The IDL software used to generate uncertainty estimates for velocity moments is included online as supporting information. The numerical data generated for this paper will be made available upon request. The authors wish to thank the members of the FPI ground operations and science team for their feedback and support. This work was supported by the Magnetospheric Multiscale Mission under WBS 943396.05.03.02.10.01 for the Fast Plasma Instrument. D.J.G. is supported by an appointment to the NASA Postdoctoral Program at Goddard Space Flight Center, administered by Oak Ridge Associated Universities. NR 33 TC 4 Z9 4 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 AUG PY 2015 VL 120 IS 8 BP 6633 EP 6645 DI 10.1002/2014JA020775 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CS5NP UT WOS:000362125300043 ER PT J AU Kim, J Oh, H Lee, J Baek, CK Meyyappan, M Lee, JS AF Kim, Jungsik Oh, Hyeongwan Lee, Junyoung Baek, Chang-Ki Meyyappan, M. Lee, Jeong-Soo TI Three-dimensional simulation of threshold voltage variations due to an oblique single grain boundary in sub-40nm polysilicon nanowire FETs SO SEMICONDUCTOR SCIENCE AND TECHNOLOGY LA English DT Article DE polysilicon channel; grain boundary; TCAD simulation ID THIN-FILM TRANSISTORS; CHANNEL AB We perform a comparative study of the threshold voltage (V-th) variation between inversion-mode and junctionless nanowire devices with oblique single grain boundary (o-SGB) in a sub-40 nm poly-silicon (Poly-Si) channel using 3D simulation. The V-th variation due to the o-SGB becomes significant as the devices scale down to 20 nm where the o-SGB can fully affect the whole channel potential. In addition, due to relatively less flat energy band in the channel, the junctionless Poly-Si nanowire devices show larger V-th variation compared with the inversion-mode devices. C1 [Kim, Jungsik] Pohang Univ Sci & Technol POSTECH, Div IT Convergence Engn, Pohang 790784, South Korea. [Oh, Hyeongwan; Lee, Junyoung; Lee, Jeong-Soo] Pohang Univ Sci & Technol POSTECH, Dept Elect Engn, Pohang 790784, South Korea. [Baek, Chang-Ki] Pohang Univ Sci & Technol POSTECH, Dept Creat IT Engn, Pohang 790784, South Korea. [Baek, Chang-Ki] Pohang Univ Sci & Technol POSTECH, Future IT Innovat Lab, Pohang 790784, South Korea. [Meyyappan, M.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Kim, J (reprint author), Pohang Univ Sci & Technol POSTECH, Div IT Convergence Engn, Pohang 790784, South Korea. EM ljs6951@postech.ac.kr FU Center for Advanced Soft-Electronics - Ministry of Science, ICT and Future Planning [2014M3A6A5060945]; National Research Foundation of Korea (NRF) - Korean government (MSIP) [2013R1A1A2007094]; IT Consilience Creative Program [NIPA-2014-H0201-14-1001]; POSTECH; Samsung Electronics Co; Samsung Display Co. FX This work was supported by the Center for Advanced Soft-Electronics funded by the Ministry of Science, ICT and Future Planning as Global Frontier Project (2014M3A6A5060945), a National Research Foundation of Korea (NRF) grant funded by the Korean government (MSIP) (No. 2013R1A1A2007094), the 'IT Consilience Creative Program' (NIPA-2014-H0201-14-1001) supervised by the National IT Industry Promotion Agency, Korea, the Semiconductor Industry Collaborative Project between POSTECH and Samsung Electronics Co, and the Semiconductor Industry Collaborative Project between POSTECH and Samsung Display Co. The TCAD Sentaurus simulator was provided by the Electronic Design Automation (EDA) tool program of IC Design Education Center (IDEC) in Korea. NR 17 TC 0 Z9 0 U1 1 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0268-1242 EI 1361-6641 J9 SEMICOND SCI TECH JI Semicond. Sci. Technol. PD AUG PY 2015 VL 30 IS 8 AR 085015 DI 10.1088/0268-1242/30/8/085015 PG 8 WC Engineering, Electrical & Electronic; Materials Science, Multidisciplinary; Physics, Condensed Matter SC Engineering; Materials Science; Physics GA CS7OI UT WOS:000362272600017 ER PT J AU Lepping, RP Wu, CC Berdichevsky, DB Szabo, A AF Lepping, R. P. Wu, C. -C. Berdichevsky, D. B. Szabo, A. TI Wind Magnetic Clouds for 2010-aEuro parts per thousand 2012: Model Parameter Fittings, Associated Shock Waves, and Comparisons to Earlier Periods SO SOLAR PHYSICS LA English DT Article DE Magnetic cloud; Interplanetary shock; Magnetic cloud-like structure; Model ID CORONAL MASS EJECTIONS; 23RD SOLAR MINIMUM; 1 AU; EMPIRICAL RECONSTRUCTION; INTERACTION REGION; INNER HELIOSPHERE; COMPLEX EJECTA; FLUX ROPES; INTERPLANETARY; EARTH AB We fitted the parameters of magnetic clouds (MCs) as identified in the Wind spacecraft data from early 2010 to the end of 2012 using the model of Lepping, Jones, and Burlaga (J. Geophys. Res. 95, 1195, 1990). The interval contains 48 MCs and 39 magnetic cloud-like (MCL) events. This work is a continuation of MC model fittings of the earlier Wind sets, including those in a recent publication, which covers 2007 to 2009. This period (2010 -aEuro parts per thousand 2012) mainly covers the maximum portion of Solar Cycle 24. Between the previous and current interval, we document 5.7 years of MCs observations. For this interval, the occurrence frequency of MCs markedly increased in the last third of the time. In addition, over approximately the last six years, the MC type (i.e. the profile of the magnetic-field direction within an MC, such as North-to-South, South-to-North, all South) dramatically evolved to mainly North-to-South types when compared to earlier years. Furthermore, this evolution of MC type is consistent with global solar magnetic-field changes predicted by Bothmer and Rust (Coronal Mass Ejections, 139, 1997). Model fit parameters for the MCs are listed for 2010 -aEuro parts per thousand 2012. For the 5.7 year interval, the observed MCs are found to be slower, weaker in estimated axial magnetic-field intensity, and shorter in duration than those of the earlier 12.3 years, yielding much lower axial magnetic-field fluxes. For about the first half of this 5.7 year period, i.e. up to the end of 2009, there were very few associated MC-driven shock waves (distinctly fewer than the long-term average of about 50 % of MCs). But since 2010, such driven shocks have increased markedly, reflecting similar statistics as the long-term averages. We estimate that 56 % of the total observed MCs have upstream shocks when the full interval of 1995 -aEuro parts per thousand 2012 is considered. However, only 28 % of the total number of MCLs have driven shocks over the same period. Some interplanetary shocks during the 2010 -aEuro parts per thousand 2012 interval are seen to apparently occur without an obvious MC-driver, probably indicating an encounter with a distant flank of a MC-driven shock. Some of these may be driven by a different kind of structure, however. C1 [Lepping, R. P.; Szabo, A.] NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Greenbelt, MD 20771 USA. [Wu, C. -C.] Naval Res Lab, Washington, DC 20375 USA. [Berdichevsky, D. B.] Univ Dist Columbia, Dept Elect & Comp Engn, Washington, DC 20008 USA. RP Lepping, RP (reprint author), NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Greenbelt, MD 20771 USA. EM Ronald.P.Lepping@gmail.com NR 50 TC 6 Z9 6 U1 0 U2 1 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-0938 EI 1573-093X J9 SOL PHYS JI Sol. Phys. PD AUG PY 2015 VL 290 IS 8 BP 2265 EP 2290 DI 10.1007/s11207-015-0755-3 PG 26 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CS3WY UT WOS:000362007300007 ER PT J AU Kirnosov, V Chang, LC Pulkkinen, A AF Kirnosov, Vladimir Chang, Lin-Ching Pulkkinen, Antti TI Automatic CME front edge detection from STEREO white-light coronagraph images SO SPACE WEATHER-THE INTERNATIONAL JOURNAL OF RESEARCH AND APPLICATIONS LA English DT Article ID 29-31 OCTOBER 2003; MASS EJECTIONS; CATALOG; PROPAGATION; TRACKING AB The coronagraph images captured by a Solar Terrestrial Relations Observatory (STEREO) Ahead/Behind (A/B) spacecraft allow tracking of a coronal mass ejection (CME) from two different viewpoints and reconstructing its propagation in three-dimensional space. The reconstruction can be done using a triangulation technique that requires a CME front edge location. There are currently no robust automatic CME front edge detection methods that can be integrated with the triangulation technique. In this paper, we propose a novel automatic method to detect the front edge of the CME using STEREO coronagraph 2 red-colored Red, Green, Blue color model images. Our method consists of two modules: preprocessing and classification. The preprocessing module decomposes each coronagraph image into its three channels and uses only the red channel image for CME segmentation. The output of the preprocessing module is a set of segmented running-difference binary images which is fed into the classification module. These images are then transformed into polar coordinates followed by CME front edge detection based on the distance that CME travels in the field of view. The proposed method was validated against a manual method using total 56 CME events, 28 from STEREO A and 28 from STEREO B, captured in the period from 1 January 2008 to 16 August 2009. The results show that the proposed method is effective for CME front edge detection. The proposed method is useful in quantitative CME processing and analysis and will be immediately applicable to assist automatic triangulation method for real-time space weather forecasting. C1 [Kirnosov, Vladimir; Chang, Lin-Ching] Catholic Univ Amer, Elect Engn & Comp Sci Dept, Washington, DC 20064 USA. [Pulkkinen, Antti] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA. RP Kirnosov, V (reprint author), Catholic Univ Amer, Elect Engn & Comp Sci Dept, Washington, DC 20064 USA. EM 57kirnosov@cardinalmail.cua.edu NR 33 TC 1 Z9 1 U1 1 U2 3 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 AUG PY 2015 VL 13 IS 8 BP 469 EP 483 DI 10.1002/2015SW001190 PG 15 WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences GA CS6QC UT WOS:000362204800006 ER PT J AU Khan, R Stanek, KZ Kochanek, CS Sonneborn, G AF Khan, Rubab Stanek, K. Z. Kochanek, C. S. Sonneborn, G. TI SPITZER POINT-SOURCE CATALOGS OF similar to 300,000 STARS IN SEVEN NEARBY GALAXIES SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE catalogs; infrared: stars; surveys; techniques: photometric ID SMALL-MAGELLANIC-CLOUD; ARRAY CAMERA IRAC; ETA CAR ANALOGS; SPACE-TELESCOPE; INFRARED PHOTOMETRY; ARAUCARIA-PROJECT; CEPHEID VARIABLES; DISTANCE; M33; PROGENITORS AB We present Spitzer IRAC 3.6-8 mu m and Multiband Imaging Photometer 24 mu m point-source catalogs for seven galaxies: NGC 6822, M33, NGC 300, NGC 2403, M81, NGC 0247, and NGC 7793. The catalogs contain a total of similar to 300,000 sources and were created by dual-band selection of sources with > 3 sigma detections at both 3.6 and 4.5 mu m. The source lists become significantly incomplete near m(3.6) = m(4.5) similar or equal to 18. We complement the 3.6 and 4.5 mu m fluxes with 5.8, 8.0, and 24 mu m fluxes or 3 sigma upper limits using a combination of PSF and aperture photometry. This catalog is a resource as an archive for studying mid-infrared transients and for planning observations with the James Webb Space Telescope. C1 [Khan, Rubab] Oak Ridge Associated Univ, NASA Postdoctoral Program, Oak Ridge, TN 37831 USA. [Khan, Rubab; Sonneborn, G.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Stanek, K. Z.; Kochanek, C. S.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Stanek, K. Z.; Kochanek, C. S.] Ohio State Univ, Ctr Cosmol & AstroParticle Phys, Columbus, OH 43210 USA. RP Khan, R (reprint author), Oak Ridge Associated Univ, NASA Postdoctoral Program, POB 117,MS 36, Oak Ridge, TN 37831 USA. EM rubab.m.khan@nasa.gov; kstanek@astronomy.ohio-state.edu; ckochanek@astronomy.ohio-state.edu; george.sonneborn-1@nasa.gov FU National Aeronautics and Space Administration (NASA); JWST Fellowship FX We thank the referee for providing helpful feedback. 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 the National Aeronautics and Space Administration (NASA). We extend our gratitude to the SINGS Legacy Survey and the LVL Survey for making their data publicly available. R.K. is supported through a JWST Fellowship hosted by the Goddard Space Flight Center and awarded as part of the NASA Postdoctoral Program operated by the Oak Ridge Associated Universities on behalf of NASA. NR 32 TC 4 Z9 4 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 EI 1538-4365 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD AUG PY 2015 VL 219 IS 2 AR 42 DI 10.1088/0067-0049/219/2/42 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CS2CY UT WOS:000361876600028 ER PT J AU Li, HX Li, D Qian, L Xu, D Goldsmith, PF Noriega-Crespo, A Wu, YF Song, YZ Nan, RD AF Li, Huixian Li, Di Qian, Lei Xu, Duo Goldsmith, Paul F. Noriega-Crespo, Alberto Wu, Yuefang Song, Yuzhe Nan, Rendong TI OUTFLOWS AND BUBBLES IN TAURUS: STAR-FORMATION FEEDBACK SUFFICIENT TO MAINTAIN TURBULENCE SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE ISM: bubbles; ISM: individual objects (Taurus); ISM: jets and outflows; ISM: kinematics and dynamics; surveys; turbulence ID VELOCITY MOLECULAR GAS; YOUNG STELLAR OBJECTS; SCALE STRUCTURE; GALACTIC DISK; DENSE CORES; CLOUD CORE; DRIVEN; CANDIDATES; PERSEUS; PROTOSTARS AB We have identified outflows and bubbles in the Taurus molecular cloud based on the similar to 100 deg(2) Five College Radio Astronomy Observatory (CO)-C-12(1-0) and (CO)-C-13(1-0) maps and the Spitzer young stellar object catalogs. In the main 44 deg(2) area of Taurus, we found 55 outflows, of which 31 were previously unknown. We also found 37 bubbles in the entire 100 deg(2) area of Taurus, none of which had been found previously. The total kinetic energy of the identified outflows is estimated to be similar to 3.9 x 10(45) erg, which is 1% of the cloud turbulent energy. The total kinetic energy of the detected bubbles is estimated to be similar to 9.2 x 10(46) erg, which is 29% of the turbulent energy of Taurus. The energy injection rate from the outflows is similar to 1.3 x 10(33) erg s(-1), which is 0.4-2 times the dissipation rate of the cloud turbulence. The energy injection rate from bubbles is similar to 6.4 x 10(33) erg s(-1), which is 2-10 times the turbulent dissipation rate of the cloud. The gravitational binding energy of the cloud is similar to 1.5 x 10(48) erg, that is, 385 and 16 times the energy of outflows and bubbles, respectively. We conclude that neither outflows nor bubbles can provide sufficient energy to balance the overall gravitational binding energy and the turbulent energy of Taurus. However, in the current epoch, stellar feedback is sufficient to maintain the observed turbulence in Taurus. C1 [Li, Huixian; Li, Di; Qian, Lei; Xu, Duo; Nan, Rendong] Chinese Acad Sci, Natl Astron Observ, Beijing 100012, Peoples R China. [Li, Huixian; Li, Di; Qian, Lei; Nan, Rendong] Chinese Acad Sci, Key Lab Radio Astron, Nanjing 210008, Jiangsu, Peoples R China. [Li, Huixian; Xu, Duo] Univ Chinese Acad Sci, Beijing 100049, Peoples R China. [Li, Di] Space Sci Inst, Boulder, CO USA. [Xu, Duo; Song, Yuzhe] Nanjing Univ, Nanjing 210093, Jiangsu, Peoples R China. [Goldsmith, Paul F.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Noriega-Crespo, Alberto] CALTECH, IPAC, Pasadena, CA 91125 USA. [Noriega-Crespo, Alberto] Space Telescope Sci Inst, JWST, Baltimore, MD 21218 USA. [Wu, Yuefang] Peking Univ, Dept Astron, Beijing 100871, Peoples R China. RP Li, HX (reprint author), Chinese Acad Sci, Natl Astron Observ, Beijing 100012, Peoples R China. EM lhx@nao.cas.cn; dili@nao.cas.cn RI Goldsmith, Paul/H-3159-2016; OI Xu, Duo/0000-0001-6216-8931 FU China Ministry of Science and Technology under State Key Development Program for Basic Research [2012CB821802]; National Natural Science Foundation of China [11373038, 11373045]; Hundred Talents Program of the Chinese Academy of Sciences; Young Researcher Grant of National Astronomical Observatories, Chinese Academy of Sciences FX We are grateful to Dr. Y. L. Yue, Dr. Z. Y. Zhang, Dr. T. Liu, Dr. X. Y. Gao, and Dr. Z. Y. Ren for their kind and valuable advice and support. We thank the anonymous referee for a careful inspection of the manuscript and constructive comments, particularly the important suggestion to examine the turbulent dissipation issue in order to improve the quality of this study. We also thank Prof. W. Butler Burton for help in the review process. This work is partly supported by the China Ministry of Science and Technology under State Key Development Program for Basic Research (2012CB821802), and the National Natural Science Foundation of China (11373038, 11373045), the Hundred Talents Program of the Chinese Academy of Sciences, and the Young Researcher Grant of National Astronomical Observatories, Chinese Academy of Sciences. NR 62 TC 5 Z9 5 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 EI 1538-4365 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD AUG PY 2015 VL 219 IS 2 AR 20 DI 10.1088/0067-0049/219/2/20 PG 94 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CS2CY UT WOS:000361876600006 ER PT J AU Barth, MC Cantrell, CA Brune, WH Rutledge, SA Crawford, JH Huntrieser, H Carey, LD MacGorman, D Weisman, M Pickering, KE Bruning, E Anderson, B Apel, E Biggerstaff, M Campos, T Campuzano-Jost, P Cohen, R Crounse, J Day, DA Diskin, G Flocke, F Fried, A Garland, C Heikes, B Honomichl, S Hornbrook, R Huey, LG Jimenez, JL Lang, T Lichtenstern, M Mikoviny, T Nault, B O'Sullivan, D Pan, LL Peischl, J Pollack, I Richter, D Riemer, D Ryerson, T Schlager, H St Clair, J Walega, J Weibring, P Weinheimer, A Wennberg, P Wisthaler, A Wooldridge, PJ Ziegler, C AF Barth, Mary C. Cantrell, Christopher A. Brune, William H. Rutledge, Steven A. Crawford, James H. Huntrieser, Heidi Carey, Lawrence D. MacGorman, Donald Weisman, Morris Pickering, Kenneth E. Bruning, Eric Anderson, Bruce Apel, Eric Biggerstaff, Michael Campos, Teresa Campuzano-Jost, Pedro Cohen, Ronald Crounse, John Day, Douglas A. Diskin, Glenn Flocke, Frank Fried, Alan Garland, Charity Heikes, Brian Honomichl, Shawn Hornbrook, Rebecca Huey, L. Gregory Jimenez, Jose L. Lang, Timothy Lichtenstern, Michael Mikoviny, Tomas Nault, Benjamin O'Sullivan, Daniel Pan, Laura L. Peischl, Jeff Pollack, Ilana Richter, Dirk Riemer, Daniel Ryerson, Thomas Schlager, Hans St Clair, Jason Walega, James Weibring, Petter Weinheimer, Andrew Wennberg, Paul Wisthaler, Armin Wooldridge, Paul J. Ziegler, Conrad TI THE DEEP CONVECTIVE CLOUDS AND CHEMISTRY (DC3) FIELD CAMPAIGN SO BULLETIN OF THE AMERICAN METEOROLOGICAL SOCIETY LA English DT Article ID STRATOSPHERIC-TROPOSPHERIC EXPERIMENT; SEVERE THUNDERSTORM ELECTRIFICATION; POLARITY ELECTRICAL STRUCTURES; AIRBORNE MEASUREMENTS; LIGHTNING ACTIVITY; NOX PRODUCTION; TROPOPAUSE REGION; SCALE MODEL; NEW-MEXICO; JULY 10 AB The Deep Convective Clouds and Chemistry (DC3) field experiment produced an exceptional dataset on thunderstorms, including their dynamical, physical, and electrical structures and their impact on the chemical composition of the troposphere. The field experiment gathered detailed information on the chemical composition of the inflow and outflow regions of midlatitude thunderstorms in northeast Colorado, west Texas to central Oklahoma, and northern Alabama. A unique aspect of the DC3 strategy was to locate and sample the convective outflow a day after active convection in order to measure the chemical transformations within the upper-tropospheric convective plume. These data are being analyzed to investigate transport and dynamics of the storms, scavenging of soluble trace gases and aerosols, production of nitrogen oxides by lightning, relationships between lightning flash rates and storm parameters, chemistry in the upper troposphere that is affected by the convection, and related source characterization of the three sampling regions. DC3 also documented biomass-burning plumes and the interactions of these plumes with deep convection. C1 [Barth, Mary C.; Weisman, Morris; Apel, Eric; Campos, Teresa; Flocke, Frank; Honomichl, Shawn; Hornbrook, Rebecca; Pan, Laura L.; Weinheimer, Andrew] Natl Ctr Atmospher Res, Boulder, CO 80307 USA. [Cantrell, Christopher A.; Campuzano-Jost, Pedro; Day, Douglas A.; Fried, Alan; Jimenez, Jose L.; Richter, Dirk; Walega, James; Weibring, Petter] Univ Colorado, Boulder, CO 80309 USA. [Brune, William H.] Penn State Univ, University Pk, PA 16802 USA. [Rutledge, Steven A.; Lang, Timothy] Colorado State Univ, Ft Collins, CO 80523 USA. [Crawford, James H.; Anderson, Bruce; Diskin, Glenn] NASA, Langley Res Ctr, Hampton, VA 23665 USA. [Lichtenstern, Michael; Schlager, Hans] Deutsch Zentrum Luft & Raumfahrt DLR, Oberpfaffenhofen, Germany. [Carey, Lawrence D.] Univ Alabama, Huntsville, AL 35899 USA. [MacGorman, Donald; Ziegler, Conrad] NOAA, Natl Severe Storms Lab, Norman, OK 73069 USA. [Pickering, Kenneth E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Bruning, Eric] Texas Tech Univ, Lubbock, TX 79409 USA. [Biggerstaff, Michael] Univ Oklahoma, Norman, OK 73019 USA. [Cohen, Ronald; Garland, Charity; Nault, Benjamin; Wooldridge, Paul J.] Univ Calif Berkeley, Berkeley, CA 94720 USA. [Crounse, John; St Clair, Jason; Wennberg, Paul] CALTECH, Pasadena, CA 91125 USA. [Heikes, Brian] Univ Rhode Isl, Sch Oceanog, Narragansett, RI USA. [Huey, L. Gregory] Georgia Inst Technol, Atlanta, GA 30332 USA. [Mikoviny, Tomas] Oak Ridge Associated Univ, Oak Ridge, TN USA. [O'Sullivan, Daniel] US Naval Acad, Annapolis, MD 21402 USA. [Peischl, Jeff; Pollack, Ilana; Ryerson, Thomas] NOAA, ESRL, Boulder, CO USA. [Riemer, Daniel] Univ Miami, Coral Gables, FL 33124 USA. [Wisthaler, Armin] Instr Ionenphys & Angew Phys, Innsbruck, Austria. RP Barth, MC (reprint author), Natl Ctr Atmospher Res, POB 3000, Boulder, CO 80307 USA. EM barthm@ucar.edu RI Jimenez, Jose/A-5294-2008; Pan, Laura/A-9296-2008; Pollack, Ilana/F-9875-2012; Cohen, Ronald/A-8842-2011; Pickering, Kenneth/E-6274-2012; Peischl, Jeff/E-7454-2010; Manager, CSD Publications/B-2789-2015; Crounse, John/C-3700-2014; OI Jimenez, Jose/0000-0001-6203-1847; Pan, Laura/0000-0001-7377-2114; Cohen, Ronald/0000-0001-6617-7691; Peischl, Jeff/0000-0002-9320-7101; Crounse, John/0000-0001-5443-729X; Hornbrook, Rebecca/0000-0002-6304-6554; O'Sullivan, Daniel/0000-0001-9104-5703; Lang, Timothy/0000-0003-1576-572X; MacGorman, Donald/0000-0002-2395-8196 FU National Science Foundation (NSF); National Aeronautics and Space Administration (NASA); Deutsches Zentrum fur Luft- und Raumfahrt (DLR); National Oceanic and Atmospheric Administration (NOAA) FX DC3 was a complex field campaign coordinating aircraft facilities and ground-based facilities at three different locations. There are many people to thank, each responsible for making the campaign successful. Specifically, we thank the DC-8 HDSP2 team-Rushan Gao, Joshua Schwarz, Anne Perring, John Holloway, and Milos Markowic-for the black carbon data used for the PM1 calculation. The National Science Foundation (NSF), the National Aeronautics and Space Administration (NASA), the Deutsches Zentrum fur Luft- und Raumfahrt (DLR), and the National Oceanic and Atmospheric Administration (NOAA) are gratefully acknowledged for sponsoring the DC3 field experiment. The field project support provided by NCAR/EOL staff, especially Vidal Salazar and Jim Moore, is greatly appreciated. Data from the field campaign can be found at the NCAR/EOL field projects catalog (www.eol.ucar.edu/projects/dc3/). NR 72 TC 38 Z9 38 U1 6 U2 38 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0003-0007 EI 1520-0477 J9 B AM METEOROL SOC JI Bull. Amer. Meteorol. Soc. PD AUG PY 2015 VL 96 IS 8 BP 1281 EP 1309 DI 10.1175/BAMS-D-13-00290.1 PG 29 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA CR5FJ UT WOS:000361365700001 ER PT J AU Ferraro, R Waliser, DE Gleckler, P Taylor, KE Eyring, V AF Ferraro, Robert Waliser, Duane E. Gleckler, Peter Taylor, Karl E. Eyring, Veronika TI Evolving Obs4MIPs to Support Phase 6 of the Coupled Model Intercomparison Project (CMIP6) SO BULLETIN OF THE AMERICAN METEOROLOGICAL SOCIETY LA English DT Article C1 [Ferraro, Robert; Waliser, Duane E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Gleckler, Peter; Taylor, Karl E.] Lawrence Livermore Natl Lab, Livermore, CA USA. [Eyring, Veronika] Deutsch Zentrum Luft & Raumfahrt, Inst Phys Atmosphare, Oberpfaffenhofen, Germany. RP Ferraro, R (reprint author), CALTECH, Jet Prop Lab, MS 301-330,4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM robert.d.ferraro@jpl.nasa.gov RI Taylor, Karl/F-7290-2011; Eyring, Veronika/O-9999-2016 OI Taylor, Karl/0000-0002-6491-2135; Eyring, Veronika/0000-0002-6887-4885 FU U.S. Department of Energy Office of Science, Climate and Environmental Sciences Division, Regional and Global Climate Modeling Program [DE-AC52-07NA27344]; DLR Earth System Model Validation (ESMVal) project FX This meeting would not have occurred without the assistance and support of Tsengdar Lee at NASA, and Renu Joseph at DOE. Thanks are also due to Michel Rixen at WCRP for providing additional meeting support. Ferraro's and Waliser's contributions to this activity were performed on behalf of the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. Work by Gleckler and Taylor was performed on behalf of Lawrence Livermore National Laboratory as a contribution to the U.S. Department of Energy Office of Science, Climate and Environmental Sciences Division, Regional and Global Climate Modeling Program, under Contract DE-AC52-07NA27344. Eyring's work was supported by the DLR Earth System Model Validation (ESMVal) project. NR 5 TC 5 Z9 5 U1 2 U2 11 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0003-0007 EI 1520-0477 J9 B AM METEOROL SOC JI Bull. Amer. Meteorol. Soc. PD AUG PY 2015 VL 96 IS 8 BP ES131 EP ES133 DI 10.1175/BAMS-D-14-00216.1 PG 3 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA CR5GB UT WOS:000361367600003 ER PT J AU Molthan, AL Case, JL Venner, J Schroeder, R Checchi, MR Zavodsky, BT Limaye, A O'Brien, RG AF Molthan, Andrew L. Case, Jonathan L. Venner, Jason Schroeder, Richard Checchi, Milton R. Zavodsky, Bradley T. Limaye, Ashutosh O'Brien, Raymond G. TI Clouds in the Cloud: Weather Forecasts and Applications within Cloud Computing Environments SO BULLETIN OF THE AMERICAN METEOROLOGICAL SOCIETY LA English DT Article ID CONVECTIVE PARAMETERIZATION; MODEL; IMPLEMENTATION; RESOLUTION; PRECIPITATION; SCHEME; SYSTEM; IMPACT; STATE AB Cloud computing offers new opportunities to the scientific community through cloud-deployed software, data-sharing and collaboration tools, and the use of cloud-based computing infrastructure to support data processing and model simulations. This article provides a review of cloud terminology of possible interest to the meteorological community, and focuses specifically on the use of infrastructure as a service (IaaS) concepts to provide a platform for regional numerical weather prediction. Special emphasis is given to developing countries that may have limited access to traditional supercomputing facilities. Amazon Elastic Compute Cloud (EC2) resources were used in an IaaS capacity to provide regional weather simulations with costs ranging from $40 to $75 per 48-h forecast, depending upon the configuration. Simulations provided a reasonable depiction of sensible weather elements and precipitation when compared against typical validation data available over Central America and the Caribbean. C1 [Molthan, Andrew L.; Zavodsky, Bradley T.] NASA, Short Term Predict Res & Transit SPoRT Ctr, Huntsville, AL USA. [Molthan, Andrew L.; Zavodsky, Bradley T.; Limaye, Ashutosh] NASA, George C Marshall Space Flight Ctr, Earth Sci Off, Huntsville, AL 35812 USA. [Case, Jonathan L.] NASA, SPoRT Ctr, Huntsville, AL USA. [Case, Jonathan L.] ENSCO Inc, Huntsville, AL USA. [Venner, Jason; Schroeder, Richard; Checchi, Milton R.; O'Brien, Raymond G.] NASA, Ames Res Ctr, Mountain View, CA USA. [Venner, Jason] Mirantis Inc, Mountain View, CA USA. [Schroeder, Richard] Dell Serv Fed Govt, Mountain View, CA USA. RP Molthan, AL (reprint author), NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. EM andrew.molthan@nasa.gov NR 28 TC 1 Z9 1 U1 1 U2 1 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0003-0007 EI 1520-0477 J9 B AM METEOROL SOC JI Bull. Amer. Meteorol. Soc. PD AUG PY 2015 VL 96 IS 8 DI 10.1175/BAMS-D-14-00013.1 PG 12 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA CR5FQ UT WOS:000361366400001 ER PT J AU Kulkarni, CS Gorospe, G Daigle, MJ Goebel, K AF Kulkarni, Chetan S. Gorospe, George Daigle, Matthew J. Goebel, Kai TI A Testbed for Implementing Prognostic Methodologies on Cryogenic Propellant Loading Systems SO IEEE INSTRUMENTATION & MEASUREMENT MAGAZINE LA English DT Article C1 [Kulkarni, Chetan S.] Honeywell Automat India Ltd, Hyderabad, Andhra Pradesh, India. [Kulkarni, Chetan S.] Indian Inst Technol, Dept Elect Engn, Bombay 400076, Maharashtra, India. [Kulkarni, Chetan S.; Daigle, Matthew J.] Vanderbilt Univ, Inst Software Integrated Syst, Nashville, TN 37235 USA. [Kulkarni, Chetan S.; Daigle, Matthew J.] Vanderbilt Univ, Dept Elect Engn & Comp Sci, Nashville, TN 37235 USA. [Kulkarni, Chetan S.] NASA, Ames Res Ctr, Prognost Ctr Excellence, SGT Inc, Moffett Field, CA 94035 USA. [Gorospe, George; Daigle, Matthew J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Daigle, Matthew J.] Univ Calif Santa Cruz, NASA, Ames Res Ctr, Santa Cruz, CA 95064 USA. [Goebel, Kai] NASA, Syst Wide Safety & Assurance Technol Project, Prognost & Decis Making, Moffett Field, CA 94035 USA. [Goebel, Kai] Gen Elect Corp Res & Dev Ctr, New York, NY USA. [Goebel, Kai] Rensselaer Polytech Inst, Dept Comp Sci, Troy, NY 12180 USA. RP Kulkarni, CS (reprint author), NASA, Ames Res Ctr, Prognost Ctr Excellence, SGT Inc, Moffett Field, CA 94035 USA. FU Advanced Ground Systems Maintenance (AGSM) project under HEOMD/ESD program; Autonomous Propellant Loading project under HEOMD/AES; System-Wide Safety AssuranceTechnologies project under AvSAFE/ARMD by U.S. Government FX This work was funded in part by the Advanced Ground Systems Maintenance (AGSM) project under the HEOMD/ESD program, the Autonomous Propellant Loading project under HEOMD/AES, and the System-Wide Safety AssuranceTechnologies project under AvSAFE/ARMD by the U.S. Government. NR 19 TC 0 Z9 0 U1 0 U2 2 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1094-6969 EI 1941-0123 J9 IEEE INSTRU MEAS MAG JI IEEE Instrum. Meas. Mag. PD AUG PY 2015 VL 18 IS 4 BP 5 EP 15 PG 11 WC Engineering, Electrical & Electronic; Instruments & Instrumentation SC Engineering; Instruments & Instrumentation GA CR1EL UT WOS:000361066600001 ER PT J AU Hirose, A Rosen, PA Yamada, H Zink, M AF Hirose, Akira Rosen, Paul A. Yamada, Hiroyoshi Zink, Manfred TI Foreword to the Special Issue on Advances in SAR and Radar Technology SO IEEE JOURNAL OF SELECTED TOPICS IN APPLIED EARTH OBSERVATIONS AND REMOTE SENSING LA English DT Editorial Material C1 [Hirose, Akira] Univ Tokyo, Dept Elect Engn & Informat Syst, Tokyo 1138656, Japan. [Rosen, Paul A.] CALTECH, Jet Prop Lab, Commun Tracking & Radar Div, Pasadena, CA 91109 USA. [Yamada, Hiroyoshi] Niigata Univ, Dept Elect & Informat Engn, Niigata 9502181, Japan. [Zink, Manfred] German Aerosp Ctr DLR, Dept Satellite SAR Syst, D-82234 Wessling, Germany. RP Hirose, A (reprint author), Univ Tokyo, Dept Elect Engn & Informat Syst, Tokyo 1138656, Japan. NR 4 TC 1 Z9 1 U1 1 U2 5 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1939-1404 EI 2151-1535 J9 IEEE J-STARS JI IEEE J. Sel. Top. Appl. Earth Observ. Remote Sens. PD AUG PY 2015 VL 8 IS 8 BP 3748 EP 3750 DI 10.1109/JSTARS.2015.2475455 PG 3 WC Engineering, Electrical & Electronic; Geography, Physical; Remote Sensing; Imaging Science & Photographic Technology SC Engineering; Physical Geography; Remote Sensing; Imaging Science & Photographic Technology GA CR4WA UT WOS:000361339200001 ER PT J AU Tsalaportas, PG Kapinas, VM Karagiannidis, GK AF Tsalaportas, Panagiotis G. Kapinas, Vasileios M. Karagiannidis, George K. TI Solar Lab Notebook (SLN): An Ultra-Portable Web-Based System for Heliophysics and High-Security Labs SO IEEE JOURNAL OF SELECTED TOPICS IN APPLIED EARTH OBSERVATIONS AND REMOTE SENSING LA English DT Article DE Archiving; browser technologies; data files; data processing; digital notes; electronic lab notebook (ELN); extensible markup language (XML); FileReader API; heliophysics; hypertext markup language (HTML); HTML5; JavaScript; LocalStorage; portable tool; schema; single page application (SPA); solar activity; solar data; solar flare; web application ID SOFTWARE TOOL; RADIATION; IMAGERY AB This paper introduces the solar lab notebook (SLN), an electronic lab notebook (ELN) for improving the process of recording and sharing solar related digital information in an organized manner. SLN is a pure web-based application (available online: http://umbra.nascom.nasa.gov/sln) that runs client-side only, employing a clean and very friendly graphical user interface (GUI) design, and thus providing a true cross-platform user experience. Furthermore, SLN leverages unique technologies offered by modern web browsers, such as the FileReader API, the Blob interface, and Local Storage mechanism; it is coded entirely using HTML5, CSS3, and JavaScript, and powered by the extremely well-documented extensible markup language (XML) file format. For high-security labs, it can be utilized as an ultra-portable and secure digital notebook solution, since it is functionally self-contained, and does not require any server-side process running on either the local or a remote system. Finally, the W3C XML Schema language is used to define a list of rules, namely a data standard, that an SLN file must conform to, in order to be valid. In this way, developers are able to implement their own validation functions in their projects, or use one of the freely available tools to check if a data file is properly structured. Similarly, scientific groups at different labs can easily share information, being confident about the integrity of the exchanged data. C1 [Tsalaportas, Panagiotis G.] NASA, Greenbelt, MD 20771 USA. [Kapinas, Vasileios M.; Karagiannidis, George K.] Aristotle Univ Thessaloniki, Dept Elect & Comp Engn, Thessaloniki 54124, Greece. [Karagiannidis, George K.] Khalifa Univ, Dept Elect & Comp Engn, Abu Dhabi 127788, U Arab Emirates. RP Tsalaportas, PG (reprint author), NASA, Greenbelt, MD 20771 USA. EM kapinas@auth.gr; geokarag@auth.gr RI Karagiannidis, George/A-5190-2014; OI Karagiannidis, George/0000-0001-8810-0345; M., Vasileios/0000-0003-1232-2915 FU European Union [European Social Fund (ESF)]; Greek national funds through the Operational Program "Education and Lifelong Learning" FX This work was supported in part by the European Union [European Social Fund (ESF)] and in part by Greek national funds through the Operational Program "Education and Lifelong Learning" of the National Strategic Reference Framework (NSRF)-Research Funding Program: THALES-NTUA MIMOSA: Reinforcement of the interdisciplinary and/or interinstitutional research and innovation. NR 41 TC 0 Z9 0 U1 1 U2 6 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1939-1404 EI 2151-1535 J9 IEEE J-STARS JI IEEE J. Sel. Top. Appl. Earth Observ. Remote Sens. PD AUG PY 2015 VL 8 IS 8 BP 4141 EP 4150 DI 10.1109/JSTARS.2015.2444332 PG 10 WC Engineering, Electrical & Electronic; Geography, Physical; Remote Sensing; Imaging Science & Photographic Technology SC Engineering; Physical Geography; Remote Sensing; Imaging Science & Photographic Technology GA CR4WA UT WOS:000361339200035 ER PT J AU Tao, ZN Yu, HB Chin, MA AF Tao, Zhining Yu, Hongbin Chin, Mian TI The Role of Aerosol-Cloud-Radiation Interactions in Regional Air Quality-A NU-WRF Study over the United States SO ATMOSPHERE LA English DT Article DE aerosol-cloud-radiation interactions; air quality; factor separation; NU-WRF ID GOCART MODEL; EAST-ASIA; SYSTEM; IMPACT; PRECIPITATION; ATMOSPHERE; EMISSIONS; POLLUTION; CHEMISTRY; CLIMATE AB This work assessed the impact of aerosol-cloud-radiation (ACR) interactions on U.S. regional ozone and PM2.5 using the NASA Unified Weather Research and Forecasting modeling system. A series of three-month simulations have been carried out for the year 2010, in which the factor separation method has been applied in order to isolate the contributions from aerosol-radiation (AR), aerosol-cloud (AC), and their synergistic effects. The overall ACR effects were to reduce the average cloud liquid water path by 25 gm(-2) (ca. 40% of the baseline) and to increase the downward shortwave radiation by 8 Wm(-2) (ca. 3% of the baseline). The spatial difference in response to ACR was large, with ca. 50 Wm(-2), 1 K, and 100 m increases in downward shortwave radiation, surface temperature, and planetary boundary layer height (PBLH), respectively, while ca. 60 gm(-2) decrease in cloud liquid water path in central Texas. The AC effect dominated for changes in downward shortwave radiation, cloud liquid water path, wind, and temperature, while both AC and AR effects contributed profoundly to PBLH change. As a result, surface ozone and PM2.5 changed with large temporal-spatial variations. More than a 10 ppbv of surface ozone and a 5 gm(-3) of PM2.5 difference induced by ACR occurred frequently in the eastern U.S. C1 [Tao, Zhining] Univ Space Res Assoc, Columbia, MD 21044 USA. [Tao, Zhining; Yu, Hongbin; Chin, Mian] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Yu, Hongbin] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20740 USA. RP Tao, ZN (reprint author), Univ Space Res Assoc, 7178 Columbia Gateway Dr, Columbia, MD 21044 USA. EM zhining.tao@nasa.gov; hongbin.yu-1@nasa.gov; mian.chin@nasa.gov RI Yu, Hongbin/C-6485-2008; Chin, Mian/J-8354-2012 OI Yu, Hongbin/0000-0003-4706-1575; FU NASA's Atmospheric Composition: Modeling and Analysis (ACMAP) program; Modeling, Analysis, and Prediction (MAP) program FX The authors would like to thank the NASA Center for Climate Simulation (NCCS) for supercomputing support. This research was funded by NASA's Atmospheric Composition: Modeling and Analysis (ACMAP) program and the Modeling, Analysis, and Prediction (MAP) program. NR 48 TC 1 Z9 1 U1 2 U2 17 PU MDPI AG PI BASEL PA POSTFACH, CH-4005 BASEL, SWITZERLAND SN 2073-4433 J9 ATMOSPHERE-BASEL JI Atmosphere PD AUG PY 2015 VL 6 IS 8 BP 1045 EP 1068 DI 10.3390/atmos6081045 PG 24 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA CQ4HM UT WOS:000360565400005 ER PT J AU Feister, U Cabrol, N Hader, D AF Feister, Uwe Cabrol, Nathalie Haeder, Donat TI UV Irradiance Enhancements by Scattering of Solar Radiation from Clouds SO ATMOSPHERE LA English DT Article DE UV-B and UV-A irradiance; cloud modification factors; cloud scattering; high-altitude radiation measurements ID PHOTOCHEMICAL ACTIVITY; SPECTRAL DEPENDENCY; BLUE JETS; ULTRAVIOLET; MODULATION; ARGENTINA; BRAZIL; MODEL; WATER AB Scattering of solar radiation by clouds can reduce or enhance solar global irradiance compared to cloudless-sky irradiance at the Earth's surface. Cloud effects to global irradiance can be described by Cloud Modification Factors (CMF). Depending on strength and duration, irradiance enhancements affect the energy balance of the surface and gain of solar power for electric energy generation. In the ultraviolet region, they increase the risk for damage to living organisms. Wavelength-dependent CMFs have been shown to reach 1.5 even in the UV-B region at low altitudes. Ground-based solar radiation measurements in the high Andes region at altitudes up to 5917 m a.s.l showed cloud-induced irradiance enhancements. While UV-A enhancements were explained by cloud scattering, both radiation scattering from clouds and Negative Ozone Anomalies (NOA) have been discussed to have caused short-time enhancement of UV-B irradiance. Based on scenarios using published CMF and additional spectroradiometric measurements at a low-altitude site, the contribution of cloud scattering to the UV-B irradiance enhancement in the Andes region has been estimated. The range of UV index estimates converted from measured UV-B and UV-A irradiance and modeled cloudless-sky ratios UV-B/erythemal UV is compatible with an earlier estimate of an extreme UV index value of 43 derived for the high Andes. C1 [Feister, Uwe] Meteorol Observ Lindenberg Richard Assmann Observ, German Meteorol Serv, D-15848 Lindenberg, Germany. [Cabrol, Nathalie] NASA, Ames Res Ctr, SETI Inst, Carl Sagan Ctr, Moffett Field, CA 94035 USA. [Haeder, Donat] Univ Erlangen Nurnberg, Dept Biol, D-91054 Erlangen, Germany. RP Cabrol, N (reprint author), NASA, Ames Res Ctr, SETI Inst, Carl Sagan Ctr, Moffett Field, CA 94035 USA. EM uwefeister@web.de; Nathalie.A.Cabrol@nasa.gov; donat@dphaeder.de FU NASA Astrobiology Institute FX We are grateful to AIRS and MODIS mission scientists and associated NASA personnel for the production of the data used in this research effort. Data availability accessible by Giovanni [34] is greatly acknowledged. We gratefully acknowledge funding of the High Lakes Project by the NASA Astrobiology Institute. We thank Ralf Becker from the Meteorological Observatory Lindenberg for the AOD data of the AErosol RObotic NETwork (AERONET). We also thank the reviewers for their careful reviews of the manuscript. NR 34 TC 1 Z9 1 U1 2 U2 12 PU MDPI AG PI BASEL PA POSTFACH, CH-4005 BASEL, SWITZERLAND SN 2073-4433 J9 ATMOSPHERE-BASEL JI Atmosphere PD AUG PY 2015 VL 6 IS 8 BP 1211 EP 1228 DI 10.3390/atmos6081211 PG 18 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA CQ4HM UT WOS:000360565400014 ER PT J AU Khavaran, A AF Khavaran, Abbas TI Jet surface interaction - scrubbing noise in a transversely sheared mean flow SO INTERNATIONAL JOURNAL OF AEROACOUSTICS LA English DT Article ID TURBULENT BOUNDARY-LAYER; TRAILING EDGE NOISE; WALL PRESSURE; SOUND; SCATTERING; GENERATION; DISTORTION; MODEL AB Generation of sound due to scrubbing of a jet flow past a nearby solid surface is investigated within the framework of the generalized acoustic analogy theory. The analysis applies to the boundary layer noise generated at and near a wall, and excludes the scattered noise component that is produced at the leading or the trailing edge. While compressibility effects are relatively unimportant at very low Mach numbers, frictional heat generation and thermal gradient normal to the surface could play important roles in generation and propagation of sound in high speed jets of practical interest. A general expression is given for the spectral density of the far field sound as governed by the variable density Pridmore-Brown equation. The propagation Green's function is solved numerically starting with the boundary conditions on the surface and subject to specified mean velocity and temperature profiles between the surface and the observer. It is shown the magnitude of the Green's function decreases with increasing source frequency or jet temperature. The phase remains constant for a rigid surface, but varies with source location when subject to an impedance type boundary condition. The equivalent sources of aerodynamic sound are associated with non-linear momentum flux and enthalpy flux terms that appear in a linear set of equations that govern the fluctuating components of the motion. These multi-pole sources are usually modeled and evaluated with input from a Reynolds-Averaged Navier-Stokes (RANS) solver with an appropriate turbulence model. C1 NASA, Glenn Res Ctr, Vantage Partners LLC, Cleveland, OH 44135 USA. RP Khavaran, A (reprint author), NASA, Glenn Res Ctr, Vantage Partners LLC, Cleveland, OH 44135 USA. EM Abbas.Khavaran-1@nasa.gov FU NASA Fundamental Aeronautics Program; Acoustics Branch at NASA Glenn Research Center FX This work was sponsored by the Fixed Wing Project in the NASA Fundamental Aeronautics Program. The author is grateful to the Acoustics Branch at NASA Glenn Research Center for supporting this research effort. NR 27 TC 0 Z9 0 U1 0 U2 0 PU MULTI-SCIENCE PUBL CO LTD PI BRENTWOOD PA 5 WATES WAY, BRENTWOOD CM15 9TB, ESSEX, ENGLAND SN 1475-472X J9 INT J AEROACOUST JI Int. J. Aeroacoust. PD AUG PY 2015 VL 14 IS 3-4 BP 373 EP 412 PG 40 WC Acoustics; Engineering, Aerospace; Mechanics SC Acoustics; Engineering; Mechanics GA CR0EC UT WOS:000360990100004 ER PT J AU Goodrich, JW AF Goodrich, John W. TI Experiments in numerical error control for sound propagation in a 2D jet using a damping layer and nonreflecting outer boundaries SO INTERNATIONAL JOURNAL OF AEROACOUSTICS LA English DT Article ID HYPERBOLIC SYSTEMS; COMPUTATIONAL AEROACOUSTICS; FLOW AB This paper reports numerical experiments for propagating a continuous acoustic pressure signal by means of the linearized Euler equations with both a uniform flow and a parallel jet as the base or mean flow. The numerical domain is embedded in a surrounding damping layer, and the outer boundaries of the damping layer are treated with weak Giles type nonreflecting boundary conditions that are introduced in this paper as interpolation constraints. We view this combination of the damping layer with the nonreflecting outer boundary conditions as the complete boundary treatment. The issue that is being addressed is not the accuracy of the numerical solution when compared to a mathematical solution, which would be improved by grid refinement, but the effect of the complete boundary treatment on the numerical solution, and to what degree the error from the complete boundary treatment can be controlled. These computational experiments show that the weak boundary conditions are stable, and the complete boundary treatment is conditionally stable, for long simulation times, and that the damping layer width and the damping amplitude can be adjusted to produce maximum relative errors that are O[10(-6)]. The complete boundary treatment is in this sense consistent with the numerical simulation of the propagation dynamics. C1 NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Goodrich, JW (reprint author), NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. EM john.w.goodrich@nasa.gov NR 29 TC 0 Z9 0 U1 0 U2 1 PU SAGE PUBLICATIONS INC PI THOUSAND OAKS PA 2455 TELLER RD, THOUSAND OAKS, CA 91320 USA SN 1475-472X EI 2048-4003 J9 INT J AEROACOUST JI Int. J. Aeroacoust. PD AUG PY 2015 VL 14 IS 3-4 BP 489 EP 519 PG 31 WC Acoustics; Engineering, Aerospace; Mechanics SC Acoustics; Engineering; Mechanics GA CR0EC UT WOS:000360990100008 ER PT J AU Dahl, MD AF Dahl, Milo D. TI Turbulence statistics for jet noise source modeling from filtered PIV measurements SO INTERNATIONAL JOURNAL OF AEROACOUSTICS LA English DT Article ID SPACE-TIME CORRELATIONS; HILBERT SPECTRUM; DECOMPOSITION; AEROACOUSTICS; SOUND; FLOW AB Time-resolved, particle image velocimetry was used to measure the velocity fluctuation field at three locations along the lipline of two subsonic jets. The time history data within these fields were filtered in the time domain using empirical mode decomposition to produce two signals from the velocity fluctuation measurements. One signal was for the low-frequency, large-scale turbulent eddy component of the velocity fluctuations and represented the computed results of a large-eddy simulation. The other signal was for the high-frequency, small-scale turbulent eddy component of the velocity fluctuations. This represented the missing scales of a large-eddy simulation. The effect of filtering on the statistical properties of the velocity fluctuations relevant to jet noise prediction modeling were studied. Two-point, space-time, cross correlations were computed for the axial velocity fluctuations. Comparisons were made for the second- and fourth-order two-point correlations, the integral phase velocities, length scales, and time scales, and the frequency dependent phase velocities, length scales, and time scales between the total, large-scale, and small-scale velocity fluctuations. C1 NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Dahl, MD (reprint author), NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. EM milo.d.dahl@nasa.gov FU NASA Wing Project of Fundamental Aeronautics Program FX The author would like to thank Dr. James Bridges for providing the measured data and the software for computing correlations and spectra. The NASA Fixed Wing Project of the Fundamental Aeronautics Program supported this work. NR 40 TC 0 Z9 0 U1 4 U2 4 PU MULTI-SCIENCE PUBL CO LTD PI BRENTWOOD PA 5 WATES WAY, BRENTWOOD CM15 9TB, ESSEX, ENGLAND SN 1475-472X J9 INT J AEROACOUST JI Int. J. Aeroacoust. PD AUG PY 2015 VL 14 IS 3-4 BP 521 EP 552 PG 32 WC Acoustics; Engineering, Aerospace; Mechanics SC Acoustics; Engineering; Mechanics GA CR0EC UT WOS:000360990100009 ER PT J AU Envia, E AF Envia, Edmane TI Aeroacoustic analysis of a high-speed open rotor SO INTERNATIONAL JOURNAL OF AEROACOUSTICS LA English DT Article ID PROPELLER NOISE; PREDICTION AB Owing to their inherent fuel efficiency, there is renewed interest in developing open rotor propulsion systems that are both efficient and quiet. The major contributor to the overall noise of an open rotor system is the propulsor noise, which is produced as a result of the interaction of the airstream with the counter-rotating blades. Prediction of the propulsor noise is, therefore, a necessary ingredient in any approach for designing low-noise open rotor systems that can meet community noise regulations and have acceptable cabin noise levels. To that end, there has been a resurgence of activities in the aeroacoustic modeling of open rotors in recent years. While direct numerical simulations are gaining traction, the bulk of existing prediction capability resides in hybrid approaches in which the aerodynamics of the open rotor system is computed via CFD and is used as input in some appropriate "linear" acoustic model for computing the open rotor noise. At NASA the focus has been on assessing the utility of hybrid approaches for accurately predicting the open rotor tone spectra with an emphasis on the understanding of the role of the various underlying mechanisms of noise generation and their relative importance at different operating conditions. Using high-fidelity aerodynamic simulations of a benchmark (non-proprietary) open rotor blade set, together with acoustic models based on a high-blade-count asymptotic approximation of the Ffowcs-Williams Hawkings equation, tone noise predictions for a number of configurations have been carried out. These aerodynamic and acoustic predictions have been compared with wind tunnel measurements of the benchmark open rotor blade set to establish the capabilities and the limitations of the hybrid approaches. The results suggest that while predicting the absolute spectral levels is difficult, the noise trends are reasonably well predicted by such hybrid approaches at a reasonable overall computational cost. C1 [Envia, Edmane] NASA, Glenn Res Ctr, Acoust Branch, Cleveland, OH 44135 USA. RP Envia, E (reprint author), NASA, Glenn Res Ctr, MS 54-3,21000 Brookpark Rd, Cleveland, OH 44135 USA. EM edmane.envia-1@nasa.gov FU NASA Fixed Wing Project FX This work was supported by the NASA Fixed Wing Project. NR 20 TC 0 Z9 0 U1 2 U2 14 PU MULTI-SCIENCE PUBL CO LTD PI BRENTWOOD PA 5 WATES WAY, BRENTWOOD CM15 9TB, ESSEX, ENGLAND SN 1475-472X J9 INT J AEROACOUST JI Int. J. Aeroacoust. PD AUG PY 2015 VL 14 IS 3-4 BP 569 EP 606 PG 38 WC Acoustics; Engineering, Aerospace; Mechanics SC Acoustics; Engineering; Mechanics GA CR0EC UT WOS:000360990100011 ER PT J AU Hermes, JJ Gansicke, BT Bischoff-Kim, A Kawaler, SD Fuchs, JT Dunlap, BH Clemens, JC Montgomery, MH Chote, P Barclay, T Marsh, TR Gianninas, A Koester, D Winget, DE Armstrong, DJ Rebassa-Mansergas, A Schreiber, MR AF Hermes, J. J. Gaensicke, B. T. Bischoff-Kim, A. Kawaler, Steven D. Fuchs, J. T. Dunlap, B. H. Clemens, J. C. Montgomery, M. H. Chote, P. Barclay, Thomas Marsh, T. R. Gianninas, A. Koester, D. Winget, D. E. Armstrong, D. J. Rebassa-Mansergas, A. Schreiber, M. R. TI Insights into internal effects of common-envelope evolution using the extended Kepler mission SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE asteroseismology; binaries: close; stars: individual: SDSS J113655.17+040952.6; white dwarfs ID DA WHITE-DWARFS; WHOLE EARTH TELESCOPE; EXTREMELY LOW-MASS; ZZ CETI STARS; PRECISION ASTEROSEISMOLOGY; INSTABILITY STRIP; GRAVITY MODES; BINARY STARS; NN SERPENTIS; V471 TAU AB We present an analysis of the binary and physical parameters of a unique pulsating white dwarf with a main-sequence companion, SDSS J1136+0409, observed for more than 77 d during the first pointing of the extended Kepler mission: K2 Campaign 1. Using new ground-based spectroscopy, we show that this post-common-envelope binary has an orbital period of 6.89760103(60) h, which is also seen in the photometry as a result of Doppler beaming and ellipsoidal variations of the secondary. We spectroscopically refine the temperature of the white dwarf to 12 330 +/- 260 K and its mass to 0.601 +/- 0.036 M-circle dot. We detect seven independent pulsation modes in the K2 light curve. A preliminary asteroseismic solution is in reasonable agreement with the spectroscopic atmospheric parameters. Three of the pulsation modes are clearly rotationally split multiplets, which we use to demonstrate that the white dwarf is not synchronously rotating with the orbital period but has a rotation period of 2.49 +/- 0.53 h. This is faster than any known isolated white dwarf, but slower than almost all white dwarfs measured in non-magnetic cataclysmic variables, the likely future state of this binary. C1 [Hermes, J. J.; Gaensicke, B. T.; Chote, P.; Marsh, T. R.; Armstrong, D. J.] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. [Bischoff-Kim, A.] Penn State Worthington Scranton, Dunmore, PA 18512 USA. [Kawaler, Steven D.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. [Fuchs, J. T.; Dunlap, B. H.; Clemens, J. C.] Univ N Carolina, Dept Phys & Astron, Chapel Hill, NC 27599 USA. [Montgomery, M. H.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Barclay, Thomas] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Barclay, Thomas] Bay Area Environm Res Inst, Sonoma, CA 95476 USA. [Gianninas, A.] Univ Oklahoma, Homer L Dodge Dept Phys & Astron, Norman, OK 73019 USA. [Koester, D.] Univ Kiel, Inst Theoret Phys & Astrophys, D-24098 Kiel, Germany. [Rebassa-Mansergas, A.] Peking Univ, Kavli Inst Astron & Astrophys, Beijing 100871, Peoples R China. [Schreiber, M. R.] Univ Valparaiso, Dept Fis & Astron, Valparaiso, Chile. RP Hermes, JJ (reprint author), Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. EM j.j.hermes@warwick.ac.uk RI Alexandros, Gianninas/B-8352-2016; Gaensicke, Boris/A-9421-2012; OI Alexandros, Gianninas/0000-0002-8655-4308; Gaensicke, Boris/0000-0002-2761-3005; Armstrong, David/0000-0002-5080-4117 FU European Research Council under the European Union [320964]; NSF [AST-1413001, AST-1312983]; NASA [NNX12AC96G]; UK Science and Technology Facilities Council (STFC) [ST/L000733/1]; NASA through Space Telescope Science Institute [HST-GO-13319.01, NAS 5-26555]; FONDECYT [1141269]; Millennium Nucleus [RC130007]; Postdoctoral Science Foundation of China [2013M530470, 2014T70010]; Research Fund for International Young Scientists by the National Natural Science Foundation of China [11350110496]; NASA Science Mission Directorate FX We thank the anonymous referee whose thorough comments significantly improved this paper. We wish to acknowledge fruitful discussions with Jim Fuller, Danny Steeghs, and Roberto Raddi. JJH, BTG, and PC acknowledge funding from the European Research Council under the European Union Seventh Framework Programme (FP/2007-2013)/ERC Grant Agreement no. 320964 (WD-Tracer). JTF acknowledges support from the NSF under award AST-1413001. MHM and DEW gratefully acknowledge the support of the NSF under grant AST-1312983. MHM acknowledges the support of NASA under grant NNX12AC96G. TRM was supported under a grant from the UK Science and Technology Facilities Council (STFC), ST/L000733/1. AG acknowledges support provided by NASA through grant number HST-GO-13319.01 from the Space Telescope Science Institute, which is operated by AURA, Inc., under NASA contract NAS 5-26555. MRS acknowledges support from FONDECYT (grant 1141269) and from the Millennium Nucleus RC130007 (Chilean Ministry of Economy). AR-M acknowledges financial support from the Postdoctoral Science Foundation of China (grants 2013M530470 and 2014T70010) and from the Research Fund for International Young Scientists by the National Natural Science Foundation of China (grant 11350110496).; This work is based on observations collected at the European Organisation for Astronomical Research in the Southern Hemisphere, Chile (083.D-0862, 093.D-0300), the SOAR telescope, and the Kepler spacecraft (GO1015). The SOAR telescope is a joint project of the Ministerio da Ciencia, Tecnologia, e Inovacao (MCTI) da Republica Federativa do Brasil, the US National Optical Astronomy Observatory (NOAO), the University of North Carolina at Chapel Hill (UNC), and Michigan State University (MSU). Funding for the Kepler mission is provided by the NASA Science Mission Directorate. NR 88 TC 9 Z9 9 U1 0 U2 2 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD AUG 1 PY 2015 VL 451 IS 2 BP 1701 EP 1712 DI 10.1093/mnras/stv1053 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CQ8BB UT WOS:000360830000044 ER PT J AU Morin, CW Monaghan, AJ Hayden, MH Barrera, R Ernst, K AF Morin, Cory W. Monaghan, Andrew J. Hayden, Mary H. Barrera, Roberto Ernst, Kacey TI Meteorologically Driven Simulations of Dengue Epidemics in San Juan, PR SO PLOS NEGLECTED TROPICAL DISEASES LA English DT Article ID AEDES-AEGYPTI DIPTERA; TEXAS-MEXICO BORDER; MARK-RELEASE-RECAPTURE; PUERTO-RICO; CLIMATE VARIABILITY; HEMORRHAGIC-FEVER; CULEX-QUINQUEFASCIATUS; POPULATION PARAMETERS; VERTICAL TRANSMISSION; MALARIA TRANSMISSION AB Meteorological factors influence dengue virus ecology by modulating vector mosquito population dynamics, viral replication, and transmission. Dynamic modeling techniques can be used to examine how interactions among meteorological variables, vectors and the dengue virus influence transmission. We developed a dengue fever simulation model by coupling a dynamic simulation model for Aedes aegypti, the primary mosquito vector for dengue, with a basic epidemiological Susceptible-Exposed-Infectious-Recovered (SEIR) model. Employing a Monte Carlo approach, we simulated dengue transmission during the period of 2010-2013 in San Juan, PR, where dengue fever is endemic. The results of 9600 simulations using varied model parameters were evaluated by statistical comparison (r(2)) with surveillance data of dengue cases reported to the Centers for Disease Control and Prevention. To identify the most influential parameters associated with dengue virus transmission for each period the top 1% of best-fit model simulations were retained and compared. Using the top simulations, dengue cases were simulated well for 2010 (r(2) = 0.90, p = 0.03), 2011 (r(2) = 0.83, p = 0.05), and 2012 (r(2) = 0.94, p = 0.01); however, simulations were weaker for 2013 (r(2) = 0.25, p = 0.25) and the entire four-year period (r(2) = 0.44, p = 0.002). Analysis of parameter values from retained simulations revealed that rain dependent container habitats were more prevalent in best-fitting simulations during the wetter 2010 and 2011 years, while human managed (i.e. manually filled) container habitats were more prevalent in best-fitting simulations during the drier 2012 and 2013 years. The simulations further indicate that rainfall strongly modulates the timing of dengue (e.g., epidemics occurred earlier during rainy years) while temperature modulates the annual number of dengue fever cases. Our results suggest that meteorological factors have a time-variable influence on dengue transmission relative to other important environmental and human factors. C1 [Morin, Cory W.] NASA, George C Marshall Space Flight Ctr, Earth Sci Off, Huntsville, AL 35812 USA. [Monaghan, Andrew J.; Hayden, Mary H.] Natl Ctr Atmospher Res, Res Applicat Lab, Boulder, CO USA. [Barrera, Roberto] Ctr Dis Control & Prevent, Dengue Branch, Entomol & Ecol Act, San Juan, PR USA. [Ernst, Kacey] Univ Arizona, Mel & Enid Zuckerman Coll Publ Hlth, Tucson, AZ USA. RP Morin, CW (reprint author), NASA, George C Marshall Space Flight Ctr, Earth Sci Off, Huntsville, AL 35812 USA. EM cory.morin@nasa.gov OI Monaghan, Andrew/0000-0002-8170-2359 FU National Oceanic and Atmospheric Administration Regional Integrated Sciences and Assessments program; National Institutes of Health [IR56AI091843, IR01AI091843]; National Institute of Allergy and Infectious Disease; National Science Foundation FX This research was supported in part by the National Oceanic and Atmospheric Administration (noaa.gov) Regional Integrated Sciences and Assessments program (CWM), as well as grants IR56AI091843 and IR01AI091843 from the National Institutes of Health (nih.gov), National Institute of Allergy and Infectious Disease (KE). The National Center for Atmospheric Research (AJM and MHH) is partially funded by the National Science Foundation (nsf.gov). The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 78 TC 4 Z9 4 U1 2 U2 20 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1935-2735 J9 PLOS NEGLECT TROP D JI Plos Neglect. Trop. Dis. PD AUG PY 2015 VL 9 IS 8 AR e0004002 DI 10.1371/journal.pntd.0004002 PG 24 WC Infectious Diseases; Parasitology; Tropical Medicine SC Infectious Diseases; Parasitology; Tropical Medicine GA CQ6IO UT WOS:000360708200043 PM 26275146 ER PT J AU Kalluri, S Gundy, J Haman, B Paullin, A Van Rompay, P Vititoe, D Weiner, A AF Kalluri, Satya Gundy, James Haman, Brian Paullin, Anthony Van Rompay, Paul Vititoe, David Weiner, Allan TI A High Performance Remote Sensing Product Generation System Based on a Service Oriented Architecture for the Next Generation of Geostationary Operational Environmental Satellites SO REMOTE SENSING LA English DT Article DE GOES-R; Product Generation; High Performance Computing (HPC); Service Oriented Architecture (SOA) ID GOES-R; ALGORITHMS AB The Geostationary Operational Environmental Satellite (GOES) series R, S, T, U (GOES-R) will collect remote sensing data at several orders of magnitude compared to legacy missions, 24 x 7, over its 20-year operational lifecycle. A suite of 34 Earth and space weather products must be produced at low latency for timely delivery to forecasters. A ground system (GS) has been developed to meet these challenging requirements, using High Performance Computing (HPC) within a Service Oriented Architecture (SOA). This approach provides a robust, flexible architecture to support the operational GS as it generates remote sensing products by ingesting and combining data from multiple sources. Test results show that the system meets the key latency and availability requirements for all products. C1 [Kalluri, Satya] NASA, Goddard Space Flight Ctr, NOAA, GOES R Program Off, Greenbelt, MD 20771 USA. [Gundy, James; Haman, Brian; Paullin, Anthony; Vititoe, David; Weiner, Allan] Harris Corp, Melbourne, FL 32904 USA. [Van Rompay, Paul] Atmospher & Environm Res, Lexington, MA 02421 USA. RP Kalluri, S (reprint author), NASA, Goddard Space Flight Ctr, NOAA, GOES R Program Off, Code 417, Greenbelt, MD 20771 USA. EM satya.kalluri@noaa.gov; jgundy@harris.com; bhaman@harris.com; apaullin@harris.com; pvanromp@aer.com; dvititoe@harris.com; aweiner@harris.com FU NOAA [DG133E-09-CN-0094] FX The views, opinions, and findings contained in this paper are those of the author(s) and should not be construed as an official National Oceanic and Atmospheric Administration or U.S. Government position, policy, or decision. Harris Corporation was funded by NOAA contract DG133E-09-CN-0094. The authors would like to thank Steven Goodman, Tim Schmit, Basil Chiasson, and the three anonymous reviewers for their valuable comments and feedback on the original manuscript. Their contributions led to significant improvements in the final published version. ABI L2+ algorithms were provided by the GOES-R Algorithm Working Group. The L1b algorithms were provided by the following instrument vendors: Exelis (ABI), Lockheed Martin (SUVI, GLM and Magnetometer), Laboratory for Atmospheric and Space Physics (EXIS), and Assurance Technology Corporation (SEISS). NR 16 TC 0 Z9 0 U1 7 U2 11 PU MDPI AG PI BASEL PA POSTFACH, CH-4005 BASEL, SWITZERLAND SN 2072-4292 J9 REMOTE SENS-BASEL JI Remote Sens. PD AUG PY 2015 VL 7 IS 8 BP 10385 EP 10399 DI 10.3390/rs70810385 PG 15 WC Remote Sensing SC Remote Sensing GA CQ7XF UT WOS:000360818800041 ER PT J AU Inamdar, AK Guillevic, PC AF Inamdar, Anand K. Guillevic, Pierre C. TI Net Surface Shortwave Radiation from GOES Imagery-Product Evaluation Using Ground-Based Measurements from SURFRAD SO REMOTE SENSING LA English DT Article ID RADIOMETER SUITE VIIRS; SATELLITE MEASUREMENTS; SOLAR-RADIATION; BUDGET NETWORK; ENERGY-BALANCE; VALIDATION; INSOLATION; MODEL; SIMULATIONS; METHODOLOGY AB The Earth's surface net radiation controls the energy and water exchanges between the Earth's surface and the atmosphere, and can be derived from satellite observations. The ability to monitor the net surface radiation over large areas at high spatial and temporal resolution is essential for many applications, such as weather forecasting, short-term climate prediction or water resources management. The objective of this paper is to derive the net surface radiation in the shortwave domain at high temporal (half-hourly) and spatial resolution (similar to 1 km) using visible imagery from Geostationary Operational Environmental Satellite (GOES). The retrieval algorithm represents an adaptation to GOES data of a standard algorithm initially developed for the NASA-operated Clouds and Earth's Radiant Energy System (CERES) scanner. The methodology relies on: (1) the estimation of top of atmosphere shortwave radiation from GOES spectral measurements; and (2) the calculation of net surface shortwave (SW) radiation accounting for atmospheric effects. Comparison of GOES-retrieved net surface shortwave radiation with ground-measurements at the National Oceanic and Atmospheric Administration's (NOAA) Surface Radiation (SURFRAD) stations yields very good agreement with average bias lower than 5W center dot m(-2) and root mean square difference around 70 W center dot m(-2). The algorithm performance is usually higher over areas characterized by low spatial variability in term of land cover type and surface biophysical properties. The technique does not involve retrieval and assessment of cloud properties and can be easily adapted to other meteorological satellites around the globe. C1 [Inamdar, Anand K.] N Carolina State Univ, CICS, Asheville, NC 28801 USA. [Inamdar, Anand K.] NOAA, Natl Ctr Environm Informat, Asheville, NC 28801 USA. [Guillevic, Pierre C.] CALTECH, Jet Prop Lab, Pasadena, CA 91011 USA. RP Inamdar, AK (reprint author), N Carolina State Univ, CICS, Asheville, NC 28801 USA. EM anand.inamdar@noaa.gov; Pierre.Guillevic@gmail.com FU NOAA through the Cooperative Institute for Climate and Satellites (CICS)-North Carolina [NA09NES4400006]; Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA; National Aeronautic and Space Administration (NASA) FX This work was supported by NOAA through the Cooperative Institute for Climate and Satellites (CICS)-North Carolina under Cooperative Agreement NA09NES4400006, and by the Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, under contract with the National Aeronautic and Space Administration (NASA). The GOES data are distributed by the NOAA's Comprehensive Large-Array Data Stewardship System (CLASS). The CERES data were obtained from the Atmospheric Sciences Data Center at the NASA Langley Research Center. The ARM/SGP and SURFRAD data were obtained from the Surface Observations provided by the CERES/ARM Validation Experiment (CAVE) web site. Authors are grateful for constructive comments provided by the reviewers which helped a great deal in improving the quality of presentation. Authors acknowledge the help rendered by Jessica Griffin (CICS) with figures. NR 38 TC 5 Z9 5 U1 3 U2 16 PU MDPI AG PI BASEL PA POSTFACH, CH-4005 BASEL, SWITZERLAND SN 2072-4292 J9 REMOTE SENS-BASEL JI Remote Sens. PD AUG PY 2015 VL 7 IS 8 BP 10788 EP 10814 DI 10.3390/rs70810788 PG 27 WC Remote Sensing SC Remote Sensing GA CQ7XF UT WOS:000360818800059 ER PT J AU Potter, C AF Potter, Christopher TI ASSESSMENT OF THE IMMEDIATE IMPACTS OF THE 2013-2014 DROUGHT ON ECOSYSTEMS OF THE CALIFORNIA CENTRAL COAST SO WESTERN NORTH AMERICAN NATURALIST LA English DT Article ID DIFFERENCE WATER INDEX; FUEL MOISTURE; VEGETATION; PATTERNS; TM AB A methodology was developed to assess the impacts of the historic 2013-2014 drought on ecosystems of California's Central Coast region, using a combination of satellite image analysis and in situ measurements of soil moisture in predominant vegetation types of the region. According to differences in Landsat drought indices for plant water stress and vegetation green cover (NDWI and NDVI, respectively), the geographic areas within the study region that were most severely impacted by the 2013 drought were the inland Carmel Valley in northern Monterey County and the coastal zones around San Simeon Point and Cambria in northern San Luis Obispo County. An expanded area of severe vegetation moisture stress, generally indicated by relative-differenced NDWI values of > 400, was detected by May 2014 in both of these same geographic areas. For more detailed examination of drought impacts, the entire study region was separated into the 3 predominant vegetation types (grasslands, shrublands, and forests) to examine changes in Landsat NDWI and NDVI in the context of differing plant community responses to severe drought. Results confirmed that higher overall drought stress in 2013 and 2014 was detected in grasslands, compared to shrublands and forests, in both years at all elevations and slopes > 200 m and > 5%, respectively. C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Potter, C (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM chris.potter@nasa.gov NR 31 TC 1 Z9 1 U1 6 U2 44 PU BRIGHAM YOUNG UNIV PI PROVO PA 290 LIFE SCIENCE MUSEUM, PROVO, UT 84602 USA SN 1527-0904 EI 1944-8341 J9 WEST N AM NATURALIST JI West. North Am. Naturalist PD AUG PY 2015 VL 75 IS 2 BP 129 EP 145 PG 17 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA CR0AA UT WOS:000360978700001 ER PT J AU Acero, F Lemoine-Goumard, M Renaud, M Ballet, J Hewitt, JW Rousseau, R Tanaka, T AF Acero, F. Lemoine-Goumard, M. Renaud, M. Ballet, J. Hewitt, J. W. Rousseau, R. Tanaka, T. TI Study of TeV shell supernova remnants at gamma-ray energies SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE ISM: supernova remnants; acceleration of particles; gamma rays: general ID LARGE-AREA TELESCOPE; RX J1713.7-3946; SN 1006; RCW 86; HESS J1731-347; PARTICLE-ACCELERATION; SOURCE CATALOG; IA SUPERNOVA; EMISSION; SN-1006 AB Context. The breakthrough developments of Cherenkov telescopes in the past decade have led to angular resolution of 0.1 degrees and an unprecedented sensitivity. This has allowed the current generation of Cherenkov telescopes (H.E.S.S., MAGIC, and VERITAS) to discover a population of supernova remnants (SNRs) radiating in very-high-energy (VHE; E > 100 GeV) gamma-rays. A number of those VHE SNRs exhibit a shell-type morphology that is spatially coincident with the shock front of the SNR. Aims. The members of this VHE shell SNR club are RXJ1713.7-3946, RXJ0852.0-4622, RCW86, SN 1006, and HESS J1731-347. The last two objects have been poorly studied in high-energy (HE; 0.1 < E < 100 GeV) gamma-rays and need to be investigated in order to draw the overall picture of this class of SNRs and to constrain the characteristics of the underlying population of accelerated particles. Methods. Using 6 years of Fermi-LAT P7 reprocessed data, we studied the GeV counterpart of the SNRs HESS J1731-347 and SN 1006. The two SNRs are not detected in the data set, and given that there is no hint of detection, we do not expect any detection in coming years from the SNRs. However in both cases, we derived upper limits that significantly constrain the gamma-ray emission mechanism and can rule out a standard hadronic scenario with a confidence level >5 sigma. Results. With this Fermi analysis, we now have a complete view of the HE to VHE gamma-ray emission of TeV shell SNRs. All five sources have a hard HE photon index (Gamma < 1.8), which suggests a common scenario where the bulk of the emission is produced by accelerated electrons radiating from radio to VHE gamma-rays through synchrotron and inverse Compton processes. In addition when correcting for the distance, all SNRs show a surprisingly similar gamma-ray luminosity supporting the idea of a common emission mechanism. While the gamma-ray emission is likely to be leptonic-dominated at the scale of the whole SNR, this does not rule out efficient hadron acceleration in those objects. C1 [Acero, F.; Ballet, J.] Univ Paris Diderot, CNRS, CEA IRFU, Lab AIM,Serv Astrophys,CEA Saclay, F-91191 Gif Sur Yvette, France. [Lemoine-Goumard, M.; Rousseau, R.] Univ Bordeaux, CNRS, IN2P3, Ctr Etud Nucl Bordeaux Gradignan, F-33175 Gradignan, France. [Renaud, M.] Univ Montpellier 2, Lab Univers & Particules Montpellier, CNRS, IN2P3, F-34090 Montpellier, France. [Hewitt, J. W.] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA. [Hewitt, J. W.] Univ Maryland Baltimore Cty, Ctr Space Sci & Technol, Baltimore, MD 21250 USA. [Hewitt, J. W.] CRESST, Greenbelt, MD 20771 USA. [Hewitt, J. W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Tanaka, T.] Kyoto Univ, Grad Sch Sci, Dept Phys, Kyoto 6068501, Japan. RP Acero, F (reprint author), Univ Paris Diderot, CNRS, CEA IRFU, Lab AIM,Serv Astrophys,CEA Saclay, F-91191 Gif Sur Yvette, France. EM fabio.acero@cea.fr FU Instituto Nazionale di Astrofisica in Italy; Centre National d'Etudes Spatiales in France FX The Fermi-LAT Collaboration acknowledges generous ongoing support from a number of agencies and institutes that have supported both the development and the operation of the LAT, as well as scientific data analysis. These include the National Aeronautics and Space Administration and the Department of Energy in the United States, the Commissariat a l'Energie Atomique and the Centre National de la Recherche Scientifique/Institut National de Physique Nucleaire et de Physique des Particules in France, the Agenzia Spaziale Italiana, the Istituto Nazionale di Fisica Nucleare, and the Istituto Nazionale di Astrofisica in Italy, the Ministry of Education, Culture, Sports, Science and Technology (MEXT), High Energy Accelerator Research Organization (KEK) and Japan Aerospace Exploration Agency (JAXA) in Japan, and the K. A. Wallenberg Foundation and the Swedish National Space Board in Sweden. Additional support for science analysis during the operations phase from the following agencies is also gratefully acknowledged: the Instituto Nazionale di Astrofisica in Italy and the Centre National d'Etudes Spatiales in France. NR 58 TC 11 Z9 11 U1 0 U2 1 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 EI 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD AUG PY 2015 VL 580 AR A74 DI 10.1051/0004-6361/201525932 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CP6TD UT WOS:000360020200074 ER PT J AU Ade, PAR Aghanim, N Arnaud, M Ashdown, M Aumont, J Baccigalupi, C Banday, AJ Barreiro, RB Battaner, E Benabed, K Benoit-Levy, A Bernard, JP Bersanelli, M Bielewicz, P Bond, JR Borrill, J Bouchet, FR Burigana, C Butler, RC Calabrese, E Chamballu, A Chiang, HC Christensen, PR Clements, DL Colombo, LPL Couchot, F Curto, A Cuttaia, F Danese, L Davies, RD Davis, RJ de Bernardis, P de Rosa, A de Zotti, G Delabrouille, J Diego, JM Dole, H Dore, O Dupac, X Ensslin, TA Eriksen, HK Fabre, O Finelli, F Forni, O Frailis, M Franceschi, E Galeotta, S Galli, S Ganga, K Giard, M Gonzalez-Nuevo, J Gorski, KM Gregorio, A Gruppuso, A Hansen, FK Hanson, D Harrison, DL Henrot-Versille, S Hernandez-Monteagudo, C Herranz, D Hildebrandt, SR Hivon, E Hobson, M Holmes, WA Hornstrup, A Hovest, W Huffenberger, KM Jaffe, AH Jones, WC Keihanen, E Keskitalo, R Kneissl, R Knoche, J Kunz, M Kurki-Suonio, H Lamarre, JM Lasenby, A Lawrence, CR Leonardi, R Lesgourgues, J Liguori, M Lilje, PB Linden-Vornle, M Lopez-Caniego, M Lubin, PM Macias-Perez, JF Mandolesi, N Maris, M Martin, PG Martinez-Gonzalez, E Masi, S Matarrese, S Mazzotta, P Meinhold, PR Melchiorri, A Mendes, L Menegoni, E Mennella, A Migliaccio, M Miville-Deschenes, MA Moneti, A Montier, L Morgante, G Moss, A Munshi, D Murphy, JA Naselsky, P Nati, F Natoli, P Norgaard-Nielsen, HU Noviello, F Novikov, D Novikov, I Oxborrow, CA Pagano, L Pajot, F Paoletti, D Pasian, F Patanchon, G Perdereau, O Perotto, L Perrotta, F Piacentini, F Piat, M Pierpaoli, E Pietrobon, D Plaszczynski, S Pointecouteau, E Polenta, G Ponthieu, N Popa, L Pratt, GW Prunet, S Rachen, JP Rebolo, R Reinecke, M Remazeilles, M Renault, C Ricciardi, S Ristorcelli, I Rocha, G Roudier, G Rusholme, B Sandri, M Savini, G Scott, D Spencer, LD Stolyarov, V Sudiwala, R Sutton, D Suur-Uski, AS Sygnet, JF Tauber, JA Tavagnacco, D Terenzi, L Toffolatti, L Tomasi, M Tristram, M Tucci, M Uzan, JP Valenziano, L Valiviita, J Van Tent, B Vielva, P Villa, F Wade, LA Yvon, D Zacchei, A Zonca, A AF Ade, P. A. R. Aghanim, N. Arnaud, M. Ashdown, M. Aumont, J. Baccigalupi, C. Banday, A. J. Barreiro, R. B. Battaner, E. Benabed, K. Benoit-Levy, A. Bernard, J. -P. Bersanelli, M. Bielewicz, P. Bond, J. R. Borrill, J. Bouchet, F. R. Burigana, C. Butler, R. C. Calabrese, E. Chamballu, A. Chiang, H. C. Christensen, P. R. Clements, D. L. Colombo, L. P. L. Couchot, F. Curto, A. Cuttaia, F. Danese, L. Davies, R. D. Davis, R. J. de Bernardis, P. de Rosa, A. de Zotti, G. Delabrouille, J. Diego, J. M. Dole, H. Dore, O. Dupac, X. Ensslin, T. A. Eriksen, H. K. Fabre, O. Finelli, F. Forni, O. Frailis, M. Franceschi, E. Galeotta, S. Galli, S. Ganga, K. Giard, M. Gonzalez-Nuevo, J. Gorski, K. M. Gregorio, A. Gruppuso, A. Hansen, F. K. Hanson, D. Harrison, D. L. Henrot-Versille, S. Hernandez-Monteagudo, C. Herranz, D. Hildebrandt, S. R. Hivon, E. Hobson, M. Holmes, W. A. Hornstrup, A. Hovest, W. Huffenberger, K. M. Jaffe, A. H. Jones, W. C. Keihaenen, E. Keskitalo, R. Kneissl, R. Knoche, J. Kunz, M. Kurki-Suonio, H. Lamarre, J. -M. Lasenby, A. Lawrence, C. R. Leonardi, R. Lesgourgues, J. Liguori, M. Lilje, P. B. Linden-Vornle, M. Lopez-Caniego, M. Lubin, P. M. Macias-Perez, J. F. Mandolesi, N. Maris, M. Martin, P. G. Martinez-Gonzalez, E. Masi, S. Matarrese, S. Mazzotta, P. Meinhold, P. R. Melchiorri, A. Mendes, L. Menegoni, E. Mennella, A. Migliaccio, M. Miville-Deschenes, M. -A. Moneti, A. Montier, L. Morgante, G. Moss, A. Munshi, D. Murphy, J. A. Naselsky, P. Nati, F. Natoli, P. Norgaard-Nielsen, H. U. Noviello, F. Novikov, D. Novikov, I. Oxborrow, C. A. Pagano, L. Pajot, F. Paoletti, D. Pasian, F. Patanchon, G. Perdereau, O. Perotto, L. Perrotta, F. Piacentini, F. Piat, M. Pierpaoli, E. Pietrobon, D. Plaszczynski, S. Pointecouteau, E. Polenta, G. Ponthieu, N. Popa, L. Pratt, G. W. Prunet, S. Rachen, J. P. Rebolo, R. Reinecke, M. Remazeilles, M. Renault, C. Ricciardi, S. Ristorcelli, I. Rocha, G. Roudier, G. Rusholme, B. Sandri, M. Savini, G. Scott, D. Spencer, L. D. Stolyarov, V. Sudiwala, R. Sutton, D. Suur-Uski, A. -S. Sygnet, J. -F. Tauber, J. A. Tavagnacco, D. Terenzi, L. Toffolatti, L. Tomasi, M. Tristram, M. Tucci, M. Uzan, J. -P. Valenziano, L. Valiviita, J. Van Tent, B. Vielva, P. Villa, F. Wade, L. A. Yvon, D. Zacchei, A. Zonca, A. CA Planck Collaboration TI Planck intermediate results XXIV. Constraints on variations in fundamental constants SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE cosmology: observations; cosmic background radiation; cosmological parameters; atomic data ID FINE-STRUCTURE CONSTANT; MICROWAVE BACKGROUND ANISOTROPIES; BARYON ACOUSTIC-OSCILLATIONS; TIME-VARIATION; PHYSICAL CONSTANTS; ANALYTIC APPROACH; HUBBLE CONSTANT; ALPHA; COSMOLOGY; UNIVERSE AB Any variation in the fundamental physical constants, more particularly in the fine structure constant, a, or in the mass of the electron, me, affects the recombination history of the Universe and cause an imprint on the cosmic microwave background angular power spectra. We show that the Planck data allow one to improve the constraint on the time variation of the fine structure constant at redshift z - 10(3) by about a factor of 5 compared to WMAP data, as well as to break the degeneracy with the Hubble constant, H-0. In addition to a, we can set a constraint on the variation in the mass of the electron, me, and in the simultaneous variation of the two constants. We examine in detail the degeneracies between fundamental constants and the cosmological parameters, in order to compare the limits obtained from Planck and WMAP and to determine the constraining power gained by including other cosmological probes. We conclude that independent time variations of the fine structure constant and of the mass of the electron are constrained by Planck to Delta alpha/alpha = (3.6 +/- 3.7) x 10(-3) and Delta m(e)/m(e) = (4 +/- 11) x 10(-3) at the 68% confidence level. We also investigate the possibility of a spatial variation of the fine structure constant. The relative amplitude of a dipolar spatial variation in a (corresponding to a gradient across our Hubble volume) is constrained to be delta alpha/alpha = (-2.4 +/- 3.7) x 10(-2). 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J.; Bernard, J. -P.; Bielewicz, P.; Forni, O.; Giard, M.; Montier, L.; Pointecouteau, E.; Ristorcelli, I.] Univ Toulouse, UPS OMP, IRAP, F-31028 Toulouse 4, France. [Battaner, E.] Univ Granada, Fac Ciencias, Dept Fis Teor & Cosmos, Granada, Spain. [Battaner, E.] Univ Granada, Inst Carlos Fis Teor & Computac 1, Granada, Spain. [Gorski, K. M.] Univ Warsaw Observ, PL-00478 Warsaw, Poland. RP Rocha, G (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. EM graca.m.rocha@jpl.nasa.gov RI Vielva, Patricio/F-6745-2014; Lopez-Caniego, Marcos/M-4695-2013; Martinez-Gonzalez, Enrique/E-9534-2015; Piacentini, Francesco/E-7234-2010; Gonzalez-Nuevo, Joaquin/I-3562-2014; Stolyarov, Vladislav/C-5656-2017; Barreiro, Rita Belen/N-5442-2014; Butler, Reginald/N-4647-2015; popa, lucia/B-4718-2012; Toffolatti, Luigi/K-5070-2014; Gruppuso, Alessandro/N-5592-2015; Herranz, Diego/K-9143-2014; Novikov, Dmitry/P-1807-2015; Valiviita, Jussi/A-9058-2016; Mazzotta, Pasquale/B-1225-2016; Kurki-Suonio, Hannu/B-8502-2016; Tomasi, Maurizio/I-1234-2016; Nati, Federico/I-4469-2016; Novikov, Igor/N-5098-2015; Colombo, Loris/J-2415-2016; Remazeilles, Mathieu/N-1793-2015; OI Vielva, Patricio/0000-0003-0051-272X; Martinez-Gonzalez, Enrique/0000-0002-0179-8590; Piacentini, Francesco/0000-0002-5444-9327; Gonzalez-Nuevo, Joaquin/0000-0003-1354-6822; Stolyarov, Vladislav/0000-0001-8151-828X; Barreiro, Rita Belen/0000-0002-6139-4272; Maris, Michele/0000-0001-9442-2754; De Zotti, Gianfranco/0000-0003-2868-2595; Butler, Reginald/0000-0003-4366-5996; Lopez-Caniego, Marcos/0000-0003-1016-9283; Paoletti, Daniela/0000-0003-4761-6147; Savini, Giorgio/0000-0003-4449-9416; Pierpaoli, Elena/0000-0002-7957-8993; Villa, Fabrizio/0000-0003-1798-861X; TERENZI, LUCA/0000-0001-9915-6379; Zacchei, Andrea/0000-0003-0396-1192; Hivon, Eric/0000-0003-1880-2733; Lilje, Per/0000-0003-4324-7794; Toffolatti, Luigi/0000-0003-2645-7386; Gruppuso, Alessandro/0000-0001-9272-5292; Herranz, Diego/0000-0003-4540-1417; Valiviita, Jussi/0000-0001-6225-3693; Mazzotta, Pasquale/0000-0002-5411-1748; Kurki-Suonio, Hannu/0000-0002-4618-3063; Tomasi, Maurizio/0000-0002-1448-6131; Nati, Federico/0000-0002-8307-5088; Colombo, Loris/0000-0003-4572-7732; Finelli, Fabio/0000-0002-6694-3269; Scott, Douglas/0000-0002-6878-9840; Frailis, Marco/0000-0002-7400-2135; Polenta, Gianluca/0000-0003-4067-9196; Sandri, Maura/0000-0003-4806-5375; Huffenberger, Kevin/0000-0001-7109-0099; Burigana, Carlo/0000-0002-3005-5796; Bouchet, Francois/0000-0002-8051-2924; Ricciardi, Sara/0000-0002-3807-4043; Masi, Silvia/0000-0001-5105-1439; Cuttaia, Francesco/0000-0001-6608-5017; Morgante, Gianluca/0000-0001-9234-7412; Remazeilles, Mathieu/0000-0001-9126-6266; Franceschi, Enrico/0000-0002-0585-6591; Valenziano, Luca/0000-0002-1170-0104; Matarrese, Sabino/0000-0002-2573-1243; Galeotta, Samuele/0000-0002-3748-5115; Pasian, Fabio/0000-0002-4869-3227 FU French state funds [ANR-11-IDEX-0004-02]; ANR VACOUL FX The development of Planck has been supported by: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MICINN, LA., and RES (Spain); Tekes, AoF, and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); and PRACE (EU). A description of the Planck Collaboration and a list of its members, including the technical or scientific activities in which they have been involved, can be found at http://www.sciops.esa.int/index.php? project=planck&page=Planck_Collaboration. Some of the results in this paper have been derived using the HEALPix package. We thank Alain Coc and Elisabeth Vangioni for discussions and S. Rouberol for running the horizon cluster, where some of the computations were performed. Some of this work was carried out at the ILP LABEX (under reference ANR-10-LABX-63) and was supported by French state funds managed by the ANR within the Investissements d'Avenir programme under reference ANR-11-IDEX-0004-02 and by the ANR VACOUL. This work was made possible thanks to the ANR Chaire d'Excellence ANR-10-CEXC-004-01. NR 116 TC 12 Z9 12 U1 6 U2 17 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD AUG PY 2015 VL 580 AR A22 DI 10.1051/0004-6361/201424496 PG 25 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CP6TD UT WOS:000360020200022 ER PT J AU Ade, PAR Aghanim, N Arnaud, M Ashdown, M Atrio-Barandela, F Aumont, J Baccigalupi, C Banday, AJ Barreiro, RB Battaner, E Benabed, K Benoit-Levy, A Bernard, JP Bersanelli, M Bielewicz, P Bobin, J Bonaldi, A Bond, JR Bouchet, FR Boulanger, F Burigana, C Cardoso, JF Catalano, A Chamballu, A Chiang, HC Christensen, PR Clements, DL Colombi, S Colombo, LPL Combet, C Couchot, F Crill, BP Cuttaia, F Danese, L Davies, RD Davis, RJ de Bernardis, P de Rosa, A de Zotti, G Delabrouille, J Dickinson, C Diego, JM Donzelli, S Dore, O Douspis, M Dupac, X Efstathiou, G Ensslin, TA Eriksen, K Finelli, F Forni, O Frailis, M Franceschi, E Galeotta, S Ganga, K Genova-Santos, RT Ghosh, T Giard, M Giardino, G Giraud-Heraud, Y Gonzalez-Nuevo, J Gorski, KM Gregorio, A Gruppuso, A Hansen, FK Harrison, DL Henrot-Versille, S Herranz, D Hildebrandt, SR Hivon, E Hobson, M Hornstrup, A Hovest, W Huffenberger, KM Jaffe, AH Jaffe, TR Jones, WC Keihanen, E Keskitalo, R Kisner, TS Kneissl, R Knoche, J Kunz, M Kurki-Suonio, H Lagache, G Lahteenmaki, A Lamarre, JM Lasenby, A Lawrence, CR Leonardi, R Liguori, M Lilje, PB Linden-Vornle, M Lopez-Caniego, M Lubin, PM Macias-Perez, F Maino, D Mandolesi, N Martin, PG Martinez-Gonzalez, E Masi, S Massardi, M Matarrese, S Mazzotta, P Meinhold, PR Melchiorri, A Mendes, L Mennella, A Migliaccio, M Mitra, S Miville-Deschenes, MA Moneti, A Montier, L Morgante, G Mortlock, D Munshi, D Murphy, JA Naselsky, P Nati, F Natoli, P Norgaard-Nielsen, HU Noviello, F Novikov, D Novikov, I Oxborrow, CA Pagano, L Pajot, F Paladini, R Paoletti, D Pasian, F Pearson, TJ Peel, M Perdereau, O Perrotta, F Piacentini, F Piat, M Pierpaoli, E Pietrobon, D Plaszczynski, S Pointecouteau, E Polenta, G Ponthieu, N Popa, L Pratt, GW Prunet, S Puget, JL Rachen, JP Reach, WT Rebolo, R Reich, W Reinecke, M Remazeilles, M Renault, C Ricciardi, S Riller, T Ristorcelli, I Rocha, G Rosset, C Roudier, G Rubino-Martin, JA Rusholme, B Sandri, M Savini, G Scott, D Spencer, LD Stolyarov, V Strong, AW Sutton, D Suur-Uski, AS Sygnet, F Tauber, JA Tavagnacco, D Terenzi, L Tibbs, CT Toffolatti, L Tomasi, M Tristram, M Tucci, M Valenziano, L Valiviita, J Van Tent, B Varis, J Vielva, P Villa, F Wade, LA Wandelt, BD Watson, R Yvon, D Zacchei, A Zonca, A AF Ade, P. A. R. Aghanim, N. Arnaud, M. Ashdown, M. Atrio-Barandela, F. Aumont, J. Baccigalupi, C. Banday, A. J. Barreiro, R. B. Battaner, E. Benabed, K. Benoit-Levy, A. Bernard, J-P. Bersanelli, M. Bielewicz, P. Bobin, J. Bonaldi, A. Bond, J. R. Bouchet, F. R. Boulanger, F. Burigana, C. Cardoso, J-F. Catalano, A. Chamballu, A. Chiang, H. C. Christensen, P. R. Clements, D. L. Colombi, S. Colombo, L. P. L. Combet, C. Couchot, F. Crill, B. P. Cuttaia, F. Danese, L. Davies, R. D. Davis, R. J. de Bernardis, P. de Rosa, A. de Zotti, G. Delabrouille, J. Dickinson, C. Diego, J. M. Donzelli, S. Dore, O. Douspis, M. Dupac, X. Efstathiou, G. Ensslin, T. A. Eriksen, K. Finelli, F. Forni, O. Frailis, M. Franceschi, E. Galeotta, S. Ganga, K. Genova-Santos, R. T. Ghosh, T. Giard, M. Giardino, G. Giraud-Heraud, Y. Gonzalez-Nuevo, J. Gorski, K. M. Gregorio, A. Gruppuso, A. Hansen, F. K. Harrison, D. L. Henrot-Versille, S. Herranz, D. Hildebrandt, S. R. Hivon, E. Hobson, M. Hornstrup, A. Hovest, W. Huffenberger, K. M. Jaffe, A. H. Jaffe, T. R. Jones, W. C. Keihanen, E. Keskitalo, R. Kisner, T. S. Kneissl, R. Knoche, J. Kunz, M. Kurki-Suonio, H. Lagache, G. Laehteenmaki, A. Lamarre, J-M. Lasenby, A. Lawrence, C. R. Leonardi, R. Liguori, M. Lilje, P. B. Linden-Vornle, M. Lopez-Caniego, M. Lubin, P. M. Macias-Perez, F. Maino, D. Mandolesi, N. Martin, P. G. Martinez-Gonzalez, E. Masi, S. Massardi, M. Matarrese, S. Mazzotta, P. Meinhold, P. R. Melchiorri, A. Mendes, L. Mennella, A. Migliaccio, M. Mitra, S. Miville-Deschenes, M-A Moneti, A. Montier, L. Morgante, G. Mortlock, D. Munshi, D. Murphy, J. A. Naselsky, P. Nati, F. Natoli, P. Norgaard-Nielsen, H. U. Noviello, F. Novikov, D. Novikov, I. Oxborrow, C. A. Pagano, L. Pajot, F. Paladini, R. Paoletti, D. Pasian, F. Pearson, T. J. Peel, M. Perdereau, O. Perrotta, F. Piacentini, F. Piat, M. Pierpaoli, E. Pietrobon, D. Plaszczynski, S. Pointecouteau, E. Polenta, G. Ponthieu, N. Popa, L. Pratt, G. W. Prunet, S. Puget, J-L. Rachen, J. P. Reach, W. T. Rebolo, R. Reich, W. Reinecke, M. Remazeilles, M. Renault, C. Ricciardi, S. Riller, T. Ristorcelli, I. Rocha, G. Rosset, C. Roudier, G. Rubino-Martin, J. A. Rusholme, B. Sandri, M. Savini, G. Scott, D. Spencer, L. D. Stolyarov, V. Strong, A. W. Sutton, D. Suur-Uski, A-S. Sygnet, J-F. Tauber, J. A. Tavagnacco, D. Terenzi, L. Tibbs, C. T. Toffolatti, L. Tomasi, M. Tristram, M. Tucci, M. Valenziano, L. Valiviita, J. Van Tent, B. Varis, J. Vielva, P. Villa, F. Wade, L. A. Wandelt, B. D. Watson, R. Yvon, D. Zacchei, A. Zonca, A. CA Planck Collaboration TI Planck intermediate results XXIII. Galactic plane emission components derived from Planck with ancillary data SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE ISM: general; Galaxy: general; radiation mechanisms: general; radio continuum: ISM; submillimeter: ISM; Galaxy: disk ID MICROWAVE-ANISOTROPY-PROBE; RECOMBINATION LINE EMISSION; RADIO-CONTINUUM SURVEY; LARGE-AREA TELESCOPE; PRE-LAUNCH STATUS; SPINNING DUST GRAINS; DIFFUSE IONIZED-GAS; GAMMA-RAY EMISSION; MILKY-WAY; SYNCHROTRON EMISSION AB Planck data when combined with ancillary data provide a unique opportunity to separate the diffuse emission components of the inner Galaxy. The purpose of the paper is to elucidate the morphology of the various emission components in the strong star-formation region lying inside the solar radius and to clarify the relationship between the various components. The region of the Galactic plane covered is 1 = 300 degrees -> 0 degrees -> 60 degrees where star-formation is highest and the emission is strong enough to make meaningful component separation. The latitude widths in this longitude range lie between 1 and 2, which correspond to FWHM z-widths of 100-200 pc at a typical distance of 6 kpc. The four emission components studied here are synchrotron, free-free, anomalous microwave emission (AME), and thermal (vibrational) dust emission. These components are identified by constructing spectral energy distributions (SEDs) at positions along the Galactic plane using the wide frequency coverage of Planck (28.4-857 GHz) in combination with low-frequency radio data at 0.408-2.3 GHz plus WMAP data at 23-94 GHz, along with far-infrared (FIR) data from COBE-DIRBE and IRAS. The free-free component is determined from radio recombination line (RRL) data. AME is found to be comparable in brightness to the free-free emission on the Galactic plane in the frequency range 20-40 GHz with a width in latitude similar to that of the thermal dust; it comprises 45 +/- 1% of the total 28.4 GHz emission in the longitude range 1 = 300 degrees -> 0 degrees -> 60 degrees. The free-free component is the narrowest, reflecting the fact that it is produced by current star-formation as traced by the narrow distribution of OB stars. It is the dominant emission on the plane between 60 and 100 GHz. RRLs from this ionized gas are used to assess its distance, leading to a free-free z-width of FWHM approximate to 100 pc. The narrow synchrotron component has a low-frequency brightness spectral index beta(synch) approximate to -2.7 that is similar to the broad synchrotron component indicating that they are both populated by the cosmic ray electrons of the same spectral index. The width of this narrow synchrotron component is significantly larger than that of the other three components, suggesting that it is generated in an assembly of older supernova remnants that have expanded to sizes of order 150 pc in 3 x 10(5) yr; pulsars of a similar age have a similar spread in latitude. The thermal dust is identified in the SEDs with average parameters of T-dust = 20.4 +/- 0.4 K, beta(FIR) = 1.94 +/- 0.03 (>353 GHz), and beta(mm) = 1.67 +/- 0.02 (<353 GHz). The latitude distributions of gamma-rays, CO, and the emission in high-frequency Planck bands have similar widths, showing that they are all indicators of the total gaseous matter on the plane in the inner Galaxy. C1 [Cardoso, J-F.; Delabrouille, J.; Ganga, K.; Giraud-Heraud, Y.; Piat, M.; Remazeilles, M.; Rosset, C.; Roudier, G.] Univ Paris Diderot, CNRS IN2P3, Sorbonne Paris Cite, APC,CEA Irfu,Observatoire Paris, F-75205 Paris 13, France. 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[Ensslin, T. A.; Hovest, W.; Knoche, J.; Rachen, J. P.; Reinecke, M.; Riller, T.] Max Planck Inst Astrophys, D-85741 Garching, Germany. [Strong, A. W.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Reich, W.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Varis, J.] VTT Tech Res Ctr Finland, MilliLab, Espoo 02044, Finland. [Murphy, J. A.] Natl Univ Ireland, Dept Expt Phys, Maynooth, Kildare, Ireland. [Christensen, P. R.; Naselsky, P.; Novikov, I.] Niels Bohr Inst, DK-2100 Copenhagen, Denmark. [Crill, B. P.] CALTECH, Observat Cosmol, Pasadena, CA 91125 USA. [Savini, G.] UCL, Optic Sci Lab, London WC1E 6BT, England. [Baccigalupi, C.; Bielewicz, P.; Danese, L.; de Zotti, G.; Gonzalez-Nuevo, J.; Perrotta, F.] SISSA, Astrophys Sector, I-34136 Trieste, Italy. [Ade, P. A. R.; Munshi, D.; Spencer, L. D.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Stolyarov, V.] Russian Acad Sci, Special Astrophys Observ, Karachai Cherkessian Rep 369167, Zelenchukskiy R, Russia. [Benabed, K.; Benoit-Levy, A.; Bouchet, F. R.; Colombi, S.; Hivon, E.; Prunet, S.; Wandelt, B. D.] Univ Paris 06, UMR7095, F-75014 Paris, France. [Banday, A. J.; Bernard, J-P.; Bielewicz, P.; Forni, O.; Giard, M.; Jaffe, T. R.; Montier, L.; Pointecouteau, E.; Ristorcelli, I.] Univ Toulouse, UPS OMP, IRAP, F-31028 Toulouse 4, France. [Reach, W. T.] Univ Space Res Assoc, Stratospher Observ Infrared Astron, Moffett Field, CA 94035 USA. [Battaner, E.] Univ Granada, Fac Ciencias, Dept Fis Teor & Cosmos, E-18071 Granada, Spain. [Gorski, K. M.] Univ Warsaw Observ, PL-00478 Warsaw, Poland. RP Davies, RD (reprint author), Univ Manchester, Jodrell Bank Ctr Astrophys, Sch Phys & Astron, Alan Turing Bldg,Oxford Rd, Manchester M13 9PL, Lancs, England. EM Rodney.Davies@manchester.ac.uk RI Remazeilles, Mathieu/N-1793-2015; Colombo, Loris/J-2415-2016; popa, lucia/B-4718-2012; Vielva, Patricio/F-6745-2014; Pearson, Timothy/N-2376-2015; Lopez-Caniego, Marcos/M-4695-2013; Martinez-Gonzalez, Enrique/E-9534-2015; Piacentini, Francesco/E-7234-2010; Gonzalez-Nuevo, Joaquin/I-3562-2014; Atrio-Barandela, Fernando/A-7379-2017; Stolyarov, Vladislav/C-5656-2017; Barreiro, Rita Belen/N-5442-2014; Lahteenmaki, Anne/L-5987-2013; Nati, Federico/I-4469-2016; Novikov, Igor/N-5098-2015; Toffolatti, Luigi/K-5070-2014; Gruppuso, Alessandro/N-5592-2015; Herranz, Diego/K-9143-2014; Novikov, Dmitry/P-1807-2015; Valiviita, Jussi/A-9058-2016; Mazzotta, Pasquale/B-1225-2016; Kurki-Suonio, Hannu/B-8502-2016; Ghosh, Tuhin/E-6899-2016; Tomasi, Maurizio/I-1234-2016 OI Watson, Robert/0000-0002-5873-0124; Zacchei, Andrea/0000-0003-0396-1192; Hivon, Eric/0000-0003-1880-2733; Lilje, Per/0000-0003-4324-7794; Paoletti, Daniela/0000-0003-4761-6147; Savini, Giorgio/0000-0003-4449-9416; Bouchet, Francois/0000-0002-8051-2924; Ricciardi, Sara/0000-0002-3807-4043; Villa, Fabrizio/0000-0003-1798-861X; TERENZI, LUCA/0000-0001-9915-6379; Reach, William/0000-0001-8362-4094; Matarrese, Sabino/0000-0002-2573-1243; Galeotta, Samuele/0000-0002-3748-5115; Pasian, Fabio/0000-0002-4869-3227; Finelli, Fabio/0000-0002-6694-3269; Frailis, Marco/0000-0002-7400-2135; Lopez-Caniego, Marcos/0000-0003-1016-9283; Polenta, Gianluca/0000-0003-4067-9196; Sandri, Maura/0000-0003-4806-5375; Huffenberger, Kevin/0000-0001-7109-0099; Burigana, Carlo/0000-0002-3005-5796; Peel, Mike/0000-0003-3412-2586; Scott, Douglas/0000-0002-6878-9840; Masi, Silvia/0000-0001-5105-1439; Cuttaia, Francesco/0000-0001-6608-5017; Morgante, Gianluca/0000-0001-9234-7412; Remazeilles, Mathieu/0000-0001-9126-6266; Franceschi, Enrico/0000-0002-0585-6591; Valenziano, Luca/0000-0002-1170-0104; Pierpaoli, Elena/0000-0002-7957-8993; Colombo, Loris/0000-0003-4572-7732; Vielva, Patricio/0000-0003-0051-272X; Pearson, Timothy/0000-0001-5213-6231; Martinez-Gonzalez, Enrique/0000-0002-0179-8590; Piacentini, Francesco/0000-0002-5444-9327; Gonzalez-Nuevo, Joaquin/0000-0003-1354-6822; Atrio-Barandela, Fernando/0000-0002-2130-2513; Stolyarov, Vladislav/0000-0001-8151-828X; Barreiro, Rita Belen/0000-0002-6139-4272; De Zotti, Gianfranco/0000-0003-2868-2595; Nati, Federico/0000-0002-8307-5088; Toffolatti, Luigi/0000-0003-2645-7386; Gruppuso, Alessandro/0000-0001-9272-5292; Herranz, Diego/0000-0003-4540-1417; Valiviita, Jussi/0000-0001-6225-3693; Mazzotta, Pasquale/0000-0002-5411-1748; Kurki-Suonio, Hannu/0000-0002-4618-3063; Tomasi, Maurizio/0000-0002-1448-6131 FU NASA Office of Space Science; STFC [ST/L000768/1]; European Research Council under the European Union's Seventh Framework Programme (FP7)/ERC [267934, 307209] FX 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. Some of the results in this paper have been derived using the HEALPix package The development of Planck has been supported by: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MICINN, JA and RES (Spain); Tekes, AoF and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); and PRACE (EU). The research leading to these results has received funding from an STFC Consolidated Grant (No. ST/L000768/1), as well as the European Research Council under the European Union's Seventh Framework Programme (FP7/2007-2013)/ERC grant agreement Nos. 267934 and 307209. A description of the Planck Collaboration and a list of its members, including the technical or scientific activities in which they have been involved, can be found at http://www.sciops.esa.int/index.php? project=planck&page=Planck_Collaboration. NR 170 TC 0 Z9 0 U1 3 U2 11 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD AUG PY 2015 VL 580 AR A13 DI 10.1051/0004-6361/201424434 PG 27 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CP6TD UT WOS:000360020200013 ER PT J AU Bihr, S Beuther, H Ott, J Johnston, KG Brunthaler, A Anderson, LD Bigiel, F Carlhoff, P Churchwell, E Glover, SCO Goldsmith, PF Heitsch, F Henning, T Heyer, MH Hill, T Hughes, A Klessen, RS Linz, H Longmore, SN McClure-Griffiths, NM Menten, KM Motte, F Nguyen-Lu'o'Ng, Q Plume, R Ragan, SE Roy, N Schilke, P Schneider, N Smith, RJ Stil, JM Urquhart, JS Walsh, AJ Walter, F AF Bihr, S. Beuther, H. Ott, J. Johnston, K. G. Brunthaler, A. Anderson, L. D. Bigiel, F. Carlhoff, P. Churchwell, E. Glover, S. C. O. Goldsmith, P. F. Heitsch, F. Henning, T. Heyer, M. H. Hill, T. Hughes, A. Klessen, R. S. Linz, H. Longmore, S. N. McClure-Griffiths, N. M. Menten, K. M. Motte, F. Nguyen-Lu'o'ng, Q. Plume, R. Ragan, S. E. Roy, N. Schilke, P. Schneider, N. Smith, R. J. Stil, J. M. Urquhart, J. S. Walsh, A. J. Walter, F. TI THOR: The HI, OH, Recombination line survey of the Milky Way The pilot study: HI observations of the giant molecular cloud W43 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE ISM: clouds; ISM: structure; ISM: atoms; stars: formation; radio lines: ISM; surveys ID GALACTIC PLANE SURVEY; NARROW SELF-ABSORPTION; NEUTRAL ATOMIC PHASES; INFRARED DARK CLOUDS; MASS STAR-FORMATION; I-21 CM ABSORPTION; HIGH-RESOLUTION; MINI-STARBURST; EXTRAGALACTIC SOURCES; INTERSTELLAR-MEDIUM AB To study the atomic, molecular, and ionized emission of giant molecular clouds (GMCs) in the Milky Way, we initiated a large program with the Karl G. Jansky Very Large Array (VLA): "THOR: The HI, OH, Recombination line survey of the Milky Way". We map the 21 cm HI line, 4 OH lines, up to 19 H alpha recombination lines and the continuum from 1 to 2 GHz of a significant fraction of the Milky Way (l = 15 degrees-67 degrees, vertical bar b vertical bar <= 1 degrees) at an angular resolution of similar to 20 ''. Starting in 2012, as a pilot study we mapped 4 square degrees of the GMC associated with the W43 star formation complex. The rest of the THOR survey area was observed during 2013 and 2014. In this paper, we focus on the Hi emission from the W43 GMC complex. Classically, the HI 21 cm line is treated as optically thin with properties such as the column density calculated under this assumption. This approach might yield reasonable results for regions of low-mass star formation, however, it is not sufficient to describe GMCs. We analyzed strong continuum sources to measure the optical depth along the line of sight, and thus correct the HI 21 cm emission for optical depth effects and weak diffuse continuum emission. Hence, we are able to measure the Hi mass of this region more accurately and our analysis reveals a lower limit for the HI mass of M = 6.6(-1.8) x 10(6) M-circle dot (nu(LSR) = 60-120 km s(-1)), which is a factor of 2.4 larger than the mass estimated with the assumption of optically thin emission. The HI column densities are as high as N-HI similar to 150 M-circle dot pc(-2) approximate to 1.9 x 10(22) cm(-2), which is an order of magnitude higher than for low-mass star formation regions. This result challenges theoretical models that predict a threshold for the HI column density of similar to 10 M-circle dot pc(-2), at which the formation of molecular hydrogen should set in. By assuming an elliptical layered structure for W43, we estimate the particle density profile. For the atomic gas particle density, we find a linear decrease toward the center of W43 with values decreasing from n(HI) = 20 cm(-3) near the cloud edge to almost 0 cm(-3) at its center. On the other hand, the molecular hydrogen, traced via dust observations with the Herschel Space Observatory, shows an exponential increase toward the center with densities increasing to n(H2) > 200 cm(-3), averaged over a region of similar to 10 pc. While atomic and molecular hydrogen are well mixed at the cloud edge, the center of the cloud is strongly dominated by H-2 emission. We do not identify a sharp transition between hydrogen in atomic and molecular form. Our results, which challenge current theoretical models, are an important characterization of the atomic to molecular hydrogen transition in an extreme environment. C1 [Bihr, S.; Beuther, H.; Henning, T.; Hughes, A.; Linz, H.; Ragan, S. E.; Walter, F.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Ott, J.] Natl Radio Astron Observ, Socorro, NM 87801 USA. [Johnston, K. G.] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England. [Brunthaler, A.; Menten, K. M.; Roy, N.; Urquhart, J. S.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Anderson, L. D.] W Virginia Univ, Dept Phys & Astron, Morgantown, WV 26506 USA. [Bigiel, F.; Glover, S. C. O.; Klessen, R. S.; Smith, R. J.] Heidelberg Univ, Inst Theoret Astrophys, Zentrum Astron, D-69120 Heidelberg, Germany. [Carlhoff, P.; Schilke, P.] Univ Cologne, Inst Phys 1, D-50937 Cologne, Germany. [Churchwell, E.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. [Goldsmith, P. F.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Heitsch, F.] Univ N Carolina, Dept Phys & Astron, Chapel Hill, NC 27599 USA. [Heyer, M. H.] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. [Hill, T.] Joint ALMA Observ, Santiago 7630355, Chile. [Klessen, R. S.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, SLAC Natl Accelerator Lab, Menlo Pk, CA 94025 USA. [Klessen, R. S.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Longmore, S. N.] Liverpool John Moores Univ, Astrophys Res Inst, Liverpool L3 5RF, Merseyside, England. [McClure-Griffiths, N. M.] CSIRO Astron & Space Sci, Australia Telescope Natl Facil, Marsfield, NSW 2122, Australia. [Motte, F.] Univ Paris Diderot, CEA, CNRS, DSM,Lab AIM,IRFU,Serv Astrophys, F-91191 Gif Sur Yvette, France. [Nguyen-Lu'o'ng, Q.] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada. [Plume, R.; Stil, J. M.] Univ Calgary, Dept Phys & Astron, Calgary, AB T2N 1N4, Canada. [Roy, N.] Indian Inst Technol Kharagpur, Dept Phys, Kharagpur 721302, W Bengal, India. [Schneider, N.] Univ Bordeaux, CNRS, INSU, Lab Astrophys Bordeaux, F-33270 Floirac, France. [Walsh, A. J.] Curtin Univ, Int Ctr Radio Astron Res, Perth, WA 6845, Australia. RP Bihr, S (reprint author), Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany. EM bihr@mpia.de; beuther@mpia.de; henning@mpia.de; hughes@mpia.de; linz@mpia.de; ragan@mpia.de; walter@mpia.de RI Walsh, Andrew/B-5627-2013; Goldsmith, Paul/H-3159-2016; OI Walsh, Andrew/0000-0001-9506-0855; Ragan, Sarah/0000-0003-4164-5588; McClure-Griffiths, Naomi/0000-0003-2730-957X FU Deutsche Forschungsgemeinschaft (DFG) via the Heidelberg Sonderforschungsbereich [SFB 881]; Schwerpunktprogramm SPP 1573 "Physics of the Interstellar Medium"; European Research Council under the European Community via the ERC Advanced Grant STARLIGHT [339177]; International Max Planck Research School for Astronomy and Cosmic Physics (IMPRS) at the University of Heidelberg FX We like to thank the anonymous referee for an excellent report with a lot of helpful comments that improved the paper. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. R.S.K., S.C.O.G., R.J.S., and S.E.R. acknowledge financial support by the Deutsche Forschungsgemeinschaft (DFG) via the Heidelberg Sonderforschungsbereich SFB 881 The Milky Way System (subprojects B1, B2, and B8) as well as the Schwerpunktprogramm SPP 1573 "Physics of the Interstellar Medium". R.S.K. further acknowledges support from the European Research Council under the European Communitys Seventh Framework Programme (FP7/2007-2013) via the ERC Advanced Grant STARLIGHT (project number 339177). We gratefully acknowledge help from the team of the Pete V. Domenici Science Operations Center (SOC) in Socorro for their help on data reduction during an extended visit in 2013. S.B. is a fellow of the International Max Planck Research School for Astronomy and Cosmic Physics (IMPRS) at the University of Heidelberg and acknowledges support. NR 67 TC 10 Z9 10 U1 1 U2 2 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 EI 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD AUG PY 2015 VL 580 AR A112 DI 10.1051/0004-6361/201425370 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CP6TD UT WOS:000360020200112 ER PT J AU Guerlet, S Fouchet, T Vinatier, S Simon, AA Dartois, E Spiga, A AF Guerlet, S. Fouchet, T. Vinatier, S. Simon, A. A. Dartois, E. Spiga, A. TI Stratospheric benzene and hydrocarbon aerosols detected in Saturn's auroral regions SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE planets and satellites: gaseous planets; planets and satellites: atmospheres; planets and satellites: composition; planets and satellites: aurorae ID HUBBLE-SPACE-TELESCOPE; HAZE FORMATION; MERIDIONAL DISTRIBUTION; CIRS/CASSINI LIMB; POLAR ATMOSPHERE; CLOUD STRUCTURE; EVOLUTION; JUPITER; SYSTEM; TEMPERATURES AB Context. Saturn's polar upper atmosphere exhibits significant auroral activity; however, its impact on stratospheric chemistry (i.e. the production of benzene and heavier hydrocarbons) and thermal structure remains poorly documented. Aims. We aim to bring new constraints on the benzene distribution in Saturn's stratosphere, to characterize polar aerosols (their vertical distribution, composition, thermal infrared optical properties), and to quantify the aerosols' radiative impact on the thermal structure. Methods. Infrared spectra acquired by the Composite Infrared Spectrometer (CIRS) on board Cassini in limb viewing geometry are analysed to derive benzene column abundances and aerosol opacity profiles over the 3 to 0.1 mbar pressure range. The spectral dependency of the haze opacity is assessed in the ranges 680-900 and 1360-1440 cm(-1). Then, a radiative climate model is used to compute equilibrium temperature profiles, with and without haze, given the haze properties derived from CIRS measurements. Results. On Saturn's auroral region (80 degrees S), benzene is found to be slightly enhanced compared to its equatorial and mid-latitude values. This contrasts with the Moses & Greathouse (2005, J. Geophys. Res., 110, 9007) photochemical model, which predicts a benzene abundance 50 times lower at 80 degrees S than at the equator. This advocates for the inclusion of ion-related reactions in Saturn's chemical models. The polar stratosphere is also enriched in aerosols, with spectral signatures consistent with vibration modes assigned to aromatic and aliphatic hydrocarbons, and presenting similarities with the signatures observed in Titan's stratosphere. The aerosol mass loading at 80 degrees S is estimated to be 1-4 x 10(-5) g cm(-2), an order of magnitude less than on Jupiter, which is consistent with the order of magnitude weaker auroral power at Saturn. We estimate that this polar haze warms the middle stratosphere by 6 K in summer and cools the upper stratosphere by 5 K in winter. Hence, aerosols linked with auroral activity can partly account for the warm polar hood observed in Saturn's summer stratosphere. C1 [Guerlet, S.; Spiga, A.] UPMC Paris 06, Univ Sorbonne, UMR 8539, LMD, F-75005 Paris, France. [Guerlet, S.; Spiga, A.] CNRS, Lab Meteorol Dynam, IPSL, UMR 8539, F-75005 Paris, France. [Fouchet, T.] UPMC Paris 06, Univ Sorbonne, UMR 8109, LESIA, F-75005 Paris, France. [Fouchet, T.; Vinatier, S.] Univ Paris Diderot, UPMC, CNRS, LESIA,Observ Paris, F-92195 Meudon, France. [Simon, A. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Dartois, E.] CNRS INSU, Inst Astrophys Spatiale, UMR 8617, F-91405 Orsay, France. RP Guerlet, S (reprint author), UPMC Paris 06, Univ Sorbonne, UMR 8539, LMD, F-75005 Paris, France. EM sandrine.guerlet@lmd.jussieu.fr RI Simon, Amy/C-8020-2012; Spiga, Aymeric/O-4858-2014; Fouchet, Thierry/C-6374-2017 OI Simon, Amy/0000-0003-4641-6186; Spiga, Aymeric/0000-0002-6776-6268; Fouchet, Thierry/0000-0001-9040-8285 FU French ANR [ANR-12-PDOC-0013]; Institut Universitaire de France FX S. Guerlet acknowledges funding by the French ANR under grant agreement ANR-12-PDOC-0013. T. Fouchet acknowledges funding by the Institut Universitaire de France. We thank Julie Moses and Jim Friedson for discussions on aerosol formation and Conor Nixon for discussions on aliasing effects in CIRS spectra, and an anonymous referee whose comments helped to improve the manuscript. We also thank the CIRS operation and calibration team for their hard work. NR 34 TC 2 Z9 2 U1 1 U2 6 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 EI 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD AUG PY 2015 VL 580 AR A89 DI 10.1051/0004-6361/201424745 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CP6TD UT WOS:000360020200089 ER PT J AU Langer, WD Pineda, JL AF Langer, W. D. Pineda, J. L. TI [C II] emission from galactic nuclei in the presence of X-rays SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE Galaxy: center; X-rays: ISM; ISM: general; atomic processes ID PHOTOIONIZATION CROSS-SECTIONS; DIELECTRONIC RECOMBINATION DATA; SPACE-OBSERVATORY MEASUREMENTS; FINITE-DENSITY PLASMAS; STAR-FORMATION RATE; 158 MU-M; INTERSTELLAR-MEDIUM; INFRARED GALAXIES; MASSIVE STARS; COLLISIONAL EXCITATION AB Context. The luminosity of [C II] is used as a probe of the star formation rate in galaxies, but the correlation breaks down in some active galactic nuclei (AGNs). Models of the [C II] emission from galactic nuclei do not include the influence of X-rays on the carbon ionization balance, which may be a factor in reducing the [C II] luminosity. Aims. We aim to determine the properties of the ionized carbon and its distribution among highly ionized states in the interstellar gas in galactic nuclei under the influence of X-ray sources. We calculate the [C II] luminosity in galactic nuclei under the influence of bright sources of soft X-rays. Methods. We solve the balance equation of the ionization states of carbon as a function of X-ray flux, electron, atomic hydrogen, and molecular hydrogen density. These are input to models of [C II] emission from the interstellar medium (ISM) in galactic nuclei representing conditions in the Galactic central molecular zone and a higher density AGN model. The behavior of the [C II] luminosity is calculated as a function of the X-ray luminosity. We also solve the distribution of the ionization states of oxygen and nitrogen in highly ionized regions. Results. We find that the dense warm ionized medium (WIM) and dense photon dominated regions (PDRs) dominate the [C ii] emission when no X-rays are present. The X-rays in galactic nuclei can affect strongly the C+ abundance in the WIM, converting some fraction to C2+ and higher ionization states and thus reducing its [C II] luminosity. For an X-ray luminosity L(X-ray) greater than or similar to 10(43) erg s(-1) the [C II] luminosity can be suppressed by a factor of a few, and for very strong sources, L(X-ray) > 10(44) erg s(-1) such as found for many AGNs, the [C II] luminosity is significantly depressed. Comparison of the model with several extragalactic sources shows that the [C II] to far-infrared ratio declines for L(X-ray) greater than or similar to 10(43) erg s(-1), in reasonable agreement with our model. Conclusions. We conclude that X-rays can suppress the C+ abundance and, therefore, the [C II] luminosity of the ISM in active galactic nuclei with a large X-ray flux. The X-ray flux can arise from a central massive accreting black hole and/or from many smaller discrete sources distributed throughout the nuclei. We also find that the lower ionization states of nitrogen and oxygen are also suppressed at high X-ray fluxes in warm ionized gas. C1 [Langer, W. D.; Pineda, J. L.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Langer, WD (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM William.Langer@jpl.nasa.gov OI Pineda, Jorge/0000-0001-8898-2800 NR 72 TC 7 Z9 7 U1 0 U2 1 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 EI 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD AUG PY 2015 VL 580 AR A5 DI 10.1051/0004-6361/201525950 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CP6TD UT WOS:000360020200005 ER PT J AU Anderson, JD Schubert, G Trimble, V Feldman, MR AF Anderson, J. D. Schubert, G. Trimble, V. Feldman, M. R. TI Comment on "Measurements of Newton's gravitational constant and the length of day" by Anderson J. D. et al. Reply SO EPL LA English DT Editorial Material C1 [Anderson, J. D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Schubert, G.] Univ Calif Los Angeles, Dept Earth Planetary & Space Sci, Los Angeles, CA 90095 USA. [Trimble, V.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. RP Anderson, JD (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. OI Feldman, Michael/0000-0003-1567-9725 NR 3 TC 4 Z9 4 U1 0 U2 7 PU EPL ASSOCIATION, EUROPEAN PHYSICAL SOCIETY PI MULHOUSE PA 6 RUE DES FRERES LUMIERE, MULHOUSE, 68200, FRANCE SN 0295-5075 EI 1286-4854 J9 EPL-EUROPHYS LETT JI EPL PD AUG PY 2015 VL 111 IS 3 AR 30003 DI 10.1209/0295-5075/111/30003 PG 2 WC Physics, Multidisciplinary SC Physics GA CQ8BE UT WOS:000360830300003 ER PT J AU Witting, D Ford, T Wang, S Neuman, M Reynolds, A AF Witting, David Ford, Tom Wang, Susan Neuman, Melissa Reynolds, Ariadne TI SPAWNING AND OUTPLANTING TECHNIQUE DEVELOPMENT FOR GREEN ABALONE (HALIOTIS FULGENS) RESTORATION IN SOUTHERN CALIFORNIA SO JOURNAL OF SHELLFISH RESEARCH LA English DT Meeting Abstract C1 [Witting, David; Wang, Susan] Natl Marine Fisheries Serv, Long Beach, CA 90802 USA. [Ford, Tom; Neuman, Melissa; Reynolds, Ariadne] Bay Fdn, Los Angeles, CA 90045 USA. NR 0 TC 0 Z9 0 U1 2 U2 9 PU NATL SHELLFISHERIES ASSOC PI GROTON PA C/O DR. SANDRA E. SHUMWAY, UNIV CONNECTICUT, 1080 SHENNECOSSETT RD, GROTON, CT 06340 USA SN 0730-8000 EI 1943-6319 J9 J SHELLFISH RES JI J. Shellfish Res. PD AUG PY 2015 VL 34 IS 2 BP 673 EP 673 PG 1 WC Fisheries; Marine & Freshwater Biology SC Fisheries; Marine & Freshwater Biology GA CQ2DV UT WOS:000360410500250 ER PT J AU Rubinstein, R AF Rubinstein, Robert TI Relaxation rates in the Maxwellian collision model and its variable hard sphere surrogate SO PHYSICS OF FLUIDS LA English DT Article ID INVERSE-POWER-LAW; MOLECULAR-MODEL AB The variable hard sphere and related models have proven to be accurate and computationally convenient replacements for the inverse power law model of classical kinetic theory in direct simulation Monte Carlo calculations. We attempt to provide theoretical support for this remarkable success by comparing the relaxation rates in the linearized Boltzmann equation for the Maxwellian collision model with those of its variable hard sphere surrogate. The comparison demonstrates that the linearized collision operator with variable hard sphere interactions can accurately approximate the linearized collision operator with Maxwellian inverse power law interactions under well-defined and broadly applicable conditions. Extensions of the analysis to the general inverse power law model and to more realistic intermolecular potentials are briefly discussed. C1 NASA, Langley Res Ctr, Computat AeroSci Branch, Hampton, VA 23681 USA. RP Rubinstein, R (reprint author), NASA, Langley Res Ctr, Computat AeroSci Branch, Hampton, VA 23681 USA. NR 9 TC 0 Z9 0 U1 1 U2 1 PU AMER INST PHYSICS PI MELVILLE PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA SN 1070-6631 EI 1089-7666 J9 PHYS FLUIDS JI Phys. Fluids PD AUG PY 2015 VL 27 IS 8 AR 087102 DI 10.1063/1.4928471 PG 8 WC Mechanics; Physics, Fluids & Plasmas SC Mechanics; Physics GA CQ5LU UT WOS:000360646600051 ER PT J AU Lakoski, SG Jones, LW Krone, RJ Stein, PK Scott, JM AF Lakoski, Susan G. Jones, Lee W. Krone, Ronald J. Stein, Phyllis K. Scott, Jessica M. TI Autonomic dysfunction in early breast cancer: Incidence, clinical importance, and underlying mechanisms SO AMERICAN HEART JOURNAL LA English DT Review ID HEART-RATE-VARIABILITY; ANTHRACYCLINE-INDUCED CARDIOMYOPATHY; RANDOMIZED CONTROLLED-TRIAL; QUALITY-OF-LIFE; CONTAINING ADJUVANT CHEMOTHERAPY; VENTRICULAR SYSTOLIC FUNCTION; SYMPATHETIC-NERVE ACTIVITY; CARDIOVASCULAR-DISEASE; MYOCARDIAL-INFARCTION; RATE RECOVERY AB Autonomic dysfunction represents a loss of normal autonomic control of the cardiovascular system associated with both sympathetic nervous system overdrive and reduced efficacy of the parasympathetic nervous system. Autonomic dysfunction is a strong predictor of future coronary heart disease, vascular disease, and sudden cardiac death. In the current review, we will discuss the clinical importance of autonomic dysfunction as a cardiovascular risk marker among breast cancer patients. We will review the effects of antineoplastic therapy on autonomic function, as well as discuss secondary exposures, such as psychological stress, sleep disturbances, weight gain/metabolic derangements, and loss of cardiorespiratory fitness, which may negatively impact autonomic function in breast cancer patients. Lastly, we review potential strategies to improve autonomic function in this population. The perspective can help guide new therapeutic interventions to promote longevity and cardiovascular health among breast cancer survivors. C1 [Lakoski, Susan G.] Univ Vermont, Dept Internal Med, Vermont Ctr Behav & Hlth, Vermont Canc Ctr, Burlington, VT USA. [Jones, Lee W.] Mem Sloan Kettering Canc Ctr, New York, NY 10021 USA. [Krone, Ronald J.] Washington Univ, Sch Med, St Louis, MO USA. [Stein, Phyllis K.] Washington Univ, Sch Med, Div Cardiol, St Louis, MO USA. [Scott, Jessica M.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Scott, Jessica M.] Univ Space Res Assoc, Houston, TX USA. RP Lakoski, SG (reprint author), Univ Vermont, Dept Internal Med, 208 South Pk Dr, Colchester, VT 05446 USA. EM susan.lakoski@uvm.edu FU National Institute of General Medical Sciences/National Institutes of Health [P20GM103644-01A1]; National Cancer Institute FX Dr Lakoski is supported in part by the National Institute of General Medical Sciences/National Institutes of Health (P20GM103644-01A1). Dr Jones is supported in part by grants from the National Cancer Institute. NR 124 TC 3 Z9 3 U1 4 U2 10 PU MOSBY-ELSEVIER PI NEW YORK PA 360 PARK AVENUE SOUTH, NEW YORK, NY 10010-1710 USA SN 0002-8703 EI 1097-5330 J9 AM HEART J JI Am. Heart J. PD AUG PY 2015 VL 170 IS 2 BP 231 EP 241 DI 10.1016/j.ahj.2015.05.014 PG 11 WC Cardiac & Cardiovascular Systems SC Cardiovascular System & Cardiology GA CQ1LV UT WOS:000360360100009 PM 26299219 ER PT J AU Mckay, CP AF Mckay, Christopher P. TI Testing the Doran summer climate rules in Upper Wright Valley, Antarctica SO ANTARCTIC SCIENCE LA English DT Article DE Antarctica; climate; Doran climate rules; Dry Valleys; lapse rate ID MCMURDO DRY VALLEYS; CRYPTOENDOLITHIC MICROBIAL ENVIRONMENT; COLD DESERT; ROSS DESERT; LAKE HOARE AB Based on data from low elevation lake sites, previous studies have suggested three quantitative relationships related to summer (December, January and February) air temperatures in the Dry Valleys of Antarctica: i) decrease with altitude at the dry lapse rate of 9.8 degrees C km(-1), ii) increase with distance from the coast at a rate of 0.09 degrees C km(-1), and iii) degree-days above freezing during the summer months is logarithmically proportional to the maximum summer air temperature. Here, we tested the first two of these rules at high elevation sites in Upper Wright Valley. Direct measurements confirmed that the summer lapse rate followed the dry lapse rate. For the three furthest stations, Tyrol Valley, Mount Fleming and Horseshoe Crater, the average difference between the measurements and the predicted summer monthly averages are -2.1 +/- 1.4 degrees C, -0.5 +/- 1.0 degrees C and -0.4 +/- 0.9 degrees C, respectively. By contrast, at Linnaeus Terrace (54 km from the coast) the monthly average is warmer than predicted by several degrees: +4.3 +/- 1.3 degrees C. The inland temperature gradient at these high elevation sites may result from sunlight effects rather than coastal wind as previously shown for the lower valleys. The warm conditions observed c. 50 km from the coast may reflect a zone affected by both sunlight and coastal wind. C1 NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA. RP Mckay, CP (reprint author), NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA. EM chris.mckay@nasa.gov FU US National Science Foundation grant [OPP 91-18730] FX This paper is dedicated to the late E.I. Friedmann who recruited me to the study of the Antarctic Dry Valleys. The data in Upper Wright Valley were collected as part of a project supported by the US National Science Foundation grant OPP 91-18730 to E.I. Friedmann. E.I. Friedmann, A.Y. Druk and H. Sun assisted in the deployment and retrieval of the stations in the field. I thank Kaj Williams for useful discussions on this topic and the reviewers for rapid and useful reviews. NR 17 TC 2 Z9 2 U1 1 U2 2 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 0954-1020 EI 1365-2079 J9 ANTARCT SCI JI Antarct. Sci. PD AUG PY 2015 VL 27 IS 4 BP 411 EP 415 DI 10.1017/S095410201500005X PG 5 WC Environmental Sciences; Geography, Physical; Geosciences, Multidisciplinary SC Environmental Sciences & Ecology; Physical Geography; Geology GA CP9GG UT WOS:000360201200011 ER PT J AU Chaves, JE Werdell, PJ Proctor, CW Neeley, AR Freeman, SA Thomas, CS Hooker, SB AF Chaves, Joaquin E. Werdell, P. Jeremy Proctor, Christopher W. Neeley, Aimee R. Freeman, Scott A. Thomas, Crystal S. Hooker, Stanford B. TI Assessment of ocean color data records from MODIS-Aqua in the western Arctic Ocean SO DEEP-SEA RESEARCH PART II-TOPICAL STUDIES IN OCEANOGRAPHY LA English DT Article DE Ocean color; Satellite remote sensing; Arctic Ocean; Spatial distribution; Semi-analytical algorithms; Chlorophyll a; POC; CDOM; MODIS1 ID INHERENT OPTICAL-PROPERTIES; PARTICULATE ORGANIC-CARBON; CHLOROPHYLL-A CONCENTRATION; ANTARCTIC PENINSULA WATERS; QUASI-ANALYTICAL ALGORITHM; ART. NO. 3228; ABSORPTION-COEFFICIENTS; BIOOPTICAL PROPERTIES; BEAUFORT SEA; PHYTOPLANKTON BLOOMS AB A broad suite of bio-optical and biogeochemical observations collected during the NASA-funded ICESCAPE expeditions to the western Arctic Ocean in 2010 and 2011 was used to validate ocean color satellite data products in this region, which is undergoing fast ecological changes in the context of a changing climate. Satellite-to-in situ match-ups for the MODIS instrument on board Aqua (MODISA) were evaluated using standard NASA empirical and semi-analytical algorithms to estimate chlorophyll-a (C-a), spectral marine inherent optical properties, and particulate organic carbon (POC). Results for the empirical algorithms were compared with those from the semi-analytical Generalized Inherent Optical Property (GIOP) algorithm. The findings presented here showed that MODISA Ca estimates were positively biased relative to in situ measurements, in agreement with previous studies that have evaluated ocean color retrievals in the Arctic Ocean. These biases were reproduced using both satellite and in situ measured remote sensing reflectances, R-rs(lambda), indicating that estimation errors are derived from the application of the empirical algorithm and not by the observed radiometry. This disparity appears to be caused by contributions of high spectral absorption from chromophoric dissolved organic matter (CDOM), which is a well-documented feature of Arctic Ocean waters. The current MODISA empirical algorithm (OC3M) appears to attribute CDOM absorption in the blue region of the spectrum to phytoplankton absorption. In contrast, GIOP showed significant improvement over OC3M C-a estimates by effectively discriminating between phytoplankton and CDOM absorption. Additionally, executing GIOP with an expanded set of spectral bands derived from in situ radiometry, instead of just six MODISA bands, further improved the performance of absorption estimates. These findings reinforce previous suggestions that semi-analytical approaches will provide more reliable data records for Arctic studies than existing empirical methods. POC estimates showed no clear bias relative to in situ measurements, suggesting that the empirical algorithm better represents high latitude oceans with regards to the bio-optical signature of suspended particulate stocks. (C) 2015 Elsevier Ltd. All rights reserved. C1 [Chaves, Joaquin E.; Werdell, P. Jeremy; Proctor, Christopher W.; Neeley, Aimee R.; Freeman, Scott A.; Thomas, Crystal S.; Hooker, Stanford B.] NASA, Goddard Space Flight Space Ctr, Greenbelt, MD 20771 USA. [Chaves, Joaquin E.; Proctor, Christopher W.; Neeley, Aimee R.; Freeman, Scott A.; Thomas, Crystal S.] Sci Syst & Applicat Inc, Lanham, MD 20706 USA. RP Chaves, JE (reprint author), NASA, Goddard Space Flight Space Ctr, Code 616, Greenbelt, MD 20771 USA. EM joaquin.chaves@nasa.gov RI Hooker, Stanford/E-2162-2012 FU NASA Ocean Biology and Biogeochemistry (OBB) program FX The NASA Ocean Biology and Biogeochemistry (OBB) program provided support for the ICESCAPE project. Additional support was provided through an award to NASA GSFC for the Field Program Support Group. We thank the officers and crew of the USCGC Healy for their logistical and technical support that made this work possible. We thank two anonymous reviewers for their many helpful suggestions. NR 81 TC 8 Z9 8 U1 3 U2 25 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0967-0645 EI 1879-0100 J9 DEEP-SEA RES PT II JI Deep-Sea Res. Part II-Top. Stud. Oceanogr. PD AUG PY 2015 VL 118 SI SI BP 32 EP 43 DI 10.1016/j.dsr2.2015.02.011 PN A PG 12 WC Oceanography SC Oceanography GA CP9ZV UT WOS:000360255300004 ER PT J AU Ahmad, T Bebist, G Regentova, E Nefian, A Fong, T AF Ahmad, Touqeer Bebist, George Regentova, Emma Nefian, Ara Fong, Terry TI Coupling Dynamic Programming with Machine Learning for Horizon Line Detection SO INTERNATIONAL JOURNAL ON ARTIFICIAL INTELLIGENCE TOOLS LA English DT Article DE Horizon line detection; skyline extraction; sky segmentation; dynamic programming ID SCALE AB In this paper, we consider the problem of segmenting an image into sky and non-sky regions, typically referred to as horizon line detection or skyline extraction. Specifically, we present a new approach to horizon line detection by coupling machine learning with dynamic programming. Given an image, the Canny edge detector is applied first and keeping only those edges which survive over a wide range of thresholds. We refer to the surviving edges as Maximally Stable Extrema' Edges (MSEEs). The number of edges is further reduced by classifying MSEEs into horizon and non-horizon edges using a Support Vector Machine (SVM) classifier. Dynamic programming is then applied on the horizon classified edges to extract the horizon line. Various local texture features and their combinations have been investigated in training the horizon edge classifier including SIFT, LBP, HOG, SIFT-LBP, SIFT-HOG, LBP-HOG and SIFT-LBP-HOG. We have also investigated various nodal costs in the context of dynamic programming including binary edge scores, normalized edge classification scores, gradient magnitude and their combinations. The proposed approach has been evaluated and compared with a competitive approach on two challenging data sets, illustrating superior performance. C1 [Ahmad, Touqeer; Bebist, George] Univ Nevada, Dept Comp Sci & Engn, Reno, NV 89557 USA. [Regentova, Emma] Univ Nevada, Dept Elect & Comp Engn, Las Vegas, NV 89154 USA. [Nefian, Ara; Fong, Terry] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Ahmad, T (reprint author), Univ Nevada, Dept Comp Sci & Engn, Reno, NV 89557 USA. EM sh.tougeerahmad@gmail.com; bebis@cse.unr.edu; emma.regentova@unlv.edu; ara.nefian@nasa.gov; terry.fong@nasa.gov FU NASA EPSCoR [NNX11AMO9A]; NSF PFI FX This work is supported by NASA EPSCoR under Cooperative Agreement No. NNX11AMO9A, and in part by NSF PFI. NR 24 TC 1 Z9 1 U1 0 U2 3 PU WORLD SCIENTIFIC PUBL CO PTE LTD PI SINGAPORE PA 5 TOH TUCK LINK, SINGAPORE 596224, SINGAPORE SN 0218-2130 EI 1793-6349 J9 INT J ARTIF INTELL T JI Int. J. Artif. Intell. Tools PD AUG PY 2015 VL 24 IS 4 SI SI AR 1540018 DI 10.1142/s0218213015400187 PG 19 WC Computer Science, Artificial Intelligence; Computer Science, Interdisciplinary Applications SC Computer Science GA CQ1TA UT WOS:000360380900005 ER PT J AU Zavada, SR McHardy, NR Gordon, KL Scott, TF AF Zavada, Scott R. McHardy, Nicholas R. Gordon, Keith L. Scott, Timothy F. TI Rapid, Puncture-Initiated Healing via Oxygen-Mediated Polymerization SO ACS MACRO LETTERS LA English DT Article ID NEAR-INFRARED SPECTROSCOPY; THIOL-ENE POLYMERS; RADICAL-ADDITION; SELF-REPAIR; CHEMISTRY; PHOTOPOLYMERIZATIONS; COMPOSITES; KINETICS AB Autonomously healing materials that utilize thiol-ene polymerization initiated by an environmentally borne reaction stimulus are demonstrated by puncturing trilayered panels, fabricated by sandwiching thiol-ene- trialkylborane resin formulations between solid polymer panels, with high velocity projectiles; as the reactive liquid layer flows into the entrance hole, contact with atmospheric oxygen initiates polymerization, converting the liquid into a solid plug. Using infrared spectroscopy, we find that formulated resins polymerize rapidly, forming a solid polymer within seconds of atmospheric contact. During high-velocity ballistics experiments, additional evidence for rapid polymerization is provided by high-speed video, demonstrating the immediate viscosity increase when the thiol-ene- trialkylborane resins contact atmospheric oxygen, and thermal imaging, where surface temperature measurements reveal the thiol-ene reaction exotherm, confirming polymerization begins immediately upon oxygen exposure. While other approaches for materials self-repair have utilized similar liquid-to-solid transitions, our approach permits the development of materials capable of sealing a breach within seconds, far faster than previously described methods. C1 [Zavada, Scott R.; Scott, Timothy F.] Univ Michigan, Macromol Sci & Engn Program, Ann Arbor, MI 48109 USA. [McHardy, Nicholas R.] Univ Michigan, Dept Mat Sci & Engn, Ann Arbor, MI 48109 USA. [Scott, Timothy F.] Univ Michigan, Dept Chem Engn, Ann Arbor, MI 48109 USA. [Gordon, Keith L.] NASA Langley Res Ctr, Adv Mat & Proc Branch, Hampton, VA 23681 USA. RP Scott, TF (reprint author), Univ Michigan, Macromol Sci & Engn Program, Ann Arbor, MI 48109 USA. EM tfscott@umich.edu FU National Aeronautics and Space Administration (NASA Space Technology Research Fellowship) [NNX12AM31H] FX The authors gratefully acknowledge funding from the National Aeronautics and Space Administration (NASA Space Technology Research Fellowship, award number NNX12AM31H). NR 30 TC 2 Z9 2 U1 4 U2 24 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 2161-1653 J9 ACS MACRO LETT JI ACS Macro Lett. PD AUG PY 2015 VL 4 IS 8 BP 819 EP 824 DI 10.1021/acsmacrolett.5b00315 PG 6 WC Polymer Science SC Polymer Science GA CP4ZN UT WOS:000359891200003 ER PT J AU Ludden, J Albarede, F Coleman, M AF Ludden, John Albarede, Francis Coleman, Max TI The Impact of Geochemistry SO ELEMENTS LA English DT Article DE economic; social; impact; communication; geochemistry AB As geochemists and mineralogists, we are well aware of the impact of our science. We can often reel off examples of how our discoveries have influenced industry and improved humankind's knowledge about how the Earth works, as well as how natural and anthropogenic processes have led to Its present state. Moreover, because of a century of analytical developments and conceptual breakthroughs, geochemists are now versatile and can now work across the entire spectrum of the Earth sciences. However, we are not so good at promoting the social and economic impacts of geochemistry. C1 [Ludden, John] British Geol Survey, Nottingham, England. [Albarede, Francis] Ecole Normale Super Lyon, F-69364 Lyon, France. [Albarede, Francis] CNRS, Lyon, France. [Coleman, Max] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. RP Ludden, J (reprint author), British Geol Survey, Nottingham, England. EM jludden@bgs.ac.uk; francis.albarede@ens-lyon.fr; max.coleman@jpl.nasa.gov RI Albarede, Francis/A-8871-2011 OI Albarede, Francis/0000-0003-1994-1428 NR 8 TC 0 Z9 0 U1 4 U2 12 PU MINERALOGICAL SOC AMER PI CHANTILLY PA 3635 CONCORDE PKWY STE 500, CHANTILLY, VA 20151-1125 USA SN 1811-5209 EI 1811-5217 J9 ELEMENTS JI Elements PD AUG PY 2015 VL 11 IS 4 BP 239 EP 240 DI 10.2113/gselements.11.4.239 PG 2 WC Geochemistry & Geophysics; Mineralogy SC Geochemistry & Geophysics; Mineralogy GA CP5AO UT WOS:000359893900004 ER PT J AU Wyrobek, AJ Rabin, B Bhatnagar, S Albertolle, M Straume, T Witkowska, HE AF Wyrobek, A. J. Rabin, B. Bhatnagar, S. Albertolle, M. Straume, T. Witkowska, H. E. TI Molecular Profiling of Neurocognitive Performance and Risk for Neurological Disease after Exposure to Ionizing Radiation. SO ENVIRONMENTAL AND MOLECULAR MUTAGENESIS LA English DT Meeting Abstract C1 [Wyrobek, A. J.; Bhatnagar, S.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. [Rabin, B.] Univ Maryland, Baltimore, MD 21201 USA. [Albertolle, M.; Witkowska, H. E.] Univ Calif San Francisco, Sandler Moore Mass Spectrometry Core Facil, San Francisco, CA 94143 USA. [Straume, T.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0893-6692 EI 1098-2280 J9 ENVIRON MOL MUTAGEN JI Environ. Mol. Mutagen. PD AUG PY 2015 VL 56 SU 1 MA S48 BP S43 EP S43 PG 1 WC Environmental Sciences; Genetics & Heredity; Toxicology SC Environmental Sciences & Ecology; Genetics & Heredity; Toxicology GA CP9PJ UT WOS:000360226400048 ER PT J AU Barnaby, HJ Vermeire, B Campola, MJ AF Barnaby, H. J. Vermeire, B. Campola, M. J. TI Improved Model for Increased Surface Recombination Current in Irradiated Bipolar Junction Transistors SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE LA English DT Article DE Base current; bipolar junction transistors; emitter-base junction; interface traps; radiation effects; recombination; space-charge ID LOW-DOSE-RATE; INDUCED GAIN DEGRADATION; RATE SENSITIVITY ELDRS; IONIZING-RADIATION; LINEAR CIRCUITS; INTEGRATED-CIRCUITS; DEVICES; BJTS; ICS; ENVIRONMENT AB Current gain degradation in irradiated bipolar junction transistors is primarily due to excess base current caused by enhanced carrier recombination in the emitter-base space-charge region (SCR). Radiation-induced traps at the interface between silicon and the bipolar base oxide facilitate the recombination process primarily above the sensitive emitter-base junction. This leads to an increase in surface recombination current in the SCR, which is a non-ideal component of the BJT's base current characteristic under active bias conditions. In this paper, we derive a precise analytical model for surface recombination current that captures bias dependencies typically omitted from traditional models. This improved model is validated by comparisons to these traditional approaches. C1 [Barnaby, H. J.] Arizona State Univ, Sch Elect Comp & Energy Engn, Tempe, AZ 85287 USA. [Vermeire, B.] Space Micro, San Diego, CA 92121 USA. [Campola, M. J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Barnaby, HJ (reprint author), Arizona State Univ, Sch Elect Comp & Energy Engn, Tempe, AZ 85287 USA. EM hbarnaby@asu.edu; bver-meire@spacemicro.com; michael.j.campola@nasa.gov FU Defense Threat Reduction Agency (DTRA) [N00164-020D06599] FX This work was supported in part by the Defense Threat Reduction Agency (DTRA) under Contract N00164-020D06599. NR 35 TC 2 Z9 2 U1 0 U2 5 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0018-9499 EI 1558-1578 J9 IEEE T NUCL SCI JI IEEE Trans. Nucl. Sci. PD AUG PY 2015 VL 62 IS 4 BP 1658 EP 1664 DI 10.1109/TNS.2015.2452229 PN 1 PG 7 WC Engineering, Electrical & Electronic; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA CP6RR UT WOS:000360016200021 ER PT J AU Balakumar, P Kegerise, MA AF Balakumar, P. Kegerise, Michael A. TI Receptivity of Hypersonic Boundary Layers over Straight and Flared Cones SO AIAA JOURNAL LA English DT Article ID FLAT-PLATE; TUNNEL AB The effects of adverse pressure gradients on the receptivity and stability of hypersonic boundary layers were numerically investigated. Simulations were performed for boundary-layer flows over a straight cone and two flared cones. The steady and the unsteady flowfields were obtained by solving the two-dimensional Navier-Stokes equations in axisymmetric coordinates using the fifth-order-accurate weighted essentially nonoscillatory scheme for space discretization and using a third-order total-variation-diminishing Runge-Kutta scheme for time integration. The mean boundary-layer profiles were analyzed using local stability and nonlocal parabolized stability equations methods. After the most amplified disturbances were identified, two-dimensional plane acoustic waves were introduced at the outer boundary of the computational domain and time-accurate simulations were performed. The adverse pressure gradient was found to affect the boundary-layer stability in two important ways. First, the frequency of the most amplified second-mode disturbance was increased relative to the zero-pressure gradient case. Second, the amplification of first-and second-mode disturbances was increased. Although an adverse pressure gradient enhances instability wave growth rates, small nose-tip bluntness was found to delay transition due to the low receptivity coefficient and the resulting weak initial amplitude of the instability waves. The computed and measured amplitudefrequency spectra in all three cases agree very well in terms of frequency and the shape except for the amplitude. C1 [Balakumar, P.; Kegerise, Michael A.] NASA, Langley Res Ctr, Flow Phys & Control Branch, Hampton, VA 23581 USA. RP Balakumar, P (reprint author), NASA, Langley Res Ctr, Flow Phys & Control Branch, Hampton, VA 23581 USA. NR 24 TC 0 Z9 0 U1 1 U2 3 PU AMER INST AERONAUTICS ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0001-1452 EI 1533-385X J9 AIAA J JI AIAA J. PD AUG PY 2015 VL 53 IS 8 BP 2097 EP 2109 DI 10.2514/1.J053432 PG 13 WC Engineering, Aerospace SC Engineering GA CO7BX UT WOS:000359313600003 ER PT J AU Miller, SAE AF Miller, Steven A. E. TI Prediction of Near-Field Jet Cross Spectra SO AIAA JOURNAL LA English DT Article ID EXPANDED SUPERSONIC JETS; HIGH-SPEED; NOISE PREDICTION; MIXING NOISE; TURBULENCE AB A prediction method is developed based on the acoustic analogy for the cross-power spectral density in the convecting near field of compressible fluid turbulence. Equivalent source near-field, midfield, and far-field terms within the model integrand create corresponding near-field, midfield, and far-field radiating waves. These equivalent sources are modeled with a single equation for the two-point cross correlation of the Lighthill stress tensor that is dependent on the jet operating conditions. An alternative equivalent source model based on steady Reynolds-averaged Navier-Stokes solutions is proposed. The cross-power spectral density model automatically reduces to a traditional autopower spectral density model when observers are at the same location. Predictions of radiation intensity and coherence compare favorably with measurements in the near field, midfield, and far field for a wide range of jet Mach numbers and temperature ratios. C1 NASA, Langley Res Ctr, Aeroacoust Branch, Hampton, VA 23681 USA. RP Miller, SAE (reprint author), NASA, Langley Res Ctr, Aeroacoust Branch, 2 N Dryden St,Mail Stop 461, Hampton, VA 23681 USA. EM s.miller@nasa.gov NR 53 TC 1 Z9 1 U1 1 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 AUG PY 2015 VL 53 IS 8 BP 2130 EP 2150 DI 10.2514/1.J053614 PG 21 WC Engineering, Aerospace SC Engineering GA CO7BX UT WOS:000359313600006 ER PT J AU Malik, M Liao, W Li, F Choudhari, M AF Malik, Mujeeb Liao, Wei Li, Fei Choudhari, Meelan TI Discrete-Roughness-Element-Enhanced Swept-Wing Natural Laminar Flow at High Reynolds Numbers SO AIAA JOURNAL LA English DT Article ID 3-DIMENSIONAL BOUNDARY-LAYERS; SECONDARY INSTABILITY; PASSIVE CONTROL; ROTATING-DISK; TRANSITION; VORTICES; STABILITY; GROWTH AB Nonlinear parabolized stability equations and secondary-instability analyses are used to provide a computational assessment of the potential use of the discrete-roughness-element technology for extending swept-wing natural laminar flow at chord Reynolds numbers relevant to transport aircraft. Computations performed for the boundary layer on a natural-laminar-flow airfoil with a leading-edge sweep angle of 34.6 deg, freestream Mach number of 0.75, and chord Reynolds numbers of 17 x 10(6), 24 x 10(6), and 30 x 10(6) suggest that discrete roughness elements could delay laminar-turbulent transition by about 20% when transition is caused by stationary crossflow disturbances. Computations show that the introduction of small-wavelength stationary crossflow disturbances (i.e., discrete roughness element) also suppresses the growth of most amplified traveling crossflow disturbances. C1 [Malik, Mujeeb; Li, Fei; Choudhari, Meelan] NASA, Langley Res Ctr, Computat AeroSci Branch, Hampton, VA 23681 USA. [Liao, Wei] Natl Inst Aerosp, Hampton, VA 23666 USA. RP Malik, M (reprint author), NASA, Langley Res Ctr, Computat AeroSci Branch, MS 128, Hampton, VA 23681 USA. EM Mujeeb.R.Malik@nasa.gov; Wei.Liao@nasa.gov; Fei.Li@nasa.gov; Meelan.M.Choudhari@nasa.gov RI Choudhari, Meelan/F-6080-2017 OI Choudhari, Meelan/0000-0001-9120-7362 FU NASA's Environmentally Responsible Aviation Project FX This work was performed in support of NASA's Environmentally Responsible Aviation Project. NR 42 TC 0 Z9 0 U1 0 U2 12 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 AUG PY 2015 VL 53 IS 8 BP 2321 EP 2334 DI 10.2514/1.J053637 PG 14 WC Engineering, Aerospace SC Engineering GA CO7BX UT WOS:000359313600020 ER PT J AU McCubbin, FM Kaaden, KEV Tartese, R Klima, RL Liu, Y Mortimer, J Barnes, JJ Shearer, CK Treiman, AH Lawrence, DJ Elardo, SM Hurley, DM Boyce, JW Anand, M AF McCubbin, Francis M. Kaaden, Kathleen E. Vander Tartese, Romain Klima, Rachel L. Liu, Yang Mortimer, James Barnes, Jessica J. Shearer, Charles K. Treiman, Allan H. Lawrence, David J. Elardo, Stephen M. Hurley, Dana M. Boyce, Jeremy W. Anand, Mahesh TI Magmatic volatiles (H, C, N, F, S, Cl) in the lunar mantle, crust, and regolith: Abundances, distributions, processes, and reservoirs SO AMERICAN MINERALOGIST LA English DT Review DE Water; apatite; hydrogen; space weathering; Moon; magma ocean; isotopes; remote sensing; Review ID NOMINALLY ANHYDROUS MINERALS; LIGHT-ELEMENT GEOCHEMISTRY; POLAR HYDROGEN DEPOSITS; HIGH-GRADE METAMORPHISM; INNER SOLAR-SYSTEM; HOSTED MELT INCLUSIONS; MARE SILICIC VOLCANISM; FORMING GIANT IMPACT; ISOTOPIC COMPOSITION; TERRESTRIAL PLANETS AB Many studies exist on magmatic volatiles (H, C, N, F, S, Cl) in and on the Moon, within the last several years, that have cast into question the post-Apollo view of lunar formation, the distribution and sources of volatiles in the Earth-Moon system, and the thermal and magmatic evolution of the Moon. However, these recent observations are not the first data on lunar volatiles. When Apollo samples were first returned, substantial efforts were made to understand volatile elements, and a wealth of data regarding volatile elements exists in this older literature. In this review paper, we approach volatiles in and on the Moon using new and old data derived from lunar samples and remote sensing. From combining these data sets, we identified many points of convergence, although numerous questions remain unanswered. The abundances of volatiles in the bulk silicate Moon (BSM), lunar mantle, and urKREEP [last similar to 1% of the lunar magma ocean (LMO)] were estimated and placed within the context of the LMO model. The lunar mantle is likely heterogeneous with respect to volatiles, and the relative abundances of F, Cl, and H2O in the lunar mantle (H2O > F >> Cl) do not directly reflect those of BSM or urKREEP (Cl > H2O F). In fact, the abundances of volatiles in the cumulate lunar mantle were likely controlled by partitioning of volatiles between LMO liquid and nominally anhydrous minerals instead of residual liquid trapped in the cumulate pile. An internally consistent model for lunar volatiles in BSM should reproduce the absolute and relative abundances of volatiles in urKREEP, the anorthositic primary crust, and the lunar mantle within the context of processes that occurred during the thermal and magmatic evolution of the Moon. Using this mass-balance constraint, we conducted LMO crystallization calculations with a specific focus on the distributions and abundances of F, Cl, and H2O to determine whether or not estimates of F, Cl, and H2O in urKREEP are consistent with those of the lunar mantle, estimated independently from the analysis of volatiles in mare volcanic materials. Our estimate of volatiles in the bulk lunar mantle are 0.54-4.5 ppm F, 0.15-5.3 ppm H2O, 0.26-2.9 ppm Cl, 0.014-0.57 ppm C, and 78.9 ppm S. Our estimates of H2O are depleted compared to independent estimates of H2O in the lunar mantle, which are largely biased toward the "wettest" samples. Although the lunar mantle is depleted in volatiles relative to Earth, unlike the Earth, the mantle is not the primary host for volatiles. The primary host of the Moon's incompatible lithophile volatiles (F, Cl, H2O) is urKREEP, which we estimate to have 660 ppm F, 300-1250 ppm H2O, and 1100-1350 ppm Cl. This urKREEP composition implies a BSM with 7.1 ppm F, 3-13 ppm H2O, and 11-14 ppm Cl. An upper bound on the abundances of F, Cl, and H2O in urKREEP and the BSM, based on F abundances in Cl carbonaceous chondrites, are reported to be 5500 ppm F, 0.26-1.09 wt% H2O, and 0.98-1.2 wt% Cl and 60 ppm F, 27-114 ppm H2O, and 100-123 ppm Cl, respectively. The role of volatiles in many lunar geologic processes was also determined and discussed. Specifically, analyses of volatiles from lunar glass beads as well as the phase assemblages present in coatings on those beads were used to infer that H-2 is likely the primary vapor component responsible for propelling the fire-fountain eruptions that produced the pyroclastic glass beads (as opposed to CO). The textural occurrences of some volatile-bearing minerals are used to identify hydrothermal alteration, which is manifested by sulfide veining and sulfide-replacement textures in silicates. Metasomatic alteration in lunar systems differs substantially from terrestrial alteration due to differences in oxygen fugacity between the two bodies that result in H2O as the primary solvent for alteration fluids on Earth and H-2 as the primary solvent for alteration fluids on the Moon (and other reduced planetary bodies). Additionally, volatile abundances in volatile-bearing materials are combined with isotopic data to determine possible secondary processes that have affected the primary magmatic volatile signatures of lunar rocks including degassing, assimilation, and terrestrial contamination; however, these processes prove difficult to untangle within individual data sets. Data from remote sensing and lunar soils are combined to understand the distribution, origin, and abundances of volatiles on the lunar surface, which can be explained largely by solar wind implantation and spallogenic processes, although some of the volatiles in the soils may also be either indigenous to the Moon or terrestrial contamination. We have also provided a complete inventory of volatile-bearing mineral phases indigenous to lunar samples and discuss some of the "unconfirmed" volatile-bearing minerals that have been reported. Finally, a compilation of unanswered questions and future avenues of research on the topic of lunar volatiles are presented, along with a critical analysis of approaches for answering these questions. C1 [McCubbin, Francis M.; Kaaden, Kathleen E. Vander; Shearer, Charles K.; Elardo, Stephen M.] Univ New Mexico, Inst Meteorit, Albuquerque, NM 87131 USA. [McCubbin, Francis M.; Kaaden, Kathleen E. Vander; Shearer, Charles K.; Elardo, Stephen M.] Univ New Mexico, Dept Earth & Planetary Sci, Albuquerque, NM 87131 USA. [Tartese, Romain; Mortimer, James; Barnes, Jessica J.; Lawrence, David J.; Hurley, Dana M.; Anand, Mahesh] Open Univ, Planetary & Space Sci, Milton Keynes MK7 6AA, Bucks, England. [Klima, Rachel L.] Johns Hopkins Univ, Dept Space, Planetary Explorat Grp, Appl Phys Lab, Laurel, MD 20723 USA. [Liu, Yang] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Barnes, Jessica J.; Anand, Mahesh] Nat Hist Museum, Dept Earth Sci, London SW7 5BD, England. [Treiman, Allan H.] USRA, Lunar & Planetary Inst, Houston, TX 77058 USA. [Elardo, Stephen M.] Carnegie Inst Sci, Geophys Lab, Washington, DC 20015 USA. [Boyce, Jeremy W.] Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90095 USA. RP McCubbin, FM (reprint author), Univ New Mexico, Inst Meteorit, 200 Yale Blvd SE, Albuquerque, NM 87131 USA. EM fmccubbi@unm.edu RI Elardo, Stephen/E-5865-2010; Hurley, Dana/F-4488-2015; Klima, Rachel/H-9383-2012; Lawrence, David/E-7463-2015; Boyce, Jeremy/A-7514-2008; OI Hurley, Dana/0000-0003-1052-1494; Klima, Rachel/0000-0002-9151-6429; Lawrence, David/0000-0002-7696-6667; Tartese, Romain/0000-0002-3490-9875 FU NASA Lunar Advanced Science and Exploration Research (LASER) [NNX13AK32G, NNXI1AB30G, NNX I 3A.158G]; NASA Cosmochemistry [NNX11AG76G, NNX11AG58G, NNX13AH85G]; U.K. Science and Technology Facilities Council grant [STFC/ST11001298/1]; Earth and Space Science Fellowship [NNX12A015H]; NASA Early Career Fellowship [NNXI3AG40G] FX We thank CAPTEM and the Meteorite Working Group at NASA JSC for allocating us and many others samples for lunar volatile work. We thank Hanna Nekvasil, Donald Lindsley, James Greenwood, Erik Hauri, Alberto Saal,JeffTaylor, Bradley Jolliff, Zach Sharp, Jim Papike, Juliane Gross, Alison Santos, Larry Taylor, and Katie Robinson for many helpful discussions concerning lunar volatiles. We also thank Noah Petro and an anonymous reviewer for helpful comments that have improved the quality of this work. We also thank Peter Isaacson for his work and comments as AE. This work was funded by NASA Lunar Advanced Science and Exploration Research (LASER) grant NNX13AK32G to F.M.M., NNXI1A B30G to Carl Agee, and NNX I 3A.158G to C.K.S., K.E.V.K. acknowledges support from NASA Cosmochemistry grant NNX11AG76G awarded to F.M.M. Y.L. acknowledges support from NASA Cosmochemistry grant NNX11AG58G to Larry Taylor, and internal support from JPL, which is managed by California Institute of Technology under a contract with NASA. M.A. acknowledges support from the U.K. Science and Technology Facilities Council grant (STFC/ST11001298/1). was supported by Earth and Space Science Fellowship NNX12A015H to S.M.E. and NASA Cosmochemistry grant NNX13AH85G to C.K.S. J.W.B. acknowledges support from a NASA Early Career Fellowship (NNXI3AG40G). This research has made use of NASA's Astrophysics Data System. NR 425 TC 19 Z9 19 U1 10 U2 49 PU MINERALOGICAL SOC AMER PI CHANTILLY PA 3635 CONCORDE PKWY STE 500, CHANTILLY, VA 20151-1125 USA SN 0003-004X EI 1945-3027 J9 AM MINERAL JI Am. Miner. PD AUG-SEP PY 2015 VL 100 IS 8-9 BP 1668 EP 1707 DI 10.2138/am-2015-4934CCBYNCND PG 40 WC Geochemistry & Geophysics; Mineralogy SC Geochemistry & Geophysics; Mineralogy GA CO9RB UT WOS:000359512100003 ER PT J AU Cooper, DJ Kaczynski, K Slayback, D Yager, K AF Cooper, David J. Kaczynski, Kristen Slayback, Daniel Yager, Karina TI Growth and organic carbon production in peatlands dominated by Distichia muscoides, Bolivia, South America SO ARCTIC ANTARCTIC AND ALPINE RESEARCH LA English DT Article ID TROPICAL ANDES; CLIMATE-CHANGE; PEAT; ALTIPLANO; SPHAGNUM; ECOSYSTEMS; VEGETATION; PATTERNS AB Little is known about the growth or production of alpine cushion plant communities in the southern hemisphere, even though they dominate many high elevation peat-accumulating ecosystems in this region. We measured the growth and organic carbon production in four Distichia muscoides cushion plant-dominated peatlands in the tropical Andes of Bolivia, South America. Height growth was measured using the modified crank wire system. Cores were collected at the end of the 18-month study period to determine the biomass and organic carbon production rate. Bulk density averaged 0.081 g cm(-3). Total height increase ranged from 0.96 to 5.37 cm yr(-1), indicating very rapid growth. Most growth occurred during the austral summer wet season. Mean organic carbon production for the four sites ranged from 1.5 to 4.0 kg C m(-2) yr(-1) and is among the most rapid rates of potential peat accumulation known for high elevation or high latitude ecosystems on Earth. C1 [Cooper, David J.; Kaczynski, Kristen] Colorado State Univ, Dept Forest & Rangeland Stewardship, Ft Collins, CO 80523 USA. [Slayback, Daniel; Yager, Karina] NASA, Goddard Space Flight Ctr, Sci Syst & Applicat Inc, Greenbelt, MD 20771 USA. RP Cooper, DJ (reprint author), Colorado State Univ, Dept Forest & Rangeland Stewardship, Campus Box 1461, Ft Collins, CO 80523 USA. EM David.Cooper@colostate.edu FU NASA; Department of Forest and Rangeland Stewardship at Colorado State University; Colorado State University FX This research was funded in part by NASA's Land Cover/Land Use change program. Additional funds were provided by the Department of Forest and Rangeland Stewardship at Colorado State University. We acknowledge support from the Colorado State University Libraries Open Access Research and Scholarship Fund. We acknowledge field assistance from Humber Alberto, Julieta Acho, Oscar Plata, Dr. Jaime Argollo, Gabriel Zeballos Castellon, and Marcelo Cabero Caballero. We appreciate access to the pastures of Manasaya allowed by Don Aurelio. NR 30 TC 5 Z9 6 U1 4 U2 16 PU INST ARCTIC ALPINE RES PI BOULDER PA UNIV COLORADO, BOULDER, CO 80309 USA SN 1523-0430 EI 1938-4246 J9 ARCT ANTARCT ALP RES JI Arct. Antarct. Alp. Res. PD AUG PY 2015 VL 47 IS 3 BP 505 EP 510 DI 10.1657/AAAR0014-060 PG 6 WC Environmental Sciences; Geography, Physical SC Environmental Sciences & Ecology; Physical Geography GA CP2AK UT WOS:000359679000008 ER PT J AU Kettler, RM Loope, DB Weber, KA Niles, PB AF Kettler, Richard M. Loope, David B. Weber, Karrie A. Niles, Paul B. TI Life and Liesegang: Outcrop-Scale Microbially Induced Diagenetic Structures and Geochemical Self-Organization Phenomena Produced by Oxidation of Reduced Iron SO ASTROBIOLOGY LA English DT Article ID SOUTH-CENTRAL UTAH; OXIDIZING BACTERIA; NAVAJO SANDSTONE; CONCRETIONS; MARS; SCHWERTMANNITE; GEOCHRONOLOGY; PRECIPITATION; FERRIHYDRITE; GALLIONELLA AB The Kanab Wonderstone is sandstone (Shinarump Member, Chinle Formation) that is cemented and stained with iron oxide. The iron-oxide cementation and staining in these rocks have been considered examples of the Liesegang phenomenon, but we will show that they comprise a microbially induced structure. The spacing of bands of iron-oxide stain follow the Jablczynski spacing law (wherein the spacing between bands of iron-oxide stain increases as one traverses a series of bands) characteristic of Liesegang. Bands of iron-oxide cement exhibit more variable spacing and exhibit a weak but significant correlation between band thickness and distance between bands of cement. The pore-filling cement contains morphotypes that are similar in size and habit to those exhibited by microaerophilic iron-oxidizing bacteria. Other disseminated iron-oxide mineralization occurs as rhombohedra interpreted to be pseudomorphs after siderite. We interpret the cement to be produced by microbially mediated oxidation of siderite (a typical early diagenetic mineral in fluvial sandstones). Iron-oxidizing bacteria colonized the redox interface between siderite-cemented sand and porous sandstone. Microbes oxidized aqueous Fe(II), generating acid that caused siderite dissolution. The iron-oxide cement is the microbial product of a geochemical drive for organization; whereas the iron-oxide stain is true Liesegang. Together, they comprise a distinctive microbially induced structure with high preservation potential. Key Words: Biosignatures-Iron oxides-Diagenesis-Iron-oxidizing bacteria-Shinarump. Astrobiology 15, 616-636. C1 [Kettler, Richard M.; Loope, David B.; Weber, Karrie A.] Univ Nebraska, Dept Earth & Atmospher Sci, Lincoln, NE 68588 USA. [Weber, Karrie A.] Univ Nebraska, Sch Biol Sci, Lincoln, NE 68588 USA. [Niles, Paul B.] NASA, Lyndon B Johnson Space Ctr, Astromat Res & Explorat Sci, Houston, TX 77058 USA. RP Kettler, RM (reprint author), Univ Nebraska, Dept Earth & Atmospher Sci, Lincoln, NE 68588 USA. EM rkettler1@unl.edu FU NASA; NASA Johnson Space Center; Mars Fundamental Research Program FX We thank Dr. H. Chen for assistance with electron microscopy and Mr. Kenneth Brown for samples and field access. Support for this research was provided by the NASA Nebraska Space Grant program and the UNL Vice-Chancellor for Research. Paul Niles acknowledges support from the NASA Johnson Space Center and the Mars Fundamental Research Program. Conversations in the field with P. Reiners and B. Toro have improved our interpretation. Reviews of multiple versions of this manuscript by five anonymous reviewers have helped to improve the final product. NR 61 TC 2 Z9 2 U1 3 U2 26 PU MARY ANN LIEBERT, INC PI NEW ROCHELLE PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA SN 1531-1074 EI 1557-8070 J9 ASTROBIOLOGY JI Astrobiology PD AUG 1 PY 2015 VL 15 IS 8 BP 616 EP 636 DI 10.1089/ast.2015.1305 PG 21 WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics; Geology GA CP0VI UT WOS:000359593800002 PM 26274864 ER PT J AU Williams, AJ Sumner, DY Alpers, CN Karunatillake, S Hofmann, BA AF Williams, Amy J. Sumner, Dawn Y. Alpers, Charles N. Karunatillake, Suniti Hofmann, Beda A. TI Preserved Filamentous Microbial Biosignatures in the Brick Flat Gossan, Iron Mountain, California SO ASTROBIOLOGY LA English DT Article ID ACID-MINE DRAINAGE; MASSIVE SULFIDE DEPOSIT; THERMAL-SPRING DEPOSITS; WEST-SHASTA DISTRICT; THIOBACILLUS-FERROOXIDANS; MERIDIANI-PLANUM; SULFATE MINERALS; SUPERFUND SITE; DRUMMOND BASIN; FOSSIL RECORD AB A variety of actively precipitating mineral environments preserve morphological evidence of microbial biosignatures. One such environment with preserved microbial biosignatures is the oxidized portion of a massive sulfide deposit, or gossan, such as that at Iron Mountain, California. This gossan may serve as a mineralogical analogue to some ancient martian environments due to the presence of oxidized iron and sulfate species, and minerals that only form in acidic aqueous conditions, in both environments. Evaluating the potential biogenicity of cryptic textures in such martian gossans requires an understanding of how microbial textures form biosignatures on Earth. The iron-oxide-dominated composition and morphology of terrestrial, nonbranching filamentous microbial biosignatures may be distinctive of the underlying formation and preservation processes. The Iron Mountain gossan consists primarily of ferric oxide (hematite), hydrous ferric oxide (HFO, predominantly goethite), and jarosite group minerals, categorized into in situ gossan, and remobilized iron deposits. We interpret HFO filaments, found in both gossan types, as HFO-mineralized microbial filaments based in part on (1) the presence of preserved central filament lumina in smooth HFO mineral filaments that are likely molds of microbial filaments, (2) mineral filament formation in actively precipitating iron-oxide environments, (3) high degrees of mineral filament bending consistent with a flexible microbial filament template, and (4) the presence of bare microbial filaments on gossan rocks. Individual HFO filaments are below the resolution of the Mars Curiosity and Mars 2020 rover cameras, but sinuous filaments forming macroscopic matlike textures are resolvable. If present on Mars, available cameras may resolve these features identified as similar to terrestrial HFO filaments and allow subsequent evaluation for their biogenicity by synthesizing geochemical, mineralogical, and morphological analyses. Sinuous biogenic filaments could be preserved on Mars in an iron-rich environment analogous to Iron Mountain, with the Pahrump Hills region and Hematite Ridge in Gale Crater as tentative possibilities. Key Words: Geobiology-Biosignatures-Filaments-Mars-Microbial fossils. Astrobiology 15, 637-668. C1 [Williams, Amy J.; Sumner, Dawn Y.] Univ Calif Davis, Dept Earth & Planetary Sci, Davis, CA 95616 USA. [Alpers, Charles N.] US Geol Survey, Calif Water Sci Ctr, Sacramento, CA USA. [Karunatillake, Suniti] Louisiana State Univ, Dept Geol & Geophys, Baton Rouge, LA 70803 USA. [Hofmann, Beda A.] Burgergemeinde Bern, Nat Hist Museum, Bern, Switzerland. RP Williams, AJ (reprint author), NASA, Goddard Space Flight Ctr, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA. EM amy.j.williams@nasa.gov RI Karunatillake, Suniti/A-5934-2009; OI Karunatillake, Suniti/0000-0001-9891-1432; Alpers, Charles/0000-0001-6945-7365 FU NASA Headquarters under the NASA Earth and Space Science Fellowship Program [NNX11AQ51H]; UCD Geology department FX This work is supported by NASA Headquarters under the NASA Earth and Space Science Fellowship Program Grant NNX11AQ51H and by the UCD Geology department Durrell Funds. Thanks to Iron Mountain operations, USEPA, USGS, T. Arman and IMM Inc., J. Peterson and T. Mackey for field assistance, A. Phan and D. McKim for assistance with filament morphology measurements, R. Southard, F. Hayes and I. Delusina for laboratory assistance. We thank Robert Bowell, Jane Hammarstrom, and two anonymous reviewers for their comments, which helped strengthen the manuscript. Any use of trade, firm, or product names is for descriptive purposes only and does not imply endorsement by the US Government. NR 86 TC 3 Z9 3 U1 2 U2 7 PU MARY ANN LIEBERT, INC PI NEW ROCHELLE PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA SN 1531-1074 EI 1557-8070 J9 ASTROBIOLOGY JI Astrobiology PD AUG 1 PY 2015 VL 15 IS 8 BP 637 EP 668 DI 10.1089/ast.2014.1235 PG 32 WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics; Geology GA CP0VI UT WOS:000359593800003 PM 26247371 ER PT J AU Morrison, IS Gowanlock, MG AF Morrison, Ian S. Gowanlock, Michael G. TI Extending Galactic Habitable Zone Modeling to Include the Emergence of Intelligent Life SO ASTROBIOLOGY LA English DT Article ID MILKY-WAY; EXTRATERRESTRIAL LIFE; CHEMICAL EVOLUTION; DRAKE EQUATION; COMPLEX LIFE; PLANETS; ENVIRONMENTS; HYPOTHESIS; STARS; EARTH AB Previous studies of the galactic habitable zone have been concerned with identifying those regions of the Galaxy that may favor the emergence of complex life. A planet is deemed habitable if it meets a set of assumed criteria for supporting the emergence of such complex life. In this work, we extend the assessment of habitability to consider the potential for life to further evolve to the point of intelligence-termed the propensity for the emergence of intelligent life, phi(I). We assume phi(I) is strongly influenced by the time durations available for evolutionary processes to proceed undisturbed by the sterilizing effects of nearby supernovae. The times between supernova events provide windows of opportunity for the evolution of intelligence. We developed a model that allows us to analyze these window times to generate a metric for phi(I), and we examine here the spatial and temporal variation of this metric. Even under the assumption that long time durations are required between sterilizations to allow for the emergence of intelligence, our model suggests that the inner Galaxy provides the greatest number of opportunities for intelligence to arise. This is due to the substantially higher number density of habitable planets in this region, which outweighs the effects of a higher supernova rate in the region. Our model also shows that phi(I) is increasing with time. Intelligent life emerged at approximately the present time at Earth's galactocentric radius, but a similar level of evolutionary opportunity was available in the inner Galaxy more than 2 Gyr ago. Our findings suggest that the inner Galaxy should logically be a prime target region for searches for extraterrestrial intelligence and that any civilizations that may have emerged there are potentially much older than our own. Key Words: Galactic habitable zone-Intelligent life-SETI. Astrobiology 15, 683-696. C1 [Morrison, Ian S.] Univ New S Wales, Sch Phys, Kensington, NSW 2033, Australia. [Morrison, Ian S.] Univ New S Wales, Australian Ctr Astrobiol, Kensington, NSW 2033, Australia. [Morrison, Ian S.] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia. [Gowanlock, Michael G.] Univ Hawaii, Dept Informat & Comp Sci, Honolulu, HI 96822 USA. [Gowanlock, Michael G.] Univ Hawaii, NASA Astrobiol Inst, Honolulu, HI 96822 USA. [Gowanlock, Michael G.] MIT, Haystack Observ, Westford, MA 01886 USA. RP Morrison, IS (reprint author), Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia. EM imorrison@swin.edu.au RI Morrison, Ian/E-4725-2016 OI Morrison, Ian/0000-0003-0833-0541 FU Australian Centre for Astrobiology at the University of New South Wales; NASA Astrobiology Institute at the University of Hawaii; National Aeronautics and Space Administration through the NASA Astrobiology Institute through the Office of Space Science [NNA08DA77A] FX The authors wish to acknowledge the support of the Australian Centre for Astrobiology at the University of New South Wales and the NASA Astrobiology Institute at the University of Hawaii. This material is based upon work supported by the National Aeronautics and Space Administration through the NASA Astrobiology Institute under Cooperative Agreement No. NNA08DA77A issued through the Office of Space Science. The authors are grateful for valuable feedback on the manuscript provided by Chris Tinney, David Flannery, Malcolm Walter, Carol Oliver, James Benford, Antonia Rowlinson, and the anonymous reviewers. Particular thanks to Chris Tinney for suggesting the inclusion of the galactic coordinate contour maps. NR 41 TC 1 Z9 1 U1 5 U2 32 PU MARY ANN LIEBERT, INC PI NEW ROCHELLE PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA SN 1531-1074 EI 1557-8070 J9 ASTROBIOLOGY JI Astrobiology PD AUG 1 PY 2015 VL 15 IS 8 BP 683 EP 696 DI 10.1089/ast.2014.1192 PG 14 WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics; Geology GA CP0VI UT WOS:000359593800005 PM 26274865 ER PT J AU Tian, L Heymsfield, GM Didlake, AC Guimond, S Li, LH AF Tian, Lin Heymsfield, Gerald M. Didlake, Anthony C. Guimond, Stephen Li, Lihua TI Velocity-Azimuth Display Analysis of Doppler Velocity for HIWRAP SO JOURNAL OF APPLIED METEOROLOGY AND CLIMATOLOGY LA English DT Article ID RADAR DATA; SQUALL LINE; WIND; ASSIMILATION; AIRCRAFT AB The velocity-azimuth display (VAD) analysis technique established for ground-based scanning radar is applied to the NASA High-Altitude Imaging Wind and Rain Airborne Profiler (HIWRAP). The VAD technique provides a mean vertical profile of the horizontal winds for each complete conical scan of the HIWRAP radar. One advantage of this technique is that it has shown great value for data assimilation and for operational forecasts. Another advantage is that it is computationally inexpensive, which makes it suitable for real-time retrievals. The VAD analysis has been applied to the HIWRAP data collected during NASA's Genesis and Rapid Intensification Processes (GRIP) mission. The traditional dual-Doppler analysis for deriving wind fields in the nadir plane is also presented and is compared with the VAD analysis. The results show that the along-track winds from the VAD technique and dual-Doppler analysis agree in general. The VAD horizontal winds capture the mean vortex structure of two tropical cyclones, and they are in general agreement with winds from nearby dropsondes. Several assumptions are made for the VAD technique. These assumptions include a stationary platform for each HIWRAP scan and constant vertical velocity of the hydrometeors along each complete scan. As a result, the VAD technique can produce appreciable errors in regions of deep convection such as the eyewall, whereas in stratiform regions the retrieval errors are minimal. Despite these errors, the VAD technique can still adequately capture the larger-scale structure of the hurricane vortex given a sufficient number of flight passes over the storm. C1 [Tian, Lin; Heymsfield, Gerald M.; Didlake, Anthony C.; Guimond, Stephen; Li, Lihua] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Tian, Lin] Morgan State Univ, Goddard Earth Sci Technol & Res, Baltimore, MD 21239 USA. [Didlake, Anthony C.] Oak Ridge Associated Univ, Oak Ridge, TN USA. [Guimond, Stephen] Univ Maryland, College Pk, MD 20742 USA. RP Didlake, AC (reprint author), NASA, Goddard Space Flight Ctr, Code 612, Greenbelt, MD 20771 USA. EM anthony.didlake@nasa.gov FU NASA Hurricane Science Research Program; NASA's Earth Venture Program FX We thank Professor Ramesh Srivastava for insightful discussions and for suggesting some of the analysis method. We also thank Dr. Jason Sippel for stimulating discussions on using Doppler radar data for data assimilation and Matthew McLinden, Jaime Cervantes, Martin Perrine, and Ed Zenker for engineering support and HIWRAP data processing. Funding for this work came from the NASA Hurricane Science Research Program under Dr. Ramesh Kakar and the Hurricane and Severe Storm Sentinel investigation under NASA's Earth Venture Program. NR 31 TC 1 Z9 1 U1 1 U2 6 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 1558-8424 EI 1558-8432 J9 J APPL METEOROL CLIM JI J. Appl. Meteorol. Climatol. PD AUG PY 2015 VL 54 IS 8 BP 1792 EP 1808 DI 10.1175/JAMC-D-14-0054.1 PG 17 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA CP0TU UT WOS:000359589500006 ER PT J AU Chen, YD Wang, HL Min, JZ Huang, XY Minnis, P Zhang, RZ Haggerty, J Palikonda, R AF Chen, Yaodeng Wang, Hongli Min, Jinzhong Huang, Xiang-Yu Minnis, Patrick Zhang, Ruizhi Haggerty, Julie Palikonda, Rabindra TI Variational Assimilation of Cloud Liquid/Ice Water Path and Its Impact on NWP SO JOURNAL OF APPLIED METEOROLOGY AND CLIMATOLOGY LA English DT Article ID RADAR DATA ASSIMILATION; INFRARED SATELLITE RADIANCES; LEVEL-II DATA; PART I; TORNADIC THUNDERSTORMS; TROPICAL CYCLONES; ANALYSIS SYSTEM; SQUALL LINE; FORT-WORTH; MODEL AB Analysis of the cloud components in numerical weather prediction models using advanced data assimilation techniques has been a prime topic in recent years. In this research, the variational data assimilation (DA) system for the Weather Research and Forecasting (WRF) Model (WRFDA) is further developed to assimilate satellite cloud products that will produce the cloud liquid water and ice water analysis. Observation operators for the cloud liquid water path and cloud ice water path are developed and incorporated into the WRFDA system. The updated system is tested by assimilating cloud liquid water path and cloud ice water path observations from Global Geostationary Gridded Cloud Products at NASA. To assess the impact of cloud liquid/ice water path data assimilation on short-term regional numerical weather prediction (NWP), 3-hourly cycling data assimilation and forecast experiments with and without the use of the cloud liquid/ice water paths are conducted. It is shown that assimilating cloud liquid/ice water paths increases the accuracy of temperature, humidity, and wind analyses at model levels between 300 and 150 hPa after 5 cycles (15 h). It is also shown that assimilating cloud liquid/ice water paths significantly reduces forecast errors in temperature and wind at model levels between 300 and 150 hPa. The precipitation forecast skills are improved as well. One reason that leads to the improved analysis and forecast is that the 3-hourly rapid update cycle carries over the impact of cloud information from the previous cycles spun up by the WRF Model. C1 [Chen, Yaodeng; Min, Jinzhong; Zhang, Ruizhi] Nanjing Univ Informat Sci & Technol, Key Lab Meteorol Disaster, Minist Educ, Nanjing, Jiangsu, Peoples R China. [Wang, Hongli] Colorado State Univ, Cooperat Inst Res Atmosphere, Ft Collins, CO 80523 USA. [Wang, Hongli] NOAA, Earth Syst Res Lab, Global Syst Div, Boulder, CO 80305 USA. [Huang, Xiang-Yu] Meteorol Serv Singapore, Ctr Climate Res Singapore, Singapore, Singapore. [Minnis, Patrick] NASA, Langley Res Ctr, Hampton, VA 23665 USA. [Haggerty, Julie] Natl Ctr Atmospher Res, Boulder, CO 80307 USA. [Palikonda, Rabindra] Sci Syst & Applicat Inc, Hampton, VA USA. RP Wang, HL (reprint author), NOAA, Earth Syst Res Lab, Global Syst Div, 325 Broadway, Boulder, CO 80305 USA. EM hongli.wang@noaa.gov RI Wang, Hongli/C-4579-2012 OI Wang, Hongli/0000-0003-0855-6743 FU 973 Program [2013CB430102]; National Natural Science Foundation of China [41205082]; Natural Science Foundation of Jiangsu [BK2012859]; Priority Academic Program Development of Jiangsu Higher Education Institutions (PAPD); NASA Model, Analysis, and Prediction Program FX This work is jointly sponsored by the 973 Program (2013CB430102), the National Natural Science Foundation of China (41205082), Natural Science Foundation of Jiangsu (BK2012859) and the Priority Academic Program Development of Jiangsu Higher Education Institutions (PAPD). Dr. Minnis and Dr. Palikonda are supported by the NASA Model, Analysis, and Prediction Program. The authors thank Dr. Thomas Auligne, Dr. Yuanfu Xie, and Dr. Zhiquan Liu for discussions on satellite radiance data assimilation. The authors also thank J. C. Osborn at NOAA for providing editorial support for this manuscript. NR 52 TC 4 Z9 4 U1 2 U2 13 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 1558-8424 EI 1558-8432 J9 J APPL METEOROL CLIM JI J. Appl. Meteorol. Climatol. PD AUG PY 2015 VL 54 IS 8 BP 1809 EP 1825 DI 10.1175/JAMC-D-14-0243.1 PG 17 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA CP0TU UT WOS:000359589500007 ER PT J AU Kang, SM Kim, BM Frierson, DMW Jeong, SJ Seo, J Chae, Y AF Kang, Sarah M. Kim, Baek-Min Frierson, Dargan M. W. Jeong, Su-Jong Seo, Jeongbin Chae, Yoojeong TI Seasonal Dependence of the Effect of Arctic Greening on Tropical Precipitation SO JOURNAL OF CLIMATE LA English DT Article ID SYSTEM MODEL; CLIMATE; AMPLIFICATION; CIRCULATION; OCEAN; ITCZ; GCM AB This paper examines the seasonal dependence of the effect of Arctic greening on tropical precipitation. In CAM3/CLM3 coupled to a mixed layer ocean, shrub and grasslands poleward of 60 degrees N are replaced with boreal forests. With darker Arctic vegetation, the absorption of solar energy increases, but primarily in boreal spring and summer since little insolation reaches the Arctic in boreal winter. The net energy input into the northern extratropics is partly balanced by southward atmospheric energy transport across the equator by an anomalous Hadley circulation, resulting in a northward shift of the tropical precipitation. In contrast, in boreal fall, the slight increase in insolation over the Arctic is more than offset by increased outgoing longwave radiation and reduced surface turbulent fluxes in midlatitudes, from the warmer atmosphere. As a result, the Northern Hemisphere atmosphere loses energy, which is compensated by a northward cross-equatorial atmospheric energy transport, leading to a southward shift of the tropical precipitation in boreal fall. Thus, although Arctic vegetation is changed throughout the year, its effect on tropical precipitation exhibits substantial seasonal variations. C1 [Kang, Sarah M.; Seo, Jeongbin; Chae, Yoojeong] Ulsan Natl Inst Sci & Technol, Sch Urban & Environm Engn, Ulsan 689798, South Korea. [Kim, Baek-Min] Korea Polar Res Inst, Div Polar Climate Change Res, Inchon, South Korea. [Frierson, Dargan M. W.] Univ Washington, Dept Atmospher Sci, Seattle, WA 98195 USA. [Jeong, Su-Jong] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Kang, SM (reprint author), Ulsan Natl Inst Sci & Technol, Sch Urban & Environm Engn, UNIST Gil 50, Ulsan 689798, South Korea. EM skang@unist.ac.kr RI Jeong, Su-Jong/J-4110-2014; Frierson, Dargan/F-1763-2010 OI Frierson, Dargan/0000-0001-8952-5644 FU Basic Science Research Program through the National Research Foundation of Korea (NRF) - Ministry of Science, ICT and Future Planning [2013R1A1A3004589]; National Research Foundation of Korea Grant - Korean Government (MSIP) [NRF-C1ABA001-2011-0021063, KOPRI-PN14083]; NSF award [AGS-0846641, AGS-0936059, AGS-1359464] FX The authors thank two anonymous reviewers and Aiko Voigt for constructive comments. SMK is supported by Basic Science Research Program through the National Research Foundation of Korea (NRF) funded by the Ministry of Science, ICT and Future Planning (2013R1A1A3004589). BMK is supported by the National Research Foundation of Korea Grant funded by the Korean Government (MSIP) (NRF-C1ABA001-2011-0021063) (KOPRI-PN14083). DMWF is supported by NSF awards AGS-0846641, AGS-0936059, and AGS-1359464. NR 25 TC 3 Z9 3 U1 1 U2 6 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0894-8755 EI 1520-0442 J9 J CLIMATE JI J. Clim. PD AUG PY 2015 VL 28 IS 15 BP 6086 EP 6095 DI 10.1175/JCLI-D-15-0079.1 PG 10 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA CO9YM UT WOS:000359532800013 ER PT J AU Del Genio, AD Wu, JB Wolf, AB Chen, YH Yao, MS Kim, D AF Del Genio, Anthony D. Wu, Jingbo Wolf, Audrey B. Chen, Yonghua Yao, Mao-Sung Kim, Daehyun TI Constraints on Cumulus Parameterization from Simulations of Observed MJO Events SO JOURNAL OF CLIMATE LA English DT Review ID MADDEN-JULIAN OSCILLATION; STATIC ENERGY BUDGET; TROPICAL INTRASEASONAL OSCILLATIONS; MOISTURE-CONVECTION FEEDBACKS; GENERAL-CIRCULATION MODELS; COUPLED EQUATORIAL WAVES; PART I; DEEP CONVECTION; CLIMATE MODELS; PHYSICAL PROCESSES AB Two recent activities offer an opportunity to test general circulation model (GCM) convection and its interaction with large-scale dynamics for observed Madden-Julian oscillation (MJO) events. This study evaluates the sensitivity of the Goddard Institute for Space Studies (GISS) GCM to entrainment, rain evaporation, downdrafts, and cold pools. Single Column Model versions that restrict weakly entraining convection produce the most realistic dependence of convection depth on column water vapor (CWV) during the Atmospheric Radiation Measurement MJO Investigation Experiment at Gan Island. Differences among models are primarily at intermediate CWV where the transition from shallow to deeper convection occurs. GCM 20-day hindcasts during the Year of Tropical Convection that best capture the shallow-deep transition also produce strong MJOs, with significant predictability compared to Tropical Rainfall Measuring Mission data. The dry anomaly east of the disturbance on hindcast day 1 is a good predictor of MJO onset and evolution. Initial CWV there is near the shallow-deep transition point, implicating premature onset of deep convection as a predictor of a poor MJO simulation. Convection weakly moistens the dry region in good MJO simulations in the first week; weakening of large-scale subsidence over this time may also affect MJO onset. Longwave radiation anomalies are weakest in the worst model version, consistent with previous analyses of cloud/moisture greenhouse enhancement as the primary MJO energy source. The authors' results suggest that both cloud-/moisture-radiative interactions and convection-moisture sensitivity are required to produce a successful MJO simulation. C1 [Del Genio, Anthony D.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Wu, Jingbo; Wolf, Audrey B.; Chen, Yonghua] Columbia Univ, Dept Appl Phys & Appl Math, New York, NY USA. [Yao, Mao-Sung] Trinnovim LLC, Inst Space Studies, New York, NY USA. [Kim, Daehyun] Univ Washington, Dept Atmospher Sci, Seattle, WA 98195 USA. RP Del Genio, AD (reprint author), NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA. EM anthony.d.delgenio@nasa.gov FU NASA [NNX09AK34G]; NASA; U.S. Department of Energy (DOE); DOE FASTER FX This research was supported by the NASA Modeling and Analysis Program through an RTOP for GISS GCM development and Grant NNX09AK34G; by a NASA Precipitation Measurement Missions Program RTOP; by an Interagency Agreement with the U.S. Department of Energy (DOE) Atmospheric System Research Program; and by a grant from the DOE FASTER Program. We thank three anonymous reviewers for constructive comments that improved the manuscript. NR 108 TC 11 Z9 11 U1 0 U2 12 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0894-8755 EI 1520-0442 J9 J CLIMATE JI J. Clim. PD AUG PY 2015 VL 28 IS 16 BP 6419 EP 6442 DI 10.1175/JCLI-D-14-00832.1 PG 24 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA CP1SJ UT WOS:000359655200008 ER PT J AU Cecil, DJ Buechler, DE Blakeslee, RJ AF Cecil, Daniel J. Buechler, Dennis E. Blakeslee, Richard J. TI TRMM LIS Climatology of Thunderstorm Occurrence and Conditional Lightning Flash Rates* SO JOURNAL OF CLIMATE LA English DT Article ID FREQUENCY AB The Lightning Imaging Sensor (LIS) on the Tropical Rainfall Measuring Mission (TRMM) satellite has previously been used to build climatologies of mean lightning flash rate across the global tropics and subtropics. This new work explores climatologies of thunderstorm occurrence as seen by LIS and the conditional mean flash rates when thunderstorms do occur. The region where thunderstorms are seen most often by LIS extends slightly farther east in central Africa than the corresponding region with the highest total mean annual flash rates. Presumably this reflects a difference between more frequent thunderstorm initiation in the east and upscale growth as storms move westward. There are some differences between locations with the greatest total lightning flash counts and those where thunderstorms occur most often. The greatest conditional mean flash rates-considering only those TRMM orbits that do have lightning in a given grid box-are found in subtropical regions. The highest values are in Argentina, with the central United States, Pakistan, eastern China, and the east coast of Australia also having particularly high values. C1 [Cecil, Daniel J.; Blakeslee, Richard J.] NASA Marshall Space Flight Ctr, Huntsville, AL USA. [Buechler, Dennis E.] Univ Alabama, Huntsville, AL 35899 USA. RP Cecil, DJ (reprint author), NASA MSFC Earth Sci Off, 320 Sparkman Dr NW, Huntsville, AL 35805 USA. EM danieljcecil@nasa.gov FU NASA FX This research benefits from over two decades of work by past and present members of the lightning team associated with NASA MSFC. In particular, the gridded climatologies were updated using source code originally developed by Dennis Boccippio. Sponsorship and support for the OTD and LIS data are from the NASA Earth Observing System and the Tropical Rainfall Measuring Mission. LIS and OTD data, including the gridded climatologies produced here, are distributed by the NASA EOSDIS Global Hydrology Resource Center DAAC, Huntsville, Alabama (http://lightning.nsstc.nasa.gov). NR 16 TC 2 Z9 2 U1 6 U2 13 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0894-8755 EI 1520-0442 J9 J CLIMATE JI J. Clim. PD AUG PY 2015 VL 28 IS 16 BP 6536 EP 6547 DI 10.1175/JCLI-D-15-0124.1 PG 12 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA CP1SJ UT WOS:000359655200015 ER PT J AU Badgley, G Fisher, JB Jimenez, C Tu, KP Vinukollu, R AF Badgley, Grayson Fisher, Joshua B. Jimenez, Carlos Tu, Kevin P. Vinukollu, Raghuveer TI On Uncertainty in Global Terrestrial Evapotranspiration Estimates from Choice of Input Forcing Datasets SO JOURNAL OF HYDROMETEOROLOGY LA English DT Article DE Hydrologic cycle; Energy budget; balance; Evapotranspiration; Trends ID CLIMATE; MODIS; WATER; BUDGET; AVHRR; ALGORITHM; GRIDS; FLUX AB Evapotranspiration ET is a critical water, energy, and climate variable, and recent work has been published comparing different global products. These comparisons have been difficult to interpret, however, because in most studies the evapotranspiration products were derived from models forced by different input data. Some studies have analyzed the uncertainty in regional evapotranspiration estimates from choice of forcings. Still others have analyzed how multiple models vary with choice of net radiation forcing data. However, no analysis has been conducted to determine the uncertainty in global evapotranspiration estimates attributable to each class of input forcing datasets. Here, one of these models [Priestly-Taylor JPL (PT-JPL)] is run with 19 different combinations of forcing data. These data include three net radiation products (SRB, CERES, and ISCCP), three meteorological datasets [CRU, Atmospheric Infrared Sounder (AIRS) Aqua, and MERRA], and three vegetation index products [MODIS; Global Inventory Modeling and Mapping Studies (GIMMS); and Fourier-Adjusted, Sensor and Solar Zenith Angle Corrected, Interpolated, Reconstructed (FASIR)]. The choice in forcing data produces an average range in global monthly evapotranspiration of 10.6 W m(-2) (similar to 20% of global mean evapotranspiration), with net radiation driving the majority of the difference. Annual average terrestrial ET varied by an average of 8 W m(-2), depending on choice of forcings. The analysis shows that the greatest disagreement between input forcings arises from choice of net radiation dataset. In particular, ISCCP data, which are frequently used in global studies, differed widely from the other radiation products examined and resulted in dramatically different estimates of global terrestrial ET. C1 [Badgley, Grayson] Carnegie Inst Sci, Dept Global Ecol, Stanford, CA 94305 USA. [Fisher, Joshua B.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Jimenez, Carlos] CNRS, Lab Etud Rayonnement & Mat Astrophys, Paris, France. [Tu, Kevin P.] Theiss Res, Davis, CA USA. [Vinukollu, Raghuveer] Swiss Re, Armonk, NY USA. RP Badgley, G (reprint author), Carnegie Inst Sci, Dept Global Ecol, 260 Panama St, Stanford, CA 94305 USA. EM badgley@stanford.edu OI Fisher, Joshua/0000-0003-4734-9085 FU NASA's Terrestrial Hydrology Program; JPL's Research and Technology Development Strategic Climate and Water Initiatives; National Aeronautics and Space Administration FX We thank the Global Modeling and Assimilation Office (GMAO) and the GES DISC for the dissemination of MERRA. MODIS data were distributed by the Land Processes Distributed Active Archive Center (LP DAAC), located at the U.S. Geological Survey (USGS) Earth Resources Observation and Science (EROS) Center (lpdaac.usgs.gov). CERES data were obtained from the NASA Langley Research Center Atmospheric Science Data Center. A special thanks to T. Troy and E. Wood for providing ISCCP and SRB net radiation data. D. Armanios assisted in processing the AIRS data. M. Jung and M. McCabe provided helpful reviews. Funding was provided by NASA's Terrestrial Hydrology Program and by JPL's Research and Technology Development Strategic Climate and Water Initiatives. The research described in this paper was carried out by the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. Government sponsorship acknowledged. NR 33 TC 7 Z9 7 U1 0 U2 10 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 1525-755X EI 1525-7541 J9 J HYDROMETEOROL JI J. Hydrometeorol. PD AUG PY 2015 VL 16 IS 4 BP 1449 EP 1455 DI 10.1175/JHM-D-14-0040.1 PG 7 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA CP3FI UT WOS:000359762700001 ER PT J AU Koster, RD Walker, GK AF Koster, R. D. Walker, G. K. TI Interactive Vegetation Phenology, Soil Moisture, and Monthly Temperature Forecasts SO JOURNAL OF HYDROMETEOROLOGY LA English DT Article DE Vegetation-atmosphere interactions; Soil moisture; Forecasting techniques; Seasonal forecasting; Vegetation-atmosphere interactions ID SOLAR-RADIATION; PART I; CLIMATE; PREDICTABILITY; VARIABILITY; SYSTEM; PARAMETERIZATION; CONVECTION; RAINFALL; DATASET AB The time scales that characterize the variations of vegetation phenology are generally much longer than those that characterize atmospheric processes. The explicit modeling of phenological processes in an atmospheric forecast system thus has the potential to provide skill to subseasonal or seasonal forecasts. We examine this possibility here using a forecast system fitted with a dynamic vegetation phenology model. We perform three experiments, each consisting of 128 independent warm-season monthly forecasts: 1) an experiment in which both soil moisture states and carbon states (e.g., those determining leaf area index) are initialized realistically, 2) an experiment in which the carbon states are prescribed to climatology throughout the forecasts, and 3) an experiment in which both the carbon and soil moisture states are prescribed to climatology throughout the forecasts. Evaluating the monthly forecasts of air temperature in each ensemble against observationsas well as quantifying the inherent predictability of temperature within each ensembleshows that dynamic phenology can indeed contribute positively to subseasonal forecasts, though only to a small extent, with an impact dwarfed by that of soil moisture. C1 [Koster, R. D.; Walker, G. K.] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA. [Walker, G. K.] Sci Syst & Applicat Inc, Lanham, MD USA. RP Koster, RD (reprint author), NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Code 610-1, Greenbelt, MD 20771 USA. EM randal.d.koster@nasa.gov RI Koster, Randal/F-5881-2012 OI Koster, Randal/0000-0001-6418-6383 FU NASA's Modeling, Analysis, and Prediction Program FX We thank Peter Thornton for his help with the development of the Catchment-CN model. This research was supported by NASA's Modeling, Analysis, and Prediction Program. NR 36 TC 2 Z9 2 U1 0 U2 19 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 1525-755X EI 1525-7541 J9 J HYDROMETEOROL JI J. Hydrometeorol. PD AUG PY 2015 VL 16 IS 4 BP 1456 EP 1465 DI 10.1175/JHM-D-14-0205.1 PG 10 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA CP3FI UT WOS:000359762700002 ER PT J AU Carr, N Kirstetter, PE Hong, Y Gourley, JJ Schwaller, M Petersen, W Wang, NY Ferraro, RR Xue, XW AF Carr, N. Kirstetter, P. -E. Hong, Y. Gourley, J. J. Schwaller, M. Petersen, W. Wang, Nai-Yu Ferraro, Ralph R. Xue, Xianwu TI The Influence of Surface and Precipitation Characteristics on TRMM Microwave Imager Rainfall Retrieval Uncertainty SO JOURNAL OF HYDROMETEOROLOGY LA English DT Article DE Precipitation; Rainfall; Microwave observations; Radars; Radar observations; Satellite observations ID NUMERICAL WEATHER PREDICTION; DATA ASSIMILATION; FUTURE-PLANS; AMSR-E; RADAR; ALGORITHMS; TMI; QPE; EMISSIVITIES; SENSORS AB Characterization of the error associated with quantitative precipitation estimates (QPEs) from spaceborne passive microwave (PMW) sensors is important for a variety of applications ranging from flood forecasting to climate monitoring. This study evaluates the joint influence of precipitation and surface characteristics on the error structure of NASA's Tropical Rainfall Measurement Mission (TRMM) Microwave Imager (TMI) surface QPE product (2A12). TMI precipitation products are compared with high-resolution reference precipitation products obtained from the NOAA/NSSL ground radar-based Multi-Radar Multi-Sensor (MRMS) system. Surface characteristics were represented via a surface classification dataset derived from NASA's Moderate Resolution Imaging Spectroradiometer (MODIS). This study assesses the ability of 2A12 to detect, classify, and quantify precipitation at its native resolution for the 2011 warm season (March-September) over the southern continental United States. Decreased algorithm performance is apparent over dry and sparsely vegetated regions, a probable result of the surface radiation signal mimicking the scattering signature associated with frozen hydrometeors. Algorithm performance is also shown to be positively correlated with precipitation coverage over the sensor footprint. The algorithm also performs better in pure stratiform and convective precipitation events, compared to events containing a mixture of stratiform and convective precipitation within the footprint. This possibly results from the high spatial gradients of precipitation associated with these events and an underrepresentation of such cases in the retrieval database. The methodology and framework developed herein apply more generally to precipitation estimates from other passive microwave sensors on board low-Earth-orbiting satellites and specifically could be used to evaluate PMW sensors associated with the recently launched Global Precipitation Measurement (GPM) mission. C1 [Carr, N.] Univ Oklahoma, Sch Meteorol, Norman, OK 73019 USA. [Carr, N.; Kirstetter, P. -E.] Natl Weather Ctr, Adv Radar Res Ctr, Norman, OK 73072 USA. [Kirstetter, P. -E.; Gourley, J. J.] NOAA, Natl Severe Storms Lab, Norman, OK 73069 USA. [Hong, Y.; Xue, Xianwu] Univ Oklahoma, Sch Civil Engn & Environm Sci, Norman, OK 73019 USA. [Schwaller, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Petersen, W.] NASA, Wallops Flight Facil, Wallops Isl, VA USA. [Wang, Nai-Yu] IM Syst Grp, College Pk, MD USA. [Ferraro, Ralph R.] NOAA, NESDIS, College Pk, MD USA. RP Carr, N (reprint author), Natl Weather Ctr, Adv Radar Res Ctr, 120 David L Boren Blvd,Rm 4630, Norman, OK 73072 USA. EM n.carr2@ou.edu RI Kirstetter, Pierre/E-2305-2013; Ferraro, Ralph/F-5587-2010; Gourley, Jonathan/C-7929-2016; Xue, Xianwu/C-8006-2016; Wang, Nai-Yu/E-5303-2016; Measurement, Global/C-4698-2015; Hong, Yang/D-5132-2009 OI Kirstetter, Pierre/0000-0002-7381-0229; Ferraro, Ralph/0000-0002-8393-7135; Gourley, Jonathan/0000-0001-7363-3755; Xue, Xianwu/0000-0002-2106-6370; Hong, Yang/0000-0001-8720-242X FU NASA Global Precipitation Measurement Mission Ground Validation Management; NASA Precipitation Measurement Mission grant FX We are very much indebted to the team responsible for the Q2 products, especially Carrie Langston. We thank Dr. G. Huffman for very insightful comments. The lead author was supported by a grant from the NASA Global Precipitation Measurement Mission Ground Validation Management. The work was cosupported by a NASA Precipitation Measurement Mission grant. NR 41 TC 3 Z9 3 U1 2 U2 7 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 1525-755X EI 1525-7541 J9 J HYDROMETEOROL JI J. Hydrometeorol. PD AUG PY 2015 VL 16 IS 4 BP 1596 EP 1614 DI 10.1175/JHM-D-14-0194.1 PG 19 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA CP3FI UT WOS:000359762700010 ER PT J AU Wood, EF Schubert, SD Wood, AW Peters-Lidard, CD Mo, KC Mariotti, A Pulwarty, RS AF Wood, Eric F. Schubert, Siegfried D. Wood, Andrew W. Peters-Lidard, Christa D. Mo, Kingtse C. Mariotti, Annarita Pulwarty, Roger S. TI Prospects for Advancing Drought Understanding, Monitoring, and Prediction SO JOURNAL OF HYDROMETEOROLOGY LA English DT Article DE ENSO; Hydrology; Nowcasting; Seasonal forecasting; Land surface model ID AMERICAN MULTIMODEL ENSEMBLE; UNITED-STATES; SOIL-MOISTURE; FRAMEWORK; TRENDS; MODEL; PRECIPITATION; SIMULATIONS; TEMPERATURE; VARIABILITY AB This paper summarizes and synthesizes the research carried out under the NOAA Drought Task Force (DTF) and submitted in this special collection. The DTF is organized and supported by NOAA's Climate Program Office with the National Integrated Drought Information System (NIDIS) and involves scientists from across NOAA, academia, and other agencies. The synthesis includes an assessment of successes and remaining challenges in monitoring and prediction capabilities, as well as a perspective of the current understanding of North American drought and key research gaps. Results from the DTF papers indicate that key successes for drought monitoring include the application of modern land surface hydrological models that can be used for objective drought analysis, including extended retrospective forcing datasets to support hydrologic reanalyses, and the expansion of near-real-time satellite-based monitoring and analyses, particularly those describing vegetation and evapotranspiration. In the area of drought prediction, successes highlighted in the papers include the development of the North American Multimodel Ensemble (NMME) suite of seasonal model forecasts, an established basis for the importance of La Nina in drought events over the southern Great Plains, and an appreciation of the role of internal atmospheric variability related to drought events. Despite such progress, there are still important limitations in our ability to predict various aspects of drought, including onset, duration, severity, and recovery. Critical challenges include (i) the development of objective, science-based integration approaches for merging multiple information sources; (ii) long, consistent hydro-meteorological records to better characterize drought; and (iii) extending skillful precipitation forecasts beyond a 1-month lead time. C1 [Wood, Eric F.] Princeton Univ, Dept Civil & Environm Engn, Princeton, NJ 08544 USA. [Schubert, Siegfried D.] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA. [Wood, Andrew W.] NCAR, Res Applicat Lab, Boulder, CO USA. [Peters-Lidard, Christa D.] NASA, Goddard Space Flight Ctr, Hydrol Sci Lab, Greenbelt, MD 20771 USA. [Mo, Kingtse C.] NOAA, NCEP, Climate Predict Ctr, College Pk, MD USA. [Mariotti, Annarita; Pulwarty, Roger S.] NOAA, Climate Program Off, OAR, Silver Spring, MD USA. [Pulwarty, Roger S.] NOAA, Div Phys Sci, ESRL, Boulder, CO USA. RP Wood, EF (reprint author), Princeton Univ, Civil & Environm Engn, Olden St,EQUAD E415, Princeton, NJ 08544 USA. EM efwood@princeton.edu RI Peters-Lidard, Christa/E-1429-2012 OI Peters-Lidard, Christa/0000-0003-1255-2876 NR 47 TC 9 Z9 9 U1 5 U2 42 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 1525-755X EI 1525-7541 J9 J HYDROMETEOROL JI J. Hydrometeorol. PD AUG PY 2015 VL 16 IS 4 BP 1636 EP 1657 DI 10.1175/JHM-D-14-0164.1 PG 22 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA CP3FI UT WOS:000359762700012 ER PT J AU Seo, BC Dolan, B Krajewski, WF Rutledge, SA Petersen, W AF Seo, Bong-Chul Dolan, Brenda Krajewski, Witold F. Rutledge, Steven A. Petersen, Walter TI Comparison of Single- and Dual-Polarization-Based Rainfall Estimates Using NEXRAD Data for the NASA Iowa Flood Studies Project SO JOURNAL OF HYDROMETEOROLOGY LA English DT Article DE Radars; Radar observations; Remote sensing ID RANGE-DEPENDENT ERROR; SMALL-SCALE RAINFALL; RADAR-RAINFALL; HYDROMETEOR CLASSIFICATION; WSR-88D; REFLECTIVITY; ALGORITHM; PRECIPITATION; VALIDATION; SATELLITE AB This study compares and evaluates single-polarization (SP)- and dual-polarization (DP)-based radar-rainfall (RR) estimates using NEXRAD data acquired during Iowa Flood Studies (IFloodS), a NASA GPM ground validation field campaign carried out in May-June 2013. The objective of this study is to understand the potential benefit of the DP quantitative precipitation estimation, which selects different rain-rate estimators according to radar-identified precipitation types, and to evaluate RR estimates generated by the recent research SP and DP algorithms. The Iowa Flood Center SP (IFC-SP) and Colorado State University DP (CSU-DP) products are analyzed and assessed using two high-density, high-quality rain gauge networks as ground reference. The CSU-DP algorithm shows superior performance to the IFC-SP algorithm, especially for heavy convective rains. We verify that dynamic changes in the proportion of heavy rain during the convective period are associated with the improved performance of CSU-DP rainfall estimates. For a lighter rain case, the IFC-SP and CSU-DP products are not significantly different in statistical metrics and visual agreement with the rain gauge data. This is because both algorithms use the identical NEXRAD reflectivity-rain rate (Z-R) relation that might lead to substantial underestimation for the presented case. C1 [Seo, Bong-Chul; Krajewski, Witold F.] Univ Iowa, IIHR Hydrosci & Engn, Iowa City, IA 52242 USA. [Dolan, Brenda; Rutledge, Steven A.] Colorado State Univ, Dept Atmospher Sci, Ft Collins, CO 80523 USA. [Petersen, Walter] NASA, GSFC, Wallops Flight Facil, Wallops, VA USA. RP Seo, BC (reprint author), Univ Iowa, IIHR Hydrosci & Engn, Maxwell Stanley Hydraul Lab 100 C, Iowa City, IA 52242 USA. EM bongchul-seo@uiowa.edu RI Measurement, Global/C-4698-2015 FU NASA Iowa Flood Studies; Iowa Flood Center; National Science Foundation [EAR-1327830]; PMM/GPM Program FX This study was supported by NASA Iowa Flood Studies collaborating with the Iowa Flood Center. The National Science Foundation provided partial support under Award EAR-1327830. The authors are grateful to Daniel Ceynar, James Niemeier, and volunteer students who contributed to the operation of rain gauge networks in Iowa City and the Turkey River basin. We thank Prof. V. Chandrasekar for providing the software for Kdp calculation and HCS-R. We would also like to thank Jeffrey Cunningham at the Radar Operations Center for assisting with NEXRAD calibration assessment and Paul Hein at Colorado State University for his help with processing the large amount of NEXRAD data. The authors are grateful to the PMM/GPM Program Management for their support of IFloodS and this research. NR 40 TC 3 Z9 3 U1 2 U2 9 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 1525-755X EI 1525-7541 J9 J HYDROMETEOROL JI J. Hydrometeorol. PD AUG PY 2015 VL 16 IS 4 BP 1658 EP 1675 DI 10.1175/JHM-D-14-0169.1 PG 18 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA CP3FI UT WOS:000359762700013 ER PT J AU Kumar, SV Peters-Lidard, CD Arsenault, KR Getirana, A Mocko, D Liu, YQ AF Kumar, Sujay V. Peters-Lidard, Christa D. Arsenault, Kristi R. Getirana, Augusto Mocko, David Liu, Yuqiong TI Quantifying the Added Value of Snow Cover Area Observations in Passive Microwave Snow Depth Data Assimilation SO JOURNAL OF HYDROMETEOROLOGY LA English DT Article DE Snowpack; Snow cover; Data assimilation; Land surface model ID LAND-SURFACE MODEL; PRODUCTS AB Accurate determination of snow conditions is important for several water management applications, partly because of the significant influence of snowmelt on seasonal streamflow prediction. This article examines an approach using snow cover area (SCA) observations as snow detection constraints during the assimilation of snow depth retrievals from passive microwave sensors. Two different SCA products [the Interactive Multi-sensor Snow and Ice Mapping System (IMS) and the Moderate Resolution Imaging Spectroradiometer (MODIS)] are employed jointly with the snow depth retrievals from a variety of sensors for data assimilation in the Noah land surface model. The results indicate that the use of MODIS data is effective in obtaining added improvements (up to 6% improvement in aggregate RMSE) in snow depth fields compared to assimilating passive microwave data alone, whereas the impact of IMS data is small. The improvements in snow depth fields are also found to translate to small yet systematic improvements in streamflow estimates, especially over the western United States, the upper Missouri River, and parts of the Northeast and upper Mississippi River. This study thus demonstrates a simple approach for exploiting the information from SCA observations in data assimilation. C1 [Kumar, Sujay V.; Arsenault, Kristi R.; Mocko, David] Sci Applicat Int Corp, Mclean, VA USA. [Kumar, Sujay V.; Peters-Lidard, Christa D.; Arsenault, Kristi R.; Getirana, Augusto; Mocko, David; Liu, Yuqiong] NASA, GSFC, Hydrol Sci Lab, Greenbelt, MD 20771 USA. [Getirana, Augusto; Liu, Yuqiong] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. [Mocko, David] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA. RP Kumar, SV (reprint author), NASA, GSFC, Hydrol Sci Lab, Code 617, Greenbelt, MD 20771 USA. EM sujay.v.kumar@nasa.gov RI Peters-Lidard, Christa/E-1429-2012 OI Peters-Lidard, Christa/0000-0003-1255-2876 FU NASA Science Mission Directorate's Earth Science Division through National Climate Assessment (NCA) project; NOAA's Climate Program Office MAPP program FX Funding for this work was provided by the NASA Science Mission Directorate's Earth Science Division through the National Climate Assessment (NCA) project and NOAA's Climate Program Office MAPP program. NR 18 TC 4 Z9 4 U1 1 U2 9 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 1525-755X EI 1525-7541 J9 J HYDROMETEOROL JI J. Hydrometeorol. PD AUG PY 2015 VL 16 IS 4 BP 1736 EP 1741 DI 10.1175/JHM-D-15-0021.1 PG 6 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA CP3FI UT WOS:000359762700017 ER PT J AU Margulis, SA Girotto, M Cortes, G Durand, M AF Margulis, Steven A. Girotto, Manuela Cortes, Gonzalo Durand, Michael TI A Particle Batch Smoother Approach to Snow Water Equivalent Estimation SO JOURNAL OF HYDROMETEOROLOGY LA English DT Article ID SIERRA-NEVADA; DATA ASSIMILATION; RIVER-BASIN; COVER DATA; MODEL; ALBEDO; MODIS; INTERPOLATION; VARIABILITY; SIMULATION AB This paper presents a newly proposed data assimilation method for historical snow water equivalent SWE estimation using remotely sensed fractional snow-covered area fSCA. The newly proposed approach consists of a particle batch smoother (PBS), which is compared to a previously applied Kalman-based ensemble batch smoother (EnBS) approach. The methods were applied over the 27-yr Landsat 5 record at snow pillow and snow course in situ verification sites in the American River basin in the Sierra Nevada (United States). This basin is more densely vegetated and thus more challenging for SWE estimation than the previous applications of the EnBS. Both data assimilation methods provided significant improvement over the prior (modeling only) estimates, with both able to significantly reduce prior SWE biases. The prior RMSE values at the snow pillow and snow course sites were reduced by 68%-82% and 60%-68%, respectively, when applying the data assimilation methods. This result is encouraging for a basin like the American where the moderate to high forest cover will necessarily obscure more of the snow-covered ground surface than in previously examined, less-vegetated basins. The PBS generally outperformed the EnBS: for snow pillows the PBS RMSE was similar to 54% of that seen in the EnBS, while for snow courses the PBS RMSE was similar to 79% of the EnBS. Sensitivity tests show relative insensitivity for both the PBS and EnBS results to ensemble size and fSCA measurement error, but a higher sensitivity for the EnBS to the mean prior precipitation input, especially in the case where significant prior biases exist. C1 [Margulis, Steven A.; Cortes, Gonzalo] Univ Calif Los Angeles, Dept Civil & Environm Engn, Los Angeles, CA 90095 USA. [Girotto, Manuela] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Girotto, Manuela] Univ Space Res Assoc, GESTAR, Columbia, MD USA. [Durand, Michael] Ohio State Univ, Sch Earth Sci, Columbus, OH 43210 USA. [Durand, Michael] Ohio State Univ, Byrd Polar Res Ctr, Columbus, OH 43210 USA. RP Margulis, SA (reprint author), Univ Calif Los Angeles, Dept Civil & Environm Engn, 5732D Boelter Hall, Los Angeles, CA 90095 USA. EM margulis@seas.ucla.edu FU National Science Foundation [EAR-0943551, EAR-0943681, EAR-1246473]; NASA Earth System Science Fellowship [NNX11AL58H] FX This was based in part upon work supported by the National Science Foundation under Grants EAR-0943551, EAR-0943681, and EAR-1246473 and a NASA Earth System Science Fellowship (Grant NNX11AL58H). The NLDAS-2 data used in this study were acquired as part of the mission of NASA's Earth Science Division and are archived and distributed by the Goddard Earth Sciences (GES) Data and Information Services Center (DISC). The raw Landsat data were obtained from the USGS Earth Explorer (http://earthexplorer.usgs.gov/). NR 46 TC 8 Z9 8 U1 3 U2 8 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 1525-755X EI 1525-7541 J9 J HYDROMETEOROL JI J. Hydrometeorol. PD AUG PY 2015 VL 16 IS 4 BP 1752 EP 1772 DI 10.1175/JHM-D-14-0177.1 PG 21 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA CP3FI UT WOS:000359762700019 ER PT J AU Hafliger, V Martin, E Boone, A Habets, F David, CH Garambois, PA Roux, H Ricci, S Berthon, L Thevenin, A Biancamaria, S AF Haefliger, Vincent Martin, Eric Boone, Aaron Habets, Florence David, Cedric H. Garambois, Pierre-A. Roux, Helene Ricci, Sophie Berthon, Lucie Thevenin, Anthony Biancamaria, Sylvain TI Evaluation of Regional-Scale River Depth Simulations Using Various Routing Schemes within a Hydrometeorological Modeling Framework for the Preparation of the SWOT Mission SO JOURNAL OF HYDROMETEOROLOGY LA English DT Article ID LAND-SURFACE; GLOBAL EVALUATION; IN-SITU; PART I; WATER; PARAMETERS; DATABASE; STORAGE; BASIN; ASSIMILATION AB The Surface Water and Ocean Topography (SWOT) mission will provide free water surface elevations, slopes, and river widths for rivers wider than 50 m. Models must be prepared to use this new finescale information by explicitly simulating the link between runoff and the river channel hydraulics. This study assesses one regional hydrometeorological model's ability to simulate river depths. The Garonne catchment in southwestern France (56 000 km(2)) has been chosen for the availability of operational gauges in the river network and finescale hydraulic models over two reaches of the river. Several routing schemes, ranging from the simple Muskingum method to time-variable parameter kinematic and diffusive waves schemes, are tested. The results show that the variable flow velocity schemes are advantageous for discharge computations when compared to the original Muskingum routing method. Additionally, comparisons between river depth computations and in situ observations in the downstream Garonne River led to root-mean-square errors of 50-60 cm in the improved Muskingum method and 40-50 cm in the kinematic-diffusive wave method. The results also highlight SWOT's potential to improve the characterization of hydrological processes for subbasins larger than 10 000 km(2), the importance of an accurate digital elevation model, and the need for spatially varying hydraulic parameters. C1 [Haefliger, Vincent; Martin, Eric; Boone, Aaron] CNRS, CNRM GAME, UMR 3589, Meteo France, F-31057 Toulouse, France. [Haefliger, Vincent] Ctr Natl Etud Spatiales, F-31055 Toulouse, France. [Habets, Florence] UPMC, CNRS, UMR METIS 7619, Paris, France. [David, Cedric H.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Garambois, Pierre-A.; Roux, Helene] Univ Toulouse, INPT, Inst Mecan Fluides Toulouse, UPS, Toulouse, France. [Ricci, Sophie; Berthon, Lucie; Thevenin, Anthony] CERFACS, URA 1875, Toulouse, France. [Biancamaria, Sylvain] Univ Toulouse 3, CNES IRD, LEGOS, UMR 5566, Toulouse, France. RP Hafliger, V (reprint author), CNRS, CNRM GAME, UMR 3589, Meteo France, 42 Av Gaspard Coriolis, F-31057 Toulouse, France. EM vincent.haefliger@yahoo.fr OI Habets, Florence/0000-0003-1950-0921 FU Meteo-France and Centre National d'Etudes Spatiales (CNES); TOSCA Programme of CNES; Jet Propulsion Laboratory, California Institute of Technology under National Aeronautics and Space Administration (NASA) FX V. Hafliger is funded by Meteo-France and Centre National d'Etudes Spatiales (CNES), as the project is partly funded by the TOSCA Programme of CNES. Cedric H. David is supported by the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration (NASA). The authors thank Florent Lobligeois (IRSTEA), Beatrice Vincendon (CNRM), Noel Watrin, Gerard Rauzy, and Didier Narbais (SPC/Garonne) for their help with accessing the hydrological data. Discharge observations were provided by the French Hydro database (Ministere de l'Ecologie, du Developpement Durable et de l'Energie; http://www.eaufrance.fr), which gathers data from many sources. The authors also thank S. Faroux and S. Donier (CNRM) for their help in installing and using computer tools and three anonymous reviewers for their valuable comments on the manuscript. NR 58 TC 1 Z9 1 U1 2 U2 17 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 1525-755X EI 1525-7541 J9 J HYDROMETEOROL JI J. Hydrometeorol. PD AUG PY 2015 VL 16 IS 4 BP 1821 EP 1842 DI 10.1175/JHM-D-14-0107.1 PG 22 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA CP3FI UT WOS:000359762700023 ER PT J AU Clairmont, RM Bommarius, AS Weber, AL AF Clairmont, Ryan M. Bommarius, Andreas S. Weber, Arthur L. TI Imidazolium Catalysts Formed by an Iterative Synthetic Process as a Model System for Chemical Evolution SO JOURNAL OF MOLECULAR EVOLUTION LA English DT Article DE Imidazolium; Catalysis; Process chemistry; Evolution; Sugars ID FORMALDEHYDE AB Processes exhibiting diversity and selection would have been necessary to promote chemical evolution on early Earth. In this work, a model process was developed using non-kinetic selection to synthesize and isolate small molecule imidazolium catalysts. These catalysts were purified by affinity chromatography and recycled back into the process, forming a product feedback loop. In dimethylformamide, the catalysts activated the coupling of formaldehyde to short chain sugars. This sugar mixture was reacted with aniline, acetic acid, and paraformaldehyde to generate new catalysts. Thus chemical diversity was produced through non-selective, multi-component synthesis. Applying sequential dilution-reaction-purification cycles it was demonstrated that this process can function independently of starting catalyst. Over three process cycles, the initiator catalyst is effectively diluted out as a new catalyst population emerges to take its place. This system offers an alternative viewpoint for chemical evolution via the generation of small molecule organocatalysts. C1 [Clairmont, Ryan M.; Bommarius, Andreas S.] Georgia Inst Technol, Sch Chem & Biomol Engn, Atlanta, GA 30332 USA. [Bommarius, Andreas S.] Georgia Inst Technol, Sch Chem & Biochem, Atlanta, GA 30332 USA. [Weber, Arthur L.] NASA, Ames Res Ctr, SETI Inst, Moffett Field, CA 94035 USA. RP Weber, AL (reprint author), NASA, Ames Res Ctr, SETI Inst, MS 239-4, Moffett Field, CA 94035 USA. EM arthur.l.weber@nasa.gov FU National Science Foundation; National Aeronautics and Space Administration Exobiology Program, under the NSF-Center for Chemical Evolution [CHE-1004570] FX Ryan Clairmont graciously thanks Dr. Ram Krishnamurthy and Dr. Charlie Liotta for helpful discussions, Anthony Thompson Jr and Christine Conwell for their indispensable support, and many colleagues for productive advice: Beth Cope, Chris Butch, Jon Park, "T" Rubin, "Mick" Robbins, Steph Didas, and Justin Vaughn. The work was jointly supported by the National Science Foundation and the National Aeronautics and Space Administration Exobiology Program, under the NSF-Center for Chemical Evolution, CHE-1004570. NR 16 TC 0 Z9 0 U1 5 U2 7 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0022-2844 EI 1432-1432 J9 J MOL EVOL JI J. Mol. Evol. PD AUG PY 2015 VL 81 IS 1-2 BP 1 EP 9 DI 10.1007/s00239-015-9687-7 PG 9 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA CP4AE UT WOS:000359823600001 PM 26194020 ER PT J AU Tompson, SR AF Tompson, Sara R. TI Street Smart: The Rise of Cities and the Fall of Cars SO LIBRARY JOURNAL LA English DT Book Review C1 [Tompson, Sara R.] Jet Prop Lab Lib, Arch & Records Sect, Pasadena, CA USA. RP Tompson, SR (reprint author), Jet Prop Lab Lib, Arch & Records Sect, Pasadena, CA USA. NR 1 TC 0 Z9 0 U1 1 U2 7 PU REED BUSINESS INFORMATION PI NEW YORK PA 360 PARK AVENUE SOUTH, NEW YORK, NY 10010 USA SN 0363-0277 J9 LIBR J JI Libr. J. PD AUG PY 2015 VL 140 IS 13 BP 115 EP 115 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA CO7IS UT WOS:000359333400254 ER PT J AU Pulschen, AA Rodrigues, F Duarte, RTD Araujo, GG Santiago, IF Paulino-Lima, IG Rosa, CA Kato, MJ Pellizari, VH Galante, D AF Pulschen, Andre A. Rodrigues, Fabio Duarte, Rubens T. D. Araujo, Gabriel G. Santiago, Iara F. Paulino-Lima, Ivan G. Rosa, Carlos A. Kato, Massuo J. Pellizari, Vivian H. Galante, Douglas TI UV-resistant yeasts isolated from a high-altitude volcanic area on the Atacama Desert as eukaryotic models for astrobiology SO MICROBIOLOGYOPEN LA English DT Article DE Astrobiology; Atacama Desert; eukaryote; extremophiles; UV radiation; yeast ID X-RAY-FLUORESCENCE; DEINOCOCCUS-RADIODURANS; ESCHERICHIA-COLI; HYPERARID CORE; SACCHAROMYCES-CEREVISIAE; CRYPTOCOCCUS-NEOFORMANS; ULTRAVIOLET-RADIATION; MICROBIAL COMMUNITIES; LOW-PRESSURE; DNA-DAMAGE AB The Sairecabur volcano (5971 m), in the Atacama Desert, is a high-altitude extreme environment with high daily temperature variations, acidic soils, intense UV radiation, and low availability of water. Four different species of yeasts were isolated from this region using oligotrophic media, identified and characterized for their tolerance to extreme conditions. rRNA sequencing revealed high identity (>98%) to Cryptococcus friedmannii, Exophiala sp., Holtermanniella watticus, and Rhodosporidium toruloides. To our knowledge, this is the first report of these yeasts in the Atacama Desert. All isolates showed high resistance to UV-C, UV-B and environmental-UV radiation, capacity to grow at moderate saline media (0.75-2.25 mol/L NaCl) and at moderate to cold temperatures, being C. friedmannii and H. watticus able to grow in temperatures down to -6.5 degrees C. The presence of pigments, analyzed by Raman spectroscopy, correlated with UV resistance in some cases, but there is evidence that, on the natural environment, other molecular mechanisms may be as important as pigmentation, which has implications for the search of spectroscopic biosignatures on planetary surfaces. Due to the extreme tolerances of the isolated yeasts, these organisms represent interesting eukaryotic models for astrobiological purposes. C1 [Pulschen, Andre A.; Rodrigues, Fabio; Kato, Massuo J.] Univ Sao Paulo, Inst Chem, Sao Paulo, Brazil. [Duarte, Rubens T. D.] Univ Fed Santa Catarina, Microbiol Immunol & Parasitol Dept, Florianopolis, SC, Brazil. [Araujo, Gabriel G.; Galante, Douglas] Univ Sao Paulo, Interun Grad Program Biotechnol, Sao Paulo, Brazil. [Araujo, Gabriel G.; Galante, Douglas] Brazilian Synchrotron Light Lab, BR-13083100 Sao Paulo, Brazil. [Santiago, Iara F.; Rosa, Carlos A.] Univ Fed Minas Gerais, Dept Microbiol, Belo Horizonte, MG, Brazil. [Paulino-Lima, Ivan G.] NASA Ames Res Ctr, NASA Postdoctoral Program, Moffett Field, CA USA. [Pellizari, Vivian H.] Univ Sao Paulo, Oceanog Inst, Sao Paulo, Brazil. RP Galante, D (reprint author), Brazilian Synchrotron Light Lab, Ave Giuseppe MaximoScolfaro,10000 Campinas, BR-13083100 Sao Paulo, Brazil. EM douglas.galante@lnls.br RI Institute of Chemistry - USP, Dept. of Chemistry/B-8988-2012; Kato, Massuo/C-1631-2014; Galante, Douglas/G-8752-2011 OI Kato, Massuo/0000-0002-3315-2129; Galante, Douglas/0000-0002-3265-2527 FU FAPESP [2012/18936-0]; CAPES; CNPq - Proantar; USP, through the Brazilian Research Unity in Astrobiology - NAP/Astrobio; NASA Postdoctoral Program FX This work was sponsored by FAPESP (Project 2012/18936-0), CAPES, CNPq - Proantar, USP, through the Brazilian Research Unity in Astrobiology - NAP/Astrobio and the NASA Postdoctoral Program. NR 84 TC 2 Z9 2 U1 6 U2 37 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 2045-8827 J9 MICROBIOLOGYOPEN JI MicrobiologyOpen PD AUG PY 2015 VL 4 IS 4 BP 574 EP 588 DI 10.1002/mbo3.262 PG 15 WC Microbiology SC Microbiology GA CP2UA UT WOS:000359731500004 PM 26147800 ER PT J AU Glancey, MM Anyamba, A Linthicum, KJ AF Glancey, Margaret M. Anyamba, Assaf Linthicum, Kenneth J. TI Epidemiologic and Environmental Risk Factors of Rift Valley Fever in Southern Africa from 2008 to 2011 SO VECTOR-BORNE AND ZOONOTIC DISEASES LA English DT Article DE Environmental factors; Geographic factors; Normalized difference vegetation index data; Rift Valley fever; Southern Africa ID SATELLITE DATA; EAST-AFRICA; OUTBREAK; VIRUS; KENYA; DISEASE; PREDICTION; RAINFALL; PATTERNS; SYSTEMS AB Background: Rift Valley fever (RVF) outbreaks have been associated with periods of widespread and above-normal rainfall over several months. Knowledge on the environmental factors influencing disease transmission dynamics has provided the basis for developing models to predict RVF outbreaks in Africa. From 2008 to 2011, South Africa experienced the worst wave of RVF outbreaks in almost 40 years. We investigated rainfall-associated environmental factors in southern Africa preceding these outbreaks. Methods: RVF epizootic records obtained from the World Animal Health Information Database (WAHID), documenting livestock species affected, location, and time, were analyzed. Environmental variables including rainfall and satellite-derived normalized difference vegetation index (NDVI) data were collected and assessed in outbreak regions to understand the underlying drivers of the outbreaks. Results: The predominant domestic vertebrate species affected in 2008 and 2009 were cattle, when outbreaks were concentrated in the eastern provinces of South Africa. In 2010 and 2011, outbreaks occurred in the interior and southern provinces affecting over 16,000 sheep. The highest number of cases occurred between January and April but epidemics occurred in different regions every year, moving from the northeast of South Africa toward the southwest with each progressing year. The outbreaks showed a pattern of increased rainfall preceding epizootics ranging from 9 to 152 days; however, NDVI and rainfall were less correlated with the start of the outbreaks than has been observed in eastern Africa. Conclusions: Analyses of the multiyear RVF outbreaks of 2008 to 2011 in South Africa indicated that rainfall, NDVI, and other environmental and geographical factors, such as land use, drainage, and topography, play a role in disease emergence. Current and future investigations into these factors will be able to contribute to improving spatial accuracy of models to map risk areas, allowing adequate time for preparation and prevention before an outbreak occurs. C1 [Glancey, Margaret M.] Johns Hopkins Bloomberg Sch Publ Hlth, Baltimore, MD USA. [Anyamba, Assaf] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Linthicum, Kenneth J.] USDA, Ctr Med Agr & Vet Entomol, Gainesville, FL USA. RP Anyamba, A (reprint author), NASA, Goddard Space Flight Ctr, Biospher Sci Lab, Code 618, Greenbelt, MD 20771 USA. EM assaf.anyamba@nasa.gov FU Universities Space Research Association's (USRA) Goddard Earth Sciences Technology and Research (GESTAR) 2013 Summer Internship Fellowship at NASA Goddard Space Flight Center; Department of Defense-Armed Forces Health Surveillance Center, Division of Global Emerging Infections Surveillance and Response System (GEIS) Operations FX Margaret Glancey was funded by Universities Space Research Association's (USRA) Goddard Earth Sciences Technology and Research (GESTAR) 2013 Summer Internship Fellowship at NASA Goddard Space Flight Center. The Rift Valley fever Monitoring and Risk Mapping project is funded by the Department of Defense-Armed Forces Health Surveillance Center, Division of Global Emerging Infections Surveillance and Response System (GEIS) Operations. We wish to acknowledge Jennifer Small for extracting the NDVI and Rainfall data used in this study. NR 46 TC 3 Z9 3 U1 2 U2 7 PU MARY ANN LIEBERT, INC PI NEW ROCHELLE PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA SN 1530-3667 EI 1557-7759 J9 VECTOR-BORNE ZOONOT JI Vector-Borne Zoonotic Dis. PD AUG 1 PY 2015 VL 15 IS 8 BP 502 EP 511 DI 10.1089/vbz.2015.1774 PG 10 WC Public, Environmental & Occupational Health; Infectious Diseases SC Public, Environmental & Occupational Health; Infectious Diseases GA CP0YZ UT WOS:000359604300007 PM 26273812 ER PT J AU Fey, AL Gordon, D Jacobs, CS Ma, C Gaume, RA Arias, EF Bianco, G Boboltz, DA Bockmann, S Bolotin, S Charlot, P Collioud, A Engelhardt, G Gipson, J Gontier, AM Heinkelmann, R Kurdubov, S Lambert, S Lytvyn, S MacMillan, DS Malkin, Z Nothnagel, A Ojha, R Skurikhina, E Sokolova, J Souchay, J Sovers, OJ Tesmer, V Titov, O Wang, G Zharov, V AF Fey, A. L. Gordon, D. Jacobs, C. S. Ma, C. Gaume, R. A. Arias, E. F. Bianco, G. Boboltz, D. A. Boeckmann, S. Bolotin, S. Charlot, P. Collioud, A. Engelhardt, G. Gipson, J. Gontier, A. -M. Heinkelmann, R. Kurdubov, S. Lambert, S. Lytvyn, S. MacMillan, D. S. Malkin, Z. Nothnagel, A. Ojha, R. Skurikhina, E. Sokolova, J. Souchay, J. Sovers, O. J. Tesmer, V. Titov, O. Wang, G. Zharov, V. TI THE SECOND REALIZATION OF THE INTERNATIONAL CELESTIAL REFERENCE FRAME BY VERY LONG BASELINE INTERFEROMETRY SO ASTRONOMICAL JOURNAL LA English DT Article DE astrometry; catalogs; quasars: general; radio continuum: galaxies; reference systems; techniques: interferometric ID VLBA CALIBRATOR SURVEY; RADIO REFERENCE FRAME; HEMISPHERE ICRF SOURCES; ASTROMETRIC SUITABILITY; SOURCE POSITIONS; TERRESTRIAL AB We present the second realization of the International Celestial Reference Frame (ICRF2) at radio wavelengths using nearly 30 years of Very Long Baseline Interferometry observations. ICRF2 contains precise positions of 3414 compact radio astronomical objects and has a positional noise floor of similar to 40 mu as and a directional stability of the frame axes of similar to 10 mu as. A set of 295 new "defining" sources was selected on the basis of positional stability and the lack of extensive intrinsic source structure. The positional stability of these 295 defining sources and their more uniform sky distribution eliminates the two greatest weaknesses of the first realization of the International Celestial Reference Frame (ICRF1). Alignment of ICRF2 with the International Celestial Reference System was made using 138 positionally stable sources common to both ICRF2 and ICRF1. The resulting ICRF2 was adopted by the International Astronomical Union as the new fundamental celestial reference frame, replacing ICRF1 as of 2010 January 1. C1 [Fey, A. L.; Gaume, R. A.; Boboltz, D. A.] US Naval Observ, Washington, DC 20392 USA. [Gordon, D.; Ma, C.; Bolotin, S.; Gipson, J.; MacMillan, D. S.] Goddard Space Flight Ctr, Natl Aeronaut & Space Adm, Greenbelt, MD 20771 USA. [Jacobs, C. S.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Arias, E. F.] Bur Int Poids & Mesures, F-92312 Sevres, France. [Bianco, G.] CGS, Agenzia Spaziale Italiana, I-75100 Matera, Italy. [Boeckmann, S.] Univ Bonn, Inst Geodasie & Geoinformat, D-53115 Bonn, Germany. [Charlot, P.; Collioud, A.] Univ Bordeaux, LAB, UMR 5804, F-33270 Floirac, France. [Charlot, P.; Collioud, A.] CNRS, LAB, UMR 5804, F-33270 Floirac, France. [Engelhardt, G.; Souchay, J.] BKG, D-60598 Frankfurt, Germany. [Gontier, A. -M.; Lambert, S.] CNRS, SYRTE, UMPC, Observ Paris,GRGS, F-75014 Paris, France. [Heinkelmann, R.] German Res Ctr Geosci GFZ, Helmholtz Ctr Potsdam, D-14473 Potsdam, Germany. [Kurdubov, S.; Skurikhina, E.] Russian Acad Sci, Inst Appl Astron, St Petersburg 191187, VA, Russia. [Lytvyn, S.] Natl Acad Sci Ukraine, Main Astron Observ, UA-03680 Kiev, Ukraine. [Malkin, Z.] Pulkovo Observ, St Petersburg 196140, Russia. [Malkin, Z.] St Petersburg State Univ, St Petersburg 198504, VA, Russia. [Ojha, R.] NASA, Goddard Space Flight Ctr, Astroparticle Phys Lab, Greenbelt, MD 20771 USA. [Sokolova, J.] Pulkovo Observ, St Petersburg 196140, Russia. [Sovers, O. J.] Remote Sensing Anal Syst, Altadena, CA 91001 USA. [Tesmer, V.] OHB Syst AG, D-28359 Bremen, Germany. [Titov, O.] Geosci Australia, Canberra, ACT 2601, Australia. [Wang, G.] Chinese Acad Sci, Shanghai Astron Observ, Shanghai 200030, Peoples R China. [Zharov, V.] Moscow MV Lomonosov State Univ, Sternberg Astron Inst, Moscow 119991, Russia. RP Fey, AL (reprint author), US Naval Observ, 3450 Massachusetts Ave NW, Washington, DC 20392 USA. RI Lambert, Sebastien/H-9647-2016; Malkin, Zinovy/C-1560-2008; OI Lambert, Sebastien/0000-0001-6759-5502; Malkin, Zinovy/0000-0002-5583-8391; Bianco, Giuseppe/0000-0002-4538-6467 NR 34 TC 28 Z9 28 U1 5 U2 16 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD AUG PY 2015 VL 150 IS 2 AR 58 DI 10.1088/0004-6256/150/2/58 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO0QL UT WOS:000358856900019 ER PT J AU Jenkins, JM Twicken, JD Batalha, NM Caldwell, DA Cochran, WD Endl, M Latham, DW Esquerdo, GA Seader, S Bieryla, A Petigura, E Ciardi, DR Marcy, GW Isaacson, H Huber, D Rowe, JF Torres, G Bryson, ST Buchhave, L Ramirez, I Wolfgang, A Li, J Campbell, JR Tenenbaum, P Sanderfer, D Henze, CE Catanzarite, JH Gilliland, RL Borucki, WJ AF Jenkins, Jon M. Twicken, Joseph D. Batalha, Natalie M. Caldwell, Douglas A. Cochran, William D. Endl, Michael Latham, David W. Esquerdo, Gilbert A. Seader, Shawn Bieryla, Allyson Petigura, Erik Ciardi, David R. Marcy, Geoffrey W. Isaacson, Howard Huber, Daniel Rowe, Jason F. Torres, Guillermo Bryson, Stephen T. Buchhave, Lars Ramirez, Ivan Wolfgang, Angie Li, Jie Campbell, Jennifer R. Tenenbaum, Peter Sanderfer, Dwight Henze, Christopher E. Catanzarite, Joseph H. Gilliland, Ronald L. Borucki, William J. TI DISCOVERY AND VALIDATION OF Kepler-452b: A 1.6 R phi SUPER EARTH EXOPLANET IN THE HABITABLE ZONE OF A G2 STAR SO ASTRONOMICAL JOURNAL LA English DT Article DE methods: statistical; planets and satellites: detection; stars: fundamental parameters; stars: individual (Kepler-452b, KIC 8311864, KOI7016.01) ID POTENTIAL TRANSIT SIGNALS; FALSE POSITIVES; MISSION DATA; SOPHIE VELOCIMETRY; EXTRASOLAR PLANETS; BLEND SCENARIOS; Y-2 ISOCHRONES; HARPS SEARCH; MILKY-WAY; SYSTEM AB We report on the discovery and validation of Kepler-452b, a transiting planet identified by a search through the 4 years of data collected by NASA's Kepler Mission. This possibly rocky 1.63(-0.20)(+0.23) R-circle plus every 384.843 (+0.007)(-0.012) days, the longest orbital period for a small (R-P < 2 R-circle plus) transiting exoplanet to date. The likelihood that this planet has a rocky composition lies between 49% and 62%. The star has an effective temperature of 5757 +/- 85 K and a log g of 4.32 +/- 0.09. At a mean orbital separation of 1.046 (-0.015) (+0.019) AU, this small planet is well within the optimistic habitable zone of its star (recent Venus/early Mars), experiencing only 10% more flux than Earth receives from the Sun today, and slightly outside the conservative habitable zone (runaway greenhouse/maximum greenhouse). The star is slightly larger and older than the Sun, with a present radius of 1.11 (-0.09) (+0.15) R-circle dot and an estimated age of similar to 6 Gyr. Thus, Kepler-452b has likely always been in the habitable zone and should remain there for another similar to 3 Gyr. C1 [Jenkins, Jon M.; Twicken, Joseph D.; Batalha, Natalie M.; Caldwell, Douglas A.; Seader, Shawn; Rowe, Jason F.; Bryson, Stephen T.; Li, Jie; Tenenbaum, Peter; Sanderfer, Dwight; Henze, Christopher E.; Catanzarite, Joseph H.; Borucki, William J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Twicken, Joseph D.; Caldwell, Douglas A.; Seader, Shawn; Huber, Daniel; Rowe, Jason F.; Li, Jie; Tenenbaum, Peter; Catanzarite, Joseph H.] SETI Inst, Mountain View, CA 94043 USA. [Cochran, William D.; Endl, Michael; Ramirez, Ivan] Univ Texas Austin, McDonald Observ, Austin, TX 78712 USA. [Cochran, William D.; Endl, Michael; Ramirez, Ivan] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Latham, David W.; Esquerdo, Gilbert A.; Bieryla, Allyson; Torres, Guillermo; Buchhave, Lars] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Petigura, Erik; Marcy, Geoffrey W.; Isaacson, Howard] Univ Calif Berkeley, Berkeley, CA 94720 USA. [Ciardi, David R.] CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA. [Huber, Daniel] Univ Sydney, Sch Phys, Sydney Inst Astron SIfA, Sydney, NSW 2006, Australia. [Huber, Daniel] Aarhus Univ, Dept Phys & Astron, Stellar Astrophys Ctr, DK-8000 Aarhus C, Denmark. [Buchhave, Lars] Univ Copenhagen, Nat Hist Museum Denmark, Ctr Star & Planet Format, DK-1350 Copenhagen, Denmark. [Wolfgang, Angie] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Campbell, Jennifer R.] NASA, Wyle Labs, Ames Res Ctr, Moffett Field, CA 94035 USA. [Gilliland, Ronald L.] Penn State Univ, Ctr Exoplanets & Habitable Worlds, University Pk, PA 16802 USA. RP Jenkins, JM (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM Jon.Jenkins@nasa.gov NR 89 TC 32 Z9 36 U1 18 U2 61 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD AUG PY 2015 VL 150 IS 2 AR 56 DI 10.1088/0004-6256/150/2/56 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO0QL UT WOS:000358856900017 ER PT J AU Naidu, SP Margot, JL Taylor, PA Nolan, MC Busch, MW Benner, LAM Brozovic, M Giorgini, JD Jao, JS Magri, C AF Naidu, S. P. Margot, J. L. Taylor, P. A. Nolan, M. C. Busch, M. W. Benner, L. A. M. Brozovic, M. Giorgini, J. D. Jao, J. S. Magri, C. TI RADAR IMAGING AND CHARACTERIZATION OF THE BINARY NEAR-EARTH ASTEROID (185851) 2000 DP107 SO ASTRONOMICAL JOURNAL LA English DT Article DE minor planets, asteroids: individual (2000 DP107); techniques: radar astronomy ID 1999 KW4; POPULATION; DYNAMICS; MODEL; SPINS AB The potentially hazardous asteroid (185851) 2000 DP107 was the first binary near-Earth asteroid to be imaged. Radar observations in 2000 provided images at 75m resolution that revealed the shape, orbit, and spin-up formation mechanism of the binary. The asteroid made a more favorable flyby of the Earth in 2008, yielding images at 30 m resolution. We used these data to obtain shape models for the two components and to improve the estimates of the mutual orbit, component masses, and spin periods. The primary has a sidereal spin period of 2.7745 +/- 0.0007 hr and is roughly spheroidal with an equivalent diameter of 863 m +/- 5%. It has a mass of 4.656 +/- 0.43 x 10(11) kg and a density of 1381 +/- 244 kgm(-3). It exhibits an equatorial ridge similar to the (66391) 1999 KW4 primary; however, the equatorial ridge in this case is not as regular and has a similar to 300 m diameter concavity on one side. The secondary has a sidereal spin period of 1.77 +/- 0.02 days commensurate with the orbital period. The secondary is slightly elongated and has overall dimensions of 377 x 314 x 268 m (6% uncertainties). Its mass is 0.178 +/- 0.021 x 10(11) kg and its density is 1047 +/- 230 kg m(-3). The mutual orbit has a semimajor axis of 2.659 +/- 0.08 km, an eccentricity of 0.019 +/- 0.01, and a period of 1.7556 +/- 0.0015 days. The normalized total angular momentum of this system exceeds the amount required for the expected spin-up formation mechanism. An increase of angular momentum from nongravitational forces after binary formation is a possible explanation. The two components have similar radar reflectivity, suggesting a similar composition consistent with formation by spin-up. The secondary appears to exhibit a larger circular polarization ratio than the primary, suggesting a rougher surface or subsurface at radar wavelength scales. C1 [Naidu, S. P.; Margot, J. L.] Univ Calif Los Angeles, Dept Earth Planetary & Space Sci, Los Angeles, CA 90095 USA. [Margot, J. L.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Taylor, P. A.; Nolan, M. C.] Arecibo Observ, Arecibo, PR 00612 USA. [Busch, M. W.] SETI Inst, Mountain View, CA 94043 USA. [Benner, L. A. M.; Brozovic, M.; Giorgini, J. D.; Jao, J. S.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Magri, C.] Univ Maine, Farmington, ME 04938 USA. RP Naidu, SP (reprint author), Univ Calif Los Angeles, Dept Earth Planetary & Space Sci, 595 Charles Young Dr East, Los Angeles, CA 90095 USA. RI Margot, Jean-Luc/A-6154-2012; OI Margot, Jean-Luc/0000-0001-9798-1797; Nolan, Michael/0000-0001-8316-0680; Naidu, Shantanu/0000-0003-4439-7014 FU National Science Foundation [AST-1211581]; National Aeronautics and Space Administration [NNX14AM95G] FX We thank Dan Scheeres and Seth Jacobson for useful discussions, and the anonymous reviewer for excellent suggestions. This material is based on work supported by the National Science Foundation under grant No. AST-1211581 and the National Aeronautics and Space Administration under grant No. NNX14AM95G. NR 33 TC 3 Z9 3 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD AUG PY 2015 VL 150 IS 2 AR 54 DI 10.1088/0004-6256/150/2/54 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO0QL UT WOS:000358856900015 ER PT J AU Vilas, F Hendrix, AR AF Vilas, Faith Hendrix, Amanda R. TI THE UV/BLUE EFFECTS OF SPACE WEATHERING MANIFESTED IN S-COMPLEX ASTEROIDS. I. QUANTIFYING CHANGE WITH ASTEROID AGE SO ASTRONOMICAL JOURNAL LA English DT Article DE minor planets, asteroids: general; planets and satellites: surfaces; ultraviolet: planetary systems ID REFLECTANCE SPECTRA; OPTICAL-PROPERTIES; FINEST FRACTION; BELT ASTEROIDS; 1998 SF36; SURFACES; LUNAR; ORIGIN AB Evidence for the manifestation of space weathering in S-complex asteroids as a bluing of the UV/blue reflectance spectrum is extended using high resolution CCD reflectance spectra of 21 main-belt, 1 Mars-crossing, and 3 near-Earth asteroids covering a wavelength range of 320-620 nm. Demonstration of the transition of iron-bearing materials from volume scattering to surface (Fresnel) scattering is apparent as an abrupt downturn at wavelengths just short of 400 nm in reflectance spectra of fresh asteroid surfaces. The weathering away of this downturn is demonstrated by its absence in reflectance spectra of mature S-complex asteroids, consistent with an increase in npFe(0) on the material's surface. Modeling of the effects of the addition of small amounts of npFe0 to particles from both a hypothetical mineral and a terrestrial basalt shows that evidence of the addition of 0.0001% npFe(0) affects the reflectance at UV/blue wavelengths, while the addition of 0.01% is required to see the visible/near-infrared reddening and diminution of absorption features. Thus, the UV/blue reflectance characteristics allow earlier detection of the onset of space weathering effects. Combining UV/blue spectral characteristics of asteroids and ordinary chondrite meteorites with estimated ages of the young Datura family, we establish a method of dating asteroid surface ages during the early stages of space weathering. We demonstrate by dating the surface of NEA 163249 2002 GT to be 109 (+/- 18) to 128 (+/- 10) Kyr. C1 [Vilas, Faith] MMT Observ, Tucson, AZ 85721 USA. [Vilas, Faith; Hendrix, Amanda R.] Planetary Sci Inst, Tucson, AZ 85719 USA. [Hendrix, Amanda R.] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Vilas, F (reprint author), MMT Observ, Tucson, AZ 85721 USA. EM fvilas@psi.edu NR 27 TC 1 Z9 1 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD AUG PY 2015 VL 150 IS 2 AR 64 DI 10.1088/0004-6256/150/2/64 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO0QL UT WOS:000358856900025 ER PT J AU Gerakines, PA Hudson, RL AF Gerakines, Perry A. Hudson, Reggie L. TI FIRST INFRARED BAND STRENGTHS FOR AMORPHOUS CO2, AN OVERLOOKED COMPONENT OF INTERSTELLAR ICES SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE astrochemistry; infrared: ISM; ISM: abundances; ISM: molecules; molecular data; planets and satellites: surfaces ID SOLID CARBON-DIOXIDE; OPTICAL-CONSTANTS; THIN-FILMS; SPECTRA; ANALOGS; IONS; IMPLANTATION; SPECTROSCOPY; MIXTURES; STARS AB Solid carbon dioxide (CO2) has long been recognized as a component of both interstellar and solar system ices, but a recent literature search has revealed significant qualitative and quantitative discrepancies in the laboratory spectra on which the abundances of extraterrestrial CO2 are based. Here we report new infrared (IR) spectra of amorphous CO2-ice along with band intensities (band strengths) of four mid-IR absorptions, the first such results in the literature. A possible thickness dependence for amorphous-CO2 IR band shapes and positions also is investigated, and the three discordant reports of amorphous CO2 spectra in the literature are addressed. Applications of our results are discussed with an emphasis on laboratory investigations and results from astronomical observations. A careful comparison with earlier work shows that the IR spectra calculated from several databases for CO2 ices, all ices being made near 10 K, are not for amorphous CO2, but rather for crystalline CO2 or crystalline-amorphous mixtures. C1 [Gerakines, Perry A.; Hudson, Reggie L.] NASA Goddard Space Flight Ctr, Astrochem Lab, Greenbelt, MD 20771 USA. RP Gerakines, PA (reprint author), NASA Goddard Space Flight Ctr, Astrochem Lab, Greenbelt, MD 20771 USA. EM Reggie.Hudson@NASA.gov RI Gerakines, Perry/D-2226-2012 OI Gerakines, Perry/0000-0002-9667-5904 FU NASA; NASA Astrobiology Institute through the Goddard Center for Astrobiology FX NASA funding through the Astrophysics Research and Analysis, Cassini Data Analysis, and Outer Planets Research programs is acknowledged. Both authors received partial support from the NASA Astrobiology Institute through the Goddard Center for Astrobiology. Mark Loeffler is particularly acknowledged for constructing the ultra-high vacuum system with which he and Marla Moore measured n and rho. Robert Ferrante and Tatiana Tway are thanked for assistance with IR measurements. NR 40 TC 4 Z9 4 U1 2 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 AUG 1 PY 2015 VL 808 IS 2 AR L40 DI 10.1088/2041-8205/808/2/L40 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO1TS UT WOS:000358938800008 ER PT J AU Wang, LH Follette-Cook, MB Newchurch, MJ Pickering, KE Pour-Biazar, A Kuang, S Koshak, W Peterson, H AF Wang, Lihua Follette-Cook, Melanie B. Newchurch, M. J. Pickering, Kenneth E. Pour-Biazar, Arastoo Kuang, Shi Koshak, William Peterson, Harold TI Evaluation of lightning-induced tropospheric ozone enhancements observed by ozone lidar and simulated by WRF/Chem SO ATMOSPHERIC ENVIRONMENT LA English DT Article DE DIAL; Lidar; LNOx; WRF/Chem; NLDN; Tropospheric ozone ID CONTINENTAL UNITED-STATES; CMAQ MODEL; NOX PRODUCTION; EMISSIONS; TRANSPORT; THUNDERSTORMS; CHEMISTRY; NITROGEN AB High spatial- and temporal-resolution ozone lidar profiles, in conjunction with ozonesonde and satellite observations, are well suited to characterize short-term ozone variations due to different physical and chemical processes, such as the impact of lightning-generated NOx (LNOx) on tropospheric ozone. This work presents the hourly variation of tropospheric-ozone profiles measured by an ozone lidar at the University of Alabama in Huntsville, on July 14, 18, and 27, 2011. These ozone lidar data are compared with two WRF/Chem simulations, one with lightning NO (LNO) emissions and the other without. On July 14, 2011, the ozone lidar observed an ozone laminar structure with elevated ozone concentrations of 65 similar to 80 ppbv below 2 km, low ozone (50 similar to 65) ppbv between 2 and 5 km, and high ozone up to 165 ppbv between 5 and 12 km AGL. WRF/Chem simulations, in conjunction with backward trajectory analysis, suggest that lightning events occurring within upwind regions resulted in an ozone enhancement of 28 ppbv at 7.5 km AGL over Huntsville. On July 27, LNO emissions were transported to Huntsville from upwind and account for 75% of NOx and an 8.3 ppbv of ozone enhancement at similar to 10 km; the model overestimates ozone between 2.5 and 5 km AGL. (C) 2015 Elsevier Ltd. All rights reserved. C1 [Wang, Lihua; Newchurch, M. J.; Pour-Biazar, Arastoo; Kuang, Shi] Univ Alabama, Huntsville, AL 35899 USA. [Follette-Cook, Melanie B.] Morgan State Univ, Baltimore, MD 21239 USA. [Pickering, Kenneth E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Koshak, William] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. [Peterson, Harold] NASA, George C Marshall Space Flight Ctr, Univ Space Res Assoc, Huntsville, AL 35812 USA. RP Wang, LH (reprint author), Univ Alabama, Huntsville, AL 35899 USA. EM lihuawang@nsstc.uah.edu RI Pickering, Kenneth/E-6274-2012; OI Kuang, Shi/0000-0003-2423-6088 FU NASA Earth Science Division FX This work was supported by NASA Earth Science Division. The NASA Lightning Image Sensor (LIS) instrument team and the LIS data center via the Global Hydrology Resource Center (GHRC) located at the Global Hydrology and Climate Center (GHCC), Huntsville, Alabama provided NLDN data through a license agreement with Vaisala, Inc. The data available from the GHRC are restricted to LIS science team collaborators and to NASA EOS and TRMM investigators. NR 40 TC 3 Z9 4 U1 2 U2 26 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 AUG PY 2015 VL 115 BP 185 EP 191 DI 10.1016/j.atmosenv.2015.05.054 PG 7 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA CN9ZL UT WOS:000358809600021 ER PT J AU Jeyapaul, E Coleman, GN Rumsey, CL AF Jeyapaul, Elbert Coleman, Gary N. Rumsey, Christopher L. TI Higher-order and length-scale statistics from DNS of a decelerated planar wall-bounded turbulent flow SO INTERNATIONAL JOURNAL OF HEAT AND FLUID FLOW LA English DT Article DE Higher-order moments; RANS closures; DNS; APG boundary layers ID ADVERSE-PRESSURE-GRADIENT; DIRECT NUMERICAL-SIMULATION; CHANNEL FLOW; LAYER; VELOCITY; FLUCTUATIONS; MOMENTS AB A DNS database is presented to document third- and fourth-order moments and their budgets for fully developed plane-channel flow and for strained plane-channel flow. The effect of straining has a similar effect on statistics, such as the skewness and flatness of velocities, as in an adverse-pressure-gradient (APG) boundary layer. In addition to higher-order statistics, some modeling implications are also described, including issues related to decomposition of the velocity-pressure gradient correlations, the assumption of dissipation isotropy and a fourth-order turbulence time scale. An analysis of two-point correlations along the inhomogeneous direction is made to include the effects of APG straining. This reveals the advantage of a one-point length-scale based on wall-normal velocity fluctuations as an alternative to the traditionally used length-scale based on turbulence kinetic energy. The present study should prove to be useful for turbulence modelers in need of data to develop and assess higher-than-second-order Reynolds-averaged Navier-Stokes closure models. Published by Elsevier Inc. C1 [Jeyapaul, Elbert] Natl Inst Aerosp, Hampton, VA 23666 USA. [Coleman, Gary N.; Rumsey, Christopher L.] NASA, Langley Res Ctr, Computat AeroSci Branch, Hampton, VA 23681 USA. RP Rumsey, CL (reprint author), NASA, Langley Res Ctr, Computat AeroSci Branch, MS 128, Hampton, VA 23681 USA. EM c.l.rumsey@nasa.gov FU NASA at Langley Research Center [NNL09AA00A]; Aeronautical Sciences Project of NASA's Fundamental Aeronautics Program FX The research was supported by NASA Cooperative agreement NNL09AA00A at Langley Research Center awarded to the National Institute of Aerospace. Computational resources were provided by NASA Advanced Supercomputing division. The work of the second and third authors is supported by the Aeronautical Sciences Project of NASA's Fundamental Aeronautics Program. NR 26 TC 2 Z9 2 U1 0 U2 6 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0142-727X EI 1879-2278 J9 INT J HEAT FLUID FL JI Int. J. Heat Fluid Flow PD AUG PY 2015 VL 54 BP 14 EP 27 DI 10.1016/j.ijheatfluidflow.2015.04.002 PG 14 WC Thermodynamics; Engineering, Mechanical; Mechanics SC Thermodynamics; Engineering; Mechanics GA CO0CM UT WOS:000358817700002 ER PT J AU Weerts, AP Putcha, L Hoag, SW Hallgren, E Van Ombergen, A Van de Heyning, PH Wuyts, FL AF Weerts, Aurelie P. Putcha, Lakshmi Hoag, Stephen W. Hallgren, Emma Van Ombergen, Angelique Van de Heyning, Paul H. Wuyts, Floris L. TI Intranasal scopolamine affects the semicircular canals centrally and peripherally SO JOURNAL OF APPLIED PHYSIOLOGY LA English DT Article DE utricles; saccules; acetylcholine antagonist; semicircular canals; motion sickness; space motion sickness ID EVOKED MYOGENIC POTENTIALS; SPACE MOTION SICKNESS; BONE-CONDUCTED VIBRATION; UTRICULAR FUNCTION; MECHANISMS; RECEPTORS; CAT; PHARMACOKINETICS; DIMENHYDRINATE; CEREBELLUM AB Space motion sickness (SMS), a condition caused by an intravestibular conflict, remains an important obstacle that astronauts encounter during the first days in space. Promethazine is currently the standard treatment of SMS, but scopolamine is used by some astronauts to prevent SMS. However, the oral and transdermal routes of administration of scopolamine are known to have substantial drawbacks. Intranasal administration of scopolamine ensures a fast absorption and rapid onset of therapeutic effect, which might prove to be suitable for use during spaceflights. The aim of this study was to evaluate the effects of intranasally administered scopolamine (0.4 mg) on the semicircular canals (SCCs) and the otoliths. This double-blind, placebo-controlled study was performed on 19 healthy male subjects. The function of the horizontal SCC and the vestibulo-ocular reflex, as well as the saccular function and utricular function, were evaluated. Scopolamine turned out to affect mainly the SCCs centrally and peripherally but also the utricles to a lesser extent. Centrally, the most probable site of action is the medial vestibular nucleus, where the highest density of muscarinic receptors has been demonstrated and afferent fibers from the SCCs and utricles synapse. Furthermore, our results suggest the presence of muscarinic receptors in the peripheral vestibular system on which scopolamine has a suppressive effect. Given the depressant actions on the SCCs, it is suggested that the pharmacodynamic effect of scopolamine may be attributed to the obliteration of intravestibular conflict that arises during (S)MS. C1 [Weerts, Aurelie P.; Hallgren, Emma; Van Ombergen, Angelique; Wuyts, Floris L.] Univ Antwerp, Univ Antwerp Hosp, Res Ctr Equilibrium & Aerosp, B-2020 Antwerp, Belgium. [Weerts, Aurelie P.; Hallgren, Emma; Van Ombergen, Angelique; Wuyts, Floris L.] Univ Antwerp, B-2020 Antwerp, Belgium. [Putcha, Lakshmi] NASA, Biomed Operat & Res Branch, Johnson Space Ctr, Houston, TX USA. [Hoag, Stephen W.] Univ Maryland, Dept Pharmaceut Sci, Sch Pharm, Baltimore, MD 21201 USA. RP Wuyts, FL (reprint author), Univ Antwerp, Univ Antwerp Hosp, Res Ctr Equilibrium & Aerosp AUREA, Groenenborgerlaan 171, B-2020 Antwerp, Belgium. EM floris.wuyts@uantwerpen.be FU European Space Agency [AO-2004-093]; Research Foundation Flanders (FWO Vlaanderen) [11N6414N] FX This research was made possible by the Belgian Science Policy program PRODEX-9 project SPIN-D in support of the European Space Agency AO-2004-093 corresponding project. This study was supported by Research Foundation Flanders (FWO Vlaanderen) Grant 11N6414N (to A. Van Ombergen). NR 37 TC 3 Z9 3 U1 1 U2 9 PU AMER PHYSIOLOGICAL SOC PI BETHESDA PA 9650 ROCKVILLE PIKE, BETHESDA, MD 20814 USA SN 8750-7587 EI 1522-1601 J9 J APPL PHYSIOL JI J. Appl. Physiol. PD AUG 1 PY 2015 VL 119 IS 3 BP 213 EP 218 DI 10.1152/japplphysiol.00149.2015 PG 6 WC Physiology; Sport Sciences SC Physiology; Sport Sciences GA CO1RL UT WOS:000358932800005 PM 25953832 ER PT J AU Yu, S Pearson, JC Drouin, BJ Crawford, T Daly, AM Elliott, B Amano, T AF Yu, S. Pearson, J. C. Drouin, B. J. Crawford, T. Daly, A. M. Elliott, B. Amano, T. TI Rotational spectroscopy of vibrationally excited N2H+ and N2D+ up to 2.7 THz SO JOURNAL OF MOLECULAR SPECTROSCOPY LA English DT Article DE N2H+ and N2D+; N-15-containing N2H+ and N2D+; Excited vibrational state; THz spectroscopy ID NEGATIVE GLOW-DISCHARGE; HYPERFINE-STRUCTURE; HN2+; ION; SPECTRA; REGION; DN2+ AB Terahertz absorption spectroscopy was employed to extend the measurements on the pure rotational transitions of N2H+, N2D+ and their N-15-containing isotopologues in the ground state and first excited vibrational states for the three fundamental vibrational modes. In total, 91 new pure rotational transitions were observed in the range of 0.7-2.7 THz. The observed transition frequencies were fit to experimental accuracy, and the improved molecular parameters were obtained. The new measurements and predictions reported here will support the analysis of high-resolution astronomical observations made with facilities such as SOFIA and ALMA where laboratory rest frequencies with uncertainties of 1 MHz or smaller are required for proper analysis of velocity resolved astrophysical components. (C) 2015 Elsevier Inc. All rights reserved. C1 [Yu, S.; Pearson, J. C.; Drouin, B. J.; Crawford, T.; Daly, A. M.; Elliott, B.; Amano, T.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Yu, S (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM shanshan.yu@jpl.nasa.gov RI Yu, Shanshan/D-8733-2016 FU NASA FX We would like to thank Professor Cristina Puzzarini for providing us with the SPFIT files fitting the N2H+ ground state hfs-resolved data published in Ref. [3]. We used these data to derive hfs free frequencies to be included in the current fit. The research described in this paper was performed at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. Funding from the NASA Herschel project is acknowledged. Copyright 2015 California Institute of Technology. NR 21 TC 1 Z9 1 U1 2 U2 9 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0022-2852 EI 1096-083X J9 J MOL SPECTROSC JI J. Mol. Spectrosc. PD AUG PY 2015 VL 314 BP 19 EP 25 DI 10.1016/j.jms.2015.05.001 PG 7 WC Physics, Atomic, Molecular & Chemical; Spectroscopy SC Physics; Spectroscopy GA CO3YC UT WOS:000359096200004 ER PT J AU Messenger, S Nakamura-Messenger, K Keller, LP Clemett, SJ AF Messenger, Scott Nakamura-Messenger, Keiko Keller, Lindsay P. Clemett, Simon J. TI Pristine stratospheric collection of interplanetary dust on an oil-free polyurethane foam substrate SO METEORITICS & PLANETARY SCIENCE LA English DT Article ID MOLECULAR-CLOUD MATERIAL; ORGANIC-MATTER; AQUEOUS ALTERATION; GEMS GRAINS; PARTICLES; METEORITES; COMETS; CARBON; MICROMETEORITES; IDENTIFICATION AB We performed chemical, mineralogical, and isotopic studies of the first interplanetary dust particles (IDPs) collected in the stratosphere without the use of silicone oil. The collection substrate, polyurethane foam, effectively traps impacting particles, but the lack of an embedding medium results in significant particle fragmentation. Two dust particles found on the collector exhibit the typical compositional and mineralogical properties of chondritic porous interplanetary dust particles (CP-IDPs). Hydrogen and nitrogen isotopic imaging revealed isotopic anomalies of typical magnitude and spatial variability observed in previous CP-IDP studies. Oxygen isotopic imaging shows that individual mineral grains and glass with embedded metal and sulfide (GEMS) grains are dominated by solar system materials. No systematic differences are observed in element abundance patterns of GEMS grains from the dry collection versus silicone oil-collected IDPs. This initial study establishes the validity of a new IDP collection substrate that avoids the use of silicone oil as a collection medium, removing the need for this problematic contaminant and the organic solvents necessary to remove it. Additional silicone oil-free collections of this type are needed to determine more accurate bulk element abundances of IDPs and to examine the indigenous soluble organic components of IDPs. C1 [Messenger, Scott; Nakamura-Messenger, Keiko; Keller, Lindsay P.; Clemett, Simon J.] NASA Johnson Space Ctr, Robert M Walker Lab Space Sci, EIS Directorate, Astromat Res & Explorat Sci Div, Houston, TX 77058 USA. [Clemett, Simon J.] ESCG ERC Inc, Houston, TX 77058 USA. RP Messenger, S (reprint author), NASA Johnson Space Ctr, Robert M Walker Lab Space Sci, EIS Directorate, Astromat Res & Explorat Sci Div, Houston, TX 77058 USA. EM scott.r.messenger@nasa.gov FU NASA Cosmochemistry program FX We gratefully acknowledge the willingness of the cosmic dust curator to fly experimental collector materials and especially the hands-on assistance of Jack Warren and Ron Bastien. This work was supported by grants from the NASA Cosmochemistry program to S. Messenger and L. Keller. NR 78 TC 2 Z9 2 U1 2 U2 12 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD AUG PY 2015 VL 50 IS 8 BP 1468 EP 1485 DI 10.1111/maps.12473 PG 18 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA CO7QW UT WOS:000359356900010 ER PT J AU Righter, K AF Righter, Kevin TI 2015 Service Award for Ralph Harvey Award SO METEORITICS & PLANETARY SCIENCE LA English DT Biographical-Item C1 NASA Johnson Space Ctr, Houston, TX 77058 USA. RP Righter, K (reprint author), NASA Johnson Space Ctr, Houston, TX 77058 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD AUG PY 2015 VL 50 IS 8 BP 1491 EP 1492 DI 10.1111/maps.12487 PG 2 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA CO7QW UT WOS:000359356900013 ER PT J AU Amari, S Messenger, S Clemett, SJ Meshik, A AF Amari, Sachiko Messenger, Scott Clemett, Simon J. Meshik, Alexander TI IDENTIFICATION OF Q FROM SARATOV (L4) SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 78th Annual Meeting of the Meteoritical-Society CY JUL 27-31, 2015 CL Berkeley, CA SP Meteorit Soc, Barringer Crater Co, Natl Aeronaut & Space Adm, Inst Space & Astronaut Sci, Japan Aerosp Explorat Agcy, Japan Polar Res Assoc, Natl Inst Polar Res, NASA Mars Program Off, Agilent Technologies, CAMECA, Lockheed Martin Space Syst Co, Natl Electrostat Corp, TESCAN, Int Meteorite Collectors Assoc, Planetary Studies Fdn, Lunar & Planetary Inst, Univ Calif, Space Sci Lab ID NOBLE-GASES; PHASE-Q; ALLENDE; CHONDRITES; METEORITE C1 [Amari, Sachiko; Meshik, Alexander] Washington Univ, Dept Phys, St Louis, MO 63130 USA. [Amari, Sachiko; Meshik, Alexander] Washington Univ, McDonnell Ctr Space Sci, St Louis, MO 63130 USA. [Messenger, Scott] NASA, Robert M Walker Lab Space Sci, EISD, ARES,Johnson Space Ctr, Houston, TX 77058 USA. [Clemett, Simon J.] ERC Inc JACOBS, Houston, TX 77023 USA. EM sa@physics.wustl.edu NR 10 TC 0 Z9 0 U1 1 U2 1 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD AUG PY 2015 VL 50 SU 1 SI SI MA 5127.pdf PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA CN7CR UT WOS:000358591900008 ER PT J AU Beaty, DW Hays, LE Williford, K Farley, K AF Beaty, D. W. Hays, L. E. Williford, K. Farley, K. TI SAMPLE SCIENCE INPUT TO LANDING SITE SELECTION FOR MARS 2020: AN IN-SITU EXPLORATION AND SAMPLE CACHING ROVER SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 78th Annual Meeting of the Meteoritical-Society CY JUL 27-31, 2015 CL Berkeley, CA SP Meteorit Soc, Barringer Crater Co, Natl Aeronaut & Space Adm, Inst Space & Astronaut Sci, Japan Aerosp Explorat Agcy, Japan Polar Res Assoc, Natl Inst Polar Res, NASA Mars Program Off, Agilent Technologies, CAMECA, Lockheed Martin Space Syst Co, Natl Electrostat Corp, TESCAN, Int Meteorite Collectors Assoc, Planetary Studies Fdn, Lunar & Planetary Inst, Univ Calif, Space Sci Lab C1 [Beaty, D. W.; Hays, L. E.; Williford, K.] CALTECH, Jet Prop Lab, Mars Program Off, Pasadena, CA 91109 USA. [Farley, K.] CALTECH, Pasadena, CA 91125 USA. EM dwbeaty@jpl.nasa.gov NR 2 TC 0 Z9 0 U1 2 U2 6 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD AUG PY 2015 VL 50 SU 1 SI SI MA 5340.pdf PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA CN7CR UT WOS:000358591900017 ER PT J AU Beaty, DW Niles, PB Bass, DS Bell, MS Bleacher, JE Cabrol, NA Conrad, PG Eppler, DB Hamilton, VE Hays, LE Head, JW Kahre, MA Levy, JS Lyons, TW Macalady, JL Rafkin, SCR Rice, JW Rice, MS AF Beaty, D. W. Niles, P. B. Bass, D. S. Bell, M. S. Bleacher, J. E. Cabrol, N. A. Conrad, P. G. Eppler, D. B. Hamilton, V. E. Hays, L. E. Head, J. W. Kahre, M. A. Levy, J. S. Lyons, T. W. Macalady, J. L. Rafkin, S. C. R. Rice, J. W. Rice, M. S. TI PLANNING AHEAD FOR MARS SAMPLE SCIENCE IN THE HUMAN EXPLORATION ERA SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 78th Annual Meeting of the Meteoritical-Society CY JUL 27-31, 2015 CL Berkeley, CA SP Meteorit Soc, Barringer Crater Co, Natl Aeronaut & Space Adm, Inst Space & Astronaut Sci, Japan Aerosp Explorat Agcy, Japan Polar Res Assoc, Natl Inst Polar Res, NASA Mars Program Off, Agilent Technologies, CAMECA, Lockheed Martin Space Syst Co, Natl Electrostat Corp, TESCAN, Int Meteorite Collectors Assoc, Planetary Studies Fdn, Lunar & Planetary Inst, Univ Calif, Space Sci Lab C1 [Beaty, D. W.; Bass, D. S.; Hays, L. E.] CALTECH, JPL, Pasadena, CA 91125 USA. [Head, J. W.] Brown Univ, Providence, RI 02912 USA. [Levy, J. S.] Univ Texas Austin, Austin, TX 78712 USA. [Lyons, T. W.] Univ Calif Riverside, Riverside, CA 92521 USA. [Macalady, J. L.] Penn State Univ, University Pk, PA 16802 USA. [Rice, J. W.] Planetary Sci Inst, Tucson, AZ USA. [Rice, M. S.] Western Washington Univ, Bellingham, WA 98225 USA. EM dwbeaty@jpl.nasa.gov NR 0 TC 0 Z9 0 U1 3 U2 4 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD AUG PY 2015 VL 50 SU 1 SI SI MA 5335.pdf PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA CN7CR UT WOS:000358591900018 ER PT J AU Beck, P Quirico, E Moroz, LV Schmitt, B Arnold, G Ciarniello, M Bonal, L Capaccioni, F Filacchione, G Erard, S Leyrat, C Bockelee-Morvan, D Tosi, F Raponi, A Capria, MT De Sanctis, MC Piccioni, G Barucci, A Drossart, P Markus, K Palomba, E Fonti, S Crovisier, J Carlson, R AF Beck, P. Quirico, E. Moroz, L. V. Schmitt, B. Arnold, G. Ciarniello, M. Bonal, L. Capaccioni, F. Filacchione, G. Erard, S. Leyrat, C. Bockelee-Morvan, D. Tosi, F. Raponi, A. Capria, M. T. De Sanctis, M. C. Piccioni, G. Barucci, A. Drossart, P. Markus, K. Palomba, E. Fonti, S. Crovisier, J. Carlson, R. CA Rosetta VIRTIS Team TI THE NUCLEUS OF 67P OBSERVED BY VIRTIS/ROSETTA: DIFFERENT FROM CARBONACOUS CHONDRITES AND SIMILAR TO D-TYPE ASTEROIDS ? SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 78th Annual Meeting of the Meteoritical-Society CY JUL 27-31, 2015 CL Berkeley, CA SP Meteorit Soc, Barringer Crater Co, Natl Aeronaut & Space Adm, Inst Space & Astronaut Sci, Japan Aerosp Explorat Agcy, Japan Polar Res Assoc, Natl Inst Polar Res, NASA Mars Program Off, Agilent Technologies, CAMECA, Lockheed Martin Space Syst Co, Natl Electrostat Corp, TESCAN, Int Meteorite Collectors Assoc, Planetary Studies Fdn, Lunar & Planetary Inst, Univ Calif, Space Sci Lab C1 [Beck, P.; Quirico, E.; Schmitt, B.; Bonal, L.] UGA, CNRS, IPAG, Grenoble, France. [Moroz, L. V.; Arnold, G.; Markus, K.] German Aerosp Ctr DLR Berlin, Berlin, Germany. [Ciarniello, M.; Capaccioni, F.; Filacchione, G.; Tosi, F.; Raponi, A.; Capria, M. T.; De Sanctis, M. C.; Piccioni, G.; Palomba, E.] INAF, IAPS, I-00133 Rome, Italy. [Erard, S.; Leyrat, C.; Bockelee-Morvan, D.; Barucci, A.; Drossart, P.; Crovisier, J.] Observ Paris, LESIA, Meudon, France. [Fonti, S.] Univ Salento, Dipartamento Matemat & Fis Ennio de Giorgi, Salento, Italy. [Carlson, R.] NASA, Jet Prop Lab, Pasadena, CA USA. EM pierre.beck@ujf-grenoble.fr NR 8 TC 0 Z9 0 U1 1 U2 5 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD AUG PY 2015 VL 50 SU 1 SI SI MA 5188.pdf PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA CN7CR UT WOS:000358591900019 ER PT J AU Bishop, JL Velbel, MA Filiberto, J AF Bishop, J. L. Velbel, M. A. Filiberto, J. TI DETERMINING MARTIAN AQUEOUS MINERALOGY THROUGH ANALYSES OF ORBITAL REMOTE SENSING & MARTIAN METEORITE GEOCHEMISTRY SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 78th Annual Meeting of the Meteoritical-Society CY JUL 27-31, 2015 CL Berkeley, CA SP Meteorit Soc, Barringer Crater Co, Natl Aeronaut & Space Adm, Inst Space & Astronaut Sci, Japan Aerosp Explorat Agcy, Japan Polar Res Assoc, Natl Inst Polar Res, NASA Mars Program Off, Agilent Technologies, CAMECA, Lockheed Martin Space Syst Co, Natl Electrostat Corp, TESCAN, Int Meteorite Collectors Assoc, Planetary Studies Fdn, Lunar & Planetary Inst, Univ Calif, Space Sci Lab ID MAWRTH VALLIS; MARS; ALH84001 C1 [Bishop, J. L.] SETI Inst, Mountain View, CA USA. [Bishop, J. L.] NASA Ames, Mountain View, CA USA. [Velbel, M. A.] Michigan State Univ, E Lansing, MI 48824 USA. [Filiberto, J.] So Illinois Univ, Carbondale, IL 62901 USA. EM jbishop@seti.org NR 16 TC 0 Z9 0 U1 4 U2 4 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD AUG PY 2015 VL 50 SU 1 SI SI MA 5113.pdf PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA CN7CR UT WOS:000358591900027 ER PT J AU Bridges, JC Schwenzer, SP Leveille, R Wiens, RC McAdam, A Conrad, P Kelley, SP AF Bridges, J. C. Schwenzer, S. P. Leveille, R. Wiens, R. C. McAdam, A. Conrad, P. Kelley, S. P. TI HEMATITE INDICATOR OF HIGH WATER TO ROCK RATIO ALTERATION IN GALE CRATER SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 78th Annual Meeting of the Meteoritical-Society CY JUL 27-31, 2015 CL Berkeley, CA SP Meteorit Soc, Barringer Crater Co, Natl Aeronaut & Space Adm, Inst Space & Astronaut Sci, Japan Aerosp Explorat Agcy, Japan Polar Res Assoc, Natl Inst Polar Res, NASA Mars Program Off, Agilent Technologies, CAMECA, Lockheed Martin Space Syst Co, Natl Electrostat Corp, TESCAN, Int Meteorite Collectors Assoc, Planetary Studies Fdn, Lunar & Planetary Inst, Univ Calif, Space Sci Lab C1 [Bridges, J. C.] Univ Leicester, Space Res Ctr, Leicester LE1 7RH, Leics, England. [Schwenzer, S. P.; Kelley, S. P.] Open Univ, Dept Environm Earth & Ecosyst, Milton Keynes MK7 6AA, Bucks, England. [Leveille, R.] McGill Univ, Montreal, PQ, Canada. [Wiens, R. C.] Los Alamos Natl Lab, Space Remote Sensing, Los Alamos, NM USA. [McAdam, A.; Conrad, P.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM j.bridges@le.ac.uk NR 5 TC 0 Z9 0 U1 0 U2 2 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD AUG PY 2015 VL 50 SU 1 SI SI MA 5293.pdf PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA CN7CR UT WOS:000358591900039 ER PT J AU Bryson, KL Agrawal, P Ostrowski, DR Sears, DWG AF Bryson, K. L. Agrawal, P. Ostrowski, D. R. Sears, D. W. G. TI FRACTURE CHARACTERIZATION OF METEORITES SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 78th Annual Meeting of the Meteoritical-Society CY JUL 27-31, 2015 CL Berkeley, CA SP Meteorit Soc, Barringer Crater Co, Natl Aeronaut & Space Adm, Inst Space & Astronaut Sci, Japan Aerosp Explorat Agcy, Japan Polar Res Assoc, Natl Inst Polar Res, NASA Mars Program Off, Agilent Technologies, CAMECA, Lockheed Martin Space Syst Co, Natl Electrostat Corp, TESCAN, Int Meteorite Collectors Assoc, Planetary Studies Fdn, Lunar & Planetary Inst, Univ Calif, Space Sci Lab ID METEOROIDS C1 [Bryson, K. L.; Agrawal, P.; Ostrowski, D. R.; Sears, D. W. G.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Bryson, K. L.; Ostrowski, D. R.; Sears, D. W. G.] BAER Inst, Ames Res Ctr, Moffett Field, CA USA. [Agrawal, P.] ERC Inc, NASA, Ames Res Ctr, Moffett Field, CA USA. EM kathryn.bryson@nasa.gov NR 3 TC 0 Z9 0 U1 0 U2 0 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD AUG PY 2015 VL 50 SU 1 SI SI MA 5361.pdf PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA CN7CR UT WOS:000358591900043 ER PT J AU Caseres, JR Liu, Y Guan, Y Chen, Y Ma, C Howarth, G Taylor, LA AF Caseres, J. R. Liu, Y. Guan, Y. Chen, Y. Ma, C. Howarth, G. Taylor, L. A. TI TRACE ELEMENT CHEMISTRY OF LARKMAN NUNATUK (LAR) 12011, A NEW OLIVINE-PHYRIC SHERGOTTITE SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 78th Annual Meeting of the Meteoritical-Society CY JUL 27-31, 2015 CL Berkeley, CA SP Meteorit Soc, Barringer Crater Co, Natl Aeronaut & Space Adm, Inst Space & Astronaut Sci, Japan Aerosp Explorat Agcy, Japan Polar Res Assoc, Natl Inst Polar Res, NASA Mars Program Off, Agilent Technologies, CAMECA, Lockheed Martin Space Syst Co, Natl Electrostat Corp, TESCAN, Int Meteorite Collectors Assoc, Planetary Studies Fdn, Lunar & Planetary Inst, Univ Calif, Space Sci Lab C1 [Caseres, J. R.; Liu, Y.; Guan, Y.; Ma, C.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Chen, Y.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Howarth, G.; Taylor, L. A.] Univ Tennessee, Planet Geosci Insititute, Knoxville, TN 37996 USA. EM jcaseres@caltech.edu NR 9 TC 0 Z9 0 U1 0 U2 1 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD AUG PY 2015 VL 50 SU 1 SI SI MA 5357.pdf PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA CN7CR UT WOS:000358591900048 ER PT J AU Chan, QHS Zolensky, ME Fries, M AF Chan, Q. H. S. Zolensky, M. E. Fries, M. TI ORGANO-CARBONATE ASSOCIATION IN CARBONACEOUS CHONDRITES SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 78th Annual Meeting of the Meteoritical-Society CY JUL 27-31, 2015 CL Berkeley, CA SP Meteorit Soc, Barringer Crater Co, Natl Aeronaut & Space Adm, Inst Space & Astronaut Sci, Japan Aerosp Explorat Agcy, Japan Polar Res Assoc, Natl Inst Polar Res, NASA Mars Program Off, Agilent Technologies, CAMECA, Lockheed Martin Space Syst Co, Natl Electrostat Corp, TESCAN, Int Meteorite Collectors Assoc, Planetary Studies Fdn, Lunar & Planetary Inst, Univ Calif, Space Sci Lab ID MATTER C1 [Chan, Q. H. S.; Zolensky, M. E.; Fries, M.] NASA, ARES, Johnson Space Ctr, Houston, TX 77058 USA. EM hschan@nasa.gov NR 8 TC 0 Z9 0 U1 1 U2 1 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD AUG PY 2015 VL 50 SU 1 SI SI MA 5138.pdf PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA CN7CR UT WOS:000358591900051 ER PT J AU Chan, QHS Zolensky, ME Tsuchiyama, A Martinez, JE AF Chan, Q. H. S. Zolensky, M. E. Tsuchiyama, A. Martinez, J. E. TI MAGNETITE SURFACE PROVIDES PREBIOTIC HOMOCHIRAL SELECTIVITY SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 78th Annual Meeting of the Meteoritical-Society CY JUL 27-31, 2015 CL Berkeley, CA SP Meteorit Soc, Barringer Crater Co, Natl Aeronaut & Space Adm, Inst Space & Astronaut Sci, Japan Aerosp Explorat Agcy, Japan Polar Res Assoc, Natl Inst Polar Res, NASA Mars Program Off, Agilent Technologies, CAMECA, Lockheed Martin Space Syst Co, Natl Electrostat Corp, TESCAN, Int Meteorite Collectors Assoc, Planetary Studies Fdn, Lunar & Planetary Inst, Univ Calif, Space Sci Lab ID AMINO-ACIDS C1 [Chan, Q. H. S.; Zolensky, M. E.] NASA, ARES, Johnson Space Ctr, Houston, TX 77058 USA. [Tsuchiyama, A.] Kyoto Univ, Grad Sch Sci, Sakyo Ku, Kyoto 6068502, Japan. [Martinez, J. E.] Jacobs Engn, Houston, TX 77058 USA. EM hschan@nasa.gov NR 5 TC 0 Z9 0 U1 3 U2 3 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD AUG PY 2015 VL 50 SU 1 SI SI MA 5179.pdf PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA CN7CR UT WOS:000358591900052 ER PT J AU Chen, Y Liu, Y Guan, Y Ma, C AF Chen, Y. Liu, Y. Guan, Y. Ma, C. TI NEW ROCK TYPES FROM MARS: TRACE ELEMENT SIGNATURES IN NWA 7034 CLASTS SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 78th Annual Meeting of the Meteoritical-Society CY JUL 27-31, 2015 CL Berkeley, CA SP Meteorit Soc, Barringer Crater Co, Natl Aeronaut & Space Adm, Inst Space & Astronaut Sci, Japan Aerosp Explorat Agcy, Japan Polar Res Assoc, Natl Inst Polar Res, NASA Mars Program Off, Agilent Technologies, CAMECA, Lockheed Martin Space Syst Co, Natl Electrostat Corp, TESCAN, Int Meteorite Collectors Assoc, Planetary Studies Fdn, Lunar & Planetary Inst, Univ Calif, Space Sci Lab ID METEORITE C1 [Chen, Y.; Liu, Y.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Guan, Y.; Ma, C.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. EM Yang.Chen@jpl.nasa.gov NR 4 TC 0 Z9 0 U1 1 U2 4 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD AUG PY 2015 VL 50 SU 1 SI SI MA 5239.pdf PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA CN7CR UT WOS:000358591900055 ER PT J AU Clemett, SJ Messenger, S Nakamura-Messenger, K Thomas-Keptra, KL AF Clemett, S. J. Messenger, S. Nakamura-Messenger, K. Thomas-Keptra, K. L. TI COORDINATED CHEMICAL AND ISOTOPIC IMAGING OF THE BELLS (CM2) METEORITE SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 78th Annual Meeting of the Meteoritical-Society CY JUL 27-31, 2015 CL Berkeley, CA SP Meteorit Soc, Barringer Crater Co, Natl Aeronaut & Space Adm, Inst Space & Astronaut Sci, Japan Aerosp Explorat Agcy, Japan Polar Res Assoc, Natl Inst Polar Res, NASA Mars Program Off, Agilent Technologies, CAMECA, Lockheed Martin Space Syst Co, Natl Electrostat Corp, TESCAN, Int Meteorite Collectors Assoc, Planetary Studies Fdn, Lunar & Planetary Inst, Univ Calif, Space Sci Lab C1 [Clemett, S. J.; Thomas-Keptra, K. L.] Jacobs Technol, JETS, Houston, TX 77058 USA. [Messenger, S.; Nakamura-Messenger, K.] NASA, Robert M Walker Lab Space Sci, ARES, JSC, Houston, TX 77058 USA. NR 6 TC 0 Z9 0 U1 0 U2 0 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD AUG PY 2015 VL 50 SU 1 SI SI MA 5339.pdf PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA CN7CR UT WOS:000358591900063 ER PT J AU Cohen, BA AF Cohen, B. A. TI THE POTASSIUM-ARGON LASER EXPERIMENT (KArLE): IN SITU GEOCHRONOLOGY FOR PLANETARY ROBOTIC MISSIONS SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 78th Annual Meeting of the Meteoritical-Society CY JUL 27-31, 2015 CL Berkeley, CA SP Meteorit Soc, Barringer Crater Co, Natl Aeronaut & Space Adm, Inst Space & Astronaut Sci, Japan Aerosp Explorat Agcy, Japan Polar Res Assoc, Natl Inst Polar Res, NASA Mars Program Off, Agilent Technologies, CAMECA, Lockheed Martin Space Syst Co, Natl Electrostat Corp, TESCAN, Int Meteorite Collectors Assoc, Planetary Studies Fdn, Lunar & Planetary Inst, Univ Calif, Space Sci Lab C1 [Cohen, B. A.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. EM barbara.a.cohen@nasa.gov NR 4 TC 0 Z9 0 U1 1 U2 1 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD AUG PY 2015 VL 50 SU 1 SI SI MA 5353.pdf PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA CN7CR UT WOS:000358591900064 ER PT J AU Cuzzi, JN AF Cuzzi, J. N. TI PLANETESIMAL FORMATION SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 78th Annual Meeting of the Meteoritical-Society CY JUL 27-31, 2015 CL Berkeley, CA SP Meteorit Soc, Barringer Crater Co, Natl Aeronaut & Space Adm, Inst Space & Astronaut Sci, Japan Aerosp Explorat Agcy, Japan Polar Res Assoc, Natl Inst Polar Res, NASA Mars Program Off, Agilent Technologies, CAMECA, Lockheed Martin Space Syst Co, Natl Electrostat Corp, TESCAN, Int Meteorite Collectors Assoc, Planetary Studies Fdn, Lunar & Planetary Inst, Univ Calif, Space Sci Lab C1 [Cuzzi, J. N.] NASA, Ames Res Ctr, Ames, IA USA. EM Jeffrey.Cuzzi@nasa.gov NR 3 TC 0 Z9 0 U1 0 U2 0 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD AUG PY 2015 VL 50 SU 1 SI SI MA 5392.pdf PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA CN7CR UT WOS:000358591900072 ER PT J AU Danielson, LR Righter, K Waeselmann, N Humayun, M AF Danielson, L. R. Righter, K. Waeselmann, N. Humayun, M. TI MAJORITE-GARNET PARTITIONING OF THE HIGHLY SIDEROPHILE ELEMENTS: NEW RESULTS AND APPLICATION TO MARS SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 78th Annual Meeting of the Meteoritical-Society CY JUL 27-31, 2015 CL Berkeley, CA SP Meteorit Soc, Barringer Crater Co, Natl Aeronaut & Space Adm, Inst Space & Astronaut Sci, Japan Aerosp Explorat Agcy, Japan Polar Res Assoc, Natl Inst Polar Res, NASA Mars Program Off, Agilent Technologies, CAMECA, Lockheed Martin Space Syst Co, Natl Electrostat Corp, TESCAN, Int Meteorite Collectors Assoc, Planetary Studies Fdn, Lunar & Planetary Inst, Univ Calif, Space Sci Lab ID MARTIAN MANTLE C1 [Danielson, L. R.] NASA, Jacobs Technol ESCG, Johnson Space Ctr, Houston, TX 77058 USA. [Righter, K.] NASA, Johnson Space Ctr, Houston, TX 77058 USA. [Waeselmann, N.; Humayun, M.] Florida State Univ, Natl High Magnet Field Lab, Tallahassee, FL 32306 USA. EM lisa.r.danielson@nasa.gov NR 7 TC 1 Z9 1 U1 0 U2 1 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD AUG PY 2015 VL 50 SU 1 SI SI MA 5343.pdf PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA CN7CR UT WOS:000358591900074 ER PT J AU Desch, SJ Turner, NJ AF Desch, Steven J. Turner, Neal J. TI HIGH-TEMPERATURE IONIZATION OF DUSTY GASES AND IMPLICATIONS FOR CHONDRULE FORMATION IN CURRENT SHEETS SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 78th Annual Meeting of the Meteoritical-Society CY JUL 27-31, 2015 CL Berkeley, CA SP Meteorit Soc, Barringer Crater Co, Natl Aeronaut & Space Adm, Inst Space & Astronaut Sci, Japan Aerosp Explorat Agcy, Japan Polar Res Assoc, Natl Inst Polar Res, NASA Mars Program Off, Agilent Technologies, CAMECA, Lockheed Martin Space Syst Co, Natl Electrostat Corp, TESCAN, Int Meteorite Collectors Assoc, Planetary Studies Fdn, Lunar & Planetary Inst, Univ Calif, Space Sci Lab C1 [Desch, Steven J.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [Turner, Neal J.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. EM steve.desch@asu.edu NR 4 TC 0 Z9 0 U1 1 U2 2 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD AUG PY 2015 VL 50 SU 1 SI SI MA 5377.pdf PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA CN7CR UT WOS:000358591900078 ER PT J AU Friedrich, JM Glavin, DP Rivers, ML Dworkin, JP AF Friedrich, J. M. Glavin, D. P. Rivers, M. L. Dworkin, J. P. TI EFFECT OF A ROUTINE SYNCHROTRON X-RAY MICROTOMOGRAPHY SCAN ON THE AMINO ACID CONTENT OF THE MURCHISON CM CHONDRITE. SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 78th Annual Meeting of the Meteoritical-Society CY JUL 27-31, 2015 CL Berkeley, CA SP Meteorit Soc, Barringer Crater Co, Natl Aeronaut & Space Adm, Inst Space & Astronaut Sci, Japan Aerosp Explorat Agcy, Japan Polar Res Assoc, Natl Inst Polar Res, NASA Mars Program Off, Agilent Technologies, CAMECA, Lockheed Martin Space Syst Co, Natl Electrostat Corp, TESCAN, Int Meteorite Collectors Assoc, Planetary Studies Fdn, Lunar & Planetary Inst, Univ Calif, Space Sci Lab C1 [Friedrich, J. M.] Fordham Univ, Dept Chem, Bronx, NY 10458 USA. [Friedrich, J. M.] Amer Museum Nat Hist, Dept Earth & Planetary Sci, New York, NY 10024 USA. [Glavin, D. P.; Dworkin, J. P.] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA. [Rivers, M. L.] Univ Chicago, Ctr Adv Radiat Sources, Argonne, IL USA. EM friedrich@fordham.edu RI Dworkin, Jason/C-9417-2012; Glavin, Daniel/D-6194-2012 OI Dworkin, Jason/0000-0002-3961-8997; Glavin, Daniel/0000-0001-7779-7765 NR 5 TC 0 Z9 0 U1 0 U2 1 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD AUG PY 2015 VL 50 SU 1 SI SI MA 5208.pdf PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA CN7CR UT WOS:000358591900102 ER PT J AU Fries, M Christou, A Archer, D Conrad, P Cooke, W Eigenbrode, J ten Kate, IL Matney, M Niles, P Sykes, M Steele, A Treiman, A AF Fries, M. Christou, A. Archer, D. Conrad, P. Cooke, W. Eigenbrode, J. ten Kate, I. L. Matney, M. Niles, P. Sykes, M. Steele, A. Treiman, A. TI A METEOR SHOWER ORIGIN FOR MARTIAN METHANE. SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 78th Annual Meeting of the Meteoritical-Society CY JUL 27-31, 2015 CL Berkeley, CA SP Meteorit Soc, Barringer Crater Co, Natl Aeronaut & Space Adm, Inst Space & Astronaut Sci, Japan Aerosp Explorat Agcy, Japan Polar Res Assoc, Natl Inst Polar Res, NASA Mars Program Off, Agilent Technologies, CAMECA, Lockheed Martin Space Syst Co, Natl Electrostat Corp, TESCAN, Int Meteorite Collectors Assoc, Planetary Studies Fdn, Lunar & Planetary Inst, Univ Calif, Space Sci Lab ID MARS; ATMOSPHERE C1 [Fries, M.; Archer, D.; Matney, M.; Niles, P.] NASA JSC, Houston, TX USA. [Christou, A.] Armagh Observ, Armagh BT61 9DG, North Ireland. [Conrad, P.; Eigenbrode, J.] NASA Goddard SFC, Greenbelt, MD USA. [Cooke, W.] NASA Marshall SFC, Huntsville, AL USA. [ten Kate, I. L.] Univ Utrecht, Dept Earth Sci, NL-3508 TC Utrecht, Netherlands. [Sykes, M.] Planetary Sci Inst, Tucson, AZ USA. [Steele, A.] Carnegie Inst Sci, Geophys Lab, Washington, DC 20015 USA. [Treiman, A.] Lunar & Planetary Inst, Houston, TX 77058 USA. NR 13 TC 0 Z9 0 U1 1 U2 7 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD AUG PY 2015 VL 50 SU 1 SI SI MA 5286.pdf PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA CN7CR UT WOS:000358591900104 ER PT J AU Fries, M Calaway, M Evans, C McCubbin, F AF Fries, M. Calaway, M. Evans, C. McCubbin, F. TI ADVANCED CURATION: SOLVING CURRENT AND FUTURE SAMPLE RETURN PROBLEMS. SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 78th Annual Meeting of the Meteoritical-Society CY JUL 27-31, 2015 CL Berkeley, CA SP Meteorit Soc, Barringer Crater Co, Natl Aeronaut & Space Adm, Inst Space & Astronaut Sci, Japan Aerosp Explorat Agcy, Japan Polar Res Assoc, Natl Inst Polar Res, NASA Mars Program Off, Agilent Technologies, CAMECA, Lockheed Martin Space Syst Co, Natl Electrostat Corp, TESCAN, Int Meteorite Collectors Assoc, Planetary Studies Fdn, Lunar & Planetary Inst, Univ Calif, Space Sci Lab C1 [Fries, M.; Evans, C.; McCubbin, F.] NASA, Lyndon B Johnson Space Ctr, Astromat Acquisit & Curat Off, ARES, Houston, TX 77058 USA. [Calaway, M.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. EM marc.d.fries@nasa.gov NR 8 TC 0 Z9 0 U1 0 U2 0 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD AUG PY 2015 VL 50 SU 1 SI SI MA 5379.pdf PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA CN7CR UT WOS:000358591900103 ER PT J AU Goodrich, CA Fioretti, AM O'Brien, DP Zolensky, M Jenniskens, P Shaddad, MH AF Goodrich, C. A. Fioretti, A. M. O'Brien, D. P. Zolensky, M. Jenniskens, P. Shaddad, M. H. TI COMPARING THE FOREIGN CLAST POPULATIONS OF ALMAHATA SITTA AND TYPICAL POLYMICT UREILITES, WITH IMPLICATIONS. SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 78th Annual Meeting of the Meteoritical-Society CY JUL 27-31, 2015 CL Berkeley, CA SP Meteorit Soc, Barringer Crater Co, Natl Aeronaut & Space Adm, Inst Space & Astronaut Sci, Japan Aerosp Explorat Agcy, Japan Polar Res Assoc, Natl Inst Polar Res, NASA Mars Program Off, Agilent Technologies, CAMECA, Lockheed Martin Space Syst Co, Natl Electrostat Corp, TESCAN, Int Meteorite Collectors Assoc, Planetary Studies Fdn, Lunar & Planetary Inst, Univ Calif, Space Sci Lab ID ASTEROID 2008 TC3; BRECCIA; IMPACT; ORIGIN C1 [Goodrich, C. A.; O'Brien, D. P.] Planet Sci Inst, Tucson, AZ USA. [Fioretti, A. M.] CNR, IGG, Ital Nat Res Council, I-00185 Rome, Italy. [Zolensky, M.] NASA, JSC, Houston, TX USA. [Jenniskens, P.] NASA Ames, SETI Inst, Ames, IA USA. [Shaddad, M. H.] Univ Khartoum, Khartoum, Sudan. EM cgoodrich@psi.edu NR 14 TC 0 Z9 0 U1 0 U2 0 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD AUG PY 2015 VL 50 SU 1 SI SI MA 5018.pdf PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA CN7CR UT WOS:000358591900112 ER PT J AU Han, J Keller, LP Needham, AW Messenger, S Simon, JI AF Han, J. Keller, L. P. Needham, A. W. Messenger, S. Simon, J. I. TI MICROSTRUCTURAL INVESTIGATION OF A WARK-LOVERING RIM ON A VIGARANO CAI SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 78th Annual Meeting of the Meteoritical-Society CY JUL 27-31, 2015 CL Berkeley, CA SP Meteorit Soc, Barringer Crater Co, Natl Aeronaut & Space Adm, Inst Space & Astronaut Sci, Japan Aerosp Explorat Agcy, Japan Polar Res Assoc, Natl Inst Polar Res, NASA Mars Program Off, Agilent Technologies, CAMECA, Lockheed Martin Space Syst Co, Natl Electrostat Corp, TESCAN, Int Meteorite Collectors Assoc, Planetary Studies Fdn, Lunar & Planetary Inst, Univ Calif, Space Sci Lab ID RICH INCLUSIONS C1 [Han, J.] USRA LPI, Houston, TX 77058 USA. [Han, J.; Keller, L. P.; Needham, A. W.; Messenger, S.; Simon, J. I.] NASA JSC, Houston, TX 77058 USA. [Needham, A. W.] Oak Ridge Associated Univ, Oak Ridge, TN 37831 USA. EM jangmi.han@nasa.gov NR 6 TC 0 Z9 0 U1 0 U2 0 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD AUG PY 2015 VL 50 SU 1 SI SI MA 5243.pdf PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA CN7CR UT WOS:000358591900124 ER PT J AU Harvey, RP AF Harvey, R. P. TI PARENT BODY VENUS: A PRIMER FOR METEORITE RESEARCHERS SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 78th Annual Meeting of the Meteoritical-Society CY JUL 27-31, 2015 CL Berkeley, CA SP Meteorit Soc, Barringer Crater Co, Natl Aeronaut & Space Adm, Inst Space & Astronaut Sci, Japan Aerosp Explorat Agcy, Japan Polar Res Assoc, Natl Inst Polar Res, NASA Mars Program Off, Agilent Technologies, CAMECA, Lockheed Martin Space Syst Co, Natl Electrostat Corp, TESCAN, Int Meteorite Collectors Assoc, Planetary Studies Fdn, Lunar & Planetary Inst, Univ Calif, Space Sci Lab ID ATMOSPHERE C1 [Harvey, R. P.] Case Western Reserve Univ, Earth Environm & Planetary Sci, Cleveland, OH 44106 USA. [Harvey, R. P.] NASA, Glenn Res Ctr, Cleveland, OH USA. EM rph@case.edu NR 8 TC 0 Z9 0 U1 0 U2 0 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD AUG PY 2015 VL 50 SU 1 SI SI MA 5036.pdf PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA CN7CR UT WOS:000358591900132 ER PT J AU Jenniskens, P Harlan, S Zolensky, M Yin, QZ Verosub, KL Jull, AJ AF Jenniskens, P. Harlan, S. Zolensky, M. Yin, Q-Z Verosub, K. L. Jull, A. J. TI METEORITES FOUND ON MISFITS FLAT DRY LAKE SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 78th Annual Meeting of the Meteoritical-Society CY JUL 27-31, 2015 CL Berkeley, CA SP Meteorit Soc, Barringer Crater Co, Natl Aeronaut & Space Adm, Inst Space & Astronaut Sci, Japan Aerosp Explorat Agcy, Japan Polar Res Assoc, Natl Inst Polar Res, NASA Mars Program Off, Agilent Technologies, CAMECA, Lockheed Martin Space Syst Co, Natl Electrostat Corp, TESCAN, Int Meteorite Collectors Assoc, Planetary Studies Fdn, Lunar & Planetary Inst, Univ Calif, Space Sci Lab C1 [Jenniskens, P.; Harlan, S.] SETI Inst, Mountain View, CA USA. [Zolensky, M.] NASA JSC, Houston, TX USA. [Yin, Q-Z; Verosub, K. L.] Univ Calif Davis, Davis, CA USA. [Jull, A. J.] Univ Arizona, Tucson, AZ USA. NR 3 TC 0 Z9 0 U1 0 U2 0 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD AUG PY 2015 VL 50 SU 1 SI SI MA 5140.pdf PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA CN7CR UT WOS:000358591900156 ER PT J AU Johnson, NM Locke, DR Yazzie, CA Ferguson, FT Nuth, JA AF Johnson, N. M. Locke, D. R. Yazzie, C. A. Ferguson, F. T. Nuth, J. A. TI ORGANIC COATINGS DEPOSITED BY FISCHER-TROPSCH-TYPE REACTIONS SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 78th Annual Meeting of the Meteoritical-Society CY JUL 27-31, 2015 CL Berkeley, CA SP Meteorit Soc, Barringer Crater Co, Natl Aeronaut & Space Adm, Inst Space & Astronaut Sci, Japan Aerosp Explorat Agcy, Japan Polar Res Assoc, Natl Inst Polar Res, NASA Mars Program Off, Agilent Technologies, CAMECA, Lockheed Martin Space Syst Co, Natl Electrostat Corp, TESCAN, Int Meteorite Collectors Assoc, Planetary Studies Fdn, Lunar & Planetary Inst, Univ Calif, Space Sci Lab C1 [Johnson, N. M.; Ferguson, F. T.] NASA GSFC, Astrochem Lab, Greenbelt, MD USA. [Locke, D. R.] NASA JSC, Jacobs JETS Contract HX5, Houston, TX USA. [Yazzie, C. A.] Dine Coll, Tsaile, AZ USA. [Ferguson, F. T.] Catholic Univ Amer, Dept Chem, Washington, DC 20064 USA. [Nuth, J. A.] NASA GSFC, Solar Syst Explorat Div 690, Greenbelt, MD USA. EM natasha.m.johnson@nasa.gov NR 5 TC 0 Z9 0 U1 1 U2 2 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD AUG PY 2015 VL 50 SU 1 SI SI MA 5370.pdf PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA CN7CR UT WOS:000358591900158 ER PT J AU Kebukawa, Y Zolensky, ME Chan, QHS Fries, M Steele, A Kilcoyne, ALD Rahman, Z Cody, GD AF Kebukawa, Y. Zolensky, M. E. Chan, Q. H. S. Fries, M. Steele, A. Kilcoyne, A. L. David Rahman, Z. Cody, G. D. TI CONSTRAINING THERMAL PROCESSING OF CARBON-RICH AGGREGATES IN XENOLITHIC CLASTS FROM SHARPS (H3.4) METEORITE. SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 78th Annual Meeting of the Meteoritical-Society CY JUL 27-31, 2015 CL Berkeley, CA SP Meteorit Soc, Barringer Crater Co, Natl Aeronaut & Space Adm, Inst Space & Astronaut Sci, Japan Aerosp Explorat Agcy, Japan Polar Res Assoc, Natl Inst Polar Res, NASA Mars Program Off, Agilent Technologies, CAMECA, Lockheed Martin Space Syst Co, Natl Electrostat Corp, TESCAN, Int Meteorite Collectors Assoc, Planetary Studies Fdn, Lunar & Planetary Inst, Univ Calif, Space Sci Lab C1 [Kebukawa, Y.] Yokohama Natl Univ, Fac Engn, Yokohama, Kanagawa 240, Japan. [Zolensky, M. E.; Chan, Q. H. S.; Fries, M.] NASA, Johnson Space Ctr, Houston, TX USA. [Steele, A.; Cody, G. D.] Carnegie Inst Sci, Geophys Lab, Washington, DC USA. [Kilcoyne, A. L. David] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Adv Light Source, Berkeley, CA 94720 USA. [Rahman, Z.] ESCG Jacobs, Houston, TX USA. EM kebukawa@ynu.ac.jp RI Kilcoyne, David/I-1465-2013 NR 4 TC 0 Z9 0 U1 0 U2 1 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD AUG PY 2015 VL 50 SU 1 SI SI MA 5158.pdf PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA CN7CR UT WOS:000358591900162 ER PT J AU Keller, LP Christoffersen, R Dukes, CA Baragiola, RA Rahman, Z AF Keller, L. P. Christoffersen, R. Dukes, C. A. Baragiola, R. A. Rahman, Z. TI Fe AND O EELS STUDIES OF ION IRRADIATED MURCHISON CM2 CARBONACEOUS CHONDRITE MATRIX. SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 78th Annual Meeting of the Meteoritical-Society CY JUL 27-31, 2015 CL Berkeley, CA SP Meteorit Soc, Barringer Crater Co, Natl Aeronaut & Space Adm, Inst Space & Astronaut Sci, Japan Aerosp Explorat Agcy, Japan Polar Res Assoc, Natl Inst Polar Res, NASA Mars Program Off, Agilent Technologies, CAMECA, Lockheed Martin Space Syst Co, Natl Electrostat Corp, TESCAN, Int Meteorite Collectors Assoc, Planetary Studies Fdn, Lunar & Planetary Inst, Univ Calif, Space Sci Lab ID NANOMETER-SCALE MEASUREMENTS; ENERGY-LOSS SPECTROSCOPY C1 [Keller, L. P.] NASA, ARES, JSC, Houston, TX 77058 USA. [Christoffersen, R.; Rahman, Z.] NASA, Jacobs, JSC, Houston, TX 77058 USA. [Dukes, C. A.; Baragiola, R. A.] Univ Virginia, Lab Atom & Surface Phys, Charlottesville, VA 22904 USA. EM Lindsay.P.Keller@nasa.gov NR 4 TC 0 Z9 0 U1 1 U2 2 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD AUG PY 2015 VL 50 SU 1 SI SI MA 5354.pdf PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA CN7CR UT WOS:000358591900163 ER PT J AU Liu, Y Ma, C Chen, Y Beckett, J Guan, YB AF Liu, Yang Ma, Chi Chen, Yang Beckett, John Guan, Yunbin TI RARE-EARTH MINERALS IN MARTIAN METEORITE NWA 7034/7533: EVIDENCE FOR FLUID-ROCK INTERACTION IN THE MARTIAN CRUST. SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 78th Annual Meeting of the Meteoritical-Society CY JUL 27-31, 2015 CL Berkeley, CA SP Meteorit Soc, Barringer Crater Co, Natl Aeronaut & Space Adm, Inst Space & Astronaut Sci, Japan Aerosp Explorat Agcy, Japan Polar Res Assoc, Natl Inst Polar Res, NASA Mars Program Off, Agilent Technologies, CAMECA, Lockheed Martin Space Syst Co, Natl Electrostat Corp, TESCAN, Int Meteorite Collectors Assoc, Planetary Studies Fdn, Lunar & Planetary Inst, Univ Calif, Space Sci Lab ID (Y+REE)-PHOSPHATE MINERALS; INDUCED NUCLEATION; APATITE C1 [Liu, Yang; Chen, Yang] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Ma, Chi; Beckett, John; Guan, Yunbin] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. EM yangliu@jpl.nasa.gov NR 9 TC 0 Z9 0 U1 2 U2 5 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD AUG PY 2015 VL 50 SU 1 SI SI MA 5051.pdf PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA CN7CR UT WOS:000358591900196 ER PT J AU Liu, Y Ma, C Beckett, J AF Liu, Yang Ma, Chi Beckett, John TI HYDROTHERMAL ALTERATION OF MARTIAN ZIRCONS IN NWA 7034/7533. SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 78th Annual Meeting of the Meteoritical-Society CY JUL 27-31, 2015 CL Berkeley, CA SP Meteorit Soc, Barringer Crater Co, Natl Aeronaut & Space Adm, Inst Space & Astronaut Sci, Japan Aerosp Explorat Agcy, Japan Polar Res Assoc, Natl Inst Polar Res, NASA Mars Program Off, Agilent Technologies, CAMECA, Lockheed Martin Space Syst Co, Natl Electrostat Corp, TESCAN, Int Meteorite Collectors Assoc, Planetary Studies Fdn, Lunar & Planetary Inst, Univ Calif, Space Sci Lab C1 [Liu, Yang] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Ma, Chi; Beckett, John] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. EM yang.liu@jpl.nasa.gov NR 5 TC 1 Z9 1 U1 1 U2 3 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD AUG PY 2015 VL 50 SU 1 SI SI MA 5080.pdf PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA CN7CR UT WOS:000358591900195 ER PT J AU Matzel, J Jacobsen, B Simon, JI AF Matzel, J. Jacobsen, B. Simon, J. I. TI ALUMINUM-MAGNESIUM CHRONOLOGY OF THE RIM OF A MURCHISON TYPE A CAI. SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 78th Annual Meeting of the Meteoritical-Society CY JUL 27-31, 2015 CL Berkeley, CA SP Meteorit Soc, Barringer Crater Co, Natl Aeronaut & Space Adm, Inst Space & Astronaut Sci, Japan Aerosp Explorat Agcy, Japan Polar Res Assoc, Natl Inst Polar Res, NASA Mars Program Off, Agilent Technologies, CAMECA, Lockheed Martin Space Syst Co, Natl Electrostat Corp, TESCAN, Int Meteorite Collectors Assoc, Planetary Studies Fdn, Lunar & Planetary Inst, Univ Calif, Space Sci Lab ID INCLUSIONS C1 [Matzel, J.; Jacobsen, B.] Lawrence Livermore Natl Lab, Livermore, CA USA. [Simon, J. I.] NASA, Johnson Space Ctr, Houston, TX USA. EM matzel2@llnl.gov NR 5 TC 0 Z9 0 U1 0 U2 0 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD AUG PY 2015 VL 50 SU 1 SI SI MA 5372.pdf PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA CN7CR UT WOS:000358591900213 ER PT J AU McFadden, LA McCord, TB Scully, JEC AF McFadden, L. A. McCord, T. B. Scully, J. E. C. CA Dawn Sci Team TI VESTA BEFORE ARRIVAL AT CERES: REGIONAL SURFACE COMPOSITION. SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 78th Annual Meeting of the Meteoritical-Society CY JUL 27-31, 2015 CL Berkeley, CA SP Meteorit Soc, Barringer Crater Co, Natl Aeronaut & Space Adm, Inst Space & Astronaut Sci, Japan Aerosp Explorat Agcy, Japan Polar Res Assoc, Natl Inst Polar Res, NASA Mars Program Off, Agilent Technologies, CAMECA, Lockheed Martin Space Syst Co, Natl Electrostat Corp, TESCAN, Int Meteorite Collectors Assoc, Planetary Studies Fdn, Lunar & Planetary Inst, Univ Calif, Space Sci Lab C1 [McFadden, L. A.] NASA, Goddard Space Flight Ctr, Silver Spring, MD USA. [McCord, T. B.] Bearfight Inst, Winthrop, WA USA. [Scully, J. E. C.] Univ Calif Los Angeles, Los Angeles, CA 90024 USA. EM lucy.mcfadden@nasa.gov NR 12 TC 0 Z9 0 U1 0 U2 0 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD AUG PY 2015 VL 50 SU 1 SI SI MA 5143.pdf PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA CN7CR UT WOS:000358591900216 ER PT J AU Messenger, S Brownlee, DE Joswiak, DJ Nguyen, AN AF Messenger, S. Brownlee, D. E. Joswiak, D. J. Nguyen, A. N. TI NEBULAR AND INTERSTELLAR MATERIALS IN A GIANT CLUSTER IDP OF PROBABLE COMETARY ORIGIN. SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 78th Annual Meeting of the Meteoritical-Society CY JUL 27-31, 2015 CL Berkeley, CA SP Meteorit Soc, Barringer Crater Co, Natl Aeronaut & Space Adm, Inst Space & Astronaut Sci, Japan Aerosp Explorat Agcy, Japan Polar Res Assoc, Natl Inst Polar Res, NASA Mars Program Off, Agilent Technologies, CAMECA, Lockheed Martin Space Syst Co, Natl Electrostat Corp, TESCAN, Int Meteorite Collectors Assoc, Planetary Studies Fdn, Lunar & Planetary Inst, Univ Calif, Space Sci Lab ID STARDUST C1 [Messenger, S.] NASA, Lyndon B Johnson Space Ctr, Robert M Walker Lab Space Sci, EISD,ARES, Houston, TX 77058 USA. [Brownlee, D. E.; Joswiak, D. J.] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Nguyen, A. N.] NASA, Lyndon B Johnson Space Ctr, JETS, Houston, TX 77058 USA. EM scott.r.messenger@nasa.gov NR 9 TC 0 Z9 0 U1 2 U2 2 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD AUG PY 2015 VL 50 SU 1 SI SI MA 5365.pdf PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA CN7CR UT WOS:000358591900222 ER PT J AU Mishra, RK Simon, JI Ross, DK Keller, LP Marhas, KK Needham, AW AF Mishra, R. K. Simon, J. I. Ross, D. K. Keller, L. P. Marhas, K. K. Needham, A. W. TI A REFRACTORY INCLUSION IN UNEQUILIBRATED ORDINARY CHONDRITE (LL3.3) ALLAN HILLS A81251. SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 78th Annual Meeting of the Meteoritical-Society CY JUL 27-31, 2015 CL Berkeley, CA SP Meteorit Soc, Barringer Crater Co, Natl Aeronaut & Space Adm, Inst Space & Astronaut Sci, Japan Aerosp Explorat Agcy, Japan Polar Res Assoc, Natl Inst Polar Res, NASA Mars Program Off, Agilent Technologies, CAMECA, Lockheed Martin Space Syst Co, Natl Electrostat Corp, TESCAN, Int Meteorite Collectors Assoc, Planetary Studies Fdn, Lunar & Planetary Inst, Univ Calif, Space Sci Lab ID AL-26 C1 [Mishra, R. K.; Needham, A. W.] Oak Ridge Associated Univ, Oak Ridge, TN 37831 USA. [Mishra, R. K.; Simon, J. I.; Ross, D. K.; Keller, L. P.; Marhas, K. K.; Needham, A. W.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Ross, D. K.] Jacobs Technol JETS, Houston, TX 77058 USA. [Marhas, K. K.] LPI, Houston, TX 77058 USA. [Marhas, K. K.] Phys Res Lab, Ahmadabad 380009, Gujarat, India. EM ritesh.k.mishra@nasa.gov NR 3 TC 0 Z9 0 U1 1 U2 1 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD AUG PY 2015 VL 50 SU 1 SI SI MA 5139.pdf PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA CN7CR UT WOS:000358591900228 ER PT J AU Mishra, RK Simon, JI Messenger, S Marhas, KK Ross, DK Needham, AW Han, J AF Mishra, R. K. Simon, J. I. Messenger, S. Marhas, K. K. Ross, D. K. Needham, A. W. Han, J. TI OXYGEN ISOTOPES IN PEROVSKITES AND ASSOCIATED MINERAL ASSEMBLAGES IN A HIBONITE-BEARING ALLENDE CAI. SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 78th Annual Meeting of the Meteoritical-Society CY JUL 27-31, 2015 CL Berkeley, CA SP Meteorit Soc, Barringer Crater Co, Natl Aeronaut & Space Adm, Inst Space & Astronaut Sci, Japan Aerosp Explorat Agcy, Japan Polar Res Assoc, Natl Inst Polar Res, NASA Mars Program Off, Agilent Technologies, CAMECA, Lockheed Martin Space Syst Co, Natl Electrostat Corp, TESCAN, Int Meteorite Collectors Assoc, Planetary Studies Fdn, Lunar & Planetary Inst, Univ Calif, Space Sci Lab C1 [Mishra, R. K.; Needham, A. W.] Oak Ridge Associated Univ, Oak Ridge, TN 37831 USA. [Mishra, R. K.; Simon, J. I.; Messenger, S.; Marhas, K. K.; Ross, D. K.; Needham, A. W.; Han, J.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Marhas, K. K.] Phys Res Lab, Ahmadabad 380009, Gujarat, India. [Marhas, K. K.; Han, J.] LPI, Houston, TX 77058 USA. [Ross, D. K.] Jacobs Technol JETS, Houston, TX 77058 USA. EM ritesh.k.mishra@nasa.gov NR 3 TC 0 Z9 0 U1 1 U2 3 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD AUG PY 2015 VL 50 SU 1 SI SI MA 5133.pdf PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA CN7CR UT WOS:000358591900227 ER PT J AU Mittlefehldt, DW Peng, ZX Torrano, ZA AF Mittlefehldt, D. W. Peng, Z. X. Torrano, Z. A. TI PETROLOGY AND IN SITU TRACE ELEMENT CHEMISTRY OF A SUITE OF R CHONDRITES. SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 78th Annual Meeting of the Meteoritical-Society CY JUL 27-31, 2015 CL Berkeley, CA SP Meteorit Soc, Barringer Crater Co, Natl Aeronaut & Space Adm, Inst Space & Astronaut Sci, Japan Aerosp Explorat Agcy, Japan Polar Res Assoc, Natl Inst Polar Res, NASA Mars Program Off, Agilent Technologies, CAMECA, Lockheed Martin Space Syst Co, Natl Electrostat Corp, TESCAN, Int Meteorite Collectors Assoc, Planetary Studies Fdn, Lunar & Planetary Inst, Univ Calif, Space Sci Lab C1 [Mittlefehldt, D. W.] NASA, Lyndon B Johnson Space Ctr, Silver Spring, MD USA. [Peng, Z. X.] Jacobs Technol Inc, Johnson Space Ctr, Pasadena, CA USA. [Torrano, Z. A.] Univ Notre Dame, Notre Dame, IN 46556 USA. EM david.w.mittlefehldt@nasa.gov NR 9 TC 0 Z9 0 U1 1 U2 1 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD AUG PY 2015 VL 50 SU 1 SI SI MA 5338.pdf PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA CN7CR UT WOS:000358591900230 ER PT J AU Mittlefehldt, DW Peng, ZX AF Mittlefehldt, D. W. Peng, Z. X. TI PETROLOGY OF ANOMALOUS EUCRITE QUE 94484. SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 78th Annual Meeting of the Meteoritical-Society CY JUL 27-31, 2015 CL Berkeley, CA SP Meteorit Soc, Barringer Crater Co, Natl Aeronaut & Space Adm, Inst Space & Astronaut Sci, Japan Aerosp Explorat Agcy, Japan Polar Res Assoc, Natl Inst Polar Res, NASA Mars Program Off, Agilent Technologies, CAMECA, Lockheed Martin Space Syst Co, Natl Electrostat Corp, TESCAN, Int Meteorite Collectors Assoc, Planetary Studies Fdn, Lunar & Planetary Inst, Univ Calif, Space Sci Lab ID BODIES C1 [Mittlefehldt, D. W.] NASA, Lyndon B Johnson Space Ctr, Silver Spring, MD USA. [Peng, Z. X.] Jacobs Technol Inc, Johnson Space Ctr, Pasadena, CA USA. EM david.w.mittlefehldt@nasa.gov NR 9 TC 0 Z9 0 U1 1 U2 4 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD AUG PY 2015 VL 50 SU 1 SI SI MA 5342.pdf PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA CN7CR UT WOS:000358591900229 ER PT J AU Nakamura-Messenger, K Messenger, S Westphal, AJ Palma, RL Pepin, RO AF Nakamura-Messenger, K. Messenger, S. Westphal, A. J. Palma, R. L. Pepin, R. O. TI MINERALOGY OF INTERPLANETARY DUST PARTICLES FROM THE COMET GIACOBINI-ZINNER DUST STREAM COLLECTIONS SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 78th Annual Meeting of the Meteoritical-Society CY JUL 27-31, 2015 CL Berkeley, CA SP Meteorit Soc, Barringer Crater Co, Natl Aeronaut & Space Adm, Inst Space & Astronaut Sci, Japan Aerosp Explorat Agcy, Japan Polar Res Assoc, Natl Inst Polar Res, NASA Mars Program Off, Agilent Technologies, CAMECA, Lockheed Martin Space Syst Co, Natl Electrostat Corp, TESCAN, Int Meteorite Collectors Assoc, Planetary Studies Fdn, Lunar & Planetary Inst, Univ Calif, Space Sci Lab C1 [Nakamura-Messenger, K.; Messenger, S.] NASA, Lyndon B Johnson Space Ctr, Robert M Walker Lab Space Sci, ARES EISD, Houston, TX 77058 USA. [Westphal, A. J.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Palma, R. L.; Pepin, R. O.] Univ Minnesota, Dept Phys, Minneapolis, MN 55455 USA. [Palma, R. L.] Minnesota State Univ, Dept Phys & Astron, Mankato, MN USA. EM keiko.nakamura-1@nasa.gov NR 4 TC 0 Z9 0 U1 0 U2 0 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD AUG PY 2015 VL 50 SU 1 SI SI MA 5322.pdf PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA CN7CR UT WOS:000358591900245 ER PT J AU Needham, AW Messenger, S Keller, LP Simon, JI Han, J Mishra, RK Marhas, KK AF Needham, A. W. Messenger, S. Keller, L. P. Simon, J. I. Han, J. Mishra, R. K. Marhas, K. K. TI ALUMINUM-MAGNESIUM ISOTOPE SYSTEMATICS IN WARK-LOVERING RIMS SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 78th Annual Meeting of the Meteoritical-Society CY JUL 27-31, 2015 CL Berkeley, CA SP Meteorit Soc, Barringer Crater Co, Natl Aeronaut & Space Adm, Inst Space & Astronaut Sci, Japan Aerosp Explorat Agcy, Japan Polar Res Assoc, Natl Inst Polar Res, NASA Mars Program Off, Agilent Technologies, CAMECA, Lockheed Martin Space Syst Co, Natl Electrostat Corp, TESCAN, Int Meteorite Collectors Assoc, Planetary Studies Fdn, Lunar & Planetary Inst, Univ Calif, Space Sci Lab ID SOLAR NEBULA C1 [Needham, A. W.; Mishra, R. K.] Oak Ridge Associated Univ, Oak Ridge, TN 37831 USA. [Needham, A. W.; Messenger, S.; Keller, L. P.; Simon, J. I.; Han, J.; Mishra, R. K.; Marhas, K. K.] NASA, Lyndon B Johnson Space Ctr, Silver Spring, MD USA. [Han, J.; Marhas, K. K.] Lunar & Planetary Inst, Houston, TX USA. [Marhas, K. K.] Phys Res Lab, Ahmadabad 380009, Gujarat, India. EM andrew.w.needham@nasa.gov NR 5 TC 0 Z9 0 U1 2 U2 3 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD AUG PY 2015 VL 50 SU 1 SI SI MA 5014.pdf PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA CN7CR UT WOS:000358591900247 ER PT J AU Nguyen, AN Berger, EL Nakamura-Messenger, K Messenger, S AF Nguyen, A. N. Berger, E. L. Nakamura-Messenger, K. Messenger, S. TI SULFUR AND OXYGEN ISOTOPIC ANALYSIS OF A COSMIC SYMPLECTITE FROM A COMET WILD 2 STARDUST TERMINAL PARTICLE SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 78th Annual Meeting of the Meteoritical-Society CY JUL 27-31, 2015 CL Berkeley, CA SP Meteorit Soc, Barringer Crater Co, Natl Aeronaut & Space Adm, Inst Space & Astronaut Sci, Japan Aerosp Explorat Agcy, Japan Polar Res Assoc, Natl Inst Polar Res, NASA Mars Program Off, Agilent Technologies, CAMECA, Lockheed Martin Space Syst Co, Natl Electrostat Corp, TESCAN, Int Meteorite Collectors Assoc, Planetary Studies Fdn, Lunar & Planetary Inst, Univ Calif, Space Sci Lab ID CHONDRITES C1 [Nguyen, A. N.] NASA JSC, JETS, Houston, TX USA. [Nguyen, A. N.; Berger, E. L.; Nakamura-Messenger, K.; Messenger, S.] NASA JSC, ARES, Robert M Walker Lab Space Sci, Houston, TX USA. [Berger, E. L.] NASA JSC, JETS, GeoControl Syst, Houston, TX USA. EM lan-anh.n.nguyen@nasa.gov NR 16 TC 0 Z9 0 U1 2 U2 6 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD AUG PY 2015 VL 50 SU 1 SI SI MA 5375.pdf PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA CN7CR UT WOS:000358591900248 ER PT J AU Nguyen, AN Keller, LP Messenger, S Rahman, Z AF Nguyen, A. N. Keller, L. P. Messenger, S. Rahman, Z. TI IDENTIFICATION OF HIGHLY FRACTIONATED O-18-RICH SILICATE GRAINS IN THE QUEEN ALEXANDRA RANGE 99177 CR3 CHONDRITE SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 78th Annual Meeting of the Meteoritical-Society CY JUL 27-31, 2015 CL Berkeley, CA SP Meteorit Soc, Barringer Crater Co, Natl Aeronaut & Space Adm, Inst Space & Astronaut Sci, Japan Aerosp Explorat Agcy, Japan Polar Res Assoc, Natl Inst Polar Res, NASA Mars Program Off, Agilent Technologies, CAMECA, Lockheed Martin Space Syst Co, Natl Electrostat Corp, TESCAN, Int Meteorite Collectors Assoc, Planetary Studies Fdn, Lunar & Planetary Inst, Univ Calif, Space Sci Lab ID MET 00426 C1 [Nguyen, A. N.; Rahman, Z.] NASA JSC, JETS, Houston, TX USA. [Nguyen, A. N.; Keller, L. P.; Messenger, S.; Rahman, Z.] NASA JSC, ARES, Robert M Walker Lab Space Sci, Houston, TX USA. EM lan-anh.n.nguyen@nasa.gov NR 6 TC 0 Z9 0 U1 0 U2 0 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD AUG PY 2015 VL 50 SU 1 SI SI MA 5386.pdf PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA CN7CR UT WOS:000358591900249 ER PT J AU Nyquist, LE Park, J Nagao, K Haba, MK Mikouchi, T Kusakabe, M Shih, CY Herzog, GF AF Nyquist, L. E. Park, J. Nagao, K. Haba, M. K. Mikouchi, T. Kusakabe, M. Shih, C. -Y. Herzog, G. F. TI "NORMAL PLANETARY" Ne-Q IN CHELYABINSK AND MARS SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 78th Annual Meeting of the Meteoritical-Society CY JUL 27-31, 2015 CL Berkeley, CA SP Meteorit Soc, Barringer Crater Co, Natl Aeronaut & Space Adm, Inst Space & Astronaut Sci, Japan Aerosp Explorat Agcy, Japan Polar Res Assoc, Natl Inst Polar Res, NASA Mars Program Off, Agilent Technologies, CAMECA, Lockheed Martin Space Syst Co, Natl Electrostat Corp, TESCAN, Int Meteorite Collectors Assoc, Planetary Studies Fdn, Lunar & Planetary Inst, Univ Calif, Space Sci Lab ID NOBLE-GASES; CHONDRITES C1 [Nyquist, L. E.] XI NASA Johnson Space Ctr, Houston, TX 77058 USA. [Park, J.; Herzog, G. F.] Rutgers State Univ, Dept Chem & Chem Biol, Piscataway, NJ 08854 USA. [Park, J.] Kingsborough Community Coll, Brooklyn, NY 11235 USA. [Nagao, K.] Korea Polar Res Inst, Inchon 406840, South Korea. [Haba, M. K.] ETH, IGP, CH-8092 Zurich, Switzerland. [Mikouchi, T.] Univ Tokyo, Dept Earth & Planetary Sci, Grad Sch Sci, Tokyo 1130033, Japan. [Kusakabe, M.] Toyama Univ, Dept Environment Biol & Chem, Toyama 9308555, Japan. [Shih, C. -Y.] NASA JSC, Jacobs, Houston, TX 77058 USA. EM laurence.e.nyquist@nasa.gov NR 8 TC 0 Z9 0 U1 0 U2 0 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD AUG PY 2015 VL 50 SU 1 SI SI MA 5054.pdf PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA CN7CR UT WOS:000358591900254 ER PT J AU Ostrowski, D Sears, DWG Bryson, K Agrawal, P AF Ostrowski, D. Sears, D. W. G. Bryson, K. Agrawal, P. TI PHYSICAL PROPERTIES OF METEORITE FALLS IN RELATION TO PLANETARY DEFENSE SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 78th Annual Meeting of the Meteoritical-Society CY JUL 27-31, 2015 CL Berkeley, CA SP Meteorit Soc, Barringer Crater Co, Natl Aeronaut & Space Adm, Inst Space & Astronaut Sci, Japan Aerosp Explorat Agcy, Japan Polar Res Assoc, Natl Inst Polar Res, NASA Mars Program Off, Agilent Technologies, CAMECA, Lockheed Martin Space Syst Co, Natl Electrostat Corp, TESCAN, Int Meteorite Collectors Assoc, Planetary Studies Fdn, Lunar & Planetary Inst, Univ Calif, Space Sci Lab C1 [Ostrowski, D.; Sears, D. W. G.; Bryson, K.; Agrawal, P.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Ostrowski, D.; Sears, D. W. G.; Bryson, K.] NASA, Ames Res Ctr, Bay Area Environm Res Inst, Moffett Field, CA 94035 USA. [Agrawal, P.] NASA, Ames Res Ctr, ERC Inc, Moffett Field, CA 94035 USA. EM daniel.r.ostrowski@nasa.gov NR 8 TC 0 Z9 0 U1 1 U2 1 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD AUG PY 2015 VL 50 SU 1 SI SI MA 5363.pdf PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA CN7CR UT WOS:000358591900257 ER PT J AU Righter, K Satterwhite, C Schutt, J AF Righter, K. Satterwhite, C. Schutt, J. TI UPDATES ON PAIRING ISSUES WITH THE US ANTARCTIC METEORITE COLLECTION SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 78th Annual Meeting of the Meteoritical-Society CY JUL 27-31, 2015 CL Berkeley, CA SP Meteorit Soc, Barringer Crater Co, Natl Aeronaut & Space Adm, Inst Space & Astronaut Sci, Japan Aerosp Explorat Agcy, Japan Polar Res Assoc, Natl Inst Polar Res, NASA Mars Program Off, Agilent Technologies, CAMECA, Lockheed Martin Space Syst Co, Natl Electrostat Corp, TESCAN, Int Meteorite Collectors Assoc, Planetary Studies Fdn, Lunar & Planetary Inst, Univ Calif, Space Sci Lab ID CHONDRITES C1 [Righter, K.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Satterwhite, C.] NASA, Lyndon B Johnson Space Ctr, Jacobs, Houston, TX 77058 USA. [Schutt, J.] Case Western Reserve Univ, Dept Earth Environm Planet Sci, Cleveland, OH 44106 USA. EM Kevin.righter-1@nasa.gov NR 5 TC 0 Z9 0 U1 1 U2 1 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD AUG PY 2015 VL 50 SU 1 SI SI MA 5266.pdf PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA CN7CR UT WOS:000358591900276 ER PT J AU Righter, K Pando, KM Danielson, LR AF Righter, K. Pando, K. M. Danielson, L. R. TI THE COMBINED STRENGTH OF THERMODYNAMICS AND COMPARATIVE PLANETOLOGY: APPLICATION OF ACTIVITY MODELS TO CORE FORMATION IN TERRESTRIAL BODIES SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 78th Annual Meeting of the Meteoritical-Society CY JUL 27-31, 2015 CL Berkeley, CA SP Meteorit Soc, Barringer Crater Co, Natl Aeronaut & Space Adm, Inst Space & Astronaut Sci, Japan Aerosp Explorat Agcy, Japan Polar Res Assoc, Natl Inst Polar Res, NASA Mars Program Off, Agilent Technologies, CAMECA, Lockheed Martin Space Syst Co, Natl Electrostat Corp, TESCAN, Int Meteorite Collectors Assoc, Planetary Studies Fdn, Lunar & Planetary Inst, Univ Calif, Space Sci Lab ID ACCRETION C1 [Righter, K.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Pando, K. M.; Danielson, L. R.] NASA, Lyndon B Johnson Space Ctr, Jacobs Technol ESCG, Houston, TX 77058 USA. EM Kevin.righter-1@nasa.gov NR 6 TC 0 Z9 0 U1 0 U2 0 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD AUG PY 2015 VL 50 SU 1 SI SI MA 5277.pdf PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA CN7CR UT WOS:000358591900275 ER PT J AU Sandford, SA Nuevo, M Materese, CK Cooper, GW AF Sandford, S. A. Nuevo, M. Materese, C. K. Cooper, G. W. TI SEARCH FOR SUGARS AND RELATED COMPOUNDS IN RESIDUES PRODUCED FROM THE UV IRRADIATION OF ASTROPHYSICAL ICE ANALOGS. SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 78th Annual Meeting of the Meteoritical-Society CY JUL 27-31, 2015 CL Berkeley, CA SP Meteorit Soc, Barringer Crater Co, Natl Aeronaut & Space Adm, Inst Space & Astronaut Sci, Japan Aerosp Explorat Agcy, Japan Polar Res Assoc, Natl Inst Polar Res, NASA Mars Program Off, Agilent Technologies, CAMECA, Lockheed Martin Space Syst Co, Natl Electrostat Corp, TESCAN, Int Meteorite Collectors Assoc, Planetary Studies Fdn, Lunar & Planetary Inst, Univ Calif, Space Sci Lab ID AMINO-ACIDS; ULTRAVIOLET-IRRADIATION C1 [Sandford, S. A.; Nuevo, M.; Materese, C. K.; Cooper, G. W.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Nuevo, M.] BAER, Petaluma, CA USA. [Materese, C. K.] ORAU, Oak Ridge, TN USA. EM Scott.A.Sandford@nasa.gov NR 10 TC 0 Z9 0 U1 4 U2 4 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD AUG PY 2015 VL 50 SU 1 SI SI MA 5142.pdf PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA CN7CR UT WOS:000358591900289 ER PT J AU Sears, DWG Ebel, DS Wallace, S Friedrich, JM AF Sears, D. W. G. Ebel, D. S. Wallace, S. Friedrich, J. M. TI X-RAY COMPUTED TOMOGRAPHY AND THE RADIATION HISTORY OF METEORITES. SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 78th Annual Meeting of the Meteoritical-Society CY JUL 27-31, 2015 CL Berkeley, CA SP Meteorit Soc, Barringer Crater Co, Natl Aeronaut & Space Adm, Inst Space & Astronaut Sci, Japan Aerosp Explorat Agcy, Japan Polar Res Assoc, Natl Inst Polar Res, NASA Mars Program Off, Agilent Technologies, CAMECA, Lockheed Martin Space Syst Co, Natl Electrostat Corp, TESCAN, Int Meteorite Collectors Assoc, Planetary Studies Fdn, Lunar & Planetary Inst, Univ Calif, Space Sci Lab ID GEOSCIENCES; CT C1 [Sears, D. W. G.] NASA, Ames Res Ctr, BAER Inst, Mountain View, CA 95035 USA. [Ebel, D. S.; Wallace, S.; Friedrich, J. M.] Amer Museum Nat Hist, New York, NY 10024 USA. [Friedrich, J. M.] Fordham Univ, Dept Chem, New York, NY 10458 USA. EM Derek.Sears@NASA.gov NR 6 TC 0 Z9 0 U1 1 U2 1 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD AUG PY 2015 VL 50 SU 1 SI SI MA 5156.pdf PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA CN7CR UT WOS:000358591900297 ER PT J AU Smith, RL Blake, GA Boogert, ACA Pontoppidan, KM Lockwood, AC AF Smith, R. L. Blake, G. A. Boogert, A. C. A. Pontoppidan, K. M. Lockwood, A. C. TI INVESTIGATING PROTOPLANETARY CARBON RESERVOIRS AND MOLECULAR INHERITANCE ALONG A GALACTIC GRADIENT. SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 78th Annual Meeting of the Meteoritical-Society CY JUL 27-31, 2015 CL Berkeley, CA SP Meteorit Soc, Barringer Crater Co, Natl Aeronaut & Space Adm, Inst Space & Astronaut Sci, Japan Aerosp Explorat Agcy, Japan Polar Res Assoc, Natl Inst Polar Res, NASA Mars Program Off, Agilent Technologies, CAMECA, Lockheed Martin Space Syst Co, Natl Electrostat Corp, TESCAN, Int Meteorite Collectors Assoc, Planetary Studies Fdn, Lunar & Planetary Inst, Univ Calif, Space Sci Lab ID CO2 C1 [Smith, R. L.] NC Museum Nat Sci, Raleigh, NC USA. [Smith, R. L.] Appalachian State Univ, Boone, NC 28608 USA. [Blake, G. A.] CALTECH, Pasadena, CA 91125 USA. [Boogert, A. C. A.] NASA Ames, SOFIA USRA, Mountain View, CA USA. [Pontoppidan, K. M.] Space Telescope Sci Inst, Baltimore, MD USA. [Lockwood, A. C.] King Abdulaziz Univ Sci & Technol, Thuwal, Saudi Arabia. EM rachel.smith@naturalsciences.org NR 9 TC 0 Z9 0 U1 2 U2 3 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD AUG PY 2015 VL 50 SU 1 SI SI MA 5385.pdf PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA CN7CR UT WOS:000358591900305 ER PT J AU Zolensky, ME Fries, M Chan, QHS Kebukawa, Y Steele, A Bodnar, RJ AF Zolensky, M. E. Fries, M. Chan, Q. H-S Kebukawa, Y. Steele, A. Bodnar, R. J. TI THE MINERALOGY OF CERES* (*OR SOMETHING AN AWFUL LOT LIKE IT) SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 78th Annual Meeting of the Meteoritical-Society CY JUL 27-31, 2015 CL Berkeley, CA SP Meteorit Soc, Barringer Crater Co, Natl Aeronaut & Space Adm, Inst Space & Astronaut Sci, Japan Aerosp Explorat Agcy, Japan Polar Res Assoc, Natl Inst Polar Res, NASA Mars Program Off, Agilent Technologies, CAMECA, Lockheed Martin Space Syst Co, Natl Electrostat Corp, TESCAN, Int Meteorite Collectors Assoc, Planetary Studies Fdn, Lunar & Planetary Inst, Univ Calif, Space Sci Lab C1 [Zolensky, M. E.; Fries, M.; Chan, Q. H-S] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Kebukawa, Y.] Yokohama Natl Univ, Yokohama, Kanagawa 2408501, Japan. [Steele, A.] Carnegie Geophys Lab, Washington, DC 20015 USA. [Bodnar, R. J.] Virginia Tech, Blacksburg, VA 24061 USA. EM Michael.e.zolensky@nasa.gov NR 6 TC 0 Z9 0 U1 0 U2 0 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD AUG PY 2015 VL 50 SU 1 SI SI PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA CN7CR UT WOS:000358591900382 ER PT J AU Moore, TE Burch, JL Torbert, RB AF Moore, Thomas Earle Burch, James L. Torbert, Roy B. TI Magnetic reconnection SO NATURE PHYSICS LA English DT Editorial Material C1 [Moore, Thomas Earle] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Burch, James L.] SW Res Inst, San Antonio, TX 78238 USA. [Torbert, Roy B.] Univ New Hampshire, Durham, NH 03824 USA. RP Moore, TE (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM thomas.e.moore@nasa.gov RI NASA MMS, Science Team/J-5393-2013 OI NASA MMS, Science Team/0000-0002-9504-5214 FU NASA Magnetospheric MultiScale mission FX This work was supported by the NASA Magnetospheric MultiScale mission and its partners. NR 6 TC 0 Z9 0 U1 1 U2 5 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 1745-2473 EI 1745-2481 J9 NAT PHYS JI Nat. Phys. PD AUG PY 2015 VL 11 IS 8 BP 611 EP 613 PG 4 WC Physics, Multidisciplinary SC Physics GA CO0OQ UT WOS:000358851900004 ER PT J AU Ghimire, B Williams, CA Collatz, GJ Vanderhoof, M Rogan, J Kulakowski, D Masek, JG AF Ghimire, Bardan Williams, Christopher A. Collatz, G. James Vanderhoof, Melanie Rogan, John Kulakowski, Dominik Masek, Jeffrey G. TI Large carbon release legacy from bark beetle outbreaks across Western United States SO GLOBAL CHANGE BIOLOGY LA English DT Article DE bark beetle; biogeochemistry; carbon cycle; disturbances; forests ID MOUNTAIN PINE-BEETLE; LODGEPOLE PINE; CLIMATE-CHANGE; TREE MORTALITY; WOODY DEBRIS; BRITISH-COLUMBIA; FOREST INVENTORY; BOREAL FOREST; CANADA; FIRE AB Warmer conditions over the past two decades have contributed to rapid expansion of bark beetle outbreaks killing millions of trees over a large fraction of western United States (US) forests. These outbreaks reduce plant productivity by killing trees and transfer carbon from live to dead pools where carbon is slowly emitted to the atmosphere via heterotrophic respiration which subsequently feeds back to climate change. Recent studies have begun to examine the local impacts of bark beetle outbreaks in individual stands, but the full regional carbon consequences remain undocumented for the western US. In this study, we quantify the regional carbon impacts of the bark beetle outbreaks taking place in western US forests. The work relies on a combination of postdisturbance forest regrowth trajectories derived from forest inventory data and a process-based carbon cycle model tracking decomposition, as well as aerial detection survey (ADS) data documenting the regional extent and severity of recent outbreaks. We find that biomass killed by bark beetle attacks across beetle-affected areas in western US forests from 2000 to 2009 ranges from 5 to 15TgCyr(-1) and caused a reduction of net ecosystem productivity (NEP) of about 6.1-9.3TgCy(-1) by 2009. Uncertainties result largely from a lack of detailed surveys of the extent and severity of outbreaks, calling out a need for improved characterization across western US forests. The carbon flux legacy of 2000-2009 outbreaks will continue decades into the future (e.g., 2040-2060) as committed emissions from heterotrophic respiration of beetle-killed biomass are balanced by forest regrowth and accumulation. C1 [Ghimire, Bardan; Williams, Christopher A.; Vanderhoof, Melanie; Rogan, John; Kulakowski, Dominik] Clark Univ, Grad Sch Geog, Worcester, MA 01610 USA. [Ghimire, Bardan] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Div Earth Sci, Berkeley, CA 94720 USA. [Collatz, G. James; Masek, Jeffrey G.] NASA, Goddard Space Flight Ctr, Biospher Sci Lab, Greenbelt, MD 20771 USA. RP Ghimire, B (reprint author), Clark Univ, Grad Sch Geog, Worcester, MA 01610 USA. EM bghimire@lbl.gov RI Masek, Jeffrey/D-7673-2012; collatz, george/D-5381-2012 FU NASA Terrestrial Ecology program [NNX10AR68G]; NASA Earth and Space Science Fellowship (NESSF) [11-Earth11F-134, 12-Earth12R-59] FX B.G., C.A.W., G.J.C., and J.M. thank the NASA Terrestrial Ecology program for financial support under grant NNX10AR68G. Additionally, M.V. received financial support from the 2011-2013 NASA Earth and Space Science Fellowship (NESSF) (11-Earth11F-134 and 12-Earth12R-59). NR 67 TC 9 Z9 9 U1 16 U2 49 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1354-1013 EI 1365-2486 J9 GLOBAL CHANGE BIOL JI Glob. Change Biol. PD AUG PY 2015 VL 21 IS 8 BP 3087 EP 3101 DI 10.1111/gcb.12933 PG 15 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA CN5QU UT WOS:000358485200023 PM 25826244 ER PT J AU Huang, K Derada, S Xue, HJ Xiu, P Chai, F Xie, Q Wang, DX AF Huang, Ke Derada, Sergio Xue, Huijie Xiu, Peng Chai, Fei Xie, Qiang Wang, Dongxiao TI A 1/8A degrees coupled biochemical-physical Indian Ocean Regional Model: Physical results and validation SO OCEAN DYNAMICS LA English DT Article DE Monsoon; Seasonal and interannual variability; Indian Ocean; Arabian Sea; Surface and subsurface variability; Wave propagation ID GENERAL-CIRCULATION MODEL; DIMENSIONAL ECOSYSTEM MODEL; PACIFIC UPWELLING SYSTEM; SOUTH EQUATORIAL CURRENT; INDO-WESTERN PACIFIC; ARABIAN SEA; EL-NINO; INTERANNUAL VARIABILITY; SURFACE SALINITY; INDONESIAN SEAS AB A coupled physical-biochemical Indian Ocean Regional Model (IORM), based on the Navy Coastal Ocean Model (NCOM) and the Carbon Silicate Nitrogen Ecosystem (CoSiNE) model was configured with the primary objective of providing an accurate estimate of the oceanic physical state along with the biochemical processes simulated by CoSiNE to understand the variability in the Indian Ocean (IO). The model did not assimilate any data; instead, weak relaxation of temperature and salinity was implemented to keep the model stable in the long-term simulations. In this study, the skill of the IORM in simulating physical states in the IO was evaluated. Basin-scale surface circulation and cross-sectional transports were compared to observations, which demonstrated that the model replicated most of the observed features with reasonably good accuracy. Consistency and biases in the upper ocean temperature, salinity, and mixed layer depth were also analyzed. Lastly, the seasonality in the IO, its response to monsoonal forcing, and the evolution and dynamics of surface and subsurface dipole events were examined. The IORM reproduced most of the dynamic features including Ekman pumping, wave propagation, and climate variability at both annual and interannual time scales. The internal ocean dynamics and behavior of the modeled sea surface temperature anomaly (SSTA) suggest a coupled ocean/atmosphere instability that will require further research, including sensitivity experiments to realize improvements in model parameterization. C1 [Huang, Ke; Xue, Huijie; Xiu, Peng; Xie, Qiang; Wang, Dongxiao] Chinese Acad Sci, South China Sea Inst Oceanol, State Key Lab Trop Oceanog, Guangzhou, Guangdong, Peoples R China. [Huang, Ke] Grad Univ Chinese Acad Sci, Beijing, Peoples R China. [Derada, Sergio] Stennis Space Ctr, Naval Res Lab, Hancock, MS 39529 USA. [Xue, Huijie; Chai, Fei] Univ Maine, Sch Marine Sci, Orono, ME 04469 USA. [Xie, Qiang] Chinese Acad Sci, Sanya Inst Deep Sea Sci & Engn, Sanya, Hainan, Peoples R China. RP Xue, HJ (reprint author), Chinese Acad Sci, South China Sea Inst Oceanol, State Key Lab Trop Oceanog, Guangzhou, Guangdong, Peoples R China. EM hxue@maine.edu RI WANG, DongXiao/B-4445-2012 FU Strategic Priority Research Program of the Chinese Academy of Sciences [XDA11010304]; China Scholarship Counsel [201304910293]; Natural Science Foundation of China [41476012]; NASA [NNX07AK82G]; Australian Government through National Collaborative Research Infrastructure Strategy (NCRIS); Super Science Initiative (SSI) FX This study was supported by the Strategic Priority Research Program of the Chinese Academy of Sciences (Grant No. XDA11010304), the China Scholarship Counsel (No. 201304910293), and the Natural Science Foundation of China (41476012). The modeling work was supported by NASA grant number NNX07AK82G, and the model simulations were performed at the Navy DoD Supercomputing Resource Center, Stennis Space Center, Mississippi. The authors thank Dr. Feng Zhou and Dr. Yan Du for their suggestions and comments. Thanks also to the NOAA/OSCAR group for providing satellite-derived current data. The RAMA data were provided by the TAO Project Office at NOAA/PMEL. The altimeter products are produced by SSALTO/DUACS and distributed by AVISO. XBT data are sourced from the Integrated Marine Observing System (IMOS); IMOS is supported by the Australian Government through the National Collaborative Research Infrastructure Strategy (NCRIS) and the Super Science Initiative (SSI). The satellite-derived salinity data were obtained from the "Centre Aval de Traitement des Donnees SMOS" (CATDS), operated for the "Centre National d'Etudes Spatiales" (CNES, France) by IFREMER (Brest, France) NR 84 TC 2 Z9 2 U1 1 U2 17 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 AUG PY 2015 VL 65 IS 8 BP 1121 EP 1142 DI 10.1007/s10236-015-0860-8 PG 22 WC Oceanography SC Oceanography GA CN7HI UT WOS:000358604600006 ER PT J AU Mathis, JT Cooley, SR Lucey, N Colt, S Ekstrom, J Hurst, T Hauri, C Evans, W Cross, JN Feely, RA AF Mathis, J. T. Cooley, S. R. Lucey, N. Colt, S. Ekstrom, J. Hurst, T. Hauri, C. Evans, W. Cross, J. N. Feely, R. A. TI Ocean acidification risk assessment for Alaska's fishery sector SO PROGRESS IN OCEANOGRAPHY LA English DT Review ID NORTHEASTERN CHUKCHI SEA; NET COMMUNITY PRODUCTION; WESTERN ARCTIC-OCEAN; PRINCE-WILLIAM-SOUND; CORAL-REEF FISHERIES; CRAB HYAS-ARANEUS; EARLY-LIFE STAGES; CARBON-DIOXIDE; CLIMATE-CHANGE; BERING-SEA AB The highly productive fisheries of Alaska are located in seas projected to experience strong global change, including rapid transitions in temperature and ocean acidification-driven changes in pH and other chemical parameters. Many of the marine organisms that are most intensely affected by ocean acidification (OA) contribute substantially to the state's commercial fisheries and traditional subsistence way of life. Prior studies of OA's potential impacts on human communities have focused only on possible direct economic losses from specific scenarios of human dependence on commercial harvests and damages to marine species. However, other economic and social impacts, such as changes in food security or livelihoods, are also likely to result from climate change. This study evaluates patterns of dependence on marine resources within Alaska that could be negatively impacted by OA and current community characteristics to assess the potential risk to the fishery sector from OA. Here, we used a risk assessment framework based on one developed by the Intergovernmental Panel on Climate Change to analyze earth-system global ocean model hindcasts and projections of ocean chemistry, fisheries harvest data, and demographic information. The fisheries examined were: shellfish, salmon and other finfish. The final index incorporates all of these data to compare overall risk among Alaska's federally designated census areas. The analysis showed that regions in southeast and southwest Alaska that are highly reliant on fishery harvests and have relatively lower incomes and employment alternatives likely face the highest risk from OA. Although this study is an intermediate step toward our full understanding, the results presented here show that OA merits consideration in policy planning, as it may represent another challenge to Alaskan communities, some of which are already under acute socio-economic strains. Published by Elsevier Ltd. C1 [Mathis, J. T.; Evans, W.; Cross, J. N.; Feely, R. A.] NOAA, Pacific Marine Environm Lab, Seattle, WA 98115 USA. [Mathis, J. T.; Evans, W.; Cross, J. N.] Univ Alaska Fairbanks, Sch Fisheries & Ocean Sci, Ocean Acidificat Res Ctr, Fairbanks, AK 99709 USA. [Cooley, S. R.] Woods Hole Oceanog Inst, Dept Marine Chem & Geochem, Woods Hole, MA 02543 USA. [Lucey, N.] Marine Environm Res Ctr ENEA, I-19100 La Spezia, Italy. [Colt, S.] Univ Alaska Anchorage, Inst Social & Econ Res, Anchorage, AK 99508 USA. [Ekstrom, J.] Nat Resources Def Council, San Francisco, CA 94104 USA. [Hurst, T.] Hatfield Marine Sci Ctr, Alaska Fisheries Sci Ctr, Resource Assessment & Conservat Engn Div, Fisheries Behav Ecol Program, Newport, OR 97365 USA. [Hurst, T.] NOAA, Natl Marine Fisheries Serv, Hatfield Marine Sci Ctr, Newport, OR 97365 USA. [Hauri, C.] Univ Alaska Fairbanks, Sch Fisheries & Ocean Sci, Inst Marine Sci, Fairbanks, AK 99709 USA. RP Mathis, JT (reprint author), NOAA, Pacific Marine Environm Lab, 7600 Sand Point Way NE, Seattle, WA 98115 USA. EM jeremy.mathis@noaa.gov OI Cross, Jessica/0000-0002-6650-9905; Lucey, Noelle/0000-0002-7975-8521 FU U.S. Department of the Interior, Bureau of Ocean Energy Management, Environmental Studies Program [M11PG00034]; U.S. Department of Commerce; National Oceanic and Atmospheric Administration (NOAA); Office of Oceanic and Atmospheric Research (OAR); Pacific Marine Environmental Laboratory (PMEL); National Oceanic and Atmospheric Administration, Climate Program Office Grant [NA11OAR4310141]; Alaska Center for Climate Assessment and Policy at the University of Alaska, Fairbanks; NOAA's Ocean Acidification Research Program; National Science Foundation (ARC) [1107997]; Bureau of Ocean Energy Management through the University of Alaska Coastal Marine Institute [M08AX12760]; Alaska Ocean Observing System under NOAA [A08NOS4730406, NA11NOS0120020]; NOAA [NA08OAR4320751]; University of Alaska; National Science Foundation Grant [ATM-0628582]; Climate and Energy Decision Making (CEDM) Center; National Science Foundation [SES-0949710]; Energy Foundation Grant [G-0905-11200] FX This study is part of the Synthesis of Arctic Research (SOAR) and was funded in part by the U.S. Department of the Interior, Bureau of Ocean Energy Management, Environmental Studies Program through Interagency Agreement No. M11PG00034 with the U.S. Department of Commerce, National Oceanic and Atmospheric Administration (NOAA), Office of Oceanic and Atmospheric Research (OAR), Pacific Marine Environmental Laboratory (PMEL). The authors would like to acknowledge and thank all of our colleagues and collaborators who contributed to this synthesis effort, especially Robert Foy at NOAA, Jim Fall and Cathy Tide at ADF&G, John Guinotte at the Marine Conservation Biology Institute, and Gunnar Knapp at UAA. We greatly appreciate the graphical and GIS support provided by the Sarah Trainor and Piaa Kortsalo at the Alaska Center for Climate Assessment and Policy. The authors are very grateful to two anonymous reviewers whose comments markedly improved the paper. This research was partially supported by the National Oceanic and Atmospheric Administration, Climate Program Office Grant NA11OAR4310141 with the Alaska Center for Climate Assessment and Policy at the University of Alaska, Fairbanks, NOAA's Ocean Acidification Research Program, the National Science Foundation (ARC - 1107997 to JTM), the Bureau of Ocean Energy Management under cooperative agreement M08AX12760 through the University of Alaska Coastal Marine Institute, the Alaska Ocean Observing System under NOAA awards A08NOS4730406 and NA11NOS0120020. This publication is the result of research sponsored by the Cooperative Institute for Alaska Research with funds from NOAA under cooperative agreement NA08OAR4320751 with the University of Alaska. Cooley was supported by National Science Foundation Grant ATM-0628582, the Climate and Energy Decision Making (CEDM) Center that is supported under a cooperative agreement with the National Science Foundation (SES-0949710). Colt was supported by The Energy Foundation Grant G-0905-11200. The findings and conclusions in this paper are those of the authors and do not necessarily represent the views of the National Marine Fisheries Service. NR 139 TC 18 Z9 18 U1 17 U2 89 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0079-6611 J9 PROG OCEANOGR JI Prog. Oceanogr. PD AUG PY 2015 VL 136 SI SI BP 71 EP 91 DI 10.1016/j.pocean.2014.07.001 PG 21 WC Oceanography SC Oceanography GA CN7PQ UT WOS:000358626900006 ER PT J AU Donnellan, A Williams, C Pierce, M AF Donnellan, Andrea Williams, Charles Pierce, Marlon TI Multihazard Simulation and Cyberinfrastructure SO PURE AND APPLIED GEOPHYSICS LA English DT Editorial Material C1 [Donnellan, Andrea] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Donnellan, Andrea] Univ So Calif, ZHS, Los Angeles, CA 90089 USA. [Williams, Charles] GNS Sci, Lower Hutt 5040, New Zealand. [Pierce, Marlon] Indiana Univ, Bloomington, IN 47408 USA. RP Donnellan, A (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM andrea.donnellan@jpl.nasa.gov; c.williams@gns.cri.nz; marpierc@iu.edu OI Pierce, Marlon/0000-0002-9582-5712 FU National Aeronautics and Space Administration; National Science Foundation; United States Geological Survey FX We thank the contributors to this and previous topical volumes. We particularly thank the authors, reviewers and Birhauser personnel, without whom this volume would not have been possible. We thank John McRaney for tireless efforts bringing this all to fruition. We also thank our sponsors the National Aeronautics and Space Administration, the National Science Foundation, and the United States Geological Survey. Portions of this work were carried out at the Jet Propulsion Laboratory, California Institute of Technology under contract with the National Aeronautics and Space Administration. NR 5 TC 0 Z9 0 U1 0 U2 1 PU SPRINGER BASEL AG PI BASEL PA PICASSOPLATZ 4, BASEL, 4052, SWITZERLAND SN 0033-4553 EI 1420-9136 J9 PURE APPL GEOPHYS JI Pure Appl. Geophys. PD AUG PY 2015 VL 172 IS 8 SI SI BP 2083 EP 2085 DI 10.1007/s00024-015-1074-1 PG 3 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA CN4QJ UT WOS:000358414800001 ER PT J AU Yoder, MR Rundle, JB Glasscoe, MT AF Yoder, Mark R. Rundle, John B. Glasscoe, Margaret T. TI Near-Field ETAS Constraints and Applications to Seismic Hazard Assessment SO PURE AND APPLIED GEOPHYSICS LA English DT Article ID AFTERSHOCK SEQUENCE; PATTERN INFORMATICS; EARTHQUAKES; MODELS; LAW AB The epidemic type aftershock sequence (ETAS) statistical model of aftershock seismicity combines various earthquake scaling relations to produce synthetic earthquake catalogs, or estimates of aftershock seismicity rates, based on recent earthquake activity. One challenge to ETAS-based hazard assessment is the large number of free parameters involved. In this paper, we introduce an approach to constrain this parameter space from canonical scaling relations, empirical observations, and fundamental physics. We show that ETAS parameters can be estimated as a function of an earthquake's magnitude m based on the finite temporal and spatial extents of the rupture area. This approach facilitates fast ETAS-based estimates of seismicity from large "seed" catalogs, and it is particularly well suited to web-based deployment and otherwise automated implementations. It constitutes a significant improvement over contemporary ETAS by mitigating variability related to instrumentation and subjective catalog selection. C1 [Yoder, Mark R.; Rundle, John B.] Univ Calif Davis, Dept Geol, Davis, CA 95616 USA. [Rundle, John B.] Univ Calif Davis, Dept Geol, Davis, CA 95616 USA. [Rundle, John B.] Santa Fe Inst, Santa Fe, NM 87501 USA. [Glasscoe, Margaret T.] NASA, Jet Prop Lab, Pasadena, CA USA. RP Yoder, MR (reprint author), Univ Calif Davis, Dept Geol, Davis, CA 95616 USA. EM mryoder@ucdavis.edu FU JPL Subcontract [1291967]; NASA [NNX08AF69G] FX This work has been supported by JPL Subcontract 1291967, and NASA Grant NNX08AF69G. NR 37 TC 2 Z9 2 U1 0 U2 2 PU SPRINGER BASEL AG PI BASEL PA PICASSOPLATZ 4, BASEL, 4052, SWITZERLAND SN 0033-4553 EI 1420-9136 J9 PURE APPL GEOPHYS JI Pure Appl. Geophys. PD AUG PY 2015 VL 172 IS 8 SI SI BP 2277 EP 2293 DI 10.1007/s00024-014-0785-z PG 17 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA CN4QJ UT WOS:000358414800014 ER PT J AU Parker, J Donnellan, A Glasscoe, M Fox, G Wang, J Pierce, M Ma, Y AF Parker, Jay Donnellan, Andrea Glasscoe, Margaret Fox, Geoffrey Wang, Jun Pierce, Marlon Ma, Yu TI Advantages to Geoscience and Disaster Response from QuakeSim Implementation of Interferometric Radar Maps in a GIS Database System SO PURE AND APPLIED GEOPHYSICS LA English DT Article DE Radar interferometry; disaster response; earthquakes; geographic information systems (GIS) AB High-resolution maps of earth surface deformation are available in public archives for scientific interpretation, but are primarily available as bulky downloads on the internet. The NASA uninhabited aerial vehicle synthetic aperture radar (UAVSAR) archive of airborne radar interferograms delivers very high resolution images (approximately seven meter pixels) making remote handling of the files that much more pressing. Data exploration requiring data selection and exploratory analysis has been tedious. QuakeSim has implemented an archive of UAVSAR data in a web service and browser system based on GeoServer (http://geoserver.org). This supports a variety of services that supply consistent maps, raster image data and geographic information systems (GIS) objects including standard earthquake faults. Browsing the database is supported by initially displaying GIS-referenced thumbnail images of the radar displacement maps. Access is also provided to image metadata and links for full file downloads. One of the most widely used features is the QuakeSim line-of-sight profile tool, which calculates the radar-observed displacement (from an unwrapped interferogram product) along a line specified through a web browser. Displacement values along a profile are updated to a plot on the screen as the user interactively redefines the endpoints of the line and the sampling density. The profile and also a plot of the ground height are available as CSV (text) files for further examination, without any need to download the full radar file. Additional tools allow the user to select a polygon overlapping the radar displacement image, specify a downsampling rate and extract a modest sized grid of observations for display or for inversion, for example, the QuakeSim simplex inversion tool which estimates a consistent fault geometry and slip model. C1 [Parker, Jay; Donnellan, Andrea; Glasscoe, Margaret] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Fox, Geoffrey; Wang, Jun; Pierce, Marlon; Ma, Yu] Indiana Univ, Bloomington, IN 47408 USA. RP Parker, J (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM jay.w.parker@jpl.nasa.gov OI Pierce, Marlon/0000-0002-9582-5712 FU National Aeronautics and Space Administration FX 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 12 TC 0 Z9 0 U1 2 U2 13 PU SPRINGER BASEL AG PI BASEL PA PICASSOPLATZ 4, BASEL, 4052, SWITZERLAND SN 0033-4553 EI 1420-9136 J9 PURE APPL GEOPHYS JI Pure Appl. Geophys. PD AUG PY 2015 VL 172 IS 8 SI SI BP 2295 EP 2304 DI 10.1007/s00024-014-0886-8 PG 10 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA CN4QJ UT WOS:000358414800015 ER PT J AU Glasscoe, MT Wang, J Pierce, ME Yoder, MR Parker, JW Burl, MC Stough, TM Granat, RA Donnellan, A Rundle, JB Ma, Y Bawden, GW Yuen, K AF Glasscoe, Margaret T. Wang, Jun Pierce, Marlon E. Yoder, Mark R. Parker, Jay W. Burl, Michael C. Stough, Timothy M. Granat, Robert A. Donnellan, Andrea Rundle, John B. Ma, Yu Bawden, Gerald W. Yuen, Karen TI E-DECIDER: Using Earth Science Data and Modeling Tools to Develop Decision Support for Earthquake Disaster Response SO PURE AND APPLIED GEOPHYSICS LA English DT Article DE Decision support; earthquakes; disaster management; cyber-infrastructure ID AFTERSHOCK SEQUENCE; BATHS LAW; VALUES AB Earthquake Data Enhanced Cyber-Infrastructure for Disaster Evaluation and Response (E-DECIDER) is a NASA-funded project developing new capabilities for decision making utilizing remote sensing data and modeling software to provide decision support for earthquake disaster management and response. E-DECIDER incorporates the earthquake forecasting methodology and geophysical modeling tools developed through NASA's QuakeSim project. Remote sensing and geodetic data, in conjunction with modeling and forecasting tools allows us to provide both long-term planning information for disaster management decision makers as well as short-term information following earthquake events (i.e. identifying areas where the greatest deformation and damage has occurred and emergency services may need to be focused). This in turn is delivered through standards-compliant web services for desktop and hand-held devices. C1 [Glasscoe, Margaret T.; Parker, Jay W.; Burl, Michael C.; Stough, Timothy M.; Granat, Robert A.; Donnellan, Andrea; Yuen, Karen] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Wang, Jun; Pierce, Marlon E.; Ma, Yu] Indiana Univ, Bloomington, IN 47408 USA. [Yoder, Mark R.; Rundle, John B.] Univ Calif Davis, Davis, CA 95616 USA. [Bawden, Gerald W.] US Geol Survey, Sacramento, CA 95819 USA. RP Glasscoe, MT (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Margaret.T.Glasscoe@jpl.nasa.gov OI Pierce, Marlon/0000-0002-9582-5712 FU NASA FX We carried out this work at the Jet Propulsion Laboratory, California Institute of Technology, Indiana University, University of California's Davis campus, and the United States Geological Survey under NASA contracts. NASA's Applied Sciences and Advanced Information Systems Technology Programs sponsored the work. NR 49 TC 1 Z9 1 U1 1 U2 5 PU SPRINGER BASEL AG PI BASEL PA PICASSOPLATZ 4, BASEL, 4052, SWITZERLAND SN 0033-4553 EI 1420-9136 J9 PURE APPL GEOPHYS JI Pure Appl. Geophys. PD AUG PY 2015 VL 172 IS 8 SI SI BP 2305 EP 2324 DI 10.1007/s00024-014-0824-9 PG 20 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA CN4QJ UT WOS:000358414800016 ER PT J AU Wang, J Pierce, M Donnellan, A Parker, J AF Wang, Jun Pierce, Marlon Donnellan, Andrea Parker, Jay TI Web Services for Dynamic Coloring of UAVSAR Images SO PURE AND APPLIED GEOPHYSICS LA English DT Article DE Earthquakes; UAVSAR; Web service ID RADAR INTERFEROMETRY AB QuakeSim has implemented a service-based Geographic Information System to enable users to access large amounts of Uninhabited Aerial Vehicle Synthetic Aperture Radar (UAVSAR) data through an online interface. The QuakeSim Interferometric Synthetic Aperture Radar (InSAR) profile tool calculates radar-observed displacement (from an unwrapped interferogram product) along user-specified lines. Pre-rendered thumbnails with InSAR fringe patterns are used to display interferogram and unwrapped phase images on a Google Map in the InSAR profile tool. One challenge with this tool lies in the user visually identifying regions of interest when drawing the profile line. This requires that the user correctly interpret the InSAR imagery, which currently uses fringe patterns. The mapping between pixel color and pixel value is not a one-to-one relationship from the InSAR fringe pattern, and it causes difficulty in understanding general displacement information for QuakeSim users. The goal of this work is to generate color maps that directly reflect the pixel values (displacement) as an addition to the pre-rendered images. Because of an extremely uneven distribution of pixel values on an InSAR image, a histogram-based, nonlinear color template generation algorithm is currently under development. A web service enables on-the-fly coloring of UAVSAR images with dynamically generated color templates. C1 [Wang, Jun; Pierce, Marlon] Indiana Univ, Pervas Technol Inst, Bloomington, IN 47408 USA. [Donnellan, Andrea; Parker, Jay] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Wang, J (reprint author), Indiana Univ, Pervas Technol Inst, 2719 East 10th St, Bloomington, IN 47408 USA. EM wang208@indiana.edu OI Pierce, Marlon/0000-0002-9582-5712 FU NASA FX This work was carried out at the Jet Propulsion Laboratory, California Institute of Technology, Indiana University, University of Southern California, and University of California's Davis and Irvine campuses under contract with NASA. The work was sponsored by NASA's Advanced Information Technologies, Earth Surface and Interior, and Applied Sciences Programs. UAVSAR data and pre-rendered images courtesy NASA/JPL-Caltech. NR 16 TC 0 Z9 0 U1 1 U2 5 PU SPRINGER BASEL AG PI BASEL PA PICASSOPLATZ 4, BASEL, 4052, SWITZERLAND SN 0033-4553 EI 1420-9136 J9 PURE APPL GEOPHYS JI Pure Appl. Geophys. PD AUG PY 2015 VL 172 IS 8 SI SI BP 2325 EP 2332 DI 10.1007/s00024-014-0941-5 PG 8 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA CN4QJ UT WOS:000358414800017 ER PT J AU Hartl, DJ Mabe, JH Benafan, O Coda, A Conduit, B Padan, R Van Doren, B AF Hartl, D. J. Mabe, J. H. Benafan, O. Coda, A. Conduit, B. Padan, R. Van Doren, B. TI Standardization of shape memory alloy test methods toward certification of aerospace applications SO SMART MATERIALS AND STRUCTURES LA English DT Article DE shape memory alloy; characterization; standards; experiments; aerospace; actuators ID TRICKS; WIRE; TIPS AB The response of shape memory alloy (SMA) components employed as actuators has enabled a number of adaptable aero-structural solutions. However, there are currently no industry or government-accepted standardized test methods for SMA materials when used as actuators and their transition to commercialization and production has been hindered. This brief fast track communication introduces to the community a recently initiated collaborative and pre-competitive SMA specification and standardization effort that is expected to deliver the first ever regulatory agency-accepted material specification and test standards for SMA as employed as actuators for commercial and military aviation applications. In the first phase of this effort, described herein, the team is working to review past efforts and deliver a set of agreed-upon properties to be included in future material certification specifications as well as the associated experiments needed to obtain them in a consistent manner. Essential for the success of this project is the participation and input from a number of organizations and individuals, including engineers and designers working in materials and processing development, application design, SMA component fabrication, and testing at the material, component, and system level. Going forward, strong consensus among this diverse body of participants and the SMA research community at large is needed to advance standardization concepts for universal adoption by the greater aerospace community and especially regulatory bodies. It is expected that the development and release of public standards will be done in collaboration with an established standards development organization. C1 [Hartl, D. J.] Texas A&M Engn Expt Stn, Aerosp Vehicle Syst Inst, College Stn, TX 77843 USA. [Mabe, J. H.] Boeing Co, Seattle, WA 98124 USA. [Benafan, O.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. [Coda, A.] SAES Getters SpA, I-20020 Lainate, MI, Italy. [Conduit, B.] Rolls Royce PLC, Derby DE24 8BJ, England. [Padan, R.] Rafael Adv Def Syst Ltd, IL-3102102 Haifa, Israel. [Van Doren, B.] ATI Specialty Alloys & Components, Albany, OR 97321 USA. RP Hartl, DJ (reprint author), Texas A&M Engn Expt Stn, Aerosp Vehicle Syst Inst, College Stn, TX 77843 USA. EM darren.hartl@tamu.edu NR 25 TC 0 Z9 0 U1 2 U2 8 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0964-1726 EI 1361-665X J9 SMART MATER STRUCT JI Smart Mater. Struct. PD AUG PY 2015 VL 24 IS 8 AR 082001 DI 10.1088/0964-1726/24/8/082001 PG 6 WC Instruments & Instrumentation; Materials Science, Multidisciplinary SC Instruments & Instrumentation; Materials Science GA CN8JH UT WOS:000358686000001 ER PT J AU Howard, AM Nibbelink, NP Madden, M Young, LA Bernardes, S Fragaszy, DM AF Howard, Allison M. Nibbelink, Nathan P. Madden, Marguerite Young, Leigh Anna Bernardes, Sergio Fragaszy, Dorothy M. TI Landscape influences on the natural and artificially manipulated movements of bearded capuchin monkeys SO ANIMAL BEHAVIOUR LA English DT Article DE animal movement; capuchin monkey; efficiency; Euclidean cognitive map; field experiment; Sapajus libidinosus; spatial cognition; spatial decision making ID CHACMA BABOONS; PAPIO-URSINUS; TRAVEL ROUTES; MAPS; RESOURCES; REFLECT; ANIMALS; FOREST; MODELS; SPIDER AB Cognitive mechanisms underlying the choice of movement patterns between resource sites for nonhuman primates are not well understood. Specifically, the influence of landscape features on decision making and spatial memory of naturally ranging animals has not been explicitly investigated. We evaluated three models of bearded capuchin monkey, Sapajus libidinosus, movement decisions that incorporated varying degrees of landscape and memory influences, and we conducted a field experiment using a novel call-back technique to test these influences. The movements and spatial decisions of the monkeys were modelled between temporal stop points and spatial change points during natural travel using straight-line path, a minimum-resistance path and landscape-perceiving path models. For these movement models, resistance was calculated as the inverse of habitat suitability, a surface based on the natural movement patterns of the study group. Of the three models, natural travel most closely resembled the straight-line path model in its landscape resistance, but not in its geometry. This result indicates that while the monkeys travel in zones of low resistance, they do not minimize distance or landscape resistance between travel nodes. When monkeys were called to an artificial resource site using the call-back experiment, their travel was more linear and higher in landscape resistance. The limited quantity and high quality of the food resource in the artificial resource sites may have influenced the nature of the monkeys' travel in these experiments. We present the advantages and challenges of the call-back method of experimental analysis of animal movement and we conclude that future analyses of spatial cognition should include consideration of landscape context. (C) 2015 The Association for the Study of Animal Behaviour. Published by Elsevier Ltd. All rights reserved. C1 [Howard, Allison M.] Univ Maryland, Dept Biol, College Pk, MD 20770 USA. [Nibbelink, Nathan P.] Univ Georgia, Warnell Sch Forestry & Nat Resources, Athens, GA 30602 USA. [Howard, Allison M.; Madden, Marguerite; Bernardes, Sergio] Univ Georgia, Ctr Geospatial Res, Athens, GA 30602 USA. [Young, Leigh Anna] Emory Univ, Yerkes Natl Primate Res Ctr, Atlanta, GA 30322 USA. [Bernardes, Sergio] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Fragaszy, Dorothy M.] Univ Georgia, Dept Psychol, Athens, GA 30602 USA. RP Howard, AM (reprint author), Univ Maryland, Dept Biol, College Pk, MD 20770 USA. EM amhoward@umd.edu OI Howard, Allison/0000-0002-0997-8588 FU American Society of Primatologists Small Research Grant FX We thank two anonymous referees for their comments and suggestions that greatly improved the quality of this paper. This work was funded by the American Society of Primatologists Small Research Grant. High-resolution satellite imagery was provided through the Intergraph (R) - DigitalGlobe Geospatial Challenge. We thank Yonat Eschar and Natalie Schwob for their assistance in conducting the field experiments and Caroline Jones for her assistance in collecting data on the spatial accuracy of the tablet computers at our field site. We also thank Marino Gomes de Oliveira's family for allowing us to conduct our research at Fazenda Boa Vista and for their assistance in data collection in the field. NR 32 TC 0 Z9 0 U1 6 U2 18 PU ACADEMIC PRESS LTD- ELSEVIER SCIENCE LTD PI LONDON PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND SN 0003-3472 EI 1095-8282 J9 ANIM BEHAV JI Anim. Behav. PD AUG PY 2015 VL 106 BP 59 EP 70 DI 10.1016/j.anbehav.2015.05.003 PG 12 WC Behavioral Sciences; Zoology SC Behavioral Sciences; Zoology GA CN3HG UT WOS:000358315700010 ER PT J AU Potter, C AF Potter, Christopher TI Vegetation cover change in the Upper Kings River basin of the Sierra Nevada detected using Landsat satellite image analysis SO CLIMATIC CHANGE LA English DT Article ID POSTFIRE VEGETATION; CLIMATE VARIABILITY; FOREST; CALIFORNIA; FIRE; TM; CALIBRATION; SEVERITY; RECOVERY; WILDFIRE AB The Sierra Nevada of California is a region where large forest fires have been suppressed for over a century and future climate warming has the potential to alter vegetation cover and surface water runoff. A detailed geographic record of recent changes in vegetation cover across the Sierra Nevada remains a gap that can be filled with satellite remote sensing data. Results from Landsat image analysis over the past 25 years in the Upper Kings River basin showed that consistent increases in the normalized difference vegetation index (NDVI) have not extended above 2000 m elevation. Moreover, mean increases in NDVI since 1986 at elevations below 2000 m (which cover about half of the total basin area) have not exceeded 9 %, even in the most extreme precipitation yearly comparisons. NDVI has decreased significantly at elevations above 2000 m throughout the basin in relatively wet year comparisons since the mid-1980s. These findings conflict with any assumptions that evapotranspiration fluxes impacting river flows downstream have been altered mainly by vegetation change over most of the Upper Kings River basin in recent decades. C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Potter, C (reprint author), NASA, Ames Res Ctr, Mail Stop 232-21, Moffett Field, CA 94035 USA. EM chris.potter@nasa.gov NR 33 TC 1 Z9 1 U1 8 U2 35 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 AUG PY 2015 VL 131 IS 4 BP 635 EP 647 DI 10.1007/s10584-015-1397-z PG 13 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA CN1KR UT WOS:000358179400013 ER PT J AU Anderson, RC Beegle, LW Hurowitz, J Hanson, C Abbey, W Seybold, C Liminodi, D Kuhn, S Jandura, L Brown, K Peters, G Roumeliotis, C Robinson, M Edgett, K Minitti, M Grotzinger, J AF Anderson, R. C. Beegle, L. W. Hurowitz, J. Hanson, C. Abbey, W. Seybold, C. Liminodi, D. Kuhn, S. Jandura, L. Brown, K. Peters, G. Roumeliotis, C. Robinson, M. Edgett, K. Minitti, M. Grotzinger, J. TI The Mars Science Laboratory scooping campaign at Rocknest SO ICARUS LA English DT Article DE Mars; Regolith; Instrumentation ID X-RAY SPECTROMETER; MARTIAN ATMOSPHERE; MERIDIANI-PLANUM; CHEMISTRY; PATHFINDER; SAMPLES; IMAGER; CRATER; ROCKS; SOILS AB During its 57th through 100th martian days (sols) in Gale Crater, the Mars Science Laboratory (MSL) Curiosity rover performed its first sample acquisition and processing of solid, granular sample. Samples were extracted from an aeolian sand deposit at a location called Rocknest. The Rocknest sampling site was identified to fit the prelaunch scientific and engineering requirements for this first time activity. Collected material was processed and delivered to two analytical instruments, Chemistry and Mineralogy (CheMin) and Sample Analysis at Mars (SAM), that both require delivery of a specific particle size range so that they can perform analyses to determine sample mineralogy and geochemistry. The choice of an aeolian sand deposit was based on requirements to ingest non-lithified, particulate sample for decontamination of the Sample Acquisition/Sample Processing and Handling (SA/SPaH) hardware, as well as to provide an opportunity to compare analytical results to aeolian deposits from elsewhere on the martian surface. (C) 2015 Elsevier Inc. All rights reserved. C1 [Anderson, R. C.; Beegle, L. W.; Hanson, C.; Abbey, W.; Seybold, C.; Liminodi, D.; Kuhn, S.; Jandura, L.; Brown, K.; Peters, G.; Roumeliotis, C.; Robinson, M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Hurowitz, J.] SUNY Stony Brook, Stony Brook, NY 11794 USA. [Edgett, K.] Malin Space Sci Syst, San Diego, CA 92191 USA. [Minitti, M.] Planetary Sci Inst, Tucson, AZ 85719 USA. [Grotzinger, J.] CALTECH, Pasadena, CA 91125 USA. RP Anderson, RC (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. OI Edgett, Kenneth/0000-0001-7197-5751 NR 31 TC 1 Z9 1 U1 1 U2 11 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD AUG PY 2015 VL 256 BP 66 EP 77 DI 10.1016/j.icarus.2015.03.033 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CM0IW UT WOS:000357362600008 ER PT J AU Salmon, M Higgins, B Stewart, J Wyneken, J AF Salmon, Michael Higgins, Benjamin Stewart, Joshua Wyneken, Jeanette TI The ontogeny of morphological defenses in Kemp's ridley (Lepidochelys kempii) and loggerhead (Caretta caretta) sea turtles SO JOURNAL OF MORPHOLOGY LA English DT Article DE morphological defenses; antipredator adaptations; ontogenetic variation; allometric growth; marine turtles ID SKELETAL GROWTH MARKS; HABITAT SHIFTS; CHELONIA-MYDAS; GREEN; HATCHLINGS; LARVAE; MODEL AB Marine turtles are large reptiles that compensate for high juvenile mortality by producing hundreds of hatchlings during a long reproductive lifespan. Most hatchlings are taken by predators during their migration to, and while resident in, the open ocean. Their survival depends upon crypticity, minimizing movement to avoid detection, and foraging efficiently to grow to a size too difficult for predators to either handle or swallow. While these behavioral antipredator tactics are known, changes in morphology accompanying growth may also improve survival prospects. These have been only superficially described in the literature. Here, we compare the similarities and differences in presumed morphological defenses of growing loggerhead (Caretta caretta) and Kemp's ridley (Lepidochelys kempii) posthatchlings, related species that differ in growth rate, timing of habitat shift (the return from oceanic to neritic locations), and size at maturity. In both species, vertebral spination and carapace widening increase disproportionally as small turtles grow, but later in ontogeny, the spines regress, sooner in ridley than in loggerhead turtles. Carapace widening occurs in both species but loggerheads are always longer than they are wide whereas in Kemp's ridley turtles, the carapace becomes as wide as long. Our analysis indicates that these changes are unrelated to when each species shifts habitat but are related to turtle size. We hypothesize that the spines function in small turtles as an early defense against gape-limited predators, but changes in body shape function throughout ontogenyinitially to make small turtles too wide to swallow and later by presenting an almost flat and hardened surface that large predators (such as a sharks) are unable to grasp. The extremely wide carapace of the Kemp's ridley may compensate for its smaller adult size (and presumed greater vulnerability) than the loggerhead. J. Morphol. 276:929-940, 2015. (c) 2015 Wiley Periodicals, Inc. C1 [Salmon, Michael; Wyneken, Jeanette] Florida Atlantic Univ, Dept Biol Sci, Boca Raton, FL 33431 USA. [Higgins, Benjamin; Stewart, Joshua] NOAA, Natl Marine Fisheries Serv, Southeast Fisheries Sci Ctr, Galveston, TX 77551 USA. RP Salmon, M (reprint author), Florida Atlantic Univ, Dept Biol Sci, 777 Glades Rd, Boca Raton, FL 33431 USA. EM salmon@fau.edu FU Save Our Seas Foundation; Disney World Wide Conservation Fund; AWC Foundation; National Save-the-Sea-Turtle Foundation; Nelligan Sea Turtle Fund; Lugger Family Foundation FX Contract grant sponsors: Save Our Seas Foundation, Disney World Wide Conservation Fund, AWC Foundation, National Save-the-Sea-Turtle Foundation, Nelligan Sea Turtle Fund, and Lugger Family Foundation. NR 51 TC 1 Z9 3 U1 4 U2 33 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0362-2525 EI 1097-4687 J9 J MORPHOL JI J. Morphol. PD AUG PY 2015 VL 276 IS 8 BP 929 EP 940 DI 10.1002/jmor.20390 PG 12 WC Anatomy & Morphology SC Anatomy & Morphology GA CN4AX UT WOS:000358371700005 PM 26126953 ER PT J AU Asrar, FM Asrar, S Clark, JB Kendall, DJW Ngo-Anh, TJ Brazeau, S Hulsroj, P Williams, RS AF Asrar, Farhan M. Asrar, Suhail Clark, Jonathan B. Kendall, David J. W. Thu Jennifer Ngo-Anh Brazeau, Stephanie Hulsroj, Peter Williams, Richard S. TI Help from above: outer space and the fight against Ebola SO LANCET INFECTIOUS DISEASES LA English DT Editorial Material C1 [Asrar, Farhan M.] Univ Toronto, Hlth & Counselling Ctr, Mississauga, ON L5L 1C6, Canada. [Asrar, Farhan M.] McMaster Univ, Fac Hlth Sci, Dept Family Med, Hamilton, ON, Canada. [Asrar, Farhan M.] Int Space Univ, Strasbourg, France. [Asrar, Suhail] Univ Toronto, Toronto, ON, Canada. [Clark, Jonathan B.] Baylor Coll Med, Dept Neurol, Ctr Space Med, Houston, TX 77030 USA. [Kendall, David J. W.] United Nations, Comm Peaceful Uses Outer Space, Vienna, Austria. [Kendall, David J. W.] John H Chapman Space Ctr, Canadian Space Agcy, St Hubert, PQ, Canada. [Thu Jennifer Ngo-Anh] European Space Agcy, Head Human Res Unit, Directorate Human Spaceflight & Operat, NL-2200 AG Noordwijk, Netherlands. [Brazeau, Stephanie] Publ Hlth Agcy Canada, Infect Dis Prevent & Control Branch, St Hyacinthe, PQ, Canada. [Hulsroj, Peter] European Space Policy Inst, Vienna, Austria. [Williams, Richard S.] Natl Aeronaut & Space Adm, Washington, DC USA. RP Asrar, FM (reprint author), Univ Toronto, Hlth & Counselling Ctr, Mississauga, ON L5L 1C6, Canada. EM farhan.asrar@utoronto.ca NR 5 TC 2 Z9 2 U1 0 U2 5 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 1473-3099 EI 1474-4457 J9 LANCET INFECT DIS JI Lancet Infect. Dis. PD AUG PY 2015 VL 15 IS 8 BP 873 EP 875 PG 4 WC Infectious Diseases SC Infectious Diseases GA CN1LW UT WOS:000358182500009 PM 26227751 ER PT J AU Roa, J Sanjurjo-Rivo, M Pelaez, J AF Roa, Javier Sanjurjo-Rivo, Manuel Pelaez, Jesus TI Singularities in Dromo formulation. Analysis of deep flybys SO ADVANCES IN SPACE RESEARCH LA English DT Article DE Numerical methods; Orbit propagation; Flyby trajectories; Dromo ID 3-BODY PROBLEM; KEPLER MOTION; IDEAL FRAMES; REGULARIZATION; COMPUTATION AB The singularities in Dromo are characterized in this paper, both from an analytical and a numerical perspective. When the angular momentum vanishes, Dromo may encounter a singularity in the evolution equations. The cancellation of the angular momentum occurs in very specific situations and may be caused by the action of strong perturbations. The gravitational attraction of a perturbing planet may lead to rapid changes in the angular momentum of the particle. In practice, this situation may be encountered during deep planetocentric flybys. The performance of Dromo is evaluated in different scenarios. First, Dromo is validated for integrating the orbit of Near Earth Asteroids. Resulting errors are of the order of the diameter of the asteroid. Second, a set of theoretical flybys are designed for analyzing the performance of the formulation in the vicinity of the singularity. New sets of Dromo variables are proposed in order to minimize the dependency of Dromo on the angular momentum. A slower time scale is introduced, leading to a more stable description of the flyby phase. Improvements in the overall performance of the algorithm are observed when integrating orbits close to the singularity. (C) 2015 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 [Roa, Javier; Pelaez, Jesus] Tech Univ, Space Dynam Grp, E-28040 Madrid, Spain. [Sanjurjo-Rivo, Manuel] Univ Carlos III Madrid, Bioengn & Aerosp Engn Dept, E-28911 Madrid, Spain. RP Roa, J (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM javier.roa@upm.es RI Pelaez, Jesus/M-7806-2016 OI Pelaez, Jesus/0000-0001-9755-1674 FU Spanish Ministry of Economy and Competitiveness [ESP2013-41634-P]; Spanish Government; La Caixa FX This work was carried out within the framework of the research project entitled Dynamic Simulation of Space Complex Systems (ESP2013-41634-P) supported by the Spanish Ministry of Economy and Competitiveness. Authors thank Spanish Government for its support, and H. Urrutxua for his help with the numerical integration. J. Roa especially thanks "La Caixa" for his doctoral fellowship. NR 39 TC 5 Z9 5 U1 0 U2 1 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0273-1177 EI 1879-1948 J9 ADV SPACE RES JI Adv. Space Res. PD AUG 1 PY 2015 VL 56 IS 3 BP 569 EP 581 DI 10.1016/j.asr.2015.03.019 PG 13 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA CM7VS UT WOS:000357905200018 ER PT J AU Andreopoulou, A Begault, DR Katz, BFG AF Andreopoulou, Areti Begault, Durand R. Katz, Brian F. G. TI Inter-Laboratory Round Robin HRTF Measurement Comparison SO IEEE JOURNAL OF SELECTED TOPICS IN SIGNAL PROCESSING LA English DT Article DE HRTF/HRIR; ITD variations; measurement; repeatability; spatial symmetry; spectral variations ID IMPULSE RESPONSES; MODEL AB Head-Related Transfer Function (HRTF) measurements underlie the signal processing used in binaural auditory displays, but measurement techniques, equipment, and post-processing vary substantially between laboratories. This variation can result in significant differences in measured spectral and timing data taken from the same subject for the same sound source locations. An ongoing project for comparing databases from laboratories across the world (colloquially titled "Club Fritz") employs a single dummy head microphone for measurements (Neumann KU-100) at various sites. The current study examines magnitude and timing differences between left and right ear data from 12 different HRTF sets taken from 10 different laboratories. Results revealed spectral magnitude variations up to 12.5 dB for frequency bands below 6 kHz and up to 23 dB above that, as well as large spectral left/right asymmetries for (d(corr) <= 0.4) for high-frequency content. Further subjective studies are necessary to determine the perceptual relevance of these findings. Nevertheless, the observed ITD variations of up to 235 mu sec are alarming as they often exceeded reported JND values. Such findings highlight the potential impact of physical spaces, measurement routines, and equipment types on the collected HRTF data. C1 [Andreopoulou, Areti; Katz, Brian F. G.] CNRS, LIMSI, Audio Acoust Grp, F-91400 Orsay, France. [Begault, Durand R.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Andreopoulou, A (reprint author), CNRS, LIMSI, Audio Acoust Grp, F-91400 Orsay, France. EM andreopoulou@limsi.fr OI Andreopoulou, Areti/0000-0003-0287-0459 FU French project BiLi ("Binaural Listening") [FUI-AAP14]; Space Human Factors Engineering Project of NASA's Human Research Program FX This work was supported in part by the French project BiLi ("Binaural Listening," www.bili-project.org, FUI-AAP14). Additional support was provided by the Space Human Factors Engineering Project of NASA's Human Research Program. The guest editor coordinating the review of this manuscript and approving it for publication was Prof. Akio Ando. NR 29 TC 3 Z9 3 U1 1 U2 4 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1932-4553 EI 1941-0484 J9 IEEE J-STSP JI IEEE J. Sel. Top. Signal Process. PD AUG PY 2015 VL 9 IS 5 BP 895 EP 906 DI 10.1109/JSTSP.2015.2400417 PG 12 WC Engineering, Electrical & Electronic SC Engineering GA CM8EW UT WOS:000357932100012 ER PT J AU Magar, KT Balas, MJ Frost, S AF Magar, Kaman Thapa Balas, Mark J. Frost, Susan TI Direct adaptive control for individual blade pitch control of wind turbines for load reduction SO JOURNAL OF INTELLIGENT MATERIAL SYSTEMS AND STRUCTURES LA English DT Article DE Adaptive control; individual blade pitch control; wind energy; load reduction AB In this article, a theory of adaptive disturbance rejection control is used to design an individual blade pitch controller to reduce the loading in a utility-scale wind turbine. The goal of the adaptive disturbance rejection control is to regulate the blade pitch angle individually to reduce the asymmetrical loading in blade due to vertical wind shear and also to reject the unnecessary disturbance introduced by the wind turbulence. The applicability of the theory is illustrated by implementing the controller in the National Renewable Energy Laboratory's 5-MW nonlinear, high-fidelity wind turbine model and simulating it in MATLAB/Simulink. C1 [Magar, Kaman Thapa; Balas, Mark J.] Embry Riddle Aeronaut Univ, Dept Aerosp Engn, Daytona Beach, FL 32114 USA. [Frost, Susan] NASA Ames Res Ctr, Moffett Field, CA USA. RP Magar, KT (reprint author), Embry Riddle Aeronaut Univ, Dept Aerosp Engn, Daytona Beach, FL 32114 USA. EM kamanmagar@hotmail.com NR 9 TC 1 Z9 1 U1 1 U2 9 PU SAGE PUBLICATIONS LTD PI LONDON PA 1 OLIVERS YARD, 55 CITY ROAD, LONDON EC1Y 1SP, ENGLAND SN 1045-389X EI 1530-8138 J9 J INTEL MAT SYST STR JI J. Intell. Mater. Syst. Struct. PD AUG PY 2015 VL 26 IS 12 BP 1564 EP 1572 DI 10.1177/1045389X14566527 PG 9 WC Materials Science, Multidisciplinary SC Materials Science GA CN0CS UT WOS:000358080700009 ER PT J AU Airey, MW Mather, TA Pyle, DM Glaze, LS Ghail, RC Wilson, CF AF Airey, M. W. Mather, T. A. Pyle, D. M. Glaze, L. S. Ghail, R. C. Wilson, C. F. TI Explosive volcanic activity on Venus: The roles of volatile contribution, degassing, and external environment SO PLANETARY AND SPACE SCIENCE LA English DT Article DE Venus; Planetary volcanism; Volcano modelling; Conduit processes ID STEEP-SIDED DOMES; MOUNT-ST-HELENS; ERUPTION COLUMNS; MAGMA FRAGMENTATION; MAGELLAN DATA; DYNAMICS; CONDUIT; MODEL; EVOLUTION; WATER AB We investigate the conditions that will promote explosive volcanic activity on Venus. Conduit processes were simulated using a steady-state, isothermal, homogeneous flow model in tandem with a degassing model. The response of exit pressure, exit velocity, and degree of volatile exsolution was explored over a range of volatile concentrations (H2O and CO2), magma temperatures, vent altitudes, and conduit geometries relevant to the Venusian environment. We find that the addition of CO2 to an H2O-driven eruption increases the final pressure, velocity, and volume fraction gas. Increasing vent elevation leads to a greater degree of magma fragmentation, due to the decrease in the final pressure at the vent, resulting in a greater likelihood of explosive activity. Increasing the magmatic temperature generates higher final pressures, greater velocities, and lower final volume fraction gas values with a correspondingly lower chance of explosive volcanism. Cross-sectionally smaller, and/or deeper, conduits were more conducive to explosive activity. Model runs show that for an explosive eruption to occur at Scathach Fluctus, at Venus' mean planetary radius (MPR), 4.5% H2O or 3% H2O with 3% CO2 (from a 25 m radius conduit) would be required to initiate fragmentation; at Ma'at Mons (similar to 9 km above MPR) only 2% H2O is required. A buoyant plume model was used to investigate plume behaviour. It was found that it was not possible to achieve a buoyant column from a 25 m radius conduit at Scathach Fluctus, but a buoyant column reaching up to similar to 20 km above the vent could be generated at Ma'at Mons with an H2O concentration of 4.7% (at 1300 K) or a mixed volatile concentration of 3% H2O with 3% CO2 (at 1200 K). We also estimate the flux of volcanic gases to the lower atmosphere of Venus, should explosive volcanism occur. Model results suggest explosive activity at Scathach Fluctus would result in an H2O flux of similar to 10(7) kg s(-1). Were Scathach Fluctus emplaced in a single event, our model suggests that it may have been emplaced in a period of similar to 15 days, supplying 1-2 x 10(4) Mt H2O to the atmosphere locally. An eruption of this scale might increase local atmospheric H2O abundance by several ppm over an area large enough to be detectable by near-infrared nightside sounding using the 1.18 mu m spectral window such as that carried out by the Venus Express/VIRTIS spectrometer. Further interrogation of the VIRTIS dataset is recommended to search for ongoing volcanism on Venus. (C) 2015 The Authors. Published by Elsevier Ltd. C1 [Airey, M. W.; Mather, T. A.; Pyle, D. M.] Univ Oxford, Dept Earth Sci, Oxford OX1 3PR, England. [Glaze, L. S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Ghail, R. C.] Univ London Imperial Coll Sci Technol & Med, Dept Civil & Environm Engn, London, England. [Wilson, C. F.] Univ Oxford, Clarendon Lab, Atmospher Ocean & Planetary Phys, Oxford OX1 3PU, England. RP Airey, MW (reprint author), Univ Oxford, Dept Earth Sci, S Parks Rd, Oxford OX1 3PR, England. EM martin.airey@earth.ox.ac.uk RI Mather, Tamsin/A-7604-2011; Pyle, David/C-5707-2009; Ghail, Richard/G-9455-2013; Glaze, Lori/D-1314-2012 OI Mather, Tamsin/0000-0003-4259-7303; Pyle, David/0000-0002-2663-9940; Ghail, Richard/0000-0002-4918-0685; FU Science and Technology Facilities Council; STFC [ST/I505880/1]; European Union [606798] FX M. Airey would like to thank the staff and his colleagues at the Department of Earth Sciences, University of Oxford for academic support, two anonymous reviewers whose comments improved the final manuscript, and the Science and Technology Facilities Council for funding the postgraduate research project, of which this paper forms a part. (STFC grant number ST/I505880/1) C. Wilson acknowledges funding from the European Union Seventh Framework Program (FP7/2007-2013) under grant agreement no 606798 (EuroVenus). NR 66 TC 3 Z9 3 U1 1 U2 11 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 AUG PY 2015 VL 113 SI SI BP 33 EP 48 DI 10.1016/j.pss.2015.01.009 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CM5UX UT WOS:000357755600004 ER PT J AU Cottini, V Ignatiev, NI Piccioni, G Drossart, P AF Cottini, V. Ignatiev, N. I. Piccioni, G. Drossart, P. TI Water vapor near Venus cloud tops from VIRTIS-H/Venus express observations 2006-2011 SO PLANETARY AND SPACE SCIENCE LA English DT Article DE Venus; Atmosphere; Water vapor; Clouds ID ATMOSPHERE; MESOSPHERE; PROFILES; OCS AB This work aims to give a summary of the water vapor at the cloud top of Venus atmosphere using the complete set of observations made using high spectral resolution channel (-H) of Visible and Infrared Thermal Imaging Spectrometer (VIRTIS), on board the ESA Venus Express orbiter, to measure the cloud top altitude and the water vapor abundance near this level. An initial analysis of these measurements by Cottini et al. (2012) was limited to data in 140 orbits in the period 2007-2008. These observations were limited to the Northern hemisphere due to observational geometry in this early part of the mission. In the present paper, the analysis is extended to a larger dataset covering the years 2006-2011, significantly improving the latitudinal coverage. Altitude of the cloud tops, corresponding to unit optical depth at a wavelength of 2.5 mu m, is equal to 69 +/- 1 km at low latitudes, and decreases toward the pole to 62-64 km. The water vapor abundance is equal to 3 +/- 1 ppm in low latitudes and it increases reaching a maximum of 5 +/- 2 ppm at 70-80 degrees of latitude in both hemispheres, with a sharp drop in the polar regions. This can be explained by the specific dynamics of the atmosphere of Venus affecting the distribution of water vapor such as the transfer of water vapor in the Hadley cell and the dynamic in the polar vortex. The average height of the cloud tops and the H2O near this level are symmetric with respect to the equator. As a function of local solar time, the water vapor shows no particular dependence, and the cloud tops exhibit just a weak maximum around noon. Over 5 years of observations the average values of the cloud top altitude and the water vapor were quite stable in low and middle latitudes, while in high latitudes both quantities in 2009-2011 years are systematically higher than in 2006-2008. Short period variations increasing with latitude are observed, from approximately less than +/- 1 km for cloud tops and +/- 1 ppm for water vapor in low latitudes to, respectively, +/- 2 km and +/- 2 ppm in high latitudes. As a rule there is no correlation between variations of the cloud top altitude, the water vapor content, and the UV brightness. However, numerous examples can be found when UV dark features, with a characteristic size of a few degrees of latitude (several hundred kilometers), coincide with regions of higher cloud tops. (C) 2015 Elsevier Ltd. All rights reserved. C1 [Cottini, V.] Univ Maryland, College Pk, MD 20742 USA. [Cottini, V.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Cottini, V.; Piccioni, G.] Ist Astrofis & Planetol Spaziali INAF IAPS, Rome, Italy. [Ignatiev, N. I.] Russian Acad Sci IKI RAN, Space Res Inst, Moscow, Russia. [Ignatiev, N. I.] Moscow Inst Phys & Technol, Dolgoprudnyi, Russia. [Drossart, P.] Observ Paris, LESIA, Meudon, France. RP Cottini, V (reprint author), Bldg 34,Room s121,Code 693,8800 Greenbelt Rd, Greenbelt, MD 20771 USA. EM valeria.cottini@nasa.gov OI Piccioni, Giuseppe/0000-0002-7893-6808 FU Agenzia Spaziale Italiana (ASI) [ASI-INAF I/050/10/0]; Centre National d'Etudes Spatiales (CNES); Russian Foundation for Basic Research [12-02-01280-a]; Ministry of Education and Science of Russian Federation of Education [11.G34.31.0074]; Presidium of Russian Academy of Sciences Program [22] FX Venus Express is a mission of the European Space Agency. We thank the Agenzia Spaziale Italiana (ASI) - grant ASI-INAF I/050/10/0 - and the Centre National d'Etudes Spatiales (CNES) for their support to the VIRTIS experiment. N. Ignatiev was supported by the Russian Foundation for Basic Research - Grant 12-02-01280-a, the Ministry of Education and Science of Russian Federation of Education - Grant 11.G34.31.0074, and the Presidium of Russian Academy of Sciences Program 22. We thank the editor Colin Wilson and the unknown referees for their suggestions for improving this paper. NR 23 TC 1 Z9 1 U1 0 U2 2 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 AUG PY 2015 VL 113 SI SI BP 219 EP 225 DI 10.1016/j.pss.2015.03.012 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CM5UX UT WOS:000357755600017 ER PT J AU Bougher, SW Brecht, AS Schulte, R Fischer, J Parkinson, CD Mahieux, A Wilquet, V Vandaele, A AF Bougher, S. W. Brecht, A. S. Schulte, R. Fischer, J. Parkinson, C. D. Mahieux, A. Wilquet, V. Vandaele, A. TI Upper atmosphere temperature structure at the Venusian terminators: A comparison of SOIR and VTGCM results SO PLANETARY AND SPACE SCIENCE LA English DT Article DE Venus; Venus Express mission; Upper atmosphere; Thermal structure; VTGCM; Thermal balance ID GENERAL-CIRCULATION; GLOBAL CIRCULATION; PHYSICAL PROCESSES; LINE OBSERVATIONS; TUNABLE FILTER; ATOMIC OXYGEN; EXPRESS; THERMOSPHERE; MESOSPHERE; MODEL AB Venus Express SOIR terminator profiles of CO2 densities and corresponding temperatures have been determined for 132 selected orbits obtained between 2006 and 2013. These recently recalibrated measurements provide temperature profiles at the Venusian terminator over approximately 70-160 km, revealing a striking permanent temperature minimum (at about 125 km) and a weaker temperature maximum (over 100-110 km). In addition, topside temperatures (above 140 km) reveal a warming trend consistent with a typical thermospheric structure. These features are reflected in the corresponding CO2 density profiles, and provide detailed constraints for global circulation models of the upper atmosphere. New Venus Thermospheric General Circulation Model (VTGCM) simulations are presented for conditions appropriate to these SOIR measurements. In particular, solar minimum to moderate fluxes are specified and mean values of eddy diffusion and wave drag parameters are utilized. Recent upgrades to the VTGCM code now include more realistic lower boundary conditions at 70 km near cloud tops. Model temperature profiles are extracted from the terminators that correspond to five latitude bins presently used in the SOIR data analysis. Averaging of VTGCM temperature profiles in each of these bins (at each terminator) is conducted to match SOIR sampling. Comparisons of these SOIR and VTGCM temperature profiles are shown. Most notably, the observed temperature minimum near 125 km and the weaker temperature maximum over 100-110 km are generally reproduced by the VTGCM at the correct pressure/altitude levels. However, magnitudes of simulated and measured temperatures are somewhat different as a function of latitude. In addition, VTGCM evening terminator (ET) temperatures are simulated to be modestly warmer than corresponding morning terminator (MT) values, a result of stronger ET than MT zonal winds at/above about 130 km. The SOIR terminator temperatures thus far do not reveal this consistent trend, suggesting the VTGCM climate based winds may not precisely represent the averaged conditions during SOIR sampling. Overall, these data-model comparisons reveal that both radiative and dynamical processes are responsible for maintaining averaged temperatures and driving significant variations in terminator temperature profiles. (C) 2015 Elsevier Ltd. All rights reserved. C1 [Bougher, S. W.; Parkinson, C. D.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. [Brecht, A. S.] Bay Area Environm Res Inst, Sonoma, CA 95476 USA. [Brecht, A. S.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Schulte, R.] Santa Clara Univ, Santa Clara, CA 95053 USA. [Fischer, J.] Univ Penn, Philadelphia, PA 19104 USA. [Mahieux, A.; Wilquet, V.; Vandaele, A.] Belgian Inst Space Aeron, Planetary Aeron, Brussels, Belgium. [Mahieux, A.] Fonds Natl Rech Sci, B-1000 Brussels, Belgium. RP Bougher, SW (reprint author), Univ Michigan, Dept Atmospher Ocean & Space Sci, Space Res Bldg,2455 Hayward St, Ann Arbor, MI 48109 USA. EM bougher@umich.edu OI Fischer, Johanna-Laina/0000-0003-1806-0653 FU NASA Venus Express Participating Scientist program through a subcontract from Southwest Research Institute (SwRI) [B99073JD]; NASA [NNX11AD81G] FX This research was funded by the NASA Venus Express Participating Scientist program through a subcontract from Southwest Research Institute (SwRI) to the University of Michigan (B99073JD). C.D. Parkinson acknowledges support with funding in part by NASA Grant #NNX11AD81G to the University of Michigan. C.D. Parkinson also wishes to thank the International Space Science Institute (ISSI) for their fruitful support for Venus team research over 2013-2015. NR 56 TC 3 Z9 3 U1 1 U2 3 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0032-0633 J9 PLANET SPACE SCI JI Planet Space Sci. PD AUG PY 2015 VL 113 SI SI BP 336 EP 346 DI 10.1016/j.pss.2015.01.012 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CM5UX UT WOS:000357755600027 ER PT J AU Stangier, T Hewagama, T Sornig, M Sonnabend, G Kostiuk, T Herrmann, M Livengood, T AF Stangier, Tobias Hewagama, Tilak Sornig, Manuela Sonnabend, Guido Kostiuk, Theodor Herrmann, Maren Livengood, Timothy TI Thermal structure of Venus' nightside mesosphere as observed by infrared heterodyne spectroscopy at 10 mu m SO PLANETARY AND SPACE SCIENCE LA English DT Article DE Venus; Temperature; Mesosphere; Nightside; Heterodyne; CO2 absorption ID 1.27-MU-M O-2 AIRGLOW; UPPER-ATMOSPHERE; LINE OBSERVATIONS; M WAVELENGTH; GENERAL-CIRCULATION; OZONE ABUNDANCE; TEMPERATURE; WINDS; CO2; THERMOSPHERE AB Ground-based heterodyne spectroscopy is used to observe the night side of Venus by probing single pressure broadened CO2 absorption lines. From the pressure induced line broadening, the predominant temperature at different altitude layers can be deduced. It is found, that heterodyne spectroscopy is sensitive to probe the mesosphere between similar to 60 km and 90 km with an altitude resolution of similar to 4.5 km. During two observing campaigns in March and May 2012, four different locations on the planet were investigated. Herein, we report on the retrieval of vertical temperature profiles in the nightside atmosphere of Venus. Retrieval of atmospheric parameters is based on a Levenberg-Marguard chi(2) optimization that iteratively compares observed data to telluric transmittance corrected Venus' top-of-atmosphere spectra calculated using a radiative transfer algorithm. The deduced profiles are compared to the Venus International Reference Atmosphere and some found to be in satisfactory agreement. Sub-Doppler resolution Infrared heterodyne observations can provide temperature measurements that complement existing sub-mm and space based observations. (C) 2015 Elsevier Ltd. All rights reserved. C1 [Stangier, Tobias] Univ Cologne, Phys Inst 1, Cologne, Germany. [Hewagama, Tilak; Kostiuk, Theodor; Livengood, Timothy] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Hewagama, Tilak; Livengood, Timothy] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Sonnabend, Guido] Radiometer Phys GmbH, Meckenheim, Germany. RP Stangier, T (reprint author), Univ Cologne, Phys Inst 1, Cologne, Germany. EM stangier@ph1.uni-koeln.de OI Livengood, Timothy/0000-0002-9947-4075 FU Deutsche Forschungsgemeinschaft (DFG) [SO1044/1-2] FX The authors want to thank the directors and staff of the NASA Infrared Telescope Facility and the McMath-Pierce Solar Observatory for their support on infrared heterodyne observations. We also thank our reviewers for many helpful comments. This work was supported by the Deutsche Forschungsgemeinschaft (DFG) through Grant SO1044/1-2. NR 64 TC 1 Z9 1 U1 0 U2 2 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 AUG PY 2015 VL 113 SI SI BP 359 EP 368 DI 10.1016/j.pss.2015.01.021 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CM5UX UT WOS:000357755600029 ER PT J AU Smialek, JL Garg, A AF Smialek, James L. Garg, Anita TI Interfacial reactions of a MAX phase/superalloy hybrid SO SURFACE AND INTERFACE ANALYSIS LA English DT Article DE Cr2AlC MAX phase; diffusion reaction; superalloys; aerospace materials; high temperature; coatings ID NICKEL-BASED SUPERALLOY; SINGLE-CRYSTAL SUPERALLOYS; HIGH-TEMPERATURE OXIDATION; NI-BASED SUPERALLOY; HOT CORROSION; DEGREES-C; ALUMINIDE COATINGS; CR2ALC; DIFFUSION; PHASES AB Oxidation resistant, strain tolerant MAX phase coatings are of general interest for high temperature applications. Accordingly, Cr2AlC MAX phase coupons were vacuum diffusion bonded to an advanced turbine disk alloy at 1100 degrees C for compatibility studies. The interface revealed an inner diffusion zone consisting of similar to 10 mu m of -Ni(Co)Al, decorated with various (Ni,Co)(3)Al, Ta(Ti,Nb)C, and W(Cr,Mo)(3)B-2 precipitates. On the Cr2AlC side, an additional similar to 40-mu m Al-depletion zone of Cr7C3 formed an interconnected network with the -Ni(Co)Al. On the superalloy side, enhanced carbide precipitation developed over a depth of similar to 80 mu m. Subsequent annealing for 100h and 1000h at 800 degrees C coarsened some features, enhanced TCP precipitation in the superalloy, but only enlarged the diffusion layers by similar to 5 mu m at most. Because of Al depletion from the MAX phase and corresponding Al enrichment of the alloy, the reaction zone displayed similarities to an oxidized Cr2AlC surface and an aluminized superalloy, respectively. Published 2015. This article is a U.S. Government work and is in the public domain in the USA. C1 [Smialek, James L.; Garg, Anita] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Smialek, JL (reprint author), NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. EM james.l.smialek@nasa.gov FU Fixed Wing Project of the NASA Fundamental Aeronautics Program FX The authors are grateful to Donald Humphrey for hot pressing and Joy Buehler for metallography. The helpful comments from Drs. T. Gabb and I. Locci are appreciated. This work has been supported by the Fixed Wing Project of the NASA Fundamental Aeronautics Program. NR 40 TC 2 Z9 2 U1 5 U2 26 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0142-2421 EI 1096-9918 J9 SURF INTERFACE ANAL JI Surf. Interface Anal. PD AUG PY 2015 VL 47 IS 8 BP 844 EP 853 DI 10.1002/sia.5784 PG 10 WC Chemistry, Physical SC Chemistry GA CM8RO UT WOS:000357969900007 ER PT J AU Yingst, RA Russell, P ten Kate, IL Noble, S Graff, T Graham, LD Eppler, D AF Yingst, R. A. Russell, P. ten Kate, I. L. Noble, S. Graff, T. Graham, L. D. Eppler, D. TI Designing remote operations strategies to optimize science mission goals: Lessons learned from the Moon Mars Analog Mission Activities Mauna Kea 2012 field test SO ACTA ASTRONAUTICA LA English DT Article DE Apollo Valley geologic map; Science operations; MER ID MIMOS-II; EXPLORATION; HAWAII; ROVER AB The Moon Mars Analog Mission Activities Mauna Kea 2012 (MMAMA 2012) field campaign aimed to assess how effectively an integrated science and engineering rover team operating on a 24-h planning cycle facilitates high-fidelity science products. The science driver of this field campaign was to determine the origin of a glacially-derived deposit: was the deposit the result of (1) glacial outwash from meltwater; or (2) the result of an ice dam breach at the head of the valley? Lessons learned from MMAMA 2012 science operations include: (1) current rover science operations scenarios tested in this environment provide adequate data to yield accurate derivative products such as geologic maps; (2) instrumentation should be selected based on both engineering and science goals; and chosen during, rather than after, mission definition; and (3) paralleling the tactical and strategic science processes provides significant efficiencies that impact science return. The MER-model concept of operations utilized, in which rover operators were sufficiently facile with science intent to alter traverse and sampling plans during plan execution, increased science efficiency, gave the Science Backroom time to develop mature hypotheses and science rationales, and partially alleviated the problem of data flow being greater than the processing speed of the scientists. (C) 2015 IAA. Published by Elsevier Ltd. on behalf of IAA. This is an open access article under the CC BY-NC-ND license (http://creativecommons.org/licensesiby-nc-nd/4.0/). C1 [Yingst, R. A.] Planetary Sci Inst, Tucson, AZ 85719 USA. [Russell, P.] Smithsonian Inst, Natl Air & Space Museum, Washington, DC 20013 USA. [ten Kate, I. L.] Univ Utrecht, Dept Earth Sci, Fac Geosci, Utrecht, Netherlands. [Noble, S.] NASA Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Graff, T.] NASA Johnson Space Ctr, Houston, TX 77058 USA. [Graham, L. D.; Eppler, D.] NASA Johnson Space Ctr, Houston, TX 77058 USA. RP Yingst, RA (reprint author), Planetary Sci Inst, 1700 E Ft Lowell St, Tucson, AZ 85719 USA. EM yingst@psi.edu; russellp@si.edu; i.l.tenkate@uu.nl; sarah.noble@nasa.gov; trevor.g.graff@nasa.gov; lee.d.graham@nasa.gov; dean.b.eppler@nasa.gov FU NASA MMAMA program [NNX12AM27G]; MMAMA program grant FX We gratefully acknowledge the work of the Rover Team and their JUNO II rover, which performed like a true wahine koa (warrior woman), making this field test possible. We also acknowledge the comments of Dr. John Moores and an anonymous reviewer that greatly improved this manuscript. This work was supported by NASA MMAMA program, Grant NNX12AM27G to RAY and an additional MMAMA program grant to ILtK. NR 31 TC 1 Z9 1 U1 1 U2 7 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0094-5765 EI 1879-2030 J9 ACTA ASTRONAUT JI Acta Astronaut. PD AUG-SEP PY 2015 VL 113 BP 120 EP 131 DI 10.1016/j.actaastro.2015.02.029 PG 12 WC Engineering, Aerospace SC Engineering GA CL8RA UT WOS:000357240600011 ER PT J AU Krisko, PH Flegel, S Matney, MJ Jarkey, DR Braun, V AF Krisko, P. H. Flegel, S. Matney, M. J. Jarkey, D. R. Braun, V. TI ORDEM 3.0 and MASTER-2009 modeled debris population comparison SO ACTA ASTRONAUTICA LA English DT Article DE Orbital debris; Engineering model; On-orbit impacts AB The latest versions of the two premier orbital debris engineering models, NASA's ORDEM 3.0 and ESA's MASTER-2009, have been publically released. Both models have gone through significant advancements since inception, and now represent the state-of-the-art in orbital debris knowledge of their respective agencies. The purpose of these models is to provide satellite designers/operators and debris researchers with reliable, and timely, estimates of the artificial debris environment in -Earth orbit, from about 200 km through about 40,000 km. The small debris environment within the "critical size range" of 1 cm to 1 mm is of particular interest to both human and robotic spacecraft programs. These objects are much more numerous than larger trackable debris and are still large enough to cause significant, if not catastrophic, damage to spacecraft upon impact. They are also small enough to elude routine detection by existing observation systems. Without reliable detection the modeling of these populations has always coupled theoretical origins with supporting observational data in different degrees. This paper offers the first cooperative comparison of the latest versions of the two models. No attempt to review model internal populations, or compare subsystems, or supporting data sets is made at this time. The models are simply run in the "Spacecraft Mode" for four test cases representing four orbital regimes, ISS (International Space Station orbit), SSO (sun synchronous orbit), GTO (geosynchronous transfer orbit), and GEO (geosynchronous orbit). Specific satellites are chosen within those categories for the analysis. Debris cumulative fluxes at three debris sizes (1 m, 10 cm, and the critical size range of 1 cm to 1 mm) are compared. At 1 m there is a very good match between ORDEM 3.0 and MASTER-2009 fluxes in the non-GEO orbits, less so in the GEO orbit. The 10 cm fluxes do not match as well, indicating possibly different treatment of uncatalogued objects. Within the critical size range it is noted that ORDEM 3.0 flux overtakes that of MASTER-2009 as debris size decreases in all test cases. In the analysis of separate model populations, the disparate usage of debris source populations (MASTER-2009) versus debris material density populations (ORDEM 3.0) is presently unresolved. MASTER-2009 populations of SRM (solid rocket motor) slag and explosion and collision fragments dominate with lower populations of ejecta debris. ORDEM 3.0 populations are dominated by medium and high density material with minor low density material populations. Undoubtedly, more in-depth collaborations will follow to hone in on population differences and sources. (C) 2015 IAA. Published by Elsevier Ltd. All rights reserved. C1 [Krisko, P. H.; Jarkey, D. R.] Jacobs, Houston, TX 77058 USA. [Flegel, S.] Fraunhofer Inst High Frequency Phys & Radar Tech, D-53343 Wachtberg, Germany. [Matney, M. J.] NASA, Orbital Debris Program Off, JSC, Houston, TX 77058 USA. [Braun, V.] Tech Univ Carolo Wilhelmina Braunschweig, Inst Aerosp Syst, D-38108 Braunschweig, Germany. RP Krisko, PH (reprint author), Jacobs, Mail Code JE104 2224 Bay Area Blvd, Houston, TX 77058 USA. EM paula.krisko-l@nasa.gov; sven.flegel@fhr.fraunhofer.de; mark.matney-l@nasa.gov; david.r.jarkey@nasa.gov; v.braun@tu-braunschweig.de NR 14 TC 4 Z9 4 U1 1 U2 8 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0094-5765 EI 1879-2030 J9 ACTA ASTRONAUT JI Acta Astronaut. PD AUG-SEP PY 2015 VL 113 BP 204 EP 211 DI 10.1016/j.actaastro.2015.03.024 PG 8 WC Engineering, Aerospace SC Engineering GA CL8RA UT WOS:000357240600018 ER PT J AU Rezac, L Kutepov, A Russell, JM Feofilov, AG Yue, J Goldberg, RA AF Rezac, L. Kutepov, A. Russell, J. M., III Feofilov, A. G. Yue, J. Goldberg, R. A. TI Simultaneous retrieval of T(p) and CO2 VMR from two-channel non-LTE limb radiances and application to daytime SABER/TIMED measurements SO JOURNAL OF ATMOSPHERIC AND SOLAR-TERRESTRIAL PHYSICS LA English DT Article DE Mesospheric temperature; Composition; Retrieval; Inversion ID ACCELERATED LAMBDA-ITERATION; NONLOCAL THERMODYNAMIC-EQUILIBRIUM; LOWER THERMOSPHERE; RADIATIVE-TRANSFER; UPPER MESOSPHERE; CARBON-DIOXIDE; SATELLITE-OBSERVATIONS; GLOBAL DISTRIBUTION; MIDDLE ATMOSPHERE; INVERSE PROBLEMS AB The kinetic temperature, T-k, and carbon dioxide, CO2 density, are key parameters that characterize the energetics and dynamics of the mesosphere and lower thermosphere (MLT) region. The Sounding of the Atmosphere using Broadband Emission Radiometry (SABER) instrument on-board the Thermosphere-Ionosphere-Mesosphere-Energetics and Dynamics (TIMED) satellite has been providing global, simultaneous measurements of limb radiance in 10 spectral channels continuously since late January 2002. In this paper we (1) present a methodology for a self-consistent simultaneous retrieval of temperature/pressure, T-k(p), and CO2 volume mixing ratio (VMR) from the broadband infrared limb measurements in the 15 and 4.3 mu m channels, and (2) qualitatively describe the first results on the CO2 VMR and T-k obtained from application of this technique to the SABER 15 and 4.3 pm channels, including issues, which demand additional constraints to be applied. The self-consistent two-channel retrieval architecture updates parameters at all altitudes simultaneously, and it is built upon iterative switching between two retrieval modules, one for CO2 and one for T-k. A detailed study of sensitivity, stability and convergence was carried out to validate the algorithm. The T-k/CO2 VMR distribution can be reliably retrieved without biases connected with this non-linear inverse problem starting with an initial guess as far as +/- 20% of CO2 VMR and +/- 15 K from the solution (as global shift, or somewhat larger if only local deviations are considered). In polar summer toward high latitudes the retrieved CO2 VMR profile shows a local peak around 90 km. We discuss details of this feature and show that: (a) it is not an algorithm artifact or instability, (b) additional a priori constraints are needed in order to obtain a physical profile and to remove this peak, and (c) several possibilities are explored as to uncover the real cause of this feature, but no firm conclusion can be reached at this time. This algorithm has been applied to all available daytime SABER measurements since 2002, and the first results of the mean CO2 VMR profiles and their distribution is discussed. In particular, the CO2 VMR profiles depart from a well mixed value at altitudes of 65-70 km during equinoxes at high and mid-latitudes, but in the summer hemisphere solstice period the SABER data is more consistent with a well mixed VMR conditions extend up to 87-90 km especially toward high latitudes. (C) 2015 Elsevier Ltd. All rights reserved. C1 [Rezac, L.] Max Planck Inst Solar Syst Res, Gottingen, Germany. [Rezac, L.; Russell, J. M., III; Yue, J.] Hampton Univ, Ctr Atmospher Sci, Hampton, VA 23668 USA. [Kutepov, A.; Goldberg, R. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Kutepov, A.] Catholic Univ Amer, Washington, DC 20064 USA. [Feofilov, A. G.] Ecole Polytech, Meteorol Dynam Lab, Palaiseau, France. RP Rezac, L (reprint author), Max Planck Inst Solar Syst Res, Justus von Liebig Weg, Gottingen, Germany. EM rezac@mps.mpg.de RI Yue, Jia/D-8177-2011; Feofilov, Artem/A-2271-2015 OI Feofilov, Artem/0000-0001-9924-4846 FU Center for Atmospheric Sciences (CAS), Hampton University, Hampton, Virginia [NNX11AD63G]; NASA GSFC [NNX11AM24G]; NASA [NNX14AF20G, NNH13ZDA001N-HGI] FX The authors would also like to thank the NASA directorate for continual support of the TIMED mission. This work has been accomplished in the Center for Atmospheric Sciences (CAS), Hampton University, Hampton, Virginia under the Grant NNX11AD63G, and in the Institute for Astrophysics and Computational Physics (IACP), the Catholic University of America, and NASA GSFC under the Grant NNX11AM24G. J.Y. was supported by NASA Grants NNX14AF20G and NNH13ZDA001N-HGI. We would like to acknowledge the hard work and support of the SABER retrieval team providing the version 2.0 data, including scientists from GATS, Inc, NASA Langley Research Center, NASA Goddard Space Flight Center and Spain (IAA) in this effort The team is also indebted to August H. Wessels from Science Systems and Applications Inc for his wonderful support which permitted this project to reach fruition in a reasonable time period, and to Michael R. Greason from Adnet Systems Inc, who designed and provided system support for our new and dedicated high-speed workstation used for the very extensive calculations this study required. We also acknowledge computer resources at Max-Planck Institute of Solar System Research, Germany and Ecole Polytechnique, Palaiseau, France. We also thank the science team of the ACE-FTS instrument for kindly providing their early 22 and the new, 3.0, version of CO2 retrievals for the first comparisons. We thank the two reviewers for their thorough review and stimulating questions, which lead to improvements on several discussions. NR 67 TC 7 Z9 7 U1 2 U2 7 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1364-6826 EI 1879-1824 J9 J ATMOS SOL-TERR PHY JI J. Atmos. Sol.-Terr. Phys. PD AUG PY 2015 VL 130 BP 23 EP 42 DI 10.1016/j.jastp.2015.05.004 PG 20 WC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences SC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences GA CM5UH UT WOS:000357754000003 ER PT J AU Bellur, K Medici, E Allen, J Choi, CK Hermanson, J Tamilarasan, A Hussey, D Jacobson, D Leao, JB McQuillen, J AF Bellur, Kishan Medici, Ezequiel Allen, Jeffrey Choi, Chang Kyoung Hermanson, Jimes Tamilarasan, Arun Hussey, Daniel Jacobson, David Leao, Juscelino B. McQuillen, John TI Neutron Radiography of Condensation and Evaporation of Hydrogen in a Cryogenic Condition SO JOURNAL OF HEAT TRANSFER-TRANSACTIONS OF THE ASME LA English DT Article C1 [Bellur, Kishan; Medici, Ezequiel; Allen, Jeffrey; Choi, Chang Kyoung] Michigan Technol Univ, Houghton, MI 49931 USA. [Hermanson, Jimes; Tamilarasan, Arun] Univ Washington, Seattle, WA 98195 USA. [Hussey, Daniel; Jacobson, David; Leao, Juscelino B.] NIST, Gaithersburg, MD 20899 USA. [McQuillen, John] NASA, Glenn Res Ctr Lewis Field, Cleveland, OH 44135 USA. RP Bellur, K (reprint author), Michigan Technol Univ, Houghton, MI 49931 USA. FU NASA [NNX14AB05G] FX These experiments were conducted at the NIST Center for Neutron Research in the Neutron Imaging Facility and the relevant work is supported by an Early stage Innovations Grant from NASA's Space Technology Research Grants Program (Grant # NNX14AB05G). NR 0 TC 0 Z9 0 U1 2 U2 2 PU ASME PI NEW YORK PA TWO PARK AVE, NEW YORK, NY 10016-5990 USA SN 0022-1481 EI 1528-8943 J9 J HEAT TRANS-T ASME JI J. Heat Transf.-Trans. ASME PD AUG PY 2015 VL 137 IS 8 AR 080901 PG 1 WC Thermodynamics; Engineering, Mechanical SC Thermodynamics; Engineering GA CM3MF UT WOS:000357585600002 ER PT J AU Park, H Jeong, SJ Ho, CH Kim, J Brown, ME Schaepman, ME AF Park, Hoonyoung Jeong, Su-Jong Ho, Chang-Hoi Kim, Jinwon Brown, Molly E. Schaepman, Michael E. TI Nonlinear response of vegetation green-up to local temperature variations in temperate and boreal forests in the Northern Hemisphere SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE Phenology; Climate variability; Rate of canopy development; Temperate and boreal forest; Northern Hemisphere; Global ecology ID GROWING-SEASON LENGTH; CLIMATE-CHANGE; SPRING PHENOLOGY; TIME-SERIES; LEAF-AREA; GROWTH; AVHRR; NDVI; VARIABILITY; MODIS AB The annual cycle of vegetation growth may be altered in response to climate changes affecting ecosystem dynamics. However, our understanding of vegetation seasonality is mostly limited to the mechanisms and attributes of phenological events, such as spring emergence and fall senescence. Here we have investigated the seasonal evolution of vegetation growth from winter dormancy to summer maturity of four forest types in the Northern Hemisphere (NH) temperate and boreal forests for 1982-2011. The present study assesses large-scale variations in the vegetation green-up rate (VG(rate)) and its connection to temperature variability using remotely sensed normalized difference vegetation index (NDVI) and surface air temperature. The average of the VG(ate) of the analysis period increases with latitude, which indicates that the canopy develops more rapidly from dormancy to maturity for vegetation in higher-latitude or colder climate zones. VG(rate) and precedent temperature also show a positive correlation (r) over temperate and boreal forests (67% of the forest area in the NH), indicating that increased temperatures lead to faster canopy development within the same climate zone or latitude band. Responsiveness of VG(rate) to temperature variability shows that despite the same magnitude of local temperature variability during extremely cold and warm years, the magnitude of VG(rate) acceleration in warm years (0.07 (15-day)(-1)) is larger than the VG(rate) deceleration in cold years (-0.03 (15-day)(-1)), suggesting that the response of VG(rate) to temperature variability is nonlinear. Among the four forest types examined in this study, the nonlinear responses are most clearly observed in deciduous broadleaf forests indicating that forest composition may regulate the large-scale response of canopy development to temperature variability. Overall, our results suggest that anomalous seasonal warming will significantly affect canopy developments over wide deciduous forest areas. (C) 2015 Elsevier Inc. All rights reserved. C1 [Park, Hoonyoung; Ho, Chang-Hoi] Seoul Natl Univ, Sch Earth & Environm Sci, Seoul, South Korea. [Jeong, Su-Jong] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Kim, Jinwon] Univ Calif Los Angeles, JIFRESSE, Los Angeles, CA USA. [Kim, Jinwon] Univ Calif Los Angeles, Dept Atmospher & Ocean Sci, Los Angeles, CA USA. [Brown, Molly E.] Univ Maryland, Dept Geog Sci, College Pk, MD 20742 USA. [Schaepman, Michael E.] Univ Zurich, Remote Sensing Labs, Zurich, Switzerland. RP Jeong, SJ (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. RI Jeong, Su-Jong/J-4110-2014; Schaepman, Michael/B-9213-2009; Brown, Molly/E-2724-2010 OI Schaepman, Michael/0000-0002-9627-9565; Brown, Molly/0000-0001-7384-3314 FU Korea Ministry of Environment under the "Climate Change Correspondence R&D Program (Technical development of vulnerability assessment for extreme climate)" FX This study was supported by the Korea Ministry of Environment under the "Climate Change Correspondence R&D Program (Technical development of vulnerability assessment for extreme climate)". Part of the research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. We acknowledge the contribution of the University of Zurich Research Priority Program on 'Global Change and Biodiversity (URPP GCB). The authors have no conflict of interests. NR 63 TC 6 Z9 6 U1 6 U2 43 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0034-4257 EI 1879-0704 J9 REMOTE SENS ENVIRON JI Remote Sens. Environ. PD AUG PY 2015 VL 165 BP 100 EP 108 DI 10.1016/j.rse.2015.04.030 PG 9 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA CM2XK UT WOS:000357545400008 ER PT J AU Yao, YJ Liang, SL Li, XL Chen, JQ Wang, KC Jia, K Cheng, J Jiang, B Fisher, JB Mu, QZ Grunwald, T Bernhofer, C Roupsard, O AF Yao, Yunjun Liang, Shunlin Li, Xianglan Chen, Jiquan Wang, Kaicun Jia, Kun Cheng, Jie Jiang, Bo Fisher, Joshua B. Mu, Qiaozhen Gruenwald, Thomas Bernhofer, Christian Roupsard, Olivier TI A satellite-based hybrid algorithm to determine the Priestley-Taylor parameter for global terrestrial latent heat flux estimation across multiple biomes SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE Global latent heat flux; Hybrid algorithm; Plant functional type; Priestley-Taylor parameter; Ecophysiological constraints ID ENERGY-BALANCE CLOSURE; RADIOMETRIC SURFACE-TEMPERATURE; NET PRIMARY PRODUCTION; ATMOSPHERE WATER FLUX; LAND-SURFACE; EDDY-COVARIANCE; CARBON-DIOXIDE; SOIL-MOISTURE; EVAPOTRANSPIRATION ESTIMATION; SCALE EVAPOTRANSPIRATION AB Accurate estimation of the terrestrial latent heat flux (LE) for each plant functional type (PET) at high spatial and temporal scales remains a major challenge. We developed a satellite-based hybrid algorithm to determine the Priestley-Taylor (PT) parameter for estimating global terrestrial LE across multiple biomes. The hybrid algorithm combines a simple empirical equation with physically based ecophysiological constraints to obtain the sum of the weighted ecophysiological constraints (f(e)) from satellite-based normalized difference vegetation index (NDVI) and ground-measured air temperature (TO, relative humidity (RH), vapor pressure deficit (VPD) and LE for 2000 to 2009 provided by 240 globally distributed FLUXNET eddy covariance (ECOR) tower sites. Cross-validation analysis indicated that the optimization at a PFT level performed well with a RMSE of less than 0.15 and a R-2 between 0.61 and 0.88 for estimated monthly f(e). Cross-validation analysis also revealed good performance of the hybrid-based PT method in estimating seasonal variability with a RMSE of the monthly LE varying from 43 W/m(2) (for 6 deciduous needleleaf forest sites) to 18.1 W/m(2) (for 34 crop sites) and with a R-2 of more than 0.67. The algorithm's performance was also good for predicting among-site and inter-annual variability with a R-2 of more than 0.78 and 0.70, respectively. We implemented the global terrestrial LE estimation from 2003 to 2005 for a spatial resolution of 0.05 degrees by recalibrating the coefficients of the hybrid algorithm using Modern Era Retrospective Analysis for Research and Applications (MERRA) meteorological data, Moderate Resolution Imaging Spectroradiometer (MODIS) NDVI product and ground-measured LE. This simple but accurate hybrid algorithm provides an alternative method for mapping global terrestrial LE, with a performance generally improved as compared to other satellite algorithms that are not calibrated with tower. The calibrated f(e) differs for different PFTs, and all driving forces of the algorithm can be acquired from satellite and meteorological observations. (C) 2015 Elsevier Inc. All rights reserved. C1 [Yao, Yunjun; Liang, Shunlin; Jia, Kun; Cheng, Jie; Jiang, Bo] Beijing Normal Univ, Sch Geog, State Key Lab Remote Sensing Sci, Beijing 100875, Peoples R China. [Yao, Yunjun; Liang, Shunlin; Li, Xianglan; Wang, Kaicun; Jia, Kun; Cheng, Jie; Jiang, Bo] Beijing Normal Univ, Coll Global Change & Earth Syst Sci, Beijing 100875, Peoples R China. [Liang, Shunlin] Univ Maryland, Dept Geog Sci, College Pk, MD 20742 USA. [Chen, Jiquan] Michigan State Univ, CGCEO Geog, E Lansing, MI 48823 USA. [Fisher, Joshua B.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Mu, Qiaozhen] Univ Montana, Dept Ecosyst & Conservat Sci, Numer Terradynam Simulat Grp, Missoula, MT 59812 USA. [Gruenwald, Thomas; Bernhofer, Christian] Tech Univ Dresden, Inst Hydrol & Meteorol, Chair Meteorol, D-01062 Dresden, Germany. [Roupsard, Olivier] CIRAD, UMR Eco&Sols Ecol Fonct & Biogeochim Sols & Agroe, F-34060 Montpellier, France. [Roupsard, Olivier] CATiE Trop Agr Ctr Res & Higher Educ, Turrialba 7170, Costa Rica. RP Yao, YJ (reprint author), Beijing Normal Univ, Beijing 100875, Peoples R China. EM boyyunjun@163.com RI Wang, Kaicun/F-7813-2012; Cheng, Jie/G-2039-2011; liang, shunlin/C-2809-2015; Chen, Jiquan/D-1955-2009; OI Wang, Kaicun/0000-0002-7414-5400; Fisher, Joshua/0000-0003-4734-9085; Jia, Kun/0000-0001-8586-4243 FU High-Tech Research and Development Program of China [2013AAl22801]; Natural Science Fund of China [41201331, 41331173, 41205104]; CarboEuropelP; FAO-GTOS-TCO; iLEAPS; Max Planck Institute for Biogeochemistry; National Science Foundation; University of Tuscia; Universite Laval; Environment Canada; US Department of Energy; National Aeronautics and Space Administration; AmeriFlux (U.S. Department of Energy, Biological and Environmental Research, Terrestrial Carbon Program) [DE-FG02-04ER63917, DE-FG02-04ER63911]; CFCAS; NSERC; BIOCAP; NRCan FX We would like to thank Prof. Shaomin Liu, Dr. Xiaotong Zhang, Dr. Xiang Zhao, Dr. Xianhong Xie, Dr. Ziwei Xu and Ms. Meng Liu from Beijing Normal University, China, and Prof. Guangsheng Zhou from the Institute of Botany, CAS, and Dr. Yan Li and Dr. Ran Liu from Xinjiang Institute of Ecology and Geography, CAS, and Prof. Guoyi Zhou and Dr. Yuelin Li from South China Botanic Garden, CAS, and Prof. Bin Zhao from Fudan University, China, for providing ground-measured data. This work used eddy covariance data acquired by the FLUXNET community and in particular by the following networks: AmeriFlux (U.S. Department of Energy, Biological and Environmental Research, Terrestrial Carbon Program (DE-FG02-04ER63917 and DE-FG02-04ER63911)), AfriFlux, AsiaFlux, CarboAfrica, CarboEuropelP, Carboitaly, CarboMont,ChinaFlux, Fluxnet-Canada (supported by CFCAS, NSERC, BIOCAP, Environment Canada, and NRCan), GreenGrass, KoFlux, LBA, NECC, OzFlux, TCOS-Siberia, USCCC. We acknowledge the financial support to the eddy covariance data harmonization provided by CarboEuropelP, FAO-GTOS-TCO, iLEAPS, Max Planck Institute for Biogeochemistry, National Science Foundation, University of Tuscia, Universite Laval, Environment Canada and US Department of Energy and the database development and technical support from Berkeley Water Center, Lawrence Berkeley National Laboratory, Microsoft Research eScience, Oak Ridge National Laboratory, University of California-Berkeley and the University of Virginia. Other ground-measured data were obtained from the GAME AAN (http://aan.suiri.tsukuba.acjp/), the Coordinated Enhanced Observation Project (CEOP) in arid and semi-arid regions of northern China (http://observation.tea.ac.cn/), and the water experiments of Environmental and Ecological Science Data Center for West China (http://westdc.westgis.ac.cn/water). MODIS LAI/FPAR, NDVI, Albedo and land cover satellite products were obtained online (http://reverb.echo.nasa.gov/reverb). This work was partially supported by the High-Tech Research and Development Program of China (No.2013AAl22801), and the Natural Science Fund of China (No.41201331, No. 41331173 and No.41205104). J.B.F. contributed to this paper from the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. NR 112 TC 6 Z9 6 U1 7 U2 29 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0034-4257 EI 1879-0704 J9 REMOTE SENS ENVIRON JI Remote Sens. Environ. PD AUG PY 2015 VL 165 BP 216 EP 233 DI 10.1016/j.rse2015.05.013 PG 18 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA CM2XK UT WOS:000357545400017 ER PT J AU Krishnan, P Kochendorfer, J Dumas, EJ Guillevic, PC Baker, CB Meyers, TP Martos, B AF Krishnan, Praveena Kochendorfer, John Dumas, Edward J. Guillevic, Pierre C. Baker, C. Bruce Meyers, Tilden P. Martos, Borja TI Comparison of in-situ, aircraft, and satellite land surface temperature measurements over a NOAA Climate Reference Network site SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE Land surface temperature; Aircraft; Satellite; MODIS; Validation; USCRN ID RADIATION BUDGET NETWORK; RADIOMETER SUITE VIIRS; SKIN TEMPERATURE; GROUND MEASUREMENTS; AIR-TEMPERATURE; OKLAHOMA MESONET; UNITED-STATES; COVER CHANGE; MODIS; VALIDATION AB Land surface temperature (LST) is a key variable for studying the energy and water vapor exchange at the biosphere-atmosphere interface. In an effort to better quantify the spatial variability and overall representativeness of single-point LST measurements being recorded at NOAA's Climate Reference Network (CRN) sites and to improve the accuracy of satellite LST measurements, airborne flight campaigns were conducted over a CRN site in Crossville, Tennessee, USA during 2010 to 2011. Multiple measurements of LST were made using infrared temperature sensors at micrometeorological tower sites and onboard an instrumented Piper Navajo airborne research aircraft. In addition to this, coincident LST products from the moderate resolution imaging spectroradiometer (MODIS) instruments (Collection 5), onboard NASA Terra and Aqua Earth Observing System satellites were used. In this paper the comparison of LST measurements made from multiple platforms are presented. Our study showed that the temporal and spatial variability of surface temperature as indicated by the standard deviation of the brightness temperature (T-b) during the flight periods were <1.7 degrees C. Aircraft and tower-based T-b during the flight periods agreed well with a root mean square error (RMSE) of <1.3 degrees C. The daytime MODIS LST was lower than the tower and aircraft-based LST, but higher than the daytime near surface air temperature (T-a). MODIS LST showed a positive and lower bias with the nighttime tower-based LST, but with slightly higher RMSE than the daytime dataset The MODIS LST showed better correlation with the tower-based LST than T-a during clear sky conditions due to the complex relationship between air and surface temperature. Including both day and nighttime data the MODIS LST showed a bias of -056 degrees C, RMSE of 2.84 degrees C, and standard deviations of the difference of 2.79 degrees C when compared to the mean tower-based LST at the site. Tower-based 11 explained 98% of the variance in LST during nighttime conditions with a bias of similar to 0.8 degrees C and RMSE of 0.86 degrees C. (C) 2015 Elsevier Inc. All rights reserved. C1 [Krishnan, Praveena; Kochendorfer, John; Dumas, Edward J.; Baker, C. Bruce; Meyers, Tilden P.] NOAA, Atmospher Turbulence & Diffus Div, ARL, Oak Ridge, TN 37830 USA. [Krishnan, Praveena; Dumas, Edward J.] Oak Ridge Associated Univ, Oak Ridge, TN USA. [Guillevic, Pierre C.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Martos, Borja] Univ Tennessee, Inst Space, Tullahoma, TN 37388 USA. RP Krishnan, P (reprint author), NOAA, Atmospher Turbulence & Diffus Div, ARL, 456 South Illinois Ave, Oak Ridge, TN 37830 USA. EM praveena.krishnan@noaa.gov RI Krishnan, Praveena/F-8169-2010; Kochendorfer, John/K-2680-2012; Dumas, Edward/C-6669-2016; Meyers, Tilden/C-6633-2016 OI Kochendorfer, John/0000-0001-8436-2460; Dumas, Edward/0000-0002-9154-9052; FU National Oceanic and Atmospheric Administration's (NOAA) U.S. Climate Reference Network program administered at NOAA's National Climatic Data Center FX This research was partially funded by the National Oceanic and Atmospheric Administration's (NOAA) U.S. Climate Reference Network program administered at NOAA's National Climatic Data Center (see www.ncdc.noaa.gov/crn/). The MODIS data used in this study are distributed by the Land Processes Distributed Active Archive Center (LPDAAC), located at USGS/EROS, Sioux Falls, SD, http://lpdaac.usgs.gov. We thank Stephen Corda and John Muratore for their support during the experimental flight campaigns. NR 89 TC 5 Z9 5 U1 2 U2 21 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0034-4257 EI 1879-0704 J9 REMOTE SENS ENVIRON JI Remote Sens. Environ. PD AUG PY 2015 VL 165 BP 249 EP 264 DI 10.1016/j.rse.2015.05.011 PG 16 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA CM2XK UT WOS:000357545400019 ER PT J AU Shemelya, CM Rivera, A Perez, AT Rocha, C Liang, M Yu, XJ Kief, C Alexander, D Stegeman, J Xin, H Wicker, RB MacDonald, E Roberson, DA AF Shemelya, Corey M. Rivera, Armando Perez, Angel Torrado Rocha, Carmen Liang, Min Yu, Xiaoju Kief, Craig Alexander, David Stegeman, James Xin, Hao Wicker, Ryan B. MacDonald, Eric Roberson, David A. TI Mechanical, Electromagnetic, and X-ray Shielding Characterization of a 3D Printable Tungsten-Polycarbonate Polymer Matrix Composite for Space-Based Applications SO JOURNAL OF ELECTRONIC MATERIALS LA English DT Article DE Polymer composites; material testing; fracture analysis; mechanical properties; 3D printing ID FILLED-POLYPROPYLENE COMPOSITES; BISPHENOL-A POLYCARBONATE; THERMAL-DEGRADATION; CARBON NANOTUBE; PARTICLE-SIZE; ELECTRONICS AB Material-extrusion three-dimensional (3D) printing has recently attracted much interest because of its process flexibility, rapid response to design alterations, and ability to create structures "on-the-go". For this reason, 3D printing has possible applications in rapid creation of space-based devices, for example cube satellites (CubeSat). This work focused on fabrication and characterization of tungsten-doped polycarbonate polymer matrix composites specifically designed for x-ray radiation-shielding applications. The polycarbonate-tungsten polymer composite obtained intentionally utilizes low loading levels to provide x-ray shielding while limiting effects on other properties of the material, for example weight, electromagnetic functionality, and mechanical strength. The fabrication process, from tungsten functionalization to filament extrusion and material characterization, is described, including printability, determination of x-ray attenuation, tensile strength, impact resistance, and gigahertz permittivity, and failure analysis. The proposed materials are uniquely advantageous when implemented in 3D printed structures, because even a small volume fraction of tungsten has been shown to substantially alter the properties of the resulting composite. C1 [Shemelya, Corey M.; Rivera, Armando; Perez, Angel Torrado; Rocha, Carmen; Wicker, Ryan B.; MacDonald, Eric; Roberson, David A.] Univ Texas El Paso, WM Keck Ctr Innovat 3D, El Paso, TX 79968 USA. [Shemelya, Corey M.; MacDonald, Eric] Univ Texas El Paso, Dept Elect & Comp Engn, El Paso, TX 79968 USA. [Perez, Angel Torrado; Rocha, Carmen; Roberson, David A.] Univ Texas El Paso, Dept Met & Mat Engn, El Paso, TX 79968 USA. [Perez, Angel Torrado; Rocha, Carmen; Roberson, David A.] Univ Texas El Paso, WM Keck Ctr Innovat 3D, Polymer Extrus Lab, El Paso, TX 79968 USA. [Liang, Min; Yu, Xiaoju; Xin, Hao] Univ Arizona, Dept Elect & Comp Engn, Tucson, AZ 85721 USA. [Kief, Craig; Alexander, David] COSMIAC, Albuquerque, NM 87106 USA. [Stegeman, James] NASA Glenn Res Ctr, Cleveland, OH 44135 USA. [Wicker, Ryan B.] Univ Texas El Paso, Dept Mech Engn, El Paso, TX 79968 USA. [Roberson, David A.] Univ Texas El Paso, Ctr Struct & Funct Mat Res & Innovat, El Paso, TX 79968 USA. RP Roberson, DA (reprint author), Univ Texas El Paso, WM Keck Ctr Innovat 3D, El Paso, TX 79968 USA. EM droberson@utep.edu FU America Makes Manufacturing Initiative; State of Texas Emerging Technology Fund; National Aeronautics and Space Administration [NNX13AB53G]; AFOSR YIP [FA9550-14-1-0260]; National Science Foundation [0823864, 0925220]; state of Arizona under TRIF; Intelligence Community Postdoctoral Research Fellowship Program through Office of the Director of National Intelligence FX We would like to thank the Intelligence Community Postdoctoral Research Fellowship Program, The University of Texas at El Paso, the W. M. Keck Center for 3D Innovation, the University of Arizona, COSMIAC, and NASA Glenn Research Center. The research presented here was performed as a result of funding in part from The America Makes Manufacturing Initiative, the State of Texas Emerging Technology Fund, the National Aeronautics and Space Administration under grant number NNX13AB53G, AFOSR YIP under grant number FA9550-14-1-0260, the National Science Foundation under awards 0823864 and 0925220, and the state of Arizona under TRIF. This project was supported by a grant from the Intelligence Community Postdoctoral Research Fellowship Program through funding from the Office of the Director of National Intelligence. All statements of fact, opinion, or analysis expressed are those of the authors and do not reflect the official positions or views of the Intelligence Community or of any other US Government agency. Nothing in the contents should be construed as asserting or implying US Government authentication of information or Intelligence Community endorsement of the author's views. NR 40 TC 6 Z9 8 U1 13 U2 74 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0361-5235 EI 1543-186X J9 J ELECTRON MATER JI J. Electron. Mater. PD AUG PY 2015 VL 44 IS 8 BP 2598 EP 2607 DI 10.1007/s11664-015-3687-7 PG 10 WC Engineering, Electrical & Electronic; Materials Science, Multidisciplinary; Physics, Applied SC Engineering; Materials Science; Physics GA CL5YL UT WOS:000357041400008 ER PT J AU Zhuo, L Han, DW Dai, Q Islam, T Srivastava, PK AF Zhuo, Lu Han, Dawei Dai, Qiang Islam, Tanvir Srivastava, Prashant K. TI Appraisal of NLDAS-2 Multi-Model Simulated Soil Moistures for Hydrological Modelling SO WATER RESOURCES MANAGEMENT LA English DT Article DE Hydrological modelling; Land surface modelling; Xinanjiang; Soil moisture deficit; NLDAS-2; Evaluation ID LAND-SURFACE MODEL; CLIMATE REFERENCE NETWORK; SMOS SATELLITE; PARAMETERIZATION; TEMPERATURE; SCHEMES; SYSTEM; WATER AB Soil moisture is a key variable in hydrological modelling, which could be estimated by land surface modelling. However the previous studies have focused on evaluating these soil moisture estimates by using point-based measurements, and there is a lack of attention for their appraisal over basin scales particularly for hydrological applications. In this study, we carry out for the first time, a detailed evaluation of five sources of soil moisture products (NLDAS-2 multi-model simulated soil moistures: Noah, VIC, Mosaic and SAC; and a ground observation), against a widely used hydrological model Xinanjiang (XAJ) as a benchmark at a U.S. basin. Generally speaking, all products have good agreements with the hydrological soil moisture simulation, with superior performance obtained from the SAC model and the VIC model. Furthermore, the results indicate that the in-situ measurements in deeper soil layer are still usable for hydrological applications. Nevertheless further improvement is still required on the definition of land surface model layer thicknesses and the related data fusion with the remotely sensed soil moisture. The potential usage of the NLDAS-2 soil moisture datasets in real-time flood forecasting is discussed. C1 [Zhuo, Lu; Han, Dawei; Dai, Qiang] Univ Bristol, Dept Civil Engn, WEMRC, Bristol, Avon, England. [Islam, Tanvir] NASA, Jet Prop Lab, Pasadena, CA USA. [Islam, Tanvir] CALTECH, Pasadena, CA 91125 USA. [Srivastava, Prashant K.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Srivastava, Prashant K.] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. [Srivastava, Prashant K.] Banaras Hindu Univ, Inst Environm & Sustainable Dev, Varanasi 221005, Uttar Pradesh, India. RP Zhuo, L (reprint author), Univ Bristol, Dept Civil Engn, WEMRC, Bristol, Avon, England. EM lz7913@bristol.ac.uk OI Islam, Tanvir/0000-0003-2429-3074 NR 55 TC 10 Z9 10 U1 5 U2 12 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0920-4741 EI 1573-1650 J9 WATER RESOUR MANAG JI Water Resour. Manag. PD AUG PY 2015 VL 29 IS 10 BP 3503 EP 3517 DI 10.1007/s11269-015-1011-1 PG 15 WC Engineering, Civil; Water Resources SC Engineering; Water Resources GA CM0CH UT WOS:000357345300003 ER PT J AU Leone, FA Davila, CG Girolamo, D AF Leone, Frank A. Davila, Carlos G. Girolamo, Donato TI Progressive damage analysis as a design tool for composite bonded joints SO COMPOSITES PART B-ENGINEERING LA English DT Article DE Finite element analysis (FEA); Adhesion; Honeycomb; Mechanical testing ID CONSTITUTIVE MODEL; DELAMINATION AB This paper discusses the application of progressive damage analysis (PDA) methods as a design tool. Two case studies are presented in which the effects of changing design features on the strength of bonded composite joints are evaluated. It is shown that the trends of parametric evaluations performed with full-featured PDA models can be unintuitive and the trends can be opposite to those obtained with traditional design criteria. The joint configurations that were tested exhibit multiple damage modes, requiring several different PDA tools to accurately predict the structural peak loads. For damage tolerant structures that exhibit complex sequences of multiple failure mechanisms, traditional failure prediction tools are insufficient. Parametric PDA models encompassing a bonded joint specimen's design space have the potential to reveal unintuitive and advantageous design changes. Published by Elsevier Ltd. C1 [Leone, Frank A.; Davila, Carlos G.] NASA, Langley Res Ctr, Hampton, VA 23681 USA. [Girolamo, Donato] N Carolina State Univ, Raleigh, NC 27695 USA. RP Leone, FA (reprint author), NASA, Langley Res Ctr, Hampton, VA 23681 USA. EM frank.a.leone@nasa.gov NR 21 TC 2 Z9 2 U1 0 U2 4 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 1359-8368 EI 1879-1069 J9 COMPOS PART B-ENG JI Compos. Pt. B-Eng. PD AUG PY 2015 VL 77 BP 474 EP 483 DI 10.1016/j.compositesb.2015.03.046 PG 10 WC Engineering, Multidisciplinary; Materials Science, Composites SC Engineering; Materials Science GA CL2DP UT WOS:000356754100051 ER PT J AU Saitta, EKH Gittings, MJ Novaes-Card, S Quinn, J Clausen, C O'Hara, S Yestrebsky, CL AF Saitta, Erin K. H. Gittings, Michael J. Novaes-Card, Simone Quinn, Jacqueline Clausen, Christian O'Hara, Suzanne Yestrebsky, Cherie L. TI Case study of a non-destructive treatment method for the remediation of military structures containing polychlorinated biphenyl contaminated paint SO JOURNAL OF ENVIRONMENTAL MANAGEMENT LA English DT Article DE PCB; Remediation; Ball mill; Magnesium; Paint ID PCB; SEDIMENTS; DECHLORINATION; BUILDINGS; SOILS AB Restricted by federal regulations and limited remediation options, buildings contaminated with paint laden with polychlorinated biphenyls (PCBs) have high costs associated with the disposal of hazardous materials. As opposed to current remediation methods which are often destructive and a risk to the surrounding environment, this study suggests a non-metal treatment system (NMTS) and a bimetallic treatment system (BTS) as versatile remediation options for painted industrial structures including concrete buildings, and metal machine parts. In this field study, four areas of a discontinued Department of Defense site were treated and monitored over 3 weeks. PCB levels in paint and treatment system samples were analyzed through gas chromatography/electron capture detection (GC-ECD). PCB concentrations were reduced by 95 percent on painted concrete and by 60-97 percent on painted metal with the majority of the PCB removal occurring within the first week of application. Post treatment laboratory studies including the utilization of an activated metal treatment system (AMTS) further degraded PCBs in BTS and NMTS by up to 82 percent and 99 percent, respectively, indicating that a two-step remediation option is viable. These findings demonstrate that the NMTS and BTS can be an effective, nondestructive, remediation process for large painted structures, allowing for the reuse or sale of remediated materials that otherwise may have been disposed. (C) 2015 Elsevier Ltd. All rights reserved. C1 [Saitta, Erin K. H.; Gittings, Michael J.; Novaes-Card, Simone; Clausen, Christian; Yestrebsky, Cherie L.] Univ Cent Florida, Dept Chem, Orlando, FL 32816 USA. [Quinn, Jacqueline] NASA, Kennedy Space Ctr, FL 32899 USA. [O'Hara, Suzanne] Geosyntec Consultants, Guelph, ON N1GG3, Canada. RP Yestrebsky, CL (reprint author), Univ Cent Florida, Dept Chem, 4000 Cent Florida Blvd, Orlando, FL 32816 USA. EM erin.saitta@ucf.edu; michael.gittings@cardno.com; simone.novaes-card@agilent.com; Jacqueline.w.quinn@NASA.gov; christian.clausen@ucf.edu; SOHara@Geosyntec.com; cherie.yestrebsky@ucf.edu FU Environmental Security Technology Certification Program (ESTCP) [N62473-06-C-3034, RC-01610]; Geosyntec FX The authors would like to thank the Environmental Security Technology Certification Program (ESTCP) contract number (N62473-06-C-3034) and project number (RC-01610) for funding this research along with Geosyntec for their additional support. NR 27 TC 0 Z9 0 U1 6 U2 18 PU ACADEMIC PRESS LTD- ELSEVIER SCIENCE LTD PI LONDON PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND SN 0301-4797 EI 1095-8630 J9 J ENVIRON MANAGE JI J. Environ. Manage. PD AUG 1 PY 2015 VL 158 BP 40 EP 47 DI 10.1016/j.jenvman.2015.04.038 PG 8 WC Environmental Sciences SC Environmental Sciences & Ecology GA CK9GI UT WOS:000356548200005 PM 25950836 ER PT J AU Colliander, A Dinnat, E Le Vine, D Chae, CS Kainulainen, J AF Colliander, Andreas Dinnat, Emmanuel Le Vine, David Chae, Chun Sik Kainulainen, Juha TI Assessing Long-Term Stability of SMOS Zero-Baseline Antenna Temperature Using the Aquarius Antenna Temperature Simulator SO IEEE GEOSCIENCE AND REMOTE SENSING LETTERS LA English DT Article DE Aquarius; Soil Moisture and Ocean Salinity (SMOS) ID SOIL-MOISTURE; CALIBRATION; PERFORMANCE; RADIOMETER AB The National Aeronautics and Space Administration's Aquarius and the European Space Agency's Soil Moisture and Ocean Salinity (SMOS) are satellite missions to make global L-band brightness temperature measurements. Aquarius uses a sophisticated antenna temperature simulator over oceans for the calibration of its brightness temperature measurements. In this investigation, the simulator was adapted to simulate the real aperture antenna temperature measured by the SMOS reference radiometers. It is found that the simulated antenna temperature is very close to the measured value. The analysis shows that the simulated antenna temperature can be utilized for SMOS calibration studies as an additional independent reference, as well as for investigating the consistency between SMOS and Aquarius brightness temperature measurements. C1 [Colliander, Andreas; Chae, Chun Sik] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Dinnat, Emmanuel] Chapman Univ, Ctr Excellence Earth Syst Modeling, Orange, CA 92866 USA. [Dinnat, Emmanuel; Le Vine, David] NASA, Goddard Space Flight Ctr, Cryospher Sci Lab, Greenbelt, MD 20771 USA. [Kainulainen, Juha] Harp Technol Ltd, Espoo 02150, Finland. RP Colliander, A (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. EM andreas.colliander@jpl.nasa.gov; emmanuel.dinnat@nasa.gov; david.m.levine@nasa.gov; chun.sik.chae@jpl.nasa.gov; juha.kainulainen@harptechnologies.com RI Dinnat, Emmanuel/D-7064-2012 OI Dinnat, Emmanuel/0000-0001-9003-1182 NR 17 TC 2 Z9 2 U1 1 U2 2 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1545-598X EI 1558-0571 J9 IEEE GEOSCI REMOTE S JI IEEE Geosci. Remote Sens. Lett. PD AUG PY 2015 VL 12 IS 8 BP 1680 EP 1684 DI 10.1109/LGRS.2015.2419173 PG 5 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA CK9DZ UT WOS:000356542100018 ER PT J AU Liu, K Wu, LL Couture, RM Li, WQ Van Cappellen, P AF Liu, Kai Wu, Lingling Couture, Raoul-Marie Li, Weiqiang Van Cappellen, Philippe TI Iron isotope fractionation in sediments of an oligotrophic freshwater lake SO EARTH AND PLANETARY SCIENCE LETTERS LA English DT Article DE Fe isotope fractionation; sediments; oligotrophic lake; pore water; dissimilatory iron reduction ID OXIDE REDUCTION; MICROBIAL REDUCTION; SIDEROPHORE COMPLEX; CONTINENTAL-SHELF; EARLY DIAGENESIS; ANCIENT EARTH; FE ISOTOPES; REDOX; SEAWATER; GROUNDWATER AB In situ iron (Fe) isotope compositions of pore water and solid-bound Fe phases were measured in sediments of an oligotrophic, sulfate-poor freshwater lake (Lake Tantare, Quebec, Canada). Previous work has shown that dissimilatory Fe(III) reduction (DIR) is the main Fe reduction pathway in this setting. Hence, the lake sediments provide a well-characterized, natural environment in which to assess the transferability of DIR-produced Fe isotope fractionations obtained in laboratory model systems. Iron redox cycling within the sediments produces isotopically light pore water Fe(II) (average delta Fe-56 = -2.1 +/- 0.6 parts per thousand) and sorbed Fe(II) (average delta Fe-56 = -1.2 +/- 0.2 parts per thousand), compared to the Fe(III) oxyhydroxide (average delta Fe-56 = +0.6 +/- 0.2 parts per thousand) and tightly solid-bound Fe(II) (average delta Fe-56 = +0.3 +/- 0.2 parts per thousand) sediment pools. The apparent isotope fractionation factor between aqueous Fe(II) and Fe(III) oxyhydroxides of -2.6 +/- 0.5 parts per thousand derived for Lake Tantare sediments falls within the range reported for experimentally determined isotopic fractionations during DIR. Our results yield the first comprehensive set of Fe isotope signatures associated with microbially driven Fe redox cycling obtained directly in sediments of an oligotrophic freshwater lake. (C) 2015 Elsevier B.V. All rights reserved. C1 [Liu, Kai; Wu, Lingling; Couture, Raoul-Marie; Van Cappellen, Philippe] Univ Waterloo, Dept Earth & Environm Sci, Waterloo, ON N2L 3G1, Canada. [Liu, Kai; Wu, Lingling; Couture, Raoul-Marie; Van Cappellen, Philippe] Univ Waterloo, Water Inst, Waterloo, ON N2L 3G1, Canada. [Couture, Raoul-Marie] Norwegian Inst Water Res NIVA, Oslo, Norway. [Li, Weiqiang] Univ Wisconsin, Dept Geosci, Madison, WI USA. [Li, Weiqiang] Univ Wisconsin, NASA Astrobiol Inst, Madison, WI USA. [Li, Weiqiang] Nanjing Univ, Sch Earth Sci & Engn, State Key Lab Mineral Deposits Res, Nanjing, Peoples R China. RP Wu, LL (reprint author), Univ Waterloo, Dept Earth & Environm Sci, Waterloo, ON N2L 3G1, Canada. EM lingling.wu@uwaterloo.ca RI Li, Weiqiang/D-2975-2011; OI Li, Weiqiang/0000-0003-2648-7630; Couture, Raoul-Marie/0000-0003-4940-3372 FU NSERC Discovery grant [RGPIN-2014-05453]; Research Council of Norway [208279] FX K.L. is deeply indebted for the training on iron isotope analysis provided by Dr. Clark Johnson and Dr. Brian Beard at University of Wisconsin-Madison. We also thank them for providing valuable feedback that greatly improved the manuscript. We thank Dr. Charles Gobeil and Dr. Jade Bergeron (Universite du Quebec, INRS-ETE) for providing pore water & sediment samples. This study was supported by an NSERC Discovery grant awarded to L.W. (no. RGPIN-2014-05453). R.M.C. acknowledges funding from the Research Council of Norway (contract no. 208279). Two anonymous journal reviewers provided much appreciated comments and suggestions. NR 74 TC 4 Z9 4 U1 6 U2 31 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 AUG 1 PY 2015 VL 423 BP 164 EP 172 DI 10.1016/j.epsl.2015.05.010 PG 9 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA CK3LG UT WOS:000356117000016 ER PT J AU Islam, T Srivastava, PK AF Islam, Tanvir Srivastava, Prashant K. TI Synergistic multi-sensor and multi-frequency retrieval of cloud ice water path constrained by CloudSat collocations SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Article DE Satellite cloud retrieval; Passive microwave radiometry; Infrared and optical; Measurements synergy; Cloud profiling radar (CPR); Global precipitation measurement (GPM) ID SMOS SATELLITE; LIQUID WATER; RADIATION; MODEL; RADAR; SENSITIVITY; SURFACE; MICROPHYSICS; TOP AB The cloud ice water path (IWP) is one of the major parameters that have a strong influence on earth's radiation budget. Onboard satellite sensors are recognized as valuable tools to measure the IWP in a global scale. Albeit, active sensors such as the Cloud Profiling Radar (CPR) onboard the CloudSat satellite has better capability to measure the ice water content profile, thus, its vertical integral, IWP, than any passive microwave (MW) or infrared (IR) sensors. In this study, we investigate the retrieval of IWP from MW and IR sensors, including AMSU-A, MHS, and HIRS instruments on-board the N19 satellite, such that the retrieval is consistent with the CloudSat IWP estimates. This is achieved through the collocations between the passive satellite measurements and CloudSat scenes. Potential benefit of synergistic multi-sensor multi-frequency retrieval is investigated. Two modeling approaches are explored for the IWP retrieval - generalized linear model (GLM) and neural network (NN). The investigation has been carried out over both ocean and land surface types. The MW/IR synergy is found to be retrieved more accurate IWP than the individual AMSU-A, MHS, or HIRS measurements. Both GLM and NN approaches have been able to exploit the synergistic retrievals. (C) 2015 Elsevier Ltd. All rights reserved. C1 [Islam, Tanvir] NASA, Jet Prop Lab, Pasadena, CA 91109 USA. [Islam, Tanvir] CALTECH, Pasadena, CA 91125 USA. [Srivastava, Prashant K.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Srivastava, Prashant K.] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. RP Islam, T (reprint author), NASA, Jet Prop Lab, Pasadena, CA 91109 USA. EM tanvir.islam@jpl.nasa.gov OI Islam, Tanvir/0000-0003-2429-3074 NR 45 TC 0 Z9 0 U1 1 U2 9 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0022-4073 EI 1879-1352 J9 J QUANT SPECTROSC RA JI J. Quant. Spectrosc. Radiat. Transf. PD AUG PY 2015 VL 161 BP 21 EP 34 DI 10.1016/j.jqsrt.2015.03.022 PG 14 WC Optics; Spectroscopy SC Optics; Spectroscopy GA CK4LW UT WOS:000356196300003 ER PT J AU Long, DA Wojtewicz, S Miller, CE Hodges, JT AF Long, D. A. Wojtewicz, S. Miller, C. E. Hodges, J. T. TI Frequency-agile, rapid scanning cavity ring-down spectroscopy (FARS-CRDS) measurements of the (30012)<-(00001) near-infrared carbon dioxide band SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Article DE Carbon dioxide; Cavity ring-down spectroscopy; Line shape effects; Line mixing ID MU-M; ACETYLENE; POSITIONS; AIR; CO2; TRANSITIONS; INTENSITIES; STANDARD; LINES AB We present new high accuracy measurements of the (30012)<-(00001) CO2 band near 1575 nm recorded with a frequency-agile, rapid scanning cavity ring-down spectrometer. The resulting spectra were fit with the partially correlated, quadratic-speed-dependent Nelkin-Ghatak profile with line mixing. Significant differences were observed between the fitted line shape parameters and those found in existing databases, which are based upon more simplistic line profiles. Absolute transition frequencies, which were referenced to an optical frequency comb, are given, as well as the other line shape parameters needed to model this line profile. These high accuracy measurements should allow for improved atmospheric retrievals of greenhouse gas concentrations by current and future remote sensing missions. Published by Elsevier Ltd. C1 [Long, D. A.; Wojtewicz, S.; Hodges, J. T.] NIST, Mat Measurement Lab, Gaithersburg, MD 20899 USA. [Miller, C. E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Wojtewicz, S.] Nicholas Copernicus Univ, Inst Phys, Fac Phys Astron & Informat, PL-87100 Torun, Poland. RP Long, DA (reprint author), NIST, Mat Measurement Lab, 100 Bur Dr, Gaithersburg, MD 20899 USA. EM david.long@nist.gov RI Wojtewicz, Szymon/A-5425-2015 FU NIST Greenhouse Gas Measurements and Climate Research Program; Foundation for Polish Science TEAM Project; EU European Regional Development Fund; Orbiting Carbon Observatory (OCO-2) mission [11-OCO211-0006 NRA NNH11ZDA001N]; National Aeronautics and Space Administration (NASA) FX Support was provided by the NIST Greenhouse Gas Measurements and Climate Research Program. S. W. was partially supported by the Foundation for Polish Science TEAM Project co-financed by the EU European Regional Development Fund. Additional support was provided by the Orbiting Carbon Observatory (OCO-2) mission (11-OCO211-0006 NRA NNH11ZDA001N). The research performed at the Jet Propulsion Laboratory (JPL), California Institute of Technology was conducted under contract from the National Aeronautics and Space Administration (NASA). NR 27 TC 4 Z9 4 U1 2 U2 23 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0022-4073 EI 1879-1352 J9 J QUANT SPECTROSC RA JI J. Quant. Spectrosc. Radiat. Transf. PD AUG PY 2015 VL 161 BP 35 EP 40 DI 10.1016/j.jqsrt.2015.03.031 PG 6 WC Optics; Spectroscopy SC Optics; Spectroscopy GA CK4LW UT WOS:000356196300004 ER PT J AU Liu, CH Kim, YJ Chun, DW Kim, G Chen, RK Yu, AW Jin, SH AF Liu, Chin-Hung Kim, Young Jin Chun, Dong Won Kim, Gunwoo Chen, Renkun Yu, Anthony W. Jin, Sungho TI Universal solders for direct bonding and packaging of optical devices SO MATERIALS LETTERS LA English DT Article DE Lead-free universal solder; Low-temperature soldering; Non-linear optics; Thermal management ID LEAD-FREE SOLDERS; INTERFACIAL REACTIONS; RELIABILITY AB For optical packaging, there is a need to directly bond non-solderable materials such as oxides, nitrides, borides and fluorides, which are very difficult to wet/bond with low melting point solders, for example, at similar to 150 degrees C or below. In this research, we describe new Pb-free universal solders with low melting point of 140 degrees C or below by doping with a small amount of rare-earth elements, especially inexpensive mischmetals, which allow direct and powerful bonding onto the surfaces of various optical and electronic devices. The microstructure of the solder bonds is described, and their potential applications for passive and active optical components assembly are discussed. (C) 2015 Elsevier B.V. All rights reserved. C1 [Liu, Chin-Hung; Kim, Young Jin; Chun, Dong Won; Kim, Gunwoo; Chen, Renkun; Jin, Sungho] Univ Calif San Diego, Mat Sci & Engn, La Jolla, CA 92093 USA. [Yu, Anthony W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Jin, SH (reprint author), Univ Calif San Diego, Mat Sci & Engn, 9500 Gilman Dr, La Jolla, CA 92093 USA. EM jin@ucsd.edu FU Iwama Endowed Fund at UC San Diego; Sigma Space Corporation, United States FX The authors acknowledge the financial support of this work by Iwama Endowed Fund at UC San Diego and Sigma Space Corporation, United States. NR 15 TC 1 Z9 1 U1 2 U2 19 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0167-577X EI 1873-4979 J9 MATER LETT JI Mater. Lett. PD AUG 1 PY 2015 VL 152 BP 232 EP 236 DI 10.1016/j.matlet.2015.03.122 PG 5 WC Materials Science, Multidisciplinary; Physics, Applied SC Materials Science; Physics GA CK4IS UT WOS:000356188100063 ER PT J AU Channon, MB Gordon, GW Morgan, JLL Skulan, JL Smith, SM Anbar, AD AF Channon, Melanie B. Gordon, Gwyneth W. Morgan, Jennifer L. L. Skulan, Joseph L. Smith, Scott M. Anbar, Ariel D. TI Using natural, stable calcium isotopes of human blood to detect and monitor changes in bone mineral balance SO BONE LA English DT Article DE Biomarkers; Isotopes; Calcium; Bone loss ID DURATION SPACE-FLIGHT; MASS-SPECTROMETRY; CA ISOTOPES; BED REST; METABOLISM; FRACTIONATION; ABSORPTION; KINETICS; EXERCISE; URINE AB We are exploring variations in the Ca isotope composition of blood and urine as a new tool for early diagnosis and monitoring of changes in bone mineral balance for patients suffering from metabolic bone disease, cancers that originate in or metastasize to bone, and for astronauts who spend time in low gravity environments. Blood samples are often collected instead of, or in addition to, urine in clinical settings, so it is useful to know if variations in the Ca isotope composition of blood carry the same information as variations in urine. We found that the Ca isotope composition of blood shifts in the same direction and to the same magnitude (similar to 2 parts per ten thousand - pptt) as that of urine in response to skeletal unloading during bed rest. However, the Ca isotope composition of blood is lighter than that of urine by 12 +/- 2 pptt This offset between blood and urine may result from Ca isotope fractionation occurring in the kidneys. This is the first study to confirm the suspected offset between the Ca isotope composition of blood and urine in humans, to directly quantify its magnitude, and to establish that either blood or urine can be used to detect and quantify bone loss. (C) 2015 Elsevier Inc. All rights reserved. C1 [Channon, Melanie B.; Gordon, Gwyneth W.; Anbar, Ariel D.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [Morgan, Jennifer L. L.; Smith, Scott M.] NASA, Biomed Res & Environm Sci Div, Johnson Space Ctr, Houston, TX 77058 USA. [Skulan, Joseph L.] Letoile, Madison, WI 53703 USA. [Anbar, Ariel D.] Arizona State Univ, Dept Chem & Biochem, Tempe, AZ 85287 USA. RP Channon, MB (reprint author), ASU Sch Earth & Space Explorat, POB 871404, Tempe, AZ 85287 USA. EM mchannon@gmail.com FU National Center for Research Resources, National Institutes of Health [1UL1RR029876-01]; NASA Human Research Program's Human Health Countermeasures Element [07-HRP-2-0042, NNX-08Aq38G] FX We thank Stephen J. Romaniello for the help and discussions on the model, and NASA Johnson Space Center Nutritional Biochemistry Laboratory personnel for the sample processing. Bed rest studies were conducted at University of Texas Medical Branch at Galveston's Institute for Translational Sciences-Clinical Research Center, and were supported in part by the National Center for Research Resources, National Institutes of Health Grant 1UL1RR029876-01. This study was funded by the NASA Human Research Program's Human Health Countermeasures Element, grants 07-HRP-2-0042 and NNX-08Aq38G. NR 21 TC 8 Z9 8 U1 4 U2 29 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 8756-3282 EI 1873-2763 J9 BONE JI Bone PD AUG PY 2015 VL 77 BP 69 EP 74 DI 10.1016/j.bone.2015.04.023 PG 6 WC Endocrinology & Metabolism SC Endocrinology & Metabolism GA CJ7ZB UT WOS:000355717800010 PM 25900894 ER PT J AU Leon, JJD Garrett, MP Zhang, JC Kobayashi, NP AF Leon, Juan J. Diaz Garrett, Matthew P. Zhang, Junce Kobayashi, Nobuhiko P. TI Aluminum titanium oxide alloys: Deposition of amorphous, transparent, corrosion-resistant films by pulsed DC reactive magnetron sputtering with RF substrate bias SO MATERIALS SCIENCE IN SEMICONDUCTOR PROCESSING LA English DT Article DE Amorphous materials; Optical properties; Reactive sputtering; Aluminum titanium oxide; Barrier; Refractive index ID LOW-EMISSIVITY COATINGS; THIN-FILMS; BARRIER PROPERTIES; PERMEATION; LAYER; MICROSTRUCTURE; DURABILITY; DEVICES; ENERGY AB Optically transparent and mechanically flexible encapsulation films are desirable for advanced optoelectronic devices. Among many variations of encapsulation, ternary metal oxide films present good optical and mechanical properties. In this study, aluminum titanium oxide (Al1-xTixOy) films were deposited with a range of Ti/(Ti+Al) molar fractions (x) using pulsed DC magnetron sputtering with RF substrate bias. Subsequently, the films were subjected to an Accelerated Weathering Environment (AWE) test at 220 degrees C, 1.6 atm and similar to 100% RH for 3 h. Optical, chemical, and morphological analyses revealed that there exists a range of Ti/(Ti+Al) molar fraction (x=0.4-0.7) where films withstood the test, maintaining their optical, chemical, and morphological integrities. The study suggests that encapsulation films with continuously and spatially varying refractive index can be available by varying x within this range, forming encapsulation with broadband, wide angle antireflective coatings. (c) 2015 Elsevier Ltd. All rights reserved. C1 [Leon, Juan J. Diaz; Garrett, Matthew P.; Zhang, Junce; Kobayashi, Nobuhiko P.] Univ Calif Santa Cruz, Baskin Sch Engn, Santa Cruz, CA 95064 USA. [Leon, Juan J. Diaz; Garrett, Matthew P.; Zhang, Junce; Kobayashi, Nobuhiko P.] Univ Calif Santa Cruz, Adv Studies Labs, NECTAR, Santa Cruz, CA 95064 USA. [Leon, Juan J. Diaz; Garrett, Matthew P.; Zhang, Junce; Kobayashi, Nobuhiko P.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Leon, JJD (reprint author), Univ Calif Santa Cruz, Baskin Sch Engn, Santa Cruz, CA 95064 USA. EM jdiazleo@ucsc.edu FU Advanced Research Project Agency Energy FX We would like to thank the MACS facility (Moffett Field, California) at Advanced Studies Laboratories, University of California Santa Cruz, and NASA Ames Research Center for continuous support on analytical equipment. We acknowledge Kailas Vodrahalli and Jacob Jasser for their help on the AWE test. We acknowledge Dr. Tom Yuzvinsky for electron microscopy and the W.M. Keck Center for Nanoscale Optofluidics for use of the FEI Quanta 3D DualBeam microscope. We acknowledge Ernest R. Demaray for the deposition of the films and Tango Systems Inc. for use of their sputtering equipment. This study was supported by the Advanced Research Project Agency Energy. NR 30 TC 1 Z9 1 U1 1 U2 24 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 1369-8001 EI 1873-4081 J9 MAT SCI SEMICON PROC JI Mater. Sci. Semicond. Process PD AUG PY 2015 VL 36 BP 96 EP 102 DI 10.1016/j.mssp.2015.03.039 PG 7 WC Engineering, Electrical & Electronic; Materials Science, Multidisciplinary; Physics, Applied; Physics, Condensed Matter SC Engineering; Materials Science; Physics GA CJ3DM UT WOS:000355363600015 ER PT J AU Cochrane, CJ Blacksberg, J AF Cochrane, Corey J. Blacksberg, Jordana TI A Fast Classification Scheme in Raman Spectroscopy for the Identification of Mineral Mixtures Using a Large Database With Correlated Predictors SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE Classification; elastic net (EN); planetary mineralogy; Raman spectroscopy; regression ID PRINCIPAL COMPONENT ANALYSIS; REGRESSION; SPECTRA; LIBS; SPECTROMETER; EXPLORATION; SHRINKAGE; SELECTION; IMAGES AB Robust classification methods are vital to the successful implementation of many material characterization techniques, particularly where large databases exist. In this paper, we demonstrate an extremely fast classification method for the identification of mineral mixtures in Raman spectroscopy using the large RRUFF database. However, this method is equally applicable to other techniques meeting the large database criteria, these including laser-induced breakdown, X-ray diffraction, and mass spectroscopy methods. Classification of these multivariate datasets can be challenging due in part to the various obscuring features inherently present within the underlying dataset and in part to the volume and variety of information known a priori. Some of the more specific challenges include the observation of mixtures with overlapping spectral features, the use of large databases (i.e., the number of predictors far outweighs the number of observations), the use of databases that contain groups of correlated spectra, and the ever present, clouding contaminants of noise, undesired background, and spectrometer artifacts. Although many existing classification algorithms attempt to address these problems individually, not many address them as a whole. Here, we apply a multistage approach, which leverages well-established constrained regression techniques, to overcome these challenges. Our modifications to conventional algorithm implementations are shown to increase speed and performance of the classification process. Unlike many other techniques, our method is able to rapidly classify mixtures while simultaneously preserving sparsity. It is easily implemented, has very few tuning parameters, does not require extensive parameter training, and does not require data dimensionality reduction prior to classification. C1 [Cochrane, Corey J.; Blacksberg, Jordana] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Cochrane, CJ (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM corey.j.cochrane@jpl.nasa.gov; Jordana.Blacksberg@jpl.nasa.gov FU NASA FX This work was supported by an appointment to the NASA Postdoctoral Program at the Jet Propulsion Laboratory, administered by Oak Ridge Associated Universities through a contract with NASA. The work described in this publication was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration (NASA). NR 42 TC 2 Z9 2 U1 6 U2 63 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0196-2892 EI 1558-0644 J9 IEEE T GEOSCI REMOTE JI IEEE Trans. Geosci. Remote Sensing PD AUG PY 2015 VL 53 IS 8 BP 4259 EP 4274 DI 10.1109/TGRS.2015.2394377 PG 16 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA CE3XQ UT WOS:000351763800011 ER PT J AU Chen, S Zhang, J Mullens, E Hong, Y Behrangi, A Tian, YD Hu, XM Hu, JJ Zhang, ZX Zhang, XH AF Chen, Sheng Zhang, Jian Mullens, Esther Hong, Yang Behrangi, Ali Tian, Yudong Hu, Xiao-Ming Hu, Junjun Zhang, Zengxin Zhang, Xinhua TI Mapping the Precipitation Type Distribution Over the Contiguous United States Using NOAA/NSSL National Multi-Sensor Mosaic QPE SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE Radar; snow ID RADAR; CLIMATOLOGY; LAND; PRODUCT AB Understanding the Earth's energy cycle and water balance requires an understanding of the distribution of precipitation types and their total equivalent water budget estimation. The fine distribution of precipitation types over the contiguous United States (CONUS) is not yet well understood due to either unavailability or coarse resolution of previous satellite-and ground radar-based precipitation products that have difficulty in classifying precipitation. The newly available NOAA/National Severe Storms Laboratory ground radar network-based National Multi-Sensor Mosaic QPE (NMQ/Q2) System has provided precipitation rates and types at unprecedented high spatiotemporal resolution. Here, four years of 1 km/5 min observations derived from the NMQ are used to probe spatiotemporal distribution and characteristics of precipitation types (stratiform, convective, snow, tropical/warm (T/W), and hail) over CONUS, resulting in assessment of occurrence and volume contribution for these precipitation types through the four-year period, including seasonal distributions, with some radar coverage artifacts. These maps in general highlight the snow distribution over northwestern and northern CONUS, convective distribution over southwestern and central CONUS, hail distribution over central CONUS, and T/W distribution over southeastern CONUS. The total occurrences (contribution of total rain amount/volume) of these types are 72.88% (53.91%) for stratiform, 21.15% (7.64%) for snow, 2.95% (19.31%) for T/W, 2.77% (14.03%) for convective, and 0.24% (5.11%) for hail. This paper makes it possible to prototype a near seamless high-resolution reference for evaluating satellite swath-based precipitation type retrievals and also a potentially useful forcing database for energy-water balance budgeting and hydrological prediction for the United States. C1 [Chen, Sheng] Chinese Acad Sci, Xinjiang Inst Ecol & Geog, State Key Labaratory Desert & Oasis Ecol, Urumqi 830011, Peoples R China. [Chen, Sheng; Hong, Yang] Univ Oklahoma, Sch Civil Engn & Environm Sci, Norman, OK 73019 USA. [Zhang, Jian] NOAA, Natl Severe Storms Lab, Norman, OK 73072 USA. [Mullens, Esther] Univ Oklahoma, South Cent Climate Sci Ctr, Norman, OK 73019 USA. [Hong, Yang] Univ Oklahoma, Sch Meteorol, Norman, OK 73019 USA. [Hong, Yang] Univ Oklahoma, Adv Radar Res Ctr, Norman, OK 73019 USA. [Behrangi, Ali] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Tian, Yudong] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20740 USA. [Tian, Yudong] NASA, Hydrol Sci Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Hu, Xiao-Ming] Univ Oklahoma, Ctr Anal & Predict Storms, Norman, OK 73072 USA. [Hu, Junjun] Univ Oklahoma, Sch Comp Sci, Norman, OK 73072 USA. [Zhang, Zengxin] Nanjing Forestry Univ, Coll Biol & Environm, Joint Innovat Ctr Modern Forestry Studies, Nanjing 210037, Jiangsu, Peoples R China. [Zhang, Xinhua] Sichuan Univ, State Key Lab Hydraul & Mt River Engn, Chengdu 610065, Peoples R China. RP Hong, Y (reprint author), Univ Oklahoma, Sch Civil Engn & Environm Sci, Norman, OK 73019 USA. EM chenshengbj@gmail.com; yanghong@ou.edu RI Hu, Xiao-Ming/D-8085-2011; Hong, Yang/D-5132-2009 OI Hu, Xiao-Ming/0000-0002-0769-5090; Hong, Yang/0000-0001-8720-242X FU Hydrometeorology and Remote Sensing (HyDROS) Laboratory at The University of Oklahoma; National Natural Science Foundation of China [51379137, 41371419]; State Key Laboratory of Hydraulics and Mountain River Engineering [SKHL1310] FX This work was supported in part by the Hydrometeorology and Remote Sensing (HyDROS) Laboratory at The University of Oklahoma, by the National Natural Science Foundation of China (No. 51379137, and No. 41371419), and by the State Key Laboratory of Hydraulics and Mountain River Engineering under Open Fund SKHL1310. (Corresponding authors: Yang Hong and Sheng Chen.) NR 29 TC 2 Z9 2 U1 3 U2 26 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0196-2892 EI 1558-0644 J9 IEEE T GEOSCI REMOTE JI IEEE Trans. Geosci. Remote Sensing PD AUG PY 2015 VL 53 IS 8 BP 4434 EP 4443 DI 10.1109/TGRS.2015.2399015 PG 10 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA CE3XQ UT WOS:000351763800023 ER PT J AU Chen, S Hong, Y Cao, Q Tian, YD Hu, JJ Zhang, XH Li, WY Carr, N Shen, XY Qiao, L AF Chen, Sheng Hong, Yang Cao, Qing Tian, Yudong Hu, Junjun Zhang, Xinhua Li, Weiyue Carr, Nicholas Shen, Xinyi Qiao, Lei TI Intercomparison of Precipitation Estimates From WSR-88D Radar and TRMM Measurement Over Continental United States SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE Quantitative precipitation estimation (QPE); radar; remote sensing; satellite ID NATIONAL MOSAIC QPE; VERSION 7; RAINFALL; PRODUCTS; ERROR; SCALES; AREAS; READY; TMPA AB This paper examines the spatial error structures of precipitation estimates derived from both WSR-88D ground radar measurements and National Aeronautics and Space Administration's Tropical Rainfall Measurement Mission (TRMM) satellite-based radar and passive microwave measurements. The surface and spaceborne precipitation products are systematically evaluated via comparison with the Climate Prediction Center Unified Gauge Analysis over the Continental United States (CONUS) from December 2008 through November 2010. The WSR-88D quantitative precipitation estimation (QPE) products analyzed include the national mosaic daily QPE products (Q2) and Stage II and Stage IV daily products. The TRMM QPE products analyzed include the version-7 real-time product 3B42RT and the research product 3B42 (3B42V7). The results of the comparison based on two-year mean daily precipitation over CONUS demonstrate the following: 1) 3B42V7 and Stage IV perform fairly similarly with correlation coefficients (CCs) of 0.92 and 0.91, relatively low (magnitude) relative biases (RBs) of -3.32% and -7.16%, and low root-mean-squared errors (RMSEs) of 0.49 and 0.54 mm/day, respectively; 2) the gauge-corrected daily Q2 product (Q2RadGC) is slightly inferior to the 3B42V7 and Stage IV products but outperforms both the real-time satellite-only product 3B42RT and the two radar-only products (Q2Rad and Stage II) in terms of both CC and RMSE; 3) Q2Rad shows similar performance to 3B42RT regarding RB and CC; and 4) Stage II has particularly poor performance and suffers from systematic precipitation overestimation, particularly in northeastern Oregon, northern Utah, northeastern Carolina, and northern Georgia. C1 [Chen, Sheng; Hong, Yang; Carr, Nicholas; Shen, Xinyi] Univ Oklahoma, Sch Civil Engn & Environm Sci, Norman, OK 73019 USA. [Chen, Sheng] Chinese Acad Sci, Xinjiang Inst Ecol & Geog, State Key Lab Desert & Oasis Ecol, Urumqi 830011, Peoples R China. [Hong, Yang; Carr, Nicholas] Univ Oklahoma, Adv Radar Res Ctr, Norman, OK 73019 USA. [Shen, Xinyi] Univ Connecticut, Dept Civil & Environm Engn, Storrs, CT 06269 USA. [Cao, Qing] Enterprise Elect Corp, Res & Innovat Div, Norman, OK 73072 USA. [Tian, Yudong] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20740 USA. [Tian, Yudong] NASA, Hydrol Sci Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Hu, Junjun] Univ Oklahoma, Sch Comp Sci, Norman, OK 73072 USA. [Zhang, Xinhua] Sichuan Univ, State Key Lab Hydraul & Mt River Engn, Chengdu 610065, Peoples R China. [Li, Weiyue] Shanghai Normal Univ, Inst Urban Study, Shanghai 200234, Peoples R China. [Qiao, Lei] Oklahoma State Univ, Dept Nat Resource Ecol & Management, Stillwater, OK 74078 USA. RP Chen, S (reprint author), Univ Oklahoma, Sch Civil Engn & Environm Sci, Norman, OK 73019 USA. EM chenshengbj@gmail.com; yanghong@ou.edu; xhzhang@scu.edu.cn RI Hong, Yang/D-5132-2009 OI Hong, Yang/0000-0001-8720-242X FU Hydrometeorology and Remote Sensing Laboratory at the University of Oklahoma; Natural Science Foundation of Guangxi, China [2012GXNSFBA053133, 2013GXNSFAA019288]; Natural Science Foundation of China [51379137, 41371419]; State Key Laboratory of Hydraulics and Mountain River Engineering [SKHL1310] FX This work was supported in part by the Hydrometeorology and Remote Sensing Laboratory at the University of Oklahoma, by the Natural Science Foundation of Guangxi, China (2012GXNSFBA053133, and No. 2013GXNSFAA019288), by the Natural Science Foundation of China (No. 51379137, and No. 41371419), and by the open fund from the State Key Laboratory of Hydraulics and Mountain River Engineering (SKHL1310). NR 42 TC 3 Z9 3 U1 2 U2 23 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0196-2892 EI 1558-0644 J9 IEEE T GEOSCI REMOTE JI IEEE Trans. Geosci. Remote Sensing PD AUG PY 2015 VL 53 IS 8 BP 4444 EP 4456 DI 10.1109/TGRS.2015.2399307 PG 13 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA CE3XQ UT WOS:000351763800024 ER PT J AU Doelling, DR Wu, AS Xiong, XX Scarino, BR Bhatt, R Haney, CO Morstad, D Gopalan, A AF Doelling, David R. Wu, Aisheng Xiong, Xiaoxiong Scarino, Benjamin R. Bhatt, Rajendra Haney, Conor O. Morstad, Daniel Gopalan, Arun TI The Radiometric Stability and Scaling of Collection 6 Terra-and Aqua-MODIS VIS, NIR, and SWIR Spectral Bands SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE Intercalibration; Moderate Resolution Imaging Spectroradiometer (MODIS); pseudoinvariant calibration sites (PICS); radiometric scaling ID INTER-CALIBRATION; SOLAR; SYSTEM; CLOUDS; FLUX; REFLECTANCE; INSTRUMENT; MISSION; AVHRR; CERES AB The Moderate Resolution Imaging Spectroradiometer (MODIS) Calibration Team has recently released the Collection 6 (C6) radiances, which offer broad improvements over Collection 5 (C5). The recharacterization of the solar diffuser, lunar measurements, and scan mirror angle corrections removed most of the visible channel calibration drifts. The visible band calibration stability was validated over the Libyan Desert, Dome-C, and deep convective cloud (DCC) invariant Earth targets, for wavelengths less than 1 mu m. The lifetime stability of Terra and Aqua C6 is both within 1%, whereas the Terra C5 degradation exceeded 2% for most visible bands. The MODIS lifetime radiance trends over the invariant targets are mostly within 1%; however, the band-specific target fluctuations are inconsistent, which suggests that the stability limits of the invariant targets have been reached. Based on Terra-and Aqua-MODIS nearly simultaneous nadir overpass (NSNO) radiance comparisons, the Terra and Aqua C6 calibration shows agreement within 1.2%, whereas the C5 calibration exceeds 2%. Because the MODIS instruments are alike, the same NSNOs are used to radiometrically scale the Terra radiances to Aqua. For most visible bands, the Terra-scaled and Aqua C6 radiances are consistent to within 0.5% over Dome-C, DCC, and for geostationary visible imagers having similar spectral response functions, which are used as transfer radiometers. For bands greater than 1 mu m, only minor calibration adjustments were made, and the C6 calibration is stable within 1% based on Libya-4. C1 [Doelling, David R.] NASA, Climate Sci Branch, Langley Res Ctr, Hampton, VA 23681 USA. [Wu, Aisheng] Sigma Space Corp, Lanham, MD 20706 USA. [Xiong, Xiaoxiong] NASA, Sci & Explorat Directorate, Goddard Space Flight Ctr, Greenbelt, MD USA. [Scarino, Benjamin R.; Bhatt, Rajendra; Haney, Conor O.; Morstad, Daniel; Gopalan, Arun] Sci Syst & Applicat Inc, Hampton, VA 23666 USA. RP Doelling, DR (reprint author), NASA, Climate Sci Branch, Langley Res Ctr, Hampton, VA 23681 USA. EM david.r.doelling@nasa.gov; Aisheng.Wu@sigmaspace.com; xiaoxiong.xiong-1@nasa.gov; Benjamin.r.scarino@nasa.gov; rajendra.bhatt@nasa.gov; conor.o.haney@nasa.gov; Daniel.morstad@nasa.gov; arun.gopalan-1@nasa.gov RI Richards, Amber/K-8203-2015 FU National Aeronautics and Space Administration Earth Science Enterprise Office through the Clouds and the Earth's Radiant Energy System Program; National Aeronautics and Space Administration Earth Science Enterprise Office through the Satellite Calibration Inter-consistency Program; National Atmospheric and Oceanic Administration Climate Data Records Program [MOA IA1-1016] FX This work was supported in part by the National Aeronautics and Space Administration Earth Science Enterprise Office through the Clouds and the Earth's Radiant Energy System and the Satellite Calibration Inter-consistency Programs and in part by the National Atmospheric and Oceanic Administration Climate Data Records Program under Grant MOA IA1-1016. NR 45 TC 18 Z9 18 U1 1 U2 23 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0196-2892 EI 1558-0644 J9 IEEE T GEOSCI REMOTE JI IEEE Trans. Geosci. Remote Sensing PD AUG PY 2015 VL 53 IS 8 BP 4520 EP 4535 DI 10.1109/TGRS.2015.2400928 PG 16 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA CE3XQ UT WOS:000351763800030 ER PT J AU Nieves, V Willis, JK Patzert, WC AF Nieves, Veronica Willis, Josh K. Patzert, William C. TI Recent hiatus caused by decadal shift in Indo-Pacific heating SO SCIENCE LA English DT Article ID WARMING HIATUS; INDONESIAN THROUGHFLOW; OCEAN; VARIABILITY; REANALYSIS AB Recent modeling studies have proposed different scenarios to explain the slowdown in surface temperature warming in the most recent decade. Some of these studies seem to support the idea of internal variability and/or rearrangement of heat between the surface and the ocean interior. Others suggest that radiative forcing might also play a role. Our examination of observational data over the past two decades shows some significant differences when compared to model results from reanalyses and provides the most definitive explanation of how the heat was redistributed. We find that cooling in the top 100-meter layer of the Pacific Ocean was mainly compensated for by warming in the 100-to 300-meter layer of the Indian and Pacific Oceans in the past decade since 2003. C1 [Nieves, Veronica] Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA 90095 USA. [Nieves, Veronica; Willis, Josh K.; Patzert, William C.] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Nieves, V (reprint author), Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA 90095 USA. EM veronica.nieves@jpl.nasa.gov FU NASA; [NNN13D772T-10-OSST10-0015] FX The research described in this paper was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. This work was supported by grant NNN13D772T-10-OSST10-0015. NR 23 TC 22 Z9 23 U1 3 U2 42 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 JUL 31 PY 2015 VL 349 IS 6247 BP 532 EP 535 DI 10.1126/science.aaa4521 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CN8SP UT WOS:000358713300055 PM 26160379 ER PT J AU Goesmann, F Rosenbauer, H Bredehoft, JH Cabane, M Ehrenfreund, P Gautier, T Giri, C Kruger, H Le Roy, L MacDermott, AJ McKenna-Lawlor, S Meierhenrich, UJ Caro, GMM Raulin, F Roll, R Steele, A Steininger, H Sternberg, R Szopa, C Thiemann, W Ulamec, S AF Goesmann, Fred Rosenbauer, Helmut Bredehoeft, Jan Hendrik Cabane, Michel Ehrenfreund, Pascale Gautier, Thomas Giri, Chaitanya Krueger, Harald Le Roy, Lena MacDermott, Alexandra J. McKenna-Lawlor, Susan Meierhenrich, Uwe J. Munoz Caro, Guillermo M. Raulin, Francois Roll, Reinhard Steele, Andrew Steininger, Harald Sternberg, Robert Szopa, Cyril Thiemann, Wolfram Ulamec, Stephan TI Organic compounds on comet 67P/Churyumov-Gerasimenko revealed by COSAC mass spectrometry SO SCIENCE LA English DT Article ID PREBIOTIC CHEMISTRY; ORIGIN; ION AB Comets harbor the most pristine material in our solar system in the form of ice, dust, silicates, and refractory organic material with some interstellar heritage. The evolved gas analyzer Cometary Sampling and Composition (COSAC) experiment aboard Rosetta's Philae lander was designed for in situ analysis of organic molecules on comet 67P/Churyumov-Gerasimenko. Twenty-five minutes after Philae's initial comet touchdown, the COSAC mass spectrometer took a spectrum in sniffing mode, which displayed a suite of 16 organic compounds, including many nitrogen-bearing species but no sulfur-bearing species, and four compounds-methyl isocyanate, acetone, propionaldehyde, and acetamide-that had not previously been reported in comets. C1 [Goesmann, Fred; Rosenbauer, Helmut; Giri, Chaitanya; Krueger, Harald; Munoz Caro, Guillermo M.; Roll, Reinhard; Steininger, Harald] Max Planck Inst Solar Syst Res, D-37077 Gottingen, Germany. [Bredehoeft, Jan Hendrik; Thiemann, Wolfram] Univ Bremen, Inst Appl & Phys Chem, D-28359 Bremen, Germany. [Cabane, Michel; Szopa, Cyril] Univ Paris 06, Sorbonne Univ, Univ Versailles St Quentin,IPSL, CNRS,Inst Natl Sci Univers,Lab Atmospheres Milieu, F-75005 Paris, France. [Ehrenfreund, Pascale] Leiden Observ, NL-2300 RA Leiden, Netherlands. [Ehrenfreund, Pascale] George Washington Univ, Inst Space Policy, Washington, DC 20052 USA. [Gautier, Thomas] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Giri, Chaitanya; Meierhenrich, Uwe J.] Univ Nice Sophia Antipolis, Inst Chim Nice, CNRS, UMR 7272, F-06108 Nice, France. [Le Roy, Lena] Univ Bern, Ctr Space & Habitabil, CH-3012 Bern, Switzerland. [MacDermott, Alexandra J.] Univ Houston Clear Lake City, Houston, TX 77058 USA. [McKenna-Lawlor, Susan] Space Technol Ireland Ltd, Maynooth, Kildare, Ireland. [Munoz Caro, Guillermo M.] CSIC, Inst Nacl Tecn Aeroespacial, Ctr Astrobiol, Madrid 28850, Spain. [Raulin, Francois; Sternberg, Robert] Univ Paris Est Creteil, UMR CNRS 7583, LISA, F-94000 Creteil, France. [Raulin, Francois; Sternberg, Robert] Univ Paris Diderot, F-94000 Creteil, France. [Steele, Andrew] Carnegie Inst Sci, Geophys Lab, Washington, DC USA. [Ulamec, Stephan] Deutsch Zentrum Luft & Raumfahrt DLR, German Aerosp Ctr, D-51147 Cologne, Germany. RP Goesmann, F (reprint author), Max Planck Inst Solar Syst Res, Justus von Liebig Weg 3, D-37077 Gottingen, Germany. EM goesmann@mps.mpg.de RI Meierhenrich, Uwe/A-1643-2008; szopa, cyril/C-6865-2015; OI Meierhenrich, Uwe/0000-0001-6422-3930; szopa, cyril/0000-0002-0090-4056; Le Roy, Lena/0000-0002-5984-6153 FU Deutsches Zentrum fur Luft- und Raumfahrt (DLR) [50 QP 1302]; Centre National d'Etudes Spatiales (CNES) grant at LATMOS; Centre National d'Etudes Spatiales (CNES) grant LISA; L'Agence Nationale de la Recherche [ANR-12-IS07-0006]; NASA Astrobiology Institute; NASA Postdoctoral Program at Goddard Space Flight Center; Programme de Developpement d'Experiences scientifiques through Enterprise Ireland; Welch Foundation FX This work was supported by Deutsches Zentrum fur Luft- und Raumfahrt (DLR) under contract no. 50 QP 1302, and by Centre National d'Etudes Spatiales (CNES) grants at LATMOS and LISA. U.J.M. was funded by L'Agence Nationale de la Recherche (ANR-12-IS07-0006). Support from the NASA Astrobiology Institute (P.E.), the NASA Postdoctoral Program at Goddard Space Flight Center (T.G.), Programme de Developpement d'Experiences scientifiques through Enterprise Ireland (S. McK.L.), and the Welch Foundation (A.J.MacD.) is acknowledged. Rosetta is a European Space Agency (ESA) mission with contributions from member states and NASA. The Philae lander was provided by a consortium led by DLR, Max-Planck-Institut fur Sonnensystemforschung, CNES, and Agenzia Spatiale Italiana. The data used in this study are available through ESA's Planetary Science Archive (www.rssd.esa.int/index.php? project=PSA&page=rosetta). NR 23 TC 49 Z9 51 U1 23 U2 91 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 JUL 31 PY 2015 VL 349 IS 6247 AR aab0689 DI 10.1126/science.aab0689 PG 3 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CN8SP UT WOS:000358713300008 PM 26228156 ER PT J AU Kofman, W Herique, A Barbin, Y Barriot, JP Ciarletti, V Clifford, S Edenhofer, P Elachi, C Eyraud, C Goutail, JP Heggy, E Jorda, L Lasue, J Levasseur-Regourd, AC Nielsen, E Pasquero, P Preusker, F Puget, P Plettemeier, D Rogez, Y Sierks, H Statz, C Svedhem, H Williams, I Zine, S Van Zyl, J AF Kofman, Wlodek Herique, Alain Barbin, Yves Barriot, Jean-Pierre Ciarletti, Valerie Clifford, Stephen Edenhofer, Peter Elachi, Charles Eyraud, Christelle Goutail, Jean-Pierre Heggy, Essam Jorda, Laurent Lasue, Jeremie Levasseur-Regourd, Anny-Chantal Nielsen, Erling Pasquero, Pierre Preusker, Frank Puget, Pascal Plettemeier, Dirk Rogez, Yves Sierks, Holger Statz, Christoph Svedhem, Hakan Williams, Iwan Zine, Sonia Van Zyl, Jakob TI Properties of the 67P/Churyumov-Gerasimenko interior revealed by CONSERT radar SO SCIENCE LA English DT Article ID POLAR LAYERED DEPOSITS; COMET 67P/CHURYUMOV-GERASIMENKO; SUBSURFACE; STARDUST; NUCLEUS; MARS; PERMITTIVITY; 81P/WILD-2; FREQUENCY; ICE AB The Philae lander provides a unique opportunity to investigate the internal structure of a comet nucleus, providing information about its formation and evolution in the early solar system. We present Comet Nucleus Sounding Experiment by Radiowave Transmission (CONSERT) measurements of the interior of Comet 67P/Churyumov-Gerasimenko. From the propagation time and form of the signals, the upper part of the "head" of 67P is fairly homogeneous on a spatial scale of tens of meters. CONSERT also reduced the size of the uncertainty of Philae's final landing site down to approximately 21 by 34 square meters. The average permittivity is about 1.27, suggesting that this region has a volumetric dust/ice ratio of 0.4 to 2.6 and a porosity of 75 to 85%. The dust component may be comparable to that of carbonaceous chondrites. C1 [Kofman, Wlodek; Herique, Alain; Pasquero, Pierre; Puget, Pascal; Rogez, Yves; Zine, Sonia] Univ Grenoble Alpes, IPAG, F-38000 Grenoble, France. [Barbin, Yves] CNRS, IPAG, F-38000 Grenoble, France. [Barbin, Yves] Aix Marseille Univ, Univ Toulon, INSU, CNRS,MIO,IRD,UM 110, F-83957 La Garde, France. [Barriot, Jean-Pierre] Geodesy Observ Tahiti, Faaa 98702, Tahiti, Fr Polynesia. [Ciarletti, Valerie; Goutail, Jean-Pierre] Univ Versailles St Quentin En Yvelines UVSQ, UPSay, F-78280 Guyancourt, France. Univ Paris 06, Sorbonne Univ, F-78280 Guyancourt, France. [Ciarletti, Valerie; Goutail, Jean-Pierre] CNRS INSU, F-78280 Guyancourt, France. [Ciarletti, Valerie; Goutail, Jean-Pierre] Inst Pierre Simon Laplace, Lab Atmospheres Milieux Observat Spatiales LATMOS, F-78280 Guyancourt, France. [Clifford, Stephen] Lunar & Planetary Inst, Houston, TX 77058 USA. [Edenhofer, Peter] Ruhr Univ Bochum, Fac Elect Engn & Informat Technol, D-44780 Bochum, Germany. [Elachi, Charles; Heggy, Essam; Van Zyl, Jakob] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Nielsen, Erling; Sierks, Holger] Max Planck Inst Sonnensyst Forsch MPS, D-37077 Gottingen, Germany. [Plettemeier, Dirk; Statz, Christoph] Tech Univ Dresden, D-01069 Dresden, Germany. [Svedhem, Hakan] ESA, European Space Res & Technol Ctr ESTEC Noordwijk, Noordwijk, Netherlands. [Williams, Iwan] Queen Mary Univ London, London E1 4NS, England. [Jorda, Laurent] Lab Astrophys Marseille Pole Etoile, F-13388 Marseille, France. [Levasseur-Regourd, Anny-Chantal] Univ Paris 06, Sorbonne Univ, F-75005 Paris, France. [Levasseur-Regourd, Anny-Chantal] UVSQ, UPSay, F-75005 Paris, France. [Levasseur-Regourd, Anny-Chantal] CNRS, INSU, F-75005 Paris, France. [Levasseur-Regourd, Anny-Chantal] LATMOS IPSL, BC 102, F-75005 Paris, France. [Lasue, Jeremie] Univ Toulouse, F-31028 Toulouse, France. [Lasue, Jeremie] UPS OMP, F-31028 Toulouse, France. [Lasue, Jeremie] IRAP, F-31028 Toulouse, France. [Lasue, Jeremie] 2 CNRS, F-31028 Toulouse, France. [Eyraud, Christelle] Aix Marseille Univ, CNRS, Cent Marseille, Inst Fresnel UMR 7249, F-13013 Marseille, France. [Preusker, Frank] German Aerosp Ctr DLR, D-12489 Berlin, Germany. [Heggy, Essam] Univ So Calif, Ming Hsieh Dept Elect Engn, Viterbi Sch Engn, Los Angeles, CA 90089 USA. RP Kofman, W (reprint author), Univ Grenoble Alpes, IPAG, F-38000 Grenoble, France. EM wlodek.kofman@obs.ujf-grenoble.fr RI Kofman, Wlodek/C-4556-2008; Herique, Alain/E-7210-2017; OI Herique, Alain/0000-0003-3699-883X; Zine, Sonia/0000-0002-2872-0291 FU CNES; CNRS; Universite Joseph Fourier (UJF); DLR; MPS; Rhone-Alpes region [CPER07_13 CIRA]; OSUG@2020 labex [ANR10 LABX56]; Equip@Meso project of the program Investissements d'Avenir [ANR-10-EQPX-29-01] FX Rosetta is an European Space Agency (ESA) mission with contributions from its member states and National Aeronautics and Space Administration (NASA). Rosetta's Philae lander is provided by a consortium led by Deutsches Zentrum fur Luft- und Raumfahrt (DLR), Max Planck Institut fur Sonnesystemforschung (MPS), Centre National d'Etudes Spatiales (CNES), and Agenzia Spaziale Italiana (ASI). The CONSERT instrument was designed, built, and operated by IPAG, LATMOS, and MPS and was financially supported by CNES, CNRS, Universite Joseph Fourier (UJF), DLR, and MPS. The authors thank the teams of Rosetta [Rosetta Mission Operation Center (RMOC) and Rosetta Science Ground Segment (RSGS)] and Philae (Rosetta Lander Control Center (LCC) and Rosetta Lander Science Operation & Navigation Center (SONC)) for making possible the CONSERT operations. Most of the computations presented in this paper were performed using the Calcul Intensif, Modelisation, Experimentation Numerique (CIMENT) infrastructure (https://ciment.ujf-grenoble.fr), including the Froggy platform, which is supported by the Rhone-Alpes region (GRANT CPER07_13 CIRA), the OSUG@2020 labex (reference ANR10 LABX56), the Equip@Meso project (reference ANR-10-EQPX-29-01) of the program Investissements d'Avenir supervised by the Agence Nationale pour la Recherche and France-Grille (www.france-grilles.fr). 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. All CONSERT data are released through the PSA archive of ESA (www.rssd.esa.int/index.php?project=PSA&page=rosetta). NR 28 TC 23 Z9 23 U1 3 U2 10 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 JUL 31 PY 2015 VL 349 IS 6247 AR aab0639 DI 10.1126/science.aab0639 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CN8SP UT WOS:000358713300005 PM 26228153 ER PT J AU Hallinan, G Littlefair, SP Cotter, G Bourke, S Harding, LK Pineda, JS Butler, RP Golden, A Basri, G Doyle, JG Kao, MM Berdyugina, SV Kuznetsov, A Rupen, MP Antonova, A AF Hallinan, G. Littlefair, S. P. Cotter, G. Bourke, S. Harding, L. K. Pineda, J. S. Butler, R. P. Golden, A. Basri, G. Doyle, J. G. Kao, M. M. Berdyugina, S. V. Kuznetsov, A. Rupen, M. P. Antonova, A. TI Magnetospherically driven optical and radio aurorae at the end of the stellar main sequence SO NATURE LA English DT Article ID SIMULTANEOUS MULTIWAVELENGTH OBSERVATIONS; BROWN DWARF; ULTRACOOL DWARFS; MAGNETIC ACTIVITY; M8.5 DWARF; VARIABILITY; EMISSIONS; ROTATION; TEMPERATURE; TRANSITION AB Aurorae are detected from all the magnetized planets in our Solar System, including Earth(1). They are powered by magnetospheric current systems that lead to the precipitation of energetic electrons into the high-latitude regions of the upper atmosphere. In the case of the gas-giant planets, these aurorae include highly polarized radio emission at kilohertz and megahertz frequencies produced by the precipitating electrons(2), as well as continuum and line emission in the infrared, optical, ultraviolet and X-ray parts of the spectrum, associated with the collisional excitation and heating of the hydrogen-dominated atmosphere(3). Here we report simultaneous radio and optical spectroscopic observations of an object at the end of the stellar main sequence, located right at the boundary between stars and brown dwarfs, from which we have detected radio and optical auroral emissions both powered by magnetospheric currents. Whereas the magnetic activity of stars like our Sun is powered by processes that occur in their lower atmospheres, these aurorae are powered by processes originating much further out in the magnetosphere of the dwarf star that couple energy into the lower atmosphere. The dissipated power is at least four orders of magnitude larger than what is produced in the Jovian magnetosphere, revealing aurorae to be a potentially ubiquitous signature of large-scale magnetospheres that can scale to luminosities far greater than those observed in our Solar System. These magnetospheric current systems may also play a part in powering some of the weather phenomena reported on brown dwarfs. C1 [Hallinan, G.; Bourke, S.; Pineda, J. S.; Kao, M. M.] CALTECH, Pasadena, CA 91125 USA. [Littlefair, S. P.] Univ Sheffield, Dept Phys & Astron, Sheffield S3 7RH, S Yorkshire, England. [Cotter, G.] Univ Oxford, Dept Astrophys, Oxford OX1 3RH, England. [Harding, L. K.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Butler, R. P.] Natl Univ Ireland, Ctr Astron, Galway, Ireland. [Golden, A.] Yeshiva Univ, Dept Math Sci, New York, NY 10033 USA. [Basri, G.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Doyle, J. G.] Armagh Observ, Armagh BT61 9DG, North Ireland. [Berdyugina, S. V.] Kiepenheuer Inst Sonnenphys, D-79104 Freiburg, Germany. [Kuznetsov, A.] Inst Solar Terr Phys, Irkutsk 664033, Russia. [Rupen, M. P.] Natl Radio Astron Observ, Socorro, NM 87801 USA. [Antonova, A.] Sofia Univ St Kliment Ohridski, Dept Astron, Fac Phys, Sofia 1164, Bulgaria. RP Hallinan, G (reprint author), CALTECH, 1200 East Calif Blvd, Pasadena, CA 91125 USA. EM gh@astro.caltech.edu RI Butler, Ray/A-6705-2012; Kuznetsov, Alexey/Q-9294-2016; OI Butler, Ray/0000-0002-8441-7596; Kuznetsov, Alexey/0000-0001-8644-8372; Pineda, J. Sebastian/0000-0002-4489-0135; Littlefair, Stuart/0000-0001-7221-855X FU W.M. Keck Foundation; Northern Ireland Department of Culture, Arts and Leisure; National Science Foundation [AST-1212226/DGE-1144469]; University of Oxford; STFC [ST/M006190/1] FX We are grateful to T. Readhead, S. Kulkarni and J. McMullin for working to ensure that simultaneous Palomar and VLA observations could occur. We thank the staff of the Palomar Observatory, the W.M. Keck Observatory and the National Radio Astronomy Observatory for their support of this project. The W.M. Keck Observatory is operated as a scientific partnership among the California Institute of Technology, the University of California and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W.M. Keck Foundation. The VLA is operated by the National Radio Astronomy Observatory, a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. Armagh Observatory is grant-aided by the Northern Ireland Department of Culture, Arts and Leisure. G.H. acknowledges the generous support of D. Castleman and H. Rosen. This material is based upon work supported by the National Science Foundation under grant number AST-1212226/DGE-1144469. G.C. acknowledges support from the University of Oxford and from STFC grant ST/M006190/1. We thank J. Linsky and P. Goldreich for comments on this manuscript. NR 34 TC 17 Z9 17 U1 1 U2 12 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 EI 1476-4687 J9 NATURE JI Nature PD JUL 30 PY 2015 VL 523 IS 7562 BP 568 EP + DI 10.1038/nature14619 PG 8 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CN7ZL UT WOS:000358655200039 PM 26223623 ER PT J AU Ellis, DL Carter, JLW Ferry, MH AF Ellis, D. L. Carter, J. L. W. Ferry, M. H. TI A statistical study of the effects of processing upon the creep properties of GRCop-84 SO MATERIALS SCIENCE AND ENGINEERING A-STRUCTURAL MATERIALS PROPERTIES MICROSTRUCTURE AND PROCESSING LA English DT Article DE Creep properties; Processing; Texture; Copper alloy ID ALLOYS AB Reusable launch vehicles require main combustion chamber liner materials that can withstand elevated temperatures and high stresses without creeping. GRCop-84 (Cu-8 at% Cr-4 at% Nb) was developed to meet this need. The Cr2Nb precipitates formed in the alloy strengthen the Cu matrix by impeding dislocation motion and inhibiting grain growth. GRCop-84 has been produced in a variety of forms, each with a unique processing history. The creep properties of the various forms were compared, and results demonstrated that processing had a statistically significant, quantifiable effect upon the creep properties of GRCop-84. The differences in creep properties could largely be explained by texture, testing environment and scatter of the test results. Even with the statistical differences, GRCop-84 did not show grossly different creep results as a function of processing, indicating that any of the processing methods would be suitable for producing a rocket engine liner. Published by Elsevier B.V. C1 [Ellis, D. L.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. [Carter, J. L. W.] Univ Calif Davis, Davis, CA 95616 USA. [Ferry, M. H.] ATI Powder Met, Pittsburgh, PA 15205 USA. RP Ellis, DL (reprint author), NASA, Glenn Res Ctr, 21000 Brookpk Rd,MS 49-117, Cleveland, OH 44135 USA. EM david.l.ellis@nasa.gov; jwc137@case.edu; Matt.Ferry@ATImetals.com RI Carter, Jennifer/A-3241-2013 OI Carter, Jennifer/0000-0001-6702-729X NR 25 TC 0 Z9 0 U1 3 U2 4 PU ELSEVIER SCIENCE SA PI LAUSANNE PA PO BOX 564, 1001 LAUSANNE, SWITZERLAND SN 0921-5093 EI 1873-4936 J9 MAT SCI ENG A-STRUCT JI Mater. Sci. Eng. A-Struct. Mater. Prop. Microstruct. Process. PD JUL 29 PY 2015 VL 640 BP 1 EP 15 DI 10.1016/j.msea.2015.05.028 PG 15 WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary; Metallurgy & Metallurgical Engineering SC Science & Technology - Other Topics; Materials Science; Metallurgy & Metallurgical Engineering GA CN7PN UT WOS:000358626600001 ER PT J AU Nathal, MV Bierer, J Evans, L Pogue, EA Ritzert, F Gabb, TP AF Nathal, M. V. Bierer, J. Evans, L. Pogue, E. A. Ritzert, F. Gabb, T. P. TI Stress relaxation behavior in single crystal superalloys SO MATERIALS SCIENCE AND ENGINEERING A-STRUCTURAL MATERIALS PROPERTIES MICROSTRUCTURE AND PROCESSING LA English DT Article DE Mechanical characterization; Nickel based superalloys; Casting ID CREEP-PROPERTIES; SUPER-ALLOY; CMSX-4; TEMPERATURE AB The objective of this study was to examine the stress relaxation response and corresponding changes in microstructure of single crystal superalloys. The effects of temperature and time on stress relaxation response were examined for single crystal superalloys CMSX-4 and EPM-102. Stress-strain rate data from relaxation tests was in good agreement with constant load tests; it was further refined by testing samples from the same casting, and by eliminating the effects of primary creep in the stress relaxation test. From these tests, it was determined that EPM-102 had higher resistance to stress relaxation than CMSX-4 at and above 982 degrees C. Additionally, time-dependent strain recovery ("viscoelasticity") was observed after unloading during these tests. The single crystal alloys displayed directional coarsening after stress relaxation testing at high temperatures. Published by Elsevier B.V. C1 [Nathal, M. V.; Evans, L.; Ritzert, F.; Gabb, T. P.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. [Bierer, J.] Vantage Partners LLC, Cleveland, OH 44135 USA. [Pogue, E. A.] Univ Illinois, Dept Mat Sci & Engn, Urbana, IL 61801 USA. RP Gabb, TP (reprint author), NASA, Glenn Res Ctr, 21000 Brookpk Rd, Cleveland, OH 44135 USA. EM Timothy.P.Gabb@nasa.gov NR 23 TC 2 Z9 2 U1 4 U2 8 PU ELSEVIER SCIENCE SA PI LAUSANNE PA PO BOX 564, 1001 LAUSANNE, SWITZERLAND SN 0921-5093 EI 1873-4936 J9 MAT SCI ENG A-STRUCT JI Mater. Sci. Eng. A-Struct. Mater. Prop. Microstruct. Process. PD JUL 29 PY 2015 VL 640 BP 295 EP 304 DI 10.1016/j.msea.2015.05.102 PG 10 WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary; Metallurgy & Metallurgical Engineering SC Science & Technology - Other Topics; Materials Science; Metallurgy & Metallurgical Engineering GA CN7PN UT WOS:000358626600034 ER PT J AU Vikram, V Chang, C Jain, B Bacon, D Amara, A Becker, MR Bernstein, G Bonnett, C Bridle, S Brout, D Busha, M Frieman, J Gaztanaga, E Hartley, W Jarvis, M Kacprzak, T Kovacs, A Lahav, O Leistedt, B Lin, H Melchior, P Peiris, H Rozo, E Rykoff, E Sanchez, C Sheldon, E Troxel, MA Wechsler, R Zuntz, J Abbott, T Abdalla, FB Armstrong, R Banerji, M Bauer, AH Benoit-Levy, A Bertin, E Brooks, D Buckley-Geer, E Burke, DL Capozzi, D Rosell, AC Kind, MC Castander, FJ Crocce, M Cunha, CE D'Andrea, CB da Costa, LN Depoy, DL Desai, S Diehl, HT Dietrich, JP Estrada, J Evrard, AE Neto, AF Fernandez, E Flaugher, B Fosalba, P Gerdes, D Gruen, D Gruendl, RA Honscheid, K James, D Kent, S Kuehn, K Kuropatkin, N Li, TS Maia, MAG Makler, M March, M Marshall, J Martini, P Merritt, KW Miller, CJ Miquel, R Neilsen, E Nichol, RC Nord, B Ogando, R Plazas, AA Romer, AK Roodman, A Sanchez, E Scarpine, V Sevilla, I Smith, RC Soares-Santos, M Sobreira, F Suchyta, E Swanson, MEC Tarle, G Thaler, J Thomas, D Walker, AR Weller, J AF Vikram, V. Chang, C. Jain, B. Bacon, D. Amara, A. Becker, M. R. Bernstein, G. Bonnett, C. Bridle, S. Brout, D. Busha, M. Frieman, J. Gaztanaga, E. Hartley, W. Jarvis, M. Kacprzak, T. Kovacs, A. Lahav, O. Leistedt, B. Lin, H. Melchior, P. Peiris, H. Rozo, E. Rykoff, E. Sanchez, C. Sheldon, E. Troxel, M. A. Wechsler, R. Zuntz, J. Abbott, T. Abdalla, F. B. Armstrong, R. Banerji, M. Bauer, A. H. Benoit-Levy, A. Bertin, E. Brooks, D. Buckley-Geer, E. Burke, D. L. Capozzi, D. Carnero Rosell, A. Kind, M. Carrasco Castander, F. J. Crocce, M. Cunha, C. E. D'Andrea, C. B. da Costa, L. N. Depoy, D. L. Desai, S. Diehl, H. T. Dietrich, J. P. Estrada, J. Evrard, A. E. Fausti Neto, A. Fernandez, E. Flaugher, B. Fosalba, P. Gerdes, D. Gruen, D. Gruendl, R. A. Honscheid, K. James, D. Kent, S. Kuehn, K. Kuropatkin, N. Li, T. S. Maia, M. A. G. Makler, M. March, M. Marshall, J. Martini, P. Merritt, K. W. Miller, C. J. Miquel, R. Neilsen, E. Nichol, R. C. Nord, B. Ogando, R. Plazas, A. A. Romer, A. K. Roodman, A. Sanchez, E. Scarpine, V. Sevilla, I. Smith, R. C. Soares-Santos, M. Sobreira, F. Suchyta, E. Swanson, M. E. C. Tarle, G. Thaler, J. Thomas, D. Walker, A. R. Weller, J. TI Wide-field lensing mass maps from Dark Energy Survey science verification data: Methodology and detailed analysis SO PHYSICAL REVIEW D LA English DT Article ID MAXIMUM-LIKELIHOOD; SHEAR MEASUREMENT; GALAXY DISTRIBUTIONS; PEAK STATISTICS; CLUSTER SURVEYS; DATA RELEASE; NOISE BIAS; SDSS-III; WEAK; CONSTRAINTS AB Weak gravitational lensing allows one to reconstruct the spatial distribution of the projected mass density across the sky. These "mass maps" provide a powerful tool for studying cosmology as they probe both luminous and dark matter. In this paper, we present a weak lensing mass map reconstructed from shear measurements in a 139 deg(2) area from the Dark Energy Survey (DES) science verification data. We compare the distribution of mass with that of the foreground distribution of galaxies and clusters. The overdensities in the reconstructed map correlate well with the distribution of optically detected clusters. We demonstrate that candidate superclusters and voids along the line of sight can be identified, exploiting the tight scatter of the cluster photometric redshifts. We cross-correlate the mass map with a foreground magnitude-limited galaxy sample from the same data. Our measurement gives results consistent with mock catalogs from N-body simulations that include the primary sources of statistical uncertainties in the galaxy, lensing, and photo-z catalogs. The statistical significance of the cross-correlation is at the 6.8 sigma level with 20 arcminute smoothing. We find that the contribution of systematics to the lensing mass maps is generally within measurement uncertainties. In this work, we analyze less than 3% of the final area that will be mapped by the DES; the tools and analysis techniques developed in this paper can be applied to forthcoming larger data sets from the survey. C1 [Vikram, V.] Argonne Natl Lab, Lemont, IL 60439 USA. [Vikram, V.; Jain, B.; Bernstein, G.; Brout, D.; Jarvis, M.; Armstrong, R.; March, M.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. [Chang, C.; Amara, A.; Hartley, W.; Kacprzak, T.] Swiss Fed Inst Technol, Dept Phys, CH-8093 Zurich, Switzerland. [Bacon, D.; Capozzi, D.; D'Andrea, C. B.; Nichol, R. C.; Thomas, D.] Univ Portsmouth, Inst Cosmol & Gravitat, Portsmouth PO1 3FX, Hants, England. [Becker, M. R.; Busha, M.; Wechsler, R.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA. [Becker, M. R.; Busha, M.; Rykoff, E.; Wechsler, R.; Burke, D. L.; Roodman, A.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA. [Bonnett, C.; Kovacs, A.; Sanchez, C.; Fernandez, E.; Miquel, R.] Univ Autonoma Barcelona, Inst Fis Altes Energies, E-08193 Barcelona, Spain. [Bridle, S.; Troxel, M. A.; Zuntz, J.] Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England. [Frieman, J.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Frieman, J.; Lin, H.; Buckley-Geer, E.; Diehl, H. T.; Estrada, J.; Flaugher, B.; Kent, S.; Kuropatkin, N.; Merritt, K. W.; Neilsen, E.; Nord, B.; Scarpine, V.; Soares-Santos, M.; Sobreira, F.] Fermilab Natl Accelerator Lab, Batavia, IL 60510 USA. [Gaztanaga, E.; Bauer, A. H.; Castander, F. J.; Crocce, M.; Fosalba, P.] IEEC CSIC, Fac Ciencies, Inst Ciencies Espai, Barcelona 08193, Spain. [Lahav, O.; Leistedt, B.; Peiris, H.; Abdalla, F. B.; Benoit-Levy, A.; Brooks, D.] UCL, Dept Phys & Astron, London WC1E 6BT, England. [Melchior, P.; Martini, P.; Suchyta, E.] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA. [Melchior, P.; Martini, P.; Suchyta, E.] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA. [Rozo, E.] Univ Arizona, Dept Phys, Tucson, AZ 85721 USA. [Rykoff, E.; Wechsler, R.; Burke, D. L.; Roodman, A.] SLAC Natl Accelerator Lab, Menlo Pk, CA 94025 USA. [Sheldon, E.; Plazas, A. A.] Brookhaven Natl Lab, Upton, NY 11973 USA. [Abbott, T.; James, D.; Smith, R. C.; Walker, A. R.] Natl Opt Astron Observ, Cerro Tololo Inter Amer Observ, La Serena, Chile. [Banerji, M.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Banerji, M.] Univ Cambridge, Kavli Inst Cosmol, Cambridge CB3 0HA, England. [Bertin, E.] Univ Paris 06, Inst Astrophys Paris, F-75014 Paris, France. [Bertin, E.] CNRS UMR7095, F-75014 Paris, France. [Carnero Rosell, A.; da Costa, L. N.; Fausti Neto, A.; Maia, M. A. G.; Ogando, R.; Sobreira, F.] Lab Interinst E Astron LIneA, BR-20921400 Rio De Janeiro, RJ, Brazil. [Carnero Rosell, A.; da Costa, L. N.; Maia, M. A. G.; Ogando, R.] Observ Nacl, BR-20921400 Rio De Janeiro, RJ, Brazil. [Kind, M. Carrasco; Gruendl, R. A.; Honscheid, K.; Sevilla, I.; Thaler, J.] Univ Illinois, Dept Phys, Urbana, IL 61801 USA. [Kind, M. Carrasco; Gruendl, R. A.; Honscheid, K.; Swanson, M. E. C.] Univ Illinois, Natl Ctr Supercomp Applicat, Urbana, IL 61801 USA. [Cunha, C. E.] Robert Bosch LLC, Palo Alto, CA 94304 USA. [Depoy, D. L.; Li, T. S.; Marshall, J.] Texas A&M Univ, George P & Cynthia Woods Mitchell Inst Fundamenta, College Stn, TX 77843 USA. [Depoy, D. L.; Li, T. S.; Marshall, J.] Texas A&M Univ, Dept Phys & Astron, College Stn, TX 77843 USA. [Desai, S.; Dietrich, J. P.; Tarle, G.; Weller, J.] Univ Munich, Dept Phys, D-81679 Munich, Germany. [Dietrich, J. P.; Weller, J.] Excellence Cluster Universe, D-85748 Garching, Germany. [Evrard, A. E.; Gerdes, D.; Miller, C. J.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA. [Gruen, D.; Weller, J.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Gruen, D.] Univ Observ Munich, D-81679 Munich, Germany. [Kuehn, K.] Australian Astron Observ, N Ryde, NSW 2113, Australia. [Makler, M.] Ctr Brasileiro Pesquisas Fis, ICRA, BR-22290180 Rio De Janeiro, RJ, Brazil. [Miller, C. J.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Miquel, R.] Inst Catalana Recerca & Estudis Avancats, E-08010 Barcelona, Spain. [Plazas, A. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Romer, A. K.] Univ Sussex, Dept Phys & Astron, Brighton BN1 9QH, E Sussex, England. [Sanchez, E.; Sevilla, I.] Ctr Invest Energet Medioambientales & Tecnol CIEM, Madrid 28040, Spain. [Thomas, D.] South East Phys Network, SEPnet, Southampton SO17 1BJ, Hants, England. RP Chang, C (reprint author), Swiss Fed Inst Technol, Dept Phys, Wolfgang Pauli Str 16, CH-8093 Zurich, Switzerland. EM chihway.chang@phys.ethz.ch RI Ogando, Ricardo/A-1747-2010; Makler, Martin/G-2639-2012; Sanchez, Eusebio/H-5228-2015; Fosalba Vela, Pablo/I-5515-2016; Sobreira, Flavia/F-4168-2015; Fernandez, Enrique/L-5387-2014; Gaztanaga, Enrique/L-4894-2014; OI Weller, Jochen/0000-0002-8282-2010; Carrasco Kind, Matias/0000-0002-4802-3194; Ogando, Ricardo/0000-0003-2120-1154; Makler, Martin/0000-0003-2206-2651; Sanchez, Eusebio/0000-0002-9646-8198; Sobreira, Flavia/0000-0002-7822-0658; Fernandez, Enrique/0000-0002-6405-9488; Gaztanaga, Enrique/0000-0001-9632-0815; Becker, Matthew/0000-0001-7774-2246; Suchyta, Eric/0000-0002-7047-9358; Dietrich, Jorg/0000-0002-8134-9591; Banerji, Manda/0000-0002-0639-5141; Abdalla, Filipe/0000-0003-2063-4345 FU Swiss National Science Foundation [200021-149442, 200021-143906]; European Research Council [240672]; Deutsche Forschungsgemeinschaft (DFG) [SFB-Transregio 33]; DFG cluster of excellence "Origin and Structure of the Universe"; CAPES [3171-13-2]; European Research Council Advanced Grant [FP7/291329]; U.S. Department of Energy; U.S. National Science Foundation; Ministry of Science and Education of Spain; Science and Technology Facilities Council of the United Kingdom; Higher Education Funding Council for England; National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign; Kavli Institute of Cosmological Physics at the University of Chicago; Center for Cosmology and Astro-Particle Physics at the Ohio State University; Mitchell Institute for Fundamental Physics and Astronomy at Texas AM University; Financiadora de Estudos e Projetos; Fundacao Carlos Chagas Filho de Amparo a Pesquisa do Estado do Rio de Janeiro; Conselho Nacional de Desenvolvimento Cientifico e Tecnologico; Ministerio da Ciencia e Tecnologia; Deutsche Forschungsgemeinschaft; National Science Foundation [AST-1138766]; MINECO [AYA2012-39559, ESP2013-48274, FPA2013-47986]; Centro de Excelencia Severo Ochoa [SEV-2012-0234]; European Union; Argonne National Laboratory; University of California at Santa Cruz; University of Cambridge; Centro de Investigaciones Energeticas; Medioambientales y Tecnologicas-Madrid; University of Chicago; University College London; DES-Brazil Consortium; Eidgenossische Technische Hochschule (ETH) Zurich; Fermi National Accelerator Laboratory; University of Edinburgh; University of Illinois at Urbana-Champaign; Institut de Ciencies de l'Espai (IEEC/CSIC); Institut de Fisica d'Altes Energies; Lawrence Berkeley National Laboratory; Ludwig-Maximilians Universitat; associated Excellence Cluster Universe; University of Michigan; National Optical Astronomy Observatory; University of Nottingham; Ohio State University; University of Pennsylvania; University of Portsmouth; SLAC National Accelerator Laboratory; Stanford University; University of Sussex; Texas AM University FX We are grateful for the extraordinary contributions of our CTIO colleagues and the DECam Construction, Commissioning and science verification teams in achieving the excellent instrument and telescope conditions that have made this work possible. The success of this project also relies critically on the expertise and dedication of the DES Data Management group. We thank Jake VanderPlas, Andy Connolly, Phil Marshall, Ludo van Waerbeke, and Rafal Szepietowski for discussions and collaborative work on mass mapping methodology. C. C and A. A. are supported by the Swiss National Science Foundation Grants No. 200021-149442 and No. 200021-143906. S. B. and J. Z. acknowledge support from European Research Council Starting Grant No. 240672. D. G. was supported by SFB-Transregio 33 "The Dark Universe" by the Deutsche Forschungsgemeinschaft (DFG) and the DFG cluster of excellence "Origin and Structure of the Universe." F. S. acknowledges financial support provided by CAPES under Contract No. 3171-13-2. O. L. acknowledges support from a European Research Council Advanced Grant No. FP7/291329. Funding for the DES Projects has been provided by the U.S. Department of Energy, the U.S. National Science Foundation, the Ministry of Science and Education of Spain, the Science and Technology Facilities Council of the United Kingdom, the Higher Education Funding Council for England, the National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign, the Kavli Institute of Cosmological Physics at the University of Chicago, the Center for Cosmology and Astro-Particle Physics at the Ohio State University, the Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M University, Financiadora de Estudos e Projetos, Fundacao Carlos Chagas Filho de Amparo a Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Cientifico e Tecnologico and the Ministerio da Ciencia e Tecnologia, the Deutsche Forschungsgemeinschaft and the collaborating institutions in the Dark Energy Survey. The DES data management system is supported by the National Science Foundation under Grant No. AST-1138766. The DES participants from Spanish institutions are partially supported by MINECO under Grants No. AYA2012-39559, No. ESP2013-48274, No. FPA2013-47986, and Centro de Excelencia Severo Ochoa No. SEV-2012-0234, some of which include ERDF funds from the European Union. The collaborating institutions are Argonne National Laboratory, the University of California at Santa Cruz, the University of Cambridge, Centro de Investigaciones Energeticas, Medioambientales y Tecnologicas-Madrid, the University of Chicago, University College London, the DES-Brazil Consortium, the Eidgenossische Technische Hochschule (ETH) Zurich, Fermi National Accelerator Laboratory, the University of Edinburgh, the University of Illinois at Urbana-Champaign, the Institut de Ciencies de l'Espai (IEEC/CSIC), the Institut de Fisica d'Altes Energies, Lawrence Berkeley National Laboratory, the Ludwig-Maximilians Universitat and the associated Excellence Cluster Universe, the University of Michigan, the National Optical Astronomy Observatory, the University of Nottingham, The Ohio State University, the University of Pennsylvania, the University of Portsmouth, SLAC National Accelerator Laboratory, Stanford University, the University of Sussex, and Texas A&M University. This paper has gone through internal review by the DES Collaboration. NR 93 TC 23 Z9 23 U1 0 U2 5 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 JUL 29 PY 2015 VL 92 IS 2 AR 022006 DI 10.1103/PhysRevD.92.022006 PG 22 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA CO0OZ UT WOS:000358853000001 ER PT J AU Chang, C Vikram, V Jain, B Bacon, D Amara, A Becker, MR Bernstein, G Bonnett, C Bridle, S Brout, D Busha, M Frieman, J Gaztanaga, E Hartley, W Jarvis, M Kacprzak, T Kovacs, A Lahav, O Lin, H Melchior, P Peiris, H Rozo, E Rykoff, E Sanchez, C Sheldon, E Troxel, MA Wechsler, R Zuntz, J Abbott, T Abdalla, FB Allam, S Annis, J Bauer, AH Benoit-Levy, A Brooks, D Buckley-Geer, E Burke, DL Capozzi, D Rosell, AC Kind, MC Castander, FJ Crocce, M D'Andrea, CB Desai, S Diehl, HT Dietrich, JP Doel, P Eifler, TF Evrard, AE Neto, AF Flaugher, B Fosalba, P Gruen, D Gruendl, RA Gutierrez, G Honscheid, K James, D Kent, S Kuehn, K Kuropatkin, N Maia, MAG March, M Martini, P Merritt, KW Miller, CJ Miquel, R Neilsen, E Nichol, RC Ogando, R Plazas, AA Romer, AK Roodman, A Sako, M Sanchez, E Sevilla, I Smith, RC Soares-Santos, M Sobreira, F Suchyta, E Tarle, G Thaler, J Thomas, D Tucker, D Walker, AR AF Chang, C. Vikram, V. Jain, B. Bacon, D. Amara, A. Becker, M. R. Bernstein, G. Bonnett, C. Bridle, S. Brout, D. Busha, M. Frieman, J. Gaztanaga, E. Hartley, W. Jarvis, M. Kacprzak, T. Kovacs, A. Lahav, O. Lin, H. Melchior, P. Peiris, H. Rozo, E. Rykoff, E. Sanchez, C. Sheldon, E. Troxel, M. A. Wechsler, R. Zuntz, J. Abbott, T. Abdalla, F. B. Allam, S. Annis, J. Bauer, A. H. Benoit-Levy, A. Brooks, D. Buckley-Geer, E. Burke, D. L. Capozzi, D. Carnero Rosell, A. Kind, M. Carrasco Castander, F. J. Crocce, M. D'Andrea, C. B. Desai, S. Diehl, H. T. Dietrich, J. P. Doel, P. Eifler, T. F. Evrard, A. E. Fausti Neto, A. Flaugher, B. Fosalba, P. Gruen, D. Gruendl, R. A. Gutierrez, G. Honscheid, K. James, D. Kent, S. Kuehn, K. Kuropatkin, N. Maia, M. A. G. March, M. Martini, P. Merritt, K. W. Miller, C. J. Miquel, R. Neilsen, E. Nichol, R. C. Ogando, R. Plazas, A. A. Romer, A. K. Roodman, A. Sako, M. Sanchez, E. Sevilla, I. Smith, R. C. Soares-Santos, M. Sobreira, F. Suchyta, E. Tarle, G. Thaler, J. Thomas, D. Tucker, D. Walker, A. R. TI Wide-Field Lensing Mass Maps from Dark Energy Survey Science Verification Data SO PHYSICAL REVIEW LETTERS LA English DT Article ID SHEAR MEASUREMENT; DATA RELEASE; MATTER; CONSTRAINTS; CFHTLENS; SIMULATIONS; SEXTRACTOR; STATISTICS; COSMOLOGY; REDSHIFTS AB We present a mass map reconstructed from weak gravitational lensing shear measurements over 139 deg(2) from the Dark Energy Survey science verification data. The mass map probes both luminous and dark matter, thus providing a tool for studying cosmology. We find good agreement between the mass map and the distribution of massive galaxy clusters identified using a red-sequence cluster finder. Potential candidates for superclusters and voids are identified using these maps. We measure the cross-correlation between the mass map and a magnitude-limited foreground galaxy sample and find a detection at the 6.8 sigma level with 20 arc min smoothing. These measurements are consistent with simulated galaxy catalogs based on N-body simulations from a cold dark matter model with a cosmological constant. This suggests low systematics uncertainties in the map. We summarize our key findings in this Letter; the detailed methodology and tests for systematics are presented in a companion paper. C1 [Chang, C.; Amara, A.; Hartley, W.; Kacprzak, T.] ETH, Dept Phys, CH-8093 Zurich, Switzerland. [Vikram, V.] Argonne Natl Lab, Lemont, IL 60439 USA. [Vikram, V.; Jain, B.; Bernstein, G.; Brout, D.; Jarvis, M.; Eifler, T. F.; March, M.; Sako, M.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. [Bacon, D.; Capozzi, D.; D'Andrea, C. B.; Nichol, R. C.; Thomas, D.] Univ Portsmouth, Inst Cosmol & Gravitat, Portsmouth PO1 3FX, Hants, England. [Becker, M. R.; Busha, M.; Wechsler, R.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA. [Becker, M. R.; Busha, M.; Rykoff, E.; Wechsler, R.; Burke, D. L.; Roodman, A.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA. [Bonnett, C.; Kovacs, A.; Sanchez, C.; Miquel, R.] Univ Autonoma Barcelona, Inst Fis Altes Energies, E-08193 Bellaterra, Barcelona, Spain. [Bridle, S.; Troxel, M. A.; Zuntz, J.] Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England. [Frieman, J.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Frieman, J.; Lin, H.; Allam, S.; Annis, J.; Buckley-Geer, E.; Diehl, H. T.; Flaugher, B.; Gutierrez, G.; Kent, S.; Kuropatkin, N.; Merritt, K. W.; Neilsen, E.; Soares-Santos, M.; Sobreira, F.; Tucker, D.] Fermilab Natl Accelerator Lab, Batavia, IL 60510 USA. [Gaztanaga, E.; Bauer, A. H.; Castander, F. J.; Crocce, M.; Fosalba, P.] CSIC, IEEC, Fac Ciencies, Inst Ciencies Espai, Bellaterra 08193, Barcelona, Spain. [Lahav, O.; Peiris, H.; Abdalla, F. B.; Benoit-Levy, A.; Brooks, D.; Doel, P.] UCL, Dept Phys & Astron, London WC1E 6BT, England. [Melchior, P.; Martini, P.; Suchyta, E.] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA. [Melchior, P.; Martini, P.; Suchyta, E.] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA. [Rozo, E.] Univ Arizona, Dept Phys, Tucson, AZ 85721 USA. [Rykoff, E.; Wechsler, R.; Burke, D. L.; Roodman, A.] SLAC Natl Accelerator Lab, Menlo Pk, CA 94025 USA. [Sheldon, E.; Plazas, A. A.] Brookhaven Natl Lab, Upton, NY 11973 USA. [Abbott, T.; James, D.; Smith, R. C.; Walker, A. R.] Natl Opt Astron Observ, Cerro Tololo Interamer Observ, La Serena, Chile. [Carnero Rosell, A.; Fausti Neto, A.; Maia, M. A. G.; Ogando, R.; Sobreira, F.] Lab Interinst E Astron LIneA, BR-20921400 Rio De Janeiro, RJ, Brazil. [Carnero Rosell, A.; Maia, M. A. G.; Ogando, R.] Observat Nacl, BR-20921400 Rio De Janeiro, RJ, Brazil. [Kind, M. Carrasco; Gruendl, R. A.; Honscheid, K.; Sevilla, I.; Thaler, J.] Univ Illinois, Dept Phys, Urbana, IL 61801 USA. [Kind, M. Carrasco; Gruendl, R. A.; Honscheid, K.] Univ Illinois, Natl Ctr Supercomp Applicat, Urbana, IL 61801 USA. [Desai, S.; Dietrich, J. P.; Tarle, G.] Univ Munich, Dept Phys, D-81679 Munich, Germany. [Dietrich, J. P.] Excellence Cluster Univ, D-85748 Garching, Germany. [Eifler, T. F.; Plazas, A. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Evrard, A. E.; Miller, C. J.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA. [Gruen, D.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Gruen, D.] Univ Observ Munich, D-81679 Munich, Germany. [Kuehn, K.] Australian Astron Observ, N Ryde, NSW 2113, Australia. [Miller, C. J.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Miquel, R.] Inst Catalana Recerca & Estudis Avancats, E-08010 Barcelona, Spain. [Romer, A. K.] Univ Sussex, Dept Phys & Astron, Brighton BN1 9QH, E Sussex, England. [Sanchez, E.; Sevilla, I.] Ctr Invest Energet Medioambient & Tecnol CIEMAT, Madrid 28040, Spain. [Thomas, D.] SEPnet, South East Phys Network, Southampton SO17 1BJ, Hants, England. RP Chang, C (reprint author), ETH, Dept Phys, Wolfgang Pauli Str 16, CH-8093 Zurich, Switzerland. EM chihway.chang@phys.ethz.ch RI Ogando, Ricardo/A-1747-2010; Sanchez, Eusebio/H-5228-2015; Fosalba Vela, Pablo/I-5515-2016; Gaztanaga, Enrique/L-4894-2014; OI Ogando, Ricardo/0000-0003-2120-1154; Sanchez, Eusebio/0000-0002-9646-8198; Gaztanaga, Enrique/0000-0001-9632-0815; Becker, Matthew/0000-0001-7774-2246; Suchyta, Eric/0000-0002-7047-9358; Dietrich, Jorg/0000-0002-8134-9591; Carrasco Kind, Matias/0000-0002-4802-3194; Abdalla, Filipe/0000-0003-2063-4345; Sobreira, Flavia/0000-0002-7822-0658; Tucker, Douglas/0000-0001-7211-5729 FU Swiss National Science Foundation [200021-149442, 200021-143906]; European Research Council Starting Grant [240672]; SFB-Transregio 33 "The Dark Universe", Deutsche Forschungsgemeinschaft (DFG); DFG cluster of excellence "Origin and Structure of the Universe"; CAPES [3171-13-2]; European Research Council Advanced Grant [FP7/291329]; U. S. Department of Energy; U. S. National Science Foundation; Ministry of Science and Education of Spain; Science and Technology Facilities Council of the United Kingdom; Higher Education Funding Council for England; National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign; Kavli Institute of Cosmological Physics at the University of Chicago; Center for Cosmology and Astro-Particle Physics at the Ohio State University; Mitchell Institute for Fundamental Physics and Astronomy at Texas AM University; Financiadora de Estudos e Projetos; Fundacao Carlos Chagas Filho de Amparo a Pesquisa do Estado do Rio de Janeiro; Conselho Nacional de Desenvolvimento Cientifico e Tecnologico; Ministerio da Ciencia e Tecnologia; Deutsche Forschungsgemeinschaft; Collaborating Institutions in the Dark Energy Survey; National Science Foundation [AST-1138766]; MINECO [AYA2012-39559, ESP2013-48274, FPA2013-47986]; Centro de Excelencia Severo Ochoa [SEV-2012-0234]; European Union; Argonne National Laboratory; University of California at Santa Cruz; University of Cambridge; Centro de Investigaciones Energeticas; Medioambientales y Tecnologicas-Madrid; University of Chicago; University College London; DES-Brazil Consortium; Eidgenossische Technische Hochschule (ETH) Zurich; fermi National Accelerator Laboratory; University of Edinburgh; University of Illinois at Urbana-Champaign; Institut de Ciencies de l'Espai (IEEC/CSIC); Institut de Fisica d'Altes Energies; Lawrence Berkeley National Laboratory; Ludwig-Maximilians Universitat; associated Excellence Cluster Universe; University of Michigan; National Optical Astronomy Observatory; University of Nottingham; Ohio State University; University of Pennsylvania; University of Portsmouth; SLAC National Accelerator Laboratory; Stanford University; University of Sussex; Texas AM University FX We are grateful for the extraordinary contributions of our CTIO colleagues and the DECam Construction, Commissioning and Science Verification teams in achieving the excellent instrument and telescope conditions that have made this work possible. The success of this project also relies critically on the expertise and dedication of the DES Data Management group. We thank Jake VanderPlas, Andy Connolly, Phil Marshall, Ludo van Waerbeke, and Rafal Szepietowski for discussions and collaborative work on mass mapping methodology. C. C. and A. A. are supported by the Swiss National Science Foundation Grants No. 200021-149442 and No. 200021-143906. S. B. and J. Z. acknowledge support from a European Research Council Starting Grant No. 240672. D. G. was supported by SFB-Transregio 33 "The Dark Universe" by the Deutsche Forschungsgemeinschaft (DFG) and the DFG cluster of excellence "Origin and Structure of the Universe". F. S. acknowledges financial support provided by CAPES under Contract No. 3171-13-2. O. L. acknowledges support from a European Research Council Advanced Grant No. FP7/291329. Funding for the DES Projects has been provided by the U. S. Department of Energy, the U. S. National Science Foundation, the Ministry of Science and Education of Spain, the Science and Technology Facilities Council of the United Kingdom, the Higher Education Funding Council for England, the National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign, the Kavli Institute of Cosmological Physics at the University of Chicago, the Center for Cosmology and Astro-Particle Physics at the Ohio State University, the Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M University, Financiadora de Estudos e Projetos, Fundacao Carlos Chagas Filho de Amparo a Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Cientifico e Tecnologico and the Ministerio da Ciencia e Tecnologia, the Deutsche Forschungsgemeinschaft, and the Collaborating Institutions in the Dark Energy Survey. The DES data management system is supported by the National Science Foundation under Grant No. AST-1138766. The DES participants from Spanish institutions are partially supported by MINECO under Grants No. AYA2012-39559, No. ESP2013-48274, No. FPA2013-47986, and Centro de Excelencia Severo Ochoa SEV-2012-0234, some of which include ERDF funds from the European Union. The Collaborating Institutions are Argonne National Laboratory, University of California at Santa Cruz, University of Cambridge, Centro de Investigaciones Energeticas, Medioambientales y Tecnologicas-Madrid, University of Chicago, University College London, DES-Brazil Consortium, Eidgenossische Technische Hochschule (ETH) Zurich, fermi National Accelerator Laboratory, University of Edinburgh, University of Illinois at Urbana-Champaign, Institut de Ciencies de l'Espai (IEEC/CSIC), Institut de Fisica d'Altes Energies, Lawrence Berkeley National Laboratory, Ludwig-Maximilians Universitat and the associated Excellence Cluster Universe, University of Michigan, National Optical Astronomy Observatory, University of Nottingham, Ohio State University, University of Pennsylvania, University of Portsmouth, SLAC National Accelerator Laboratory, Stanford University, University of Sussex, and Texas A&M University. This paper has gone through internal review by the DES collaboration. NR 57 TC 18 Z9 18 U1 0 U2 6 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 0031-9007 EI 1079-7114 J9 PHYS REV LETT JI Phys. Rev. Lett. PD JUL 29 PY 2015 VL 115 IS 5 AR 051301 DI 10.1103/PhysRevLett.115.051301 PG 8 WC Physics, Multidisciplinary SC Physics GA CO0SO UT WOS:000358862800002 PM 26274409 ER PT J AU Tiwari, SK Falconer, DA Moore, RL Venkatakrishnan, P Winebarger, AR Khazanov, IG AF Tiwari, Sanjiv K. Falconer, David A. Moore, Ronald L. Venkatakrishnan, P. Winebarger, Amy R. Khazanov, Igor G. TI Near-Sun speed of CMEs and the magnetic nonpotentiality of their source active regions SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE CMEs; ARs; vector magnetograms; speed ID CORONAL MASS EJECTIONS; MAJOR SOLAR-FLARES; FORCE-FREE; VECTOR MAGNETOGRAMS; FIELD; PRODUCTIVITY; ENERGY; TWIST AB We show that the speed of the fastest coronal mass ejections (CMEs) that an active region (AR) can produce can be predicted from a vector magnetogram of the AR. This is shown by logarithmic plots of CME speed (from the SOHO Large Angle and Spectrometric Coronagraph CME catalog) versus each of ten AR-integrated magnetic parameters (AR magnetic flux, three different AR magnetic-twist parameters, and six AR free-magnetic-energy proxies) measured from the vertical and horizontal field components of vector magnetograms (from the Solar Dynamics Observatory's Helioseismic and Magnetic Imager) of the source ARs of 189 CMEs. These plots show the following: (1) the speed of the fastest CMEs that an AR can produce increases with each of these whole-AR magnetic parameters and (2) that one of the AR magnetic-twist parameters and the corresponding free-magnetic-energy proxy each determine the CME-speed upper limit line somewhat better than any of the other eight whole-AR magnetic parameters. C1 [Tiwari, Sanjiv K.; Falconer, David A.; Moore, Ronald L.; Winebarger, Amy R.] NASA Marshall Space Flight Ctr, Huntsville, AL 35812 USA. [Falconer, David A.; Moore, Ronald L.; Khazanov, Igor G.] Univ Alabama, Ctr Space Plasma & Aeron Res, Huntsville, AL USA. [Venkatakrishnan, P.] Phys Res Lab, Udaipur Solar Observ, Udaipur, India. RP Tiwari, SK (reprint author), NASA Marshall Space Flight Ctr, Huntsville, AL 35812 USA. EM sanjiv.k.tiwari@nasa.gov FU NASA MSFC; LWS TRT Program of the Heliophysics Division of NASAs SMD; NASA's Game Changing Development Program; Johnson Space Center's Space Radiation Analysis Group (SRAG); University of Alabama in Huntsville FX S.K.T would like to thank Tibor Torok and Yang Liu for the useful discussion on this work during the AGU-2014 meeting. We acknowledge Phyllis Whittlesey and Malte Broese, students from Joint Space Weather Summer Camp 2014 (sponsored by the University of Alabama in Huntsville and its Center for Space Plasma and Aeronomic Research, University of Rostock and its LeibnizInstitute of Atmospheric Physics, and the German Aerospace Center (DLR)), for initially identifying some of the CMEs and their source ARs. S.K.T. is supported by an appointment to the NASA Postdoctoral Program at the NASA MSFC, administered by ORAU through a contract with NASA. R.L.M. and A.R.W. are supported by funding from the LWS TRT Program of the Heliophysics Division of NASAs SMD. Support for MAG4 development comes from NASA's Game Changing Development Program and Johnson Space Center's Space Radiation Analysis Group (SRAG). Use of SOHO LASCO CME catalog, and data from AIA and HMI (SDO), STEREO, and SOHO are sincerely acknowledged. The CME catalog is generated and maintained at the CDAW Data Center by NASA and The Catholic University of America in cooperation with the NRL. SOHO is a project of international cooperation between ESA and NASA. NR 48 TC 1 Z9 1 U1 0 U2 3 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD JUL 28 PY 2015 VL 42 IS 14 BP 5702 EP 5710 DI 10.1002/2015GL064865 PG 9 WC Geosciences, Multidisciplinary SC Geology GA CO7CU UT WOS:000359316100004 ER PT J AU Rignot, E Fenty, I Xu, Y Cai, C Kemp, C AF Rignot, Eric Fenty, Ian Xu, Yun Cai, Cilan Kemp, Chris TI Undercutting of marine-terminating glaciers in West Greenland SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE Glaciology; Greenland; multibeam echo sounding; physical oceanography; bathymetry; ice-ocean interactions ID SEA-LEVEL RISE; TIDEWATER GLACIERS; OCEAN WATERS; ICE-SHEET; ACCELERATION; ISBRAE; FJORD AB Marine-terminating glaciers control most of Greenland's ice discharge into the ocean, but little is known about the geometry of their frontal regions. Here we use side-looking, multibeam echo sounding observations to reveal that their frontal ice cliffs are grounded deeper below sea level than previously measured and their ice faces are neither vertical nor smooth but often undercut by the ocean and rough. Deep glacier grounding enables contact with subsurface, warm, salty Atlantic waters (AW) which melts ice at rates of meters per day. We detect cavities undercutting the base of the calving faces at the sites of subglacial water (SGW) discharge predicted by a hydrological model. The observed pattern of undercutting is consistent with numerical simulations of ice melt in which buoyant plumes of SGW transport warm AW to the ice faces. Glacier undercutting likely enhances iceberg calving, impacting ice front stability and, in turn, the glacier mass balance. C1 [Rignot, Eric; Xu, Yun; Cai, Cilan] Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA 92697 USA. [Rignot, Eric; Fenty, Ian] Jet Prop Lab, Pasadena, CA USA. [Kemp, Chris] Terrasond Ltd, Seattle, WA USA. RP Rignot, E (reprint author), Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA 92697 USA. EM erignot@uci.edu RI Rignot, Eric/A-4560-2014 OI Rignot, Eric/0000-0002-3366-0481 FU University of California Irvine from Gordon and Betty Moore Foundation [3280]; UC Irvine; National Aeronautics and Space Administration's Cryospheric Science Program [NNX12AB86G]; Jet Propulsion Laboratory; California Institute of Technology from NASA; Oak Ridge Associate Universities through NASA; NSFgrant [ARC-1023499] FX This work was performed at the University of California Irvine under grant 3280 from the Gordon and Betty Moore Foundation, start up funds from UC Irvine, and grant NNX12AB86G from the National Aeronautics and Space Administration's Cryospheric Science Program and at the Jet Propulsion Laboratory, California Institute of Technology under a grant from NASA. IF's research was carried out in part by an appointment to the NASA Postdoctoral Program at the Jet Propulsion Laboratory, California Institute of Technology, administered by Oak Ridge Associate Universities through a contract with NASA and in part through NSFgrant ARC-1023499. NR 26 TC 16 Z9 16 U1 4 U2 33 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD JUL 28 PY 2015 VL 42 IS 14 BP 5909 EP 5917 DI 10.1002/2015GL064236 PG 9 WC Geosciences, Multidisciplinary SC Geology GA CO7CU UT WOS:000359316100029 ER PT J AU McGillen, MR Bernard, F Fleming, EL Burkholder, JB AF McGillen, Max R. Bernard, Francois Fleming, Eric L. Burkholder, James B. TI HCFC-133a (CF3CH2Cl): OH rate coefficient, UV and infrared absorption spectra, and atmospheric implications SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE ozone-depleting substance; photolysis; hydrochlorofluorocarbon; UV cross section ID OZONE-DEPLETING SUBSTANCES; RATE CONSTANTS; ULTRAVIOLET-ABSORPTION; HALOGENATED METHANES; STRATOSPHERIC OZONE; TEMPERATURE-RANGE; KINETICS; RADICALS; ETHANES; IMPACT AB HCFC-133a (CF3CH2Cl), an ozone-depleting substance, is primarily removed from the atmosphere by gas-phase reaction with OH radicals and by UV photolysis. The rate coefficient, k, for the OH+HCFC-133a reaction was measured between 233 and 379K and is given by k(T)=(9.320.8)x10(-13)exp(-(1296 +/- 28)/T), where k(296K) was measured to be (1.10 +/- 0.02)x10(-14) (cm(3)molecule(-1)s(-1)) (2 sigma precision uncertainty). The HCFC-133a UV absorption spectrum was measured between 184.95 and 240nm at 213-323K, and a spectrum parameterization is presented. The HCFC-133a atmospheric loss processes, lifetime, ozone depletion potential, and uncertainties were evaluated using a 2-D atmospheric model. The global annually averaged steady state lifetime and ozone depletion potential (ODP) were determined to be 4.45 (4.04-4.90)years and 0.017 (0.001), respectively, where the ranges are based solely on the 2 sigma uncertainty in the kinetic and photochemical parameters. The infrared absorption spectrum of HCFC-133a was measured, and its global warming potential was determined to be 380 on the 100year time horizon. C1 [McGillen, Max R.; Bernard, Francois; Burkholder, James B.] NOAA, Earth Syst Res Lab, Div Chem Sci, Boulder, CO 80305 USA. [McGillen, Max R.; Bernard, Francois] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA. [Fleming, Eric L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Fleming, Eric L.] Sci Syst & Applicat Inc, Lanham, MD USA. RP Burkholder, JB (reprint author), NOAA, Earth Syst Res Lab, Div Chem Sci, Boulder, CO 80305 USA. EM James.B.Burkholder@noaa.gov RI McGillen, Max/G-5196-2011; BERNARD, Francois/F-2864-2014; Manager, CSD Publications/B-2789-2015 OI McGillen, Max/0000-0002-1623-5985; BERNARD, Francois/0000-0002-6116-3167; FU NOAA's Atmospheric Chemistry, Carbon Cycle, and Climate (AC4) Program; NASA's Atmospheric Composition Program FX This work was supported in part by NOAA's Atmospheric Chemistry, Carbon Cycle, and Climate (AC4) Program and NASA's Atmospheric Composition Program. Supporting data are included as a data set and as one figure and five tables in an SI file; any additional data may be obtained from J.B.B. (email: James.B.Burkholder@noaa.gov). NR 29 TC 1 Z9 1 U1 2 U2 12 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD JUL 28 PY 2015 VL 42 IS 14 BP 6098 EP 6105 DI 10.1002/2015GL064939 PG 8 WC Geosciences, Multidisciplinary SC Geology GA CO7CU UT WOS:000359316100052 ER PT J AU Bates, CM Chang, AB Momcilovic, N Jones, SC Grubbs, RH AF Bates, Christopher M. Chang, Alice B. Momcilovic, Nebojsa Jones, Simon C. Grubbs, Robert H. TI ABA Triblock Brush Polymers: Synthesis, Self-Assembly, Conductivity, and Rheological Properties SO MACROMOLECULES LA English DT Article ID BLOCK-COPOLYMER ELECTROLYTES; IONIC-CONDUCTIVITY; LITHIUM BATTERIES; MOLECULAR-WEIGHT; SOLID-STATE; CROSS-LINKING; SALT; TRANSPORT AB The synthesis, self-assembly; conductivity, and rheological properties of ABA triblock brush polymers (BBCPs) with grafted polystyrene (A block, N-PS = 21) and poly,(ethylene oxide) (B block, N-PEO = 45) side chains are reported. Two backbone molecular weights (N-A:N-B:N-A = 11:78:11 and 15:119:15) were investigated with lithium bis(trifluoromethane)sulfonimide (LiTFSI) doping ratios 2 <= [EO]:[Li+] <= 20. Blends with 2 <= [EO]: [Li+] <= 10 suppress PEO crystallization and self-assemble into hexagonally packed cylinders of the minority gPS component. Conductivity is on the order of 10(-3) S/cm at 105 degrees C with a corresponding elastic modulus ca. 10(4) Pa. The optimum conductivity occurs at a blend ratio near 10:1 [EO]: [Li+], similar to that reported for linear block copolymer analogues. C1 [Bates, Christopher M.; Chang, Alice B.; Momcilovic, Nebojsa; Grubbs, Robert H.] CALTECH, Arnold & Mabel Beckman Labs Chem Synth, Pasadena, CA 91125 USA. [Jones, Simon C.] CALTECH, Jet Prop Lab, Electrochem Technol Grp, Pasadena, CA 91109 USA. RP Grubbs, RH (reprint author), CALTECH, Arnold & Mabel Beckman Labs Chem Synth, Pasadena, CA 91125 USA. EM simon.c.jones@jpl.nasa.gov; rhg@caltech.edu FU Dreyfus Foundation [EP-13-142]; U.S. Department of Defense through the NDSEG; DOE Office of Science [DE-AC02-06CH11357] FX We thank Prof. Julia Kornfield for use of her rheometer. C.M.B. thanks the Dreyfus Foundation for Environmental Postdoc Fellowship EP-13-142. A.B.C. thanks the U.S. Department of Defense for support through the NDSEG fellowship. This research used resources of the Advanced Photon Source, a U.S. DOE Office of Science User Facility operated for the DOE Office of Science by Argonne National Laboratory under Contract DE-AC02-06CH11357. NR 37 TC 18 Z9 18 U1 17 U2 87 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0024-9297 EI 1520-5835 J9 MACROMOLECULES JI Macromolecules PD JUL 28 PY 2015 VL 48 IS 14 BP 4967 EP 4973 DI 10.1021/acs.macromol.5b00880 PG 7 WC Polymer Science SC Polymer Science GA CO0EQ UT WOS:000358823300022 ER PT J AU Shen, MG Piao, SL Jeong, SJ Zhou, LM Zeng, ZZ Ciais, P Chen, DL Huang, MT Jin, CS Li, LZX Li, Y Myneni, RB Yang, K Zhang, GX Zhang, YJ Yao, TD AF Shen, Miaogen Piao, Shilong Jeong, Su-Jong Zhou, Liming Zeng, Zhenzhong Ciais, Philippe Chen, Deliang Huang, Mengtian Jin, Chun-Sil Li, Laurent Z. X. Li, Yue Myneni, Ranga B. Yang, Kun Zhang, Gengxin Zhang, Yangjian Yao, Tandong TI Evaporative cooling over the Tibetan Plateau induced by vegetation growth SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE climate change; feedback; evapotranspiration; vegetation; Tibetan Plateau ID DIURNAL TEMPERATURE-RANGE; CLIMATE-CHANGE; CONVECTIVE PARAMETERIZATION; ALPINE MEADOW; IMPACTS; MODIS; RADIATION; MODEL; PRECIPITATION; SENSITIVITY AB In the Arctic, climate warming enhances vegetation activity by extending the length of the growing season and intensifying maximum rates of productivity. In turn, increased vegetation productivity reduces albedo, which causes a positive feedback on temperature. Over the Tibetan Plateau (TP), regional vegetation greening has also been observed in response to recent warming. Here, we show that in contrast to arctic regions, increased growing season vegetation activity over the TP may have attenuated surface warming. This negative feedback on growing season vegetation temperature is attributed to enhanced evapotranspiration (ET). The extra energy available at the surface, which results from lower albedo, is efficiently dissipated by evaporative cooling. The net effect is a decrease in daily maximum temperature and the diurnal temperature range, which is supported by statistical analyses of in situ observations and by decomposition of the surface energy budget. A daytime cooling effect from increased vegetation activity is also modeled from a set of regional weather research and forecasting (WRF) mesoscale model simulations, but with a magnitude smaller than observed, likely because the WRF model simulates a weaker ET enhancement. Our results suggest that actions to restore native grasslands in degraded areas, roughly one-third of the plateau, will both facilitate a sustainable ecological development in this region and have local climate cobenefits. More accurate simulations of the biophysical coupling between the land surface and the atmosphere are needed to help understand regional climate change over the TP, and possible larger scale feedbacks between climate in the TP and the Asian monsoon system. C1 [Shen, Miaogen; Piao, Shilong; Yang, Kun; Zhang, Gengxin; Yao, Tandong] Chinese Acad Sci, Inst Tibetan Plateau Res, Beijing 100101, Peoples R China. [Shen, Miaogen; Piao, Shilong; Yang, Kun; Zhang, Yangjian; Yao, Tandong] Chinese Acad Sci, Ctr Excellence Tibetan Plateau Earth Sci, Beijing 100101, Peoples R China. [Piao, Shilong; Zeng, Zhenzhong; Huang, Mengtian; Li, Yue] Peking Univ, Coll Urban & Environm Sci, Dept Ecol, Beijing 100871, Peoples R China. [Jeong, Su-Jong] CALTECH, Jet Prop Lab, Pasadena, CA 91011 USA. [Zhou, Liming] SUNY Albany, Dept Atmospher & Environm Sci, Albany, NY 12222 USA. [Ciais, Philippe] Univ Versailles St Quentin En Yvelines, Lab Sci Climat & Environm, UMR Commissariat Energie Atom CNRS 1572, F-91191 Gif Sur Yvette, France. [Chen, Deliang] Univ Gothenberg, Dept Earth Sci, S-40530 Gothenburg, Sweden. [Jin, Chun-Sil] Seoul Natl Univ, Sch Earth & Environm Sci, Seoul 151747, South Korea. [Li, Laurent Z. X.] Univ Paris 06, CNRS, Lab Meteorol Dynam, F-75252 Paris, France. [Myneni, Ranga B.] Boston Univ, Dept Earth & Environm, Boston, MA 02215 USA. [Zhang, Yangjian] Chinese Acad Sci, Inst Geog Sci & Nat Resources Res, Key Lab Ecosyst Network Observat & Modeling, Beijing 100101, Peoples R China. RP Shen, MG (reprint author), Chinese Acad Sci, Inst Tibetan Plateau Res, Beijing 100101, Peoples R China. EM shen.miaogen@gmail.com; slpiao@pku.edu.cn RI Myneni, Ranga/F-5129-2012; Shen, Miaogen/A-8374-2011; Jeong, Su-Jong/J-4110-2014; Chen, Deliang/A-5107-2013; Yang, Kun/G-8390-2011; Zhou, Liming/A-2688-2012; OI Shen, Miaogen/0000-0001-5742-8807; Chen, Deliang/0000-0003-0288-5618; Yang, Kun/0000-0002-0809-2371; Li, Laurent/0000-0002-3855-3976 FU Chinese Academy of Sciences [XDB03030404]; National Basic Research Program of China [2013CB956303]; National Natural Science Foundation of China [41125004]; Youth Innovation Promotion Association of the Chinese Academy of Sciences [2015055] FX This study was funded by the Strategic Priority Research Program (B) of the Chinese Academy of Sciences (Grant XDB03030404), a National Basic Research Program of China (Grant 2013CB956303), a program of National Natural Science Foundation of China (Grant 41125004), and a grant from Youth Innovation Promotion Association of the Chinese Academy of Sciences (Grant 2015055). NR 55 TC 21 Z9 22 U1 16 U2 97 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 JUL 28 PY 2015 VL 112 IS 30 BP 9299 EP 9304 DI 10.1073/pnas.1504418112 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CN7ZW UT WOS:000358656500056 PM 26170316 ER PT J AU Fan, YZ Li, W Calzado, VS Trees, C Stamnes, S Fournier, G McKee, D Stamnes, K AF Fan, Yongzhen Li, Wei Calzado, Violeta Sanjuan Trees, Charles Stamnes, Snorre Fournier, Georges McKee, David Stamnes, Knut TI Inferring inherent optical properties and water constituent profiles from apparent optical properties SO OPTICS EXPRESS LA English DT Article ID IRRADIANCE INVERSION ALGORITHM; ATMOSPHERE-OCEAN SYSTEM; PHASE FUNCTION; BACKSCATTERING COEFFICIENTS; RADIATIVE-TRANSFER; LIGHT-SCATTERING; COASTAL WATERS; NATURAL-WATERS; CASE-1 WATERS; ABSORPTION AB The BP09 experiment conducted by the Centre for Maritime Research and Experimentation in the Ligurian Sea in March 2009 provided paired vertical profiles of nadir-viewing radiances L-u (z) and downward irradiances E-d (z) and inherent optical properties (IOPs, absorption, scattering and backscattering coefficients). An inversion algorithm was implemented to retrieve IOPs from apparent optical properties (AOPs, radiance reflectance R-L, irradiance reflectance R-E and diffuse attenuation coefficient K-d) derived from the radiometric measurements. Then another inversion algorithm was developed to infer vertical profiles of water constituent concentrations, including chlorophyll-a concentration, non-algal particle concentration, and colored dissolved organic matter from the retrieved IOPs based on a bio-optical model. The algorithm was tested on a synthetic dataset and found to give reliable results with an accuracy better than 1%. When the algorithm was applied to the BP09 dataset it was found that good retrievals of IOPs could be obtained for sufficiently deep waters, i.e. for L-u (z) and E-d (z) measurements conducted to depths of 50 m or more. This requirement needs to be satisfied in order to obtain a good estimation of the backscattering coefficient. For such radiometric measurements a correlation of 0.88, 0.96 and 0.93 was found between retrieved and measured absorption, scattering and backscattering coefficients, respectively. A comparison between water constituent values derived from the measured IOPs and in-situ measured values, yielded a correlation of 0.80, 0.78, and 0.73 for chlorophyll-a concentration, non-algal particle concentration, and absorption coefficient of colored dissolved organic matter at 443 nm, respectively. This comparison indicates that adjustments to the bio-optical model are needed in order to obtain a better match between inferred and measured water constituent values in the Ligurian Sea using the methodology developed in this paper. (C) 2015 Optical Society of America C1 [Fan, Yongzhen; Li, Wei; Stamnes, Knut] Stevens Inst Technol, Dept Phys & Engn Phys, Light & Life Lab, Hoboken, NJ 07307 USA. [Calzado, Violeta Sanjuan; Trees, Charles] NATO Ctr Maritime Res & Experimentat CMRE, La Spezia, Italy. [Stamnes, Snorre] NASA Langley Res Ctr, Hampton, VA USA. [Fournier, Georges] Def Res & Dev Canada, Valcartier Res Ctr, Quebec City, PQ, Canada. [McKee, David] Univ Strathclyde, Dept Phys, Glasgow, Lanark, Scotland. RP Fan, YZ (reprint author), Stevens Inst Technol, Dept Phys & Engn Phys, Light & Life Lab, Hoboken, NJ 07307 USA. EM yfan@stevens.edu FU Natural Environment Research Council [NE/E013678/1] NR 31 TC 0 Z9 0 U1 2 U2 3 PU OPTICAL SOC AMER PI WASHINGTON PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA SN 1094-4087 J9 OPT EXPRESS JI Opt. Express PD JUL 27 PY 2015 VL 23 IS 15 BP A987 EP A1009 DI 10.1364/OE.23.00A987 PG 23 WC Optics SC Optics GA CR0TE UT WOS:000361035300021 PM 26367699 ER PT J AU Bergman, JW Pfister, L Yang, Q AF Bergman, J. W. Pfister, L. Yang, Q. TI Identifying robust transport features of the upper tropical troposphere SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE upper tropical troposphere; transport; multimodel ensemble ID STRATOSPHERIC WATER-VAPOR; TROPOPAUSE LAYER; CIRRUS CLOUDS; RADIATIVE PROPERTIES; ACCURATE PARAMETERIZATION; AIRCRAFT OBSERVATIONS; CLIMATE MODELS; ASIAN MONSOON; DEHYDRATION; OZONE AB Multimodel ensembles of back trajectories calculated from four different analysis data sets and two different trajectory formulations (diabatic and kinematic) are analyzed to investigate seasonal mean boundary layer-to-tropopause (100hPa) transport in the tropics. Transport paths are separated into two legs: convective uplift (boundary layer to detrainment) and radiative ascent (detrainment to tropopause). The following three diagnostic measures are used: source location, source-to-tropopause transport time, and the source influence (i.e., the fraction of air with short transport times) at 100hPa. Ensemble means and standard deviations identify robust features (i.e., common to all ensemble members) while experimental hybrid calculations explain model-to-model discrepancies. Convective uplift is a major contributor to uncertainties in boundary layer-to-tropopause transport times and source locations. Spatial patterns of boundary layer influence at 100hPa are nevertheless robust. Detrainment-to-tropopause transport times are robust despite substantial model-to-model variations of convective detrainment height because ascent rates are faster at low altitudes than at high altitudes. Detrainment-to-tropopause transport also has robust horizontal spatial patterns for both convective sources and convective influence, particularly during boreal winter. Most model-to-model discrepancies occur at small spatial scales and are associated with differing distributions of convection. The location of maximum convective influence associated with the Asian summer monsoon is a notable exception. This exceptionally large discrepancy is associated primarily with radiative ascent. The fact that the observed maxima of important tropospheric constituents are collocated with the maximum convective influence for the diabatic calculations but not for the kinematic calculations suggests that diabatic trajectories could be more reliable in this region. C1 [Bergman, J. W.] Bay Area Environm Res Inst, Petaluma, CA 94952 USA. [Bergman, J. W.] Natl Ctr Atmospher Res, Atmospher Chem Observat & Modeling Lab, Boulder, CO 80307 USA. [Pfister, L.] NASA Ames Res Ctr, Earth Sci Div, Moffett Field, CA USA. [Yang, Q.] Univ Washington, Joint Inst Study Atmosphere & Ocean, Seattle, WA 98195 USA. [Yang, Q.] Univ Washington, Dept Atmospher Sci, Seattle, WA 98195 USA. RP Bergman, JW (reprint author), Bay Area Environm Res Inst, Petaluma, CA 94952 USA. EM jwbergman921@gmail.com FU National Science Foundation FX This work benefitted from discussions with E. Jensen and L. Pan and from the comments of three anonymous reviewers. ERA-interim, CFSR, and GSF data were obtained from the CISL Data Support Section at the National Center for Atmospheric Research (NCAR). MERRA, TRMM, and IR data were obtained from the Goddard Earth Sciences Data and Information Services Center. J. Bergman was a visitor at the Atmospheric Chemistry Observations and Modeling Laboratory at NCAR during the execution of this study. NCAR is operated by the University Corporation for Atmospheric Research, under sponsorship of the National Science Foundation. Data used in this study can be obtained free of charge by contacting J. Bergman (jwbergman921@gmail.com). NR 67 TC 3 Z9 3 U1 3 U2 6 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD JUL 27 PY 2015 VL 120 IS 14 BP 6758 EP 6776 DI 10.1002/2015JD023523 PG 19 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA CP3TL UT WOS:000359804900003 ER PT J AU Boisvert, LN Wu, DL Shie, CL AF Boisvert, L. N. Wu, D. L. Shie, C. -L. TI Increasing evaporation amounts seen in the Arctic between 2003 and 2013 from AIRS data SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE moisture flux; Arctic; AIRS; evaporation; skin temperature; clouds ID SURFACE HEAT-BUDGET; SEA-ICE; TURBULENT EXCHANGE; BOUNDARY-LAYER; ENERGY BUDGET; ANNUAL CYCLE; ERA-INTERIM; CLOUD; OCEAN; CLIMATE AB The vertical moisture flux (i.e., evaporation) plays an important role in the Arctic energy budget, the water vapor feedback, and Arctic amplification. It is one of the most uncertain variables, especially in this new Arctic climate system, which is dominated by large ice-free ocean areas for a longer portion of the year. Moisture flux rates, produced using Atmospheric Infrared Sounder (AIRS) data, from the Arctic Ocean and surrounding seas were found to have increased between 2003 and 2013 by 7.2x10(-4)gm(-2)s(-1) per year (equivalent to 1.79Wm(-2) per year in latent heat). This is a 7% increase in the average moisture flux each year and a 0.12% increase in the yearly global ocean latent heat flux, with some months increasing more than others. The largest increases seen are in the Arctic coastal seas during the spring and fall where there has been a reduction in sea ice cover and an increase in sea surface temperatures. Increases in the moisture flux from the surface also correspond to increases in total atmospheric column water vapor and low-level clouds, especially in the central Arctic regions. Changes in the atmospheric water vapor in the surrounding seas (e.g., East Greenland) are most likely due to lower latitude transport of moisture rather than from the surface. Yearly, the moisture flux from the surface supplies about 10% of the total column atmosphere water vapor. C1 [Boisvert, L. N.] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. [Wu, D. L.] NASA Goddard Space Flight Ctr, Greenbelt, MD USA. [Shie, C. -L.] Univ Maryland, Joint Ctr Earth Syst Technol, Catonsville, MD 21228 USA. RP Boisvert, LN (reprint author), Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. EM linette.n.boisvert@nasa.gov RI Wu, Dong/D-5375-2012 FU Earth System Science Interdisciplinary Center (ESSIC) Task 683; NASA-ROSES IDS [12-IDS12-0120] FX The work of Linette Boisvert was supported by the Earth System Science Interdisciplinary Center (ESSIC) Task 683 and NASA-ROSES 2012 IDS proposal: 12-IDS12-0120. Support for the work of Dong Wu was provided by NASA-ROSES 2012 IDS proposal: 12-IDS12-0120. Chung-Lin Shie is a research faculty at the Joint Center for Earth Systems Technology (JCET). Contact Boisvert (linette.n.boisvert@nasa.gov) for the moisture flux and AIRS data. NR 55 TC 3 Z9 3 U1 3 U2 18 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD JUL 27 PY 2015 VL 120 IS 14 BP 6865 EP 6881 DI 10.1002/2015JD023258 PG 17 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA CP3TL UT WOS:000359804900009 ER PT J AU Xu, XG Wang, J Zeng, J Spurr, R Liu, X Dubovik, O Li, L Li, ZQ Mishchenko, MI Siniuk, A Holben, BN AF Xu, Xiaoguang Wang, Jun Zeng, Jing Spurr, Robert Liu, Xiong Dubovik, Oleg Li, Li Li, Zhengqiang Mishchenko, Michael I. Siniuk, Aliaksandr Holben, Brent N. TI Retrieval of aerosol microphysical properties from AERONET photopolarimetric measurements: 2. A new research algorithm and case demonstration SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE AERONET; polarization; aerosol retrieval algorithm; single-scattering albedo; remote sensing; absorption ID SKY RADIANCE MEASUREMENTS; BOUND CONSTRAINED OPTIMIZATION; OPTICAL-PROPERTIES; IMAGING SPECTRORADIOMETER; BIDIRECTIONAL REFLECTANCE; SPACEBORNE MEASUREMENTS; SATELLITE RETRIEVALS; TROPOSPHERIC AEROSOL; INVERSION ALGORITHM; INTEGRAL EQUATIONS AB A new research algorithm is presented here as the second part of a two-part study to retrieve aerosol microphysical properties from the multispectral and multiangular photopolarimetric measurements taken by Aerosol Robotic Network's (AERONET's) new-generation Sun photometer. The algorithm uses an advanced UNified and Linearized Vector Radiative Transfer Model and incorporates a statistical optimization approach. While the new algorithm has heritage from AERONET operational inversion algorithm in constraining a priori and retrieval smoothness, it has two new features. First, the new algorithm retrieves the effective radius, effective variance, and total volume of aerosols associated with a continuous bimodal particle size distribution (PSD) function, while the AERONET operational algorithm retrieves aerosol volume over 22 size bins. Second, our algorithm retrieves complex refractive indices for both fine and coarse modes, while the AERONET operational algorithm assumes a size-independent aerosol refractive index. Mode-resolved refractive indices can improve the estimate of the single-scattering albedo (SSA) for each aerosol mode and thus facilitate the validation of satellite products and chemistry transport models. We applied the algorithm to a suite of real cases over Beijing_RADI site and found that our retrievals are overall consistent with AERONET operational inversions but can offer mode-resolved refractive index and SSA with acceptable accuracy for the aerosol composed by spherical particles. Along with the retrieval using both radiance and polarization, we also performed radiance-only retrieval to demonstrate the improvements by adding polarization in the inversion. Contrast analysis indicates that with polarization, retrieval error can be reduced by over 50% in PSD parameters, 10-30% in the refractive index, and 10-40% in SSA, which is consistent with theoretical analysis presented in the companion paper of this two-part study. C1 [Xu, Xiaoguang; Wang, Jun; Zeng, Jing] Univ Nebraska, Earth & Atmospher Sci, Lincoln, NE 68588 USA. [Spurr, Robert] RT Solut Inc, Cambridge, MA USA. [Liu, Xiong] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Dubovik, Oleg] Univ Lille 1, CNRS, Lab Opt Atmospher, F-59655 Villeneuve Dascq, France. [Li, Li; Li, Zhengqiang] Chinese Acad Sci, State Environm Protect Key Lab Satellites Remote, Inst Remote Sensing & Digital Earth, Beijing, Peoples R China. [Mishchenko, Michael I.] NASA Goddard Inst Space Studies, New York, NY USA. [Siniuk, Aliaksandr; Holben, Brent N.] NASA Goddard Space Flight Ctr, Greenbelt, MD USA. RP Wang, J (reprint author), Univ Nebraska, Earth & Atmospher Sci, Lincoln, NE 68588 USA. EM jwangjun@gmail.com RI Liu, Xiong/P-7186-2014; Xu, Xiaoguang/B-8203-2016; Wang, Jun/A-2977-2008; OI Liu, Xiong/0000-0003-2939-574X; Xu, Xiaoguang/0000-0001-9583-980X; Wang, Jun/0000-0002-7334-0490; Li, Zhengqiang/0000-0002-7795-3630 FU NASA Earth and Space Science Fellowship; NASA Radiation Sciences Program; NASA Glory Mission Program FX This research is supported by a NASA Earth and Space Science Fellowship managed by Mingying Wei, as well as the NASA Radiation Sciences Program and the Glory Mission Program managed by Hal Maring. We acknowledge the data services provided by the AERONET team at NASA GSFC, and the computational support from the Holland Computing Center at the University of Nebraska. The data presented in the manuscript can be available upon request through email to the corresponding author at jwangjun@gmail.com. J. Zeng and J. Wang also thank Qingyuang Han for inspiring them to conduct this work. NR 80 TC 10 Z9 10 U1 1 U2 14 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD JUL 27 PY 2015 VL 120 IS 14 BP 7079 EP 7098 DI 10.1002/2015JD023113 PG 20 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA CP3TL UT WOS:000359804900024 ER PT J AU Cuesta, J Eremenko, M Flamant, C Dufour, G Laurent, B Bergametti, G Hopfner, M Orphal, J Zhou, D AF Cuesta, Juan Eremenko, Maxim Flamant, Cyrille Dufour, Gaelle Laurent, Benoit Bergametti, Gilles Hoepfner, Michael Orphal, Johannes Zhou, Daniel TI Three-dimensional distribution of a major desert dust outbreak over East Asia in March 2008 derived from IASI satellite observations SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE dust 3D distribution; thermal infrared aerosol optical depth; MetOp satellites ID OPTICAL DEPTH; AIR-QUALITY; RADIATIVE PROPERTIES; EXTINCTION SPECTRA; SOURCE AREAS; AEROSOLS; EMISSION; SCATTERING; RETRIEVAL; AFRICAN AB We describe the daily evolution of the three-dimensional (3D) structure of a major dust outbreak initiated by an extratropical cyclone over East Asia in early March 2008, using new aerosol retrievals derived from satellite observations of IASI (Infrared Atmospheric Sounding Interferometer). A novel auto-adaptive Tikhonov-Phillips-type approach called AEROIASI is used to retrieve vertical profiles of dust extinction coefficient at 10 mu m for most cloud-free IASI pixels, both over land and ocean. The dust vertical distribution derived from AEROIASI is shown to agree remarkably well with along-track transects of CALIOP spaceborne lidar vertical profiles (mean biases less than 110m, correlation of 0.95, and precision of 260m for mean altitudes of the dust layers). AEROIASI allows the daily characterization of the 3D transport pathways across East Asia of two dust plumes originating from the Gobi and North Chinese deserts. From AEROIASI retrievals, we provide evidence that (i) both dust plumes are transported over the Beijing region and the Yellow Sea as elevated layers above a shallow boundary layer, (ii) as they progress eastward, the dust layers are lifted up by the ascending motions near the core of the extratropical cyclone, and (iii) when being transported over the warm waters of the Japan Sea, turbulent mixing in the deep marine boundary layer leads to high dust concentrations down to the surface. AEROIASI observations and model simulations also show that the progression of the dust plumes across East Asia is tightly related to the advancing cold front of the extratropical cyclone. C1 [Cuesta, Juan; Eremenko, Maxim; Dufour, Gaelle; Laurent, Benoit; Bergametti, Gilles] Univ Paris Diderot, Univ Paris Est Creteil, UMR CNRS 7583, Lab Interuniv Syst Atmospher, Creteil, France. [Flamant, Cyrille] Univ Paris 06, Univ Sorbonne, CNRS, Paris, France. [Flamant, Cyrille] LATMOS, UVSQ, UMR 8190, Paris, France. [Hoepfner, Michael; Orphal, Johannes] Karlsruher Inst Technol, Inst Meteorol & Klimaforsch, Karlsruhe, Germany. [Zhou, Daniel] NASA, Langley Res Ctr, Hampton, VA 23665 USA. RP Cuesta, J (reprint author), Univ Paris Diderot, Univ Paris Est Creteil, UMR CNRS 7583, Lab Interuniv Syst Atmospher, Creteil, France. EM cuesta@lisa.u-pec.fr RI Hopfner, Michael/A-7255-2013; OI Hopfner, Michael/0000-0002-4174-9531; Cuesta, Juan/0000-0001-9330-6401 FU Centre National des Etudes Spatiales (CNES, the French Space Agency); Universite Paris Est Creteil (UPEC); Centre National des Recherches Scientifiques - Institut National des Sciences de l'Univers (CNRS-INSU); Programme National de Teledetection Spatiale (PNTS) [PNTS-2013-05]; project "IASI-TOSCA" (Terre, Ocean, Surfaces continentals, Atmosphere) from CNES; "Chaire d'Excellence" of UPEC and CNES FX The authors are grateful for the financial support given by the Centre National des Etudes Spatiales (CNES, the French Space Agency), the Universite Paris Est Creteil (UPEC), the Centre National des Recherches Scientifiques - Institut National des Sciences de l'Univers (CNRS-INSU), and the Programme National de Teledetection Spatiale (PNTS, http://www.insu.cnrs.fr/actions-sur-projets/pnts-programme-national-de-t eledetection-spatiale, grant PNTS-2013-05, project "SYNAEROZON") for achieving this research work and its publication. This study also was financed by the project "IASI-TOSCA" (Terre, Ocean, Surfaces continentals, Atmosphere) from CNES and by a "Chaire d'Excellence" of UPEC and CNES. IASI is a joint mission of EUMETSAT and CNES. We acknowledge the support by the data centers ETHER (http://www.poleether.fr), ICARE (http://www.icare.univlille1.fr), and NASA (http://ladsweb.nascom.nasa.gov) for providing respectively data sets from IASI (level 1C, originally supplied by EUMETSAT through the Eumetcast system distribution, http://www.eumetsat.int), CALIPSO (level 1), and MODIS (level 2). Meteorological reanalyses are produced by ECMWF and supplied by CLIMSERV (http://climserv.ipsl.polytechnique.fr). We acknowledge the University of Wyoming (Larry Oolman) for providing the horizontal visibility data sets (http://weather.uwyo.edu), the National Institute for Environmental Studies for ground-based lidar measurements (http://www-lidar.nies.go.jp), the AERONET network for sun photometer observations over East Asia (http://aeronet.gsfc.nasa.gov), and the NOAA/OAR/ESRL PSD (Boulder, Colorado, USA; http://www.esrl.noaa.gov/psd) for the NOAA_OI_SST_V2 data. We thank G. Foret, C. Di Biagio, and P. Formenti from LISA for fruitful discussions on desert dust. NR 80 TC 2 Z9 2 U1 1 U2 9 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD JUL 27 PY 2015 VL 120 IS 14 BP 7099 EP 7127 DI 10.1002/2014JD022406 PG 29 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA CP3TL UT WOS:000359804900025 ER PT J AU Voulgarakis, A Marlier, ME Faluvegi, G Shindell, DT Tsigaridis, K Mangeon, S AF Voulgarakis, Apostolos Marlier, Miriam E. Faluvegi, Greg Shindell, Drew T. Tsigaridis, Kostas Mangeon, Stephane TI Interannual variability of tropospheric trace gases and aerosols: The role of biomass burning emissions SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE Interannual variability; biomass burning; carbon monoxide; ozone; hydroxyl radicals; aerosols ID ORGANIC-COMPOUND EMISSIONS; SATELLITE-OBSERVATIONS; ATMOSPHERIC CHEMISTRY; CLIMATE VARIABILITY; ACCURATE SIMULATION; CHEMICAL-MODELS; AURA SATELLITE; FIRE EMISSIONS; OPTICAL DEPTH; GLOBAL-MODEL AB Fires are responsible for a range of gaseous and aerosol emissions. However, their influence on the interannual variability of atmospheric trace gases and aerosols has not been systematically investigated from a global perspective. We examine biomass burning emissions as a driver of interannual variability of large-scale abundances of short-lived constituents such as carbon monoxide (CO), hydroxyl radicals (OH), ozone, and aerosols using the Goddard Institute for Space Studies ModelE composition-climate model and a range of observations, with an emphasis on satellite information. Our model captures the observed variability of the constituents examined in most cases, but with substantial underestimates in boreal regions. The strongest interannual variability on a global scale is found for carbon monoxide (similar to 10% for its global annual burden), while the lowest is found for tropospheric ozone (similar to 1% for its global annual burden). Regionally, aerosol optical depth shows the largest variability which exceeds 50%. Areas of strong variability of both aerosols and CO include the tropical land regions (especially Equatorial Asia and South America) and northern high latitudes, while even regions in the northern midlatitudes experience substantial interannual variability of aerosols. Ozone variability peaks over equatorial Asia in boreal autumn, partly due to varying biomass burning emissions, and over the western and central Pacific in the rest of the year, mainly due to meteorological fluctuations. We find that biomass burning emissions are almost entirely responsible for global CO interannual variability, and similarly important for OH variability. The same is true for global and regional aerosol variability, especially when not taking into account dust and sea-salt particles. We show that important implications can arise from such interannual influences for regional climate and air quality. C1 [Voulgarakis, Apostolos; Mangeon, Stephane] Univ London Imperial Coll Sci Technol & Med, Dept Phys, London, England. [Marlier, Miriam E.] Columbia Univ, Dept Ecol Evolut & Environm Biol, New York, NY USA. [Faluvegi, Greg; Tsigaridis, Kostas] Columbia Univ, Ctr Climate Syst Res, New York, NY USA. [Faluvegi, Greg; Tsigaridis, Kostas] NASA Goddard Inst Space Studies, New York, NY USA. [Shindell, Drew T.] Duke Univ, Nicholas Sch Environm, Durham, NC 27708 USA. RP Voulgarakis, A (reprint author), Univ London Imperial Coll Sci Technol & Med, Dept Phys, London, England. EM a.voulgarakis@imperial.ac.uk RI Shindell, Drew/D-4636-2012 FU NASA ACMAP; European Commission's Marie Curie International Research Staff Exchange Scheme (IRSES); National Science Foundation's Graduate Research Fellowship Program (NSF GRFP) FX The authors wish to thank NASA ACMAP for funding and the NASA High-End Computing (HEC) Program for computation resources through the NASA Center for Climate Simulation (NCCS) at Goddard Space Flight Center. Also, the authors thank the European Commission's Marie Curie International Research Staff Exchange Scheme (IRSES) for funding under the project titled "Regional climate-air quality interactions (REQUA)." M. Marlier would like to thank the National Science Foundation's Graduate Research Fellowship Program (NSF GRFP) for funding. The satellite and nonsatellite data sets used for this analysis are publicly available from the corresponding data set websites (TES: ftp://l5eil01.larc.nasa.gov/TES/, MODIS: http://modis-atmos.gsfc.nasa.gov/MOD08_M3/, MISR: https://eosweb.larc.nasa.gov/project/misr/version/pge12c, GMD: ftp://ftp.cmdl.noaa.gov/data/trace_gases/co/flask/, and WOUDC: http://beta.woudc.org/data/stations/, AERONET: http://aeronet.gsfc.nasa.gov/). All the model output data and the analysis codes used here are available for free from the lead author upon request (a.voulgarakis@imperial.ac.uk). We thank the TES, MODIS, MISR, GMD, WOUDC, and AERONET PIs and their staff for establishing and maintaining the websites used in this investigation. NR 70 TC 13 Z9 13 U1 2 U2 30 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD JUL 27 PY 2015 VL 120 IS 14 BP 7157 EP 7173 DI 10.1002/2014JD022926 PG 17 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA CP3TL UT WOS:000359804900028 ER PT J AU Zhang, Q Natraj, V Li, KF Shia, RL Fu, DJ Pongetti, TJ Sander, SP Roehl, CM Yung, YL AF Zhang, Qiong Natraj, Vijay Li, King-Fai Shia, Run-Lie Fu, Dejian Pongetti, Thomas J. Sander, Stanley P. Roehl, Coleen M. Yung, Yuk L. TI Accounting for aerosol scattering in the CLARS retrieval of column averaged CO2 mixing ratios SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE aerosol; scattering; X-CO2 ID LOS-ANGELES; AIR-QUALITY; MODEL; EMISSIONS; NETWORK; AERONET AB The California Laboratory for Atmospheric Remote Sensing Fourier transform spectrometer (CLARS-FTS) deployed at Mount Wilson, California, has been measuring column abundances of greenhouse gases in the Los Angeles (LA) basin in the near-infrared spectral region since August 2011. CLARS-FTS measures reflected sunlight and has high sensitivity to absorption and scattering in the boundary layer. In this study, we estimate the retrieval biases caused by aerosol scattering and present a fast and accurate approach to correct for the bias in the CLARS column averaged CO2 mixing ratio product, X-CO2. The high spectral resolution of 0.06cm(-1) is exploited to reveal the physical mechanism for the bias. We employ a numerical radiative transfer model to simulate the impact of neglecting aerosol scattering on the CO2 and O-2 slant column densities operationally retrieved from CLARS-FTS measurements. These simulations show that the CLARS-FTS operational retrieval algorithm likely underestimates CO2 and O-2 abundances over the LA basin in scenes with moderate aerosol loading. The bias in the CO2 and O-2 abundances due to neglecting aerosol scattering cannot be canceled by ratioing each other in the derivation of the operational product of X-CO2. We propose a new method for approximately correcting the aerosol-induced bias. Results for CLARS X-CO2 are compared to direct-Sun X-CO2 retrievals from a nearby Total Carbon Column Observing Network (TCCON) station. The bias-correction approach significantly improves the correlation between the X-CO2 retrieved from CLARS and TCCON, demonstrating that this approach can increase the yield of useful data from CLARS-FTS in the presence of moderate aerosol loading. C1 [Zhang, Qiong; Shia, Run-Lie; Roehl, Coleen M.; Yung, Yuk L.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Natraj, Vijay; Fu, Dejian; Pongetti, Thomas J.; Sander, Stanley P.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Li, King-Fai] Univ Washington, Dept Appl Math, Seattle, WA 98195 USA. RP Zhang, Q (reprint author), CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. EM qzh@caltech.edu OI Li, King-Fai/0000-0003-0150-2910 FU NASA [NNX13AK34G]; Jet Propulsion Laboratory [P1367828]; KISS program at Caltech; California Air Resources Board; NOAA Climate Program; NIST GHG and Climate Science Program; NASA Carbon Cycle Science Program; JPL Earth Science and Technology Directorate FX We thank Paul Wennberg, C. Wong, J. Margolis, S. Newman, C. Miller, D. Crisp, M. Gerstell, X. Xi, P. Kopparla, P. Gao, R. Hu, and L. Kuai for their helpful comments. We thank Jochen Stutz and his staff for establishing and maintaining the AERONET Caltech site used in this investigation. We also thank the anonymous reviewers whose comments helped improve the manuscript significantly. This research was supported in part by NASA grant NNX13AK34G to the California Institute of Technology, grant P1367828 from the Jet Propulsion Laboratory, and the KISS program at Caltech. Support for CLARS from the California Air Resources Board, NOAA Climate Program, NIST GHG and Climate Science Program, NASA Carbon Cycle Science Program, and JPL Earth Science and Technology Directorate is gratefully acknowledged. TCCON data were obtained from the TCCON Data Archive, hosted by the Carbon Dioxide Information Analysis Center-tccon.onrl.gov. AERONET data for this paper can be downloaded online. CLARS-FTS data are available from the authors upon request. NR 33 TC 3 Z9 3 U1 1 U2 6 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD JUL 27 PY 2015 VL 120 IS 14 BP 7205 EP 7218 DI 10.1002/2015JD023499 PG 14 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA CP3TL UT WOS:000359804900031 ER PT J AU Nair, PJ Froidevaux, L Kuttippurath, J Zawodny, JM Russell, JM Steinbrecht, W Claude, H Leblanc, T van Gijsel, JAE Johnson, B Swart, DPJ Thomas, A Querel, R Wang, R Anderson, J AF Nair, P. J. Froidevaux, L. Kuttippurath, J. Zawodny, J. M. Russell, J. M., III Steinbrecht, W. Claude, H. Leblanc, T. van Gijsel, J. A. E. Johnson, B. Swart, D. P. J. Thomas, A. Querel, R. Wang, R. Anderson, J. TI Subtropical and midlatitude ozone trends in the stratosphere: Implications for recovery SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE stratospheric ozone trends; ozone recovery; midlatitude ozone; subtropical ozone; lidar measurements; satellite observations ID SAGE II; TOTAL COLUMN; TIME-SERIES; SATELLITE; VARIABILITY; EVOLUTION; PROFILES; STATIONS; LIDAR; HCL AB We present a comprehensive analysis of the trends of stratospheric ozone in the midlatitudes and subtropics. The analysis is performed using ground-based and space-based measurements over the light detection and ranging stations for the period 1985-2012. Also, trends are estimated for the zonal mean data made from a merged satellite data set, Global OZone Chemistry And Related trace gas Data records for the Stratosphere, over 1979-2012. The linear trends in stratospheric ozone are estimated using piecewise linear trend (PWLT) functions. The ozone trends during the increasing phase of halogens (before 1997) range from -0.2 0.08 to -1 0.07%yr(-1) in the midlatitudes and -0.2 0.06 to -0.7 0.05%yr(-1) in the subtropics at 15-45km, depending on altitude. In 1997-2012, the PWLT analyses show a positive trend, significantly different from zero at the 95% confidence intervals, toward ozone recovery in the middle- and low-latitude upper stratosphere (35-45km), and the trends are about +0.5 +/- 0.07%yr(-1) at midlatitudes and about +0.3 +/- 0.05%yr(-1) at subtropical latitudes. However, negative and insignificant trends are estimated in the lower stratosphere (15-20km) over 1997-2012 in the midlatitudes, mainly due to the dynamics, as demonstrated by the large (50-60%) contributions from the quasi-biennial oscillation, El Nino-Southern Oscillation, and planetary wave activity to recent ozone changes. This suggests that the ozone changes are governed by the interannual variations in meteorology and dynamics of the regions; these factors will influence the recovery detection time and the behavior of the recovery path to pre-1980 levels. C1 [Nair, P. J.] Ctr Earth Sci Studies, Thiruvananthapuram, Kerala, India. [Froidevaux, L.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Kuttippurath, J.] Indian Inst Technol Kharagpur, Kharagpur, W Bengal, India. [Zawodny, J. M.] NASA Langley Res Ctr, Hampton, VA USA. [Russell, J. M., III; Anderson, J.] Hampton Univ, Hampton, VA 23668 USA. [Steinbrecht, W.; Claude, H.] Deutsch Wetterdienst, Hohenpeissenberg, Germany. [Leblanc, T.] CALTECH, Jet Prop Lab, Wrightwood, CA USA. [van Gijsel, J. A. E.] Royal Netherlands Meteorol Inst, NL-3730 AE De Bilt, Netherlands. [Johnson, B.] NOAA, Boulder, CO USA. [Swart, D. P. J.] Natl Inst Publ Hlth & Environm, NL-3720 BA Bilthoven, Netherlands. [Thomas, A.; Querel, R.] Natl Inst Water & Atmospher Res, Lauder, New Zealand. [Wang, R.] Georgia Inst Technol, Atlanta, GA 30332 USA. RP Nair, PJ (reprint author), Ctr Earth Sci Studies, Thiruvananthapuram, Kerala, India. EM pjnnair@yahoo.in RI Steinbrecht, Wolfgang/G-6113-2010; Querel, Richard/D-3770-2015; van Gijsel, Joanna/F-8087-2010 OI Steinbrecht, Wolfgang/0000-0003-0680-6729; Querel, Richard/0000-0001-8792-2486; FU New Zealands Ministry of Business, Innovation and Employment; NASA FX The ground-based lidar and ozonesonde data were obtained from the publicly available NDACC (http://www.ndacc.org) and WOUDC (http://www.woudc.org). Measurements at NIWA Lauder are core funded through New Zealands Ministry of Business, Innovation and Employment. The satellite data HALOE are from http://haloe.gats-inc.com/download/index.php, SAGE II from https://eosweb.larc.nasa.gov/, and MLS from http://disc.sci.gsfc.nasa.gov/services. We thank the National Aeronautics and Space Administration (NASA) Langley Research Center (LaRC) and the NASA Langley Chemistry and Dynamics Branch for providing SAGE II data, the collaborative institutes of the NASA-LaRC for maintaining HALOE data, and the NASA Goddard Earth Sciences Data and Information Services Center (GES DISC) for the MLS data. The GOZCARDS data used in this effort were acquired as part of the activities of NASA's Science Mission Directorate and are archived and distributed by the GES DISC at http://disc.sci.gsfc.nasa.gov. All the proxy data (QBO, ENSO, Aerosol, and Solar Flux) used for the regression analysis are available online, and the data sources are given in the text itself (section 3). We thank H. Nakane, National Institute for Environmental Studies, Ibaraki, Japan, and T. Uekubo, Japan Meteorological Agency, Japan, for providing the lidar and ozonesonde data, respectively. A part of this work was performed during P.J.N.'s tenure at CESS Thiruvananthapuram, and hence, the affiliation of that institute is given there. P.J.N. thanks N.P. Kurian, the director of CESS, and V. Nandakumar for their help. We thank E. Kyrola of FMI, Finland, for his help with providing the trend values from their study. Work at the Jet Propulsion Laboratory, California Institute of Technology was done under contract with the NASA. NR 31 TC 2 Z9 2 U1 3 U2 14 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD JUL 27 PY 2015 VL 120 IS 14 BP 7247 EP 7257 DI 10.1002/2014JD022371 PG 11 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA CP3TL UT WOS:000359804900034 ER PT J AU Jin, J Puigibert, MG Giner, L Slater, JA Lamont, MRE Verma, VB Shaw, MD Marsili, F Nam, SW Oblak, D Tittel, W AF Jin, J. Puigibert, M. Grimau Giner, L. Slater, J. A. Lamont, M. R. E. Verma, V. B. Shaw, M. D. Marsili, F. Nam, S. W. Oblak, D. Tittel, W. TI Entanglement swapping with quantum-memory-compatible photons SO PHYSICAL REVIEW A LA English DT Article ID ENTANGLING PHOTONS; SINGLE PHOTONS; LINEAR OPTICS; STATE; INTERFERENCE; EFFICIENCY; REPEATERS; DETECTORS; QUBITS; SYSTEM AB We report entanglement swapping with time-bin entangled photon pairs, each constituted of a 795-nm photon and a 1533-nm photon, that are created via spontaneous parametric down conversion in a nonlinear crystal. After projecting the two 1533-nm photons onto a Bell state, entanglement between the two 795-nm photons is verified by means of quantum state tomography. As an important feature, the wavelength and bandwidth of the 795-nm photons is compatible with Tm:LiNbO3-based quantum memories, making our experiment an important step towards the realization of a quantum repeater. C1 [Jin, J.; Puigibert, M. Grimau; Giner, L.; Slater, J. A.; Lamont, M. R. E.; Oblak, D.; Tittel, W.] Univ Calgary, Inst Quantum Sci & Technol, Dept Phys & Astron, Calgary, AB T2N 1N4, Canada. [Verma, V. B.; Nam, S. W.] Natl Inst Stand & Technol, Boulder, CO 80305 USA. [Shaw, M. D.; Marsili, F.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Jin, J (reprint author), Univ Waterloo, Inst Quantum Comp, Dept Phys & Astron, 200 Univ Ave West, Waterloo, ON N2L 3G1, Canada. EM wtittel@ucalgary.ca RI Slater, Joshua/F-2523-2011; Tittel, Wolfgang/A-1600-2011 FU Alberta Innovates Technology Futures (AITF); National Science and Engineering Research Council of Canada (NSERC); U.S. Defense Advanced Research Projects Agency (DARPA) Quiness Program; U.S. Defense Advanced Research Projects Agency (DARPA) InPho Program; Killam Trusts FX The authors thank V. Kiselyov for support with electrical engineering. We gratefully acknowledge support through Alberta Innovates Technology Futures (AITF), the National Science and Engineering Research Council of Canada (NSERC), the U.S. Defense Advanced Research Projects Agency (DARPA) Quiness and InPho Programs, and the Killam Trusts. Part of the research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. W.T. acknowledges support as a senior fellow of the Canadian Institute for Advanced Research (CIFAR). NR 40 TC 1 Z9 1 U1 2 U2 17 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1050-2947 EI 1094-1622 J9 PHYS REV A JI Phys. Rev. A PD JUL 27 PY 2015 VL 92 IS 1 AR 012329 DI 10.1103/PhysRevA.92.012329 PG 6 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA CN7EW UT WOS:000358597900009 ER PT J AU Okada, T Zolensky, ME Ireland, TR Yada, T AF Okada, Tatsuaki Zolensky, Michael E. Ireland, Trevor R. Yada, Toru TI The Earth, Planets and Space Special Issue: "Science of solar system materials examined from Hayabusa and future missions" SO EARTH PLANETS AND SPACE LA English DT Editorial Material ID ITOKAWA DUST PARTICLES; ASTEROID 25143 ITOKAWA; ISOTOPIC COMPOSITIONS; MINERALOGY; REGOLITH; SAMPLES; ORIGIN; EVOLUTION; CHONDRITES C1 [Okada, Tatsuaki; Yada, Toru] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2525210, Japan. [Zolensky, Michael E.] NASA, Lyndon B Johnson Space Ctr, Astromat Res & Explorat Sci, Houston, TX 77058 USA. [Ireland, Trevor R.] Australian Natl Univ, Res Sch Earth Sci, Canberra, ACT 0200, Australia. RP Okada, T (reprint author), Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2525210, Japan. EM okada@planeta.sci.isas.jaxa.jp RI Ireland, Trevor/A-4993-2008 OI Ireland, Trevor/0000-0001-7617-3889 NR 26 TC 3 Z9 3 U1 1 U2 10 PU SPRINGER HEIDELBERG PI HEIDELBERG PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY SN 1880-5981 J9 EARTH PLANETS SPACE JI Earth Planets Space PD JUL 26 PY 2015 VL 67 AR 116 DI 10.1186/s40623-015-0235-x PG 4 WC Geosciences, Multidisciplinary SC Geology GA CQ2KA UT WOS:000360427500001 ER PT J AU Work, TM Balazs, GH Summers, TM Hapdei, JR Tagarino, AP AF Work, Thierry M. Balazs, George H. Summers, Tammy M. Hapdei, Jessy R. Tagarino, Alden P. TI Causes of mortality in green turtles from Hawaii and the insular Pacific exclusive of fibropapillomatosis SO DISEASES OF AQUATIC ORGANISMS LA English DT Article DE Green turtle; Chelonia mydas; Mortality; Pathology; Trauma; Infectious disease; Nutrition; Pacific ID CHELONIA-MYDAS; SEA-TURTLES; LOGGERHEAD TURTLE; CARETTA-CARETTA; YOLK COELOMITIS; CANARY-ISLANDS; INFECTION; PATHOLOGY; OSTEOARTHRITIS; STRANDINGS AB Fibropapillomatosis (FP) comprises a majority of green turtle stranding in Hawaii; however, green turtles in the Pacific are also susceptible to non-FP related causes of death. We present here necropsy findings from 230 free-ranging green turtles originating from Hawaii, the Mariana archipelago, Palmyra Atoll, American Samoa, and Johnston Atoll that died from non-FP related causes. Most turtles died from fishing-induced or boat strike trauma followed by infectious/inflammatory diseases, nutritional problems (mainly cachexia), and an array of physiologic problems. Infectious/inflammatory problems included bacterial diseases of the lungs, eyes, liver or intestines, spirorchid fluke infection, or polyarthritis of unknown origin. Likelihood of a successful diagnosis of cause of death was a function of post-mortem decomposition. Fibropapillomatosis was not seen in turtles submitted from outside Hawaii. The preponderance of anthropogenic causes of mortality offers some management opportunities to mitigate causes of death in these animals by, for example, implementing measures to decrease boating and fishing interactions. C1 [Work, Thierry M.] US Geol Survey, Natl Wildlife Hlth Ctr, Honolulu Field Stn, Honolulu, HI 96850 USA. [Balazs, George H.] NOAA, Natl Marine Fisheries Serv, Pacific Isl Fisheries Sci Ctr, Honolulu, HI 96818 USA. [Summers, Tammy M.; Hapdei, Jessy R.] Commonwealth Northern Marianas Dept Land & Nat Re, Sea Turtle Program, Saipan, CM 96950 USA. [Tagarino, Alden P.] Amer Samoa Govt, Dept Marine & Wildlife Resources, Wildlife Div, Pago Pago, AS 96799 USA. RP Work, TM (reprint author), US Geol Survey, Natl Wildlife Hlth Ctr, Honolulu Field Stn, POB 50167, Honolulu, HI 96850 USA. EM thierry_work@usgs.gov NR 29 TC 3 Z9 4 U1 4 U2 37 PU INTER-RESEARCH PI OLDENDORF LUHE PA NORDBUNTE 23, D-21385 OLDENDORF LUHE, GERMANY SN 0177-5103 EI 1616-1580 J9 DIS AQUAT ORGAN JI Dis. Aquat. Org. PD JUL 23 PY 2015 VL 115 IS 2 BP 103 EP 110 DI 10.3354/dao02890 PG 8 WC Fisheries; Veterinary Sciences SC Fisheries; Veterinary Sciences GA CN5ZK UT WOS:000358512700002 PM 26203881 ER PT J AU Shultz, MJ Vu, TH AF Shultz, Mary Jane Tuan Hoang Vu TI Hydrogen Bonding between Water and Tetrahydrofuran Relevant to Clathrate Formation SO JOURNAL OF PHYSICAL CHEMISTRY B LA English DT Article ID HYDROPHOBIC ENVIRONMENT; CARBON-TETRACHLORIDE; HYDRATE; INTERFACE; GAS; AIR; TEMPERATURE; TRANSITION; CLUSTERS; SYSTEMS AB Tetrahydrofuran (THF) is well-known as a clathrate former as well as a promoter for gas hydrate formation. This work examines interactions between water and tetrahydrofuran via the effect on waters vibrational spectrum. Due to waters large oscillator strength in the hydrogen-bonded region, interactions are diagnosed by isolating small clusters in a transparent medium (carbon tetrachloride in this study). A weak THF/water hydrogen bond is reflected by a 3450 cm(-1) OH-donor vibration (blue shifted from the water/water hydrogen bond) and a 3685 cm(-1) nonbonded OH stretch (blue shifted 22 cm(-1) from the decoupled OH stretch in this medium). Increasing the THF concentration results in another 20 cm(-1) blue shift of the OH-donor stretch. Additional THF does not complex with free water but rather joins with existing THF/water structures to form a cluster enriched in THF. These results complement previous work examining THF vibrations in clathrate hydrates. Together, they generate a picture in which water mediates between THF pairs - mediation that affects vibrational frequencies of both species. In addition to a frequency shift, waters hydrogen-bonded resonance gains oscillator strength due to its mediating configuration. C1 [Shultz, Mary Jane] Tufts Univ, Dept Chem, Lab Water & Surface Anal, Medford, MA 02155 USA. [Tuan Hoang Vu] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Shultz, MJ (reprint author), Tufts Univ, Dept Chem, Lab Water & Surface Anal, Medford, MA 02155 USA. EM Mary.Shultz@Tufts.edu; Tuan.H.Vu@JPL.nasa.gov RI Vu, Tuan/F-5223-2017 OI Vu, Tuan/0000-0001-6839-9765 FU U.S. National Science Foundation [CHE1306933] FX The authors gratefully acknowledge U.S. National Science Foundation Grant CHE1306933 for partial financial support of this work. NR 44 TC 3 Z9 3 U1 2 U2 27 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 JUL 23 PY 2015 VL 119 IS 29 BP 9167 EP 9172 DI 10.1021/jp509343x PG 6 WC Chemistry, Physical SC Chemistry GA CN7OM UT WOS:000358623900039 PM 25427311 ER PT J AU Sterling, AC Moore, RL Falconer, DA Adams, M AF Sterling, Alphonse C. Moore, Ronald L. Falconer, David A. Adams, Mitzi TI Small-scale filament eruptions as the driver of X-ray jets in solar coronal holes SO NATURE LA English DT Article ID MASS EJECTIONS; FLUX EMERGENCE; BLOWOUT JET; QUIET SUN; MAGNETIC RECONNECTION; BRIGHT POINTS; ALFVEN WAVES; HOT-PLASMA; FLARES; HINODE AB Solar X-ray jets are thought to be made by a burst of reconnection of closed magnetic field at the base of a jet with ambient open field(1,2). In the accepted version of the 'emerging-flux' model, such a reconnection occurs at a plasma current sheet between the open field and the emerging closed field, and also forms a localized X-ray brightening that is usually observed at the edge of the jet's base(1,3). Here we report high-resolution X-ray and extreme-ultraviolet observations of 20 randomly selected X-ray jets that form in coronal holes at the Sun's poles. In each jet, contrary to the emerging-flux model, a miniature version of the filament eruptions that initiate coronal mass ejections(4-7) drives the jet-producing reconnection. The X-ray bright point occurs by reconnection of the 'legs' of the minifilament-carrying erupting closed field, analogous to the formation of solar flares in larger-scale eruptions. Previous observations have found that some jets are driven by base-field eruptions(8-11), but only one such study, of only one jet, provisionally questioned the emerging-flux model(12). Our observations support the view that solar filament eruptions are formed by a fundamental explosive magnetic process that occurs on a vast range of scales, from the biggest mass ejections and flare eruptions down to X-ray jets, and perhaps even down to smaller jets that may power coronal heating(10,13,14). A similar scenario has previously been suggested, but was inferred from different observations and based on a different origin of the erupting minifilament(15). C1 [Sterling, Alphonse C.; Moore, Ronald L.; Falconer, David A.; Adams, Mitzi] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. [Moore, Ronald L.; Falconer, David A.] Univ Alabama, Ctr Space Plasma & Aeron Res, Huntsville, AL 35899 USA. RP Sterling, AC (reprint author), NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. EM alphonse.sterling@nasa.gov; ron.moore@nasa.gov FU Heliophysics Division of NASA's Science Mission Directorate through the Living With A Star Targeted Research and Technology Program(LWS TRT); Hinode Project FX A.C.S. and R.L.M. were supported by funding from the Heliophysics Division of NASA's Science Mission Directorate through the Living With A Star Targeted Research and Technology Program(LWS TR&T), and the Hinode Project. Both benefited from TR&T discussions and from discussions with S. K. Antiochos. We thank D. M. Zarro for assistance with video development. A.C.S. benefited from discussions held at the International Space Science Institute (ISSI; Switzerland) International Team on Solar Coronal Jets (led by N. Raouafi). Hinode is a Japanese mission developed and launched by the Institute of Space and Astronautical Science (ISAS) of the Japan Aerospace Exploration Agency (JAXA), with the National Astronomical Observatory Japan (NAOJ) as a domestic partner, and NASA and the Science and Technology Facilities Council (UK) as international partners. It is operated by these agencies in cooperation with the European Space Agency and Norwegian Space Agency. NR 45 TC 25 Z9 25 U1 0 U2 4 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 EI 1476-4687 J9 NATURE JI Nature PD JUL 23 PY 2015 VL 523 IS 7561 BP 437 EP U130 DI 10.1038/nature14556 PG 12 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CN4DD UT WOS:000358378900031 PM 26147079 ER PT J AU Bellinger, MR Banks, MA Bates, SJ Crandall, ED Garza, JC Sylvia, G Lawson, PW AF Bellinger, M. Renee Banks, Michael A. Bates, Sarah J. Crandall, Eric D. Garza, John Carlos Sylvia, Gil Lawson, Peter W. TI Geo-Referenced, Abundance Calibrated Ocean Distribution of Chinook Salmon (Oncorhynchus tshawytscha) Stocks across the West Coast of North America SO PLOS ONE LA English DT Article ID PACIFIC SALMON; COHO SALMON; TEMPORAL PATTERNS; BRITISH-COLUMBIA; GENETIC DATA; IDENTIFICATION; CALIFORNIA; MANAGEMENT; FISHERIES; DNA AB Understanding seasonal migration and localized persistence of populations is critical for effective species harvest and conservation management. Pacific salmon (genus Oncorhynchus) forecasting models predict stock composition, abundance, and distribution during annual assessments of proposed fisheries impacts. Most models, however, fail to account for the influence of biophysical factors on year-to-year fluctuations in migratory distributions and stock-specific survival. In this study, the ocean distribution and relative abundance of Chinook salmon (O. tshawytscha) stocks encountered in the California Current large marine ecosystem, U.S. A were inferred using catch-per-unit effort (CPUE) fisheries and genetic stock identification data. In contrast to stock distributions estimated through coded-wire-tag recoveries (typically limited to hatchery salmon), stock-specific CPUE provides information for both wild and hatchery fish. Furthermore, in contrast to stock composition results, the stock-specific CPUE metric is independent of other stocks and is easily interpreted over multiple temporal or spatial scales. Tests for correlations between stock-specific CPUE and stock composition estimates revealed these measures diverged once proportional contributions of locally rare stocks were excluded from data sets. A novel aspect of this study was collection of data both in areas closed to commercial fisheries and during normal, open commercial fisheries. Because fishing fleet efficiency influences catch rates, we tested whether CPUE differed between closed area (non-retention) and open area (retention) data sets. A weak effect was indicated for some, but not all, analyzed cases. Novel visualizations produced from stock-specific CPUE-based ocean abundance facilitates consideration of how highly refined, spatial and genetic information could be incorporated in ocean fisheries management systems and for investigations of biogeographic factors that influence migratory distributions of fish. C1 [Bellinger, M. Renee; Banks, Michael A.] Oregon State Univ, Hatfield Marine Sci Ctr, Dept Fisheries & Wildlife, Coastal Oregon Marine Expt Stn, Newport, OR 97365 USA. [Bates, Sarah J.] Calif Salmon Council, Oakland, CA USA. [Crandall, Eric D.; Garza, John Carlos] Natl Marine Fisheries Serv, Natl Oceanog & Atmospher Adm, Southwest Fisheries Sci Ctr, Santa Cruz, CA USA. [Garza, John Carlos] Univ Calif Santa Cruz, Inst Marine Sci, Santa Cruz, CA 95064 USA. [Sylvia, Gil] Oregon State Univ, Hatfield Marine Sci Ctr, Dept Appl Econ, Coastal Oregon Marine Expt Stn, Newport, OR 97365 USA. [Lawson, Peter W.] Natl Marine Fisheries Serv, Natl Oceanog & Atmospher Adm, Northwest Fisheries Sci Ctr, Newport, OR USA. RP Bellinger, MR (reprint author), Oregon State Univ, Hatfield Marine Sci Ctr, Dept Fisheries & Wildlife, Coastal Oregon Marine Expt Stn, Newport, OR 97365 USA. EM reneebellinger@gmail.com FU National Oceanic and Atmospheric Administration (NOAA); NOAA [NA07NMF4540337]; California Salmon Council; [NA07NMF4540337 NA08NMF4720662 NA09NMF4720381]; [NA08NMF4270421] FX This study was designed and conducted as an industry-science collaboration between industry partners California Salmon Council and OregonSalmon Commission and scientific investigators affiliated with academic and federal institutions. Major funding originated from the National Oceanic and Atmospheric Administration (NOAA). Funds were awarded to Nancy Fitzpatrick, Oregon Salmon Commission and David Goldenberg, California Salmon Council NA07NMF4540337 NA08NMF4720662 NA09NMF4720381, Saltonstall Kennedy Grant Program NA08NMF4270421. NOAA scientists and university scientists were co-Principal Investigators on all major grants except the Saltonstall-Kennedy Grant (University only). Pacific States Marine Fisheries Commission acted via contract with NOAA to help distribute Klamath Disaster funds (NA07NMF4540337) to the states. The California Salmon Council and Oregon Salmon Commission helped to facilitate the industry partnership and distributed funds to industry for their participation in at-sea sampling and data collection. The California Salmon Council provided support in the form of salary for author SJB, who was hired to manage California at-sea sample collections and contribute to manuscript preparation. The specific role of this author is articulated in the 'author contributions' section. NR 50 TC 2 Z9 2 U1 2 U2 17 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD JUL 22 PY 2015 VL 10 IS 7 AR e0131276 DI 10.1371/journal.pone.0131276 PG 25 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CN7EO UT WOS:000358597100013 PM 26200779 ER PT J AU Taylor, SR Mingarelli, CMF Gair, JR Sesana, A Theureau, G Babak, S Bassa, CG Brem, P Burgay, M Caballero, RN Champion, DJ Cognard, I Desvignes, G Guillemot, L Hessels, JWT Janssen, GH Karuppusamy, R Kramer, M Lassus, A Lazarus, P Lentati, L Liu, K Oslowski, S Perrodin, D Petiteau, A Possenti, A Purver, MB Rosado, PA Sanidas, SA Smits, R Stappers, B Tiburzi, C van Haasteren, R Vecchio, A Verbiest, JPW AF Taylor, S. R. Mingarelli, C. M. F. Gair, J. R. Sesana, A. Theureau, G. Babak, S. Bassa, C. G. Brem, P. Burgay, M. Caballero, R. N. Champion, D. J. Cognard, I. Desvignes, G. Guillemot, L. Hessels, J. W. T. Janssen, G. H. Karuppusamy, R. Kramer, M. Lassus, A. Lazarus, P. Lentati, L. Liu, K. Oslowski, S. Perrodin, D. Petiteau, A. Possenti, A. Purver, M. B. Rosado, P. A. Sanidas, S. A. Smits, R. Stappers, B. Tiburzi, C. van Haasteren, R. Vecchio, A. Verbiest, J. P. W. CA EPTA Collaboration TI Limits on Anisotropy in the Nanohertz Stochastic Gravitational Wave Background SO PHYSICAL REVIEW LETTERS LA English DT Article ID BLACK-HOLE BINARIES; PULSAR TIMING ARRAYS; COVARIANCE MATRICES; COALESCENCE RATE; COSMIC STRINGS; RADIATION; SYSTEMS; PACKAGE; TEMPO2 AB The paucity of observed supermassive black hole binaries (SMBHBs) may imply that the gravitational wave background (GWB) from this population is anisotropic, rendering existing analyses suboptimal. We present the first constraints on the angular distribution of a nanohertz stochastic GWB from circular, inspiral-driven SMBHBs using the 2015 European Pulsar Timing Array data. Our analysis of the GWB in the similar to 2-90 nHz band shows consistency with isotropy, with the strain amplitude in l > 0 spherical harmonic multipoles less than or similar to 40% of the monopole value. We expect that these more general techniques will become standard tools to probe the angular distribution of source populations. C1 [Taylor, S. R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Taylor, S. R.; Gair, J. R.; van Haasteren, R.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Mingarelli, C. M. F.] CALTECH, TAPIR Theoret Astrophys, Pasadena, CA 91125 USA. [Mingarelli, C. M. F.; Caballero, R. N.; Champion, D. J.; Desvignes, G.; Karuppusamy, R.; Kramer, M.; Lassus, A.; Lazarus, P.; Liu, K.; Oslowski, S.; Verbiest, J. P. W.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Mingarelli, C. M. F.; Sesana, A.; Vecchio, A.] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. [Sesana, A.; Babak, S.; Brem, P.] Albert Einstein Inst, Max Planck Inst Gravitat Phys, D-14476 Golm, Germany. [Theureau, G.; Cognard, I.; Guillemot, L.; Lassus, A.] Univ Orleans, CNRS, Lab Phys & Chim Environm & Espace LPC2E, F-45071 Orleans, France. [Theureau, G.; Cognard, I.; Guillemot, L.] CNRS INSU, Stn Radioastron Nancay, Observ Paris, F-18330 Nancay, France. [Theureau, G.] Univ Paris Diderot, CNRS INSU, Lab Univ & Theories LUTh, Observ Paris, F-92190 Meudon, France. [Bassa, C. G.; Hessels, J. W. T.; Janssen, G. H.; Smits, R.] Netherlands Inst Radio Astron, ASTRON, NL-7990 AA Dwingeloo, Netherlands. [Bassa, C. G.; Janssen, G. H.; Kramer, M.; Purver, M. B.; Sanidas, S. A.; Stappers, B.] Univ Manchester, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England. [Burgay, M.; Perrodin, D.; Possenti, A.; Tiburzi, C.] INAF Osservatorio Astron Cagliari, I-09047 Selargius, CA, Italy. [Hessels, J. W. T.; Sanidas, S. A.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 XH Amsterdam, Netherlands. [Lentati, L.] Cavendish Lab, Astrophys Grp, Cambridge CB3 0HE, England. [Oslowski, S.; Verbiest, J. P. W.] Univ Bielefeld, Fak Phys, D-33501 Bielefeld, Germany. [Petiteau, A.] Univ Paris 07, APC UFR Phys, F-75205 Paris 13, France. [Rosado, P. A.] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia. [Rosado, P. A.] Albert Einstein Inst, Max Planck Inst Gravitat Phys, D-30167 Hannover, Germany. [Tiburzi, C.] Univ Cagliari, Dipartimento Fis, I-09042 Monserrato, CA, Italy. RP Taylor, SR (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Stephen.R.Taylor@jpl.nasa.gov RI Perrodin, Delphine/L-1916-2016; Vecchio, Alberto/F-8310-2015; Sesana, Alberto/Q-9826-2016; OI Perrodin, Delphine/0000-0002-1806-2483; Vecchio, Alberto/0000-0002-6254-1617; Sesana, Alberto/0000-0003-4961-1606; Burgay, Marta/0000-0002-8265-4344; Taylor, Stephen/0000-0003-0264-1453; Oslowski, Stefan/0000-0003-0289-0732 FU "Programme National de Cosmologie and Galaxies" (PNCG) of CNRS/INSU, France; STFC in the UK; Netherlands Foundation for Scientific Research NWO; STFC; RAS; NASA Postdoctoral Program at the Jet Propulsion Laboratory; NASA; Marie Curie International Outgoing Fellowship within the 7th European Community Framework Programme; NSF under MRI-R2 award [PHY-0960291]; Sherman Fairchild Foundation; Higher Education Funding Council for England; Royal Society; Junior Research Fellowship at Trinity Hall College, Cambridge University; NWO Vidi fellowship; International Max Planck Research School Bonn/Cologne; Bonn-Cologne Graduate School; National Natural Science Foundation of China [11373011]; NASA Einstein Fellowship [PF3-140116]; ERC Starting Grant 'DRAGNET' [337062]; European Research Council [610058]; Alexander von Humboldt Foundation; NSF [PHY-1066293] FX This work was carried out under the aegis of the EPTA. Part of this work is based on observations with the 100-m telescope of the Max-Planck-Institut fur Radioastronomie (MPIfR) at Effelsberg. The Nancay Radio Observatory is operated by the Paris Observatory, associated to the French Centre National de la Recherche Scientifique (CNRS). We acknowledge financial support from "Programme National de Cosmologie and Galaxies" (PNCG) of CNRS/INSU, France. Pulsar research at the Jodrell Bank Centre for Astrophysics and the observations using the Lovell telescope is supported by a consolidated grant from the STFC in the UK. The Westerbork Synthesis Radio Telescope is operated by the Netherlands Institute for Radio Astronomy (ASTRON) with support from The Netherlands Foundation for Scientific Research NWO. S. R. T. acknowledges the support of the STFC and the RAS. This research was in part supported by S. R. T's appointment to the NASA Postdoctoral Program at the Jet Propulsion Laboratory, administered by Oak Ridge Associated Universities through a contract with NASA. C. M. F. M. was supported by a Marie Curie International Outgoing Fellowship within the 7th European Community Framework Programme. This research was performed in part using the Zwicky computer cluster at Caltech supported by NSF under MRI-R2 award No. PHY-0960291 and by the Sherman Fairchild Foundation. This work was in part performed using the Darwin Supercomputer of the University of Cambridge High Performance Computing Service, provided by Dell Inc. using Strategic Research Infrastructure Funding from the Higher Education Funding Council for England and funding from the STFC. A. S. and J. G. are supported by the Royal Society. L. L. was supported by a Junior Research Fellowship at Trinity Hall College, Cambridge University. S. A. S. acknowledges funding from an NWO Vidi fellowship (PI: J. W. T. H.). R. N. C. acknowledges the support of the International Max Planck Research School Bonn/Cologne and the Bonn-Cologne Graduate School. K. J. L. is supported by the National Natural Science Foundation of China (Grant No. 11373011). R. vH. is supported by NASA Einstein Fellowship grant PF3-140116. J. W. T. H. acknowledges funding from an NWO Vidi fellowship and ERC Starting Grant 'DRAGNET' (337062). P. L. acknowledges the support of the International Max Planck Research School Bonn/Cologne. K. L. acknowledges the financial support by the European Research Council for the ERC Synergy Grant BlackHoleCam under Contract No. 610058. S. O. is supported by the Alexander von Humboldt Foundation. The authors also acknowledge support of NSFAward No. PHY-1066293 and the hospitality of the Aspen Center for Physics. NR 52 TC 11 Z9 11 U1 2 U2 9 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 0031-9007 EI 1079-7114 J9 PHYS REV LETT JI Phys. Rev. Lett. PD JUL 22 PY 2015 VL 115 IS 4 AR 041101 DI 10.1103/PhysRevLett.115.041101 PG 6 WC Physics, Multidisciplinary SC Physics GA CN4AA UT WOS:000358369000001 PM 26252674 ER PT J AU Allison, R Lindsay, SN Sherwin, BD de Bernardis, F Bond, JR Calabrese, E Devlin, MJ Dunkley, J Gallardo, P Henderson, S Hincks, AD Hlozek, R Jarvis, M Kosowsky, A Louis, T Madhavacheril, M McMahon, J Moodley, K Naess, S Newburgh, L Niemack, MD Page, LA Partridge, B Sehgal, N Spergel, DN Staggs, ST van Engelen, A Wollack, EJ AF Allison, Rupert Lindsay, Sam N. Sherwin, Blake D. de Bernardis, Francesco Bond, J. Richard Calabrese, Erminia Devlin, Mark J. Dunkley, Joanna Gallardo, Patricio Henderson, Shawn Hincks, Adam D. Hlozek, Renee Jarvis, Matt Kosowsky, Arthur Louis, Thibaut Madhavacheril, Mathew McMahon, Jeff Moodley, Kavilan Naess, Sigurd Newburgh, Laura Niemack, Michael D. Page, Lyman A. Partridge, Bruce Sehgal, Neelima Spergel, David N. Staggs, Suzanne T. van Engelen, Alexander Wollack, Edward J. TI The Atacama Cosmology Telescope: measuring radio galaxy bias through cross-correlation with lensing SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE large-scale structure of Universe-radio continuum: galaxies ID MICROWAVE BACKGROUND POLARIZATION; ACTIVE GALACTIC NUCLEI; LARGE-SCALE BIAS; VLA SKY SURVEY; K-Z RELATION; DARK-MATTER; 1ST SURVEY; LUMINOSITY FUNCTIONS; CONTINUUM SURVEYS; REDSHIFT CUTOFF AB We correlate the positions of radio galaxies in the FIRST survey with the cosmic microwave background lensing convergence estimated from the Atacama Cosmology Telescope over 470 deg(2) to determine the bias of these galaxies. We remove optically cross-matched sources below redshift z = 0.2 to preferentially select active galactic nuclei (AGN). We measure the angular cross-power spectrum C-t(kg) at 4.4 sigma significance in the multipole range 100 < 1 < 3000, corresponding to physical scales within approximate to 2-60 Mpc at an effective redshift z(eff) = 1.5. Modelling the AGN population with a redshift-dependent bias, the cross-spectrum is well fitted by the Planck best-fitting A cold dark matter cosmological model. Fixing the cosmology and assumed redshift distribution of sources, we fit for the overall bias model normalization, finding b(z(eff)) = 3.5 +/- 0.8 for the full galaxy sample and b(z(eff)) = 4.0 +/- 1.1(3.0 +/- 1.1) for sources brighter (fainter) than 2.5 mJy. This measurement characterizes the typical halo mass of radio-loud AGN: we find log (M-halo/M-circle dot) = 13.6(-0.4)(+0.3). C1 [Allison, Rupert; Lindsay, Sam N.; Calabrese, Erminia; Dunkley, Joanna; Jarvis, Matt; Louis, Thibaut; Naess, Sigurd] Univ Oxford, Subdept Astrophys, Oxford OX1 3RH, England. [Sherwin, Blake D.] Univ Calif Berkeley, Berkeley Ctr Cosmol Phys, LBL, Berkeley, CA 94720 USA. [Sherwin, Blake D.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [de Bernardis, Francesco; Gallardo, Patricio; Henderson, Shawn; Niemack, Michael D.] Cornell Univ, Dept Phys, Ithaca, NY 14853 USA. [Bond, J. Richard; van Engelen, Alexander] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada. [Devlin, Mark J.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. [Hincks, Adam D.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z4, Canada. [Hlozek, Renee; Spergel, David N.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Jarvis, Matt] Univ Western Cape, Dept Phys, ZA-7535 Bellville, South Africa. [Kosowsky, Arthur] Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA. [Madhavacheril, Mathew; Sehgal, Neelima] SUNY Stony Brook, Dept Phys & Astron, Stony Brook, NY 11794 USA. [McMahon, Jeff] Univ Michigan, Dept Phys, Ann Arbor, MI 48103 USA. [Moodley, Kavilan] Univ KwaZulu Natal, Astrophys & Cosmol Res Unit, Sch Math Stat & Comp Sci, ZA-4041 Durban, South Africa. [Newburgh, Laura] Univ Toronto, Dunlap Inst Astron & Astrophys, Toronto, ON M5S 3H4, Canada. [Page, Lyman A.; Staggs, Suzanne T.] Princeton Univ, Joseph Henry Labs Phys, Princeton, NJ 08544 USA. [Partridge, Bruce] Haverford Coll, Dept Phys & Astron, Haverford, PA 19041 USA. [Wollack, Edward J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Allison, R (reprint author), Univ Oxford, Subdept Astrophys, Denys Wilkinson Bldg, Oxford OX1 3RH, England. EM rupert.allison@astro.ox.ac.uk RI DE BERNARDIS, FLAVIA/C-9589-2016; Wollack, Edward/D-4467-2012 OI DE BERNARDIS, FLAVIA/0000-0001-9440-8629; Wollack, Edward/0000-0002-7567-4451 FU STFC PhD studentship; US National Science Foundation [AST-0408698, AST-0965625, PHY-0855887, PHY-1214379]; Princeton University; University of Pennsylvania; Cornell University; Canada Foundation for Innovation (CFI); Comision Nacional de Investigacion Cientifica y Tecnologica de Chile (CONICYT); CFI under Compute Canada; Government of Ontario; Ontario Research Fund; University of Toronto; NASA [NNX13AE56G, NNX14AB58G]; ERC [259505]; CONICYT [QUIMAL-120001, FONDECYT-1141113]; Misrahi research fund; Wilkinson research fund FX RA is supported by an STFC PhD studentship. This work was supported by the US National Science Foundation through awards AST-0408698 and AST-0965625 for the ACT project, as well as awards PHY-0855887 and PHY-1214379. Funding was also provided by Princeton University, the University of Pennsylvania, Cornell University and a Canada Foundation for Innovation (CFI) award to UBC. ACT operates in the Parque Astronomic Atacama in Northern Chile under the auspices of the Comision Nacional de Investigacion Cientifica y Tecnologica de Chile (CONICYT). Computations were performed on the GPC supercomputer at the SciNet HPC Consortium. SciNet is funded by the CFI under the auspices of Compute Canada, the Government of Ontario, the Ontario Research Fund 1/2 Research Excellence and the University of Toronto. The development of multichroic detectors and lenses was supported by NASA grants NNX13AE56G and NNX14AB58G. Funding from ERC grant 259505 supports SN, JD and TL. RD was supported by CONICYT grants QUIMAL-120001 and FONDECYT-1141113. We gratefully acknowledge support from the Misrahi and Wilkinson research funds. NR 84 TC 9 Z9 9 U1 0 U2 2 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUL 21 PY 2015 VL 451 IS 1 BP 849 EP 858 DI 10.1093/mnras/stv991 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CQ8AH UT WOS:000360827800064 ER PT J AU Just, AC Wright, RO Schwartz, J Coull, BA Baccarelli, AA Tellez-Rojo, MM Moody, E Wang, YJ Lyapustin, A Kloog, I AF Just, Allan C. Wright, Robert O. Schwartz, Joel Coull, Brent A. Baccarelli, Andrea A. Maria Tellez-Rojo, Martha Moody, Emily Wang, Yujie Lyapustin, Alexei Kloog, Itai TI Using High-Resolution Satellite Aerosol Optical Depth To Estimate Daily PM2.5 Geographical Distribution in Mexico City SO ENVIRONMENTAL SCIENCE & TECHNOLOGY LA English DT Article ID LAND-USE REGRESSION; AIR-POLLUTION; MEASUREMENT ERROR; ASTHMATIC-CHILDREN; PARTICULATE MATTER; MODEL; EXPOSURES; HEALTH; EPIDEMIOLOGY; CAMPAIGN AB Recent advances in estimating fine particle (PM2.5) ambient concentrations use daily Satellite measurements of aerosol optical depth (AOD) for spatially and temporally resolved exposure estimates: Mexico City is a dense megacity that differs from other previously modeled regions in several ways: it has bright land surface, a distinctive climatological cycle, and an elevated semi-enclosed air :basin with a unique planetary boundary layer dynamic. We extend our previous Satellite methodology to the Mexico City area, a region with higher PM2.5 than most U.S. and European urban areas. Using a novel 1 km resolution AOD product from the MODIS instrument, we constructed daily predictions across the greater Mexico City area for 2004-2014. We calibrated the association of AOD to PM2.5 daily using municipal ground monitors, land use, and meteorological features. Predictions used Spatial and temporal smoothing to estimate AOD) when satellite data were missing. Our model performed well, resulting in an out-of-sample cross-validation R-2 of 0.724. Cross-validated root-mean-squared prediction error (RMSPE) of the model was 5.55 mu g/m(3). This novel model reconstructs long- and short-term spatially resolved exposure to PM2.5 for epidemiological Studies in Mexico City. C1 [Just, Allan C.; Schwartz, Joel; Baccarelli, Andrea A.] Harvard Univ, TH Chan Sch Publ Hlth, Dept Environm Hlth, Boston, MA 02215 USA. [Wright, Robert O.] Icahn Sch Med Mt Sinai, Dept Prevent Med, New York, NY 10029 USA. [Coull, Brent A.] Harvard Univ, TH Chan Sch Publ Hlth, Dept Biostat, Boston, MA 02215 USA. [Maria Tellez-Rojo, Martha] Natl Inst Publ Hlth, Ctr Nutr & Hlth Res, Cuernavaca 62100, Morelos, Mexico. [Moody, Emily] Univ Minnesota, Med Ctr, Dept Internal Med Pediat, Minneapolis, MN 55455 USA. [Wang, Yujie] Univ Maryland Baltimore Cty, Baltimore, MD 21250 USA. [Lyapustin, Alexei] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Kloog, Itai] Ben Gurion Univ Negev, Dept Geog & Environm Dev, IL-8410501 Beer Sheva, Israel. RP Just, AC (reprint author), Harvard Univ, TH Chan Sch Publ Hlth, Dept Environm Hlth, Boston, MA 02215 USA. EM acjust@hsph.harvard.edu OI Baccarelli, Andrea/0000-0002-3436-0640; Just, Allan/0000-0003-4312-5957 FU National Institute of Environmental Health Sciences (NIEHS) [K99ES023460, R01ES013744, R01ES020268, T32ES007069, P30ES023515] FX The authors thank the staff of the Instituto Nacional de Salud Publica (INSP) and the Instituto Nacional de Ecologia y Cambio Climatico (INECC) for assisting in collecting geospatial datasets and Marianthi-Anna Kioumourtzoglou for advice on statistical modeling. Grant support came from National Institute of Environmental Health Sciences (NIEHS) Grants K99ES023460, R01ES013744, R01ES020268, T32ES007069, and P30ES023515. NR 32 TC 13 Z9 14 U1 8 U2 44 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0013-936X EI 1520-5851 J9 ENVIRON SCI TECHNOL JI Environ. Sci. Technol. PD JUL 21 PY 2015 VL 49 IS 14 BP 8576 EP 8584 DI 10.1021/acs.est.5b00859 PG 9 WC Engineering, Environmental; Environmental Sciences SC Engineering; Environmental Sciences & Ecology GA CN6PY UT WOS:000358557900036 PM 26061488 ER PT J AU Zevalkink, A Star, K Aydemir, U Snyder, GJ Fleurial, JP Bux, S Vo, T von Allmen, P AF Zevalkink, Alex Star, Kurt Aydemir, Umut Snyder, G. Jeffrey Fleurial, Jean-Pierre Bux, Sabah Trinh Vo von Allmen, Paul TI Electronic structure and thermoelectric properties of pnictogen-substituted ASn(1.5)Te(1.5) (A=Co, Rh, Ir) skutterudites SO JOURNAL OF APPLIED PHYSICS LA English DT Article ID ANTIMONIDES; TRANSPORT; CRYSTALS; MODES; POWER AB Substituting group 14 and 16 elements on the pnictogen site in the skutterudite structure yields a class of valence-precise ternary AX(1.5)Y(1.5) compounds (A = Co, Rh, Ir, X = Sn, Ge, and Y = S, Se, Te), in which X and Y form an ordered sub-structure. Compared with unfilled binary skutterudites, pnictogen-substituted phases exhibit extremely low lattice thermal conductivity due to increased structural complexity. Here, we investigate the role of the transition metal species in determining the electronic structure and transport properties of ASn(1.5)Te(1.5) compounds with A = Co, Rh, Ir. Density functional calculations using fully ordered structures reveal semiconducting behavior in all three compounds, with the band gap varying from 0.2 to 0.45 eV. In CoSn1.5Te1.5, the electronic density of states near the gap is significantly higher than for A = Ir or Rh, leading to higher effective masses and higher Seebeck coefficients. Experimentally, Ir and Rh samples exhibit relatively large p-type carrier concentrations and degenerate semiconducting behavior. In contrast, CoSn1.5Te1.5 shows mixed conduction, with n-type carriers dominating the Seebeck coefficient and light, high mobility holes dominating the Hall coefficient. zT values of up to 0.35 were obtained, and further improvement is expected upon optimization of the carrier concentration or with n-type doping. (C) 2015 AIP Publishing LLC. C1 [Zevalkink, Alex; Star, Kurt; Fleurial, Jean-Pierre; Bux, Sabah] CALTECH, Jet Prop Lab, Thermal Energy Convers Technol Grp, Pasadena, CA 91109 USA. [Zevalkink, Alex; Aydemir, Umut; Snyder, G. Jeffrey] CALTECH, Dept Mat Sci, Pasadena, CA 91125 USA. [Trinh Vo; von Allmen, Paul] CALTECH, Jet Prop Lab, Instrument Software & Sci Data Syst Grp, Pasadena, CA 91109 USA. RP Zevalkink, A (reprint author), CALTECH, Jet Prop Lab, Thermal Energy Convers Technol Grp, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. RI Snyder, G/I-2263-2015; Snyder, G. Jeffrey/E-4453-2011; Aydemir, Umut/P-8424-2015 OI Snyder, G. Jeffrey/0000-0003-1414-8682; Aydemir, Umut/0000-0003-1164-1973 FU National Aeronautics and Space Administration; NASA Science Missions Directorate's Radioisotope Power Systems Technology Advancement Program; Scientific and Technological Research Council of Turkey; NASA FX This research was carried out in part at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration and was supported by the NASA Science Missions Directorate's Radioisotope Power Systems Technology Advancement Program. We gratefully acknowledge Gregory Gerig for performing Seebeck measurements. Financial assistance of the Scientific and Technological Research Council of Turkey and NASA Postdoctoral Fellowship Program are acknowledged by A. U. and A. Z., respectively. NR 42 TC 2 Z9 2 U1 1 U2 22 PU AMER INST PHYSICS PI MELVILLE PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA SN 0021-8979 EI 1089-7550 J9 J APPL PHYS JI J. Appl. Phys. PD JUL 21 PY 2015 VL 118 IS 3 AR 035107 DI 10.1063/1.4926479 PG 8 WC Physics, Applied SC Physics GA CN4VT UT WOS:000358429200046 ER PT J AU Zhang, J Fryauf, DM Garrett, M Logeeswaran, VJ Sawabe, A Islam, MS Kobayashi, NP AF Zhang, Junce Fryauf, David M. Garrett, Matthew Logeeswaran, V. J. Sawabe, Atsuhito Islam, M. Saif Kobayashi, Nobuhiko P. TI Phenomenological Model of the Growth of Ultrasmooth Silver Thin Films Deposited with a Germanium Nucleation Layer SO LANGMUIR LA English DT Article ID SELF-ASSEMBLED MONOLAYERS; FORCE MICROSCOPY; WETTING LAYER; SEED LAYER; SURFACE; SMOOTH; AG; SPECTROSCOPY; GE; ALKANETHIOLS AB The structural properties of optically thin (15 silver.(Ag) films deposited on SiO2/Si(100) substrates with a germanium (Ge) nucleation layer were studied. The morphological and crystallographical characteristics of Ag thin films with different Ge nucleation layer thicknesses were assessed by cross-sectional transmission electron Microscopy (XTEM), reflection high-energy electron diffraction (RHEED), X-ray diffractometry (XRD), grazing incidence X-ray diffractometry (GIXRD), X-ray reflection (XRR), and Fourier transform infrared spectroscopy (FTIR). The surface roughness of Ag thin films was found to decrease significantly by inserting a Ge nucleation layer with a thickness in the range of 1 to 2 nm smoothing mode). However, as the Ge nucleation layer thickness increased beyond 2 nm, the surface roughness increased Concomitantly (i.e., roughing mode). For the smoothing mode, the role of the Ge nucleation layer in the Ag film deposition is discussed by invoking the surface energy of Ge, the bond dissociation energy of Ag-Ge, and the deposition mechanisms of Ag thin films on a given characteristic Ge nucleation layer. Additionally, Ge island formation, the precipitation of Ge from Ag-Ge alloys, and the penetration of Ge into SiO2 are suggested for the roughing mode. This demonstration of ultrasmooth Ag thin films would offer an advantageous material platform with scalability for applications such as optics, plasmonics, and photonics. C1 [Zhang, Junce; Fryauf, David M.; Garrett, Matthew; Kobayashi, Nobuhiko P.] Univ Calif Santa Cruz, Jack Baskin Sch Engn, Santa Cruz, CA 95064 USA. [Zhang, Junce; Fryauf, David M.; Garrett, Matthew; Kobayashi, Nobuhiko P.] NASA Ames Res Ctr, Adv Studies Labs, NECTAR, Moffett Field, CA 94035 USA. [Logeeswaran, V. J.; Islam, M. Saif] Univ Calif Davis, Dept Elect & Comp Engn, Davis, CA 95616 USA. [Sawabe, Atsuhito] Aoyama Gakuin Univ, Coll Sci & Engn, Dept Elect Engn & Elect, Chuo Ku, Sagamihara, Kanagawa 2525258, Japan. RP Zhang, J (reprint author), Univ Calif Santa Cruz, Jack Baskin Sch Engn, Santa Cruz, CA 95064 USA. EM jzhang37@ucsc.edu NR 50 TC 2 Z9 2 U1 5 U2 22 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0743-7463 J9 LANGMUIR JI Langmuir PD JUL 21 PY 2015 VL 31 IS 28 BP 7852 EP 7859 DI 10.1021/acs.langmuir.5b01244 PG 8 WC Chemistry, Multidisciplinary; Chemistry, Physical; Materials Science, Multidisciplinary SC Chemistry; Materials Science GA CN6LV UT WOS:000358547200019 PM 26126182 ER PT J AU Sanin, AB Mitrofanov, IG Litvak, ML Lisov, DI Starr, R Boynton, W Behar, A DeFlores, L Fedosov, F Golovin, D Hardgrove, C Harshman, K Jun, I Kozyrev, AS Kuzmin, RO Malakhov, A Milliken, R Mischna, M Moersch, J Mokrousov, MI Nikiforov, S Shvetsov, VN Tate, C Tret'yakov, VI Vostrukhin, A AF Sanin, A. B. Mitrofanov, I. G. Litvak, M. L. Lisov, D. I. Starr, R. Boynton, W. Behar, A. DeFlores, L. Fedosov, F. Golovin, D. Hardgrove, C. Harshman, K. Jun, I. Kozyrev, A. S. Kuzmin, R. O. Malakhov, A. Milliken, R. Mischna, M. Moersch, J. Mokrousov, M. I. Nikiforov, S. Shvetsov, V. N. Tate, C. Tret'yakov, V. I. Vostrukhin, A. TI Data processing of the active neutron experiment DAN for a Martian regolith investigation SO NUCLEAR INSTRUMENTS & METHODS IN PHYSICS RESEARCH SECTION A-ACCELERATORS SPECTROMETERS DETECTORS AND ASSOCIATED EQUIPMENT LA English DT Article DE Active neutron experiment; Mars; MSL; DAN; Water ID LABORATORYS DYNAMIC ALBEDO; RAY SPECTROMETER; INSTRUMENT SUITE; MARS ODYSSEY; GALE CRATER; SCIENCE; HYDROGEN; CALIBRATION; CURIOSITY; ROVER AB Searching for water in the soil of Gale Crater is one of the primary tasks for the NASA Mars Science Laboratory rover named Curiosity. The primary task of the Dynamic Albedo of Neutrons (DAN) experiment on board the rover is to investigate and qualitatively characterize the presence of water along the rover's traverse across Gale Crater. The water depth distribution may be found from measurements of neutrons generated by the Pulsing Neutron Generator (PNG) included in the DAN instrument, scattered by the regolith and returned back to the detectors. This paper provides a description of the data processing of such measurements and data products of DAN investigation. (C) 2015 Elsevier B.V. All rights reserved. C1 [Sanin, A. B.; Mitrofanov, I. G.; Litvak, M. L.; Lisov, D. I.; Fedosov, F.; Golovin, D.; Kozyrev, A. S.; Kuzmin, R. O.; Malakhov, A.; Mokrousov, M. I.; Nikiforov, S.; Tret'yakov, V. I.; Vostrukhin, A.] RAS, Space Res Inst IKI, Moscow 117901, Russia. [Starr, R.] Catholic Univ Amer, Washington, DC 20064 USA. [Boynton, W.; Harshman, K.] Univ Arizona, Tucson, AZ USA. [Behar, A.; DeFlores, L.; Jun, I.; Mischna, M.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Hardgrove, C.; Moersch, J.; Tate, C.] Univ Tennessee, Knoxville, TN USA. [Kuzmin, R. O.] Vernadsky Inst Geochem & Analyt Chem, Moscow, Russia. [Milliken, R.] Brown Univ, Providence, RI 02912 USA. [Hardgrove, C.; Moersch, J.; Tate, C.] Joint Inst Nucl Res, Dubna, Russia. RP Sanin, AB (reprint author), RAS, Space Res Inst IKI, Moscow 117901, Russia. EM sanin@mx.iki.rssi.ru FU Russian Science Foundation [14-22-00249] FX This work is partially supported by the grant no. 14-22-00249 from Russian Science Foundation. NR 25 TC 2 Z9 2 U1 0 U2 6 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0168-9002 EI 1872-9576 J9 NUCL INSTRUM METH A JI Nucl. Instrum. Methods Phys. Res. Sect. A-Accel. Spectrom. Dect. Assoc. Equip. PD JUL 21 PY 2015 VL 789 BP 114 EP 127 DI 10.1010/j.nima.2015.03.085 PG 14 WC Instruments & Instrumentation; Nuclear Science & Technology; Physics, Nuclear; Physics, Particles & Fields SC Instruments & Instrumentation; Nuclear Science & Technology; Physics GA CI6LV UT WOS:000354871700013 ER PT J AU Katsuda, S Mori, K Maeda, K Tanaka, M Koyama, K Tsunemi, H Nakajima, H Maeda, Y Ozaki, M Petre, R AF Katsuda, Satoru Mori, Koji Maeda, Keiichi Tanaka, Masaomi Koyama, Katsuji Tsunemi, Hiroshi Nakajima, Hiroshi Maeda, Yoshitomo Ozaki, Masanobu Petre, Robert TI KEPLER'S SUPERNOVA: AN OVERLUMINOUS TYPE Ia EVENT INTERACTING WITH A MASSIVE CIRCUMSTELLAR MEDIUM AT A VERY LATE PHASE SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; ISM: individual objects (Kepler's SNR); ISM: supernova remnants; supernovae: general; X-rays: general ID LARGE-MAGELLANIC-CLOUD; REFLECTION GRATING SPECTROMETER; DELAYED-DETONATION MODELS; X-RAY-EMISSION; XMM-NEWTON; PROGENITOR SYSTEM; SODIUM-ABSORPTION; HUBBLE CONSTANT; COMPANION STAR; PROPER MOTIONS AB We have analyzed XMM-Newton, Chandra, and Suzaku observations of three similarly aged, ejecta-dominated supernova remnants (SNRs), Kepler's SNR, Tycho's SNR, and SNR 0509-67.5, to investigate the properties of the SN ejecta and the circumstellar medium (CSM). By simply comparing the X-ray spectra, we find that line intensity ratios of iron-group elements (IGEs) to intermediate-mass elements (IMEs) for Kepler's SNR and SNR 050-967.5 are much higher than those for Tycho's SNR. Given that Tycho's SNR and SNR 0509-67.5 are thought to be the remnants of a typical SN Ia and an overluminous SN Ia, respectively, we argue that Kepler is the product of an overlumious SN Ia. This inference is supported by our spectral modeling, which reveals the IGE and IME masses, respectively, to be 0.95(-0.37)(+0.34) M-circle dot and 0.12(-0.05)(+0.19) M-circle dot (Kepler's SNR), 0.75(-0.15)(+0.51) M-circle dot and 0.34(-0.25)(+0.08) M-circle dot (SNR 0509-67.5), and 0.35(-0.15)(+0.55) M-circle dot and 0.70(-0.28)(+0.12) M-circle dot (Tycho's SNR). We find that the CSM component in Kepler's SNR consists of tenuous diffuse gas (similar to 0.3 M-circle dot) present throughout the entire remnant, plus dense knots (similar to 0.035 M-circle dot). Since both of them show N overabundance, their origin would be CNO-processed material from the progenitor system. The mass of the diffuse CSM allows us to infer the pre-SN mass-loss rate to be similar to 1.5 x 10(-5)(v(w)/10 km s(-1)) M-circle dot yr(-1). The dense knots have slow proper motions and relatively small ionization timescales; hence, they were likely located a few parsecs away from the progenitor at the explosion. We thus argue that Kepler's SN was an overluminous (91T-like) event that recently started to interact with the massive CSM. This supports the possible link between 91T-like SNe and "Ia-CSM" SNe. C1 [Katsuda, Satoru; Maeda, Yoshitomo; Ozaki, Masanobu] Japan Aerosp Explorat Agcy JAXA, ISAS, Chuo Ku, Sagamihara, Kanagawa 2525210, Japan. [Mori, Koji] Miyazaki Univ, Fac Engn, Dept Appl Phys & Elect Engn, Miyazaki 8892192, Japan. [Maeda, Keiichi] Kyoto Univ, Dept Astron, Sakyo Ku, Kyoto 6068502, Japan. [Maeda, Keiichi] Univ Tokyo, Kavli Inst Phys & Math Universe WPI, Kashiwa, Chiba 2778583, Japan. [Tanaka, Masaomi] Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan. [Koyama, Katsuji; Tsunemi, Hiroshi; Nakajima, Hiroshi] Osaka Univ, Dept Earth & Space Sci, Toyonaka, Osaka 5600043, Japan. [Koyama, Katsuji] Kyoto Univ, Grad Sch Sci, Dept Phys, Sakyo Ku, Kyoto 6068502, Japan. [Petre, Robert] NASA Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. RP Katsuda, S (reprint author), Japan Aerosp Explorat Agcy JAXA, ISAS, Chuo Ku, 3-1-1 Yoshinodai, Sagamihara, Kanagawa 2525210, Japan. EM katsuda@astro.isas.jaxa.jp RI XRAY, SUZAKU/A-1808-2009 FU Japan Society for the Promotion of Science KAKENHI [25800119, 24740167, 23740141, 26800100, 24740117, 15H02075, 15H00788, 24540229, 23000004, 26670560, 25105516, 24654052] FX This work is supported by Japan Society for the Promotion of Science KAKENHI Grant Numbers 25800119 (S. Katsuda), 24740167 (K. Mori), 23740141, 26800100 (K. Maeda), 24740117, 15H02075, 15H00788 (M. Tanaka), 24540229 (K. Koyama), 23000004 (H. Tsunemi), 26670560 (H. Nakajima), 25105516 (Y. Maeda), and 24654052 (M. Ozaki). NR 98 TC 2 Z9 2 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 20 PY 2015 VL 808 IS 1 AR 49 DI 10.1088/0004-637X/808/1/49 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO3MS UT WOS:000359062500049 ER PT J AU Kitiashvili, IN Couvidat, S Lagg, A AF Kitiashvili, I. N. Couvidat, S. Lagg, A. TI USING REALISTIC MHD SIMULATIONS FOR THE MODELING AND INTERPRETATION OF QUIET-SUN OBSERVATIONS WITH THE SOLAR DYNAMICS OBSERVATORY HELIOSEISMIC AND MAGNETIC IMAGER SO ASTROPHYSICAL JOURNAL LA English DT Article DE methods: numerical; Sun: chromosphere; Sun: photosphere; techniques: polarimetric ID TO-LIMB VARIATION; FLOWS; HMI; CONVECTION AB The solar atmosphere is extremely dynamic, and many important phenomena develop on small scales that are unresolved in observations with the Helioseismic and Magnetic Imager (HMI) instrument on the Solar Dynamics Observatory. For correct calibration and interpretation of the observations, it is very important to investigate the effects of small-scale structures and dynamics on the HMI observables, such as Doppler shift, continuum intensity, spectral line depth, and width. We use 3D radiative hydrodynamics simulations of the upper turbulent convective layer and the atmosphere of the Sun, and a spectro-polarimetric radiative transfer code to study observational characteristics of the Fe I 6173 angstrom line observed by HMI in quiet-Sun regions. We use the modeling results to investigate the sensitivity of the line Doppler shift to plasma velocity, and also sensitivities of the line parameters to plasma temperature and density, and determine effective line formation heights for observations of solar regions located at different distances from the disk center. These estimates are important for the interpretation of helioseismology measurements. In addition, we consider various center-to-limb effects, such as convective blueshift, variations of helioseismic travel-times, and the "concave" Sun effect, and show that the simulations can qualitatively reproduce the observed phenomena, indicating that these effects are related to a complex interaction of the solar dynamics and radiative transfer. C1 [Kitiashvili, I. N.] NASA Ames Res Ctr, Mountain View, CA 94035 USA. [Kitiashvili, I. N.; Couvidat, S.] Stanford Univ, Stanford, CA 94305 USA. [Lagg, A.] Max Planck Inst Solar Syst Res, D-37077 Gottingen, Germany. RP Kitiashvili, IN (reprint author), NASA Ames Res Ctr, Mountain View, CA 94035 USA. OI Kitiashvili, Irina/0000-0003-4144-2270 FU NASA [NNX10AC55G, NNH11ZDA001N-LWSCSW, NNH13AV81I, NNX15AL64G]; Oak Ridge Associated Universities FX The simulation results were obtained on the NASA's Pleiades supercomputer at the NASA Ames Research Center. This work was partially supported by the NASA grants NNX10AC55G, NNH11ZDA001N-LWSCSW, NNH13AV81I, NNX15AL64G, and Oak Ridge Associated Universities. We would also like to acknowledge the NASA Ames's user support team and, in particular, Yan-Tyng Chang, Johnny Chang, and Steve Heistand. NR 33 TC 1 Z9 1 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 20 PY 2015 VL 808 IS 1 AR 59 DI 10.1088/0004-637X/808/1/59 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO3MS UT WOS:000359062500059 ER PT J AU Mukherjee, ES Walton, DJ Bachetti, M Harrison, FA Barret, D Bellm, E Boggs, SE Christensen, FE Craig, WW Fabian, AC Fuerst, F Grefenstette, BW Hailey, CJ Madsen, KK Middleton, MJ Miller, JM Rana, V Stern, D Zhang, W AF Mukherjee, E. S. Walton, D. J. Bachetti, M. Harrison, F. A. Barret, D. Bellm, E. Boggs, S. E. Christensen, F. E. Craig, W. W. Fabian, A. C. Fuerst, F. Grefenstette, B. W. Hailey, C. J. Madsen, K. K. Middleton, M. J. Miller, J. M. Rana, V. Stern, D. Zhang, W. TI A HARD X-RAY STUDY OF THE ULTRALUMINOUS X-RAY SOURCE NGC 5204 X-1 WITH NuSTAR AND XMM-NEWTON SO ASTROPHYSICAL JOURNAL LA English DT Article DE black hole physics; X-rays: binaries; X-rays: individual (NGC 5204 X-1) ID HOLMBERG IX X-1; MASS BLACK-HOLES; ACCRETION DISKS; BROAD-BAND; NEARBY GALAXIES; CYGNUS X-1; SOFT STATE; SPECTRA; SPECTROSCOPY; REFLECTION AB We present the results from coordinated X-ray observations of the ultraluminous X-ray source NGC 5204 X-1 performed by the Nuclear Spectroscopic Telescope Array and XMM-Newton in early 2013. These observations provide the first detection of NGC 5204 X-1 above 10 keV, extending the broadband coverage to 0.3-20 keV. The observations were carried out in two epochs separated by approximately 10 days, and showed little spectral variation with an observed luminosity of L-X = (4.95 +/- 0.11) x 10(39) erg s(-1). The broadband spectrum robustly confirms the presence of a clear spectral downturn above 10 keV seen in some previous observations. This cutoff is inconsistent with the standard low/hard state seen in Galactic black hole binaries, as would be expected from an intermediate-mass black hole accreting at significantly sub-Eddington rates given the observed luminosity. The continuum is apparently dominated by two optically thick thermal-like components, potentially accompanied by a faint high-energy tail. The broadband spectrum is likely associated with an accretion disk that differs from a standard Shakura & Sunyaev thin disk. C1 [Mukherjee, E. S.; Walton, D. J.; Harrison, F. A.; Bellm, E.; Fuerst, F.; Grefenstette, B. W.; Madsen, K. K.; Rana, V.] CALTECH, Space Radiat Lab, Pasadena, CA 91125 USA. [Walton, D. J.; Stern, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Bachetti, M.; Barret, D.] Univ Toulouse, UPS OMP, IRAP, Toulouse, France. [Bachetti, M.; Barret, D.] CNRS, IRAP, F-31028 Toulouse 4, France. [Boggs, S. E.; Craig, W. W.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Christensen, F. E.] Tech Univ Denmark, DTU Space, Natl Space Inst, DK-2800 Lyngby, Denmark. [Fabian, A. C.; Middleton, M. J.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Hailey, C. J.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Miller, J. M.] Univ Michigan, Dept Astron, Ann Arbor, MI 49109 USA. [Zhang, W.] NASA Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Mukherjee, ES (reprint author), CALTECH, Space Radiat Lab, Pasadena, CA 91125 USA. RI Boggs, Steven/E-4170-2015; OI Boggs, Steven/0000-0001-9567-4224; Bachetti, Matteo/0000-0002-4576-9337; Rana, Vikram/0000-0003-1703-8796 FU NASA; ESA Member States FX The authors thank the referee for useful feedback which helped improve the final manuscript. This research has made use of data obtained with the NuSTAR mission, a project led by the California Institute of Technology (Caltech), managed by the Jet Propulsion Laboratory (JPL) and funded by NASA, and with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA. We thank the NuSTAR Operations, Software, and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NUSTARDAS), jointly developed by the ASI Science Data Center (ASDC, Italy) and Caltech (USA). NR 54 TC 9 Z9 9 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 20 PY 2015 VL 808 IS 1 AR 64 DI 10.1088/0004-637X/808/1/64 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO3MS UT WOS:000359062500064 ER PT J AU Paganini, L Mumma, MJ Villanueva, GL DiSanti, MA Bonev, BP AF Paganini, L. Mumma, M. J. Villanueva, G. L. DiSanti, M. A. Bonev, B. P. TI THE VOLATILE COMPOSITION OF COMET C/2003 K4 (LINEAR) AT NEAR-IR WAVELENGTHS-COMPARISONS WITH RESULTS FROM THE NANCAY RADIO TELESCOPE AND FROM THE ODIN, SPITZER, AND SOHO SPACE OBSERVATORIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE comets: general; comets: individual (C/2003 K4 (LINEAR)); techniques: spectroscopic ID OORT CLOUD COMETS; ORTHO-PARA RATIO; O1 HALE-BOPP; P1 GARRADD; INFRARED WAVELENGTHS; ROTATIONAL TEMPERATURE; CHEMICAL-COMPOSITION; Q2 MACHHOLZ; INNER COMA; KECK II AB We observed comet C/2003 K4 (LINEAR) using NIRSPEC at the Keck Observatory on UT 2004 November 28, when the comet was at 1.28 AU from the Sun (post-perihelion) and 1.38 AU from Earth. We detected six gaseous species (H2O, OH*, C2H6, CH3OH, CH4, and HCN) and obtained upper limits for three others (H2CO, C2H2, and NH3). Our results indicate a water production rate of (1.72 +/- 0.18) x 10(29) molecules s(-1), in reasonable agreement with production rates from SOHO (on the same day), Odin (one day earlier), and Nancay (about two weeks earlier). We also report abundances (relative to water) for seven trace species: CH3OH (similar to 1.8%), CH4 (similar to 0.9%), and C2H6 (similar to 0.4%) that were consistent with mean values among Oort cloud (OC) comets, while NH3 (<0.55%), HCN (similar to 0.07%), H2CO (<0.07%), and C2H2 (<0.04%) were "lower" than the mean values in other OC comets. We extracted inner-coma rotational temperatures for four species (H2O, C2H6, CH3OH, and CH4), all of which are consistent with 70 K (within 1 sigma). The extracted ortho-para ratio for water was 3.0 +/- 0.15, corresponding to spin temperatures larger than 39 K (at the 1 sigma level) and agreeing with those obtained with the Spitzer Space Telescope at the 2 sigma level. C1 [Paganini, L.; Mumma, M. J.; Villanueva, G. L.; DiSanti, M. A.; Bonev, B. P.] NASA GSFC, Goddard Ctr Astrobiol, Greenbelt, MD 20771 USA. [Paganini, L.; Villanueva, G. L.; Bonev, B. P.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA. RP Paganini, L (reprint author), NASA GSFC, Goddard Ctr Astrobiol, MS 690, Greenbelt, MD 20771 USA. EM lucas.paganini@nasa.gov OI Mumma, Michael/0000-0003-4627-750X FU NASA's Planetary Astronomy Program; NASA's Astrobiology Institute through GSFC; NSF FX We gratefully acknowledge support by NASA's Planetary Astronomy Program (L.P., M.J.M, M.A.D., and G.L.V.), NASA's Astrobiology Institute through its member Team at GSFC (M.J.M., M.A.D., and B.P.B.), and NSF (B.P.B.). We also gratefully acknowledge Jacques Crovisier for providing Nancay results prior to publication, and Michael Combi for providing SWAN results prior to publication. The authors acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. NR 52 TC 2 Z9 2 U1 1 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 20 PY 2015 VL 808 IS 1 AR 1 DI 10.1088/0004-637X/808/1/1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO3MS UT WOS:000359062500001 ER PT J AU Parker, ML Tomsick, JA Miller, JM Yamaoka, K Lohfink, A Nowak, M Fabian, AC Alston, WN Boggs, SE Christensen, FE Craig, WW Furst, F Gandhi, P Grefenstette, BW Grinberg, V Hailey, CJ Harrison, FA Kara, E King, AL Stern, D Walton, DJ Wilms, J Zhang, WW AF Parker, M. L. Tomsick, J. A. Miller, J. M. Yamaoka, K. Lohfink, A. Nowak, M. Fabian, A. C. Alston, W. N. Boggs, S. E. Christensen, F. E. Craig, W. W. Fuerst, F. Gandhi, P. Grefenstette, B. W. Grinberg, V. Hailey, C. J. Harrison, F. A. Kara, E. King, A. L. Stern, D. Walton, D. J. Wilms, J. Zhang, W. W. TI NuSTAR AND SUZAKU OBSERVATIONS OF THE HARD STATE IN CYGNUS X-1: LOCATING THE INNER ACCRETION DISK SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; black hole physics; X-rays: binaries; X-rays: individual (Cygnus X-1) ID X-RAY REFLECTION; ADVECTION-DOMINATED ACCRETION; SPECTROSCOPIC-TELESCOPE-ARRAY; BROAD-BAND SPECTRUM; BLACK-HOLE; LOW/HARD STATE; CYCLOTRON LINE; XMM-NEWTON; SOFT STATE; HDE 226868 AB We present simultaneous Nuclear Spectroscopic Telescope Array (NuSTAR) and Suzaku. observations of the X-ray binary Cygnus X-1 in the hard state. This is the first time this state has been observed in Cyg X-1 with NuSTAR, which enables us to study the reflection and broadband spectra in unprecedented detail. We confirm that the iron line cannot be fit with a combination of narrow lines and absorption features, instead requiring. a relativistically blurred profile in combination with a narrow line and absorption from the companion wind. We use the reflection models of Garcia et al. to simultaneously measure the black hole spin, disk inner radius, and coronal height in a self-consistent manner. Detailed fits to the iron line profile indicate a high level of relativistic blurring, indicative of reflection from the inner accretion disk. We find a high spin, a small inner disk radius, and a low source height. and rule out truncation to greater than three gravitational radii at the 3 sigma confidence level. In addition, we find that the line profile has not changed greatly in the switch from soft to hard states, and that the differences are consistent with changes in the underlying reflection spectrum rather than the relativistic blurring. We find that the blurring parameters are consistent when fitting either just the iron line or the entire broadband spectrum, which is well modeled with a Comptonized continuum plus reflection model. C1 [Parker, M. L.; Lohfink, A.; Fabian, A. C.; Alston, W. N.; Kara, E.] Inst Astron, Cambridge CB3 0HA, England. [Tomsick, J. A.; Boggs, S. E.; Craig, W. W.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Miller, J. M.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Yamaoka, K.] Nagoya Univ, Dept Particles & Astron, Solar Terr Environm Lab, Chikusa Ku, Nagoya, Aichi 4648601, Japan. [Nowak, M.; Grinberg, V.] MIT, Kavli Inst Astrophys, Cambridge, MA 02139 USA. [Christensen, F. E.] Danish Tech Univ, DK-2800 Lyngby, Denmark. [Craig, W. W.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA. [Fuerst, F.; Grefenstette, B. W.; Harrison, F. A.; Walton, D. J.] CALTECH, Pasadena, CA 91125 USA. [Gandhi, P.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Hailey, C. J.] Columbia Univ, New York, NY 10027 USA. [King, A. L.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA. [Stern, D.; Walton, D. J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Wilms, J.] Dr Karl Remeis Observ, D-96049 Bamberg, Germany. [Wilms, J.] Erlangen Ctr Astroparticle Phys, D-96049 Bamberg, Germany. [Zhang, W. W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Parker, ML (reprint author), Inst Astron, Madingley Rd, Cambridge CB3 0HA, England. RI Wilms, Joern/C-8116-2013; XRAY, SUZAKU/A-1808-2009; Boggs, Steven/E-4170-2015; OI Wilms, Joern/0000-0003-2065-5410; Boggs, Steven/0000-0001-9567-4224; Parker, Michael/0000-0002-8466-7317 FU Science and Technology Facilities Council (STFC); NASA ADAP grant [NNX13AE98G]; European Union Seventh Framework Programme (FP7), StrongGravity [312789]; Deutsches Zentrum fur Luft- und Raumfahrt grant [50 OR 1411]; National Aeronautics and Space Administration FX M.L.P. acknowledges financial support from the Science and Technology Facilities Council (STFC) and is grateful to Simon Gibbons for helpful discussions. J.A.T. acknowledges partial support from NASA ADAP grant NNX13AE98G. W.N.A., E.K., and A.C.F. acknowledge support from the European Union Seventh Framework Programme (FP7/2013-2017) under grant agreement no. 312789, StrongGravity. J.W. acknowledges support from Deutsches Zentrum fur Luft- und Raumfahrt grant 50 OR 1411. This work made use of data from the NuSTAR. mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. This research has made use of the NuSTAR. Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). This research has made use of data obtained from the Suzaku. satellite, a collaborative mission between the space agencies of Japan (JAXA) and the USA (NASA). NR 81 TC 10 Z9 10 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 20 PY 2015 VL 808 IS 1 AR 9 DI 10.1088/0004-637X/808/1/9 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO3MS UT WOS:000359062500009 ER PT J AU Richardson, ND Moffat, AFJ Gull, TR Lindler, DJ Gies, DR Corcoran, MF Chene, AN AF Richardson, Noel D. Moffat, Anthony F. J. Gull, Theodore R. Lindler, Don J. Gies, Douglas R. Corcoran, Michael F. Chene, Andre-Nicolas TI HST/STIS ULTRAVIOLET SPECTROSCOPY OF THE COMPONENTS OF THE MASSIVE TRIPLE STAR delta ORI A SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: spectroscopic; binaries: visual; stars: individual (delta Ori); ultraviolet: stars ID BLANKETED MODEL ATMOSPHERES; O-TYPE STARS; ORIONIS-A; BINARY; MASSES; SYSTEM AB The multiple star system of delta Orionis is one of the closest examples of a system containing a luminous O-type, bright giant star (component Aa1). It is often used as a spectral-type standard and has the highest observed X-ray flux of any hot-star binary. The main component Aa1 is orbited by two lower mass stars, faint Aa2 in a 5.7 day eclipsing binary, and Ab, an astrometric companion with an estimated period of 346 years. Generally the flux from all three stars is recorded in ground-based spectroscopy, and the spectral decomposition of the components has proved difficult. Here we present Hubble Space Telescope/Space Telescope Imaging Spectrograph ultraviolet spectroscopy of delta Ori A that provides us with spatially separated spectra of Aa and Ab for the first time. We measured radial velocities for Aa1 and Ab in two observations made near the velocity extrema of Aa1. We show tentative evidence for the detection of the Aa2 component in cross-correlation functions of the observed and model spectra. We discuss the appearance of the UV spectra of Aa1 and Ab with reference to model spectra. Both stars have similar effective temperatures, but Ab is fainter and is a rapid rotator. The results will help in the interpretation of ground-based spectroscopy and in understanding the physical and evolutionary parameters of these massive stars. C1 [Richardson, Noel D.; Moffat, Anthony F. J.] Univ Montreal, Dept Phys, Montreal, PQ H3C 3J7, Canada. [Richardson, Noel D.; Moffat, Anthony F. J.] Univ Montreal, CRAQ, Montreal, PQ H3C 3J7, Canada. [Gull, Theodore R.; Lindler, Don J.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Gies, Douglas R.] Georgia State Univ, Ctr High Angular Resolut Astron, Atlanta, GA 30302 USA. [Gies, Douglas R.] Georgia State Univ, Dept Phys & Astron, Atlanta, GA 30302 USA. [Corcoran, Michael F.] NASA, GSFC, CRESST, Greenbelt, MD USA. [Corcoran, Michael F.] NASA, GSFC, Xray Astrophys Lab, Greenbelt, MD USA. [Corcoran, Michael F.] Univ Space Res Assoc, Columbia, MD 21046 USA. [Chene, Andre-Nicolas] Northern Operat Ctr, Gemini Observ, Hilo, HI 96720 USA. RP Richardson, ND (reprint author), Univ Montreal, Dept Phys, CP 6128,Succ Ctr Ville, Montreal, PQ H3C 3J7, Canada. EM richardson@astro.umontreal.ca; moffat@astro.umontreal.ca; theodore.r.gull@nasa.gov; don.j.lindler@nasa.gov; gies@chara.gsu.edu; michael.f.corcoran@nasa.gov; achene@gemini.edu OI Richardson, Noel/0000-0002-2806-9339 FU NASA from the Space Telescope Science Institute [13450]; NASA [NAS 5-26555]; CRAQ (Quebec) fellowship; NSERC (Canada); FRQNT (Quebec) FX We are grateful to Charles Proffitt and Denise Taylor of STScI for their aid in planning the observations with HST. We thank Brian Mason, William Hartkopf, and Andrei Tokovinin for information about their speckle observations of delta Ori, and we also thank Tomer Shenar for sharing results in advance of publication. A preliminary AO image was obtained with Gemini-N/GNIRS under program GN-2014-q73, which was used to confirm the astrometry of d Ori Ab relative to Aa prior to the HST visit. Support for program # 13450 was provided by NASA through a grant from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. N.D.R. gratefully acknowledges his CRAQ (Quebec) fellowship. A.F.J.M. is grateful for financial aid to NSERC (Canada) and FRQNT (Quebec). NR 26 TC 3 Z9 3 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 20 PY 2015 VL 808 IS 1 AR 88 DI 10.1088/0004-637X/808/1/88 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO3MS UT WOS:000359062500088 ER PT J AU Sharykin, IN Kosovichev, AG AF Sharykin, I. N. Kosovichev, A. G. TI DYNAMICS OF ELECTRIC CURRENTS, MAGNETIC FIELD TOPOLOGY, AND HELIOSEISMIC RESPONSE OF A SOLAR FLARE SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun: flares; Sun: helioseismology; sunspots; Sun: X-rays; gamma rays ID SEISMIC SOURCES; ENERGY; OPTIMIZATION; RHESSI; SUN AB The solar flare on 2011 July 30 was of a modest X-ray class (M9.3), but it made a strong photospheric impact and produced a "sunquake," which was observed with the Helioseismic and Magnetic Imager on board NASA's Solar Dynamics Observatory. In addition to the helioseismic waves, the flare caused a large expanding area of white-light emission and was accompanied by the rapid formation of a sunspot structure in the flare region. The flare produced hard X-ray (HXR) emission less then 300 keV and no coronal mass ejection (CME). The absence of CME rules out magnetic rope eruption as a mechanism of helioseismic waves. The sunquake impact does not coincide with the strongest HXR source, which contradicts the standard beam-driven mechanism of sunquake generation. We discuss the connectivity of the flare energy release with the electric currents dynamics and show the potential importance of high-speed plasma flows in the lower solar atmosphere during the flare energy release. C1 [Sharykin, I. N.; Kosovichev, A. G.] New Jersey Inst Technol, Big Bear Solar Observ, Big Bear City, CA 92314 USA. [Sharykin, I. N.] Russian Acad Sci, Space Res Inst IKI, Moscow 117901, Russia. [Kosovichev, A. G.] Stanford Univ, Stanford, CA 94305 USA. [Kosovichev, A. G.] NASA Ames Res Ctr, Mountain View, CA 94035 USA. RP Sharykin, IN (reprint author), New Jersey Inst Technol, Big Bear Solar Observ, Big Bear City, CA 92314 USA. FU RFBR [3-02-91165, 15-32-21078]; NASA [NNX14AB70G]; NJIT grant; [MK-3931.2013.2] FX The work was partially supported by RFBR grants 13-02-91165 and 15-32-21078, President's grant MK-3931.2013.2, NASA grant NNX14AB70G, and an NJIT grant. The authors also thank the SDO and RHESSI teams for the available data and software. NR 31 TC 5 Z9 5 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 20 PY 2015 VL 808 IS 1 AR 72 DI 10.1088/0004-637X/808/1/72 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO3MS UT WOS:000359062500072 ER PT J AU Swartz, DA Pavlov, GG Clarke, T Castelletti, G Zavlin, VE Bucciantini, N Karovska, M van der Horst, AJ Yukita, M Weisskopf, MC AF Swartz, Douglas A. Pavlov, George G. Clarke, Tracy Castelletti, Gabriela Zavlin, Vyacheslav E. Bucciantini, Niccolo Karovska, Margarita van der Horst, Alexander J. Yukita, Mihoko Weisskopf, Martin C. TI HIGH SPATIAL RESOLUTION X-RAY SPECTROSCOPY OF THE IC 443 PULSAR WIND NEBULA AND ENVIRONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: individual objects (G189.22+2.90, IC 443); ISM: supernova remnants; stars: neutron; X-rays: individual (CXOU J061705.3+222127); X-rays: ISM ID SUPERNOVA REMNANT IC-443; BOW-SHOCK NEBULAE; VELA PULSAR; EMISSION; ROTATION; SPECTRUM; JET AB Deep Chandra ACIS observations of the region around the putative pulsar, CXOU J061705.3+222127, in the supernova remnant (SNR) IC 443 reveal an similar to 5 '' radius ring-like structure surrounding the pulsar and a jet-like feature oriented roughly north-south across the ring and through the pulsar's location at 06(h)17(m)5(s).200 + 22 degrees 21' 27 ''.52 (J2000.0 coordinates). The observations further confirm that (1) the spectrum and flux of the central object are consistent with a rotation-powered pulsar, (2) the non-thermal spectrum and morphology of the surrounding nebula are consistent with a pulsar wind, and (3) the spectrum at greater distances is consistent with thermal emission from the SNR. The cometary shape of the nebula, suggesting motion toward the southwest, appears to be subsonic: There is no evidence either spectrally or morphologically for a bow shock or contact discontinuity; the nearly circular ring is not distorted by motion through the ambient medium; and the shape near the apex of the nebula is narrow. Comparing this observation with previous observations of the same target, we set a 99% confidence upper limit to the proper motion of CXOU J061705.3+222127 to be less than 44 mas yr(-1) (310 km s(-1) for a distance of 1.5 kpc), with the best-fit (but not statistically significant) projected direction toward the west. C1 [Swartz, Douglas A.; Zavlin, Vyacheslav E.] NASA, USRA, Astrophys Off, Marshall Space Flight Ctr, Huntsville, AL 35812 USA. [Pavlov, George G.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Clarke, Tracy] Naval Res Lab, Remote Sensing Div, Washington, DC USA. [Castelletti, Gabriela] UBA, CONICET, IAFE, Buenos Aires, DF, Argentina. [Bucciantini, Niccolo] INAF Osservatorio Astrofis Arcetri, I-50125 Florence, Italy. [Bucciantini, Niccolo] INFN Sez Firenze, I-50019 Florence, Italy. [Karovska, Margarita] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [van der Horst, Alexander J.] George Washington Univ, Dept Phys, Washington, DC 20052 USA. [Yukita, Mihoko] Johns Hopkins Univ, Baltimore, MD 21218 USA. [Yukita, Mihoko] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Weisskopf, Martin C.] NASA, Astrophys Off, Marshall Space Flight Ctr, Huntsville, AL 35812 USA. RP Swartz, DA (reprint author), NASA, USRA, Astrophys Off, Marshall Space Flight Ctr, ZP12, Huntsville, AL 35812 USA. RI Yukita, Mihoko/E-4135-2017; OI Bucciantini, Niccolo'/0000-0002-8848-1392 FU National Aeronautics Space Administration [NAS8-03060]; 6.1 Base funding FX The Chandra observations were obtained in response to Chandra Proposal Number 13500093 by the Chandra X-ray Observatory Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of the National Aeronautics Space Administration under contract NAS8-03060. Optical observations were obtained with the SARA Observatory 0.9 m telescope at Kitt Peak, which is owned and operated by the Southeastern Association for Research in Astronomy. Basic research in radio astronomy at the Naval Research Laboratory (TC) is supported by 6.1 Base funding. NR 36 TC 1 Z9 1 U1 1 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 20 PY 2015 VL 808 IS 1 AR 84 DI 10.1088/0004-637X/808/1/84 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO3MS UT WOS:000359062500084 ER PT J AU Temim, T Slane, P Kolb, C Blondin, J Hughes, JP Bucciantini, N AF Temim, Tea Slane, Patrick Kolb, Christopher Blondin, John Hughes, John P. Bucciantini, Niccolo TI LATE-TIME EVOLUTION OF COMPOSITE SUPERNOVA REMNANTS: DEEP CHANDRA OBSERVATIONS AND HYDRODYNAMICAL MODELING OF A CRUSHED PULSAR WIND NEBULA IN SNR G327.1-1.1 SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: individual objects (G327.1-1.1); ISM: supernova remnants; pulsars: general; radiation mechanisms: non-thermal; stars: neutron ID AREA TELESCOPE OBSERVATIONS; X-RAY; EMISSION AB In an effort to better understand the evolution of composite supernova remnants (SNRs) and the eventual fate of relativistic particles injected by their pulsars, we present a multifaceted investigation of the interaction between a pulsar wind nebula (PWN) and its host SNR G327.1-1.1. Our 350 Chandra X-ray observations of SNR G327.1-1.1 reveal a highly complex morphology: a cometary structure resembling a bow shock, prong-like features extending into large arcs in the SNR interior, and thermal emission from the SNR shell. Spectral analysis of the non-thermal emission offers clues about the origin of the PWN structures, while enhanced abundances in the PWN region provide evidence for a mixing of supernova ejecta with PWN material. The overall morphology and spectral properties of the SNR suggest that the PWN has undergone an asymmetric interaction with the SNR reverse shock (RS), whichcan occur as a result of a density gradient in the ambient medium and/or a moving pulsar that displaces the PWN from the center of the remnant. We present hydrodynamical simulations of G327.1-1.1 that show that its morphology and evolution can be described by a similar to 17,000-year-old composite SNR that expanded into a density gradient with an orientation perpendicular to the pulsar's motion. We also show that the RS/PWN interaction scenario can reproduce the broadband spectrum of the PWN from radio to.-ray wavelengths. The analysis and modeling presented in this work have important implications for our general understanding of the structure and evolution of composite SNRs. C1 [Temim, Tea] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA. [Temim, Tea] Univ Maryland, CRESST, College Pk, MD 20742 USA. [Slane, Patrick] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kolb, Christopher; Blondin, John] N Carolina State Univ, Raleigh, NC 27695 USA. [Hughes, John P.] Rutgers State Univ, New Brunswick, NJ 08901 USA. [Bucciantini, Niccolo] INAF Osservatorio Astrofis Arcetri, I-50125 Florence, Italy. RP Temim, T (reprint author), NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Code 665, Greenbelt, MD 20771 USA. OI Bucciantini, Niccolo'/0000-0002-8848-1392; Blondin, John/0000-0001-9691-6803; Temim, Tea/0000-0001-7380-3144 FU NASA [GO2-13075A, NAS8-03060] FX This work was supported by NASA under the grant number GO2-13075A. P.S. acknowledge support from the NASA Contract NAS8-03060. NR 27 TC 2 Z9 2 U1 2 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 20 PY 2015 VL 808 IS 1 AR 100 DI 10.1088/0004-637X/808/1/100 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO3MS UT WOS:000359062500100 ER PT J AU Tendulkar, SP Hascoet, R Yang, CW Kaspi, VM Beloborodov, AM An, HJ Bachetti, M Boggs, SE Christensen, FE Craig, WW Guiilot, S Hailey, CA Harrison, FA Stern, D Zhang, W AF Tendulkar, Shriharsh P. Hascoeet, Romain Yang, Chengwei Kaspi, Victoria M. Beloborodov, Andrei M. An, Hongjun Bachetti, Matteo Boggs, Steven E. Christensen, Finn E. Craig, William W. Guiilot, Sebastien Hailey, Charles A. Harrison, Fiona A. Stern, Daniel Zhang, William TI PHASE-RESOLVED NuSTAR AND SWIFT-XRT OBSERVATIONS OF MAGNETAR 4U 0142+61 SO ASTROPHYSICAL JOURNAL LA English DT Article DE pulsars: individual (4U 0142+61); stars: magnetars; stars: neutron ID X-RAY PULSARS; SOFT GAMMA-REPEATERS; HIGH-ENERGY CHARACTERISTICS; SOLAR-SYSTEM ABUNDANCES; NEUTRON-STARS; XMM-NEWTON; CHEMICAL-COMPOSITION; INTERSTELLAR-MEDIUM; CROSS-SECTIONS; 1E 1048.1-5937 AB We present temporal and spectral analysis of simultaneous 0.5-79 keV Swift-XRT and Nuclear Spectroscopic Telescope Array observations of the magnetar 4U 0142+61. The pulse profile changes significantly with photon energy between 3 and 35 keV. The pulse fraction increases with energy, reaching a value of approximate to 20%, similar to that observed in 1E 1841-045 and much lower than the approximate to 80% pulse fraction observed in 1E 2259+586. We do not detect the 55 ks phase modulation reported in previous Suzaku-HXD observations. The phase-averaged spectrum of 4U 0142+61 above 20 keV is dominated by a hard power law (PL) with a photon index Gamma(H) similar to 0.65, and the spectrum below 20 keV can be described by two blackbodies, a blackbody plus a soft PL, or by a Comptonized blackbody model. We study the full phase-resolved spectra using the e(+/-) outflow model of Beloborodov. Our results are consistent with the parameters of the active j-bundle derived from INTEGRAL data by Hascoet et al. We find that a significant degeneracy appears in the inferred parameters if the footprint of the j-bundle is allowed to be a thin ring instead of a polar cap. The degeneracy is reduced when the footprint is required to be the hot spot inferred from the soft X-ray data. C1 [Tendulkar, Shriharsh P.; Harrison, Fiona A.] CALTECH, Space Radiat Lab, Pasadena, CA 91125 USA. [Hascoeet, Romain; Beloborodov, Andrei M.; Hailey, Charles A.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Yang, Chengwei] Beijing Inst Technol, Beijing 100081, Peoples R China. [Yang, Chengwei; Kaspi, Victoria M.; Guiilot, Sebastien] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [An, Hongjun] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA. [Bachetti, Matteo] Osservatorio Astron Cagliari, INAF, I-09047 Selargius, CA, Italy. [Boggs, Steven E.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Christensen, Finn E.; Craig, William W.] Tech Univ Denmark, Natl Space Inst, DTU Space, DK-2800 Lyngby, Denmark. [Craig, William W.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA. [Guiilot, Sebastien] Pontificia Univ Catolica Chile, Fac Fis, Inst Astrofis, Santiago 7820436, Chile. [Stern, Daniel] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Zhang, William] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. RP Tendulkar, SP (reprint author), CALTECH, Space Radiat Lab, 1200 E Calif Blvd,MC 249-17, Pasadena, CA 91125 USA. EM spt@astro.caltech.edu RI XRAY, SUZAKU/A-1808-2009; Boggs, Steven/E-4170-2015; OI Boggs, Steven/0000-0001-9567-4224; Bachetti, Matteo/0000-0002-4576-9337; An, Hongjun/0000-0002-6389-9012; Tendulkar, Shriharsh/0000-0003-2548-2926 FU NASA [NNG08FD60C, NNX13AI34G]; National Aeronautics and Space Administration; NSERC Discovery Grant and Accelerator Supplement; FQRNT Centre de Recherche Astrophysique du Quebec; R. Howard Webster Foundation Fellowship from Canadian Institute for Advanced Research (CIFAR); Canada Research Chairs Program; Lorne Trottier Chair in Astrophysics and Cosmology FX This work was supported under NASA Contract No. NNG08FD60C, and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). V. M. K. acknowledges support from an NSERC Discovery Grant and Accelerator Supplement, the FQRNT Centre de Recherche Astrophysique du Quebec, an R. Howard Webster Foundation Fellowship from the Canadian Institute for Advanced Research (CIFAR), the Canada Research Chairs Program and the Lorne Trottier Chair in Astrophysics and Cosmology. A.M.B. acknowledges the support by NASA grant NNX13AI34G. NR 67 TC 5 Z9 5 U1 0 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 20 PY 2015 VL 808 IS 1 AR 32 DI 10.1088/0004-637X/808/1/32 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO3MS UT WOS:000359062500032 ER PT J AU Tomsick, JA Rahoui, F Kolehmainen, M Miller-Jones, J Furst, F Yamaoka, K Akitaya, H Corbel, S Coriat, M Done, C Gandhi, P Harrison, FA Huang, KY Kaaret, P Kalemci, E Kanda, Y Migliari, S Miller, JM Moritani, Y Stern, D Uemura, M Urata, Y AF Tomsick, John A. Rahoui, Farid Kolehmainen, Mari Miller-Jones, James Fuerst, Felix Yamaoka, Kazutaka Akitaya, Hiroshi Corbel, Stephane Coriat, Mickael Done, Chris Gandhi, Poshak Harrison, Fiona A. Huang, Kuiyun Kaaret, Philip Kalemci, Emrah Kanda, Yuka Migliari, Simone Miller, Jon M. Moritani, Yuki Stern, Daniel Uemura, Makoto Urata, Yuji TI THE ACCRETING BLACK HOLE SWIFT J1753.5-0127 FROM RADIO TO HARD X-RAY SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; black hole physics; stars: individual (Swift J1753.5-0127); X-rays: general; X-rays: stars ID BINARY MAXI J1836-194; INNER COOL DISKS; LOW/HARD STATE; GX 339-4; CYGNUS X-1; GAMMA-RAY; COMPACT JET; MULTIWAVELENGTH OBSERVATIONS; SPECTRAL STATES; OUTBURST DECAY AB We report on multiwavelength measurements of the accreting black hole Swift J1753.5-0127 in the hard state at low luminosity (L similar to 2.7 x 10(36) erg s(-1) assuming a distance of d = 3 kpc) in 2014 April. The radio emission is optically thick synchrotron, presumably from a compact jet. We take advantage of the low extinction (E (B - V) = 0.45 from earlier work) and model the near-IR to UV emission with a multitemperature disk model. Assuming a black hole mass of M-BH = 5M(circle dot) and a system inclination of i = 40 degrees, the fits imply an inner radius for the disk of R-in/R-g > 212 d(3)(M-BH/5M(circle dot))(-1), where R-g is the gravitational radius of the black hole. and d(3) is the distance to the source in units of 3 kpc. The outer radius is R-out/R-g = 90,000 d(3)(M-BH/5M(circle dot))(-1), which corresponds to 6.6 x 10(10) d(3) cm, consistent with the expected size of the disk given previous measurements of the size of the companion's Roche lobe. The 0.5-240 keV energy spectrum measured by Swift/X-ray Telescope (XRT), Suzaku (XIS, PIN, and GSO), and Nuclear Spectroscopic Telescope Array is relatively well characterized by an absorbed power. law with a photon index of Gamma = 1.722 +/- 0.003 (90% confidence error), but a significant improvement is seen when a second continuum component is added. Reflection is a possibility, but no iron line is detected, implying a low iron abundance. We are able to fit the entire (radio to 240 keV) spectral energy distribution (SED) with a multitemperature disk component, a Comptonization component, and a broken power. law, representing the emission from the compact jet. The broken power. law cannot significantly contribute to the soft X-ray emission, and this may be related to why Swift J1753.5-0127 is an outlier in the radio/X-ray correlation. The broken power. law (i.e., the jet) might dominate above 20 keV, which would constrain the break frequency to be between 2.4 x 10(10) and 3.6 x 10(12) Hz. Although the fits to the full SED do not include significant thermal emission in the X-ray band, previous observations have consistently seen such a component, and we find that there is evidence at the 3.1s level for a disk-blackbody component with a temperature of kT(in) = 150(-20)(+30) eV and an inner radius of 5R(g)-14R(g). If this component is real, it might imply the presence of an inner optically thick accretion disk in addition to the strongly truncated (R-in > 212R(g)) disk. We also perform X-ray timing analysis, and the power spectrum is dominated by a Lorentzian component with.max = 0.110 (C) 0.003 Hz and sigma(max) = 0.16 +/- 0.04 Hz as measured by XIS and XRT, respectively. C1 [Tomsick, John A.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Rahoui, Farid] European So Observ, D-85748 Garching, Germany. [Rahoui, Farid] Harvard Univ, Dept Astron, Cambridge, MA 02138 USA. [Kolehmainen, Mari] Univ Oxford, Dept Phys, Astrophys, Oxford OX1 3RH, England. [Miller-Jones, James] Curtin Univ, Int Ctr Radio Astron Res, Perth, WA 6845, Australia. [Fuerst, Felix; Harrison, Fiona A.] CALTECH, Pasadena, CA 91125 USA. [Yamaoka, Kazutaka] Nagoya Univ, Solar Terr Environm Lab, Chikusa Ku, Nagoya, Aichi 4648601, Japan. [Yamaoka, Kazutaka; Moritani, Yuki; Uemura, Makoto] Nagoya Univ, Dept Phys, Div Particle & Astrophys Sci, Chikusa Ku, Nagoya, Aichi 4648602, Japan. [Akitaya, Hiroshi] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Hiroshima 7398526, Japan. [Corbel, Stephane] Univ Paris Diderot, CNRS INSU, CEA IRFU, Lab AIM,CEA DSM IRFU SAp, F-91191 Gif Sur Yvette, France. [Corbel, Stephane] Univ Orleans, PSL Res Univ, CNRS, Stn Radioastron Nancay,Observ Paris,OSUC, F-18330 Nancay, France. [Coriat, Mickael] IRAP, F-31028 Toulouse 4, France. [Done, Chris] Univ Durham, Dept Phys, Durham DH1 3LE, England. [Gandhi, Poshak] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Huang, Kuiyun] Natl Taiwan Normal Univ, Dept Math & Sci, New Taipei City 24449, Taiwan. [Kaaret, Philip] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. [Kalemci, Emrah] Sabanci Univ, TR-34956 Istanbul, Turkey. [Kanda, Yuka] Hiroshima Univ, Dept Phys Sci, Higashihiroshima 7398526, Japan. [Migliari, Simone] European Space Astron Ctr, E-28691 Madrid, Spain. [Miller, Jon M.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Moritani, Yuki] Univ Tokyo, Kavli Inst Phys & Math Universe WPI, Kashiwa, Chiba 2778583, Japan. [Stern, Daniel] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Urata, Yuji] Natl Cent Univ, Inst Astron, Chungli 32054, Taiwan. RP Tomsick, JA (reprint author), Univ Calif Berkeley, Space Sci Lab, 7 Gauss Way, Berkeley, CA 94720 USA. RI Miller-Jones, James/B-2411-2013; XRAY, SUZAKU/A-1808-2009; done, chris/D-4605-2016 OI Miller-Jones, James/0000-0003-3124-2814; done, chris/0000-0002-1065-7239 FU NASA [NNG08FD60C, NNX13AJ81G, NNX14AC56G]; National Aeronautics and Space Administration; National Aeronautics and Space Administration through the Planetary Science Division of the NASA Science Mission Directorate [NNX08AR22G]; UnivEarthS Labex program of Sorbonne Paris Cite [ANR-10-LABX-0023, ANR-11-IDEX-0005-02]; French Research National Agency [ANR-12-BS05-0009]; Australian Research Council (ARC) [FT140101082]; TUBITAK BIDEB 2219 program; Spanish Ministerio de Economa y Competitividad (MINECO) [AYA2013-47447-C3-1-P] FX We thank the referee for useful comments that helped to improve the manuscript. This work was supported under NASA Contract No. NNG08FD60C. and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software, and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS), jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). The PS1 Surveys have been made possible through contributions of the Institute for Astronomy, the University of Hawaii, the Pan-STARRS Project Office, the Max-Planck Society and its participating institutes, the Max Planck Institute for Astronomy, Heidelberg and the Max Planck Institute for Extraterrestrial Physics, Garching, Johns Hopkins University, Durham University, the University of Edinburgh, Queen's University Belfast, the Harvard-Smithsonian Center for Astrophysics, the Las Cumbres Observatory Global Telescope Network, Incorporated, the National Central University of Taiwan, and the National Aeronautics and Space Administration under Grant No. NNX08AR22G issued through the Planetary Science Division of the NASA Science Mission Directorate. J.A.T. acknowledges partial support from NASA under Swift Guest Observer grants NNX13AJ81G and NNX14AC56G. S.C. acknowledges the financial support from the UnivEarthS Labex program of Sorbonne Paris Cite (ANR-10-LABX-0023 and ANR-11-IDEX-0005-02). and from the CHAOS project ANR-12-BS05-0009 supported by the French Research National Agency. J.M.-J. is supported by an Australian Research Council (ARC) Future Fellowship (FT140101082) and also acknowledges support from an ARC Discovery Grant. E.K. acknowledges support from TUBITAK BIDEB 2219 program. This work was supported by the Spanish Ministerio de Economa y Competitividad (MINECO) under grant AYA2013-47447-C3-1-P (S.M.). NR 115 TC 6 Z9 6 U1 1 U2 9 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 20 PY 2015 VL 808 IS 1 AR 85 DI 10.1088/0004-637X/808/1/85 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO3MS UT WOS:000359062500085 ER PT J AU Uchida, H Koyama, K Yamaguchi, H AF Uchida, Hiroyuki Koyama, Katsuji Yamaguchi, Hiroya TI N49: THE FIRST ROBUST DISCOVERY OF RECOMBINING PLASMA IN AN EXTRA GALACTIC SUPERNOVA REMNANT SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: abundances; ISM: individual objects (DEM L71, N23, N49, N49B); ISM: supernova remnants; X-rays: ISM ID LARGE-MAGELLANIC-CLOUD; X-RAY-EMISSION; XMM-NEWTON; OVERIONIZED PLASMA; MASER EMISSION; RICH EJECTA; DEM L71; IC 443; SPECTROSCOPY; ABUNDANCES AB Recent discoveries of recombining plasmas (RPs) in supernova remnants (SNRs) have dramatically changed our understanding of SNR evolution. To date, a dozen RP SNRs have been identified in the Galaxy. Here, we present Suzaku deep observations of four SNRs in the LMC, namely, N49, N49B, N23, and DEM L71, for accurate determination of their plasma states. Our uniform analysis reveals that of these SNRs, only N49 is in the recombining state, which is the first robust discovery of an RP from an extra-galactic SNR. Given that RPs have only been identified in core-collapse SNRs, our results strongly suggest a massive star origin for this SNR. On the other hand, no clear evidence of an RP is confirmed in N23, for which detection of recombination lines and continua was previously claimed. Comparing the physical properties of the RP SNRs identified so far, we find that all of them can be categorized into the "mixed-morphology" class, interacting with surrounding molecular clouds. This might be a key to determining the formation mechanisms of RPs. C1 [Uchida, Hiroyuki; Koyama, Katsuji] Kyoto Univ, Grad Sch Sci, Dept Phys, Sakyo Ku, Kyoto 6068502, Japan. [Koyama, Katsuji] Osaka Univ, Grad Sch Sci, Dept Earth & Space Sci, Toyonaka, Osaka 5600043, Japan. [Yamaguchi, Hiroya] NASA Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Yamaguchi, Hiroya] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. RP Uchida, H (reprint author), Kyoto Univ, Grad Sch Sci, Dept Phys, Sakyo Ku, Kitashirakawa Oiwake Cho, Kyoto 6068502, Japan. EM uchida@cr.scphys.kyoto-u.ac.jp RI XRAY, SUZAKU/A-1808-2009 FU JSPS [26800102, 2450229] FX The authors thank Dr. T. G. Tsuru for a careful reading of our manuscript. This work is supported by JSPS KAKENHI grant Nos. 26800102 (H.U.) and 2450229 (K.K.). NR 77 TC 2 Z9 2 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 20 PY 2015 VL 808 IS 1 AR 77 DI 10.1088/0004-637X/808/1/77 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO3MS UT WOS:000359062500077 ER PT J AU van Engelen, A Sherwin, BD Sehgal, N Addison, GE Allison, R Battaglia, N de Bernardis, F Bond, JR Calabrese, E Coughlin, K Crichton, D Datta, R Devlin, MJ Dunkley, J Dunner, R Gallardo, P Grace, E Gralla, M Hajian, A Hasselfield, M Henderson, S Hill, JC Hilton, M Hincks, AD Hlozek, R Huffenberger, KM Hughes, JP Koopman, B Kosowsky, A Louis, T Lungu, M Madhavacheril, M Maurin, L McMahon, J Moodley, K Munson, C Naess, S Nati, F Newburgh, L Niemack, MD Nolta, MR Page, LA Pappas, C Partridge, B Schmitt, BL Sievers, JL Simon, S Spergel, DN Staggs, ST Switzer, ER Ward, JT Wollack, EJ AF van Engelen, Alexander Sherwin, Blake D. Sehgal, Neelima Addison, Graeme E. Allison, Rupert Battaglia, Nick de Bernardis, Francesco Bond, J. Richard Calabrese, Erminia Coughlin, Kevin Crichton, Devin Datta, Rahul Devlin, Mark J. Dunkley, Joanna Duenner, Rolando Gallardo, Patricio Grace, Emily Gralla, Megan Hajian, Amir Hasselfield, Matthew Henderson, Shawn Hill, J. Colin Hilton, Matt Hincks, Adam D. Hlozek, Renee Huffenberger, Kevin M. Hughes, John P. Koopman, Brian Kosowsky, Arthur Louis, Thibaut Lungu, Marius Madhavacheril, Mathew Maurin, Loic McMahon, Jeff Moodley, Kavilan Munson, Charles Naess, Sigurd Nati, Federico Newburgh, Laura Niemack, Michael D. Nolta, Michael R. Page, Lyman A. Pappas, Christine Partridge, Bruce Schmitt, Benjamin L. Sievers, Jonathan L. Simon, Sara Spergel, David N. Staggs, Suzanne T. Switzer, Eric R. Ward, Jonathan T. Wollack, Edward J. TI THE ATACAMA COSMOLOGY TELESCOPE: LENSING OF CMB TEMPERATURE AND POLARIZATION DERIVED FROM COSMIC INFRARED BACKGROUND CROSS-CORRELATION SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmic background radiation; cosmology: observations; infrared: diffuse background; large-scale structure of universe ID SOUTH-POLE TELESCOPE; PROBE WMAP OBSERVATIONS; POWER SPECTRUM; DUST EMISSION; MICROWAVE; MAPS; GALAXIES; MASS; SKY; RECONSTRUCTION AB We present a measurement of the gravitational lensing of the Cosmic Microwave Background (CMB) temperature and polarization fields obtained by cross-correlating the reconstructed convergence signal from the first season of Atacama Cosmology Telescope Polarimeter data at 146 GHz with Cosmic Infrared Background (CIB) fluctuations measured using the Planck satellite. Using an effective overlap area of 92.7 square degrees, we detect gravitational lensing of the CMB polarization by large-scale structure at a statistical significance of 4.5 sigma. Combining both CMB temperature and polarization data gives a lensing detection at 9.1 sigma significance. A B-mode polarization lensing signal is present with a significance of 3.2 sigma. We also present the first measurement of CMB lensing-CIB correlation at small scales corresponding to l > 2000. Null tests and systematic checks show that our results are not significantly biased by astrophysical or instrumental systematic effects, including Galactic dust. Fitting our measurements to the best-fit lensing-CIB cross-power spectrum measured in Planck data, scaled by an amplitude A, gives A = 1.02(-0.08)(+0.12)(stat.) +/- 0.06(syst.), consistent with the Planck results. C1 [van Engelen, Alexander; Bond, J. Richard; Hajian, Amir; Nolta, Michael R.; Switzer, Eric R.] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada. [van Engelen, Alexander; Sehgal, Neelima; Madhavacheril, Mathew] SUNY Stony Brook, Dept Phys & Astron, Stony Brook, NY 11794 USA. [Sherwin, Blake D.] Univ Calif Berkeley, LBL, Berkeley Ctr Cosmol Phys, Berkeley, CA 94720 USA. [Sherwin, Blake D.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Addison, Graeme E.; Hasselfield, Matthew; Hincks, Adam D.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z4, Canada. [Allison, Rupert; Calabrese, Erminia; Dunkley, Joanna; Louis, Thibaut; Naess, Sigurd] Univ Oxford, Subdept Astrophys, Oxford OX1 3RH, England. [Battaglia, Nick] Carnegie Mellon Univ, McWilliams Ctr Cosmol, Dept Phys, Pittsburgh, PA 15213 USA. [de Bernardis, Francesco; Gallardo, Patricio; Henderson, Shawn; Koopman, Brian; Niemack, Michael D.] Cornell Univ, Dept Phys, Ithaca, NY 14853 USA. [Coughlin, Kevin; Datta, Rahul; McMahon, Jeff; Munson, Charles] Univ Michigan, Dept Phys, Ann Arbor, MI 48103 USA. [Crichton, Devin; Gralla, Megan] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Devlin, Mark J.; Lungu, Marius; Schmitt, Benjamin L.; Ward, Jonathan T.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. [Duenner, Rolando; Maurin, Loic] Pontificia Univ Catolica Chile, Dept Astron & Astrofis, Santiago 22, Chile. [Grace, Emily; Page, Lyman A.; Pappas, Christine; Sievers, Jonathan L.; Simon, Sara; Staggs, Suzanne T.] Princeton Univ, Joseph Henry Labs Phys, Princeton, NJ 08544 USA. [Hasselfield, Matthew; Hlozek, Renee; Spergel, David N.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Hill, J. Colin] Columbia Univ, Dept Astron, New York, NY 10027 USA. [Hilton, Matt; Moodley, Kavilan] Univ KwaZulu Natal, Sch Math Stat & Comp Sci, Astrophys & Cosmol Res Unit, Durban 4041, South Africa. [Huffenberger, Kevin M.] Florida State Univ, Dept Phys, Tallahassee, FL 32306 USA. [Hughes, John P.] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. [Kosowsky, Arthur] Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA. [Nati, Federico] Univ Roma La Sapienza, Dipartimento Fis, I-00185 Rome, Italy. [Newburgh, Laura] Univ Toronto, Dunlap Inst Astron & Astrophys, Toronto, ON M5S 3H4, Canada. [Partridge, Bruce] Haverford Coll, Dept Phys & Astron, Haverford, PA 19041 USA. [Sievers, Jonathan L.] Univ KwaZulu Natal, Sch Chem & Phys, Astrophys & Cosmol Res Unit, Durban 4041, South Africa. [Sievers, Jonathan L.] Univ KwaZulu Natal, Natl Inst Theoret Phys NITheP, Durban 4000, South Africa. [Switzer, Eric R.; Wollack, Edward J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP van Engelen, A (reprint author), Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada. RI Nati, Federico/I-4469-2016; Wollack, Edward/D-4467-2012; OI Nati, Federico/0000-0002-8307-5088; Wollack, Edward/0000-0002-7567-4451; Madhavacheril, Mathew/0000-0001-6740-5350; Sievers, Jonathan/0000-0001-6903-5074; Huffenberger, Kevin/0000-0001-7109-0099 FU U.S. National Science Foundation [AST-0408698, AST-0965625, PHY-0855887, PHY-1214379]; Princeton University; University of Pennsylvania; Cornell University; University of Michigan; Canada Foundation for Innovation (CFI) award; NSF [AST-13122380]; Misrahi research fund; Oxford ERC grant [259505]; NASA [NNX13AE56G, NNX14AB58G]; CONICYT [QUIMAL-120001, FONDECYT-1141113]; Comision Nacional de Investigacion Cientifica y Tecnologica de Chile (CONICYT); Government of Ontario; Ontario Research Fund-Research Excellence; University of Toronto; Wilkinson research fund; Compute Canada FX We thank Duncan Hanson for discussion and clarification regarding Section 7. We additionally thank Olivier Dore, Gil Holder, Guilaine Lagache, and Marco Viero for useful correspondence. This work was supported by the U.S. National Science Foundation through awards AST-0408698 and AST-0965625 for the ACT project, as well as awards PHY-0855887 and PHY-1214379. Funding was also provided by Princeton University, the University of Pennsylvania, Cornell University, the University of Michigan, and a Canada Foundation for Innovation (CFI) award to U.B.C. A.K. is supported by NSF grant AST-13122380. We gratefully acknowledge support from the Misrahi and Wilkinson research funds. We acknowledge Oxford ERC grant 259505. The development of detectors and lenses was supported by NASA grants NNX13AE56G and NNX14AB58G. We also acknowledge support from CONICYT grants QUIMAL-120001 and FONDECYT-1141113. ACT operates in the Parque Astronomico Atacama in northern Chile under the auspices of the Comision Nacional de Investigacion Cientifica y Tecnologica de Chile (CONICYT). Computations were performed on the GPC supercomputer at the SciNet HPC Consortium. SciNet is funded by the CFI under the auspices of Compute Canada, the Government of Ontario, the Ontario Research Fund-Research Excellence; and the University of Toronto. NR 69 TC 24 Z9 24 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 20 PY 2015 VL 808 IS 1 AR 7 DI 10.1088/0004-637X/808/1/7 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO3MS UT WOS:000359062500007 ER PT J AU Yoon, Y Im, M Jeon, Y Lee, SK Choi, P Gehrels, N Pak, S Sakamoto, T Urata, Y AF Yoon, Yongmin Im, Myungshin Jeon, Yiseul Lee, Seong-Kook Choi, Philip Gehrels, Neil Pak, Soojong Sakamoto, Takanori Urata, Yuji TI HOST GALAXY PROPERTIES AND BLACK HOLE MASS OF SWIFT J164449.3+573451 FROM MULTI-WAVELENGTH LONG-TERM MONITORING AND HST DATA SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: nuclei; galaxies: photometry; galaxies: structure; techniques: photometric ID ACTIVE GALACTIC NUCLEI; BULGE SCALING RELATIONS; TIDALLY DISRUPTED STAR; BH-SIGMA RELATION; COSMIC EVOLUTION; VELOCITY DISPERSION; M-BH-SIGMA(ASTERISK) RELATION; RELATIVISTIC OUTFLOW; POPULATION SYNTHESIS; CLASSICAL BULGES AB We study the host galaxy properties of the tidal disruption object Swift J164449.3+573451 using long-term optical to near-infrared (NIR) data. First, we decompose the galaxy surface brightness distribution and analyze the morphology of the host galaxy using high-resolution Hubble Space Telescope WFC3 images. We conclude that the host galaxy is bulge-dominant and well described by a single Sersic model with Sersic index n = 3.43 +/- 0.05. Adding a disk component, the bulge to total host galaxy flux ratio (B/T) is 0.83 +/- 0.03, which still indicates a bulge-dominant galaxy. Second, we estimate multi-band fluxes of the host galaxy through long-term light curves. Our long-term NIR light curves reveal the pure host galaxy fluxes similar to 500 days after the burst. We fit spectral energy distribution models to the multi-band fluxes from the optical to NIR of the host galaxy and determine its properties. The stellar mass, the star formation rate, and the age of the stellar population are log(M-*/M-circle dot) 9.14(-0.10)(+0.13) , 0.03(-0.03)(+0.28) M-circle dot yr(-1),and 0.63(-0.43)(+0.95) Gyr. Finally, we estimate the mass of the central super massive black hole which is responsible for the tidal disruption event. The black hole mass is estimated to be 10(6.7 +/- 0.4) M-circle dot from M-BH-M-*,M-bul and M-BH-L-bul relations for the K band, although a smaller value of similar to 10(5) M-circle dot cannot be excluded convincingly if the host galaxy harbors a pseudobulge. C1 [Yoon, Yongmin; Im, Myungshin; Jeon, Yiseul; Lee, Seong-Kook] Seoul Natl Univ, Dept Phys & Astron, Astron Program, CEOU, Seoul 151742, South Korea. [Choi, Philip] Pomona Coll, Dept Phys & Astron, Claremont, CA 91711 USA. [Gehrels, Neil] NASA, Goddard Space Flight Ctr, Astroparticle Phys Div, Greenbelt, MD 20771 USA. [Pak, Soojong] Kyung Hee Univ, Sch Space Res, Yongin 446741, Gyeonggi Do, South Korea. [Pak, Soojong] Kyung Hee Univ, Inst Nat Sci, Yongin 446741, Gyeonggi Do, South Korea. [Sakamoto, Takanori] Aoyama Gakuin Univ, Coll Sci & Engn, Dept Math & Phys, Chuo Ku, Sagamihara, Kanagawa 2525258, Japan. [Urata, Yuji] Natl Cent Univ, Inst Astron, Chungli 32054, Taiwan. RP Yoon, Y (reprint author), Seoul Natl Univ, Dept Phys & Astron, Astron Program, CEOU, 599 Gwanak Ro, Seoul 151742, South Korea. EM yymx2@astro.snu.ac.kr; mim@astro.snu.ac.kr OI Im, Myungshin/0000-0002-8537-6714; Pak, Soojong/0000-0002-2548-238X FU National Research Foundation of Korea (NRF) [2008-0060544]; Korea government (MSIP); NASA [NNX10AF39G]; Korea Institute FX This work was supported by the National Research Foundation of Korea (NRF) grant No. 2008-0060544, funded by the Korea government (MSIP). We thank the observers who obtained the CQUEAN and UKIRT data that were used in our analysis. This paper includes the data taken at the McDonald Observatory of the University of Texas at Austin. At the time of the UKIRT observation, UKIRT was operated by the Joint Astronomy Centre on behalf of the Science and Technology Facilities Council of the U.K. This work is based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. We acknowledge the use of public data from the Swift data archive. C.P., T.S., and N.G. acknowledge support from the NASA research grant NNX10AF39G. M.I. gratefully acknowledges the hospitality and support of the Korea Institute of Advanced Study where part of this was carried out. NR 67 TC 6 Z9 6 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 20 PY 2015 VL 808 IS 1 AR 96 DI 10.1088/0004-637X/808/1/96 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO3MS UT WOS:000359062500096 ER PT J AU Yusef-Zadeh, F Wardle, M Sewilo, M Roberts, DA Smith, I Arendt, R Cotton, W Lacy, J Martin, S Pound, MW Rickert, M Royster, M AF Yusef-Zadeh, F. Wardle, M. Sewilo, M. Roberts, D. A. Smith, I. Arendt, R. Cotton, W. Lacy, J. Martin, S. Pound, M. W. Rickert, M. Royster, M. TI SIGNATURES OF YOUNG STAR FORMATION ACTIVITY WITHIN TWO PARSECS OF Sgr A SO ASTROPHYSICAL JOURNAL LA English DT Article DE Galaxy: center; ISM: clouds; ISM: general; stars: black hole; stars: formation; stars: protostars ID SPECTRAL ENERGY-DISTRIBUTIONS; GALACTIC-CENTER; STELLAR OBJECTS; A-ASTERISK; CIRCUMNUCLEAR DISK; BLACK-HOLE; MOLECULAR-HYDROGEN; OH/IR STARS; IONIZED-GAS; GALAXY AB We present radio and infrared observations indicating ongoing star formation activity inside the similar to 2-5 pc circumnuclear ring at the Galactic center. Collectively these measurements suggest a continued disk-based mode of ongoing star formation has taken place near Sgr A* over the last few million years. First, Very Large Array observations with spatial resolution 2 ''.. 17 x 0 ''. 81 reveal 13 water masers, several of which have multiple velocity components. The presence of interstellar water masers suggests gas densities that are sufficient for self-gravity to overcome the tidal shear of the 4 x 10(6) M-circle dot black hole. Second, spectral energy distribution modeling of stellar sources indicates massive young stellar object (YSO) candidates interior to the molecular ring, supporting in situ star formation near Sgr A* and appear to show a distribution similar to that of the counter-rotating disks of similar to 100 OB stars orbiting Sgr A*. Some YSO candidates (e.g., IRS 5) have bow shock structures, suggesting that they have gaseous disks that are phototoevaporated and photoionized by the strong radiation field. Third, we detect clumps of SiO (2-1) and (5-4) line emission in the ring based on Combined Array for Research in Millimeter-wave Astronomy and Sub-Millimeter Array observations. The FWHM and luminosity of the SiO emission is consistent with shocked protostellar outflows. Fourth, two linear ionized features with an extent of similar to 0.8 pc show blue and redshifted velocities between +50 and -40 km s(-1), suggesting protostellar jet driven outflows with mass-loss rates of similar to 5 x 10(-5) M-circle dot yr(-1). Finally, we present the imprint of radio dark clouds at 44 GHz, representing a reservoir of molecular gas that feeds star formation activity close to Sgr A*. C1 [Yusef-Zadeh, F.; Roberts, D. A.; Rickert, M.; Royster, M.] Northwestern Univ, Dept Phys & Astron, Evanston, IL 60208 USA. [Yusef-Zadeh, F.; Roberts, D. A.; Rickert, M.; Royster, M.] Northwestern Univ, CIERA, Evanston, IL 60208 USA. [Wardle, M.; Smith, I.] Macquarie Univ, Dept Phys & Astron, Sydney, NSW 2109, Australia. [Wardle, M.; Smith, I.] Macquarie Univ, Res Ctr Astron Astrophys & Astrophoton, Sydney, NSW 2109, Australia. [Sewilo, M.] Space Sci Inst, Boulder, CO 80301 USA. [Arendt, R.] NASA, GSFC, UMBC, CRESST, Greenbelt, MD 20771 USA. [Cotton, W.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. [Lacy, J.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Martin, S.] Inst Radio Astron Millimetr, F-38406 St Martin Dheres, France. [Pound, M. W.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. RP Yusef-Zadeh, F (reprint author), Northwestern Univ, Dept Phys & Astron, Evanston, IL 60208 USA. OI Wardle, Mark/0000-0002-1737-0871; Arendt, Richard/0000-0001-8403-8548 FU NSF [AST-0807400]; ADS/JAO.ALMA [2011.0.00005.SV] FX We are grateful to S. Gillessen and the MPE group for providing us with a 3.8 mu m image of the Galactic center. This work is partially supported by the grant AST-0807400 from the NSF. The National Radio Astronomy Observatory is a facility of the National Science Foundation, operated under a cooperative agreement by Associated Universities, Inc. We thank the referee for useful comments. This paper makes use of the following ALMA data: ADS/JAO.ALMA\#2011.0.00005.SV Project code. ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada) and NSC and ASIAA (Taiwan), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO and NAOJ. NR 67 TC 4 Z9 4 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 20 PY 2015 VL 808 IS 1 AR 97 DI 10.1088/0004-637X/808/1/97 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO3MS UT WOS:000359062500097 ER PT J AU Fomalont, EB Vlahakis, C Corder, S Remijan, A Barkats, D Lucas, R Hunter, TR Brogan, CL Asaki, Y Matsushita, S Dent, WRF Hills, RE Phillips, N Richards, AMS Cox, P Amestica, R Broguiere, D Cotton, W Hales, AS Hiriart, R Hirota, A Hodge, JA Impellizzeri, CMV Kern, J Kneissl, R Liuzzo, E Marcelino, N Marson, R Mignano, A Nakanishi, K Nikolic, B Perez, JE Perez, LM Toledo, I Aladro, R Butler, B Cortes, J Cortes, P Dhawan, V Di Francesco, J Espada, D Galarza, F Garcia-Appadoo, D Guzman-Ramirez, L Humphreys, EM Jung, T Kameno, S Laing, RA Leon, S Mangum, J Marconi, G Nagai, H Nyman, LA Radiszcz, M Rodon, JA Sawada, T Takahashi, S Tilanus, RPJ van Kempen, T Vilaro, BV Watson, LC Wiklind, T Gueth, F Tatematsu, K Wootten, A Castro-Carrizo, A Chapillon, E Dumas, G de Gregorio-Monsalvo, I Francke, H Gallardo, J Garcia, J Gonzalez, S Hibbard, JE Hill, T Kaminski, T Karim, A Krips, M Kurono, Y Lopez, C Martin, S Maud, L Morales, F Pietu, V Plarre, K Schieven, G Testi, L Videla, L Villard, E Whyborn, N Zwaan, MA Alves, F Andreani, P Avison, A Barta, M Bedosti, F Bendo, GJ Bertoldi, F Bethermin, M Biggs, A Boissier, J Brand, J Burkutean, S Casasola, V Conway, J Cortese, L Dabrowski, B Davis, TA Trigo, MD Fontani, F Franco-Hernandez, R Fuller, G Madrid, RG Giannetti, A Ginsburg, A Graves, SF Hatziminaoglou, E Hogerheijde, M Jachym, P Serra, IJ Karlicky, M Klaasen, P Kraus, M Kunneriath, D Lagos, C Longmore, S Leurini, S Maercker, M Magnelli, B Vidal, IM Massardi, M Maury, A Muehle, S Muller, S Muxlow, T O'Gorman, E Paladino, R Petry, D Pineda, J Randall, S Richer, JS Rossetti, A Rushton, A Rygl, K Monge, AS Schaaf, R Schilke, P Stanke, T Schmalzl, M Stoehr, F Urban, S van Kampen, E Vlemmings, W Wang, K Wild, W Yang, Y Iguchi, S Hasegawa, T Saito, M Inatani, J Mizuno, N Asayama, S Kosugi, G Morita, KI Chiba, K Kawashima, S Okumura, SK Ohashi, N Ogasawara, R Sakamoto, S Noguchi, T Huang, YD Liu, SY Kemper, F Koch, PM Chen, MT Chikada, Y Hiramatsu, M Iono, D Shimojo, M Komugi, S Kim, J Lyo, AR Muller, E Herrera, C Miura, RE Ueda, J Chibueze, J Su, YN Trejo-Cruz, A Wang, KS Kiuchi, H Ukita, N Sugimoto, M Kawabe, R Hayashi, M Miyama, S Ho, PTP Kaifu, N Ishiguro, M Beasley, AJ Bhatnagar, S Braatz, JA Brisbin, DG Brunetti, N Carilli, C Crossley, JH D'Addario, L Meyer, JLD Emerson, DT Evans, AS Fisher, P Golap, K Griffith, DM Hale, AE Halstead, D Hardy, EJ Hatz, MC Holdaway, M Indebetouw, R Jewell, PR Kepley, AA Kim, DC Lacy, MD Leroy, AK Liszt, HS Lonsdale, CJ Matthews, B McKinnon, M Mason, BS Moellenbrock, G Moullet, A Myers, ST Ott, J Peck, AB Pisano, J Radford, SJE Randolph, WT Venkata, UR Rawlings, MG Rosen, R Schnee, SL Scott, KS Sharp, NK Sheth, K Simon, RS Tsutsumi, T Wood, SJ AF Fomalont, E. B. Vlahakis, C. Corder, S. Remijan, A. Barkats, D. Lucas, R. Hunter, T. R. Brogan, C. L. Asaki, Y. Matsushita, S. Dent, W. R. F. Hills, R. E. Phillips, N. Richards, A. M. S. Cox, P. Amestica, R. Broguiere, D. Cotton, W. Hales, A. S. Hiriart, R. Hirota, A. Hodge, J. A. Impellizzeri, C. M. V. Kern, J. Kneissl, R. Liuzzo, E. Marcelino, N. Marson, R. Mignano, A. Nakanishi, K. Nikolic, B. Perez, J. E. Perez, L. M. Toledo, I. Aladro, R. Butler, B. Cortes, J. Cortes, P. Dhawan, V. Di Francesco, J. Espada, D. Galarza, F. Garcia-Appadoo, D. Guzman-Ramirez, L. Humphreys, E. M. Jung, T. Kameno, S. Laing, R. A. Leon, S. Mangum, J. Marconi, G. Nagai, H. Nyman, L. -A. Radiszcz, M. Rodon, J. A. Sawada, T. Takahashi, S. Tilanus, R. P. J. van Kempen, T. Vila Vilaro, B. Watson, L. C. Wiklind, T. Gueth, F. Tatematsu, K. Wootten, A. Castro-Carrizo, A. Chapillon, E. Dumas, G. de Gregorio-Monsalvo, I. Francke, H. Gallardo, J. Garcia, J. Gonzalez, S. Hibbard, J. E. Hill, T. Kaminski, T. Karim, A. Krips, M. Kurono, Y. Lopez, C. Martin, S. Maud, L. Morales, F. Pietu, V. Plarre, K. Schieven, G. Testi, L. Videla, L. Villard, E. Whyborn, N. Zwaan, M. A. Alves, F. Andreani, P. Avison, A. Barta, M. Bedosti, F. Bendo, G. J. Bertoldi, F. Bethermin, M. Biggs, A. Boissier, J. Brand, J. Burkutean, S. Casasola, V. Conway, J. Cortese, L. Dabrowski, B. Davis, T. A. Trigo, M. Diaz Fontani, F. Franco-Hernandez, R. Fuller, G. Galvan Madrid, R. Giannetti, A. Ginsburg, A. Graves, S. F. Hatziminaoglou, E. Hogerheijde, M. Jachym, P. Serra, I. Jimenez Karlicky, M. Klaasen, P. Kraus, M. Kunneriath, D. Lagos, C. Longmore, S. Leurini, S. Maercker, M. Magnelli, B. Vidal, I. Marti Massardi, M. Maury, A. Muehle, S. Muller, S. Muxlow, T. O'Gorman, E. Paladino, R. Petry, D. Pineda, J. Randall, S. Richer, J. S. Rossetti, A. Rushton, A. Rygl, K. Monge, A. Sanchez Schaaf, R. Schilke, P. Stanke, T. Schmalzl, M. Stoehr, F. Urban, S. van Kampen, E. Vlemmings, W. Wang, K. Wild, W. Yang, Y. Iguchi, S. Hasegawa, T. Saito, M. Inatani, J. Mizuno, N. Asayama, S. Kosugi, G. Morita, K. -I. Chiba, K. Kawashima, S. Okumura, S. K. Ohashi, N. Ogasawara, R. Sakamoto, S. Noguchi, T. Huang, Y. -D. Liu, S. -Y. Kemper, F. Koch, P. M. Chen, M. -T. Chikada, Y. Hiramatsu, M. Iono, D. Shimojo, M. Komugi, S. Kim, J. Lyo, A. -R. Muller, E. Herrera, C. Miura, R. E. Ueda, J. Chibueze, J. Su, Y. -N. Trejo-Cruz, A. Wang, K. -S. Kiuchi, H. Ukita, N. Sugimoto, M. Kawabe, R. Hayashi, M. Miyama, S. Ho, P. T. P. Kaifu, N. Ishiguro, M. Beasley, A. J. Bhatnagar, S. Braatz, J. A., III Brisbin, D. G. Brunetti, N. Carilli, C. Crossley, J. H. D'Addario, L. Meyer, J. L. Donovan Emerson, D. T. Evans, A. S. Fisher, P. Golap, K. Griffith, D. M. Hale, A. E. Halstead, D. Hardy, E. J. Hatz, M. C. Holdaway, M. Indebetouw, R. Jewell, P. R. Kepley, A. A. Kim, D. -C. Lacy, M. D. Leroy, A. K. Liszt, H. S. Lonsdale, C. J. Matthews, B. McKinnon, M. Mason, B. S. Moellenbrock, G. Moullet, A. Myers, S. T. Ott, J. Peck, A. B. Pisano, J. Radford, S. J. E. Randolph, W. T. Venkata, U. Rao Rawlings, M. G. Rosen, R. Schnee, S. L. Scott, K. S. Sharp, N. K. Sheth, K. Simon, R. S. Tsutsumi, T. Wood, S. J. CA ALMA Partnership TI THE 2014 ALMA LONG BASELINE CAMPAIGN: AN OVERVIEW SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE instrumentation: interferometers; submillimeter: general; techniques: high angular resolution; techniques: interferometric; telescopes ID PHASE; CALIBRATION; RESOLUTION AB A major goal of the Atacama Large Millimeter/submillimeter Array (ALMA) is to make accurate images with resolutions of tens of milliarcseconds, which at submillimeter (submm) wavelengths requires baselines up to similar to 15 km. To develop and test this capability, a Long Baseline Campaign (LBC) was carried out from 2014 September to late November, culminating in end-to-end observations, calibrations, and imaging of selected Science Verification (SV) targets. This paper presents an overview of the campaign and its main results, including an investigation of the short-term coherence properties and systematic phase errors over the long baselines at the ALMA site, a summary of the SV targets and observations, and recommendations for science observing strategies at long baselines. Deep ALMA images of the quasar 3C 138 at 97 and 241 GHz are also compared to VLA 43 GHz results, demonstrating an agreement at a level of a few percent. As a result of the extensive program of LBC testing, the highly successful SV imaging at long baselines achieved angular resolutions as fine as 19 mas at similar to 350 GHz. Observing with ALMA on baselines of up to 15 km is now possible, and opens up new parameter space for submm astronomy. C1 [Fomalont, E. B.; Vlahakis, C.; Corder, S.; Remijan, A.; Barkats, D.; Dent, W. R. F.; Phillips, N.; Cox, P.; Hales, A. S.; Hirota, A.; Impellizzeri, C. M. V.; Kneissl, R.; Nakanishi, K.; Toledo, I.; Cortes, J.; Cortes, P.; Espada, D.; Galarza, F.; Garcia-Appadoo, D.; Kameno, S.; Leon, S.; Marconi, G.; Nyman, L. -A.; Radiszcz, M.; Sawada, T.; Takahashi, S.; Vila Vilaro, B.; Wiklind, T.; de Gregorio-Monsalvo, I.; Francke, H.; Gallardo, J.; Garcia, J.; Gonzalez, S.; Hill, T.; Kurono, Y.; Lopez, C.; Morales, F.; Plarre, K.; Videla, L.; Villard, E.; Whyborn, N.; Avison, A.; Mizuno, N.; Morita, K. -I.; Sugimoto, M.] Joint ALMA Observ, Santiago, Chile. [Fomalont, E. B.; Remijan, A.; Brogan, C. L.; Hales, A. S.; Hodge, J. A.; Impellizzeri, C. M. V.; Perez, J. E.; Butler, B.; Cortes, J.; Mangum, J.; Wootten, A.; Hibbard, J. E.; Beasley, A. J.; Braatz, J. A., III; Brisbin, D. G.; Brunetti, N.; Crossley, J. H.; Meyer, J. L. Donovan; Emerson, D. T.; Evans, A. S.; Griffith, D. M.; Hale, A. E.; Halstead, D.; Hatz, M. C.; Kepley, A. A.; Kim, D. -C.; Lacy, M. D.; Leroy, A. K.; Liszt, H. S.; Lonsdale, C. J.; McKinnon, M.; Mason, B. S.; Moullet, A.; Peck, A. B.; Pisano, J.; Rawlings, M. G.; Scott, K. S.; Sheth, K.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. [Vlahakis, C.; Barkats, D.; Dent, W. R. F.; Phillips, N.; Cox, P.; Kneissl, R.; Aladro, R.; Garcia-Appadoo, D.; Guzman-Ramirez, L.; Leon, S.; Marconi, G.; Nyman, L. -A.; Rodon, J. A.; Vila Vilaro, B.; Watson, L. C.; Wiklind, T.; de Gregorio-Monsalvo, I.; Hill, T.; Kaminski, T.; Villard, E.; Whyborn, N.] European So Observ, Santiago 19, Chile. [Lucas, R.] Inst Planetol & Astrophys Grenoble, UMR 5274, F-38041 Grenoble 9, France. [Asaki, Y.; Hirota, A.; Nakanishi, K.; Espada, D.; Kameno, S.; Nagai, H.; Sawada, T.; Takahashi, S.; Tatematsu, K.; Kurono, Y.; Iguchi, S.; Hasegawa, T.; Saito, M.; Inatani, J.; Mizuno, N.; Asayama, S.; Morita, K. -I.; Chiba, K.; Kawashima, S.; Ohashi, N.; Ogasawara, R.; Sakamoto, S.; Noguchi, T.; Chikada, Y.; Hiramatsu, M.; Iono, D.; Shimojo, M.; Komugi, S.; Muller, E.; Herrera, C.; Miura, R. E.; Ueda, J.; Chibueze, J.; Kiuchi, H.; Ukita, N.; Sugimoto, M.; Kawabe, R.; Hayashi, M.; Kaifu, N.; Ishiguro, M.] Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan. [Asaki, Y.] JAXA, ISAS, Chuo Ku, Sagamihara, Kanagawa 2525210, Japan. [Matsushita, S.; Huang, Y. -D.; Liu, S. -Y.; Kemper, F.; Koch, P. M.; Chen, M. -T.; Su, Y. -N.; Trejo-Cruz, A.; Wang, K. -S.; Ho, P. T. P.] Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan. [Hills, R. E.; Nikolic, B.; Avison, A.; Graves, S. F.; Richer, J. S.] Univ Cambridge, Cavendish Lab, Astrophys Grp, Cambridge CB3 0HE, England. [Richards, A. M. S.; Avison, A.; Bendo, G. J.; Fuller, G.; Muxlow, T.] Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England. [Broguiere, D.; Gueth, F.; Castro-Carrizo, A.; Chapillon, E.; Dumas, G.; Krips, M.; Martin, S.; Pietu, V.; Avison, A.; Boissier, J.] Inst Radioastron Millimetr IRAM, F-38406 St Martin Dheres, France. [Hiriart, R.; Kern, J.; Marson, R.; Perez, L. M.; Dhawan, V.; Bhatnagar, S.; Carilli, C.; Golap, K.; Moellenbrock, G.; Myers, S. T.; Ott, J.; Venkata, U. Rao; Tsutsumi, T.] Natl Radio Astron Observ, Socorro, NM 87801 USA. [Liuzzo, E.; Marcelino, N.; Mignano, A.; Bedosti, F.; Brand, J.; Massardi, M.; Paladino, R.; Rossetti, A.; Rygl, K.] CNR, Ist Radioastron, INAF, I-40129 Bologna, Italy. [Di Francesco, J.; Schieven, G.; Matthews, B.] Natl Res Council Herzberg Astron & Astrophys, Victoria, BC V9E 2E7, Canada. [Humphreys, E. M.; Laing, R. A.; Testi, L.; Zwaan, M. A.; Andreani, P.; Bethermin, M.; Biggs, A.; Trigo, M. Diaz; Ginsburg, A.; Hatziminaoglou, E.; Serra, I. Jimenez; Lagos, C.; Longmore, S.; Petry, D.; Randall, S.; Stanke, T.; Stoehr, F.; van Kampen, E.; Wang, K.; Wild, W.] European So Observ, D-85748 Garching, Germany. [Jung, T.; Yang, Y.; Kim, J.; Lyo, A. -R.] Korea Astron & Space Sci Inst, Taejon 305349, South Korea. [Tilanus, R. P. J.; van Kempen, T.; Maud, L.; Hogerheijde, M.; Klaasen, P.; Schmalzl, M.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Chapillon, E.] Univ Bordeaux, LAB, UMR 5804, F-33270 Floirac, France. [Chapillon, E.] CNRS, LAB, UMR 5804, F-33270 Floirac, France. [Karim, A.; Bertoldi, F.; Burkutean, S.; Giannetti, A.; Magnelli, B.; Muehle, S.; Schaaf, R.] Univ Bonn, Argelander Inst Astron, D-53121 Bonn, Germany. [Alves, F.; Pineda, J.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Barta, M.; Jachym, P.; Karlicky, M.; Kraus, M.; Kunneriath, D.; Urban, S.] Acad Sci Czech Republic, Inst Astron, CS-25165 Ondrejov, Czech Republic. [Casasola, V.; Fontani, F.] INAF Oss Astrofisco Arcetri, Florence, Italy. [Avison, A.; Conway, J.; Maercker, M.; Vidal, I. Marti; Vlemmings, W.] Chalmers, Dept Earth & Space Sci, Onsala Space Observ, SE-43992 Onsala, Sweden. [Cortese, L.] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia. [Dabrowski, B.] Univ Warmia & Mazury, Space Radio Diagnost Res Ctr, Geodesy & Land Management, Olsztyn, Poland. [Davis, T. A.] Univ Hertfordshire, Sci & Technol Res Inst, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England. [Franco-Hernandez, R.; Hardy, E. J.] Univ Chile, Dept Astron, Santiago, Chile. [Galvan Madrid, R.] Univ Nacl Autonoma Mexico, Ctr Radiostron & Astrofis, Morelia 58089, Michoacan, Mexico. [Leurini, S.; Muller, S.; O'Gorman, E.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. Liverpool John Moores Univ, Astrophys Res Inst, Liverpool L3 5RF, Merseyside, England. [Maury, A.] Univ Paris Diderot, CNRS, CEA DSM, IRFU Serv Astrophys,Lab AIM, F-91191 Gif Sur Yvette, France. [Rushton, A.] Univ Oxford, Dept Phys, Astrophys, Oxford OX1 3RH, England. [Monge, A. Sanchez; Schilke, P.] Univ Cologne, Inst Phys 1, D-50937 Cologne, Germany. [Okumura, S. K.] Japan Womens Univ, Fac Sci, Bunkyo Ku, Tokyo 1128681, Japan. [Komugi, S.] Kogakuin Univ, Hachioji, Tokyo 1920015, Japan. [Chibueze, J.] Univ Nigeria, Dept Phys & Astron, Nsukka 410001, Nigeria. [Miyama, S.] Natl Inst Nat Sci, Minato Ku, Tokyo 1050001, Japan. [Miyama, S.] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Higashihiroshima, Hiroshima 7398526, Japan. [D'Addario, L.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Evans, A. S.; Indebetouw, R.] Univ Virginia, Dept Astron, Charlottesville, VA 22903 USA. [Hardy, E. J.] Natl Radio Astron Observ, Santiago, Chile. [Radford, S. J. E.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. RP Fomalont, EB (reprint author), Joint ALMA Observ, Alonso de Cordova 3107, Santiago, Chile. EM efomalon@nrao.edu RI Marti-Vidal, Ivan/A-8799-2017; Shimojo, Masumi/J-2605-2016; Barta, Miroslav/C-7069-2012; Kunneriath, Devaky/G-8513-2014; Jachym, Pavel/G-9019-2014; Karlicky, Marian/G-9023-2014; Kraus, Michaela/G-9900-2014; MIYAMA, Shoken/A-3598-2015; Dabrowski, Bartosz/G-9007-2014; Dabrowski, Bartosz/L-1442-2016; Kemper, Francisca/D-8688-2011; OI Davis, Timothy/0000-0003-4932-9379; Brunetti, Nathan/0000-0002-0154-7724; radford, simon/0000-0001-9113-1660; Tsutsumi, Takahiro/0000-0002-4298-4461; Mangum, Jeffrey/0000-0003-1183-9293; Wang, Ke/0000-0002-7237-3856; Barkats, Denis/0000-0002-8971-1954; Hunter, Todd/0000-0001-6492-0090; Ginsburg, Adam/0000-0001-6431-9633; /0000-0002-2700-9916; Brogan, Crystal/0000-0002-6558-7653; Bethermin, Matthieu/0000-0002-3915-2015; Marti-Vidal, Ivan/0000-0003-3708-9611; Shimojo, Masumi/0000-0002-2350-3749; Brand, Jan/0000-0003-1615-9043; Muxlow, Thomas/0000-0001-5797-8796; Jachym, Pavel/0000-0002-1640-5657; Kemper, Francisca/0000-0003-2743-8240; Nikolic, Bojan/0000-0001-7168-2705; Asaki, Yoshiharu/0000-0002-0976-4010; Cortese, Luca/0000-0002-7422-9823; Vlahakis, Catherine/0000-0003-3745-4228; /0000-0002-9931-1313 FU Science and Technology Facilities Council [ST/M000966/1] NR 20 TC 17 Z9 17 U1 4 U2 21 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD JUL 20 PY 2015 VL 808 IS 1 AR L1 DI 10.1088/2041-8205/808/1/L1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CN9OO UT WOS:000358778900001 ER PT J AU Mroczkowski, T Kovacs, A Bulbul, E Staguhn, J Benford, DJ Clarke, TE van Weeren, RJ Intema, HT Randall, S AF Mroczkowski, T. Kovacs, A. Bulbul, E. Staguhn, J. Benford, D. J. Clarke, T. E. van Weeren, R. J. Intema, H. T. Randall, S. TI RESOLVING THE MERGING PLANCK CLUSTER PLCK G147.3-16.6 WITH GISMO SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE cosmology: observations; galaxies: clusters: general; galaxies: clusters: individual (PLCK G147.3-16.6); galaxies: clusters: intracluster medium; X-rays: galaxies: clusters ID SPT-SZ SURVEY; GALAXY CLUSTERS; RADIO HALO; ZELDOVICH; GHZ; TELESCOPE; EMISSION AB The Planck satellite has recently completed an all-sky galaxy cluster survey exploiting the thermal Sunyaev-Zel'dovich (SZ) effect to locate some of the most massive systems observable. With a median redshift of < z > = 0.22, the clusters found by Planck at z > 0.3 are proving to be exceptionally massive and/or disturbed systems. One notable Planck discovery at z = 0.645, PLCK G147.3-16.6, has an elongated core and hosts a radio halo, indicating it is likely in the process of merging. We present a 16 ''.5 resolution SZ observation of this high-z merger using the Goddard-IRAM Superconducting 2-Millimeter Observer, and compare it to X-ray follow-up observations with XMM-Newton. We find the SZ pressure substructure is offset from the core components seen in X-ray. We interpret this as possible line of sight temperature or density substructure due to the on-going merger. C1 [Mroczkowski, T.; Clarke, T. E.] US Navy, Res Lab, Washington, DC 20375 USA. [Kovacs, A.] CALTECH, Pasadena, CA 91125 USA. [Kovacs, A.] Univ Minnesota, Inst Astrophys, Minneapolis, MN 55455 USA. [Bulbul, E.; van Weeren, R. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Staguhn, J.; Benford, D. J.] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Code 665, Greenbelt, MD 20771 USA. [Staguhn, J.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Intema, H. T.] Natl Radio Astron Observ, Socorro, NM 87801 USA. [Mroczkowski, T.] Natl Acad Sci, Natl Res Council, London, England. RP Mroczkowski, T (reprint author), US Navy, Res Lab, 4555 Overlook Ave SW, Washington, DC 20375 USA. EM anthony.mroczkowski.ctr@nrl.navy.mil RI Kovacs, Attila/C-1171-2010; Intema, Huib/D-1438-2012; Benford, Dominic/D-4760-2012; OI Kovacs, Attila/0000-0001-8991-9088; Intema, Huib/0000-0002-5880-2730; Benford, Dominic/0000-0002-9884-4206; Mroczkowski, Tony/0000-0003-3816-5372; van Weeren, Reinout/0000-0002-0587-1660 FU 6.1 Base funding; NASA ADP grant [NNX13AE83G]; NASA through the Einstein Postdoctoral grant by the Chandra X-ray Center [PF2-130104]; NASA [NAS8-03060]; National Radio Astronomy Observatory, a facility of the National Science Foundation (NSF); NSF [1020981, 1106284]; INSU/CNRS (France); MPG (Germany); IGN (Spain) FX This research was performed while TM held a National Research Council Research Associateship Award at the Naval Research Laboratory (NRL). Basic research in radio astronomy at NRL by TM and TEC is supported by 6.1 Base funding. EB is supported in part by NASA ADP grant NNX13AE83G. RJvW is supported by NASA through the Einstein Postdoctoral grant number PF2-130104 awarded by the Chandra X-ray Center, which is operated by the Smithsonian Astrophysical Observatory for NASA under contract NAS8-03060. HTI is supported by the National Radio Astronomy Observatory, a facility of the National Science Foundation (NSF) operated under cooperative agreement by Associated Universities, Inc. The GISMO instrument and team are supported through NSF ATI grants 1020981 and 1106284. IRAM is supported by INSU/CNRS (France), MPG (Germany), and IGN (Spain). NR 31 TC 1 Z9 1 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD JUL 20 PY 2015 VL 808 IS 1 AR L6 DI 10.1088/2041-8205/808/1/L6 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CN9OO UT WOS:000358778900006 ER PT J AU Straatman, CMS Labbe, I Spitler, LR Glazebrook, K Tomczak, A Allen, R Brammer, GB Cowley, M van Dokkum, P Kacprzak, GG Kawinwanichakij, L Mehrtens, N Nanayakkara, T Papovich, C Persson, SE Quadri, RF Rees, G Tilvi, V Tran, KVH Whitaker, KE AF Straatman, Caroline M. S. Labbe, Ivo Spitler, Lee R. Glazebrook, Karl Tomczak, Adam Allen, Rebecca Brammer, Gabriel B. Cowley, Michael van Dokkum, Pieter Kacprzak, Glenn G. Kawinwanichakij, Lalit Mehrtens, Nicola Nanayakkara, Themiya Papovich, Casey Persson, S. Eric Quadri, Ryan F. Rees, Glen Tilvi, Vithal Tran, Kim-Vy H. Whitaker, Katherine E. TI THE SIZES OF MASSIVE QUIESCENT AND STAR-FORMING GALAXIES AT z similar to 4 WITH ZFOURGE AND CANDELS SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE cosmology: observations; galaxies: evolution; galaxies: formation; galaxies: high-redshift; infrared: galaxies ID DEEP-FIELD-SOUTH; EXTRAGALACTIC LEGACY SURVEY; SUBMILLIMETER GALAXIES; PHOTOMETRIC REDSHIFTS; EVOLVED GALAXIES; STELLAR MASSES; GOODS-NORTH; SKY SURVEY; EVOLUTION; COMPACT AB We study the rest-frame ultraviolet (UV) sizes of massive (similar to 0.8 x 10(11)M(circle dot).) galaxies at 3.4 <= z < 4.2, selected from the FourStar Galaxy Evolution Survey, by fitting single Sersic profiles to Hubble Space Telescope/WFC3/F160W images from the Cosmic Assembly Near-infrared Deep Extragalactic Legacy Survey. Massive quiescent galaxies are very compact, with a median circularized half-light radius re = 0.63 +/- 0.18 kpc. Removing 5 16 (31%) sources with signs of active galactic nucleus activity does not change the result. Star-forming galaxies have re = 2.0 +/- 0.60 kpc, 3.2 +/- 1.3 x larger than quiescent galaxies. Quiescent galaxies at z similar to 4 are on average 6.0 +/- 1.7 x smaller than at z similar to 0 and 1.9 +/- 0.7 x smaller than at z similar to 2. Star-forming galaxies of the same stellar mass are 2.4 +/- 0.7 x smaller than at z similar to 0. Overall, the size evolution at 0 < z < 4 is well described by a power law, with re 5.08 +/- 0.28(1 + z)(-1.44 perpendicular to 0.08) kpc for quiescent galaxies and r(e) = 6.02 +/- 0.28(1 + z)(-0.72 perpendicular to 0.05) kpc for star-forming galaxies. Compact star-forming galaxies are rare in our sample: we find only1/14 (7%) with r(e)/(M/10(11)M(circle dot))(0.75) < 1.5 11 0.75 <., whereas 13 16 (81%) of the quiescent galaxies are compact. The number density of compact quiescent galaxies at z similar to 4 is 1.8 +/- 0.8 x 10(-5) Mpc(-3) and increases rapidly, by > 5x, between 2 < z < 4. The paucity of compact star-forming galaxies at z similar to 4 and their large rest-frame UV median sizes suggest that the formation phase of compact cores is very short and/or highly dust obscured. C1 [Straatman, Caroline M. S.; Labbe, Ivo] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Spitler, Lee R.; Cowley, Michael] Australian Astron Observ, N Ryde, NSW 1670, Australia. [Spitler, Lee R.; Cowley, Michael; Rees, Glen] Macquarie Univ, Dept Phys & Astron, N Ryde, NSW 2109, Australia. [Glazebrook, Karl; Allen, Rebecca; Kacprzak, Glenn G.; Nanayakkara, Themiya] Swinburne Univ Technol, Ctr Astrophys & Supercomput, Hawthorn, Vic 3122, Australia. [Tomczak, Adam; Kawinwanichakij, Lalit; Mehrtens, Nicola; Papovich, Casey; Quadri, Ryan F.; Tilvi, Vithal; Tran, Kim-Vy H.] Texas A&M Univ, George P & Cynthia W Mitchell Inst Fundamental Ph, Dept Phys & Astron, College Stn, TX 77843 USA. [Brammer, Gabriel B.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [van Dokkum, Pieter] Yale Univ, Dept Astron, New Haven, CT 06520 USA. [Persson, S. Eric] Carnegie Observ, Pasadena, CA 91101 USA. [Whitaker, Katherine E.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. RP Straatman, CMS (reprint author), Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands. EM straatman@strw.leidenuniv.nl RI Glazebrook, Karl/N-3488-2015; OI Glazebrook, Karl/0000-0002-3254-9044; Tomczak, Adam/0000-0003-2008-1752; Straatman, Caroline/0000-0001-5937-4590 FU George P. and Cynthia Woods Mitchell Institute for Fundamental Physics and Astronomy; National Science Foundation [AST-1009707]; NL-NWO Spinoza Grant; Australian Research Council Future Fellowship [FT140100933]; NASA FX This research was supported by the George P. and Cynthia Woods Mitchell Institute for Fundamental Physics and Astronomy, the National Science Foundation grant AST-1009707, and the NL-NWO Spinoza Grant. Australian access to the Magellan Telescopes was supported through the National Collaborative Research Infrastructure Strategy of the Australian Federal Government. G.G.K. is supported by an Australian Research Council Future Fellowship FT140100933. K.E.W. is 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. We thank Arjen van der Wel, Darren Croton, Duncan Forbes, and Alister Graham for useful discussions. We thank the anonymous referee for helpful suggestions. NR 44 TC 9 Z9 10 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD JUL 20 PY 2015 VL 808 IS 1 AR L29 DI 10.1088/2041-8205/808/1/L29 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CN9OO UT WOS:000358778900029 ER PT J AU Williams, BJ Fox, OD AF Williams, Brian J. Fox, Ori D. TI SOFIA OBSERVATIONS OF SN 2010jl: ANOTHER NON-DETECTION OF THE 9.7 mu m SILICATE DUST FEATURE SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE dust, extinction; supernovae: general; supernovae: individual (SN 2010jl) ID CORE-COLLAPSE SUPERNOVAE; BLUE VARIABLE ERUPTIONS; IIN SUPERNOVAE; CIRCUMSTELLAR INTERACTION; SPITZER SPECTROSCOPY; OPTICAL-PROPERTIES; STAR; PROGENITORS; GRAINS; MINERALOGY AB We present photometric observations from the Stratospheric Observatory for Infrared Astronomy (SOFIA) at 11.1 mu m of the Type IIn supernova (SN IIn) 2010jl. The SN is undetected by SOFIA, but the upper limits obtained, combined with new and archival detections from Spitzer at 3.6 and 4.5 mu m, allow us to characterize the composition of the dust present. Dust in other SN IIn has been shown in previous works to reside in a circumstellar shell of material ejected by the progenitor system in the few millenia prior to explosion. Our model fits show that the dust in the system shows no evidence for the strong, ubiquitous 9.7 mu m feature from silicate dust, suggesting the presence of carbonaceous grains. The observations are best fit with 0.01-0.05M(circle dot) of carbonaceous dust radiating at a temperature of similar to 550-620 K. The dust composition may reveal clues concerning the nature of the progenitor system, which remains ambiguous for this subclass. Most of the single star progenitor systems proposed for SNe IIn, such as luminous blue variables, red supergiants, yellow hypergiants, and B[e] stars, all clearly show silicate dust in their pre-SN outflows. However, this post-SN result is consistent with the small sample of SNe IIn with mid-IR observations, none of which show signs of emission from silicate dust in their IR spectra. C1 [Williams, Brian J.] NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA. [Williams, Brian J.] NASA GSFC, Xray Astrophys Lab, Greenbelt, MD USA. [Fox, Ori D.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. RP Williams, BJ (reprint author), NASA, Goddard Space Flight Ctr, CRESST, Code 662,8800 Greenbelt Rd, Greenbelt, MD 20771 USA. EM brian.j.williams@nasa.gov OI Williams, Brian/0000-0003-2063-381X NR 47 TC 1 Z9 1 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD JUL 20 PY 2015 VL 808 IS 1 AR L22 DI 10.1088/2041-8205/808/1/L22 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CN9OO UT WOS:000358778900022 ER PT J AU Williams, BJ Rangelov, B Kargaltsev, O Pavlov, GG AF Williams, Brian J. Rangelov, Blagoy Kargaltsev, Oleg Pavlov, George G. TI MAGNESIUM-RICH EJECTA IN THE SNR G284.3-1.8 AROUND THE HIGH-MASS GAMMA-RAY BINARY 1FGL J1018.6-5856 SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE ISM: individual objects (G284.3, 1.8); ISM: supernova remnants; stars: individual (1FGL 1018.6, 5856); X-rays: binaries ID SUPERNOVA REMNANT; EVOLUTION; EMISSION; REGION; STARS AB We present results from two Chandra observations of the 16.6 day X-ray/gamma-ray high-mass binary 1FGL J1018.6-5856 located at the center of the supernova remnant (SNR) G284.3-1.8. The binary spectra, separated by 0.25 in binary phase, are fit with an absorbed power-law model with Gamma approximate to 1.7-1.8 for both observations (the flux during the second observation is a factor of 1.7 smaller). In the high-resolution ACIS-I image we found a hint of extended emission approximate to 2 ''-3 '' southeast of the binary, significant at the 3s level. Binary evolution codes reproduce the system's observed properties with two massive stars with an initial 18 day period, undergoing mass transfer and leaving behind a heavy approximate to 2 M-circle dot neutron star. The initial mass of the progenitor star in this scenario is 27 +/- 4 M-circle dot. Chandra and XMM-Newton images of the remnant show it has a relatively low X-ray surface brightness. The two brightest regions of extended X-ray emission, with luminosities similar to 10(33) erg s(-1) for d = 5 kpc, lie in the northern and western portions and show significantly different spectra. The northern patch is consistent with shocked ISM, with a low temperature and long ionization timescale. However, the western patch is dominated by ejecta, and shows significantly enhanced Mg content relative to other ejecta products. The abundance ratios inferred resemble those from the Large Magellanic Cloud remnant N49B. To our knowledge, this is only the second case of such Mg-rich ejecta found in an SNR. Nucleosynthesis models for core-collapse supernovae predict Mg-rich ejecta from very massive progenitors of >25 M-circle dot. C1 [Williams, Brian J.] NASA GSFC, CRESST, Greenbelt, MD 20771 USA. [Williams, Brian J.] NASA GSFC, Xray Astrophys Lab, Greenbelt, MD USA. [Rangelov, Blagoy; Kargaltsev, Oleg] George Washington Univ, Dept Phys, Washington, DC 20052 USA. [Pavlov, George G.] Penn State Univ, University Pk, PA 16802 USA. RP Williams, BJ (reprint author), NASA GSFC, CRESST, Code 662,8800 Greenbelt Rd, Greenbelt, MD 20771 USA. EM brian.j.williams@nasa.gov OI Williams, Brian/0000-0003-2063-381X; Rangelov, Blagoy/0000-0002-9282-5207 FU Chandra grant [G03-14047] FX We thank the anonymous referee for useful comments. We acknowledge useful discussions with Steve Snowden on the XMM-Newton Extended Source Analysis Software (ESAS), a part of the SAS software distributed by the XMM-Newton Guest Observer Facility. We acknowledge Chandra grant G03-14047. NR 20 TC 1 Z9 1 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD JUL 20 PY 2015 VL 808 IS 1 AR L19 DI 10.1088/2041-8205/808/1/L19 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CN9OO UT WOS:000358778900019 ER PT J AU Graff, PB Buonanno, A Sathyaprakash, BS AF Graff, Philip B. Buonanno, Alessandra Sathyaprakash, B. S. TI Missing Link: Bayesian detection and measurement of intermediate-mass black-hole binaries SO PHYSICAL REVIEW D LA English DT Article ID X-RAY SOURCE; GRAVITATIONAL-WAVES; COALESCING BINARIES; PARAMETERS; EVOLUTION; EFFICIENT; CLUSTERS; CHOICE AB We perform Bayesian analysis of gravitational-wave signals from nonspinning, intermediate-mass black-hole binaries (IMBHBs) with observed total mass, M-obs, from 50M(circle dot) to 500M(circle dot) and mass ratio 1-4 using advanced LIGO and Virgo detectors. We employ inspiral-merger-ringdown waveform models based on the effective-one-body formalism and include subleading modes of radiation beyond the leading (2,2) mode. The presence of subleading modes increases signal power for inclined binaries and allows for improved accuracy and precision in measurements of the masses as well as breaking of degeneracies in distance, orientation and polarization. For low total masses, M-obs less than or similar to 50M(circle dot), for which the inspiral signal dominates, the observed chirp mass M-obs = M-obs eta(3/5) (eta being the symmetric mass ratio) is better measured. In contrast, as increasing power comes from merger and ringdown, we find that the total mass Mobs has better relative precision than M-obs. Indeed, at high M-obs (>= 300M(circle dot)), the signal resembles a burst and the measurement thus extracts the dominant frequency of the signal that depends on Mobs. Depending on the binary's inclination, at signal-to-noise ratio (SNR) of 12, uncertainties in Mobs can be as large as similar to 20-25% while uncertainties in Mobs are similar to 50-60% in binaries with unequal masses (those numbers become similar to 17% vs. similar to 22% in more symmetric mass-ratio binaries). Although large, those uncertainties in M-obs will establish the existence of IMBHs. We find that effective-one-body waveforms with subleading modes are essential to confirm a signal's presence in the data, with calculated Bayesian evidences yielding a false alarm probability below 10(-5) for SNR greater than or similar to 9 in Gaussian noise. Our results show that gravitational-wave observations can offer a unique tool to observe and understand the formation, evolution and demographics of IMBHs, which are difficult to observe in the electromagnetic window. C1 [Graff, Philip B.; Buonanno, Alessandra] Univ Maryland, Dept Phys, College Pk, MD 20742 USA. [Graff, Philip B.] NASA, Goddard Space Flight Ctr, Gravitat Astrophys Lab, Greenbelt, MD 20771 USA. [Graff, Philip B.] Univ Maryland, Joint Space Sci Inst, College Pk, MD 20742 USA. [Buonanno, Alessandra; Sathyaprakash, B. S.] Max Planck Inst Gravitat Phys, Albert Einstein Inst, D-14476 Potsdam, Germany. [Sathyaprakash, B. S.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. RP Graff, PB (reprint author), Univ Maryland, Dept Phys, College Pk, MD 20742 USA. EM pgraff@umd.edu FU NASA [NNX12AN10G]; NSF [PHY-1208881]; National Science Foundation [PHY-0757058]; Max-Planck Institute of Gravitational Physics, Potsdam, Germany; STFC [ST/J000345/1]; Center for Gravitation and Cosmology at UWM under NSF [PHY-0923409, PHY-0600953] FX We thank Cole Miller for very useful discussions and comments and Collin Capano for a careful reading of the manuscript and comments. A. B. and P. G. acknowledge partial support from NASA Grant No. NNX12AN10G. A. B. also acknowledges partial support from NSF Grant No. PHY-1208881. P. G. was also supported during this work 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. B. S. S. acknowledges the support of the LIGO Visitor Program through the National Science Foundation Award No. PHY-0757058, Max-Planck Institute of Gravitational Physics, Potsdam, Germany, and STFC Grant No. ST/J000345/1. Results presented here were produced using the NEMO computing cluster at the Center for Gravitation and Cosmology at UWM under NSF Grants No. PHY-0923409 and No. PHY-0600953. NR 72 TC 12 Z9 12 U1 0 U2 1 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 2470-0010 EI 2470-0029 J9 PHYS REV D JI Phys. Rev. D PD JUL 20 PY 2015 VL 92 IS 2 AR 022002 DI 10.1103/PhysRevD.92.022002 PG 19 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA CN2ND UT WOS:000358257500004 ER PT J AU Bauschlicher, CW AF Bauschlicher, Charles W., Jr. TI The growth of phenanthrene from naphthalene by C2H2 additions SO MOLECULAR PHYSICS LA English DT Article DE five-membered rings; density functional theory (DFT); ring growth ID SET MODEL CHEMISTRY; REACTION PATHS; REAXFF AB Two paths are investigated for the growth of phenanthrene from naphthalene by the addition of C2H2 groups. The first series of steps leads to acenaphthylene (ACN), which is consistent with the path found previously. The addition of C2H2 to ACN can yield a product with two adjacent five-membered rings. Opening one five-membered ring produces a five-membered ring with CH2 side group. This can be converted to a six-membered ring in a manner analogous to the hydrogen atom catalysed fulvene to benzene conversion. A second path, with a somewhat higher barrier, can also lead to the phenanthrene product. The transition state for the second path is essentially isoenergetic with the stating material of ACN + C2H2 + H. C1 NASA, Entry Syst & Technol Div, Ames Res Ctr, Mountain View, CA 94035 USA. RP Bauschlicher, CW (reprint author), NASA, Entry Syst & Technol Div, Ames Res Ctr, Mail Stop 230-3, Mountain View, CA 94035 USA. EM Charles.W.Bauschlicher@nasa.gov NR 21 TC 0 Z9 0 U1 1 U2 6 PU TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND SN 0026-8976 EI 1362-3028 J9 MOL PHYS JI Mol. Phys. PD JUL 18 PY 2015 VL 113 IS 13-14 SI SI BP 1834 EP 1838 DI 10.1080/00268976.2015.1017016 PG 5 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA CM8FJ UT WOS:000357933400034 ER PT J AU Fortenberry, RC Lee, TJ AF Fortenberry, Ryan C. Lee, Timothy J. TI Rovibrational and energetic analysis of the hydroxyethynyl anion (CCOH-) SO MOLECULAR PHYSICS LA English DT Article DE astrochemistry; quartic force fields; vibrational configuration interaction theory; anions; vibrational frequencies; vibrational perturbation theory ID QUARTIC FORCE-FIELDS; VIBRATIONAL FREQUENCIES; SPECTROSCOPIC CONSTANTS; ASTRONOMICAL IDENTIFICATION; ELECTRON-AFFINITIES; INTERSTELLAR ANION; EXCITED-STATES; WAVE-FUNCTIONS; BASIS-SETS; DIPOLE AB For the first time, high-level structural and rovibrational data are provided for the hyroxyethynyl anion, CCOH-. CCOH- is a promising molecule for interstellar detection even though no new anions have been observed in the interstellar medium for the past half-decade. The large dipole moment of the corresponding neutral radical may be key for its creation as has been hypothesised and supported for other anions known to exist in various astronomical environments. Highly accurate quartic force fields are employed where previous benchmarks have produced spectroscopic constants and anharmonic vibrational frequencies within 20 MHz and 1 cm(-1), respectively, of experiment. This same approach is applied here for CCOH- and its deuterated isotopologue with the goal of assisting laboratory experiments and/or astronomical observers in the potential detection of this anion. C1 [Fortenberry, Ryan C.] Georgia So Univ, Dept Chem, Statesboro, GA 30460 USA. [Lee, Timothy J.] NASA, Div Space Sci & Astrobiol, Ames Res Ctr, Moffett Field, CA USA. RP Fortenberry, RC (reprint author), Georgia So Univ, Dept Chem, Statesboro, GA 30460 USA. EM rfortenberry@georgiasouthern.edu RI Lee, Timothy/K-2838-2012 FU Georgia Southern University; NASA [NASA 12-APRA12-0107] FX Ryan C. Fortenberry: Georgia Southern University; NASA Postdoctoral Program. Timothy J. Lee and Ryan C. Fortenberry: NASA [NASA 12-APRA12-0107 grant]. NR 66 TC 5 Z9 5 U1 0 U2 11 PU TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND SN 0026-8976 EI 1362-3028 J9 MOL PHYS JI Mol. Phys. PD JUL 18 PY 2015 VL 113 IS 13-14 SI SI BP 2012 EP 2017 DI 10.1080/00268976.2015.1031841 PG 6 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA CM8FJ UT WOS:000357933400051 ER PT J AU Birn, J Liu, YH Daughton, W Hesse, M Schindler, K AF Birn, Joachim Liu, Yi-Hsin Daughton, William Hesse, Michael Schindler, Karl TI Reconnection and interchange instability in the near magnetotail SO EARTH PLANETS AND SPACE LA English DT Article DE Reconnection; Interchange; Magnetotail dynamics; Substorms ID MAGNETIC RECONNECTION; PLASMA SHEET; FLOW; CLUSTER AB This paper provides insights into the possible coupling between reconnection and interchange/ballooning in the magnetotail related to substorms and flow bursts. The results presented are largely based on recent simulations of magnetotail dynamics, exploring onset and progression of reconnection. 2.5-dimensional particle-in-cell (PIC) simulations with different tail deformation demonstrate a clear boundary between stable and unstable cases depending on the amount of deformation, explored up to the real proton/electron mass ratio. The evolution prior to onset, as well as the evolution of stable cases, are governed by the conservation of integral flux tube entropy S as imposed in ideal MHD, maintaining a monotonic increase with distance downtail. This suggests that ballooning instability in the tail should not be expected prior to the onset of tearing and reconnection. 3-D MHD simulations confirm this conclusion, showing no indication of ballooning prior to reconnection, if the initial state is ballooning stable. The simulation also shows that, after imposing resistivity necessary to initiate reconnection, the reconnection rate and energy release initially remain slow. However, when S becomes reduced from plasmoid ejection and lobe reconnection, forming a negative slope in S as a function of distance from Earth, the reconnection rate and energy release increase drastically. The latter condition has been shown to be necessary for ballooning/interchange instability, and the cross-tail structures that develop subsequently in the MHD simulation are consistent with such modes. The simulations support a concept in which tail activity is initiated by tearing instability but significantly enhanced by the interaction with ballooning/interchange enabled by plasmoid loss and lobe reconnection. C1 [Birn, Joachim] Space Sci Inst, Boulder, CO 80301 USA. [Birn, Joachim] Los Alamos Natl Lab, Los Alamos, NM USA. [Liu, Yi-Hsin; Hesse, Michael] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Daughton, William] Los Alamos Natl Lab, Los Alamos, NM USA. [Schindler, Karl] Ruhr Univ Bochum, Bochum, Germany. RP Birn, J (reprint author), Space Sci Inst, Boulder, CO 80301 USA. EM jbirn@spacescience.org RI Daughton, William/L-9661-2013; NASA MMS, Science Team/J-5393-2013 OI NASA MMS, Science Team/0000-0002-9504-5214 FU NSF's GEM program; NASA's MMS/SMART Theory and Modeling program; Heliophysics Theory Program; NSF [OCI 07-25070]; state of Illinois.; SRT Program FX Part of this work was performed at Los Alamos under the auspices of the US Department of Energy, supported by the NSF's GEM and by NASA's MMS/SMART Theory and Modeling, SR&T and Heliophysics Theory Programs. The simulations were performed using resources from the Los Alamos Institutional Computing Program, with further resources from the Blue Waters sustained-petascale computing project, which is supported by the NSF (OCI 07-25070) and the state of Illinois. NR 24 TC 1 Z9 1 U1 1 U2 10 PU SPRINGER HEIDELBERG PI HEIDELBERG PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY SN 1880-5981 J9 EARTH PLANETS SPACE JI Earth Planets Space PD JUL 16 PY 2015 VL 67 AR 110 DI 10.1186/s40623-015-0282-3 PG 9 WC Geosciences, Multidisciplinary SC Geology GA CN6SO UT WOS:000358564700001 ER PT J AU Wing, S Fairfield, DH Johnson, JR Ohtani, SI AF Wing, Simon Fairfield, Donald H. Johnson, Jay R. Ohtani, Shin-I. TI On the field-aligned electric field in the polar cap SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE polar cap; polar rain; field-aligned electric field; parallel electric potential; electron acceleration; monoenergetic electron ID MAGNETIC-FIELD; HIGH-LATITUDES; PLASMA SHEET; LOW-ALTITUDE; PRECIPITATION; ARCS; CURRENTS; DAYSIDE; REGIONS; CUSP AB The Johns Hopkins University Applied Physics Laboratory open-field line particle precipitation model predicts downward field-aligned electric field to maintain charge quasi-neutrality. Previous studies confirmed the existence of such electric fields. However, the present study shows that upward field-aligned electric field can be found within upward field-aligned current (FAC) region. In the upward FAC region, upward electric field that accelerates electron downward is seen with the occurrence rates of 82%-96%. In contrast, the occurrence rates in the downward FAC regions are 3%-11%. Polar rain electrons located in the upward FAC region adjacent to closed field lines often show a ramping up of energy with increasing latitude before reaching a plateau. This plateau may be attributed to the magnetosheath electrons that progressively have higher antisunward velocity and lower density with increasing distance from the subsolar point before they asymptotically reach the solar wind values. C1 [Wing, Simon; Ohtani, Shin-I.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Fairfield, Donald H.] NASA, Goddard Space Flight Ctr, Space Weather Lab, Greenbelt, MD 20771 USA. [Johnson, Jay R.] Princeton Univ, Plasma Phys Lab, Princeton, NJ USA. RP Wing, S (reprint author), Johns Hopkins Univ, Appl Phys Lab, Johns Hopkins Rd, Laurel, MD 20723 USA. EM simon.wing@jhuapl.edu RI Ohtani, Shinichi/E-3914-2016 OI Ohtani, Shinichi/0000-0002-9565-6840 FU NSF [AGS-1058456, ATM0902730, AGS-1203299]; NASA [NNX13AE12G, NNX15AJ01G, NNH11AR07I, NNX14AM27G, NNH14AY20I]; DOE [DE-AC02-09CH11466] FX The Air Force Research Laboratory has been helpful in the acquisition of DMSP SSJ4/SSJ5 and magnetometer data, as has the World Data Center in Boulder, Colorado. NASA OMNIWeb Plus (http://omniweb.gsfc.nasa.gov/) provides the solar wind data. All the derived data products in this paper are available upon request by e-mail (simon.wing@jhuapl.edu). Simon Wing acknowledges support from NSF grant AGS-1058456 and NASA grants (NNX13AE12G and NNX15AJ01G). Jay R. Johnson acknowledges support from NASA grants (NNH11AR07I, NNX14AM27G, and NNH14AY20I), NSF grants (ATM0902730 and AGS-1203299), and DOE contract DE-AC02-09CH11466. NR 32 TC 3 Z9 3 U1 2 U2 7 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD JUL 16 PY 2015 VL 42 IS 13 BP 5090 EP 5099 DI 10.1002/2015GL064229 PG 10 WC Geosciences, Multidisciplinary SC Geology GA CN8LG UT WOS:000358691300002 ER PT J AU Halekas, JS Benna, M Mahaffy, PR Elphic, RC Poppe, AR Delory, GT AF Halekas, J. S. Benna, M. Mahaffy, P. R. Elphic, R. C. Poppe, A. R. Delory, G. T. TI Detections of lunar exospheric ions by the LADEE neutral mass spectrometer SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE Moon; exosphere; plasma ID ATMOSPHERE; INSTRUMENT AB The Lunar Atmosphere and Dust Environment Explorer (LADEE) Neutral Mass Spectrometer (NMS), operating in ion mode, provides sensitive detections of ions from the lunar exosphere. By analyzing ion-mode data from the entire mission, utilizing Acceleration, Reconnection, Turbulence, and Electrodynamics of the Moon's Interaction with the Sun (ARTEMIS) plasma and magnetic field measurements to organize NMS data and eliminate background sources, we identify highly significant detections of lunar ions at mass per charge of 2, 4, 12, 20, 28, 39, and 40, moderately significant detections at 14 and 23, and weak detections at 24, 25, and 36. Unlike many previous observations of Moon-derived ions, an outward pointing viewing geometry ensures that these ions originate from the exosphere, rather than directly from the surface. For species with known neutral distributions, inferred ion production rates appear consistent with expectations for both magnitude and spatial distribution, assuming photoionization as the predominant source mechanism. Unexpected signals at mass per charge 12 and 28 suggest the presence of a significant exospheric population of carbon-bearing molecules. C1 [Halekas, J. S.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. [Benna, M.; Mahaffy, P. R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Benna, M.] Univ Maryland, CSST, Baltimore, MD 21201 USA. [Elphic, R. C.; Delory, G. T.] NASA, Ames Res Ctr, Mountain View, CA USA. [Poppe, A. R.; Delory, G. T.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. RP Halekas, JS (reprint author), Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. EM jasper-halekas@uiowa.edu RI Benna, Mehdi/F-3489-2012; OI Poppe, Andrew/0000-0001-8137-8176; Halekas, Jasper/0000-0001-5258-6128 FU LADEE Guest Investigator Program [NNX14AR24G]; SSERVI; NASA LASER [NNX13AJ97G]; NASA [NAS5-02099]; German Ministry for Economy and Technology; German Center for Aviation and Space (DLR) [50 OC 0302] FX We acknowledge support from the LADEE Guest Investigator Program under grant NNX14AR24G and also thank SSERVI for supporting this study. A.R.P. was supported by NASA LASER grant #NNX13AJ97G. We acknowledge NASA contract NAS5-02099 for use of data from ARTEMIS, specifically J.P. McFadden and C.W. Carlson for ESA data and K.H. Glassmeier, U. Auster, and W. Baumjohann for FGM data provided under the lead of the Technical University of Braunschweig and with financial support through the German Ministry for Economy and Technology and the German Center for Aviation and Space (DLR) under contract 50 OC 0302. We acknowledge http://phidrates.space.swri.edu/ Huebner et al. [1992] for photoionization rates. ARTEMIS data are publicly available on NASA's CDAWeb. LADEE data are publicly available through the Planetary Data System. NR 25 TC 8 Z9 8 U1 2 U2 6 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD JUL 16 PY 2015 VL 42 IS 13 BP 5162 EP 5169 DI 10.1002/2015GL064746 PG 8 WC Geosciences, Multidisciplinary SC Geology GA CN8LG UT WOS:000358691300011 ER PT J AU Geng, L Zatko, MC Alexander, B Fudge, TJ Schauer, AJ Murray, LT Mickley, LJ AF Geng, Lei Zatko, Maria C. Alexander, Becky Fudge, T. J. Schauer, Andrew J. Murray, Lee T. Mickley, Loretta J. TI Effects of postdepositional processing on nitrogen isotopes of nitrate in the Greenland Ice Sheet Project 2 ice core SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE ice core; nitrate; nitrogen isotopes; postdepositional processing ID FACTORS CONTROLLING VARIABILITY; ATMOSPHERIC NITRATE; REACTIVE NITROGEN; SNOW; ANTARCTICA; CHEMISTRY; EMISSIONS; CONSTRAINTS; CAPACITY; SULFUR AB Records of ice core nitrate and its isotopes hold the potential to assess past atmospheric conditions regarding NOx and oxidant levels. However, relating such records to past atmospheric conditions requires a site-specific understanding of the postdepositional processing of snow nitrate. We report N-15(NO3-) records from the Greenland Ice Sheet Project 2 (GISP2) ice core over major climate transitions. Model calculations and comparison with records of parameters influencing UV-driven postdepositional processing of snow nitrate suggest that the observed variability in GISP2 N-15(NO3-) over major climate transitions is primarily driven by changes in the degree of postdepositional loss of snow nitrate. Estimates of the fractional loss of snow nitrate is (16-23)% in the Holocene and (45-53)% in the glacial period, suggesting a (4132)% lower nitrate depositional flux to Greenland during the glacial period relative to the Holocene. C1 [Geng, Lei; Zatko, Maria C.; Alexander, Becky] Univ Washington, Dept Atmospher Sci, Seattle, WA 98195 USA. [Fudge, T. J.; Schauer, Andrew J.] Univ Washington, Dept Earth & Space Sci, Seattle, WA 98195 USA. [Murray, Lee T.] NASA Goddard Inst Space Studies, New York, NY USA. [Murray, Lee T.] Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY USA. [Mickley, Loretta J.] Harvard Univ, Sch Engn & Appl Sci, Cambridge, MA 02138 USA. RP Geng, L (reprint author), Univ Washington, Dept Atmospher Sci, Seattle, WA 98195 USA. EM leigeng@uw.edu RI Murray, Lee/F-2296-2014; Alexander, Becky/N-7048-2013 OI Murray, Lee/0000-0002-3447-3952; Alexander, Becky/0000-0001-9915-4621 FU NSF [AGS 1103163, PLR 1106317, PLR 1244817]; [NSF-AGS 1102880] FX DELTA;15N(NO3-) data are available in the supporting information as Data Set S1. We acknowledge financial support from NSF (awards AGS 1103163, PLR 1106317, and PLR 1244817 to B. Alexander). L.J. Mickley and L.T. Murray acknowledge support from NSF-AGS 1102880. We also want to thank the National Ice Core Laboratory for providing the GISP2 ice core samples and the GISP2 team for ice core drilling. NR 38 TC 1 Z9 1 U1 1 U2 14 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD JUL 16 PY 2015 VL 42 IS 13 BP 5346 EP 5354 DI 10.1002/2015GL064218 PG 9 WC Geosciences, Multidisciplinary SC Geology GA CN8LG UT WOS:000358691300033 ER PT J AU Pincus, R Mlawer, EJ Oreopoulos, L Ackerman, AS Baek, S Brath, M Buehler, SA Cady-Pereira, KE Cole, JNS Dufresne, JL Kelley, M Li, JN Manners, J Paynter, DJ Roehrig, R Sekiguchi, M Schwarzkopf, DM AF Pincus, Robert Mlawer, Eli J. Oreopoulos, Lazaros Ackerman, Andrew S. Baek, Sunghye Brath, Manfred Buehler, Stefan A. Cady-Pereira, Karen E. Cole, Jason N. S. Dufresne, Jean-Louis Kelley, Maxwell Li, Jiangnan Manners, James Paynter, David J. Roehrig, Romain Sekiguchi, Miho Schwarzkopf, Daniel M. TI Radiative flux and forcing parameterization error in aerosol-free clear skies SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE Radiation; Parameterization; Radiative forcing ID CLIMATE MODELS; COOLING RATES; ATMOSPHERES; CODES; COMPUTATION; ABSORPTION; CONTINUUM; LBLRTM; CMIP5; CO2 AB This article reports on the accuracy in aerosol- and cloud-free conditions of the radiation parameterizations used in climate models. Accuracy is assessed relative to observationally validated reference models for fluxes under present-day conditions and forcing (flux changes) from quadrupled concentrations of carbon dioxide. Agreement among reference models is typically within 1 W/m(2), while parameterized calculations are roughly half as accurate in the longwave and even less accurate, and more variable, in the shortwave. Absorption of shortwave radiation is underestimated by most parameterizations in the present day and has relatively large errors in forcing. Error in present-day conditions is essentially unrelated to error in forcing calculations. Recent revisions to parameterizations have reduced error in most cases. A dependence on atmospheric conditions, including integrated water vapor, means that global estimates of parameterization error relevant for the radiative forcing of climate change will require much more ambitious calculations. C1 [Pincus, Robert] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA. [Pincus, Robert] NOAA, Phys Sci Div, Earth Syst Res Lab, Boulder, CO USA. [Mlawer, Eli J.; Cady-Pereira, Karen E.] Atmospher & Environm Res, Lexington, MA USA. [Oreopoulos, Lazaros] NASA, Goddard Space Flight Ctr, Earth Sci Div, Greenbelt, MD 20771 USA. [Ackerman, Andrew S.; Kelley, Maxwell] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Baek, Sunghye; Dufresne, Jean-Louis] Univ Paris 06, CNRS, IPSL, LMD, Paris, France. [Baek, Sunghye] Korea Inst Atmospher Predict Syst, Seoul, South Korea. [Brath, Manfred; Buehler, Stefan A.] Univ Hamburg, Inst Meteorol, Hamburg, Germany. [Cole, Jason N. S.; Li, Jiangnan] Environm Canada, Canadian Ctr Climate Modelling & Anal, Victoria, BC, Canada. [Kelley, Maxwell] Trinnovim LLC, New York, NY USA. [Manners, James] Met Off, Exeter, Devon, England. [Paynter, David J.; Schwarzkopf, Daniel M.] NOAA, Geophys Fluid Dynam Lab, Princeton, NJ USA. [Roehrig, Romain] Meteo France, Ctr Natl Rech Meteorol GAME, Toulouse, France. [Roehrig, Romain] CNRS, Toulouse, France. [Sekiguchi, Miho] Tokyo Univ Marine Sci & Technol, Dept Marine Elect & Mech Engn, Tokyo, Japan. RP Pincus, R (reprint author), Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA. EM Robert.Pincus@colorado.edu RI Oreopoulos, Lazaros/E-5868-2012; Pincus, Robert/B-1723-2013; Dufresne, Jean-Louis/I-5616-2015; Buehler, Stefan Alexander/A-4056-2009; Li, Jiangnan/J-6262-2016; OI Oreopoulos, Lazaros/0000-0001-6061-6905; Pincus, Robert/0000-0002-0016-3470; Dufresne, Jean-Louis/0000-0003-4764-9600; Buehler, Stefan Alexander/0000-0001-6389-1160; Cole, Jason/0000-0003-0450-2748 FU US Department of Energy Office of Environmental and Biological Sciences [DE-SC0012549, DE-SC0012399]; NASA; Cluster of Excellence "CliSAP", Universitat Hamburg - German Science Foundation (DFG) [EXC177]; Labex L-IPSL - ANR [ANR-10-LABX-0018]; European FP7 IS-ENES2 project [312979] FX The data on which this paper is based, including atmospheric profiles used in the radiative transfer calculations and the results of the calculations as provided by participants, are included in the supporting information. We are grateful for helpful comments from two anonymous reviewers. This work was financially supported by the Regional and Global Climate Modeling Program of the US Department of Energy Office of Environmental and Biological Sciences (grants DE-SC0012549 to R.P. and DE-SC0012399 to E.J.M.). A.S.A., L.O., and M.K. were supported by the NASA Modeling, Analysis, and Prediction program. S.B. was partially supported through the Cluster of Excellence "CliSAP" (EXC177), Universitat Hamburg, funded through the German Science Foundation (DFG). S.B. and J.L.D. were partially supported by the Labex L-IPSL which is funded by the ANR (grant ANR-10-LABX-0018) and by the European FP7 IS-ENES2 project (grant 312979). NR 38 TC 7 Z9 7 U1 3 U2 22 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD JUL 16 PY 2015 VL 42 IS 13 BP 5485 EP 5492 DI 10.1002/2015GL064291 PG 8 WC Geosciences, Multidisciplinary SC Geology GA CN8LG UT WOS:000358691300050 ER PT J AU Lavers, DA Ralph, FM Waliser, DE Gershunov, A Dettinger, MD AF Lavers, David A. Ralph, F. Martin Waliser, Duane E. Gershunov, Alexander Dettinger, Michael D. TI Climate change intensification of horizontal water vapor transport in CMIP5 SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE water vapor transport; CMIP5; climate change ID ATMOSPHERIC RIVERS; PRECIPITATION EXTREMES; MULTIMODEL ASSESSMENT; PACIFIC-OCEAN; WEST-COAST; CALIFORNIA; MODELS; PROJECTIONS; ENSEMBLE; IMPACTS AB Global warming of the Earth's atmosphere is hypothesized to lead to an intensification of the global water cycle. To determine associated hydrological changes, most previous research has used precipitation. This study, however, investigates projected changes to global atmospheric water vapor transport (integrated vapor transport (IVT)), the key link between water source and sink regions. Using 22 global circulation models from the Climate Model Intercomparison Project Phase 5, we evaluate, globally, the mean, standard deviation, and the 95th percentiles of IVT from the historical simulations (1979-2005) and two emissions scenarios (2073-2099). Considering the more extreme emissions, multimodel mean IVT increases by 30-40% in the North Pacific and North Atlantic storm tracks and in the equatorial Pacific Ocean trade winds. An acceleration of the high-latitude IVT is also shown. Analysis of low-altitude moisture and winds suggests that these changes are mainly due to higher atmospheric water vapor content. C1 [Lavers, David A.; Ralph, F. Martin; Waliser, Duane E.; Gershunov, Alexander; Dettinger, Michael D.] Univ Calif San Diego, Scripps Inst Oceanog, Ctr Western Weather & Water Extremes, La Jolla, CA 92093 USA. [Waliser, Duane E.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Gershunov, Alexander] Univ Calif San Diego, Scripps Inst Oceanog, CASPO, La Jolla, CA 92093 USA. [Dettinger, Michael D.] US Geol Survey, Scripps Inst Oceanog, La Jolla, CA USA. RP Lavers, DA (reprint author), Univ Calif San Diego, Scripps Inst Oceanog, Ctr Western Weather & Water Extremes, La Jolla, CA 92093 USA. EM dlavers@ucsd.edu OI Dettinger, Michael/0000-0002-7509-7332 FU California Department of Water Resources; NASA FX We thank Mary Tyree for retrieving the CMIP5 data and California Department of Water Resources for their financial support. D.W.'s contribution was carried out on behalf of the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. Comments from Jonathan Rutz helped improve the manuscript. NR 34 TC 12 Z9 12 U1 4 U2 22 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD JUL 16 PY 2015 VL 42 IS 13 BP 5617 EP 5625 DI 10.1002/2015GL064672 PG 9 WC Geosciences, Multidisciplinary SC Geology GA CN8LG UT WOS:000358691300067 ER PT J AU Fuchs, BR Rutledge, SA Bruning, EC Pierce, JR Kodros, JK Lang, TJ MacGorman, DR Krehbiel, PR Rison, W AF Fuchs, Brody R. Rutledge, Steven A. Bruning, Eric C. Pierce, Jeffrey R. Kodros, John K. Lang, Timothy J. MacGorman, Donald R. Krehbiel, Paul R. Rison, William TI Environmental controls on storm intensity and charge structure in multiple regions of the continental United States SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE lightning; cloud processes; thermodynamics; aerosols; charge structure ID GROUND LIGHTNING POLARITY; SECONDARY ICE PARTICLES; SEVERE THUNDERSTORM ELECTRIFICATION; MIXED-PHASE MICROPHYSICS; VERTICAL VELOCITY; PRECIPITATION; RADAR; AEROSOL; DISTRIBUTIONS; SUPERCELL AB A database consisting of approximately 4000 storm observations has been objectively analyzed to determine environmental characteristics that produce high radar reflectivities above the freezing level, large total lightning flash rates on the order of 10 flashes per minute, and anomalous vertical charge structures (most notably, dominant midlevel positive charge). The storm database is drawn from four regions of the United States featuring distinct environments, each with coinciding Lightning Mapping Array (LMA) network data. LMAs are able to infer total lightning flash rates using flash clustering algorithms, such as the one implemented in this study. Results show that anomalous charge structures inferred from LMA data, significant lightning flash rates, and increased radar reflectivities above the freezing level tend to be associated with environments that have high cloud base heights (approximately 3km above ground level) and large atmospheric instability, quantified by normalized convective available potential energy (NCAPE) near 0.2ms(-2). Additionally, we infer that aerosols may affect storm intensity. Maximum flash rates were observed in storms with attributed aerosol concentrations near 1000cm(-3), while total flash rates decrease when aerosol concentrations exceed 1500cm(-3), consistent with previous studies. However, this effect is more pronounced in regions where the NCAPE and cloud base height are low. The dearth of storms with estimated aerosol concentrations less than 700cm(-3) (approximately 1% of total sample) does not provide a complete depiction of aerosol invigoration. C1 [Fuchs, Brody R.; Rutledge, Steven A.; Pierce, Jeffrey R.; Kodros, John K.] Colorado State Univ, Dept Atmospher Sci, Ft Collins, CO 80523 USA. [Bruning, Eric C.] Texas Tech Univ, Dept Geosci, Lubbock, TX 79409 USA. [Lang, Timothy J.] NASA Marshall Space Flight Ctr, Huntsville, AL USA. [MacGorman, Donald R.] Natl Severe Storms Lab, Norman, OK 73069 USA. [Krehbiel, Paul R.; Rison, William] New Mexico Inst Min & Technol, Langmuir Lab Atmospher Res, Geophys Res Ctr, Socorro, NM 87801 USA. RP Fuchs, BR (reprint author), Colorado State Univ, Dept Atmospher Sci, Ft Collins, CO 80523 USA. EM brfuchs@atmos.colostate.edu RI Pierce, Jeffrey/E-4681-2013; OI Pierce, Jeffrey/0000-0002-4241-838X; MacGorman, Donald/0000-0002-2395-8196; Fuchs, Brody/0000-0002-7629-0687 FU NSF [AGS1010657] FX The authors wish to thank Doug Stolz and Brett Basarab at CSU for the discussions related to this work. General technical help from Paul Hein was crucial to the completion of this study. The authors would also like to thank the three anonymous reviewers for their suggestions and comments that improved the paper. Information about NMQ mosaic radar data can be found at http://www.nssl.noaa.gov/projects/q2/. A portion of the LMA data was provided by Rich Blakeslee. The LMA networks and data are maintained at New Mexico Tech. For more information about the flash clustering algorithm visit https://github.com/deeplycloudy/lmatools. NLDN data were provided via subscription by Vaisala Inc. (http://www.vaisala.com/en/pages/default.aspx). Environmental analysis data were provided by the National Climatic Data Center (NCDC). Supplemental environmental data were provided by Dan Lindsey. Inquiries or supplemental information about the data used in this study should be directed to the corresponding author (brfuchs@atmos.colostate.edu). Funding for this study was provided by NSF grant AGS1010657. NR 119 TC 9 Z9 9 U1 1 U2 14 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD JUL 16 PY 2015 VL 120 IS 13 BP 6575 EP 6596 DI 10.1002/2015JD023271 PG 22 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA CN8MN UT WOS:000358695200017 ER PT J AU Sutanto, SJ Hoffmann, G Worden, J Scheepmaker, RA Aben, I Rockmann, T AF Sutanto, S. J. Hoffmann, G. Worden, J. Scheepmaker, R. A. Aben, I. Rockmann, T. TI Atmospheric processes governing the changes in water isotopologues during ENSO events from model and satellite measurements SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE water isotopologues; ENSO; satellite; model ID SCIAMACHY HDO/H2O MEASUREMENTS; GENERAL-CIRCULATION MODEL; NINO SOUTHERN-OSCILLATION; TRMM PRECIPITATION RADAR; STABLE-ISOTOPES; EL-NINO; SURFACE TEMPERATURES; RAIN EVAPORATION; DIURNAL CYCLE; VAPOR AB ENSO (El Nino-Southern Oscillation) has profound effects on the global water cycle, which can be examined at the process level by investigating the associated water isotopologues. Many isotope-based studies are aimed at understanding ENSO variability in the tropics, however, focusing principally on near-surface processes and isotopologue signals. The goal of the present study is to investigate the atmospheric processes governing the changes in the isotopic composition of water vapor both near the surface and at midtroposphere in the Pacific region during ENSO events, using a combination of remote sensing data and model simulations. For the lower atmosphere (i.e., 1000hPa), our results show that rainout processes, less rain reevaporation of falling droplets, and increase of convective updrafts and diffusive exchange within the convective systems contribute to the isotope amount effect and isotopically deplete the water vapor during wet conditions, in agreement with previous studies. However, we find that the ENSO-associated isotopic signal in the midtroposphere (i.e., 500hPa) diverges from the near-surface response. Analysis suggests that transport of enriched water vapor from lower atmospheric layers through convective updrafts controls the enrichment of midtropospheric water vapor over the Pacific Ocean. In the observations, a strong positive correlation between the increase of convective precipitation and the isotopic composition of water vapor clearly points to such a mechanism (R of 0.7-0.8 in the Central Pacific and 0.5-0.6 in the West Pacific). Model results confirm this mechanisms though producing slightly lower correlation values, with R values of 0.6 in the Central Pacific and 0.5 in the West Pacific. However, the distinction between convective and stratiform precipitation remains a result of model-dependent parameterization. Our analysis suggests that two issues should be investigated in more detail in further studies: (1) the equilibrium and disequilibrium between rain droplets and surrounding vapor for convective and stratiform precipitation and (2) different convection schemes in the different isotopic general circulation models (GCMs) describing the triggering of convection and uplift of lower layer air to higher layers. Ideally, such a comparison of different isotopic GCMs can provide us with an interesting benchmark test for the performance of the different convection schemes during ENSO and can help to disentangle the importance of the different processes contributing to the amount effect. C1 [Sutanto, S. J.; Hoffmann, G.; Rockmann, T.] Univ Utrecht, Inst Marine & Atmosphere Res Utrecht, Utrecht, Netherlands. [Sutanto, S. J.] Res Ctr Water Resources, Bandung, Indonesia. [Hoffmann, G.] LCSE Orme, Lab Sci Climat & Environm, Gif Sur Yvette, France. [Worden, J.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Scheepmaker, R. A.; Aben, I.] SRON Netherlands Inst Space Res, Utrecht, Netherlands. RP Sutanto, SJ (reprint author), Univ Utrecht, Inst Marine & Atmosphere Res Utrecht, Utrecht, Netherlands. EM S.J.Sutanto@uu.nl RI Rockmann, Thomas/F-4479-2015; OI Rockmann, Thomas/0000-0002-6688-8968; Sutanto, Samuel Jonson/0000-0003-4903-6445 FU NWO (The Netherlands Organization for Scientific Research) [ALW-GO-AO/10-11]; Netherlands Space Office as part of the User Support Program Space Research [GO-AO/16] FX This study was funded by NWO (The Netherlands Organization for Scientific Research) project number ALW-GO-AO/10-11. R.A. Scheepmaker acknowledges funding from the Netherlands Space Office as part of the User Support Program Space Research under project GO-AO/16. The TES and SCIAMACHY satellite data were obtained from the NASA Jet Propulsion Laboratory (JPL) and SRON Netherlands Institute for Space Research, respectively. The ECHAM4 data were downloaded from the SWING2 database, National Aeronautics and Space Administration (NASA) Goddard Institute for Space Studies. The TRMM and ECMWF precipitation data were obtained from the NASA Goddard Earth Sciences Data and Information Service Center and the ECMWF data center, respectively. The GNIP data were downloaded from Water Isotope System for Data Analysis, Visualization, and Electronic Retrieval (WISER), International Atomic Energy Agency (IAEA). All data used in the study can be obtained from the authors (S.J.Sutanto@uu.nl). NR 74 TC 4 Z9 4 U1 4 U2 20 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD JUL 16 PY 2015 VL 120 IS 13 BP 6712 EP 6729 DI 10.1002/2015JD023228 PG 18 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA CN8MN UT WOS:000358695200025 ER PT J AU Hornbuckle, BC Yu, XX Noebe, RD Martens, R Weaver, ML Thompson, GB AF Hornbuckle, B. Chad Yu, Xiao X. Noebe, Ronald D. Martens, Richard Weaver, Mark L. Thompson, Gregory B. TI Hardening behavior and phase decomposition in very Ni-rich Nitinol alloys SO MATERIALS SCIENCE AND ENGINEERING A-STRUCTURAL MATERIALS PROPERTIES MICROSTRUCTURE AND PROCESSING LA English DT Article DE Nitinol; Precipitation strengthening; Phase stability; Microstructural characterization ID SHAPE-MEMORY ALLOYS; MARTENSITIC-TRANSFORMATION; ELECTRON-MICROSCOPY AB A series of Ni-rich Nitinol compositions spanning from 53NiTi to 58NiTi (at%) have been solutionized at 1050 degrees C and aged at 400 degrees C, 625 degrees C, and 750 degrees C for varying times to determine the correlation between microstructure and hardenability. Compositions of 55NiT, 56NiTi, and 57NiTi displayed peak hardness values near 650 VHN upon quenching, which are on par with tool steels. Upon aging at 400 degrees C, all but the 55NiTi and 56NiTi compositions exhibited a decrease in hardness initiating, between 1 and 10 h for the lower Ni alloys and after 100 h for the highest Ni containing alloys. The high hardness, including the solution treated condition, was attributed to the precipitation of a large volume fraction of nanoscale Ni4Ti3 platelets that resulted in narrow B2 NiTi matrix channels. These channels provided a microstructure-driven strengthening morphology. Upon increasing Ni content to greater than 56NiTi and increasing the aging time and temperature, the Ni4Ti3 phase decomposed to either Ni3Ti2 and/or Ni3Ti with a subsequent loss in hardness. The decomposition morphology between the precipitates was characterized by serial sectioning showing that Ni4Ti3 platelets acted as a heterogeneous nucleation site and subsequent Ni-reservoir during the growth of globular Ni3Ti precipitates. (C) 2015 Elsevier B.V. All rights reserved. C1 [Hornbuckle, B. Chad; Yu, Xiao X.; Weaver, Mark L.; Thompson, Gregory B.] Univ Alabama, Dept Met & Mat Engn, Tuscaloosa, AL 35487 USA. [Noebe, Ronald D.] NASA, Glenn Res Ctr, Mat & Struct Div, Cleveland, OH 44135 USA. [Martens, Richard] Univ Alabama, Cent Analyt Facil, Tuscaloosa, AL 35487 USA. RP Thompson, GB (reprint author), Univ Alabama, Dept Met & Mat Engn, Tuscaloosa, AL 35487 USA. EM gthompson@eng.ua.edu FU NASA [NNX09AO61A]; NASA Transformative Aeronautics Concepts Program, Transformation Tools & Technologies Project (Dale Hopkins, Technical Lead for Structure & Materials Discipline) FX The authors gratefully acknowledge funding for this research under NASA Grant NNX09AO61A and from the NASA Transformative Aeronautics Concepts Program, Transformation Tools & Technologies Project (Dale Hopkins, Technical Lead for Structure & Materials Discipline). UA's Central Analytical Facility (www.caf.ua.edu) is recognized for additional support and access to the microscopes used in this study. Lastly, the authors thank Katherine Vinson and Thomas Burton for their assistance in post processing of the EBSD and 3D serial sectioning reconstructions, respectively. NR 31 TC 2 Z9 2 U1 5 U2 13 PU ELSEVIER SCIENCE SA PI LAUSANNE PA PO BOX 564, 1001 LAUSANNE, SWITZERLAND SN 0921-5093 EI 1873-4936 J9 MAT SCI ENG A-STRUCT JI Mater. Sci. Eng. A-Struct. Mater. Prop. Microstruct. Process. PD JUL 15 PY 2015 VL 639 BP 336 EP 344 DI 10.1016/j.msea.2015.04.079 PG 9 WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary; Metallurgy & Metallurgical Engineering SC Science & Technology - Other Topics; Materials Science; Metallurgy & Metallurgical Engineering GA CM2YV UT WOS:000357549200044 ER PT J AU Hayne, PO Hendrix, A Sefton-Nash, E Siegler, MA Lucey, PG Retherford, KD Williams, JP Greenhagen, BT Paige, DA AF Hayne, Paul O. Hendrix, Amanda Sefton-Nash, Elliot Siegler, Matthew A. Lucey, Paul G. Retherford, Kurt D. Williams, Jean-Pierre Greenhagen, Benjamin T. Paige, David A. TI Evidence for exposed water ice in the Moon's south polar regions from Lunar Reconnaissance Orbiter ultraviolet albedo and temperature measurements SO ICARUS LA English DT Article DE Moon; Ices; Ices, UV spectroscopy; Moon, surface ID BIDIRECTIONAL REFLECTANCE SPECTROSCOPY; SHACKLETON CRATER; RADIOMETER OBSERVATIONS; LCROSS IMPACT; RADAR; DEPOSITS; SURFACE; POLES; ASTEROIDS; MERCURY AB We utilize surface temperature measurements and ultraviolet albedo spectra from the Lunar Reconnaissance Orbiter to test the hypothesis that exposed water frost exists within the Moon's shadowed polar craters, and that temperature controls its concentration and spatial distribution. For locations with annual maximum temperatures T-max, greater than the H2O sublimation temperature of similar to 110 K, we find no evidence for exposed water frost, based on the LAMP UV spectra. However, we observe a strong change in spectral behavior at locations perennially below similar to 110 K, consistent with cold-trapped ice on the surface. In addition to the temperature association, spectral evidence for water frost comes from the following spectral features: (a) decreasing Lyman-alpha. albedo, (b) decreasing "on-band" (129.57-155.57 nm) albedo, and (c) increasing "off-band" (155.57-189.57 nm) albedo. All of these features are consistent with the UV spectrum of water ice, and are expected for water ice layers >similar to 100 nm in thickness. High regolith porosity, which would darken the surface at all wavelengths, cannot alone explain the observed spectral changes at low temperatures. Given the observed LAMP off-band/on-band albedo ratios at a spatial scale of 250 m, the range of water ice concentrations within the cold traps with T-max < 110 K is similar to 0.1-2.0% by mass, if the ice is intimately mixed with dry regolith. If pure water ice is exposed instead, then up to similar to 10% of the surface area on the 250-m scale of the measurements may be ice-covered. The observed distribution of exposed water ice is highly heterogeneous, with some cold traps <110 K having little to no apparent water frost, and others with a significant amount of water frost. As noted by Gladstone et al. (Gladstone, G.R. et al. [2012]. J. Geophys. Res.: Planets 117(E12)), this heterogeneity may be a consequence of the fact that the net supply rate of H2O molecules to the lunar poles is very similar to the net destruction rate within the cold traps. However, an observed increase in apparent H2O abundance with decreasing temperature from similar to 110 K to 65 K suggests that destruction of surface frosts by impact gardening and space weathering is spatially heterogeneous. We find a loosely bimodal distribution of apparent ice concentrations with temperature, possibly due to competition between vertical mixing by impact gardening and resupply of H2O by vapor diffusion at sites -110 K. Finally, we cannot rule out the possibility that the colder population of ice deposits is in fact primarily carbon dioxide ice, although peak temperatures of similar to 65 K are slightly higher than the usual CO2 sublimation temperature of similar to 60 K. (c) 2015 Elsevier Inc. All rights reserved. C1 [Hayne, Paul O.; Siegler, Matthew A.; Greenhagen, Benjamin T.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Hendrix, Amanda] Planetary Sci Inst, Pasadena, CA 91106 USA. [Sefton-Nash, Elliot; Williams, Jean-Pierre; Paige, David A.] Univ Calif Los Angeles, Los Angeles, CA 90095 USA. [Lucey, Paul G.] Univ Hawaii, Honolulu, HI 96822 USA. [Retherford, Kurt D.] SW Res Inst, Boulder, CO 80302 USA. RP Hayne, PO (reprint author), CALTECH, Jet Prop Lab, MS 183-301,4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Paul.O.Hayne@jpl.nasa.gov RI Williams, Jean-Pierre/C-3531-2009; Greenhagen, Benjamin/C-3760-2016 OI Williams, Jean-Pierre/0000-0003-4163-2760; NR 49 TC 11 Z9 12 U1 6 U2 21 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD JUL 15 PY 2015 VL 255 SI SI BP 58 EP 69 DI 10.1016/j.icarus.2015.03.032 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CJ6YJ UT WOS:000355640800008 ER PT J AU Tye, AR Fassett, CI Head, JW Mazarico, E Basilevsky, AT Neumann, GA Smith, DE Zuber, MT AF Tye, A. R. Fassett, C. I. Head, J. W. Mazarico, E. Basilevsky, A. T. Neumann, G. A. Smith, D. E. Zuber, M. T. TI The age of lunar south circumpolar craters Haworth, Shoemaker, Faustini, and Shackleton: Implications for regional geology, surface processes, and volatile sequestration SO ICARUS LA English DT Article DE Ices; Moon, surface; Cratering; Geological processes; Regoliths ID POLE; ICE; DEGRADATION; DEPOSITS; EROSION AB The interiors of the lunar south circumpolar craters Haworth, Shoemaker, Faustini, and Shackleton contain permanently shadowed regions (PSRs) and have been interpreted to contain sequestered volatiles including water ice. Altimetry data from the Lunar Orbiter Laser Altimeter (LOLA) onboard the Lunar Reconnaissance Orbiter provide a new means of examining the permanently shadowed interiors of these craters in unprecedented detail. In this study, we used extremely high-resolution gridded LOLA data of Haworth, Shoemaker, Faustini, and Shackleton to determine the size-frequency distributions and the spatial density of craters superposing their rims, inner slopes, and floors. Based on their population of superposed D >= 2 km craters, Haworth, Shoemaker, and Faustini have pre-Nectarian formation ages. Shackleton is interpreted as having a Late Imbrian age on the basis of craters with diameter D >= 0.5 km superposed on its rim. The local density of craters with sub-km diameters across our study area is strongly dependent on slope; because of its steep interior slopes, the lifetime of craters on the interior of Shackleton is limited. The slope-dependence of the small crater population implies that the population in this size range is controlled primarily by the rate at which craters are destroyed. This is consistent with the hypothesis that crater removal and resurfacing is a result of slope-dependent processes such as diffusive mass wasting and seismic shaking, linked to micrometeorite and meteorite bombardment. Epithermal neutron flux data and UV albedo data show that these circumpolar PSRs, particularly Shoemaker, may have similar to 1-2% water ice by mass in their highly porous surface regolith, and that Shoemaker may have similar to 5% or more water ice by mass in the near subsurface. The ancient formation ages of Shoemaker, Faustini and Haworth, and the Late Imbrian (similar to 3.5 Ga) crater retention ages of their floors suggests that any water ice that might have been deposited in their permanently shadowed areas was insufficient to modify the superposed crater population since that time. (c) 2015 Elsevier Inc. All rights reserved. C1 [Tye, A. R.; Head, J. W.] Brown Univ, Dept Earth Environm & Planetary Sci, Providence, RI 02912 USA. [Tye, A. R.] Univ Michigan, Dept Earth & Environm Sci, Ann Arbor, MI 48109 USA. [Fassett, C. I.] Mt Holyoke Coll, Dept Astron, S Hadley, MA 01075 USA. [Mazarico, E.; Neumann, G. A.; Smith, D. E.] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA. [Basilevsky, A. T.] Russian Acad Sci, Vernadsky Inst Geochem & Analyt Chem, Moscow 119991, Russia. [Smith, D. E.; Zuber, M. T.] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA. RP Head, JW (reprint author), Brown Univ, Dept Earth Environm & Planetary Sci, Providence, RI 02912 USA. RI Mazarico, Erwan/N-6034-2014; Neumann, Gregory/I-5591-2013 OI Mazarico, Erwan/0000-0003-3456-427X; Neumann, Gregory/0000-0003-0644-9944 FU NASA Lunar Reconnaissance Orbiter (LRO) Mission, Lunar Orbiter Laser Altimeter (LOLA) Experiment Team [NNX11AK29G, NNX13AO77G]; NASA Solar System Exploration Research Virtual Institute (SSERVI) grant for Evolution and Environment of Exploration Destinations at Brown University [NNA14AB01A] FX We gratefully acknowledge financial support from the NASA Lunar Reconnaissance Orbiter (LRO) Mission, Lunar Orbiter Laser Altimeter (LOLA) Experiment Team (Grants NNX11AK29G and NNX13AO77G), and the NASA Solar System Exploration Research Virtual Institute (SSERVI) grant for Evolution and Environment of Exploration Destinations under cooperative Agreement No. NNA14AB01A at Brown University. NR 24 TC 4 Z9 4 U1 0 U2 5 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD JUL 15 PY 2015 VL 255 SI SI BP 70 EP 77 DI 10.1016/j.icarus.2015.03.016 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CJ6YJ UT WOS:000355640800009 ER PT J AU Siegler, M Paige, D Williams, JP Bills, B AF Siegler, Matt Paige, David Williams, Jean-Pierre Bills, Bruce TI Evolution of lunar polar ice stability SO ICARUS LA English DT Article DE Moon, surface; Ices; Regoliths; Planetary dynamics ID EARTH-MOON SYSTEM; SOUTH-POLE; WATER ICE; SHACKLETON CRATER; SPIN AXIS; SURFACE; VOLATILES; MERCURY; DEPOSITS; DRIVEN AB The polar regions of the Moon and Mercury both have permanently shadowed environments, potentially capable of harboring ice (cold traps). While cold traps are likely to have been stable for nearly 4 Gyr on Mercury, this has not been the case for the Moon. Roughly 3 +/- 1 Gya, when the Moon is believed to have resided at approximately half of its current semimajor axis, lunar obliquities have been calculated to have reached as high as 77 degrees. At this time, lunar polar temperatures were much warmer and cold traps did not exist. Since that era, lunar obliquity has secularly decreased, creating environments over approximately the last 1-2 Gyr where ice could be stable (assuming near current recession rates). We argue that the paucity of ice in the present lunar cold traps is evidence that no cometary impact has occurred in the past billion years that is similar to the one(s) which are thought to have delivered volatiles to Mercury's poles. However, the present ice distribution may be compatible with a cometary impact if it occurred not in today's lunar thermal environment, but in a past one. If ice were delivered during a past epoch, the distribution of ground ice would be dictated not by present day temperatures, but rather by these ancient, warmer, temperatures. In this paper, we attempt to recreate the thermal environments for past lunar orbital configurations to characterize the history of lunar environments capable of harboring ice. We will develop models of ice stability and mobility to examine likely fossil remains of past ice delivery (e.g. a comet impact) that could be observed on the present Moon. We attempt to quantify when in the Moon's outward evolution areas first became stable for ice deposition and when ice mobility would have ceased. (c) 2014 Elsevier Inc. All rights reserved. C1 [Siegler, Matt; Bills, Bruce] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Paige, David; Williams, Jean-Pierre] Univ Calif Los Angeles, Los Angeles, CA 90095 USA. RP Siegler, M (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. RI Williams, Jean-Pierre/C-3531-2009 OI Williams, Jean-Pierre/0000-0003-4163-2760 FU Diviner Lunar Radiometer; Jet Propulsion Laboratory Early Career Fellowship FX Thank you to the Diviner Lunar Radiometer and the Jet Propulsion Laboratory Early Career Fellowship for partial funding of this work. Thanks to Dr. Norbert Schorghofer for help digesting his collection of papers on this topic over the course of several years. The research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. (c) 2014. All rights reserved. NR 51 TC 7 Z9 7 U1 2 U2 12 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD JUL 15 PY 2015 VL 255 SI SI BP 78 EP 87 DI 10.1016/j.icarus.2014.09.037 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CJ6YJ UT WOS:000355640800010 ER PT J AU McClanahan, TP Mitrofanov, IG Boynton, WV Chin, G Bodnarik, J Droege, G Evans, LG Golovin, D Hamara, D Harshman, K Litvak, M Livengood, TA Malakhov, A Mazarico, E Milikh, G Nandikotkur, G Parsons, A Sagdeev, R Sanin, A Starr, RD Su, JJ Murray, J AF McClanahan, T. P. Mitrofanov, I. G. Boynton, W. V. Chin, G. Bodnarik, J. Droege, G. Evans, L. G. Golovin, D. Hamara, D. Harshman, K. Litvak, M. Livengood, T. A. Malakhov, A. Mazarico, E. Milikh, G. Nandikotkur, G. Parsons, A. Sagdeev, R. Sanin, A. Starr, R. D. Su, J. J. Murray, J. TI Evidence for the sequestration of hydrogen-bearing volatiles towards the Moon's southern pole-facing slopes SO ICARUS LA English DT Article DE Moon; Ices; Moon, surface; Regoliths ID LUNAR RECONNAISSANCE ORBITER; NEUTRON DETECTOR; EXPERIMENT LEND; SOLAR-WIND; COLD TRAPS; WATER ICE; SURFACE; PROSPECTOR; MISSION; CHANDRAYAAN-1 AB The Lunar Exploration Neutron Detector (LEND) onboard the Lunar Reconnaissance Orbiter (LRO) detects a widespread suppression of the epithermal neutron leakage flux that is coincident with the pole-facing slopes (PFS) of the Moon's southern hemisphere. Suppression of the epithermal neutron flux is consistent with an interpretation of enhanced concentrations of hydrogen-bearing volatiles within the upper meter of the regolith. Localized flux suppression in PFS suggests that the reduced solar irradiation and lowered temperature on PFS constrains volatility to a greater extent than in surrounding regions. Epithermal neutron flux mapped with LEND's Collimated Sensor for Epithermal Neutrons (CSETN) was analyzed as a function of slope geomorphology derived from the Lunar Orbiting Laser Altimeter (LOLA) and the results compared to co-registered maps of diurnally averaged temperature from the Diviner Lunar Radiometer Experiment and an averaged illumination map derived from LOLA. The suppression in the average south polar epithermal neutron flux on equator-facing slopes (EFS) and PFS (85-90 degrees S) is 3.3 +/- 0.04% and 4.3 +/- 0.05% respectively (one-sigma-uncertainties), relative to the average count-rate in the latitude band 45-90 degrees S. The discrepancy of 1.0 +/- 0.06% between EFS and PFS neutron flux corresponds to an average of similar to 23 parts-per-million-by-weight (ppmw) more hydrogen on PFS than on EFS. Results show that the detection of hydrogen concentrations on PFS is dependent on their spatial scale. Epithermal flux suppression on large scale PFS was found to be enhanced to 5.2 +/- 0.13%, a discrepancy of similar to 45 ppmw hydrogen relative to equivalent EFS. Enhanced poleward hydration of PFS begins between 50 degrees S and 60 degrees S latitude. Polar regolith temperature contrasts do not explain the suppression of epithermal neutrons on pole-facing slopes. The Supplemental on-line materials include supporting results derived from the uncollimated Lunar Prospector Neutron Spectrometer and the LEND Sensor for Epithermal Neutrons. Published by Elsevier Inc. C1 [McClanahan, T. P.; Chin, G.; Evans, L. G.; Livengood, T. A.; Mazarico, E.; Parsons, A.; Starr, R. D.] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA. [Boynton, W. V.; Bodnarik, J.; Droege, G.; Hamara, D.; Harshman, K.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85719 USA. [Mitrofanov, I. G.; Golovin, D.; Litvak, M.; Malakhov, A.; Sanin, A.] RAS, Inst Space Res, Moscow 117997, Russia. [Livengood, T. A.; Milikh, G.; Sagdeev, R.; Su, J. J.; Murray, J.] Univ Maryland, College Pk, MD 20742 USA. [Evans, L. G.] Comp Sci Corp, Lanham, MD 20706 USA. [Starr, R. D.] Catholic Univ Amer, Washington, DC 20064 USA. [Nandikotkur, G.] Fairleigh Dickinson Univ, Sch Nat Sci, Teaneck, NJ 07666 USA. RP McClanahan, TP (reprint author), NASA, Goddard Space Flight Ctr, Bldg 34,Rm W218,Code 691, Greenbelt, MD 20771 USA. EM timothy.p.mcclanahan@nasa.gov RI Mazarico, Erwan/N-6034-2014 OI Mazarico, Erwan/0000-0003-3456-427X FU Russian Scientific Foundation [14-22-00249] FX We lastly thank the Lunar Reconnaissance Orbiter (LRO) project 879 for their ongoing contributions to Lunar science and the NASA 880 Planetary Data System (PDS) for their continued maintenance of 881 these critically essential archives. We also acknowledge Jay Freidlander at the Goddard Space Flight Center for his work on this 882 paper's figures and graphics. Contributions from the Russian co-authors of his paper were supported by grant No. 14-22-00249 of the Russian Scientific Foundation. NR 65 TC 6 Z9 7 U1 0 U2 10 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD JUL 15 PY 2015 VL 255 SI SI BP 88 EP 99 DI 10.1016/j.icarus.2014.10.001 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CJ6YJ UT WOS:000355640800011 ER PT J AU Livengood, TA Chin, G Sagdeev, RZ Mitrofanov, IG Boynton, WV Evans, LG Litvak, ML McClanahan, TP Sanin, AB Starr, RD Su, JJ AF Livengood, T. A. Chin, G. Sagdeev, R. Z. Mitrofanov, I. G. Boynton, W. V. Evans, L. G. Litvak, M. L. McClanahan, T. P. Sanin, A. B. Starr, R. D. Su, J. J. TI Moonshine: Diurnally varying hydration through natural distillation on the Moon, detected by the Lunar Exploration Neutron Detector (LEND) SO ICARUS LA English DT Article DE Ices; Moon, surface; Regoliths; Terrestrial planets ID RECONNAISSANCE ORBITER; SOLAR-WIND; WATER; ATMOSPHERE; PROSPECTOR; HYDROXYL; CHANDRAYAAN-1; SPECTROMETER; VARIABILITY; MIGRATION AB The Lunar Exploration Neutron Detector (LEND), on the polar-orbiting Lunar Reconnaissance Orbiter (LRO) spacecraft, has detected suppression in the Moon's naturally-occurring epithermal neutron leakage flux that is consistent with the presence of diurnally varying quantities of hydrogen in the regolith near the equator. Peak hydrogen concentration (neutron flux suppression) is on the dayside of the dawn terminator and diminishes through the dawn-to-noon sector. The minimum concentration of hydrogen is in the late afternoon and dusk sector. The chemical form of hydrogen is not determinable from these measurements, but other remote sensing methods and anticipated elemental availability suggest water molecules or hydroxyl ions. Signal-to-noise ratio at maximum contrast is 5.6 sigma in each of two detector systems. Volatiles are deduced to collect in or on the cold nightside surface and distill out of the regolith after dawn as rotation exposes the surface to sunlight. Liberated volatiles migrate away from the warm subsolar region toward the nearby cold nightside surface beyond the terminator, resulting in maximum concentration at the dawn terminator. The peak concentration within the upper similar to 1 m of regolith is estimated to be 0.0125 +/- 0.0022 weight-percent water-equivalent hydrogen (wt% WEH) at dawn, yielding an accumulation of 190 +/- 30 ml recoverable water per square meter of regolith at each dawn. Volatile transport over the lunar surface in opposition to the Moon's rotation exposes molecules to solar ultraviolet radiation. The short lifetime against photolysis and permanent loss of hydrogen from the Moon requires a resupply rate that greatly exceeds anticipated delivery of hydrogen by solar wind implantation or by meteoroid impacts, suggesting that the surface inventory must be continually resupplied by release from a deep volatile inventory in the Moon. The natural distillation of water from the regolith by sunlight and its capture on the cold night surface may provide energy-efficient access to volatiles for in situ resource utilization (ISRU) by direct capture before volatiles can enter the surface, eliminating the need to actively mine regolith for volatile resource recovery. (c) 2015 The Authors. Published by Elsevier Inc. C1 [Livengood, T. A.] Univ Maryland, NASA, Goddard Space Flight Ctr, CRESST,Planetary Syst Lab, Greenbelt, MD 20771 USA. [Chin, G.] NASA, Goddard Space Flight Ctr, Planetaly Syst Lab, Greenbelt, MD 20771 USA. [Sagdeev, R. Z.; Su, J. J.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA. [Mitrofanov, I. G.; Litvak, M. L.; Sanin, A. B.] Russian Acad Sci, Inst Space Res, Moscow V71, Russia. [Boynton, W. V.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Evans, L. G.] Comp Sci Corp, Lanham, MD 20706 USA. [McClanahan, T. P.] NASA, Goddard Space Flight Ctr, Astrochem Lab, Greenbelt, MD 20771 USA. [Starr, R. D.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA. RP Livengood, TA (reprint author), NASA, Goddard Space Flight Ctr, Code 693, Greenbelt, MD 20771 USA. EM timothy.a.livengood@nasa.gov FU National Aeronautics and Space Administration Lunar Reconnaissance Orbiter mission; Russian Scientific Foundation [14-22-00249]; NASA's Lunar Reconnaissance Orbiter project under NASA [NNG06EO90A]; NASA; University of Maryland; Catholic University of America FX Data for the work presented here are archived with the Geosciences Node of the Planetary Data System at http://www-pds.wustl.edu. This work was supported by the National Aeronautics and Space Administration Lunar Reconnaissance Orbiter mission; the Russian co-authors of this paper (IGM, MLL, ABS) were supported by grant No. 14-22-00249 of the Russian Scientific Foundation. TAL was supported by NASA's Lunar Reconnaissance Orbiter project under NASA award number NNG06EO90A to the University of Maryland. RZS and JJS were supported by the LRO project through a cooperative agreement between NASA and the University of Maryland; RDS was supported by a cooperative agreement between NASA and the Catholic University of America; WVB was supported by contract to the University of Arizona; and LGE was supported by contract to the Computer Sciences Corporation. The Russian Federal Space Agency supplied the LEND instrument to NASA and the LRO project. The authors would like to thank J. Keller and P. Romani for insight into photolysis/photodissociation and its relevance to lunar volatiles. The authors thank the referees for detailed comments that have resulted in a stronger interpretation of the LEND data. NR 46 TC 4 Z9 4 U1 0 U2 6 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD JUL 15 PY 2015 VL 255 SI SI BP 100 EP 115 DI 10.1016/j.icarus.2015.04.004 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CJ6YJ UT WOS:000355640800012 ER PT J AU Farrell, WM Hurley, DM Zimmerman, MI AF Farrell, W. M. Hurley, D. M. Zimmerman, M. I. TI Solar wind implantation into lunar regolith: Hydrogen retention in a surface with defects SO ICARUS LA English DT Article DE Moon; Solar wind; Regolith ID POLAR-REGIONS; WATER; MOON; HYDROXYL; ICE; VOLATILES; BODIES AB Solar wind protons are implanted directly into the top 100 nm of the lunar near-surface region, but can either quickly diffuse out of the surface or be retained, depending upon surface temperature and the activation energy, U, associated with the implantation site. In this work, we explore the distribution of activation energies upon implantation and the associated hydrogen-retention times; this for comparison with recent observation of OH on the lunar surface. We apply a Monte Carlo approach: for simulated solar wind protons at a given local time, we assume a distribution of U values with a central peak, U-c and width, U-w, and derive the fraction retained for long periods in the near-surface. We find that surfaces characterized by a distribution with predominantly large values of U (>1 eV) like that expected at defect sites will retain implanted H (to likely form OH). Surfaces with the distribution predominantly at small values of U (<0.2 eV) will quickly diffuse away implanted H. However, surfaces with a large portion of activation energies between 0.3 eV < U< 0.9 eV will tend to be H-retentive in cool conditions but transform into H-emissive surfaces when warmed (as when the surface rotates into local noon). These mid-range activation energies give rise to a diurnal effect with diffusive loss of H at noontime. Published by Elsevier Inc. C1 [Farrell, W. M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Hurley, D. M.; Zimmerman, M. I.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Farrell, W. M.; Hurley, D. M.; Zimmerman, M. I.] NASA, Ames Res Ctr, NASAs Solar Syst Explorat Res Virtual Inst, Moffett Field, CA 94035 USA. RP Farrell, WM (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RI Hurley, Dana/F-4488-2015; Farrell, William/I-4865-2013 OI Hurley, Dana/0000-0003-1052-1494; FU NASA's Lunar Science Institute (NLSI); Solar System Exploration Research Virtual Institute (SSERVI) FX The authors gratefully acknowledge support from NASA's Lunar Science Institute (NLSI) and Solar System Exploration Research Virtual Institute (SSERVI) in completion of this work. NR 40 TC 7 Z9 7 U1 0 U2 4 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD JUL 15 PY 2015 VL 255 SI SI BP 116 EP 126 DI 10.1016/j.icarus.2014.09.014 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CJ6YJ UT WOS:000355640800013 ER PT J AU Hurley, DM Sarantos, M Grava, C Williams, JP Retherford, KD Siegler, M Greenhagen, B Paige, D AF Hurley, Dana M. Sarantos, Menelaos Grava, Cesare Williams, Jean-Pierre Retherford, Kurt D. Siegler, Matthew Greenhagen, Benjamin Paige, David TI An analytic function of lunar surface temperature for exospheric modeling SO ICARUS LA English DT Article DE Moon, surface; Satellites, atmospheres; Atmospheres, structure ID HYDROGEN; MERCURY; MOON AB We present an analytic expression to represent the lunar surface temperature as a function of Sun-state latitude and local time. The approximation represents neither topographical features nor compositional effects and therefore does not change as a function of selenographic latitude and longitude. The function reproduces the surface temperature measured by Diviner to within +/- 10 K at 72% of grid points for dayside solar zenith angles of <80 degrees, and at 98% of grid points for nightside solar zenith angles >100 degrees. The analytic function is least accurate at the terminator, where there is a strong gradient in the temperature, and the polar regions. Topographic features have a larger effect on the actual temperature near the terminator than at other solar zenith angles. For exospheric modeling the effects of topography on the thermal model can be approximated by using an effective longitude for determining the temperature. This effective longitude is randomly redistributed with 1 sigma of 4.5 degrees. The resulting "roughened" analytical model well represents the statistical dispersion in the Diviner data and is expected to be generally useful for future models of lunar surface temperature, especially those implemented within exospheric simulations that address questions of volatile transport. (c) 2014 Elsevier Inc. All rights reserved. C1 [Hurley, Dana M.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Sarantos, Menelaos] Univ Maryland Baltimore Cty, Goddard Planetary Heliophys Inst, Baltimore, MD 21228 USA. [Grava, Cesare; Retherford, Kurt D.] Southwest Res Inst, San Antonio, TX 78228 USA. [Williams, Jean-Pierre; Paige, David] Univ Calif Los Angeles, Los Angeles, CA 90095 USA. [Siegler, Matthew; Greenhagen, Benjamin] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Sarantos, Menelaos] NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Greenbelt, MD 20771 USA. RP Hurley, DM (reprint author), Johns Hopkins Univ, Appl Phys Lab, Johns Hopkins Rd, Laurel, MD 20723 USA. RI Williams, Jean-Pierre/C-3531-2009; Hurley, Dana/F-4488-2015; Greenhagen, Benjamin/C-3760-2016 OI Williams, Jean-Pierre/0000-0003-4163-2760; Hurley, Dana/0000-0003-1052-1494; FU NASA Lunar Reconnaissance Orbiter project through the LAMP team FX This work was supported by the NASA Lunar Reconnaissance Orbiter project through the LAMP team. DMH thanks Rick Elphic and an anonymous referee for helpful suggestions. NR 10 TC 9 Z9 9 U1 1 U2 6 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD JUL 15 PY 2015 VL 255 SI SI BP 159 EP 163 DI 10.1016/j.icarus.2014.08.043 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CJ6YJ UT WOS:000355640800017 ER PT J AU Wei, SJ Avouac, JP Hudnut, KW Donnellan, A Parker, JW Graves, RW Helmberger, D Fielding, E Liu, Z Cappa, F Eneva, M AF Wei, Shengji Avouac, Jean-Philippe Hudnut, Kenneth W. Donnellan, Andrea Parker, Jay W. Graves, Robert W. Helmberger, Don Fielding, Eric Liu, Zhen Cappa, Frederic Eneva, Mariana TI The 2012 Brawley swarm triggered by injection-induced aseismic slip SO EARTH AND PLANETARY SCIENCE LETTERS LA English DT Article DE fluid injection; aseismic slip; high frequency waveform modeling; UAVSAR and InSAR; geothermal; finite fault model ID IMPERIAL-VALLEY; SOUTHERN-CALIFORNIA; EARTHQUAKE SWARM; SUPERSTITION HILLS; FAULT; RUPTURE; SEQUENCE AB It has long been known that fluid injection or withdrawal can induce earthquakes, but the underlying mechanisms remain elusive. For example, the 2012 Brawley swarm, which produced two strike-slip shocks with magnitudes larger than 5.3 and surface ruptures in the close vicinity of a geothermal field, started with earthquakes about 5 km deeper than the injection depth (similar to 1.5 km). This makes the causality between the injection and seismicity unclear. Here, we jointly analyze broadband and strong motion waveforms, UAVSAR, leveling measurements and field observations to reveal the detailed seismic and aseismic faulting behaviors associated with the 2012 Brawley swarm. In particular, path calibration established from smaller events in the swarm allows waveform inversion to be conducted up to 3 Hz to resolve finite rupture process of the Mw 4.7 normal event. Our results show that the 2012 earthquake sequence was preceded by aseismic slip on a shallow normal fault beneath the geothermal field. Aseismic slip initiated in 2010 when injection rate rapidly increased and triggered the following earthquakes subsequently, including unusually shallow and relatively high frequency seismic excitations on the normal fault. In this example, seismicity is induced indirectly by fluid injection, a result of mediation by aseismic creep, rather than directly by a pore pressure increase at the location of the earthquakes. (C) 2015 Elsevier B.V. All rights reserved. C1 [Wei, Shengji; Avouac, Jean-Philippe; Helmberger, Don; Cappa, Frederic] CALTECH, Geol & Planetary Sci, Pasadena, CA 91125 USA. [Hudnut, Kenneth W.; Graves, Robert W.] US Geol Survey, Pasadena, CA 91106 USA. [Donnellan, Andrea; Parker, Jay W.; Fielding, Eric; Liu, Zhen] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Cappa, Frederic] Univ Nice Sophia Antipolis, CNRS, IRD, Observ Cote Azur,Geoazur UMR 7329, F-06560 Valbonne, France. [Eneva, Mariana] Imageair Inc, Reno, NV 89509 USA. [Wei, Shengji] Nanyang Technol Univ, Earth Observ Singapore EOS, Singapore 639798, Singapore. RP Wei, SJ (reprint author), Nanyang Technol Univ, Earth Observ Singapore EOS, Singapore 639798, Singapore. EM shjwei@ntu.edu.sg RI Hudnut, Kenneth/B-1945-2009; Avouac, Jean-Philippe/B-5699-2015; Wei, Shengji/M-2137-2015; Fielding, Eric/A-1288-2007; Cappa, Frederic/B-4014-2017; Liu, Zhen/D-8334-2017 OI Hudnut, Kenneth/0000-0002-3168-4797; Avouac, Jean-Philippe/0000-0002-3060-8442; Wei, Shengji/0000-0002-0319-0714; Fielding, Eric/0000-0002-6648-8067; Cappa, Frederic/0000-0003-4859-8024; FU National Aeronautics and Space Administration; NASA [102443-281945.02.47.02.89] FX The seismic data were downloaded from Southern California Seismic Data Center and strong motion data center (strongmotion-center.org). We thank the Omar Company for providing the leveling data used in this study. We are grateful to Elizabeth Cochran and two anonymous reviewers for their insightful and constructive comments. Suzanne Donovan helped editing the manuscript. Part of the research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. Part of this research was supported by NASA's Earth Surface and Interior and Geodetic Imaging programs (grant number 102443-281945.02.47.02.89). We thank the UAVSAR team and in particular Scott Hensley, Yunling Lou, Brian Hawkins, Naiara Pinto, and Yang Zheng for collection and processing of the UAVSAR data. NR 36 TC 8 Z9 8 U1 0 U2 14 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 JUL 15 PY 2015 VL 422 BP 115 EP 125 DI 10.1016/j.epsl.2015.03.054 PG 11 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA CJ2YN UT WOS:000355350700013 ER PT J AU Ma, C Tschauner, O Beckett, JR Liu, Y Rossman, GR Zhuravlev, K Prakapenka, V Dera, P Taylor, LA AF Ma, Chi Tschauner, Oliver Beckett, John R. Liu, Yang Rossman, George R. Zhuravlev, Kirill Prakapenka, Vitali Dera, Przemyslaw Taylor, Lawrence A. TI Tissintite, (Ca, Na, square)AlSi2O6, a highly-defective, shock-induced, high-pressure clinopyroxene in the Tissint martian meteorite SO EARTH AND PLANETARY SCIENCE LETTERS LA English DT Article DE tissintite; (CaNa square)AlSi2O6; new high-pressure pyroxene; Ca-Eskola; Tissint martian shergottite; synchrotron diffraction ID CRYSTAL-STRUCTURE REFINEMENT; SUBSOLIDUS PHASE-RELATIONS; CA-ESKOLA COMPONENT; ECLOGITIC CLINOPYROXENE; LOWER-MANTLE; ORDINARY CHONDRITES; MIXING PROPERTIES; SYSTEM; JADEITE; PLAGIOCLASE AB Tissintite is a new vacancy-rich, high-pressure clinopyroxene, with a composition essentially equivalent to plagioclase. It was discovered in maskelynite (shocked plagioclase) and is commonly observed included within, or in contact with, shock-melt pockets in the Tissint meteorite, a depleted olivine-phyric shergottite fall from Mars. The simple composition of tissintite (An58-69) and its precursor plagioclase (An59-69) together with the limited occurrence, both spatially (only in maskelynite less than similar to 25 mu m of a shock melt pocket) and in terms of bulk composition, make tissintite a "goldilocks" phase. It formed during a shock event severe enough to allow nucleation and growth of vacancy-rich clinopyroxene from a melt of not too calcic and not too sodic plagioclase composition that was neither too hot nor too cold. With experimental calibration, these limitations on occurrence can be used to place strong constraints on the thermal history of a shock event. The kinetics for nucleation and growth of tissintite are probably slower for more-sodic plagioclase precursors, so tissintite is most likely to occur in depleted olivinephyric shergottites like Tissint and other highly shocked meteorites and lunar and terrestrial rocks that consistently contained calcic plagioclase precursors in the appropriate compositional range for a shock of given intensity. Tissintite, (Ca0.45Na0.31 square(0.24))(Al0.97Fe0.03Mg0.01)(Si1.80Al0,20)O-6, is a C2/c clinopyroxene, containing 42-60 mol% of the Ca-Eskola component, by far the highest known. The cell parameters are a = 9.21 (17) angstrom, b = 9.09 (4) angstrom, c = 5.20 (2) angstrom, beta = 109.6 (9)degrees, V = 410 (8) angstrom(3), Z = 4. The density is 3.32 g/cm(3) and we estimate a cell volume for the Ca-Eskola end-member pyroxene of 411 +/- 13 angstrom(3), which is consistent with a previous estimate and, therefore, supports the importance of this component in clinopyroxenes from ultra-high pressure metamorphic rocks from the Earth's upper mantle. At least in C2/c clinopyroxenes as sodic as tissintite, the a- and b-cell parameters as a function of vacancy concentration intersect at similar to 0.3 vacancies pfu, much lower than the Ca-Eskola end-member (0.5), an inversion of anisotropy suggesting an elastic instability that drives clinopyroxene toward a disordered trigonal structure closely related to that of wadeite; it may mark the boundary beyond which the breakdown of vacancy-rich clinopyroxene to a wadeite-structured phase + stishovite becomes stable, although this was not observed in Tissint (C) 2015 Elsevier B.V. All rights reserved, C1 [Ma, Chi; Beckett, John R.; Rossman, George R.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Tschauner, Oliver] Univ Nevada, High Pressure Sci & Engn Ctr, Las Vegas, NV 89154 USA. [Tschauner, Oliver] Univ Nevada, Dept Geosci, Las Vegas, NV 89154 USA. [Liu, Yang] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Zhuravlev, Kirill; Prakapenka, Vitali] Univ Chicago, Argonne Natl Lab, GSECARS, Argonne, IL 60439 USA. [Dera, Przemyslaw] Univ Hawaii Manoa, Sch Ocean & Earth Sci & Technol, Hawail Inst Geophys & Planetol, Honolulu, HI 96822 USA. [Taylor, Lawrence A.] Univ Tennessee, Planetcny Geosci Inst, Dept Earth & Planetary Sci, Knoxville, TN 37996 USA. RP Ma, C (reprint author), CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. EM chi@gps.caltech.edu OI Rossman, George/0000-0002-4571-6884 FU NSF [EAR-0318518, DMR-0080065] FX SEM, EBSD and EPMA analyses were carried out at the Caltech GPS Division Analytical Facility, which is supported, in part, by NSF Grants EAR-0318518 and DMR-0080065. Synchrotron diffraction was carried out at the 13-IDD beamline of the Advanced Photon Source and the 12.2.2 beamline of the Advanced Light Source. Use of the Advanced Photon Source, an Office of Science User Facility operated for the U.S. Department of Energy (DOE) Office of Science by Argonne National Laboratory, was supported by the U.S. DOE under Contract No. DE-ACO2-06CH11357. The Advanced Light Source is supported by the Director, Office of Science, Office of Basic Energy Sciences, of the U.S. Department of Energy under Contract No. DE-ACO2-05CH11231. OT acknowledges the support from DOE Cooperative Agreement #DE-NA0001982. GRR acknowledges NSF EAR grant 322082. YL acknowledges support from Jet Propulsion Laboratory, which is managed by California Institute of Technology under a contract with NASA, and NASA grant NNN13D465T. LAT and JRB acknowledge NASA Cosmochemistry grants NNX11AG58G and NNX12AH63G, respectively. PD gratefully acknowledges support from NSF grants EAR 1344942 and 1440005. Formal reviews by A. El Goresy and an anonymous reviewer and additional comments by T. Kubo all led to significant improvements. NR 74 TC 9 Z9 9 U1 9 U2 21 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 JUL 15 PY 2015 VL 422 BP 194 EP 205 DI 10.1016/j.epsl.2015.03.057 PG 12 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA CJ2YN UT WOS:000355350700020 ER PT J AU Hunter, MO Keller, M Morton, D Cook, B Lefsky, M Ducey, M Saleska, S de Oliveira, RC Schietti, J AF Hunter, Maria O. Keller, Michael Morton, Douglas Cook, Bruce Lefsky, Michael Ducey, Mark Saleska, Scott de Oliveira, Raimundo Cosme, Jr. Schietti, Juliana TI Structural Dynamics of Tropical Moist Forest Gaps SO PLOS ONE LA English DT Article ID RAIN-FOREST; CANOPY GAPS; PHASE REGENERATION; CENTRAL AMAZONIA; TREE DIVERSITY; BRAZILIAN AMAZON; STEADY-STATE; FIRME FOREST; IVORY-COAST; LIDAR DATA AB Gap phase dynamics are the dominant mode of forest turnover in tropical forests. However, gap processes are infrequently studied at the landscape scale. Airborne lidar data offer detailed information on three-dimensional forest structure, providing a means to characterize fine-scale (1 m) processes in tropical forests over large areas. Lidar-based estimates of forest structure (top down) differ from traditional field measurements (bottom up), and necessitate clear-cut definitions unencumbered by the wisdom of a field observer. We offer a new definition of a forest gap that is driven by forest dynamics and consistent with precise ranging measurements from airborne lidar data and tall, multi-layered tropical forest structure. We used 1000 ha of multi-temporal lidar data (2008, 2012) at two sites, the Tapajos National Forest and Ducke Reserve, to study gap dynamics in the Brazilian Amazon. Here, we identified dynamic gaps as contiguous areas of significant growth, that correspond to areas > 10 m(2), with height < 10 m. Applying the dynamic definition at both sites, we found over twice as much area in gap at Tapajos National Forest (4.8 %) as compared to Ducke Reserve (2.0 %). On average, gaps were smaller at Ducke Reserve and closed slightly more rapidly, with estimated height gains of 1.2 m y(-1) versus 1.1 m y(-1) at Tapajos. At the Tapajos site, height growth in gap centers was greater than the average height gain in gaps (1.3 m y(-1) versus 1.1 m y(-1)). Rates of height growth between lidar acquisitions reflect the interplay between gap edge mortality, horizontal ingrowth and gap size at the two sites. We estimated that approximately 10% of gap area closed via horizontal ingrowth at Ducke Reserve as opposed to 6 % at Tapajos National Forest. Height loss (interpreted as repeat damage and/or mortality) and horizontal ingrowth accounted for similar proportions of gap area at Ducke Reserve (13% and 10 %, respectively). At Tapajos, height loss had a much stronger signal (23 % versus 6 %) within gaps. Both sites demonstrate limited gap contagiousness defined by an increase in the likelihood of mortality in the immediate vicinity (similar to 6 m) of existing gaps. C1 [Hunter, Maria O.] Univ New Hampshire, Earth Sci Res Ctr, Durham, NH 03824 USA. [Keller, Michael] USDA Forest Serv, Int Inst Trop Forestry, San Juan, PR USA. [Keller, Michael] EMBRAPA Monitoramento Satelite, Campinas, SP, Brazil. [Morton, Douglas; Cook, Bruce] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Lefsky, Michael] Colorado State Univ, Nat Resource Ecol Lab, Ft Collins, CO 80523 USA. [Ducey, Mark] Univ New Hampshire, Dept Nat Resources, Durham, NH 03824 USA. [Saleska, Scott] Univ Arizona, Dept Ecol & Evolutionary Biol, Tucson, AZ USA. [de Oliveira, Raimundo Cosme, Jr.] EMBRAPA Amazonia Oriental, Belem, Para, Brazil. [Schietti, Juliana] Inst Nacl de Pesquisas da Amazonia, Manaus, Amazonas, Brazil. RP Hunter, MO (reprint author), Univ New Hampshire, Earth Sci Res Ctr, Durham, NH 03824 USA. EM Hunter.maria@gmail.com RI Keller, Michael/A-8976-2012; Morton, Douglas/D-5044-2012; Ducey, Mark/K-1101-2016 OI Keller, Michael/0000-0002-0253-3359; FU NASA [NNX09AO46H, NNG06GE11A, NNX09AI33G, NNG04G073G, NNX06AH36G]; NSF [DEB0721140]; USAid Sustainable Landscapes FX Funding provided by NASA Grant NNX09AO46H, NASA grant NNG06GE11A, NASA grant NNX09AI33G, NASA grant NNG04G073G, NASA grant NNX06AH36G, NSF grant DEB0721140, USAid Sustainable Landscapes (www.nasa.gov,www.nsf.gov,www.usaid.gov/climate/sustainablelandscapes). The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 78 TC 5 Z9 5 U1 4 U2 17 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD JUL 13 PY 2015 VL 10 IS 7 AR e0132144 DI 10.1371/journal.pone.0132144 PG 19 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CN1PW UT WOS:000358193100024 PM 26168242 ER PT J AU Kwok, R Cunningham, GF AF Kwok, R. Cunningham, G. F. TI Variability of Arctic sea ice thickness and volume from CryoSat-2 SO PHILOSOPHICAL TRANSACTIONS OF THE ROYAL SOCIETY A-MATHEMATICAL PHYSICAL AND ENGINEERING SCIENCES LA English DT Article DE Arctic ocean; ice volume; ice thickness; ice deformation; ice drift ID AIRBORNE DATA; SNOW DEPTH; FREEBOARD; RETRIEVAL AB We present our estimates of the thickness and volume of the Arctic Ocean ice cover from CryoSat-2 data acquired between October 2010 and May 2014. Average ice thickness and draft differences are within 0.16m of measurements from other sources (moorings, submarine, electromagnetic sensors, IceBridge). The choice of parameters that affect the conversion of ice freeboard to thickness is discussed. Estimates between 2011 and 2013 suggest moderate decreases in volume followed by a notable increase of more than 2500km(3) (or 0.34m of thickness over the basin) in 2014, which could be attributed to not only a cooler summer in 2013 but also to large-scale ice convergence just west of the Canadian Arctic Archipelago due to wind-driven onshore drift. Variability of volume and thickness in the multiyear ice zone underscores the importance of dynamics in maintaining the thickness of the Arctic ice cover. Volume estimates are compared with those from ICESat as well as the trends in ice thickness derived from submarine ice draft between 1980 and 2004. The combined ICESat and CryoSat-2 record yields reduced trends in volume loss compared with the 5 year ICESat record, which was weighted by the record-setting ice extent after the summer of 2007. C1 [Kwok, R.; Cunningham, G. F.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Kwok, R (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM ronald.kwok@jpl.nasa.gov OI Kwok, Ronald/0000-0003-4051-5896 NR 37 TC 14 Z9 15 U1 7 U2 32 PU ROYAL SOC PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 1364-503X EI 1471-2962 J9 PHILOS T R SOC A JI Philos. Trans. R. Soc. A-Math. Phys. Eng. Sci. PD JUL 13 PY 2015 VL 373 IS 2045 AR 20140157 DI 10.1098/rsta.2014.0157 PG 20 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CM0BM UT WOS:000357343200001 ER PT J AU Bours, MCP Marsh, TR Gansicke, BT Tauris, TM Istrate, AG Badenes, C Dhillon, VS Gal-Yam, A Hermes, JJ Kengkriangkrai, S Kilic, M Koester, D Mullally, F Prasert, N Steeghs, D Thompson, SE Thorstensen, JR AF Bours, M. C. P. Marsh, T. R. Gaensicke, B. T. Tauris, T. M. Istrate, A. G. Badenes, C. Dhillon, V. S. Gal-Yam, A. Hermes, J. J. Kengkriangkrai, S. Kilic, M. Koester, D. Mullally, F. Prasert, N. Steeghs, D. Thompson, S. E. Thorstensen, J. R. TI A double white dwarf with a paradoxical origin? SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE binaries: close; stars: individual: SDSS J125733.63+542850.5; white dwarfs ID DIGITAL SKY SURVEY; CATACLYSMIC VARIABLE-STARS; CANUM-VENATICORUM BINARIES; MILLISECOND PULSAR; METAL-RICH; SPECTROSCOPIC ANALYSIS; GRAVITATIONAL-WAVES; MERGER SYSTEMS; SDSS 1257+5428; MASS AB We present Hubble Space Telescope UV spectra of the 4.6-h-period double white dwarf SDSS J125733.63+542850.5. Combined with Sloan Digital Sky Survey optical data, these reveal that the massive white dwarf (secondary) has an effective temperature T-2 = 13 030 +/- 70 +/- 150 K and a surface gravity log g(2) = 8.73 +/- 0.05 +/- 0.05 (statistical and systematic uncertainties, respectively), leading to amass of M-2 = 1.06 M-circle dot. The temperature of the extremely low-mass white dwarf (primary) is substantially lower at T-1 = 6400 +/- 37 +/- 50 K, while its surface gravity is poorly constrained by the data. The relative flux contribution of the two white dwarfs across the spectrum provides a radius ratio of R-1/R-2 similar or equal to 4.2, which, together with evolutionary models, allows us to calculate the cooling ages. The secondary massive white dwarf has a cooling age of similar to 1 Gyr, while that of the primary low-mass white dwarf is likely to be much longer, possibly greater than or similar to 5 Gyr, depending on its mass and the strength of chemical diffusion. These results unexpectedly suggest that the low-mass white dwarf formed long before the massive white dwarf, a puzzling discovery which poses a paradox for binary evolution. C1 [Bours, M. C. P.; Marsh, T. R.; Gaensicke, B. T.; Hermes, J. J.; Steeghs, D.] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. [Tauris, T. M.; Istrate, A. G.] Univ Bonn, Argelander Inst Astronomie, D-53121 Bonn, Germany. [Tauris, T. M.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Badenes, C.] Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA. [Dhillon, V. S.] Univ Sheffield, Dept Phys & Astron, Sheffield S3 7RH, S Yorkshire, England. [Gal-Yam, A.] Weizmann Inst Sci, Dept Particle Phys & Astrophys, IL-76100 Rehovot, Israel. [Kengkriangkrai, S.; Prasert, N.] Nat Astron Res Inst Thailand, Chiang Mai 50200, Thailand. [Kilic, M.] Univ Oklahoma, Dept Phys & Astron, Norman, OK 73019 USA. [Koester, D.] Univ Kiel, Inst Theoret Phys & Astrophys, D-24098 Kiel, Germany. [Mullally, F.; Thompson, S. E.] Ames Res Ctr, SETI Inst NASA, Moffett Field, CA 94035 USA. [Thorstensen, J. R.] Dartmouth Coll, Dept Phys & Astron, Hanover, NH 03755 USA. RP Bours, MCP (reprint author), Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. EM m.c.p.bours@warwick.ac.uk RI Gaensicke, Boris/A-9421-2012; Istrate, Alina/N-7827-2016 OI Gaensicke, Boris/0000-0002-2761-3005; Istrate, Alina/0000-0002-8811-8171 FU NASA [NAS 5-26555]; European Research Council under the European Union [320964]; STFC [ST/L000733/1]; VSD [ST/J001589/1]; NSF [AST-1312678]; JRT [AST-1008217]; [12207] FX We thank the referee for comments that helped improve the manuscript, and D. Townsley for useful discussions regarding the effect of accretion heating. The analysis presented in this paper is based on observations made with the NASA/ESA HST, 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 programme #12207. The research leading to these results has received funding from the European Research Council under the European Union's Seventh Framework Programme (FP/2007-2013)/ERC Grant Agreement no. 320964 (WDTracer). TRM and DS acknowledge financial support from STFC under grant number ST/L000733/1, and VSD under ST/J001589/1. MK gratefully acknowledges support of the NSF under grant AST-1312678, and JRT under AST-1008217. NR 65 TC 3 Z9 3 U1 0 U2 2 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUL 11 PY 2015 VL 450 IS 4 BP 3966 EP 3974 DI 10.1093/mnras/stv889 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CQ7YY UT WOS:000360824000045 ER PT J AU Buddendiek, A Schrabback, T Greer, CH Hoekstra, H Sommer, M Eifler, T Erben, T Erler, J Hicks, AK High, FW Hildebrandt, H Marrone, DP Morris, RG Muzzin, A Reiprich, TH Schirmer, M Schneider, P von der Linden, A AF Buddendiek, A. Schrabback, T. Greer, C. H. Hoekstra, H. Sommer, M. Eifler, T. Erben, T. Erler, J. Hicks, A. K. High, F. W. Hildebrandt, H. Marrone, D. P. Morris, R. G. Muzzin, A. Reiprich, T. H. Schirmer, M. Schneider, P. von der Linden, A. TI Optical and Sunyaev-Zel'dovich observations of a new sample of distant rich galaxy clusters in the ROSAT All Sky SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE cosmology: observations ID SOUTH-POLE TELESCOPE; X-RAY-PROPERTIES; SCALING RELATIONS; DARK-MATTER; COSMOLOGICAL CONSTRAINTS; LUMINOSITY FUNCTION; MASS FUNCTION; DATA RELEASE; IMAGING DATA; DEEP SURVEY AB Finding a sample of the most massive clusters with redshifts z > 0.6 can provide an interesting consistency check of the Lambda cold dark matter (Lambda CDM) model. Here, we present results from our search for clusters with 0.6 less than or similar to z less than or similar to 1.0 where the initial candidates were selected by cross-correlating the ROSAT All Sky Survey (RASS) faint and bright source catalogues with red galaxies from the Sloan Digital Sky Survey DR8. Our survey thus covers approximate to 10 000 deg(2), much larger than previous studies of this kind. Deeper follow-up observations in three bands using the William Herschel Telescope and the Large Binocular Telescope were performed to confirm the candidates, resulting in a sample of 44 clusters for which we present richnesses and red sequence redshifts, as well as spectroscopic redshifts for a subset. At least two of the clusters in our sample are comparable in richness to RCS2-J232727.7-020437, one of the richest systems discovered to date. We also obtained new observations with the Combined Array for Research in Millimeter Astronomy for a subsample of 21 clusters. For 11 of those we detect the Sunyaev-Zel'dovich effect signature. The Sunyaev-Zel'dovich signal allows us to estimate M-200 and check for tension with the cosmological standard model. We find no tension between our cluster masses and the Lambda CDM model. C1 [Buddendiek, A.; Schrabback, T.; Sommer, M.; Erben, T.; Erler, J.; Hildebrandt, H.; Reiprich, T. H.; Schneider, P.] Univ Bonn, Argelander Inst Astron, D-53121 Bonn, Germany. [Schrabback, T.; Hoekstra, H.; Muzzin, A.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Schrabback, T.; Morris, R. G.; von der Linden, A.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA. [Greer, C. H.; Marrone, D. P.] Univ Arizona, Steward Observ, Tucson, AZ 85121 USA. [Eifler, T.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Eifler, T.] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA. [Hicks, A. K.] Eureka Sci, Oakland, CA 94602 USA. [High, F. W.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Morris, R. G.] SLAC Natl Accelerator Lab, Menlo Pk, CA 94025 USA. [Schirmer, M.] SLAC Natl Accelerator Lab, Menlo Pk, CA 94025 USA. [von der Linden, A.] Univ Copenhagen, Dark Cosmol Ctr, Niels Bohr Inst, DK-2100 Copenhagen O, Denmark. [von der Linden, A.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA. RP Buddendiek, A (reprint author), Univ Bonn, Argelander Inst Astron, Hugel 71, D-53121 Bonn, Germany. EM abuddend@astro.uni-bonn.de OI Marrone, Daniel/0000-0002-2367-1080 FU International Max Planck Research School (IMPRS) for Astronomy and Astrophysics at the University of Bonn; Transregional Collaborative Research Centre of the DFG [TR 33]; NSF [AST-1140019]; German Federal Ministry of Economics and Technology (BMWi) through DLR [50 OR 1308]; DFG [TR 33, Hi 1495/2-1, RE 1462/5, RE 1462/6]; US Department of Energy [DE-AC02-76SF00515]; Danish National Research Foundation; International Max Planck Research School (IMPRS) for Astronomy and Astrophysics at the University of Cologne FX AB was supported for this research partly through a stipend from the International Max Planck Research School (IMPRS) for Astronomy and Astrophysics at the Universities of Bonn and Cologne and through funding from the Transregional Collaborative Research Centre (TR 33) of the DFG.; CHG is supported by NSF grant AST-1140019.; TS acknowledges support from the German Federal Ministry of Economics and Technology (BMWi) provided through DLR under project 50 OR 1308.; HH is supported by the DFG Emmy Noether grant Hi 1495/2-1.; RGM is supported in part by the US Department of Energy under contract number DE-AC02-76SF00515.; THR acknowledges support from the DFG through the Heisenberg research grant RE 1462/5, from grant RE 1462/6, and from TR 33 (project B18).; The Dark Cosmology Centre is funded by the Danish National Research Foundation. NR 99 TC 1 Z9 1 U1 0 U2 1 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUL 11 PY 2015 VL 450 IS 4 BP 4248 EP 4276 DI 10.1093/mnras/stv783 PG 29 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CQ7YY UT WOS:000360824000068 ER PT J AU Biller, BA Liu, MC Rice, K Wahhaj, Z Nielsen, E Hayward, T Kuchner, MJ Close, LM Chun, M Ftaclas, C Toomey, DW AF Biller, Beth A. Liu, Michael C. Rice, Ken Wahhaj, Zahed Nielsen, Eric Hayward, Thomas Kuchner, Marc J. Close, Laird M. Chun, Mark Ftaclas, Christ Toomey, Douglas W. TI The Gemini NICI Planet-Finding Campaign: asymmetries in the HD 141569 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE circumstellar matter; infrared: stars ID CIRCUMSTELLAR DISK; GIANT PLANETS; STELLAR COMPANIONS; DEBRIS DISK; STARS; HD-141569; GAS; FREQUENCY; SYSTEM; EXOPLANETS AB We report here the highest resolution near-IR imaging to date of the HD 141569A disc taken as part of the NICI (near infrared coronagraphic imager) Science Campaign. We recover four main features in the NICI images of the HD 141569 disc discovered in previous Hubble Space Telescope (HST) imaging: (1) an inner ring/spiral feature. Once deprojected, this feature does not appear circular. (2) An outer ring which is considerably brighter on the western side compared to the eastern side, but looks fairly circular in the deprojected image. (3) An additional arc-like feature between the inner and outer ring only evident on the east side. In the deprojected image, this feature appears to complete the circle of the west side inner ring and (4) an evacuated cavity from 175 au inwards. Compared to the previous HST imaging with relatively large coronagraphic inner working angles (IWA), the NICI coronagraph allows imaging down to an IWA of 0.3 arcsec. Thus, the inner edge of the inner ring/spiral feature is well resolved and we do not find any additional disc structures within 175 au. We note some additional asymmetries in this system. Specifically, while the outer ring structure looks circular in this deprojection, the inner bright ring looks rather elliptical. This suggests that a single deprojection angle is not appropriate for this system and that there may be an offset in inclination between the two ring/spiral features. We find an offset of 4 +/- 2 au between the inner ring and the star centre, potentially pointing to unseen inner companions. C1 [Biller, Beth A.; Rice, Ken] Univ Edinburgh, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland. [Liu, Michael C.; Ftaclas, Christ] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Wahhaj, Zahed] European So Observ, Santiago 19001, Chile. [Nielsen, Eric] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA. [Nielsen, Eric] Carl Sagan Ctr, SETI Inst, Mountain View, CA 94043 USA. [Hayward, Thomas] AURA, Southern Operat Ctr, Gemini Observ, La Serena, Chile. [Kuchner, Marc J.] NASA Goddard Space Flight Ctr, Exoplanets & Stellar Astrophys Lab, Greenbelt, MD 20771 USA. [Close, Laird M.] Univ Arizona, Steward Observ, Tucson, AZ USA. [Chun, Mark] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Toomey, Douglas W.] Mauna Kea Infrared LLC, Hilo, HI 96720 USA. RP Biller, BA (reprint author), Univ Edinburgh, Inst Astron, Blackford Hill, Edinburgh EH9 3HJ, Midlothian, Scotland. EM bb@roe.ac.uk RI Rice, Ken/H-5084-2011 OI Rice, Ken/0000-0002-6379-9185 FU Hubble Fellowship - Space Telescope Science Institute [HST-HF-01204.01-A, NAS 5-26555]; NSF [AST-0713881, AST-0709484, AAG-1109114]; NASA [NNX11 AC31G] FX Based on observations obtained at the Gemini Observatory, which is operated by the Association of Universities for Research in Astronomy, Inc., under a cooperative agreement with the NSF on behalf of the Gemini partnership: the National Science Foundation (United States), the National Research Council (Canada), CONICYT (Chile), the Australian Research Council (Australia), Ministerio da Ciencia, Tecnologia e Inovacao (Brazil) and Ministerio de Ciencia, Tecnologia e Innovacion Productiva (Argentina). BAB was supported by Hubble Fellowship grant HST-HF-01204.01-A awarded by the Space Telescope Science Institute, which is operated by AURA for NASA, under contract NAS 5-26555. This work was supported in part by NSF grants AST-0713881 and AST-0709484 awarded to M. Liu, NASA Origins grant NNX11 AC31G awarded to M. Liu, and NSF grant AAG-1109114 awarded to L. Close. We thank Alycia Weinberger for providing reduced HST NICMOS images for comparison with the NICI images and the anonymous referee for useful suggestions which helped improve the manuscript. NR 41 TC 14 Z9 14 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 JUL 11 PY 2015 VL 450 IS 4 BP 4446 EP 4457 DI 10.1093/mnras/stv870 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CQ7YY UT WOS:000360824000081 ER PT J AU Litvak, ML Mitrofanov, IG Sanin, AB Jun, I Kozyrev, AS Krylov, A Shvetsov, VN Timoshenko, GN Starr, R Zontikov, A AF Litvak, M. L. Mitrofanov, I. G. Sanin, A. B. Jun, I. Kozyrev, A. S. Krylov, A. Shvetsov, V. N. Timoshenko, G. N. Starr, R. Zontikov, A. TI Ground tests with active neutron instrumentation for the planetary science missions SO NUCLEAR INSTRUMENTS & METHODS IN PHYSICS RESEARCH SECTION A-ACCELERATORS SPECTROMETERS DETECTORS AND ASSOCIATED EQUIPMENT LA English DT Article DE Active neutron spectrometer; Pulse neutron generator; Water; DAN ID GAMMA-RAY; DYNAMIC ALBEDO; EXPERIMENT ONBOARD; NUCLEAR TECHNIQUES; DAN EXPERIMENT; MARS ODYSSEY; SPECTROMETER; HYDROGEN; DETECTOR; LUNAR AB We present results of experimental work performed with a spare flight model of the DAN/MSL instrument in a newly built ground test facility at the joint Institute for Nuclear Research. This instrument was selected for the tests as a flight prototype of an active neutron spectrometer applicable for future landed missions to various solid solar system bodies. In our experiment we have fabricated simplified samples of planetary material and tested the capability of neutron activation methods to detect thin layers of water/water ice lying on top of planetary dry regolith or buried within a dry regolith at different depths. (C) 2015 Elsevier B.V. All rights reserved. C1 [Litvak, M. L.; Mitrofanov, I. G.; Sanin, A. B.; Kozyrev, A. S.] RAS, Space Res Inst, Moscow 117997, Russia. [Jun, I.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Krylov, A.; Shvetsov, V. N.; Timoshenko, G. N.; Zontikov, A.] Joint Inst Nucl Res, Dubna, Russia. [Starr, R.] Catholic Univ Amer, Washington, DC 20064 USA. RP Litvak, ML (reprint author), RAS, Space Res Inst, Moscow 117997, Russia. EM litvak@mx.iki.rssi.ru FU Russian Science Foundation [14-22-00249] FX This work is supported by the Grant #14-22-00249 from Russian Science Foundation. NR 52 TC 3 Z9 3 U1 0 U2 6 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0168-9002 EI 1872-9576 J9 NUCL INSTRUM METH A JI Nucl. Instrum. Methods Phys. Res. Sect. A-Accel. Spectrom. Dect. Assoc. Equip. PD JUL 11 PY 2015 VL 788 BP 194 EP 202 DI 10.1016/j.nima.2015.03.066 PG 9 WC Instruments & Instrumentation; Nuclear Science & Technology; Physics, Nuclear; Physics, Particles & Fields SC Instruments & Instrumentation; Nuclear Science & Technology; Physics GA CI6LM UT WOS:000354870700031 ER PT J AU Francis, SP Shaddock, DA Sutton, AJ de Vine, G Ware, B Spero, RE Klipstein, WM McKenzie, K AF Francis, Samuel P. Shaddock, Daniel A. Sutton, Andrew J. de Vine, Glenn Ware, Brent Spero, Robert E. Klipstein, William M. McKenzie, Kirk TI Tone-assisted time delay interferometry on GRACE Follow-On SO PHYSICAL REVIEW D LA English DT Article ID LISA AB We have demonstrated the viability of using the Laser Ranging Interferometer on the Gravity Recovery and Climate Experiment Follow-On (GRACE-FO) space mission to test key aspects of the interspacecraft interferometry proposed for detecting gravitational waves. The Laser Ranging Interferometer on GRACE-FO will be the first demonstration of interspacecraft interferometry. GRACE-FO shares many similarities with proposed space-based gravitational wave detectors based on the Laser Interferometer Space Antenna (LISA) concept. Given these similarities, GRACE-FO provides a unique opportunity to test novel interspacecraft interferometry techniques that a LISA-like mission will use. The LISA Experience from GRACE-FO Optical Payload (LEGOP) is a project developing tests of arm locking and time delay interferometry (TDI), two frequency stabilization techniques, that could be performed on GRACE-FO. In the proposed LEGOP TDI demonstration one GRACE-FO spacecraft will have a free-running laser while the laser on the other spacecraft will be locked to a cavity. It is proposed that two one-way interspacecraft phase measurements will be combined with an appropriate delay in order to produce a round-trip, dual one-way ranging (DOWR) measurement independent of the frequency noise of the free-running laser. This paper describes simulated and experimental tests of a tone-assisted TDI ranging (TDIR) technique that uses a least-squares fitting algorithm and fractional-delay interpolation to find and implement the delays needed to form the DOWRTDI combination. The simulation verifies tone-assisted TDIR works under GRACE-FO conditions. Using simulated GRACE-FO signals the tone-assisted TDIR algorithm estimates the time-varying interspacecraft range with a rms error of +/- 0.2 m, suppressing the free-running laser frequency noise by 8 orders of magnitude. The experimental results demonstrate the practicability of the technique, measuring the delay at the 6 ns level in the presence of a significant displacement signal. C1 [Francis, Samuel P.; Shaddock, Daniel A.; Sutton, Andrew J.] Australian Natl Univ, Dept Quantum Sci, Canberra, ACT 2601, Australia. [Shaddock, Daniel A.; de Vine, Glenn; Ware, Brent; Spero, Robert E.; Klipstein, William M.; McKenzie, Kirk] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Francis, SP (reprint author), Australian Natl Univ, Dept Quantum Sci, GPO Box 4, Canberra, ACT 2601, Australia. EM samuel.francis@anu.edu.au FU Australian Research Council's Discovery Projects funding scheme [DP140103575]; National Aeronautics and Space Administration; NASA FX This research was supported under the Australian Research Council's Discovery Projects funding scheme (Project No. DP140103575). Part of this research was performed at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration, with support from an appointment to the NASA Postdoctoral Program, administered by Oak Ridge Associated Universities through a contract with NASA. NR 37 TC 1 Z9 1 U1 3 U2 5 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 2470-0010 EI 2470-0029 J9 PHYS REV D JI Phys. Rev. D PD JUL 10 PY 2015 VL 92 IS 1 AR 012005 DI 10.1103/PhysRevD.92.012005 PG 13 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA CV8YH UT WOS:000364573700001 ER PT J AU Ackermann, M Arcavi, I Baldini, L Ballet, J Barbiellini, G Bastieri, D Bellazzini, R Bissaldi, E Blandford, RD Bonino, R Bottacini, E Brandt, TJ Bregeon, J Bruel, P Buehler, R Buson, S Caliandro, GA Cameron, RA Caragiulo, M Caraveo, PA Cavazzuti, E Cecchi, C Charles, E Chekhtman, A Chiang, J Chiaro, G Ciprini, S Claus, R Cohen-Tanugi, J Cutini, S D'Ammando, F de Angelis, A de Palma, F Desiante, R Di Venere, L Drell, PS Favuzzi, C Fegan, SJ Franckowiak, A Funk, S Fusco, P Gal-Yam, A Gargano, F Gasparrini, D Giglietto, N Giordano, F Giroletti, M Glanzman, T Godfrey, G Grenier, IA Grove, JE Guiriec, S Harding, AK Hayashi, K Hewitt, JW Hill, AB Horan, D Jogler, T Johannesson, G Kocevski, D Kuss, M Larsson, S Lashner, J Latronico, L Li, J Li, L Longo, F Loparco, F Lovellette, MN Lubrano, P Malyshev, D Mayer, M Mazziotta, MN McEnery, JE Michelson, PF Mizuno, T Monzani, ME Morselli, A Murase, K Nugent, P Nuss, E Ofek, E Ohsugi, T Orienti, M Orlando, E Ormes, JF Paneque, D Pesce-Rollins, M Piron, F Pivato, G Raino, S Rando, R Razzano, M Reimer, A Reimer, O Schulz, A Sgro, C Siskind, EJ Spada, F Spandre, G Spinelli, P Suson, DJ Takahashi, H Thayer, JB Tibaldo, L Torres, DF Troja, E Vianello, G Werner, M Wood, KS Wood, M AF Ackermann, M. Arcavi, I. Baldini, L. Ballet, J. Barbiellini, G. Bastieri, D. Bellazzini, R. Bissaldi, E. Blandford, R. D. Bonino, R. Bottacini, E. Brandt, T. J. Bregeon, J. Bruel, P. Buehler, R. Buson, S. Caliandro, G. A. Cameron, R. A. Caragiulo, M. Caraveo, P. A. Cavazzuti, E. Cecchi, C. Charles, E. Chekhtman, A. Chiang, J. Chiaro, G. Ciprini, S. Claus, R. Cohen-Tanugi, J. Cutini, S. D'Ammando, F. de Angelis, A. de Palma, F. Desiante, R. Di Venere, L. Drell, P. S. Favuzzi, C. Fegan, S. J. Franckowiak, A. Funk, S. Fusco, P. Gal-Yam, A. Gargano, F. Gasparrini, D. Giglietto, N. Giordano, F. Giroletti, M. Glanzman, T. Godfrey, G. Grenier, I. A. Grove, J. E. Guiriec, S. Harding, A. K. Hayashi, K. Hewitt, J. W. Hill, A. B. Horan, D. Jogler, T. Johannesson, G. Kocevski, D. Kuss, M. Larsson, S. Lashner, J. Latronico, L. Li, J. Li, L. Longo, F. Loparco, F. Lovellette, M. N. Lubrano, P. Malyshev, D. Mayer, M. Mazziotta, M. N. McEnery, J. E. Michelson, P. F. Mizuno, T. Monzani, M. E. Morselli, A. Murase, K. Nugent, P. Nuss, E. Ofek, E. Ohsugi, T. Orienti, M. Orlando, E. Ormes, J. F. Paneque, D. Pesce-Rollins, M. Piron, F. Pivato, G. Raino, S. Rando, R. Razzano, M. Reimer, A. Reimer, O. Schulz, A. Sgro, C. Siskind, E. J. Spada, F. Spandre, G. Spinelli, P. Suson, D. J. Takahashi, H. Thayer, J. B. Tibaldo, L. Torres, D. F. Troja, E. Vianello, G. Werner, M. Wood, K. S. Wood, M. TI SEARCH FOR EARLY GAMMA-RAY PRODUCTION IN SUPERNOVAE LOCATED IN A DENSE CIRCUMSTELLAR MEDIUM WITH THE FERMI LAT SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmic rays; gamma rays: general; methods: data analysis; supernovae: general ID LARGE-AREA TELESCOPE; SHOCK BREAKOUT; SN 2010JL; CONFIDENCE-INTERVALS; EMISSION; EXPLOSIONS; WIND AB Supernovae (SNe) exploding in a dense circumstellar medium (CSM) are hypothesized to accelerate cosmic rays in collisionless shocks and emit GeV gamma-rays and TeV neutrinos on a timescale of several months. We perform the first systematic search for gamma-ray emission in Fermi Large Area Telescope data in the energy range from 100 MeV to 300 GeV from the ensemble of 147 SNe Type IIn exploding in a dense CSM. We search for a gamma-ray excess at each SNe location in a one-year time window. In order to enhance a possible weak signal, we simultaneously study the closest and optically brightest sources of our sample in a joint-likelihood analysis in three different time windows (1 year, 6 months, and 3 months). For the most promising source of the sample, SN 2010jl (PTF 10aaxf), we repeat the analysis with an extended time window lasting 4.5 years. We do not find a significant excess in gamma-rays for any individual source nor for the combined sources and provide model-independent flux upper limits for both cases. In addition, we derive limits on the gamma-ray luminosity and the ratio of gamma-ray-to-optical luminosity ratio as a function of the index of the proton injection spectrum assuming a generic gamma-ray production model. Furthermore, we present detailed flux predictions based on multi-wavelength observations and the corresponding flux upper limit at a 95% confidence level (CL) for the source SN 2010jl (PTF 10aaxf). C1 [Ackermann, M.; Buehler, R.; Mayer, M.; Schulz, A.] Deutsch Elektronen Synchrotron DESY, D-15738 Zeuthen, Germany. [Baldini, L.] Univ Pisa, I-56127 Pisa, Italy. [Baldini, L.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy. [Ballet, J.; Grenier, I. A.] Univ Paris Diderot, CEA Saclay, CNRS, Lab AIM,CEA IRFU,Serv Astrophys, F-91191 Gif Sur Yvette, France. [Barbiellini, G.; Desiante, R.; Longo, F.] Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy. [Barbiellini, G.; Longo, F.] Univ Trieste, Dipartimento Fis, I-34127 Trieste, Italy. [Bastieri, D.; Buson, S.; Rando, R.] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy. [Bastieri, D.; Buson, S.; Chiaro, G.; Rando, R.] Univ Padua, Dipartimento Fis & Astron G Galilei, I-35131 Padua, Italy. [Bellazzini, R.; Kuss, M.; Pesce-Rollins, M.; Pivato, G.; Razzano, M.; Sgro, C.; Spada, F.; Spandre, G.; Spinelli, P.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy. [Bissaldi, E.; Caragiulo, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Gargano, F.; Giglietto, N.; Giordano, F.; Loparco, F.; Mazziotta, M. N.; Raino, S.; Spinelli, P.] Ist Nazl Fis Nucl, Sez Bari, I-70126 Bari, Italy. [Blandford, R. D.; Bottacini, E.; Caliandro, G. A.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; Drell, P. S.; Franckowiak, A.; Funk, S.; Glanzman, T.; Godfrey, G.; Hill, A. B.; Jogler, T.; Malyshev, D.; Michelson, P. F.; Monzani, M. E.; Orlando, E.; Paneque, D.; Reimer, A.; Reimer, O.; Thayer, J. B.; Tibaldo, L.; Vianello, G.; Wood, M.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Dept Phys, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA. [Blandford, R. D.; Bottacini, E.; Caliandro, G. A.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; Drell, P. S.; Franckowiak, A.; Funk, S.; Glanzman, T.; Godfrey, G.; Hill, A. B.; Jogler, T.; Malyshev, D.; Michelson, P. F.; Monzani, M. E.; Orlando, E.; Paneque, D.; Reimer, A.; Reimer, O.; Thayer, J. B.; Tibaldo, L.; Vianello, G.; Wood, M.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA. [Bonino, R.; Latronico, L.] Ist Nazl Fis Nucl, Sez Torino, I-10125 Turin, Italy. [Bonino, R.] Univ Turin, Dipartimento Fis Gen Amadeo Avogadro, I-10125 Turin, Italy. [Brandt, T. J.; Guiriec, S.; Harding, A. K.; Hewitt, J. W.; Kocevski, D.; McEnery, J. E.; Troja, E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Bregeon, J.; Cohen-Tanugi, J.; Nuss, E.; Piron, F.] Univ Montpellier, IN2P3, CNRS, Lab Univers & Particules Montpellier, F-34059 Montpellier, France. [Bruel, P.; Fegan, S. J.; Horan, D.] Ecole Polytech, CNRS, IN2P3, Lab Leprince Ringuet, F-91128 Palaiseau, France. [Caliandro, G. A.] Consorzio Interuniv Fis Spaziale CIFS, I-10133 Turin, Italy. [Caraveo, P. A.] INAF Ist Astrofis Spaziale & Fis Cosm, I-20133 Milan, Italy. [Cavazzuti, E.; Ciprini, S.; Cutini, S.; Gasparrini, D.] Agenzia Spaziale Italiana ASI Sci Data Ctr, I-00133 Rome, Italy. [Cecchi, C.; Ciprini, S.; Cutini, S.; Gasparrini, D.; Lubrano, P.] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy. [Cecchi, C.; Lubrano, P.] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy. [Chekhtman, A.] George Mason Univ, Coll Sci, Fairfax, VA 22030 USA. [Chekhtman, A.] Naval Res Lab, Washington, DC 20375 USA. [Ciprini, S.; Cutini, S.; Gasparrini, D.] Osserv Astron Roma, INAF, I-00040 Rome, Italy. [D'Ammando, F.; Giroletti, M.; Orienti, M.] Ist Radioastron, INAF, I-40129 Bologna, Italy. [D'Ammando, F.] Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy. [de Angelis, A.] Univ Udine, Dipartimento Fis, I-33100 Udine, Italy. [de Angelis, A.] Ist Nazl Fis Nucl, Grp Collegato Udine, Sez Trieste, I-33100 Udine, Italy. [de Palma, F.] Univ Telemat Pegaso, I-80132 Naples, Italy. [Desiante, R.] Univ Udine, I-33100 Udine, Italy. [Di Venere, L.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Giordano, F.; Loparco, F.; Raino, S.; Spinelli, P.] Univ Bari, Dipartimento Fis M Merlin, I-70126 Bari, Italy. [Di Venere, L.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Giordano, F.; Loparco, F.; Raino, S.; Spinelli, P.] Politecn Bari, I-70126 Bari, Italy. [Grove, J. E.; Lovellette, M. N.; Wood, K. S.] Naval Res Lab, Div Space Sci, Washington, DC 20375 USA. [Hayashi, K.] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Chuo Ku, Sagamihara, Kanagawa 2525210, Japan. [Hewitt, J. W.] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA. [Hewitt, J. W.] Univ Maryland Baltimore Cty, Ctr Space Sci & Technol, Baltimore, MD 21250 USA. [Hewitt, J. W.] Ctr Res & Explorat Space Sci & Technol CRESST, Greenbelt, MD 20771 USA. [Hill, A. B.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Johannesson, G.] Univ Iceland, Inst Sci, IS-107 Reykjavik, Iceland. [Larsson, S.] Stockholm Univ, Dept Phys, AlbaNova, SE-10691 Stockholm, Sweden. [Larsson, S.; Li, L.] Oskar Klein Ctr Cosmoparticle Phys, AlbaNova, SE-10691 Stockholm, Sweden. [Larsson, S.] Stockholm Univ, Dept Astron, SE-10691 Stockholm, Sweden. [Lashner, J.] Wesleyan Univ, Middletown, CT 06459 USA. [Li, J.; Torres, D. F.] CSIC, Inst Space Sci, IEEC, E-08193 Barcelona, Spain. [Li, L.] KTH Royal Inst Technol, Dept Phys, AlbaNova, SE-10691 Stockholm, Sweden. [McEnery, J. E.; Troja, E.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA. [McEnery, J. E.; Troja, E.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Mizuno, T.; Ohsugi, T.] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Higashihiroshima, Hiroshima 7398526, Japan. [Morselli, A.] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, I-00133 Rome, Italy. [Murase, K.] Inst Adv Study, Princeton, NJ 08540 USA. [Murase, K.] Penn State Univ, Dept Astron & Astrophys, Dept Phys, Ctr Particle & Gravitat Astrophys, University Pk, PA 16802 USA. [Nugent, P.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. [Nugent, P.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Ofek, E.] Weizmann Inst Sci, Benoziyo Ctr Astrophys, IL-76100 Rehovot, Israel. [Ormes, J. F.] Univ Denver, Dept Phys & Astron, Denver, CO 80208 USA. [Paneque, D.] Max Planck Inst Phys & Astrophys, D-80805 Munich, Germany. [Reimer, A.; Reimer, O.; Werner, M.] Leopold Franzens Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria. [Reimer, A.; Reimer, O.; Werner, M.] Leopold Franzens Univ Innsbruck, Inst Theoret Phys, A-6020 Innsbruck, Austria. [Siskind, E. J.] NYCB Real Time Comp Inc, Lattingtown, NY 11560 USA. [Suson, D. J.] Purdue Univ Calumet, Dept Chem & Phys, Hammond, IN 46323 USA. [Takahashi, H.] Hiroshima Univ, Dept Phys Sci, Higashihiroshima, Hiroshima 7398526, Japan. [Torres, D. F.] Inst Catalana Recerca & Estudis Avancats ICREA, Barcelona, Spain. [Gal-Yam, A.; Guiriec, S.] Weizmann Inst Sci, Dept Particle Phys & Astrophys, IL-76100 Rehovot, Israel. [Arcavi, I.; Hill, A. B.] Las Cumbres Observ Global Telescope Network, Goleta, CA 93117 USA. [Arcavi, I.; Razzano, M.] Univ Calif Santa Barbara, Kavli Inst Theoret Phys, Santa Barbara, CA 93106 USA. RP Ackermann, M (reprint author), Deutsch Elektronen Synchrotron DESY, D-15738 Zeuthen, Germany. EM afrancko@slac.stanford.edu RI Morselli, Aldo/G-6769-2011; Reimer, Olaf/A-3117-2013; Funk, Stefan/B-7629-2015; Johannesson, Gudlaugur/O-8741-2015; Loparco, Francesco/O-8847-2015; Mazziotta, Mario /O-8867-2015; Gargano, Fabio/O-8934-2015; giglietto, nicola/I-8951-2012; Sgro, Carmelo/K-3395-2016; Bissaldi, Elisabetta/K-7911-2016; Torres, Diego/O-9422-2016; Orlando, E/R-5594-2016; Bonino, Raffaella/S-2367-2016; Di Venere, Leonardo/C-7619-2017 OI Gasparrini, Dario/0000-0002-5064-9495; Baldini, Luca/0000-0002-9785-7726; Giordano, Francesco/0000-0002-8651-2394; Caraveo, Patrizia/0000-0003-2478-8018; Sgro', Carmelo/0000-0001-5676-6214; SPINELLI, Paolo/0000-0001-6688-8864; Hill, Adam/0000-0003-3470-4834; Pesce-Rollins, Melissa/0000-0003-1790-8018; orienti, monica/0000-0003-4470-7094; Giroletti, Marcello/0000-0002-8657-8852; Bonino, Raffaella/0000-0002-4264-1215; Murase, Kohta/0000-0002-5358-5642; Morselli, Aldo/0000-0002-7704-9553; Reimer, Olaf/0000-0001-6953-1385; Funk, Stefan/0000-0002-2012-0080; Johannesson, Gudlaugur/0000-0003-1458-7036; Loparco, Francesco/0000-0002-1173-5673; Mazziotta, Mario /0000-0001-9325-4672; Gargano, Fabio/0000-0002-5055-6395; giglietto, nicola/0000-0002-9021-2888; Bissaldi, Elisabetta/0000-0001-9935-8106; Torres, Diego/0000-0002-1522-9065; Di Venere, Leonardo/0000-0003-0703-824X FU W.M. Keck Foundation; Willner Family Leadership Institute Ilan Gluzman (Secaucus NJ); Israeli Ministry of Science; Israel Science Foundation; Minerva; I-CORE Program of the Planning and Budgeting Committee; EU/FP7 via ERC grant [307260]; Quantum Universe I-Core program by the Israeli Committee for Planning and Budgeting; ISF; WIS-UK "Making Connections"; Kimmel award; ARCHES award FX The Fermi-LAT Collaboration acknowledges generous ongoing support from a number of agencies and institutes that have supported both the development and the operation of the LAT as well as scientific data analysis. These include the National Aeronautics and Space Administration and the Department of Energy in the United States, the Commissariat a l'Energie Atomique and the Centre National de la Recherche Scientifique/Institut National de Physique Nucleaire et de Physique des Particules in France, the Agenzia Spaziale Italiana and the Istituto Nazionale di Fisica Nucleare in Italy, the Ministry of Education, Culture, Sports, Science and Technology (MEXT), High Energy Accelerator Research Organization (KEK) and Japan Aerospace Exploration Agency (JAXA) in Japan, and the K.A. Wallenberg Foundation, the Swedish Research Council and the Swedish National Space Board in Sweden. Additional support for science analysis during the operations phase is gratefully acknowledged from the Istituto Nazionale di Astrofisica in Italy and the Centre National d'Etudes Spatiales in France. This paper is based on observations obtained with the Samuel Oschin Telescope as part of the Palomar Transient Factory project, a scientific collaboration between the California Institute of Technology, Columbia University, Las Cumbres Observatory, the Lawrence Berkeley National Laboratory, the National Energy Research Scientific Computing Center, the University of Oxford, and the Weizmann Institute of Science. Some of the data presented herein were obtained at the W.M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and NASA; the Observatory was made possible by the generous financial support of the W.M. Keck Foundation. We are grateful for excellent staff assistance at the Palomar, Lick, and Keck Observatories. E.O.O. is the incumbent of the Arye Dissentshik career development chair and is grateful for support by grants from the Willner Family Leadership Institute Ilan Gluzman (Secaucus NJ), the Israeli Ministry of Science, the Israel Science Foundation, Minerva and the I-CORE Program of the Planning and Budgeting Committee and The Israel Science Foundation. A.G.-Y. is supported by the EU/FP7 via ERC grant No. 307260, the Quantum Universe I-Core program by the Israeli Committee for Planning and Budgeting and the ISF, Minerva and ISF grants, WIS-UK "Making Connections", and Kimmel and ARCHES awards. NR 34 TC 4 Z9 4 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 10 PY 2015 VL 807 IS 2 AR 169 DI 10.1088/0004-637X/807/2/169 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO2EB UT WOS:000358967000055 ER PT J AU Brown, JC Carlson, RW Toner, MP AF Brown, John C. Carlson, Robert W. Toner, Mark P. TI DESTRUCTION AND OBSERVATIONAL SIGNATURES OF SUN-IMPACTING COMETS SO ASTROPHYSICAL JOURNAL LA English DT Article DE comets: general; Sun: flares; Sun: helioseismology ID SOLAR-FLARES; SEISMIC EMISSION; EXTREME-ULTRAVIOLET; SUNGRAZING COMETS; SHOEMAKER-LEVY-9; JUPITER; ATMOSPHERE; CORONA; DISINTEGRATION; TEMPERATURE AB Motivated by recent data on comets in the low corona, we discuss destruction of "Sun-impacting" comets in the dense lower atmosphere. Perihelion distances q less than or similar to R-circle dot and masses M-o >> 10(12) g are required to reach such depths. Extending earlier work on planetary atmosphere impacts to solar conditions, we evaluate the mechanisms and distribution of nucleus mass and energy loss as functions of M-o and q, and of parameter X = 2Q/C(H)v(o)(2). Q is the total specific energy for ablative mass-loss, C-H the bow-shock heat-transfer efficiency, and v(o) the solar escape speed (619 km s(-1)). We discuss factors affecting Q and C-H and conclude that, for solar v(o), X is most likely <1 and solar-impactors mostly ablated before decelerating. Sun-impacting comets have energies M(o)v(o)(2)/2 similar to 2 x 10(30) x (M-o/10(15) g) 15 erg, (comparable to magnetic flares similar to 10(29-33)). This is released as a localized explosive airburst within a few scale heights H similar or equal to 200 km of the photosphere, depending weakly on M-o, q and X. For X = 10(-2) and M-o = 10(15) g , a shallow incidence (e.g., polar theta similar to cos(-1)(0.01)) Kreutz comet airburst occurs at atmospheric density n similar to 3 x 10(15) cm(-3)-a height of 700 km (3.5 H) above the photosphere (where n = n(o) = 10(17) cm(-3)). The airburst n scales as similar to(MoX cos(3)theta)(1/2) (while height z (km) 200 ln(n(o)/n) so n increases 1000 x (700 km deeper) for vertical entry. Such airbursts drive flare-like phenomena including prompt radiation, hot rising plumes, and photospheric ripples, the observability and diagnostic value of which we discuss. C1 [Brown, John C.] Univ Glasgow, Sch Phys & Astron, Glasgow G12 8QQ, Lanark, Scotland. [Carlson, Robert W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Brown, JC (reprint author), Univ Glasgow, Sch Phys & Astron, Glasgow G12 8QQ, Lanark, Scotland. EM john.brown@glasgow.ac.uk FU Leverhulme Emeritus Fellowship; NASA JPL Visitor Funds; ISSI Bern's Near Sun Comet Workshop FX We thank the anonymous referee for comments improving greatly the content clarity and accuracy of the paper and for suggesting more discussion of the possible observation and value of Sun-impactors. The paper has also benefited from discussions with Karl Battams, Paul Bryans, Matthew Knight, John Raymond, Karl Schrijver, and Dimitri Veras. J. C. B. also gratefully acknowledges the financial support of a Leverhulme Emeritus Fellowship, NASA JPL Visitor Funds, and funds from ISSI Bern's Near Sun Comet Workshop led by Geraint Jones (University College London). He would also like to thank Keri Simpson for valuable proof-reading and comments. Portions of this work were performed at the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA. NR 57 TC 1 Z9 1 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 10 PY 2015 VL 807 IS 2 AR 165 DI 10.1088/0004-637X/807/2/165 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO2EB UT WOS:000358967000051 ER PT J AU Good, SW Forsyth, RJ Raines, JM Gershman, DJ Slavin, JA Zurbuchen, TH AF Good, S. W. Forsyth, R. J. Raines, J. M. Gershman, D. J. Slavin, J. A. Zurbuchen, T. H. TI RADIAL EVOLUTION OF A MAGNETIC CLOUD: MESSENGER, STEREO, AND VENUS EXPRESS OBSERVATIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE magnetic fields; solar wind; Sun: coronal mass ejections (CMEs); Sun: heliosphere ID ENERGETIC PARTICLE; SOLAR-WIND; FLUX ROPES; 1 AU; HELICITY; MISSION; PLASMA; ORIENTATION; INSTRUMENT; DEPENDENCE AB The Solar Orbiter and Solar Probe Plus missions will provide observations of magnetic clouds closer to the Sun than ever before, and it will be good preparation for these missions to make full use of the most recent in situ data sets from the inner heliosphere-namely, those provided by MErcury Surface, Space ENvironment, GEochemistry, and Ranging (MESSENGER) and Venus Express-for magnetic cloud studies. We present observations of the same magnetic cloud made by MESSENGER at Mercury and later by Solar TErrestrial RElations Observatory-B (STEREO-B), while the spacecraft were radially aligned in 2011 November. Few such radial observations of magnetic clouds have been previously reported. Estimates of the solar wind speed at MESSENGER are also presented, calculated through the application of a previously established technique. The cloud's flux rope has been analyzed using force-free fitting; the rope diameter increased from 0.18 to 0.41 AU (corresponding to an. r(H)(0.94) dependence on heliocentric distance, r(H)), and the axial magnetic field strength dropped from 46.0 to 8.7 nT (an. r(H)(-1.84) dependence) between the spacecraft, clear indications of an expanding structure. The axial magnetic flux was similar to 0.50 nT AU(2) at both spacecraft, suggesting that the rope underwent no significant erosion through magnetic reconnection between MESSENGER and STEREO-B. Further, we estimate the change in the cloud's angular width by assuming helicity conservation. It has also been found that the rope axis rotated by 30 degrees between the spacecraft to lie close to the solar equatorial plane at STEREO-B. Such a rotation, if it is a common feature of coronal mass ejection propagation, would have important implications for space weather forecasting. C1 [Good, S. W.; Forsyth, R. J.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, London SW7 2AZ, England. [Raines, J. M.; Slavin, J. A.; Zurbuchen, T. H.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. [Gershman, D. J.] NASA, Goddard Space Flight Ctr, Geospace Phys Lab, Greenbelt, MD 20771 USA. RP Good, SW (reprint author), Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Prince Consort Rd, London SW7 2AZ, England. EM simon.good07@imperial.ac.uk RI Slavin, James/H-3170-2012; OI Slavin, James/0000-0002-9206-724X; Good, Simon/0000-0002-4921-4208 FU UK Science and Technology Facilities Council; European Union [606692] FX We wish to thank the MESSENGER, STEREO, Venus Express, and SOHO instrument teams for providing the data used in this work, as well as the PDS:PPI, IGPP UCLA, ESA PSA, and CDAW data archives for their distribution of the data. This work has been supported with funding provided by the UK Science and Technology Facilities Council and the European Union's Seventh Framework Programme for research, technological development, and demonstration under grant agreement No. 606692 [HELCATS]. In addition, we wish to thank J. Eastwood and M. O. Archer for useful discussions of this work. The thoughtful and constructive input from the referee is also very much appreciated. NR 50 TC 4 Z9 4 U1 0 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 10 PY 2015 VL 807 IS 2 AR 177 DI 10.1088/0004-637X/807/2/177 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO2EB UT WOS:000358967000063 ER PT J AU Guiriec, S Kouveliotou, C Daigne, F Zhang, B Hascoet, R Nemmen, RS Thompson, DJ Bhat, PN Gehrels, N Gonzalez, MM Kaneko, Y McEnery, J Mochkovitch, R Racusin, JL Ryde, F Sacahui, JR Unsal, AM AF Guiriec, S. Kouveliotou, C. Daigne, F. Zhang, B. Hascoet, R. Nemmen, R. S. Thompson, D. J. Bhat, P. N. Gehrels, N. Gonzalez, M. M. Kaneko, Y. McEnery, J. Mochkovitch, R. Racusin, J. L. Ryde, F. Sacahui, J. R. Unsal, A. M. TI TOWARD A BETTER UNDERSTANDING OF THE GRB PHENOMENON: A NEW MODEL FOR GRB PROMPT EMISSION AND ITS EFFECTS ON THE NEW L-i(NT)-E-peak,i(rest,NT) RELATION SO ASTROPHYSICAL JOURNAL LA English DT Article DE acceleration of particles; black hole physics; distance scale; gamma-ray burst: general; radiation mechanisms: non-thermal; radiation mechanisms: thermal ID GAMMA-RAY-BURSTS; HIGH-ENERGY EMISSION; LARGE-AREA TELESCOPE; DECAYING MAGNETIC-FIELD; SYNCHROTRON SHOCK MODEL; E-P EVOLUTION; PHOTOSPHERIC EMISSION; SPECTRAL COMPONENT; FERMI OBSERVATIONS; COMPREHENSIVE ANALYSIS AB Gamma-ray burst (GRB) prompt emission spectra in the keV-MeV energy range are usually considered to be adequately fitted with the empirical Band function. Recent observations with the Fermi Gamma-ray Space Telescope (Fermi) revealed deviations from the Band function, sometimes in the form of an additional blackbody (BB) component, while on other occasions in the form of an additional power law (PL) component extending to high energies. In this article we investigate the possibility that the three components may be present simultaneously in the prompt emission spectra of two very bright GRBs (080916C and 090926A) observed with Fermi, and how the three components may affect the overall shape of the spectra. While the two GRBs are very different when fitted to a single Band function, they look like "twins" in the three-component scenario. Through fine-time spectroscopy down to the 100 ms timescale, we follow the evolution of the various components. We succeed in reducing the number of free parameters in the three-component model, which results in a new semi-empirical model-but with physical motivations-to be competitive with the Band function in terms of number of degrees of freedom. From this analysis using multiple components, the Band function is globally the most intense component, although the additional PL can overpower the others in sharp time structures. The Band function and the BB component are the most intense at early times and globally fade across the burst duration. The additional PL is the most intense component at late time and may be correlated with the extended high-energy emission observed thousands of seconds after the burst with Fermi/Large Area Telescope. Unexpectedly, this analysis also shows that the additional PL may be present from the very beginning of the burst, where it may even overpower the other components at low energy. We investigate the effect of the three components on the new time-resolved luminosity-hardness relation in both the observer and rest frames and show that a strong correlation exists between the flux of the non-thermal Band function and its E-peak only when the three components are fitted simultaneously to the data (i.e., F-i(NT)-E-peak,i(NT) relation). In addition, this result points toward a universal relation between those two quantities when transposed to the central engine rest frame for all GRBs (i.e., L-i(NT)-E-peak,i(rest,NT) relation). We discuss a possible theoretical interpretation of the three spectral components within this new empirical model. We suggest that (i) the BB component may be interpreted as the photosphere emission of a magnetized relativistic outflow, (ii) the Band component has synchrotron radiation in an optically thin region above the photosphere, either from internal shocks or magnetic field dissipation, and (iii) the extra PL component extending to high energies likely has an inverse Compton origin of some sort, even though its extension to a much lower energy remains a mystery. C1 [Guiriec, S.; Thompson, D. J.; Gehrels, N.; McEnery, J.; Racusin, J. L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Guiriec, S.; Gonzalez, M. M.; McEnery, J.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA. [Guiriec, S.; Gonzalez, M. M.; McEnery, J.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Guiriec, S.] NASA, George C Marshall Space Flight Ctr, CRESST, Huntsville, AL 35812 USA. [Kouveliotou, C.] NASA, George C Marshall Space Flight Ctr, Off Sci & Technol, Huntsville, AL 35812 USA. [Kouveliotou, C.] George Washington Univ, Dept Phys, Washington, DC 20052 USA. [Daigne, F.; Mochkovitch, R.] UPMC, CNRS, UMR7095, Inst Astrophys Paris, F-75014 Paris, France. [Zhang, B.] Univ Nevada, Dept Phys & Astron, Las Vegas, NV 89012 USA. [Hascoet, R.] Columbia Univ, Dept Phys, New York, NY 10027 USA. [Hascoet, R.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Nemmen, R. S.] Univ Sao Paulo, Inst Astron Geofis & Ciencias Atmosfer, BR-05508090 Sao Paulo, SP, Brazil. [Bhat, P. N.] Univ Alabama, NSSTC, Huntsville, AL 35805 USA. [Gonzalez, M. M.] Univ Nacl Autonoma Mexico, Inst Astron, Mexico City 04510, DF, Mexico. [Kaneko, Y.; Unsal, A. M.] Sabanci Univ, Fac Engn & Nat Sci, TR-34956 Istanbul, Turkey. [Ryde, F.] Royal Inst Technol, Dept Phys, AlbaNova, SE-10691 Stockholm, Sweden. [Ryde, F.] AlbaNova, Oskar Klein Ctr Cosmo Particle Phys, SE-10691 Stockholm, Sweden. [Sacahui, J. R.] INPE, BR-12227010 So Jos Dos Campos, SP, Brazil. RP Guiriec, S (reprint author), NASA, Postdoctoral Program, Greenbelt, MD 20771 USA. EM sylvain.guiriec@nasa.gov FU NASA Postdoctoral Program (NPP) at the NASA/Goddard Space Flight Center; NASA [NNH11ZDA001N, NNH13ZDA001N] FX To complete this project, S.G. was supported by the NASA Postdoctoral Program (NPP) at the NASA/Goddard Space Flight Center, administered by Oak Ridge Associated Universities through a contract with NASA as well as by the NASA grants NNH11ZDA001N and NNH13ZDA001N awarded to S.G. during the cycles 5 and 7 of the NASA Fermi Guest Investigator Program. NR 115 TC 18 Z9 18 U1 1 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 10 PY 2015 VL 807 IS 2 AR 148 DI 10.1088/0004-637X/807/2/148 PG 55 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO2EB UT WOS:000358967000034 ER PT J AU Holczer, T Shporer, A Mazeh, T Fabrycky, D Nachmani, G McQuillan, A Sanchis-Ojeda, R Orosz, JA Welsh, WF Ford, EB Jontof-Hutter, D AF Holczer, Tomer Shporer, Avi Mazeh, Tsevi Fabrycky, Daniel Nachmani, Gil McQuillan, Amy Sanchis-Ojeda, Roberto Orosz, Jerome A. Welsh, William F. Ford, Eric B. Jontof-Hutter, Daniel TI TIME VARIATION OF KEPLER TRANSITS INDUCED BY STELLAR SPOTS-A WAY TO DISTINGUISH BETWEEN PROGRADE AND RETROGRADE MOTION. II. APPLICATION TO KOIs SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems; stars: activity; stars: rotation; techniques: photometric ID SPIN-ORBIT ALIGNMENT; MULTIPLE-PLANET SYSTEMS; SUPER-NEPTUNE HAT-P-11B; SUN-LIKE STAR; HOT-JUPITER; TIMING OBSERVATIONS; ECLIPSING BINARIES; EXOPLANETARY SYSTEM; ROTATION PERIODS; DATA RELEASE AB Mazeh et al. have presented an approach that can, in principle, use the derived transit timing variation (TTV) of some transiting planets observed by the Kepler mission to distinguish between the prograde and retrograde motion of their orbits with respect to their parent stars' rotation. The approach utilizes TTVs induced by spot-crossing events that occur when the planet moves across a spot on the stellar surface, looking for a correlation between the derived TTVs and the stellar brightness derivatives at the corresponding transits. This can work even in data that cannot temporally resolve the spot-crossing events themselves. Here, we apply this approach to the Kepler KOIs, identifying nine systems where the photometric spot modulation is large enough and the transit timing accurate enough to allow detection of a TTV-brightness-derivatives correlation. Of those systems, five show highly significant prograde motion (Kepler-17b, Kepler-71b, KOI-883.01, KOI-895.01, and KOI-1074.01), while no system displays retrograde motion, consistent with the suggestion that planets orbiting cool stars have prograde motion. All five systems have impact parameter 0.2 less than or similar to b less than or similar to 0.5, and all systems within that impact parameter range show significant correlation, except HAT-P-11b where the lack of a correlation follows its large stellar obliquity. Our search suffers from an observational bias against detection of high impact parameter cases, and the detected sample is extremely small. Nevertheless, our findings may suggest that stellar spots, or at least the larger ones, tend to be located at low stellar latitude, but not along the stellar equator, similar to the Sun. C1 [Holczer, Tomer; Mazeh, Tsevi; Nachmani, Gil; McQuillan, Amy] Tel Aviv Univ, Raymond & Beverly Sackler Fac Exact Sci, Sch Phys & Astron, IL-69978 Tel Aviv, Israel. [Shporer, Avi] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Shporer, Avi] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Mazeh, Tsevi] Univ Calif Santa Barbara, Kavli Inst Theoret Phys, Santa Barbara, CA 93106 USA. [Fabrycky, Daniel] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Sanchis-Ojeda, Roberto] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Orosz, Jerome A.; Welsh, William F.] San Diego State Univ, Dept Astron, San Diego, CA 92182 USA. [Ford, Eric B.; Jontof-Hutter, Daniel] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Ford, Eric B.] Penn State Univ, Ctr Exoplanets & Habitable Worlds, University Pk, PA 16802 USA. RP Holczer, T (reprint author), Tel Aviv Univ, Raymond & Beverly Sackler Fac Exact Sci, Sch Phys & Astron, IL-69978 Tel Aviv, Israel. EM holczer@gmail.com OI /0000-0001-6545-639X; Shporer, Avi/0000-0002-1836-3120 FU European Research Council under the EU's Seventh Framework Programme (FP7)/ERC Grant [291352]; Israel Science Foundation [1423/11]; Israeli Centers of Research Excellence (I-CORE) [1829/12]; NASA Kepler Participating Scientist Program award [NNX12AF73G]; NASA Origins of Solar Systems award [NNX14AI76G]; NASA Exoplanet Research Program award [NNX15AE21G]; Pennsylvania State University; Eberly College of Science; Pennsylvania Space Grant Consortium; NSF [AST-1109928]; NASA [NNX13AI76G-3, NNX14AB91G, NAS5-26555]; National Aeronautics and Space Administration [NNX14AB87G]; NASA through the Sagan Fellowship Program; NASA Office of Space Science [NNX09AF08G] FX We wish to warmly thank Jason Rowe, Fergal Mullally, and Jack Lissauer, for discussions and feedback that helped improve this paper. The research leading to these results has received funding from the European Research Council under the EU's Seventh Framework Programme (FP7/(2007-2013)/ERC Grant Agreement No. 291352). T.M. acknowledges support from the Israel Science Foundation (grant No. 1423/11) and the Israeli Centers of Research Excellence (I-CORE, grant No. 1829/12). E. B. F. was supported in part by NASA Kepler Participating Scientist Program award NNX12AF73G, NASA Origins of Solar Systems award NNX14AI76G, and NASA Exoplanet Research Program award NNX15AE21G. The Center for Exoplanets and Habitable Worlds is supported by the Pennsylvania State University, the Eberly College of Science, and the Pennsylvania Space Grant Consortium. W.F.W. and J.A.O. gratefully acknowledge support from the NSF via grant AST-1109928, and from NASA via grants NNX13AI76G-3 and NNX14AB91G. D.F. was supported by the National Aeronautics and Space Administration under Grant No. NNX14AB87G issued through the Kepler Participating Scientists Program. The last phase of this study was done when T.M. and R.S. were members of the KITP program of "Dynamics and Evolution of earth-like Planets." They wish to thank the director of KITP, Lars Bidsten, and the coordinators of the program, Eric Ford, Louise Kellogg, Geoff Marcy, and Burkhard Militzer, for participation in the program. This work was performed in part at the Jet Propulsion Laboratory, under contract with the California Institute of Technology (Caltech) funded by NASA through the Sagan Fellowship Program executed by the NASA Exoplanet Science Institute. All photometric data presented in this paper were obtained from the Mikulsky Archive for Space Telescopes (MAST). STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. Support for MAST for non-HST data is provided by the NASA Office of Space Science via grant NNX09AF08G and by other grants and contracts. NR 59 TC 5 Z9 5 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 10 PY 2015 VL 807 IS 2 AR 170 DI 10.1088/0004-637X/807/2/170 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO2EB UT WOS:000358967000056 ER PT J AU Koss, MJ Romero-Canizales, C Baronchelli, L Teng, SH Balokovic, M Puccetti, S Bauer, FE Arevalo, P Assef, R Ballantyne, DR Brandt, WN Brightman, M Comastri, A Gandhi, P Harrison, FA Luo, B Schawinski, K Stern, D Treister, E AF Koss, Michael J. Romero-Canizales, C. Baronchelli, L. Teng, S. H. Balokovic, M. Puccetti, S. Bauer, F. E. Arevalo, P. Assef, R. Ballantyne, D. R. Brandt, W. N. Brightman, M. Comastri, A. Gandhi, P. Harrison, F. A. Luo, B. Schawinski, K. Stern, D. Treister, E. TI BROADBAND OBSERVATIONS OF THE COMPTON-THICK NUCLEUS OF NGC 3393 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: individual (NGC 3393); galaxies: Seyfert; X-rays: galaxies ID ACTIVE GALACTIC NUCLEI; SUPERMASSIVE BLACK-HOLES; SIMILAR-TO 2; RESOLUTION SPECTRAL TEMPLATES; HEAVILY OBSCURED QUASAR; X-RAY-EMISSION; XMM-NEWTON; LOCAL UNIVERSE; HOST GALAXIES; SEYFERT-GALAXIES AB We present new Nuclear Spectroscopic Telescope Array (NuSTAR) and Chandra observations of NGC 3393, a galaxy reported to host the smallest separation dual active galactic nuclei (AGN) resolved in the X-rays. While past results suggested a 150 pc separation dual AGN, three times deeper Chandra imaging, combined with adaptive optics and radio imaging suggest a single, heavily obscured, radio-bright AGN. Using Very Large Array and Very Long Baseline Array data, we find an AGN with a two-sided jet rather than a dual AGN and that the hard X-ray, UV, optical, near-infrared, and radio emission are all from a single point source with a radius <0.'' 2. We find that the previously reported dual AGN is most likely a spurious detection resulting from the low number of X-ray counts (<160) at 6-7 keV and Gaussian smoothing of the data on scales much smaller than the point-spread function (PSF) (0.'' 25 versus 0.'' 80 FWHM). We show that statistical noise in a single Chandra PSF generates spurious dual peaks of the same separation (0.'' 55 +/- 0.'' 07 versus 0.'' 6) and flux ratio (39%+/- 9% versus 32% counts) as the purported dual AGN. With NuSTAR, we measure a Compton-thick source (N-H = 2.2 +/- 0.4 x 10(24) cm(-2)) with a large torus half-opening angle, theta tor = 79-(+1)(19)degrees which we postulate results from feedback from strong radio jets. This AGN shows a 2-10 keV intrinsic-to-observed flux ratio of approximate to 150 (L2-10 keV int = 2.6 +/- 0.3 x 10(43) erg s(-1) versus L2-10 keV observed = 1.7 +/- 0.2 x 10(41) erg s(-1)). Using simulations, we find that even the deepest Chandra observations would severely underestimate the intrinsic luminosity of NGC 3393 above z > 0.2, but would detect an unobscured AGN of this luminosity out to high redshift (z approximate to 5). C1 [Koss, Michael J.; Baronchelli, L.; Schawinski, K.] ETH, Dept Phys, Inst Astron, CH-8093 Zurich, Switzerland. [Koss, Michael J.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Romero-Canizales, C.] Millennium Inst Astrophys, Santiago 7820436, Chile. [Romero-Canizales, C.; Bauer, F. E.] Pontificia Univ Catolica Chile, Fac Fis, Inst Astrofis, Santiago 22, Chile. [Teng, S. H.] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA. [Teng, S. H.] Univ Maryland, Dept Astron, CRESST, College Pk, MD 20742 USA. [Balokovic, M.; Brightman, M.; Harrison, F. A.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Puccetti, S.] Osserv Astron Roma, INAF, I-00040 Monte Porzio Catone, RM, Italy. [Puccetti, S.] ASDC ASI, I-00133 Rome, Italy. [Bauer, F. E.] Space Sci Inst, Boulder, CO 80301 USA. [Arevalo, P.] Univ Valparaiso, Fac Ciencias, Inst Fis & Astron, Valparaiso, Chile. [Assef, R.] Univ Diego Portales, Fac Ingn, Nucleo Astron, Santiago, Chile. [Ballantyne, D. R.; Luo, B.] Georgia Inst Technol, Sch Phys, Ctr Relativist Astrophys, Atlanta, GA 30332 USA. [Brandt, W. N.] Penn State Univ, Davey Lab 525, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Comastri, A.] Osservatorio Astron Bologna, INAF, I-40127 Bologna, Italy. [Gandhi, P.] Univ Durham, Dept Phys, Durham DH1 3LE, England. [Gandhi, P.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Stern, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Treister, E.] Univ Concepcion, Dept Astron, Concepcion, Chile. RP Koss, MJ (reprint author), ETH, Dept Phys, Inst Astron, Wolfgang Pauli Str 27, CH-8093 Zurich, Switzerland. EM mkoss@phys.ethz.ch RI Koss, Michael/B-1585-2015; Brandt, William/N-2844-2015; Comastri, Andrea/O-9543-2015; OI Koss, Michael/0000-0002-7998-9581; Brandt, William/0000-0002-0167-2453; Comastri, Andrea/0000-0003-3451-9970; Puccetti, Simonetta/0000-0002-2734-7835; Schawinski, Kevin/0000-0001-5464-0888 FU Swiss National Science Foundation (SNSF) through the Ambizione fellowship grant [PZ00P2 154799/1]; Swiss National Science Foundation (NSF) [PP00P2 138979/1]; National Aeronautics and Space Administration through Chandra Award [AR3-14010X]; National Aeronautics Space Administration [NAS8-03060]; ALMA-CONICYT FUND Project [31100004]; CONICYT through FONDECYT grant [3150238]; Millennium Institute of Astrophysics (MAS) - Iniciativa Cientifica Milenio del Ministerio Economia, Fomento y Turismo de Chile [IC120009]; ASI/INAF [I/037/12/0 011/13]; Caltech Kingsley visitor program; NASA postdoctoral fellowship program; Center of Excellence in Astrophysics and Associated Technologies [PFB 06]; FONDECYT regular grant [1120061]; CONICYT Anillo project [ACT1101]; NASA Headquarters under the NASA Earth and Space Science Fellowship Program [NNX14AQ07H]; Gemini-CONICYT grant [32120009]; National Aeronautics and Space Administration; ESA Member States; NASA; JPL FX We thank Jim Condon, Fred Lo, and Antxon Alberdi for their useful discussion of radio data and astrometry. We thank Harvey Tananbaum and Diab Jerius for useful discussions of the Chandra PSF and using the MARX software. We thank Pepi Fabbiano and Alessandro Paggi for useful discussions of previous NGC 3393 papers. M.K. acknowledges support from the Swiss National Science Foundation (SNSF) through the Ambizione fellowship grant PZ00P2 154799/1. M.K. and K.S. acknowledge support from Swiss National Science Foundation (NSF) grant PP00P2 138979/1. M.K. also acknowledges support for this work was provided by the National Aeronautics and Space Administration through Chandra Award Number AR3-14010X issued by the Chandra X-ray Observatory Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of the National Aeronautics Space Administration under contract NAS8-03060. C.R.C. acknowledges financial support from the ALMA-CONICYT FUND Project 31100004. We also acknowledge support from CONICYT through FONDECYT grant 3150238 (C.R.C.) and from project IC120009 Millennium Institute of Astrophysics (MAS) funded by the Iniciativa Cientifica Milenio del Ministerio Economia, Fomento y Turismo de Chile (C.R.C, F.E.B.). A.C. acknowledges support from the ASI/INAF grant I/037/12/0 011/13 and the Caltech Kingsley visitor program. ST acknowledges support from the NASA postdoctoral fellowship program. Support for the work of ET was provided by the Center of Excellence in Astrophysics and Associated Technologies (PFB 06), by the FONDECYT regular grant 1120061 and by the CONICYT Anillo project ACT1101. M.B. acknowledges support from NASA Headquarters under the NASA Earth and Space Science Fellowship Program, grant NNX14AQ07H. R.J.A. was supported by Gemini-CONICYT grant number 32120009. This work made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science DataCenter (ASDC, Italy) and the California Institute of Technology (USA). This research has made use of software provided by the Chandra X-ray Center (CXC) in the application packages CIAO, ChIPS, and Sherpa. The scientific results reported in this article are based on data obtained from the Chandra Data Archive. This research made use of the XRT Data Analysis Software (XRTDAS), archival data, software and on-line services provided by the ASDC. Based on observations obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA. The Cornell Atlas of Spitzer IRS Sources (CASSIS) is a product of the Infrared Science Center at Cornell University, supported by NASA and JPL. We used observations made with the NASA/ESA Hubble Space Telescope, and obtained from the Hubble Legacy Archive, which is a collaboration between the Space Telescope Science Institute (STScI/NASA), the Space Telescope European Coordinating Facility (ST-ECF/ESA), and the Canadian Astronomy Data Centre (CADC/NRC/CSA). This research made use of the Chandra Transmission Grating Catalog and archive (http://tgcat.mit.edu).; This paper is based on observations made with the VLA and the Very Long Baseline Array (VLBA) of the National Radio Astronomy Observatory (NRAO); the NRAO is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. NR 74 TC 16 Z9 16 U1 1 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 10 PY 2015 VL 807 IS 2 AR 149 DI 10.1088/0004-637X/807/2/149 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO2EB UT WOS:000358967000035 ER PT J AU Line, MR Teske, J Burningham, B Fortney, JJ Marley, MS AF Line, Michael R. Teske, Johanna Burningham, Ben Fortney, Jonathan J. Marley, Mark S. TI UNIFORM ATMOSPHERIC RETRIEVAL ANALYSIS OF ULTRACOOL DWARFS. I. CHARACTERIZING BENCHMARKS, Gl 570D AND HD 3651B SO ASTROPHYSICAL JOURNAL LA English DT Article DE brown dwarfs; radiative transfer; stars: abundances; stars: atmospheres; stars: individual (Gl 570, HD 3651) ID SOLAR-TYPE STARS; EXOPLANET HOST STAR; GIANT PLANET ATMOSPHERES; OPEN CLUSTER DWARFS; TO-OXYGEN RATIO; BROWN DWARF; LINE FORMATION; PHYSICAL-PROPERTIES; ABUNDANCE ANALYSIS; O-I AB Interpreting the spectra of brown dwarfs is key to determining the fundamental physical and chemical processes occurring in their atmospheres. Powerful Bayesian atmospheric retrieval tools have recently been applied to both exoplanet and brown dwarf spectra to tease out the thermal structures and molecular abundances to understand those processes. In this manuscript we develop a significantly upgraded retrieval method and apply it to the SpeX spectral library data of two benchmark late T. dwarfs, Gl 570D and HD 3651B, to establish the validity of our upgraded forward model parameterization and Bayesian estimator. Our retrieved metallicities, gravities, and effective temperatures are consistent with the metallicity and presumed ages of the systems. We add the carbon-to-oxygen ratio as a new dimension to benchmark systems and find good agreement between carbon-to-oxygen ratios derived in the brown dwarfs and the host stars. Furthermore, we have for the first time unambiguously determined the presence of ammonia in the low-resolution spectra of these two late T. dwarfs. We also show that the retrieved results are not significantly impacted by the possible presence of clouds, though some quantities are significantly impacted by uncertainties in photometry. This investigation represents a watershed study in establishing the utility of atmospheric retrieval approaches on brown dwarf spectra. C1 [Line, Michael R.; Fortney, Jonathan J.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Teske, Johanna] Carnegie DTM, Washington, DC 20015 USA. [Burningham, Ben; Marley, Mark S.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Burningham, Ben] Univ Hertfordshire, Sci & Technol Res Inst, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England. RP Line, MR (reprint author), Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. EM mrline@ucsc.edu OI Marley, Mark/0000-0002-5251-2943; Burningham, Ben/0000-0003-4600-5627 FU Carnegie Origins Postdoctoral Fellowship Program; European Commission [PIOF-GA-2013-629435]; NSF [AST-1312545]; NASA Astrophysics Theory and Planetary Atmospheres programs FX The authors would like to thank Adam Burgasser, Brendan Bowler, Kelle Cruz, Mike Cushing, Michael Liu, and Emily Rice for useful discussions on benchmark systems, data treatment, and various data-model comparison approaches. The authors thank Richard Freedman and Roxana Lupu for providing gas opacities and Caroline Morley for radiative transfer code comparisons and helpful discussions. We thank Jacob Lustig-Yeager and Kyle Luther for rewriting portions of the code in python and C for significant speed improvements and also Dan Foreman-Mackey for making EMCEE available to the community. Finally, we thank the anonymous referee and statistics consultant for useful and insightful comments. J.T. acknowledges financial support from the Carnegie Origins Postdoctoral Fellowship Program. B.B. acknowledges financial support from the European Commission in the form of a Marie Curie International Outgoing Fellowship (PIOF-GA-2013-629435). J.F. acknowledges funding support from NSF award AST-1312545. M.M. acknowledges support from the NASA Astrophysics Theory and Planetary Atmospheres programs. NR 119 TC 8 Z9 8 U1 1 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 10 PY 2015 VL 807 IS 2 AR 183 DI 10.1088/0004-637X/807/2/183 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO2EB UT WOS:000358967000069 ER PT J AU Stern, D AF Stern, Daniel TI THE X-RAY TO MID-INFRARED RELATION OF AGNs AT HIGH LUMINOSITY SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active ID ACTIVE GALACTIC NUCLEI; IDENTIFICATION SEXSI PROGRAM; DIGITAL SKY SURVEY; SIMILAR-TO 2; EXTRAGALACTIC SURVEY; INFRARED GALAXIES; OBSCURED QUASARS; STAR-FORMATION; DATA RELEASE; XMM-NEWTON AB The X-ray and mid-IR emission from active galactic nuclei (AGNs) are strongly correlated. However, while various published parameterizations of this correlation are consistent with the low-redshift, local Seyfert galaxy population, extrapolations of these relations to high luminosity differ by an order of magnitude at vL(v)(6 mu m) similar to 10(47) erg s(-1). Using data from the Wide-field Infrared Survey Explorer, we determine the mid-IR luminosities of the most luminous quasars from the Sloan Digital Sky Survey and present a revised formulation of the X-ray to mid-IR relation of AGNs which is appropriate from the Seyfert regime to the powerful quasar regime. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Stern, D (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,Mail Stop 169-221, Pasadena, CA 91109 USA. EM daniel.k.stern@jpl.nasa.gov FU National Aeronautics and Space Administration; NASA through ADAP award [12-ADAP12-109] FX The author gratefully acknowledges communications and input from close collaborators on the NuSTAR and WISE science teams, particularly David Alexander, Neil Brandt, Peter Eisenhardt, Poshak Gandhi, Michael Koss, George Lansbury, and Ezequiel Treister. I am also grateful to the referee, whose suggestions have improved the paper. This publication makes use of data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration. The author also acknowledges support from NASA through ADAP award 12-ADAP12-109. NR 50 TC 28 Z9 28 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 10 PY 2015 VL 807 IS 2 AR 129 DI 10.1088/0004-637X/807/2/129 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO2EB UT WOS:000358967000015 ER PT J AU Tagliaferri, G Ghisellini, G Perri, M Hayashida, M Balokovic, M Covino, S Giommi, P Madejski, GM Puccetti, S Sbarrato, T Boggs, SE Chiang, J Christensen, FE Craig, WW Hailey, CJ Harrison, FA Stern, D Zhang, WW AF Tagliaferri, G. Ghisellini, G. Perri, M. Hayashida, M. Balokovic, M. Covino, S. Giommi, P. Madejski, G. M. Puccetti, S. Sbarrato, T. Boggs, S. E. Chiang, J. Christensen, F. E. Craig, W. W. Hailey, C. J. Harrison, F. A. Stern, D. Zhang, W. W. TI NuSTAR AND MULTIFREQUENCY STUDY OF THE TWO HIGH-REDSHIFT BLAZARS S5 0836+710 AND PKS 2149-306 SO ASTROPHYSICAL JOURNAL LA English DT Article DE BL Lacertae objects: individual (PKS 2149-306, S5 0836+710); galaxies: active; galaxies: jets; quasars: general; X-rays: general ID ACTIVE GALACTIC NUCLEI; LARGE-AREA TELESCOPE; RADIO-LOUD QUASARS; BLACK-HOLE; X-RAY; RELATIVISTIC JETS; SIMPLIFIED VIEW; DISTANT BLAZAR; SOURCE CATALOG; FERMI BLAZARS AB Powerful blazars are flat-spectrum radio quasars whose emission is dominated by a Compton component peaking between a few hundred keV and a few hundred MeV. We observed two bright blazars, PKS 2149-306 at redshift z = 2.345 and S5 0836+710 at z = 2.172, in the hard X-ray band with the Nuclear Spectroscopic Telescope Array satellite. Simultaneous soft-X-rays and UV-optical observations were performed with the Swift satellite, while near-infrared (near-IR) data were obtained with the Rapid Eye Mount telescope. To study their variability, we repeated these observations for both sources on a timescale of a few months. While no fast variability was detected during a single observation, both sources were variable in the X-ray band, up to 50%, between the two observations, with larger variability at higher energies. No variability was detected in the optical/NIR band. These data, together with Fermi-Large Area Telescope, Wide-field Infrared Survey Explorer, and other literature data, are then used to study the overall spectral energy distributions (SEDs) of these blazars. Although the jet nonthermal emission dominates the SED, it leaves the UV band unhidden, allowing us to detect the thermal emission of the disk. and to estimate the black hole mass. The nonthermal emission is well reproduced by a one-zone leptonic model by the synchrotron, self-Compton, and external Compton processes. Our data are better reproduced if we assume that the location of the dissipation region of the jet, R-diss, is in. between the torus and the broad-line region. The observed variability is explained by changing a minimum number of model parameters by a very small amount. C1 [Tagliaferri, G.; Ghisellini, G.; Covino, S.; Sbarrato, T.] INAF Osservatorio Astron Brera, I-23807 Merate, Italy. [Perri, M.; Giommi, P.; Puccetti, S.] ASI Sci Data Ctr, I-00133 Rome, Italy. [Perri, M.; Puccetti, S.] INAF Osservatorio Astron Roma, I-00040 Monte Porzio Catone, Italy. [Hayashida, M.] Univ Tokyo, Inst Cosm Ray Res, Kashiwa, Chiba 2778582, Japan. [Balokovic, M.; Harrison, F. A.] CALTECH, Cahill Ctr Astrophys, Pasadena, CA 91125 USA. [Madejski, G. M.; Chiang, J.] SLAC Natl Accelerator Lab, Kavli Inst Particle Astrophys & Cosmol, Menlo Pk, CA 94025 USA. [Sbarrato, T.] Univ Milano Bicocca, Dipartimento Fis G Occhialini, I-20126 Milan, Italy. [Boggs, S. E.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Christensen, F. E.; Craig, W. W.] Tech Univ Denmark, DTU Space Natl Space Inst, DK-2800 Lyngby, Denmark. [Craig, W. W.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA. [Hailey, C. J.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Stern, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Zhang, W. W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Tagliaferri, G (reprint author), INAF Osservatorio Astron Brera, Via E Bianchi 46, I-23807 Merate, Italy. EM gianpiero.tagliaferri@brera.inaf.it RI Boggs, Steven/E-4170-2015; OI Boggs, Steven/0000-0001-9567-4224; Puccetti, Simonetta/0000-0002-2734-7835; Sbarrato, Tullia/0000-0002-3069-9399; Covino, Stefano/0000-0001-9078-5507; giommi, paolo/0000-0002-2265-5003; Perri, Matteo/0000-0003-3613-4409; Tagliaferri, Gianpiero/0000-0003-0121-0723; Ghisellini, Gabriele/0000-0002-0037-1974 FU ASI-INAF grant [I/037/12/0]; NASA [NNG08FD60C] FX We acknowledge financial support from the ASI-INAF grant I/037/12/0. This work was supported under NASA Contract No. NNG08FD60C and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by NASA. We thank the NuSTAR Operations, Software and Calibration teams for support with the execution and analysis of these observations. We also thank the Swift team for quickly approving and executing the requested ToO observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (Caltech, USA). The Fermi-LAT Collaboration acknowledges generous ongoing support from a number of agencies and institutes that have supported both the development and the operation of the LAT, as well as scientific data analysis. These include the National Aeronautics and Space Administration and the Department of Energy in the United States; the Commissariat a l'Energie Atomique and the Centre National de la Recherche Scientifique/Institut National de Physique Nucleaire et de Physique des Particules in France; the Agenzia Spaziale Italiana and the Istituto Nazionale di Fisica Nucleare in Italy; the Ministry of Education, Culture, Sports, Science and Technology (MEXT), High Energy Accelerator Research Organization (KEK), and Japan Aerospace Exploration Agency (JAXA) in Japan; and the K. A. Wallenberg Foundation, the Swedish Research Council, and the Swedish National Space Board in Sweden. Additional support for science analysis during the operations phase is gratefully acknowledged from the Istituto Nazionale di Astrofisica in Italy and the Centre National d'Etudes Spatiales in France. Part of this work is based on archival data, software, or online services provided by the ASI Data Center (ASDC). NR 72 TC 6 Z9 6 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 10 PY 2015 VL 807 IS 2 AR 167 DI 10.1088/0004-637X/807/2/167 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO2EB UT WOS:000358967000053 ER PT J AU Venter, C Kopp, A Harding, AK Gonthier, PL Busching, I AF Venter, C. Kopp, A. Harding, A. K. Gonthier, P. L. Buesching, I. TI COSMIC-RAY POSITRONS FROM MILLISECOND PULSARS SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmic rays; pulsars: general; stars: neutron ID LARGE-AREA TELESCOPE; INTERSTELLAR RADIATION-FIELD; GALACTIC MAGNETIC-FIELD; HIGH-ENERGY ELECTRONS; X-RAY; PARTICLE-ACCELERATION; SUPERNOVA-REMNANTS; BINARY-SYSTEMS; NEARBY PULSARS; PAIR FORMATION AB Observations by the Fermi Large Area Telescope of gamma-ray millisecond pulsar (MSP) light curves imply copious pair production in their magnetospheres, and not exclusively in those of younger pulsars. Such pair cascades may be a primary source of Galactic electrons and positrons, contributing to the observed enhancement in positron flux above similar to 10 GeV. Fermi has also uncovered many new MSPs, impacting Galactic stellar population models. We investigate the contribution of Galactic MSPs to the flux of terrestrial cosmic-ray electrons and positrons. Our population synthesis code predicts the source properties of present-day MSPs. We simulate their pair spectra invoking an offset-dipole magnetic field. We also consider positrons and electrons that have been further accelerated to energies of several TeV by strong intrabinary shocks in black widow (BW) and redback (RB) systems. Since MSPs are not surrounded by pulsar wind nebulae or supernova shells, we assume that the pairs freely escape and undergo losses only in the intergalactic medium. We compute the transported pair spectra at Earth, following their diffusion and energy loss through the Galaxy. The predicted particle flux increases for non-zero offsets of the magnetic polar caps. Pair cascades from the magnetospheres of MSPs are only modest contributors around a few tens of GeV to the lepton fluxes measured by the Alpha Magnetic Spectrometer, PAMELA, and Fermi, after which this component cuts off. The contribution by BWs and RBs may, however, reach levels of a few tens of percent at tens of TeV, depending on model parameters. C1 [Venter, C.; Kopp, A.; Buesching, I.] North West Univ, Ctr Space Res, ZA-2520 Potchefstroom, South Africa. [Harding, A. K.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Gonthier, P. L.] Hope Coll, Dept Phys, Holland, MI 49423 USA. RP Venter, C (reprint author), North West Univ, Ctr Space Res, Potchefstroom Campus,Private Bag X6001, ZA-2520 Potchefstroom, South Africa. FU South African National Research Foundation; NASA Astrophysics Theory Program; National Science Foundation RUI program; Michigan Space Grant Consortium FX C.V. is supported by the South African National Research Foundation. A.K.H. and P.L.G. acknowledge support from the NASA Astrophysics Theory Program. P.L.G. also acknowledges support from the National Science Foundation RUI program and the Michigan Space Grant Consortium. We thank Julie McEnery, Chuck Dermer, Kent Wood, Marius Potgieter, Driaan Bisschoff (and also acknowledge the late Okkie de Jager) for stimulating discussions. NR 131 TC 5 Z9 5 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 10 PY 2015 VL 807 IS 2 AR 130 DI 10.1088/0004-637X/807/2/130 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO2EB UT WOS:000358967000016 ER PT J AU Viall, NM Vourlidas, A AF Viall, Nicholeen M. Vourlidas, Angelos TI PERIODIC DENSITY STRUCTURES AND THE ORIGIN OF THE SLOW SOLAR WIND SO ASTROPHYSICAL JOURNAL LA English DT Article DE solar wind; Sun: corona; Sun: heliosphere ID CLIMATIC TIME-SERIES; HELIUM ABUNDANCE; MAGNETOHYDRODYNAMIC MODELS; CORONAL STREAMERS; WAVES; DRIVEN; CYCLE; EVOLUTION; LATITUDE; EJECTION AB The source of the slow solar wind has challenged scientists for years. Periodic density structures (PDSs), observed regularly in the solar wind at 1 AU, can be used to address this challenge. These structures have length scales of hundreds to several thousands of megameters and frequencies of tens to hundreds of minutes. Two lines of evidence indicate that PDSs are formed in the solar corona as part of the slow solar wind release and/or acceleration processes. The first is corresponding changes in compositional data in situ, and the second is PDSs observed in the inner Heliospheric Imaging data on board the Solar Terrestrial Relations Observatory (STEREO)/Sun Earth Connection Coronal and Heliospheric Investigation (SECCHI) suite. The periodic nature of these density structures is both a useful identifier as well as an important physical constraint on their origin. In this paper, we present the results of tracking periodic structures identified in the inner Heliospheric Imager in SECCHI back in time through the corresponding outer coronagraph (COR2) images. We demonstrate that the PDSs are formed around or below 2.5 solar radii-the inner edge of the COR2 field of view. We compute the occurrence rates of PDSs in 10 days of COR2 images both as a function of their periodicity and location in the solar corona, and we find that this set of PDSs occurs preferentially with a periodicity of similar to 90 minutes and occurs near streamers. Lastly, we show that their acceleration and expansion through COR2 is self-similar, thus their frequency is constant at distances beyond 2.5 solar radii. C1 [Viall, Nicholeen M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Vourlidas, Angelos] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. RP Viall, NM (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RI Vourlidas, Angelos/C-8231-2009; OI Vourlidas, Angelos/0000-0002-8164-5948; Viall, Nicholeen/0000-0003-1692-1704 FU NASA GI grant; NASA [S-136361Y] FX N.M.V. gratefully acknowledges the 2011 Structure of the Slow Solar Wind workshop organized by Joseph Borovsky. The work of N.M.V. was partially supported by a NASA GI grant. A.V. work was supported by NASA contract S-136361Y to NRL and various NASA Living-With-a-Star grants. We also thank the STEREO/SECCHI team for the use of the COR2 data. We thank G. Petrie for providing the PFSS data. NR 61 TC 6 Z9 6 U1 1 U2 10 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 10 PY 2015 VL 807 IS 2 AR 176 DI 10.1088/0004-637X/807/2/176 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO2EB UT WOS:000358967000062 ER PT J AU Marshall, FE Guillemot, L Harding, AK Martin, P Smith, DA AF Marshall, F. E. Guillemot, L. Harding, A. K. Martin, P. Smith, D. A. TI DISCOVERY OF A SPIN-DOWN STATE CHANGE IN THE LMC PULSAR B0540-69 SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE pulsars: individual (PSR B0540-69) ID LARGE-MAGELLANIC-CLOUD; 50 MILLISECOND PULSAR; PSR B0540-69; BRAKING INDEX; RAY; GLITCHES; RADIO; MAGNETOSPHERES; ROTATION; MISSION AB We report the discovery of a large, sudden, and persistent increase in the spin-down rate of B0540-69, a young pulsar in the Large Magellanic Cloud, using observations from the Swift and RXTE satellites. The relative increase in the spin-down rate nu of 36% is unprecedented for B0540-69. No accompanying change in the spin rate is seen, and no change is seen in the pulsed X-ray emission from B0540-69 following the change in the spin-down rate. Such large relative changes in the spin-down rate are seen in the recently discovered class of "intermittent pulsars," and we compare the properties of B0540-69 to such pulsars. We consider possible changes in the magnetosphere of the pulsar that could cause such a large change in the spin-down rate. C1 [Marshall, F. E.; Harding, A. K.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Guillemot, L.] Univ Orleans, CNRS, LPC2E, F-45071 Orleans, France. [Guillemot, L.] INSU, CNRS, Observ Paris, Stn Radioastron Nancay, F-18330 Nancay, France. [Martin, P.] UPS, CNRS, UMR5277, Inst Rech Astrophys & Planetol, F-31028 Toulouse 4, France. [Smith, D. A.] Univ Bordeaux 1, CNRS, IN2P3, Ctr Etud Nucl Bordeaux Gradignam, F-33175 Gradignan, France. RP Marshall, FE (reprint author), NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. EM frank.marshall@nasa.gov OI Smith, David/0000-0002-7833-0275 NR 29 TC 5 Z9 5 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD JUL 10 PY 2015 VL 807 IS 2 AR L27 DI 10.1088/2041-8205/807/2/L27 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CM8HC UT WOS:000357938600007 ER PT J AU Mukai, K Rana, V Bernardini, F de Martino, D AF Mukai, K. Rana, V. Bernardini, F. de Martino, D. TI UNAMBIGUOUS DETECTION OF REFLECTION IN MAGNETIC CATACLYSMIC VARIABLES: JOINT NuSTAR-XMM-NEWTON OBSERVATIONS OF THREE INTERMEDIATE POLARS SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE novae, cataclysmic variables; X-rays: binaries ID X-RAY-SPECTRUM; AM-HERCULIS; WHITE-DWARF; LIGHT CURVES; EMISSION; COMPLEX; SHOCK AB In magnetic cataclysmic variables (CVs), X-ray emission regions are located close to the white dwarf surface, which is expected to reflect a significant fraction of intrinsic X-rays above 10 keV, producing a Compton reflection hump. However, up to now, a secure detection of this effect in magnetic CVs has largely proved elusive because of the limited sensitivity of non-imaging X-ray detectors. Here we report our analysis of joint NuSTAR-XMM-Newton observations of three magnetic CVs, V709 Cas, NY Lup, and V1223 Sgr. The improved hard X-ray sensitivity of the imaging NuSTAR data has resulted in the first robust detection of Compton hump in all three objects, with amplitudes of similar to 1 or greater in NY Lup, and likely <1.0 in the other two. We also confirm earlier reports of a strong spin modulation above 10 keV in V709 Cas, and we report the first detection of small spin amplitudes in the others. We interpret this as due to different height of the X-ray emitting region among these objects. A height of similar to 0.2 white dwarf radii provides a plausible explanation for the low reflection amplitude of V709 Cas. Since emission regions above both poles are visible at certain spin phases, this can also explain the strong hard X-ray spin modulation. A shock height of similar to 0.05 white dwarf radii can explain our results on V1223 Sgr, while the shock height in NY Lup appears negligible. C1 [Mukai, K.] NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA. [Mukai, K.] NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, Greenbelt, MD 20771 USA. [Rana, V.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Bernardini, F.] New York Univ Abu Dhabi, Abu Dhabi, U Arab Emirates. [de Martino, D.] Osserv Astron Capodimonte, INAF, I-80131 Naples, Italy. [Mukai, K.] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA. RP Mukai, K (reprint author), NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA. EM Koji.Mukai@nasa.gov OI Bernardini, Federico/0000-0001-5326-2010; de Martino, Domitilla/0000-0002-5069-4202; Rana, Vikram/0000-0003-1703-8796; Mukai, Koji/0000-0002-8286-8094 FU NASA; NASA under XMM-Newton grant [NNX15AK63G]; ASI/INAF [I/037/12/0] FX This research has made use of data obtained with the NuSTAR mission, a project led by the California Institute of Technology (Caltech), managed by the Jet Propulsion Laboratory (JPL) and funded by NASA. We acknowledge financial support from NASA under XMM-Newton grant NNX15AK63G and from ASI/INAF contract I/037/12/0. NR 32 TC 5 Z9 5 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD JUL 10 PY 2015 VL 807 IS 2 AR L30 DI 10.1088/2041-8205/807/2/L30 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CM8HC UT WOS:000357938600010 ER PT J AU Huang, K Le Jeannic, H Ruaudel, J Verma, VB Shaw, MD Marsili, F Nam, SW Wu, E Zeng, H Jeong, YC Filip, R Morin, O Laurat, J AF Huang, K. Le Jeannic, H. Ruaudel, J. Verma, V. B. Shaw, M. D. Marsili, F. Nam, S. W. Wu, E. Zeng, H. Jeong, Y. -C. Filip, R. Morin, O. Laurat, J. TI Optical Synthesis of Large-Amplitude Squeezed Coherent-State Superpositions with Minimal Resources SO PHYSICAL REVIEW LETTERS LA English DT Article ID QUANTUM TELEPORTATION; HYBRID ENTANGLEMENT; GENERATION; PHOTONS AB We propose and experimentally realize a novel versatile protocol that allows the quantum state engineering of heralded optical coherent-state superpositions. This scheme relies on a two-mode squeezed state, linear mixing, and a n-photon detection. It is optimally using expensive non-Gaussian resources to build up only the key non-Gaussian part of the targeted state. In the experimental case of a two-photon detection based on high-efficiency superconducting nanowire single-photon detectors, the freely propagating state exhibits a 67% fidelity with a squeezed even coherent-state superposition with a size vertical bar alpha vertical bar(2) = 3. The demonstrated procedure and the achieved rate will facilitate the use of such superpositions in subsequent protocols, including fundamental tests and optical hybrid quantum information implementations. C1 [Huang, K.; Le Jeannic, H.; Ruaudel, J.; Jeong, Y. -C.; Morin, O.; Laurat, J.] UPMC, Univ Paris 04, ENS PSL Res Univ, Coll France,CNRS,Lab Kastler Brossel, F-75005 Paris, France. [Huang, K.; Wu, E.; Zeng, H.] E China Normal Univ, State Key Lab Precis Spect, Shanghai 200062, Peoples R China. [Verma, V. B.; Nam, S. W.] NIST, Boulder, CO 80305 USA. [Shaw, M. D.; Marsili, F.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Filip, R.] Palacky Univ, Dept Opt, Olomouc 77146, Czech Republic. RP Huang, K (reprint author), UPMC, Univ Paris 04, ENS PSL Res Univ, Coll France,CNRS,Lab Kastler Brossel, 4 Pl Jussieu, F-75005 Paris, France. EM julien.laurat@upmc.fr RI LAURAT, Julien /A-8542-2011; MORIN, Olivier/A-1075-2017 OI LAURAT, Julien /0000-0001-8318-6514; FU ERA-Net CHIST-ERA (QScale); European Research Council (Starting Grant HybridNet); Foundation for the Author of National Excellent Doctoral Dissertation of China [PY2012004]; China Scholarship Council; DARPA Information in a Photon (InPho) program; QUINESS program; Czech Science Foundation [GA14-36681G] FX This work was supported by the ERA-Net CHIST-ERA (QScale) and the European Research Council (Starting Grant HybridNet). 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. V. B. V. and S. W. N. acknowledge partial funding for detector development from the DARPA Information in a Photon (InPho) and QUINESS programs. K. H. was supported by the Foundation for the Author of National Excellent Doctoral Dissertation of China (No. PY2012004) and the China Scholarship Council, and R. F. by Grant No. GA14-36681G of the Czech Science Foundation. The authors also acknowledge the technical assistance provided by B. Huard's Quantum Electronics group at LPA, Paris. J. L. is a member of the Institut Universitaire de France. NR 41 TC 13 Z9 13 U1 5 U2 16 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 0031-9007 EI 1079-7114 J9 PHYS REV LETT JI Phys. Rev. Lett. PD JUL 9 PY 2015 VL 115 IS 2 AR 023602 DI 10.1103/PhysRevLett.115.023602 PG 6 WC Physics, Multidisciplinary SC Physics GA CM4HS UT WOS:000357646000001 PM 26207468 ER PT J AU Adams, T Leong, JR Slutsky, J Was, M Affeldt, C Degallaix, J Dooley, KL Grote, H Hild, S Luck, H Macleod, DM Nuttall, LK Prijatelj, M Schreiber, E Sorazu, B Strain, KA Sutton, PJ Vahlbruch, H Wittel, H Danzmann, K AF Adams, T. Leong, J. R. Slutsky, J. Was, M. Affeldt, C. Degallaix, J. Dooley, K. L. Grote, H. Hild, S. Lueck, H. Macleod, D. M. Nuttall, L. K. Prijatelj, M. Schreiber, E. Sorazu, B. Strain, K. A. Sutton, P. J. Vahlbruch, H. Wittel, H. Danzmann, K. TI Cost-benefit analysis for commissioning decisions in GEO600 SO CLASSICAL AND QUANTUM GRAVITY LA English DT Article DE gravitational waves; commissioning; detector characterization AB Gravitational wave (GW) interferometers are complex instruments, requiring years of commissioning to achieve the required sensitivities for the detection of GWs, of order less than or similar to 10(-21) in dimensionless detector strain, in the tens of Hz to several kHz frequency band. Investigations carried out by the GEO 600 detector characterization group have shown that detector characterization techniques are useful when planning for commissioning work. At the time of writing, GEO 600 is the only large scale laser interferometer currently in operation running with a high duty factor, similar to 70%, limited chiefly by the time spent commissioning the detector. The number of observable GW sources scales as the product of the volume of space to which the detector is sensitive and the observation time, so the goal of commissioning is to improve the detector sensitivity with the least possible detector down-time. We demonstrate a method for increasing the number of sources observable by such a detector, by assessing the severity of non-astrophysical noise contaminations to efficiently guide commissioning. This method will be particularly useful in the early stages and during the initial science runs of the aLIGO and adVirgo detectors, as they are brought up to design performance. C1 [Adams, T.; Was, M.] Univ Savoie, CNRS IN2P3, LAPP, F-74941 Annecy Le Vieux, France. [Adams, T.; Sutton, P. J.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Leong, J. R.; Slutsky, J.; Was, M.; Affeldt, C.; Dooley, K. L.; Grote, H.; Lueck, H.; Schreiber, E.; Vahlbruch, H.; Wittel, H.; Danzmann, K.] Albert Einstein Inst, Max Planck Inst Gravitationsphys, D-30167 Hannover, Germany. [Leong, J. R.; Slutsky, J.; Was, M.; Affeldt, C.; Dooley, K. L.; Grote, H.; Lueck, H.; Schreiber, E.; Vahlbruch, H.; Wittel, H.; Danzmann, K.] Leibniz Univ Hannover, D-30167 Hannover, Germany. [Slutsky, J.] NASA GSFC, CRESST, Greenbelt, MD 20771 USA. [Slutsky, J.] NASA GSFC, Gravitat Astrophys Lab, Greenbelt, MD 20771 USA. [Degallaix, J.] Univ Lyon, CNRS, IN2P3, LMA, F-69622 Lyon, France. [Hild, S.; Sorazu, B.; Strain, K. A.] Univ Glasgow, SUPA, Glasgow G12 8QQ, Lanark, Scotland. [Macleod, D. M.] Louisiana State Univ, Baton Rouge, LA 70803 USA. [Nuttall, L. K.] Univ Wisconsin, Milwaukee, WI 53201 USA. [Prijatelj, M.] European Gravitat Observ, I-56021 Pisa, Italy. RP Adams, T (reprint author), Univ Savoie, CNRS IN2P3, LAPP, F-74941 Annecy Le Vieux, France. EM thomas.adams@ligo.org RI Hild, Stefan/A-3864-2010; Strain, Kenneth/D-5236-2011; OI Strain, Kenneth/0000-0002-2066-5355; Sorazu, Borja/0000-0002-6178-3198 FU STFC [PP/F001096/1, ST/I000887/1]; STFC Long Term Attachment [ST/I505621/1] FX We would like to thank the LIGO scientific, Virgo, and GEO collaborations for providing a medium where stimulating discussions and analyses took place which have contributed to this work. In particular Sergey Kimenko, Gabriele Vedovato and Igor Yakushin from the coherent wave burst group ran the two detector network analysis mentioned in section 5.3. The aforementioned collaborations have also allowed the use of GEO 600 GW data published here. The Max Planck Society, Leibniz Universitt Hannover, the Science and Technology Facilities Council in the UK, the Bundesministerium fur Bildung und Forschung and the state of Lower Saxony in Germany, and the Volkswagen Foundation all made generous contributions which helped to make GEO 600 a reality. Many people over many years have also worked hard on the design and construction, as well as upgrades to GEO 600 that make it what it is today. The GEO 600 operators, in addition, play a large role in keeping GEO 600 operational. We also acknowledge the institutes out of which the authors work. This work was supported in part by STFC grant nos. PP/F001096/1 and ST/I000887/1 and by the STFC Long Term Attachment ST/I505621/1. This paper has been assigned LIGO Document No. P1300202. NR 18 TC 1 Z9 1 U1 0 U2 4 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 JUL 9 PY 2015 VL 32 IS 13 AR 135014 DI 10.1088/0264-9381/32/13/135014 PG 26 WC Astronomy & Astrophysics; Physics, Multidisciplinary; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA CL0KO UT WOS:000356631800017 ER PT J AU Gordon, PV Gotti, DJ Hegde, UG Hicks, MC Kulis, MJ Sivashinsky, GI AF Gordon, Peter V. Gotti, Daniel J. Hegde, Uday G. Hicks, Michael C. Kulis, Michael J. Sivashinsky, Gregory I. TI An elementary model for autoignition of laminar jets SO PROCEEDINGS OF THE ROYAL SOCIETY A-MATHEMATICAL PHYSICAL AND ENGINEERING SCIENCES LA English DT Article DE autoignition; hydrothermal flames; diffusion flames; heat equation; blow-up; thermal runaway ID PARABOLIC DIFFERENTIAL-EQUATIONS; DIFFUSION FLAMES; HYDROTHERMAL FLAMES; SUPERCRITICAL WATER; IGNITION; REACTOR; COMBUSTION AB In this paper, we formulate and analyse an elementary model for autoignition of cylindrical laminar jets of fuel injected into an oxidizing ambient at rest. This study is motivated by renewed interest in analysis of hydrothermal flames for which such configuration is common. As a result of our analysis, we obtain a sharp characterization of the autoignition position in terms of the principal physical and geometrical parameters of the problem. C1 [Gordon, Peter V.] Univ Akron, Dept Math, Akron, OH 44325 USA. [Gotti, Daniel J.] Univ Space Res Assoc, Cleveland, OH 44135 USA. [Hicks, Michael C.; Kulis, Michael J.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. [Hegde, Uday G.] Case Western Reserve Univ, Cleveland, OH 44106 USA. [Sivashinsky, Gregory I.] Tel Aviv Univ, Sch Math Sci, IL-69978 Tel Aviv, Israel. RP Gordon, PV (reprint author), Univ Akron, Dept Math, Akron, OH 44325 USA. EM pgordon@uakron.edu FU NASA Space Life and Physical Sciences Research and Applications Program; US-Israel Binational Science Foundation [2012057]; Israel Science Foundation [335/13]; Simons Foundation [317882] FX The work of D.J.G, U.G.H., M.C.H. and M.J.K. was supported by the NASA Space Life and Physical Sciences Research and Applications Program. The work of P.V.G. and G.I.S. was supported, in part, by the US-Israel Binational Science Foundation under grant no. 2012057. G.I.S. also acknowledges support of the Israel Science Foundation via grant no. 335/13. P.V.G. was also supported by grant no. 317882 from Simons Foundation. NR 27 TC 2 Z9 2 U1 1 U2 4 PU ROYAL SOC PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 1364-5021 EI 1471-2946 J9 P ROY SOC A-MATH PHY JI Proc. R. Soc. A-Math. Phys. Eng. Sci. PD JUL 8 PY 2015 VL 471 IS 2179 AR 20150059 DI 10.1098/rspa.2015.0059 PG 13 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CS1MP UT WOS:000361830300010 PM 26345080 ER PT J AU Bi, L Yang, P Kattawar, GW Mishchenko, MI AF Bi, Lei Yang, Ping Kattawar, George W. Mishchenko, Michael I. TI Optical tunneling by arbitrary macroscopic three-dimensional objects SO PHYSICAL REVIEW A LA English DT Article ID HIGH-FREQUENCY SCATTERING; ELECTROMAGNETIC-WAVES; MIE SCATTERING; DIFFRACTION; RAINBOW; SPHERE; LIGHT AB Electromagnetic wavefront portions grazing or nearly grazing the surface of a macroscopic particle contribute to the extinction of the incident radiation through a tunneling process similar to the scenario of barrier penetration in quantum mechanics. The aforesaid tunneling contribution, referred to as the edge effect, is critical to a correct depiction of the physical mechanism of electromagnetic extinction. Although an analytical solution for the edge effect in the case of a sphere has been reported in the literature, the counterparts for nonspherical particles remain unknown. The conventional curvature-based formalism of the edge effect breaks down in the case of faceted particles. This paper reports a method, based on the invariant imbedding principle and the Debye expansion technique, to accurately quantify the edge effect associated with an arbitrarily shaped three-dimensional object. The present method also provides a rigorous capability to facilitate the validation of various empirical approximations for electromagnetic extinction. Canonical results are presented to illustrate optical tunneling for two nonspherical geometries. C1 [Bi, Lei; Yang, Ping] Texas A&M Univ, Dept Atmospher Sci, College Stn, TX 77843 USA. [Yang, Ping; Kattawar, George W.] Texas A&M Univ, Dept Phys & Astron, College Stn, TX 77843 USA. [Mishchenko, Michael I.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. RP Yang, P (reprint author), Texas A&M Univ, Dept Atmospher Sci, College Stn, TX 77843 USA. EM pyang@tamu.edu RI Yang, Ping/B-4590-2011; Bi, Lei/B-9242-2011 FU NSF grant [AGS-1338440]; NASA grant [NNX11AK37G]; NASA Remote Sensing Theory program FX This study was supported by an NSF grant (AGS-1338440) and an NASA grant (NNX11AK37G). P.Y. and M.I.M. acknowledge support from the NASA Remote Sensing Theory program. NR 22 TC 2 Z9 2 U1 0 U2 8 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1050-2947 EI 1094-1622 J9 PHYS REV A JI Phys. Rev. A PD JUL 8 PY 2015 VL 92 IS 1 AR 013814 DI 10.1103/PhysRevA.92.013814 PG 8 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA CM4DI UT WOS:000357634000012 ER PT J AU Ko, MD Rim, T Kim, K Meyyappan, M Baek, CK AF Ko, Myung-Dong Rim, Taiuk Kim, Kihyun Meyyappan, M. Baek, Chang-Ki TI High efficiency silicon solar cell based on asymmetric nanowire SO SCIENTIFIC REPORTS LA English DT Article ID PHOTOVOLTAIC APPLICATIONS; OPTICAL-ABSORPTION; SI MICROWIRE; ARRAYS; ENHANCEMENT; PLANAR AB Improving the efficiency of solar cells through novel materials and devices is critical to realize the full potential of solar energy to meet the growing worldwide energy demands. We present here a highly efficient radial p-n junction silicon solar cell using an asymmetric nanowire structure with a shorter bottom core diameter than at the top. A maximum short circuit current density of 27.5 mA/ cm(2) and an efficiency of 7.53% were realized without anti-reflection coating. Changing the silicon nanowire (SiNW) structure from conventional symmetric to asymmetric nature improves the efficiency due to increased short circuit current density. From numerical simulation and measurement of the optical characteristics, the total reflection on the sidewalls is seen to increase the light trapping path and charge carrier generation in the radial junction of the asymmetric SiNW, yielding high external quantum efficiency and short circuit current density. The proposed asymmetric structure has great potential to effectively improve the efficiency of the SiNW solar cells. C1 [Ko, Myung-Dong; Baek, Chang-Ki] Pohang Univ Sci & Technol POSTECH, Dept Elect Engn, Pohang, Kyeongbuk, South Korea. [Rim, Taiuk; Kim, Kihyun; Meyyappan, M.; Baek, Chang-Ki] Pohang Univ Sci & Technol POSTECH, Dept Creat IT Engn, Pohang, Kyeongbuk, South Korea. [Rim, Taiuk; Kim, Kihyun; Meyyappan, M.; Baek, Chang-Ki] Pohang Univ Sci & Technol POSTECH, Future IT Innovat Lab, POSTECH I Lab, Pohang, Kyeongbuk, South Korea. [Meyyappan, M.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Baek, CK (reprint author), Pohang Univ Sci & Technol POSTECH, Dept Elect Engn, 77 Cheongam Ro, Pohang, Kyeongbuk, South Korea. EM baekck@postech.ac.kr FU MSIP (Ministry of Science, ICT and Future Planning), Korea, under the "ICT Consilience Creative Program" [IITP-2015-R0346-15-1007] FX This research was supported by the MSIP (Ministry of Science, ICT and Future Planning), Korea, under the "ICT Consilience Creative Program" (IITP-2015-R0346-15-1007) supervised by the IITP (Institute for Information & communications Technology Promotion). NR 19 TC 6 Z9 6 U1 4 U2 38 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 2045-2322 J9 SCI REP-UK JI Sci Rep PD JUL 8 PY 2015 VL 5 AR 11646 DI 10.1038/srep11646 PG 8 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CM3ID UT WOS:000357574500001 PM 26152914 ER PT J AU Hajra, R Tsurutani, BT Echer, E Gonzalez, WD Brum, CGM Vieira, LEA Santolik, O AF Hajra, Rajkumar Tsurutani, Bruce T. Echer, Ezequiel Gonzalez, Walter D. Brum, Christiano Garnett Marques Antunes Vieira, Luis Eduardo Santolik, Ondrej TI Relativistic electron acceleration during HILDCAA events: are precursor CIR magnetic storms important? SO EARTH PLANETS AND SPACE LA English DT Article DE HILDCAAs; High-speed streams; CIRs; Chorus plasma waves; Radiation belt; Magnetospheric relativistic electrons; Solar wind; Geomagnetic storms ID COROTATING INTERACTION REGIONS; RADIATION-BELT ELECTRONS; WHISTLER-MODE CHORUS; SOLAR-WIND CONTROL; GEOMAGNETIC-ACTIVITY; HIGH-INTENSITY; LONG-DURATION; RESONANT DIFFUSION; ALFVEN WAVES; MAGNETOSPHERE AB We present a comparative study of high-intensity long-duration continuous AE activity (HILDCAA) events, both isolated and those occurring in the "recovery phase" of geomagnetic storms induced by corotating interaction regions (CIRs). The aim of this study is to determine the difference, if any, in relativistic electron acceleration and magnetospheric energy deposition. All HILDCAA events in solar cycle 23 (from 1995 through 2008) are used in this study. Isolated HILDCAA events are characterized by enhanced fluxes of relativistic electrons compared to the pre-event flux levels. CIR magnetic storms followed by HILDCAA events show almost the same relativistic electron signatures. Cluster 1 spacecraft showed the presence of intense whistler-mode chorus waves in the outer magnetosphere during all HILDCAA intervals (when Cluster data were available). The storm-related HILDCAA events are characterized by slightly lower solar wind input energy and larger magnetospheric/ionospheric dissipation energy compared with the isolated events. A quantitative assessment shows that the mean ring current dissipation is similar to 34 % higher for the storm-related events relative to the isolated events, whereas Joule heating and auroral precipitation display no (statistically) distinguishable differences. On the average, the isolated events are found to be comparatively weaker and shorter than the storm-related events, although the geomagnetic characteristics of both classes of events bear no statistically significant difference. It is concluded that the CIR storms preceding the HILDCAAs have little to do with the acceleration of relativistic electrons. Our hypothesis is that similar to 10-100-keV electrons are sporadically injected into the magnetosphere during HILDCAA events, the anisotropic electrons continuously generate electromagnetic chorus plasma waves, and the chorus then continuously accelerates the high-energy portion of this electron spectrum to MeV energies. C1 [Hajra, Rajkumar; Echer, Ezequiel; Gonzalez, Walter D.; Antunes Vieira, Luis Eduardo] INPE, BR-12227010 Sao Jose Dos Campos, SP, Brazil. [Hajra, Rajkumar; Brum, Christiano Garnett Marques] Natl Astron & Ionosphere Ctr, Arecibo Observ, Space & Atmospher Sci Dept, Arecibo, PR 00613 USA. [Tsurutani, Bruce T.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Santolik, Ondrej] Inst Atmospher Phys AS CR, Prague, Czech Republic. RP Hajra, R (reprint author), INPE, Av Astronautas 1758, BR-12227010 Sao Jose Dos Campos, SP, Brazil. EM rajkumarhajra@yahoo.co.in RI Santolik, Ondrej/F-7766-2014; OI Hajra, Rajkumar/0000-0003-0447-1531 FU Fundacao de Amparo a Pesquisa do Estado de Sao Paulo (FAPESP); Brazilian CNPq [301233/2011-0]; National Science Foundation [1160876]; Premium Academiae [LH12231, LH14010] FX The work of RH is financially supported by Fundacao de Amparo a Pesquisa do Estado de Sao Paulo (FAPESP) through post-doctoral research fellowship at INPE. EE would like to thank to the Brazilian CNPq (301233/2011-0) agency for financial support. Portions of this research were performed at the Jet Propulsion Laboratory, California Institute of Technology under contract with NASA. The Arecibo Observatory is operated by SRI International in collaboration with the Universities Space Research Association and Universidade Metropolitana under a cooperative agreement with National Science Foundation, award number 1160876. OS acknowledges funding from Premium Academiae, and grants LH12231 and LH14010. NR 86 TC 5 Z9 5 U1 0 U2 9 PU SPRINGER HEIDELBERG PI HEIDELBERG PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY SN 1880-5981 J9 EARTH PLANETS SPACE JI Earth Planets Space PD JUL 7 PY 2015 VL 67 AR 109 DI 10.1186/s40623-015-0280-5 PG 11 WC Geosciences, Multidisciplinary SC Geology GA CN3IU UT WOS:000358319900001 ER PT J AU Li, WQ Beard, BL Johnson, CM AF Li, Weiqiang Beard, Brian L. Johnson, Clark M. TI Biologically recycled continental iron is a major component in banded iron formations SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE BIF; DIR; iron shuttle; Nd isotope; Fe isotope ID RARE-EARTH-ELEMENTS; WESTERN-AUSTRALIA; HAMERSLEY GROUP; SOUTH-AFRICA; GEOCHEMISTRY; SEAWATER; ORIGIN; DEPOSITION; SEDIMENTS; ISOTOPES AB Banded iron formations (BIFs) record a time of extensive Fe deposition in the Precambrian oceans, but the sources and pathways for metals in BIFs remain controversial. Here, we present Fe-and Nd-isotope data that indicate two sources of Fe for the large BIF units deposited 2.5 billion y ago. High-epsilon(Nd) and -delta Fe-56 signatures in some BIF samples record a hydrothermal component, but correlated decreases in epsilon(Nd)- and delta Fe-56 values reflect contributions from a continental component. The continental Fe source is best explained by Fe mobilization on the continental margin by microbial dissimilatory iron reduction (DIR) and confirms for the first time, to our knowledge, a microbially driven Fe shuttle for the largest BIFs on Earth. Detailed sampling at various scales shows that the proportions of hydrothermal and continental Fe sources were invariant over periods of 10(0)-10(3) y, indicating that there was no seasonal control, although Fe sources varied on longer timescales of 10(5)-10(6) y, suggesting a control by marine basin circulation. These results show that Fe sources and pathways for BIFs reflect the interplay between abiologic (hydrothermal) and biologic processes, where the latter reflects DIR that operated on a basin-wide scale in the Archean. C1 [Li, Weiqiang; Beard, Brian L.; Johnson, Clark M.] Univ Wisconsin, Dept Geosci, Madison, WI 53706 USA. [Li, Weiqiang; Beard, Brian L.; Johnson, Clark M.] NASA Astrobiol Inst, Madison, WI 53706 USA. [Li, Weiqiang] Nanjing Univ, State Key Lab Mineral Deposits Res, Sch Earth Sci & Engn, Nanjing 210093, Jiangsu, Peoples R China. RP Li, WQ (reprint author), Univ Wisconsin, Dept Geosci, Madison, WI 53706 USA. EM liweiqiang@nju.edu.cn RI Li, Weiqiang/D-2975-2011 OI Li, Weiqiang/0000-0003-2648-7630 FU NASA Astrobiology Institute; 1000 Talent Program of China FX This study benefited from discussions with Xinyuan Zheng, who also provided the compiled rare earth element data for modern midocean ridge hydrothermal vent fluids, and reviews by Kurt Konhauser and Balz Kamber. This study was supported by the NASA Astrobiology Institute. W.L. was supported by the 1000 Talent Program of China. NR 44 TC 16 Z9 16 U1 9 U2 43 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 JUL 7 PY 2015 VL 112 IS 27 BP 8193 EP 8198 DI 10.1073/pnas.1505515112 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CM2QU UT WOS:000357527600036 PM 26109570 ER PT J AU Seidler, RD Mulavara, AP Bloomberg, JJ Peters, BT AF Seidler, Rachael D. Mulavara, Ajitkumar P. Bloomberg, Jacob J. Peters, Brian T. TI Individual predictors of sensorimotor adaptability SO FRONTIERS IN SYSTEMS NEUROSCIENCE LA English DT Review DE adaptation; motor learning; predictors; genetics; motor cortex ID LONG-DURATION SPACEFLIGHT; NEUROMUSCULAR ACTIVATION PATTERNS; SPATIAL WORKING-MEMORY; RESTING HUMAN BRAIN; SIMPLE AIMING TASK; SPACE-FLIGHT; FUNCTIONAL CONNECTIVITY; TREADMILL WALKING; VISUOMOTOR ADAPTATION; ARM MOVEMENTS AB There are large individual variations in strategies and rates of sensorimotor adaptation to spaceflight. This is seen in both the magnitude of performance disruptions when crewmembers are first exposed to microgravity, and in the rate of re-adaptation when they return to Earth's gravitational environment. Understanding the sources of this variation can lead to a better understanding of the processes underlying adaptation, as well as provide insight into potential routes for facilitating performance of "slow adapters". Here we review the literature on brain, behavioral, and genetic predictors of motor learning, recovery of motor function following neural insult, and sensorimotor adaptation. For example, recent studies have identified specific genetic polymorphisms that are associated with faster adaptation on manual joystick tasks and faster recovery of function following a stroke. Moreover, the extent of recruitment of specific brain regions during learning and adaptation has been shown to be predictive of the magnitude of subsequent learning. We close with suggestions for forward work aimed at identifying predictors of spaceflight adaptation success. Identification of "slow adapters" prior to spaceflight exposure would allow for more targeted preflight training and/or provision of booster training and adaptation adjuncts during spaceflight. C1 [Seidler, Rachael D.] Univ Michigan, Psychol Kinesiol Neurosci Neuromotor Behav Lab, Ann Arbor, MI 48109 USA. [Mulavara, Ajitkumar P.] Univ Space Res Assoc, Houston, TX USA. [Mulavara, Ajitkumar P.; Bloomberg, Jacob J.] NASA, Johnson Space Center, Houston, TX USA. [Peters, Brian T.] Wyle Sci Technol & Engn Grp, Houston, TX USA. RP Seidler, RD (reprint author), Univ Michigan, Psychol Kinesiol Neurosci Neuromotor Behav Lab, 401 Washtenaw Ave, Ann Arbor, MI 48109 USA. EM rseidler@umich.edu NR 116 TC 1 Z9 1 U1 1 U2 4 PU FRONTIERS MEDIA SA PI LAUSANNE PA PO BOX 110, EPFL INNOVATION PARK, BUILDING I, LAUSANNE, 1015, SWITZERLAND SN 1662-5137 J9 FRONT SYST NEUROSCI JI Front. Syst. Neurosci. PD JUL 6 PY 2015 VL 9 AR 100 DI 10.3389/fnsys.2015.00100 PG 10 WC Neurosciences SC Neurosciences & Neurology GA CU9DY UT WOS:000363844900001 PM 26217197 ER PT J AU Kraemer, BM Hook, S Huttula, T Kotilainen, P O'Reilly, CM Peltonen, A Plisnier, PD Sarvala, J Tamatamah, R Vadeboncoeur, Y Wehrli, B McIntyre, PB AF Kraemer, Benjamin M. Hook, Simon Huttula, Timo Kotilainen, Pekka O'Reilly, Catherine M. Peltonen, Anu Plisnier, Pierre-Denis Sarvala, Jouko Tamatamah, Rashid Vadeboncoeur, Yvonne Wehrli, Bernhard McIntyre, Peter B. TI Century-Long Warming Trends in the Upper Water Column of Lake Tanganyika SO PLOS ONE LA English DT Article ID CLIMATE-CHANGE; TEMPERATURE-DEPENDENCE; EAST-AFRICA; IMPACTS; LIPIDS; TAHOE AB Lake Tanganyika, the deepest and most voluminous lake in Africa, has warmed over the last century in response to climate change. Separate analyses of surface warming rates estimated from in situ instruments, satellites, and a paleolimnological temperature proxy (TEX86) disagree, leaving uncertainty about the thermal sensitivity of Lake Tanganyika to climate change. Here, we use a comprehensive database of in situ temperature data from the top 100 meters of the water column that span the lake's seasonal range and lateral extent to demonstrate that long-term temperature trends in Lake Tanganyika depend strongly on depth, season, and latitude. The observed spatiotemporal variation in surface warming rates accounts for small differences between warming rate estimates from in situ instruments and satellite data. However, after accounting for spatiotemporal variation in temperature and warming rates, the TEX86 paleolimnological proxy yields lower surface temperatures (1.46 degrees C lower on average) and faster warming rates (by a factor of three) than in situ measurements. Based on the ecology of Thaumarchaeota (the microbes whose biomolecules are involved with generating the TEX86 proxy), we offer a reinterpretation of the TEX86 data from Lake Tanganyika as the temperature of the low-oxygen zone, rather than of the lake surface temperature as has been suggested previously. Our analyses provide a thorough accounting of spatiotemporal variation in warming rates, offering strong evidence that thermal and ecological shifts observed in this massive tropical lake over the last century are robust and in step with global climate change. C1 [Kraemer, Benjamin M.; McIntyre, Peter B.] Univ Wisconsin, Ctr Limnol, Madison, WI 53706 USA. [Hook, Simon] NASA, Jet Prop Lab, Pasadena, CA USA. [Huttula, Timo] Finnish Environm Inst, Freshwater Ctr, Jyvaskyla, Finland. [Kotilainen, Pekka] Finnish Environm Inst, Ctr Marine Res, Helsinki, Finland. [O'Reilly, Catherine M.] Illinois State Univ, Dept Geog Geol, Normal, IL 61761 USA. [Peltonen, Anu] Ctr Econ Dev Transport & Environm Pirkanmaa, Tampere, Finland. [Plisnier, Pierre-Denis] Royal Museum Cent Africa, Tervuren, Belgium. [Sarvala, Jouko] Univ Turku, Dept Biol, SF-20500 Turku, Finland. [Tamatamah, Rashid] Univ Dar Es Salaam, Dept Aquat Sci & Fisheries, Dar Es Salaam, Tanzania. [Vadeboncoeur, Yvonne] Wright State Univ, Dept Biol Sci, Dayton, OH 45435 USA. [Wehrli, Bernhard] Swiss Fed Inst Aquat Sci & Technol Eawag, Surface Waters Dept, Kastanienbaum, Switzerland. [Wehrli, Bernhard] ETH, Inst Biogeochem & Pollutant Dynam, Zurich, Switzerland. RP Kraemer, BM (reprint author), Univ Wisconsin, Ctr Limnol, Madison, WI 53706 USA. EM ben.m.kraemer@gmail.com RI Wehrli, Bernhard/A-4406-2013; Hook, Simon/D-5920-2016 OI Wehrli, Bernhard/0000-0001-7029-1972; Hook, Simon/0000-0002-0953-6165 FU National Science Foundation (NSF) [DEB-1030242, DEB-0842253]; Global Lake Temperature Collaboration (National Aeronautics and Space Administration (NASA) Research Opportunities in Space and Earth Sciences (ROSES) Grant, Institute of Agricultural and Natural Resources (IANR), University of Nebraska-Lincoln) [DEB-1147666] FX The authors are grateful for field research funding from the National Science Foundation (NSF) (DEB-1030242 and DEB-0842253), and encouragement from the Global Lake Temperature Collaboration (DEB-1147666, National Aeronautics and Space Administration (NASA) Research Opportunities in Space and Earth Sciences (ROSES) Grant, Institute of Agricultural and Natural Resources (IANR), University of Nebraska-Lincoln). NR 49 TC 8 Z9 8 U1 4 U2 21 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD JUL 6 PY 2015 VL 10 IS 7 AR e0132490 DI 10.1371/journal.pone.0132490 PG 17 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CN1DQ UT WOS:000358157600287 PM 26147964 ER PT J AU Barge, LM Abedian, Y Russell, MJ Doloboff, IJ Cartwright, JHE Kidd, RD Kanik, I AF Barge, Laura M. Abedian, Yeghegis Russell, Michael J. Doloboff, Ivria J. Cartwright, Julyan H. E. Kidd, Richard D. Kanik, Isik TI From Chemical Gardens to Fuel Cells: Generation of Electrical Potential and Current Across Self-Assembling Iron Mineral Membranes SO ANGEWANDTE CHEMIE-INTERNATIONAL EDITION LA English DT Article DE chemical gardens; hydrothermal chimneys; inorganic membranes; iron sulfide; membrane potentials ID GREEN RUST; LIFE; REDUCTION; EVOLUTION; ONSET AB We examine the electrochemical gradients that form across chemical garden membranes and investigate how self-assembling, out-of-equilibrium inorganic precipitatesmimicking in some ways those generated in far-from-equilibrium natural systemscan generate electrochemical energy. Measurements of electrical potential and current were made across membranes precipitated both by injection and solution interface methods in iron-sulfide and iron-hydroxide reaction systems. The battery-like nature of chemical gardens was demonstrated by linking multiple experiments in series which produced sufficient electrical energy to light an external light-emitting diode (LED). This work paves the way for determining relevant properties of geological precipitates that may have played a role in hydrothermal redox chemistry at the origin of life, and materials applications that utilize the electrochemical properties of self-organizing chemical systems. C1 [Barge, Laura M.; Abedian, Yeghegis; Russell, Michael J.; Doloboff, Ivria J.; Kidd, Richard D.; Kanik, Isik] NASA, Astrobiol Inst, JPL Icy Worlds, Pasadena, CA 91109 USA. [Barge, Laura M.; Abedian, Yeghegis; Russell, Michael J.; Doloboff, Ivria J.; Kidd, Richard D.; Kanik, Isik] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Cartwright, Julyan H. E.] Univ Granada, CSIC, Inst Andaluz Ciencias Tierra, Granada, Spain. RP Barge, LM (reprint author), NASA, Astrobiol Inst, JPL Icy Worlds, Pasadena, CA 91109 USA. EM laura.m.barge@jpl.nasa.gov RI Cartwright, Julyan/C-1387-2016 OI Cartwright, Julyan/0000-0001-7392-0957 FU NASA Astrobiology Institute (Icy Worlds); JPL Planetary Instrument Advanced Concept Development grant [S40AC1/42.14.101.07]; NAI through the NASA Postdoctoral Program; Spanish Ministerio de Ciencia e Innovacion [FIS2013-48444-C2-2-P] FX This research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration with support by the NASA Astrobiology Institute (Icy Worlds), and supported by a JPL Planetary Instrument Advanced Concept Development grant (grant number S40AC1/42.14.101.07). L.M.B. was supported by the NAI through the NASA Postdoctoral Program, administered by Oak Ridge Associated Universities through a contract with NASA. JHEC is supported by the Spanish Ministerio de Ciencia e Innovacion (grant number FIS2013-48444-C2-2-P). We acknowledge useful discussions with members of the NAI Thermodynamics, Disequilibrium, and Evolution Focus Group, and thank Dr. Bethany Theiling for the table-of-contents photo. Copyright 2015, all rights reserved. NR 23 TC 10 Z9 10 U1 4 U2 35 PU WILEY-V C H VERLAG GMBH PI WEINHEIM PA BOSCHSTRASSE 12, D-69469 WEINHEIM, GERMANY SN 1433-7851 EI 1521-3773 J9 ANGEW CHEM INT EDIT JI Angew. Chem.-Int. Edit. PD JUL 6 PY 2015 VL 54 IS 28 BP 8184 EP 8187 DI 10.1002/anie.201501663 PG 4 WC Chemistry, Multidisciplinary SC Chemistry GA CL8FO UT WOS:000357209000027 PM 25968422 ER PT J AU Weissman, P AF Weissman, Paul TI PLANETARY SCIENCE Sink holes and dust jets on comet 67P SO NATURE LA English DT Editorial Material AB Analyses of images taken by the Rosetta spacecraft reveal the complex landscape of a comet in rich detail. Close-up views of the surface indicate that some dust jets are being emitted from active pits undergoing sublimation. C1 NASA, Jet Prop Lab, Pasadena, CA 91109 USA. RP Weissman, P (reprint author), NASA, Jet Prop Lab, Pasadena, CA 91109 USA. EM weissman@jpl.nasa.gov NR 6 TC 0 Z9 0 U1 0 U2 5 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 EI 1476-4687 J9 NATURE JI Nature PD JUL 2 PY 2015 VL 523 IS 7558 BP 42 EP 43 PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CL7RN UT WOS:000357169500025 PM 26135444 ER PT J AU Angerhausen, D Mandushev, G Mandell, A Dunham, E Becklin, E Collins, P Hamilton, R Logsdon, SE McElwain, M McLean, I Pfuller, E Savage, M Shenoy, S Vacca, W Van Cleve, J Wolff, J AF Angerhausen, Daniel Mandushev, Georgi Mandell, Avi Dunham, Edward Becklin, Eric Collins, Peter Hamilton, Ryan Logsdon, Sarah E. McElwain, Michael McLean, Ian Pfueller, Enrico Savage, Maureen Shenoy, Sachindev Vacca, William Van Cleve, Jeff Wolff, Juergen TI First exoplanet transit observation with the Stratospheric Observatory for Infrared Astronomy: confirmation of Rayleigh scattering in HD 189733 b with the High-Speed Imaging Photometer for Occultations SO JOURNAL OF ASTRONOMICAL TELESCOPES INSTRUMENTS AND SYSTEMS LA English DT Article DE atmospheric characterization; individual HD 189733 b; SOFIA; High-Speed Imaging Photometer for Occultations; FLIPO; FLITECAM ID NICMOS TRANSMISSION SPECTROSCOPY; HUBBLE-SPACE-TELESCOPE; EXTRASOLAR PLANET; LIGHT CURVES; EMISSION-SPECTRUM; GIANT PLANETS; WATER-VAPOR; ATMOSPHERE; SOFIA; METALLICITY AB Here, we report on the first successful exoplanet transit observation with the Stratospheric Observatory for Infrared Astronomy (SOFIA). We observed a single transit of the hot Jupiter HD 189733 b, obtaining two simultaneous primary transit lightcurves in the B and z' bands as a demonstration of SOFIA's capability to perform absolute transit photometry. We present a detailed description of our data reduction, in particular, the correlation of photometric systematics with various in-flight parameters unique to the airborne observing environment. The derived transit depths at B and z' wavelengths confirm a previously reported slope in the optical transmission spectrum of HD 189733 b. Our results give new insights to the current discussion about the source of this Rayleigh scattering in the upper atmosphere and the question of fixed limb darkening coefficients in fitting routines. (C) 2015 Society of Photo-Optical Instrumentation Engineers (SPIE) C1 [Angerhausen, Daniel; Mandell, Avi; McElwain, Michael] NASA, Goddard Space Flight Ctr, Exoplanets & Stellar Astrophys Lab, Code 667, Greenbelt, MD 20771 USA. [Angerhausen, Daniel] Rensselaer Polytech Inst, Troy, NY 12180 USA. [Mandushev, Georgi; Dunham, Edward; Collins, Peter] Lowell Observ, Flagstaff, AZ 86001 USA. [Becklin, Eric; Logsdon, Sarah E.; McLean, Ian] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Becklin, Eric; Hamilton, Ryan; Savage, Maureen; Shenoy, Sachindev; Vacca, William; Van Cleve, Jeff] NASA, USRA SOFIA Sci Ctr, Ames Res Ctr, Moffett Field, CA 94035 USA. [Pfueller, Enrico; Wolff, Juergen] Univ Stuttgart, Deutsch SOFIA Inst, D-70569 Stuttgart, Germany. RP Angerhausen, D (reprint author), NASA, Goddard Space Flight Ctr, Exoplanets & Stellar Astrophys Lab, Code 667, Greenbelt, MD 20771 USA. EM daniel.angerhausen@nasa.gov NR 50 TC 1 Z9 1 U1 0 U2 0 PU SPIE-SOC PHOTO-OPTICAL INSTRUMENTATION ENGINEERS PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98225 USA SN 2329-4124 EI 2329-4221 J9 J ASTRON TELESC INST JI J. Astron. Telesc. Instrum. Syst. PD JUL PY 2015 VL 1 IS 3 AR 034002 DI 10.1117/1.JATIS.1.3.034002 PG 12 WC Engineering, Aerospace; Instruments & Instrumentation; Optics SC Engineering; Instruments & Instrumentation; Optics GA DJ4OV UT WOS:000374187000003 ER PT J AU Maeda, Y Ichihara, K Kan, H Shionome, Y Sato, T Sato, T Hayashi, T Ishida, M Namba, Y Takahashi, H Miyazawa, T Ishibashi, K Sakai, M Sugita, S Haba, Y Matsumoto, H Mori, H AF Maeda, Yoshitomo Ichihara, Kou Kan, Hiroaki Shionome, Yu Sato, Takuro Sato, Toshiki Hayashi, Takayuki Ishida, Manabu Namba, Yoshiharu Takahashi, Hideaki Miyazawa, Takuya Ishibashi, Kazunori Sakai, Michito Sugita, Satoshi Haba, Yoshito Matsumoto, Hironori Mori, Hideyuki TI Thermal stress test of the depth-graded platinum/carbon reflectors SO JOURNAL OF ASTRONOMICAL TELESCOPES INSTRUMENTS AND SYSTEMS LA English DT Article DE ASTRO-H; hard x-ray telescope; x-ray optics AB The ASTRO-H hard x-ray telescope (HXT) is designed to reflect hard x-rays with energies up to 80 keV. It will make use of thin-foil, multinested conical optics with depth-graded platinum/carbon (Pt/C) multilayers. We report on thermal stress tests of the HXT reflectors. The reflectors were fabricated on a heat-formed aluminum substrate of thickness gauged at 200 mu m of the alloy 5052. This was followed by an epoxy replication on Pt/C-sputtered smooth Pyrex cylindrical mandrels to acquire the x-ray reflective surface. For the thermal tests, the reflectors were maintained at three different temperatures: -5, 50, and 60 degrees C, respectively, for a week. We found that the surface of the reflectors were significantly changed at temperatures of 60 degrees C or higher. The change appears as wrinkles with a typical scale length of a few tens of microns. No changes on the surface were observed from the -5 and 50 degrees C samples. There was also no change in the x-ray reflectivity for these two temperatures. (C) The Authors. Published by SPIE under a Creative Commons Attribution 3.0 Unported License. C1 [Maeda, Yoshitomo; Ichihara, Kou; Shionome, Yu; Sato, Takuro; Sato, Toshiki; Ishida, Manabu] Japan Aerosp Explorat Agcy JAXA, Inst Space & Astronaut Sci, Chuo Ku, 3-1-1 Yoshinodai, Sagamihara, Kanagawa 2525210, Japan. [Maeda, Yoshitomo; Ishida, Manabu] SOKENDAI Grad Univ Adv Studies, Dept Space & Astronaut Sci, Sch Phys Sci, Chuo Ku, Sagamihara, Kanagawa 2525210, Japan. [Ichihara, Kou; Shionome, Yu; Sato, Takuro; Sato, Toshiki; Ishida, Manabu] Tokyo Metropolitan Univ, Dept Phys, Hachioji, Tokyo 1920397, Japan. [Kan, Hiroaki] Osaka Univ, Dept Earth & Space Sci, Grad Sch Sci, Toyonaka, Osaka 5600043, Japan. [Hayashi, Takayuki; Miyazawa, Takuya; Ishibashi, Kazunori; Matsumoto, Hironori; Mori, Hideyuki] Nagoya Univ, Dept Phys, Chikusa Ku, Nagoya, Aichi 4648602, Japan. [Namba, Yoshiharu; Takahashi, Hideaki] Chubu Univ, Dept Mech Engn, Kasugai, Aichi 4878501, Japan. [Sakai, Michito] Japan Aerosp Explorat Agcy JAXA, Res & Dev Directorate, Tsukuba, Ibaraki 3058505, Japan. [Sugita, Satoshi] Ehime Univ, Matsuyama, Ehime 7908577, Japan. [Haba, Yoshito] Aichi Univ Educ, Kariya, Aichi 4488542, Japan. [Mori, Hideyuki] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Maeda, Y (reprint author), Japan Aerosp Explorat Agcy JAXA, Inst Space & Astronaut Sci, Chuo Ku, 3-1-1 Yoshinodai, Sagamihara, Kanagawa 2525210, Japan. EM ymaeda@astro.isas.jaxa.jp NR 9 TC 0 Z9 0 U1 1 U2 2 PU SPIE-SOC PHOTO-OPTICAL INSTRUMENTATION ENGINEERS PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98225 USA SN 2329-4124 EI 2329-4221 J9 J ASTRON TELESC INST JI J. Astron. Telesc. Instrum. Syst. PD JUL PY 2015 VL 1 IS 3 AR 034001 DI 10.1117/1.JATIS.1.3.034001 PG 4 WC Engineering, Aerospace; Instruments & Instrumentation; Optics SC Engineering; Instruments & Instrumentation; Optics GA DJ4OV UT WOS:000374187000002 ER PT J AU Spangelo, SC Katti, RM Unwin, SC Bock, JJ AF Spangelo, Sara C. Katti, Raj M. Unwin, Stephen C. Bock, Jamie J. TI All-sky survey mission observing scenario strategy SO JOURNAL OF ASTRONOMICAL TELESCOPES INSTRUMENTS AND SYSTEMS LA English DT Article DE all-sky survey; observing strategy; scheduling; SPHEREx AB This paper develops an observing strategy for space missions performing all-sky surveys, where a single spacecraft maps the celestial sphere subject to realistic constraints. The strategy is flexible, accommodates targeted observations of specific areas of the sky, and achieves the desired trade-off between survey goals. This paper focuses on missions operating in low Earth orbit with interactive and dynamic thermal and stray-light constraints due to the Sun, Earth, and Moon. The approach is applicable to broader mission classes, such as those that operate in different orbits or that survey the Earth. First, the instrument and spacecraft configuration is optimized to enable visibility of the targeted observations throughout the year. Second, a constraint-based strategy is presented for scheduling the observations throughout the year subject to a simplified subset of the constraints. Third, a heuristic-based scheduling algorithm is developed to assign the all-sky observations over short planning horizons. The constraint-based approach guarantees solution feasibility. The approach is applied to the proposed SPHEREx mission, which includes coverage of the north and south celestial poles, galactic plane, and a uniform coverage all-sky survey that maps the entire celestial sphere twice per year. Visualizations demonstrate how the all-sky survey achieves its redundancy requirements over time. (C) 2015 Society of Photo-Optical Instrumentation Engineers (SPIE) C1 [Spangelo, Sara C.; Unwin, Stephen C.; Bock, Jamie J.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Katti, Raj M.; Bock, Jamie J.] CALTECH, Pasadena, CA 91125 USA. RP Spangelo, SC (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Sara.Spangelo@jpl.nasa.gov NR 9 TC 0 Z9 0 U1 1 U2 1 PU SPIE-SOC PHOTO-OPTICAL INSTRUMENTATION ENGINEERS PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98225 USA SN 2329-4124 EI 2329-4221 J9 J ASTRON TELESC INST JI J. Astron. Telesc. Instrum. Syst. PD JUL PY 2015 VL 1 IS 3 AR 037001 DI 10.1117/1.JATIS.1.3.037001 PG 11 WC Engineering, Aerospace; Instruments & Instrumentation; Optics SC Engineering; Instruments & Instrumentation; Optics GA DJ4OV UT WOS:000374187000009 ER PT J AU Sugai, H Tamura, N Karoji, H Shimono, A Takato, N Kimura, M Ohyama, Y Ueda, A Aghazarian, H de Arruda, MV Barkhouser, RH Bennett, CL Bickerton, S Bozier, A Braun, DF Bui, K Capocasale, CM Carr, MA Castilho, B Chang, YC Chen, HY Chou, RCY Dawson, OR Dekany, RG Ek, EM Ellis, RS English, RJ Ferrand, D Ferreira, D Fisher, CD Golebiowski, M Gunn, JE Hart, M Heckman, TM Ho, PTP Hope, S Hovland, LE Hsu, SF Hu, YS Huang, PJ Jaquet, M Karr, JE Kempenaar, JG King, ME Le Fevre, O Le Mignant, D Ling, HH Loomis, C Lupton, RH Madec, F Mao, P Marrara, LS Menard, B Morantz, C Murayama, H Murray, GJ de Oliveira, AC de Oliveira, CM de Oliveira, LS Orndorff, JD Vilaca, RD Partos, EJ Pascal, S Pegot-Ogier, T Reiley, DJ Riddle, R Santos, L dos Santos, JB Schwochert, MA Seiffert, MD Smee, SA Smith, RM Steinkraus, RE Sodre, L Spergel, DN Surace, C Tresse, L Vidal, C Vives, S Wang, SY Wen, CY Wu, AC Wyse, R Yan, CH AF Sugai, Hajime Tamura, Naoyuki Karoji, Hiroshi Shimono, Atsushi Takato, Naruhisa Kimura, Masahiko Ohyama, Youichi Ueda, Akitoshi Aghazarian, Hrand de Arruda, Marcio Vital Barkhouser, Robert H. Bennett, Charles L. Bickerton, Steve Bozier, Alexandre Braun, David F. Bui, Khanh Capocasale, Christopher M. Carr, Michael A. Castilho, Bruno Chang, Yin-Chang Chen, Hsin-Yo Chou, Richard C. Y. Dawson, Olivia R. Dekany, Richard G. Ek, Eric M. Ellis, Richard S. English, Robin J. Ferrand, Didier Ferreira, Decio Fisher, Charles D. Golebiowski, Mirek Gunn, James E. Hart, Murdock Heckman, Timothy M. Ho, Paul T. P. Hope, Stephen Hovland, Larry E. Hsu, Shu-Fu Hu, Yen-Shan Huang, Pin Jie Jaquet, Marc Karr, Jennifer E. Kempenaar, Jason G. King, Matthew E. Le Fevre, Olivier Le Mignant, David Ling, Hung-Hsu Loomis, Craig Lupton, Robert H. Madec, Fabrice Mao, Peter Marrara, Lucas Souza Menard, Brice Morantz, Chaz Murayama, Hitoshi Murray, Graham J. de Oliveira, Antonio Cesar de Oliveira, Claudia Mendes de Oliveira, Ligia Souza Orndorff, Joe D. Vilaca, Rodrigo de Paiva Partos, Eamon J. Pascal, Sandrine Pegot-Ogier, Thomas Reiley, Daniel J. Riddle, Reed Santos, Leandro dos Santos, Jesulino Bispo Schwochert, Mark A. Seiffert, Michael D. Smee, Stephen A. Smith, Roger M. Steinkraus, Ronald E. Sodre, Laerte, Jr. Spergel, David N. Surace, Christian Tresse, Laurence Vidal, Clement Vives, Sebastien Wang, Shiang-Yu Wen, Chih-Yi Wu, Amy C. Wyse, Rosie Yan, Chi-Hung TI Prime Focus Spectrograph for the Subaru telescope: massively multiplexed optical and near-infrared fiber spectrograph SO JOURNAL OF ASTRONOMICAL TELESCOPES INSTRUMENTS AND SYSTEMS LA English DT Article DE spectrographs; fiber applications; optical systems; infrared systems; astronomy ID EXCHANGER; SYSTEM AB The Prime Focus Spectrograph (PFS) is an optical/near-infrared multifiber spectrograph with 2394 science fibers distributed across a 1.3-deg diameter field of view at the Subaru 8.2-m telescope. The wide wavelength coverage from 0.38 mu m to 1.26 mu m, with a resolving power of 3000, simultaneously strengthens its ability to target three main survey programs: cosmology, galactic archaeology and galaxy/AGN evolution. A medium resolution mode with a resolving power of 5000 for 0.71 mu m to 0.89 mu m will also be available by simply exchanging dispersers. We highlight some of the technological aspects of the design. To transform the telescope focal ratio, a broad-band coated microlens is glued to each fiber tip. A higher transmission fiber is selected for the longest part of the cable system, optimizing overall throughput; a fiber with low focal ratio degradation is selected for the fiber-positioner and fiber-slit components, minimizing the effects of fiber movements and fiber bending. Fiber positioning will be performed by a positioner consisting of two stages of piezo-electric rotary motors. The positions of these motors are measured by taking an image of artificially back-illuminated fibers with the metrology camera located in the Cassegrain container; the fibers are placed in the proper location by iteratively measuring and then adjusting the positions of the motors. Target light reaches one of the four identical fast-Schmidt spectrograph modules, each with three arms. The PFS project has passed several project-wide design reviews and is now in the construction phase. (C) The Authors. Published by SPIE under a Creative Commons Attribution 3.0 Unported License. C1 [Sugai, Hajime; Tamura, Naoyuki; Karoji, Hiroshi; Shimono, Atsushi; Bickerton, Steve; Murayama, Hitoshi] Univ Tokyo, Kavli Inst Phys & Math Universe WPI, 5-1-5 Kashiwanoha, Kashiwa, Chiba 2778583, Japan. [Takato, Naruhisa] Natl Astron Observ Japan, Subaru Telescope, 650 North Aohoku Pl, Hilo, HI 96720 USA. [Kimura, Masahiko; Ohyama, Youichi; Chang, Yin-Chang; Chen, Hsin-Yo; Chou, Richard C. Y.; Ho, Paul T. P.; Hsu, Shu-Fu; Hu, Yen-Shan; Huang, Pin Jie; Karr, Jennifer E.; Ling, Hung-Hsu; Wang, Shiang-Yu; Wen, Chih-Yi; Yan, Chi-Hung] Acad Sinica, Inst Astron & Astrophys, POB 23-141, Taipei, Taiwan. [Ueda, Akitoshi] Natl Astron Observ Japan, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan. [Aghazarian, Hrand; Braun, David F.; Capocasale, Christopher M.; Dawson, Olivia R.; Ek, Eric M.; English, Robin J.; Fisher, Charles D.; Hovland, Larry E.; Kempenaar, Jason G.; King, Matthew E.; Morantz, Chaz; Partos, Eamon J.; Schwochert, Mark A.; Seiffert, Michael D.; Steinkraus, Ronald E.; Wu, Amy C.] Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [de Arruda, Marcio Vital; Castilho, Bruno; Ferreira, Decio; Marrara, Lucas Souza; de Oliveira, Antonio Cesar; de Oliveira, Ligia Souza; Vilaca, Rodrigo de Paiva; Santos, Leandro; dos Santos, Jesulino Bispo] MCTI, Lab Nacl Astrofis, Bairro Nacoes, Rua Estados Unidos 154, Itajuba, MG, Brazil. [Barkhouser, Robert H.; Bennett, Charles L.; Golebiowski, Mirek; Hart, Murdock; Heckman, Timothy M.; Hope, Stephen; Menard, Brice; Orndorff, Joe D.; Smee, Stephen A.; Wyse, Rosie] Johns Hopkins Univ, Dept Phys & Astron, 3400 North Charles St, Baltimore, MD 21218 USA. [Bozier, Alexandre; Ferrand, Didier; Jaquet, Marc; Le Fevre, Olivier; Le Mignant, David; Madec, Fabrice; Pascal, Sandrine; Pegot-Ogier, Thomas; Surace, Christian; Tresse, Laurence; Vidal, Clement; Vives, Sebastien] Aix Marseille Univ, CNRS, LAM Lab Astrophys Marseille, UMR 7326, F-13388 Marseille, France. [Bui, Khanh; Murray, Graham J.] CALTECH, Dept Astron, 1200 East Calif Blvd, Pasadena, CA 91125 USA. [Carr, Michael A.; Gunn, James E.; Loomis, Craig; Lupton, Robert H.; Spergel, David N.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Dekany, Richard G.; Smith, Roger M.] Caltech Opt Observ, 1201 East Calif Blvd, Pasadena, CA 91125 USA. [Bui, Khanh; Murray, Graham J.] Univ Durham, Ctr Adv Instrumentat, Dept Phys, Rochester Bldg,South Rd, Durham DH1 3LE, England. [de Oliveira, Claudia Mendes; Sodre, Laerte, Jr.] Univ Sao Paulo, Inst Astron Geofis & Ciencias Atmosfer, Rua Matao,1226 Cidade Univ, BR-05508090 Sao Paulo, Brazil. RP Sugai, H (reprint author), Univ Tokyo, Kavli Inst Phys & Math Universe WPI, 5-1-5 Kashiwanoha, Kashiwa, Chiba 2778583, Japan. EM hajime.sugai@ipmu.jp RI Sodre, Laerte/P-6045-2016 OI Sodre, Laerte/0000-0002-3876-268X NR 28 TC 8 Z9 8 U1 1 U2 1 PU SPIE-SOC PHOTO-OPTICAL INSTRUMENTATION ENGINEERS PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98225 USA SN 2329-4124 EI 2329-4221 J9 J ASTRON TELESC INST JI J. Astron. Telesc. Instrum. Syst. PD JUL PY 2015 VL 1 IS 3 AR UNSP 035001 DI 10.1117/1.JATIS.1.3.035001 PG 11 WC Engineering, Aerospace; Instruments & Instrumentation; Optics SC Engineering; Instruments & Instrumentation; Optics GA DJ4OV UT WOS:000374187000007 ER PT J AU Drob, DP Emmert, JT Meriwether, JW Makela, JJ Doornbos, E Conde, M Hernandez, G Noto, J Zawdie, KA McDonald, SE Huba, JD Klenzing, JH AF Drob, Douglas P. Emmert, John T. Meriwether, John W. Makela, Jonathan J. Doornbos, Eelco Conde, Mark Hernandez, Gonzalo Noto, John Zawdie, Katherine A. McDonald, Sarah E. Huba, Joe D. Klenzing, Jeff H. TI An update to the Horizontal Wind Model (HWM): The quiet time thermosphere SO EARTH AND SPACE SCIENCE LA English DT Article ID INCOHERENT-SCATTER RADAR; NEUTRAL WINDS; F-REGION; GLOBAL-MODEL; DYNAMICS EXPLORER; SOLAR MINIMUM; IONOSPHERE; EQUATORIAL; SATELLITE; TEMPERATURES AB The Horizontal Wind Model (HWM) has been updated in the thermosphere with new observations and formulation changes. These new data are ground-based 630 nm Fabry-Perot Interferometer (FPI) measurements in the equatorial and polar regions, as well as cross-track winds from the Gravity Field and Steady State Ocean Circulation Explorer (GOCE) satellite. The GOCE wind observations provide valuable wind data in the twilight regions. The ground-based FPI measurements fill latitudinal data gaps in the prior observational database. Construction of this reference model also provides the opportunity to compare these new measurements. The resulting update (HWM14) provides an improved time-dependent, observationally based, global empirical specification of the upper atmospheric general circulation patterns and migrating tides. In basic agreement with existing accepted theoretical knowledge of the thermosphere general circulation, additional calculations indicate that the empirical wind specifications are self-consistent with climatological ionosphere plasma distribution and electric field patterns. C1 [Drob, Douglas P.; Emmert, John T.; Zawdie, Katherine A.; McDonald, Sarah E.] Naval Res Lab, Space Sci Div, Washington, DC 20375 USA. [Meriwether, John W.] Clemson Univ, Dept Phys & Astron, Clemson, SC 29634 USA. [Makela, Jonathan J.] Univ Illinois, Dept Elect & Comp Engn, Urbana, IL USA. [Doornbos, Eelco] Delft Univ Technol, Dept Earth Observat & Space Syst, Delft, Netherlands. [Conde, Mark] Univ Alaska Fairbanks, Inst Geophys, Fairbanks, AK 99775 USA. [Hernandez, Gonzalo] Univ Washington, Dept Earth & Space Sci, Seattle, WA 98195 USA. [Noto, John] Sci Solut Inc, Chelmsford, MA USA. [Huba, Joe D.] Naval Res Lab, Plasma Phys Div, Washington, DC 20375 USA. [Klenzing, Jeff H.] NASA, Goddard Space Flight Ctr, Space Weather Lab, Greenbelt, MD USA. RP Drob, DP (reprint author), Naval Res Lab, Space Sci Div, Washington, DC 20375 USA. EM douglas.drob@nrl.navy.mil OI Hernandez, Gonzalo/0000-0003-4245-8696; Doornbos, Eelco/0000-0002-9790-8546 NR 71 TC 34 Z9 34 U1 1 U2 3 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2333-5084 J9 Earth Space Sci JI Earth Space Sci. PD JUL PY 2015 VL 2 IS 7 BP 301 EP 319 DI 10.1002/2014EA000089 PG 19 WC Geosciences, Multidisciplinary SC Geology GA DE6NJ UT WOS:000370750300006 ER PT J AU Jain, RK Lim, JW Jayaraman, B AF Jain, Rohit K. Lim, Joon W. Jayaraman, Buvana TI Modular Multisolver Approach for Efficient High-Fidelity Simulation of the HART II Rotor SO JOURNAL OF THE AMERICAN HELICOPTER SOCIETY LA English DT Article; Proceedings Paper CT 5th Decennial-American-Helicopter-Society Aeromechanics Specialists' Conference CY JAN 22-24, 2014 CL San Francisco, CA SP Decennial Amer Helicopter Soc AB High-resolution computational fluid dynamics simulations of the Higher-harmonic Aeroacoustics Rotor Test (HART) II rotor are performed using the U.S. Department of Defense Computational Research and Engineering Acquisition Tools and Environments-Air Vehicles (CREATE (TM)-AV) Helios software. The newly added triple-mesh capability has been utilized for computational efficiency. Rotor blades are modeled using high-resolution structured and unstructured meshes, the fuselage and hub are modeled using unstructured meshes, and the rotor wake region is modeled using high-resolution Cartesian meshes. Predictions for tip vortex strength and position and airloads are validated, and marked improvements over previous computational investigations are demonstrated. C1 [Jain, Rohit K.; Lim, Joon W.] US Army Aviat Dev Directorate AFDD, Aviat & Missile Res Dev & Engn Ctr, Res Dev & Engn Command RDECOM, Moffett Field, CA USA. [Jayaraman, Buvana] Sci & Technol Corp, Ames Res Ctr, Moffett Field, CA USA. RP Jain, RK (reprint author), US Army Aviat Dev Directorate AFDD, Aviat & Missile Res Dev & Engn Ctr, Res Dev & Engn Command RDECOM, Moffett Field, CA USA. EM rkj238@gmail.com NR 21 TC 0 Z9 0 U1 0 U2 0 PU AMER HELICOPTER SOC INC PI ALEXANDRIA PA 217 N WASHINGTON ST, ALEXANDRIA, VA 22314 USA SN 0002-8711 EI 2161-6027 J9 J AM HELICOPTER SOC JI J. Am. Helicopter Soc. PD JUL PY 2015 VL 60 IS 3 AR 032001 DI 10.4050/JAHS.60.032001 PG 11 WC Engineering, Aerospace SC Engineering GA DE1LJ UT WOS:000370388200001 ER PT J AU Ramasamy, M AF Ramasamy, Manikandan TI Hover Performance Measurements Toward Understanding Aerodynamic Interference in Coaxial, Tandem, and Tilt Rotors SO JOURNAL OF THE AMERICAN HELICOPTER SOCIETY LA English DT Article AB The aerodynamic interference between rotors in a multirotor system in hover was analyzed using a series of experiments. First, single-rotor measurements were acquired over a wide range of test conditions by varying thrust, tip speed, and number of blades (two to six). Next, parametric studies were conducted methodically on torque-balanced coaxial-, tandem-, and tilt rotors. For coaxial rotors, the effects of axial separation distance, blade twist distribution, and rotor rotation direction on the system performance were studied. For the tandem rotors, the effect of overlap between rotors on the system performance was measured using untwisted and twisted blades. A unique aspect of the experiment was the ability to measure the performance of the individual rotors even when they were operated as part of a torque-balanced multirotor system. The multirotor measurements, when compared with isolated single-rotor measurements, revealed the influence of one rotor on the other, thereby enabling various interference loss factors to be quantified. Momentum theory and blade-element momentum theory were used to understand and explain the measurements. C1 [Ramasamy, Manikandan] NASA, Ames Res Ctr, UARC, Moffett Field, CA 94035 USA. RP Ramasamy, M (reprint author), NASA, Ames Res Ctr, UARC, Moffett Field, CA 94035 USA. EM manikandan.ramasamy.civ@mail.mil NR 32 TC 2 Z9 2 U1 2 U2 3 PU AMER HELICOPTER SOC INC PI ALEXANDRIA PA 217 N WASHINGTON ST, ALEXANDRIA, VA 22314 USA SN 0002-8711 EI 2161-6027 J9 J AM HELICOPTER SOC JI J. Am. Helicopter Soc. PD JUL PY 2015 VL 60 IS 3 AR 032005 DI 10.4050/JAHS.60.032005 PG 17 WC Engineering, Aerospace SC Engineering GA DE1LJ UT WOS:000370388200005 ER PT J AU Gange, G Navas, JA Schachte, P Sondergaard, H Stuckey, PJ AF Gange, Graeme Navas, Jorge A. Schachte, Peter Sondergaard, Harald Stuckey, Peter J. TI Horn clauses as an intermediate representation for program analysis and transformation SO THEORY AND PRACTICE OF LOGIC PROGRAMMING LA English DT Article; Proceedings Paper CT 31st International Conference on Logic Programming (ICLP) Co-located with the 21st International Conference on Principles and Practice of Constraint Programming (CP) CY AUG 31-SEP 04, 2015 CL Cork, IRELAND SP Associat Log Programming, European Coordinating Comm Artificial Intelligence, Insight Ctr Data Analyt, Sci Fdn Ireland, Springer, Univ Coll Cork DE compilers; control flow graphs; intermediate representation; program analysis and transformation; SSA ID SINGLE ASSIGNMENT FORM; MODEL CHECKING; CLP; SSA AB Many recent analyses for conventional imperative programs begin by transforming programs into logic programs, capitalising on existing LP analyses and simple LP semantics. We propose using logic programs as an intermediate program representation throughout the compilation process. With restrictions ensuring determinism and single-modedness, a logic program can easily be transformed to machine language or other low-level language, while maintaining the simple semantics that makes it suitable as a language for program analysis and transformation. We present a simple LP language that enforces determinism and single-modedness, and show that it makes a convenient program representation for analysis and transformation. C1 [Gange, Graeme; Schachte, Peter; Sondergaard, Harald; Stuckey, Peter J.] Univ Melbourne, Dept Comp & Informat Syst, Melbourne, Vic 3010, Australia. [Navas, Jorge A.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Gange, G (reprint author), Univ Melbourne, Dept Comp & Informat Syst, Melbourne, Vic 3010, Australia. EM gkgange@unimelb.edu.au; jorge.a.navaslaserna@nasa.gov; schachte@unimelb.edu.au; harald@unimelb.edu.au; pstuckey@unimelb.edu.au RI Schachte, Peter/H-4848-2016; OI Schachte, Peter/0000-0001-5959-3769; Gange, Graeme/0000-0002-1354-431X; Sondergaard, Harald/0000-0002-2352-1883 FU Australian Research Council [DP140102194] FX This work was supported by the Australian Research Council through Discovery Project Grant DP140102194. NR 30 TC 0 Z9 0 U1 0 U2 0 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 1471-0684 EI 1475-3081 J9 THEOR PRACT LOG PROG JI Theory Pract. Log. Program. PD JUL PY 2015 VL 15 SI SI BP 526 EP 542 DI 10.1017/S1471068415000204 PN 4-5 PG 17 WC Computer Science, Software Engineering; Computer Science, Theory & Methods; Logic SC Computer Science; Science & Technology - Other Topics GA DA3JE UT WOS:000367692200009 ER PT J AU Burcar, BT Barge, LM Trail, D Watson, EB Russell, MJ McGown, LB AF Burcar, Bradley T. Barge, Laura M. Trail, Dustin Watson, E. Bruce Russell, Michael J. McGown, Linda B. TI RNA Oligomerization in Laboratory Analogues of Alkaline Hydrothermal Vent Systems SO ASTROBIOLOGY LA English DT Article DE RNA world; Hydrothermal systems; Prebiotic chemistry; Nucleic acids; Mass spectrometry ID MONTMORILLONITE-CATALYZED FORMATION; CHEMICAL GARDENS; LIFE; ORIGIN; OLIGONUCLEOTIDES; NUCLEOTIDES; HYDROLYSIS; WORLD; RIBONUCLEOTIDES; SERPENTINITE AB Discovering pathways leading to long-chain RNA formation under feasible prebiotic conditions is an essential step toward demonstrating the viability of the RNA World hypothesis. Intensive research efforts have provided evidence of RNA oligomerization by using circular ribonucleotides, imidazole-activated ribonucleotides with montmorillonite catalyst, and ribonucleotides in the presence of lipids. Additionally, mineral surfaces such as borates, apatite, and calcite have been shown to catalyze the formation of small organic compounds from inorganic precursors (Cleaves, 2008), pointing to possible geological sites for the origins of life. Indeed, the catalytic properties of these particular minerals provide compelling evidence for alkaline hydrothermal vents as a potential site for the origins of life since, at these vents, large metal-rich chimney structures can form that have been shown to be energetically favorable to diverse forms of life. Here, we test the ability of iron- and sulfur-rich chimneys to support RNA oligomerization reactions using imidazole-activated and non-activated ribonucleotides. The chimneys were synthesized in the laboratory in aqueous ocean solutions under conditions consistent with current understanding of early Earth. Effects of elemental composition, pH, inclusion of catalytic montmorillonite clay, doping of chimneys with small organic compounds, and in situ ribonucleotide activation on RNA polymerization were investigated. These experiments, under certain conditions, showed successful dimerization by using unmodified ribonucleotides, with the generation of RNA oligomers up to 4 units in length when imidazole-activated ribonucleotides were used instead. Elemental analysis of the chimney precipitates and the reaction solutions showed that most of the metal cations that were determined were preferentially partitioned into the chimneys. C1 [Burcar, Bradley T.; Trail, Dustin; Watson, E. Bruce; McGown, Linda B.] Rensselaer Polytech Inst, New York Ctr Astrobiol, Troy, NY 12180 USA. [Burcar, Bradley T.; McGown, Linda B.] Rensselaer Polytech Inst, Dept Chem & Chem Biol, Troy, NY 12180 USA. [Barge, Laura M.; Russell, Michael J.] CALTECH, Jet Prop Lab, NASA, Pasadena, CA USA. [Barge, Laura M.; Russell, Michael J.] Icy Worlds, NASA Astrobiol Inst, Mountain View, CA USA. [Trail, Dustin; Watson, E. Bruce] Rensselaer Polytech Inst, Sch Sci, Dept Earth & Environm Sci, Troy, NY 12180 USA. RP McGown, LB (reprint author), Rensselaer Polytech Inst, Dept Chem & Chem Biol, 120 Cogswell 110 8th St, Troy, NY 12180 USA. EM mcgowl@rpi.edu FU NASA Astrobiology Institute (NAI) through New York Center for Astrobiology at Rensselaer Polytechnic Institute [NNA09-DA80A]; Icy Worlds team at NASA's Jet Propulsion Laboratory; NAI through Astrobiology Program Early Career Collaboration Award; RPI's James P. Ferris Fellowship in Astrobiology; NAI through the NASA Postdoctoral Program FX This research was funded by the NASA Astrobiology Institute (NAI) through the New York Center for Astrobiology at Rensselaer Polytechnic Institute (Grant NNA09-DA80A) and the Icy Worlds team at NASA's Jet Propulsion Laboratory. Parts of this research were carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. Additional funding was provided from the NAI through an Astrobiology Program Early Career Collaboration Award to B.T.B. and L.M.B. B.T.B. is supported through RPI's James P. Ferris Fellowship in Astrobiology, and L.M.B. is supported by the NAI through the NASA Postdoctoral Program, administered by Oak Ridge Associated Universities through a contract with NASA. NR 66 TC 4 Z9 4 U1 11 U2 33 PU MARY ANN LIEBERT, INC PI NEW ROCHELLE PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA SN 1531-1074 EI 1557-8070 J9 ASTROBIOLOGY JI Astrobiology PD JUL 1 PY 2015 VL 15 IS 7 BP 509 EP 522 DI 10.1089/ast.2014.1280 PG 14 WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics; Geology GA CV0IH UT WOS:000363933700001 PM 26154881 ER PT J AU Hwang, YS Kim, HJ Anderson, T Angelaszek, D Copley, M Coutu, S Han, JH Huh, HG Kah, DH Kim, KC Kwashnak, K Lee, MH Link, JT Lutz, L Malinin, A Mitchell, JW Nutter, S Ofoha, O Jeon, HB Hyun, HJ Park, H Park, JM Patterson, P Seo, ES Wu, J Yoon, YS AF Hwang, Y. S. Kim, H. J. Anderson, T. Angelaszek, D. Copley, M. Coutu, S. Han, J. H. Huh, H. G. Kah, D. H. Kim, K. C. Kwashnak, K. Lee, M. H. Link, J. T. Lutz, L. Malinin, A. Mitchell, J. W. Nutter, S. Ofoha, O. Jeon, H. B. Hyun, H. J. Park, H. Park, J. M. Patterson, P. Seo, E. S. Wu, J. Yoon, Y. S. TI Construction and testing of a Top Counting Detector and a Bottom Counting Detector for the Cosmic Ray Energetics And Mass experiment on the International Space Station SO JOURNAL OF INSTRUMENTATION LA English DT Article DE Space instrumentation; Particle detectors ID ENERGY; CREAM; PERFORMANCE; RADIATION; ELECTRONS; SPECTRA; NUCLEI; REGION AB The Cosmic Ray Energetics And Mass (CREAM) mission is planned for launch in 2015 to the International Space Station (ISS) to research high-energy cosmic rays. Its aim is to understand the acceleration and propagation mechanism of high-energy cosmic rays by measuring their compositions. The Top Counting Detector and Bottom Counting Detector (T/BCD) were built to discriminate electrons from protons by using the difference in cascade shapes between electromagnetic and hadronic showers. The T/BCD provides a redundant instrument trigger in flight as well as a low-energy calibration trigger for ground testing. Each detector consists of a plastic scintillator and two-dimensional silicon photodiode array with readout electronics. The TCD is located between the carbon target and the calorimeter, and the BCD is located below the calorimeter. In this paper, we present the design, assembly, and performance of the T/BCD. C1 [Hwang, Y. S.; Kim, H. J.; Kah, D. H.; Jeon, H. B.; Hyun, H. J.; Park, H.; Park, J. M.] Kyungpook Natl Univ, Daegu 702701, South Korea. [Anderson, T.; Coutu, S.] Penn State Univ, University Pk, PA 16802 USA. [Angelaszek, D.; Copley, M.; Han, J. H.; Huh, H. G.; Kim, K. C.; Kwashnak, K.; Lee, M. H.; Lutz, L.; Malinin, A.; Ofoha, O.; Patterson, P.; Seo, E. S.; Wu, J.; Yoon, Y. S.] Univ Maryland, College Pk, MD 20742 USA. [Link, J. T.; Mitchell, J. W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Link, J. T.] CRESST USRA, Columbia, MD 21044 USA. [Nutter, S.] No Kentucky Univ, Highland Hts, KY 41076 USA. RP Kim, HJ (reprint author), Kyungpook Natl Univ, Daegu 702701, South Korea. EM hongjoo@knu.ac.kr RI Yoon, Young Soo/O-8580-2014 OI Yoon, Young Soo/0000-0001-7023-699X FU National Research Foundation (NRF) of Korea - Korean Government [NRF-2011-0016260]; NASA [NNX11AC52G, NNX08AC15G, NNX08AC16G]; RTOP; Ministry of Oceans and Fisheries, Korea FX That was supported by National Research Foundation (NRF) of Korea grants funded by the Korean Government (NRF-2011-0016260). The authors thank NASA Goddard Space Flight Center (GSFC) Wallops Flight Facility for project management and engineering support, and NASA Johnson Space Center ISS Program Office for launch support and ISS accommodations. This work was supported in the United States by NASA grants NNX11AC52G, NNX08AC15G, and NNX08AC16G and their predecessor grants, as well as by directed RTOP funds to the NASA GSFC. It was partially funded by the project titled "Research on fundamental core technology for ubiquitous shipping and logistics" funded by Ministry of Oceans and Fisheries, Korea. NR 36 TC 0 Z9 0 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 1748-0221 J9 J INSTRUM JI J. Instrum. PD JUL PY 2015 VL 10 AR P07018 DI 10.1088/1748-0221/10/07/P07018 PG 18 WC Instruments & Instrumentation SC Instruments & Instrumentation GA CS7LR UT WOS:000362265600037 ER PT J AU Yu, Q Burleigh, SC Wang, RH Zhao, KL AF Yu, Qian Burleigh, Scott C. Wang, Ruhai Zhao, Kanglian TI Performance Modeling of Licklider Transmission Protocol (LTP) in Deep-Space Communication SO IEEE TRANSACTIONS ON AEROSPACE AND ELECTRONIC SYSTEMS LA English DT Article ID FILE-DELIVERY PROTOCOL; INTERPLANETARY INTERNET; SATELLITE-COMMUNICATIONS; TOLERANT NETWORKING; DTN; DELAY; TRANSPORT; LINKS; CHALLENGES; BUNDLES AB Delay/disruption tolerant networking (DTN) offers a solution to communications in "challenged" networks. Some work has been seen in evaluating the performance of DTN protocols based on simulated or emulated file transfer experiments. However, there is a need for a model of the performance of the DTN Licklider transmission protocol (LTP), which particularly targets reliable data transmission in deep space. In this paper, we present a performance model of LTP-based DTN data transmission in challenging communications characterized by extremely long signal propagation delay, lengthy link disruptions, and highly lossy channels that are typical of deep-space links. The model is verified by file-transfer experiments using a PC-based testbed. C1 [Yu, Qian] Soochow Univ, Sch Elect & Informat Engn, Suzhou 215006, Jiangsu, Peoples R China. [Burleigh, Scott C.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Wang, Ruhai] Lamar Univ, Phillip M Drayer Dept Elect Engn, Beaumont, TX 77710 USA. [Zhao, Kanglian] Nanjing Univ, Sch Elect Sci & Engn, Nanjing 210093, Jiangsu, Peoples R China. RP Zhao, KL (reprint author), Nanjing Univ, Sch Elect Sci & Engn, Nanjing 210093, Jiangsu, Peoples R China. EM zhaokanglian@nju.edu.cn RI Zhao, Kanglian/N-9276-2015 FU National Aeronautics and Space Administration FX 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. The authors would like to acknowledge Dr. Thomas Robertazzi at Stony Brook University for the help in improving the technical quality of the paper. NR 38 TC 5 Z9 5 U1 1 U2 5 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0018-9251 EI 1557-9603 J9 IEEE T AERO ELEC SYS JI IEEE Trans. Aerosp. Electron. Syst. PD JUL PY 2015 VL 51 IS 3 BP 1609 EP 1620 DI 10.1109/TAES.2014.130763 PG 12 WC Engineering, Aerospace; Engineering, Electrical & Electronic; Telecommunications SC Engineering; Telecommunications GA CS4AA UT WOS:000362015800003 ER PT J AU Rumsey, CL Slotnick, JP AF Rumsey, Christopher L. Slotnick, Jeffrey P. TI Overview and Summary of the Second AIAA High-Lift Prediction Workshop SO JOURNAL OF AIRCRAFT LA English DT Article ID TURBULENCE MODELS AB The Second AIAA CFD High-Lift Prediction Workshop was held in San Diego, California in June 2013. The goals of the workshop continued in the tradition of the first high-lift workshop: to assess the numerical prediction capability of current-generation computational fluid dynamics technology for swept, medium-/high-aspect-ratio wings in landing/takeoff (high-lift) configurations. This workshop analyzed the flow over the DLR-F11 model in landing configuration at two different Reynolds numbers. Twenty-six participants submitted a total of 48 data sets of computational fluid dynamics results. Avariety of grid systems (both structured and unstructured) were used. Trends due to grid density and Reynolds number were analyzed, and effects of support brackets were also included. This paper analyzes the combined results from all workshop participants. Comparisons with experimental data are made. A statistical summary of the computational fluid dynamics results is also included. C1 [Rumsey, Christopher L.] NASA Langley Res Ctr, Computat AeroSci Branch, Hampton, VA 23681 USA. [Slotnick, Jeffrey P.] Boeing Co, Computat Sci, Huntington Beach, CA 92647 USA. RP Rumsey, CL (reprint author), NASA Langley Res Ctr, Computat AeroSci Branch, Mail Stop 128, Hampton, VA 23681 USA. NR 53 TC 1 Z9 1 U1 0 U2 0 PU AMER INST AERONAUTICS ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0021-8669 EI 1533-3868 J9 J AIRCRAFT JI J. Aircr. PD JUL-AUG PY 2015 VL 52 IS 4 BP 1006 EP 1025 DI 10.2514/1.C032864 PG 20 WC Engineering, Aerospace SC Engineering GA CS4JD UT WOS:000362041200002 ER PT J AU Lee-Rausch, EM Rumsey, CL Park, MA AF Lee-Rausch, E. M. Rumsey, C. L. Park, M. A. TI Grid-Adapted FUN3D Computations for the Second High-Lift Prediction Workshop SO JOURNAL OF AIRCRAFT LA English DT Article ID UNSTRUCTURED GRIDS; TURBULENT FLOWS; IMPLICIT AB Contributions of the unstructured Reynolds-averaged Navier-Stokes code FUN3D to the 2nd AIAA Computational Fluid Dynamics High-Lift Prediction Workshop are described, and detailed comparisons are made with experimental data. Using workshop-supplied grids, FUN3D results for the simplified high-lift configuration are compared with results from the structured code CFL3D. Using the same turbulence model, both codes compare reasonably well in terms of total forces and moment, and the maximum lift is similarly over-predicted for both codes compared to experiment. By including more representative geometry features such as slat and flap support brackets and slat pressure tube bundles, FUN3D captures the general effects of the Reynolds number variation, but under-predicts maximum lift on workshop-supplied grids in comparison with the experimental data due to excessive separation. However, when output-based, off-body grid adaptation in FUN3D is employed, results improve considerably. In particular, when the geometry includes both brackets and the pressure tube bundles, grid adaptation results in a more accurate prediction of lift near stall in comparison with the wind-tunnel data. Furthermore, a rotation-corrected turbulence model shows improved pressure predictions on the outboard span when using adapted grids. C1 [Lee-Rausch, E. M.; Rumsey, C. L.; Park, M. A.] NASA Langley Res Ctr, Computat AeroSci Branch, Hampton, VA 23681 USA. RP Lee-Rausch, EM (reprint author), NASA Langley Res Ctr, Computat AeroSci Branch, Hampton, VA 23681 USA. EM E.Lee-Rausch@nasa.gov; C.L.Rumsey@nasa.gov; M.A.Park@nasa.gov NR 36 TC 0 Z9 0 U1 0 U2 0 PU AMER INST AERONAUTICS ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0021-8669 EI 1533-3868 J9 J AIRCRAFT JI J. Aircr. PD JUL-AUG PY 2015 VL 52 IS 4 BP 1098 EP 1111 DI 10.2514/1.C033192 PG 14 WC Engineering, Aerospace SC Engineering GA CS4JD UT WOS:000362041200008 ER PT J AU Rodio, JJ Xiao, X Hassan, HA Rumsey, CL AF Rodio, J. J. Xiao, X. Hassan, H. A. Rumsey, C. L. TI NASA Trapezoidal-Wing Simulation Using Stress-omega, and One- and Two-Equation Turbulence Models SO JOURNAL OF AIRCRAFT LA English DT Article ID FLOW; CHANNEL; LIFT AB The Wilcox 2006 stress-omega model (also referred to as WilcoxRSM-w2006) has been implemented in the NASA Langley Research Center code CFL3D, and used to study a variety of two-dimensional and three-dimensional configurations. It predicted a variety of basic cases reasonably well, including secondary flow in a supersonic rectangular duct. One-and two-equation turbulence models that employ the Boussinesq constitutive relation were unable to predict this secondary flow accurately because it is driven by normal turbulent-stress differences. For the NASA trapezoidal wing at high angles of attack, the WilcoxRSM-w2006 model predicted lower maximum lift than the experiment, similar to the results of a two-equation model. C1 [Rodio, J. J.; Hassan, H. A.] N Carolina State Univ, Mech & Aerosp Engn, Raleigh, NC 27695 USA. [Xiao, X.] Corvid Technol, Mooresville, NC 28117 USA. [Hassan, H. A.] N Carolina State Univ, AIAA, Raleigh, NC 27695 USA. [Rumsey, C. L.] NASA, Langley Res Ctr, Computat AeroSci Branch, Hampton, VA 23681 USA. RP Rodio, JJ (reprint author), N Carolina State Univ, Mech & Aerosp Engn, Raleigh, NC 27695 USA. NR 28 TC 0 Z9 0 U1 1 U2 1 PU AMER INST AERONAUTICS ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0021-8669 EI 1533-3868 J9 J AIRCRAFT JI J. Aircr. PD JUL-AUG PY 2015 VL 52 IS 4 BP 1189 EP 1200 DI 10.2514/1.C032848 PG 12 WC Engineering, Aerospace SC Engineering GA CS4JD UT WOS:000362041200015 ER PT J AU Stanford, BK Dunning, PD AF Stanford, Bret K. Dunning, Peter D. TI Optimal Topology of Aircraft Rib and Spar Structures Under Aeroelastic Loads SO JOURNAL OF AIRCRAFT LA English DT Article ID OPTIMIZATION; DESIGN; FLUTTER; CONSTRAINTS; WEIGHT; WINGS AB Several topology optimization problems are conducted within the ribs and spars of a wing box. It is desired to locate the best position of lightening holes, truss/cross-bracing, etc. A variety of aeroelastic metrics are isolated for each of these problems: elastic wing compliance under trim loads and taxi loads, stress distribution, and crushing loads. Aileron effectiveness under a constant roll rate is considered as are dynamic metrics: natural vibration frequency and flutter. This approach helps uncover the relationship between topology and aeroelasticity in subsonic transport wings and can therefore aid in understanding the complex aircraft design process that must eventually consider all these metrics and load cases simultaneously. C1 [Stanford, Bret K.] NASA, Langley Res Ctr, Aeroelast Branch, Hampton, VA 23681 USA. [Dunning, Peter D.] Natl Inst Aerosp, Hampton, VA 23666 USA. RP Stanford, BK (reprint author), NASA, Langley Res Ctr, Aeroelast Branch, Hampton, VA 23681 USA. EM bret.k.stanford@nasa.gov; peter.d.dunning@nasa.gov OI Dunning, Peter/0000-0002-7645-7598 NR 37 TC 3 Z9 3 U1 2 U2 10 PU AMER INST AERONAUTICS ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0021-8669 EI 1533-3868 J9 J AIRCRAFT JI J. Aircr. PD JUL-AUG PY 2015 VL 52 IS 4 BP 1298 EP 1311 DI 10.2514/1.C032913 PG 14 WC Engineering, Aerospace SC Engineering GA CS4JD UT WOS:000362041200025 ER PT J AU Riel, B Milillo, P Simons, M Lundgren, P Kanamori, H Samsonov, S AF Riel, B. Milillo, P. Simons, M. Lundgren, P. Kanamori, H. Samsonov, S. TI The collapse of Bardarbunga caldera, Iceland SO GEOPHYSICAL JOURNAL INTERNATIONAL LA English DT Article DE Satellite geodesy; Radar interferometry; Magma chamber processes; Calderas; Remote sensing of volcanoes ID VERTICAL-CLVD EARTHQUAKES; MAGMA-CHAMBER GEOMETRY; ANOMALOUS EARTHQUAKES; GALAPAGOS-ISLANDS; ACTIVE VOLCANOS; DEFORMATION; MECHANISM; MODELS; JAPAN; INJECTION AB Lying below Vatnajokull ice cap in Iceland, Bardarbunga stratovolcano began experiencing wholesale caldera collapse in 2014 August 16, one of the largest such events recorded in the modern instrumental era. Simultaneous with this collapse is the initiation of a plate boundary rifting episode north of the caldera. Observations using the international constellation of radar satellites indicate rapid 50 cm d(-1) subsidence of the glacier surface overlying the collapsing caldera and metre-scale crustal deformation in the active rift zone. Anomalous earthquakes around the rim of the caldera with highly nondouble-couple focal mechanisms provide a mechanical link to the dynamics of the collapsing magma chamber. A model of the collapse consistent with available geodetic and seismic observations suggests that the majority of the observed subsidence occurs aseismically via a deflating sill-like magma chamber. C1 [Riel, B.; Milillo, P.; Simons, M.; Kanamori, H.] CALTECH, Seismol Lab, Pasadena, CA 91125 USA. [Milillo, P.] Univ Basilicata, Scuola Ingn, I-85100 Potenza, Italy. [Lundgren, P.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Samsonov, S.] Canada Ctr Mapping & Earth Observat, Nat Resources, Ottawa, ON K1S 5K2, Canada. RP Riel, B (reprint author), CALTECH, Seismol Lab, 1200 E Calif Blvd, Pasadena, CA 91125 USA. EM briel@caltech.edu RI GEOFON, GlobalSeismicNetwork/E-4273-2012; OI Milillo, Pietro/0000-0002-1171-3976; Samsonov, Sergey/0000-0002-6798-4847 FU National Aeronautics and Space Administration (NASA); President's and Director's Fund Program FX We thank Egill Hauksson and Hilary Martens for discussions in the early phase of this study. We also thank Agust Gudmundsson, Jurg Schuler and three anonymous reviewers for their helpful comments and for improving the quality of this manuscript. BR was supported under a National Aeronautics and Space Administration (NASA) Earth and Space Science Fellowship. Part of this research was carried out at the Jet Propulsion Laboratory and the California Institute of Technology under a contract with NASA and funded through the President's and Director's Fund Program. This research was carried out using COSMO-SkyMed (CSK (R)) products delivered under an Italian Space Agency (ASI) license and is made possible through a collaboration between JPL/Caltech/CIDOT and NASA/ASI. NR 36 TC 13 Z9 13 U1 9 U2 26 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0956-540X EI 1365-246X J9 GEOPHYS J INT JI Geophys. J. Int. PD JUL PY 2015 VL 202 IS 1 BP 446 EP 453 DI 10.1093/gji/ggv157 PG 8 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA CQ5DL UT WOS:000360623400031 ER PT J AU Fu, YN Liu, Z Freymueller, JT AF Fu, Yuning Liu, Zhen Freymueller, Jeffrey T. TI Spatiotemporal variations of the slow slip event between 2008 and 2013 in the southcentral Alaska subduction zone SO GEOCHEMISTRY GEOPHYSICS GEOSYSTEMS LA English DT Article DE slow slip event; Alaska; GPS; spatiotemporal variation ID NEW-ZEALAND; SILENT SLIP; EARTHQUAKE RUPTURE; GREAT EARTHQUAKES; TREMOR; INTERFACE; JAPAN; CASCADIA; GUERRERO; DEFORMATION AB We apply a Kalman filter-based time-dependent slip inversion method to model a long-term Slow Slip Event (SSE) in the southcentral Alaska subduction zone from 2008 to 2013. This event occurred downdip of the asperity that ruptured in the 1964 earthquake, the same part of plate interface that slipped during a previous SSE between 1998 and 2001. Most of the slip deficit that accumulated during the steady period between 2001 and 2008 (8 years total) in the SSE source region was released by this SSE. Our results indicate both lateral and downdip propagation during this event. The SSE started at the end of 2008 at the upper section of the slip patch, and gradually propagated to the east and to the deeper part of the interface. Our results indicate no connection between this SSE in Upper Cook Inlet and another SSE in Lower Cook Inlet that started in 2010. Analysis of the earthquake catalog in the southcentral Alaska subduction zone shows a clear increase in seismicity associated with the 2008-2013 SSE. With the data from a newly available continuous GPS site, we now can better constrain the start time of the 1998-2001 SSE as approximate to 1998.58. C1 [Fu, Yuning; Liu, Zhen] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Freymueller, Jeffrey T.] Univ Alaska Fairbanks, Inst Geophys, Fairbanks, AK 99775 USA. RP Liu, Z (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. EM zhen.liu@jpl.nasa.gov RI Liu, Zhen/D-8334-2017 FU NASA Postdoctoral Program at Jet Propulsion Laboratory; NSF [EAR12-15933]; National Aeronautics and Space Administration (NASA) FX The authors thank UNAVCO for maintaining the PBO GPS network in Alaska as part of the NSF EarthScope program. We appreciate Susan Owen for helpful discussions. The comments from two anonymous reviewers significantly improved the manuscript. We thank Jim Mitchell of Crazy Mountains Joint Venture for providing the CMJV data. All the data and results derived in the study are available from the authors. Y.F. was partly supported by the NASA Postdoctoral Program at Jet Propulsion Laboratory. J.T.F was supported by NSF grant EAR12-15933. The research by Y.F. and Z.L. described in this paper was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration (NASA). NR 61 TC 2 Z9 2 U1 1 U2 4 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 1525-2027 J9 GEOCHEM GEOPHY GEOSY JI Geochem. Geophys. Geosyst. PD JUL PY 2015 VL 16 IS 7 BP 2450 EP 2461 DI 10.1002/2015GC005904 PG 12 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA CP9WX UT WOS:000360247200023 ER PT J AU Dorelli, JC Glocer, A Collinson, G Toth, G AF Dorelli, J. C. Glocer, Alex Collinson, Glyn Toth, Gabor TI The role of the Hall effect in the global structure and dynamics of planetary magnetospheres: Ganymede as a case study SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article DE Ganymede; Magnetic Reconnection; Hall MHD ID COLLISIONLESS MAGNETIC RECONNECTION; ION-CYCLOTRON; LARGE SYSTEMS; FIELDS; MHD; MAGNETOHYDRODYNAMICS; ANTIPARALLEL; MAGNETOTAIL; TRANSITION; CHALLENGE AB We present high-resolution Hall MHD simulations of Ganymede's magnetosphere demonstrating that Hall electric fields in ion-scale magnetic reconnection layers have significant global effects not captured in resistive MHD simulations. Consistent with local kinetic simulations of magnetic reconnection, our global simulations show the development of intense field-aligned currents along the magnetic separatrices. These currents extend all the way down to the moon's surface, where they may contribute to Ganymede's aurora. Within the magnetopause and magnetotail current sheets, Hall J x B forces accelerate ions to the local Alfven speed in the out-of-plane direction, producing a global system of ion drift belts that circulates Jovian magnetospheric plasma throughout Ganymede's magnetosphere. We discuss some observable consequences of these Hall-induced currents and ion drifts: the appearance of a sub-Jovian double magnetopause structure, an Alfvenic ion jet extending across the upstream magnetopause, and an asymmetric pattern of magnetopause Kelvin-Helmholtz waves. C1 [Dorelli, J. C.; Glocer, Alex; Collinson, Glyn] NASA, Goddard Space Flight Ctr, Geospace Phys Lab, Greenbelt, MD 20771 USA. [Toth, Gabor] Univ Michigan, Ctr Space Environm Modeling, Ann Arbor, MI 48109 USA. RP Dorelli, JC (reprint author), NASA, Goddard Space Flight Ctr, Geospace Phys Lab, Greenbelt, MD 20771 USA. EM john.dorelli@nasa.gov RI Toth, Gabor/B-7977-2013 OI Toth, Gabor/0000-0002-5654-9823 NR 51 TC 3 Z9 3 U1 2 U2 4 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD JUL PY 2015 VL 120 IS 7 BP 5377 EP 5392 DI 10.1002/2014JA020951 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CQ1TF UT WOS:000360381400012 ER PT J AU Engebretson, MJ Posch, JL Wygant, JR Kletzing, CA Lessard, MR Huang, CL Spence, HE Smith, CW Singer, HJ Omura, Y Horne, RB Reeves, GD Baker, DN Gkioulidou, M Oksavik, K Mann, IR Raita, T Shiokawa, K AF Engebretson, M. J. Posch, J. L. Wygant, J. R. Kletzing, C. A. Lessard, M. R. Huang, C. -L. Spence, H. E. Smith, C. W. Singer, H. J. Omura, Y. Horne, R. B. Reeves, G. D. Baker, D. N. Gkioulidou, M. Oksavik, K. Mann, I. R. Raita, T. Shiokawa, K. TI Van Allen probes, NOAA, GOES, and ground observations of an intense EMIC wave event extending over 12 h in magnetic local time SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article DE EMIC waves; radiation belts; magnetospheric compressions ID ION-CYCLOTRON WAVES; RELATIVISTIC ELECTRON-PRECIPITATION; SUBAURORAL PROTON PRECIPITATION; PITCH-ANGLE SCATTERING; EQUATORIAL MAGNETOSPHERE; ENERGETIC PARTICLE; GEOMAGNETIC STORMS; RADIATION BELTS; PULSATIONS; EMISSIONS AB Although most studies of the effects of electromagnetic ion cyclotron (EMIC) waves on Earth's outer radiation belt have focused on events in the afternoon sector in the outer plasmasphere or plume region, strong magnetospheric compressions provide an additional stimulus for EMIC wave generation across a large range of local times and L shells. We present here observations of the effects of a wave event on 23 February 2014 that extended over 8h in UT and over 12h in local time, stimulated by a gradual 4h rise and subsequent sharp increases in solar wind pressure. Large-amplitude linearly polarized hydrogen band EMIC waves (up to 25nT p-p) appeared for over 4h at both Van Allen Probes, from late morning through local noon, when these spacecraft were outside the plasmapause, with densities similar to 5-20cm(-3). Waves were also observed by ground-based induction magnetometers in Antarctica (near dawn), Finland (near local noon), Russia (in the afternoon), and in Canada (from dusk to midnight). Ten passes of NOAA-POES and METOP satellites near the northern foot point of the Van Allen Probes observed 30-80keV subauroral proton precipitation, often over extended L shell ranges; other passes identified a narrow L shell region of precipitation over Canada. Observations of relativistic electrons by the Van Allen Probes showed that the fluxes of more field-aligned and more energetic radiation belt electrons were reduced in response to both the emission over Canada and the more spatially extended emission associated with the compression, confirming the effectiveness of EMIC-induced loss processes for this event. C1 [Engebretson, M. J.; Posch, J. L.] Augsburg Coll, Dept Phys, Minneapolis, MN 55454 USA. [Wygant, J. R.] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA. [Kletzing, C. A.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. [Lessard, M. R.; Huang, C. -L.; Spence, H. E.; Smith, C. W.] Univ New Hampshire, Ctr Space Sci, Durham, NH 03824 USA. [Singer, H. J.] NOAA, Boulder, CO USA. [Omura, Y.] Kyoto Univ, Res Inst Sustainable Humanosphere, Kyoto, Japan. [Horne, R. B.] British Antarctic Survey, Cambridge CB3 0ET, England. [Reeves, G. D.] Los Alamos Natl Lab, Space Sci & Applicat Grp, Los Alamos, NM USA. [Baker, D. N.] Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80309 USA. [Gkioulidou, M.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA. [Oksavik, K.] Univ Bergen, Birkeland Ctr Space Sci, Dept Phys & Technol, Bergen, Norway. [Oksavik, K.] Univ Ctr Svalbard, Longyearbyen, Norway. [Mann, I. R.] Univ Alberta, Dept Phys, Edmonton, AB, Canada. [Mann, I. R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Raita, T.] Univ Oulu, Sodankyla Geophys Observ, Sodankyla, Finland. [Shiokawa, K.] Nagoya Univ, STELAB, Toyokawa, Japan. RP Engebretson, MJ (reprint author), Augsburg Coll, Dept Phys, Minneapolis, MN 55454 USA. EM engebret@augsburg.edu RI Reeves, Geoffrey/E-8101-2011; Gkioulidou, Matina/G-9009-2015; Omura, Yoshiharu/P-8565-2014; OI Reeves, Geoffrey/0000-0002-7985-8098; Gkioulidou, Matina/0000-0001-9979-2164; Omura, Yoshiharu/0000-0002-6683-3940; Horne, Richard/0000-0002-0412-6407; Kletzing, Craig/0000-0002-4136-3348; Oksavik, Kjellmar/0000-0003-4312-6992 FU NSF [ANT-1142045, PLR-1341493, ANT-1141987, PLR-1341677]; Van Allen Probes mission; NASA [NAS5-01072]; Research Council of Norway [223252, 212014] FX This research was supported by NSF grants ANT-1142045 and PLR-1341493 to Augsburg College and NSF grants ANT-1141987 and PLR-1341677 to the University of New Hampshire. Work performed by M.J.E. at NASA/GSFC was supported by the Van Allen Probes mission. Van Allen Probes research at the University of Minnesota, University of Iowa, University of New Hampshire, and Los Alamos National Laboratory was supported by NASA prime contract NAS5-01072 to The Johns Hopkins University Applied Physics Laboratory. Work performed by K.O. at the University of Bergen was supported by the Research Council of Norway under contracts 223252 and 212014. We thank David Sibeck, Brian Anderson, Shrikanth Kanekal, Sasha Ukhorskiy, Yuri Shprits, Viacheslav Pilipenko, Finn Soraas, and Barry Mauk for helpful comments The Halley research station in Antarctica is operated by the British Antarctic Survey. We thank R.A. Rakhmatulin for providing Mondy induction magnetometer data, we thank the referees for their helpful comments, and we gratefully acknowledge use of NASA/GSFC's Space Physics Data Facility's OMNIWeb, SSCweb, and CDAWeb data. NR 76 TC 24 Z9 24 U1 3 U2 9 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD JUL PY 2015 VL 120 IS 7 BP 5465 EP 5488 DI 10.1002/2015JA021227 PG 24 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CQ1TF UT WOS:000360381400018 ER PT J AU Moya, PS Pinto, VA Vinas, AF Sibeck, DG Kurth, WS Hospodarsky, GB Wygant, JR AF Moya, Pablo. S. Pinto, Victor A. Vinas, Adolfo F. Sibeck, David G. Kurth, William S. Hospodarsky, George B. Wygant, John R. TI Weak kinetic Alfven waves turbulence during the 14November2012 geomagnetic storm: Van Allen Probes observations SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article DE magnetic storms; radiation belts; Van Allen Probes; kinetic AlfvenAlfven waves ID ION-CYCLOTRON WAVES; PITCH-ANGLE SCATTERING; MAGNETIC-FIELD FLUCTUATIONS; RING CURRENT; SOLAR-WIND; EQUATORIAL MAGNETOSPHERE; PARAMETRIC DECAY; LOW-FREQUENCY; PLASMA; POLARIZATION AB In the dawn sector, L approximate to 5.5 and MLT approximate to 4-7, from 01:30 to 06:00UT during the 14 November 2012 geomagnetic storm, both Van Allen Probes observed an alternating sequence of locally quiet and disturbed intervals with two strikingly different power fluctuation levels and magnetic field orientations: either small (approximate to 10(-2)nT(2)) total power with strong GSM B-x and weak B-y or large (approximate to 10nT(2)) total power with weak B-x and strong B-y and B-z components. During both kinds of intervals the fluctuations occur in the vicinity of the local ion gyrofrequencies (0.01-10Hz) in the spacecraft frame, propagate oblique to the magnetic field, ( approximate to 60 degrees), and have magnetic compressibility C=|B-vertical bar|/|B|approximate to 1, where B-vertical bar(B) are the average amplitudes of the fluctuations parallel(perpendicular) to the mean field. Electric field fluctuations are present whenever the magnetic field is disturbed, and large electric field fluctuations follow the same pattern for quiet and disturbed intervals. Magnetic frequency power spectra at both spacecraft correspond to steep power laws approximate to f(-) with 4 < < 5 for f less than or similar to 2Hz, and 1.1 < < 1.7 for f 2Hz, spectral profiles that are consistent with weak kinetic Alfven wave (KAW) turbulence. Electric power is larger than magnetic power for all frequencies above 0.1Hz, and the ratio increases with increasing frequency. Vlasov linear analysis is consistent with the presence of compressive KAW with ki less than or similar to 1, right-handed polarization and positive magnetic helicity, in the plasma frame, considering a multiion plasma. All these results suggest the presence of weak KAW turbulence which dissipates the energy associated with the intermittent sudden changes in the magnetic field during the main phase of the storm. C1 [Moya, Pablo. S.; Vinas, Adolfo F.] NASA, Goddard Space Flight Ctr, Geospace Phys Lab, Greenbelt, MD 20771 USA. [Moya, Pablo. S.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA. [Moya, Pablo. S.] Univ Chile, Fac Ciencias, Dept Fis, Santiago, Chile. [Pinto, Victor A.] Univ Calif Los Angeles, Dept Atmospher & Ocean Sci, Los Angeles, CA USA. [Sibeck, David G.] NASA, Goddard Space Flight Ctr, Space Weather Lab, Greenbelt, MD 20771 USA. [Kurth, William S.; Hospodarsky, George B.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. [Wygant, John R.] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA. RP Moya, PS (reprint author), NASA, Goddard Space Flight Ctr, Geospace Phys Lab, Greenbelt, MD 20771 USA. EM pablo.s.moyafuentes@nasa.gov RI Moya, Pablo/C-3163-2011; Pinto, Victor/C-9585-2011; OI Moya, Pablo/0000-0002-9161-0888; Pinto, Victor/0000-0003-1210-167X; Hospodarsky, George/0000-0001-9200-9878; Kurth, William/0000-0002-5471-6202 FU JHU/APL contract under NASA Prime contract [921647, NAS5-01072]; Van Allen Probe mission funds at NASA/GSFC; Comision Nacional de Ciencia y Tecnologia (CONICyT, Chile) FX We acknowledge Craig Kletzing for useful discussions and for providing data from the EMFISIS instrument suite of the Van Allen Probes Mission. Data sets were provided by the Space Physics Data Facility at Goddard Space Flight Center through their Coordinated Data Analysis Web (http://cdaweb.gsfc.nasa.gov). We would like to thank Kyoung-Joo Hwang, Alex Glocer, Elizabeth MacDonald, and Bea Gallardo-Lacourt for useful discussions. Portions of this work were performed under the support of JHU/APL contract 921647 under NASA Prime contract NAS5-01072. A portion of this work was supported by Van Allen Probe mission funds at NASA/GSFC. We also thank Comision Nacional de Ciencia y Tecnologia (CONICyT, Chile) for providing financial support for postdoctoral (P.S.M.) and doctoral (V.A.P.) fellows. NR 90 TC 8 Z9 8 U1 0 U2 5 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD JUL PY 2015 VL 120 IS 7 BP 5504 EP 5523 DI 10.1002/2014JA020281 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CQ1TF UT WOS:000360381400020 ER PT J AU Katus, RM Gallagher, DL Liemohn, MW Keesee, AM Sarno-Smith, LK AF Katus, R. M. Gallagher, D. L. Liemohn, M. W. Keesee, A. M. Sarno-Smith, L. K. TI Statistical storm time examination of MLT-dependent plasmapause location derived from IMAGE EUV SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article DE plasmapause; geomagnetic storms; IMAGE EUV data; normalized superposed epoch analysis ID SUPERPOSED EPOCH ANALYSIS; HIGH-SPEED STREAMS; ELECTRIC-FIELD; SOLAR-WIND; GEOMAGNETIC STORMS; MAGNETIC CLOUDS; DRIVEN STORMS; RING CURRENT; PLASMASPHERE; MAGNETOSPHERE AB The location of the outer edge of the plasmasphere (the plasmapause) as a function of geomagnetic storm time is identified and investigated statistically in regard to the solar wind driver. Imager for Magnetopause-to-Aurora Global Exploration (IMAGE) extreme ultraviolet (EUV) data are used to create an automated method that locates and extracts the plasmapause. The plasmapause extraction technique searches a set range of possible plasmasphere densities for a maximum gradient. The magnetic local time (MLT)-dependent plasmapause results are compared to manual extraction results. The plasmapause results from 39 intense storms are examined along a normalized epoch storm timeline to determine the average plasmapause L shell as a function of MLT and storm time. The average extracted plasmapause L shell follows the expected storm time plasmapause behavior. The results show that during the main phase, the plasmapause moves earthward and a plasmaspheric drainage plume forms near dusk and across the dayside during strong convection. During the recovery phase, the plume rejoins the corotationally driven plasma while the average plasmapause location moves farther from the Earth. The results are also examined in terms of the solar wind driver. We find evidence that shows that the different categories of solar wind drivers result in different plasmaspheric configurations. During magnetic cloud-driven events the plasmaspheric drainage plume appears at the start of the main phase. During sheath-driven events the plume forms later but typically extends further in MLT. C1 [Katus, R. M.; Liemohn, M. W.; Sarno-Smith, L. K.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. [Katus, R. M.; Keesee, A. M.] W Virginia Univ, Dept Phys & Astron, Morgantown, WV 26506 USA. [Gallagher, D. L.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. RP Katus, RM (reprint author), Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. EM rkatus@umich.edu OI Keesee, Amy/0000-0002-9719-3229; Sarno-Smith, Lois/0000-0002-0964-7607 FU NASA [NNX08AQ15G, NNX09AF45G, NNX10AQ34C, NNX11AO60G]; NSF [ATM-0802705, ATM-0903596, AGS-1102863, AGS-1113478]; NASA Graduate Student Research Program fellowship from Marshall Space Flight Center [NNX10AL32H] FX The authors would like to thank NASA and NSF for funding this research through various grants (specifically from NASA via grants NNX08AQ15G, NNX09AF45G, NNX10AQ34C, and NNX11AO60G and NSF through grants ATM-0802705, ATM-0903596, AGS-1102863, and AGS-1113478), including a NASA Graduate Student Research Program fellowship from Marshall Space Flight Center (grant NNX10AL32H). The authors would also like to thank the Kyoto World Data Center (http://wdc.kugi.kyoto-u.ac.jp/index.html) for providing access to the Dst and SYM-H indices, CDAWeb (http://cdaweb.gsfc.nasa.gov/istp_public/) for providing access to the solar wind data, and University of Arizona (http://euv.lpl.arizona.edu/euv/) for providing access to the IMAGE EUV data and software. Special thanks go to Peter Chi for his help in making the plasmapause data available on the GEMWiki (http://www-ssc.igpp.ucla.edu/gemwiki/index.php/Data_and_Models). NR 53 TC 4 Z9 4 U1 0 U2 2 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD JUL PY 2015 VL 120 IS 7 BP 5545 EP 5559 DI 10.1002/2015JA021225 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CQ1TF UT WOS:000360381400022 ER PT J AU Walsh, BM Thomas, EG Hwang, KJ Baker, JBH Ruohoniemi, JM Bonnell, JW AF Walsh, B. M. Thomas, E. G. Hwang, K. -J. Baker, J. B. H. Ruohoniemi, J. M. Bonnell, J. W. TI Dense plasma and Kelvin-Helmholtz waves at Earth's dayside magnetopause SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article DE Kelvin-Helmholtz; magnetopause ID FLUX-TRANSFER EVENTS; INTERACTION OFMAGNETIC RECONNECTION; UPSTREAM PRESSURE VARIATIONS; MAGNETIC RECONNECTION; PLASMASPHERIC PLUME; MAGNETOTAIL BOUNDARY; GEOTAIL OBSERVATIONS; SPECTRAL WIDTH; INSTABILITY; VORTICES AB Spacecraft observations of boundary waves at the dayside terrestrial magnetopause and their ground-based signatures are presented. Time History of Events and Macroscale Interactions during Substorms (THEMIS) spacecraft measured boundary waves at the magnetopause while ground-based HF radar measured corresponding signatures in the ionosphere indicating a large-scale response and tailward propagating waves. The properties of the oscillations are consistent with linear phase Kelvin-Helmholtz waves along the magnetopause boundary. During this time period multiple THEMIS spacecraft also measured a plasmaspheric plume contacting the local magnetopause and mass loading the boundary. Previous work has demonstrated that increasing the density at the magnetopause can lower the efficiency of reconnection. Extending this further, present observations suggest that a plume can modulate instability processes such as the Kelvin-Helmholtz instability and allow them to form closer to the subsolar point along the magnetopause than without a plume. The current THEMIS observations from 21 September 2010 are consistent with a theory which predicts that increasing the density at the boundary will lower the Kelvin-Helmholtz threshold and allow waves to form for a lower velocity shear. C1 [Walsh, B. M.; Bonnell, J. W.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Walsh, B. M.] Boston Univ, Dept Mech Engn, Boston, MA 02215 USA. [Walsh, B. M.] Boston Univ, Ctr Space Phys, Boston, MA 02215 USA. [Thomas, E. G.; Baker, J. B. H.; Ruohoniemi, J. M.] Virginia Polytech Inst & State Univ, Bradley Dept Elect & Comp Engn, Blacksburg, VA 24061 USA. [Hwang, K. -J.] NASA, Goddard Space Flight Ctr, Heliophys Div, Greenbelt, MD 20771 USA. [Hwang, K. -J.] Univ Maryland Baltimore Cty, Goddard Planetary & Heliophys Inst, Baltimore, MD 21228 USA. RP Walsh, BM (reprint author), Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. EM bwalsh@ssl.berkeley.edu RI Walsh, Brian/C-4899-2016 OI Walsh, Brian/0000-0001-7426-5413 FU NASA [NNX14AK41G, NAS5-02099]; National Science Foundation [AGS-0946900, AGS-0838219] FX Support was given by the NASA grant NNX14AK41G. We acknowledge NASA contract NAS5-02099 and instrument teams for use of the data from the THEMIS Mission, Specifically, C. W. Carlson and J. P. McFadden for use of ESA data, J. W. Bonnell and F. S. Mozer for use of EFI data, and K. H. Glassmeier, U. Auster, and W. Baumjohann for the use of FGM data. THEMIS data can be accessed freely from the mission website (http://themis.ssl.berkeley.edu/). The authors acknowledge the use of SuperDARN data (accessible at http://vt.superdarn.org/). SuperDARN is a collection of radars funded by national scientific funding agencies of Australia, Canada, China, France, Japan, South Africa, United Kingdom, and the United States of America. B.M.W. would like to acknowledge the International Space Science Institute, specifically the "Dawn-Dusk Asymmetries in the Coupled Solar Wind Magnetosphere Ionosphere System" team. The authors from Virginia Tech thank the National Science Foundation for support under grants AGS-0946900 and AGS-0838219. Special thanks are given to X. Ma and D. Sibeck for useful scientific discussions. NR 73 TC 3 Z9 3 U1 2 U2 7 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD JUL PY 2015 VL 120 IS 7 BP 5560 EP 5573 DI 10.1002/2015JA021014 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CQ1TF UT WOS:000360381400023 ER PT J AU Dewey, RM Baker, DN Anderson, BJ Benna, M Johnson, CL Korth, H Gershman, DJ Ho, GC McClintock, WE Odstrcil, D Philpott, LC Raines, JM Schriver, D Slavin, JA Solomon, SC Winslow, RM Zurbuchen, TH AF Dewey, Ryan M. Baker, Daniel N. Anderson, Brian J. Benna, Mehdi Johnson, Catherine L. Korth, Haje Gershman, Daniel J. Ho, George C. McClintock, William E. Odstrcil, Dusan Philpott, Lydia C. Raines, Jim M. Schriver, David Slavin, James A. Solomon, Sean C. Winslow, Reka M. Zurbuchen, Thomas H. TI Improving solar wind modeling at Mercury: Incorporating transient solar phenomena into the WSA-ENLIL model with the Cone extension SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article DE MESSENGER ID MESSENGER OBSERVATIONS; MAGNETIC-FIELD; BOW SHOCK; MAGNETOSPHERE; MAGNETOPAUSE; INSTRUMENT; CME; INTERPLANETARY; SPECTROMETER; RECONNECTION AB Coronal mass ejections (CMEs) and other transient solar phenomena play important roles in magnetospheric and exospheric dynamics. Although a planet may interact only occasionally with the interplanetary consequences of these events, such transient phenomena can result in departures from the background solar wind that often involve more than an order of magnitude greater ram pressure and interplanetary electric field applied to the planetary magnetosphere. For Mercury, an order of magnitude greater ram pressure combined with high Alfven speeds and reconnection rates can push the magnetopause essentially to the planet's surface, exposing the surface directly to the solar wind flow. In order to understand how the solar wind interacts with Mercury's magnetosphere and exosphere, previous studies have used the Wang-Sheeley-Arge (WSA)-ENLIL solar wind modeling tool to calculate basic and composite solar wind parameters at Mercury's orbital location. This model forecasts only the background solar wind, however, and does not include major transient events. The Cone extension permits the inclusion of CMEs and related solar wind perturbations and thus enables characterization of the effects of strong solar wind disturbances on the Mercury system. The Cone extension is predicated on the assumption of constant angular and radial velocities of CMEs to integrate these phenomena into the WSA-ENLIL coupled model. Comparisons of the model results with observations by the MESSENGER spacecraft indicate that the WSA-ENLIL+Cone model more accurately forecasts total solar wind conditions at Mercury and has greater predictive power for magnetospheric and exospheric processes than the WSA-ENLIL model alone. C1 [Dewey, Ryan M.; Baker, Daniel N.; McClintock, William E.] Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80309 USA. [Anderson, Brian J.; Korth, Haje; Ho, George C.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA. [Benna, Mehdi] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA. [Johnson, Catherine L.; Philpott, Lydia C.; Winslow, Reka M.] Univ British Columbia, Dept Earth Ocean & Atmospher Sci, Vancouver, BC V5Z 1M9, Canada. [Johnson, Catherine L.] Planetary Sci Inst, Tucson, AZ USA. [Gershman, Daniel J.; Raines, Jim M.; Slavin, James A.; Zurbuchen, Thomas H.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. [Baker, Daniel N.] NASA, Goddard Space Flight Ctr, Geospace Phys Lab, Greenbelt, MD 20771 USA. [Odstrcil, Dusan] George Mason Univ, Computat & Data Sci, Fairfax, VA 22030 USA. [Odstrcil, Dusan] NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Greenbelt, MD 20771 USA. [Schriver, David] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA USA. [Solomon, Sean C.] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC 20015 USA. [Solomon, Sean C.] Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY USA. [Winslow, Reka M.] Univ New Hampshire, Inst Study Earth Ocean & Space, Durham, NH 03824 USA. RP Dewey, RM (reprint author), Univ Colorado, Atmospher & Space Phys Lab, Campus Box 392, Boulder, CO 80309 USA. EM ryan.dewey@colorado.edu RI Benna, Mehdi/F-3489-2012; Slavin, James/H-3170-2012; OI Slavin, James/0000-0002-9206-724X; Philpott, Lydia/0000-0002-5286-8528 FU NASA Discovery Program [NASW-00002, NAS5-97271]; MESSENGER Participating Scientist Program; Natural Sciences and Engineering Research Council, Canada; National Science Foundation's Center for Integrated Space Weather Modeling FX The MESSENGER project is supported by the NASA Discovery Program under contracts NASW-00002 to the Carnegie Institution of Washington and NAS5-97271 to The Johns Hopkins University Applied Physics Laboratory and the MESSENGER Participating Scientist Program. C.L.J. and L.C.P. also acknowledge support from the Natural Sciences and Engineering Research Council, Canada. All original MESSENGER data reported in this paper are archived by the NASA Planetary Data System. The modeling techniques described here were originally developed under the auspices of the National Science Foundation's Center for Integrated Space Weather Modeling. Model outputs were provided by Dusan Odstrcil and can be obtained by contacting the corresponding author. NR 63 TC 1 Z9 1 U1 0 U2 7 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD JUL PY 2015 VL 120 IS 7 BP 5667 EP 5685 DI 10.1002/2015JA021194 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CQ1TF UT WOS:000360381400031 ER PT J AU Kress, BT Hudson, MK Selesnick, RS Mertens, CJ Engel, M AF Kress, B. T. Hudson, M. K. Selesnick, R. S. Mertens, C. J. Engel, M. TI Modeling geomagnetic cutoffs for space weather applications SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article DE Geomagnetic cutoffs ID SOLAR PROTONS; PARTICLE EVENTS; FIELD; RIGIDITY; PENETRATION; RADIATION; MAGNETOSPHERE; STATION AB Access of solar and galactic cosmic rays to the Earth's magnetosphere is quantified in terms of geomagnetic cutoff rigidity. Numerically computed grids of cutoff rigidities are used to model cosmic ray flux in Earth's atmosphere and in low Earth orbit. In recent years, the development of more accurate dynamic geomagnetic field models and an increase in computer power have made a real-time data-driven geomagnetic cutoff computation extending over the inner magnetosphere possible. For computational efficiency, numerically computed cutoffs may be scaled to different altitudes and directions of arrival using the known analytic variation of cutoff in a pure dipole magnetic field. This paper is a presentation of numerical techniques developed to compute effective cutoff rigidities for space weather applications. Numerical tests to determine the error associated with scaling vertical cutoff rigidities with altitude in a realistic geomagnetic field model are included. The tests were performed to guide the development of spatial grids for modeling cosmic ray access to the inner magnetosphere and to gain a better understanding of the accuracy of numerically modeled cutoffs. C1 [Kress, B. T.] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA. [Kress, B. T.] NOAA, Natl Geophys Data Ctr, Boulder, CO 80303 USA. [Hudson, M. K.; Engel, M.] Dartmouth Coll, Dept Phys & Astron, Hanover, NH 03755 USA. [Selesnick, R. S.] Air Force Res Lab, Space Vehicles Directorate, Kirtland AFB, Albuquerque, NM USA. [Mertens, C. J.] NASA, Langley Res Ctr, Hampton, VA 23665 USA. RP Kress, BT (reprint author), Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA. EM bkress@northstar.dartmouth.edu FU National Science Foundation [ATM-0921979, ATM-1023332]; NSF [AGS-1023339] FX This work was supported by the National Science Foundation awards ATM-0921979 and ATM-1023332. Support was also provided by NSF grant AGS-1023339. The Dartmouth College radiation belt and geomagnetic cutoff codes used to produce the results presented in this paper are freely available to the public and can be obtained by contacting the author at brian.kress@colorado.edu. NR 29 TC 0 Z9 0 U1 2 U2 4 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD JUL PY 2015 VL 120 IS 7 BP 5694 EP 5702 DI 10.1002/2014JA020899 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CQ1TF UT WOS:000360381400034 ER PT J AU Weimer, DR Mlynczak, MG Hunt, LA Tobiska, WK AF Weimer, D. R. Mlynczak, M. G. Hunt, L. A. Tobiska, W. Kent TI High correlations between temperature and nitric oxide in the thermosphere SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article DE nitric oxide; thermosphere; neutral density; exosphere; temperature ID IONOSPHERIC ELECTRODYNAMIC MODELS; POLAR-CAP INDEX; TERRESTRIAL THERMOSPHERE; SOLAR STORMS; APRIL 2002; ART.; DENSITY; ENERGY AB Obtaining accurate predictions of the neutral density in the thermosphere has been a long-standing problem. During geomagnetic storms the auroral heating in the polar ionospheres quickly raises the temperature of the thermosphere, resulting in higher neutral densities that exert a greater drag force on objects in low Earth orbit. Rapid increases and decreases in the temperature and density may occur within a couple days. A key parameter in the thermosphere is the total amount of nitric oxide (NO). The production of NO is accelerated by the auroral heating, and since NO is an efficient radiator of thermal energy, higher concentrations of this molecule accelerate the rate at which the thermosphere cools. This paper describes an improved technique that calculates changes in the global temperature of the thermosphere. Starting from an empirical model of the Poynting flux into the ionosphere, a set of differential equations derives the minimum, global value of the exospheric temperature, which can be used in a neutral density model to calculate the global values. The relative variations in NO content are used to obtain more accurate cooling rates. Comparisons with the global rate of NO emissions that are measured with the Sounding of the Atmosphere using Broadband Emission Radiometry instrument show that there is very good agreement with the predicted values. The NO emissions correlate highly with the total auroral heating that has been integrated over time. We also show that the NO emissions are highly correlated with thermospheric temperature, as well as indices of solar extreme ultraviolet radiation. C1 [Weimer, D. R.] Virginia Polytech Inst & State Univ, Ctr Space Sci & Engn Res, Blacksburg, VA 24061 USA. [Weimer, D. R.] Natl Inst Aerosp, Hampton, VA 23665 USA. [Mlynczak, M. G.] NASA, Langley Res Ctr, Sci Directorate, Hampton, VA 23665 USA. [Hunt, L. A.] Sci Syst & Applicat Inc, Hampton, VA USA. [Tobiska, W. Kent] Space Environm Technol, Pacific Palisades, CA USA. RP Weimer, DR (reprint author), Virginia Polytech Inst & State Univ, Ctr Space Sci & Engn Res, Blacksburg, VA 24061 USA. EM dweimer@vt.edu; m.g.mlynczak@nasa.gov FU NASA [NNX13AD73G]; NASA Heliophysics Division Thermosphere-Ionosphere-Mesosphere Energetics and Dynamics Project FX The authors thank Eric Sutton for providing the neutral density data from the GRACE satellite. The NASA National Space Science Data Center, the Space Physics Data Facility, ACE Principal Investigators, Edward C. Stone, Charles Smith, and David McComas, are acknowledged for usage of the ACE data. The work at Virginia Tech was supported by NASA grant NNX13AD73G. Authors M.G.M. and L.A.H. acknowledge support from the NASA Heliophysics Division Thermosphere-Ionosphere-Mesosphere Energetics and Dynamics Project. The CHAMP and GRACE density measurements are available online at http://sisko.colorado.edu/sutton/data.html. The level 2 ACE data can be obtained from the NASA archives at ftp://cdaweb.gsfc.nasa.gov/pub/data/ace. The code for the JB2008 neutral density model is at http://sol.spacenvironment.net/similar to JB2008/code.html, and the solar indices used in this paper are at http://sol.spacenvironment.net/similar to JB2008/indices.html. The empirical W05 heating model is available by contacting author D.R.W. (email:dweimer@vt.edu). The SABER measurements can be obtained from author M.G.M. (email: m.g.mlynczak@nasa.gov). NR 38 TC 2 Z9 2 U1 6 U2 14 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD JUL PY 2015 VL 120 IS 7 BP 5998 EP 6009 DI 10.1002/2015JA021461 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CQ1TF UT WOS:000360381400056 PM 27668141 ER PT J AU Todling, R AF Todling, Ricardo TI A lag-1 smoother approach to system-error estimation: sequential method SO QUARTERLY JOURNAL OF THE ROYAL METEOROLOGICAL SOCIETY LA English DT Article DE Kalman filtering; fixed-lag smoothing; innovations process; model error; system error ID ATMOSPHERIC DATA ASSIMILATION; RETROSPECTIVE DATA ASSIMILATION; MODEL-ERROR; COVARIANCE PARAMETERS; KALMAN SMOOTHER; FORECAST; DYNAMICS; 4D-VAR; PERFORMANCE; DIAGNOSIS AB Starting from sequential data assimilation arguments, the present work shows how to use residual statistics from filtering and lag-1 (6 h) smoothing to infer components of the system (model) error covariance matrix that project on to a dense observing network. The residuals relationships involving the system-error covariance matrix are similar to those available to derive background, observation and analysis-error covariance information from filter residual statistics. An illustration of the approach is given for two low-dimensional dynamical systems: a linear damped harmonic oscillator and the nonlinear Lorenz system. The application examples consider the important case of evaluating the ability to estimate the model-error covariance from residual time series obtained from suboptimal filters and smoothers that assume the model to be perfect. The examples show the residuals to contain the necessary information to allow for such estimation. The examples also illustrate the consequences of estimating covariances through time series of residuals (available in practice) instead of multiple realizations from Monte Carlo sampling. A recast of the sequential approach into variational approach language will appear in a companion article. C1 [Todling, Ricardo] NASA, Global Modeling & Assimilat Off, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Todling, R (reprint author), NASA, Goddard Space Flight Ctr, Code 610-1, Greenbelt, MD 20771 USA. EM Ricardo.Todling@nasa.gov NR 40 TC 3 Z9 3 U1 3 U2 5 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0035-9009 EI 1477-870X J9 Q J ROY METEOR SOC JI Q. J. R. Meteorol. Soc. PD JUL PY 2015 VL 141 IS 690 BP 1502 EP 1513 DI 10.1002/qj.2460 PN A PG 12 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA CP9HE UT WOS:000360203800002 ER PT J AU Ham, SH Kato, S Barker, HW Rose, FG Sun-Mack, S AF Ham, Seung-Hee Kato, Seiji Barker, Howard W. Rose, Fred G. Sun-Mack, Sunny TI Improving the modelling of short-wave radiation through the use of a 3D scene construction algorithm SO QUARTERLY JOURNAL OF THE ROYAL METEOROLOGICAL SOCIETY LA English DT Article DE scene construction algorithm (SCA); three-dimensional (3D) radiative transfer; independent column approximation (ICA); CERES; CloudSat; CALIPSO ID ANGULAR-DISTRIBUTION MODELS; ENERGY SYSTEM INSTRUMENT; SURFACE IRRADIANCE; TERRA SATELLITE; FLUX ESTIMATION; MONTE-CARLO; CLOUDS; ABSORPTION; PARAMETERIZATION; APPROXIMATION AB Active satellite sensors, such as Cloud-Aerosol Lidar and Infrared Pathfinder Satellite Observation (CALIPSO) and CloudSat, provide cloud properties that are not available from passive sensors, such as MODerate-resolution Imaging Spectroradiometer (MODIS). While active sensors provide vertical profiles of clouds, their spatial coverage is limited to their narrow, nadir ground-track. As a result, estimation of radiation by combining active sensors and broadband instrument has limitations due to their different spatial coverages. This study uses a scene construction algorithm (SCA) and MODIS data to extend two-dimensional (2D) nadir cloud profiles into the cross-track direction, and examines how the resulting constructed 3D cloud fields improve simulation of solar radiative transfer. Clouds and the Earth's Radiant Energy System (CERES) radiances are used as references to assess the improvements. While use of constructed 3D cloud fields only slightly impacts mean-bias errors for instantaneous 20 km CERES footprint-averaged top-of-atmosphere (TOA) radiances, reductions in random errors are about 40%. The largest improvements in TOA radiance simulation are for clouds with small-scale horizontal inhomogeneity such as stratocumulus and cumulus. In contrast, uniform clouds such as nimbostratus, and deep convective clouds (Dc) show little response to the SCA. The impact of using the SCA on instantaneous surface irradiances is significant for stratocumulus and cumulus, but weak for nimbostratus and Dc. Conversely, SCA significantly influences atmospheric absorption and heating rates for nimbostratus and Dc. Differences in TOA radiances simulated by 1D and 3D transfer models are smaller than differences due to use of only the 2D nadir cross-sections and the 3D constructed fields. This is because of smoothing of 3D radiative effects when averaged up to CERES footprints. For surface irradiance and atmospheric absorption, however, differences simulated by 1D and 3D transfer models are more comparable to differences that stem from use of 2D and 3D cloud information. C1 [Ham, Seung-Hee; Kato, Seiji] NASA, Langley Res Ctr, Hampton, VA 23681 USA. [Barker, Howard W.] Environm Canada, Toronto, ON, Canada. [Rose, Fred G.; Sun-Mack, Sunny] Sci Syst & Applicat Inc, Hampton, VA USA. RP Ham, SH (reprint author), NASA, Langley Res Ctr, 100 NASA Rd,Mailstop 420, Hampton, VA 23681 USA. EM seung-hee.ham@nasa.gov OI Rose, Fred G/0000-0003-0769-0772 FU Clouds and the Earth's Radiant Energy System (CERES); NASA Energy Water Cycle Study (NEWS) project; European Space Agency; NASA Postdoctoral Program at the NASA Langley Research Center FX The authors thank the CloudSat and CALIPSO science teams for publicly releasing data products, and two anonymous reviewers for their constructive and valuable comments. This work was supported by the Clouds and the Earth's Radiant Energy System (CERES), NASA Energy Water Cycle Study (NEWS) project, and the European Space Agency. S.-H. Ham is also supported by the NASA Postdoctoral Program at the NASA Langley Research Center, as administered by Oak Ridge Associated Universities (ORAU). NR 43 TC 0 Z9 0 U1 4 U2 11 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0035-9009 EI 1477-870X J9 Q J ROY METEOR SOC JI Q. J. R. Meteorol. Soc. PD JUL PY 2015 VL 141 IS 690 BP 1870 EP 1883 DI 10.1002/qj.2491 PN A PG 14 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA CP9HE UT WOS:000360203800030 ER PT J AU Bousserez, N Henze, DK Perkins, A Bowman, KW Lee, M Liu, J Deng, F Jones, DBA AF Bousserez, N. Henze, D. K. Perkins, A. Bowman, K. W. Lee, M. Liu, J. Deng, F. Jones, D. B. A. TI Improved analysis-error covariance matrix for high-dimensional variational inversions: application to source estimation using a 3D atmospheric transport model SO QUARTERLY JOURNAL OF THE ROYAL METEOROLOGICAL SOCIETY LA English DT Article DE data assimilation; variational methods; uncertainty quantification; analysis error; BFGS algorithm ID LIMITED-MEMORY PRECONDITIONERS; DATA ASSIMILATION; KALMAN FILTER; CO2; ALGORITHMS; ADJOINT; STORAGE; 4D-VAR; SINKS; BFGS AB Variational methods are widely used to solve geophysical inverse problems. Although gradient-based minimization algorithms are available for high-dimensional problems (dimension >10(6)), they do not provide an estimate of the errors in the optimal solution. In this study, we assess the performance of several numerical methods to approximate the analysis-error covariance matrix, assuming reasonably linear models. The evaluation is performed for a CO2 flux estimation problem using synthetic remote-sensing observations of CO2 columns. A low-dimensional experiment is considered in order to compare the analysis error approximations to a full-rank finite-difference inverse Hessian estimate, followed by a realistic high-dimensional application. Two stochastic approaches, a Monte-Carlo simulation and a method based on random gradients of the cost function, produced analysis error variances with a relative error <10%. The long-distance error correlations due to sampling noise are significantly less pronounced for the gradient-based randomization, which is also particularly attractive when implemented in parallel. Deterministic evaluations of the inverse Hessian using the Broyden-Fletcher-Goldfarb-Shanno (BFGS) algorithm are also tested. While existing BFGS preconditioning techniques yield poor approximations of the error variances (relative error >120%), a new preconditioner that efficiently accumulates information on the diagonal of the inverse Hessian dramatically improves the results (relative error <50%). Furthermore, performing several cycles of the BFGS algorithm using the same gradient and vector pairs enhances its performance (relative error <30%) and is necessary to obtain convergence. Leveraging those findings, we proposed a BFGS hybrid approach which combines the new preconditioner with several BFGS cycles using information from a few (3-5) Monte-Carlo simulations. Its performance is comparable to the stochastic approximations for the low-dimensional case, while good scalability is obtained for the high-dimensional experiment. Potential applications of these new BFGS methods range from characterizing the information content of high-dimensional inverse problems to improving the convergence rate of current minimization algorithms. C1 [Bousserez, N.; Henze, D. K.; Perkins, A.] Univ Colorado, Dept Mech Engn, Boulder, CO 80309 USA. [Bowman, K. W.; Lee, M.; Liu, J.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Deng, F.; Jones, D. B. A.] Univ Toronto, Dept Phys, Toronto, ON M5S 1A1, Canada. [Jones, D. B. A.] Univ Calif Los Angeles, JIFRESSE, Los Angeles, CA USA. RP Bousserez, N (reprint author), ECES, 1111 Engn Dr UCB 427, Boulder, CO 80309 USA. EM nicolas.bousserez@colorado.edu RI Jones, Dylan/O-2475-2014; OI Jones, Dylan/0000-0002-1935-3725; Perkins, Walter/0000-0001-7742-7609; Deng, Feng/0000-0002-1381-0243 FU NASA CMS program [NNX12AR31G]; NASA [NNX10AT42G, NNX10AR06G]; National Science Foundation [CNS-0821794]; University of Colorado Boulder FX This work has been funded by the NASA CMS program (grant number NNX12AR31G), the NASA Atmospheric CO2 Observations from Space program (grant number NNX10AT42G), as well as the NASA New Investigator Program NNX10AR06G. This work utilized the Janus supercomputer, which is supported by the National Science Foundation (award number CNS-0821794) and the University of Colorado Boulder. The Janus supercomputer is a joint effort of the University of Colorado Boulder, the University of Colorado Denver and the National Center for Atmospheric Research. The first author would also like to thank Richard Byrd for a number of useful discussions about the BFGS minimization method. NR 42 TC 10 Z9 10 U1 0 U2 7 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0035-9009 EI 1477-870X J9 Q J ROY METEOR SOC JI Q. J. R. Meteorol. Soc. PD JUL PY 2015 VL 141 IS 690 BP 1906 EP 1921 DI 10.1002/qj.2495 PN A PG 16 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA CP9HE UT WOS:000360203800033 ER PT J AU Schinder, PJ Flasar, FM Marouf, EA French, RG Anabtawi, A Barbinis, E Kliore, AJ AF Schinder, P. J. Flasar, F. M. Marouf, E. A. French, R. G. Anabtawi, A. Barbinis, E. Kliore, A. J. TI A numerical technique for two-way radio occultations by oblate axisymmetric atmospheres with zonal winds SO RADIO SCIENCE LA English DT Article DE occultation; technique; two way ID TITANS ATMOSPHERE; B RING; VENUS; MARS AB The Ultra Stable Oscillator aboard the Cassini spacecraft failed in late 2011, which means that all radio occultations after that date have to be done in two-way mode, using a ground-based signal transmitted to the spacecraft as the frequency reference. Here we present the numerical technique we use to analyze the data from the two-way atmospheric radio occultations of both Saturn and Titan that have occurred since the Ultra Stable Oscillator (USO) failure, along with the theoretical reasons behind this technique. Since our two-way technique is based upon our earlier one-way technique which used the USO as the frequency reference, we also present our one-way technique which we used for Saturn occultations prior to the loss of the USO. C1 [Schinder, P. J.] Cornell Univ, Ctr Radiophys & Space Res, Ithaca, NY 14853 USA. [Flasar, F. M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Marouf, E. A.] San Jose State Univ, Dept Elect Engn, San Jose, CA 95192 USA. [French, R. G.] Wellesley Coll, Dept Astron, Wellesley, MA 02181 USA. [Anabtawi, A.; Barbinis, E.; Kliore, A. J.] CALTECH, Jet Prop Lab, Pasadena, CA 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 21 TC 1 Z9 1 U1 1 U2 2 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0048-6604 EI 1944-799X J9 RADIO SCI JI Radio Sci. PD JUL PY 2015 VL 50 IS 7 BP 712 EP 727 DI 10.1002/2015RS005690 PG 16 WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences; Remote Sensing; Telecommunications SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences; Remote Sensing; Telecommunications GA CP7NQ UT WOS:000360075300012 ER PT J AU Tan, FY Lim, HS Abdullah, K Yoon, TL Holben, B AF Tan, Fuyi Lim, Hwee San Abdullah, Khiruddin Yoon, Tiem Leong Holben, Brent TI AERONET data-based determination of aerosol types SO ATMOSPHERIC POLLUTION RESEARCH LA English DT Article DE Seasonal monsoon; aerosol; aerosol optical depth (AOD); angstrom exponent; precipitable water (PW) ID TROPICAL COASTAL STATION; SUN-PHOTOMETER DATA; OPTICAL DEPTH; ANGSTROM EXPONENT; TEMPORAL HETEROGENEITY; ATMOSPHERIC AEROSOL; URBAN AREA; ACE-ASIA; PART 1; MODELS AB Aerosols are among the most interesting topics investigated by researchers because of their complicated characteristics and poor quantification. Moreover, significant uncertainties are associated with changes in the Earth's radiation budget. Previous studies have shown numerous difficulties and challenges in quantifying aerosol influences. In addition, the heterogeneity from aerosol loading and properties, including spatial, temporal, size, and composition features, presents a challenge. In this study, we investigated aerosol characteristics over two regions with different environmental conditions and aerosol sources. The study sites are Penang and Kuching in Malaysia, where a ground-based AErosol RObotic NETwork (AERONET) sun-photometer was deployed. The types of aerosol, such as biomass burning, urban/industrial, marine, and dust aerosols, for both study sites were identified by analyzing aerosol optical depth and angstrom exponent. Seasonal monsoon variation results in different aerosol optical properties, characteristics, and types of aerosols that are dominant in Penang and Kuching. Seasonal monsoon flow trend patterns from a seven-day back-trajectory frequency plotted by the Hybrid Single-Particle Lagrangian Integrated Trajectory model illustrated the distinct origins of trans-boundary aerosol sources. Finally, we improved our findings in Malaysian sites using the AERONET data from Singapore and Indonesia. Similarities in the optical properties of aerosols and the distribution types (referred to as homogeneous aerosol) were observed in the Penang-Singapore and the Kuching-Pontianak sites. The dominant aerosol distribution types were completely different for locations in the western (Penang-Singapore) and eastern (Kuching-Pontianak) parts of the South China Sea. This is a result of spatial and temporal heterogeneity. The spatial and temporal heterogeneities for the western and eastern portions of South China Sea provide information on the natural or anthropogenic processes that take place. C1 [Tan, Fuyi; Lim, Hwee San; Abdullah, Khiruddin; Yoon, Tiem Leong] Univ Sains Malaysia, Sch Phys, Gelugor, Penang, Malaysia. [Holben, Brent] NASA, Goddard Space Flight Ctr, Bethesda, MD USA. RP Tan, FY (reprint author), Univ Sains Malaysia, Sch Phys, Gelugor, Penang, Malaysia. EM fuyitan@yahoo.com RI Lim, Hwee San/F-6580-2010 OI Lim, Hwee San/0000-0002-4835-8015 FU RU [1001/PFIZIK/811228]; RUI-PRGS grant [1001/PFIZIK/846083]; Universiti Sains Malaysia-Short Term Grant [304/PFIZIK/6310057] FX The authors gratefully acknowledge the financial support provided by RU (Grant No. 1001/PFIZIK/811228) and RUI-PRGS grants (Grant No. 1001/PFIZIK/846083). The Universiti Sains Malaysia-Short Term Grant 304/PFIZIK/6310057 was likewise used to implement this project. The authors are also grateful to the members of the NASA Goddard Space Flight Center who helped with the set up and the site members who helped to maintain AERONET in Penang and Kuching. The authors also acknowledge Dr. Smimov from NASA for fruitful discussions on certain issues. The author also would like to thank Hui Qi Lim and Yeap Eng Choon who provided information for this study. NR 45 TC 2 Z9 2 U1 1 U2 10 PU TURKISH NATL COMMITTEE AIR POLLUTION RES & CONTROL-TUNCAP PI BUCA PA DOKUZ EYLUL UNIV, DEPT ENVIRONMENTAL ENGINEERING, TINAZTEPE CAMPUS, BUCA, IZMIR 35160, TURKEY SN 1309-1042 J9 ATMOS POLLUT RES JI Atmos. Pollut. Res. PD JUL PY 2015 VL 6 IS 4 BP 682 EP 695 DI 10.5094/APR.2015.077 PG 14 WC Environmental Sciences SC Environmental Sciences & Ecology GA CP5UW UT WOS:000359951500017 ER PT J AU Hegerl, GC Black, E Allan, RP Ingram, WJ Polson, D Trenberth, KE Chadwick, RS Arkin, PA Sarojini, BB Becker, A Dai, AG Durack, PJ Easterling, D Fowler, HJ Kendon, EJ Huffman, GJ Liu, CL Marsh, R New, M Osborn, TJ Skliris, N Stott, PA Vidale, PL Wijffels, SE Wilcox, LJ Willett, KM Zhang, XB AF Hegerl, Gabriele C. Black, Emily Allan, Richard P. Ingram, William J. Polson, Debbie Trenberth, Kevin E. Chadwick, Robin S. Arkin, Phillip A. Sarojini, Beena Balan Becker, Andreas Dai, Aiguo Durack, Paul J. Easterling, David Fowler, Hayley J. Kendon, Elizabeth J. Huffman, George J. Liu, Chunlei Marsh, Robert New, Mark Osborn, Timothy J. Skliris, Nikolaos Stott, Peter A. Vidale, Pier-Luigi Wijffels, Susan E. Wilcox, Laura J. Willett, Kate M. Zhang, Xuebin TI CHALLENGES IN QUANTIFYING CHANGES IN THE GLOBAL WATER CYCLE SO BULLETIN OF THE AMERICAN METEOROLOGICAL SOCIETY LA English DT Article ID EXPLAINING EXTREME EVENTS; CLIMATE-CHANGE; PRECIPITATION EXTREMES; ANTHROPOGENIC AEROSOLS; TROPICAL PRECIPITATION; HYDROLOGICAL CYCLE; SURFACE HUMIDITY; INTENSE PRECIPITATION; REGIONAL PERSPECTIVE; NORTHERN-HEMISPHERE C1 [Hegerl, Gabriele C.; Polson, Debbie] Univ Edinburgh, Sch GeoSci, Grant Inst, Edinburgh EH8 9YL, Midlothian, Scotland. [Black, Emily; Allan, Richard P.; Sarojini, Beena Balan; Liu, Chunlei; Vidale, Pier-Luigi; Wilcox, Laura J.] Univ Reading, Dept Meteorol, Natl Ctr Atmospher Sci Climate, Reading, Berks, England. [Ingram, William J.; Chadwick, Robin S.; Kendon, Elizabeth J.; Stott, Peter A.; Willett, Kate M.] Hadley Ctr, Met Off, Exeter, Devon, England. [Ingram, William J.] Univ Oxford, Dept Phys, Oxford, England. [Trenberth, Kevin E.; Dai, Aiguo] Natl Ctr Atmospher Res, Boulder, CO 80307 USA. [Arkin, Phillip A.] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. [Becker, Andreas] Deutsch Wetterdienst, Offenbach, Germany. [Dai, Aiguo] SUNY Albany, Dept Atmospher & Environm Sci, Albany, NY 12222 USA. [Durack, Paul J.] Lawrence Livermore Natl Lab, Program Climate Model Diag & Intercomparison, Livermore, CA USA. [Durack, Paul J.; Wijffels, Susan E.] CSIRO, Hobart, Tas, Australia. [Easterling, David] NOAA, Natl Climat Data Ctr, Asheville, NC USA. [Fowler, Hayley J.] Newcastle Univ, Sch Civil Engn & Geosci, Newcastle Upon Tyne NE1 7RU, Tyne & Wear, England. [Huffman, George J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Marsh, Robert; Skliris, Nikolaos] Univ Southampton, Ocean & Earth Sci, Southampton, Hants, England. [New, Mark] Univ Cape Town, ZA-7700 Cape Town, South Africa. [Osborn, Timothy J.] Univ E Anglia, Sch Environm Sci, Climat Res Unit, Norwich NR4 7TJ, Norfolk, England. [Zhang, Xuebin] Environm Canada, Div Climate Res, Toronto, ON, Canada. RP Hegerl, GC (reprint author), Grant Inst, GeoSci, Kings Bldg,James Hutton Rd, Edinburgh EH9 3FE, Midlothian, Scotland. EM gabi.hegerl@ed.ac.uk RI New, Mark/A-7684-2008; Huffman, George/F-4494-2014; Durack, Paul/A-8758-2010; Stott, Peter/N-1228-2016; Trenberth, Kevin/A-5683-2012; Allan, Richard/B-5782-2008; Dai, Aiguo/D-3487-2009 OI New, Mark/0000-0001-6082-8879; Huffman, George/0000-0003-3858-8308; Durack, Paul/0000-0003-2835-1438; Stott, Peter/0000-0003-4853-7686; Trenberth, Kevin/0000-0002-1445-1000; Allan, Richard/0000-0003-0264-9447; Fowler, Hayley/0000-0001-8848-3606; Vidale, Pier Luigi/0000-0002-1800-8460; Marsh, Robert/0000-0002-1051-8749; FU U.K. Natural Environment Research Council (NERC) [NE/I006672/1]; DECC/Defra Met Office Hadley Centre Climate Programme [GA01101]; Lawrence Livermore National Laboratory - U.S. Department of Energy [DE-AC52-07NA27344]; NERC [NE/I00680X/1]; NCAS; NASA [NNX11AG69G]; PAGODA project of the Changing Water Cycle programme of NERC [NE/I006672/1]; ERC [EC320691]; NSF [AGS-1353740]; Wolfson Foundation; Royal Society as Royal Society Wolfson Research Merit Award [WM140025, WM130060]; European Research Council (TITAN) [ERC-2012-AdG 320691]; CONVEX project of the Changing Water Cycle programme of NERC [NE/I006680/1]; European Research Council FX We thank several anonymous reviewers for their helpful and perceptive suggestions. The workshop that formed the basis for this paper was funded by the U.K. Natural Environment Research Council (NERC Grant NE/I006672/1). We thank Eleanor Blyth and David Parker for comments. Robin Chadwick, Kate Willett, William Ingram, Lizzie Kendon, and Peter Stott were supported by the Joint DECC/Defra Met Office Hadley Centre Climate Programme (GA01101). Paul Durack is supported by the Lawrence Livermore National Laboratory that is funded by the U.S. Department of Energy under Contract DE-AC52-07NA27344, and William Ingram is partly supported by NERC Grant NE/I00680X/1. Gabi Hegerl and Richard Allan are partly supported by NCAS. Kevin Trenberth is supported by NASA Grant NNX11AG69G. P. L. Vidale, R. P. Allan, B. Balan Sarojini, C. Liu, E. Black, P. Stott, G. Hegerl, D. Polson, R. Marsh, N. Skliris, and Laura Wilcox are supported by the PAGODA project of the Changing Water Cycle programme of NERC under Grant NE/I006672/1. G. Hegerl and D. Polson are supported by the ERC Grant EC320691. A. Dai acknowledges the support of NSF Grant AGS-1353740. H. J. Fowler and G. Hegerl are funded by the Wolfson Foundation and the Royal Society as Royal Society Wolfson Research Merit Award (WM140025 and WM130060, respectively) holders. G. Hegerl is further supported by the European Research Council (TITAN, ERC-2012-AdG 320691). H. J. Fowler is supported by the CONVEX project of the Changing Water Cycle programme of NERC under Grant NE/I006680/1 and European Research Council funded INTENSE (ERC-2013-CoG). NR 164 TC 16 Z9 16 U1 13 U2 60 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0003-0007 EI 1520-0477 J9 B AM METEOROL SOC JI Bull. Amer. Meteorol. Soc. PD JUL PY 2015 VL 96 IS 7 BP 1097 EP 1115 PG 19 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA CP4LX UT WOS:000359854600004 ER PT J AU Richey, AS Thomas, BF Lo, MH Famiglietti, JS Swenson, S Rodell, M AF Richey, Alexandra S. Thomas, Brian F. Lo, Min-Hui Famiglietti, James S. Swenson, Sean Rodell, Matthew TI Uncertainty in global groundwater storage estimates in a Total Groundwater Stress framework SO WATER RESOURCES RESEARCH LA English DT Article DE groundwater resilience; aquifer storage; depletion timescales; total stress; remote sensing ID HIGH-PLAINS AQUIFER; WATER-RESOURCES; GRACE MEASUREMENTS; CLIMATE-CHANGE; SOIL-MOISTURE; SUSTAINABILITY; DEPLETION; SYSTEM; VULNERABILITY; RESILIENCE AB Groundwater is a finite resource under continuous external pressures. Current unsustainable groundwater use threatens the resilience of aquifer systems and their ability to provide a long-term water source. Groundwater storage is considered to be a factor of groundwater resilience, although the extent to which resilience can be maintained has yet to be explored in depth. In this study, we assess the limit of groundwater resilience in the world's largest groundwater systems with remote sensing observations. The Total Groundwater Stress (TGS) ratio, defined as the ratio of total storage to the groundwater depletion rate, is used to explore the timescales to depletion in the world's largest aquifer systems and associated groundwater buffer capacity. We find that the current state of knowledge of large-scale groundwater storage has uncertainty ranges across orders of magnitude that severely limit the characterization of resilience in the study aquifers. Additionally, we show that groundwater availability, traditionally defined as recharge and redefined in this study as total storage, can alter the systems that are considered to be stressed versus unstressed. We find that remote sensing observations from NASA's Gravity Recovery and Climate Experiment can assist in providing such information at the scale of a whole aquifer. For example, we demonstrate that a groundwater depletion rate in the Northwest Sahara Aquifer System of 2.690.8 km(3)/yr would result in the aquifer being depleted to 90% of its total storage in as few as 50 years given an initial storage estimate of 70 km(3). C1 [Richey, Alexandra S.; Famiglietti, James S.] Univ Calif Irvine, Dept Civil & Environm Engn, Irvine, CA 92697 USA. [Thomas, Brian F.; Famiglietti, James S.] CALTECH, NASA, Jet Prop Lab, Pasadena, CA 91125 USA. [Lo, Min-Hui] Natl Taiwan Univ, Dept Atmospher Sci, Taipei 10764, Taiwan. [Famiglietti, James S.] Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA USA. [Swenson, Sean] Natl Ctr Atmospher Res, Climate & Global Dynam Div, Boulder, CO 80307 USA. [Rodell, Matthew] NASA, Goddard Space Flight Ctr, Hydrol Sci Lab, Greenbelt, MD 20771 USA. RP Famiglietti, JS (reprint author), Univ Calif Irvine, Dept Civil & Environm Engn, Irvine, CA 92697 USA. EM jfamigli@uci.edu RI Rodell, Matthew/E-4946-2012; OI Rodell, Matthew/0000-0003-0106-7437; LO, MIN-HUI/0000-0002-8653-143X FU U.S. National Aeronautics and Space Administration under the GRACE Science Team program; U.S. National Aeronautics and Space Administration under Earth and Space Science Fellowship; University of California Office of the President Multicampus Research Programs and Initiatives program; MOST [104-2923-M-002-002-MY4]; National Aeronautics and Space Administration FX We gratefully acknowledge support from the U.S. National Aeronautics and Space Administration under the GRACE Science Team program and an Earth and Space Science Fellowship awarded to the first author. Critical support was also provided by the University of California Office of the President Multicampus Research Programs and Initiatives program. Min-Hui Lo is supported by the grant of MOST 104-2923-M-002-002-MY4. A portion of the research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. This study was also made possible using freely available data from the Global Land Data Assimilation System (http://disc.sci.gsfc.nasa.gov/hydrology/data-holdings). Additional data used in this study are available from the authors upon request (arichey@uci.edu). The authors thank the anonymous reviewers for their insights and recommendations, which have greatly improved this work. Finally, we thank John Thomas Reager and Caroline deLinage for their thoughtful contributions to the direction of this work. NR 113 TC 21 Z9 21 U1 10 U2 51 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0043-1397 EI 1944-7973 J9 WATER RESOUR RES JI Water Resour. Res. PD JUL PY 2015 VL 51 IS 7 BP 5198 EP 5216 DI 10.1002/2015WR017351 PG 19 WC Environmental Sciences; Limnology; Water Resources SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Water Resources GA CP7PM UT WOS:000360080200018 ER PT J AU Richey, AS Thomas, BF Lo, MH Reager, JT Famiglietti, JS Voss, K Swenson, S Rodell, M AF Richey, Alexandra S. Thomas, Brian F. Lo, Min-Hui Reager, John T. Famiglietti, James S. Voss, Katalyn Swenson, Sean Rodell, Matthew TI Quantifying renewable groundwater stress with GRACE SO WATER RESOURCES RESEARCH LA English DT Article DE stress regimes; large aquifers; remote sensing; anthropogenic biomes; groundwater stress ID WATER-TABLE DYNAMICS; SYNTHETIC-APERTURE RADAR; DESERT VADOSE ZONES; LAND-SURFACE SCHEME; HIGH-PLAINS AQUIFER; CLIMATE-CHANGE; FRESH-WATER; SAFE YIELD; CENTRAL-AFRICA; BUDGET MYTH AB Groundwater is an increasingly important water supply source globally. Understanding the amount of groundwater used versus the volume available is crucial to evaluate future water availability. We present a groundwater stress assessment to quantify the relationship between groundwater use and availability in the world's 37 largest aquifer systems. We quantify stress according to a ratio of groundwater use to availability, which we call the Renewable Groundwater Stress ratio. The impact of quantifying groundwater use based on nationally reported groundwater withdrawal statistics is compared to a novel approach to quantify use based on remote sensing observations from the Gravity Recovery and Climate Experiment (GRACE) satellite mission. Four characteristic stress regimes are defined: Overstressed, Variable Stress, Human-dominated Stress, and Unstressed. The regimes are a function of the sign of use (positive or negative) and the sign of groundwater availability, defined as mean annual recharge. The ability to mitigate and adapt to stressed conditions, where use exceeds sustainable water availability, is a function of economic capacity and land use patterns. Therefore, we qualitatively explore the relationship between stress and anthropogenic biomes. We find that estimates of groundwater stress based on withdrawal statistics are unable to capture the range of characteristic stress regimes, especially in regions dominated by sparsely populated biome types with limited cropland. GRACE-based estimates of use and stress can holistically quantify the impact of groundwater use on stress, resulting in both greater magnitudes of stress and more variability of stress between regions. C1 [Richey, Alexandra S.; Famiglietti, James S.] Univ Calif Irvine, Dept Civil & Environm Engn, Irvine, CA 92697 USA. [Thomas, Brian F.; Reager, John T.; Famiglietti, James S.] CALTECH, NASA, Jet Prop Lab, Pasadena, CA 91125 USA. [Lo, Min-Hui] Natl Taiwan Univ, Dept Atmospher Sci, Taipei 10764, Taiwan. [Famiglietti, James S.] Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA USA. [Voss, Katalyn] Univ Calif Santa Barbara, Dept Geog, Santa Barbara, CA 93106 USA. [Swenson, Sean] Natl Ctr Atmospher Res, Climate & Global Dynam Div, Boulder, CO 80307 USA. [Rodell, Matthew] NASA, Goddard Space Flight Ctr, Hydrol Sci Lab, Greenbelt, MD 20771 USA. RP Famiglietti, JS (reprint author), Univ Calif Irvine, Dept Civil & Environm Engn, Irvine, CA 92697 USA. EM jfamigli@uci.edu RI Rodell, Matthew/E-4946-2012; OI Rodell, Matthew/0000-0003-0106-7437; LO, MIN-HUI/0000-0002-8653-143X FU U.S. National Aeronautics and Space Administration under the GRACE Science Team program; U.S. National Aeronautics and Space Administration under Earth and Space Science Fellowship; University of California Office of the President Multicampus Research Programs and Initiatives program; MOST [104-2923-M-002-002-MY4]; National Aeronautics and Space Administration FX We gratefully acknowledge support from the U.S. National Aeronautics and Space Administration under the GRACE Science Team program and an Earth and Space Science Fellowship awarded to the first author. Critical support was also provided by the University of California Office of the President Multicampus Research Programs and Initiatives program. Min-Hui Lo is supported by the grant of MOST 104-2923-M-002-002-MY4. A portion of the research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. This study was also made possible using freely available data from the Global Land Data Assimilation System (http://disc.sci.gsfc.nasa.gov/hydrology/data-holdings), the GWSP Digital Water Atlas (http://atlas.gwsp.org/), and the Anthropogenic Biomes of the World, Version 1 dataset from the NASA Socioeconomic Data and Applications Center (SEDAC, http://sedac.ciesin.columbia.edu/). Additional data used in this study is available from the authors upon request (arichey@uci.edu). Thank you to the editor who's comments and suggestions greatly improved the manuscript. Finally, we thank Caroline deLinage for her thoughtful contributions to the direction of this work. NR 110 TC 52 Z9 52 U1 15 U2 80 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0043-1397 EI 1944-7973 J9 WATER RESOUR RES JI Water Resour. Res. PD JUL PY 2015 VL 51 IS 7 BP 5217 EP 5238 DI 10.1002/2015WR017349 PG 22 WC Environmental Sciences; Limnology; Water Resources SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Water Resources GA CP7PM UT WOS:000360080200019 ER PT J AU Draper, DW Newell, DA Wentz, FJ Krimchansky, S Skofronick-Jackson, GM AF Draper, David W. Newell, David A. Wentz, Frank J. Krimchansky, Sergey Skofronick-Jackson, Gail M. TI The Global Precipitation Measurement (GPM) Microwave Imager (GMI): Instrument Overview and Early On-Orbit Performance SO IEEE JOURNAL OF SELECTED TOPICS IN APPLIED EARTH OBSERVATIONS AND REMOTE SENSING LA English DT Article; Proceedings Paper CT IEEE Joint International Geoscience and Remote Sensing Symposium (IGARSS) / 35th Canadian Symposium on Remote Sensing CY JUL 13-18, 2014 CL Quebec City, CANADA SP IEEE, Inst Elect & Elect Engineers, Geoscience & Remote Sensing Soc, Canadian Remote Sensing Soc DE Calibration accuracy; passive microwave remote sensing; radiometric sensitivity ID MEASURING MISSION TRMM; OCEAN SURFACE; CALIBRATION AB The Global Precipitation Measurement (GPM) mission is an international satellite mission that uses measurements from an advanced radar/radiometer system on a core observatory as reference standards to unify and advance precipitation estimates made by a constellation of research and operational microwave sensors. The GPM core observatory was launched on February 27, 2014 at 18: 37 UT in a 65. inclination nonsun-synchronous orbit. GPM focuses on precipitation as a key component of the Earth's water and energy cycle, and has the capability to provide near-real-time observations for tracking severe weather events, monitoring freshwater resources, and other societal applications. The GPM microwave imager (GMI) on the core observatory provides the direct link to the constellation radiometer sensors, which fly mainly in polar orbits. The GMI sensitivity, accuracy, and stability play a crucial role in unifying the measurements from the GPM constellation of satellites. The instrument has exhibited highly stable operations through the duration of the calibration/validation period. This paper provides an overview of the GMI instrument and a report of early on-orbit commissioning activities. It discusses the on-orbit radiometric sensitivity, absolute calibration accuracy, and stability for each radiometric channel. C1 [Draper, David W.; Newell, David A.] Ball Aerosp & Technol Corp, Boulder, CO 80301 USA. [Wentz, Frank J.] Remote Sensing Syst, Santa Rosa, CA 95401 USA. [Krimchansky, Sergey; Skofronick-Jackson, Gail M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Draper, DW (reprint author), Ball Aerosp & Technol Corp, Boulder, CO 80301 USA. EM ddraper@ball.com; dnewell@ball.com; frank.wentz@remss.com; sergey.krimchansky@nasa.gov; gail.s.jackson@nasa.gov RI Skofronick-Jackson, Gail/D-5354-2012; Measurement, Global/C-4698-2015 FU Goddard Space Flight Center GPM program FX This work was supported by the Goddard Space Flight Center GPM program. NR 17 TC 24 Z9 24 U1 2 U2 14 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1939-1404 EI 2151-1535 J9 IEEE J-STARS JI IEEE J. Sel. Top. Appl. Earth Observ. Remote Sens. PD JUL PY 2015 VL 8 IS 7 SI SI BP 3452 EP 3462 DI 10.1109/JSTARS.2015.2403303 PG 11 WC Engineering, Electrical & Electronic; Geography, Physical; Remote Sensing; Imaging Science & Photographic Technology SC Engineering; Physical Geography; Remote Sensing; Imaging Science & Photographic Technology GA CP0AR UT WOS:000359538700019 ER PT J AU Kim, SB Jackson, TJ Yueh, SH Xu, XL Hensley, S AF Kim, Seung-bum Jackson, Thomas J. Yueh, Simon H. Xu, Xiaolan Hensley, Scott TI Feasibility of Inter-Comparing Airborne and Spaceborne Observations of Radar Backscattering Coefficients SO IEEE JOURNAL OF SELECTED TOPICS IN APPLIED EARTH OBSERVATIONS AND REMOTE SENSING LA English DT Article; Proceedings Paper CT IEEE Joint International Geoscience and Remote Sensing Symposium (IGARSS) / 35th Canadian Symposium on Remote Sensing CY JUL 13-18, 2014 CL Quebec City, CANADA SP IEEE, Inst Elect & Elect Engineers, Geoscience & Remote Sensing Soc, Canadian Remote Sensing Soc DE Calibration; scatterometer; soil moisture; soil moisture active passive (SMAP); synthetic aperture radar (SAR) ID EXPERIMENT 2012 SMAPVEX12; SOIL-MOISTURE RETRIEVAL; ACTIVE L-BAND; VALIDATION AB This paper investigates the feasibility of using an airborne synthetic aperture radar (SAR) to validate spaceborne SAR data. This is directed at soil moisture sensing and the recently launched soil moisture active passive (SMAP) satellite. The value of this approach is related to the fact that vicarious targets such as rain forests and oceans calibrate only the extrema of backscattering coefficients (sigma(0)) and that the relationship between soil moisture and sigma(0) is nonlinear. Furthermore, corner reflectors are difficult to deploy to calibrate medium resolution (1-3 km) spaceborne sensors such as the one onboard SMAP. A challenge with the approach is the varying incidence angle (theta(inc)) of the airborne sensor versus the constant value used by SMAP. The impact of this on the inter-comparison of airborne and SMAP data is analyzed through simulation and aircraft data analysis. In the absence of the SMAP SAR data, the airborne SAR and scatterometer sigma(0) from the recent field campaign provided the imaging geometry similar to the spaceborne case. The effect of theta(inc) on the intercomparison using these two airborne data sets was found to be small if the landcover within the footprint is homogeneous and if sigma(0) (natural unit) changes very little or approximately linearly with theta(inc). Over heterogeneous pixels consisting of pasture, grass, forest, and growing corn, the simulation shows that the mean and standard deviation of the difference in sigma(0) between the SAR and scatterometer data are smaller than 0.4 and 0.3 dB, respectively. The test results with the airborne data are generally consistent with the simulation results: the mean and standard deviation of the difference are smaller than 0.9 dB for HH, VV, and HV. These magnitudes are comparable with those of the major sources of the difference: the relative calibration errors of the airborne instruments (<0.3 dB), speckle noise (similar to 0.35 dB), effect of theta(inc) variation within the footprint (<0.4 dB), and geolocation uncertainty in the airborne scatterometer data (<0.5 dB). The findings from this study are expected to apply to the inter-comparison of the SMAP and airborne data after considering the details affecting the comparison: imaging geometry, temporal synchronization, spatial collocation, antenna gain, speckle noise, and spatial resolution. When applied, the inter-comparison will provide more confidence in the calibration of SMAP. C1 [Kim, Seung-bum; Yueh, Simon H.; Xu, Xiaolan; Hensley, Scott] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Jackson, Thomas J.] USDA, ARS Hydrol & Remote Sensing Lab, Beltsville, MD 20705 USA. RP Kim, SB (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. EM seungbum.kim@jpl.nasa.gov NR 21 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 1939-1404 EI 2151-1535 J9 IEEE J-STARS JI IEEE J. Sel. Top. Appl. Earth Observ. Remote Sens. PD JUL PY 2015 VL 8 IS 7 SI SI BP 3507 EP 3519 DI 10.1109/JSTARS.2015.2424715 PG 13 WC Engineering, Electrical & Electronic; Geography, Physical; Remote Sensing; Imaging Science & Photographic Technology SC Engineering; Physical Geography; Remote Sensing; Imaging Science & Photographic Technology GA CP0AR UT WOS:000359538700024 ER PT J AU Lee, SK Fatoyinbo, TE AF Lee, Seung-Kuk Fatoyinbo, Temilola E. TI TanDEM-X Pol-InSAR Inversion for Mangrove Canopy Height Estimation SO IEEE JOURNAL OF SELECTED TOPICS IN APPLIED EARTH OBSERVATIONS AND REMOTE SENSING LA English DT Article; Proceedings Paper CT IEEE Joint International Geoscience and Remote Sensing Symposium (IGARSS) / 35th Canadian Symposium on Remote Sensing CY JUL 13-18, 2014 CL Quebec City, CANADA SP IEEE, Inst Elect & Elect Engineers, Geoscience & Remote Sensing Soc, Canadian Remote Sensing Soc DE Mangrove; Pol-InSAR; single- and dual-pol; TanDEM-X (TDX); water-level elevation ID POLARIMETRIC SAR INTERFEROMETRY; COHERENT SCATTERERS; ELEVATION DATA; RADAR; FORESTS; DECORRELATION; ICESAT/GLAS; TOPOGRAPHY; BIOMASS; MODEL AB This paper presents mangrove canopy height estimations using single-and dual-pol TanDEM-X (TDX) data by means of Pol-InSAR techniques. Using the TDX data for forest applications, the penetration capability of X-band into the volume and the polarimetric diversity of interferometric coherence can create false effects that could sometimes lead to biased three-dimensional (3-D) forest parameter estimation. Moreover, in the case of single-pol TDX acquisition (i.e., one independent complex interferometric coherence), it is not possible to perform the inversion without external topographic information due to the underdetermined problem for Pol-InSAR inversion. To solve these problems, the ground phase in the Pol-InSAR model has been estimated directly from TDX interferograms with an assumption that the underlying topography (i.e., water surface level) over mangroves is flat and negligible. With the estimated ground phase that represents water-level elevation in mangroves, the Pol-InSAR inversion from the single-and dual-pol TDX data did not rely on an external DTM data set. The inversion results were validated against airborne lidar measurements in Campeche, Mexico, and in the Zambezi Delta, Mozambique. The single-and dual-pol inversion results showed a successful inversion performance with a high correlation coefficient (0.851-0.919) and with low RMSEs (1.069-1.727 m). The entire inversion performance quality over mangroves at X-band could reach to 10% height estimation accuracy. In addition to Pol-InSAR inversion results, the location of phase center was checked and assessed. The results showed a surprisingly deep location of phase centers from top mangrove canopy (5-7 m, up to 12.36 m) with a similarity at HH and VV polarization. C1 [Lee, Seung-Kuk; Fatoyinbo, Temilola E.] NASA GSFC, Biospher Sci Lab, Greenbelt, MD 20771 USA. RP Lee, SK (reprint author), NASA GSFC, Biospher Sci Lab, Greenbelt, MD 20771 USA. EM SeungKuk.Lee@nasa.gov; Lola.fatoyinbo@nasa.gov RI Fatoyinbo, Temilola/G-6104-2012 OI Fatoyinbo, Temilola/0000-0002-1130-6748 FU National Aeronautics and Space Administration (NASA) Postdoctoral Program; NASA Carbon Monitoring System Program FX This research was supported in part by the National Aeronautics and Space Administration (NASA) Postdoctoral Program and in part by the NASA Carbon Monitoring System Program. NR 38 TC 6 Z9 6 U1 2 U2 8 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1939-1404 EI 2151-1535 J9 IEEE J-STARS JI IEEE J. Sel. Top. Appl. Earth Observ. Remote Sens. PD JUL PY 2015 VL 8 IS 7 SI SI BP 3608 EP 3618 DI 10.1109/JSTARS.2015.2431646 PG 11 WC Engineering, Electrical & Electronic; Geography, Physical; Remote Sensing; Imaging Science & Photographic Technology SC Engineering; Physical Geography; Remote Sensing; Imaging Science & Photographic Technology GA CP0AR UT WOS:000359538700033 ER PT J AU Tan, S Aksoy, M Brogioni, M Macelloni, G Durand, M Jezek, KC Wang, TL Tsang, L Johnson, JT Drinkwater, MR Brucker, L AF Tan, Shurun Aksoy, Mustafa Brogioni, Marco Macelloni, Giovanni Durand, Michael Jezek, Kenneth C. Wang, Tian-Lin Tsang, Leung Johnson, Joel T. Drinkwater, Mark R. Brucker, Ludovic TI Physical Models of Layered Polar Firn Brightness Temperatures From 0.5 to 2 GHz SO IEEE JOURNAL OF SELECTED TOPICS IN APPLIED EARTH OBSERVATIONS AND REMOTE SENSING LA English DT Article; Proceedings Paper CT IEEE Joint International Geoscience and Remote Sensing Symposium (IGARSS) / 35th Canadian Symposium on Remote Sensing CY JUL 13-18, 2014 CL Quebec City, CANADA SP IEEE, Inst Elect & Elect Engineers, Geoscience & Remote Sensing Soc, Canadian Remote Sensing Soc DE Brightness temperature; coherent; incoherent; layered polar firn emission; Ultra Wide Band Software Defined Radiometer (UWBRAD) ID COMPLEX DIELECTRIC-CONSTANT; MICROWAVE EMISSION MODEL; ICE-SHEET; DOME-C; GRAIN-SIZE; SNOW; ANTARCTICA; SNOWPACKS AB We investigate physical effects influencing 0.5-2 GHz brightness temperatures of layered polar firn to support the Ultra Wide Band Software Defined Radiometer (UWBRAD) experiment to be conducted in Greenland and in Antarctica. We find that because ice particle grain sizes are very small compared to the 0.5-2 GHz wavelengths, volume scattering effects are small. Variations in firn density over cm-to m-length scales, however, cause significant effects. Both incoherent and coherent models are used to examine these effects. Incoherent models include a "cloud model" that neglects any reflections internal to the ice sheet, and the DMRT-ML and MEMLS radiative transfer codes that are publicly available. The coherent model is based on the layered medium implementation of the fluctuation dissipation theorem for thermal microwave radiation from a medium having a nonuniform temperature. Density profiles are modeled using a stochastic approach, and model predictions are averaged over a large number of realizations to take into account an averaging over the radiometer footprint. Density profiles are described by combining a smooth average density profile with a spatially correlated random process to model density fluctuations. It is shown that coherent model results after ensemble averaging depend on the correlation lengths of the vertical density fluctuations. If the correlation length is moderate or long compared with the wavelength (similar to 0.6x longer or greater for Gaussian correlation function without regard for layer thinning due to compaction), coherent and incoherent model results are similar (within similar to 1 K). However, when the correlation length is short compared to the wavelength, coherentmodel results are significantly different from the incoherent model by several tens of kelvins. For a 10-cm correlation length, the differences are significant between 0.5 and 1.1 GHz, and less for 1.1-2 GHz. Model results are shown to be able to match the v-pol SMOS data closely and predict the h-pol data for small observation angles. C1 [Tan, Shurun; Wang, Tian-Lin; Tsang, Leung] Univ Michigan, Dept Elect Engn & Comp Sci, Radiat Lab, Ann Arbor, MI 48109 USA. [Tan, Shurun; Wang, Tian-Lin; Tsang, Leung] Univ Washington, Dept Elect Engn, Seattle, WA 98195 USA. [Aksoy, Mustafa; Johnson, Joel T.] Ohio State Univ, Electrosci Lab, Columbus, OH 43212 USA. [Brogioni, Marco; Macelloni, Giovanni] Natl Res Council CNR, Nello Carrara Inst Appl Phys IFAC, I-50019 Florence, Italy. [Durand, Michael; Jezek, Kenneth C.] Ohio State Univ, Byrd Polar Res Ctr, Sch Earth Sci, Columbus, OH 43210 USA. [Drinkwater, Mark R.] European Space Agcy, European Space Res & Technol Ctr, Earth Observat Programmes, Miss Sci Div, NL-2201 AZ Noordwijk, Netherlands. [Brucker, Ludovic] NASA, Goddard Space Flight Ctr, Cryospher Sci Lab, Greenbelt, MD 20771 USA. [Brucker, Ludovic] Univ Space Res Assoc, Goddard Earth Sci Technol & Res Studies & Invest, Greenbelt, MD 20771 USA. RP Tan, S (reprint author), Univ Michigan, Elect Engn & Comp Sci, Ann Arbor, MI 48109 USA. RI Brucker, Ludovic/A-8029-2010; OI Brucker, Ludovic/0000-0001-7102-8084; Drinkwater, Mark/0000-0002-9250-3806 FU NASA's Instrument Incubator Program; NASA's Cryosphere Program FX This work was supported by Grants from NASA's Instrument Incubator Program and NASA's Cryosphere Program. NR 30 TC 4 Z9 4 U1 5 U2 9 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1939-1404 EI 2151-1535 J9 IEEE J-STARS JI IEEE J. Sel. Top. Appl. Earth Observ. Remote Sens. PD JUL PY 2015 VL 8 IS 7 SI SI BP 3681 EP 3691 DI 10.1109/JSTARS.2015.2403286 PG 11 WC Engineering, Electrical & Electronic; Geography, Physical; Remote Sensing; Imaging Science & Photographic Technology SC Engineering; Physical Geography; Remote Sensing; Imaging Science & Photographic Technology GA CP0AR UT WOS:000359538700040 ER PT J AU Li, J Carlson, BE Rossow, WB Lacis, AA Zhang, YC AF Li, Jing Carlson, Barbara E. Rossow, William B. Lacis, Andrew A. Zhang, Yuanchong TI An Intercomparison of the Spatiotemporal Variability of Satellite- and Ground-Based Cloud Datasets Using Spectral Analysis Techniques SO JOURNAL OF CLIMATE LA English DT Article ID AEROSOL OPTICAL DEPTH; STATISTICAL-ANALYSIS; DATA PRODUCTS; LEVEL CLOUDS; PART I; ISCCP; MODIS; CLIMATOLOGY; SYNERGY; CALIPSO AB Because of the importance of clouds in modulating Earth's energy budget, it is critical to understand their variability in space and time for climate and modeling studies. This study examines the consistency of the spatiotemporal variability of cloud amount (CA) and cloud-top pressure (CTP) represented by five 7-yr satellite datasets from the Global Energy and Water Cycle Experiment (GEWEX) cloud assessment project, and total cloud fraction observation from the Extended Edited Cloud Reports Archive (EECRA). Two spectral analysis techniques, namely combined maximum covariance analysis (CMCA) and combined principal component analysis (CPCA), are used to extract the dominant modes of variability from the combined datasets, and the resulting spatial patterns are compared in parallel. The results indicate that the datasets achieve overall excellent agreement on both seasonal and interannual scales of variability, with the correlations between the spatial patterns mostly above 0.6 and often above 0.8. For seasonal variability, the largest differences are found in the Northern Hemisphere high latitudes and near the South African coast for CA and in the Sahel region for CTP, where some differences in the phase and strength of the seasonal cycle are found. On interannual scales, global cloud variability is mostly associated with major climate modes, including El Nino-Southern Oscillation (ENSO), the Pacific decadal oscillation (PDO), and the Indian Ocean dipole mode (IODM), and the datasets also agree reasonably well. The good agreement across the datasets supports the conclusion that they are describing cloud variations with these climate modes. C1 [Li, Jing; Zhang, Yuanchong] Columbia Univ, NASA, Goddard Inst Space Studies, New York, NY USA. [Li, Jing; Zhang, Yuanchong] Columbia Univ, Dept Appl Phys & Appl Math, New York, NY USA. [Li, Jing; Carlson, Barbara E.; Lacis, Andrew A.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Rossow, William B.] CUNY City Coll, Cooperat Remote Sensing Sci & Technol Ctr, New York, NY 10031 USA. RP Li, J (reprint author), NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA. EM jl2862@columbia.edu FU NASA [509496.02.08.04.24]; Hal Maring; NASA FX We thank the GEWEX Cloud Assessment work group for providing the satellite datasets used in this study. The GEWEX Cloud Assessment datasets were obtained from the ClimServ Data Center of IPSL/CNRS, at http://climserv.ipsl.polytechnique.fr/gewexca/. The ISCCP D2 data were downloaded from NASA Langley Research Center Atmospheric Science Data Center (ASDC) at http://eosweb.larc.nasa.gov. The EECRA surface data are provided by the Research Data Archive at the National Center for Atmospheric Research, Computational and Information Systems Laboratory (http://rda.ucar.edu/datasets/ds292.2/). The data were accessed on 10 September 2013. The MEI ENSO index is provided by the NOAA Earth System Research Laboratory, available from http://www.esrl.noaa.gov/psd/ enso/mei/. The PDO index is downloaded from http://jisao.washington.edu/pdo/PDO.latest, and the DMI index is downloaded from http://www.jamstec.go.jp/. This study is funded by NASA Climate Grant 509496.02.08.04.24. Jing Li also acknowledges Hal Maring and the NASA Radiation Science program for providing funding for this investigation. NR 40 TC 1 Z9 1 U1 0 U2 3 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0894-8755 EI 1520-0442 J9 J CLIMATE JI J. Clim. PD JUL PY 2015 VL 28 IS 14 BP 5716 EP 5736 DI 10.1175/JCLI-D-14-00537.1 PG 21 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA CP1LR UT WOS:000359637800013 ER PT J AU Cheng, AN Xu, KM AF Cheng, Anning Xu, Kuan-Man TI Improved Low-Cloud Simulation from the Community Atmosphere Model with an Advanced Third-Order Turbulence Closure SO JOURNAL OF CLIMATE LA English DT Article ID BOUNDARY-LAYER CLOUDS; GENERAL-CIRCULATION MODEL; STRATOCUMULUS CLOUDS; CLIMATE SIMULATIONS; SOUTHEAST PACIFIC; PART II; CUMULUS CONVECTION; STRATIFORM CLOUDS; RADIATION BUDGET; RESOLVING MODEL AB In this study, a simplified intermediately prognostic higher-order turbulence closure (IPHOC) is implemented in the Community Atmosphere Model, version 5 (CAM5), to provide a consistent treatment of subgrid-scale cloud processes, except for deep convection. The planetary boundary layer (PBL) height is prognosticated to better resolve the discontinuity of temperature and moisture above the PBL top. Single-column model tests show that fluxes of liquid water potential temperature and total water, cloud fraction, and liquid water content are improved with this approach. The simplified IPHOC package replaces the boundary layer dry and moist turbulence parameterizations, the shallow convection parameterization, and the liquid-phase part of the cloud macrophysics parameterization in CAM5. CAM5-IPHOC improves the simulation of the low-level clouds off the west coasts of continents and the storm track region in the Southern Hemisphere (SH). The transition from stratocumulus to cumulus clouds is more gradual. There are also improvements on the cloud radiative forcing, especially shortwave, in the subsidence regime. The improvements in the relationships among low cloud amount, surface relative humidity, lower tropospheric stability, and PBL depth are seen in some stratocumulus regions. CAM5-IPHOC, however, produces weaker precipitation at the South Pacific convergence zone than CAM5 because of less energy flux into the SH atmosphere. The more downward surface shortwave radiative cooling and the less top-of-the-atmosphere longwave cloud radiative heating in the SH relative to the Northern Hemisphere explains the anomalous cooling and the lesser energy flux into the SH, which is related to the underestimate of extratropical middle/high clouds in the SH. C1 [Cheng, Anning] Sci Syst & Applicat Inc, Hampton, VA USA. [Cheng, Anning; Xu, Kuan-Man] NASA, Climate Sci Branch, Langley Res Ctr, Hampton, VA 23681 USA. RP Cheng, AN (reprint author), NASA, Climate Sci Branch, Langley Res Ctr, Mail Stop 420, Hampton, VA 23681 USA. EM anning.cheng@nasa.gov RI Xu, Kuan-Man/B-7557-2013 OI Xu, Kuan-Man/0000-0001-7851-2629 FU DOE [DE-SC0005450, DE-SC0008779] FX This work was supported by the DOE Atmospheric System Research Program under Interagency Agreements DE-SC0005450 and DE-SC0008779. The computational resources are provided by the local Icluster and Kcluster. The C3Mdata and CERES-EBAF version 2.6 data were obtained from the NASA Langley Research Center CERES ordering tool (http://ceres.larc.nasa.gov/). The GPCP data are maintained by and downloaded from NOAA/OAR/ESRL PSD, Boulder, Colorado (http://www.esrl.noaa.gov/psd/). NR 67 TC 7 Z9 7 U1 1 U2 10 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0894-8755 EI 1520-0442 J9 J CLIMATE JI J. Clim. PD JUL PY 2015 VL 28 IS 14 BP 5737 EP 5762 DI 10.1175/JCLI-D-14-00776.1 PG 26 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA CP1LR UT WOS:000359637800014 ER PT J AU Oh, JH Jiang, X Waliser, DE Moncrieff, MW Johnson, RH AF Oh, Ji-Hyun Jiang, Xianan Waliser, Duane E. Moncrieff, Mitchell W. Johnson, Richard H. TI Convective Momentum Transport Associated with the Madden-Julian Oscillation Based on a Reanalysis Dataset SO JOURNAL OF CLIMATE LA English DT Article ID TOGA COARE IOP; SIMPLE MULTICLOUD PARAMETERIZATION; GENERAL-CIRCULATION MODELS; TROPICAL WESTERN PACIFIC; CLOUD-RESOLVING MODEL; PART I; CLIMATE MODELS; COUPLED WAVES; INTRASEASONAL OSCILLATIONS; TRIMODAL CHARACTERISTICS AB A better understanding of multiscale interactions within the Madden-Julian oscillation (MJO), including momentum exchanges, is critical for improved MJO prediction skill. In this study, convective momentum transport (CMT) associated with the MJO is analyzed based on the NOAA Climate Forecast System Reanalysis (CFSR). A three-layer vertical structure associated with the MJO, as previously suggested in the mesoscale momentum tendency profile based on global cloud-resolving model simulations, is evident in the subgrid-scale momentum tendency from the CFSR. Positive (negative) subgrid-scale momentum tendency anomalies are found near the surface, negative (positive) anomalies are found in the low to midtroposphere, and positive (negative) anomalies in the upper troposphere are found within and to the west (east) of the MJO convection. This tends to damp the MJO circulation in the free atmosphere, while enhancing MJO winds near the surface. In addition, it could also reduce the MJO eastward propagation speed and lead to the backward tilt with height in the observed MJO structure through a secondary circulation near the MJO center. Further analyses illustrate that this three-layer vertical structure in subgrid-scale momentum tendency largely balances the grid-scale momentum transport of the zonal wind component u, mainly through the transport of seasonal mean u by the MJO-scale vertical motion. Synoptic-scale systems, which were previously proposed to be essential for the u-momentum transport of the MJO, however, are found to play a minor role for the total grid-scale momentum tendency. The above momentum tendency structure is also confirmed with the ECMWF analysis for the Year of Tropical Convection (YOTC) that lends confidence to these above results based on the CFSR. C1 [Oh, Ji-Hyun; Jiang, Xianan; Waliser, Duane E.] Univ Calif Los Angeles, Joint Inst Reg Earth Syst & Engn, Los Angeles, CA USA. [Oh, Ji-Hyun; Jiang, Xianan; Waliser, Duane E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Moncrieff, Mitchell W.] Natl Ctr Atmospher Res, Boulder, CO 80307 USA. [Johnson, Richard H.] Colorado State Univ, Ft Collins, CO 80523 USA. RP Jiang, X (reprint author), CALTECH, Jet Prop Lab, MS 233-300,4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM xianan@ucla.edu FU NSF Climate and Large-Scale Dynamics Program [AGS-1228302, AGS-1221013, AGS-1360237]; NOAA MAPP Program [NA12OAR4310075] FX We thank anonymous reviewers for their critical comments on an earlier version of this paper. This work has greatly benefited from stimulating discussions with Drs. A. Majda, T. Miyakawa, B. Mapes, M. Zhao, and G. Zhang, and helpful comments from Drs. J. Stachnik, J. Han, and T. Kubar. We acknowledge support by the NSF Climate and Large-Scale Dynamics Program under Awards AGS-1228302 (XJ), AGS-1221013 (DW), and AGS-1360237 (RJ), and the NOAA MAPP Program under Award NA12OAR4310075 (XJ). 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 91 TC 2 Z9 2 U1 2 U2 5 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0894-8755 EI 1520-0442 J9 J CLIMATE JI J. Clim. PD JUL PY 2015 VL 28 IS 14 BP 5763 EP 5782 DI 10.1175/JCLI-D-14-00570.1 PG 20 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA CP1LR UT WOS:000359637800015 ER PT J AU Santanello, JA Roundy, J Dirmeyer, PA AF Santanello, Joseph A., Jr. Roundy, Joshua Dirmeyer, Paul A. TI Quantifying the Land-Atmosphere Coupling Behavior in Modern Reanalysis Products over the U.S. Southern Great Plains SO JOURNAL OF CLIMATE LA English DT Article ID BOUNDARY-LAYER INTERACTIONS; AMERICAN REGIONAL REANALYSIS; DIURNAL TIME SCALES; UNITED-STATES; SOIL-MOISTURE; VERTICAL DIFFUSION; PART II; SURFACE; PRECIPITATION; PREDICTION AB The coupling of the land with the planetary boundary layer (PBL) on diurnal time scales is critical to regulating the strength of the connection between soil moisture and precipitation. To improve understanding of land-atmosphere (L-A) interactions, recent studies have focused on the development of diagnostics to quantify the strength and accuracy of the land-PBL coupling at the process level. In this paper, the authors apply a suite of local land-atmosphere coupling (LoCo) metrics to modern reanalysis (RA) products and observations during a 17-yr period over the U.S. southern Great Plains. Specifically, a range of diagnostics exploring the links between soil moisture, evaporation, PBL height, temperature, humidity, and precipitation is applied to the summertime monthly mean diurnal cycles of the North American Regional Reanalysis (NARR), Modern-Era Retrospective Analysis for Research and Applications (MERRA), and Climate Forecast System Reanalysis (CFSR). Results show that CFSR is the driest and MERRA the wettest of the three RAs in terms of overall surface-PBL coupling. When compared against observations, CFSR has a significant dry bias that impacts all components of the land-PBL system. CFSR and NARR are more similar in terms of PBL dynamics and response to dry and wet extremes, while MERRA is more constrained in terms of evaporation and PBL variability. Each RA has a unique land-PBL coupling that has implications for downstream impacts on the diurnal cycle of PBL evolution, clouds, convection, and precipitation as well as representation of extremes and drought. As a result, caution should be used when treating RAs as truth in terms of their water and energy cycle processes. C1 [Santanello, Joseph A., Jr.; Roundy, Joshua] NASA, Goddard Space Flight Ctr, Hydrol Sci Lab, Greenbelt, MD 20771 USA. [Dirmeyer, Paul A.] George Mason Univ, Dept Atmospher Ocean & Earth Sci, Fairfax, VA 22030 USA. RP Santanello, JA (reprint author), NASA GSFC, Code 617,Bldg 22,Room G220, Greenbelt, MD 20771 USA. EM joseph.a.santanello@nasa.gov RI Dirmeyer, Paul/B-6553-2016; Roundy, Joshua/H-9377-2016; Santanello, Joseph/D-4438-2012 OI Dirmeyer, Paul/0000-0003-3158-1752; Roundy, Joshua/0000-0003-0328-3248; Santanello, Joseph/0000-0002-0807-6590 FU NASA FX This work was supported by NASA's Energy and Water Cycle Study (NEWS) and theirModeling, Analysis, and Prediction (MAP) Program. In addition, Joshua Roundy was supported by an appointment to the NASA Postdoctoral Program at the Goddard Space Flight Center, administered byOak Ridge Associated Universities through a contract with NASA. Many thanks go to Bob Dattore at UCAR for producing the monthly mean diurnal cycle data and variables from CFSR specifically for this study. We also thank David Troyan at Brookhaven National Laboratory for the reprocessing of ARM SGP MERGESONDE data to better incorporate radiosonde data in the PBL. Finally, the guidance of Michael Bosilovich was invaluable in terms of the MERRA data processing and interpretation. NR 51 TC 3 Z9 3 U1 2 U2 18 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0894-8755 EI 1520-0442 J9 J CLIMATE JI J. Clim. PD JUL PY 2015 VL 28 IS 14 BP 5813 EP 5829 DI 10.1175/JCLI-D-14-00680.1 PG 17 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA CP1LR UT WOS:000359637800018 ER PT J AU Driscoll, PE AF Driscoll, Peter E. TI Testing the dynamic coupling of the core-mantle and inner core boundaries SO JOURNAL OF GEOPHYSICAL RESEARCH-SOLID EARTH LA English DT Article DE inner core; core dynamics; core-mantle boundary; convection; dynamo; Earth evolution ID UNIFORM HEAT-FLUX; NUMERICAL DYNAMOS; EARTHS CORE; MAGNETIC-FIELD; CONVECTION; HETEROGENEITY; CONDUCTIVITY; TOMOGRAPHY; GEODYNAMO; SURFACE AB The proposal that the seismically observed hemispherical asymmetry of Earth's inner core is controlled by the heat flux structure imposed on the outer core by the lower mantle is tested with numerical dynamo models driven by mixed thermochemical convection. We find that models driven by a single core-mantle boundary (CMB) spherical harmonic of degree and mode 2, the dominant mode in lower mantle seismic shear velocity tomography, produce a similar structure at the inner core boundary (ICB) shifted 30(degrees) westward. The sensitivity of the ICB to the CMB is further tested by increasing the CMB heterogeneity amplitude. In addition, two seismic tomographic models are tested: first with CMB resolution up to degree and order 4, and second with resolution up to degree and order 8. We find time-averaged ICB heat flux in these cases to be similar at large scale, with small-scale differences due to higher CMB harmonics (above degree 4). The tomographic models produce Earth-like magnetic fields, while similar models with twice the CMB heat flow amplitudes produce less Earth-like fields, implying that increasing CMB heterogeneity forces the model out of an Earth-like regime. The dynamic ICB heat fluxes are compared to the proposed translation mode of the inner core to test whether the CMB controls inner core growth and structure. This test indicates that, although CMB tomography is unlikely to be driving inner core translation, the ICB heat flux response is weak enough to not interfere with the most unstable translation mode, if it is occurring. C1 [Driscoll, Peter E.] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Driscoll, Peter E.] Univ Washington, NASA, Astrobiol Inst, Virtual Planetary Lab Lead Team, Seattle, WA 98195 USA. RP Driscoll, PE (reprint author), Univ Washington, Dept Astron, Seattle, WA 98195 USA. EM ped13@uw.edu OI Driscoll, Peter/0000-0001-6241-3925 FU National Aeronautics and Space Administration through the NASA Astrobiology Institute [NNH05ZDA001C] FX The author would like to thank R. Deguen, C. Davies, J. Aubert, and H. Amit for many helpful conversations, and two reviewers for constructive comments that lead to significant improvements. This work was performed as part of the NASA Astrobiology Institute's Virtual Planetary Laboratory Lead Team, supported by the National Aeronautics and Space Administration through the NASA Astrobiology Institute under Cooperative Agreement solicitation NNH05ZDA001C. Calculations were performed in part using the HYAK cluster at the University of Washington eScience Institute. The data for this paper are available by contacting the author. NR 41 TC 2 Z9 2 U1 2 U2 24 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9313 EI 2169-9356 J9 J GEOPHYS RES-SOL EA JI J. Geophys. Res.-Solid Earth PD JUL PY 2015 VL 120 IS 7 BP 4689 EP 4701 DI 10.1002/2014JB011682 PG 13 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA CP2ZN UT WOS:000359746700002 ER PT J AU Collier, MR Porter, FS Sibeck, DG Carter, JA Chiao, MP Chornay, DJ Cravens, TE Galeazzi, M Keller, JW Koutroumpa, D Kujawski, J Kuntz, K Read, AM Robertson, IP Sembay, S Snowden, SL Thomas, N Uprety, Y Walsh, BM AF Collier, Michael R. Porter, F. Scott Sibeck, David G. Carter, Jenny A. Chiao, Meng P. Chornay, Dennis J. Cravens, Thomas E. Galeazzi, Massimiliano Keller, John W. Koutroumpa, Dimitra Kujawski, Joseph Kuntz, Kip Read, Andy M. Robertson, Ina P. Sembay, Steve Snowden, Steven L. Thomas, Nicholas Uprety, Youaraj Walsh, Brian M. TI Invited Article: First flight in space of a wide-field-of-view soft x-ray imager using lobster-eye optics: Instrument description and initial flight results SO REVIEW OF SCIENTIFIC INSTRUMENTS LA English DT Article ID WIND CHARGE-EXCHANGE; LOCAL HOT BUBBLE; SOLAR-WIND; XMM-NEWTON; EMISSION; MARS; DISCOVERY; CHANDRA; SIMULATIONS; VENUS AB We describe the development, launch into space, and initial results from a prototype wide field-of-view soft X-ray imager that employs lobster-eye optics and targets heliophysics, planetary, and astrophysics science. The sheath transport observer for the redistribution of mass is the first instrument using this type of optics launched into space and provides proof-of-concept for future flight instruments capable of imaging structures such as the terrestrial cusp, the entire dayside magnetosheath from outside the magnetosphere, comets, the Moon, and the solar wind interaction with planetary bodies like Venus and Mars [Kuntz et al., Astrophys. J. (in press)]. (C) 2015 AIP Publishing LLC. C1 [Collier, Michael R.; Porter, F. Scott; Sibeck, David G.; Chiao, Meng P.; Chornay, Dennis J.; Keller, John W.; Snowden, Steven L.; Thomas, Nicholas] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Carter, Jenny A.; Read, Andy M.; Sembay, Steve] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Cravens, Thomas E.; Robertson, Ina P.] Univ Kansas, Dept Phys & Astron, Lawrence, KS 66045 USA. [Galeazzi, Massimiliano; Uprety, Youaraj] Univ Miami, Dept Phys, Coral Gables, FL 33124 USA. [Koutroumpa, Dimitra] Univ Paris 06, Sorbonne Univ, Univ Versailles St Quentin, CNRS,INSU,LATMOS,IPSL, F-78280 Guyancourt, France. [Kujawski, Joseph] Siena Coll, Dept Phys, Loudonville, NY 12211 USA. [Kuntz, Kip] Johns Hopkins Univ, Henry A Rowland Dept Phys & Astron, Baltimore, MD 21218 USA. [Walsh, Brian M.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. RP Collier, MR (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM michael.r.collier@nasa.gov; frederick.s.porter@nasa.gov; david.g.sibeck@nasa.gov; jac48@leicester.ac.uk; meng.p.chiao@nasa.gov; dennis.j.chornay@nasa.gov; cravens@ku.edu; galeazzi@physics.miami.edu; john.w.keller@nasa.gov; dimitra.koutroumpa@latmos.ipsl.fr; jkujawski@siena.edu; kuntz@pha.jhu.edu; amr30@leicester.ac.uk; robertin@ku.edu; sfs5@leicester.ac.uk; steven.l.snowden@nasa.gov; nicholas.e.thomas@nasa.gov; ubaraj@physics.miami.edu; bwalsh@ssl.berkeley.edu RI Porter, Frederick/D-3501-2012; Collier, Michael/I-4864-2013; OI Porter, Frederick/0000-0002-6374-1119; Collier, Michael/0000-0001-9658-6605; Walsh, Brian/0000-0001-7426-5413 FU Planetary Division at GSFC through Goddard's Internal Research and Development (IRAD) program; Heliophysics Division at GSFC through Goddard's Internal Research and Development (IRAD) program; Astrophysics Division at GSFC through Goddard's Internal Research and Development (IRAD) program; French space agency CNES; National Program "Physique Chimie du Milieu Interstellaire" of the Institut National des Sciences de l'Univers (INSU) FX Thanks to the Wallops Flight Facility and White Sands Missile Range personnel who supported the DXL mission, including DXL/STORM vibration testing, and were so generally helpful for DXL/STORM. Special thanks to Paul Rozmarynowski for mechanical design support, Kenneth Simms for assembly support, and Norman Dobson for GSE support. Also thanks to Steve Brown in the GSFC radiation facility for support for the proton beam testing and to Dan McCammon for pointing out useful references. The flight instrument development described in this paper was funded through the Planetary, Heliophysics, and Astrophysics Divisions at GSFC through Goddard's Internal Research and Development (IRAD) program. D.K. acknowledges financial support for her activity through the program "Soleil Heliosphere Magnetosphere" of the French space agency CNES and the National Program "Physique Chimie du Milieu Interstellaire" of the Institut National des Sciences de l'Univers (INSU). NR 40 TC 3 Z9 3 U1 0 U2 3 PU AMER INST PHYSICS PI MELVILLE PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA SN 0034-6748 EI 1089-7623 J9 REV SCI INSTRUM JI Rev. Sci. Instrum. PD JUL PY 2015 VL 86 IS 7 AR 071301 DI 10.1063/1.4927259 PG 8 WC Instruments & Instrumentation; Physics, Applied SC Instruments & Instrumentation; Physics GA CO1SB UT WOS:000358934400001 PM 26233339 ER PT J AU Huang, WS Shastry, R AF Huang, Wensheng Shastry, Rohit TI Analysis of Wien filter spectra from Hall thruster plumes SO REVIEW OF SCIENTIFIC INSTRUMENTS LA English DT Article AB A method for analyzing the Wien filter spectra obtained from the plumes of Hall thrusters is derived and presented. The new method extends upon prior work by deriving the integration equations for the current and species fractions. Wien filter spectra from the plume of the NASA-300M Hall thruster are analyzed with the presented method and the results are used to examine key trends. The new integration method is found to produce results slightly different from the traditional area-under-the-curve method. The use of different velocity distribution forms when performing curve-fits to the peaks in the spectra is compared. Additional comparison is made with the scenario where the current fractions are assumed to be proportional to the heights of peaks. The comparison suggests that the calculated current fractions are not sensitive to the choice of form as long as both the height and width of the peaks are accounted for. Conversely, forms that only account for the height of the peaks produce inaccurate results. Also presented are the equations for estimating the uncertainty associated with applying curve fits and charge-exchange corrections. These uncertainty equations can be used to plan the geometry of the experimental setup. C1 [Huang, Wensheng; Shastry, Rohit] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Huang, WS (reprint author), NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. EM wensheng.huang@nasa.gov FU NASA Space Technology Mission Directorate In-Space Propulsion project FX We thank the NASA Space Technology Mission Directorate In-Space Propulsion project for funding this work and Timothy D. Smith for managing the work. NR 21 TC 0 Z9 0 U1 0 U2 1 PU AMER INST PHYSICS PI MELVILLE PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA SN 0034-6748 EI 1089-7623 J9 REV SCI INSTRUM JI Rev. Sci. Instrum. PD JUL PY 2015 VL 86 IS 7 AR 073502 DI 10.1063/1.4923282 PG 11 WC Instruments & Instrumentation; Physics, Applied SC Instruments & Instrumentation; Physics GA CO1SB UT WOS:000358934400040 PM 26233378 ER PT J AU Walker, J Langendorf, S Walker, M Polzin, K Kimberlin, A AF Walker, J. Langendorf, S. Walker, M. Polzin, K. Kimberlin, A. TI Velocimetry of cathode particles in a magnetoplasmadynamic thruster discharge plasma SO REVIEW OF SCIENTIFIC INSTRUMENTS LA English DT Article AB With high-speed imaging, it is possible to directly observe the time-evolution of the macroscopic behavior of the discharge plasma in a magnetoplasmadynamic thruster (MPDT). By utilizing direct high-speed imaging capable of capturing many images over the course of a single discharge, the velocity of the cathode erosion particles can be measured, opening the possibility of a novel, noninvasive technique for discharge plasma flow field velocimetry. In this work, an 8 kA argon MPDT discharge is imaged at 26 173 fps utilizing a 0.9 neutral density filter. The camera is aligned with thruster centerline 4 m downstream of the thruster exit plane. By tracking visible particles appearing in the multiple images, the particle motion in the radial and azimuthal directions is directly imaged. Through the use of traditional techniques in digital particle image velocimetry, the cathode particles emanating from the discharge are measured to have a mean radial velocity of 44.6 +/- 6.0 m/s with a 95% confidence interval and a statistically insignificant azimuthal velocity. The setup and analysis employed permits measurement of the particle velocity in orthogonal direction to the image sensor plane using a single camera. By combining a background removal subtraction technique and knowledge of the optical focal plane, the estimated mean axial velocity of the particles is 1.59 km/s. This investigation ends with a discussion of important factors to consider for future MPDT high-speed imaging particle velocimetry, such as frame-rate, image size, spatial resolution, optics, and data handling selections. (C) 2015 AIP Publishing LLC. C1 [Walker, J.; Langendorf, S.; Walker, M.] Georgia Inst Technol, Sch Aerosp Engn, Atlanta, GA 30332 USA. [Polzin, K.; Kimberlin, A.] NASA Marshall Space Flight Ctr, Prop Res & Technol Applicat Branch, Huntsville, AL 35811 USA. RP Walker, J (reprint author), Georgia Inst Technol, Sch Aerosp Engn, 270 Ferst Dr, Atlanta, GA 30332 USA. EM jwalker30@gatech.edu; mitchell.walker@ae.gatech.edu FU National Science Foundation Graduate Research Fellowship Program FX J. A. Walker would like to thank the National Science Foundation Graduate Research Fellowship Program for funding that enabled this research to be accomplished. We are grateful for the efforts of Nicole Tyman and Joshua Mann for their assistance in the installation and operation of the MPDT support facilities. NR 21 TC 0 Z9 0 U1 1 U2 2 PU AMER INST PHYSICS PI MELVILLE PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA SN 0034-6748 EI 1089-7623 J9 REV SCI INSTRUM JI Rev. Sci. Instrum. PD JUL PY 2015 VL 86 IS 7 AR 073513 DI 10.1063/1.4927477 PG 10 WC Instruments & Instrumentation; Physics, Applied SC Instruments & Instrumentation; Physics GA CO1SB UT WOS:000358934400051 PM 26233389 ER PT J AU Bozzo, E Romano, P Falanga, M Ferrigno, C Papitto, A Krimm, HA AF Bozzo, E. Romano, P. Falanga, M. Ferrigno, C. Papitto, A. Krimm, H. A. TI Swift J1734.5-3027: a new long Type-I X-ray bursting source SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE X-rays: binaries; X-rays: individuals: Swift J1734.5-3027 ID LIGHT CURVES; RXTE OBSERVATIONS; IGR J00291+5934; NEUTRON-STAR; ACCRETION; OUTBURST; BINARIES; MONITOR; IMAGER AB Swift J1734.5-3027 is a hard X-ray transient discovered by Swift while undergoing an outburst in September 2013. Archival observations showed that this source underwent a previous episode of enhanced X-ray activity in 2013 May-June. In this paper we report on the analysis of all X-ray data collected during the outburst in 2013 September, the first that could be intensively followed up by several X-ray facilities. Our dataset includes INTEGRAL, Swift, and XMM-Newton observations. From the timing and spectral analysis of these observations, we show that a long Type-I X-ray burst took place during the source outburst, making Swift J1734.5-3027 a new member of the class of bursting neutron star low-mass X-ray binaries. The burst lasted for about 1.9 ks and reached a peak flux of (6.0 +/- 1.8) x 10(-8) erg cm(-2) s(-1) in the 0.5-100 keV energy range. The estimated burst fluence in the same energy range is (1.10 +/- 0.10) x 10(-5) erg cm(-2). By assuming that a photospheric radius expansion took place during the first similar to 200 s of the burst and that the accreted material was predominantly composed by He, we derived a distance to the source of 7.2 +/- 1.5 kpc. C1 [Bozzo, E.; Ferrigno, C.] ISDC Data Ctr Astrophys, CH-1290 Versoix, Switzerland. [Romano, P.] Ist Astrofis Spaziale & Fis Cosm Palermo, INAF, I-90146 Palermo, Italy. [Falanga, M.] Int Space Sci Inst, CH-3012 Bern, Switzerland. [Ferrigno, C.] Int Space Sci Inst Beijing, Beijing 100190, Peoples R China. [Papitto, A.] Inst Ciencies Espai IEEC CSIC, Barcelona, Spain. [Krimm, H. A.] Ctr Res & Explorat Space Sci & Technol CRESST, Greenbelt, MD 20771 USA. [Krimm, H. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Krimm, H. A.] Univ Space Res Assoc, Columbia, MD 21046 USA. RP Bozzo, E (reprint author), ISDC Data Ctr Astrophys, Chemin Ecogia 16, CH-1290 Versoix, Switzerland. EM enrico.bozzo@unige.ch FU Juan de la Cierva; [AYA2012-39303]; [SGR2009-811]; [iLINK2011-0303]; [ASI-INAF I/004/11/0] FX E.B. thanks the New York University at Abu Dhabi for the kind hospitality during part of this work and Milvia Capalbi for her precious support during the analysis of some XRT observations. We thank Phil Evans for useful discussions. A.P. is supported by a Juan de la Cierva fellowship, and acknowledges grants AYA2012-39303, SGR2009-811, and iLINK2011-0303. P.R. acknowledges contract ASI-INAF I/004/11/0. We thank N. Schartel and the XMM-Newton team for having promptly performed the ToO observation analyzed in this paper. We are indebted to the Swift PI and operations team for the continuous support during the monitoring campaign of X-ray transients. NR 49 TC 2 Z9 2 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUL PY 2015 VL 579 AR A56 DI 10.1051/0004-6361/201526150 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO0XL UT WOS:000358877100068 ER PT J AU Gaspari, M Brighenti, F Temi, P AF Gaspari, M. Brighenti, F. Temi, P. TI Chaotic cold accretion on to black holes in rotating atmospheres SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE accretion, accretion disks; black hole physics; hydrodynamics; galaxies: ISM; instabilities; turbulence ID EARLY-TYPE GALAXIES; COOLING FLOW CLUSTERS; ACTIVE GALACTIC NUCLEI; INEFFICIENT STAR-FORMATION; MECHANICAL AGN FEEDBACK; GIANT ELLIPTIC GALAXIES; HOT INTERSTELLAR-MEDIUM; X-RAY SPECTROSCOPY; H-ALPHA FILAMENTS; GROUP NGC 5044 AB The fueling of black holes is one key problem in the evolution of baryons in the universe. Chaotic cold accretion (CCA) profoundly differs from classic accretion models, as Bondi and thin disc theories. Using 3D high-resolution hydrodynamic simulations, we now probe the impact of rotation on the hot and cold accretion flow in a typical massive galaxy. In the hot mode, with or without turbulence, the pressure-dominated flow forms a geometrically thick rotational barrier, suppressing the black hole accretion rate to similar to 1/3 of the spherical case value. When radiative cooling is dominant, the gas loses pressure support and quickly circularizes in a cold thin disk; the accretion rate is decoupled from the cooling rate, although it is higher than that of the hot mode. In the more common state of a turbulent and heated atmosphere, CCA drives the dynamics if the gas velocity dispersion exceeds the rotational velocity, i.e., turbulent Taylor number Ta-t < 1. Extended multiphase filaments condense out of the hot phase via thermal instability (TI) and rain toward the black hole, boosting the accretion rate up to 100 times the Bondi rate ((M) over dot(center dot) similar to (M) over dot(cool)). Initially, turbulence broadens the angular momentum distribution of the hot gas, allowing the cold phase to condense with prograde or retrograde motion. Subsequent chaotic collisions between the cold filaments, clouds, and a clumpy variable torus promote the cancellation of angular momentum, leading to high accretion rates. As turbulence weakens (Ta-t > 1), the broadening of the distribution and the efficiency of collisions diminish, damping the accretion rate proportional to Ta-t(-1), until the cold disk drives the dynamics. This is exacerbated by the increased difficulty to grow TI in a rotating halo. The simulated sub-Eddington accretion rates cover the range inferred from AGN cavity observations. CCA predicts inner flat X-ray temperature and r(-1) density profiles, as recently discovered in M 87 and NGC 3115. The synthetic H-alpha images reproduce the main features of cold gas observations in massive ellipticals, as the line fluxes and the filaments versus disk morphology. Such dichotomy is key for the long-term AGN feedback cycle. As gas cools, filamentary CCA develops and boosts AGN heating; the cold mode is thus reduced and the rotating disk remains the sole cold structure. Its consumption leaves the atmosphere in hot mode with suppressed accretion and feedback, reloading the cycle. C1 [Gaspari, M.] Max Planck Inst Astrophys, D-85741 Garching, Germany. [Brighenti, F.] Univ Bologna, Dept Astron, I-40127 Bologna, Italy. [Temi, P.] NASA, Astrophys Branch, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Gaspari, M (reprint author), Max Planck Inst Astrophys, Karl Schwarzschild Str 1, D-85741 Garching, Germany. EM mgaspari@mpa-garching.mpg.de FU Max Planck Fellowship; Prin MIUR [2010LY5N2T]; NASA/Ames HEC Program [SMD-13-4373, SMD-13-4377, SMD-14-4819] FX The FLASH code was in part developed by the DOE NNSA-ASC OASCR Flash center at the University of Chicago. M.G. is grateful for the financial support provided by the Max Planck Fellowship. F.B. is in part supported by the Prin MIUR grant 2010LY5N2T. HPC resources were provided by the NASA/Ames HEC Program (SMD-13-4373, SMD-13-4377, SMD-14-4819; Pleiades) and CLS center. The post-processing analysis was in part performed with YT (Turk et al. 2011). We thank R. Sunyaev, N. Werner, M. Anderson, R. Khatri, P. Girichidis, and A. Gatto for helpful discussions. We are grateful to N. Werner, who allowed us to reproduce the H alpha SOAR images. We thank the anonymous referee who helped to improve the manuscript. NR 153 TC 19 Z9 19 U1 1 U2 2 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUL PY 2015 VL 579 AR A62 DI 10.1051/0004-6361/201526151 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO0XL UT WOS:000358877100074 ER PT J AU Girardi, M Mercurio, A Balestra, I Nonino, M Biviano, A Grillo, C Rosati, P Annunziatella, M Demarco, R Fritz, A Gobat, R Lemze, D Presotto, V Scodeggio, M Tozzi, P Caminha, GB Brescia, M Coe, D Kelson, D Koekemoer, A Lombardi, M Medezinski, E Postman, M Sartoris, B Umetsu, K Zitrin, A Boschin, W Czoske, O De Lucia, G Kuchner, U Maier, C Meneghetti, M Monaco, P Monna, A Munari, E Seitz, S Verdugo, M Ziegler, B AF Girardi, M. Mercurio, A. Balestra, I. Nonino, M. Biviano, A. Grillo, C. Rosati, P. Annunziatella, M. Demarco, R. Fritz, A. Gobat, R. Lemze, D. Presotto, V. Scodeggio, M. Tozzi, P. Caminha, G. Bartosch Brescia, M. Coe, D. Kelson, D. Koekemoer, A. Lombardi, M. Medezinski, E. Postman, M. Sartoris, B. Umetsu, K. Zitrin, A. Boschin, W. Czoske, O. De Lucia, G. Kuchner, U. Maier, C. Meneghetti, M. Monaco, P. Monna, A. Munari, E. Seitz, S. Verdugo, M. Ziegler, B. TI CLASH-VLT: Substructure in the galaxy cluster MACS J1206.2-0847 from kinematics of galaxy populations SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE galaxies: clusters: individual: MACS J1206.2-0847; galaxies: clusters: general; galaxies: kinematics and dynamics; galaxies: evolution; cosmology: observations ID SCALE-INDEPENDENT METHOD; POST-STARBURST GALAXIES; STAR-FORMATION ACTIVITY; HUBBLE-SPACE-TELESCOPE; X-RAY-CLUSTERS; DISTANT CLUSTERS; RICH CLUSTERS; VELOCITY DISPERSIONS; MASSIVE CLUSTER; ENVIRONMENTAL DEPENDENCE AB Aims. In the effort to understand the link between the structure of galaxy clusters and their galaxy populations, we focus on MACS J1206.2-0847 at z similar to 0.44 and probe its substructure in the projected phase space through the spectrophotometric properties of a large number of galaxies from the CLASH-VLT survey. Methods. Our analysis is mainly based on an extensive spectroscopic dataset of 445 member galaxies, mostly acquired with VIMOS at VLT as part of our ESO Large Programme, sampling the cluster out to a radius similar to 2R(200) (4 h(70)(-1) Mpc). We classify 412 galaxies as passive, with strong H delta absorption (red and blue galaxies), and with emission lines from weak to very strong. A number of tests for substructure detection are applied to analyze the galaxy distribution in the velocity space, in 2D space, and in 3D projected phase-space. Results. Studied in its entirety, the cluster appears as a large-scale relaxed system with a few secondary, minor overdensities in 2D distribution. We detect no velocity gradients or evidence of deviations in local mean velocities. The main feature is the WNW-ESE elongation. The analysis of galaxy populations per spectral class highlights a more complex scenario. The passive galaxies and red strong H delta galaxies trace the cluster center and the WNW-ESE elongated structure. The red strong H delta galaxies also mark a secondary, dense peak similar to 2 h(70)(-1) Mpc at ESE. The emission line galaxies cluster in several loose structures, mostly outside R-200. Two of these structures are also detected through our 3D analysis. The observational scenario agrees with MACS J1206.2-0847 having WNW-ESE as the direction of the main cluster accretion, traced by passive galaxies and red strong H delta galaxies. The red strong H delta galaxies, interpreted as poststarburst galaxies, date a likely important event 1-2 Gyr before the epoch of observation. The emission line galaxies trace a secondary, ongoing infall where groups are accreted along several directions. C1 [Girardi, M.; Annunziatella, M.; Presotto, V.; Sartoris, B.; Monaco, P.; Munari, E.] Univ Trieste, Dipartimento Fis, I-34143 Trieste, Italy. [Girardi, M.; Balestra, I.; Nonino, M.; Biviano, A.; Annunziatella, M.; Sartoris, B.; De Lucia, G.; Monaco, P.; Munari, E.] INAF Osservatorio Astron Trieste, I-34133 Trieste, Italy. [Mercurio, A.; Brescia, M.] INAF Osservatorio Astron Capodimonte, I-80131 Naples, Italy. [Grillo, C.] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen, Denmark. [Rosati, P.; Caminha, G. Bartosch] Univ Ferrara, Dipartimento Fis & Sci Terra, I-44122 Ferrara, Italy. [Demarco, R.] Univ Concepcion, Dept Astron, Concepcion, Chile. [Fritz, A.; Scodeggio, M.] INAF IASF Milano, I-20133 Milan, Italy. [Gobat, R.] KIAS, Seoul 130722, South Korea. [Lemze, D.; Medezinski, E.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Tozzi, P.] INAF Osservatorio Astrofis Arcetri, I-50125 Florence, Italy. [Coe, D.; Koekemoer, A.; Postman, M.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Kelson, D.] Observ Carnegie Inst Washington, Pasadena, CA 91101 USA. [Lombardi, M.] Univ Milan, Dipartimento Fis, I-20133 Milan, Italy. [Umetsu, K.] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan. [Zitrin, A.] CALTECH, Pasadena, CA 91125 USA. [Boschin, W.] Fdn Galileo Galilei INAF, Brena Baja 38712, La Palma, Spain. [Boschin, W.] Inst Astrofis Canarias, Tenerife 38205, Spain. [Boschin, W.] Univ La Laguna, Dept Astrofis, E-38206 Tenerife, Spain. [Czoske, O.; Kuchner, U.; Maier, C.; Verdugo, M.; Ziegler, B.] Univ Vienna, Dept Astrophys, A-1180 Vienna, Austria. [Meneghetti, M.] INAF Osservatorio Astron Bologna, I-40127 Bologna, Italy. [Meneghetti, M.] Ist Nazl Fis Nucl, Sez Bologna, I-40127 Bologna, Italy. [Meneghetti, M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Monna, A.; Seitz, S.] Univ Observ Munich, D-81679 Munich, Germany. [Seitz, S.] Max Planck Inst Extraterr Phys, D-85741 Garching, Germany. RP Girardi, M (reprint author), Univ Trieste, Dipartimento Fis, Via Tiepolo 11, I-34143 Trieste, Italy. EM girardi@oats.inaf.it RI Bartosch Caminha, Gabriel/C-8952-2013; Meneghetti, Massimo/O-8139-2015; OI Monaco, Pierluigi/0000-0003-2083-7564; Koekemoer, Anton/0000-0002-6610-2048; Tozzi, Paolo/0000-0003-3096-9966; Bartosch Caminha, Gabriel/0000-0001-6052-3274; Meneghetti, Massimo/0000-0003-1225-7084; Maier, Christian/0000-0001-6405-2182; Balestra, Italo/0000-0001-9660-894X; Scodeggio, Marco/0000-0002-2282-5850; Brescia, Massimo/0000-0001-9506-5680; LOMBARDI, MARCO/0000-0002-3336-4965; Umetsu, Keiichi/0000-0002-7196-4822; Biviano, Andrea/0000-0002-0857-0732; Nonino, Mario/0000-0001-6342-9662 FU MIUR PRIN [J91J12000450001]; MIUR PRIN INAF; European Union [267251]; DNRF; Consorzio per la Fisica - Trieste; BASAL Center for Astrophysics and Associated Technologies (CATA); FONDECYT [1130528]; INAF; NASA [HST-HF2-51334.001-A]; STScI FX We thank the referee for invaluable comments. This research is partly supported by the MIUR PRIN2010-2011 (J91J12000450001) and PRIN INAF 2014. I.B. acknowledges funding from the European Union Seventh Framework Programme (FP7/2007-2013) under grant agreement n. 267251 "Astronomy Fellowships in Italy" (astroFit). The Dark Cosmology Centre is funded by the DNRF. B.S. and V.P. acknowledge a grant from "Consorzio per la Fisica - Trieste". R.D. gratefully acknowledges the support provided by the BASAL Center for Astrophysics and Associated Technologies (CATA), and by FONDECYT grant N. 1130528. A.F. acknowledges support by INAF through VIPERS grants PRIN 2008 and PRIN 2010. Support for A.Z. was provided by NASA through Hubble Fellowship grant #HST-HF2-51334.001-A awarded by STScI. The research is based in part on data collected at Subaru Telescope, which is operated by the National Astronomical Observatory of Japan, and obtained from the SMOKA, which is operated by the Astronomy Data Center, National Astronomical Observatory of Japan. NR 131 TC 9 Z9 9 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 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUL PY 2015 VL 579 AR A4 DI 10.1051/0004-6361/201425599 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO0XL UT WOS:000358877100016 ER PT J AU Lellouch, E Moreno, R Orton, GS Feuchtgruber, H Cavalie, T Moses, JI Hartogh, P Jarchow, C Sagawa, H AF Lellouch, E. Moreno, R. Orton, G. S. Feuchtgruber, H. Cavalie, T. Moses, J. I. Hartogh, P. Jarchow, C. Sagawa, H. TI New constraints on the CH4 vertical profile in Uranus and Neptune from Herschel observations SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE planetary systems; planets and satellites: gaseous planets; planets and satellites: individual: Uranus; planets and satellites: individual: Neptune ID MIDINFRARED SPECTROSCOPY; OCCULTATION MEASUREMENTS; UPPER TROPOSPHERE; PACS OBSERVATIONS; STRATOSPHERE; SPECTROMETER; METHANE; ATMOSPHERE; TEMPERATURES; INSTRUMENT AB Dedicated line observations of CH4 rotational lines performed with Herschel/PACS and HIFI in 2009-2011 provide new inferences of the mean methane profile in the upper tropospheres and stratospheres of Uranus and Neptune. At Uranus, CH4 is found to be near saturation, with a similar to 9 x 10(4) tropopause/lower stratosphere mole fraction. This is nominally six times larger than inferred from Spitzer in 2007, although reconciliation may be possible if the CH4 abundance decreases sharply from similar to 100 to 2 mbar. This unexpected situation might reflect heterogeneous conditions in Uranus' stratosphere, with local CH4 depletions and heating associated with downwelling motions. Higher CH4 abundances compared to values inferred under solstitial conditions by Voyager in 1989 suggest that atmospheric mixing is effectively subdued at high latitudes and/or is time-variable. At Neptune, the mid-stratosphere CH4 abundance is (1.15 +/- 0.10) x 10(-3), in agreement with earlier determinations and indicative of either leakage through a warmer polar region or upwelling at low or middle latitudes. On both planets, spatially resolved observations of temperature and methane in the stratosphere are needed to further identify the physical processes at work. C1 [Lellouch, E.; Moreno, R.] Observ Paris, LESIA, F-92195 Meudon, France. [Orton, G. S.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Feuchtgruber, H.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Cavalie, T.; Hartogh, P.; Jarchow, C.] Max Planck Inst Sonnensyst Forsch, D-37077 Gottingen, Germany. [Moses, J. I.] Space Sci Inst, Boulder, CO 80301 USA. [Sagawa, H.] Kyoto Sangyo Univ, Fac Sci, Kita Ku, Kyoto 6038555, Japan. RP Lellouch, E (reprint author), Observ Paris, LESIA, 5 Pl Jules Janssen, F-92195 Meudon, France. EM emmanuel.lellouch@obspm.fr RI Moses, Julianne/I-2151-2013 OI Moses, Julianne/0000-0002-8837-0035 FU BMVIT (Austria); ESA-PRODEX (Belgium); CEA/CNES (France); DLR (Germany); ASI (Italy); CICT/MCT (Spain); ESA FX HIFI has been designed and built by a consortium of institutes and university departments from across Europe, Canada, and the United States under the leadership of SRON Netherlands Institute for Space Research, Groningen, The Netherlands, and with major contributions from Germany, France, and the US. Consortium members are: Canada: CSA, U. Waterloo; France: CESR, LAB, LERMA, IRAM; Germany: KOSMA, MPIfR, MPS; Ireland, NUI Maynooth; Italy: ASI, IFS I-INAF, Osservatorio Astrofisico di Arcetri-INAF; Netherlands: SRON, TUD; Poland: CAMK, CBK; Spain: Observatorio Astronomico Naci onal (IGN), Centro de Astrobiologia (CSIC-INTA). Sweden: Chalmers University of Technology - MC2, RSS & GARD; Onsala Space Observatory; Swedish National Space Board, Stockholm University - Stockholm Observatory; Switzerland: ETH Zurich, FHNW; USA: Caltech, JPL, NHSC. PACS has been developed by a consortium of institutes led by MPE (Germany) and including UVIE (Austria); KUL, CSL, IMEC (Belgium); CEA, OAMP (France); MPIA (Germany); IFSI, OAP/AOT, OAA/CAISMI, LENS, SISSA (Italy); IAC (Spain). This development has been supported by the funding agencies BMVIT (Austria), ESA-PRODEX (Belgium), CEA/CNES (France), DLR (Germany), ASI (Italy), and CICT/MCT (Spain). Additional funding support for some instrument activities has been provided by ESA. Data presented in this paper were analysed using "HIPE", a joint development by the Herschel Science Ground Segment Consortium, consisting of ESA, the NASA Herschel Science Center, and the HIFI, PACS and SPIRE consortia. NR 34 TC 1 Z9 1 U1 0 U2 2 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 EI 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUL PY 2015 VL 579 AR A121 DI 10.1051/0004-6361/201526518 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO0XL UT WOS:000358877100133 ER PT J AU Maire, AL Skemer, AJ Hinz, PM Desidera, S Esposito, S Gratton, R Marzari, F Skrutskie, MF Biller, BA Defrere, D Bailey, VP Leisenring, JM Apai, D Bonnefoy, M Brandner, W Buenzli, E Claudi, RU Close, LM Crepp, JR De Rosa, RJ Eisner, JA Fortney, JJ Henning, T Hofmann, KH Kopytova, TG Males, JR Mesa, D Morzinski, KM Oza, A Patience, J Pinna, E Rajan, A Schertl, D Schlieder, JE Su, KYL Vaz, A Ward-Duong, K Weigelt, G Woodward, CE AF Maire, A-L Skemer, A. J. Hinz, P. M. Desidera, S. Esposito, S. Gratton, R. Marzari, F. Skrutskie, M. F. Biller, B. A. Defrere, D. Bailey, V. P. Leisenring, J. M. Apai, D. Bonnefoy, M. Brandner, W. Buenzli, E. Claudi, R. U. Close, L. M. Crepp, J. R. De Rosa, R. J. Eisner, J. A. Fortney, J. J. Henning, T. Hofmann, K. -H. Kopytova, T. G. Males, J. R. Mesa, D. Morzinski, K. M. Oza, A. Patience, J. Pinna, E. Rajan, A. Schertl, D. Schlieder, J. E. Su, K. Y. L. Vaz, A. Ward-Duong, K. Weigelt, G. Woodward, C. E. TI The LEECH Exoplanet Imaging Survey. Further constraints on the planet architecture of the HR 8799 system (vol 576, pg A133, 2015) SO ASTRONOMY & ASTROPHYSICS LA English DT Correction DE stars: individual: HR 8799; planetary systems; instrumentation: adaptive optics; techniques: high angular resolution; methods: data analysis; errata, addenda C1 [Maire, A-L; Desidera, S.; Gratton, R.; Claudi, R. U.; Mesa, D.] Osserv Astron Padova, INAF, I-35122 Padua, Italy. [Skemer, A. J.; Hinz, P. M.; Defrere, D.; Bailey, V. P.; Leisenring, J. M.; Apai, D.; Close, L. M.; Eisner, J. A.; Males, J. R.; Morzinski, K. M.; Su, K. Y. L.; Vaz, A.] Univ Arizona, Dept Astron, Steward Observ, Tucson, AZ 85721 USA. [Esposito, S.; Pinna, E.] Osservatorio Astrofis Arcetri, INAF, I-50125 Florence, Italy. [Marzari, F.] Univ Padua, Dipartimento Fis & Astron, I-35131 Padua, Italy. [Skrutskie, M. F.; Oza, A.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. [Biller, B. A.] Univ Edinburgh, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland. [Biller, B. A.; Bonnefoy, M.; Brandner, W.; Buenzli, E.; Henning, T.; Kopytova, T. G.; Schlieder, J. E.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Bonnefoy, M.] Univ Grenoble Alpes, IPAG, F-38000 Grenoble, France. [Bonnefoy, M.] CNRS, IPAG, F-38000 Grenoble, France. [Crepp, J. R.] Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA. [De Rosa, R. J.; Patience, J.; Rajan, A.; Ward-Duong, K.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [De Rosa, R. J.] Univ Exeter, Sch Phys, Astrophys Grp, Exeter EX4 4QL, Devon, England. [Fortney, J. J.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Hofmann, K. -H.; Schertl, D.; Weigelt, G.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Kopytova, T. G.] Int Max Planck Res Sch Astron & Space Phys, Heidelberg, Germany. [Schlieder, J. E.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Woodward, C. E.] Univ Minnesota, Minnesota Inst Astrophys, Minneapolis, MN 55455 USA. RP Maire, AL (reprint author), Osserv Astron Padova, INAF, Vicolo Osservatorio 5, I-35122 Padua, Italy. EM annelise.maire@oapd.inaf.it NR 1 TC 1 Z9 1 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 EI 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUL PY 2015 VL 579 AR C2 DI 10.1051/0004-6361/201425185e PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO0XL UT WOS:000358877100002 ER PT J AU Mancini, L Esposito, M Covino, E Raia, G Southworth, J Tregloan-Reed, J Biazzo, K Bonomo, AS Desidera, S Lanza, AF Maciejewski, G Poretti, E Sozzetti, A Borsa, F Bruni, I Ciceri, S Claudi, R Cosentino, R Gratton, R Fiorenzano, AFM Lodato, G Lorenzi, V Marzari, F Murabito, S Affer, L Bignamini, A Bedin, LR Boccato, C Damasso, M Henning, T Maggio, A Micela, G Molinari, E Pagano, I Piotto, G Rainer, M Scandariato, G Smareglia, R Sanchez, RZ AF Mancini, L. Esposito, M. Covino, E. Raia, G. Southworth, J. Tregloan-Reed, J. Biazzo, K. Bonomo, A. S. Desidera, S. Lanza, A. F. Maciejewski, G. Poretti, E. Sozzetti, A. Borsa, F. Bruni, I. Ciceri, S. Claudi, R. Cosentino, R. Gratton, R. Martinez Fiorenzano, A. F. Lodato, G. Lorenzi, V. Marzari, F. Murabito, S. Affer, L. Bignamini, A. Bedin, L. R. Boccato, C. Damasso, M. Henning, Th. Maggio, A. Micela, G. Molinari, E. Pagano, I. Piotto, G. Rainer, M. Scandariato, G. Smareglia, R. Sanchez, R. Zanmar TI The GAPS Programme with HARPS-N at TNG VIII. Observations of the Rossiter-McLaughlin effect and characterisation of the transiting planetary systems HAT-P-36 and WASP-11/HAT-P-10 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE planetary systems; stars: fundamental parameters; techniques: photometric; techniques: radial velocities; stars: individual: HAT-P-36; stars: individual: WASP-11/HAT-P-10 ID STELLAR EVOLUTION DATABASE; EXTRASOLAR PLANETS; EXOPLANETARY SYSTEM; LIGHT-CURVE; TRANSMISSION SPECTRUM; PHYSICAL-PROPERTIES; STARS; MASS; PARAMETERS; ISOCHRONES AB Context. Orbital obliquity is thought to be a fundamental parameter in tracing the physical mechanisms that cause the migration of giant planets from the snow line down to roughly 10-2 au from their host stars. We are carrying out a large programme to estimate the spin-orbit alignment of a sample of transiting planetary systems to study what the possible configurations of orbital obliquity are and whether they correlate with other stellar or planetary properties. Aims. We determine the true and the projected obliquity of HAT-P-36 and WASP-11/HAT-P-10 systems, respectively, which are both composed of a relatively cool star (with effective temperature T-eff < 6100 K) and a hot-Jupiter planet. Methods. Thanks to the high-resolution spectrograph HARPS-N, we observed the Rossiter-McLaughlin effect for both systems by acquiring precise (3-8ms(-1)) radial-velocity measurements during planetary transit events. We also present photometric observations comprising six light curves that cover five transit events, which were obtained using three medium-class telescopes. One transit of WASP-11/HAT-P-10 was followed simultaneously from two observatories. The three transit light curves of HAT-P-36 b show anomalies that are attributable to starspot complexes on the surface of the parent star, in agreement with the analysis of its spectra that indicates moderate activity (log R-HK' = -4.65 dex). By analysing the complete HATNet data set of HAT-P-36, we estimated the stellar rotation period by detecting a periodic photometric modulation in the light curve caused by star spots, obtaining P-rot = 15.3+/-0.4 days, which implies that the inclination of the stellar rotational axis with respect to the line of sight is i(star) = 65 degrees +/- 34 degrees. Results. We used the new spectroscopic and photometric data to revise the main physical parameters and measure the sky-projected misalignment angle of the two systems. We found lambda = -14 degrees +/- 18 degrees for HAT-P-36 and lambda = degrees +/- 5 degrees for WASP-11/HAT-P-10, indicating in both cases a good spin-orbit alignment. In the case of HAT-P-36, we were also able to estimate an upper limit of its real obliquity, which turned out to be psi < 63 degrees. C1 [Mancini, L.; Ciceri, S.; Henning, Th.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Mancini, L.; Bonomo, A. S.; Sozzetti, A.; Damasso, M.] Osserv Astron Torino, INAF, I-10025 Pino Torinese, Italy. [Esposito, M.; Murabito, S.] Inst Astrofis Canarias, Tenerife 38205, Spain. [Esposito, M.; Murabito, S.] Univ La Laguna, Dept Astrofis, E-38206 Tenerife, Spain. [Covino, E.; Raia, G.] Osserv Astron Capodimonte, INAF, I-80131 Naples, Italy. [Southworth, J.] Keele Univ, Astrophys Grp, Keele ST5 5BG, Staffs, England. [Tregloan-Reed, J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Biazzo, K.; Lanza, A. F.; Pagano, I.; Scandariato, G.; Sanchez, R. Zanmar] Osserv Astrofis Catania, INAF, I-95123 Catania, Italy. [Desidera, S.; Claudi, R.; Gratton, R.; Marzari, F.; Bedin, L. R.; Boccato, C.; Piotto, G.] Osserv Astron Padova, INAF, I-35122 Padua, Italy. [Maciejewski, G.] Nicholas Copernicus Univ, Ctr Astron, PL-87100 Torun, Poland. [Poretti, E.; Borsa, F.; Rainer, M.] Osserv Astron Brera, INAF, I-23807 Merate, Lecco, Italy. [Bruni, I.] Osservatorio Astron Bologna, INAF, I-40127 Bologna, Italy. [Cosentino, R.; Martinez Fiorenzano, A. F.; Lorenzi, V.; Marzari, F.; Molinari, E.] Fdn Galileo Galilei, INAF, Tenerife, Spain. [Lodato, G.] Univ Milan, Dipartimento Fis, I-20133 Milan, Italy. [Affer, L.; Maggio, A.; Micela, G.] Osserv Astron Palermo, INAF, I-90134 Palermo, Italy. [Bignamini, A.; Smareglia, R.] Osserv Astron Trieste, INAF, I-34143 Trieste, Italy. [Molinari, E.] IASF Milano, INAF, I-20133 Milan, Italy. [Piotto, G.] Univ Padua, Dip Fis & Astron Galileo Galilei, I-35122 Padua, Italy. RP Mancini, L (reprint author), Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany. EM mancini@mpia.de RI Maggio, Antonio/P-5700-2015; Pagano, Isabella/I-6934-2015; Maciejewski, Gracjan/D-6241-2014; OI Smareglia, Riccardo/0000-0001-9363-3007; Bruni, Ivan/0000-0002-1560-4590; Biazzo, Katia/0000-0002-1892-2180; Boccato, Caterina/0000-0002-6177-9703; Sozzetti, Alessandro/0000-0002-7504-365X; Gratton, Raffaele/0000-0003-2195-6805; bedin, luigi/0000-0003-4080-6466; Lanza, Antonino Francesco/0000-0001-5928-7251; Piotto, Giampaolo/0000-0002-9937-6387; Maggio, Antonio/0000-0001-5154-6108; Pagano, Isabella/0000-0001-9573-4928; Covino, Elvira/0000-0002-6187-6685; Desidera, Silvano/0000-0001-8613-2589; Molinari, Emilio/0000-0002-1742-7735; Micela, Giuseppina/0000-0002-9900-4751 FU INAF through the "Progetti Premiali" funding scheme of the Italian Ministry of Education, University, and Research FX The HARPS-N instrument has been built by the HARPS-N Consortium, a collaboration between the Geneva Observatory (PI Institute), the Harvard-Smithonian Center for Astrophysics, the University of St. Andrews, the University of Edinburgh, the Queen's University of Belfast, and INAF. Operations at the Calar Alto telescopes are jointly performed by the Max-Planck Institut fur Astronomie (MPIA) and the Instituto de Astrofisica de Andalucia (CSIC). The reduced light curves presented in this work will be made available at the CDS (http://cdsweb.u-strasbg.fr/). The GAPS project in Italy acknowledges support from INAF through the "Progetti Premiali" funding scheme of the Italian Ministry of Education, University, and Research. We acknowledge the use of the following internet-based resources: the ESO Digitized Sky Survey; the TEPCat catalogue; the SIMBAD data base operated at the CDS, Strasbourg, France; and the arXiv scientific paper preprint service operated by Cornell University. NR 70 TC 9 Z9 10 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 EI 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUL PY 2015 VL 579 AR A136 DI 10.1051/0004-6361/201526030 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO0XL UT WOS:000358877100148 ER PT J AU Paraschiv, AR Bemporad, A Sterling, AC AF Paraschiv, A. R. Bemporad, A. Sterling, A. C. TI Physical properties of solar polar jets A statistical study with Hinode XRT data SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE Sun: corona; Sun: activity; Sun: X-rays, gamma rays; methods: data analysis ID X-RAY JETS; CORONAL HOLE JETS; BRIGHT POINTS; SOHO MISSION; BLOWOUT JETS; A MISSION; TELESCOPE; PARAMETERS; DICHOTOMY; DYNAMICS AB Aims. The target of this work is to investigate the physical nature of polar jets in the solar corona and their possible contribution to coronal heating and solar wind flow based on the analysis of X-ray images acquired by the Hinode XRT telescope. We estimate the different forms of energy associated with many of these small-scale eruptions, in particular the kinetic energy and enthalpy. Methods. Two Hinode XRT campaign datasets focusing on the two polar coronal holes were selected to analyze the physical properties of coronal jets; the analyzed data were acquired using a series of three XRT filters. Typical kinematical properties (e.g., length, thickness, lifetime, ejection rate, and velocity) of 18 jets are evaluated from the observed sequences, thus providing information on their possible contribution to the fast solar wind flux escaping from coronal holes. Electron temperatures and densities of polar-jet plasmas are also estimated using ratios of the intensities observed in different filters. Results. We find that the largest amount of energy eventually provided to the corona is thermal. The energy due to waves may also be significant, but its value is comparatively uncertain. The kinetic energy is lower than thermal energy, while other forms of energy are comparatively low. Lesser and fainter events seem to be hotter, thus the total contribution by polar jets to the coronal heating could have been underestimated so far. The kinetic energy flux is usually around three times smaller than the enthalpy counterpart, implying that this energy is converted into plasma heating more than in plasma acceleration. This result suggests that the majority of polar jets are most likely not escaping from the Sun and that only cooler ejections could possibly have enough kinetic energy to contribute to the total solar wind flow. C1 [Paraschiv, A. R.; Bemporad, A.] INAF Turin Astrophys Observ, I-10025 Pino Torinese, Italy. [Sterling, A. C.] NASA Marshall Space Flight Ctr, Huntsville, AL 35812 USA. [Paraschiv, A. R.] Romanian Acad, Inst Geodynam Sabba S Stefanescu, Bucharest, Romania. RP Paraschiv, AR (reprint author), INAF Turin Astrophys Observ, Via Osservatorio 20, I-10025 Pino Torinese, Italy. EM paraschiv.alin.razvan@gmail.com; bemporad@oato.inaf.it; Alphonse.Sterling@nasa.gov OI Bemporad, Alessandro/0000-0001-5796-5653 FU INAF-Turin Astrophysical Observatory; Faculty of Physics of the University of Bucharest; Department of Physics of the University of Turin; NASA's Office of Space Science FX A.R.P. would like to thank the INAF-Turin Astrophysical Observatory, the Faculty of Physics of the University of Bucharest, and the Department of Physics of the University of Turin for funding and support of this work. A.C.S. was supported by funding from NASA's Office of Space Science through the Living With a Star Targeted Research & Technology Program. A.C.S. also benefited from discussions held at the International Space Science Institute's (ISSI, Bern, Switzerland) International Team on Solar Coronal Jets. Hinode is a solar physics science mission of the Japan Aerospace Exploration Agency (JAXA) in collaboration with the United States and the UK. NR 43 TC 5 Z9 5 U1 1 U2 1 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUL PY 2015 VL 579 AR A96 DI 10.1051/0004-6361/201525671 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO0XL UT WOS:000358877100108 ER PT J AU Popesso, P Biviano, A Finoguenov, A Wilman, D Salvato, M Magnelli, B Gruppioni, C Pozzi, F Rodighiero, G Ziparo, F Berta, S Elbaz, D Dickinson, M Lutz, D Altieri, B Aussel, H Cimatti, A Fadda, D Ilbert, O Le Floch, E Nordon, R Poglitsch, A Genel, S Xu, CK AF Popesso, P. Biviano, A. Finoguenov, A. Wilman, D. Salvato, M. Magnelli, B. Gruppioni, C. Pozzi, F. Rodighiero, G. Ziparo, F. Berta, S. Elbaz, D. Dickinson, M. Lutz, D. Altieri, B. Aussel, H. Cimatti, A. Fadda, D. Ilbert, O. Le Floch, E. Nordon, R. Poglitsch, A. Genel, S. Xu, C. K. TI The role of massive halos in the star formation history of the Universe SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE galaxies: evolution; galaxies: star formation; galaxies: groups: general ID INFRARED LUMINOSITY FUNCTIONS; DEEP-FIELD-SOUTH; HIERARCHICAL GALAXY FORMATION; GALACTIC NUCLEUS FEEDBACK; SUPERMASSIVE BLACK-HOLES; REST-FRAME ULTRAVIOLET; X-RAY GROUPS; FORMING GALAXIES; COSMOS FIELD; SPITZER VIEW AB Context. The most striking feature of the cosmic star formation history (CSFH) of the Universe is a dramatic drop in the star formation (SF) activity after z similar to 1. Aims. In this work we investigate whether the very same process of assembly and growth of structures is one of the major drivers of the observed decline in the Universe's SF activity. Methods. We study the contribution to the CSFH of galaxies in halos of different masses. This is done by studying the total SF ratehalo mass-redshift plane from redshift 0 to redshift similar to 1.6 in a sample of 57 groups and clusters by using the deepest available mid- and far-infrared surveys conducted with Spitzer MIPS and Herschel PACS and SPIRE, on blank (ECDFS, CDFN, and the COSMOS) and cluster fields. Results. Our results show that low mass groups (M-halo similar to 6 x 10(12) - 6 x 10(13) M-circle dot) provide a 60-80% contribution to the CSFH at z similar to 1. This contribution has declined faster than the CSFH in the past 8 billion years to less than 10% at z < 0.3, where the overall SF activity is sustained by lower mass halos. More massive systems (M-halo > 6 x 10(13) M-circle dot) provide only a marginal contribution (<10%) at any epoch. A simplified abundance-matching method shows that the large contribution of low mass groups at z similar to 1 is due to a large fraction (>50%) of very massive, highly star-forming main sequence galaxies. Below z similar to 1 a quenching process must take place in massive halos to cause the observed faster suppression of their SF activity. Such a process must be a slow one, though, since most of the models implementing a rapid quenching of the SF activity in accreting satellites significantly underpredict the observed SF level in massive halos at any redshift. This would rule out short time-scale mechanisms such as ram pressure stripping. Instead, starvation or the satellite's transition from cold to hot accretion would provide a quenching timescale of 1 to few Gyr that is more consistent with the observations. Conclusions. Our results suggest a scenario in which, owing to the structure formation process, more and more galaxies experience the group environment and the associated quenching process in the past 8 billion years. This leads to the progressive suppression of their SF activity so that it shapes the CSFH below z similar to 1. C1 [Popesso, P.] Excellence Cluster Universe, D-85748 Garching, Germany. [Popesso, P.; Finoguenov, A.; Wilman, D.; Salvato, M.; Magnelli, B.; Ziparo, F.; Berta, S.; Lutz, D.; Nordon, R.; Poglitsch, A.] Max Planck Inst Extraterr Phys MPE, D-85741 Garching, Germany. [Biviano, A.] Osserv Astron Trieste, INAF, I-34143 Trieste, Italy. [Gruppioni, C.] Osservatorio Astron Bologna, INAF, I-40127 Bologna, Italy. [Pozzi, F.] Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy. [Rodighiero, G.; Cimatti, A.] Univ Padua, Dipartimento Astron, I-35122 Padua, Italy. [Elbaz, D.; Dickinson, M.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Aussel, H.; Le Floch, E.] Univ Paris Diderot, CNRS, CEA DSM, Lab AIM,IRFU,Serv Astrophys,CEA Saclay, F-91191 Gif Sur Yvette, France. [Altieri, B.] ESA, European Space Astron Ctr, Herschel Sci Ctr, Madrid 28691, Spain. [Fadda, D.] Caltech 100 22, NASA, Herschel Sci Ctr, Pasadena, CA 91125 USA. [Ilbert, O.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Genel, S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Xu, C. K.] Caltech 100 22, IPAC, Pasadena, CA 91125 USA. RP Popesso, P (reprint author), Excellence Cluster Universe, Boltzmannstr 2, D-85748 Garching, Germany. EM popesso@mpe.mpg.de OI Gruppioni, Carlotta/0000-0002-5836-4056; Wilman, David/0000-0002-1822-4462; Rodighiero, Giulia/0000-0002-9415-2296 FU BMVIT (Austria); ESA-PRODEX (Belgium); CEA/CNES (France); DLR (Germany); ASI (Italy); CICYT/MCYT (Spain); NASA; Sloan Foundation; NSF; US Department of Energy; Japanese Monbukagakusho; Max Planck Society; Higher Education Funding Council of England FX The authors thank G. Zamorani for the very useful comments on an early draft of this paper. PACS has been developed by a consortium of institutes led by MPE (Germany) and including UVIE (Austria); KUL, CSL, IMEC (Belgium); CEA, OAMP (France); MPIA (Germany); IFSI, OAP/AOT, OAA/CAISMI, LENS, SISSA (Italy); IAC (Spain). This development has been supported by the funding agencies BMVIT (Austria), ESA-PRODEX (Belgium), CEA/CNES (France), DLR (Germany), ASI (Italy), and CICYT/MCYT (Spain). We gratefully acknowledge the contributions of the entire COSMOS collaboration consisting of more than 100 scientists. More information about the COSMOS survey is available at http://www.astro.caltech.edu/similar to cosmos. This research has made use of NASA's Astrophysics Data System, of NED, which is operated by JPL/Caltech, under contract with NASA, and of SDSS, which has been funded by the Sloan Foundation, NSF, the US Department of Energy, NASA, the Japanese Monbukagakusho, the Max Planck Society, and the Higher Education Funding Council of England. The SDSS is managed by the participating institutions (www.sdss.org/collaboration/credits.html). NR 112 TC 6 Z9 6 U1 3 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 EI 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUL PY 2015 VL 579 AR A132 DI 10.1051/0004-6361/201424715 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO0XL UT WOS:000358877100144 ER PT J AU Stock, DJ Wolfire, MG Peeters, E Tielens, AGGM Vandenbussche, B Boersma, C Cami, J AF Stock, D. J. Wolfire, M. G. Peeters, E. Tielens, A. G. G. M. Vandenbussche, B. Boersma, C. Cami, J. TI Herschel PACS and SPIRE spectroscopy of the photodissociation regions associated with S 106 and IRAS 23133+6050 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE ISM: general; ISM: molecules; photon-dominated region (PDR); infrared: ISM; stars: formation; stars: massive ID PHOTON-DOMINATED REGION; YOUNG STELLAR OBJECTS; STAR-FORMING REGION; H-II REGIONS; LONG-WAVELENGTH SPECTROMETER; FAR-INFRARED OBSERVATIONS; ULTRACOMPACT HII-REGIONS; ORION MOLECULAR CLOUD; LINE EMISSION; PHYSICAL CONDITIONS AB Context. Photodissociation regions (PDRs) contain a large portion of all of the interstellar matter in galaxies. Classical examples include the boundaries between ionized regions and molecular clouds in regions of massive star-formation, marking the point where all of the photons that are energetic enough to ionize hydrogen have been absorbed. Aims. To determine the physical properties of the PDRs associated with the star-forming regions IRAS 23133+6050 and S 106 and present them in the context of other Galactic PDRs associated with massive star-forming regions. Methods. We employ Herschel PACS and SPIRE spectroscopic observations to construct a full 55-650 mu m spectrum of each object from which we measure the PDR cooling lines, other fine-structure lines, CO lines, and the total far-infrared flux. These measurements (and combinations thereof) are then compared to standard PDR models. Subsequently, detailed numerical PDR models are compared to these predictions, yielding additional insight into the dominant thermal processes in the PDRs and their structures. Results. We find that the PDRs of each object are very similar and can be characterized by a two-phase PDR model with a very dense, highly UV irradiated phase (n similar to 10(6) cm(-3), G(0) similar to 10(5)) interspersed within a lower density, weaker radiation field phase (n similar to 10(4) cm(-3), G(0) similar to 10(4)). We employed two different numerical models to investigate the data. We first used RADEX models to fit the peak of the (CO)-C-12 ladder, which in conjunction with the properties derived, yielded a temperature of around 300 K. Subsequent numerical modeling with a full PDR model revealed that the dense phase has a filling factor of around 0.6 in both objects. The shape of the (CO)-C-12 ladder was consistent with these components, with heating dominated by grain photoelectric heating. An extra excitation component for the hightest-J lines (J > 20) is required for S 106. C1 [Stock, D. J.; Peeters, E.; Cami, J.] Univ Western Ontario, Dept Phys & Astron, London, ON N6A 3K7, Canada. [Wolfire, M. G.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Peeters, E.; Cami, J.] SETI Inst, Mountain View, CA 94043 USA. [Tielens, A. G. G. M.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Vandenbussche, B.] Katholieke Univ Leuven, Inst Sterrenkunde, B-3001 Louvain, Belgium. [Boersma, C.] NASA, Div Space Sci, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Stock, DJ (reprint author), Univ Western Ontario, Dept Phys & Astron, London, ON N6A 3K7, Canada. EM dstock4@uwo.ca FU NSERC; NSF [AST-1411827]; European Research Council [246976]; Dutch Science Agency, NWO, as part of the Dutch Astrochemistry Network; Dutch Science Agency, NWO FX D.J.S. thanks the referee, N. Schneider, for a very thorough and thoughtful referee report which has greatly improved the discussion sections of the paper. D.J.S. also thanks E. Polehampton at Rutherford Appleton Laboratories for his assistance in reducing the SPIRE data and understanding the Herschel SPIRE beam profiles. D.J.S. and E.P. acknowledge support from an NSERC Discovery Grant and an NSERC Discovery Accelerator Grant. M.G.W. was supported in part by NSF grant AST-1411827. Studies of interstellar chemistry at Leiden Observatory are supported through advanced-ERC grant 246976 from the European Research Council, through a grant by the Dutch Science Agency, NWO, as part of the Dutch Astrochemistry Network, and through the Spinoza premie from the Dutch Science Agency, NWO. C.B. is grateful for an appointment at NASA's Ames Research Center through San Jose State University Research Foundation (NNX14AG80A). J.C. acknowledges support from an NSERC Discovery Grant. This research has made use of NASA's Astrophysics Data System Bibliographic Services. NR 117 TC 2 Z9 2 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 EI 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUL PY 2015 VL 579 AR A67 DI 10.1051/0004-6361/201425245 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO0XL UT WOS:000358877100079 ER PT J AU Alam, S Albareti, FD Prieto, CA Anders, F Anderson, SF Anderton, T Andrews, BH Armengaud, E Aubourg, E Bailey, S Basu, S Bautista, JE Beaton, RL Beers, TC Bender, CF Berlind, AA Beutler, F Bhardwaj, V Bird, JC Bizyaev, D Blake, CH Blanton, MR Blomqvist, M Bochanski, JJ Bolton, AS Bovy, J Bradley, AS Brandt, WN Brauer, DE Brinkmann, J Brown, PJ Brownstein, JR Burden, A Burtin, E Busca, NG Cai, Z Capozzi, D Rosell, AC Carr, MA Carrera, R Chambers, KC Chaplin, WJ Chen, YC Chiappini, C Chojnowski, SD Chuang, CH Clerc, N Comparat, J Covey, K Croft, RAC Cuesta, AJ Cunha, K da Costa, LN Da Rio, N Davenport, JRA Dawson, KS De Lee, N Delubac, T Deshpande, R Dhital, S Dutra-Ferreira, L Dwelly, T Ealet, A Ebelke, GL Edmondson, EM Eisenstein, DJ Ellsworth, T Elsworth, Y Epstein, CR Eracleous, M Escoffier, S Esposito, M Evans, ML Fan, XH Fernandez-Alvar, E Feuillet, D Ak, NF Finley, H Finoguenov, A Flaherty, K Fleming, SW Font-Ribera, A Foster, J Frinchaboy, PM Galbraith-Frew, JG Garcia, RA Garcia-Hernandez, DA Perez, AEG Gaulme, P Ge, J Genova-Santos, R Georgakakis, A Ghezzi, L Gillespie, BA Girardi, L Goddard, D Gontcho, SGA Hernandez, JIG Grebel, EK Green, PJ Grieb, JN Grieves, N Gunn, JE Guo, H Harding, P Hasselquist, S Hawley, SL Hayden, M Hearty, FR Hekker, S Ho, S Hogg, DW Holley-Bockelmann, K Holtzman, JA Honscheid, K Huber, D Huehnerhoff, J Ivans, II Jiang, LH Johnson, JA Kinemuchi, K Kirkby, D Kitaura, F Klaene, MA Knapp, GR Kneib, JP Koenig, XP Lam, CR Lan, TW Lang, DT Laurent, P Le Goff, JM Leauthaud, A Lee, KG Lee, YS Licquia, TC Liu, J Long, DC Lopez-Corredoira, M Lorenzo-Oliveira, D Lucatello, S Lundgren, B Lupton, RH Mack, CE Mahadevan, S Maia, MAG Majewski, SR Malanushenko, E Malanushenko, V Manchado, A Manera, M Mao, QQ Maraston, C Marchwinski, RC Margala, D Martell, SL Martig, M Masters, KL Mathur, S McBride, CK McGehee, PM McGreer, ID McMahon, RG Menard, B Menzel, ML Merloni, A Meszaros, S Miller, AA Miralda-Escude, J Miyatake, H Montero-Dorta, AD More, S Morganson, E Morice-Atkinson, X Morrison, HL Mosser, B Muna, D Myers, AD Nandra, K Newman, JA Neyrinck, M Nguyen, DC Nichol, RC Nidever, DL Noterdaeme, P Nuza, SE O'Connell, JE O'Connell, RW O'Connell, R Ogando, RLC Olmstead, MD Oravetz, AE Oravetz, DJ Osumi, K Owen, R Padgett, DL Padmanabhan, N Paegert, M Palanque-Delabrouille, N Pan, KK Parejko, JK Paris, I Park, C Pattarakijwanich, P Pellejero-Ibanez, M Pepper, J Percival, WJ Perez-Fournon, I Perez-Rafols, I Petitjean, P Pieri, MM Pinsonneault, MH de Mello, GFP Prada, F Prakash, A Price-Whelan, AM Protopapas, P Raddick, MJ Rahman, M Reid, BA Rich, J Rix, HW Robin, AC Rockosi, CM Rodrigues, TS Rodriguez-Torres, S Roe, NA Ross, AJ Ross, NP Rossi, G Ruan, JJ Rubino-Martin, JA Rykoff, ES Salazar-Albornoz, S Salvato, M Samushia, L Sanchez, AG Santiago, B Sayres, C Schiavon, RP Schlegel, DJ Schmidt, SJ Schneider, DP Schultheis, M Schwope, AD Scoccola, CG Scott, C Sellgren, K Seo, HJ Serenelli, A Shane, N Shen, Y Shetrone, M Shu, YP Aguirre, VS Sivarani, T Skrutskie, MF Slosar, A Smith, VV Sobreira, F Souto, D Stassun, KG Steinmetz, M Stello, D Strauss, MA Streblyanska, A Suzuki, N Swanson, MEC Tan, JC Tayar, J Terrien, RC Thakar, AR Thomas, D Thomas, N Thompson, BA Tinker, JL Tojeiro, R Troup, NW Vargas-Magana, M Vazquez, JA Verde, L Viel, M Vogt, NP Wake, DA Wang, J Weaver, BA Weinberg, DH Weiner, BJ White, M Wilson, JC Wisniewski, JP Wood-Vasey, WM Yeche, C York, DG Zakamska, NL Zamora, O Zasowski, G Zehavi, I Zhao, GB Zheng, Z Zhou, X Zhou, ZM Zou, H Zhu, GT AF Alam, Shadab Albareti, Franco D. Allende Prieto, Carlos Anders, F. Anderson, Scott F. Anderton, Timothy Andrews, Brett H. Armengaud, Eric Aubourg, Eric Bailey, Stephen Basu, Sarbani Bautista, Julian E. Beaton, Rachael L. Beers, Timothy C. Bender, Chad F. Berlind, Andreas A. Beutler, Florian Bhardwaj, Vaishali Bird, Jonathan C. Bizyaev, Dmitry Blake, Cullen H. Blanton, Michael R. Blomqvist, Michael Bochanski, John J. Bolton, Adam S. Bovy, Jo Bradley, A. Shelden Brandt, W. N. Brauer, D. E. Brinkmann, J. Brown, Peter J. Brownstein, Joel R. Burden, Angela Burtin, Etienne Busca, Nicolas G. Cai, Zheng Capozzi, Diego Rosell, Aurelio Carnero Carr, Michael A. Carrera, Ricardo Chambers, K. C. Chaplin, William James Chen, Yen-Chi Chiappini, Cristina Chojnowski, S. Drew Chuang, Chia-Hsun Clerc, Nicolas Comparat, Johan Covey, Kevin Croft, Rupert A. C. Cuesta, Antonio J. Cunha, Katia da Costa, Luiz N. Da Rio, Nicola Davenport, James R. A. Dawson, Kyle S. De Lee, Nathan Delubac, Timothee Deshpande, Rohit Dhital, Saurav Dutra-Ferreira, Leticia Dwelly, Tom Ealet, Anne Ebelke, Garrett L. Edmondson, Edward M. Eisenstein, Daniel J. Ellsworth, Tristan Elsworth, Yvonne Epstein, Courtney R. Eracleous, Michael Escoffier, Stephanie Esposito, Massimiliano Evans, Michael L. Fan, Xiaohui Fernandez-Alvar, Emma Feuillet, Diane Ak, Nurten Filiz Finley, Hayley Finoguenov, Alexis Flaherty, Kevin Fleming, Scott W. Font-Ribera, Andreu Foster, Jonathan Frinchaboy, Peter M. Galbraith-Frew, J. G. Garcia, Rafael A. Garcia-Hernandez, D. A. Garcia Perez, Ana E. Gaulme, Patrick Ge, Jian Genova-Santos, R. Georgakakis, A. Ghezzi, Luan Gillespie, Bruce A. Girardi, Leo Goddard, Daniel Gontcho, Satya Gontcho A. Gonzalez Hernandez, Jonay I. Grebel, Eva K. Green, Paul J. Grieb, Jan Niklas Grieves, Nolan Gunn, James E. Guo, Hong Harding, Paul Hasselquist, Sten Hawley, Suzanne L. Hayden, Michael Hearty, Fred R. Hekker, Saskia Ho, Shirley Hogg, David W. Holley-Bockelmann, Kelly Holtzman, Jon A. Honscheid, Klaus Huber, Daniel Huehnerhoff, Joseph Ivans, Inese I. Jiang, Linhua Johnson, Jennifer A. Kinemuchi, Karen Kirkby, David Kitaura, Francisco Klaene, Mark A. Knapp, Gillian R. Kneib, Jean-Paul Koenig, Xavier P. Lam, Charles R. Lan, Ting-Wen Lang, Dustin Laurent, Pierre Le Goff, Jean-Marc Leauthaud, Alexie Lee, Khee-Gan Lee, Young Sun Licquia, Timothy C. Liu, Jian Long, Daniel C. Lopez-Corredoira, Martin Lorenzo-Oliveira, Diego Lucatello, Sara Lundgren, Britt Lupton, Robert H. Mack, Claude E., III Mahadevan, Suvrath Maia, Marcio A. G. Majewski, Steven R. Malanushenko, Elena Malanushenko, Viktor Manchado, A. Manera, Marc Mao, Qingqing Maraston, Claudia Marchwinski, Robert C. Margala, Daniel Martell, Sarah L. Martig, Marie Masters, Karen L. Mathur, Savita McBride, Cameron K. McGehee, Peregrine M. McGreer, Ian D. McMahon, Richard G. Menard, Brice Menzel, Marie-Luise Merloni, Andrea Meszaros, Szabolcs Miller, Adam A. Miralda-Escude, Jordi Miyatake, Hironao Montero-Dorta, Antonio D. More, Surhud Morganson, Eric Morice-Atkinson, Xan Morrison, Heather L. Mosser, Benoit Muna, Demitri Myers, Adam D. Nandra, Kirpal Newman, Jeffrey A. Neyrinck, Mark Nguyen, Duy Cuong Nichol, Robert C. Nidever, David L. Noterdaeme, Pasquier Nuza, Sebastian E. O'Connell, Julia E. O'Connell, Robert W. O'Connell, Ross Ogando, Ricardo L. C. Olmstead, Matthew D. Oravetz, Audrey E. Oravetz, Daniel J. Osumi, Keisuke Owen, Russell Padgett, Deborah L. Padmanabhan, Nikhil Paegert, Martin Palanque-Delabrouille, Nathalie Pan, Kaike Parejko, John K. Paris, Isabelle Park, Changbom Pattarakijwanich, Petchara Pellejero-Ibanez, M. Pepper, Joshua Percival, Will J. Perez-Fournon, Ismael Perez-Rafols, Ignasi Petitjean, Patrick Pieri, Matthew M. Pinsonneault, Marc H. Porto de Mello, Gustavo F. Prada, Francisco Prakash, Abhishek Price-Whelan, Adrian M. Protopapas, Pavlos Raddick, M. Jordan Rahman, Mubdi Reid, Beth A. Rich, James Rix, Hans-Walter Robin, Annie C. Rockosi, Constance M. Rodrigues, Thaise S. Rodriguez-Torres, Sergio Roe, Natalie A. Ross, Ashley J. Ross, Nicholas P. Rossi, Graziano Ruan, John J. Rubino-Martin, J. A. Rykoff, Eli S. Salazar-Albornoz, Salvador Salvato, Mara Samushia, Lado Sanchez, Ariel G. Santiago, Basilio Sayres, Conor Schiavon, Ricardo P. Schlegel, David J. Schmidt, Sarah J. Schneider, Donald P. Schultheis, Mathias Schwope, Axel D. Scoccola, C. G. Scott, Caroline Sellgren, Kris Seo, Hee-Jong Serenelli, Aldo Shane, Neville Shen, Yue Shetrone, Matthew Shu, Yiping Aguirre, V. Silva Sivarani, Thirupathi Skrutskie, M. F. Slosar, Anze Smith, Verne V. Sobreira, Flavia Souto, Diogo Stassun, Keivan G. Steinmetz, Matthias Stello, Dennis Strauss, Michael A. Streblyanska, Alina Suzuki, Nao Swanson, Molly E. C. Tan, Jonathan C. Tayar, Jamie Terrien, Ryan C. Thakar, Aniruddha R. Thomas, Daniel Thomas, Neil Thompson, Benjamin A. Tinker, Jeremy L. Tojeiro, Rita Troup, Nicholas W. Vargas-Magana, Mariana Vazquez, Jose A. Verde, Licia Viel, Matteo Vogt, Nicole P. Wake, David A. Wang, Ji Weaver, Benjamin A. Weinberg, David H. Weiner, Benjamin J. White, Martin Wilson, John C. Wisniewski, John P. Wood-Vasey, W. M. Yeche, Christophe York, Donald G. Zakamska, Nadia L. Zamora, O. Zasowski, Gail Zehavi, Idit Zhao, Gong-Bo Zheng, Zheng Zhou, Xu Zhou, Zhimin Zou, Hu Zhu, Guangtun TI THE ELEVENTH AND TWELFTH DATA RELEASES OF THE SLOAN DIGITAL SKY SURVEY: FINAL DATA FROM SDSS-III SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE atlases; catalogs; surveys ID OSCILLATION SPECTROSCOPIC SURVEY; GALACTIC EVOLUTION EXPERIMENT; BARYON ACOUSTIC-OSCILLATIONS; LOW-MASS STELLAR; 1ST DATA RELEASE; SOLAR-LIKE STARS; FIXED-DELAY INTERFEROMETRY; CATALOG ARCHIVE SERVER; BROWN DWARF CANDIDATE; MAIN-SEQUENCE STARS AB The third generation of the Sloan Digital Sky Survey (SDSS-III) took data from 2008 to 2014 using the original SDSS wide-field imager, the original and an upgraded multi-object fiber-fed optical spectrograph, a new near-infrared high-resolution spectrograph, and a novel optical interferometer. All of the data from SDSS-III are now made public. In particular, this paper describes Data Release 11 (DR11) including all data acquired through 2013 July, and Data Release 12 (DR12) adding data acquired through 2014 July (including all data included in previous data releases), marking the end of SDSS-III observing. Relative to our previous public release (DR10), DR12 adds one million new spectra of galaxies and quasars from the Baryon Oscillation Spectroscopic Survey (BOSS) over an additional 3000 deg(2) of sky, more than triples the number of H-band spectra of stars as part of the Apache Point Observatory (APO) Galactic Evolution Experiment (APOGEE), and includes repeated accurate radial velocity measurements of 5500 stars from the Multi-object APO Radial Velocity Exoplanet Large-area Survey (MARVELS). The APOGEE outputs now include the measured abundances of 15 different elements for each star. In total, SDSS-III added 5200 deg(2) of ugriz imaging; 155,520 spectra of 138,099 stars as part of the Sloan Exploration of Galactic Understanding and Evolution 2 (SEGUE-2) survey; 2,497,484 BOSS spectra of 1,372,737 galaxies, 294,512 quasars, and 247,216 stars over 9376 deg(2); 618,080 APOGEE spectra of 156,593 stars; and 197,040 MARVELS spectra of 5513 stars. Since its first light in 1998, SDSS has imaged over 1/3 of the Celestial sphere in five bands and obtained over five million astronomical spectra. C1 [Alam, Shadab; Croft, Rupert A. C.; Ho, Shirley; Lang, Dustin; O'Connell, Ross; Osumi, Keisuke; Vargas-Magana, Mariana] Carnegie Mellon Univ, Dept Phys, McWilliams Ctr Cosmol, Pittsburgh, PA 15213 USA. [Albareti, Franco D.; Chuang, Chia-Hsun; Comparat, Johan; Prada, Francisco; Rodriguez-Torres, Sergio] Univ Autonoma Madrid, Inst Fis Teor, UAM CSIC, E-28049 Madrid, Spain. [Allende Prieto, Carlos; Carrera, Ricardo; Esposito, Massimiliano; Fernandez-Alvar, Emma; Garcia-Hernandez, D. A.; Garcia Perez, Ana E.; Genova-Santos, R.; Gonzalez Hernandez, Jonay I.; Lopez-Corredoira, Martin; Manchado, A.; Pellejero-Ibanez, M.; Perez-Fournon, Ismael; Rubino-Martin, J. A.; Scoccola, C. G.; Streblyanska, Alina; Zamora, O.] IAC, E-38200 Tenerife, Spain. [Allende Prieto, Carlos; Carrera, Ricardo; Esposito, Massimiliano; Fernandez-Alvar, Emma; Garcia-Hernandez, D. A.; Garcia Perez, Ana E.; Genova-Santos, R.; Gonzalez Hernandez, Jonay I.; Lopez-Corredoira, Martin; Manchado, A.; Pellejero-Ibanez, M.; Perez-Fournon, Ismael; Rubino-Martin, J. A.; Scoccola, C. G.; Streblyanska, Alina; Zamora, O.] Univ La Laguna, Dept Astrofis, E-38206 Tenerife, Spain. [Anders, F.; Brauer, D. E.; Chiappini, Cristina; Kitaura, Francisco; Mack, Claude E., III; Nuza, Sebastian E.; Schwope, Axel D.; Steinmetz, Matthias] Leibniz Inst Astrophys Potsdam AIP, D-14482 Potsdam, Germany. [Anderson, Scott F.; Bhardwaj, Vaishali; Bochanski, John J.; Davenport, James R. A.; Eracleous, Michael; Evans, Michael L.; Hawley, Suzanne L.; Owen, Russell; Ruan, John J.; Sayres, Conor] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Anderton, Timothy; Bolton, Adam S.; Brownstein, Joel R.; Dawson, Kyle S.; Ellsworth, Tristan; Galbraith-Frew, J. G.; Guo, Hong; Ivans, Inese I.; Montero-Dorta, Antonio D.; Olmstead, Matthew D.; Shu, Yiping; Zheng, Zheng] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA. [Andrews, Brett H.; Epstein, Courtney R.; Johnson, Jennifer A.; Muna, Demitri; Pinsonneault, Marc H.; Schmidt, Sarah J.; Sellgren, Kris; Tayar, Jamie; Weinberg, David H.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Andrews, Brett H.; Licquia, Timothy C.; Newman, Jeffrey A.; Prakash, Abhishek; Wood-Vasey, W. M.] Univ Pittsburgh, Dept Phys & Astron, PITT PACC, Pittsburgh, PA 15260 USA. [Armengaud, Eric; Burtin, Etienne; Laurent, Pierre; Le Goff, Jean-Marc; Palanque-Delabrouille, Nathalie; Rich, James; Rossi, Graziano; Yeche, Christophe] CEA, Ctr Saclay, Irfu SPP, F-91191 Gif Sur Yvette, France. [Aubourg, Eric; Bautista, Julian E.; Busca, Nicolas G.] Univ Paris Diderot, Sorbonne Paris Cite, Observ Paris, APC,CNRS IN2P3,CEA IRFU, F-75205 Paris, France. [Bailey, Stephen; Beutler, Florian; Bhardwaj, Vaishali; Font-Ribera, Andreu; Reid, Beth A.; Roe, Natalie A.; Schlegel, David J.; White, Martin] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. [Basu, Sarbani; Koenig, Xavier P.; Wang, Ji] Yale Univ, Dept Astron, New Haven, CT 06520 USA. [Beaton, Rachael L.; Ebelke, Garrett L.; Garcia Perez, Ana E.; Lam, Charles R.; Majewski, Steven R.; O'Connell, Robert W.; Shane, Neville; Skrutskie, M. F.; Troup, Nicholas W.; Wilson, John C.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. [Beaton, Rachael L.; Shen, Yue] Observ Carnegie Inst Washington, Pasadena, CA 91101 USA. [Beers, Timothy C.] Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA. [Beers, Timothy C.] Univ Notre Dame, JINA Ctr Evolut Elements, Notre Dame, IN 46556 USA. [Bender, Chad F.; Brandt, W. N.; Deshpande, Rohit; Eracleous, Michael; Ak, Nurten Filiz; Hearty, Fred R.; Mahadevan, Suvrath; Marchwinski, Robert C.; Schneider, Donald P.; Terrien, Ryan C.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA. [Bender, Chad F.; Deshpande, Rohit; Mahadevan, Suvrath; Marchwinski, Robert C.; Terrien, Ryan C.] Penn State Univ, Ctr Exoplanets & Habitable Worlds, Davey Lab 525, University Pk, PA 16802 USA. [Berlind, Andreas A.; Bird, Jonathan C.; Holley-Bockelmann, Kelly; Mack, Claude E., III; Mao, Qingqing; Paegert, Martin; Pepper, Joshua; Stassun, Keivan G.] Vanderbilt Univ, Dept Phys & Astron, Nashville, TN 37235 USA. [Bizyaev, Dmitry; Bradley, A. Shelden; Brinkmann, J.; Gaulme, Patrick; Huehnerhoff, Joseph; Kinemuchi, Karen; Klaene, Mark A.; Long, Daniel C.; Malanushenko, Elena; Malanushenko, Viktor; Oravetz, Audrey E.; Oravetz, Daniel J.; Pan, Kaike] Apache Point Observ, Sunspot, NM 88349 USA. [Bizyaev, Dmitry; Chojnowski, S. Drew; Feuillet, Diane; Hasselquist, Sten; Hayden, Michael; Holtzman, Jon A.; Kinemuchi, Karen; Long, Daniel C.; Malanushenko, Elena; Malanushenko, Viktor; Oravetz, Audrey E.; Vogt, Nicole P.] New Mexico State Univ, Dept Astron, Las Cruces, NM 88003 USA. [Bizyaev, Dmitry] Moscow MV Lomonosov State Univ, Sternberg Astron Inst, Moscow 119992, Russia. [Blake, Cullen H.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. [Blanton, Michael R.; Hogg, David W.; Tinker, Jeremy L.; Weaver, Benjamin A.] NYU, Dept Phys, Ctr Cosmol & Particle Phys, New York, NY 10003 USA. [Blomqvist, Michael; Kirkby, David; Margala, Daniel] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. [Bochanski, John J.] Rider Univ, Lawrenceville, NJ 08648 USA. [Bovy, Jo] Inst Adv Study, Princeton, NJ 08540 USA. [Brandt, W. N.; Eracleous, Michael; Ak, Nurten Filiz; Schneider, Donald P.] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA. [Brandt, W. N.] Penn State Univ, Dept Phys, University Pk, PA 16802 USA. [Brown, Peter J.] Texas A&M Univ, George P & Cynthia Woods Mitchell Inst Fundamenta, Dept Phys & Astron, College Stn, TX 77843 USA. [Burden, Angela; Capozzi, Diego; Edmondson, Edward M.; Goddard, Daniel; Manera, Marc; Maraston, Claudia; Masters, Karen L.; Morice-Atkinson, Xan; Nichol, Robert C.; Percival, Will J.; Pieri, Matthew M.; Ross, Ashley J.; Thomas, Daniel; Zhao, Gong-Bo] Univ Portsmouth, Inst Cosmol & Gravitat, Portsmouth PO1 3FX, Hants, England. [Busca, Nicolas G.; Rosell, Aurelio Carnero; Cunha, Katia; da Costa, Luiz N.; Ghezzi, Luan; Maia, Marcio A. G.; Ogando, Ricardo L. C.; Souto, Diogo] Observ Nacl, BR-20921400 Rio De Janeiro, RJ, Brazil. [Busca, Nicolas G.; Rosell, Aurelio Carnero; Chiappini, Cristina; da Costa, Luiz N.; Dutra-Ferreira, Leticia; Girardi, Leo; Lorenzo-Oliveira, Diego; Maia, Marcio A. G.; Ogando, Ricardo L. C.; Porto de Mello, Gustavo F.; Rodrigues, Thaise S.; Santiago, Basilio; Sobreira, Flavia] Lab Interinstituc & Astron LIneA, BR-20921400 Rio De Janeiro, RJ, Brazil. [Cai, Zheng; Cunha, Katia; Fan, Xiaohui; McGreer, Ian D.; Weiner, Benjamin J.] Steward Observ, Tucson, AZ 85721 USA. [Carr, Michael A.; Gunn, James E.; Knapp, Gillian R.; Lupton, Robert H.; Miyatake, Hironao; Pattarakijwanich, Petchara; Strauss, Michael A.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Chambers, K. C.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Chaplin, William James; Elsworth, Yvonne] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. [Chaplin, William James; Elsworth, Yvonne; Hekker, Saskia; Huber, Daniel; Aguirre, V. Silva; Stello, Dennis] Aarhus Univ, Dept Phys & Astron, SAC, DK-8000 Aarhus C, Denmark. [Chen, Yen-Chi] Carnegie Mellon Univ, Dept Stat, Bruce & Astrid McWilliams Ctr Cosmol, Pittsburgh, PA 15213 USA. [Clerc, Nicolas; Dwelly, Tom; Georgakakis, A.; Grieb, Jan Niklas; Menzel, Marie-Luise; Merloni, Andrea; Nandra, Kirpal; Salazar-Albornoz, Salvador; Salvato, Mara; Sanchez, Ariel G.] Max Planck Inst Extraterr Phys, D-85741 Garching, Germany. [Covey, Kevin] Lowell Observ, Flagstaff, AZ 86001 USA. [Covey, Kevin] Western Washington Univ, Dept Phys & Astron, Bellingham, WA 98225 USA. [Cuesta, Antonio J.; Gontcho, Satya Gontcho A.; Miralda-Escude, Jordi; Perez-Rafols, Ignasi; Verde, Licia] Univ Barcelona, Inst Ciencies Cosmos, IEEC, E-08028 Barcelona, Spain. [Cuesta, Antonio J.; Foster, Jonathan; Padmanabhan, Nikhil] Yale Univ, Yale Ctr Astron & Astrophys, New Haven, CT 06520 USA. [Da Rio, Nicola; Ge, Jian; Grieves, Nolan; Liu, Jian; Tan, Jonathan C.; Thomas, Neil] Univ Florida, Dept Astron, Bryant Space Sci Ctr, Gainesville, FL 32611 USA. [De Lee, Nathan] No Kentucky Univ, Dept Phys & Geol, Highland Hts, KY 41099 USA. [Delubac, Timothee; Kneib, Jean-Paul] EPFL, Lab Astrophys, Observ Sauverny, CH-1290 Versoix, Switzerland. [Dhital, Saurav] Embry Riddle Aeronaut Univ, Dept Phys Sci, Daytona Beach, FL 32114 USA. [Dutra-Ferreira, Leticia; Lorenzo-Oliveira, Diego; Porto de Mello, Gustavo F.] Univ Fed Rio de Janeiro, Observ Valongo, BR-20080090 Rio De Janeiro, Brazil. [Dutra-Ferreira, Leticia] Univ Fed Rio Grande do Norte, Dept Fis, BR-59072970 Natal, RN, Brazil. [Ealet, Anne; Escoffier, Stephanie] Aix Marseille Univ, Ctr Phys Particules Marseille, CNRS IN2P3, F-13288 Marseille, France. [Eisenstein, Daniel J.; Ghezzi, Luan; Green, Paul J.; McBride, Cameron K.; Morganson, Eric; Scott, Caroline; Swanson, Molly E. C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Eracleous, Michael] Georgia Inst Technol, Ctr Relativist Astrophys, Atlanta, GA 30332 USA. [Ak, Nurten Filiz] Erciyes Univ, Dept Astron & Space Sci, Fac Sci, TR-38039 Kayseri, Turkey. [Finley, Hayley; Noterdaeme, Pasquier; Petitjean, Patrick] UPMC, Inst Astrophys Paris, CNRS, UMR7095, F-75014 Paris, France. [Finoguenov, Alexis] Univ Helsinki, Dept Phys, FI-00140 Helsinki, Finland. [Flaherty, Kevin] Wesleyan Univ, Van Vleck Observ, Dept Astron, Middletown, CT 06459 USA. [Fleming, Scott W.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Fleming, Scott W.] Comp Sci Corp, Baltimore, MD 21218 USA. [Frinchaboy, Peter M.; O'Connell, Julia E.; Thompson, Benjamin A.] Texas Christian Univ, Dept Phys & Astron, Ft Worth, TX 76129 USA. [Garcia, Rafael A.] Univ Paris Diderot, Lab AIM, Ctr Saclay, CEA DSM,CNRS,IRFU SAp, F-91191 Gif Sur Yvette, France. [Gillespie, Bruce A.; Lan, Ting-Wen; Menard, Brice; Neyrinck, Mark; Raddick, M. Jordan; Rahman, Mubdi; Thakar, Aniruddha R.; Zakamska, Nadia L.; Zasowski, Gail; Zhu, Guangtun] Johns Hopkins Univ, Ctr Astrophys Sci, Dept Phys & Astron, Baltimore, MD 21218 USA. [Girardi, Leo; Lucatello, Sara; Rodrigues, Thaise S.] INAF, Osservatorio Astron Padova, I-35122 Padua, Italy. [Grebel, Eva K.] Heidelberg Univ, Zentrum Astron, Astron Rech Inst, D-69120 Heidelberg, Germany. [Harding, Paul; Morrison, Heather L.; Zehavi, Idit] Case Western Reserve Univ, Dept Astron, Cleveland, OH 44106 USA. [Hekker, Saskia] Max Planck Inst Sonnensystemforsch, D-37077 Gottingen, Germany. [Honscheid, Klaus] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA. [Honscheid, Klaus; Johnson, Jennifer A.; Ross, Ashley J.] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA. [Huber, Daniel; Stello, Dennis] Univ Sydney, Sch Phys, Sydney Inst Astron SIfA, Sydney, NSW 2006, Australia. [Huber, Daniel] SETI Inst, Mountain View, CA 94043 USA. [Jiang, Linhua; Shen, Yue] Peking Univ, Kavli Inst Astron & Astrophys, Beijing 100871, Peoples R China. [Kneib, Jean-Paul] Univ Provence, CNRS, Lab Astrophys Marseille, F-13388 Marseille 13, France. [Leauthaud, Alexie; Menard, Brice; Miyatake, Hironao; More, Surhud; Suzuki, Nao] Univ Tokyo, Todai Inst Adv Study, Kavli Inst Phys Math Univ Kavli IPMU, WPI, Kashiwa, Chiba 2778583, Japan. [Lee, Khee-Gan; Martig, Marie; Rix, Hans-Walter] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Lee, Young Sun] Chungnam Natl Univ, Dept Astron & Space Sci, Taejon 305764, South Korea. [Lundgren, Britt; Wake, David A.] Univ Wisconsin, Dept Astron, Madison, WI 53703 USA. [Manera, Marc] UCL, London WC1E 6BT, England. [Martell, Sarah L.] Univ New S Wales, Sch Phys, Sydney, NSW 2052, Australia. [Mathur, Savita] Space Sci Inst, Boulder, CO 80301 USA. [McGehee, Peregrine M.] CALTECH, IPAC, Pasadena, CA 91125 USA. [McMahon, Richard G.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [McMahon, Richard G.] Univ Cambridge, Kavli Inst Cosmol, Cambridge CB3 0HA, England. [Meszaros, Szabolcs] ELTE Gothard Astrophys Observ, H-9704 Szombathely, Hungary. [Miller, Adam A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Miller, Adam A.] CALTECH, Dept Astron, Pasadena, CA 91125 USA. [Miralda-Escude, Jordi; Verde, Licia] Inst Catalana Recerca & Estudis Avancats, E-08010 Barcelona, Spain. [Mosser, Benoit] Univ Paris 07, Univ Paris 06, Observ Paris, LESIA,UMR 8109, F-92195 Meudon, France. [Myers, Adam D.] Univ Wyoming, Dept Phys & Astron, Laramie, WY 82071 USA. [Nguyen, Duy Cuong] Univ Toronto, Dunlap Inst Astron & Astrophys, Toronto, ON M5S 3H4, Canada. [Nidever, David L.] Univ Michigan, Dept Astron, Ann Arbor, MI 48104 USA. [Olmstead, Matthew D.] Kings Coll, Dept Chem & Phys, Wilkes Barre, PA 18711 USA. [Padgett, Deborah L.] NASA GSFC, Greenbelt, MD USA. [Parejko, John K.] Yale Univ, Dept Phys, New Haven, CT USA. [Paris, Isabelle; Viel, Matteo] INAF, Osservatorio Astron Trieste, I-34131 Trieste, Italy. [Park, Changbom] Korea Inst Adv Study, Sch Phys, Seoul 130722, South Korea. [Pepper, Joshua] Lehigh Univ, Dept Phys, Bethlehem, PA 18015 USA. [Perez-Rafols, Ignasi] Univ Barcelona, Fac Fis, Dept Astron & Meteorol, E-08028 Barcelona, Spain. [Pieri, Matthew M.] Aix Marseille Univ, A MIDEX, CNRS, LAM UMR 7326, F-13388 Marseille 13, France. [Prada, Francisco; Rodriguez-Torres, Sergio] Campus Int Excellence UAM CSIC, E-28049 Madrid, Spain. [Prada, Francisco] CSIC, Inst Astrofis Andalucia, E-18080 Granada, Spain. [Price-Whelan, Adrian M.] Columbia Univ, Dept Astron, New York, NY 10027 USA. [Protopapas, Pavlos] Harvard Univ, SEAS, Inst Appl Computat Sci, Cambridge, MA 02138 USA. [Reid, Beth A.; White, Martin] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Robin, Annie C.] Univ Franche Comte, Inst Utinam, UMR CNRS 6213, OSU Theta, F-25010 Besancon, France. [Rockosi, Constance M.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Rodrigues, Thaise S.] Univ Padua, Dipartimento Fis & Astron, I-35122 Padua, Italy. [Ross, Nicholas P.] Drexel Univ, Dept Phys, Philadelphia, PA 19104 USA. [Rossi, Graziano] Sejong Univ, Dept Astron & Space Sci, Seoul 143747, South Korea. [Rykoff, Eli S.] SLAC Natl Accelerator Lab, Menlo Pk, CA 94025 USA. [Salazar-Albornoz, Salvador] Univ Sternwarte, D-81679 Munich, Germany. [Salvato, Mara] Cluster Excellence, D-85748 Garching, Germany. [Samushia, Lado] Kansas State Univ, Dept Phys, Manhattan, KS 66506 USA. [Samushia, Lado] Ilia State Univ, Natl Abastumani Astrophys Observ, GE-1060 Tbilisi, Rep of Georgia. [Santiago, Basilio] Univ Fed Rio Grande do Sul, Inst Fis, BR-91501970 Porto Alegre, RS, Brazil. [Schiavon, Ricardo P.] Gemini Observ, Hilo, HI 96720 USA. [Schiavon, Ricardo P.] Liverpool John Moores Univ, Astrophys Res Inst, Liverpool L3 5RF, Merseyside, England. [Schultheis, Mathias] Univ Nice Sophia Antipolis, CNRS, Observ Cote dAzur, Lab Lagrange, F-06304 Nice 4, France. [Seo, Hee-Jong] Ohio Univ, Dept Phys & Astron, Athens, OH 45701 USA. [Serenelli, Aldo] CSIC IEEC, Inst Ciencias Espacio, Fac Ciencias, E-08193 Bellaterra, Spain. [Shetrone, Matthew] Univ Texas Austin, Hobby Eberly Telescope, McDonald Observatory, TX 79734 USA. [Sivarani, Thirupathi] Indian Inst Astrophys, Bangalore 560034, Karnataka, India. [Slosar, Anze; Vazquez, Jose A.] Brookhaven Natl Lab, Upton, NY 11973 USA. [Smith, Verne V.] Natl Opt Astron Observ, Tucson, AZ USA. [Sobreira, Flavia] Fermilab Natl Accelerator Lab, Batavia, IL 60510 USA. [Stassun, Keivan G.] Fisk Univ, Dept Phys, Nashville, TN 37208 USA. [Terrien, Ryan C.] Penn State Univ, Penn State Astrobiol Res Ctr, University Pk, PA 16802 USA. [Thomas, Daniel] South East Phys Network, SEPnet, Southampton, Hants, England. [Tojeiro, Rita] Univ St Andrews, Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland. [Verde, Licia] Univ Oslo, Inst Theoret Astrophys, NO-0315 Oslo, Norway. [Viel, Matteo] Ist Nazl Fis Nucl, I-34127 Trieste, Italy. [Wake, David A.] Open Univ, Dept Phys Sci, Milton Keynes MK7 6AA, Bucks, England. [Wisniewski, John P.] Univ Oklahoma, HL Dodge Dept Phys & Astron, Norman, OK 73019 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. [Zhao, Gong-Bo] Chinese Acad Sci, Natl Astron Observ, Beijing 100012, Peoples R China. [Zhou, Xu; Zhou, Zhimin; Zou, Hu] Chinese Acad Sci, Key Lab Opt Astron, Natl Astron Observ, Beijing 100012, Peoples R China. RP Wood-Vasey, WM (reprint author), Univ Pittsburgh, Dept Phys & Astron, PITT PACC, 3941 OHara St, Pittsburgh, PA 15260 USA. RI Ogando, Ricardo/A-1747-2010; White, Martin/I-3880-2015; Brandt, William/N-2844-2015; Meszaros, Szabolcs/N-2287-2014; Georgakakis, Antonis/K-4457-2013; Mao, Qingqing/E-2043-2016; Sobreira, Flavia/F-4168-2015; Jiang, Linhua/H-5485-2016; Croft, Rupert/N-8707-2014; EPFL, Physics/O-6514-2016; Carrera, Ricardo/K-8760-2014; OI Ogando, Ricardo/0000-0003-2120-1154; White, Martin/0000-0001-9912-5070; Brandt, William/0000-0002-0167-2453; Meszaros, Szabolcs/0000-0001-8237-5209; Mao, Qingqing/0000-0001-6001-6723; Sobreira, Flavia/0000-0002-7822-0658; Jiang, Linhua/0000-0003-4176-6486; Croft, Rupert/0000-0003-0697-2583; Carrera, Ricardo/0000-0001-6143-8151; Rahman, Mubdi/0000-0003-1842-6096; Escoffier, Stephanie/0000-0002-2847-7498; Covey, Kevin/0000-0001-6914-7797; Davenport, James/0000-0002-0637-835X; Georgakakis, Antonis/0000-0002-3514-2442; Garcia, Rafael/0000-0002-8854-3776; Serenelli, Aldo/0000-0001-6359-2769; Chambers, Kenneth /0000-0001-6965-7789; Pepper, Joshua/0000-0002-3827-8417; Beaton, Rachael/0000-0002-1691-8217; Shane, Neville/0000-0003-1024-7739; Kirkby, David/0000-0002-8828-5463; Viel, Matteo/0000-0002-2642-5707; Schmidt, Sarah/0000-0002-7224-7702; Zhu, Guangtun/0000-0002-7574-8078; Beutler, Florian/0000-0003-0467-5438; Finley, Hayley/0000-0002-1216-8914; Cuesta Vazquez, Antonio Jose/0000-0002-4153-9470; Fleming, Scott/0000-0003-0556-027X; /0000-0002-1891-3794; Verde, Licia/0000-0003-2601-8770; Martig, Marie/0000-0001-5454-1492; McMahon, Richard/0000-0001-8447-8869; Hogg, David/0000-0003-2866-9403 NR 157 TC 340 Z9 341 U1 18 U2 53 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 EI 1538-4365 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD JUL PY 2015 VL 219 IS 1 AR 12 DI 10.1088/0067-0049/219/1/12 PG 27 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO0RE UT WOS:000358858900012 ER PT J AU Bull, P Wehus, IK Eriksen, HK Ferreira, PG Fuskeland, U Gorski, KM Jewell, JB AF Bull, Philip Wehus, Ingunn K. Eriksen, Hans Kristian Ferreira, Pedro G. Fuskeland, Unni Gorski, Krzysztof M. Jewell, Jeffrey B. TI A CMB GIBBS SAMPLER FOR LOCALIZED SECONDARY ANISOTROPIES SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE cosmic background radiation; galaxies: clusters: general; large-scale structure of universe ID INTEGRATED SACHS-WOLFE; SUNYAEV-ZELDOVICH CLUSTERS; POWER SPECTRUM ESTIMATION; GALAXY CLUSTERS; CATALOG; PROBE; MAPS; CONSTRAINTS; ALGORITHMS; PLANCK AB In addition to primary fluctuations, cosmic microwave background (CMB) temperature maps contain a wealth of additional information in the form of secondary anisotropies. However, secondary effects that can be identified with individual objects, such as the thermal and kinetic Sunyaev-Zel'dovich (TSZ-KSZ) effects due to galaxy clusters, are difficult to unambiguously disentangle from foreground contamination and the primary CMB. We develop a Bayesian formalism to rigorously characterize anisotropies that are localized on the sky, taking the TSZ and KSZ effects as an example. Using a Gibbs sampling scheme, we are able to efficiently sample from the joint posterior distribution for a multi-component model of the sky with many thousands of correlated physical parameters. The posterior can then be exactly marginalized to estimate the properties of the secondary anisotropies, fully taking into account degeneracies with the other signals in the CMB map. We show that this method is computationally tractable using a simple implementation based on the existing Commander component separation code and discuss how other types of secondary anisotropy can be accommodated within our framework. C1 [Bull, Philip; Eriksen, Hans Kristian; Fuskeland, Unni] Univ Oslo, Inst Theoret Astrophys, N-0315 Oslo, Norway. [Bull, Philip; Wehus, Ingunn K.; Ferreira, Pedro G.] Univ Oxford, Astrophys, DWB, Oxford OX1 3RH, England. [Wehus, Ingunn K.; Gorski, Krzysztof M.; Jewell, Jeffrey B.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Gorski, Krzysztof M.] Univ Warsaw Observ, PL-00478 Warsaw, Poland. RP Bull, P (reprint author), Univ Oslo, Inst Theoret Astrophys, POB 1029 Blindern, N-0315 Oslo, Norway. EM p.j.bull@astro.uio.no OI Bull, Philip/0000-0001-5668-3101 FU ERC [StG2010-257080, 259505]; STFC; Leverhulme; BIPAC; Oxford Martin School; NASA FX We are grateful to G. Addison, R. Battye, T. Louis, E. Macaulay, and M. Schammel for useful discussions, and to the anonymous referee for a number of suggestions that have substantially improved the paper. This project was supported by ERC Starting Grant StG2010-257080. P.B. acknowledges additional support from STFC, and hospitality from Caltech/JPL. I.K.W. acknowledges support from ERC grant 259505. P.G.F. acknowledges support from Leverhulme, STFC, BIPAC, and the Oxford Martin School. Part of the research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. Some of the results in this paper have been derived using the HEALPix software and analysis package (Gorski et al. 2005). NR 94 TC 3 Z9 3 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 EI 1538-4365 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD JUL PY 2015 VL 219 IS 1 AR 10 DI 10.1088/0067-0049/219/1/10 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO0RE UT WOS:000358858900010 ER PT J AU Ryer, CH Long, WC Spencer, ML Iseri, P AF Ryer, Clifford H. Long, William C. Spencer, Mara L. Iseri, Paul TI Depth distribution, habitat associations, and differential growth of newly settled southern Tanner crab (Chionoecetes bairdi) in embayments around Kodiak Island, Alaska SO FISHERY BULLETIN LA English DT Article ID RED KING CRAB; NORTHERN ROCK SOLE; PARALITHODES-CAMTSCHATICUS TILESIUS; JUVENILE BLUE-CRAB; EASTERN BERING-SEA; CALLINECTES-SAPIDUS; NURSERY GROUNDS; LEPIDOPSETTA-POLYXYSTRA; PREDATION RISK; CHESAPEAKE BAY AB We examined depth distribution, habitat association, and growth of newly settled southern Tanner crab (Chionoecetes bairdi) at 4 sites around the eastern end of Kodiak Island, Alaska, during 2010 and 2011. Settlement was from April through July, and crab density peaked during May July, at 10 crabs/m(2) in 2010 and 2.3 crabs/m(2) in 2011. By the end of August most crabs had progressed through 3-5 molt stages (instars). An association between crabs and tubes of the ampharetid polychaete Sabellides sibirica was observed in 2010, but it was not seen in 2011 when both crabs and worms were less abundant. Crabs in protected embayments were larger in August than crabs at open coastal sites. Crabs at protected sites were also found in shallower water than at open coastal sites a difference that may have exposed them to higher ambient water temperature and may have accelerated their growth. Accelerated growth may in turn result in earlier maturation. Southern Tanner crabs probably settle over a wide range of depths, but shallow embayments (depths <50 m) may play a disproportionately large role in providing recruits to the adult population, due to accelerated crab growth and survival. C1 [Ryer, Clifford H.; Spencer, Mara L.; Iseri, Paul] NOAA, Fisheries Behav Ecol Program, Alaska Fisheries Sci Ctr, Natl Marine Fisheries Serv, Newport, OR 97365 USA. [Long, William C.] NOAA, Shellfish Assessment Program, Alaska Fisheries Sci Ctr, Natl Marine Fisheries Serv, Kodiak, AK 99615 USA. RP Ryer, CH (reprint author), NOAA, Fisheries Behav Ecol Program, Alaska Fisheries Sci Ctr, Natl Marine Fisheries Serv, 2030 Marine Sci Dr, Newport, OR 97365 USA. EM cliff.ryer@noaa.gov RI Long, William/C-7074-2009 OI Long, William/0000-0002-7095-1245 FU Essential Fish Habitat funds from the NOAA Alaska Fisheries Science Center FX We thank M. Ottmar, S. Haines, and C. Sweitzer for assistance with logistics. R. Foy, E. Munk, P. Cummiski, and K. Swiney provided logistical support in Kodiak. We also wish to thank the captain of the FV Miss-O, T. Tripp, for valuable assistance on the water. Two anonymous reviewers provided helpful comments on an early draft of this manuscript. This work was supported by 2010 and 2011 Essential Fish Habitat funds from the NOAA Alaska Fisheries Science Center. NR 47 TC 1 Z9 1 U1 1 U2 10 PU NATL MARINE FISHERIES SERVICE SCIENTIFIC PUBL OFFICE PI SEATTLE PA 7600 SAND POINT WAY NE BIN C15700, SEATTLE, WA 98115 USA SN 0090-0656 EI 1937-4518 J9 FISH B-NOAA JI Fish. Bull. PD JUL PY 2015 VL 113 IS 3 BP 256 EP 269 DI 10.7755/FB.113.3.3 PG 14 WC Fisheries SC Fisheries GA CO3XZ UT WOS:000359095900003 ER PT J AU Spangelo, S Longmier, B AF Spangelo, Sara Longmier, Benjamin TI Optimization of CubeSat System-Level Design and Propulsion Systems for Earth-Escape Missions SO JOURNAL OF SPACECRAFT AND ROCKETS LA English DT Article ID SOLAR ELECTRIC PROPULSION AB Small spacecraft can now perform trajectory maneuvers resulting in significant orbit changes that were once only feasible with larger spacecraft due to the development of miniaturized propulsion technology. This paper addresses the feasibility of using CubeSat Ambipolar Thruster, a large Delta V miniaturized propulsion system for constellation control, Earth escape, and planetary flybys, to enable Earth-escape maneuvers on a CubeSat form factor. Operational and trajectory variables include the power setting during thrust maneuvers, when to thrust, and the attitude control inputs. The dynamic energy available through the maneuvers, which is constrained by the power available from the sun depending on the orbit and is consumed in propulsion, is modeled as well as attitude control maneuvers and realistic battery degradation. To explore the design space of this capability, the sensitivity of solutions to spacecraft mass, fuel quantity, initial orbit, solar power collection, and battery size is demonstrated. Optimal orbit-raising techniques are compared and the optimal approach depending on the goals is discussed (i.e., minimize time, minimize fuel, minimize batteries, minimize propulsion system volume, and minimize accumulated radiation). The models and results presented lay the groundwork for future work in integrated vehicle and operational design optimization problems with both interplanetary and constellation architectures. C1 [Spangelo, Sara] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Longmier, Benjamin] Univ Michigan, Aerosp Engn, Ann Arbor, MI 48109 USA. RP Spangelo, S (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. FU NASA [NNX13AR18A] FX The authors acknowledge support by NASA cooperative agreement NNX13AR18A. Part of the research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. NR 45 TC 1 Z9 2 U1 5 U2 19 PU AMER INST AERONAUTICS ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0022-4650 EI 1533-6794 J9 J SPACECRAFT ROCKETS JI J. Spacecr. Rockets PD JUL PY 2015 VL 52 IS 4 BP 1009 EP 1020 DI 10.2514/1.A33136 PG 12 WC Engineering, Aerospace SC Engineering GA CO4VH UT WOS:000359158400001 ER PT J AU Fieseler, P Anderson, KR Cable, V AF Fieseler, Paul Anderson, Kevin R. Cable, Vaughn TI Critical Look at the Solar Photon Thruster Concept SO JOURNAL OF SPACECRAFT AND ROCKETS LA English DT Article ID OPTICAL-PROPERTIES; THERMAL-STABILITY; SILVER; SAIL; SPACECRAFT; MIRRORS; FILMS AB A solar photon thruster is a class of solar sail using multiple reflecting surfaces. Herein, the details of solar photon thruster design are investigated to allow comparison against more typical solar sail configurations. Many potential problems with the solar photon thruster concept have been sidestepped in the literature. Therefore, issues relevant to solar photon thruster operation were investigated, such as the following questions: 1) What are the realistic thrust levels and performance that such a vehicle might experience? 2) Do lightweight materials capable of handling the high heat fluxes, where the light is concentrated and reflected, exist? 3) How significant are the reflection losses due to having multiple reflective surfaces? 4) Can a large flexible mirror really focus the light sufficiently well to allow the solar photon thruster concept to work? It is found that any solar photon thruster will have a significantly inferior performance to a similarly sized flat solar sail. The maximum reflectivity of the surfaces typically used by solar sails and solar photon thrusters is determined; it is also found that the thermal issues of concentrating sunlight to a small focus are difficult but manageable and that using a large flexible metallized plastic surface as the main light-collecting surface, although suitable for a normal solar sail, is an extreme challenge for the solar photon thruster concept. C1 [Fieseler, Paul] CALTECH, Jet Prop Lab, Flight Engn, Pasadena, CA 91109 USA. [Anderson, Kevin R.] CALTECH, Jet Prop Lab, Thermal Technol & Fluids, Pasadena, CA 91109 USA. [Cable, Vaughn] CALTECH, Jet Prop Lab, Comm Syst & Operat, Pasadena, CA 91109 USA. RP Fieseler, P (reprint author), CALTECH, Jet Prop Lab, Flight Engn, MS 264-828,4800 Oak Grove Dr, Pasadena, CA 91109 USA. FU Jet Propulsion Laboratory, California Institute of Technology; NASA FX This work was carried out under a Division Technologist Discretionary Task award from the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. NR 38 TC 0 Z9 0 U1 2 U2 7 PU AMER INST AERONAUTICS ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0022-4650 EI 1533-6794 J9 J SPACECRAFT ROCKETS JI J. Spacecr. Rockets PD JUL PY 2015 VL 52 IS 4 BP 1152 EP 1162 DI 10.2514/1.A33249 PG 11 WC Engineering, Aerospace SC Engineering GA CO4VH UT WOS:000359158400012 ER PT J AU Mahzari, M Braun, RD White, TR Bose, D AF Mahzari, Milad Braun, Robert D. White, Todd R. Bose, Deepak TI Inverse Estimation of the Mars Science Laboratory Entry Aeroheating and Heatshield Response SO JOURNAL OF SPACECRAFT AND ROCKETS LA English DT Article ID ABLATION AB The Mars Science Laboratory entry vehicle successfully landed the Curiosity rover on the Martian surface on 5 August 2012. A phenolic impregnated carbon ablator heatshield was used to protect the spacecraft against the severe aeroheating environments of atmospheric entry. This heatshield was instrumented with a comprehensive set of pressure and temperature sensors. The objective of this paper is to perform an inverse estimation of the entry vehicle's surface heating and heatshield material properties. The surface heating is estimated using the flight temperature data from the shallowest thermocouple. The sensitivity of the estimated surface heating profile to estimation tuning parameters, measurement errors, recession uncertainty, and material property uncertainty is investigated. A Monte Carlo analysis is conducted to quantify the uncertainty bounds associated with the nominal estimated surface heating. Additionally, a thermocouple driver approach is employed to estimate heatshield material properties using the flight data from the deeper thermocouples while applying the shallowest thermocouple temperature as the surface boundary condition. C1 [Mahzari, Milad] Georgia Inst Technol, Guggenheim Sch Aerosp Engn, Atlanta, GA 30332 USA. [Braun, Robert D.] Georgia Inst Technol, Daniel Guggenheim Sch Aerosp Engn, Space Technol, Atlanta, GA 30332 USA. [White, Todd R.] ERC Inc, Aerothermodynam Branch, Moffett Field, CA 94035 USA. [Bose, Deepak] NASA, Ames Res Ctr, Aerothermodynam Branch, Moffett Field, CA 94035 USA. RP Mahzari, M (reprint author), Georgia Inst Technol, Guggenheim Sch Aerosp Engn, Atlanta, GA 30332 USA. FU NASA grant from the NASA Research Announcement Research Opportunities in Aeronautics [NNX12AF94A]; NASA [NNA10DE12C] FX This work was funded by NASA grant NNX12AF94A from the NASA Research Announcement Research Opportunities in Aeronautics 2010. Portions of this work were conducted under the NASA contract NNA10DE12C to ERC, Inc. The authors are grateful to Karl Edquist, Jay Feldman, Jose Santos, Michael Wright, Soumyo Dutta, David Saunders, and Bernie Laub for their time in discussing some aspects of this work. NR 37 TC 2 Z9 2 U1 2 U2 3 PU AMER INST AERONAUTICS ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0022-4650 EI 1533-6794 J9 J SPACECRAFT ROCKETS JI J. Spacecr. Rockets PD JUL PY 2015 VL 52 IS 4 BP 1203 EP 1216 DI 10.2514/1.A33053 PG 14 WC Engineering, Aerospace SC Engineering GA CO4VH UT WOS:000359158400017 ER PT J AU Perino, SV Bayandor, J Samareh, JA Armand, SC AF Perino, Scott V. Bayandor, Javid Samareh, Jamshid A. Armand, Sasan C. TI Contemporary Impact Analysis Methodology for Planetary Sample Return Missions SO JOURNAL OF SPACECRAFT AND ROCKETS LA English DT Article ID EARTH; METAL AB Development of an Earth entry vehicle and the methodology created to evaluate the vehicle's impact landing response when returning to Earth is reported. NASA's future Mars Sample Return Mission requires a robust vehicle to return Martian samples back to Earth for analysis. The Earth entry vehicle is a proposed solution to this Mars mission requirement. During Earth reentry, the vehicle slows within the atmosphere and then impacts the ground at its terminal velocity. To protect the Martian samples, a spherical energy absorber called an impact sphere is under development. The impact sphere is composed of hybrid composite and crushable foam elements that endure large plastic deformations during impact and cause a highly nonlinear vehicle response. The developed analysis methodology captures a range of complex structural interactions and much of the failure physics that occurs during impact. Numerical models were created and benchmarked against experimental tests conducted at NASA Langley Research Center. The postimpact structural damage assessment showed close correlation between simulation predictions and experimental results. Acceleration, velocity, displacement, damage modes, and failure mechanisms were all effectively captured. These investigations demonstrate that the Earth entry vehicle has great potential in facilitating future sample return missions. C1 [Perino, Scott V.; Bayandor, Javid] Virginia Polytech Inst & State Univ, Dept Mech Engn, Crashworthiness Aerosp Struct & Hybrids Lab, Blacksburg, VA 24061 USA. [Samareh, Jamshid A.] NASA, Langley Res Ctr, Vehicle Anal Branch, Hampton, VA 23681 USA. [Armand, Sasan C.] NASA, Langley Res Ctr, Struct & Thermal Syst Branch, Hampton, VA 23681 USA. RP Perino, SV (reprint author), Virginia Polytech Inst & State Univ, Dept Mech Engn, Crashworthiness Aerosp Struct & Hybrids Lab, Blacksburg, VA 24061 USA. FU NASA In-Space Propulsion Technology program FX This project was funded by the NASA In-Space Propulsion Technology program. The authors would like to acknowledge, Bo Walkley of the National Institute of Aerospace and Aaron Horning of Analytical Mechanics Associates, Inc., for their extensive support and collaborative assistance on this project. NR 27 TC 1 Z9 1 U1 0 U2 4 PU AMER INST AERONAUTICS ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0022-4650 EI 1533-6794 J9 J SPACECRAFT ROCKETS JI J. Spacecr. Rockets PD JUL PY 2015 VL 52 IS 4 BP 1217 EP 1227 DI 10.2514/1.A33033 PG 11 WC Engineering, Aerospace SC Engineering GA CO4VH UT WOS:000359158400018 ER PT J AU Rathsam, J Loubeau, A Klos, J AF Rathsam, Jonathan Loubeau, Alexandra Klos, Jacob TI Effects of indoor rattle sounds on annoyance caused by sonic booms SO JOURNAL OF THE ACOUSTICAL SOCIETY OF AMERICA LA English DT Article ID PEOPLE AB To expand national air transportation capabilities, NASA's Commercial Supersonic Technology Project is working to make supersonic flight practical for commercial passengers. As an aid in designing and certifying quiet supersonic aircraft, a noise metric is sought that will correspond to indoor annoyance caused by sonic booms, including the effects of indoor rattle sounds. This study examines how well several common aircraft noise metrics predict indoor annoyance based on the indoor and outdoor sound fields. The results suggest notional community annoyance models that include the effects of indoor rattle sounds. C1 [Rathsam, Jonathan; Loubeau, Alexandra; Klos, Jacob] NASA Langley Res Ctr, Struct Acoust Branch, Hampton, VA 23681 USA. RP Rathsam, J (reprint author), NASA Langley Res Ctr, Struct Acoust Branch, Hampton, VA 23681 USA. EM jonathan.rathsam@nasa.gov; a.loubeau@nasa.gov; j.klos@nasa.gov FU NASA's Commercial Supersonic Technology Project FX This work was supported by NASA's Commercial Supersonic Technology Project. Kevin Shepherd provided guidance throughout the research effort. Regina Johns recruited test subjects and performed audiograms. In addition, Aric Aumann maintained and improved the software controlling the simulator. NR 12 TC 0 Z9 0 U1 2 U2 5 PU ACOUSTICAL SOC AMER AMER INST PHYSICS PI MELVILLE PA STE 1 NO 1, 2 HUNTINGTON QUADRANGLE, MELVILLE, NY 11747-4502 USA SN 0001-4966 EI 1520-8524 J9 J ACOUST SOC AM JI J. Acoust. Soc. Am. PD JUL PY 2015 VL 138 IS 1 BP EL43 EP EL48 DI 10.1121/1.4922535 PG 6 WC Acoustics; Audiology & Speech-Language Pathology SC Acoustics; Audiology & Speech-Language Pathology GA CO1QB UT WOS:000358929000008 PM 26233059 ER PT J AU Andersson, SM Martinsson, BG Vernier, JP Friberg, J Brenninkmeijer, CAM Hermann, M van Velthoven, PFJ Zahn, A AF Andersson, Sandra M. Martinsson, Bengt G. Vernier, Jean-Paul Friberg, Johan Brenninkmeijer, Carl A. M. Hermann, Markus van Velthoven, Peter F. J. Zahn, Andreas TI Significant radiative impact of volcanic aerosol in the lowermost stratosphere SO NATURE COMMUNICATIONS LA English DT Article ID GLOBAL CLIMATE-CHANGE; SULFUR-DIOXIDE; OPTICAL DEPTHS; INSTRUMENT; ERUPTIONS; CLOUDS; SYSTEM; LAYER; SIZE; TROPOPAUSE AB Despite their potential to slow global warming, until recently, the radiative forcing associated with volcanic aerosols in the lowermost stratosphere (LMS) had not been considered. Here we study volcanic aerosol changes in the stratosphere using lidar measurements from the NASA CALIPSO satellite and aircraft measurements from the IAGOS-CARIBIC observatory. Between 2008 and 2012 volcanism frequently affected the Northern Hemisphere stratosphere aerosol loadings, whereas the Southern Hemisphere generally had loadings close to background conditions. We show that half of the global stratospheric aerosol optical depth following the Kasatochi, Sarychev and Nabro eruptions is attributable to LMS aerosol. On average, 30% of the global stratospheric aerosol optical depth originated in the LMS during the period 2008-2011. On the basis of the two independent, high-resolution measurement methods, we show that the LMS makes an important contribution to the overall volcanic forcing. C1 [Andersson, Sandra M.; Martinsson, Bengt G.; Friberg, Johan] Lund Univ, Dept Phys, S-22100 Lund, Sweden. [Vernier, Jean-Paul] Sci Syst & Applicat Inc, Hampton, VA 23666 USA. [Vernier, Jean-Paul] NASA, Langley Res Ctr, Hampton, VA 23681 USA. [Brenninkmeijer, Carl A. M.] Max Planck Inst Chem, Dept Atmospher Chem, D-55128 Mainz, Germany. [Hermann, Markus] Leibniz Inst Tropospher Res, Dept Expt Aerosol & Cloud Microphys, D-04318 Leipzig, Germany. [van Velthoven, Peter F. J.] Climate Res, Royal Netherlands Meteorol Div Chem & Climate, NL-3730 AE De Bilt, Netherlands. [Zahn, Andreas] KIT, Inst Meteorol & Climate Res, Atmospher Trace Gases & Remote Sensing, D-76021 Karlsruhe, Germany. RP Martinsson, BG (reprint author), Lund Univ, Dept Phys, POB 118, S-22100 Lund, Sweden. EM bengt.martinsson@nuclear.lu.se RI Zahn, Andreas/K-2567-2012; Hermann, Markus/B-7527-2013 OI Zahn, Andreas/0000-0003-3153-3451; Hermann, Markus/0000-0002-5124-1571 FU German Federal Ministry of Education and Research (BMBF); German Research Foundation (DFG) [1,294]; Frankfurt Airport AG FX We acknowledge all members of the CARIBIC project and Lufthansa and Lufthansa Technik for enabling the CARIBIC observatory. We also thank Andre Ahlgren for support with programming. Aerosol measurements from CALIPSO were produced by NASA Langley Research Center. We thank the German Federal Ministry of Education and Research (BMBF) for financing the instruments operation as part of the Joint Project IAGOS-D. We also thank the German Research Foundation (DFG) for their financial support of the data analysis within the Priority Programme 1,294 (HALO). Financial support from Frankfurt Airport AG is gratefully acknowledged. NR 56 TC 11 Z9 12 U1 6 U2 30 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 2041-1723 J9 NAT COMMUN JI Nat. Commun. PD JUL PY 2015 VL 6 AR 7692 DI 10.1038/ncomms8692 PG 8 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CO0QW UT WOS:000358858100036 PM 26158244 ER PT J AU Khazanov, GV Sibeck, DG Tel'nikhin, AA Kronberg, TK AF Khazanov, G. V. Sibeck, D. G. Tel'nikhin, A. A. Kronberg, T. K. TI Stochastic acceleration of ions driven by Pc1 wave packets SO PHYSICS OF PLASMAS LA English DT Article ID VAN ALLEN PROBES; CYCLOTRON WAVES; PEARL PULSATIONS; ALFVEN WAVES; PC-1 WAVES; MAGNETOSPHERE; DISTRIBUTIONS AB The stochastic motion of protons and He+ ions driven by Pc1 wave packets is studied in the context of resonant particle heating. Resonant ion cyclotron heating typically occurs when wave powers exceed 10(-4) nT(2)/Hz. Gyroresonance breaks the first adiabatic invariant and energizes keV ions. Cherenkov resonances with the electrostatic component of wave packets can also accelerate ions. The main effect of this interaction is to accelerate thermal protons to the local Alfven speed. The dependencies of observable quantities on the wave power and plasma parameters are determined, and estimates for the heating extent and rate of particle heating in these wave-particle interactions are shown to be in reasonable agreement with known empirical data. (C) 2015 AIP Publishing LLC. C1 [Khazanov, G. V.; Sibeck, D. G.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Tel'nikhin, A. A.; Kronberg, T. K.] Altai State Univ, Dept Phys & Technol, Barnaul 656099, Russia. RP Khazanov, GV (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM george.v.khazanov@nasa.gov FU National Aeronautics and Space Administration SMD/Heliophysics Supporting Research; Living With a Star programs for Geospace SRT; NASA Van Allen Probes FX This material is based upon work supported by the National Aeronautics and Space Administration SMD/Heliophysics Supporting Research, Living With a Star programs for Geospace SR&T, and NASA Van Allen Probes (formerly known as the Radiation Belt Storm Probes (RBSP)). NR 30 TC 1 Z9 1 U1 0 U2 2 PU AMER INST PHYSICS PI MELVILLE PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA SN 1070-664X EI 1089-7674 J9 PHYS PLASMAS JI Phys. Plasmas PD JUL PY 2015 VL 22 IS 7 AR 072901 DI 10.1063/1.4926823 PG 8 WC Physics, Fluids & Plasmas SC Physics GA CO1RT UT WOS:000358933600046 ER PT J AU Aartsen, MG Ackermann, M Adams, J Aguilar, JA Ahlers, M Ahrens, M Altmann, D Anderson, T Archinger, M Arguelles, C Arlen, TC Auffenberg, J Bai, X Barwick, SW Baum, V Bay, R Baker, M Beatty, JJ Tjus, JB Becker, KH BenZvi, S Berghaus, P Berley, D Bernardini, E Bernhard, A Besson, DZ Binder, G Bindig, D Bissok, M Blaufuss, E Blumenthal, J Boersma, DJ Bohm, C Bos, F Bose, D Boser, S Botner, O Brayeur, L Bretz, HP Brown, AM Buzinsky, N Casey, J Casier, M Cheung, E Chirkin, D Christov, A Christy, B Clark, K Classen, L Clevermann, F Coenders, S Cowen, DF Silva, AHC Daughhetee, J Davis, JC Day, M de Andre, JPAM De Clercq, C Dembinski, H De Ridder, S Desiati, P de Vries, KD de Wasseige, G de With, M DeYoung, T Diaz-Velez, JC Dumm, JP Dunkman, M Eagan, R Eberhardt, B Ehrhardt, T Eichmann, B Eisch, J Euler, S Evenson, PA Fadiran, O Fazely, AR Fedynitch, A Feintzeig, J Felde, J Filimonov, K Finley, C Fischer-Wasels, T Flis, S Frantzen, K Fuchs, T Gaisser, TK Gaior, R Gallagher, J Gerhardt, L Gier, D Gladstone, L Glusenkamp, T Goldschmidt, A Golup, G Gonzalez, JG Goodman, JA Gora, D Grant, D Gretskov, P Groh, JC Gross, A Ha, C Haack, C Ismail, AH Hallen, P Hallgren, A Halzen, F Hanson, K Hebecker, D Heereman, D Heinen, D Helbing, K Hellauer, R Hellwig, D Hickford, S Hignight, J Hill, GC Hoffman, KD Hoffmann, R Homeier, A Hoshina, K Huang, F Huelsnitz, W Hulth, PO Hultqvist, K In, S Ishihara, A Jacobi, E Jacobsen, J Japaridze, GS Jero, K Jurkovic, M Kaminsky, B Kappes, A Karg, T Karle, A Kauer, M Keivani, A Kelley, JL Kheirandish, A Kiryluk, J Klas, J Klein, SR Kohne, JH Kohnen, G Kolanoski, H Koob, A Kopke, L Kopper, C Kopper, S Koskinen, DJ Kowalski, M Krings, K Kroll, G Kroll, M Kunnen, J Kurahashi, N Kuwabara, T Labare, M Lanfranchi, JL Larsen, DT Larson, MJ Lesiak-Bzdak, M Leuermann, M Lunemann, J Madsen, J Maggi, G Mahn, KBM Maruyama, R Mase, K Matis, HS Maunu, R McNally, F Meagher, K Medici, M Meli, A Meures, T Miarecki, S Middell, E Middlemas, E Milke, N Miller, J Mohrmann, L Montaruli, T Morse, R Nahnhauer, R Naumann, U Niederhausen, H Nowicki, SC Nygren, DR Obertacke, A Olivas, A Omairat, A O'Murchadha, A Palczewski, T Paul, L Pepper, JA de los Heros, CP Pfendner, C Pieloth, D Pinat, E Posselt, J Price, PB Przybylski, GT Putz, J Quinnan, M Radel, L Rameez, M Rawlins, K Redl, P Rees, I Reimann, R Relich, M Resconi, E Rhode, W Richman, M Riedel, B Robertson, S Rodrigues, JP Rongen, M Rott, C Ruhe, T Ruzybayev, B Ryckbosch, D Saba, SM Sander, HG Sandroos, J Santander, M Sarkar, S Schatto, K Scheriau, F Schmidt, T Schmitz, M Schoenen, S Schoneberg, S Schonwald, A Schukraft, A Schulte, L Schulz, O Seckel, D Sestayo, Y Seunarine, S Shanidze, R Smith, MWE Soldin, D Spiczak, GM Spiering, C Stamatikos, M Stanev, T Stanisha, NA Stasik, A Stezelberger, T Stokstad, RG Stossl, A Strahler, EA Strom, R Strotjohann, NL Sullivan, GW Sutherland, M Taavola, H Taboada, I Tamburro, A Ter-Antonyan, S Terliuk, A Tesic, G Tilav, S Toale, PA Tobin, MN Tosi, D Tselengidou, M Unger, E Usner, M Vallecorsa, S van Eijndhoven, N Vandenbroucke, J van Santen, J Vanheule, S Vehring, M Voge, M Vraeghe, M Walck, C Wallraff, M Weaver, C Wellons, M Wendt, C Westerhoff, S Whelan, BJ Whitehorn, N Wichary, C Wiebe, K Wiebusch, CH Williams, DR Wissing, H Wolf, M Wood, TR Woschnagg, K Xu, DL Xu, XW Xu, Y Yanez, JP Yodh, G Yoshida, S Zarzhitsky, P Ziemann, J Zoll, M AF Aartsen, M. G. Ackermann, M. Adams, J. Aguilar, J. A. Ahlers, M. Ahrens, M. Altmann, D. Anderson, T. Archinger, M. Arguelles, C. Arlen, T. C. Auffenberg, J. Bai, X. Barwick, S. W. Baum, V. Bay, R. Baker, M. Beatty, J. J. Tjus, J. Becker Becker, K. -H. BenZvi, S. Berghaus, P. Berley, D. Bernardini, E. Bernhard, A. Besson, D. Z. Binder, G. Bindig, D. Bissok, M. Blaufuss, E. Blumenthal, J. Boersma, D. J. Bohm, C. Bos, F. Bose, D. Boeser, S. Botner, O. Brayeur, L. Bretz, H. -P. Brown, A. M. Buzinsky, N. Casey, J. Casier, M. Cheung, E. Chirkin, D. Christov, A. Christy, B. Clark, K. Classen, L. Clevermann, F. Coenders, S. Cowen, D. F. Silva, A. H. Cruz Daughhetee, J. Davis, J. C. Day, M. de Andre, J. P. A. M. De Clercq, C. Dembinski, H. De Ridder, S. Desiati, P. de Vries, K. D. de Wasseige, G. de With, M. DeYoung, T. Diaz-Velez, J. C. Dumm, J. P. Dunkman, M. Eagan, R. Eberhardt, B. Ehrhardt, T. Eichmann, B. Eisch, J. Euler, S. Evenson, P. A. Fadiran, O. Fazely, A. R. Fedynitch, A. Feintzeig, J. Felde, J. Filimonov, K. Finley, C. Fischer-Wasels, T. Flis, S. Frantzen, K. Fuchs, T. Gaisser, T. K. Gaior, R. Gallagher, J. Gerhardt, L. Gier, D. Gladstone, L. Gluesenkamp, T. Goldschmidt, A. Golup, G. Gonzalez, J. G. Goodman, J. A. Gora, D. Grant, D. Gretskov, P. Groh, J. C. Gross, A. Ha, C. Haack, C. Ismail, A. Haj Hallen, P. Hallgren, A. Halzen, F. Hanson, K. Hebecker, D. Heereman, D. Heinen, D. Helbing, K. Hellauer, R. Hellwig, D. Hickford, S. Hignight, J. Hill, G. C. Hoffman, K. D. Hoffmann, R. Homeier, A. Hoshina, K. Huang, F. Huelsnitz, W. Hulth, P. O. Hultqvist, K. In, S. Ishihara, A. Jacobi, E. Jacobsen, J. Japaridze, G. S. Jero, K. Jurkovic, M. Kaminsky, B. Kappes, A. Karg, T. Karle, A. Kauer, M. Keivani, A. Kelley, J. L. Kheirandish, A. Kiryluk, J. Klaes, J. Klein, S. R. Koehne, J. -H. Kohnen, G. Kolanoski, H. Koob, A. Koepke, L. Kopper, C. Kopper, S. Koskinen, D. J. Kowalski, M. Krings, K. Kroll, G. Kroll, M. Kunnen, J. Kurahashi, N. Kuwabara, T. Labare, M. Lanfranchi, J. L. Larsen, D. T. Larson, M. J. Lesiak-Bzdak, M. Leuermann, M. Luenemann, J. Madsen, J. Maggi, G. Mahn, K. B. M. Maruyama, R. Mase, K. Matis, H. S. Maunu, R. McNally, F. Meagher, K. Medici, M. Meli, A. Meures, T. Miarecki, S. Middell, E. Middlemas, E. Milke, N. Miller, J. Mohrmann, L. Montaruli, T. Morse, R. Nahnhauer, R. Naumann, U. Niederhausen, H. Nowicki, S. C. Nygren, D. R. Obertacke, A. Olivas, A. Omairat, A. O'Murchadha, A. Palczewski, T. Paul, L. Pepper, J. A. de los Heros, C. Perez Pfendner, C. Pieloth, D. Pinat, E. Posselt, J. Price, P. B. Przybylski, G. T. Puetz, J. Quinnan, M. Raedel, L. Rameez, M. Rawlins, K. Redl, P. Rees, I. Reimann, R. Relich, M. Resconi, E. Rhode, W. Richman, M. Riedel, B. Robertson, S. Rodrigues, J. P. Rongen, M. Rott, C. Ruhe, T. Ruzybayev, B. Ryckbosch, D. Saba, S. M. Sander, H. -G. Sandroos, J. Santander, M. Sarkar, S. Schatto, K. Scheriau, F. Schmidt, T. Schmitz, M. Schoenen, S. Schoeneberg, S. Schoenwald, A. Schukraft, A. Schulte, L. Schulz, O. Seckel, D. Sestayo, Y. Seunarine, S. Shanidze, R. Smith, M. W. E. Soldin, D. Spiczak, G. M. Spiering, C. Stamatikos, M. Stanev, T. Stanisha, N. A. Stasik, A. Stezelberger, T. Stokstad, R. G. Stoessl, A. Strahler, E. A. Strom, R. Strotjohann, N. L. Sullivan, G. W. Sutherland, M. Taavola, H. Taboada, I. Tamburro, A. Ter-Antonyan, S. Terliuk, A. Tesic, G. Tilav, S. Toale, P. A. Tobin, M. N. Tosi, D. Tselengidou, M. Unger, E. Usner, M. Vallecorsa, S. van Eijndhoven, N. Vandenbroucke, J. van Santen, J. Vanheule, S. Vehring, M. Voge, M. Vraeghe, M. Walck, C. Wallraff, M. Weaver, Ch. Wellons, M. Wendt, C. Westerhoff, S. Whelan, B. J. Whitehorn, N. Wichary, C. Wiebe, K. Wiebusch, C. H. Williams, D. R. Wissing, H. Wolf, M. Wood, T. R. Woschnagg, K. Xu, D. L. Xu, X. W. Xu, Y. Yanez, J. P. Yodh, G. Yoshida, S. Zarzhitsky, P. Ziemann, J. Zoll, M. CA IceCube Collaboration TI SEARCHES FOR TIME-DEPENDENT NEUTRINO SOURCES WITH ICECUBE DATA FROM 2008 TO 2012 SO ASTROPHYSICAL JOURNAL LA English DT Article DE astroparticle physics; binaries: general; BL Lacertae objects: general; galaxies: active; neutrinos; X-rays: binaries ID GAMMA-RAY EMISSION; ACTIVE GALACTIC NUCLEI; LS I+61-DEGREES-303; PROTON BLAZAR; LAC OBJECTS; COSMIC-RAYS; ACCELERATION; TEV; MODEL; 1ES-1959+650 AB In this paper searches for flaring astrophysical neutrino sources and sources with periodic emission with the IceCube neutrino telescope are presented. In contrast to time-integrated searches, where steady emission is assumed, the analyses presented here look for a time-dependent signal of neutrinos using the information from the neutrino arrival times to enhance the discovery potential. A search was performed for correlations between neutrino arrival times and directions, as well as neutrino emission following time-dependent light curves, sporadic emission, or periodicities of candidate sources. These include active galactic nuclei, soft gamma-ray repeaters, supernova remnants hosting pulsars, microquasars, and X-ray binaries. The work presented here updates and extends previously published results to a longer period that covers 4 years. of data from 2008 April 5 to 2012 May 16, including the first year of operation of the completed 86 string detector. The analyses did not find any significant time-dependent point sources of neutrinos, and the results were used to set upper limits on the neutrino flux from source candidates. C1 [Aartsen, M. G.; Hill, G. C.; Robertson, S.; Whelan, B. J.] Univ Adelaide, Sch Chem & Phys, Adelaide, SA 5005, Australia. [Ackermann, M.; Berghaus, P.; Bernardini, E.; Bretz, H. -P.; Silva, A. H. Cruz; Gluesenkamp, T.; Gora, D.; Jacobi, E.; Kaminsky, B.; Karg, T.; Kowalski, M.; Middell, E.; Mohrmann, L.; Nahnhauer, R.; Schoenwald, A.; Shanidze, R.; Spiering, C.; Stasik, A.; Stoessl, A.; Strotjohann, N. L.; Terliuk, A.; Usner, M.; Yanez, J. P.] DESY, D-15735 Zeuthen, Germany. [Adams, J.; Brown, A. M.] Univ Canterbury, Dept Phys & Astron, Christchurch 1, New Zealand. [Aguilar, J. A.; Hanson, K.; Heereman, D.; Meures, T.; O'Murchadha, A.; Pinat, E.] Univ Libre Bruxelles, Fac Sci, B-1050 Brussels, Belgium. [Ahlers, M.; Arguelles, C.; Baker, M.; BenZvi, S.; Chirkin, D.; Day, M.; Desiati, P.; Diaz-Velez, J. C.; Eisch, J.; Fadiran, O.; Feintzeig, J.; Gladstone, L.; Halzen, F.; Hoshina, K.; Jacobsen, J.; Jero, K.; Karle, A.; Kauer, M.; Kelley, J. L.; Kheirandish, A.; Larsen, D. T.; McNally, F.; Middlemas, E.; Morse, R.; Rees, I.; Rodrigues, J. P.; Santander, M.; Tobin, M. 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[Auffenberg, J.; Bissok, M.; Blumenthal, J.; Christov, A.; Gier, D.; Gretskov, P.; Haack, C.; Hallen, P.; Heinen, D.; Hellwig, D.; Keivani, A.; Koob, A.; Leuermann, M.; Paul, L.; Puetz, J.; Raedel, L.; Reimann, R.; Rongen, M.; Schoenen, S.; Schukraft, A.; Vehring, M.; Wallraff, M.; Wichary, C.; Wiebusch, C. H.] Rhein Westfal TH Aachen, Inst Phys, D-52056 Aachen, Germany. [Bai, X.] South Dakota Sch Mines & Technol, Dept Phys, Rapid City, SD 57701 USA. [Barwick, S. W.; Yodh, G.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. [Bay, R.; Binder, G.; Filimonov, K.; Gerhardt, L.; Ha, C.; Klein, S. R.; Miarecki, S.; Price, P. B.; Woschnagg, K.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Beatty, J. J.; Davis, J. C.; Pfendner, C.; Stamatikos, M.; Sutherland, M.] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA. [Beatty, J. J.; Christov, A.; Davis, J. C.; Pfendner, C.; Stamatikos, M.; Sutherland, M.] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA. [Beatty, J. J.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Tjus, J. Becker; Bos, F.; Eichmann, B.; Fedynitch, A.; Kroll, M.; Saba, S. M.; Schoeneberg, S.] Ruhr Univ Bochum, Fak Phys & Astron, D-44780 Bochum, Germany. [Becker, K. -H.; Bindig, D.; Christov, A.; Fischer-Wasels, T.; Helbing, K.; Hickford, S.; Hoffmann, R.; Klaes, J.; Kopper, S.; Naumann, U.; Obertacke, A.; Omairat, A.; Posselt, J.; Soldin, D.] Univ Gesamthsch Wuppertal, Dept Phys, D-42119 Wuppertal, Germany. [Berley, D.; Blaufuss, E.; Cheung, E.; Christov, A.; Christy, B.; Felde, J.; Goodman, J. A.; Hellauer, R.; Hoffman, K. D.; Huelsnitz, W.; Keivani, A.; Maunu, R.; Meagher, K.; Olivas, A.; Redl, P.; Richman, M.; Schmidt, T.; Sullivan, G. W.; Wissing, H.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA. [Bernhard, A.; Christov, A.; Coenders, S.; Gross, A.; Jurkovic, M.; Keivani, A.; Krings, K.; Olivas, A.; Resconi, E.; Schulz, O.; Sestayo, Y.] Tech Univ Munich, D-85748 Garching, Germany. [Besson, D. Z.] Univ Kansas, Dept Phys & Astron, Lawrence, KS 66045 USA. [Binder, G.; Gerhardt, L.; Goldschmidt, A.; Ha, C.; Klein, S. R.; Matis, H. S.; Miarecki, S.; Nygren, D. R.; Przybylski, G. T.; Stezelberger, T.; Stokstad, R. G.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. [Boersma, D. J.; Botner, O.; Euler, S.; Hallgren, A.; Strom, R.; Taavola, H.; Unger, E.] Uppsala Univ, Dept Phys & Astron, S-75120 Uppsala, Sweden. [Bose, D.; In, S.; Rott, C.] Sungkyunkwan Univ, Dept Phys, Suwon 440746, South Korea. [Brayeur, L.; Casier, M.; De Clercq, C.; de Vries, K. D.; de Wasseige, G.; Golup, G.; Kunnen, J.; Maggi, G.; Miller, J.; Strahler, E. A.; van Eijndhoven, N.] Vrije Univ Brussel, Dienst ELEM, B-1050 Brussels, Belgium. [Buzinsky, N.; Grant, D.; Kopper, C.; Nowicki, S. C.; Riedel, B.; Wood, T. R.] Univ Alberta, Dept Phys, Edmonton, AB T6G 2E1, Canada. [Casey, J.; Daughhetee, J.; Taboada, I.] Georgia Inst Technol, Sch Phys, Atlanta, GA 30332 USA. [Casey, J.; Daughhetee, J.; Taboada, I.] Georgia Inst Technol, Ctr Relativist Astrophys, Atlanta, GA 30332 USA. [Christov, A.; Montaruli, T.; Rameez, M.; Vallecorsa, S.] Univ Geneva, Dept Phys Nucl & Corpusculaire, CH-1211 Geneva, Switzerland. [Clark, K.] Univ Toronto, Dept Phys, Toronto, ON M5S 1A7, Canada. [Clevermann, F.; Frantzen, K.; Fuchs, T.; Koehne, J. -H.; Milke, N.; Pieloth, D.; Rhode, W.; Ruhe, T.; Scheriau, F.; Schmitz, M.; Ziemann, J.] TU Dortmund Univ, Dept Phys, D-44221 Dortmund, Germany. [Cowen, D. F.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [de Andre, J. P. A. M.; DeYoung, T.; Hignight, J.; Mahn, K. B. M.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. [Dembinski, H.; Evenson, P. A.; Gaisser, T. K.; Gonzalez, J. G.; Ruzybayev, B.; Seckel, D.; Stanev, T.; Tamburro, A.; Tilav, S.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA. [Dembinski, H.; Evenson, P. A.; Gaisser, T. K.; Gonzalez, J. G.; Ruzybayev, B.; Seckel, D.; Stanev, T.; Tamburro, A.; Tilav, S.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA. [De Ridder, S.; Ismail, A. Haj; Labare, M.; Meli, A.; Ryckbosch, D.; Vanheule, S.; Vraeghe, M.] Univ Ghent, Dept Phys & Astron, B-9000 Ghent, Belgium. [de With, M.; Hebecker, D.; Kolanoski, H.; Kowalski, M.] Humboldt Univ, Inst Phys, D-12489 Berlin, Germany. [Fazely, A. R.; Ter-Antonyan, S.; Xu, X. W.] Southern Univ, Dept Phys, Baton Rouge, LA 70813 USA. [Gaior, R.; Ishihara, A.; Kuwabara, T.; Mase, K.; Relich, M.; Yoshida, S.] Chiba Univ, Dept Phys, Chiba 2638522, Japan. [Gallagher, J.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. [Homeier, A.; Schulte, L.; Voge, M.] Univ Bonn, Inst Phys, D-53115 Bonn, Germany. [Japaridze, G. S.] Clark Atlanta Univ, CTSPS, Atlanta, GA 30314 USA. [Kauer, M.; Maruyama, R.] Yale Univ, Dept Phys, New Haven, CT 06520 USA. [Kiryluk, J.; Lesiak-Bzdak, M.; Niederhausen, H.; Xu, Y.] SUNY Stony Brook, Dept Phys & Astron, Stony Brook, NY 11794 USA. [Kohnen, G.] Univ Mons, B-7000 Mons, Belgium. [Koskinen, D. J.; Larson, M. J.; Medici, M.; Sandroos, J.; Sarkar, S.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark. [Kurahashi, N.; Meures, T.] Drexel Univ, Dept Phys, Philadelphia, PA 19104 USA. [Madsen, J.; Seunarine, S.; Spiczak, G. M.] Univ Wisconsin, Dept Phys, River Falls, WI 54022 USA. [Palczewski, T.; Pepper, J. A.; Toale, P. A.; Williams, D. R.; Xu, D. L.; Zarzhitsky, P.] Univ Alabama, Dept Phys & Astron, Tuscaloosa, AL 35487 USA. [Rawlins, K.] Univ Alaska Anchorage, Dept Phys & Astron, Anchorage, AK 99508 USA. [Sarkar, S.] Univ Oxford, Dept Phys, Oxford OX1 3NP, England. [Hoshina, K.] Univ Tokyo, Earthquake Res Inst, Bunkyo Ku, Tokyo 1130032, Japan. [Stamatikos, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Aartsen, MG (reprint author), Univ Adelaide, Sch Chem & Phys, Adelaide, SA 5005, Australia. RI Maruyama, Reina/A-1064-2013; Koskinen, David/G-3236-2014; Tjus, Julia/G-8145-2012; Beatty, James/D-9310-2011; Sarkar, Subir/G-5978-2011; Wiebusch, Christopher/G-6490-2012; OI Maruyama, Reina/0000-0003-2794-512X; Koskinen, David/0000-0002-0514-5917; Beatty, James/0000-0003-0481-4952; Sarkar, Subir/0000-0002-3542-858X; Wiebusch, Christopher/0000-0002-6418-3008; Schukraft, Anne/0000-0002-9112-5479; Groh, John/0000-0001-9880-3634; Larsen, Dag Toppe/0000-0002-9898-2174; Perez de los Heros, Carlos/0000-0002-2084-5866; Aguilar Sanchez, Juan Antonio/0000-0003-2252-9514; Strotjohann, Nora Linn/0000-0002-4667-6730; Dembinski, Hans/0000-0003-3337-3850; Arguelles Delgado, Carlos/0000-0003-4186-4182 FU U.S. National Science Foundation-Office of Polar Programs; U.S. National Science Foundation-Physics Division; University of Wisconsin Alumni Research Foundation; Grid Laboratory Of Wisconsin (GLOW) grid infrastructure at the University of Wisconsin-Madison; Open Science Grid (OSG) grid infrastructure; U.S. Department of Energy; National Energy Research Scientific Computing Center; Louisiana Optical Network Initiative (LONI) grid computing resources; Natural Sciences and Engineering Research Council of Canada; WestGrid and Compute/Calcul Canada; Swedish Research Council; Swedish Polar Research Secretariat; Swedish National Infrastructure for Computing (SNIC); Knut and Alice Wallenberg Foundation, Sweden; German Ministry for Education and Research (BMBF); Deutsche Forschungsgemeinschaft (DFG); Helmholtz Alliance for Astroparticle Physics (HAP); Research Department of Plasmas with Complex Interactions (Bochum), Germany; Fund for Scientific Research (FNRS-FWO); FWO Odysseus programme; Flanders Institute to encourage scientific and technological research in industry (IWT); Belgian Federal Science Policy Office (Belspo); University of Oxford, United Kingdom; Marsden Fund, New Zealand; Australian Research Council; Japan Society for Promotion of Science (JSPS); Swiss National Science Foundation (SNSF), Switzerland; National Research Foundation of Korea (NRF); Danish National Research Foundation, Denmark (DNRF) FX We acknowledge the support from the following agencies: U.S. National Science Foundation-Office of Polar Programs, U.S. National Science Foundation-Physics Division, University of Wisconsin Alumni Research Foundation, the Grid Laboratory Of Wisconsin (GLOW) grid infrastructure at the University of Wisconsin-Madison, the Open Science Grid (OSG) grid infrastructure; U.S. Department of Energy, and National Energy Research Scientific Computing Center, the Louisiana Optical Network Initiative (LONI) grid computing resources; Natural Sciences and Engineering Research Council of Canada, WestGrid and Compute/Calcul Canada; Swedish Research Council, Swedish Polar Research Secretariat, Swedish National Infrastructure for Computing (SNIC), and Knut and Alice Wallenberg Foundation, Sweden; German Ministry for Education and Research (BMBF), Deutsche Forschungsgemeinschaft (DFG), Helmholtz Alliance for Astroparticle Physics (HAP), Research Department of Plasmas with Complex Interactions (Bochum), Germany; Fund for Scientific Research (FNRS-FWO), FWO Odysseus programme, Flanders Institute to encourage scientific and technological research in industry (IWT), Belgian Federal Science Policy Office (Belspo); University of Oxford, United Kingdom; Marsden Fund, New Zealand; Australian Research Council; Japan Society for Promotion of Science (JSPS); the Swiss National Science Foundation (SNSF), Switzerland; National Research Foundation of Korea (NRF); Danish National Research Foundation, Denmark (DNRF). NR 63 TC 6 Z9 6 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 JUL 1 PY 2015 VL 807 IS 1 AR 46 DI 10.1088/0004-637X/807/1/46 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO1VX UT WOS:000358945200046 ER PT J AU An, HJ Archibald, RF Hascoet, R Kaspi, VM Beloborodov, AM Archibald, AM Beardmore, A Boggs, SE Christensen, FE Craig, WW Gehrels, N Hailey, CJ Harrison, FA Kennea, J Kouveliotou, C Stern, D Younes, G Zhang, WW AF An, Hongjun Archibald, Robert F. Hascoet, Romain Kaspi, Victoria M. Beloborodov, Andrei M. Archibald, Anne M. Beardmore, Andy Boggs, Steven E. Christensen, Finn E. Craig, William W. Gehrels, Niel Hailey, Charles J. Harrison, Fiona A. Kennea, Jamie Kouveliotou, Chryssa Stern, Daniel Younes, George Zhang, William W. TI DEEP NuSTAR AND SWIFT MONITORING OBSERVATIONS OF THE MAGNETAR 1E 1841-045 SO ASTROPHYSICAL JOURNAL LA English DT Article DE pulsars: individual (1E 1841-045); stars: magnetars; stars: neutron; X-rays: bursts ID X-RAY PULSARS; SOFT GAMMA-REPEATERS; NEUTRON-STARS; KES 73; 4U 0142+61; SPIN-DOWN; EMISSION; BURSTS; OUTBURST; RXTE AB We report on a 350 ks NuSTAR observation of the magnetar 1E 1841-045 taken in 2013 September. During the observation, NuSTAR detected six bursts of short duration, with T-90 less than or similar to 1 s. An elevated level of emission tail is detected after the brightest burst, persisting for similar to 1 ks. The emission showed a power-law decay with a temporal index of 0.5 before returning to the persistent emission level. The long observation also provided detailed phase-resolved spectra of the persistent X-ray emission of the source. By comparing the persistent spectrum with that previously reported, we find that the source hard-band emission has been stable for over approximately 10 yr. The persistent hard-X-ray emission is well fitted by a coronal outflow model, where e(+/-) pairs in the magnetosphere upscatter thermal X-rays. Our fit of phase-resolved spectra allowed us to estimate the angle between the rotational and magnetic dipole axes of the magnetar, alpha(mag) = 0.25, the twisted magnetic flux, 2.5 x 10(26) G cm(2), and the power released in the twisted magnetosphere, L-j = 6 x 10(36) erg s(-1). Assuming this model for the hard-X-ray spectrum, the soft-X-ray component is well fit by a two-blackbody model, with the hotter blackbody consistent with the footprint of the twisted magnetic field lines on the star. We also report on the 3 yr. Swift monitoring observations obtained since 2011 July. The soft-X-ray spectrum remained stable during this period, and the timing behavior was noisy, with large timing residuals. C1 [An, Hongjun; Archibald, Robert F.; Kaspi, Victoria M.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [An, Hongjun] Stanford Univ, Dept Phys, KIPAC, Stanford, CA 94305 USA. [Hascoet, Romain; Beloborodov, Andrei M.; Hailey, Charles J.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Archibald, Anne M.] ASTRON, Netherlands Inst Radio Astron, NL-7990 AA Dwingeloo, Netherlands. [Beardmore, Andy] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Boggs, Steven E.; Craig, William W.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Christensen, Finn E.] Tech Univ Denmark, Natl Space Inst, DTU Space, DK-2800 Lyngby, Denmark. [Craig, William W.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA. [Gehrels, Niel] NASA, Astrophys Sci Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Harrison, Fiona A.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Kennea, Jamie] Penn State Univ, Dept Astron & Astrophys, Lab 525, University Pk, PA 16802 USA. [Kouveliotou, Chryssa; Younes, George] NASA, Space Sci Off, Marshall Space Flight Ctr, Huntsville, AL 35812 USA. [Stern, Daniel] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Zhang, William W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP An, HJ (reprint author), McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. RI Boggs, Steven/E-4170-2015; OI Boggs, Steven/0000-0001-9567-4224; An, Hongjun/0000-0002-6389-9012; Archibald, Anne/0000-0003-0638-3340; Archibald, Robert/0000-0002-4017-8837 FU NASA [NNG08FD60C, NAS5-00147, NNX13AI34G]; National Aeronautics and Space Administration; Kavli Institute for Particle Astrophysics and Cosmology; NSERC; FQRNT Centre de Recherche Astrophysique du Quebec; R. Howard Webster Foundation Fellowship from the Canadian Institute for Advanced Research (CIFAR); Canada Research Chairs Program; Lorne Trottier Chair in Astrophysics and Cosmology FX This work was supported under NASA Contract No. NNG08FD60C and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software, and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). H.A. acknowledges support provided by the NASA sponsored Fermi Contract NAS5-00147 and by Kavli Institute for Particle Astrophysics and Cosmology. V.M.K. acknowledges support from an NSERC Discovery Grant and Accelerator Supplement, the FQRNT Centre de Recherche Astrophysique du Quebec, an R. Howard Webster Foundation Fellowship from the Canadian Institute for Advanced Research (CIFAR), the Canada Research Chairs Program, and the Lorne Trottier Chair in Astrophysics and Cosmology. A.M.B. acknowledges the support by NASA grant NNX13AI34G. NR 57 TC 6 Z9 6 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 1 PY 2015 VL 807 IS 1 AR 93 DI 10.1088/0004-637X/807/1/93 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO1VX UT WOS:000358945200093 ER PT J AU Andrews, H Boersma, C Werner, MW Livingston, J Allamandola, LJ Tielens, AGGM AF Andrews, H. Boersma, C. Werner, M. W. Livingston, J. Allamandola, L. J. Tielens, A. G. G. M. TI PAH EMISSION AT THE BRIGHT LOCATIONS OF PDRs: THE grandPAH HYPOTHESIS SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrochemistry; ISM: individual objects (NGC 7023, NGC 2023, NGC 1333); photon-dominated region (PDR) ID POLYCYCLIC AROMATIC-HYDROCARBONS; BLIND SIGNAL SEPARATION; PHOTODISSOCIATION REGIONS; INFRARED-EMISSION; SPECTROSCOPIC DATABASE; REFLECTION NEBULAE; TEMPERATURE-FLUCTUATIONS; INTERSTELLAR GRAINS; PHYSICAL CONDITIONS; RING DEFECTS AB The polycyclic aromatic hydrocarbon (PAH) emission observed in the Spitzer Infrared Spectrograph spectra of bright mid-IR locations of NGC 7023, NGC 2023, and NGC 1333 was analyzed. These objects show large variations in PAH band ratios when studied through spectral mapping. Nevertheless, the mid-IR spectra at these bright spots show a remarkably similar PAH emission. We used the NASA Ames PAH IR Spectroscopic Database to fit the observations and analyze the derived PAH populations. Our results show that PAH emission in the 5-15 mu m range appears to be rather insensitive to variations of the radiation field. Similar PAH populations of neutral small to medium- sized PAHs (similar to 50%), with ionized species contributing in slightly less than 50%, provide very good fits. Analyzing the degeneracy of the results shows that subtle (but intrinsic) variations in the emission properties of individual PAHs lead to observable differences in the resulting spectra. On top of this, we found that variations of <30% in the PAH abundances would lead to noticeable spectral differences between the three photodissociation regions (PDRs). Therefore, PAH populations must be remarkably similar at these different lines of sight. To account for this, we suggest the concept of grandPAHs as a unique mixture of the most stable PAHs emitting at these spots. Using NGC 7023 as an example, the grandPAHs refer to the robust PAH population that results from the intense processing of PAHs at the border limit between the PDR and the molecular cloud, where, due to the UV radiation that destroys the PAH population, the abundance of PAHs starts decreasing as we move toward the star. C1 [Andrews, H.; Tielens, A. G. G. M.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Boersma, C.; Allamandola, L. J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Werner, M. W.; Livingston, J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Andrews, H (reprint author), Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands. EM heandrew@strw.leidenuniv.nl; Christiaan.Boersma@nasa.gov FU ERC grant from the European Research Council [246976]; Dutch Science Agency, NWO, as part of the Dutch Astrochemistry Network; NASA's "Carbon in the Galaxy" consortium grant [NNH10ZDA001N]; NASA's Astrobiology, Astronomy and Physics Research and Analysis (APRA) [NNX07AH02G]; Spitzer Space Telescope Support programs [50082]; Dutch Science Agency, NWO FX Studies of interstellar PAHs at Leiden Observatory are supported through advanced ERC grant 246976 from the European Research Council, through a grant by the Dutch Science Agency, NWO, as part of the Dutch Astrochemistry Network, and through the Spinoza premie from the Dutch Science Agency, NWO. 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. C.B. and L.A. gratefully acknowledge support from NASA's "Carbon in the Galaxy" consortium grant (NNH10ZDA001N) and NASA's Astrobiology, Astronomy and Physics Research and Analysis (APRA; NNX07AH02G), and Spitzer Space Telescope Support programs (50082). C.B. is grateful for an appointment at NASA's Ames Research Center through San Jose State University Research Foundation (NNX14AG80A). NR 72 TC 9 Z9 9 U1 2 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 1 PY 2015 VL 807 IS 1 AR 99 DI 10.1088/0004-637X/807/1/99 PG 24 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO1VX UT WOS:000358945200099 ER PT J AU Bechtol, K Drlica-Wagner, A Balbinot, E Pieres, A Simon, JD Yanny, B Santiago, B Wechsler, RH Frieman, J Walker, AR Williams, P Rozo, E Rykoff, ES Queiroz, A Luque, E Benoit-Levy, A Tucker, D Sevilla, I Gruendl, RA da Costa, LN Neto, AF Maia, MAG Abbott, T Allam, S Armstrong, R Bauer, AH Bernstein, GM Bernstein, RA Bertin, E Brooks, D Buckley-Geer, E Burke, DL Rosell, AC Castander, FJ Covarrubias, R D'Andrea, CB DePoy, DL Desai, S Diehl, HT Eifler, TF Estrada, J Evrard, AE Fernandez, E Finley, DA Flaugher, B Gaztanaga, E Gerdes, D Girardi, L Gladders, M Gruen, D Gutierrez, G Hao, J Honscheid, K Jain, B James, D Kent, S Kron, R Kuehn, K Kuropatkin, N Lahav, O Li, TS Lin, H Makler, M March, M Marshall, J Martini, P Merritt, KW Miller, C Miquel, R Mohr, J Neilsen, E Nichol, R Nord, B Ogando, R Peoples, J Petravick, D Plazas, AA Romer, AK Roodman, A Sako, M Sanchez, E Scarpine, V Schubnell, M Smith, RC Soares-Santos, M Sobreira, F Suchyta, E Swanson, MEC Tarle, G Thaler, J Thomas, D Wester, W Zuntz, J AF Bechtol, K. Drlica-Wagner, A. Balbinot, E. Pieres, A. Simon, J. D. Yanny, B. Santiago, B. Wechsler, R. H. Frieman, J. Walker, A. R. Williams, P. Rozo, E. Rykoff, E. S. Queiroz, A. Luque, E. Benoit-Levy, A. Tucker, D. Sevilla, I. Gruendl, R. A. da Costa, L. N. Fausti Neto, A. Maia, M. A. G. Abbott, T. Allam, S. Armstrong, R. Bauer, A. H. Bernstein, G. M. Bernstein, R. A. Bertin, E. Brooks, D. Buckley-Geer, E. Burke, D. L. Carnero Rosell, A. Castander, F. J. Covarrubias, R. D'Andrea, C. B. DePoy, D. L. Desai, S. Diehl, H. T. Eifler, T. F. Estrada, J. Evrard, A. E. Fernandez, E. Finley, D. A. Flaugher, B. Gaztanaga, E. Gerdes, D. Girardi, L. Gladders, M. Gruen, D. Gutierrez, G. Hao, J. Honscheid, K. Jain, B. James, D. Kent, S. Kron, R. Kuehn, K. Kuropatkin, N. Lahav, O. Li, T. S. Lin, H. Makler, M. March, M. Marshall, J. Martini, P. Merritt, K. W. Miller, C. Miquel, R. Mohr, J. Neilsen, E. Nichol, R. Nord, B. Ogando, R. Peoples, J. Petravick, D. Plazas, A. A. Romer, A. K. Roodman, A. Sako, M. Sanchez, E. Scarpine, V. Schubnell, M. Smith, R. C. Soares-Santos, M. Sobreira, F. Suchyta, E. Swanson, M. E. C. Tarle, G. Thaler, J. Thomas, D. Wester, W. Zuntz, J. CA DES Collaboration TI EIGHT NEW MILKY WAY COMPANIONS DISCOVERED IN FIRST-YEAR DARK ENERGY SURVEY DATA SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: dwarf; Local Group ID DWARF SPHEROIDAL GALAXIES; ULTRA-FAINT SATELLITES; STAR-FORMATION HISTORY; DIGITAL SKY SURVEY; GLOBULAR-CLUSTERS; LOCAL GROUP; URSA-MAJOR; STRUCTURAL-PROPERTIES; SPECTROSCOPIC SURVEY; STELLAR POPULATIONS AB We report the discovery of eight new Milky Way companions in similar to 1800 deg(2) of optical imaging data collected during the first year of the Dark Energy Survey (DES). Each system is identified as a statistically significant over-density of individual stars consistent with the expected isochrone and luminosity function of an old and metal-poor stellar population. The objects span a wide range of absolute magnitudes (M-V from -2.2 to -7.4 mag), physical sizes (10-170 pc), and heliocentric distances (30-330 kpc). Based on the low surface brightnesses, large physical sizes, and/or large Galactocentric distances of these objects, several are likely to be new ultra-faint satellite galaxies of the Milky Way and/or Magellanic Clouds. We introduce a likelihood-based algorithm to search for and characterize stellar over-densities, as well as identify stars with high satellite membership probabilities. We also present completeness estimates for detecting ultra-faint galaxies of varying luminosities, sizes, and heliocentric distances in the first-year DES data. C1 [Bechtol, K.; Frieman, J.; Williams, P.; Gladders, M.; Kron, R.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Drlica-Wagner, A.; Yanny, B.; Frieman, J.; Tucker, D.; Allam, S.; Buckley-Geer, E.; Diehl, H. T.; Estrada, J.; Finley, D. A.; Flaugher, B.; Gutierrez, G.; Hao, J.; Kent, S.; Kuropatkin, N.; Lin, H.; Merritt, K. W.; Neilsen, E.; Nord, B.; Peoples, J.; Scarpine, V.; Soares-Santos, M.; Sobreira, F.; Wester, W.] Fermilab Natl Accelerator Lab, Batavia, IL 60510 USA. [Balbinot, E.] Univ Surrey, Dept Phys, Guildford GU2 7XH, Surrey, England. [Balbinot, E.; Pieres, A.; Santiago, B.; Queiroz, A.; Luque, E.; da Costa, L. N.; Fausti Neto, A.; Maia, M. A. G.; Carnero Rosell, A.; Ogando, R.; Sobreira, F.] Lab Interinst eAstron LIneA, BR-20921400 Rio De Janeiro, RJ, Brazil. [Pieres, A.; Santiago, B.; Queiroz, A.; Luque, E.] Univ Fed Rio Grande do Sul, Inst Fis, BR-91501970 Porto Alegre, RS, Brazil. [Simon, J. D.; Bernstein, R. A.] Carnegie Observ, Pasadena, CA 91101 USA. [Wechsler, R. H.; Roodman, A.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA. [Wechsler, R. H.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA. [Wechsler, R. H.; Rozo, E.; Rykoff, E. S.; Burke, D. L.] SLAC Natl Accelerator Lab, Menlo Pk, CA 94025 USA. [Walker, A. R.; Abbott, T.; James, D.; Roodman, A.; Smith, R. C.] Natl Opt Astron Observ, Cerro Tololo Inter Amer Observ, La Serena, Chile. [Rozo, E.] Univ Arizona, Dept Phys, Tucson, AZ 85721 USA. [Benoit-Levy, A.; Brooks, D.; Lahav, O.] UCL, Dept Phys & Astron, London WC1E 6BT, England. [Sevilla, I.; Gruendl, R. A.] Univ Illinois, Dept Astron, Urbana, IL 61801 USA. [Sevilla, I.; Sanchez, E.] Ctr Invest Energet Medioambientales & Tecnol CIEM, Madrid, Spain. [Gruendl, R. A.; Covarrubias, R.; Petravick, D.; Swanson, M. E. C.] Univ Illinois, Natl Ctr Supercomp Applicat, Urbana, IL 61801 USA. [da Costa, L. N.; Maia, M. A. G.; Carnero Rosell, A.; Girardi, L.; Ogando, R.] Observ Nacl, BR-20921400 Rio De Janeiro, RJ, Brazil. [Allam, S.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Armstrong, R.; Bernstein, G. M.; Eifler, T. F.; Jain, B.; March, M.; Sako, M.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. [Bauer, A. H.; Castander, F. J.; Gaztanaga, E.] Fac Ciencies, IEEC CSIC, Inst Ciencies Espai, E-08193 Bellaterra, Barcelona, Spain. [Bertin, E.] Univ Paris 06, Sorbonne Univ, Inst Astrophys Paris, UMR 7095, F-75014 Paris, France. [Bertin, E.] Inst Astrophys Paris, CNRS, UMR 7095, F-75014 Paris, France. [D'Andrea, C. B.; Nichol, R.; Thomas, D.] Univ Portsmouth, Inst Cosmol & Gravitat, Portsmouth PO1 3FX, Hants, England. [DePoy, D. L.; Li, T. S.; Marshall, J.] Texas A&M Univ, George P & Cynthia Woods Mitchell Inst Fundamenta, College Stn, TX 77843 USA. [DePoy, D. L.; Li, T. S.; Marshall, J.] Texas A&M Univ, Dept Phys & Astron, College Stn, TX 77843 USA. [Desai, S.; Mohr, J.] Univ Munich, Dept Phys, D-81679 Munich, Germany. [Desai, S.] Excellence Cluster Universe, D-85748 Garching, Germany. [Eifler, T. F.; Plazas, A. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Evrard, A. E.; Gerdes, D.; Miller, C.; Schubnell, M.; Tarle, G.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA. [Fernandez, E.; Gladders, M.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Fernandez, E.; Miquel, R.] Inst Catalana Recerca & Estudis Avancats, E-08010 Barcelona, Spain. [Gruen, D.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Gruen, D.] Univ Observ Munich, D-81679 Munich, Germany. [Honscheid, K.; Suchyta, E.] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA. [Honscheid, K.; Martini, P.; Suchyta, E.] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA. [Kuehn, K.] Australian Astron Observ, N Ryde, NSW 2113, Australia. [Kuehn, K.] Argonne Natl Lab, Argonne, IL 60439 USA. [Makler, M.] Ctr Brasileiro Pesquisas Fis, ICRA, BR-22290180 Rio De Janeiro, RJ, Brazil. [Martini, P.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Miller, C.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Miquel, R.] Univ Autonoma Barcelona, Inst Fis Altes Energies, E-08193 Bellaterra, Barcelona, Spain. [Plazas, A. A.] Brookhaven Natl Lab, Upton, NY 11973 USA. [Romer, A. K.] Univ Sussex, Ctr Astron, Brighton BN1 9QH, E Sussex, England. [Thaler, J.] Univ Illinois, Dept Phys, Urbana, IL 61801 USA. [Zuntz, J.] Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, Oxford M13 9PL, England. RP Bechtol, K (reprint author), Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. EM bechtol@kicp.uchicago.edu; kadrlica@fnal.gov RI Ogando, Ricardo/A-1747-2010; Makler, Martin/G-2639-2012; Sanchez, Eusebio/H-5228-2015; Sobreira, Flavia/F-4168-2015; Fernandez, Enrique/L-5387-2014; Gaztanaga, Enrique/L-4894-2014; Balbinot, Eduardo/E-8019-2015; OI Ogando, Ricardo/0000-0003-2120-1154; Makler, Martin/0000-0003-2206-2651; Tucker, Douglas/0000-0001-7211-5729; Sanchez, Eusebio/0000-0002-9646-8198; Sobreira, Flavia/0000-0002-7822-0658; Fernandez, Enrique/0000-0002-6405-9488; Gaztanaga, Enrique/0000-0001-9632-0815; Balbinot, Eduardo/0000-0002-1322-3153; Suchyta, Eric/0000-0002-7047-9358 FU National Science Foundation [1138766, AST-1138766]; PAPDRJ CAPES/FAPERJ Fellowship; DOE grant [DE-AC02-98CH10886]; JPL; U.S. Department of Energy; U.S. National Science Foundation; Ministry of Science and Education of Spain; Science and Technology Facilities Council of the United Kingdom; Higher Education Funding Council for England; National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign; Kavli Institute of Cosmological Physics at the University of Chicago; Center for Cosmology and Astro-Particle Physics at the Ohio State University; Mitchell Institute for Fundamental Physics and Astronomy at Texas AM University; Financiadora de Estudos e Projetos; Fundacao Carlos Chagas Filho de Amparo a Pesquisa do Estado do Rio de Janeiro; Conselho Nacional de Desenvolvimento Cientifico e Tecnologico; Ministerio da Ciencia, Tecnologia e Inovacao; Deutsche Forschungsgemeinschaft; MINECO [AYA2012-39559, ESP2013-48274, FPA2013-47986]; Centro de Excelencia Severo Ochoa [SEV-2012-0234]; European Union; Argonne National Laboratory; University of California at Santa Cruz; University of Cambridge; Centro de Investigaciones Energeticas, Medioambientales y Tecnologicas-Madrid; University of Chicago; University College London; DES-Brazil Consortium; University of Edinburgh; Eidgenossische Technische Hochschule (ETH) Zurich; Fermi National Accelerator Laboratory; University of Illinois at Urbana-Champaign; Institut de Ciencies de l'Espai (IEEC/CSIC); Institut de Fisica d'Altes Energies; Ludwig-Maximilians Universitat Munchen; University of Michigan; National Optical Astronomy Observatory; University of Nottingham; Ohio State University; University of Pennsylvania; University of Portsmouth; SLAC National Accelerator Laboratory, Stanford University; University of Sussex; Texas AM University; Lawrence Berkeley National Laboratory FX We thank Sergey Koposov and collaborators for sending a copy of their submitted paper with their nine discoveries, and Helmut Jerjen for pointing out the association between Kim 2 and DES J2108.8-5109. Marla Geha provided useful comments on the presentation of these results. K.B. and A.D.W. thank Beth Willman for advice regarding the search for ultra-faint galaxies. A.D.W. thanks Ellen Bechtol for her generous hospitality during the preparation of this manuscript. We acknowledge helpful suggestions from the anonymous referee. This work made use of computational resources at the SLAC National Accelerator Laboratory and University of Chicago Research Computing Center. This material is based upon work supported by the National Science Foundation under Grant Number (1138766). A.C.R. acknowledges financial support provided by the PAPDRJ CAPES/FAPERJ Fellowship. A.A.P. was supported by DOE grant DE-AC02-98CH10886 and by JPL, run by Caltech under a contract for NASA. Funding for the DES Projects has been provided by the U.S. Department of Energy, the U.S. National Science Foundation, the Ministry of Science and Education of Spain, the Science and Technology Facilities Council of the United Kingdom, the Higher Education Funding Council for England, the National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign, the Kavli Institute of Cosmological Physics at the University of Chicago, the Center for Cosmology and Astro-Particle Physics at the Ohio State University, the Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M University, Financiadora de Estudos e Projetos, Fundacao Carlos Chagas Filho de Amparo a Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Cientifico e Tecnologico and the Ministerio da Ciencia, Tecnologia e Inovacao, the Deutsche Forschungsgemeinschaft and the Collaborating Institutions in the Dark Energy Survey. The DES data management system is supported by the National Science Foundation under Grant Number AST-1138766. The DES participants from Spanish institutions are partially supported by MINECO under grants AYA2012-39559, ESP2013-48274, FPA2013-47986, and Centro de Excelencia Severo Ochoa SEV-2012-0234, some of which include ERDF funds from the European Union. The Collaborating Institutions are Argonne National Laboratory, the University of California at Santa Cruz, the University of Cambridge, Centro de Investigaciones Energeticas, Medioambientales y Tecnologicas-Madrid, the University of Chicago, University College London, the DES-Brazil Consortium, the University of Edinburgh, the Eidgenossische Technische Hochschule (ETH) Zurich, Fermi National Accelerator Laboratory, the University of Illinois at Urbana-Champaign, the Institut de Ciencies de l'Espai (IEEC/CSIC), the Institut de Fisica d'Altes Energies, Lawrence Berkeley National Laboratory, the Ludwig-Maximilians Universitat Munchen and the associated Excellence Cluster universe, the University of Michigan, the National Optical Astronomy Observatory, the University of Nottingham, The Ohio State University, the University of Pennsylvania, the University of Portsmouth, SLAC National Accelerator Laboratory, Stanford University, the University of Sussex, and Texas A&M University. NR 102 TC 108 Z9 108 U1 4 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 JUL 1 PY 2015 VL 807 IS 1 AR 50 DI 10.1088/0004-637X/807/1/50 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO1VX UT WOS:000358945200050 ER PT J AU Gelfand, JD Slane, PO Temim, T AF Gelfand, Joseph D. Slane, Patrick O. Temim, Tea TI THE PROPERTIES OF THE PROGENITOR SUPERNOVA, PULSAR WIND, AND NEUTRON STAR INSIDE PWN G54.1+0.3 SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: individual objects (PWN G54.1+0.3); ISM: supernova remnants; pulsars: individual (PSR J1930+1852); X-rays: individual (PWN G54.1+0.3) ID RELATIVISTIC COLLISIONLESS SHOCKS; PAIR PRODUCTION MULTIPLICITIES; GALACTIC ABUNDANCE GRADIENT; REMNANT G54.1+0.3; NEBULA G54.1+0.3; CRAB-NEBULA; SPECTRAL EVOLUTION; ACCRETION SHOCK; RADIO-EMISSION; SIGMA-PROBLEM AB The evolution of a pulsar wind nebula (PWN) inside a supernova remnant (SNR) is sensitive to the properties of the central neutron star, pulsar wind, progenitor supernova, and interstellar medium. These properties are both difficult to measure directly and critical for understanding the formation of neutron stars and their interaction with the surrounding medium. In this paper, we determine these properties for PWN G54.1+0.3 by fitting its observed properties with a model for the dynamical and radiative evolution of a PWN inside an SNR. Our modeling suggests that the progenitor of G54.1+0.3 was an isolated similar to 15-20 M-circle dot star which exploded inside a massive star cluster, creating a neutron star initially spinning with a period of P-0 similar to 30-80 ms. We also find that greater than or similar to 99.9% of the pulsar's rotational energy is injected into the PWN as relativistic electrons and positrons whose energy spectrum is well characterized by a broken power law. Finally, we propose future observations which can both test the validity of this model and better determine the properties of this source-in particular, its distance and the initial spin period of the central pulsar. C1 [Gelfand, Joseph D.] NYU Abu Dhabi, New York, NY 10276 USA. [Slane, Patrick O.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Temim, Tea] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA. [Gelfand, Joseph D.] NYU, Ctr Cosmol & Particle Phys, New York, NY 10003 USA. [Temim, Tea] Oak Ridge Associated Univ, Oak Ridge, TN 37831 USA. RP Gelfand, JD (reprint author), NYU Abu Dhabi, POB 903, New York, NY 10276 USA. EM jg168@nyu.edu OI Gelfand, Joseph/0000-0003-4679-1058; Temim, Tea/0000-0001-7380-3144 FU NASA [RSA 1479542] FX Support for this work was provided by NASA through an award issued by JPL/Caltech (RSA 1479542). J.D.G. will like to thank Erin Sheldon for the IDL code used in the MCMC fits, Kaisey Mandel and David Hogg for useful discussions concerning MCMC fitting, Ester Aliu for information regarding the GeV spectrum, and Roger Chevalier, Vikram Dwarkadas, Daniel Patnaude, and Lorenzo Sironi for useful advice. NR 56 TC 1 Z9 1 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 1 PY 2015 VL 807 IS 1 AR 30 DI 10.1088/0004-637X/807/1/30 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO1VX UT WOS:000358945200030 ER PT J AU Gicquel, A Milam, SN Coulson, IM Villanueva, GL Cordiner, MA Charnley, SB DiSanti, MA Mumma, MJ Szutowicz, S AF Gicquel, A. Milam, S. N. Coulson, I. M. Villanueva, G. L. Cordiner, M. A. Charnley, S. B. DiSanti, M. A. Mumma, M. J. Szutowicz, S. TI THE EVOLUTION OF VOLATILE PRODUCTION IN COMET C/2009 P1 (GARRADD) DURING ITS 2011-2012 APPARITION SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrobiology; comets: individual (C/2009 P1 (Garradd)); submillimeter: planetary systems; techniques: spectroscopic ID 103P/HARTLEY 2; HALE-BOPP; C/1995 O1; WATER; PHOTODISSOCIATION; PREPERIHELION; HCN; AU AB We report observations at millimeter and submillimeter wavelengths of comet C/2009 P1 (Garradd) from 2011 December 28 to 2012 April 24, using the Arizona Radio Observatory submillimeter telescope (SMT) and the James Clerk Maxwell Telescope (JCMT). Garradd is a dynamically young long-period comet from the Oort Cloud, with a periodicity of 127,000 yr, that reached perihelion on 2011 December 23 (at R-h = 1.55 AU and Delta = 20.1 AU) and made its closest approach to the Earth on 2012 March 05 (at R-h = 1.84 AU and Delta = 1.26 AU). We obtained gas production rates, and molecular abundances relative to water for HCN, ortho-H2CO, CS, CO and CH3OH. A rotational temperature, T-rot approximate to 50 K, was determined by observing multiple methanol lines with the JCMT. By averaging the abundance ratio relative to water from the SMT and the JCMT we derive: CO: 7.03% +/- 1.84%, HCN: 0.04% +/- 0.01%, o-H2CO: 0.14% +/- 0.03% as a parent molecule (and 0.28% +/- 0.06% as an extended source), CS: 0.03% +/- 0.01% and CH3OH: 3.11(-0.51)(+1.86)%. We concluded that Garradd is normal in CH3OH, depleted in HCN, o-H2CO and CS and slightly enriched in CO with respect to typically observed cometary mixing ratios. We also studied the temporal evolution of HCN and CO and find that the production of HCN has a trend similar to water (but with short-term variation), with a decrease after perihelion, while that of CO shows contrary behavior: remaining constant or increasing after perihelion. C1 [Gicquel, A.; Milam, S. N.; Villanueva, G. L.; Cordiner, M. A.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA. [Gicquel, A.; Villanueva, G. L.; Cordiner, M. A.; Charnley, S. B.; DiSanti, M. A.; Mumma, M. J.] NASA, Goddard Space Flight Ctr, Goddard Ctr Astrobiol, Greenbelt, MD 20771 USA. [Coulson, I. M.] Joint Astron Ctr, Hilo, HI 96720 USA. [Szutowicz, S.] PAS, Space Res Ctr, PL-00716 Warsaw, Poland. RP Gicquel, A (reprint author), Catholic Univ Amer, Dept Phys, 620 Michigan Ave NE, Washington, DC 20064 USA. EM adeline.gicquel@nasa.gov; stefanie.n.milam@nasa.gov; i.coulson@jach.hawaii.edu; geronimo.villanueva@nasa.gov; martin.a.cordiner@nasa.gov; steven.b.charnley@nasa.gov; michael.a.disanti@nasa.gov; michael.j.mumma@nasa.gov; slawka@cbk.waw.pl RI Milam, Stefanie/D-1092-2012 OI Milam, Stefanie/0000-0001-7694-4129 FU Research Corporation; NASA's Planetary Astronomy and Planetary Atmospheres Programs FX The James Clerk Maxwell Telescope was operated during 2011/12 by the Joint Astronomy Centre on behalf of the Science and Technology Facilities Council of the United Kingdom, the National Research Council of Canada, and the Netherlands Organisation for Scientific Research. The data presented here were taken for approved observing programs s11bu01 and m12au39. The Kitt Peak 12 m telescope and the Submillimeter telescope are currently operated by the Arizona Observatory (ARO), Steward Observatory, and University of Arizona, with partial funding from the Research Corporation. This work was supported by NASA's Planetary Astronomy and Planetary Atmospheres Programs. NR 38 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 EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 1 PY 2015 VL 807 IS 1 AR 19 DI 10.1088/0004-637X/807/1/19 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO1VX UT WOS:000358945200019 ER PT J AU Hayashida, M Nalewajko, K Madejski, GM Sikora, M Itoh, R Ajello, M Blandford, RD Buson, S Chiang, J Fukazawa, Y Furniss, AK Urry, CM Hasan, I Harrison, FA Alexander, DM Balokovic, M Barret, D Boggs, SE Christensen, FE Craig, WW Forster, K Giommi, P Grefenstette, B Hailey, C Hornstrup, A Kitaguchi, T Koglin, JE Madsen, KK Mao, PH Miyasaka, H Mori, K Perri, M Pivovaroff, MJ Puccetti, S Rana, V Stern, D Tagliaferri, G Westergaard, NJ Zhang, WW Zoglauer, A Gurwell, MA Uemura, M Akitaya, H Kawabata, KS Kawaguchi, K Kanda, Y Moritani, Y Takaki, K Ui, T Yoshida, M Agarwal, A Gupta, AC AF Hayashida, M. Nalewajko, K. Madejski, G. M. Sikora, M. Itoh, R. Ajello, M. Blandford, R. D. Buson, S. Chiang, J. Fukazawa, Y. Furniss, A. K. Urry, C. M. Hasan, I. Harrison, F. A. Alexander, D. M. Balokovic, M. Barret, D. Boggs, S. E. Christensen, F. E. Craig, W. W. Forster, K. Giommi, P. Grefenstette, B. Hailey, C. Hornstrup, A. Kitaguchi, T. Koglin, J. E. Madsen, K. K. Mao, P. H. Miyasaka, H. Mori, K. Perri, M. Pivovaroff, M. J. Puccetti, S. Rana, V. Stern, D. Tagliaferri, G. Westergaard, N. J. Zhang, W. W. Zoglauer, A. Gurwell, M. A. Uemura, M. Akitaya, H. Kawabata, K. S. Kawaguchi, K. Kanda, Y. Moritani, Y. Takaki, K. Ui, T. Yoshida, M. Agarwal, A. Gupta, A. C. TI RAPID VARIABILITY OF BLAZAR 3C 279 DURING FLARING STATES IN 2013-2014 WITH JOINT FERMI-LAT, NuSTAR, SWIFT, AND GROUND-BASED MULTI-WAVELENGTH OBSERVATIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: jets; gamma rays: galaxies; quasars: individual (3C 279); radiation mechanisms: non-thermal; X-rays: galaxies ID ACTIVE GALACTIC NUCLEI; LARGE-AREA TELESCOPE; EXTRAGALACTIC RADIO-SOURCES; ENERGY GAMMA-RADIATION; LUMINOUS BLAZARS; PKS 1510-089; MAGNETIC RECONNECTION; RELATIVISTIC JET; BRIGHT BLAZARS; QUASAR 3C-279 AB We report the results of a multiband observing campaign on the famous blazar 3C 279 conducted during a phase of increased activity from 2013 December to 2014 April, including first observations of it with NuSTAR. The gamma-ray emission of the source measured by Fermi-LAT showed multiple distinct flares reaching the highest flux level measured in this object since the beginning of the Fermi mission, with F(E > 100 MeV) of 10(-5) photons cm(-2) s(-1), and with a flux-doubling time scale as short as 2 hr. The gamma-ray spectrum during one of the flares was very hard, with an index of Gamma(gamma) = 1.7 +/- 0.1, which is rarely seen in flat-spectrum radio quasars. The lack of concurrent optical variability implies a very high Compton dominance parameter L-gamma/L-syn > 300. Two 1 day NuSTAR observations with accompanying Swift pointings were separated by 2 weeks, probing different levels of source activity. While the 0.5 - 70 keV X-ray spectrum obtained during the first pointing, and fitted jointly with Swift-XRT is well-described by a simple power law, the second joint observation showed an unusual spectral structure: the spectrum softens by Delta Gamma(X) similar or equal to 0.4 at similar to 4 keV. Modeling the broadband spectral energy distribution during this flare with the standard synchrotron plus inverse-Compton model requires: (1) the location of the gamma-ray emitting region is comparable with the broad-line region radius, (2) a very hard electron energy distribution index p similar or equal to 1, (3) total jet power significantly exceeding the accretion-disk luminosity L-j/L-d greater than or similar to 10, and (4) extremely low jet magnetization with L-B/L-j less than or similar to 10(-4). We also find that single-zone models that match the observed gamma-ray and optical spectra cannot satisfactorily explain the production of X-ray emission. C1 [Hayashida, M.] Univ Tokyo, Inst Cosm Ray Res, Kashiwa, Chiba 2778582, Japan. [Nalewajko, K.; Madejski, G. M.; Blandford, R. D.; Chiang, J.; Furniss, A. K.; Koglin, J. E.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Dept Phys, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA. [Nalewajko, K.; Madejski, G. M.; Blandford, R. D.; Chiang, J.; Furniss, A. K.; Koglin, J. E.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA. [Sikora, M.] Nicolaus Copernicus Astron Ctr, PL-00716 Warsaw, Poland. [Itoh, R.; Fukazawa, Y.; Kawaguchi, K.; Kanda, Y.; Takaki, K.; Ui, T.] Hiroshima Univ, Dept Phys Sci, Higashihiroshima, Hiroshima 7398526, Japan. [Ajello, M.] Clemson Univ, Dept Phys & Astron, Kinard Lab Phys, Clemson, SC 29634 USA. [Buson, S.] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy. [Buson, S.] Univ Padua, Dipartimento Fis & Astron G Galilei, I-35131 Padua, Italy. [Urry, C. M.; Hasan, I.] Yale Univ, Yale Ctr Astron & Astrophys, Dept Phys, New Haven, CT 06520 USA. [Harrison, F. A.; Balokovic, M.; Forster, K.; Grefenstette, B.; Madsen, K. K.; Mao, P. H.; Miyasaka, H.; Rana, V.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Alexander, D. M.] Univ Durham, Dept Phys, Durham DH1 3LE, England. [Barret, D.] Univ Toulouse, UPS OMP, IRAP, Toulouse, France. [Barret, D.; Craig, W. W.] CNRS, Inst Rech Astrophys & Planetol, F-31028 Toulouse 4, France. [Boggs, S. E.; Zoglauer, A.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Christensen, F. E.; Hornstrup, A.; Westergaard, N. J.] Tech Univ Denmark, Natl Space Inst, DTU Space, DK-2800 Lyngby, Denmark. [Craig, W. W.; Pivovaroff, M. J.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA. [Giommi, P.; Perri, M.; Puccetti, S.] ASI Sci Data Ctr, D-52425 Rome, Italy. [Hailey, C.; Mori, K.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Kitaguchi, T.] Hiroshima Univ, Grad Sch Sci, Core Res Energet Universe, Higashihiroshima, Hiroshima 7398526, Japan. [Perri, M.; Puccetti, S.] INAF, Osservatorio Astron Roma, I-00040 Monte Porzio Catone, Italy. [Stern, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Tagliaferri, G.] INAF, Osservatorio Astron Brera, I-23807 Merate, Italy. [Zhang, W. W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Gurwell, M. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Uemura, M.; Akitaya, H.; Kawabata, K. S.; Moritani, Y.; Yoshida, M.] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Higashihiroshima, Hiroshima 7398526, Japan. [Agarwal, A.; Gupta, A. C.] Aryabhatta Res Inst Observat Sci ARIES, Naini Tal 263002, India. RP Hayashida, M (reprint author), Univ Tokyo, Inst Cosm Ray Res, 5-1-5 Kashiwanoha, Kashiwa, Chiba 2778582, Japan. EM mahaya@icrr.u-tokyo.ac.jp; knalew@stanford.edu RI Boggs, Steven/E-4170-2015; OI Boggs, Steven/0000-0001-9567-4224; Perri, Matteo/0000-0003-3613-4409; giommi, paolo/0000-0002-2265-5003; Puccetti, Simonetta/0000-0002-2734-7835; Rana, Vikram/0000-0003-1703-8796; Urry, Meg/0000-0002-0745-9792; Ajello, Marco/0000-0002-6584-1703 FU NASA [NNG08FD60C, NAS8-03060]; NASA through Einstein Postdoctoral Fellowship - Chandra X-ray Center [PF3-140130]; NASA Headquarters under the NASA earth and Space Science Fellowship Program [NNX14AQ07H]; Smithsonian Institution; Academia Sinica FX This work was partially supported under the NASA contract no. NNG08FD60C, and made use of observations from the NuSTAR mission, a project led by California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by NASA. We thank the NuSTAR Operations, Software, and Calibration teams for support of the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). This research has made use of the XRT Data Analysis Software (XRTDAS) developed under the responsibility of the ASI Science Data Center (ASDC), Italy. The Submillimeter Array is a joint project between the Smithsonian Astrophysical Observatory and the Academia Sinica Institute of Astronomy and Astrophysics and is funded by the Smithsonian Institution and the Academia Sinica.; K.N. was supported by NASA through Einstein Postdoctoral Fellowship grant number PF3-140130 awarded by the Chandra X-ray Center, which is operated by the Smithsonian Astrophysical Observatory for NASA under contract NAS8-03060. M.B. acknowledges support from NASA Headquarters under the NASA earth and Space Science Fellowship Program, grant NNX14AQ07H. NR 81 TC 33 Z9 33 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 1 PY 2015 VL 807 IS 1 AR 79 DI 10.1088/0004-637X/807/1/79 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO1VX UT WOS:000358945200079 ER PT J AU Hu, RY Seager, S Yung, YL AF Hu, Renyu Seager, Sara Yung, Yuk L. TI HELIUM ATMOSPHERES ON WARM NEPTUNE- AND SUB-NEPTUNE-SIZED EXOPLANETS AND APPLICATIONS TO GJ 436b SO ASTROPHYSICAL JOURNAL LA English DT Article DE atmospheric effects; planetary systems; planets and satellites: individual (GJ 436b); radiative transfer; techniques: spectroscopic ID HUBBLE-SPACE-TELESCOPE; STELLAR X-RAY; SUPER-EARTHS; HOT-NEPTUNE; HD 209458B; TRANSMISSION SPECTRUM; HYDROGEN-RICH; PLANET ATMOSPHERES; MASS FRACTIONATION; MINI-NEPTUNES AB Warm Neptune- and sub-Neptune-sized exoplanets in orbits smaller than Mercury's are thought to have experienced extensive atmospheric evolution. Here we propose that a potential outcome of this atmospheric evolution is the formation of helium-dominated atmospheres. The hydrodynamic escape rates of Neptune- and sub-Neptune-sized exoplanets are comparable to the diffusion-limited escape rate of hydrogen, and therefore the escape is heavily affected by diffusive separation between hydrogen and helium. A helium atmosphere can thus be formed -from a primordial hydrogen-helium atmosphere-via atmospheric hydrodynamic escape from the planet. The helium atmosphere has very different abundances of major carbon and oxygen species from those of a hydrogen atmosphere, leading to distinctive transmission and thermal emission spectral features. In particular, the hypothesis of a helium-dominated atmosphere can explain the thermal emission spectrum of GJ 436b, a warm Neptune- sized exoplanet, while also being consistent with the transmission spectrum. This model atmosphere contains trace amounts of hydrogen, carbon, and oxygen, with the predominance of CO over CH4 as the main form of carbon. With our atmospheric evolution model, we find that if the mass of the initial atmosphere envelope is 10-3 planetary mass, hydrodynamic escape can reduce the hydrogen abundance in the atmosphere by several orders of magnitude in similar to 10 billion years. Observations of exoplanet transits may thus detect signatures of helium atmospheres and probe the evolutionary history of small exoplanets. C1 [Hu, Renyu; Yung, Yuk L.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Hu, Renyu; Yung, Yuk L.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Seager, Sara] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA. RP Hu, RY (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. EM renyu.hu@jpl.nasa.gov FU NASA through Hubble Fellowship - Space Telescope Science Institute [51332]; NASA [NAS 5-26555]; NAI Virtual Planetary Laboratory grant NASA [NNX09AB72G] FX We appreciate comments on the manuscript made by members of the Yuk Yung research group at the California Institute of Technology. R.H. thanks Robert Johnson, Jeffrey Linsky, and Edwin Kite for helpful discussion. This work has utilized the MUSCLES M dwarf UV radiation database. Support for this work was provided by NASA through Hubble Fellowship grant #51332 awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS 5-26555. Y.L.Y. and R.H. (in the later phase of this work) were supported in part by an NAI Virtual Planetary Laboratory grant NASA grant NNX09AB72G to the California Institute of Technology. Part of the research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. NR 92 TC 9 Z9 9 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 1 PY 2015 VL 807 IS 1 AR 8 DI 10.1088/0004-637X/807/1/8 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO1VX UT WOS:000358945200008 ER PT J AU Janches, D Swarnalingam, N Plane, JMC Nesvorny, D Feng, W Vokrouhlicky, D Nicolls, MJ AF Janches, D. Swarnalingam, N. Plane, J. M. C. Nesvorny, D. Feng, W. Vokrouhlicky, D. Nicolls, M. J. TI RADAR DETECTABILITY STUDIES OF SLOW AND SMALL ZODIACAL DUST CLOUD PARTICLES. II. A STUDY OF THREE RADARS WITH DIFFERENT SENSITIVITY SO ASTROPHYSICAL JOURNAL LA English DT Article DE meteorites, meteors, meteoroids; zodiacal dust ID HEAD ECHO OBSERVATIONS; METEOR OBSERVATIONS; MU RADAR; ARECIBO; IONIZATION; MODEL AB The sensitivity of radar systems to detect different velocity populations of the incoming micrometeoroid flux is often the first argument considered to explain disagreements between models of the Near-Earth dust environment and observations. Recently, this was argued by Nesvorny et al. to support the main conclusions of a Zodiacal Dust Cloud (ZDC) model which predicts a flux of meteoric material into the Earth's upper atmosphere mostly composed of small and very slow particles. In this paper, we expand on a new methodology developed by Janches et al. to test the ability of powerful radars to detect the meteoroid populations in question. In our previous work, we focused on Arecibo 430 MHz observations since it is the most sensitive radar that has been used for this type of observation to date. In this paper, we apply our methodology to two other systems, the 440 MHz Poker Flat Incoherent Scatter Radar and the 46.5 Middle and Upper Atmosphere radar. We show that even with the less sensitive radars, the current ZDC model over-predicts radar observations. We discuss our results in light of new measurements by the Planck satellite which suggest that the ZDC particle population may be characterized by smaller sizes than previously believed. We conclude that the solution to finding agreement between the ZDC model and sensitive high power and large aperture meteor observations must be a combination of a re-examination not only of our knowledge of radar detection biases, but also the physical assumptions of the ZDC model itself. C1 [Janches, D.; Swarnalingam, N.] NASA, Goddard Space Flight Ctr, Space Weather Lab, Greenbelt, MD 20771 USA. [Swarnalingam, N.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA. [Plane, J. M. C.; Feng, W.] Univ Leeds, Sch Chem, Leeds LS2 9JT, W Yorkshire, England. [Nesvorny, D.] SW Res Inst, Boulder, CO USA. [Vokrouhlicky, D.] Charles Univ Prague, Inst Astron, Prague, Czech Republic. [Nicolls, M. J.] SRI Int, Menlo Pk, CA 94025 USA. RP Janches, D (reprint author), NASA, Goddard Space Flight Ctr, Space Weather Lab, Mail Code 674, Greenbelt, MD 20771 USA. EM diego.janches@nasa.gov; nimalan.swarnalingam@nasa.gov; j.m.c.plane@leeds.ac.uk; davidn@boulder.swri.edu; w.feng@leeds.ac.uk; vokrouhl@cesnet.cz; Michael.Nicolls@sri.com RI Plane, John/C-7444-2015; Janches, Diego/D-4674-2012; FENG, WUHU/B-8327-2008 OI Plane, John/0000-0003-3648-6893; Janches, Diego/0000-0001-8615-5166; FENG, WUHU/0000-0002-9907-9120 FU NASA [12-PAST12-0007, 12-PATM12-0006]; NASA's Solar System Works; European Research Council [291332-CODITA]; Czech Grant Agency [P209-13-01308S]; Japanese Society for the Promotion of Science (JSPS) FX D.J. is supported by NASA awards 12-PAST12-0007 and 12-PATM12-0006. D.N. has been supported through NASA's Solar System Works. J.M.C.P. and W.F. are supported by the European Research Council (project number 291332-CODITA) and the work of D.V. was partly supported by the Czech Grant Agency (grant P209-13-01308S). The Arecibo Observatory is operated by SRI International under a cooperative agreement with the National Science Foundation. The Poker Flat Incoherent Scatter Radar (PFISR) is operated by SRI International on behalf of the US National Science Foundation under NSF Cooperative Agreement AGS-1133009. The MU radar system belongs to and is operated by the Research Institute of Sustainable Humanosphere (RISH), Kyoto University, Uji, Kyoto, Japan. D.J. is grateful to the Japanese Society for the Promotion of Science (JSPS) who supported his visit to the University of Kyoto, Japan, in 2009 under a short term fellowship, making the observations presented here and this study possible. The authors wish to thank Prof. T. Nakamura and Dr. J. Kero for useful discussion regarding the MU radar system. NR 28 TC 5 Z9 5 U1 3 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 JUL 1 PY 2015 VL 807 IS 1 AR 13 DI 10.1088/0004-637X/807/1/13 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO1VX UT WOS:000358945200013 ER PT J AU Kraus, AL Cody, AM Covey, KR Rizzuto, AC Mann, AW Ireland, MJ AF Kraus, Adam L. Cody, Ann Marie Covey, Kevin R. Rizzuto, Aaron C. Mann, Andrew W. Ireland, Michael J. TI THE MASS-RADIUS RELATION OF YOUNG STARS. I. USCO 5, AN M4.5 ECLIPSING BINARY IN UPPER SCORPIUS OBSERVED BY K2 SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: eclipsing; stars: evolution; stars: fundamental parameters; stars: individual (UScoCTIO 5); stars: low-mass; stars: pre-main sequence ID MAIN-SEQUENCE STARS; PICTORIS MOVING GROUP; ORION NEBULA CLUSTER; SOLAR-TYPE STARS; BROWN DWARFS; OB ASSOCIATION; EVOLUTIONARY MODELS; LIGHT CURVES; EFFECTIVE TEMPERATURE; CIRCUMBINARY DISK AB We present the discovery that UScoCTIO 5, a known spectroscopic binary in the Upper Scorpius star-forming region (P = 34 days, M-tot sin(i) = 0.64M(circle dot)), is an eclipsing system with both primary and secondary eclipses apparent in K2 light curves obtained during Campaign 2. We have simultaneously fit the eclipse profiles from the K2 light curves and the existing RV data to demonstrate that UScoCTIO 5 consists of a pair of nearly identical M4.5 stars with M-A = 0.329 +/- 0.002 M-circle dot, R-A = 0.834 +/- 0.006 R-circle dot, M-B = 0.317 +/- 0.002 M-circle dot, and R-B = 0.810 +/- 0.006 R-circle dot. The radii are broadly consistent with pre-main-sequence ages predicted by stellar evolutionary models, but none agree to within the uncertainties. All models predict systematically incorrect masses at the 25%-50% level for the HR diagram position of these mid-M dwarfs, suggesting significant modifications to mass-dependent outcomes of star and planet formation. The form of the discrepancy for most model sets is not that they predict luminosities that are too low, but rather that they predict temperatures that are too high, suggesting that the models do not fully encompass the physics of energy transport (via convection and/or missing opacities) and/or a miscalibration of the SpT-T-eff scale. The simplest modification to the models (changing T-eff to match observations) would yield an older age for this system, in line with the recently proposed older age of Upper Scorpius (tau similar to 11 Myr). C1 [Kraus, Adam L.; Rizzuto, Aaron C.; Mann, Andrew W.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Cody, Ann Marie] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Covey, Kevin R.] Western Washington Univ, Bellingham, WA 98225 USA. [Ireland, Michael J.] Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT 2611, Australia. RP Kraus, AL (reprint author), Univ Texas Austin, Dept Astron, RLM 15308, Austin, TX 78712 USA. OI Ireland, Michael/0000-0002-6194-043X; Covey, Kevin/0000-0001-6914-7797 FU NASA Science Mission directorate; W. M. Keck Foundation FX We thank T. Dupuy, K. Larson, G. Herczeg, A. Dotter, G. Feiden, and M. Bessel for helpful discussions, and J. Bento and R. Kuruwita for assisting with the WiFeS observations. We also thank the referee, Eric Mamajek, for providing an insightful and prompt critique that improved the quality of this work. This research was partially supported by an appointment to the NASA Postdoctoral Program at the Ames Research Center, administered by Oak Ridge Associated Universities through a contract with NASA. This paper includes data collected by the K2 mission. Funding for the K2 mission is provided by the NASA Science Mission directorate. The K2 data presented in this paper were obtained from the Mikulski Archive for Space Telescopes (MAST). This research also has made use of the Keck Observatory Archive (KOA), which is operated by the W. M. Keck Observatory and the NASA Exoplanet Science Institute (NExScI), under contract with the National Aeronautics and Space Administration. The archival Keck/HIRES observations herein were obtained at the W. M. Keck Observatory by PIs G. Basri, W. Sargent, and J. Kuhn. Keck is operated as a scientific partnership among the California Institute of Technology, the University of California and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community. The archival PIs were most fortunate to have the opportunity to conduct observations from this mountain. NR 106 TC 23 Z9 23 U1 1 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 1 PY 2015 VL 807 IS 1 AR 3 DI 10.1088/0004-637X/807/1/3 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO1VX UT WOS:000358945200003 ER PT J AU Law, CJ Bower, GC Burke-Spolaor, S Butler, B Lawrence, E Lazio, TJW Mattmann, CA Rupen, M Siemion, A VanderWiel, S AF Law, Casey J. Bower, Geoffrey C. Burke-Spolaor, Sarah Butler, Bryan Lawrence, Earl Lazio, T. Joseph W. Mattmann, Chris A. Rupen, Michael Siemion, Andrew VanderWiel, Scott TI A MILLISECOND INTERFEROMETRIC SEARCH FOR FAST RADIO BURSTS WITH THE VERY LARGE ARRAY SO ASTROPHYSICAL JOURNAL LA English DT Article DE instrumentation: interferometers; intergalactic medium; pulsars: general; radio continuum: general; surveys ID GAMMA-RAY BURSTS; COSMOLOGICAL DISTANCES; TRANSIENT DETECTION; MISSING BARYONS; PULSAR SURVEY; SCINTILLATION; DISCOVERIES; REDSHIFT; MERGERS AB We report on the first millisecond timescale radio interferometric search for the new class of transient known as fast radio bursts (FRBs). We used the Very Large Array (VLA) for a 166 hr, millisecond imaging campaign to detect and precisely localize an FRB. We observed at 1.4 GHz and produced visibilities with 5 ms time resolution over 256 MHz of bandwidth. Dedispersed images were searched for transients with dispersion measures from 0 to 3000 pc cm(-3). No transients were detected in observations of high Galactic latitude fields taken from 2013 September though 2014 October. Observations of a known pulsar show that images typically had a thermal-noise limited sensitivity of 120 mJy beam(-1) (8 sigma; Stokes I) in 5 ms and could detect and localize transients over a wide field of view. Our nondetection limits the FRB rate to less than 7 x 10(4) sky(-1) day(-1) (95% confidence) above a fluence limit of 1.5 Jy ms. The VLA rate limit is consistent with past estimates when published flux limits are recalculated with a homogeneous definition that includes effects of primary beam attenuation, dispersion, pulse width, and sky brightness. This calculation revises the FRB rate downward by a factor of 2, giving the VLA observations a roughly 50% chance of detecting a typical FRB, assuming a pulse width of 3 ms. A 95% confidence constraint would require 600 hr of similar VLA observing. Our survey also limits the repetition rate of an FRB to 2 times less than any known repeating millisecond radio transient. C1 [Law, Casey J.; Siemion, Andrew] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Law, Casey J.; Siemion, Andrew] Univ Calif Berkeley, Radio Astron Lab, Berkeley, CA 94720 USA. [Bower, Geoffrey C.] Acad Sinica, Inst Astron & Astrophys, Hilo, HI 96720 USA. [Burke-Spolaor, Sarah; Lazio, T. Joseph W.; Mattmann, Chris A.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Burke-Spolaor, Sarah; Butler, Bryan] Natl Radio Astron Observ, Socorro, NM 87801 USA. [Lawrence, Earl; VanderWiel, Scott] Los Alamos Natl Lab, Los Alamos, NM USA. [Rupen, Michael] NRC Herzberg, Penticton, BC, Canada. RP Law, CJ (reprint author), Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA. OI Law, Casey/0000-0002-4119-9963 FU University of California Office of the President under Lab Fees Research Program Award [237863]; Office of Science of the U.S. Department of Energy [DE-AC02-05CH11231] FX We thank the VLA staff, particularly Martin Pokorny, Ken Sowinski, Vivek Dhawan, James Robnett, and Joan Wrobel, for working tirelessly to support this challenging observing mode. Peter Williams contributed with wide-ranging Python expertise. This project was supported by the University of California Office of the President under Lab Fees Research Program Award 237863. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. 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. This research used resources of the National Energy Research Scientific Computing Center, a DOE Office of Science User Facility supported by the Office of Science of the U.S. Department of Energy under Contract No. DE-AC02-05CH11231. NR 43 TC 23 Z9 23 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 1 PY 2015 VL 807 IS 1 AR 16 DI 10.1088/0004-637X/807/1/16 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO1VX UT WOS:000358945200016 ER PT J AU Neufeld, DA Black, JH Gerin, M Goicoechea, JR Goldsmith, PF Gry, C Gupta, H Herbst, E Indriolo, N Lis, D Menten, KM Monje, R Mookerjea, B Persson, C Schilke, P Sonnentrucker, P Wolfire, MG AF Neufeld, David A. Black, John H. Gerin, Maryvonne Goicoechea, Javier R. Goldsmith, Paul F. Gry, Cecile Gupta, Harshal Herbst, Eric Indriolo, Nick Lis, Dariusz Menten, Karl M. Monje, Raquel Mookerjea, Bhaswati Persson, Carina Schilke, Peter Sonnentrucker, Paule Wolfire, Mark G. TI HERSCHEL OBSERVATIONS OF INTERSTELLAR CHLORONIUM. II. DETECTIONS TOWARD G29.96-0.02, W49N, W51, AND W3(OH), AND DETERMINATIONS OF THE ORTHO-TO-PARA AND (CI)-C-35/(CI)-C-37 ISOTOPIC SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrochemistry; ISM: abundances; ISM: clouds; ISM: molecules; molecular processes; submillimeter: ISM ID PARA RATIO; HYDROGEN-CHLORIDE; MOLECULAR CLOUDS; GALAXY; H2CL+; WATER; HIFI; H2O+; GAS; ABSORPTION AB We report additional detections of the chloronium molecular ion, H2Cl+, toward four bright submillimeter continuum sources: G29.96-0.02, W49N, W51, and W3(OH). With the use of the HIFI instrument on board the Herschel Space Observatory, we observed the 2(12)-1(01) transition of ortho-(H2Cl+)-Cl-35 at 781.627 GHz in absorption toward all four sources. Much of the detected absorption arises in diffuse foreground clouds that are unassociated with the background continuum sources and in which our best estimates of the N(H2Cl+)/N(H) ratio lie in the range (0.9-4.8) x 10(-9). These chloronium abundances relative to atomic hydrogen can exceed the predictions of current astrochemical models by up to a factor of 5. Toward W49N, we have also detected the 2(12)-1(01) transition of ortho-(H2Cl+)-Cl-37 at 780.053 GHz and the 1(11)-1(00) transition of para-(H2Cl+)-Cl-35 at 485.418 GHz. These observations imply (H2Cl+)-Cl-35/ (H2Cl+)-Cl-37 column density ratios that are consistent with the solar system Cl-35/Cl-37 isotopic ratio of 3.1, and chloronium ortho-to-para ratios consistent with 3, the ratio of spin statistical weights. C1 [Neufeld, David A.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Black, John H.; Persson, Carina] Chalmers, Dept Earth & Space Sci, Onsala, Sweden. [Gerin, Maryvonne; Lis, Dariusz] PSL Res Univ, CNRS, Observ Paris, LERMA,CNRS,UMR 8112, F-75014 Paris, France. [Gerin, Maryvonne] Univ Paris 06, Sorbonne Univ, LERMA, UMR 8112, F-75005 Paris, France. [Goicoechea, Javier R.] CSIC, ICMM, Grp Astrofis Mol, E-28049 Madrid, Spain. [Goldsmith, Paul F.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Gry, Cecile] Aix Marseille Univ, CNRS, LAM, UMR 7326, F-13388 Marseille, France. [Gupta, Harshal; Lis, Dariusz; Monje, Raquel] CALTECH, Pasadena, CA 91125 USA. [Herbst, Eric] Univ Virginia, Dept Chem, Charlottesville, VA 22904 USA. [Herbst, Eric] Univ Virginia, Dept Phys & Astron, Charlottesville, VA 22904 USA. [Indriolo, Nick] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Menten, Karl M.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Mookerjea, Bhaswati] Tata Inst Fundamental Res, Bombay 400005, Maharashtra, India. [Schilke, Peter] Univ Cologne, Inst Phys 1, D-50937 Cologne, Germany. [Sonnentrucker, Paule] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Wolfire, Mark G.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. RP Neufeld, DA (reprint author), Johns Hopkins Univ, Dept Phys & Astron, 3400 N Charles St, Baltimore, MD 21218 USA. RI Goldsmith, Paul/H-3159-2016 FU NASA; MINECO [CSD2009-00038, AYA2009-07304, AYA2012-32032] FX HIFI has been designed and built by a consortium of institutes and university departments from across Europe, Canada and the United States under the leadership of SRON Netherlands Institute for Space Research, Groningen, The Netherlands and with major contributions from Germany, France and the United States. Consortium members are: Canada: CSA, U. Waterloo; France: CESR, LAB, LERMA, IRAM; Germany: KOSMA, MPIfR, MPS; Ireland, NUI Maynooth; Italy: ASI, IFSI-INAF, Osservatorio Astrofisico di Arcetri-INAF; Netherlands: SRON, TUD; Poland: CAMK, CBK; Spain: Observatorio Astronomico Nacional (IGN), Centro de Astrobiologia (CSIC-INTA). Sweden: Chalmers University of Technology-MC2, RSS & GARD; Onsala Space Observatory; Swedish National Space Board, Stockholm University-Stockholm Observatory; Switzerland: ETH Zurich, FHNW; USA: Caltech, JPL, NHSC. Support for this work was provided by NASA through an award issued by JPL/Caltech. J.R.G. thanks MINECO for funding support under grants CSD2009-00038, AYA2009-07304 and AYA2012-32032. NR 38 TC 4 Z9 4 U1 1 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 1 PY 2015 VL 807 IS 1 AR 54 DI 10.1088/0004-637X/807/1/54 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO1VX UT WOS:000358945200054 ER PT J AU Riebel, D Boyer, ML Srinivasan, S Whitelock, P Meixner, M Babler, B Feast, M Groenewegen, MAT Ita, Y Meade, M Shiao, B Whitney, B AF Riebel, D. Boyer, M. L. Srinivasan, S. Whitelock, P. Meixner, M. Babler, B. Feast, M. Groenewegen, M. A. T. Ita, Y. Meade, M. Shiao, B. Whitney, B. TI SAGE-VAR: AN INFRARED SURVEY OF VARIABILITY IN THE MAGELLANIC CLOUDS SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars: AGB and post-AGB; stars: mass-loss; stars: variables: general; stars: variables: Cepheids; Magellanic Clouds ID GRAVITATIONAL LENSING EXPERIMENT.; OGLE-III CATALOG; ASYMPTOTIC GIANT BRANCH; YOUNG STELLAR OBJECTS; PERIOD-LUMINOSITY RELATIONS; CARNEGIE HUBBLE PROGRAM; SPITZER-SPACE-TELESCOPE; MASS-LOSS RETURN; MU-M RANGE; AGB STARS AB We present the first results from the Surveying the Agents of Galaxy Evolution (SAGE)-Var program, a follow up to the Spitzer legacy program SAGE (Meixner et al.). We obtained four epochs of photometry at 3.6 and 4.5 mu m covering the bar of the LMC and the central region of the SMC in order to probe the variability of extremely red sources missed by variability surveys conducted at shorter wavelengths, and to provide additional epochs of observation for known variables. Our six total epochs of observations allow us to probe infrared (IR) variability on 15 different timescales ranging from similar to 20 days to similar to 5 yr. Out of a full catalog of 1 717 554 (LMC) and 457 760 (SMC) objects, we find 10 (LMC) and 6 (SMC) large amplitude Asymptotic Giant Branch (AGB) variables without optically measured variability owing to circumstellar dust obscuration. The catalog also contains multiple observations of known AGB variables, type I and II Cepheids, eclipsing variables, R CrB stars, and young stellar objects, which will be discussed in following papers. Here we present IR Period-Luminosity (PL) relations for classical Cepheids in the Magellanic Clouds, as well as improved PL relationships for AGB stars pulsating in the fundamental mode using mean magnitudes constructed from six epochs of observations. C1 [Riebel, D.] US Naval Acad, Dept Phys, Annapolis, MD 21402 USA. [Boyer, M. L.] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA. [Srinivasan, S.] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan. [Whitelock, P.; Feast, M.] Univ Cape Town, Dept Astron, Astrophys Cosmol & Grav Ctr, ZA-7701 Rondebosch, South Africa. [Whitelock, P.; Feast, M.] S African Astron Observ, ZA-7935 Observatory, South Africa. [Meixner, M.; Shiao, B.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Meixner, M.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Babler, B.; Meade, M.; Whitney, B.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. [Groenewegen, M. A. T.] Royal Observ Belgium, B-1180 Brussels, Belgium. [Ita, Y.] Tohoku Univ, Grad Sch Sci, Astron Inst, Aoba Ku, Sendai, Miyagi 9808578, Japan. RP Riebel, D (reprint author), US Naval Acad, Dept Phys, 572 C Holloway Rd, Annapolis, MD 21402 USA. EM riebel.d@gmail.com OI Babler, Brian/0000-0002-6984-5752 FU National Research Foundation (NRF) of South Africa; NASA [NAG5-12595]; Spitzer [NM0710076]; NASA Postdoctoral Program at the Goddard Space Flight Center; National Science Council; Ministry of Science and Technology [MOST103-2112-M-001-033-] FX This publication made use of the VizieR database operated by CDS, Strasbourg, France. M.W.F. and P.A.W. gratefully acknowledge the receipt of research grants from the National Research Foundation (NRF) of South Africa. Meixner acknowledges support from NASA NAG5-12595, and Spitzer contract NM0710076. 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. M.L.B. is supported by the NASA Postdoctoral Program at the Goddard Space Flight Center, administered by ORAU through a contract with NASA. S.S. acknowledges support from the National Science Council and the Ministry of Science and Technology in the form of grant MOST103-2112-M-001-033-. NR 55 TC 6 Z9 6 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 1 PY 2015 VL 807 IS 1 AR 1 DI 10.1088/0004-637X/807/1/1 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO1VX UT WOS:000358945200001 ER PT J AU Rodriguez, J Grinberg, V Laurent, P Bel, MC Pottschmidt, K Pooley, G Bodaghee, A Wilms, J Gouiffes, C AF Rodriguez, Jerome Grinberg, Victoria Laurent, Philippe Bel, Marion Cadolle Pottschmidt, Katja Pooley, Guy Bodaghee, Arash Wilms, Joern Gouiffes, Christian TI SPECTRAL STATE DEPENDENCE OF THE 0.4-2 MEV POLARIZED EMISSION IN CYGNUS X-1 SEEN WITH INTEGRAL/IBIS, AND LINKS WITH THE AMI RADIO DATA SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; black hole physics; stars: individual (Cyg X-1); X-rays: stars ID LONG-TERM VARIABILITY; GAMMA-RAY EMISSION; BLACK-HOLE BINARIES; GX 339-4; LOW/HARD STATE; HARD STATE; HDE 226868; COMPTONIZATION MODELS; COMPACT JETS; GRS 1915+105 AB Polarization of the greater than or similar to 400 keV hard tail of the microquasar Cygnus X-1 has been independently reported by INTEGRAL/Imager on Board the INTEGRAL Satellite (IBIS), and INTEGRAL/SPectrometer on INTEGRAL and interpreted as emission from a compact jet. These conclusions were, however, based on the accumulation of all INTEGRAL data regardless of the spectral state. We utilize additional INTEGRAL exposure accumulated until 2012 December, and include the AMI/Ryle (15 GHz) radio data in our study. We separate the observations into hard, soft, and intermediate/transitional states and detect radio emission from a compact jet in hard and intermediate states (IS), but not in the soft. The 10-400 keV INTEGRAL (JEM-X and IBIS) state resolved spectra are well modeled with thermal Comptonization and reflection components. We detect a hard tail in the 0.4-2 MeV range for the hard state only. We extract the state dependent polarigrams of Cyg X-1, which are all compatible with no or an undetectable level of polarization except in the 400-2000 keV range in the hard state where the polarization fraction is 75% +/- 32% and the polarization angle 40.degrees 0 +/- 14.degrees 3. An upper limit on the 0.4-2 MeV soft state polarization fraction is 70%. Due to the short exposure, we obtain no meaningful constraint for the IS. The likely detection of a >400 keV polarized tail in the hard state, together with the simultaneous presence of a radio jet, reinforce the notion of a compact jet origin of the >400 keV emission. C1 [Rodriguez, Jerome; Gouiffes, Christian] Univ Paris Diderot, CNRS, CEA DSM, IRFU SAp,Lab AIM,UMR 7158, F-91191 Gif Sur Yvette, France. [Grinberg, Victoria; Wilms, Joern] Univ Erlangen Nurnberg, Dr Karl Remeis Sternwarte & Erlangen Ctr Astropar, D-96049 Bamberg, Germany. [Grinberg, Victoria] MIT, Kavli Inst Astrophys, Cambridge, MA 02139 USA. [Laurent, Philippe] Univ Paris Diderot, CNRS, CEA DSM, Lab APC,UMR 7164, Paris, France. [Bel, Marion Cadolle] Excellence Cluster Univ, LMU, D-85748 Garching, Germany. [Pottschmidt, Katja] Univ Maryland Baltimore Cty, CRESST, Baltimore, MD 21250 USA. [Pottschmidt, Katja] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Pooley, Guy] Cavendish Lab, Astrophys, Cambridge CB3 0HE, England. [Bodaghee, Arash] Georgia Coll & State Univ, Dept Chem Phys & Astron, Milledgeville, GA 31061 USA. RP Rodriguez, J (reprint author), Univ Paris Diderot, CNRS, CEA DSM, IRFU SAp,Lab AIM,UMR 7158, F-91191 Gif Sur Yvette, France. EM jrodriguez@cea.fr RI Wilms, Joern/C-8116-2013; OI Wilms, Joern/0000-0003-2065-5410; Rodriguez, Jerome/0000-0002-4151-4468 FU French Research National Agency: CHAOS project [ANR-12-BS05-0009]; UnivEarthS Labex program of Sorbonne Paris Cite [ANR-10-LABX-0023, ANR-11-IDEX-0005-02]; Bundesministerium fur Wirtschaft und Technologie under Deutsches Zentrum fur Luft- und Raumfahrt [50 OR 1007, 50 OR 1411]; NASA through the Smithsonian Astrophysical Observatory (SAO) [SV3-73016]; NASA [NAS8-03060]; DFG Cluster of Excellence "Origin and Structure of the Universe"; ESA member states (Denmark); ESA member states (France); ESA member states (Germany); ESA member states (Italy); ESA member states (Switzerland); ESA member states (Spain) FX This paper is based on observations with INTEGRAL, an ESA project with instruments and a science data center funded by ESA member states (especially the PI countries: Denmark, France, Germany, Italy, Switzerland, Spain) and with the participation of Russia and the USA. We acknowledge S. Corbel, R. Belmont, J. Chenevez, and J. A. Tomsick for very fruitful discussions about several aspects presented in this paper. J.R. acknowledges funding support from the French Research National Agency: CHAOS project ANR-12-BS05-0009 (http://www.chaos-project.fr), and from the UnivEarthS Labex program of Sorbonne Paris Cite (ANR-10-LABX-0023 and ANR-11-IDEX-0005-02). This work has been partially funded by the Bundesministerium fur Wirtschaft und Technologie under Deutsches Zentrum fur Luft- und Raumfahrt Grants 50 OR 1007 and 50 OR 1411. V.G. acknowledges support provided by NASA through the Smithsonian Astrophysical Observatory (SAO) contract SV3-73016 to MIT for Support of the Chandra X-ray Center (CXC) and Science Instruments; CXC is operated by SAO for and on behalf of NASA under contract NAS8-03060. We acknowledge the support by the DFG Cluster of Excellence "Origin and Structure of the Universe." We are grateful for the support of M. Cadolle Bel through the Computational Center for Particle and Astrophysics (C2PAP). NR 69 TC 10 Z9 10 U1 3 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 1 PY 2015 VL 807 IS 1 AR 17 DI 10.1088/0004-637X/807/1/17 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO1VX UT WOS:000358945200017 ER PT J AU Sharykin, IN Kosovichev, AG Zimovets, IV AF Sharykin, I. N. Kosovichev, A. G. Zimovets, I. V. TI ENERGY RELEASE AND INITIATION OF A SUNQUAKE IN A C-CLASS FLARE SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun: chromosphere; Sun: flares; Sun: helioseismology; Sun: magnetic fields; Sun: X-rays, gamma rays ID SOLAR-FLARES; ELECTRIC-CURRENTS; SEISMIC SOURCES; RHESSI; RECONNECTION; SUN AB We present an analysis of the C7.0 solar flare from 2013 February 17, revealing a strong helioseismic response (sunquake) caused by a compact impact observed with the Helioseismic and Magnetic Imager on board the Solar Dynamics Observatory (SDO) in the low atmosphere. This is the weakest known C-class flare generating a sunquake event. To investigate the possible mechanisms of this event and understand the role of accelerated charged particles and photospheric electric currents, we use data from three space observatories: RHESSI, SDO, and Geostationary Operational Environmental Satellite. We find that the photospheric flare impact does not spatially correspond to the strongest hard X-ray emission source, but both of these events are parts of the same energy release. Our analysis reveals a close association of the flare energy release with a rapid increase in the electric currents and suggests that the sunquake initiation is unlikely to be caused by the impact of high-energy electrons, but may be associated with rapid current dissipation or a localized impulsive Lorentz force in the lower layers of the solar atmosphere. C1 [Sharykin, I. N.; Kosovichev, A. G.; Zimovets, I. V.] New Jersey Inst Technol, Big Bear Solar Observ, Big Bear City, CA 92314 USA. [Sharykin, I. N.; Zimovets, I. V.] Russian Acad Sci, Space Res Inst, Moscow 117997, Russia. [Kosovichev, A. G.] Stanford Univ, Stanford, CA 94305 USA. [Kosovichev, A. G.] NASA, Ames Res Ctr, Mountain View, CA 94035 USA. RP Sharykin, IN (reprint author), New Jersey Inst Technol, Big Bear Solar Observ, Big Bear City, CA 92314 USA. RI Zimovets, Ivan/E-4431-2017 OI Zimovets, Ivan/0000-0001-6995-3684 FU NASA grant [NNX14AB70G]; NJIT grant; RFBR grant [15-32-21078] FX The work was partially supported by NASA grant NNX14AB70G, an NJIT grant, and RFBR grant 15-32-21078. NR 31 TC 3 Z9 3 U1 1 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 1 PY 2015 VL 807 IS 1 AR 102 DI 10.1088/0004-637X/807/1/102 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO1VX UT WOS:000358945200102 ER PT J AU Zemko, P Mukai, K Orio, M AF Zemko, P. Mukai, K. Orio, M. TI SUZAKU OBSERVATION OF THE CLASSICAL NOVA V2491 Cyg IN QUIESCENCE SO ASTROPHYSICAL JOURNAL LA English DT Article DE novae, cataclysmic variables; X-rays: binaries; X-rays: individual (V2491 Cyg) ID MAGNETIC CATACLYSMIC VARIABLES; X-RAY OBSERVATIONS; INTERMEDIATE POLARS; RECURRENT NOVAE; WHITE-DWARFS; SPECTRAL-ANALYSIS; LIGHT-CURVE; V4743 SGR; POST-NOVA; PHASE AB We present the Suzaku XIS observation of V2491 Cyg (Nova Cyg 2008 No. 2) obtained in quiescence, more than two years after the outburst. The nova was detected as a very luminous source in a wide spectral range from soft to hard X-rays. A very soft blackbody-like component peaking at 0.5 keV indicates that we observe either remaining, localized hydrogen burning on the surface of the white dwarf, or accretion onto a magnetized polar cap. In the second case, V2491 Cyg is a candidate "soft intermediate polar." We obtained the best fit for the X-ray spectra with several components: two of thermal plasma, a blackbody and a complex absorber. The latter is typical of intermediate polars. The X-ray light curve shows a modulation with a period of similar to 38 minutes. The amplitude of this modulation is strongly energy-dependent and reaches a maximum in the range 0.8-2.0 keV. We discuss the origin of the X-ray emission and pulsations, and the likelihood of the intermediate polar scenario. C1 [Zemko, P.] Univ Padua, Dept Phys & Astron, I-35122 Padua, Italy. [Mukai, K.] NASA, CRESST, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Mukai, K.] NASA Goddard Space Flight Ctr, Xray Astrophys Lab, Greenbelt, MD 20771 USA. [Mukai, K.] Univ Maryland, Dept Phys, Baltimore, MD 21250 USA. [Orio, M.] INAF Osservatorio Padova, I-35122 Padua, Italy. [Orio, M.] Univ Wisconsin, Dept Astron, Madison, WI 53704 USA. RP Zemko, P (reprint author), Univ Padua, Dept Phys & Astron, Vicolo Osservatorio 3, I-35122 Padua, Italy. EM polina.zemko@studenti.unipd.it; koji.mukai@umbc.edu; marina.orio@oapd.inaf.it RI XRAY, SUZAKU/A-1808-2009 NR 49 TC 4 Z9 4 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 1 PY 2015 VL 807 IS 1 AR 61 DI 10.1088/0004-637X/807/1/61 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO1VX UT WOS:000358945200061 ER PT J AU Zhao, L DeVore, CR Antiochos, SK Zurbuchen, TH AF Zhao, L. DeVore, C. R. Antiochos, S. K. Zurbuchen, T. H. TI NUMERICAL SIMULATIONS OF HELICITY CONDENSATION IN THE SOLAR CORONA (vol 805, 61, 2015) SO ASTROPHYSICAL JOURNAL LA English DT Correction C1 [Zhao, L.; Zurbuchen, T. H.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48105 USA. [DeVore, C. R.; Antiochos, S. K.] NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Greenbelt, MD 20771 USA. RP Zhao, L (reprint author), Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48105 USA. OI Zhao, Liang/0000-0002-5975-7476 NR 1 TC 0 Z9 0 U1 1 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 1 PY 2015 VL 807 IS 1 AR 113 DI 10.1088/0004-637X/807/1/113 PG 1 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO1VX UT WOS:000358945200113 ER PT J AU Cahalan, JA Gasper, J Mondragon, J AF Cahalan, Jennifer A. Gasper, Jason Mondragon, Jennifer TI Catch estimation in the federal trawl fisheries off Alaska: a simulation approach to compare the statistical properties of three trip-specific catch estimators SO CANADIAN JOURNAL OF FISHERIES AND AQUATIC SCIENCES LA English DT Article ID BY-CATCH; DISCARD DATA; SEA; MANAGEMENT; IMPUTATION; VARIANCE; FLEET AB Quantifying catch has been recognized worldwide as a critical component in fisheries management. Assessment of discard is challenging because of the requirement for at-sea observation, which is both logistically difficult and costly to fishery agencies. Statistical estimators using robust sampling methods may yield accurate and imprecise estimates given the variability associated with many at-sea discard species and inability for agencies to obtain high sampling fractions. However, biased estimates occur if an inappropriate estimator is used. Using Alaska trawl fisheries as an example, we investigated the statistical properties and implementation issues for three commonly used estimators: the ratio estimator; a simple mean estimator; and a deterministic imputation method currently in use in federal fisheries off Alaska. We used a simulation approach to evaluate the performance of these estimators to estimate trip-specific catch. Several statistical properties were evaluated: bias of the estimators, variability of the estimators, and accuracy of the variance estimators. The simple mean estimator had the best performance for vessels landing catch at shoreside processors. The choice of estimator was less clear for vessels processing catch, owing to sensitivity associated with species composition and implementation issues for the simple mean and ratio estimators. C1 [Cahalan, Jennifer A.] Pacific States Marine Fishery Commiss, Seattle, WA 98115 USA. [Gasper, Jason; Mondragon, Jennifer] Natl Marine Fisheries Serv, Alaska Reg Off, Sustainable Fisheries Div, Juneau, AK 99801 USA. RP Cahalan, JA (reprint author), Pacific States Marine Fishery Commiss, 7600 Sand Point Way NE, Seattle, WA 98115 USA. EM jcahalan@psmfc.org NR 33 TC 0 Z9 0 U1 2 U2 8 PU CANADIAN SCIENCE PUBLISHING, NRC RESEARCH PRESS PI OTTAWA PA 65 AURIGA DR, SUITE 203, OTTAWA, ON K2E 7W6, CANADA SN 0706-652X EI 1205-7533 J9 CAN J FISH AQUAT SCI JI Can. J. Fish. Aquat. Sci. PD JUL PY 2015 VL 72 IS 7 BP 1024 EP 1036 DI 10.1139/cjfas-2014-0347 PG 13 WC Fisheries; Marine & Freshwater Biology SC Fisheries; Marine & Freshwater Biology GA CN7IM UT WOS:000358607900007 ER PT J AU Perry, LG Reynolds, LV Beechie, TJ Collins, MJ Shafroth, PB AF Perry, Laura G. Reynolds, Lindsay V. Beechie, Timothy J. Collins, Mathias J. Shafroth, Patrick B. TI Incorporating climate change projections into riparian restoration planning and design SO ECOHYDROLOGY LA English DT Article; Proceedings Paper CT Restoring Functional Riparian Ecosystems - Concepts and Applications Symposium at the 5th World Conference on Ecological Restoration CY 2013 CL Madison, WI DE climate adaptation; global change; hydrology; ecological restoration; riparian ecosystems; river management; streamflow ID WESTERN UNITED-STATES; FRESH-WATER ECOSYSTEMS; SCALE FLOW EXPERIMENTS; RIVER RESTORATION; ENVIRONMENTAL FLOWS; SOUTH-AFRICA; MANAGEMENT DECISIONS; STREAM RESTORATION; NORTH-AMERICA; PHENOLOGICAL RESPONSE AB Climate change and associated changes in streamflow may alter riparian habitats substantially in coming decades. Riparian restoration provides opportunities to respond proactively to projected climate change effects, increase riparian ecosystem resilience to climate change, and simultaneously address effects of both climate change and other human disturbances. However, climate change may alter which restoration methods are most effective and which restoration goals can be achieved. Incorporating climate change into riparian restoration planning and design is critical to long-term restoration of desired community composition and ecosystem services. In this review, we discuss and provide examples of how climate change might be incorporated into restoration planning at the key stages of assessing the project context, establishing restoration goals and design criteria, evaluating design alternatives, and monitoring restoration outcomes. Restoration planners have access to numerous tools to predict future climate, streamflow, and riparian ecology at restoration sites. Planners can use those predictions to assess which species or ecosystem services will be most vulnerable under future conditions, and which sites will be most suitable for restoration. To accommodate future climate and streamflow change, planners may need to adjust methods for planting, invasive species control, channel and floodplain reconstruction, and water management. Given the considerable uncertainty in future climate and streamflow projections, riparian ecological responses, and effects on restoration outcomes, planners will need to consider multiple potential future scenarios, implement a variety of restoration methods, design projects with flexibility to adjust to future conditions, and plan to respond adaptively to unexpected change. Copyright (c) 2015 John Wiley & Sons, Ltd. C1 [Perry, Laura G.; Reynolds, Lindsay V.] Colorado State Univ, Dept Biol, Ft Collins, CO 80523 USA. [Perry, Laura G.; Reynolds, Lindsay V.; Shafroth, Patrick B.] US Geol Survey, Ft Collins Sci Ctr, Ft Collins, CO USA. [Beechie, Timothy J.] NOAA, Natl Marine Fisheries Serv, NW Fisheries Sci Ctr, Fish Ecol Div, Seattle, WA 98115 USA. [Collins, Mathias J.] NOAA, Natl Marine Fisheries Serv, Restorat Ctr, Gloucester, MA USA. RP Perry, LG (reprint author), Colorado State Univ, Dept Biol, Ft Collins, CO 80523 USA. EM perryl@usgs.gov OI Collins, Mathias/0000-0003-4238-2038 NR 203 TC 3 Z9 3 U1 19 U2 102 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1936-0584 EI 1936-0592 J9 ECOHYDROLOGY JI Ecohydrology PD JUL PY 2015 VL 8 IS 5 SI SI BP 863 EP 879 DI 10.1002/eco.1645 PG 17 WC Ecology; Environmental Sciences; Water Resources SC Environmental Sciences & Ecology; Water Resources GA CN6IR UT WOS:000358538800011 ER PT J AU Chahat, N Tang, A Lee, C Sauleau, R Chattopadhyay, G AF Chahat, Nacer Tang, Adrian Lee, Choonsup Sauleau, Ronan Chattopadhyay, Goutam TI Efficient CMOS Systems With Beam-Lead Interconnects for Space Instruments SO IEEE TRANSACTIONS ON TERAHERTZ SCIENCE AND TECHNOLOGY LA English DT Article DE Off-chip antenna; millimeter-wave; submillimeter-wave; CMOS RFIC; on-chip antenna; transmitter; silicon micromachined antenna; beam-lead interconnection ID FLIP-CHIP INTERCONNECTS; WAVE TRANSCEIVERS; ANTENNA; PERFORMANCE; TECHNOLOGY; LENS; GHZ AB One of the main reasons CMOS systems has low overall efficiency is the performance of the on-chip antennas. With the recent severe metal density rules the problem has become more severe. Hence, antenna engineers need to move toward systems-in-package involving off-chip antenna solutions for high-efficiency performance. We introduce a new metal beam-lead interconnection technique which offers better matching control and lower loss at higher frequencies. The metal beam-lead interconnection appears to be a good solution for CMOS circuits at millimeter- and submillimeter-wave frequencies where off-chip connections are required. In this paper, we report performance of a 150 GHz CMOS transmitter which uses metal beam-lead interconnect between a high efficiency silicon antenna and a CMOS transmitter. C1 [Chahat, Nacer; Sauleau, Ronan] Univ Rennes 1, UMR CNRS 6164, Inst Elect & Telecommun Rennes, F-35042 Rennes, France. [Chahat, Nacer; Tang, Adrian; Lee, Choonsup; Chattopadhyay, Goutam] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Chahat, N (reprint author), Univ Rennes 1, UMR CNRS 6164, Inst Elect & Telecommun Rennes, F-35042 Rennes, France. EM nacer.e.chahat@jpl.nasa.gov FU Direction Generale de l'Armement (DGA), France FX The authors would like to acknowledge Direction Generale de l'Armement (DGA), France, for their support, and TSMC (R.O.C.) for excellent 65 nm foundry support. NR 31 TC 2 Z9 2 U1 0 U2 2 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 2156-342X J9 IEEE T THZ SCI TECHN JI IEEE Trans. Terahertz Sci. Technol. PD JUL PY 2015 VL 5 IS 4 BP 637 EP 644 DI 10.1109/TTHZ.2015.2446200 PG 8 WC Engineering, Electrical & Electronic; Optics; Physics, Applied SC Engineering; Optics; Physics GA CN8VF UT WOS:000358722600017 ER PT J AU Rai, MM AF Rai, Man Mohan TI Detached shear-layer instability and entrainment in the wake of a flat plate with turbulent separating boundary layers SO JOURNAL OF FLUID MECHANICS LA English DT Article DE shear layer turbulence; vortex shedding; wakes ID DIRECT NUMERICAL-SIMULATION; CIRCULAR-CYLINDER; MECHANISM; FLOW AB The near and very near wake of a flat plate with a circular trailing edge, with vigorous vortex shedding, is investigated with data from direct numerical simulations (DNS). Computations were performed for four different combinations of the Reynolds numbers based on plate thickness (D) and momentum thickness near the trailing edge (theta). Unlike the case of the cylinder, these Reynolds numbers are independent parameters for the flat plate. The objectives of the study are twofold, to investigate the entrainment process when the separating boundary layers are turbulent and to better understand the instability of the detached shear layers (DSLs). A visualization of the entrainment process, the effect of changing the ratio theta/D on entrainment and wake-velocity statistics, and a way of understanding entrainment in a phase-averaged sense via distributions of the turbulent transport rate are provided here. The discussion on shear-layer instability focuses on the role of log-layer eddies in the destabilization process, the effect of high-speed streaks in the turbulent boundary layer in the vicinity of the trailing edge on shear-layer vortex generation rates, and a relationship between the prevalence of shear-layer vortex generation and shedding phase that is a result of an interaction between the shedding process and the shear-layer instability mechanism. A power-law relationship between the ratio of shear-layer and shedding frequencies and the Reynolds numbers mentioned above is obtained. A discussion of the relative magnitudes of the exponents is provided. A second power-law relationship between shed-vortex strength and these two Reynolds numbers is also proposed. C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Rai, MM (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM man.m.rai@nasa.gov NR 20 TC 0 Z9 0 U1 2 U2 7 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 0022-1120 EI 1469-7645 J9 J FLUID MECH JI J. Fluid Mech. PD JUL PY 2015 VL 774 BP 5 EP 36 DI 10.1017/jfm.2015.254 PG 32 WC Mechanics; Physics, Fluids & Plasmas SC Mechanics; Physics GA CN8SQ UT WOS:000358713400006 ER PT J AU Hand, KP Carlson, RW AF Hand, Kevin P. Carlson, Robert W. TI Sea Salt on Europa SO NATURAL HISTORY LA English DT Article C1 [Hand, Kevin P.] CALTECH, NASA, Jet Prop Lab, Solar Syst Explorat Directorate, Pasadena, CA 91125 USA. [Carlson, Robert W.] JPL, Planetary Ices Grp, Planetary & Astrobiol Sect, Pasadena, CA USA. RP Hand, KP (reprint author), CALTECH, NASA, Jet Prop Lab, Solar Syst Explorat Directorate, Pasadena, CA 91125 USA. NR 0 TC 0 Z9 0 U1 3 U2 9 PU NATURAL HISTORY MAGAZINE PI NEW YORK PA 36 WEST 25TH STREET, FIFTH FLOOR, NEW YORK, NY 10010 USA SN 0028-0712 J9 NAT HIST JI Nat. Hist. PD JUL-AUG PY 2015 VL 123 IS 6 BP 34 EP 37 PG 4 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA CO1DQ UT WOS:000358893500015 ER PT J AU Rieke, GH Wright, GS Boker, T Bouwman, J Colina, L Glasse, A Gordon, KD Greene, TP Gudel, M Henning, T Justtanont, K Lagage, PO Meixner, ME Norgaard-Nielsen, HU Ray, TP Ressler, ME van Dishoeck, EF Waelkens, C AF Rieke, G. H. Wright, G. S. Boeker, T. Bouwman, J. Colina, L. Glasse, Alistair Gordon, K. D. Greene, T. P. Guedel, Manuel Henning, Th Justtanont, K. Lagage, P-O. Meixner, M. E. Norgaard-Nielsen, H-U. Ray, T. P. Ressler, M. E. van Dishoeck, E. F. Waelkens, C. TI The Mid-Infrared Instrument for the James Webb Space Telescope, I: Introduction SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article ID POPULATION III GALAXIES; STAR-FORMATION RATE; 1ST GALAXIES; RESOLUTION SPECTROMETER; GIANT PLANETS; HIGH-REDSHIFT; SUPER-EARTHS; ATMOSPHERES; PARAMETERS; LUMINOSITY AB MIRI (the Mid-Infrared Instrument for the James Webb Space Telescope [JWST]) operates from 5 to 28: 5 mu m and combines over this range: (1) unprecedented sensitivity levels; (2) subarcsecond angular resolution; (3) freedom from atmospheric interference; (4) the inherent stability of observing in space; and (5) a suite of versatile capabilities including imaging, low- and medium-resolution spectroscopy (with an integral field unit), and coronagraphy. We illustrate the potential uses of this unique combination of capabilities with various science examples: (1) imaging exoplanets; (2) transit and eclipse spectroscopy of exoplanets; (3) probing the first stages of star and planet formation, including identifying bioactive molecules; (4) determining star formation rates and mass growth as galaxies are assembled; and (5) characterizing the youngest massive galaxies. C1 [Rieke, G. H.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Wright, G. S.; Glasse, Alistair] Royal Observ, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland. [Boeker, T.] European Space Agcy, STScI, Baltimore, MD 21218 USA. [Bouwman, J.; Henning, Th] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Colina, L.] CSIC, INTA, Ctr Astrobiol, Dept Astrofis, Madrid 28850, Spain. [Gordon, K. D.; Meixner, M. E.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Gordon, K. D.] Univ Ghent, Sterrenkundig Observ, B-9000 Ghent, Belgium. [Greene, T. P.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Guedel, Manuel] Univ Vienna, Dept Astrophys, A-1180 Vienna, Austria. [Guedel, Manuel] Swiss Fed Inst Technol, Inst Astron, CH-8093 Zurich, Switzerland. [Justtanont, K.] Chalmers, Onsala Space Observ, S-43992 Onsala, Sweden. [Lagage, P-O.] Univ Paris Diderot, CNRS, Lab AIM Paris Saclay, CEA,IRFU,SAp, F-91191 Gif Sur Yvette, France. [Meixner, M. E.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Norgaard-Nielsen, H-U.] Tech Univ Denmark, Natl Space Inst, DTU Space, DK-2100 Copenhagen, Denmark. [Ray, T. P.] Dublin Inst Adv Studies, Sch Cosm Phys, Dublin 2, Ireland. [Ressler, M. E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [van Dishoeck, E. F.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Waelkens, C.] Katholieke Univ Leuven, Inst Astron, B-3001 Leuven, Belgium. RP Rieke, GH (reprint author), Univ Arizona, Steward Observ, 933 N Cherry Ave, Tucson, AZ 85721 USA. RI Guedel, Manuel/C-8486-2015; OI Guedel, Manuel/0000-0001-9818-0588; Ray, Tom/0000-0002-2110-1068; /0000-0003-1689-9201 NR 57 TC 19 Z9 18 U1 4 U2 19 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6280 EI 1538-3873 J9 PUBL ASTRON SOC PAC JI Publ. Astron. Soc. Pac. PD JUL PY 2015 VL 127 IS 953 BP 584 EP 594 DI 10.1086/682252 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO0MY UT WOS:000358847000002 ER PT J AU Wright, GS Wright, D Goodson, GB Rieke, GH Aitink-Kroes, G Amiaux, J Aricha-Yanguas, A Azzollini, R Banks, K Barrado-Navascues, D Belenguer-Davila, T Bloemmart, JADL Bouchet, P Brandl, BR Colina, L Detre, O Diaz-Catala, E Eccleston, P Friedman, SD Garcia-Marin, M Gudel, M Glasse, A Glauser, AM Greene, TP Groezinger, U Grundy, T Hastings, P Henning, T Hofferbert, R Hunter, F Jessen, NC Justtanont, K Karnik, AR Khorrami, MA Krause, O Labiano, A Lagage, PO Langer, U Lemke, D Lim, T Lorenzo-Alvarez, J Mazy, E McGowan, N Meixner, ME Morris, N Morrison, JE Muller, F Rgaard-Nielson, HUN Olofsson, G O'Sullivan, B Pel, JW Penanen, K Petach, MB Pye, JP Ray, TP Renotte, E Renouf, I Ressler, ME Samara-Ratna, P Scheithauer, S Schneider, A Shaughnessy, B Stevenson, T Sukhatme, K Swinyard, B Sykes, J Thatcher, J Tikkanen, T van Dishoeck, EF Waelkens, C Walker, H Wells, M Zhender, A AF Wright, G. S. Wright, David Goodson, G. B. Rieke, G. H. Aitink-Kroes, Gabby Amiaux, J. Aricha-Yanguas, Ana Azzollini, Ruyman Banks, Kimberly Barrado-Navascues, D. Belenguer-Davila, T. Bloemmart, J. A. D. L. Bouchet, Patrice Brandl, B. R. Colina, L. Detre, Oers Diaz-Catala, Eva Eccleston, Paul Friedman, Scott D. Garcia-Marin, Macarena Guedel, Manuel Glasse, Alistair Glauser, Adrian M. Greene, T. P. Groezinger, Uli Grundy, Tim Hastings, Peter Henning, Th Hofferbert, Ralph Hunter, Faye Jessen, N. C. Justtanont, K. Karnik, Avinash R. Khorrami, Mori A. Krause, Oliver Labiano, Alvaro Lagage, P. -O. Langer, Ulrich Lemke, Dietrich Lim, Tanya Lorenzo-Alvarez, Jose Mazy, Emmanuel McGowan, Norman Meixner, M. E. Morris, Nigel Morrison, Jane E. Mueller, Friedrich Rgaard-Nielson, H. -U. No Olofsson, Goran O'Sullivan, Brian Pel, J. -W. Penanen, Konstantin Petach, M. B. Pye, J. P. Ray, T. P. Renotte, Etienne Renouf, Ian Ressler, M. E. Samara-Ratna, Piyal Scheithauer, Silvia Schneider, Analyn Shaughnessy, Bryan Stevenson, Tim Sukhatme, Kalyani Swinyard, Bruce Sykes, Jon Thatcher, John Tikkanen, Tuomo van Dishoeck, E. F. Waelkens, C. Walker, Helen Wells, Martyn Zhender, Alex TI The Mid-Infrared Instrument for the James Webb Space Telescope, II: Design and Build SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article ID RESOLUTION SPECTROMETER; MIRI AB The Mid-InfraRed Instrument (MIRI) on the James Webb Space Telescope (JWST) provides measurements over the wavelength range 5 to 28: 5 mu m. MIRI has, within a single "package," four key scientific functions: photometric imaging, coronagraphy, single-source low-spectral resolving power (R similar to 100) spectroscopy, and medium-resolving power (R similar to 1500 to 3500) integral field spectroscopy. An associated cooler system maintains MIRI at its operating temperature of <6.7 K. This paper describes the driving principles behind the design of MIRI, the primary design parameters, and their realization in terms of the "as-built" instrument. It also describes the test program that led to delivery of the tested and calibrated Flight Model to NASA in 2012, and the confirmation after delivery of the key interface requirements. C1 [Wright, G. S.; Glasse, Alistair; Hastings, Peter; Wells, Martyn] Royal Observ, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland. [Wright, David] Stinger Ghaffarian Technol Inc, Greenbelt, MD 20770 USA. [Goodson, G. B.; Khorrami, Mori A.; Penanen, Konstantin; Ressler, M. E.; Schneider, Analyn; Sukhatme, Kalyani] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Rieke, G. H.; Morrison, Jane E.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Aitink-Kroes, Gabby] NOVA Opt IR Grp, NL-7990 AA Dwingeloo, Netherlands. [Amiaux, J.; Bouchet, Patrice; Lagage, P. -O.] Univ Paris Diderot, CNRS, CEA IRFU SAp, Lab AIM Paris Saclay, F-91191 Gif Sur Yvette, France. [Aricha-Yanguas, Ana; Belenguer-Davila, T.; Diaz-Catala, Eva] INTA, Madrid 28850, Spain. [Azzollini, Ruyman; Ray, T. P.] Dublin Inst Adv Studies, Sch Cosm Phys, Dublin 2, Ireland. [Azzollini, Ruyman; Barrado-Navascues, D.; Colina, L.] Ctr Astrobiol INTA CSIC, Dept Astrofis, Madrid 28850, Spain. [Banks, Kimberly] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Bloemmart, J. A. D. L.; Waelkens, C.] Katholieke Univ Leuven, Inst Astron, B-3001 Leuven, Belgium. [Bloemmart, J. A. D. L.] Vrije Univ Brussel, Astron & Astrophys Res Grp, Dept Phys & Astrophys, B-1050 Ixelles, Belgium. [Bloemmart, J. A. D. L.] Flemish Inst Technol Res VITO, B-2400 Mol, Belgium. [Brandl, B. R.; van Dishoeck, E. F.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Detre, Oers; Groezinger, Uli; Henning, Th; Hofferbert, Ralph; Krause, Oliver; Lemke, Dietrich; Mueller, Friedrich; Scheithauer, Silvia] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Eccleston, Paul; Grundy, Tim; Lim, Tanya; Morris, Nigel; Shaughnessy, Bryan; Swinyard, Bruce; Walker, Helen] Rutherford Appleton Lab, STFC, RAL Space, Didcot OX11 0QX, Oxon, England. [Friedman, Scott D.; Meixner, M. E.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Garcia-Marin, Macarena] Univ Cologne, Inst Phys 1, D-50937 Cologne, Germany. [Guedel, Manuel] Univ Vienna, Dept Astrophys, A-1180 Vienna, Austria. [Guedel, Manuel; Glauser, Adrian M.; Labiano, Alvaro] ETH, Inst Astron, CH-8093 Zurich, Switzerland. [Greene, T. P.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Hunter, Faye; McGowan, Norman; Renouf, Ian] Airbus Def & Space, Portsmouth PO3 5PU, Hants, England. [Jessen, N. C.; Rgaard-Nielson, H. -U. No] Tech Univ Denmark, Natl Space Inst DTU Space, DK-2100 Copenhagen, Denmark. [Justtanont, K.; Olofsson, Goran] Chalmers, Onsala Space Observ, S-43992 Onsala, Sweden. [Langer, Ulrich] RUAG Space, CH-8052 Zurich, Switzerland. [Lorenzo-Alvarez, Jose] Estec, NL-2201 AZ Noordwijk, Netherlands. [Mazy, Emmanuel; Renotte, Etienne] Ctr Spatial Liege, B-4031 Angleur, Belgium. [Meixner, M. E.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [O'Sullivan, Brian] Airbus Def & Space, Portsmouth PO3 5PU, Hants, England. [Pel, J. -W.] Univ Groningen, Kapteyn Inst, NL-9700 Groningen, Netherlands. [Petach, M. B.] Northrop Grumman Aerosp Syst, Redondo Beach, CA 90278 USA. [Pye, J. P.; Samara-Ratna, Piyal; Sykes, Jon; Tikkanen, Tuomo] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Stevenson, Tim] Jodrell Bank Observ, SKA Org, Macclesfield SK11 9DL, Cheshire, England. [Swinyard, Bruce] UCL, Dept Phys & Astron, London WC1E 6BT, England. [Thatcher, John] Airbus Def & Space, Stevenage SG1 2AS, Herts, England. [Zhender, Alex] Paul Scherrer Inst, CH-5232 Villigen, Switzerland. RP Wright, GS (reprint author), Royal Observ, UK Astron Technol Ctr, Blackford Hill, Edinburgh EH9 3HJ, Midlothian, Scotland. RI Guedel, Manuel/C-8486-2015; Barrado Navascues, David/C-1439-2017; OI Guedel, Manuel/0000-0001-9818-0588; Barrado Navascues, David/0000-0002-5971-9242; /0000-0003-1689-9201; Ray, Tom/0000-0002-2110-1068 NR 24 TC 10 Z9 10 U1 0 U2 6 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6280 EI 1538-3873 J9 PUBL ASTRON SOC PAC JI Publ. Astron. Soc. Pac. PD JUL PY 2015 VL 127 IS 953 BP 595 EP 611 DI 10.1086/682253 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO0MY UT WOS:000358847000003 ER PT J AU Bouchet, P Garcia-Marin, M Lagage, PO Amiaux, J Augueres, JL Bauwens, E Blommaert, JADL Chen, CH Detre, OH Dicken, D Dubreuil, D Galdemard, P Gastaud, R Glasse, A Gordon, KD Gougnaud, F Guillard, P Justtanont, K Krause, O Leboeuf, D Longval, Y Martin, L Mazy, E Moreau, V Olofsson, G Ray, TP Rees, JM Renotte, E Ressler, ME Ronayette, S Salasca, S Scheithauer, S Sykes, J Thelen, MP Wells, M Wright, D Wright, GS AF Bouchet, Patrice Garcia-Marin, Macarena Lagage, P. -O. Amiaux, Jerome Augueres, J. -L. Bauwens, Eva Blommaert, J. A. D. L. Chen, C. H. Detre, O. H. Dicken, Dan Dubreuil, D. Galdemard, Ph. Gastaud, R. Glasse, A. Gordon, K. D. Gougnaud, F. Guillard, Phillippe Justtanont, K. Krause, Oliver Leboeuf, Didier Longval, Yuying Martin, Laurant Mazy, Emmanuel Moreau, Vincent Olofsson, Goran Ray, T. P. Rees, J. -M. Renotte, Etienne Ressler, M. E. Ronayette, Samuel Salasca, Sophie Scheithauer, Silvia Sykes, Jon Thelen, M. P. Wells, Martyn Wright, David Wright, G. S. TI The Mid-Infrared Instrument for the James Webb Space Telescope, III: MIRIM, The MIRI Imager SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article ID SPECTROMETER; MICHELLE AB In this article, we describe the Mid-Infrared Imager Module (MIRIM), which provides broadband imaging in the 5-27 mu m wavelength range for the James Webb Space Telescope. The imager has a 0 ''.11 pixel scale and a total unobstructed view of 74 '' x 113 '' The remainder of its nominal 113 '' x 113 '' field is occupied by the coronagraphs and the low-resolution spectrometer. We present the instrument optical and mechanical design. We show that the test data, as measured during the test campaigns undertaken at CEA-Saclay, at the Rutherford Appleton Laboratory, and at the NASA Goddard Space Flight Center, indicate that the instrument complies with its design requirements and goals. We also discuss the operational requirements (multiple dithers and exposures) needed for optimal scientific utilization of the MIRIM. C1 [Bouchet, Patrice; Lagage, P. -O.; Amiaux, Jerome; Augueres, J. -L.; Dicken, Dan; Dubreuil, D.; Galdemard, Ph.; Moreau, Vincent; Ronayette, Samuel] Univ Paris Diderot, CNRS, CEA IRFU SAp, Lab AIM Paris Saclay, F-91191 Gif Sur Yvette, France. [Garcia-Marin, Macarena] Univ Cologne, Inst Phys 1, D-50937 Cologne, Germany. [Bauwens, Eva; Blommaert, J. A. D. L.] Katholieke Univ Leuven, Inst Astron, B-3001 Leuven, Belgium. [Blommaert, J. A. D. L.] Vrije Univ Brussel, Dept Phys & Astrophys, B-1050 Ixelles, Belgium. [Blommaert, J. A. D. L.] Flemish Inst Technol Res VITO, B-2400 Mol, Belgium. [Chen, C. H.; Gordon, K. D.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Detre, O. H.; Krause, Oliver; Scheithauer, Silvia] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Gastaud, R.; Gougnaud, F.; Leboeuf, Didier] CEA Saclay, DSM Irfu SIS, F-91191 Gif Sur Yvette, France. [Glasse, A.; Wells, Martyn; Wright, G. S.] Royal Observ, STFC, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland. [Gordon, K. D.] Univ Ghent, Sterrenkundig Observ, Ghent, Belgium. [Guillard, Phillippe; Longval, Yuying] Univ Paris 11, CNRS, UMR 8617, Inst Astrophys Spatiale, F-91405 Orsay, France. [Justtanont, K.; Olofsson, Goran] Chalmers, Onsala Space Observ, S-43992 Onsala, Sweden. [Martin, Laurant] Univ Aix Marseille, LAM, CNRS, UMR 7326, F-13388 Marseille, France. [Mazy, Emmanuel; Renotte, Etienne] Ctr Spatial Liege, B-4031 Angleur, Belgium. [Ray, T. P.] Dublin Inst Adv Studies, Sch Cosm Phys, Dublin 2, Ireland. [Rees, J. -M.] Univ Paris Diderot, Univ Paris 06, CNRS, LESIA,Observ Paris Meudon, F-92195 Meudon, France. [Ressler, M. E.; Thelen, M. P.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Salasca, Sophie] Ctr Etud Cadarache, CEA IRFM SIPP GIPM, F-13108 St Paul Les Durance, France. [Sykes, Jon] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Wright, David] Stinger Ghaffarian Technol Inc, Greenbelt, MD 20770 USA. RP Bouchet, P (reprint author), Univ Paris Diderot, CNRS, CEA IRFU SAp, Lab AIM Paris Saclay, F-91191 Gif Sur Yvette, France. EM Patrice.Bouchet@cea.fr OI /0000-0003-1689-9201; Ray, Tom/0000-0002-2110-1068 NR 16 TC 13 Z9 12 U1 0 U2 4 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6280 EI 1538-3873 J9 PUBL ASTRON SOC PAC JI Publ. Astron. Soc. Pac. PD JUL PY 2015 VL 127 IS 953 BP 612 EP 622 DI 10.1086/682254 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO0MY UT WOS:000358847000004 ER PT J AU Kendrew, S Scheithauer, S Bouchet, P Amiaux, J Azzollini, R Bouwman, J Chen, CH Dubreuil, D Fischer, S Glasse, A Greene, TP Lagage, PO Lahuis, F Ronayette, S Wright, D Wright, GS AF Kendrew, Sarah Scheithauer, Silvia Bouchet, Patrice Amiaux, Jerome Azzollini, Ruyman Bouwman, Jeroen Chen, C. H. Dubreuil, D. Fischer, Sebastian Glasse, Alistair Greene, T. P. Lagage, P-O. Lahuis, Fred Ronayette, Samuel Wright, David Wright, G. S. TI The Mid-Infrared Instrument for the James Webb Space Telescope, IV: The Low-Resolution Spectrometer SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article ID CALIBRATION AB The low-resolution spectrometer of the MIRI, which forms part of the imager module, will provide R similar to 100 long-slit and slitless spectroscopy from 5 to 12 mu m. The design is optimized for observations of compact sources, such as exoplanet host stars. We provide here an overview of the design of the LRS, and its performance as measured during extensive test campaigns, examining in particular the delivered image quality, dispersion, and resolving power, as well as spectrophotometric performance, flatfield accuracy, and the effects of fringing. We describe the operational concept of the slitless mode, which is optimally suited to transit spectroscopy of exoplanet atmospheres. The LRS mode of the MIRI was found to perform consistently with its requirements and goals. C1 [Kendrew, Sarah] Univ Oxford, Dept Phys, Oxford OX1 3RH, England. [Kendrew, Sarah; Scheithauer, Silvia; Bouwman, Jeroen] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Kendrew, Sarah; Lahuis, Fred] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Bouchet, Patrice; Amiaux, Jerome; Dubreuil, D.; Lagage, P-O.; Ronayette, Samuel] Univ Paris Diderot, CEA, IRFU, Lab AIM Paris Saclay,SAp,CNRS, F-91191 Gif Sur Yvette, France. [Azzollini, Ruyman] Dublin Inst Adv Studies, Sch Cosm Phys, Dublin 2, Ireland. [Azzollini, Ruyman] CSIC, INTA, Ctr Astrobiol, Dept Astrofis, Madrid 28850, Spain. [Chen, C. H.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Fischer, Sebastian] Deutsch Zentrum Luft & Raumfahrt DLR, D-53227 Bonn, Germany. [Fischer, Sebastian] Univ Cologne, Inst Phys 1, D-50937 Cologne, Germany. [Glasse, Alistair; Wright, G. S.] Royal Observ, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland. [Greene, T. P.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Lahuis, Fred] SRON Groningen Landleven, NL-9747 AD Groningen, Netherlands. [Wright, David] Stinger Ghaffarian Technol Inc, Greenbelt, MD 20770 USA. RP Kendrew, S (reprint author), Univ Oxford, Dept Phys, Denys Wilkinson Bldg,Keble Rd, Oxford OX1 3RH, England. EM sarah.kendrew@astro.ox.ac.uk NR 18 TC 15 Z9 14 U1 1 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6280 EI 1538-3873 J9 PUBL ASTRON SOC PAC JI Publ. Astron. Soc. Pac. PD JUL PY 2015 VL 127 IS 953 BP 623 EP 632 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO0MY UT WOS:000358847000005 ER PT J AU Boccaletti, A Lagage, PO Baudoz, P Beichman, C Bouchet, P Cavarroc, C Dubreuil, D Glasse, A Glauser, AM Hines, DC Lajoie, CP Lebreton, J Perrin, MD Pueyo, L Reess, JM Rieke, GH Ronayette, S Rouan, D Soummer, R Wright, GS AF Boccaletti, A. Lagage, P-O. Baudoz, P. Beichman, C. Bouchet, P. Cavarroc, C. Dubreuil, D. Glasse, Alistair Glauser, A. M. Hines, D. C. Lajoie, C-P. Lebreton, J. Perrin, M. D. Pueyo, L. Reess, J. M. Rieke, G. H. Ronayette, S. Rouan, D. Soummer, R. Wright, G. S. TI The Mid-Infrared Instrument for the James Webb Space Telescope, V: Predicted Performance of the MIRI Coronagraphs SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article ID 4-QUADRANT PHASE-MASK; BETA-PICTORIS; DEBRIS DISKS; EXOPLANETS; PLANETS AB The imaging channel on the Mid-Infrared Instrument (MIRI) is equipped with four coronagraphs that provide high-contrast imaging capabilities for studying faint point sources and extended emission that would otherwise be overwhelmed by a bright point-source in its vicinity. Such targets might include stars that are orbited by exoplanets and circumstellar material, mass-loss envelopes around post-main-sequence stars, the near-nuclear environments in active galaxies, and the host galaxies of distant quasars. This paper describes the coronagraphic observing modes of MIRI, as well as performance estimates based on measurements of the MIRI flight model during cryo-vacuum testing. A brief outline of coronagraphic operations is also provided. Finally, simulated MIRI coronagraphic observations of a few astronomical targets are presented for illustration. C1 [Boccaletti, A.; Baudoz, P.; Reess, J. M.; Rouan, D.] Univ Paris Diderot, Univ Paris 06, CNRS, LESIA,Observ Paris Meudon, F-92195 Meudon, France. [Lagage, P-O.; Bouchet, P.; Cavarroc, C.; Dubreuil, D.; Ronayette, S.] Univ Paris Diderot, Lab AIM Paris Saclay, CNRS, CEA,IRFU,SAp, F-91191 Gif Sur Yvette, France. [Beichman, C.; Lebreton, J.] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA. [Beichman, C.; Lebreton, J.] CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA. [Beichman, C.] CALTECH, Jet Prop Lab, Pasadena, CA 91107 USA. [Glasse, Alistair; Wright, G. S.] Royal Observ, UK Astron Technol Ctr, STFC, Edinburgh EH9 3HJ, Midlothian, Scotland. [Glauser, A. M.] Swiss Fed Inst Technol, Inst Astron, CH-8093 Zurich, Switzerland. [Hines, D. C.; Lajoie, C-P.; Perrin, M. D.; Pueyo, L.; Soummer, R.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Rieke, G. H.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. RP Boccaletti, A (reprint author), Univ Paris Diderot, Univ Paris 06, CNRS, LESIA,Observ Paris Meudon, 5 Pl Jules Janssen, F-92195 Meudon, France. NR 31 TC 10 Z9 10 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6280 EI 1538-3873 J9 PUBL ASTRON SOC PAC JI Publ. Astron. Soc. Pac. PD JUL PY 2015 VL 127 IS 953 BP 633 EP 645 DI 10.1086/682256 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO0MY UT WOS:000358847000006 ER PT J AU Wells, M Pel, JW Glasse, A Wright, GS Aitink-Kroes, G Azzollini, R Beard, S Brandl, BR Gallie, A Geers, VC Glauser, AM Hastings, P Henning, T Jager, R Justtanont, K Kruizinga, B Lahuis, F Lee, D Martinez-Delgado, I Martinez-Galarza, JR Meijers, M Morrison, JE Muller, F Nakos, T O'Sullivan, B Oudenhuysen, A Parr-Burman, P Pauwels, E Rohloff, RR Schmalzl, E Sykes, J Thelen, MP van Dishoeck, EF Vandenbussche, B Venema, LB Visser, H Waters, LBFM Wright, D AF Wells, Martyn Pel, J. -W. Glasse, Alistair Wright, G. S. Aitink-Kroes, Gabby Azzollini, Ruyman Beard, Steven Brandl, B. R. Gallie, Angus Geers, V. C. Glauser, A. M. Hastings, Peter Henning, Th. Jager, Rieks Justtanont, K. Kruizinga, Bob Lahuis, Fred Lee, David Martinez-Delgado, I. Martinez-Galarza, J. R. Meijers, M. Morrison, Jane E. Mueller, Friedrich Nakos, Thodori O'Sullivan, Brian Oudenhuysen, Ad Parr-Burman, P. Pauwels, Evert Rohloff, R. -R. Schmalzl, Eva Sykes, Jon Thelen, M. P. van Dishoeck, E. F. Vandenbussche, Bart Venema, Lars B. Visser, Huib Waters, L. B. F. M. Wright, David TI The Mid-Infrared Instrument for the James Webb Space Telescope, VI: The Medium Resolution Spectrometer SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article ID THERMAL-EXPANSION MEASUREMENTS; OPTICAL MATERIALS; TEMPERATURE AB We describe the design and performance of the Medium Resolution Spectrometer (MRS) for the JWST-MIRI instrument. The MRS incorporates four coaxial spectral channels in a compact opto-mechanical layout that generates spectral images over fields of view up to 7.7 x 7.7 '' in extent and at spectral resolving powers ranging from 1300 to 3700. Each channel includes an all-reflective integral field unit (IFU): an "image slicer" that reformats the input field for presentation to a grating spectrometer. Two 1024 x 1024 focal plane detector arrays record the output spectral images with an instantaneous spectral coverage of approximately one third of the full wavelength range of each channel. The full 5-28.5 mu m spectrum is then obtained by making three exposures using gratings and pass-band-determining filters that are selected using just two three-position mechanisms. The expected on-orbit optical performance is presented, based on testing of the MIRI Flight Model and including spectral and spatial coverage and resolution. The point spread function of the reconstructed images is shown to be diffraction limited and the optical transmission is shown to be consistent with the design expectations. C1 [Wells, Martyn; Glasse, Alistair; Wright, G. S.; Beard, Steven; Gallie, Angus; Hastings, Peter; Lee, David; Parr-Burman, P.] Royal Observ, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland. [Pel, J. -W.] Univ Groningen, Kapteyn Inst, NL-9700 Groningen, Netherlands. [Aitink-Kroes, Gabby; Jager, Rieks; Meijers, M.; Oudenhuysen, Ad; Pauwels, Evert] NOVA Opt IR Grp, NL-7990 AA Dwingeloo, Netherlands. [Azzollini, Ruyman; Geers, V. C.] Dublin Inst Adv Studies, Sch Cosm Phys, Dublin 2, Ireland. [Azzollini, Ruyman; Martinez-Delgado, I.] Ctr Astrobiol INTA CSIC, Dept Astrofis, Madrid 28850, Spain. [Brandl, B. R.; Lahuis, Fred; Martinez-Galarza, J. R.; Schmalzl, Eva; van Dishoeck, E. F.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Glauser, A. M.] ETH, Inst Astron, CH-8093 Zurich, Switzerland. [Henning, Th.; Mueller, Friedrich; Rohloff, R. -R.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Justtanont, K.] Chalmers, Onsala Space Observ, S-43992 Onsala, Sweden. [Kruizinga, Bob; Visser, Huib] TNO Opt, NL-2600 AD Delft, Netherlands. [Lahuis, Fred; Waters, L. B. F. M.] SRON Netherlands Inst Space Res, NL-3584 CA Utrecht, Netherlands. [Martinez-Galarza, J. R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Morrison, Jane E.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Nakos, Thodori] Sterrenkundig Observ UGent, B-9000 Ghent, Belgium. [O'Sullivan, Brian] Airbus Def & Space, Portsmouth PO3 5PU, Hants, England. [Pauwels, Evert; Venema, Lars B.] Pi Environm BV, NL-2221 AC Katwijk, Netherlands. [Sykes, Jon] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Thelen, M. P.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Vandenbussche, Bart] Inst Astron KU Leuven, B-3001 Leuven, Belgium. [Waters, L. B. F. M.] Univ Amsterdam, Sterrenkundig Inst Anton Pannekoek, NL-1098 Amsterdam, Netherlands. [Wright, David] Stinger Ghaffarian Technol Inc, Greenbelt, MD 20770 USA. RP Wells, M (reprint author), Royal Observ, UK Astron Technol Ctr, Blackford Hill, Edinburgh EH9 3HJ, Midlothian, Scotland. OI /0000-0003-1689-9201 NR 23 TC 14 Z9 13 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6280 EI 1538-3873 J9 PUBL ASTRON SOC PAC JI Publ. Astron. Soc. Pac. PD JUL PY 2015 VL 127 IS 953 BP 646 EP 664 DI 10.1086/682255 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO0MY UT WOS:000358847000007 ER PT J AU Rieke, GH Ressler, ME Morrison, JE Bergeron, L Bouchet, P Garcia-Marin, M Greene, TP Regan, MW Sukhatme, KG Walker, H AF Rieke, G. H. Ressler, M. E. Morrison, Jane E. Bergeron, L. Bouchet, Patrice Garcia-Marin, Macarena Greene, T. P. Regan, M. W. Sukhatme, K. G. Walker, Helen TI The Mid-Infrared Instrument for the James Webb Space Telescope, VII: The MIRI Detectors SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article ID ARRAY-CAMERA IRAC; MULTIBAND IMAGING PHOTOMETER; IN-FLIGHT PERFORMANCE; FOCAL-PLANE ARRAYS; REDUCTION ALGORITHMS; SPITZER; CALIBRATION AB The MIRI Si: As IBC detector arrays extend the heritage technology from the Spitzer IRAC arrays to a 1024 x 1024 pixel format. We provide a short discussion of the principles of operation, design, and performance of the individual MIRI detectors, in support of a description of their operation in arrays provided in an accompanying paper. We then describe modeling of their response. We find that electron diffusion is an important component of their performance, although it was omitted in previous models. Our new model will let us optimize the bias voltage while avoiding avalanche gain. It also predicts the fraction of the IR-active layer that is depleted (and thus contributes to the quantum efficiency) as signal is accumulated on the array amplifier. Another set of models accurately predicts the nonlinearity of the detector-amplifier unit and has guided determination of the corrections for nonlinearity. Finally, we discuss how diffraction at the interpixel gaps and total internal reflection can produce the extended cross-like artifacts around images with these arrays at short wavelengths, similar to 5 mu m. The modeling of the behavior of these devices is helping optimize how we operate them and also providing inputs to the development of the data pipeline. C1 [Rieke, G. H.; Morrison, Jane E.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Ressler, M. E.; Sukhatme, K. G.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Bergeron, L.; Regan, M. W.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Bouchet, Patrice] Univ Paris Diderot, Lab AIM Paris Saclay, CNRS, CEA,IRFU,SAp, F-91191 Gif Sur Yvette, France. [Garcia-Marin, Macarena] Univ Cologne, Inst Phys 1, D-50937 Cologne, Germany. [Greene, T. P.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Walker, Helen] Rutherford Appleton Lab, RALSpace, STFC, Didcot OX11 0QX, Oxon, England. RP Rieke, GH (reprint author), Univ Arizona, Steward Observ, 933 N Cherry Ave, Tucson, AZ 85721 USA. NR 36 TC 5 Z9 5 U1 1 U2 5 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6280 EI 1538-3873 J9 PUBL ASTRON SOC PAC JI Publ. Astron. Soc. Pac. PD JUL PY 2015 VL 127 IS 953 BP 665 EP 674 DI 10.1086/682257 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO0MY UT WOS:000358847000008 ER PT J AU Ressler, ME Sukhatme, KG Franklin, BR Mahoney, JC Thelen, MP Bouchet, P Colbert, JW Cracraft, M Dicken, D Gastaud, R Goodson, GB Eccleston, P Moreau, V Rieke, GH Schneider, A AF Ressler, M. E. Sukhatme, K. G. Franklin, B. R. Mahoney, J. C. Thelen, M. P. Bouchet, P. Colbert, J. W. Cracraft, Misty Dicken, D. Gastaud, R. Goodson, G. B. Eccleston, Paul Moreau, V. Rieke, G. H. Schneider, Analyn TI The Mid-Infrared Instrument for the James Webb Space Telescope, VIII: The MIRI Focal Plane System SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article ID COSMIC-RAY REJECTION; ARRAY CAMERA IRAC; SPITZER; CALIBRATION; DETECTORS; NOISE AB We describe the layout and unique features of the focal plane system for MIRI. We begin with the detector array and its readout integrated circuit (combining the amplifier unit cells and the multiplexer), the electronics, and the steps by which the data collection is controlled and the output signals are digitized and delivered to the JWST spacecraft electronics system. We then discuss the operation of this MIRI data system, including detector readout patterns, operation of subarrays, and data formats. Finally, we summarize the performance of the system, including remaining anomalies that need to be corrected in the data pipeline. C1 [Ressler, M. E.; Sukhatme, K. G.; Franklin, B. R.; Mahoney, J. C.; Thelen, M. P.; Goodson, G. B.; Schneider, Analyn] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Bouchet, P.; Dicken, D.; Moreau, V.] Univ Paris Diderot, Lab AIM Paris Saclay, CNRS, CEA,IRFU,SAp, F-91191 Gif Sur Yvette, France. [Cracraft, Misty] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Gastaud, R.] CEA Saclay, DSM, Irfu, SEDI, F-91191 Gif Sur Yvette, France. [Eccleston, Paul] Rutherford Appleton Lab, RAL Space, STFC, Didcot OX11 0QX, Oxon, England. [Rieke, G. H.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. RP Ressler, ME (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Michael.E.Ressler@jpl.nasa.gov OI Cracraft, Misty/0000-0002-7698-3002 NR 24 TC 10 Z9 9 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6280 EI 1538-3873 J9 PUBL ASTRON SOC PAC JI Publ. Astron. Soc. Pac. PD JUL PY 2015 VL 127 IS 953 BP 675 EP 685 DI 10.1086/682258 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO0MY UT WOS:000358847000009 ER PT J AU Glasse, A Rieke, GH Bauwens, E Garcia-Marin, M Ressler, ME Rost, S Tikkanen, TV Vandenbussche, B Wright, GS AF Glasse, Alistair Rieke, G. H. Bauwens, E. Garcia-Marin, Macarena Ressler, M. E. Rost, Steffen Tikkanen, T. V. Vandenbussche, B. Wright, G. S. TI The Mid-Infrared Instrument for the James Webb Space Telescope, IX: Predicted Sensitivity SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article AB We present an estimate of the performance that will be achieved during on-orbit operations of the JWST mid-infrared instrument, MIRI. The efficiency of the main imager and spectrometer systems in detecting photons from an astronomical target are presented, based on measurements at subsystem and instrument-level testing, with the end-to-end transmission budget discussed in some detail. The brightest target fluxes that can be measured without saturating the detectors are provided. The sensitivity for long-duration observations of faint sources is presented in terms of the target flux required to achieve a signal-to-noise ratio of 10 after a 10,000 s observation. The algorithms used in the sensitivity model are presented, including the understanding gained during testing of the MIRI flight model and flight-like detectors. C1 [Glasse, Alistair; Wright, G. S.] Royal Observ, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland. [Rieke, G. H.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Bauwens, E.; Vandenbussche, B.] Katholieke Univ Leuven, Inst Astron, B-3001 Leuven, Belgium. [Garcia-Marin, Macarena; Rost, Steffen] Univ Cologne, Inst Phys 1, D-50937 Cologne, Germany. [Ressler, M. E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Tikkanen, T. V.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. RP Glasse, A (reprint author), Royal Observ, UK Astron Technol Ctr, Blackford Hill, Edinburgh EH9 3HJ, Midlothian, Scotland. NR 13 TC 13 Z9 12 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 JUL PY 2015 VL 127 IS 953 BP 686 EP 695 DI 10.1086/682259 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO0MY UT WOS:000358847000010 ER PT J AU Gordon, KD Chen, CH Anderson, RE Azzollini, R Bergeron, L Bouchet, P Bouwman, J Cracraft, M Fischer, S Friedman, SD Garcia-Marin, M Glasse, A Glauser, AM Goodson, GB Greene, TP Hines, DC Khorrami, MA Lahuis, F Lajoie, CP Meixner, ME Morrison, JE O'Sullivan, B Pontoppidan, KM Regan, MW Ressler, ME Rieke, GH Scheithauer, S Walker, H Wright, GS AF Gordon, Karl D. Chen, C. H. Anderson, Rachel E. Azzollini, Ruyman Bergeron, L. Bouchet, Patrice Bouwman, Jeroen Cracraft, Misty Fischer, Sebastian Friedman, Scott D. Garcia-Marin, Macarena Glasse, Alistair Glauser, Adrian M. Goodson, G. B. Greene, T. P. Hines, Dean C. Khorrami, M. A. Lahuis, Fred Lajoie, C. -P. Meixner, M. E. Morrison, Jane E. O'Sullivan, Brian Pontoppidan, K. M. Regan, M. W. Ressler, M. E. Rieke, G. H. Scheithauer, Silvia Walker, Helen Wright, G. S. TI The Mid-Infrared Instrument for the James Webb Space Telescope, X: Operations and Data Reduction SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article ID GUIDE-STAR-CATALOG; OPTIMAL EXTRACTION; DETECTORS; ALGORITHM; SPECTRA; SPITZER AB We describe the operations concept and data reduction plan for the Mid-Infrared Instrument (MIRI) for the James Webb Space Telescope (JWST). The overall JWST operations concept is to use observation templates (OTs) to provide a straightforward and intuitive way for users to specify observations. MIRI has four OTs that correspond to the four observing modes: (1) imaging, (2) coronagraphy, (3) low-resolution spectroscopy, and (4) medium-resolution spectroscopy. We outline the user choices and expansion of these choices into detailed instrument operations. The data reduction plans for MIRI are split into three stages, where the specificity of the reduction steps to the observation type increases with stage. The reduction starts with integration ramps: stage 1 yields uncalibrated slope images; stage 2 calibrates the slope images; and then stage 3 combines multiple calibrated slope images into high-level data products (e.g., mosaics, spectral cubes, and extracted source information). Finally, we give examples of the data and data products that will be derived from each of the four different OTs. C1 [Gordon, Karl D.; Chen, C. H.; Anderson, Rachel E.; Bergeron, L.; Cracraft, Misty; Friedman, Scott D.; Hines, Dean C.; Lajoie, C. -P.; Meixner, M. E.; Pontoppidan, K. M.; Regan, M. W.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Gordon, Karl D.] Univ Ghent, Sterrenkundig Observ, Ghent, Belgium. [Azzollini, Ruyman] Dublin Inst Adv Studies, Sch Cosm Phys, Dublin 2, Ireland. [Azzollini, Ruyman] Ctr Astrobiol INTA CSIC, Dept Astrofis, Madrid 28850, Spain. [Bouchet, Patrice] Univ Paris Diderot, CNRS, CEA IRFU SAp, Lab AIM Paris Saclay, F-91191 Gif Sur Yvette, France. [Bouwman, Jeroen; Scheithauer, Silvia] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Fischer, Sebastian] Deutsch Zentrum Luft & Raumfahrt DLR, D-53227 Bonn, Germany. [Fischer, Sebastian; Garcia-Marin, Macarena] Univ Cologne, Inst Phys 1, D-50937 Cologne, Germany. [Glasse, Alistair; Wright, G. S.] Royal Observ, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland. [Glauser, Adrian M.] ETH, Inst Astron, CH-8093 Zurich, Switzerland. [Goodson, G. B.; Khorrami, M. A.; Ressler, M. E.] CALTECH, Jet Prop Lab, Pasadena, CA 91108 USA. [Greene, T. P.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Lahuis, Fred] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Lahuis, Fred] SRON Netherlands Inst Space Res, NL-9700 AV Groningen, Netherlands. [Meixner, M. E.] Johns Hopkins Univ, Dept Phys & Astron, Bloomberg Ctr 366, Baltimore, MD 21218 USA. [Morrison, Jane E.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [O'Sullivan, Brian] Airbus Def & Space, Stevenage SG1 2AS, Herts, England. [Walker, Helen] Rutherford Appleton Lab, STFC, RALSpace, Didcot OX11 0QX, Oxon, England. RP Gordon, KD (reprint author), Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA. OI Cracraft, Misty/0000-0002-7698-3002 NR 37 TC 6 Z9 5 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 JUL PY 2015 VL 127 IS 953 BP 696 EP 711 DI 10.1086/682260 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO0MY UT WOS:000358847000011 ER PT J AU Kepko, L McPherron, RL Amm, O Apatenkov, S Baumjohann, W Birn, J Lester, M Nakamura, R Pulkkinen, TI Sergeev, V AF Kepko, L. McPherron, R. L. Amm, O. Apatenkov, S. Baumjohann, W. Birn, J. Lester, M. Nakamura, R. Pulkkinen, T. I. Sergeev, V. TI Substorm Current Wedge Revisited SO SPACE SCIENCE REVIEWS LA English DT Review DE Substorm; Substorm current wedge; Field-aligned currents; Birkeland currents ID FIELD-ALIGNED CURRENTS; BURSTY BULK FLOWS; WESTWARD TRAVELING SURGE; POLAR MAGNETIC SUBSTORMS; STEADY MAGNETOSPHERIC CONVECTION; HEIGHT-INTEGRATED CONDUCTIVITY; RAPID FLUX TRANSPORT; CENTRAL PLASMA SHEET; EARTH CURRENT SHEET; HIGH-SPEED FLOWS AB Almost 40 years ago the concept of the substorm current wedge was developed to explain the magnetic signatures observed on the ground and in geosynchronous orbit during substorm expansion. In the ensuing decades new observations, including radar and low-altitude spacecraft, MHD simulations, and theoretical considerations have tremendously advanced our understanding of this system. The AMPTE/IRM, THEMIS and Cluster missions have added considerable observational knowledge, especially on the important role of fast flows in producing the stresses that generate the substorm current wedge. Recent detailed, multi-spacecraft, multi-instrument observations both in the magnetosphere and in the ionosphere have brought a wealth of new information about the details of the temporal evolution and structure of the current system. While the large-scale picture remains valid, the new details call for revision and an update of the original view. In this paper we briefly review the historical development of the substorm current wedge, review recent in situ and ground-based observations and theoretical work, and discuss the current active research areas. We conclude with a revised, time-dependent picture of the substorm current wedge that follows its evolution from the initial substorm flows through substorm expansion and recovery. C1 [Kepko, L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [McPherron, R. L.] Univ Calif Los Angeles, Los Angeles, CA USA. [Amm, O.] Finnish Meteorol Inst, FIN-00101 Helsinki, Finland. [Apatenkov, S.; Sergeev, V.] St Petersburg State Univ, St Petersburg 199034, Russia. [Baumjohann, W.; Nakamura, R.] Austrian Acad Sci, Space Res Inst, A-8010 Graz, Austria. [Birn, J.] Space Sci Inst, Boulder, CO USA. [Lester, M.] Univ Leicester, Leicester, Leics, England. [Pulkkinen, T. I.] Aalto Univ, Sch Elect Engn, Aalto, Finland. RP Kepko, L (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM larry.kepko@nasa.gov RI Apatenkov, Sergey/J-4899-2013; Nakamura, Rumi/I-7712-2013; Baumjohann, Wolfgang/A-1012-2010; Pulkkinen, Tuija/D-8403-2012; Sergeev, Victor/H-1173-2013; OI Nakamura, Rumi/0000-0002-2620-9211; Baumjohann, Wolfgang/0000-0001-6271-0110; Pulkkinen, Tuija/0000-0002-6317-381X; Sergeev, Victor/0000-0002-4569-9631; Apatenkov, Sergey/0000-0001-8959-3479 FU NASA [NNX13AD10G, NNX13AD21G]; NSF [1203711]; Los Alamos National Laboratory; STFC [ST/K001000/1]; Austrian Science Fund FWF [I429-N16, P23862-N16]; Academy of Finland [267073/2013]; RSF [14-17-00072] FX This publication is the result of "The Substorm Current Wedge" International Space Science Institute (ISSI) team selected in 2010, and we are grateful to ISSI for their hospitality during three in-person meetings, and for their support that made them possible. L. Kepko thanks the team for their dedication and patience as this review paper was written, and for their insight, knowledge and camaraderie. J. Birn acknowledges support through NASA grants NNX13AD10G and NNX13AD21G and NSF grant 1203711, as well as support from Los Alamos National Laboratory under a Guest Scientist agreement. M. Lester acknowledges support from STFC on grant ST/K001000/1. The work by R. Nakamura is supported by Austrian Science Fund FWF I429-N16 and P23862-N16. The work of T. Pulkkinen was supported by the Academy of Finland under the grant 267073/2013. V. Sergeev and S. Apatenkov thank support from RSF grant 14-17-00072. The team also thanks S. Cowley for providing helpful comments and suggestions. NR 227 TC 20 Z9 20 U1 1 U2 16 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-6308 EI 1572-9672 J9 SPACE SCI REV JI Space Sci. Rev. PD JUL PY 2015 VL 190 IS 1-4 BP 1 EP 46 DI 10.1007/s11214-014-0124-9 PG 46 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CN7HX UT WOS:000358606300001 ER PT J AU Teolis, BD Niemann, HB Waite, JH Gell, DA Perryman, RS Kasprzak, WT Mandt, KE Yelle, RV Lee, AY Pelletier, FJ Miller, GP Young, DT Bell, JM Magee, BA Patrick, EL Grimes, J Fletcher, GG Vuitton, V AF Teolis, B. D. Niemann, H. B. Waite, J. H. Gell, D. A. Perryman, R. S. Kasprzak, W. T. Mandt, K. E. Yelle, R. V. Lee, A. Y. Pelletier, F. J. Miller, G. P. Young, D. T. Bell, J. M. Magee, B. A. Patrick, E. L. Grimes, J. Fletcher, G. G. Vuitton, V. TI A Revised Sensitivity Model for Cassini INMS: Results at Titan SO SPACE SCIENCE REVIEWS LA English DT Review DE Cassini; Ion Neutral Mass Spectrometer; Cassini INMS; Instrument sensitivity; Titan; Saturn; Enceladus; Monte Carlo simulations; Gas conductance; Atmospheres; Attitude and articulation control; Thrusters; Spacecraft navigation; Instrument calibration ID MASS-SPECTROMETER MEASUREMENTS; UPPER-ATMOSPHERE; ION; CHEMISTRY; ESCAPE; DIFFUSION; METHANE; SYSTEMS AB Cassini Ion Neutral Mass Spectrometer (INMS) measurements from roughly a hundred Titan encounters over the Cassini mission yield neutral and ion densities systematically lower, by factors approximately 2 to 3, than estimates from several other spacecraft systems, including the Attitude and Articulation Control System, and Navigation system. In this paper we present a new INMS instrument sensitivity model, obtained by re-analyzing (1) the capture and transmission of neutral gas through the instrument, and (2) the detector gain reduction during pre-launch testing. By correcting for an under-estimation of gas leakage out of the instrument into space by the original calibration model, and adjusting for the gain change, the new model brings INMS densities into much closer agreement with the other Cassini systems. Accordingly, the INMS ion densities are revised upward by a constant detector sensitivity correction factor of 1.55 +/- 21 %, while the neutral sensitivities have a complex instrument pointing direction dependence, due (mostly) to the effect of the INMS vent and antechamber-to-closed source tube. In the special case of on-ram pointing the neutral densities are revised upward by a constant factor of 2.2 +/- 23 %. The corrected neutral and ion sensitivities given here are applicable to all previously published INMS results at Titan, Enceladus and elsewhere in the Saturn system. The new model gives reliable densities at high ram angles, in some cases above 90 degrees, thereby expanding the list of Titan flybys from which INMS densities may be extracted. We apply the model to obtain accurate densities from several off-ram Titan flybys which gave unusual neutral density vs. altitude profiles, or unreasonably high densities, with the original calibration. C1 [Teolis, B. D.; Waite, J. H.; Gell, D. A.; Perryman, R. S.; Mandt, K. E.; Miller, G. P.; Young, D. T.; Bell, J. M.; Magee, B. A.; Patrick, E. L.; Grimes, J.; Fletcher, G. G.] Southwest Res Inst, Div Space Sci, San Antonio, TX 78238 USA. [Niemann, H. B.; Kasprzak, W. T.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Yelle, R. V.] Univ Arizona, Dept Planetary Sci, Tucson, AZ 85721 USA. [Lee, A. Y.; Pelletier, F. J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Bell, J. M.] Natl Inst Aerosp, Hampton, VA 23666 USA. [Vuitton, V.] Univ Grenoble Alpes, CNRS, Inst Planetol & Astrophys Grenoble, F-38000 Grenoble, France. RP Teolis, BD (reprint author), Southwest Res Inst, Div Space Sci, 6220 Culebra Rd, San Antonio, TX 78238 USA. EM ben.teolis@swri.org OI Mandt, Kathleen/0000-0001-8397-3315 FU NASA; Jet Propulsion Laboratory under SwRI [1405853]; Centre National d'Etudes Spatiales Cassini Participating Scientist grant FX The INMS team acknowledges support from NASA and the Jet Propulsion Laboratory under SwRI subcontract 1405853. Support for this work was provided by a Centre National d'Etudes Spatiales Cassini Participating Scientist grant (to VV). Titan atmospheric densities estimated by the Attitude Control team represent work done by many individuals. T. Barber, T. Burk, A. Feldman, R.S. Lim, Siamak Sarani (formerly with JPL), E.K. Wang, J.L. Webster, and Genevie Yang, our colleagues at JPL, have provided us with invaluable support. We are especially grateful to co-author and Cassini INMS Co-Investigator Hasso Niemman, who passed away July 11, 2013. Hasso leaves a decades long legacy in the field of space-flight mass spectrometry, and his insight, analysis and detailed knowledge of the INMS were essential to this work. He will be missed by the team and the community. NR 51 TC 8 Z9 8 U1 5 U2 11 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-6308 EI 1572-9672 J9 SPACE SCI REV JI Space Sci. Rev. PD JUL PY 2015 VL 190 IS 1-4 BP 47 EP 84 DI 10.1007/s11214-014-0133-8 PG 38 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CN7HX UT WOS:000358606300002 ER PT J AU Smeltzer, CC Lukinova, NI Towcimak, ND Yan, XL Mann, DM Drohan, WN Griko, YV AF Smeltzer, Claudia C. Lukinova, Nina I. Towcimak, Nicole D. Yan, Xiaoli Mann, David M. Drohan, William N. Griko, Yuri V. TI Effect of gamma irradiation on the structural stability and functional activity of plasma-derived IgG SO BIOLOGICALS LA English DT Article DE Immunoglobulin; Radiation; Integrity; Stability ID INFRARED-SPECTROSCOPY; PATHOGEN INACTIVATION; SECONDARY STRUCTURE; CIRCULAR-DICHROISM; PROTEINS; GLOBULIN; RADIATION; SPECTRA; VIRUSES AB Plasma-originated commercial intravenous immunoglobulin, which is used for a variety of clinical purposes, has been studied to determine the effect of virus-inactivating doses of gamma irradiation on the structural-functional characteristics of the protein. A detailed analysis has been performed in response to a concern that the use of conventional gamma irradiation may damage biologically active proteins. The results demonstrate that although gamma irradiation of the IgG may have some impact on protein structure, the damage can be reduced or even prevented by appropriate irradiation conditions. At the virucidal dose of gamma irradiation (50 kGy) and a temperature of -80 degrees C, the integrity of the polypeptide chain of immunoglobulin and the secondary structure of IgG can be completely protected, while conformational changes in tertiary structure are significantly minimized to a level that preserves functional activity. The irradiated IgG retains specific antigen-binding properties and Fe-binding activity, indicating that the conformational integrity of the most important structural regions is not affected by gamma-irradiation. These results present strong evidence that gamma irradiation treatment can be effectively implemented for inactivation of pathogens in IgG solutions that are used for intravenous injection. Published by Elsevier Ltd on behalf of The International Alliance for Biological Standardization. C1 [Smeltzer, Claudia C.; Lukinova, Nina I.; Towcimak, Nicole D.; Yan, Xiaoli; Mann, David M.; Drohan, William N.; Griko, Yuri V.] Clearant Inc, Gaithersburg, MD 20878 USA. [Griko, Yuri V.] NASA Ames Res Ctr, Moffett Field, CA 94035 USA. RP Griko, YV (reprint author), NASA Ames, Space Biosci Div, Res Ctr, MS 261-3, Moffett Field, CA 94035 USA. EM Yuri.V.Griko@nasa.gov NR 30 TC 1 Z9 1 U1 0 U2 1 PU ACADEMIC PRESS LTD- ELSEVIER SCIENCE LTD PI LONDON PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND SN 1045-1056 EI 1095-8320 J9 BIOLOGICALS JI Biologicals PD JUL PY 2015 VL 43 IS 4 BP 242 EP 249 DI 10.1016/j.biologicals.2015.04.003 PG 8 WC Biochemical Research Methods; Biotechnology & Applied Microbiology; Pharmacology & Pharmacy SC Biochemistry & Molecular Biology; Biotechnology & Applied Microbiology; Pharmacology & Pharmacy GA CN4GM UT WOS:000358388600006 PM 25962339 ER PT J AU Greenberg, PS Fischer, DG AF Greenberg, Paul S. Fischer, David G. TI Detection of spacecraft fire signatures and post-fire aerosols Part I: Ground-based results SO FIRE SAFETY JOURNAL LA English DT Article DE Fire signatures; particles; detection; scattering ID FIREFIGHTERS AB Preventing fires in spacecraft and other remote platforms is an important facet of avoiding fires that potentially compromise missions, hardware, and crew. If a fire occurs, the objective is to detect the associated fire signatures at the earliest possible time from inception, thus minimizing propagation and collateral damage while providing maximal margin for suppression. The goal is to provide detection sensitivity without introducing spurious false alarms that compromise operations and trigger responsive abatement and containment provisions. A related issue in sealed, self-contained environments is post-fire clean up, and sensors to evaluate the environmental suitability in crewed quarters. In both situations, knowledge of the particulate and/or gaseous fire signatures as they occur under the unique combination of a reduced-gravity environment and materials typical of spaceflight applications is essential for the design of spacecraft fire detectors and habitat sensors. This paper describes recent ground and spaced-based data on fire signatures, and the response of a novel multi-channel optical scattering sensor. This detector, known as the Multi-Parameter Aerosol Scattering Sensor (MPASS), determines multiple moments of the aerosol distributions. The methodology for designing a sensor with the desired response function is discussed, as well as test results that demonstrate the performance of prototype devices. Published by Elsevier Ltd. C1 [Greenberg, Paul S.; Fischer, David G.] NASA, Glenn Res Ctr, Cleveland, OH 44136 USA. RP Greenberg, PS (reprint author), NASA, Glenn Res Ctr, 21000 Brookpk Rd, Cleveland, OH 44136 USA. EM Paul.S.Greenberg@nasa.gov NR 15 TC 0 Z9 0 U1 1 U2 2 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0379-7112 EI 1873-7226 J9 FIRE SAFETY J JI Fire Saf. J. PD JUL PY 2015 VL 75 BP 36 EP 44 DI 10.1016/j.firesaf.2015.04.004 PG 9 WC Engineering, Civil; Materials Science, Multidisciplinary SC Engineering; Materials Science GA CN2RC UT WOS:000358268600004 ER PT J AU Joy, KH Visscher, C Zolensky, ME Mikouchi, T Hagiya, K Ohsumi, K Kring, DA AF Joy, Katherine H. Visscher, Channon Zolensky, Michael E. Mikouchi, Takashi Hagiya, Kenji Ohsumi, Kazumasa Kring, David A. TI Identification of magnetite in lunar regolith breccia 60016: Evidence for oxidized conditions at the lunar surface SO METEORITICS & PLANETARY SCIENCE LA English DT Review ID APOLLO 16 REGOLITH; PLANETARY BASALTS; OXIDATION-STATE; VALENCE OXYBAROMETER; ISOTOPIC COMPOSITION; MAGMATIC VOLATILES; VOLCANIC GLASSES; MELT INCLUSIONS; OXYGEN FUGACITY; MOONS INTERIOR AB Lunar regolith breccias are temporal archives of magmatic and impact bombardment processes on the Moon. Apollo 16 sample 60016 is an ancient feldspathic regolith breccia that was converted from a soil to a rock at similar to 3.8Ga. The breccia contains a small (70x50m) rock fragment composed dominantly of an Fe-oxide phase with disseminated domains of troilite. Fragments of plagioclase (An(95-97)), pyroxene (En(74-75), Fs(21-22),Wo(3-4)), and olivine (Fo(66-67)) are distributed in and adjacent to the Fe-oxide. The silicate minerals have lunar compositions that are similar to anorthosites. Mineral chemistry, synchrotron X-ray absorption near edge spectroscopy (XANES) and X-ray diffraction (XRD) studies demonstrate that the oxide phase is magnetite with an estimated Fe3+/sigma Fe ratio of similar to 0.45. The presence of magnetite in 60016 indicates that oxygen fugacity during formation was equilibrated at, or above, the Fe-magnetite or wustite-magnetite oxygen buffer. This discovery provides direct evidence for oxidized conditions on the Moon. Thermodynamic modeling shows that magnetite could have been formed from oxidization-driven mineral replacement of Fe-metal or desulphurisation from Fe-sulfides (troilite) at low temperatures (<570 degrees C) in equilibrium with H2O steam/liquid or CO2 gas. Oxidizing conditions may have arisen from vapor transport during degassing of a magmatic source region, or from a hybrid endogenic-exogenic process when gases were released during an impacting asteroid or comet impact. C1 [Joy, Katherine H.; Kring, David A.] Lunar & Planetary Inst USRA, Ctr Lunar Sci & Explorat, Houston, TX 77058 USA. [Joy, Katherine H.; Kring, David A.] NASA Solar Syst Explorat Res Virtual Inst, New York, NY USA. [Joy, Katherine H.] Univ Manchester, Sch Earth Atmospher & Environm Sci, Manchester M13 9PL, Lancs, England. [Visscher, Channon] Dordt Coll, Sioux Ctr, IA 51250 USA. [Zolensky, Michael E.] NASA Johnson Space Ctr, ARES, Houston, TX 77058 USA. [Mikouchi, Takashi] Univ Tokyo, Grad Sch Sci, Dept Earth & Planetary Sci, Bunkyo Ku, Tokyo 1130033, Japan. [Hagiya, Kenji] Univ Hyogo, Grad Sch Sci, Kamigori, Hyogo 6781297, Japan. [Ohsumi, Kazumasa] Japan Synchrotron Radiat Res Inst JASRI, Sayo, Hyogo 6795198, Japan. RP Joy, KH (reprint author), Lunar & Planetary Inst USRA, Ctr Lunar Sci & Explorat, 3600 Bay Area Blvd, Houston, TX 77058 USA. EM katherine.joy@manchester.ac.uk OI Joy, Katherine/0000-0003-4992-8750 FU NASA Lunar Science Institute cooperative [NNA09DB33A]; Solar System Exploration Research Virtual Institute [NNA14AB07A]; Leverhulme Grant [2011-569]; Photon Factory research programs [2010G142, 2010G534] FX Thanks to Anne Peslier and Kent Ross for laboratory assistance at JSC. Thanks to CAPTEM for Apollo sample allocation. Thanks to Romain Tartese for helpful discussions. We appreciate the helpful reviews by Malcolm Rutherford and an anonymous reviewer and the editorial guidance of Randy Korotev to help improve this manuscript. This research was funded by NASA Lunar Science Institute cooperative NNA09DB33A and Solar System Exploration Research Virtual Institute cooperative agreement NNA14AB07A (David A. Kring PI). KHJ also acknowledges Leverhulme Grant 2011-569. SR-XRD and SR-XANES analyses were performed by the Photon Factory research programs #2010G142 and #2010G534, respectively. This is LPI contribution number 1837. NR 127 TC 4 Z9 4 U1 1 U2 12 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD JUL PY 2015 VL 50 IS 7 BP 1157 EP 1172 DI 10.1111/maps.12462 PG 16 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA CN0TH UT WOS:000358126000001 ER PT J AU Komatsu, M Fagan, TJ Mikouchi, T Petaev, MI Zolensky, ME AF Komatsu, Mutsumi Fagan, Timothy J. Mikouchi, Takashi Petaev, Michail I. Zolensky, Michael E. TI LIME silicates in amoeboid olivine aggregates in carbonaceous chondrites: Indicator of nebular and asteroidal processes SO METEORITICS & PLANETARY SCIENCE LA English DT Review ID AL-RICH INCLUSIONS; UNEQUILIBRATED ORDINARY CHONDRITES; OXYGEN ISOTOPIC COMPOSITIONS; EARLY SOLAR-SYSTEM; CV3 CHONDRITES; REFRACTORY INCLUSIONS; ALLENDE METEORITE; AQUEOUS ALTERATION; FAYALITIC OLIVINE; DARK INCLUSIONS AB MnO/FeO ratios in olivine from amoeboid olivine aggregates (AOAs) reflect conditions of nebular condensation and can be used in concert with matrix textures to compare metamorphic conditions in carbonaceous chondrites. LIME (low-iron, Mn-enriched) olivine was identified in AOAs from Y-81020 (CO3.05), Kaba (CV similar to 3.1), and in Y-86009 (CV3), Y-86751 (CV3), NWA 1152 (CR/CV3), but was not identified in AOAs from Efremovka (CV3.1-3.4) or Allende (CV>3.6). According to thermodynamic models of nebular condensation, LIME olivine is stable at lower temperatures than Mn-poor olivine and at low oxygen fugacities (dust enrichment <10x solar). Although this set of samples does not represent a single metamorphic sequence, the higher subtypes tend to have AOA olivine with lower Mn/Fe, suggesting that Mn/Fe decreases during parent body metamorphism. Y-81020 has the lowest subtype and most forsteritic AOA olivine (Fo(>95)) in our study, whereas Efremovka AOAs are slightly Fe-rich (Fo(>92)). AOA olivines from Kaba are mostly forsteritic, but rare Fe-rich olivine precipitated from an aqueous fluid. A combination of precipitation of Fe-rich olivine and diffusion of Fe into primary olivine grains resulted in iron-rich compositions (Fo(97-59)) in Allende AOAs. Variations from fine-grained, nonporous matrix toward higher porosity and coarser lath-like matrix olivine can be divided into six stages represented by (1) Y-81020, Efremovka, NWA 1152; (2) Y-86751 lithology B; (3) Y-86009; (4) Kaba; (5) Y-86751 lithology A; (6) Allende. These stages are inferred to represent general degree of metamorphism, although the specific roles of thermally driven grain growth and diffusion versus aqueous dissolution and precipitation remain uncertain. C1 [Komatsu, Mutsumi; Fagan, Timothy J.] Waseda Univ, Dept Earth Sci, Tokyo 1698050, Japan. [Komatsu, Mutsumi] Waseda Univ, Waseda Inst Adv Study, Tokyo 1698050, Japan. [Mikouchi, Takashi] Univ Tokyo, Dept Earth & Planetary Sci, Tokyo 1130033, Japan. [Petaev, Michail I.] Harvard Univ, Dept Earth & Planetary Sci, Cambridge, MA 02138 USA. [Petaev, Michail I.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Zolensky, Michael E.] NASA Johnson Space Ctr, ARES, Houston, TX 77058 USA. RP Komatsu, M (reprint author), Waseda Univ, Dept Earth Sci, Tokyo 1698050, Japan. EM komatsu@aoni.waseda.jp FU Japan Society for the Promotion of Science [24740358]; Waseda University Grant for Special Research Projects [2013A-097]; NASA Cosmochemistry Program; LARS Program FX We thank the Japanese National Institute of Polar Research (NIPR) for sample allocation of Antarctic meteorites and Efremovka. We thank Naoji Sugiura for discussions on condensation of AOAs. Parts of this work have been presented previously at meetings, where we have benefited from discussions with Alexander N. Krot, Denton Ebel, Herbert Palme, and Munir Humayun, among many others. This work was supported by Grant-in-Aid for JSPS Fellows, JSPS Grant-in-Aid for Young Scientists (B) from Japan Society for the Promotion of Science (no. 24740358 to MK), and a Waseda University Grant for Special Research Projects (2013A-097 to MK). MEZ acknowledges support from the NASA Cosmochemistry and LARS Programs. We thank Mike Weisberg, Dominik Hezel, and an anonymous reviewer for insightful reviews, and Gretchen Benedix for editorial guidance. NR 105 TC 1 Z9 1 U1 1 U2 4 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD JUL PY 2015 VL 50 IS 7 BP 1271 EP 1294 DI 10.1111/maps.12460 PG 24 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA CN0TH UT WOS:000358126000008 ER PT J AU Islam, T Srivastava, PK Dai, Q Gupta, M Zhuo, L AF Islam, Tanvir Srivastava, Prashant K. Dai, Qiang Gupta, Manika Zhuo, Lu TI An introduction to factor analysis for radio frequency interference detection on satellite observations SO METEOROLOGICAL APPLICATIONS LA English DT Article DE radio frequency interference; TRMM Microwave Imager; Advanced Microwave Scanning Radiometer-Earth Observing System; passive microwave radiometry; land surface retrieval; identification algorithm ID RADIOFREQUENCY INTERFERENCE; AMSR-E; SOIL-MOISTURE; MICROWAVE RADIOMETERS; SMOS SATELLITE; LAND; SCALE; TRMM AB A novel radio frequency interference (RFI) detection method is introduced for satellite-borne passive microwave radiometer observations. This method is based on factor analysis, in which variability among observed and correlated variables is described in terms of factors. In the present study, this method is applied to the Tropical Rainfall Measuring Mission (TRMM)/TRMM Microwave Imager (TMI) and Aqua/Advanced Microwave Scanning Radiometer-Earth Observing System (AMSR-E) satellite measurements over the land surface to detect the RFI signals, respectively, in 10 and 6GHz channels. The RFI detection results are compared with other traditional methods, such as spectral difference method and principal component analysis (PCA) method. It has been found that the newly proposed method is able to detect RFI signals in the C- and X-band radiometer channels as effectively as the conventional PCA method. C1 [Islam, Tanvir] NOAA, NESDIS, Ctr Satellite Applicat & Res, College Pk, MD USA. [Islam, Tanvir] Colorado State Univ, Cooperat Inst Res Atmosphere, Ft Collins, CO 80523 USA. [Islam, Tanvir; Srivastava, Prashant K.; Dai, Qiang; Zhuo, Lu] Univ Bristol, Dept Civil Engn, Bristol BS8 1TH, Avon, England. [Srivastava, Prashant K.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Srivastava, Prashant K.] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. [Gupta, Manika] Indian Inst Technol Delhi, Dept Civil Engn, Delhi, India. RP Islam, T (reprint author), NOAA, Ctr Satellite Applicat & Res STAR, Natl Environm Satellite Data & Informat Serv, College Pk, MD 20740 USA. EM tanvir.islam@noaa.gov OI Islam, Tanvir/0000-0003-2429-3074 NR 25 TC 2 Z9 2 U1 2 U2 9 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1350-4827 EI 1469-8080 J9 METEOROL APPL JI Meteorol. Appl. PD JUL PY 2015 VL 22 IS 3 BP 436 EP 443 DI 10.1002/met.1473 PG 8 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA CM7NZ UT WOS:000357882500015 ER PT J AU Fryauf, DM Norris, KJ Zhang, JC Wang, SY Kobayashi, NP AF Fryauf, David M. Norris, Kate J. Zhang, Junce Wang, Shih-Yuan Kobayashi, Nobuhiko P. TI Titanium oxide vertical resistive random-access memory device SO MICRO & NANO LETTERS LA English DT Article DE platinum; titanium compounds; semiconductor materials; metal-semiconductor-metal structures; resistive RAM; photolithography; electron beam deposition; vacuum deposition; atomic layer deposition; electrical resistivity; scanning electron microscopy; transmission electron microscopy; vertical resistive random-access memory switching devices; vertical three-dimensional structure; photolithography; electron-beam evaporation; electrodes; atomic layer deposition; dielectric layers; active switching cross-sectional area; nanosized devices; structural integrity; electrical characteristics; cross-sectional scanning electron microscopy; transmission electron microscopy; current-voltage characteristics; Pt-TiO2-Pt ID MEMRISTIVE DEVICES; MECHANISM; SYSTEMS AB Pt/TiO2/Pt vertical resistive random-access memory switching devices were fabricated in a vertical three-dimensional structure by combining conventional photolithography, electron-beam evaporation for electrodes and atomic layer deposition for dielectric layers. The active switching cross-sectional area was approximate to 0.02 mu m(2), which is comparable to nanosized devices that require more elaborative fabrication processes. Structural integrity and electrical characteristics of the vertical memory device were analysed by cross-sectional scanning, transmission electron microscopy and current-voltage characteristics. C1 [Fryauf, David M.; Norris, Kate J.; Zhang, Junce; Wang, Shih-Yuan; Kobayashi, Nobuhiko P.] Univ Calif Santa Cruz, Dept Elect Engn, Santa Cruz, CA 95064 USA. [Fryauf, David M.; Norris, Kate J.; Zhang, Junce; Wang, Shih-Yuan; Kobayashi, Nobuhiko P.] Univ Calif Santa Cruz, Ames Res Ctr, Nanostruct Energy Convers Technol & Res NECTAR Gr, Adv Studies Lab,NASA, Moffett Field, CA 94035 USA. RP Fryauf, DM (reprint author), Univ Calif Santa Cruz, Dept Elect Engn, Santa Cruz, CA 95064 USA. EM dfryauf@ucsc.edu FU National Science Foundation [DGE-0809125-006] FX The authors thank Hewlett-Packard Labs (Palo Alto, California) for their extensive assistance with fabrication and characterisation. They thank the MACS facility (Moffett Field, California) at Advanced Studies Laboratories, University of California Santa Cruz, and NASA Ames Research Center for continuous support on analytical equipment. This work was supported by the National Science Foundation Graduate Research Fellowship under grant no. DGE-0809125-006. NR 25 TC 0 Z9 0 U1 4 U2 19 PU INST ENGINEERING TECHNOLOGY-IET PI HERTFORD PA MICHAEL FARADAY HOUSE SIX HILLS WAY STEVENAGE, HERTFORD SG1 2AY, ENGLAND SN 1750-0443 J9 MICRO NANO LETT JI Micro Nano Lett. PD JUL PY 2015 VL 10 IS 7 BP 321 EP 323 DI 10.1049/mnl.2015.0021 PG 3 WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary SC Science & Technology - Other Topics; Materials Science GA CN4OU UT WOS:000358410500001 ER PT J AU Allwood, A AF Allwood, Abigail TI Mars 2020: Seeking Evidence of Life with Micro-XRF SO SPECTROSCOPY LA English DT Editorial Material AB The new Mars rover that is being developed for launch in 2020 by the National Aeronautics and Space Administration (NASA) will include a micro-X-ray fluorescence instrument called "PIXL," for Planetary Instrument for X-Ray Lithochemistry. PIXL will be mounted at the end of the rover's robotic arm and is designed to provide fine-scale identification of the elemental composition of rocks and soils on Mars. It is one of seven instruments on the Mars 2020 rover to seek evidence of past life on Mars. Abigail Allwood, the principal investigator for PIXL at NASA's Jet Propulsion Laboratory, in Pasadena, California, spoke to us about the development of the instrument and how it will be used. C1 NASA, Jet Prop Lab, PIXL, Pasadena, CA 91109 USA. RP Allwood, A (reprint author), NASA, Jet Prop Lab, PIXL, Pasadena, CA 91109 USA. NR 1 TC 2 Z9 2 U1 6 U2 26 PU ADVANSTAR COMMUNICATIONS INC PI DULUTH PA 131 W 1ST STREET, DULUTH, MN 55802 USA SN 0887-6703 J9 SPECTROSCOPY-US JI Spectroscopy PD JUL PY 2015 VL 30 IS 7 BP 22 EP + PG 2 WC Spectroscopy SC Spectroscopy GA CN3QE UT WOS:000358340600002 ER PT J AU Bondar, RL AF Bondar, Roberta L. TI Heaven on Earth SO ARCHITECTURAL DESIGN LA English DT Article DE Tree islands; Wood Buffalo National Park of Canada; Alberta; Carina Nebula; Hubble Space Telescope; Jupiter; Neptune; Moon; Earth; Mobius loop AB By 2050 we will have probed the universe even further, peeling back time as we strive for some sense of creation and meaning.' The world's first neurologist in space, Roberta L Bondar, who conducted international experiments on space mission STS 42 and has subsequently undertaken neurological research with NASA, urges us to look up and into space, which is set to remain a rich area of exploration, scientific investigation and wonder, with the discovery of new planets, light, patterns and materials on the not-so-distant horizon. C1 [Bondar, Roberta L.] NASA, Int Res Team, Washington, DC USA. NR 0 TC 0 Z9 0 U1 2 U2 4 PU WILEY PERIODICALS, INC PI SAN FRANCISCO PA ONE MONTGOMERY ST, SUITE 1200, SAN FRANCISCO, CA 94104 USA SN 0003-8504 EI 1554-2769 J9 ARCHIT DESIGN JI Archit. Des. PD JUL-AUG PY 2015 VL 85 IS 4 SI SI BP 98 EP 99 DI 10.1002/ad.1934 PG 2 WC Architecture SC Architecture GA CM6PI UT WOS:000357810500017 ER PT J AU Acikmese, B Bayard, DS AF Acikmese, Behcet Bayard, David S. TI Markov Chain Approach to Probabilistic Guidance for Swarms of Autonomous Agents SO ASIAN JOURNAL OF CONTROL LA English DT Article DE Swarm control; probabilistic methods; Markov chains ID COORDINATION; AVOIDANCE; SYSTEMS AB Motivated by biological swarms occurring in nature, there is recent interest in developing swarms comprised completely of engineered agents. The main challenge for developing swarm guidance laws compared to earlier formation flying and multi-vehicle coordination approaches is the sheer number of agents involved. While formation flying applications might involve up to 10 to 20 agents, swarms are desired to contain hundreds to many thousands of agents. In order to deal with the sheer size, the present paper makes a break with past deterministic methods, and considers the swarm as a statistical ensemble for which guidance can be performed from a probabilistic point of view. The probability-based approach takes advantage of the law of large numbers, and leads to computationally tractable and implementable swarm guidance laws. Agents following a probabilistic guidance algorithm make statistically independent probabilistic decisions based solely on their own state, which ultimately guides the swarm to the desired density distribution in the configuration space. Two different synthesis methods are introduced for designing probabilistic guidance laws. The first is based on the Metropolis-Hastings (M-H) algorithm, and the second is based on using linear matrix inequalities (LMIs). The M-H approach ensures convergent swarm behavior subject to enforced desired motion constraints, while the LMI approach additionally ensures exponential convergence with a prescribed decay rate, and allows minimization of a cost function that reflects fuel expenditure. In addition, both algorithms endow the swarm with the property of self-repair, and the capability to strictly enforce zero-probability keep-out regions. This last property requires a slight generalization of the Perron-Frobenius theory, and can be very useful in swarm applications that contain regions where no agents are allowed to go. Simulation examples are given to illustrate the methods and demonstrate desired properties of the guided swarm. C1 [Acikmese, Behcet] Univ Texas Austin, Aerosp Engn & Engn Mech, Austin, TX 78712 USA. [Bayard, David S.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Acikmese, B (reprint author), Univ Texas Austin, Aerosp Engn & Engn Mech, 210 E 24th St, Austin, TX 78712 USA. EM behcet@austin.utexas.edu; David.S.Bayard@jpl.nasa.gov FU National Aeronautics and Space Administration FX The authors gratefully acknowledge Fred Hadaegh, Lars Blackmore, Milan Mandic, Marco Quadrelli, and Edward Mettler of Jet Propulsion Laboratory and Marco Pavone of Stanford University for their valuable comments. We also acknowledge Mehran Mesbahi of University of Washington for the insights he provided on graph theory of multiagent networks. This research was partially performed at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. NR 47 TC 3 Z9 3 U1 0 U2 4 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1561-8625 EI 1934-6093 J9 ASIAN J CONTROL JI Asian J. Control PD JUL PY 2015 VL 17 IS 4 BP 1105 EP 1124 DI 10.1002/asjc.982 PG 20 WC Automation & Control Systems SC Automation & Control Systems GA CM8TJ UT WOS:000357974700001 ER PT J AU Rafelski, M Teplitz, HI Gardner, JP Coe, D Bond, NA Koekemoer, AM Grogin, N Kurczynski, P McGrath, EJ Bourque, M Atek, H Brown, TM Colbert, JW Codoreanu, A Ferguson, HC Finkelstein, SL Gawiser, E Giavalisco, M Gronwall, C Hanish, DJ Lee, KS Mehta, V De Mello, DF Ravindranath, S Ryan, RE Scarlata, C Siana, B Soto, E Voyer, EN AF Rafelski, Marc Teplitz, Harry I. Gardner, Jonathan P. Coe, Dan Bond, Nicholas A. Koekemoer, Anton M. Grogin, Norman Kurczynski, Peter McGrath, Elizabeth J. Bourque, Matthew Atek, Hakim Brown, Thomas M. Colbert, James W. Codoreanu, Alex Ferguson, Henry C. Finkelstein, Steven L. Gawiser, Eric Giavalisco, Mauro Gronwall, Caryl Hanish, Daniel J. Lee, Kyoung-Soo Mehta, Vihang De Mello, Duilia F. Ravindranath, Swara Ryan, Russell E. Scarlata, Claudia Siana, Brian Soto, Emmaris Voyer, Elysse N. TI UVUDF: ULTRAVIOLET THROUGH NEAR-INFRARED CATALOG AND PHOTOMETRIC REDSHIFTS OF GALAXIES IN THE HUBBLE ULTRA DEEP FIELD SO ASTRONOMICAL JOURNAL LA English DT Article DE cosmology: observations; galaxies: distances and redshifts; galaxies: evolution; galaxies: high-redshift; galaxies: photometry ID STAR-FORMING GALAXIES; LYMAN-BREAK GALAXIES; GOODS-SOUTH FIELD; SIMILAR-TO 2; CHARGE-TRANSFER INEFFICIENCY; REST-FRAME ULTRAVIOLET; UV LUMINOSITY FUNCTION; EXTRAGALACTIC LEGACY SURVEY; CONTINUUM ESCAPE FRACTION; FORMATION RATE DENSITY AB We present photometry and derived redshifts from up to eleven bandpasses for 9927 galaxies in the Hubble Ultra Deep field (UDF), covering an observed wavelength range from the near-ultraviolet (NUV) to the near-infrared (NIR) with Hubble Space Telescope observations. Our Wide Field Camera 3 (WFC3)/UV F225W, F275W, and F336W image mosaics from the ultra-violet UDF (UVUDF) imaging campaign are newly calibrated to correct for charge transfer inefficiency, and use new dark calibrations to minimize background gradients and pattern noise. Our NIR WFC3/IR image mosaics combine the imaging from the UDF09 and UDF12 campaigns with CANDELS data to provide NIR coverage for the entire UDF field of view. We use aperture-matched point-spread function corrected photometry to measure photometric redshifts in the UDF, sampling both the Lyman break and Balmer break of galaxies at z similar to 0.8-3.4, and one of the breaks over the rest of the redshift range. Our comparison of these results with a compilation of robust spectroscopic redshifts shows an improvement in the galaxy photometric redshifts by a factor of two in scatter and a factor three in outlier fraction (OLF) over previous UDF catalogs. The inclusion of the new NUV data is responsible for a factor of two decrease in the OLF compared to redshifts determined from only the optical and NIR data, and improves the scatter at z < 0.5 and at z > 2. The panchromatic coverage of the UDF from the NUV through the NIR yields robust photometric redshifts of the UDF, with the lowest OLF available. C1 [Rafelski, Marc; Gardner, Jonathan P.; Bond, Nicholas A.; De Mello, Duilia F.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Rafelski, Marc; Teplitz, Harry I.; Colbert, James W.; Hanish, Daniel J.] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA. [Coe, Dan; Koekemoer, Anton M.; Grogin, Norman; Bourque, Matthew; Brown, Thomas M.; Ferguson, Henry C.; Ravindranath, Swara; Ryan, Russell E.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Kurczynski, Peter; Gawiser, Eric] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. [McGrath, Elizabeth J.] Colby Coll, Dept Phys & Astron, Waterville, ME 04901 USA. [Atek, Hakim] EPFL, Lab Astrophys, Observatoire, CH-1290 Sauverny, Switzerland. [Codoreanu, Alex] Swinburne Univ Technol, Ctr Astrophys & Supercomputing, Hawthorn, Vic 3122, Australia. [Finkelstein, Steven L.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Giavalisco, Mauro] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. [Gronwall, Caryl] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Gronwall, Caryl] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA. [Lee, Kyoung-Soo] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. [Mehta, Vihang; Scarlata, Claudia] Univ Minnesota, Sch Phys & Astron, Minnesota Inst Astrophys, Minneapolis, MN 55455 USA. [De Mello, Duilia F.; Soto, Emmaris] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA. [Siana, Brian] Univ Calif Riverside, Dept Phys & Astron, Riverside, CA 92521 USA. [Voyer, Elysse N.] Aix Marseille Univ, CNRS, LAM, UMR 7326, F-13388 Marseille, France. RP Rafelski, M (reprint author), NASA, Goddard Space Flight Ctr, Code 665, Greenbelt, MD 20771 USA. EM marc.a.rafelski@nasa.gov OI Koekemoer, Anton/0000-0002-6610-2048; Brown, Thomas/0000-0002-1793-9968 FU NASA through Space Telescope Science Institute [GO-12534]; NASA [NAS5-26555]; HST [GO-13389, GO-13309]; Harriett G. Jenkins Graduate Fellowship Program [NNX13AT09H] FX We would like to thank Sylvia Baggett and Jay Anderson at the Space Telescope Science Institute for their help with solving new calibration and CTE challenges in the Epoch 3 NUV data. We thank Gabe Brammer, Kate Whitaker, Chun Ly, and Daniel Angerhausen for useful discussions. We also thank the referee, Dr. Michael Drinkwater, for his helpful comments. Support for HST Program GO-12534 was provided by NASA through grants from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. M.R. also acknowledges support from an appointment to the NASA Postdoctoral Program at Goddard Space Flight Center, as well as support from HST GO-13389 and HST GO-13309. E.S. acknowledges support from the Harriett G. Jenkins Graduate Fellowship Program, grant NNX13AT09H. NR 194 TC 20 Z9 20 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD JUL PY 2015 VL 150 IS 1 AR 31 DI 10.1088/0004-6256/150/1/31 PG 25 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CM5QU UT WOS:000357744400031 ER PT J AU Kadler, M Ojha, R AF Kadler, M. Ojha, R. CA TANAMI Collaboration TI TANAMI: Multiwavelength and multimessenger observations of active galaxies SO ASTRONOMISCHE NACHRICHTEN LA English DT Article; Proceedings Paper CT 87th Annual International Scientific Meeting of the Astronomische Gesellschaft CY SEP 22-22, 2014 CL Bamberg, GERMANY DE BL Lacertae objects: general; galaxies: active; galaxies: jets; neutrinos; quasars: general ID LARGE-AREA TELESCOPE; GAMMA-RAY EMISSION; SPECTRAL ENERGY-DISTRIBUTION; PARSEC-SCALE STRUCTURE; COMPACT RADIO-SOURCES; SOURCE PMN J1603-4904; BL LACERTAE OBJECTS; LINE SEYFERT 1; GALACTIC NUCLEI; RELATIVISTIC JETS AB Extragalactic jets launched from the immediate vicinity of supermassive black holes in radio-loud active galactic nuclei (AGN) are key objects in modern astronomy and astroparticle physics. AGN jets carry a fraction of the total gravitational energy released during the accretion of matter onto supermassive black holes and are prime suspects as possible sources of ultrahigh-energy cosmic rays and the recently detected extraterrestrial neutrinos at PeV energies. TANAMI (Tracking Active galactic Nuclei with Austral Milliarcsecond Interferometry) is a multiwavelength program monitoring AGN jets of the southern sky. It combines high-resolution imaging and spectral monitoring at radio wavelengths with higher-frequency observations at IR, optical/UV, X-ray, and -ray energies. We review recent results of the TANAMI program, highlighting AGN candidate neutrino-emitters in the error circles of the IceCube PeV neutrino events. ((c) 2015 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim) C1 [Kadler, M.] Inst Theoret Phys & Astrophys, D-97074 Wurzburg, Germany. [Ojha, R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Ojha, R.] Catholic Univ Amer, Washington, DC 20064 USA. [Ojha, R.] Univ Maryland Baltimore Cty, Baltimore, MD 21250 USA. RP Kadler, M (reprint author), Inst Theoret Phys & Astrophys, Emil Fischer Str 31, D-97074 Wurzburg, Germany. EM matthias.kadler@astro.uni-wuerzburg.de OI Kadler, Matthias/0000-0001-5606-6154 FU Commonwealth of Australia; AuScope Ltd under the National Collaborative Research Infrastructure Strategy (NCRIS), an Australian Commonwealth Government Programme FX The authors thank the rest of the TANAMI team for their manifold contributions to the overall program and for advise and comments on the manuscript. The Australia 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. This study made use of data collected through the AuScope initiative. AuScope Ltd is funded under the National Collaborative Research Infrastructure Strategy (NCRIS), an Australian Commonwealth Government Programme. NR 73 TC 6 Z9 6 U1 0 U2 2 PU WILEY-V C H VERLAG GMBH PI WEINHEIM PA POSTFACH 101161, 69451 WEINHEIM, GERMANY SN 0004-6337 EI 1521-3994 J9 ASTRON NACHR JI Astro. Nachr. PD JUL PY 2015 VL 336 IS 5 BP 499 EP 504 DI 10.1002/asna.201512186 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CM8ND UT WOS:000357957500011 ER PT J AU Holzmann, GJ AF Holzmann, Gerard J. TI Points of Truth SO IEEE SOFTWARE LA English DT Editorial Material C1 Jet Prop Lab, Pasadena, CA 91109 USA. RP Holzmann, GJ (reprint author), Jet Prop Lab, Pasadena, CA 91109 USA. EM gholzmann@acm.org NR 2 TC 0 Z9 0 U1 0 U2 0 PU IEEE COMPUTER SOC PI LOS ALAMITOS PA 10662 LOS VAQUEROS CIRCLE, PO BOX 3014, LOS ALAMITOS, CA 90720-1314 USA SN 0740-7459 EI 1937-4194 J9 IEEE SOFTWARE JI IEEE Softw. PD JUL-AUG PY 2015 VL 32 IS 4 BP 18 EP 21 PG 4 WC Computer Science, Software Engineering SC Computer Science GA CM4KK UT WOS:000357653200005 ER PT J AU Wrzesien, ML Pavelsky, TM Kapnick, SB Durand, MT Painter, TH AF Wrzesien, Melissa L. Pavelsky, Tamlin M. Kapnick, Sarah B. Durand, Michael T. Painter, Thomas H. TI Evaluation of snow cover fraction for regional climate simulations in the Sierra Nevada SO INTERNATIONAL JOURNAL OF CLIMATOLOGY LA English DT Article DE WRF; snow; mountain hydrology; regional climate ID ASSIMILATION SYSTEM NLDAS; WESTERN UNITED-STATES; CONVECTIVE PARAMETERIZATION; MODELING SYSTEM; SEASONAL SNOW; GRAIN-SIZE; LAND; PRECIPITATION; IMPLEMENTATION; TEMPERATURE AB Mountain snow cover plays an important role in regional climate due to its high albedo, its effects on atmospheric convection, and its influence on runoff. Snowpack water storage is also a critical water resource and understanding how it varies is of great social value. Models are often employed to reconstruct snowpack and explore and understand snow cover variability. Here, we use a new, accurate satellite-derived snow product to evaluate the ability of the Weather Research and Forecasting (WRF) regional climate model, combined with the Noah land surface model with multi-parameterization options (Noah-MP), to simulate snow cover fraction (SCF) and snow water equivalent (SWE) in a 3-km domain over the central Sierra Nevada. WRF/Noah-MP SWE simulations improve on previous versions of the Noah land surface model by removing an early bias in snow melt, though a 2-day positive melt bias in SWE timing remains significant at the 90% confidence level. In addition, WRF/Noah-MP identifies the areas where snow is present to within 94.3% and captures large-scale variability in SCF. Temporal root mean squared error (RMSE) of the domain-average SCF was 1938.6km(2) (24%). However, our study shows that WRF/Noah-MP struggles to simulate SCF at finer spatial scales. The parameterization for SCF fails to produce temporal variations in grid-scale SCF, and depletion occurs too rapidly. As a result, the WRF/Noah-MP SCF parameterization reduces to a binary function in mountain environments. Sensitivity tests show that adjustment of the parameterization may improve simulation of SCF during accumulation or melt but does not remove the bias for the entire snow season. Although WRF/Noah-MP accurately simulates the presence or absence of snow, high-resolution, reliable SCF estimates may only be attainable if snow depletion parameterizations are designed specifically for complex topographical areas. C1 [Wrzesien, Melissa L.; Durand, Michael T.] Ohio State Univ, Sch Earth Sci, Columbus, OH 43210 USA. [Wrzesien, Melissa L.; Pavelsky, Tamlin M.] Univ N Carolina, Dept Geol Sci, Chapel Hill, NC USA. [Kapnick, Sarah B.] Princeton Univ, Program Atmospher & Ocean Sci, Princeton, NJ 08544 USA. [Kapnick, Sarah B.] NOAA, Geophys Fluid Dynam Lab, Silver Spring, MD USA. [Durand, Michael T.] Ohio State Univ, Byrd Polar Res Ctr, Columbus, OH 43210 USA. [Painter, Thomas H.] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Wrzesien, ML (reprint author), Ohio State Univ, Sch Earth Sci, Columbus, OH 43210 USA. EM wrzesien.1@osu.edu RI Kapnick, Sarah/C-5209-2014; Painter, Thomas/B-7806-2016 OI Kapnick, Sarah/0000-0003-0979-3070; FU American Meteorological Society; NASA [NNX13AB63G]; NASA FX This work was supported in part by an American Meteorological Society Graduate Fellowship and NASA grant NNX13AB63G. Part of this work was performed at the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. We thank the Renaissance Computing Institute (RENCI) in Chapel Hill, NC for providing access to high-performance computing resources. We also thank two anonymous reviewers for their useful comments. NR 53 TC 4 Z9 4 U1 5 U2 30 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0899-8418 EI 1097-0088 J9 INT J CLIMATOL JI Int. J. Climatol. PD JUL PY 2015 VL 35 IS 9 BP 2472 EP 2484 DI 10.1002/joc.4136 PG 13 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA CM7RO UT WOS:000357894100020 ER PT J AU Salgi, P Balakotaiah, V Rame, E Motil, BJ AF Salgi, Paul Balakotaiah, Vemuri Rame, Enrique Motil, Brian J. TI Pulse properties in gas-liquid flow through randomly packed beds under microgravity conditions SO INTERNATIONAL JOURNAL OF MULTIPHASE FLOW LA English DT Article DE Packed beds; Gas-liquid flow; Pulse characteristics; Microgravity ID COCURRENT DOWNFLOW; HYDRODYNAMIC PROPERTIES; MAGNETIC EMULATION; ARTIFICIAL GRAVITY; PRESSURE-DROP; 2-PHASE FLOW; REACTORS; COLUMNS; REGIMES C1 [Salgi, Paul; Balakotaiah, Vemuri] Univ Houston, Dept Chem & Biomol Engn, Houston, TX 77004 USA. [Rame, Enrique] NASA, Natl Ctr Space Explorat & Res, Glenn Res Ctr, Cleveland, OH USA. [Motil, Brian J.] NASA, Glenn Res Ctr, Cleveland, OH USA. RP Salgi, P (reprint author), Univ Houston, Dept Chem & Biomol Engn, Houston, TX 77004 USA. EM psalgi@central.uh.edu FU NASA Glenn Research Center [NNX14AD28G] FX This work was supported by a grant from the NASA Glenn Research Center (Grant # NNX14AD28G). NR 22 TC 1 Z9 1 U1 3 U2 4 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0301-9322 EI 1879-3533 J9 INT J MULTIPHAS FLOW JI Int. J. Multiph. Flow PD JUL PY 2015 VL 73 BP 11 EP 16 DI 10.1016/j.ijmultiphaseflow.2015.02.020 PG 6 WC Mechanics SC Mechanics GA CN0HL UT WOS:000358094600003 ER PT J AU Zhang, J Lee, C Votava, P Lee, TJ Wang, S Sriram, V Saini, N Rao, P Nemani, R AF Zhang, Jia Lee, Chris Votava, Petr Lee, Tsengdar J. Wang, Shuai Sriram, Venkatesh Saini, Neeraj Rao, Pujita Nemani, Ramakrishna TI A Trust-Powered Technique to Facilitate Scientific Tool Discovery and Recommendation SO INTERNATIONAL JOURNAL OF WEB SERVICES RESEARCH LA English DT Article DE Knowledge-Social-Trust (KST) Network Model; Scientific Workflows; Social Networks; Trust-based Recommendation; Workflow Recommendation AB While the open science community engenders many similar scientific tools as services, how to differentiate them and help scientists select and reuse existing software services developed by peers remains a challenge. Most of the existing service discovery approaches focus on finding candidate services based on functional and non-functional requirements as well as historical usage analysis. Complementary to the existing methods, this paper proposes to leverage human trust to facilitate software service selection and recommendation. A trust model is presented that leverages the implicit human factor to help quantify the trustworthiness of candidate services. A hierarchical Knowledge-Social-Trust (KST(network model is established to extract hidden knowledge from various publication repositories (e.g., DBLP(and social networks (e.g., Twitter and DBLP). As a proof of concept, a prototyping service has been developed to help scientists evaluate and visualize trust of services. The performance factor is studied and experience is reported. C1 [Zhang, Jia; Lee, Chris] Carnegie Mellon Univ, Silicon Valley, CA 94027 USA. [Votava, Petr] NASA, Ames Res Ctr, Silicon Valley, CA USA. [Votava, Petr; Lee, Tsengdar J.] NASA Headquarters, Sci Mission Directorate, Washington, DC USA. [Wang, Shuai; Sriram, Venkatesh; Saini, Neeraj; Rao, Pujita] Carnegie Mellon Univ, Informat Networking Inst, Silicon Valley, CA USA. [Nemani, Ramakrishna] NASA, Ames Res Ctr, Ecol Forecasting Lab, Silicon Valley, CA USA. RP Zhang, J (reprint author), Carnegie Mellon Univ, Silicon Valley, CA 94027 USA. FU National Aeronautics and Space Administration [NASA NNX13AB38G] FX We appreciate Shrikant Adhikarla, Isaraporn Kulkumjon (Cherry), Matthew Schlau, and Divya Natesan, for their contribution to the earlier phase of this work. This work is partially supported by National Aeronautics and Space Administration, under grant NASA NNX13AB38G. NR 30 TC 0 Z9 0 U1 1 U2 5 PU IGI PUBL PI HERSHEY PA 701 E CHOCOLATE AVE, STE 200, HERSHEY, PA 17033-1240 USA SN 1545-7362 EI 1546-5004 J9 INT J WEB SERV RES JI Int. J. Web. Serv. Res. PD JUL-SEP PY 2015 VL 12 IS 3 BP 25 EP 47 DI 10.4018/IJWSR.2015070102 PG 23 WC Computer Science, Information Systems; Computer Science, Software Engineering SC Computer Science GA CN0AG UT WOS:000358073300002 ER PT J AU Andersen, DT McKay, CP Lagun, V AF Andersen, Dale T. McKay, Christopher P. Lagun, Victor TI Climate Conditions at Perennially Ice-Covered Lake Untersee, East Antarctica SO JOURNAL OF APPLIED METEOROLOGY AND CLIMATOLOGY LA English DT Article ID MCMURDO DRY VALLEYS; DRONNING MAUD LAND; CORELESS WINTER; FOEHN WINDS; HOARE; VARIABILITY; EVOLUTION; THICKNESS AB In November 2008 an automated meteorological station was established at Lake Untersee in East Antarctica, producing a 5-yr data record of meteorological conditions at the lake. This dataset includes five austral summer seasons composed of December, January, and February (DJF). The average solar flux at Lake Untersee for the four years with complete solar flux data is 99.2 +/- 0.6 W m(-2). The mean annual temperature at Lake Untersee was determined to be -10.6 degrees +/- 0.6 degrees C. The annual degree-days above freezing for the five years were 9.7, 37.7, 22.4, 7.0, and 48.8, respectively, with summer (DJF) accounting for virtually all of this. For these five summers the average DJF temperatures were -3.5 degrees, -1.9 degrees, -2.2 degrees, -2.6 degrees, and -2.5 degrees C. The maximum (minimum) temperatures were +5.3 degrees, +7.6 degrees, +5.7 degrees, +4.4 degrees, and +9.0 degrees C (-13.8 degrees, -12.8 degrees, -12.9 degrees, -13.5 degrees, and -12.1 degrees C). The average of the wind speed recorded was 5.4 m s(-1), the maximum was 35.7 m s(-1), and the average daily maximum was 15 m s(-1). The wind speed was higher in the winter, averaging 6.4 m s(-1). Summer winds averaged 4.7 m s(-1). The dominant wind direction for strong winds is from the south for all seasons, with a secondary source of strong winds in the summer from the east-northeast. Relative humidity averages 37%; however, high values will occur with an average period of ~10 days, providing a strong indicator of the quasi-periodic passage of storms across the site. Low summer temperatures and high wind speeds create conditions at the surface of the lake ice resulting in sublimation rather than melting as the main mass-loss process. C1 [Andersen, Dale T.] Carl Sagan Ctr, SETI Inst, Mountain View, CA 94043 USA. [McKay, Christopher P.] NASA Ames Res Ctr, Moffett Field, CA USA. [Lagun, Victor] Arctic & Antarctic Res Inst, St Petersburg 199226, Russia. RP Andersen, DT (reprint author), Carl Sagan Ctr, SETI Inst, 189 Bernardo Ave,Suite 100, Mountain View, CA 94043 USA. EM dandersen@carlsagancenter.org FU Tawani Foundation of Chicago; Trottier Family Foundation; NASA's Exobiology and Astrobiology Programs; Arctic and Antarctic Research Institute/Russian Antarctic Expedition's Subprogram "Study and Research of the Antarctic" of the Federal Target Program "World Ocean" FX Primary support for this research was provided by the Tawani Foundation of Chicago, the Trottier Family Foundation, NASA's Exobiology and Astrobiology Programs, and the Arctic and Antarctic Research Institute/Russian Antarctic Expedition's Subprogram "Study and Research of the Antarctic" of the Federal Target Program "World Ocean." Thanks are given to the University of Minnesota's Polar Geospatial Information Center for help with Antarctic mapping. Logistics support was provided by Antarctic Logistics Centre International (ALCI), Cape Town, South Africa, and the Von Braun Center for Science Innovation. We are grateful to Colonel (IL) J. N. Pritzker, IL ARNG (retired), of the Tawani Foundation, Lorne Trottier of the Trottier Family Foundation, Marty Kress of VCSI, Inc., and fellow field team members for their support during the expedition. We also thank John Ferreira, Tomoko Ishihara, and Harry Steel for assistance with the data analysis and graphics. NR 45 TC 0 Z9 0 U1 1 U2 3 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 1558-8424 EI 1558-8432 J9 J APPL METEOROL CLIM JI J. Appl. Meteorol. Climatol. PD JUL PY 2015 VL 54 IS 7 BP 1393 EP 1412 DI 10.1175/JAMC-D-14-0251.1 PG 20 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA CM9AT UT WOS:000357998100002 ER PT J AU Behrangi, A Nguyen, H Granger, S AF Behrangi, Ali Hai Nguyen Granger, Stephanie TI Probabilistic Seasonal Prediction of Meteorological Drought Using the Bootstrap and Multivariate Information SO JOURNAL OF APPLIED METEOROLOGY AND CLIMATOLOGY LA English DT Article ID STANDARDIZED PRECIPITATION INDEX; EL-NINO; SOIL-MOISTURE; PREDICTABILITY; ENSO; TEMPERATURES; VEGETATION; FREQUENCY; ILLINOIS; SCALE AB In the present work, a probabilistic ensemble method using the bootstrap is developed to predict the future state of the standard precipitation index (SPI) commonly used for drought monitoring. The methodology is data driven and has the advantage of being easily extended to use more than one variable as predictors. Using 110 years of monthly observations of precipitaton, surface air temperature, and the Nino-3.4 index, the method was employed to assess the impact of the different variables in enhancing the prediction skill. A predictive probability density function (PDF) is produced for future 6-month SPI, and a log-likelihood skill score is used to cross compare various combination scenarios using the entire predictive PDF and with reference to the observed values set aside for validation. The results suggest that the multivariate prediction using complementary information from 3- and 6-month SPI and initial surface air temperature significantly improves seasonal prediction skills for capturing drought severity and delineation of drought areas based on observed 6-month SPI. The improvement is observed across all seasons and regions over the continental United States relative to other prediction scenarios that ignore the surface air temperature information. C1 [Behrangi, Ali; Hai Nguyen; Granger, Stephanie] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Behrangi, A (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,MS 233-304, Pasadena, CA 91109 USA. EM ali.behrangi@jpl.nasa.gov FU National Aeronautics and Space Administration FX The research described in this paper was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. Government sponsorship is acknowledged. NR 53 TC 3 Z9 3 U1 2 U2 15 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 1558-8424 EI 1558-8432 J9 J APPL METEOROL CLIM JI J. Appl. Meteorol. Climatol. PD JUL PY 2015 VL 54 IS 7 BP 1510 EP 1522 DI 10.1175/JAMC-D-14-0162.1 PG 13 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA CM9AT UT WOS:000357998100009 ER PT J AU Del Genio, AD Chen, YH Kim, D Yao, MS AF Del Genio, Anthony D. Chen, Yonghua Kim, Daehyun Yao, Mao-Sung TI The MJO transition from shallow to deep convection in CloudSat/CALIPSO data and GISS GCM simulations (vol 25, pg 3755, 2012) SO JOURNAL OF CLIMATE LA English DT Correction DE Tropics; Madden-Julian oscillation; Convective clouds; Satellite observations; General circulation models C1 [Del Genio, Anthony D.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Chen, Yonghua] Columbia Univ, Dept Appl Phys & Appl Math, New York, NY USA. [Kim, Daehyun] Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY USA. [Yao, Mao-Sung] NASA, Goddard Space Flight Ctr, Inst Space Studies, Sigma Space Partners, New York, NY 10025 USA. RP Del Genio, AD (reprint author), NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA. EM anthony.d.delgenio@nasa.gov NR 1 TC 0 Z9 0 U1 1 U2 9 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0894-8755 EI 1520-0442 J9 J CLIMATE JI J. Clim. PD JUL PY 2015 VL 28 IS 13 BP 5471 EP 5473 DI 10.1175/JCLI-D-15-0293.1 PG 3 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA CM2BZ UT WOS:000357485900001 ER PT J AU Mayewski, PA Bracegirdle, T Goodwin, I Schneider, D Bertler, NAN Birkel, S Carleton, A England, MH Kang, JH Khan, A Russell, J Turner, J Velicogna, I AF Mayewski, P. A. Bracegirdle, T. Goodwin, I. Schneider, D. Bertler, N. A. N. Birkel, S. Carleton, A. England, M. H. Kang, J-H. Khan, A. Russell, J. Turner, J. Velicogna, I. TI Potential for Southern Hemisphere climate surprises SO JOURNAL OF QUATERNARY SCIENCE LA English DT Article DE Antarctica; climate modeling; paleoclimate; Southern Hemisphere climate; westerlies ID WEST ANTARCTICA; NEW-ZEALAND; SEA-LEVEL; VARIABILITY; HOLOCENE; CIRCULATION; GREENLAND; FREQUENCY; RETREAT; RECORD AB Climate model results suggest that future climate change in Antarctica will be accompanied by continued strengthening and poleward contraction of the Southern Ocean westerly wind belt. Paleoclimate records suggest past changes in the westerly winds can be abrupt and that healing of the Antarctic ozone hole could lead to poleward contraction of the westerlies and increased meridional atmospheric transport of warm air regionally into Antarctica. An abrupt shift to more meridional circulation could lead to notable changes in moisture availability for extra-Antarctic regions, increased Antarctic ice sheet disintegration and more rapid sea-level rise. Copyright (C) 2015 The Authors. Journal of Quaternary Science Published by John Wiley & Sons, Ltd. C1 [Mayewski, P. A.; Birkel, S.] Univ Maine, Climate Change Inst, Orono, ME 04469 USA. [Bracegirdle, T.; Turner, J.] British Antarctic Survey, Cambridge CB3 0ET, England. [Goodwin, I.] Macquarie Univ, Climate Futures, N Ryde, NSW 2109, Australia. [Goodwin, I.] Macquarie Univ, Dept Environm Sci, N Ryde, NSW 2109, Australia. [Schneider, D.] Natl Ctr Atmospher Res, Boulder, CO 80307 USA. [Bertler, N. A. N.] Victoria Univ Wellington, Joint Antarctic Res Inst, Wellington, New Zealand. [Bertler, N. A. N.] GNS Sci, Wellington, New Zealand. [Carleton, A.] Penn State Univ, Dept Geog, University Pk, PA 16802 USA. [Carleton, A.] Penn State Univ, Earth & Environm Syst Inst, University Pk, PA 16802 USA. [England, M. H.] Univ New S Wales, Climate Change Res Ctr, Sydney, NSW 2052, Australia. [Kang, J-H.] Korea Polar Res Inst, Div Polar Climate Change Sci, Inchon, South Korea. [Khan, A.] Univ Colorado, Inst Arctic & Alpine Res, Boulder, CO 80309 USA. [Russell, J.] Univ Arizona, Dept Geosci, Tucson, AZ 85721 USA. [Velicogna, I.] Univ Calif Irvine, Pasadena, CA USA. [Velicogna, I.] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Mayewski, PA (reprint author), Univ Maine, Climate Change Inst, Orono, ME 04469 USA. EM paul.mayewski@maine.edu RI Schneider, David/E-2726-2010; OI Russell, Joellen/0000-0001-9937-6056; England, Matthew/0000-0001-9696-2930 FU SCAR; US NSF [1042883] FX Support for the preparation of this report came from SCAR and US NSF (1042883). NR 37 TC 3 Z9 3 U1 2 U2 28 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0267-8179 EI 1099-1417 J9 J QUATERNARY SCI JI J. Quat. Sci. PD JUL PY 2015 VL 30 IS 5 BP 391 EP 395 DI 10.1002/jqs.2794 PG 5 WC Geography, Physical; Geosciences, Multidisciplinary SC Physical Geography; Geology GA CN0NZ UT WOS:000358111900001 ER PT J AU Geller, MA Zhou, TH Love, PT AF Geller, Marvin A. Zhou, Tiehan Love, Peter T. TI Tropical Gravity Wave Momentum Fluxes and Latent Heating Distributions SO JOURNAL OF THE ATMOSPHERIC SCIENCES LA English DT Article ID DRAG PARAMETERIZATION; TRMM MEASUREMENTS; CLIMATE MODELS; PART I; CONVECTION; SPECTRUM AB Recent satellite determinations of global distributions of absolute gravity wave (GW) momentum fluxes in the lower stratosphere show maxima over the summer subtropical continents and little evidence of GW momentum fluxes associated with the intertropical convergence zone (ITCZ). This seems to be at odds with parameterizations for GW momentum fluxes, where the source is a function of latent heating rates, which are largest in the region of the ITCZ in terms of monthly averages. The authors have examined global distributions of atmospheric latent heating, cloud-top-pressure altitudes, and lower-stratosphere absolute GW momentum fluxes and have found that monthly averages of the lower-stratosphere GW momentum fluxes more closely resemble the monthly mean cloud-top altitudes rather than the monthly mean rates of latent heating. These regions of highest cloud-top altitudes occur when rates of latent heating are largest on the time scale of cloud growth. This, plus previously published studies, suggests that convective sources for stratospheric GW momentum fluxes, being a function of the rate of latent heating, will require either a climate model to correctly model this rate of latent heating or some ad hoc adjustments to account for shortcomings in a climate model's land-sea differences in convective latent heating. C1 [Geller, Marvin A.] SUNY Stony Brook, Stony Brook, NY 11794 USA. [Zhou, Tiehan] NASA Goddard Inst Space Studies, New York, NY USA. [Zhou, Tiehan] Columbia Univ, Ctr Climate Syst Res, New York, NY USA. [Love, Peter T.] Australian Antarctic Div, Kingston, Tas, Australia. RP Geller, MA (reprint author), SUNY Stony Brook, 111 Endeavour Hall, Stony Brook, NY 11794 USA. EM marvin.geller@sunysb.edu FU NASA's Earth Science Modeling and Analysis program; NSF's Climate and Large-Scale Dynamics program FX This research has been supported by research grants from NASA's Earth Science Modeling and Analysis program and NSF's Climate and Large-Scale Dynamics program. We thank Dr. M. Joan Alexander for providing the satellite-derived GWMFs, and we acknowledge very useful discussions with Drs. Alexander and H.-Y. Chun. Finally, we also acknowledge three very perceptive sets of comments from anonymous reviewers. NR 32 TC 3 Z9 3 U1 0 U2 2 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0022-4928 EI 1520-0469 J9 J ATMOS SCI JI J. Atmos. Sci. PD JUL PY 2015 VL 72 IS 7 BP 2762 EP 2768 DI 10.1175/JAS-D-15-0020.1 PG 7 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA CM3OY UT WOS:000357593300013 ER PT J AU Hafiychuk, V Foygel, M Ponizovskaya-Devine, E Smelyanskiy, V Watson, MD Brown, B Goodrich, C AF Hafiychuk, V. Foygel, M. Ponizovskaya-Devine, E. Smelyanskiy, V. Watson, M. D. Brown, B. Goodrich, C. TI Moving-Boundary Model of Cryogenic Fuel Loading, I: Two-Phase Flow in a Pipe SO JOURNAL OF THERMOPHYSICS AND HEAT TRANSFER LA English DT Article ID DYNAMIC SIMULATION-MODEL; GENERAL CORRELATION; HEAT PIPES; EVAPORATORS; REFRIGERATION; FORMULATION; CONDENSERS AB Amoving-boundary model of two-phase flow in a cross-country cryogenic fuel supply line has been developed. It is based on time-dependent one-dimensional ordinary differential equations that describe mass and energy conservation of the flowing cryogen that exchanges heat with the tubes' walls. Momentum conservation is taken into consideration by relating the pressure drop across the boundaries of the control volumes with the corresponding inlet and outlet mass flow rates through the boundaries of these volumes. With a relatively small computational effort, compared to full-scale schemes, the model describes pressure and temperature variations together with the kinetics of vapor void fraction and of the interphase boundary motion in the different parts of the spatially distributed system. In this paper, special attention is given to the detailed study of the transient and steady-state two-phase cryogenic movement in a long horizontal pipe with different regimes of flow: with and without heat exchange between the tube walls and the cryogen, and between the walls and the environment; in the presence of local mass and heat leaks, and of sudden obstructions, etc. The convergence of the computational procedure with respect to the number of the control volumes is discussed. C1 [Hafiychuk, V.; Foygel, M.; Ponizovskaya-Devine, E.; Smelyanskiy, V.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Watson, M. D.] NASA, Marshall Space Flight Ctr, Huntsville, AL 35805 USA. [Brown, B.; Goodrich, C.] NASA, Kennedy Space Ctr, Merritt Isl, FL 32899 USA. RP Hafiychuk, V (reprint author), SGT Inc, 7701 Greenbelt Rd,Suite 400, Greenbelt, MD 20770 USA. NR 25 TC 0 Z9 0 U1 0 U2 3 PU AMER INST AERONAUTICS ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0887-8722 EI 1533-6808 J9 J THERMOPHYS HEAT TR JI J. Thermophys. Heat Transf. PD JUL PY 2015 VL 29 IS 3 BP 533 EP 544 DI 10.2514/1.T4481 PG 12 WC Thermodynamics; Engineering, Mechanical SC Thermodynamics; Engineering GA CM8HR UT WOS:000357940400011 ER PT J AU Hafiychuk, V Foygel, M Ponizovskaya-Devine, E Smelyanskiy, V Watson, MD Brown, B Goodrich, C AF Hafiychuk, V. Foygel, M. Ponizovskaya-Devine, E. Smelyanskiy, V. Watson, M. D. Brown, B. Goodrich, C. TI Moving-Boundary Model of Cryogenic Fuel Loading, II: Theory Versus Experiments SO JOURNAL OF THERMOPHYSICS AND HEAT TRANSFER LA English DT Article ID DYNAMIC SIMULATION-MODEL; 2-PHASE FLOWS; HEAT PIPES; EVAPORATORS; REFRIGERATION; FORMULATION; CONDENSERS AB A moving-boundary model of two-phase cryogenic flow, which was developed in the companion paper (Hafiychuk, V., Foygel, M., Ponizovskaya-Devine, E., Smelyanskiy, V., Watson, M., Brown, B., and Goodrich, C., "Moving-Boundary Model of Cryogenic Fuel Loading, I: Two-Phase Flow in a Long Pipe," Journal of Thermophysics and Heat Transfer, Vol. 29, No. 3, 2015, pp. 524-532.), is applied toward simulation of liquid nitrogen flow data collected for the cooldown regime in two different experimental fuel transfer lines: 1) the 1966 National Bureau of Standards (now the National Institute of Standards and Technology) setup and 2) the novel NASA Kennedy Space Center cryogenic testbed. With relatively small computational effort compared to full-scale schemes, the model describes pressure and temperature histories, kinetics of the vapor void fraction, and interphase boundary motion in two different parts of the transfer lines. The aforementioned time-dependent characteristics are shown to be in a good agreement with the experimental data on the cooldown stage of liquid nitrogen loading obtained at the National Bureau of Standards setup (with no fitting parameters used) and in a fair agreement with the NASA Kennedy Space Center testbed setup (with a small fitting) for chilldown and fast fill operations. The fast and accurate modeling procedure accounts for cryogen fueling operations in both the nominal and major fault regimes. C1 [Hafiychuk, V.; Foygel, M.; Ponizovskaya-Devine, E.; Smelyanskiy, V.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Watson, M. D.] NASA, Marshall Space Flight Ctr, Huntsville, AL 35805 USA. [Brown, B.; Goodrich, C.] NASA, Kennedy Space Ctr, Merritt Isl, FL 32899 USA. RP Hafiychuk, V (reprint author), SGT Inc, 7701 Greenbelt Rd,Suite 400, Greenbelt, MD 20770 USA. NR 15 TC 0 Z9 0 U1 2 U2 5 PU AMER INST AERONAUTICS ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0887-8722 EI 1533-6808 J9 J THERMOPHYS HEAT TR JI J. Thermophys. Heat Transf. PD JUL PY 2015 VL 29 IS 3 BP 545 EP 550 DI 10.2514/1.T4482 PG 6 WC Thermodynamics; Engineering, Mechanical SC Thermodynamics; Engineering GA CM8HR UT WOS:000357940400012 ER PT J AU BastaniNejad, M Elmustafa, AA Forman, E Covert, S Hansknecht, J Hernandez-Garcia, C Poelker, M Das, L Kelley, M Williams, P AF BastaniNejad, Mahzad Elmustafa, Abdelmageed A. Forman, Eric Covert, Steven Hansknecht, John Hernandez-Garcia, Carlos Poelker, Matthew Das, Lopa Kelley, Michael Williams, Phillip TI Evaluation of electropolished stainless steel electrodes for use in DC high voltage photoelectron guns SO JOURNAL OF VACUUM SCIENCE & TECHNOLOGY A LA English DT Article ID VACUUM; HELIUM; METALS AB DC high voltage photoelectron guns are used to produce polarized electron beams for accelerator-based nuclear and high-energy physics research. Low-level field emission (similar to nA) from the cathode electrode degrades the vacuum within the photogun and reduces the photoelectron yield of the delicate GaAs-based photocathode used to produce the electron beams. High-level field emission (> mu A) can cause significant damage the photogun. To minimize field emission, stainless steel electrodes are typically diamond-paste polished, a labor-intensive process often yielding field emission performance with a high degree of variability, sample to sample. As an alternative approach and as comparative study, the performance of electrodes electropolished by conventional commercially available methods is presented. Our observations indicate the electropolished electrodes exhibited less field emission upon the initial application of high voltage, but showed less improvement with gas conditioning compared to the diamond-paste polished electrodes. In contrast, the diamond-paste polished electrodes responded favorably to gas conditioning, and ultimately reached higher voltages and field strengths without field emission, compared to electrodes that were only electropolished. The best performing electrode was one that was both diamond-paste polished and electropolished, reaching a field strength of 18.7 MV/m while generating less than 100 pA of field emission. The authors speculate that the combined processes were the most effective at reducing both large and small scale topography. However, surface science evaluation indicates topography cannot be the only relevant parameter when it comes to predicting field emission performance. (C) 2015 American Vacuum Society. C1 [BastaniNejad, Mahzad; Elmustafa, Abdelmageed A.] Old Dominion Univ, Dept Mech Engn, Norfolk, VA 23529 USA. [Forman, Eric; Covert, Steven; Hansknecht, John; Hernandez-Garcia, Carlos; Poelker, Matthew] Thomas Jefferson Natl Accelerator Facil, Newport News, VA 23606 USA. [Das, Lopa; Kelley, Michael] Coll William & Mary, Williamsburg, VA 23187 USA. [Williams, Phillip] NASA Langley, Hampton, VA 23681 USA. RP BastaniNejad, M (reprint author), Old Dominion Univ, Dept Mech Engn, Norfolk, VA 23529 USA. EM Mahhzad@gmail.com FU Jefferson Science Associates under U.S. DOE [DE-AC05-84ER40150]; DOE Office of High Energy Physics; Americas Region ILC RD program FX Authored by Jefferson Science Associates under U.S. DOE Contract No. DE-AC05-84ER40150 and with funding from the DOE Office of High Energy Physics and the Americas Region ILC R&D program. The U.S. Government retains a nonexclusive, paid-up, irrevocable, world-wide license to publish or reproduce this manuscript for U.S. Government purposes. NR 27 TC 1 Z9 1 U1 2 U2 8 PU A V S AMER INST PHYSICS PI MELVILLE PA STE 1 NO 1, 2 HUNTINGTON QUADRANGLE, MELVILLE, NY 11747-4502 USA SN 0734-2101 EI 1520-8559 J9 J VAC SCI TECHNOL A JI J. Vac. Sci. Technol. A PD JUL PY 2015 VL 33 IS 4 AR 041401 DI 10.1116/1.4920984 PG 9 WC Materials Science, Coatings & Films; Physics, Applied SC Materials Science; Physics GA CM6UQ UT WOS:000357826400010 ER PT J AU Sridharan, DM Chappell, LJ Whalen, MK Cucinotta, FA Pluth, JM AF Sridharan, Deepa M. Chappell, Lori J. Whalen, Mary K. Cucinotta, Francis A. Pluth, Janice M. TI Defining the Biological Effectiveness of Components of High-LET Track Structure SO RADIATION RESEARCH LA English DT Article ID HISTONE H2AX PHOSPHORYLATION; DNA-DAMAGE RESPONSE; MAMMALIAN-CELLS; X-RAYS; IONIZING-RADIATION; SPACE EXPLORATION; HZE PARTICLES; REPAIR FOCI; ENERGY; ATM AB During space travel, astronauts are exposed to a wide array of high-linear energy transfer (LET) particles, with differing energies and resulting biological effects. Risk assessment of these exposures carries a large uncertainty predominantly due to the unique track structure of the particle's energy deposition. The complex damage elicited by high charge and energy (HZE) particles results from both lesions along the track core and from energetic electrons, delta rays, generated as a consequence of particle traversal. To better define how cells respond to this complex radiation exposure, a normal hTERT immortalized skin fibroblast cell line was exposed to a defined panel of particles carefully chosen to tease out track structure effects. Phosphorylation kinetics for several key double-strand break (DSB) response proteins (gamma-H2AX, pATF2 and pSMC1) were defined after exposure to ten different high-LET radiation qualities and one low-LET radiation (X ray), at two doses (0.5-2 Gy) and time points (2 and 24 h). The results reveal that the lower energy particles (Fe 300, Si 93 and Ti 300 MeV/u), with a narrower track width and higher number and intensity of d rays, cause the highest degree of persistent damage response. The persistent gamma-H2AX signal at lower energies suggests that damage from these exposures are more difficult to resolve, likely due to the greater complexity of the associated DNA lesions. However, different kinetics were observed for the solely ATM-mediated phosphorylations (pATF2 and pSMC1), revealing a shallow induction at early times and a higher level of residual phosphorylation compared to gamma-H2AX. The differing phospho-protein profiles exhibited, compared to gamma-H2AX, suggests additional functions for these proteins within the cell. The strong correspondence between the predicted curves for energy deposition per nucleosome for each ion/energy combination and the persistent levels of gamma-H2AX indicates that the nature of energy distribution defines residual levels of gamma-H2AX, an indicator of unrepaired DSBs. Our results suggest that decreasing the energy of a particle results in more complex damage that may increase genomic instability and increase the risk of carcinogenesis. (C) 2015 by Radiation Research Society C1 [Sridharan, Deepa M.; Whalen, Mary K.; Pluth, Janice M.] Lawrence Berkeley Natl Lab, Div Life Sci, Albany, CA 94710 USA. [Chappell, Lori J.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Cucinotta, Francis A.] Univ Nevada, Hlth Phys & Diagnost Sci, Las Vegas, NV 89154 USA. RP Pluth, JM (reprint author), Lawrence Berkeley Natl Lab, Dept Canc, Albany, CA 94710 USA. EM jmpluth@lbl.gov FU NASA [NNA06CD661] FX We would like to thank Dr. Ianik Plante for helpful discussions. We also thank Michelle Scott in the LBNL FACS core for assistance with flow cytometry, and Dr. Adam Rusek and the Physics team at NSRL for making this work possible. We also extend a special thanks to our undergraduate interns Jeffrey Liu and Ramey Chan for assisting in this project. This project was supported by NASA award NNA06CD661 to JMP. NR 37 TC 7 Z9 7 U1 1 U2 2 PU RADIATION RESEARCH SOC PI LAWRENCE PA 810 E TENTH STREET, LAWRENCE, KS 66044 USA SN 0033-7587 EI 1938-5404 J9 RADIAT RES JI Radiat. Res. PD JUL PY 2015 VL 184 IS 1 BP 105 EP 119 DI 10.1667/RR13684.1 PG 15 WC Biology; Biophysics; Radiology, Nuclear Medicine & Medical Imaging SC Life Sciences & Biomedicine - Other Topics; Biophysics; Radiology, Nuclear Medicine & Medical Imaging GA CM8NA UT WOS:000357957100012 PM 26114329 ER PT J AU Valley, JW Reinhard, DA Cavosie, AJ Ushikubo, T Lawrence, DF Larson, DJ Kelly, TF Snoeyenbos, DR Strickland, A AF Valley, John W. Reinhard, David A. Cavosie, Aaron J. Ushikubo, Takayuki Lawrence, Daniel F. Larson, David J. Kelly, Thomas F. Snoeyenbos, David R. Strickland, Ariel TI Nano- and micro-geochronology in Hadean and Archean zircons by atom-probe tomography and SIMS: New tools for old minerals SO AMERICAN MINERALOGIST LA English DT Article DE Atom-probe tomography; APT; radiation damage; SIMS; zircon; nano-geochronology; oxygen isotopes; Hadean ID OXYGEN-ISOTOPE RATIOS; TRACE-ELEMENT COMPOSITION; METAMORPHIC CORE COMPLEX; RARE-EARTH ELEMENTS; MA DETRITAL ZIRCONS; RADIATION-DAMAGE; WESTERN-AUSTRALIA; JACK HILLS; METAMICT ZIRCON; GA ZIRCONS AB Atom-probe tomography (APT) and secondary ion mass spectrometry (SIMS) provide complementary in situ element and isotope data in minerals such as zircon. SIMS measures isotope ratios and trace elements from 1-20 mu m spots with excellent accuracy and precision. APT identifies mass/charge and three-dimensional position of individual atoms (+/- 0.3 nm) in 100 nm-scale samples, volumes up to one million times smaller than SIMS. APT data provide unique information for understanding element and isotope distribution; crystallization and thermal history; and mechanisms of mineral reaction and exchange. This atomistic view enables evaluation of the fidelity of geochemical data for zircon because it provides new understanding of radiation damage, and can test for intracrystalline element mobility. Nano-geochronology is one application of APT in which Pb isotope ratios from sub-micrometer domains of zircon provide model ages of crystallization and identify later magmatic and metamorphic reheating. Based on SEM imaging and SIMS analysis, 11 needle-shaped specimens similar to 100 nm in diameter were sampled from one Archean and two Hadean zircons by focused ion-beam milling and analyzed with APT. The three-dimensional distribution of Pb and nominally incompatible elements (Y, REEs) differs at the atomic scale in each zircon. Zircon JH4.0 (4.007 Ga, Jack Hills, Western Australia) is homogeneous in Pb, Y, and REEs. In contrast, Pb and Y and REEs are clustered in sub-equant similar to 10 nm diameter domains, spaced 10-40 nm apart in zircons ARG2.5 (2.542 Ga, Grouse Creek Mountains, Utah) and JH4.4 (4.374 Ga, Jack Hills). Most clusters are flattened parallel to (100) or (010). U and Th are not collocated with Pb in clusters and appear to be homogeneously distributed in all three zircons. The analyzed domains experienced 4 to 8 x 10(15) alpha-decay events/mg due to U and Th decay and yet all zircons yield U-Pb ages by SIMS that are better than 97% concordant, consistent with annealing of most radiation damage. The Pb-207/Pb-206 ratios for the 100 nm-scale specimens measured by APT average 0.17 for ARG2.5, 0.42 for the JH4.0, and 0.52 for JH4.4. These ratios are less precise (+/- 10-18% 2 sigma) due to the ultra-small sample size, but in excellent agreement with values measured by SIMS (0.1684, 0.4269, and 0.5472, respectively) and the crystallization ages of the zircons. Thus Pb in these clusters is radiogenic, but unsupported, meaning that the Pb is not spatially associated with its parent isotopes of U and Th. For the domain outside of clusters in JH4.4, the Pb-207/Pb-206 ratio is 0.3, consistent with the SIMS value of 0.2867 for the zircon overgrowth rim and an age of 3.4 Ga. In ARG2.5, all Pb is concentrated in clusters and there is no detectable Pb remaining outside of the clusters. The Pb-Y-REE-rich clusters and lack of correlation with U in ARG2.5 and JH4.4 are best explained by diffusion of Pb and other elements into similar to 10 nm amorphous domains formed by alpha-recoil. Diffusion distances of similar to 20 nm for these elements in crystalline zircon are consistent with heating at temperatures of 800 degrees C for similar to 2 m.y. Such later reheating events are identified and dated by APT from Pb-207/Pb-206 Pb model ages of clusters in JH4.4 and by the absence of detectable Pb outside of clusters in ARG2.5. SIMS dates for the zircon rims independently confirm reheating of ARG2.5 and JH4.4, which were xenocrysts in younger magmas when rims formed. It is proposed that most domains damaged by alpha-recoil were annealed at ambient temperatures above 200-300 degrees C before reheating and only a small number of domains were amorphous and available to concentrate Pb at the time of reheating. The size, shapes, and orientations of clusters were altered by annealing after formation. The absence of enriched clusters in JH4.0 shows that this zircon was not similarly reheated. Thus APT data provide thermochronologic information about crustal reworking even for zircons where no overgrowth is recognized. The clusters in JH4.4 document Pb mobility at the sub-50 nm scale, but show that the much larger 20 mu m-scale domains analyzed by SIMS were closed systems. The reliability of oxygen isotope ratios and other geochemical data from zircon can be evaluated by these means. These results verify the age of this zircon and support previous proposals that differentiated crust existed by 4.4 Ga and that the surface of Earth was relatively cool with habitable oceans before 4.3 Ga. These analytical techniques are of general applicability to minerals of all ages and open many new research opportunities. C1 [Valley, John W.; Cavosie, Aaron J.; Ushikubo, Takayuki; Strickland, Ariel] Univ Wisconsin, Dept Geosci, WiscSIMS, Madison, WI 53706 USA. [Valley, John W.; Cavosie, Aaron J.] Univ Wisconsin, Dept Geosci, NASA Astrobiol Inst, Madison, WI 53706 USA. [Reinhard, David A.; Lawrence, Daniel F.; Larson, David J.; Kelly, Thomas F.] CAMECA Instruments, Madison, WI 53711 USA. [Cavosie, Aaron J.] Univ Puerto Rico, Dept Geol, Mayaguez, PR 00681 USA. [Snoeyenbos, David R.] Univ Massachusetts, Dept Geosci, Amherst, MA 01003 USA. RP Valley, JW (reprint author), Univ Wisconsin, Dept Geosci, WiscSIMS, Madison, WI 53706 USA. EM valley@geology.wisc.edu FU U.S. National Science Foundation [EAR-0838058]; U.S. Department of Energy Office of Science, Office of Basic Energy Sciences [DE-FG02-93ER14389]; NASA Astrobiology Institute; [NSF-EAR-1053466]; [NSF-EAR-1355590] FX The authors thank Brian Hess for sample preparation and polishing; John Fournelle and Phil Gopon for assistance with EPMA and SEM; Noriko Kita and Jim Kern for assistance with SIMS; and David Valley for assistance in fieldwork. John Craven assisted with SIMS analysis in Edinburgh and has been of invaluable assistance in many of the first author's in situ studies of oxygen isotope ratio. We thank Tyler Blum, Kouki Kitajima, Dunyi Liu, Des Moser, Mike Spicuzza, Simon Wilde, and our colleagues at CAMECA in Madison, Wisconsin, for their contributions to these efforts. D.A.R., D.F.L., D.J.L., and T.F.K. are employees of CAMECA who manufactures the LEAP instrument that was used in this study. This research was supported by the U.S. National Science Foundation (EAR-0838058); the U.S. Department of Energy Office of Science, Office of Basic Energy Sciences under Award Number DE-FG02-93ER14389; and the NASA Astrobiology Institute. WiscSIMS is partly supported by NSF-EAR-1053466 and NSF-EAR-1355590. NR 134 TC 9 Z9 9 U1 14 U2 36 PU MINERALOGICAL SOC AMER PI CHANTILLY PA 3635 CONCORDE PKWY STE 500, CHANTILLY, VA 20151-1125 USA SN 0003-004X EI 1945-3027 J9 AM MINERAL JI Am. Miner. PD JUL PY 2015 VL 100 IS 7 BP 1355 EP 1377 PG 23 WC Geochemistry & Geophysics; Mineralogy SC Geochemistry & Geophysics; Mineralogy GA CM1HK UT WOS:000357431700005 ER PT J AU Currie, T Lisse, CM Kuchner, M Madhusudhan, N Kenyon, SJ Thalmann, C Carson, J Debes, J AF Currie, Thayne Lisse, Carey M. Kuchner, Marc Madhusudhan, Nikku Kenyon, Scott J. Thalmann, Christian Carson, Joseph Debes, John TI DIRECT IMAGING AND SPECTROSCOPY OF A YOUNG EXTRASOLAR KUIPER BELT IN THE NEAREST OB ASSOCIATION SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE planetary systems; stars: early-type; stars: individual (HD 115600) ID DEBRIS DISK; HR 4796A; EVOLUTIONARY MODELS; SCORPIUS-CENTAURUS; CIRCUMSTELLAR DISK; PLANET FORMATION; BURNING LIMIT; MAIN-SEQUENCE; STARS; SYSTEM AB We describe the discovery of a bright, young Kuiper belt-like debris disk around HD 115600, a similar to 1.4-1.5 M-circle dot, similar to 15 Myr old member of the Sco-Cen OB Association. Our H-band coronagraphy/integral field spectroscopy from the Gemini Planet Imager shows the ring has a (luminosity-scaled) semimajor axis of (similar to 22 AU) similar to 48 AU, similar to the current Kuiper belt. The disk appears to have neutral-scattering dust, is eccentric (e similar to 0.1-0.2), and could be sculpted by analogs to the outer solar system planets. Spectroscopy of the disk ansae reveal a slightly blue to gray disk color, consistent with major Kuiper belt chemical constituents, where water ice is a very plausible dominant constituent. Besides being the first object discovered with the next generation of extreme adaptive optics systems (i.e., SCExAO, GPI, SPHERE), HD 115600's debris ring and planetary system provide a key reference point for the early evolution of the solar system, the structure, and composition of the Kuiper belt and the interaction between debris disks and planets. C1 [Currie, Thayne] Natl Inst Nat Sci, Natl Astron Observ Japan, Subaru Telescope, Hilo, HI 96720 USA. [Lisse, Carey M.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA. [Kuchner, Marc] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Madhusudhan, Nikku] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Kenyon, Scott J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Thalmann, Christian] ETH, Zurich, Switzerland. [Carson, Joseph] Coll Charleston, Dept Phys & Astron, Charleston, SC 29401 USA. [Debes, John] Space Telescope Sci Inst, Baltimore, MD 21218 USA. RP Currie, T (reprint author), Natl Inst Nat Sci, Natl Astron Observ Japan, Subaru Telescope, 650 N Aohoku Pl, Hilo, HI 96720 USA. RI Lisse, Carey/B-7772-2016 OI Kenyon, Scott/0000-0003-0214-609X; Lisse, Carey/0000-0002-9548-1526 FU GPI Early Science Time Allocation Committee; Gemini Director Markus Kissler-Patig FX We thank the anonymous referee, Wladimir Lyra, Eric Mamajek, and Mengshu Xu for helpful comments; Fredrik Rantakryo for executing these queue-mode observations; and the GPI Early Science Time Allocation Committee and Gemini Director Markus Kissler-Patig for supporting this program. NR 46 TC 14 Z9 14 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD JUL 1 PY 2015 VL 807 IS 1 AR L7 DI 10.1088/2041-8205/807/1/L7 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL8YY UT WOS:000357262100007 ER PT J AU Ullman, DJ Carlson, AE Anslow, FS LeGrande, AN Licciardi, JM AF Ullman, David J. Carlson, Anders E. Anslow, Faron S. LeGrande, Allegra N. Licciardi, Joseph M. TI Laurentide ice-sheet instability during the last deglaciation SO NATURE GEOSCIENCE LA English DT Article ID ENERGY-BALANCE; GLACIAL CYCLES; BRITISH-COLUMBIA; LATE PLEISTOCENE; ROCKY-MOUNTAINS; HIGH-RESOLUTION; MONSOON RECORD; PAST CLIMATE; GREENLAND; INSOLATION AB Changes in the amount of summer incoming solar radiation (insolation) reaching the Northern Hemisphere are the underlying pacemaker of glacial cycles(1-6). However, not all rises in boreal summer insolation over the past 800,000 years resulted in deglaciation to present-day ice volumes(1-3,6-8), suggesting that there may be a climatic threshold for the disappearance of land-based ice. Here we assess the surface mass balance stability(9) of the Laurentide ice sheet-the largest glacial ice mass in the Northern Hemisphere-during the last deglaciation (24,000 to 9,000 years ago). We run a surface energy balance model(10,11) with climate data from simulations with a fully coupled atmosphere-ocean general circulation model for key time slices during the last deglaciation. We find that the surface mass balance of the Laurentide ice sheet was positive throughout much of the deglaciation, and suggest that dynamic discharge was mainly responsible for mass loss during this time. Total surface mass balance became negative only in the early Holocene, indicating the transition to a new state where ice loss occurred primarily by surface ablation. We conclude that the Laurentide ice sheet remained a viable ice sheet before the Holocene and began to fully deglaciate only once summer temperatures and radiative forcing over the ice sheet increased by 6-7 degrees C and 16-20 W m(-2), respectively, relative to full glacial conditions. C1 [Ullman, David J.; Carlson, Anders E.] Univ Wisconsin, Dept Geosci, Madison, WI 53706 USA. [Ullman, David J.; Carlson, Anders E.] Oregon State Univ, Coll Earth Ocean & Atmospher Sci, Corvallis, OR 97331 USA. [Anslow, Faron S.] Univ Victoria, Pacific Climate Impacts Consortium, Victoria, BC V8W 2Y2, Canada. [LeGrande, Allegra N.] Columbia Univ, NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [LeGrande, Allegra N.] Columbia Univ, Ctr Climate Syst Res, New York, NY 10025 USA. [Licciardi, Joseph M.] Univ New Hampshire, Dept Earth Sci, Durham, NH 03824 USA. RP Ullman, DJ (reprint author), Univ Wisconsin, Dept Geosci, Madison, WI 53706 USA. EM dullman@coas.oregonstate.edu FU United States National Science Foundation [AGS-0753660, AGS-0753868]; National Aeronautics and Space Administration FX United States National Science Foundation awards AGS-0753660 (A.E.C.), AGS-0753868 (A.N.L.), and the National Aeronautics and Space Administration supported this research. NR 75 TC 6 Z9 6 U1 3 U2 30 PU NATURE PUBLISHING GROUP PI NEW YORK PA 75 VARICK ST, 9TH FLR, NEW YORK, NY 10013-1917 USA SN 1752-0894 EI 1752-0908 J9 NAT GEOSCI JI Nat. Geosci. PD JUL PY 2015 VL 8 IS 7 BP 534 EP U140 DI 10.1038/NGEO2463 PG 7 WC Geosciences, Multidisciplinary SC Geology GA CM0XV UT WOS:000357404200015 ER PT J AU Campbell, MR Charles, JB AF Campbell, Mark R. Charles, John B. TI Historical Review of Lower Body Negative Pressure Research in Space Medicine SO AEROSPACE MEDICINE AND HUMAN PERFORMANCE LA English DT Review DE weightlessness; microgravity; Apollo program; Skylab program; International Space Station; shuttle program; orthostatic intolerance; spaceflight countermeasures ID MANNED SKYLAB MISSION; 70 DEGREES TILT; BED REST; ORTHOSTATIC INTOLERANCE; CIRCULATORY RESPONSES; VASCULAR-RESPONSES; WATER-IMMERSION; ZERO GRAVITY; LEG VOLUME; SHORT-TERM AB Cephalad redistribution of intravascular and extravascular fluid occurs as a result of weightlessness during spaceflight. This provokes cardiovascular, cardiopulmonary, and autonomic nervous system responses. The resulting altered functional state can result in orthostatic hypotension and intolerance upon landing and return to a gravity environment. In-flight lower body negative pressure (LBNP) transiently restores normal body fluid distribution. Early in the U.S. space program, LBNP was devised as a way to test for orthostatic intolerance. With the development of the Skylab Program and longer duration spaceflight, it was realized that it could provide a method of monitoring orthostatic intolerance in flight and predicting the post-landing orthostatic response. LBNP was also investigated not only as an in-flight cardiovascular orthostatic stress test, but also as a countermeasure to cardiovascular deconditioning on Soviet space stations, Skylab, and the Shuttle. It is still being used by the Russian program on the International Space Station as an end-of-flight countermeasure. C1 Paris Reg Med Ctr, Gen Surg, Paris, TX USA. NASA, Johnson Space Ctr, Human Res Program, Houston, TX USA. RP Campbell, MR (reprint author), 420 Collegiate 300, Paris, TX 75460 USA. EM mcamp@1starnet.com NR 71 TC 2 Z9 2 U1 1 U2 11 PU AEROSPACE MEDICAL ASSOC PI ALEXANDRIA PA 320 S HENRY ST, ALEXANDRIA, VA 22314-3579 USA SN 2375-6314 EI 2375-6322 J9 AEROSP MED HUM PERF JI Aerosp. Med.Hum. Perform. PD JUL PY 2015 VL 86 IS 7 BP 633 EP 640 DI 10.3357/AMHP.4246.2015 PG 8 WC Biophysics; Public, Environmental & Occupational Health; Medicine, Research & Experimental SC Biophysics; Public, Environmental & Occupational Health; Research & Experimental Medicine GA CM0RG UT WOS:000357385400007 PM 26102144 ER PT J AU Memarsadeghi, N AF Memarsadeghi, Nargess TI Citizen Science INTRODUCTION SO COMPUTING IN SCIENCE & ENGINEERING LA English DT Editorial Material DE scientific computing; citizen science; crowdsourcing; distributed computing; STEM; education; FPCCS C1 NASA, Goddard Space Flight Ctr, Washington, DC 20546 USA. RP Memarsadeghi, N (reprint author), NASA, Goddard Space Flight Ctr, Washington, DC 20546 USA. EM Nargess.Memarsadeghi@nasa.gov NR 0 TC 1 Z9 1 U1 4 U2 19 PU IEEE COMPUTER SOC PI LOS ALAMITOS PA 10662 LOS VAQUEROS CIRCLE, PO BOX 3014, LOS ALAMITOS, CA 90720-1314 USA SN 1521-9615 EI 1558-366X J9 COMPUT SCI ENG JI Comput. Sci. Eng. PD JUL-AUG PY 2015 VL 17 IS 4 BP 8 EP 10 DI 10.1109/MCSE.2015.72 PG 3 WC Computer Science, Interdisciplinary Applications SC Computer Science GA CL4CO UT WOS:000356900400002 ER PT J AU Nyeo, SL Ansari, RR AF Nyeo, Su-Long Ansari, Rafat R. TI Data inversion for dynamic light scattering using Fisher information SO LASER PHYSICS LA English DT Article DE photon correlation spectroscopy; inverse problems; Fisher information; Tikhonov regularization ID MAXIMUM-ENTROPY ANALYSIS; CORRELATION SPECTROSCOPY DATA; FREDHOLM INTEGRAL-EQUATIONS; REGULARIZATION PARAMETER; TIKHONOV REGULARIZATION; 1ST KIND; L-CURVE; POLYDISPERSITY; TOMOGRAPHY; ALGORITHM AB Dynamic light scattering is a promising technique for characterizing colloidal particles as their size distribution. The determination of a size distribution is however an ill-posed inverse problem, which requires efficient and well-tested numerical algorithms. In this paper, the inverse problem is studied numerically using the Tikhonov regularization method with Fisher information as a regularization function. A numerical algorithm is described to obtain well-defined solutions to the problem and an optimal solution is determined by the L-curve criterion. Simulated data are created from unimodal and bimodal distributions and analyzed to evaluate the performance of the algorithm. It is shown that the algorithm can efficiently retrieve a unimodal distribution of a very broad support and bimodal distributions with higher accuracy than the well-known algorithms of the constrained regularization method (CONTIN) and the maximum-entropy method (MEM). C1 [Nyeo, Su-Long] Natl Cheng Kung Univ, Dept Phys, Tainan 70101, Taiwan. [Ansari, Rafat R.] NASA John H Glenn Res Ctr Lewis Field, Fluid Phys & Transport Proc Branch, Cleveland, OH 44135 USA. RP Nyeo, SL (reprint author), Natl Cheng Kung Univ, Dept Phys, Tainan 70101, Taiwan. EM t14269@mail.ncku.edu.tw; Rafat.R.Ansari@nasa.gov FU Ministry of Science and Technology of the Republic of China; Research and Technology Directorate of the NASA Glenn Research Center FX Dr Nyeo would like to acknowledge support from the Ministry of Science and Technology of the Republic of China, and Dr Ansari would like to acknowledge support from the Research and Technology Directorate of the NASA Glenn Research Center. NR 28 TC 0 Z9 0 U1 2 U2 8 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 1054-660X EI 1555-6611 J9 LASER PHYS JI Laser Phys. PD JUL PY 2015 VL 25 IS 7 AR 075703 DI 10.1088/1054-660X/25/7/075703 PG 7 WC Optics; Physics, Applied SC Optics; Physics GA CL7VN UT WOS:000357180200021 ER PT J AU Murphy, TE Pilorz, S Prufert-Bebout, L Bebout, B AF Murphy, Thomas E. Pilorz, Stuart Prufert-Bebout, Leslie Bebout, Brad TI A Novel Microsensor for Measuring Angular Distribution of Radiative Intensity SO PHOTOCHEMISTRY AND PHOTOBIOLOGY LA English DT Article ID SPECTRAL LIGHT MEASUREMENTS; DISTRIBUTION CAMERA SYSTEM; MICROBIAL MATS; SCALAR IRRADIANCE; FIBEROPTIC MICROPROBE; RADIANCE DISTRIBUTION; PHOTOSYNTHETIC COMMUNITIES; BIOFILM PHOTOBIOREACTOR; ULTRAVIOLET-RADIATION; SEDIMENTS AB This article presents the design, construction and characterization of a novel type of light probe for measuring the angular radiance distribution of light fields. The differential acceptance angle (DAA) probe can resolve the directionality of a light field in environments with steep light gradients, such as microbial mats, without the need to remove, reorient, and reinsert the probe, a clear advantage over prior techniques. The probe consists of an inner irradiance sensor inside a concentric, moveable light-absorbing sheath. The radiative intensity in a specific zenith direction can be calculated by comparing the irradiance onto the sensor at different acceptance angles. We used this probe to measure the angular radiance distribution of two sample light fields, and observed good agreement with a conventional radiance probe. The DAA probe will aid researchers in understanding light transfer physics in dense microbial communities and expedite validation of numerical radiative transfer models for these environments. C1 [Murphy, Thomas E.; Prufert-Bebout, Leslie; Bebout, Brad] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Pilorz, Stuart] SETI Inst, Mountain View, CA USA. RP Murphy, TE (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM thomasemurphy@utexas.edu FU NASA FX The authors gratefully acknowledge the financial support provided by the NASA Postdoctoral Program. NR 51 TC 0 Z9 0 U1 2 U2 3 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0031-8655 EI 1751-1097 J9 PHOTOCHEM PHOTOBIOL JI Photochem. Photobiol. PD JUL-AUG PY 2015 VL 91 IS 4 BP 862 EP 868 DI 10.1111/php.12452 PG 7 WC Biochemistry & Molecular Biology; Biophysics SC Biochemistry & Molecular Biology; Biophysics GA CM0MZ UT WOS:000357373700012 PM 25763775 ER PT J AU Margolis, HA Nelson, RF Montesano, PM Beaudoin, A Sun, GQ Andersen, HE Wulder, MA AF Margolis, Hank A. Nelson, Ross F. Montesano, Paul M. Beaudoin, Andre Sun, Guoqing Andersen, Hans-Erik Wulder, Michael A. TI Combining satellite lidar, airborne lidar, and ground plots to estimate the amount and distribution of aboveground biomass in the boreal forest of North America SO CANADIAN JOURNAL OF FOREST RESEARCH LA English DT Article DE aboveground biomass; lidar; North American boreal forest; ICESat-GLAS; Landsat; MODIS; forest inventory; kNN ID HEDMARK COUNTY; SPACEBORNE LIDAR; CLIMATE-CHANGE; SAMPLE SURVEY; LASER DATA; CANADA; AREA; CARBON; INVENTORY; NORWAY AB We report estimates of the amount, distribution, and uncertainty of aboveground biomass (AGB) of the different ecoregions and forest land cover classes within the North American boreal forest, analyze the factors driving the error estimates, and compare our estimates with other reported values. A three-phase sampling strategy was used (i) to tie ground plot AGB to airborne profiling lidar metrics and (ii) to link the airborne estimates of AGB to ICESat-GLAS lidar measurements such that (iii) GLAS could be used as a regional sampling tool. We estimated the AGB of the North American boreal forest at 21.8 Pg, with relative error of 1.9% based on 256 GLAS orbits (229 086 pulses). The distribution of AGB was 46.6% for western Canada, 43.7% for eastern Canada, and 9.7% for Alaska. With a single exception, relative errors were under 4% for the three regions and for the major cover types and under 10% at the ecoregion level. The uncertainties of the estimates were calculated using a variance estimator that accounted for only sampling error, i.e., the variability among GLAS orbital estimates, and airborne to spaceborne regression error, i.e., the uncertainty of the model coefficients. Work is ongoing to develop robust statistical techniques for integrating other sources of error such as ground to air regression error and allometric error. Small ecoregions with limited east-west extents tended to have fewer GLAS orbits and a greater percent sampling error. AGB densities derived from GLAS agreed closely with the estimates derived from both forest inventories (<17%) and a MODIS-based interpolation technique (<26%) for more southern, well-inventoried ecoregions, whereas differences were much greater for unmanaged northern and (or) mountainous ecoregions. C1 [Margolis, Hank A.] Univ Laval, Fac Foresterie Geog & Geomat, Ctr Etud Foret, Quebec City, PQ G1V 0A6, Canada. [Margolis, Hank A.; Nelson, Ross F.; Montesano, Paul M.; Sun, Guoqing] NASA, Goddard Space Flight Ctr, Biospher Sci Lab, Greenbelt, MD 20771 USA. [Montesano, Paul M.] NASA, Goddard Space Flight Ctr, Sci Syst & Applicat Inc, Greenbelt, MD 20771 USA. [Beaudoin, Andre] Nat Resources Canada, Canadian Forest Serv, Laurentian Forestry Ctr, Quebec City, PQ G1V 4C7, Canada. [Sun, Guoqing] Univ Maryland, Dept Geog Sci, College Pk, MD 20742 USA. [Andersen, Hans-Erik] US Forest Serv, USDA, Pacific Northwest Res Stn, Seattle, WA 98195 USA. [Wulder, Michael A.] Nat Resources Canada, Canadian Forest Serv, Pacific Forestry Ctr, Victoria, BC V8Z 1M5, Canada. RP Margolis, HA (reprint author), Univ Laval, Fac Foresterie Geog & Geomat, Ctr Etud Foret, Quebec City, PQ G1V 0A6, Canada. EM Hank.Margolis@sbf.ulaval.ca RI Wulder, Michael/J-5597-2016 OI Wulder, Michael/0000-0002-6942-1896 NR 47 TC 11 Z9 13 U1 4 U2 23 PU CANADIAN SCIENCE PUBLISHING, NRC RESEARCH PRESS PI OTTAWA PA 65 AURIGA DR, SUITE 203, OTTAWA, ON K2E 7W6, CANADA SN 0045-5067 EI 1208-6037 J9 CAN J FOREST RES JI Can. J. For. Res. PD JUL PY 2015 VL 45 IS 7 BP 838 EP 855 DI 10.1139/cjfr-2015-0006 PG 18 WC Forestry SC Forestry GA CL7FB UT WOS:000357136800006 ER PT J AU Tuzcu, I Nguyen, N AF Ilhan Tuzcu Nhan Nguyen TI Flutter of Maneuvering Aircraft SO JOURNAL OF AEROSPACE ENGINEERING LA English DT Article DE Flexible aircraft; Flight dynamics; Aeroelasticity; Unsteady aerodynamics; Flutter; Steady level flight; Steady turn; Steady climb; Gliding flight ID NONLINEAR FLIGHT DYNAMICS; RATIO FLYING WINGS; FLEXIBLE AIRCRAFT; HIGH-ALTITUDE; AEROELASTICITY; STABILITY; MODELS AB The objective of this paper is to investigate how the aeroelastic stability, particularly flutter, is affected by aircraft maneuvers. The authors' investigation is based on a comprehensive mathematical model of aircraft, which is achieved by seamlessly integrating all the disciplines pertinent to flight of aircraft. The aircraft is treated as an unstrained, flexible multibody system subject to unsteady aerodynamics. The bodies are fuselage, wing, and horizontal and vertical stabilizers, whose structures are modeled as beams in bending and torsion. The equations of motion are derived using Lagrange's equations in quasi-coordinates. The resulting equations are a set of nonlinear ordinary differential equations of relatively high order. The final model is used to determine flutter speeds of aircraft at steady level turn and steady climb at various altitudes. These maneuvers are especially chosen to keep the equations time invariant. The numerical results are given for a generic transport model (GTM). The stability of a GTM is affected by turn radius, climb angle, and altitude. The results for climbing flight can be extended to address stability of gliding flight. (C) 2014 American Society of Civil Engineers. C1 [Ilhan Tuzcu] Calif State Univ Sacramento, Dept Mech Engn, Sacramento, CA 95819 USA. [Nhan Nguyen] NASA Ames Res Ctr, Intelligent Syst Div, Moffett Field, CA 94035 USA. RP Tuzcu, I (reprint author), Calif State Univ Sacramento, Dept Mech Engn, Sacramento, CA 95819 USA. EM tuzcui@ecs.csus.edu NR 38 TC 0 Z9 0 U1 2 U2 7 PU ASCE-AMER SOC CIVIL ENGINEERS PI RESTON PA 1801 ALEXANDER BELL DR, RESTON, VA 20191-4400 USA SN 0893-1321 EI 1943-5525 J9 J AEROSPACE ENG JI J. Aerosp. Eng. PD JUL PY 2015 VL 28 IS 4 AR 04014094 DI 10.1061/(ASCE)AS.1943-5525.0000415 PG 15 WC Engineering, Aerospace; Engineering, Civil SC Engineering GA CK7NT UT WOS:000356420000006 ER PT J AU Mehta, SK Fujiwara, M Tsuda, T Vernier, JP AF Mehta, Sanjay Kumar Fujiwara, Masatomo Tsuda, Toshitaka Vernier, Jean-Paul TI Effect of recent minor volcanic eruptions on temperatures in the upper troposphere and lower stratosphere SO JOURNAL OF ATMOSPHERIC AND SOLAR-TERRESTRIAL PHYSICS LA English DT Article ID QUASI-BIENNIAL OSCILLATION; GPS RADIO OCCULTATION; CLIMATE-CHANGE; MODEL; AEROSOL; PINATUBO; CONFIGURATION; UNCERTAINTY; ATMOSPHERE; ACCOUNT AB The impact of the recent minor volcanic eruptions during 2001-2010 in the temperature of the upper troposphere and lower stratosphere (UTLS) is investigated using data from the Global Positioning System Radio Occultation (GPS RO), three radiosonde compilations and two reanalyses (ERA-Interim and MERRA). The volcanic signals are identified in the residual temperature time series after removal of the linear trend, the quasi-biennial oscillation and El Nino Southern Oscillation components. Eight minor volcanic eruptions (six from the tropics and two from midlatitude) over the last decade (2001-2010) are analyzed in this study. We found significant volcanic signals in the UTLS temperature only in association with the tropical Soufriere Hills and Tavurvur eruptions (in May 2006 and in October 2006, respectively). Other four tropical eruptions had very small aerosol perturbations and did not show any significant UTLS temperature change. Out of the two midlatitude eruptions, Sarychev peak had similar stratospheric aerosol perturbations as Soufriere Hills and Tavurvur eruptions, but did not show any significant UTLS temperature change. The volcanic signals in the UTLS temperature from the tropical Soufriere Hills and Tavurvur eruptions were observed for the period of 7 months after August 2006. A warming of 0.5-0.8 K in the tropical 16-18.5 km (100-70 hPa) layer was observed in association with these two tropical eruptions. (c) 2015 Elsevier Ltd. All rights reserved. C1 [Mehta, Sanjay Kumar; Tsuda, Toshitaka] Kyoto Univ, RISH, Kyoto 6068501, Japan. [Fujiwara, Masatomo] Hokkaido Univ, Fac Environm Earth Sci, Sapporo, Hokkaido 060, Japan. [Vernier, Jean-Paul] Sci Syst & Applicat Inc, Hampton, VA 23666 USA. [Vernier, Jean-Paul] NASA, Langley Res Ctr, Hampton, VA 23666 USA. RP Mehta, SK (reprint author), SRM Univ, Res Inst, Madras, Tamil Nadu, India. EM sanjaymehta@rish.kyoto-u.ac.jp FU Kyoto University [11380599]; Japan Society for the Promotion of Science (JSPS) Foundation [P12025]; [21340138] FX The first author (SKM) thanks Kyoto University for providing a grant for this study under the Mission Oriented Research Program (ID No. 11380599). This work is supported in part by the Japan Society for the Promotion of Science (JSPS) Foundation (ID No. P12025). This study was also supported in part by Grants-in-Aid for Scientific Research (No. 21340138). SKM thanks to Susan Solomon and Karen Rosenlof of NOAA, William Randel of National Center for Atmospheric Research and Masato Shiotani of Kyoto University for their valuable suggestions. NR 48 TC 1 Z9 1 U1 0 U2 11 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1364-6826 EI 1879-1824 J9 J ATMOS SOL-TERR PHY JI J. Atmos. Sol.-Terr. Phys. PD JUL PY 2015 VL 129 BP 99 EP 110 DI 10.1016/j.jastp.2015.04.009 PG 12 WC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences SC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences GA CK9JZ UT WOS:000356557700013 ER PT J AU Barre, J Edwards, D Worden, H Da Silva, A Lahoz, W AF Barre, Jerome Edwards, David Worden, Helen Da Silva, Arlindo Lahoz, William TI On the feasibility of monitoring carbon monoxide in the lower troposphere from a constellation of Northern Hemisphere geostationary satellites. (Part 1) SO ATMOSPHERIC ENVIRONMENT LA English DT Article DE Geostationary constellation; Observing system simulation experiments; Atmospheric composition; Air quality; Carbon monoxide; Global scale ID AIR-QUALITY; NEXT-GENERATION; OZONE; ASSIMILATION; POLLUTION; MISSION; EVENTS; MODEL; CO AB By the end of the current decade, there are plans to deploy several geostationary Earth orbit (GEO) satellite missions for atmospheric composition over North America, East Asia and Europe with additional missions proposed. Together, these present the possibility of a constellation of geostationary platforms to achieve continuous time-resolved high-density observations over continental domains for mapping pollutant sources and variability at diurnal and local scales. In this paper, we use a novel approach to sample a very high global resolution model (GEOS-5 at 7 km horizontal resolution) to produce a dataset of synthetic carbon monoxide pollution observations representative of those potentially obtainable from a GEO satellite constellation with predicted measurement sensitivities based on current remote sensing capabilities. Part 1 of this study focuses on the production of simulated synthetic measurements for air quality OSSEs (Observing System Simulation Experiments). We simulate carbon monoxide nadir retrievals using a technique that provides realistic measurements with very low computational cost. We discuss the sampling methodology: the projection of footprints and areas of regard for geostationary geometries over each of the North America, East Asia and Europe regions; the regression method to simulate measurement sensitivity; and the measurement error simulation. A detailed analysis of the simulated observation sensitivity is performed, and limitations of the method are discussed. We also describe impacts from clouds, showing that the efficiency of an instrument making atmospheric composition measurements on a geostationary platform is dependent on the dominant weather regime over a given region and the pixel size resolution. These results demonstrate the viability of the "instrument simulator" step for an OSSE to assess the performance of a constellation of geostationary satellites for air quality measurements. We describe the OSSE results in a follow up paper (Part 2 of this study). (C) 2015 Elsevier Ltd. All rights reserved. C1 [Barre, Jerome; Edwards, David; Worden, Helen] Natl Ctr Atmospher Res, Boulder, CO 80307 USA. [Da Silva, Arlindo] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Lahoz, William] NILU, Kjeller, Norway. RP Barre, J (reprint author), Natl Ctr Atmospher Res, POB 3000, Boulder, CO 80307 USA. EM barre@ucar.edu FU NASA [NNX09AH03G S02, NNX11AI10G, NNX11AG63G]; National Science Foundation FX This work was partly supported by NASA grants NNX09AH03G S02, NNX11AI10G and NNX11AG63G. The National Center for Atmospheric Research is sponsored by the National Science Foundation. NR 27 TC 2 Z9 2 U1 0 U2 8 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1352-2310 EI 1873-2844 J9 ATMOS ENVIRON JI Atmos. Environ. PD JUL PY 2015 VL 113 BP 63 EP 77 DI 10.1016/j.atmosenv.2015.04.069 PG 15 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA CK9GA UT WOS:000356547400008 ER PT J AU Sullivan, RC Levy, RC Pryor, SC AF Sullivan, R. C. Levy, R. C. Pryor, S. C. TI Spatiotemporal coherence of mean and extreme aerosol particle events over eastern North America as observed from satellite SO ATMOSPHERIC ENVIRONMENT LA English DT Article DE MODIS; AOD; Angstrom exponent; Extreme aerosol loading; Synoptic meteorology ID FINE PARTICULATE MATTER; UNITED-STATES; AIR-POLLUTION; OPTICAL DEPTH; VARIABILITY; PM2.5; US; PRECIPITATION; PRODUCTS; NETWORK AB Quantifying spatiotemporal scales of coherence and variability of aerosol particle properties provides (i) metrics for evaluating observational data sets and model simulations, (ii) inferences regarding dominant causes of variability, and (iii) information that is necessary to determine their climate forcing and air quality impacts. Accordingly, analyses of columnar aerosol optical depth (ADD) and Angstrom exponent (AE) from the MODerate resolution Imaging Spectroradiometer (MODIS) on the Aqua and Terra satellites, and AErosol RObotic NETwork (AERONET) stations are used to evaluate the spatially averaged (Level-3) MODIS products, and to characterize the spatiotemporal scales of variability (and coherence) of aerosol particles over eastern North America (2000-2013). Results show a high degree of consistency in AOD retrievals from the different data sets but larger discrepancies in AE estimates, highest mean AOD and lowest day-to-day variability during the summer, and largest scales of spatial coherence in summer and fall. Consistent with the scales of spatial coherence from MODIS data, in both data sets power spectra indicate AOD variability is manifest primarily on synoptic and annual time scales. Conversely, AE variability in MODIS data is primarily focused on seasonal, semiannual, and annual time scales, and there is an additional mode of AE variability at similar to 30 days in the AERONET measurements. The frequency of co-occurrence of extreme AOD values (>local 90th percentile) decreases to below 50% at similar to 150 km from a central grid cell, but is above that expected by random chance over almost all of eastern North America, indicating supra-regional scale extreme events. (C) 2015 Elsevier Ltd. All rights reserved. C1 [Sullivan, R. C.; Pryor, S. C.] Cornell Univ, Dept Earth & Atmospher Sci, Ithaca, NY 14853 USA. [Levy, R. C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Sullivan, RC (reprint author), Cornell Univ, Dept Earth & Atmospher Sci, 306 Tower Rd, Ithaca, NY 14853 USA. EM rcs365@cornell.edu; robert.c.levy@nasa.gov; sp2279@cornell.edu RI Levy, Robert/M-7764-2013; OI Levy, Robert/0000-0002-8933-5303; Sullivan, Ryan/0000-0002-3500-1842 FU NASA Headquarters under the NASA Earth and Space Science Fellowship Program [14-EARTH14F-0207]; SCP from NSF [1102309, 1517365] FX This work was supported by NASA Headquarters under the NASA Earth and Space Science Fellowship Program - Grant "14-EARTH14F-0207" and a grant to SCP from NSF (1102309, 1517365). The data used in this study were acquired as part of the NASA's Earth-Sun System Division and archived and distributed by the MODIS Level 1 and Atmosphere Archive and Distribution System (LAADS). The authors acknowledge useful conversations with R.J. Barthelmie and G. Filippelli, valuable input from two anonymous reviewers, and B. Holben, C. Lehmann, and M. Tragesser for establishing and maintaining the Bondville and Dayton AERONET sites. NR 35 TC 5 Z9 5 U1 0 U2 14 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1352-2310 EI 1873-2844 J9 ATMOS ENVIRON JI Atmos. Environ. PD JUL PY 2015 VL 112 BP 126 EP 135 DI 10.1016/j.atmosenv.2015.04.026 PG 10 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA CK4JT UT WOS:000356190800013 ER PT J AU Stark, SC Enquist, BJ Saleska, SR Leitold, V Schietti, J Longo, M Alves, LF Camargo, PB Oliveira, RC AF Stark, Scott C. Enquist, Brian J. Saleska, Scott R. Leitold, Veronika Schietti, Juliana Longo, Marcos Alves, Luciana F. Camargo, Plinio B. Oliveira, Raimundo C. TI Linking canopy leaf area and light environments with tree size distributions to explain Amazon forest demography SO ECOLOGY LETTERS LA English DT Article DE Amazon forest; canopy plasticity; canopy structure; forest dynamics; leaf area profiles; LiDAR; light competition; metabolic scaling theory; remote sensing; tree demography ID GENERAL QUANTITATIVE THEORY; NEOTROPICAL RAIN-FOREST; TROPICAL FOREST; METABOLIC ECOLOGY; CARBON DYNAMICS; SHADE TOLERANCE; BIOMASS; LIDAR; DISTURBANCE; ECOSYSTEM AB Forest biophysical structure - the arrangement and frequency of leaves and stems - emerges from growth, mortality and space filling dynamics, and may also influence those dynamics by structuring light environments. To investigate this interaction, we developed models that could use LiDAR remote sensing to link leaf area profiles with tree size distributions, comparing models which did not (metabolic scaling theory) and did allow light to influence this link. We found that a light environment-to-structure link was necessary to accurately simulate tree size distributions and canopy structure in two contrasting Amazon forests. Partitioning leaf area profiles into size-class components, we found that demographic rates were related to variation in light absorption, with mortality increasing relative to growth in higher light, consistent with a light environment feedback to size distributions. Combining LiDAR with models linking forest structure and demography offers a high-throughput approach to advance theory and investigate climate-relevant tropical forest change. C1 [Stark, Scott C.; Enquist, Brian J.; Saleska, Scott R.] Univ Arizona, Dept Ecol & Evolutionary Biol, Tucson, AZ 85721 USA. [Stark, Scott C.] Michigan State Univ, Dept Forestry, E Lansing, MI 48824 USA. [Enquist, Brian J.] Santa Fe Inst, Santa Fe, NM 87501 USA. [Leitold, Veronika] INPE, BR-12201970 Sao Paulo, Brazil. [Schietti, Juliana] INPA, Coordenacao Pesquisa Biodiversidade, BR-69011970 Manaus, Amazonas, Brazil. [Longo, Marcos] Harvard Univ, Fac Arts & Sci, Cambridge, MA 02138 USA. [Alves, Luciana F.] IAC, Ctr Pesquisa & Desenvolvimento Recursos Genet Veg, BR-13012970 Sao Paulo, Brazil. [Alves, Luciana F.] Univ Estadual Campinas UNICAMP, Dept Biol Vegetal, BR-13093970 Sao Paulo, Brazil. [Camargo, Plinio B.] Univ Sao Paulo, CENA, Lab Ecol Isotop, BR-13400970 Sao Paulo, Brazil. [Oliveira, Raimundo C.] Embrapa Amazonia Oriental, NAPT Medio Amazonas, BR-68035110 Santarem, Para, Brazil. [Oliveira, Raimundo C.] NASA, Goddard Space Flight Ctr, Biospher Sci Lab, Greenbelt, MD 20771 USA. [Oliveira, Raimundo C.] Empresa Brasileira Pesquisa Agr Embrapa, Monitoramento Satelite, BR-13070115 Sao Paulo, Brazil. RP Stark, SC (reprint author), Univ Arizona, Dept Ecol & Evolutionary Biol, Tucson, AZ 85721 USA. EM scott.c.stark@gmail.com RI Camargo, Plinio/D-6635-2012; Alves, Luciana/E-1141-2012; Longo, Marcos/F-5033-2014; OI Alves, Luciana/0000-0002-8944-1851; Longo, Marcos/0000-0001-5062-6245; Enquist, Brian/0000-0002-6124-7096 FU National Science Foundation [DDIG 0807221, DEB 0721140, OISE-PIRE 0730305, DEB-MSB 1340604]; National Air and Space Administration [NNX09AI33G]; NSF GRFP; NSF PIRE FX This work was supported by National Science Foundation awards (DDIG 0807221, DEB 0721140, OISE-PIRE 0730305, DEB-MSB 1340604) and the National Air and Space Administration (contract NNX09AI33G) while Stark was also supported by NSF GRFP and NSF PIRE fellowships. Extensive scientific field and logistical support were provided by administrators and technicians associated with the Brazilian institutions INPA-LBA, Embrapa Amazonia Oriental, INPA-Biodiversity, and PPBio/CENBAM, as well as local communities, in Santarem and Manaus. We acknowledge anonymous reviewers and members of the Saleska lab (U of A) and Kobe lab (MSU) for their excellent feedback that improved this manuscript. NR 50 TC 3 Z9 4 U1 6 U2 38 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1461-023X EI 1461-0248 J9 ECOL LETT JI Ecol. Lett. PD JUL PY 2015 VL 18 IS 7 BP 636 EP 645 DI 10.1111/ele.12440 PG 10 WC Ecology SC Environmental Sciences & Ecology GA CL0CJ UT WOS:000356606100004 PM 25963522 ER PT J AU Kohler, P Guanter, L Frankenberg, C AF Koehler, Philipp Guanter, Luis Frankenberg, Christian TI Simplified Physically Based Retrieval of Sun-Induced Chlorophyll Fluorescence From GOSAT Data SO IEEE GEOSCIENCE AND REMOTE SENSING LETTERS LA English DT Article DE Biosphere; environmental monitoring; geophysical measurement techniques; remote sensing; spectral analysis ID SPACE; SIMULATIONS; SATELLITE AB First global retrievals of sun-induced chlorophyll fluorescence (F-s) have been achieved in the last years by using data from the Fourier transform spectrometer (FTS) onboard the Japanese Greenhouse Gases Observing Satellite (GOSAT). The high spectral resolution (approximately 0.025 nm) of the FTS enables measurements of F-s by the evaluation of the in-filling of solar Fraunhofer lines around 755 nm. This study presents a new F-s retrieval algorithm (GARLiC, for GOSAT retrieval of chlorophyll fluorescence) and compares its results to F-s from two previously implemented approaches. GARLiC is intended to simplify some of the assumptions of existing retrieval approaches without a loss in retrieval accuracy. We show that GARLiC F-s retrievals are comparable to the previously used methods. We also assess the effect of clouds on F-s retrieval from GOSAT data through the analysis of the effect of different cloud filter thresholds on F-s time series. Our results show a low sensitivity of Fraunhofer-line-based F-s retrievals to cloud contamination. C1 [Koehler, Philipp; Guanter, Luis] German Ctr Geosci GFZ, Dept Geodesy & Remote Sensing, D-14473 Potsdam, Germany. [Frankenberg, Christian] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Kohler, P (reprint author), German Ctr Geosci GFZ, Dept Geodesy & Remote Sensing, D-14473 Potsdam, Germany. EM philipp.koehler@gfz-potsdam.de; luis.guanter@wew.fu-berlin.de; Christian.Frankenberg@jpl.nasa.gov RI Guanter, Luis/I-1588-2015; Frankenberg, Christian/A-2944-2013 OI Guanter, Luis/0000-0002-8389-5764; Frankenberg, Christian/0000-0002-0546-5857 NR 14 TC 1 Z9 1 U1 3 U2 25 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1545-598X EI 1558-0571 J9 IEEE GEOSCI REMOTE S JI IEEE Geosci. Remote Sens. Lett. PD JUL PY 2015 VL 12 IS 7 BP 1446 EP 1450 DI 10.1109/LGRS.2015.2407051 PG 5 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA CK9EJ UT WOS:000356543100003 ER PT J AU Rosette, J Cook, B Nelson, R Huang, CQ Masek, J Tucker, C Sun, GQ Huang, WL Montesano, P Rubio-Gil, J Ranson, J AF Rosette, Jacqueline Cook, Bruce Nelson, Ross Huang, Chengquan Masek, Jeff Tucker, Compton Sun, Guoqing Huang, Wenli Montesano, Paul Rubio-Gil, Jeremy Ranson, Jon TI Sensor Compatibility for Biomass Change Estimation Using Remote Sensing Data Sets: Part of NASA's Carbon Monitoring System Initiative SO IEEE GEOSCIENCE AND REMOTE SENSING LETTERS LA English DT Article DE Forest biomass change; landsat disturbance; LiDAR; remote sensing time-series analysis ID FOREST BIOMASS; DETECTING TRENDS; LIDAR DATA; DISTURBANCE; AIRBORNE; HISTORY AB Time series of remote sensing data offers the opportunity to predict changes in vegetation extent and to estimate forest parameter change such as biomass. However, as sensors and technology advance, it is important to ensure that estimates obtained from different time periods or using different, but related, instruments are consistent in order to have confidence in detected change. This study compares estimates of biomass from small-footprint discrete-return LiDAR data and medium-footprint full-waveform LiDAR for Howland Experimental Forest, Maine, USA. Data were collected from both sensors during Summer 2009. Similar results were found using the same height metric with R-2 = 0.67, SE = 58.5 Mg ha(-1) and R-2 = 0.52, SE = 58.1 Mg ha(-1), respectively. The predicted model of the relationship between LiDAR metrics and biomass was applied to data captured in 2003. Identified areas of change corresponded well with a map of forest management operations of varying intensities. Where sensitivity to change allows, vegetation age estimated using time series of Landsat observations, combined with biomass estimates, allows growth curves to be produced to monitor the effect of pests or disease, recovery rates following disturbance, or carbon sequestration. C1 [Rosette, Jacqueline; Cook, Bruce; Nelson, Ross; Masek, Jeff; Tucker, Compton; Sun, Guoqing; Montesano, Paul; Rubio-Gil, Jeremy; Ranson, Jon] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Rosette, Jacqueline; Huang, Chengquan; Sun, Guoqing; Huang, Wenli; Rubio-Gil, Jeremy] Univ Maryland, College Pk, MD 20742 USA. [Montesano, Paul] Sigma Space Corp, Greenbelt, MD 20771 USA. [Rubio-Gil, Jeremy] Univ Toulouse, Ctr Etudes Spati BIOsphere CESBIO, F-31401 Toulouse, France. RP Rosette, J (reprint author), Forest Res Northern Res Stn, Roslin EH25 9SY, Midlothian, Scotland. EM j.a.rosette@swansea.ac.uk; bruce.cook@nasa.gov; Ross.F.Nelson@nasa.gov; cqhuang@umd.edu; jeffrey.g.masek@nasa.gov; compton.j.tucker@nasa.gov; guoqing.sun-1@nasa.gov; wlhuang@nasa.gov; Paul.M.Montesano@nasa.gov; jeremy.rubio-1@nasa.gov; kenneth.j.ranson@nasa.gov RI Masek, Jeffrey/D-7673-2012; Beckley, Matthew/D-4547-2013 NR 34 TC 1 Z9 1 U1 5 U2 19 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1545-598X EI 1558-0571 J9 IEEE GEOSCI REMOTE S JI IEEE Geosci. Remote Sens. Lett. PD JUL PY 2015 VL 12 IS 7 BP 1511 EP 1515 DI 10.1109/LGRS.2015.2411262 PG 5 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA CK9EJ UT WOS:000356543100016 ER PT J AU Kalmus, P Wong, S Teixeira, J AF Kalmus, Peter Wong, Sun Teixeira, Joao TI The Pacific Subtropical Cloud Transition: A MAGIC Assessment of AIRS and ECMWF Thermodynamic Structure SO IEEE GEOSCIENCE AND REMOTE SENSING LETTERS LA English DT Article DE Clouds; infrared spectroscopy AB We use radiosonde data from the ship-based Marine ARM GPCI Investigation of Clouds (MAGIC) campaign in the northeast Pacific to validate temperature and moisture profiles from the satellite-based Atmospheric Infrared Sounder (AIRS) instrument and from European Centre for Medium-Range Weather Forecasts (ECMWF) ERA-Interim reanalysis data. We find that AIRS and ECMWF rms errors and biases are largest near the boundary layer inversion. In the mean vertical profile over the entire MAGIC track, the largest AIRS biases for T and q are 0.4 K and -0.6 g kg(-1) at 516 hPa and 866 hPa, respectively. We also find that AIRS and ECMWF slightly underestimate the boundary layer height in the region. C1 [Kalmus, Peter; Wong, Sun; Teixeira, Joao] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Kalmus, P (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM peter.m.kalmus@jpl.nasa.gov FU U.S. Department of Energy FX The research described in this letter was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration (NASA). The authors would also like to acknowledge the NASA Making Earth System Data Records for Use in Research Environments (MEaSUREs) program. Publicly available data were obtained from the NASA CloudSat and Atmospheric Infrared Sounder projects, the European Centre for Medium-Range Weather Forecasts reanalysis, and the Atmospheric Radiation Measurement Program sponsored by the U.S. Department of Energy. NR 15 TC 1 Z9 1 U1 1 U2 2 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1545-598X EI 1558-0571 J9 IEEE GEOSCI REMOTE S JI IEEE Geosci. Remote Sens. Lett. PD JUL PY 2015 VL 12 IS 7 BP 1586 EP 1590 DI 10.1109/LGRS.2015.2413771 PG 5 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA CK9EJ UT WOS:000356543100031 ER PT J AU Sharma, A Melancon, JM Bailey, SG Zivanovic, SR AF Sharma, Ashish Melancon, Justin M. Bailey, Sheila G. Zivanovic, Sandra R. TI Betavoltaic Cells Using P3HT Semiconductive Conjugated Polymer SO IEEE TRANSACTIONS ON ELECTRON DEVICES LA English DT Article DE Beta rays; betavoltaic; degradation; electron beam (e-beam); optical polymers; phosphors; poly(3-hexylthiophene): indene-C-60 bisadduct (P3HT:ICBA); scintillator ID SOLAR-CELLS; EFFICIENCY; PERFORMANCE AB The need for extreme-duration light-weight power sources for space applications motivates the study and development of polymer-based betavoltaics. The betavoltaic device, based on the semiconductive polymer-fullerene blend of poly(3-hexylthiophene): indene-C-60 bisadduct (P3HT:ICBA), is demonstrated here for the first time. Both direct and indirect energy conversion methods were explored. For the indirect conversion method, a phosphor intermediate layer of cerium-doped yttrium aluminum garnet (Ce:YAG) was used on top of the polymer device. A high open circuit voltage of 0.56 V has been achieved in the betavoltaic device fabricated on a polyethylene terephthalate (PET) substrate with indirect energy conversion at 30-keV electron kinetic energy. The maximum output electrical power of 62 nW was achieved at 30-keV input electron beam (e-beam) energy. The highest betavoltaic power conversion efficiency of 0.78% was achieved at an e-beam energy of 10 keV. Using the thin PET substrate instead of a glass substrate for the polymer device and phosphor screen fabrication, the betavoltaic device performance has been significantly improved due to a reduction in physical distance between photon-generating Ce:YAG phosphor screen and photon-absorbing P3HT:ICBA layer. The use of the PET substrates helped by significantly decreasing the directional and external interaction losses. C1 [Sharma, Ashish; Zivanovic, Sandra R.] Louisiana Tech Univ, Inst Micromfg, Ruston, LA 71272 USA. [Melancon, Justin M.] Louisiana Tech Univ, Ruston, LA 71272 USA. [Bailey, Sheila G.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Sharma, A (reprint author), Louisiana Tech Univ, Inst Micromfg, Ruston, LA 71272 USA. EM ash046@latech.edu; jmmelancon@gmail.com; Sheila.G.Bailey@nasa.gov; sz@latech.edu FU NASA Experimental Program to Stimulate Competitive Research (EPSCoR)/Louisiana Board of Regents [NNX13AB14A [LEQSF-EPS (2013)-RAP-03]] FX Manuscript received February 25, 2015; revised May 4, 2015; accepted May 14, 2015. Date of publication June 5, 2015; date of current version June 17, 2015. This work was supported by the NASA Experimental Program to Stimulate Competitive Research (EPSCoR)/Louisiana Board of Regents, under Grant NNX13AB14A [LEQSF-EPS (2013)-RAP-03]. The review of this paper was arranged by Editor A. G. Aberle. NR 20 TC 0 Z9 0 U1 2 U2 19 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0018-9383 EI 1557-9646 J9 IEEE T ELECTRON DEV JI IEEE Trans. Electron Devices PD JUL PY 2015 VL 62 IS 7 BP 2320 EP 2326 DI 10.1109/TED.2015.2434852 PG 7 WC Engineering, Electrical & Electronic; Physics, Applied SC Engineering; Physics GA CK7ZY UT WOS:000356457900037 ER PT J AU Quadrelli, MB Wood, LJ Riedel, JE McHenry, MC Aung, M Cangahuala, LA Volpe, RA Beauchamp, PM Cutts, JA AF Quadrelli, Marco B. Wood, Lincoln J. Riedel, Joseph E. McHenry, Michael C. Aung, MiMi Cangahuala, Laureano A. Volpe, Richard A. Beauchamp, Patricia M. Cutts, James A. TI Guidance, Navigation, and Control Technology Assessment for Future Planetary Science Missions SO JOURNAL OF GUIDANCE CONTROL AND DYNAMICS LA English DT Article ID DEEP SPACE NAVIGATION; EXPLORATION; DESCENT; CHALLENGES; ALGORITHM; EVOLUTION; TRACKING; ENTRY C1 [Quadrelli, Marco B.; Wood, Lincoln J.; Riedel, Joseph E.; McHenry, Michael C.; Aung, MiMi; Cangahuala, Laureano A.; Volpe, Richard A.; Beauchamp, Patricia M.; Cutts, James A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Quadrelli, MB (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 46 TC 6 Z9 7 U1 1 U2 14 PU AMER INST AERONAUTICS ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0731-5090 EI 1533-3884 J9 J GUID CONTROL DYNAM JI J. Guid. Control Dyn. PD JUL PY 2015 VL 38 IS 7 BP 1165 EP 1186 DI 10.2514/1.G000525 PG 22 WC Engineering, Aerospace; Instruments & Instrumentation SC Engineering; Instruments & Instrumentation GA CK4HB UT WOS:000356183800001 ER PT J AU Govindarajan, N de Visser, CC van Kampen, E Krishnakumar, K Barlow, J Stepanyan, V AF Govindarajan, N. de Visser, C. C. van Kampen, E. Krishnakumar, K. Barlow, J. Stepanyan, V. TI Optimal Control Framework for Estimating Autopilot Safety Margins SO JOURNAL OF GUIDANCE CONTROL AND DYNAMICS LA English DT Article ID ENVELOPE PROTECTION; TRAJECTORY OPTIMIZATION; AIRCRAFT AB This paper presents an optimal control framework to determine a collection of open-loop command signals that mathematically guarantees operation of an aircraft within certain prescribed state constraints. The framework is specifically applied to estimate margins for the reference command inputs of aircraft autopilot systems so that safe operation within a given flight envelope can be assured under appropriate control action. Flight envelope excursions are generally considered as precursors to loss-of-control incidents; hence, these margins contain safety-critical information that can help improve the situational awareness onboard the aircraft. In off-nominal conditions, the computed safety margins provide indications of a degraded aircraft with reduced flying and handling qualities. These indications appear in the form of increasingly more strict limits on the autopilot reference command input. The entire framework is illustrated on an example problem involving a pitch dynamics model with state constraints on the pitch attitude. Simulations are conducted wherein margins are computed for the reference pitch command of the pitch hold system, while the aircraft enters an off-nominal condition with severely degraded system dynamics and reduced elevator effectiveness. C1 [Govindarajan, N.] Delft Univ Technol, Fac Mech Maritime & Mat Engn, Delft Ctr Syst & Control, NL-2629 HS Delft, Netherlands. [de Visser, C. C.; van Kampen, E.] Delft Univ Technol, Fac Aerosp Engn, Control & Simulat, NL-2629 HS Delft, Netherlands. [Krishnakumar, K.] NASA, Ames Res Ctr, Intelligent Syst Div, Automat Syst & Robot, Moffett Field, CA 94035 USA. [Barlow, J.] NASA, Ames Res Ctr, Stinger Ghaffarian Technol Inc, Moffett Field, CA 94035 USA. [Stepanyan, V.] NASA, Ames Res Ctr, Mission Crit Technol Inc, Moffett Field, CA 94035 USA. RP Govindarajan, N (reprint author), Delft Univ Technol, Fac Mech Maritime & Mat Engn, Delft Ctr Syst & Control, NL-2629 HS Delft, Netherlands. EM nithin.govindarajan@gmail.com; C.C.deVisser@tudelft.nl; E.vankampen@tudelft.nl; kalmanje.krishnakumar@nasa.gov; jonathan.s.Barlow@nasa.gov; vahram.stepanyan@nasa.gov NR 30 TC 2 Z9 2 U1 2 U2 8 PU AMER INST AERONAUTICS ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0731-5090 EI 1533-3884 J9 J GUID CONTROL DYNAM JI J. Guid. Control Dyn. PD JUL PY 2015 VL 38 IS 7 BP 1197 EP 1207 DI 10.2514/1.G000271 PG 11 WC Engineering, Aerospace; Instruments & Instrumentation SC Engineering; Instruments & Instrumentation GA CK4HB UT WOS:000356183800003 ER PT J AU Semper, SR Crassidis, JL George, J Mukherjee, S Singla, P AF Semper, Sean R. Crassidis, John L. George, Jemin Mukherjee, Siddharth Singla, Puneet TI Rao-Blackwellization for Adaptive Gaussian Sum Nonlinear Model Propagation SO JOURNAL OF GUIDANCE CONTROL AND DYNAMICS LA English DT Article ID STATE-SPACE MODELS; PARTICLE FILTERS C1 [Semper, Sean R.] NASA, Goddard Space Flight Ctr, Guidance Nav & Control Hardware, Greenbelt, MD 20771 USA. [Semper, Sean R.] NASA, Components Branch, Greenbelt, MD 20771 USA. [George, Jemin] SUNY Buffalo, Dept Mech & Aerosp Engn, Space Situat Awareness, Amherst, NY 14260 USA. [George, Jemin] US Army Res Lab, Networked Sensing & Fus Branch, Adelphi, MD 20783 USA. [Mukherjee, Siddharth; Singla, Puneet] SUNY Buffalo, Dept Mech & Aerosp Engn, Amherst, NY 14260 USA. RP Semper, SR (reprint author), NASA, Goddard Space Flight Ctr, Guidance Nav & Control Hardware, Greenbelt, MD 20771 USA. EM sean.r.semper@nasa.gov; johnc@buffalo.edu; jemin.george.civ@mail.mil; smukherj@buffalo.edu; psingla@buffalo.edu RI Singla, Puneet/D-3642-2012 OI Singla, Puneet/0000-0002-2441-2531 NR 12 TC 1 Z9 1 U1 0 U2 0 PU AMER INST AERONAUTICS ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0731-5090 EI 1533-3884 J9 J GUID CONTROL DYNAM JI J. Guid. Control Dyn. PD JUL PY 2015 VL 38 IS 7 BP 1290 EP 1295 DI 10.2514/1.G001042 PG 6 WC Engineering, Aerospace; Instruments & Instrumentation SC Engineering; Instruments & Instrumentation GA CK4HB UT WOS:000356183800011 ER PT J AU Zanetti, R AF Zanetti, Renato TI Adaptable Recursive Update Filter SO JOURNAL OF GUIDANCE CONTROL AND DYNAMICS LA English DT Article ID COVARIANCES C1 NASA, Johnson Space Ctr, Aerosci & Flight Mech Div, Houston, TX 77058 USA. RP Zanetti, R (reprint author), NASA, Johnson Space Ctr, Aerosci & Flight Mech Div, 2101 NASA Parkway, Houston, TX 77058 USA. NR 12 TC 1 Z9 1 U1 0 U2 1 PU AMER INST AERONAUTICS ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0731-5090 EI 1533-3884 J9 J GUID CONTROL DYNAM JI J. Guid. Control Dyn. PD JUL PY 2015 VL 38 IS 7 BP 1296 EP U9 DI 10.2514/1.G001031 PG 5 WC Engineering, Aerospace; Instruments & Instrumentation SC Engineering; Instruments & Instrumentation GA CK4HB UT WOS:000356183800012 ER PT J AU Healy, AF Tack, LA Schneider, VI Barshi, I AF Healy, Alice F. Tack, Lindsay Anderson Schneider, Vivian I. Barshi, Immanuel TI Training specificity and transfer in time and distance estimation SO MEMORY & COGNITION LA English DT Article DE Skill acquisition; Time estimation; Distance estimation; Training specificity; Transfer ID BASIC ARITHMETIC SKILLS; FLUID INTELLIGENCE; WORKING-MEMORY; TASK AB Learning is often specific to the conditions of training, making it important to identify which aspects of the testing environment are crucial to be matched in the training environment. In the present study, we examined training specificity in time and distance estimation tasks that differed only in the focus of processing (FOP). External spatial cues were provided for the distance estimation task and for the time estimation task in one condition, but not in another. The presence of a concurrent alphabet secondary task was manipulated during training and testing in all estimation conditions in Experiment 1. For distance as well as for time estimation in both conditions, training of the primary estimation task was found to be specific to the presence of the secondary task. In Experiments 2 and 3, we examined transfer between one estimation task and another, with no secondary task in either case. When all conditions were equal aside from the FOP instructions, including the presence of external spatial cues, Experiment 2 showed "transfer" between tasks, suggesting that training might not be specific to the FOP. When the external spatial cues were removed from the time estimation task, Experiment 3 showed no transfer between time and distance estimations, suggesting that external task cues influenced the procedures used in the estimation tasks. C1 [Healy, Alice F.; Tack, Lindsay Anderson; Schneider, Vivian I.] Univ Colorado, Dept Psychol & Neurosci, Boulder, CO 80309 USA. [Barshi, Immanuel] NASA, Human Syst Integrat Div, Ames Res Ctr, Mountain View, CA USA. RP Healy, AF (reprint author), Univ Colorado, Dept Psychol & Neurosci, Muenzinger Bldg,345 UCB, Boulder, CO 80309 USA. EM alice.healy@colorado.edu FU National Aeronautics and Space Administration [NNX10AC87A, NNX14AB75A] FX This research was supported in part by National Aeronautics and Space Administration Grant Numbers NNX10AC87A and NNX14AB75A to the University of Colorado. We thank the members of the Center for Research on Training at the University of Colorado for helpful suggestions about this research. We are indebted to Robert Proctor, Timothy Rickard, Steven Pan, and an anonymous reviewer for helpful comments on an earlier version of this article; Mary Guhl and Simone Addison for help testing the subjects in Experiment 1; Lakshmi Lalchandani for help with data tabulation; Mark Thrasher for help testing the subjects in Experiments 2 and 3; and Ernest Mross for programming the experiments. Experiments 2 and 3 were summarized in a poster at the 2011 meeting of the Psychonomic Society in Seattle, WA. Experiment 1 was conducted after Experiments 2 and 3, but is reported first for ease of exposition. NR 22 TC 0 Z9 0 U1 2 U2 4 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0090-502X EI 1532-5946 J9 MEM COGNITION JI Mem. Cogn. PD JUL PY 2015 VL 43 IS 5 BP 736 EP 747 DI 10.3758/s13421-015-0503-9 PG 12 WC Psychology, Experimental SC Psychology GA CL1UG UT WOS:000356729800004 PM 25616777 ER PT J AU Cardoso, CV Burningham, B Smart, RL van Spaandonk, L Baker, D Smith, LC Zhang, ZH Andrei, AH Bucciarelli, B Dhital, S Jones, HRA Lattanzi, MG Magazzu, A Pinfield, DJ Tinney, CG AF Cardoso, C. V. Burningham, B. Smart, R. L. van Spaandonk, L. Baker, D. Smith, L. C. Zhang, Z. H. Andrei, A. H. Bucciarelli, B. Dhital, S. Jones, H. R. A. Lattanzi, M. G. Magazzu, A. Pinfield, D. J. Tinney, C. G. TI 49 new T dwarfs identified using methane imaging SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE surveys; brown dwarfs; stars: low-mass ID DIGITAL SKY SURVEY; LARGE-AREA SURVEY; L/T TRANSITION; BROWN DWARF; UKIDSS; STARS; CATALOG; PERFORMANCE; DENSITY; MISSION AB We present the discovery of 49 new photometrically classified T dwarfs from the combination of large infrared and optical surveys combined with follow-up Telescopio Nazionale Galileo photometry. We used multiband infrared and optical photometry from the United Kingdom Infrared Telescope and Sloan Digital Sky Surveys to identify possible brown dwarf candidates, which were then confirmed using methane filter photometry. We have defined a new photometric conversion between CH(4)s - CH(4)l colour and spectral type for T4-T8 brown dwarfs based on a part of the sample that has been followed up using methane photometry and spectroscopy. Using methane differential photometry as a proxy for spectral type for T dwarfs has proved to be a very efficient technique. Of a subset of 45 methane selected brown dwarfs that were observed spectroscopically, 100 per cent were confirmed as T dwarfs. Future deep imaging surveys will produce large samples of faint brown dwarf candidates, for which spectroscopy will not be feasible. When broad wavelength coverage is unavailable, methane imaging offers a means to efficiently classify candidates from such surveys using just a pair of near-infrared images. C1 [Cardoso, C. V.; Smart, R. L.; Bucciarelli, B.; Lattanzi, M. G.] Osservatorio Astrofis Torino, Ist Nazl Astrofis, I-10025 Pino Torinese, Italy. [Cardoso, C. V.; Burningham, B.; van Spaandonk, L.; Baker, D.; Smith, L. C.; Zhang, Z. H.; Andrei, A. H.; Jones, H. R. A.; Pinfield, D. J.] Univ Hertfordshire, Ctr Astrophys Res, Sci & Technol Res Inst, Hatfield AL10 9AB, Herts, England. [Burningham, B.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [van Spaandonk, L.] King Edward VI Sch, Stratford Upon Avon CV37 6HB, Warwick, England. [Zhang, Z. H.] Inst Astrofis Canarias, E-38205 Tenerife, Spain. [Zhang, Z. H.] Univ La Laguna, Dept Astrofis, E-38206 Tenerife, Spain. [Andrei, A. H.] Observ Nacl, BR-20921400 Rio De Janeiro, RJ, Brazil. [Andrei, A. H.] Observ Paris, SYRTE, F-75014 Paris, France. [Andrei, A. H.] Observ Valongo UFRJ, BR-20080090 Rio De Janeiro, RJ, Brazil. [Dhital, S.] Boston Univ, Dept Astron, Boston, MA 02215 USA. [Magazzu, A.] Fdn Galileo Galilei INAF, E-38712 Brena Baja, Spain. [Tinney, C. G.] Univ New S Wales, Australian Ctr Astrobiol, Sydney, NSW 2052, Australia. [Tinney, C. G.] Univ New S Wales, Sch Phys, Sydney, NSW 2052, Australia. RP Cardoso, CV (reprint author), Osservatorio Astrofis Torino, Ist Nazl Astrofis, Str Osservatorio 20, I-10025 Pino Torinese, Italy. EM b.burningham@herts.ac.uk OI Magazzu, Antonio/0000-0003-1259-4371; Lattanzi, Mario Gilberto/0000-0003-0429-7748; Smart, Richard/0000-0002-4424-4766; Burningham, Ben/0000-0003-4600-5627; Tinney, Christopher/0000-0002-7595-0970; Jones, Hugh/0000-0003-0433-3665 FU European Commission [PIOF-GA-2013-629435]; Marie Curie 7th European Community [236735, 247593] FX The author's would like to thank the staff of the TNG for their excellent support during of the very large programme on which this work is based. BB acknowledges financial support from the European Commission in the form of a Marie Curie International Outgoing Fellowship (PIOF-GA-2013-629435). This research has benefitted from the SpeX Prism Spectral Libraries, maintained by Adam Burgasser at http://pono.ucsd.edu/similar to adam/browndwarfs/spexprism. The authors also acknowledge the Marie Curie 7th European Community Framework Programme grant no. 236735 Parallaxes of Southern Extremely Cool objects (PARSEC) International Incoming Fellowship and grant no. 247593 Interpretation and Parametrization of Extremely Red COOL dwarfs (IPERCOOL) International Research Staff Exchange Scheme. Based on observations made with the Italian TNG operated on the island of La Palma by the Fundacin Galileo Galilei of the Istituto Nazionale di Astrofisica at the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias. The United Kingdom Infrared Telescope (UKIRT) was operated by the Joint Astronomy Centre on behalf of the Science and Technology Facilities Council of the UK. This work is based in part on data obtained as part of the UKIRT Infrared Deep Sky Survey. NR 40 TC 1 Z9 1 U1 1 U2 7 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUL 1 PY 2015 VL 450 IS 3 BP 2486 EP 2499 DI 10.1093/mnras/stv380 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CK6LJ UT WOS:000356339300021 ER PT J AU Saez, C Lehmer, BD Bauer, FE Stern, D Gonzales, A Rreza, I Alexander, DM Matsuda, Y Geach, JE Harrison, FA Hayashino, T AF Saez, C. Lehmer, B. D. Bauer, F. E. Stern, D. Gonzales, A. Rreza, I. Alexander, D. M. Matsuda, Y. Geach, J. E. Harrison, F. A. Hayashino, T. TI An extragalactic spectroscopic survey of the SSA22 field SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE techniques: imaging spectroscopy; surveys; galaxies: active; galaxies: clusters: general; X-rays: galaxies ID ACTIVE GALACTIC NUCLEI; VLT DEEP SURVEY; ABSORPTION-LINE QUASARS; LYMAN-BREAK GALAXIES; DIGITAL SKY SURVEY; LY-ALPHA BLOBS; REDSHIFT RADIO GALAXIES; STAR-FORMING GALAXIES; FAINT X-RAY; DIFFERENTIAL REFRACTION AB We present Very Large Telescope VIMOS, Keck DEIMOS and Keck LRIS multi-object spectra of 367 sources in the field of the z a parts per thousand 3.09 protocluster SSA22. Sources are spectroscopically classified via template matching, allowing new identifications for 206 extragalactic sources, including 36 z > 2 Lyman-break galaxies (LBGs) and Lyman alpha emitters (LAEs), eight protocluster members, and 94 X-ray sources from the similar to 400 ks Chandra deep survey of SSA22. Additionally, in the area covered by our study, we have increased by a parts per thousand 4, 13, and 6 times the number of reliable redshifts of sources at 1.0 < z < 2.0, at z > 3.4, and with X-ray emission, respectively. We compare our results with past spectroscopic surveys of SSA22 to investigate the completeness of the LBGs and the X-ray properties of the new spectroscopically classified sources in the SSA22 field. C1 [Saez, C.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Lehmer, B. D.] Johns Hopkins Univ, Baltimore, MD 21218 USA. [Lehmer, B. D.] NASA Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Bauer, F. E.] Pontificia Univ Catolica Chile, Fac Fis, Inst Astrofis, Santiago 306 22, Chile. [Bauer, F. E.] Millennium Inst Astrophys, Santiago, Chile. [Bauer, F. E.] Space Sci Inst, Boulder, CO 80301 USA. [Stern, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Gonzales, A.] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA. [Rreza, I.; Harrison, F. A.] CALTECH, Cahill Ctr Astrophys, Pasadena, CA 91125 USA. [Alexander, D. M.] Univ Durham, Dept Phys, Durham DH1 3LE, England. [Matsuda, Y.] Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan. [Matsuda, Y.] Grad Univ Adv Studies SOKENDAI, Mitaka, Tokyo 1810015, Japan. [Geach, J. E.] Univ Hertfordshire, Sci Technol Res Inst, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England. [Hayashino, T.] Tohoku Univ, Inst Astron, Aoba Ku, Sendai, Miyagi 9808578, Japan. RP Saez, C (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA. EM csaez@astro.umd.edu FU CONICYT-Chile [FONDECYT 3120198, Becas Chile 74140006, Anillo ACT1101, Basal-CATA PFB-06/2007, FONDECYT 1141218, Gemini-CONICYT 32120003, 'EMBIGGEN" Anillo ACT1101]; Millennium Institute of Astrophysics (MAS)' - Iniciativa Cientifica Milenio del Ministerio de Economia, Fomento y Turismo [IC120009]; NASA; ESO Telescopes at the Paranal Observatory [085.A-0616, 089.A-0405]; W.M. Keck Foundation FX We would like to thank Ezequiel Treister and the anonymous referee for helpful discussions regarding the interpretations of our results. We would also like to thank Scott Chapman for providing radio images of the SSA22 field. CS acknowledges support from CONICYT-Chile (FONDECYT 3120198, Becas Chile 74140006, and the Anillo ACT1101). FEB acknowledges support from CONICYT-Chile (Basal-CATA PFB-06/2007, FONDECYT 1141218, Gemini-CONICYT 32120003, 'EMBIGGEN" Anillo ACT1101), and Project IC120009 'Millennium Institute of Astrophysics (MAS)' funded by the Iniciativa Cientifica Milenio del Ministerio de Economia, Fomento y Turismo. The work of DS was carried out at Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. JEG thanks the Royal Society.; Based on observations made with ESO Telescopes at the Paranal Observatory under programme IDs 085.A-0616 and 089.A-0405. 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 wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. NR 73 TC 4 Z9 4 U1 1 U2 4 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUL 1 PY 2015 VL 450 IS 3 BP 2615 EP 2630 DI 10.1093/mnras/stv747 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CK6LJ UT WOS:000356339300029 ER PT J AU Ng, C Champion, DJ Bailes, M Barr, ED Bates, SD Bhat, NDR Burgay, M Burke-Spolaor, S Flynn, CML Jameson, A Johnston, S Keith, MJ Kramer, M Levin, L Petroff, E Possenti, A Stappers, BW van Straten, W Tiburzi, C Eatough, RP Lyne, AG AF Ng, C. Champion, D. J. Bailes, M. Barr, E. D. Bates, S. D. Bhat, N. D. R. Burgay, M. Burke-Spolaor, S. Flynn, C. M. L. Jameson, A. Johnston, S. Keith, M. J. Kramer, M. Levin, L. Petroff, E. Possenti, A. Stappers, B. W. van Straten, W. Tiburzi, C. Eatough, R. P. Lyne, A. G. TI The High Time Resolution Universe Pulsar Survey - XII. Galactic plane acceleration search and the discovery of 60 pulsars SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE methods: data analysis; surveys; stars: neutron; pulsars: general ID WHITE-DWARF COMPANIONS; 5 MILLISECOND PULSARS; BINARY RADIO PULSAR; INITIAL DISCOVERIES; RECYCLED PULSARS; PSR J1614-2230; SPIN PERIODS; POPULATION; I.; EVOLUTION AB We present initial results from the low-latitude Galactic plane region of the High Time Resolution Universe pulsar survey conducted at the Parkes 64-m radio telescope. We discuss the computational challenges arising from the processing of the terabyte-sized survey data. Two new radio interference mitigation techniques are introduced, as well as a partially coherent segmented acceleration search algorithm which aims to increase our chances of discovering highly relativistic short-orbit binary systems, covering a parameter space including potential pulsar-black hole binaries. We show that under a constant acceleration approximation, a ratio of data length over orbital period of a parts per thousand 0.1 results in the highest effectiveness for this search algorithm. From the 50 per cent of data processed thus far, we have redetected 435 previously known pulsars and discovered a further 60 pulsars, two of which are fast-spinning pulsars with periods less than 30 ms. PSR J1101-6424 is a millisecond pulsar whose heavy white dwarf (WD) companion and short spin period of 5.1 ms indicate a rare example of full-recycling via Case A Roche lobe overflow. PSR J1757-27 appears to be an isolated recycled pulsar with a relatively long spin period of 17 ms. In addition, PSR J1244-6359 is a mildly recycled binary system with a heavy WD companion, PSR J1755-25 has a significant orbital eccentricity of 0.09 and PSR J1759-24 is likely to be a long-orbit eclipsing binary with orbital period of the order of tens of years. Comparison of our newly discovered pulsar sample to the known population suggests that they belong to an older population. Furthermore, we demonstrate that our current pulsar detection yield is as expected from population synthesis. C1 [Ng, C.; Champion, D. J.; Eatough, R. P.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Bailes, M.; Barr, E. D.; Bhat, N. D. R.; Flynn, C. M. L.; Jameson, A.; van Straten, W.] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia. [Bailes, M.; Barr, E. D.; Bhat, N. D. R.; Flynn, C. M. L.; Petroff, E.; van Straten, W.] Swinburne Univ Technol, ARC Ctr Excellence All Sky Astron CAASTRO, Hawthorn, Vic 3122, Australia. [Bates, S. D.] Natl Radio Astron Observ, Green Bank, WV 24944 USA. [Bates, S. D.; Keith, M. J.; Kramer, M.; Stappers, B. W.; Lyne, A. G.] Univ Manchester, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England. [Bhat, N. D. R.] Curtin Univ, Int Ctr Radio Astron Res, Bentley, WA 6102, Australia. [Burgay, M.; Possenti, A.] INAF Osservatorio Astron Cagliari, I-09047 Selargius, Italy. [Burke-Spolaor, S.] NASA Jet Prop Lab, Pasadena, CA 91106 USA. [Johnston, S.; Petroff, E.] CSIRO Astron & Space Sci, Australia Telescope Natl Facil, Epping, NSW 1710, Australia. [Levin, L.] W Virginia Univ, Dept Phys, Morgantown, WV 26506 USA. [Tiburzi, C.] Univ Cagliari, Dipartimento Fis, I-09042 Monserrato, CA, Italy. RP Ng, C (reprint author), Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany. EM cherryng@mpifr-bonn.mpg.de OI Champion, David/0000-0003-1361-7723; Burgay, Marta/0000-0002-8265-4344; van Straten, Willem/0000-0003-2519-7375 FU Commonwealth of Australia; Science and Technology Facilities Council (STFC); International Max Planck Research School (IM-PRS) for Astronomy and Astrophysics at the Universities of Bonn; Cologne FX The Parkes Observatory 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. A large amount of the crucial computing resources needed for the data processing work is supported by the Australian National Computational Infrastructure (NCI) high performance computing centre at The Australian National University (ANU) and the ARC Centre of Excellence for All-sky Astrophysics (CAASTRO), as well as the HYDRA computer cluster funded by the Science and Technology Facilities Council (STFC). The authors would like to thank Anthony Holloway for providing constant support on the use of the HYDRA facilities, as well as the CAASTRO help desk for their every time swift replies. We thank Sally Cooper and Robert Dickson of the University of Manchester for helping the logistics of tape changing. We also thank Johnathon Kocz for useful discussion on RFI mitigation techniques, Thomas Tauris for sharing his knowledge on pulsar evolution, Paulo Freire for teaching the art of solving binary pulsars, Gregory Desvignes for his advices on pulsar timing, for reviewing the paper and providing many constructive suggestions, Lucas Guillemot for checking Fermi associations and Pablo Torne for carefully reading the manuscripts. We thank our summer student April Liska who has contributed to three of the pulsar discoveries presented in this paper, as well as the thorough work on data base cross-checking by her and our work shadowing student William Mccorkindale. CN was supported for this research through a stipend from the International Max Planck Research School (IM-PRS) for Astronomy and Astrophysics at the Universities of Bonn and Cologne. NR 72 TC 0 Z9 0 U1 0 U2 1 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUL 1 PY 2015 VL 450 IS 3 BP 2922 EP 2947 DI 10.1093/mnras/stv753 PG 26 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CK6LJ UT WOS:000356339300052 ER PT J AU Mandelbaum, R Rowe, B Armstrong, R Bard, D Bertin, E Bosch, J Boutigny, D Courbin, F Dawson, WA Donnarumma, A Conti, IF Gavazzi, R Gentile, M Gill, MSS Hogg, DW Huff, EM Jee, MJ Kacprzak, T Kilbinger, M Kuntzer, T Lang, D Luo, WT March, MC Marshall, PJ Meyers, JE Miller, L Miyatake, H Nakajima, R Mboula, FMN Nurbaeva, G Okura, Y Stephane, H Rhodes, J Schneider, MD Shan, HY Sheldon, ES Simet, M Starck, JL Sureau, F Tewes, M Adami, KZ Zhang, J Zuntz, J AF Mandelbaum, Rachel Rowe, Barnaby Armstrong, Robert Bard, Deborah Bertin, Emmanuel Bosch, James Boutigny, Dominique Courbin, Frederic Dawson, William A. Donnarumma, Annamaria Conti, Ian Fenech Gavazzi, Raphael Gentile, Marc Gill, Mandeep S. S. Hogg, David W. Huff, Eric M. Jee, M. James Kacprzak, Tomasz Kilbinger, Martin Kuntzer, Thibault Lang, Dustin Luo, Wentao March, Marisa C. Marshall, Philip J. Meyers, Joshua E. Miller, Lance Miyatake, Hironao Nakajima, Reiko Ngole Mboula, Fred Maurice Nurbaeva, Guldariya Okura, Yuki Paulin-Henriksson, Stephane Rhodes, Jason Schneider, Michael D. Shan, Huanyuan Sheldon, Erin S. Simet, Melanie Starck, Jean-Luc Sureau, Florent Tewes, Malte Adami, Kristian Zarb Zhang, Jun Zuntz, Joe TI GREAT3 results - I. Systematic errors in shear estimation and the impact of real galaxy morphology SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE gravitational lensing: weak; methods: data analysis; techniques: image processing; cosmology: observations ID WEAK LENSING ANALYSIS; SPACE-TELESCOPE OBSERVATIONS; IMAGE-ANALYSIS COMPETITION; SPREAD FUNCTION CORRECTION; ELLIPTIC-WEIGHTED HOLICS; DIGITAL SKY SURVEY; SHAPE MEASUREMENTS; COSMIC SHEAR; NOISE BIAS; GRAVITATIONAL SHEAR AB We present first results from the third GRavitational lEnsing Accuracy Testing (GREAT3) challenge, the third in a sequence of challenges for testing methods of inferring weak gravitational lensing shear distortions from simulated galaxy images. GREAT3 was divided into experiments to test three specific questions, and included simulated space- and ground-based data with constant or cosmologically varying shear fields. The simplest (control) experiment included parametric galaxies with a realistic distribution of signal-to-noise, size, and ellipticity, and a complex point spread function (PSF). The other experiments tested the additional impact of realistic galaxy morphology, multiple exposure imaging, and the uncertainty about a spatially varying PSF; the last two questions will be explored in Paper II. The 24 participating teams competed to estimate lensing shears to within systematic error tolerances for upcoming Stage-IV dark energy surveys, making 1525 submissions overall. GREAT3 saw considerable variety and innovation in the types of methods applied. Several teams now meet or exceed the targets in many of the tests conducted (to within the statistical errors). We conclude that the presence of realistic galaxy morphology in simulations changes shear calibration biases by similar to 1 per cent for a wide range of methods. Other effects such as truncation biases due to finite galaxy postage stamps, and the impact of galaxy type as measured by the S,rsic index, are quantified for the first time. Our results generalize previous studies regarding sensitivities to galaxy size and signal-to-noise, and to PSF properties such as seeing and defocus. Almost all methods' results support the simple model in which additive shear biases depend linearly on PSF ellipticity. C1 [Mandelbaum, Rachel; Lang, Dustin; Simet, Melanie] Carnegie Mellon Univ, Dept Phys, McWilliams Ctr Cosmol, Pittsburgh, PA 15213 USA. [Rowe, Barnaby; Kacprzak, Tomasz] UCL, Dept Phys & Astron, London WC1E 6BT, England. [Armstrong, Robert; Bosch, James; Miyatake, Hironao] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Bard, Deborah; Gill, Mandeep S. S.; Marshall, Philip J.; Meyers, Joshua E.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Dept Phys, Stanford, CA 94305 USA. [Bard, Deborah; Boutigny, Dominique; Gill, Mandeep S. S.] SLAC Natl Accelerator Lab, Menlo Pk, CA 94025 USA. [Bertin, Emmanuel; Donnarumma, Annamaria; Gavazzi, Raphael] Univ Paris 06, Inst Astrophys Paris, UMR CNRS 7095, F-75014 Paris, France. [Boutigny, Dominique] CNRS IN2P3, USR 6402, IN2P3, Ctr Calcul, F-69622 Villeurbanne, France. [Courbin, Frederic; Gentile, Marc; Kuntzer, Thibault; Nurbaeva, Guldariya; Shan, Huanyuan] Ecole Polytech Fed Lausanne, Astrophys Lab, Observ Sauverny, CH-1290 Versoix, Switzerland. [Dawson, William A.; Schneider, Michael D.] Lawrence Livermore Natl Lab, Livermore, CA 94551 USA. [Conti, Ian Fenech; Adami, Kristian Zarb] Univ Malta, ISSA, Msida 2080, Msd, Malta. [Hogg, David W.] NYU, Dept Phys, Ctr Cosmol & Particle Phys, New York, NY 10003 USA. [Huff, Eric M.] Ohio State Univ, Ctr Cosmol & AstroParticle Phys CCAPP, Columbus, OH 43210 USA. [Huff, Eric M.] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA. [Jee, M. James] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. [Kacprzak, Tomasz] ETH, Inst Astron, CH-8093 Zurich, Switzerland. [Kilbinger, Martin; Ngole Mboula, Fred Maurice; Paulin-Henriksson, Stephane; Starck, Jean-Luc; Sureau, Florent] CEA Saclay, Lab AIM, UMR CEA CNRS Paris 7, Irfu,SAp SEDI,Serv Astrophys, F-91191 Gif Sur Yvette, France. [Luo, Wentao] Shanghai Astron Observ, Key Lab Res Galaxies & Cosmol, Shanghai 200030, Peoples R China. [March, Marisa C.] Univ Penn, David Rittenhouse Lab, Philadelphia, PA 19104 USA. [Miller, Lance; Adami, Kristian Zarb] Univ Oxford, Dept Phys, Oxford OX1 3RH, England. [Miyatake, Hironao] Univ Tokyo, Kavli Inst Phys & Math Universe, WPI, Kashiwa, Chiba 2778582, Japan. [Nakajima, Reiko; Tewes, Malte] Argelander Inst Astron, D-53121 Bonn, Germany. [Okura, Yuki] Natl Astron Observ Japan, Tokyo 1818588, Japan. [Rhodes, Jason] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Rhodes, Jason] CALTECH, Pasadena, CA 91125 USA. [Sheldon, Erin S.] Brookhaven Natl Lab, Upton, NY 11973 USA. [Zhang, Jun] Shanghai Jiao Tong Univ, Dept Phys & Astron, Ctr Astron & Astrophys, Shanghai 200240, Peoples R China. [Zuntz, Joe] Univ Manchester, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England. RP Mandelbaum, R (reprint author), Carnegie Mellon Univ, Dept Phys, McWilliams Ctr Cosmol, 5000 Forbes Ave, Pittsburgh, PA 15213 USA. EM rmandelb@andrew.cmu.edu; barney@barnabyrowe.net RI Mandelbaum, Rachel/N-8955-2014; Zhang, Jun/O-3283-2015; Simet, Melanie/A-3415-2016; EPFL, Physics/O-6514-2016; Shan, Huanyuan/G-3353-2015; OI Starck, Jean-Luc/0000-0003-2177-7794; Mandelbaum, Rachel/0000-0003-2271-1527; Simet, Melanie/0000-0001-8823-8926; Shan, Huanyuan/0000-0001-8534-837X; Rowe, Barnaby/0000-0002-7042-9174; Kilbinger, Martin/0000-0001-9513-7138; Hogg, David/0000-0003-2866-9403 FU PASCAL-2 network; NASA via the Strategic University Research Partnership (SURP) Program of the Jet Propulsion Laboratory, California Institute of Technology; IST Programme of the European Community, under the PASCAL2 Network of Excellence [IST-2007-216886]; National Science Foundation [PHYS-1066293, PHY-0969487]; NASA through a grant from the Space Telescope Science Institute [HST-AR-12857.01-A]; NASA [NAS5-26555]; Alfred P. Sloan Fellowship from the Sloan Foundation; Department of Energy Early Career Award Program; European Research Council [240672]; Japan Society for the Promotion of Science (JSPS) Postdoctoral Fellowships for Research Abroad; JSPS Research Fellowships for Young Scientists; Agence Nationale de la Recherche (ANR Grant 'AMALGAM'); Centre National des Etudes Spatiales (CNES); Deutsche Forschungsgemeinschaft (DFG) [Hi 1495/2-1]; Swiss National Science Foundation (SNSF) [CRSII2_147678, 200020_146813, 200021_146770]; US Department of Energy at Lawrence Livermore National Laboratory [DE-AC52-07NA27344]; US Department of Energy at SLAC National Accelerator Laboratory [DE-AC02-76SF00515]; Marie Curie International Incoming Fellowship within the Seventh European Community Framework Programme; NSFC of China [11103011]; national science foundation of China [11273018, 11433001]; national basic research programme of China [2013CB834900, 2015CB857001]; European Research Council grant SparseAstro [ERC-228261] FX We thank Gary Bernstein and Mike Jarvis for providing helpful feedback on this paper, Peter Freeman for providing guidance on the statistical interpretation of results, and the anonymous referee for making suggestions that improved the presentation of results in the paper. We thank the PASCAL-2 network for its sponsorship of the challenge. This project was supported in part by NASA via the Strategic University Research Partnership (SURP) Program of the Jet Propulsion Laboratory, California Institute of Technology; and by the IST Programme of the European Community, under the PASCAL2 Network of Excellence, IST-2007-216886. This article only reflects the authors' views. This work was supported in part by the National Science Foundation under Grant no. PHYS-1066293 and the hospitality of the Aspen Center for Physics.; RM was supported during the development of the GREAT3 challenge in part by program HST-AR-12857.01-A, provided by NASA through a grant from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555, and in part through an Alfred P. Sloan Fellowship from the Sloan Foundation; her work on the final analysis of results was supported by the Department of Energy Early Career Award Program. BR, JZuntz, and TKacprzak acknowledge support from the European Research Council in the form of a Starting Grant with number 240672. HM acknowledges support from Japan Society for the Promotion of Science (JSPS) Postdoctoral Fellowships for Research Abroad and JSPS Research Fellowships for Young Scientists. The Amalgam@IAP Team (AD, EB, RG) acknowledges the Agence Nationale de la Recherche (ANR Grant 'AMALGAM') and Centre National des Etudes Spatiales (CNES) for financial support. MT acknowledges support from the Deutsche Forschungsgemeinschaft (DFG) grant Hi 1495/2-1. TKuntzer, MGentile, HYS, and FC acknowledge support from the Swiss National Science Foundation (SNSF) under grants CRSII2_147678, 200020_146813 and 200021_146770. Part of the work carried out by the MBI team was performed under the auspices of the US Department of Energy at Lawrence Livermore National Laboratory under contract number DE-AC52-07NA27344 and SLAC National Accelerator Laboratory under contract number DE-AC02-76SF00515. HYS acknowledges the support by a Marie Curie International Incoming Fellowship within the Seventh European Community Framework Programme, and NSFC of China under grants 11103011. JEM was supported by National Science Foundation grant PHY-0969487. JZhang is supported by the national science foundation of China (Grant no. 11273018, 11433001), and the national basic research programme of China (Grant no. 2013CB834900, 2015CB857001). J-LS, MK, FS, and FMNM were supported by the European Research Council grant SparseAstro (ERC-228261). EMH is grateful to Christopher Hirata for insightful discussion and feedback on the MetaCalibration idea. NR 84 TC 21 Z9 21 U1 2 U2 11 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUL 1 PY 2015 VL 450 IS 3 BP 2963 EP 3007 DI 10.1093/mnras/stv781 PG 45 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CK6LJ UT WOS:000356339300054 ER PT J AU Ventura, P Karakas, AI Dell'Agli, F Boyer, ML Garcia-Hernandez, DA Di Criscienzo, M Schneider, R AF Ventura, P. Karakas, A. I. Dell'Agli, F. Boyer, M. L. Garcia-Hernandez, D. A. Di Criscienzo, M. Schneider, R. TI The Large Magellanic Cloud as a laboratory for hot bottom burning in massive asymptotic giant branch stars SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE stars: abundances; stars: AGB and post-AGB; dust; extinction ID METALLICITY GLOBULAR-CLUSTERS; 3RD DREDGE-UP; AGB STARS; DUST PRODUCTION; STELLAR WINDS; MINERAL FORMATION; GALAXY EVOLUTION; TURBULENT CONVECTION; HERSCHEL INVENTORY; AGENTS AB We use Spitzer observations of the rich population of asymptotic giant branch (AGB) stars in the Large Magellanic Cloud (LMC) to test models describing the internal structure and nucleosynthesis of the most massive of these stars, i.e. those with initial mass above similar to 4 M-aS (TM). To this aim, we compare Spitzer observations of LMC stars with the theoretical tracks of AGB models, calculated with two of the most popular evolution codes, that are known to differ in particular for the treatment of convection. Although the physical evolution of the two models are significantly different, the properties of dust formed in their winds are surprisingly similar, as is their position in the colour-colour and colour-magnitude diagrams obtained with the Spitzer bands. This model-independent result allows us to select a well-defined region in the ([3.6]-[4.5], [5.8]-[8.0]) plane, populated by AGB stars experiencing hot bottom burning, the progeny of stars with mass M similar to 5.5 M-aS (TM). This result opens up an important test of the strength hot bottom burning using detailed near-IR (H and K bands) spectroscopic analysis of the oxygen-rich, high-luminosity candidates found in the well-defined region of the colour-colour plane. This test is possible because the two stellar evolution codes we use predict very different results for the surface chemistry, and the C/O ratio in particular, owing to their treatment of convection in the envelope and of convective boundaries during third dredge-up. The differences in surface chemistry are most apparent when the model stars reach the phase with the largest infrared emission. C1 [Ventura, P.; Dell'Agli, F.; Di Criscienzo, M.; Schneider, R.] INAF Osservatorio Astron Roma, I-00040 Monte Porzio Catone, RM, Italy. [Karakas, A. I.] Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT 2611, Australia. [Dell'Agli, F.] Univ Roma La Sapienza, Dipartimento Fis, I-00143 Rome, Italy. [Boyer, M. L.] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA. [Boyer, M. L.] Oak Ridge Associated Univ, Oak Ridge, TN 37831 USA. [Garcia-Hernandez, D. A.] Inst Astrofis Canarias, E-38200 Tenerife, Spain. [Garcia-Hernandez, D. A.] Univ La Laguna, Dept Astrofis, E-38206 Tenerife, Spain. RP Ventura, P (reprint author), INAF Osservatorio Astron Roma, Via Frascati 33, I-00040 Monte Porzio Catone, RM, Italy. EM paolo.ventura@oa-roma.inaf.it RI Schneider, Raffaella/E-4216-2017; OI Schneider, Raffaella/0000-0001-9317-2888; Ventura, Paolo/0000-0002-5026-6400 FU PRIN MIUR [prot. 2010LY5N2T]; Australian Research Council [FT110100475]; Spanish Ministry of Economy and Competitiveness [AYA-2011-27754]; European Research Council under the European Unions [306476] FX PV was supported by PRIN MIUR 2011 'The Chemical and Dynamical Evolution of the Milky Way and Local Group Galaxies' (PI: F. Matteucci), prot. 2010LY5N2T. AIK was supported through an Australian Research Council Future Fellowship (FT110100475). DAGH acknowledges support provided by the Spanish Ministry of Economy and Competitiveness under grant AYA-2011-27754. RS acknowledges funding from the European Research Council under the European Unions Seventh Framework Programme (FP/2007-2013)/ERC Grant Agreement no. 306476. NR 67 TC 12 Z9 12 U1 0 U2 1 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUL 1 PY 2015 VL 450 IS 3 BP 3181 EP 3190 DI 10.1093/mnras/stv918 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CK6LJ UT WOS:000356339300069 ER PT J AU Li, ZJ McWilliams, JC Ide, K Farrara, JD AF Li, Zhijin McWilliams, James C. Ide, Kayo Farrara, John D. TI Coastal ocean data assimilation using a multi-scale three-dimensional variational scheme SO OCEAN DYNAMICS LA English DT Article DE Multi-scale data assimilation; Variational data assimilation; Fine-resolution model; Ocean prediction; Observing system; Coastal ocean ID FORECAST ERROR COVARIANCES; PART I; MODELING SYSTEM; MONTEREY BAY; CALIFORNIA; INTERPOLATION; STATISTICS; MESOSCALE AB A multi-scale three-dimensional variational scheme (MS-3DVAR) is implemented to improve the effectiveness of the assimilation of both very sparse and high-resolution observations into models with resolutions down to 1 km. The improvements are realized through the use of background error covariances of multi-decorrelation length scales and by reducing the inherent observational representativeness errors. MS-3DVAR is applied to coastal ocean data assimilation to handle the wide range of spatial scales that exist in both the dynamics and observations. In the implementation presented here, the cost function consists of two components for large and small scales, and MS-3DVAR is implemented sequentially from large to small scales. A set of observing system simulation experiments (OSSEs) are performed to illustrate the advantages of MS-3DVAR over conventional 3DVAR in assimilating two of the most common types of observations-sparse vertical profiles and high-resolution surface measurements-simultaneously. One month of results from an operational implementation show that both the analysis error and bias are reduced more effectively when using MS-3DVAR. C1 [Li, Zhijin] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [McWilliams, James C.] Univ Calif Los Angeles, Dept Atmospher & Ocean Sci, Los Angeles, CA USA. [Ide, Kayo] Univ Maryland, Inst Phys Sci & Technol, Earth Syst Sci Interdisciplinary Ctr, Ctr Sci Computat & Math Modeling,Dept Atmospher &, College Pk, MD 20742 USA. [Farrara, John D.] Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA USA. RP Li, ZJ (reprint author), CALTECH, Jet Prop Lab, M-S 300-323,4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Zhijin.Li@jpl.nasa.gov FU Office of Naval Research [N00014-12-1-093, N00014-10-1-0557] FX The research described in this publication was carried out, in part, at the Jet Propulsion Laboratory (JPL), California Institute of Technology, under a contract with the National Aeronautics and Space Administration (NASA). We gratefully acknowledge the multi-year support from Dr. Yi Chao, Remote Sensing Solutions, Inc., to the development of the MS-3DVAR system for the SCB region and also many discussions with him that help improve the system. This research was supported in part by the Office of Naval Research (N00014-12-1-093) and (N00014-10-1-0557). The authors thank the anonymous reviewers for comments that were very helpful in improving the manuscript. NR 42 TC 5 Z9 5 U1 1 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 JUL PY 2015 VL 65 IS 7 BP 1001 EP 1015 DI 10.1007/s10236-015-0850-x PG 15 WC Oceanography SC Oceanography GA CK9AZ UT WOS:000356533600005 ER PT J AU Park, RS Bills, B Buffington, BB Folkner, WM Konopliv, AS Martin-Mur, TJ Mastrodemos, N McElrath, TP Riedel, JE Watkins, MM AF Park, Ryan S. Bills, Bruce Buffington, Brent B. Folkner, William M. Konopliv, Alexander S. Martin-Mur, Tomas J. Mastrodemos, Nickolaos McElrath, Timothy P. Riedel, Joseph E. Watkins, Michael M. TI Improved detection of tides at Europa with radiometric and optical tracking during flybys SO PLANETARY AND SPACE SCIENCE LA English DT Article DE Europa tides; Europa Love numbers; Europa gravity field ID NONSYNCHRONOUS ROTATION; SATELLITES; OCEAN; SHELL; MOONS AB Due to its eccentric orbit about Jupiter, Europa experiences periodic tidal deformation, which causes changes in its gravitational field and induces both radial and transverse displacements of the surface. The amplitude and phase of these tidal changes are diagnostic of internal structure, and can be measured with sufficient radiometric and optical tracking of a spacecraft during a series of flyby encounters with Europa This paper presents results of the simulated accuracy for recovery of the tides of Europa through measuring the second-degree tidal Love numbers k(2), h(2), and l(2). A reference trajectory, which consists of a total of 45 close flybys, was considered and a detailed covariance analysis was performed. The study was based on Earth-based Doppler tracking during +/- 2 h of each periapsis passage and surface imaging data taken below 500 km altitude. The result shows that the formal uncertainty of the second-degree tidal Love numbers can be estimated to be sigma(k2) = 0.01, sigma(h2) = 0.02, and sigma(l2) = 0.01, which is sufficient to constrain the global ice thickness to about 10 km under reasonable assumptions. Moreover, the forced librations of Europa can be measured to 0.3" accuracy, which can further constrain Europa's interior structure. (C) 2015 Elsevier Ltd. All rights reserved. C1 [Park, Ryan S.; Bills, Bruce; Buffington, Brent B.; Folkner, William M.; Konopliv, Alexander S.; Martin-Mur, Tomas J.; Mastrodemos, Nickolaos; McElrath, Timothy P.; Riedel, Joseph E.; Watkins, Michael M.] CALTECH, Jet Prop Lab, Pasadena, CA 91101 USA. RP Park, RS (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91101 USA. EM Ryan.S.Park@jpl.nasa.gov FU National Aeronautics and Space Administration FX The research described in this paper was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. NR 25 TC 0 Z9 0 U1 1 U2 8 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0032-0633 J9 PLANET SPACE SCI JI Planet Space Sci. PD JUL PY 2015 VL 112 BP 10 EP 14 DI 10.1016/j.pss.2015.04.005 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CK4MA UT WOS:000356196700002 ER PT J AU Orosei, R Jordan, RL Morgan, DD Cartacci, M Cicchetti, A Duru, F Gurnett, DA Heggy, E Kirchner, DL Noschese, R Kofman, W Masdea, A Plaut, JJ Seu, R Watters, TR Picardi, G AF Orosei, R. Jordan, R. L. Morgan, D. D. Cartacci, M. Cicchetti, A. Duru, F. Gurnett, D. A. Heggy, E. Kirchner, D. L. Noschese, R. Kofman, W. Masdea, A. Plaut, J. J. Seu, R. Watters, T. R. Picardi, G. TI Mars Advanced Radar for Subsurface and Ionospheric Sounding (MARSIS) after nine years of operation: A summary SO PLANETARY AND SPACE SCIENCE LA English DT Article DE Mars Express; Mars; Ground Penetrating Radar (GPR); Ionosphere; Ice; Water ID ELECTRON-DENSITY PROFILES; MEDUSAE FOSSAE FORMATION; MARTIAN GEOLOGIC RECORD; EXPRESS; DEPOSITS; ICE; STRATIGRAPHY; REFLECTIVITY; FREQUENCY; SIGNALS AB Mars Express, the first European interplanetary mission, carries the Mars Advanced Radar for Subsurface and Ionosphere Sounding (MARSIS) to search for ice and water in the Martian subsurface. Developed by an Italian-US team, MARSIS transmits low-frequency, wide-band radio pulses penetrating below the surface and reflected by dielectric discontinuities linked to structural or compositional changes. MARSIS is also a topside ionosphere sounder, transmitting a burst of short, narrow-band pulses at different frequencies that are reflected by plasma with varying densities at different altitudes. The radar operates since July 2005, after the successful deployment of its 40 m antenna, acquiring data at altitudes lower than 1200 km. Subsurface sounding (SS) data are processed on board by stacking together a batch of echoes acquired at the same frequency. On ground, SS data are further processed by correlating the received echo with the transmitted waveform and compensating, de-focusing caused by the dispersive ionosphere. Ground processing of active ionospheric sounding (AIS) data consists in the reconstruction of the electron density profile as a function of altitude. MARSIS observed the internal structure of Planum Boreum outlining the Basal Unit, an icy deposit lying beneath the North Polar Layered Deposits thought to have formed in an epoch in which climate was markedly different from the current one. The total volume of ice in polar layered deposits could be estimated, and parts of the Southern residual ice cap were revealed to consist of approximate to 10 m of CO2 ice. Radar properties of the Vastitas Borealis Formation point to the presence of large quantities of ice buried beneath the surface. Observations of the ionosphere revealed the complex interplay between plasma, crustal magnetic field and solar wind, contributing to space weather studies at Mars. The presence of three-dimensional plasma structures in the ionosphere was revealed for the first time. MARSIS could successfully operate at Phobos, becoming the first instrument of its kind to observe an asteroid-like body. The main goal pursued by MARSIS, the search for liquid water beneath the surface, remains elusive. However, because of the many factors affecting detection and of the difficulties in identifying water in radar echoes, a definitive conclusion on its presence cannot yet be drawn. (C) 2014 Elsevier Ltd. All rights reserved. C1 [Orosei, R.] Ist Nazl Astrofis, Ist Radioastron, I-40129 Bologna, Italy. [Jordan, R. L.; Heggy, E.; Plaut, J. J.] CALTECH, Jet Prop Lab, Pasadena, CA 91009 USA. [Morgan, D. D.; Duru, F.; Gurnett, D. A.; Kirchner, D. L.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. [Cartacci, M.; Cicchetti, A.; Noschese, R.] Ist Nazl Astrofis, Ist Astrofis & Planetol Spaziali, I-00133 Rome, Italy. [Kofman, W.] Inst Planetol & Astrophys Grenoble, F-38041 Grenoble 9, France. [Kofman, W.] Polish Acad Sci, Space Res Ctr, PL-01237 Warsaw, Poland. [Masdea, A.; Seu, R.; Picardi, G.] Univ Roma La Sapienza, Dipartimento Ingn Informaz Elettron & Telecomunic, I-00184 Rome, Italy. [Watters, T. R.] Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20013 USA. RP Orosei, R (reprint author), Ist Nazl Astrofis, Ist Radioastron, Via Piero Gobetti 101, I-40129 Bologna, Italy. EM roberto.orosei@inaf.it RI Kofman, Wlodek/C-4556-2008; OI CICCHETTI, ANDREA/0000-0002-9588-6531; Cartacci, Marco/0000-0001-9825-1817; Noschese, Raffaella/0000-0003-0502-0337 FU Italian Space Agency (ASI) [I/032/12/0] FX This work was supported by the Italian Space Agency (ASI) through Contract no. I/032/12/0. This research has made use of NASA's Astrophysics Data System. NR 90 TC 5 Z9 5 U1 1 U2 13 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0032-0633 J9 PLANET SPACE SCI JI Planet Space Sci. PD JUL PY 2015 VL 112 BP 98 EP 114 DI 10.1016/j.pss.2014.07.010 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CK4MA UT WOS:000356196700009 ER PT J AU Zwieback, S Hensley, S Hajnsek, I AF Zwieback, Simon Hensley, Scott Hajnsek, Irena TI Assessment of soil moisture effects on L-band radar interferometry SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE Radar interferometry; Differential interferometry; Displacement; Deformation; DInSAR; Soil moisture; Microwave scattering; Vegetation ID DIFFERENTIAL SAR INTERFEROMETRY; SURFACE; DINSAR; DECORRELATION; FEATURES; AREAS; MODEL AB Differential SAR interferometry, a popular technique for measuring displacements of the Earth's surface, is potentially influenced by changes in soil moisture. Different mechanisms for this impact have been proposed, but its magnitude, sign and even presence remain poorly understood. In this study the dependence of the phase, the coherence magnitude as well as the phase triplets on soil moisture was inferred empirically with regression techniques: this was done for two airborne data sets at L-band. The phase dependence was significant (at a significance level of 0.05) for more than 70% of the fields at HH polarization, its sign corresponding to an increase in optical path upon wetting, and the magnitude of the associated deformation commonly exceeding 2 cm for a change in soil moisture of 20%. This trend was similar in both campaigns, whereas the prevalence of soil moisture-related decorrelafion differs. These results are only consistent with a dielectric origin of the soil moisture effects, and not with soil swelling or the penetration depth hypothesis. Changes in vegetation impact the phase depending on the crop and polarization, with the vegetation influence at VV being more pronounced for the agricultural crops present in the study area. (C) 2015 The Authors. Published by Elsevier Inc. C1 [Zwieback, Simon; Hajnsek, Irena] ETH, Inst Environm Engn, Zurich, Switzerland. [Hensley, Scott] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Hajnsek, Irena] German Aerosp Ctr DLR, Microwaves & Radar Inst, Wessling, Germany. RP Zwieback, S (reprint author), Stefano Franscini Pl 3, CH-8093 Zurich, Switzerland. EM zwieback@ifu.baug.ethz.ch NR 56 TC 7 Z9 8 U1 1 U2 17 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0034-4257 EI 1879-0704 J9 REMOTE SENS ENVIRON JI Remote Sens. Environ. PD JUL PY 2015 VL 164 BP 77 EP 89 DI 10.1016/j.rse.2015.04.012 PG 13 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA CK9IU UT WOS:000356554600008 ER PT J AU Goldsmith, P Lis, D AF Goldsmith, Paul Lis, Darek TI OUR OCEANS' ORIGINS SO SCIENTIFIC AMERICAN LA English DT Letter C1 [Goldsmith, Paul] NASA, Jet Prop Lab, Washington, DC 20024 USA. [Lis, Darek] Lab Studies Radiat & Matter Astrophys & Atmospher, Paris, France. RP Goldsmith, P (reprint author), NASA, Jet Prop Lab, Washington, DC 20024 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU NATURE PUBLISHING GROUP PI NEW YORK PA 75 VARICK ST, 9TH FLR, NEW YORK, NY 10013-1917 USA SN 0036-8733 J9 SCI AM JI Sci.Am. PD JUL PY 2015 VL 313 IS 1 BP 6 EP 6 PG 1 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CL0KY UT WOS:000356632800005 ER PT J AU Rury, AS Mansour, K Yu, N AF Rury, Aaron S. Mansour, Kamjou Yu, Nan TI All-electronic line width reduction in a semiconductor diode laser using a crystalline microresonator SO APPLIED PHYSICS B-LASERS AND OPTICS LA English DT Article ID GALLERY-MODE-RESONATOR; FREQUENCY STABILIZATION; REFERENCE CAVITY; LINEWIDTH; PHASE; MICROCAVITIES; FINESSE AB This study examines the capability to significantly suppress the frequency noise of a semiconductor distributed feedback diode laser using a universally applicable approach: a combination of a high-Q crystalline whispering gallery mode microresonator reference and the Pound-Drever-Hall locking scheme using an all-electronic servo loop. An out-of-loop delayed self-heterodyne measurement system demonstrates the ability of this approach to reduce a test laser's absolute line width by nearly a factor of 100. In addition, in-loop characterization of the laser stabilized using this method demonstrates a 1-kHz residual line width with reference to the resonator frequency. Based on these results, we propose that utilization of an all-electronic loop combined with the use of the wide transparency window of crystalline materials enable this approach to be readily applicable to diode lasers emitting in other regions of the electromagnetic spectrum, especially in the UV and mid-IR . C1 [Rury, Aaron S.; Mansour, Kamjou; Yu, Nan] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Rury, AS (reprint author), Univ So Calif, Dept Chem, Los Angeles, CA 90089 USA. EM arury@usc.edu; nan.yu@jpl.nasa.gov OI Rury, Aaron/0000-0002-1836-1424 FU National Aeronautics and Space Administration FX We would like to thank Lukas Baumgartel and Ivan Grudinin for useful discussions and support with the lasers used in this study. The research described in this paper was carried out by the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. Also authors would like to acknowledge the California Institute of Technology and its Government sponsorship. NR 26 TC 1 Z9 1 U1 1 U2 15 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 JUL PY 2015 VL 120 IS 1 BP 155 EP 160 DI 10.1007/s00340-015-6118-9 PG 6 WC Optics; Physics, Applied SC Optics; Physics GA CJ9YY UT WOS:000355861600022 ER PT J AU Theisen, CH Sumner, DY Mackey, TJ Lim, DSS Brady, AL Slater, GF AF Theisen, C. Harwood Sumner, D. Y. Mackey, T. J. Lim, D. S. S. Brady, A. L. Slater, G. F. TI Carbonate fabrics in the modern microbialites of Pavilion Lake: two suites of microfabrics that reflect variation in microbial community morphology, growth habit, and lithification SO GEOBIOLOGY LA English DT Article ID FRESH-WATER MICROBIALITES; MODERN MARINE STROMATOLITES; PALEOZOIC LIME MUD; WESTERN-AUSTRALIA; CYANOBACTERIAL FILAMENTS; CUATRO CIENEGAS; WALKER LAKE; SHARK BAY; MATS; CALCIFICATION AB Modern microbialites in Pavilion Lake, BC, provide an analog for ancient non-stromatolitic microbialites that formed from insitu mineralization. Because Pavilion microbialites are mineralizing under the influence of microbial communities, they provide insights into how biological processes influence microbialite microfabrics and mesostructures. Hemispherical nodules and micrite-microbial crusts are two mesostructures within Pavilion microbialites that are directly associated with photosynthetic communities. Both filamentous cyanobacteria in hemispherical nodules and branching filamentous green algae in micrite-microbial crusts were associated with calcite precipitation at microbialite surfaces and with characteristic microfabrics in the lithified microbialite. Hemispherical nodules formed at microbialite surfaces when calcite precipitated around filamentous cyanobacteria with a radial growth habit. The radial filament pattern was preserved within the microbialite to varying degrees. Some subsurface nodules contained well-defined filaments, whereas others contained only dispersed organic inclusions. Variation in filament preservation is interpreted to reflect differences in timing and amount of carbonate precipitation relative to heterotrophic decay, with more defined filaments reflecting greater lithification prior to degradation than more diffuse filaments. Micrite-microbial crusts produce the second suite of microfabrics and form in association with filamentous green algae oriented perpendicular to the microbialite surface. Some crusts include calcified filaments, whereas others contained voids that reflect the filamentous community in shape, size, and distribution. Pavilion microbialites demonstrate that microfabric variation can reflect differences in lithification processes and microbial metabolisms as well as microbial community morphology and organization. Even when the morphology of individual filaments or cells is not well preserved, the microbial growth habit can be captured in mesoscale microbialite structures. These results suggest that when petrographic preservation is extremely good, ancient microbialite growth structures and microfabrics can be interpreted in the context of variation in community organization, community composition, and lithification history. Even in the absence of distinct microbial microfabrics, mesostructures can capture microbial community morphology. C1 [Theisen, C. Harwood; Sumner, D. Y.; Mackey, T. J.] Univ Calif Davis, Dept Earth & Planetary Sci, Davis, CA 95616 USA. [Lim, D. S. S.] Bay Area Environm Res Inst, Petaluma, CA USA. [Lim, D. S. S.] NASA Ames Res Ctr, Moffett Field, CA USA. [Brady, A. L.; Slater, G. F.] McMaster Univ, Sch Geog & Earth Sci, Hamilton, ON, Canada. RP Theisen, CH (reprint author), Univ Calif Davis, Dept Earth & Planetary Sci, Davis, CA 95616 USA. EM clharwood@ucdavis.edu FU NASA Moon and Mars Analog Mission Activities (MMAMA) grant; Natural Sciences and Engineering Research Council (NSERC) of Canada; Canadian Space Agency's (CSA) Canadian Analogue Research Network (CARN); Canadian Space Agency's (CSA) Analogue Missions programs; NASA Exobiology Program (DTA); Nuytco Research; National Geographic Society; Tula Foundation FX We would like to thank all scientists and volunteers associated with the Pavilion Lake Research Project (PLRP), especially the SCUBA divers, submarine operators, and photographers. Rebekah Shepard, Donnie Reid, and Ian Hawes are especially deserving of thanks for collecting samples and taking photographs used in this study. The bathymetric data set used in this manuscript is courtesy of Art Trembanis and was processed by Alex Forrest. We acknowledge support from funding sources, including a NASA Moon and Mars Analog Mission Activities (MMAMA) grant to D. Lim, Natural Sciences and Engineering Research Council (NSERC) of Canada Discovery Grant, the Canadian Space Agency's (CSA) Canadian Analogue Research Network (CARN) and Analogue Missions programs, the NASA Exobiology Program (DTA), Nuytco Research, the National Geographic Society, and the Tula Foundation. We are also grateful to Linda and Mickey Macri for hosting the PLRP project from 2004 to present and to the Ts'Kw'aylaxw First Nation and British Columbia Parks for their continued support of our research. This work was performed in partial fulfillment of requirements for a Ph.D. degree for C. Harwood Theisen at teh University of California, Davis. NR 68 TC 2 Z9 2 U1 5 U2 26 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1472-4677 EI 1472-4669 J9 GEOBIOLOGY JI Geobiology PD JUL PY 2015 VL 13 IS 4 BP 357 EP 372 DI 10.1111/gbi.12134 PG 16 WC Biology; Environmental Sciences; Geosciences, Multidisciplinary SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Geology GA CK3AP UT WOS:000356087700005 PM 25809931 ER PT J AU Popova, Y Boyle, R AF Popova, Yekaterina Boyle, Richard TI Neural response in vestibular organ of Helix aspersa to centrifugation and re-adaptation to normal gravity SO JOURNAL OF COMPARATIVE PHYSIOLOGY A-NEUROETHOLOGY SENSORY NEURAL AND BEHAVIORAL PHYSIOLOGY LA English DT Article DE Gravity; Statocyst; Electrophysiology; Behavior; Tilt ID HAIR-CELLS; SENSORY NEURONS; SPACE-FLIGHT; STATOCYST; SEROTONIN; HYPERGRAVITY; RECEPTORS; AFFERENT; SYSTEM; MICROGRAVITY AB Gravity plays a key role in shaping the vestibular sensitivity (VS) of terrestrial organisms. We studied VS changes in the statocyst of the gastropod Helix aspersa immediately after 4-, 16-, and 32-day exposures to a 1.4G hypergravic field or following a 7-day recovery period. In the same animals we measured latencies of behavioral "negative gravitaxis" responses to a head-down pitch before and after centrifugation and found significant delays after 16- and 32-day runs. In an isolated neural preparation we recorded the electrophysiological responses of the statocyst nerve to static tilt (+/- 19A degrees) and sinusoids (+/- 12A degrees; 0.1 Hz). Spike sorting software was used to separate individual sensory cells' patterns out of a common trace. In correspondence with behavior we observed a VS decrease in animals after 16- (p < 0.05) and 32-day (p < 0.01) centrifugations. These findings reveal the capability of statoreceptors to adjust their sensitivity in response to a prolonged change in the force of gravity. Interestingly, background discharge rate increased after 16 and 32 days in hypergravity and continued to rise through the recovery period. This result indicates that adaptive mechanisms to novel gravity levels were long lasting, and re-adaptation from hypergravity is a more complex process than just "return to normal". C1 [Popova, Yekaterina; Boyle, Richard] NASA Ames Res Ctr, Space Biosci Res Branch, Mountain View, CA 94035 USA. RP Boyle, R (reprint author), NASA Ames Res Ctr, Space Biosci Res Branch, Mail Stop 239-11, Mountain View, CA 94035 USA. EM richard.boyle@nasa.gov FU NASA Postdoctoral Program; NASA [11_Omni_2-0002]; NASA Human Research Program FX This work was funded by NASA Postdoctoral Program administered by Oak Ridge Associated Universities (to YP) and in part by NASA grant (11_Omni_2-0002) and the NASA Human Research Program (to RB). We thank A. Intravaia for assistance in constructing the centrifuge arm and habitat holding device. We also thank the laboratory of Pavel Balaban at the Institute of Higher Nervous Activity and Neurophysiology, Russian Academy of Sciences, Moscow, Russia, for guiding us to the snail model. Although the Animal Welfare Act Regulations or the Public Health Service Policy on Humane Care and Use of Laboratory Animals do not cover invertebrates, we followed the ethical guidelines given in NIH "Guide for the Care and Use of Laboratory Animals". NR 57 TC 0 Z9 0 U1 1 U2 4 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0340-7594 EI 1432-1351 J9 J COMP PHYSIOL A JI J. Comp. Physiol. A -Neuroethol. Sens. Neural Behav. Physiol. PD JUL PY 2015 VL 201 IS 7 BP 717 EP 729 DI 10.1007/s00359-015-1003-x PG 13 WC Behavioral Sciences; Neurosciences; Physiology; Zoology SC Behavioral Sciences; Neurosciences & Neurology; Physiology; Zoology GA CK2OB UT WOS:000356049100006 PM 25801308 ER PT J AU Mishra, AK Ines, AVM Das, NN Khedun, CP Singh, VP Sivakumar, B Hansen, JW AF Mishra, Ashok K. Ines, Amor V. M. Das, Narendra N. Khedun, C. Prakash Singh, Vijay P. Sivakumar, Bellie Hansen, James W. TI Anatomy of a local-scale drought: Application of assimilated remote sensing products, crop model, and statistical methods to an agricultural drought study SO JOURNAL OF HYDROLOGY LA English DT Article DE Drought anatomy; Data assimilation; Crop yield; Copulas; Root zone soil moisture ID NATURAL DISASTER REDUCTION; FREQUENCY-ANALYSIS; WAVELET ANALYSIS; YIELD FORECASTS; CLIMATE-CHANGE; SOIL-MOISTURE; PRECIPITATION; WATER; SIMULATION; VEGETATION AB Drought is of global concern for society but it originates as a local problem. It has a significant impact on water quantity and quality and influences food, water, and energy security. The consequences of drought vary in space and time, from the local scale (e.g. county level) to regional scale (e.g. state or country level) to global scale. Within the regional scale, there are multiple socio-economic impacts (i.e., agriculture, drinking water supply, and stream health) occurring individually or in combination at local scales, either in clusters or scattered. Even though the application of aggregated drought information at the regional level has been useful in drought management, the latter can be further improved by evaluating the structure and evolution of a drought at the local scale. This study addresses a local-scale agricultural drought anatomy in Story County in Iowa, USA. This complex problem was evaluated using assimilated AMSR-E soil moisture and MODIS-LAI data into a crop model to generate surface and sub-surface drought indices to explore the anatomy of an agricultural drought. Quantification of moisture supply in the root zone remains a gray area in research community, this challenge can be partly overcome by incorporating assimilation of soil moisture and leaf area index into crop modeling framework for agricultural drought quantification, as it performs better in simulating crop yield. It was noted that the persistence of subsurface droughts is in general higher than surface droughts, which can potentially improve forecast accuracy. It was found that both surface and subsurface droughts have an impact on crop yields, albeit with different magnitudes, however, the total water available in the soil profile seemed to have a greater impact on the yield. Further, agricultural drought should not be treated equal for all crops, and it should be calculated based on the root zone depth rather than a fixed soil layer depth. We envisaged that the results of this study will enhance our understanding of agricultural droughts in different parts of the world. (C) 2014 Elsevier B.V. All rights reserved. C1 [Mishra, Ashok K.] Clemson Univ, Glenn Dept Civil Engn, Clemson, SC 29634 USA. [Ines, Amor V. M.; Hansen, James W.] Columbia Univ, Earth Inst, Int Res Inst Climate & Soc, Palisades, NY 10964 USA. [Das, Narendra N.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Khedun, C. Prakash; Singh, Vijay P.] Texas A&M Univ, Dept Biol & Agr Engn, Water Management & Hydrol Sci, College Stn, TX 77843 USA. [Singh, Vijay P.] Texas A&M Univ, Zachry Dept Civil Engn, Water Management & Hydrol Sci, College Stn, TX 77843 USA. [Sivakumar, Bellie] Univ New S Wales, Sch Civil & Environm Engn, Sydney, NSW 2052, Australia. [Sivakumar, Bellie] Univ Calif Davis, Dept Land Air & Water Resources, Davis, CA 95616 USA. RP Mishra, AK (reprint author), Clemson Univ, Glenn Dept Civil Engn, 202 B Lowry Hall, Clemson, SC 29634 USA. EM ashokm@clemson.edu; ines@iri.columbia.edu; Naraindra.N.Das@jpl.nasa.gov; pkhedun@tamu.edu; vsingh@tamu.edu; s.bellie@unsw.edu.au; jhansen@iri.columbia.edu RI Hansen, James/M-1449-2015 OI Hansen, James/0000-0002-8599-7895 FU CCAFS, NASA/JPL SERVIR project; NASA; NOAA [NA05OAR4311004] FX We acknowledge the supports of CCAFS, NASA/JPL SERVIR project, NASA SMAP Early Adopter and NOAA Cooperative Grant #NA05OAR4311004 in developing the crop model-data assimilation system. We thank two anonymous reviewers for their positive and constructive comments on an earlier version of this manuscript. NR 60 TC 11 Z9 12 U1 13 U2 58 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0022-1694 EI 1879-2707 J9 J HYDROL JI J. Hydrol. PD JUL PY 2015 VL 526 SI SI BP 15 EP 29 DI 10.1016/j.jhydrol.2014.10.038 PG 15 WC Engineering, Civil; Geosciences, Multidisciplinary; Water Resources SC Engineering; Geology; Water Resources GA CK0KS UT WOS:000355894700003 ER PT J AU Li, BL Rodell, M AF Li, Bailing Rodell, Matthew TI Evaluation of a model-based groundwater drought indicator in the conterminous US SO JOURNAL OF HYDROLOGY LA English DT Article DE Groundwater drought indicator; Groundwater persistence; GRACE data assimilation; Groundwater temporal variability ID UNITED-STATES; GRACE; ASSIMILATION; DEPLETION; SYSTEM AB Monitoring groundwater drought using land surface models is a valuable alternative given the current lack of systematic in situ measurements at continental and global scales and the low resolution of current remote sensing based groundwater data. However, uncertainties inherent to land surface models may impede drought detection, and thus should be assessed using independent data sources. In this study, we evaluated a groundwater drought index (GWI) derived from monthly groundwater storage output from the Catchment Land Surface Model (CLSM) using a GWI similarly derived from in situ groundwater observations. Groundwater observations were obtained from unconfined or semi-confined aquifers in eight regions of the central and northeastern U.S. Regional average GWI derived from CLSM exhibited strong correlation with that from observation wells, with correlation coefficients between 0.43 and 0.92. GWI from both in situ data and CLSM was generally better correlated with the Standard Precipitation Index (SPI) at 12 and 24 month timescales than at shorter timescales, but it varied depending on climate conditions. The correlation between CLSM derived GWI and SPI generally decreases with increasing depth to the water table, which in turn depends on both bedrock depth (a CLSM parameter) and mean annual precipitation. The persistence of CLSM derived GWI is spatially varied and again shows a strong influence of depth to groundwater. CLSM derived GWI generally persists longer than GWI derived from in situ data, due at least in part to the inability of coarse model inputs to capture high frequency meteorological variability at local scales. The study also showed that groundwater can have a significant impact on soil moisture persistence where the water table is shallow. Soil moisture persistence was estimated to be longer in the eastern U.S. than in the west, in contrast to previous findings that were based on models that did not represent groundwater. Assimilation of terrestrial water storage data from the Gravity Recovery and Climate Experiment (GRACE) satellite mission improved the correlation between CLSM based regional average GWI and that based on in situ data in six of the eight regions. Practical issues regarding the application of GRACE assimilated groundwater storage for drought detection are discussed. An important conclusion of this study is that model parameters that control the depth to the water table, including bedrock depth, strongly influence the evolution and persistence of simulated groundwater and require careful configuration for drought monitoring. (C) 2014 Elsevier B.V. All rights reserved, C1 [Li, Bailing] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. [Li, Bailing; Rodell, Matthew] NASA, Hydrol Sci Lab, Goddard Space Flight Ctr, Greenbelt, MD USA. RP Li, BL (reprint author), Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. EM Bailing.li@nasa.gov RI Rodell, Matthew/E-4946-2012 OI Rodell, Matthew/0000-0003-0106-7437 FU GRACE Science Team; NASA Centers National Climate Assessment; NASA's Terrestrial Hydrology Program FX This study was supported by NASA's Terrestrial Hydrology Program and GRACE Science Team, and by the NASA Centers National Climate Assessment. We thank the valuable comments made by Yoshihide Wada and another reviewer which have helped improve the quality of this paper. NR 38 TC 15 Z9 16 U1 5 U2 46 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0022-1694 EI 1879-2707 J9 J HYDROL JI J. Hydrol. PD JUL PY 2015 VL 526 SI SI BP 78 EP 88 DI 10.1016/j.jhydrol.2014.09.027 PG 11 WC Engineering, Civil; Geosciences, Multidisciplinary; Water Resources SC Engineering; Geology; Water Resources GA CK0KS UT WOS:000355894700008 ER PT J AU Van den Hoek, J Burnicki, AC Ozdogan, M Zhu, AX AF Van den Hoek, Jamon Burnicki, Amy C. Ozdogan, Mutlu Zhu, A-Xing TI Using a pattern metric-based analysis to examine the success of forest policy implementation in Southwest China SO LANDSCAPE ECOLOGY LA English DT Article DE Pattern analysis; Forest policy; NFPP; SLCP; Forest cover change; Temporal resolution; Yunnan; China ID NORTHWEST YUNNAN PROVINCE; LAND-USE CHANGE; DEFORESTATION; CONSERVATION; ACCESSIBILITY; DISTURBANCE; VIETNAM; FRAGMENTATION; TRANSITIONS; ENVIRONMENT AB The National Forest Protection Program (NFPP) and sloping land conversion program (SLCP) were introduced in 1998 and 2000, respectively, with the shared goal of increasing forest cover and decreasing forest loss across China. The NFPP banned commercial logging and funded tree planting efforts while the SLCP subsidized tree planting on steeply sloping and otherwise disused lands. This study quantifies the patterns of forest loss and gain before and during policy implementation to gauge implementation effectiveness. By measuring patterns associated with spatially explicit processes linking land managers and forest resources, this study improves upon overly simplified assessments of implementation effectiveness that only consider the area of forest cover change. The shifting patterns of short- and long-term forest cover change in Diqing Prefecture, southwest China, are measured between 1990 and 2009. Eleven pattern metrics quantify the area, topography, and landscape feature proximity of forest loss or gain patches based on Landsat imagery-derived forest cover changes. Trends generally conformed to those expected under successful policy implementation: the proportion and fragmentation of forest loss declined, loss patches were found closer to villages and at lower elevations, and forest gain increased in proportion and median patch area. However, median loss patch area increased, suggesting greater localized harvesting intensity, and loss sites occupied steeper slopes contrary to SLCP goals. Forest cover change patterns did not wholly align with those expected of successful implementation but rather deviated due to the influences of regional tourism development and village- and household-level forest resource scarcity. C1 [Van den Hoek, Jamon; Zhu, A-Xing] Univ Wisconsin, Dept Geog, Madison, WI 53706 USA. [Burnicki, Amy C.] Univ Connecticut, Dept Civil & Environm Engn, Storrs, CT 06269 USA. [Ozdogan, Mutlu] Univ Wisconsin, Dept Forest & Wildlife Ecol, Madison, WI 53706 USA. RP Van den Hoek, J (reprint author), NASA, Biospher Sci Lab, Goddard Space Flight Ctr, 8800 Greenbelt Rd, Greenbelt, MD 20711 USA. EM jamon.vandenhoek@nasa.gov FU National Science Foundation [DGE-0549369] FX The fieldwork for this article was completed by the first author in 2008-2010 and supported by the National Science Foundation under Grant No. DGE-0549369 IGERT: Training Program on Biodiversity Conservation and Sustainable Development in Southwest China at the University of Wisconsin-Madison. NR 85 TC 1 Z9 1 U1 5 U2 25 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0921-2973 EI 1572-9761 J9 LANDSCAPE ECOL JI Landsc. Ecol. PD JUL PY 2015 VL 30 IS 6 BP 1111 EP 1127 DI 10.1007/s10980-015-0171-y PG 17 WC Ecology; Geography, Physical; Geosciences, Multidisciplinary SC Environmental Sciences & Ecology; Physical Geography; Geology GA CJ7EM UT WOS:000355657200011 ER PT J AU Dai, Q Han, DW Zhuo, L Huang, J Islam, T Srivastava, PK AF Dai, Qiang Han, Dawei Zhuo, Lu Huang, Jing Islam, Tanvir Srivastava, Prashant K. TI Impact of complexity of radar rainfall uncertainty model on flow simulation SO ATMOSPHERIC RESEARCH LA English DT Article DE Ensemble generator; MDEG; Copula; Flow simulation; Model uncertainty ID MEAN-FIELD BIAS; PRECIPITATION ESTIMATION; PARAMETER UNCERTAINTY; CATCHMENT MODELS; REAL; CALIBRATION; ACCURACY; COPULA; PREDICTION; RESOLUTION AB A large number of radar rainfall uncertainty (RRU) models have been proposed due to many error sources in weather radar measurements. It is recognized that these models should be integrated into overall uncertainty analysis schemes with other kinds of model uncertainties such as model parameter uncertainty when the radar rainfall is applied in hydrological modeling. We expect that the RRU model can be expressed in a mathematically extensible and simple format. However, the complexity of the RRU has been growing as more and more factors are considered such as spatio-temporal dependence and non-Gaussian distribution. This study analyzes how the RRU propagates through a hydrological model (the Xinanjiang model) and investigates which features of the RRU model have significant impacts on flow simulation. A RRU model named Multivariate Distributed Ensemble Generator (MDEG) is implemented in the Brue catchment in England under different model complexities. The generated ensemble rainfall values by MDEG are then input into the Xinanjiang model to produce uncertainty bands of ensemble flows. Comparison of five important indicators that describe the characteristics of uncertainty bands shows that the ensemble flows generated by MDEG with non-Gaussian marginal and joint distributions are close to the ones with Gaussian distributions. In addition, the dispersion of the uncertainty bands increases dramatically with the growth of the MDEG model complexity. It is concluded that the Gaussian marginal distribution and spatio-temporal dependence using Gaussian copula is considered to be the preferred configuration of the MDEG model for hydrological model uncertainty analysis. Further studies should be carried out in a variety of catchments under different climate conditions and geographical locations to check if the conclusion is valid beyond the Brue catchment under the British climate. (C) 2015 Elsevier B.V. All rights reserved. C1 [Dai, Qiang] Nanjing Normal Univ, Minist Educ, Key Lab VGE, Nanjing, Jiangsu, Peoples R China. [Dai, Qiang; Han, Dawei; Zhuo, Lu] Univ Bristol, Dept Civil Engn, WEMRC, Bristol, Avon, England. [Dai, Qiang] Nanjing Normal Univ, Jiangsu Ctr Collaborat Innovat Geog Informat Reso, Nanjing, Jiangsu, Peoples R China. [Huang, Jing] Hohai Univ, State Key Lab Hydrol Water Resources & Hydraul En, Nanjing, Jiangsu, Peoples R China. [Islam, Tanvir] NOAA, NESDIS, Ctr Satellite Applicat & Res, College Pk, MD USA. [Srivastava, Prashant K.] NASA, Goddard Space Flight Ctr, Hydrol Sci, Greenbelt, MD 20771 USA. RP Dai, Q (reprint author), Nanjing Normal Univ, Minist Educ, Key Lab VGE, Nanjing, Jiangsu, Peoples R China. EM q.dai@bristol.ac.uk OI Islam, Tanvir/0000-0003-2429-3074 FU National Natural Science Foundation of China [41171301]; Priority Academic Program Development of Jiangsu Higher Education Institutions (PAPD) program FX This work is supported by the National Natural Science Foundation of China (Grant No. 41171301) and the Priority Academic Program Development of Jiangsu Higher Education Institutions (PAPD) program. The authors acknowledge the British Atmospheric Data Centre, Digimap Resource Centre and the Land Resource Management Unit of the European Commission Joint Research Centre for providing the data. NR 58 TC 0 Z9 0 U1 2 U2 11 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0169-8095 EI 1873-2895 J9 ATMOS RES JI Atmos. Res. PD JUL-AUG PY 2015 VL 161 BP 93 EP 101 DI 10.1016/j.atmosres.2015.04.002 PG 9 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA CJ7XB UT WOS:000355712600009 ER PT J AU Lombardi-Carlson, LA Andrews, AH AF Lombardi-Carlson, Linda A. Andrews, Allen H. TI Age estimation and lead-radium dating of golden tilefish, Lopholatilus chamaeleonticeps SO ENVIRONMENTAL BIOLOGY OF FISHES LA English DT Article DE Age validation; Radiometric ageing; Lead-210; Radium-226; Malacanthidae; Great Northern tilefish ID TOOTHFISH DISSOSTICHUS-ELEGINOIDES; ROUGHY HOPLOSTETHUS-ATLANTICUS; BOMB RADIOCARBON; MID-ATLANTIC; SEX-CHANGE; GROWTH; VALIDATION; FISHERIES; OTOLITHS; SOUTHERN AB There is a growing concern over the lack of life history information for many deepwater fisheries species, including golden tilefish, Lopholatilus chamaeleonticeps. Fundamental life history characteristics, like age and growth, are required for effective, age-structured stock assessments and management decisions. A previous effort to validate golden tilefish age estimates using bomb radiocarbon dating was inconclusive, which led to an application of lead-radium dating in the current study. Lead-radium dating uses the radioactive disequilibrium of lead-210 (Pb-210) and radium-226 (Ra-226) in otoliths as an independent estimate of age. Ages were also estimated using traditional age estimates by counting growth zones in thin otolith sections and lead-radium dating was used to test these estimates. Radiometric ages (corrected for time since capture) were similar to age estimates from growth zone counts for two of the female age groups and the two oldest age groups of unknown sex, which confirmed an annual growth zone deposition. However, radiometric ages did not agree with age estimates from growth zone counts for males. The difference may be attributed to geographical variations in radium levels, growth rates and growth zone formation by gender or gender transition. Male sagittal otoliths revealed inconsistent growth zone patterns in thin sections, which may have contributed to underageing. Golden tilefish longevity was confirmed to 26 years. C1 [Lombardi-Carlson, Linda A.] Univ Florida, Sch Forest Resources & Conservat, Fisheries & Aquat Sci Program, Gainesville, FL USA. [Andrews, Allen H.] Pacif Islands Fisheries Sci Ctr, Natl Marine Fisheries Serv, Honolulu, HI 96818 USA. RP Lombardi-Carlson, LA (reprint author), Southeast Fisheries Sci Ctr, Natl Marine Fisheries Serv, 3500 Delwood Beach Rd, Panama City, FL 32408 USA. EM Linda.Lombardi@noaa.gov RI Andrews, Allen/G-3686-2016 OI Andrews, Allen/0000-0002-9001-8305 FU U.S. Department of Commerce, National Marine Fisheries Service, Marine Fisheries Initiative Program [07MFIH007] FX We thank Heather Hawk at Moss Landing Marine Laboratories for assistance with sample processing and Craig Lundstrom at University of Illinois at Urbana-Champaign for ICP-MS processing of the purified radium samples. We appreciate Claudia Dennis (National Marine Fisheries Service, Miami, FL) for collection of biological samples at the docks and Laura Goetz Thorton (National Marine Fisheries Service, Panama City, FL) for sectioning the otoliths used in this study. We also thank Bryon White and Marcel Reichert at South Carolina Department of Natural Resources, Marine Resources Research Institute, Marine Resources Monitoring, Assessment and Predication Program in providing golden tilefish radiocarbon values and otolith sections. The primary author recognizes her doctoral committee (Micheal Allen, William E. Pine, III, Carl Walters, Debra Murie, Alan Bolten, and Clay Porch) at the University of Florida, School of Forest Resources and Conservation, Fisheries and Aquatic Sciences Program for their comments and suggestions on this research as it appears in her dissertation. Opinions expressed herein are of the authors and do not imply endorsement by National Marine Fisheries Service. Financial support was provided by the U.S. Department of Commerce, National Marine Fisheries Service, Marine Fisheries Initiative Program (07MFIH007). NR 59 TC 1 Z9 1 U1 2 U2 6 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0378-1909 EI 1573-5133 J9 ENVIRON BIOL FISH JI Environ. Biol. Fishes PD JUL PY 2015 VL 98 IS 7 BP 1787 EP 1801 DI 10.1007/s10641-015-0398-0 PG 15 WC Ecology; Marine & Freshwater Biology SC Environmental Sciences & Ecology; Marine & Freshwater Biology GA CJ6RJ UT WOS:000355620700006 ER PT J AU Hu, SW Blakely, WF Cucinotta, FA AF Hu, Shaowen Blakely, William F. Cucinotta, Francis A. TI HEMODOSE: A Biodosimetry Tool Based on Multi-type Blood Cell Counts SO HEALTH PHYSICS LA English DT Article ID SEVERE RADIATION ACCIDENTS; EARLY DOSE ASSESSMENT; IONIZING-RADIATION; MEDICAL-MANAGEMENT; BIOLOGICAL DOSIMETRY; EXPOSURE; HEMATOPOIESIS; MODEL; RECOMMENDATIONS; PREDICTION AB Peripheral blood cell counts are important biomarkers of radiation exposure. In this work, a simplified compartmental modeling approach is applied to simulate the perturbation of the hematopoiesis system in humans after radiation exposure, and HemoDose software is reported to estimate individuals' absorbed doses based on multi-type blood cell counts. Testing with patient data in some historical accidents indicates that either single or serial granulocyte, lymphocyte, leukocyte, and platelet counts after exposure can be robust indicators of the absorbed doses. In addition, such correlation exists not only in the early time window (1 or 2 d) but also in the late phase (up to 4 wk) after exposure, when the four types of cell counts are combined for analysis. These demonstrate the capability of HemoDose as a rapid point-of-care diagnostic or centralized high-throughput assay system for personnel exposed to unintended high doses of radiation, especially in large-scale nuclear/radiological disaster scenarios involving mass casualties. C1 [Hu, Shaowen] NASA, Wyle Labs, Johnson Space Ctr, Houston, TX 77058 USA. [Blakely, William F.] Uniformed Serv Univ Hlth Sci, Sci Res Dept, Armed Forces Radiobiol Res Inst, Bethesda, MD 20889 USA. [Cucinotta, Francis A.] Univ Nevada, Las Vegas, NV 89154 USA. RP Hu, SW (reprint author), NASA, Wyle Labs, Johnson Space Ctr, Houston, TX 77058 USA. EM Shaowen.Hu-1@nasa.gov FU NASA Space Radiation Risk Assessment Project; University of Nevada, Las Vegas FX The opinions or assertions contained herein are the private views of the authors and are not necessarily those of the Wyle Laboratories, the Armed Forces Radiobiology Research Institute, the Uniformed Services University of the Health Sciences, the University of Nevada, the U.S. Department of Defense, or National Aeronautics and Space Administration (NASA). We thank Alan H. Feiveson for proofreading our manuscript. This work was supported by NASA Space Radiation Risk Assessment Project and the University of Nevada, Las Vegas. We are thankful for many years of collaboration with Olga Smirnova. NR 48 TC 3 Z9 3 U1 2 U2 5 PU LIPPINCOTT WILLIAMS & WILKINS PI PHILADELPHIA PA TWO COMMERCE SQ, 2001 MARKET ST, PHILADELPHIA, PA 19103 USA SN 0017-9078 EI 1538-5159 J9 HEALTH PHYS JI Health Phys. PD JUL PY 2015 VL 109 IS 1 BP 54 EP 68 DI 10.1097/HP.0000000000000295 PG 15 WC Environmental Sciences; Public, Environmental & Occupational Health; Nuclear Science & Technology; Radiology, Nuclear Medicine & Medical Imaging SC Environmental Sciences & Ecology; Public, Environmental & Occupational Health; Nuclear Science & Technology; Radiology, Nuclear Medicine & Medical Imaging GA CJ6PL UT WOS:000355615700006 PM 26011498 ER PT J AU Garg, NK Gupta, M AF Garg, N. K. Gupta, Manika TI Assessment of improved soil hydraulic parameters for soil water content simulation and irrigation scheduling SO IRRIGATION SCIENCE LA English DT Article ID PEDO-TRANSFER FUNCTIONS; PEDOTRANSFER FUNCTIONS; UNSATURATED SOILS; RETENTION CURVES; MOISTURE; CONDUCTIVITY; MODEL; ALGORITHM; CAPACITY; DATABASE AB The efficient irrigation systems utilizing numerical models based on Richard's flow equation require key input parameters, soil hydraulic parameters (SHPs). The present study proposes a method to determine the SHPs from the soil water contents at field capacity and wilting point, which are determined for irrigation scheduling. It also compares them with the SHPs estimated by various pedotransfer functions (PTFs) to simulate respective soil water retention curves (SWRCs). High efficiencies of 70-80 % were obtained in simulating the SWRCs by the proposed method as compared to PTFs. In order to further assess the applicability of the SHPs as determined, the experiments were conducted under real field conditions for wheat crop in Roorkee, India, and SWRCs were experimentally determined. These different sets of SHPs, along with experimentally determined saturated permeability, were then used as input parameters in root water uptake model and the results of observed and simulated soil water contents were compared under three different irrigation treatments. It was found that the experimentally obtained SHPs and those obtained by the proposed method were able to simulate the soil water contents with efficiencies of 70-80 % at all the depths for all the three irrigation treatments, while the PTFs performed poorly. C1 [Garg, N. K.; Gupta, Manika] Indian Inst Technol Delhi, Dept Civil Engn, New Delhi 110016, India. [Gupta, Manika] Univ Space Res Assoc, Goddard Earth Sci Technol & Res, Columbia, MD USA. [Gupta, Manika] NASA Goddard Space Flight Ctr, Hydrol Sci Lab, Greenbelt, MD 20071 USA. RP Gupta, M (reprint author), Indian Inst Technol Delhi, Dept Civil Engn, New Delhi 110016, India. EM manikagup@gmail.com FU University Grant Commission, Government of India FX The financial support from University Grant Commission, Government of India, to Manika Gupta is acknowledged, for the time at IIT when the work was conducted. The authors would also like to thank National Institute of Hydrology, Roorkee, for providing facilities for soil physical analysis. The views expressed here are those of the authors solely and do not constitute a statement of policy, decision, or position on behalf of NASA. NR 52 TC 1 Z9 1 U1 2 U2 20 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0342-7188 EI 1432-1319 J9 IRRIGATION SCI JI Irrig. Sci. PD JUL PY 2015 VL 33 IS 4 BP 247 EP 264 DI 10.1007/s00271-015-0463-7 PG 18 WC Agronomy; Water Resources SC Agriculture; Water Resources GA CJ8LJ UT WOS:000355751800001 ER PT J AU Matsubara, Y Howard, AD Burr, DM Williams, RME Dietrich, WE Moore, JM AF Matsubara, Yo Howard, Alan D. Burr, Devon M. Williams, Rebecca M. E. Dietrich, William E. Moore, Jeffery M. TI River meandering on Earth and Mars: A comparative study of Aeolis Dorsa meanders, Mars and possible terrestrial analogs of the Usuktuk River, AK, and the Quinn River, NV SO GEOMORPHOLOGY LA English DT Article; Proceedings Paper CT 45th Annual Binghamton Geomorphology Symposium CY SEP 12-14, 2014 CL Knoxville, TN DE Meandering rivers; Terrestrial analog; Aeolis Dorsa; Mud-dominated; Permafrost controlled ID MEDUSAE FOSSAE FORMATION; MARTIAN OUTFLOW CHANNELS; ARCTIC COASTAL-PLAIN; THAW LAKE BASINS; RIPARIAN VEGETATION; BONNEVILLE BASIN; GREAT-BASIN; FLOODPLAIN FORMATION; SEDIMENT TRANSPORT; WIDTH ADJUSTMENT AB The paleo-meanders in the Aeolis Dorsa (AD) region show that meandering channels can develop in the absence of vegetation. Three possible mechanisms other than vegetation could contribute to the bank cohesion required to promote meandering: permafrost, abundant mud, and chemical cementation. Banks at the meandering Quinn River show little vegetation cover. Almost all sediment samples collected from the Quinn River deposits contain at least 41% mud (silt/clay), which is much higher than for most meandering streams. Ion chromatography (IC) analysis and scanning electron microscope (SEM) images showed presence of salts in river waters and sediments which may induce fine sediment to flocculate and be deposited. We find that bank cohesion promoting meandering can be provided by silt/clay, the deposition of which may be induced by dissolved salts. The sinuous Usuktuk River in the continuous permafrost region near Barrow, Alaska exhibited no exposed permafrost on stream banks. Instead vegetation seemed to be the dominant control of bank erosion. We have not found evidence for ice control of bank cohesion in this or other terrestrial rivers of similar size and in meandering pattern to the Martian AD meanders. We conclude that bank cohesion in the AD meanders was probably provided by deposition of fine suspended sediment that was flocculated by dissolved salts. (C) 2014 Elsevier B.V. All rights reserved. C1 [Matsubara, Yo] Ctr Earth & Planetary Studies, Natl Air & Space Museum, Smithsonian Inst, Washington, DC 20013 USA. [Howard, Alan D.] Univ Virginia, Dept Environm Sci, Charlottesville, VA 22904 USA. [Burr, Devon M.] Univ Tennessee, Dept Earth & Planetary Sci, Knoxville, TN 37996 USA. [Williams, Rebecca M. E.] Planetary Sci Inst, Tucson, AZ 85719 USA. [Dietrich, William E.] Univ Calif Berkeley, Dept Earth & Planetary Sci, Berkeley, CA 94720 USA. [Moore, Jeffery M.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Matsubara, Y (reprint author), Ctr Earth & Planetary Studies, Natl Air & Space Museum, Smithsonian Inst, Independence Ave ,6th St SW,MRC 315,POB 37012, Washington, DC 20013 USA. EM matsubaray@si.edu OI Howard, Alan/0000-0002-5423-1600 NR 175 TC 5 Z9 5 U1 3 U2 30 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0169-555X EI 1872-695X J9 GEOMORPHOLOGY JI Geomorphology PD JUL 1 PY 2015 VL 240 SI SI BP 102 EP 120 DI 10.1016/j.geomorph.2014.08.031 PG 19 WC Geography, Physical; Geosciences, Multidisciplinary SC Physical Geography; Geology GA CJ3AK UT WOS:000355355600009 ER PT J AU Beyer, RA AF Beyer, Ross A. TI An introduction to the data and tools of planetary geomorphology SO GEOMORPHOLOGY LA English DT Article DE Planetary; GIS; Image processing; Stereo; Mars ID IMAGING PHOTOPOLARIMETER EXPERIMENT; ORBITER LASER ALTIMETER; SCIENCE; MISSION; MARS; SYSTEM; CAMERA; HORIZONS; MERCURY; PHOTOCLINOMETRY AB This manuscript presents a review of data used by planetary geomorphologists and the software tools needed to prepare, process, and analyze those data, along with an example of doing so. Visible image capture and the photometric and geometric processing of those images are reviewed, as are laser altimetry data, and terrain data derived from images via stereogrammetry. Image processing, geographic, and geospatial software tools are discussed. (C) 2014 The Author. Published by Elsevier B.V. C1 [Beyer, Ross A.] SETI Inst, Sagan Ctr, Mountain View, CA 94043 USA. [Beyer, Ross A.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Beyer, RA (reprint author), SETI Inst, Sagan Ctr, Mountain View, CA 94043 USA. EM Ross.A.Beyer@nasa.gov OI Beyer, Ross/0000-0003-4503-3335 NR 66 TC 0 Z9 1 U1 3 U2 14 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0169-555X EI 1872-695X J9 GEOMORPHOLOGY JI Geomorphology PD JUL 1 PY 2015 VL 240 SI SI BP 137 EP 145 DI 10.1016/j.geomorph.2014.11.022 PG 9 WC Geography, Physical; Geosciences, Multidisciplinary SC Physical Geography; Geology GA CJ3AK UT WOS:000355355600011 ER PT J AU Lee, H Kim, J Waliser, DE Loikith, PC Mattmann, CA McGinnis, S AF Lee, Huikyo Kim, Jinwon Waliser, Duane E. Loikith, Paul C. Mattmann, Chris A. McGinnis, Seth TI Using joint probability distribution functions to evaluate simulations of precipitation, cloud fraction and insolation in the North America Regional Climate Change Assessment Program (NARCCAP) SO CLIMATE DYNAMICS LA English DT Article DE Regional climate model evaluation; NARCCAP; Cloud, precipitation and radiation; Joint probability distribution ID DENSITY-FUNCTIONS; MODEL; TEMPERATURE; VARIABILITY; MULTIYEAR; MESOSCALE; TERRAIN AB This study evaluates model fidelity in simulating relationships between seasonally averaged precipitation, cloud fraction and surface insolation from the North American Regional Climate Change Assessment Project (NARCCAP) hindcast using observational data from ground stations and satellites. Model fidelity is measured in terms of the temporal correlation coefficients between these three variables and the similarity between the observed and simulated joint probability distribution functions (JPDFs) in 14 subregions over the conterminous United States. Observations exhibit strong negative correlations between precipitation/cloud fraction and surface insolation for all seasons, whereas the relationship between precipitation and cloud fraction varies according to regions and seasons. The skill in capturing these observed relationships varies widely among the NARCCAP regional climate models, especially in the Midwest and Southeast coast regions where observations show weak (or even negative) correlations between precipitation and cloud fraction in winter due to frequent non-precipitating stratiform clouds. Quantitative comparison of univariate and JPDFs indicates that model performance varies markedly between regions as well as seasons. This study also shows that comparison of JPDFs is useful for summarizing the performance of and highlighting problems with some models in simulating cloud fraction and surface insolation. Our quantitative metric may be useful in improving climate models by highlighting shortcomings in the formulations related with the physical processes involved in precipitation, clouds and radiation or other multivariate processes in the climate system. C1 [Lee, Huikyo; Waliser, Duane E.; Loikith, Paul C.; Mattmann, Chris A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Kim, Jinwon; Waliser, Duane E.; Mattmann, Chris A.] Univ Calif Los Angeles, Los Angeles, CA USA. [McGinnis, Seth] Natl Ctr Atmospher Res, Boulder, CO 80307 USA. RP Lee, H (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr M-S 300-233, Pasadena, CA 91109 USA. EM huikyo.lee@jpl.nasa.gov OI McGinnis, Seth/0000-0001-8082-834X FU National Aeronautics and Space Administration; NASA National Climate Assessment project [11-NCA11-0028]; NASA AIST project [AIST-QRS-12-0002]; NSF ExArch [1125798] FX The contributions by H.K., D.E.W., P.C.L. and C.A.M. to this study were carried out on behalf of the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. This research was funded by NASA National Climate Assessment 11-NCA11-0028 and AIST AIST-QRS-12-0002 projects, and the NSF ExArch 1125798 (P.C.L., J.K., H.L., and D.E.W). NR 57 TC 0 Z9 0 U1 1 U2 7 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0930-7575 EI 1432-0894 J9 CLIM DYNAM JI Clim. Dyn. PD JUL PY 2015 VL 45 IS 1-2 BP 309 EP 323 DI 10.1007/s00382-014-2253-y PG 15 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA CI4IS UT WOS:000354712500018 ER PT J AU Kang, IS Yang, YM Tao, WK AF Kang, In-Sik Yang, Young-Min Tao, Wei-Kuo TI GCMs with implicit and explicit representation of cloud microphysics for simulation of extreme precipitation frequency SO CLIMATE DYNAMICS LA English DT Article DE Frequency of heavy precipitation; Cloud resolving model; GCM; Cold-cloud processes; Cloud microphysics ID GENERAL-CIRCULATION MODEL; TROPICAL INTRASEASONAL OSCILLATION; CLIMATE MODEL; CONVECTION PARAMETERIZATION; CUMULUS PARAMETERIZATION; HORIZONTAL RESOLUTION; AGCM SIMULATIONS; CMIP5 MODELS; TOGA COARE; VARIABILITY AB The present study aims to develop a general circulation model (GCM) with improved simulation of heavy precipitation frequency by improving the representations of cloud and rain processes. GCMs with conventional convective parameterizations produce common bias in precipitation frequency: they overestimate light precipitation and underestimate heavy precipitation with respect to observed values. This frequency shift toward light precipitation is attributed here to a lack of consideration of cloud microphysical processes related to heavy precipitation. The budget study of cloud microphysical processes using a cloud-resolving model shows that the melting of graupel and accretion of cloud water by graupel and rain water are important processes in the generation of heavy precipitation. However, those processes are not expressed explicitly in conventional GCMs with convective parameterizations. In the present study, the cloud microphysics is modified to allow its implementation into a GCM with a horizontal resolution of 50 km. The newly developed GCM, which includes explicit cloud microphysics, produces more heavy precipitation and less light precipitation than conventional GCMs, thus simulating a precipitation frequency that is closer to the observed. This study demonstrates that the GCM requires a full representation of cloud microphysics to simulate the extreme precipitation frequency realistically. It is also shown that a coarse-resolution GCM with cloud microphysics requires an additional mixing process in the lower troposphere. C1 [Kang, In-Sik] Seoul Natl Univ, Sch Earth & Environm Sci, Seoul 151747, South Korea. [Yang, Young-Min] Univ Hawaii, SOEST, Int Pacific Res Ctr, Honolulu, HI 96822 USA. [Tao, Wei-Kuo] NASA, Goddard Space Flight Ctr, Mesoscale Atmospher Proc Lab, Greenbelt, MD 20771 USA. RP Kang, IS (reprint author), Seoul Natl Univ, Sch Earth & Environm Sci, Seoul 151747, South Korea. EM kang@climate.snu.ac.kr RI Measurement, Global/C-4698-2015; 안, 민섭/D-9972-2015 FU National Research Foundation of Korea (NRF) - Korean government (MEST) [NRF-2012M1A2A2671775]; Brain Korea 21 Plus; NASA Precipitation Measurement Missions (PMM), the NASA Modeling, Analysis, and Prediction (MAP) Program FX This work was supported by a National Research Foundation of Korea (NRF) grant funded by the Korean government (MEST) (NRF-2012M1A2A2671775) and by the Brain Korea 21 Plus. Wei-Kuo Tao was supported by the NASA Precipitation Measurement Missions (PMM), the NASA Modeling, Analysis, and Prediction (MAP) Program. NR 47 TC 5 Z9 5 U1 0 U2 10 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0930-7575 EI 1432-0894 J9 CLIM DYNAM JI Clim. Dyn. PD JUL PY 2015 VL 45 IS 1-2 BP 325 EP 335 DI 10.1007/s00382-014-2376-1 PG 11 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA CI4IS UT WOS:000354712500019 ER PT J AU Larson, EJL Toon, OB West, RA Friedson, AJ AF Larson, Erik J. L. Toon, Owen B. West, Robert A. Friedson, A. James TI Microphysical modeling of Titan's detached haze layer in a 3D GCM SO ICARUS LA English DT Article DE Titan, atmosphere; Atmospheres, structure; Atmospheres, dynamics ID UPPER-ATMOSPHERE; OPTICAL-CONSTANTS; AEROSOLS; MESOSPHERE; THERMOSPHERE; SCATTERING; DYNAMICS; ORIGIN; SIZE AB We use a 3D GCM with coupled aerosol microphysics to investigate the formation and seasonal cycle of the detached haze layer in Titan's upper atmosphere. The base of the detached haze layer is defined by a local minimum in the vertical extinction profile. The detached haze is seen at all latitudes including the south pole as seen in Cassini images from 2005-2012. The layer merges into the winter polar haze at high latitudes where the Hadley circulation carries the particles downward. The hemisphere in which the haze merges with the polar haze varies with season. We find that the base of the detached haze layer occurs where there is a near balance between vertical winds and particle fall velocities. Generally the vertical variation of particle concentration in the detached haze region is simply controlled by sedimentation, so the concentration and the extinction vary roughly in proportion to air density. This variation explains why the upper part of the main haze layer, and the bulk of the detached haze layer follow exponential profiles. However, the shape of the profile is modified in regions where the vertical wind velocity is comparable to the particle fall velocity. Our simulations closely match the period when the base of the detached layer in the tropics is observed to begin its seasonal drop in altitude, and the total range of the altitude drop. However, the simulations have the base of the detached layer about 100 km lower than observed, and the time for the base to descend is slower in the simulations than observed. These differences may point to the model having somewhat lower vertical winds than occur on Titan, or somewhat too large of particle sizes, or some combination of both. Our model is consistent with a dynamical origin for the detached haze rather than a chemical or microphysical one. This balance between the vertical wind and particle fall velocities occurs throughout the summer hemisphere and tropics. The particle concentration gradients that are established in the summer hemisphere are transported to the winter hemisphere by meridional winds from the overturning Hadley cell. Our model is consistent with the disappearance of the detached haze layer in early 2014. Our simulations predict the detached haze and gap will reemerge at its original high altitude between mid 2014 and early 2015. (C) 2015 Elsevier Inc. All rights reserved. C1 [Larson, Erik J. L.; Toon, Owen B.] Univ Colorado, Dept Atmospher & Ocean Sci, Boulder, CO 80309 USA. [Larson, Erik J. L.; Toon, Owen B.] Univ Colorado, Lab Atmospher & Space Phys, Boulder, CO 80309 USA. [West, Robert A.; Friedson, A. James] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Larson, EJL (reprint author), NOAA, ESRL, Div Chem Sci, 325 Broad Way, Boulder, CO 80305 USA. EM larsonej@colorado.edu RI Larson, Erik/A-8668-2015 OI Larson, Erik/0000-0002-8994-1258 NR 27 TC 4 Z9 4 U1 0 U2 11 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD JUL 1 PY 2015 VL 254 BP 122 EP 134 DI 10.1016/j.icarus.2015.03.010 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CI8KU UT WOS:000355022000010 ER PT J AU Heldmann, JL Lamb, J Asturias, D Colaprete, A Goldstein, DB Trafton, LM Varghese, PL AF Heldmann, Jennifer L. Lamb, Justin Asturias, Daniel Colaprete, Anthony Goldstein, David B. Trafton, Laurence M. Varghese, Philip L. TI Evolution of the dust and water ice plume components as observed by the LCROSS visible camera and UV-visible spectrometer SO ICARUS LA English DT Article DE Moon; Spectroscopy; Moon, surface; Regoliths; Ices ID LUNAR SOUTH-POLE; COLD TRAP; IMPACT; DEPOSITS; MOON; PROSPECTOR AB The LCROSS (Lunar Crater Observation and Sensing Satellite) impacted the Cabeus crater near the lunar South Pole on 9 October 2009 and created an impact plume that was observed by the LCROSS Shepherding Spacecraft. Here we analyze data from the ultraviolet-visible spectrometer and visible context camera aboard the spacecraft. We use these data to constrain a numerical model to understand the physical evolution of the resultant plume. The UV-visible light curve peaks in brightness 18 s after impact and then decreases in radiance but never returns to the pre-impact radiance value for the similar to 4 min of observation by the Shepherding Spacecraft. The blue:red spectral ratio increases in the first 10 s, decreases over the following 50 s, remains constant for approximately 150 s, and then begins to increase again similar to 180 s after impact. Constraining the modeling results with spacecraft observations, we conclude that lofted dust grains remained suspended above the lunar surface for the entire 250 s of observation after impact. The impact plume was composed of both a high angle spike and low angle plume component. Numerical modeling is used to evaluate the relative effects of various plume parameters to further constrain the plume properties when compared with the observational data. Dust particle sizes lofted above the lunar surface were micron to sub-micron in size. Water ice particles were also contained within the ejecta cloud and simultaneously photo-dissociated and sublimated after reaching sunlight. Published by Elsevier Inc. C1 [Heldmann, Jennifer L.; Colaprete, Anthony] NASA, Ames Res Ctr, Div Space Sci & Astrobiol, Moffett Field, CA 94035 USA. [Lamb, Justin; Asturias, Daniel; Goldstein, David B.; Trafton, Laurence M.; Varghese, Philip L.] Univ Texas Austin, Austin, TX 78712 USA. RP Heldmann, JL (reprint author), NASA, Ames Res Ctr, Mail Stop 245-3, Moffett Field, CA 94035 USA. EM Jennifer.Heldmann@nasa.gov FU NASA LASER (Lunar Advanced Science and Exploration Research) [NNX13AH12A] FX This work was supported by NASA LASER (Lunar Advanced Science and Exploration Research) grant # NNX13AH12A. NR 37 TC 1 Z9 1 U1 1 U2 4 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD JUL 1 PY 2015 VL 254 BP 262 EP 275 DI 10.1016/j.icarus.2015.02.026 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CI8KU UT WOS:000355022000022 ER PT J AU Toigo, AD French, RG Gierasch, PJ Guzewich, SD Zhu, X Richardson, MI AF Toigo, Anthony D. French, Richard G. Gierasch, Peter J. Guzewich, Scott D. Zhu, Xun Richardson, Mark I. TI General circulation models of the dynamics of Pluto's volatile transport on the eve of the New Horizons encounter SO ICARUS LA English DT Article DE Pluto; Pluto, atmosphere; Atmospheres, dynamics ID STELLAR OCCULTATION; THERMAL STRUCTURE; ATMOSPHERE; SURFACE AB Pluto's atmospheric dynamics occupy an interesting regime in which the radiative time constant is quite long, the combined effects of high obliquity and a highly eccentric orbit can produce strong seasonal variations in atmospheric pressure, and the strong coupling between the atmosphere and volatile transport on the surface results in atmospheric flows that are quite sensitive to surface and subsurface properties that at present are poorly constrained by direct observations. In anticipation of the New Horizons encounter with the Pluto system in July 2015, we present a Pluto-specific three-dimensional general circulation model (GCM), PlutoWRF, incorporating the most accurate current radiative transfer models of Pluto's atmosphere, a physically robust treatment of nitrogen volatile transport, and the flexibility to accommodate richly detailed information about the surface and subsurface conditions as new data become available. We solve for a physically self-consistent, equilibrated combination of surface, subsurface, and atmospheric conditions to specify the boundary conditions and initial state values for each GCM run. This is accomplished using two reduced versions of PlutoWRF: a two-dimensional surface volatile exchange model to specify the properties of surface nitrogen ice and the initial atmospheric surface pressure, and a one-dimensional radiative-conductive-convective model that uses the two-dimensional model predictions to determine the corresponding global-mean atmospheric thermal profile. We illustrate the capabilities of PlutoWRF in predicting Pluto's general circulation, thermal state, and volatile transport of nitrogen by calculating the dynamical response of Pluto's atmosphere, based on four different idealized models of Pluto's surface ice distribution from Young (Young, L.A. [2013]. Astrophys. J. 766, L22) and Hansen et al. (Hansen, C.J., Paige, D.A., Young, LA. [2015]. Icarus 246, 183). Our GCM runs typically span 30 years, from 1985 to 2015, covering the period from the discovery of Pluto's atmosphere to present. For most periods simulated, zonal winds are strongly forced by a gradient wind balance, relaxing in later (recent) years to an angular momentum conservation balance of the seasonal polar cap sublimation flow. Near-surface winds generally follow a sublimation flow from the sunlit polar cap to the polar night cap, with a Coriolis turning of the wind as the air travels from pole to pole. We demonstrate the strong contribution of nitrogen sublimation and deposition to Pluto's atmospheric circulation. As New Horizons data become available, PlutoWRF can be used to construct models of Pluto's atmospheric dynamics and surface wind regimes more constrained by physical observations. (C) 2015 Elsevier Inc. All rights reserved. C1 [Toigo, Anthony D.; Zhu, Xun] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [French, Richard G.] Wellesley Coll, Wellesley, MA 02492 USA. [Gierasch, Peter J.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. [Guzewich, Scott D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Richardson, Mark I.] Ashima Res, Pasadena, CA 91106 USA. RP Toigo, AD (reprint author), Johns Hopkins Univ, Appl Phys Lab, Johns Hopkins Rd, Laurel, MD 20723 USA. EM Anthony.Toigo@jhuapl.edu RI Zhu, Xun/C-2097-2016; OI Zhu, Xun/0000-0001-7860-6430; Guzewich, Scott/0000-0003-1149-7385 FU NASA's Planetary Atmospheres Program Grant [NNX11AD83G] FX This work was supported in part by NASA's Planetary Atmospheres Program Grant NNX11AD83G. NR 30 TC 3 Z9 3 U1 1 U2 12 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD JUL 1 PY 2015 VL 254 BP 306 EP 323 DI 10.1016/j.icarus.2015.03.034 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CI8KU UT WOS:000355022000025 ER PT J AU Farrell, WM McLain, JL Collier, MR Keller, JW Jackson, TJ Delory, GT AF Farrell, W. M. McLain, J. L. Collier, M. R. Keller, J. W. Jackson, T. J. Delory, G. T. TI Is the electron avalanche process in a martian dust devil self-quenching? SO ICARUS LA English DT Article DE Mars; Meteorology ID OXIDANT ENHANCEMENT; MARS; STORMS; FIELDS AB Viking era laboratory experiments show that mixing tribocharged grains in a low pressure CO2 gas can form a discharge that glows, indicating the presence of an excited electron population that persists over many seconds. Based on these early experiments, it has been predicted that martian dust devils and storms may also contain a plasma and new plasma chemical species as a result of dust grain tribo-charging. However, recent results from modeling suggest a contrasting result: that a sustained electron discharge may not be easily established since the increase in gas conductivity would act to short-out the local E-fields and quickly dissipate the charged grains driving the process. In essence, the system was thought to be self-quenching (i.e., turn itself off). In this work, we attempt to reconcile the difference between observation and model via new laboratory measurements. We conclude that in a Mars-like low pressure CO2 atmosphere and expected E-fields, the electron current remains (for the most part) below the expected driving tribo-electric dust currents (similar to 10 mu A/m(2)), thereby making quenching unlikely. Published by Elsevier Inc. C1 [Farrell, W. M.; Collier, M. R.; Keller, J. W.; Jackson, T. J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [McLain, J. L.] Univ Maryland, College Pk, MD 20742 USA. [Delory, G. T.] Univ Calif Berkeley, Berkeley, CA 94720 USA. RP Farrell, WM (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RI Farrell, William/I-4865-2013; Collier, Michael/I-4864-2013 OI Collier, Michael/0000-0001-9658-6605 FU NASA's Mars Fundamental Research Program FX We gratefully acknowledge funding from NASA's Mars Fundamental Research Program. NR 23 TC 2 Z9 2 U1 2 U2 9 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD JUL 1 PY 2015 VL 254 BP 333 EP 337 DI 10.1016/j.icarus.2015.04.003 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CI8KU UT WOS:000355022000027 ER PT J AU Traub, WA AF Traub, Wesley A. TI Steps towards eta-Earth, from Kepler data SO INTERNATIONAL JOURNAL OF ASTROBIOLOGY LA English DT Article DE eta-Earth; Exoplanet; habitable zone; Kepler; noise estimation; terrestrial planets AB The goal of this paper is to take steps towards estimating the frequency of terrestrial planets in the habitable zones of their host stars, using planet counts from the Kepler mission. The method is to assume that an analytical form for the underlying distribution function, numerically simulate the observing procedure, compare the simulated and real observations, and iterate the model parameters to achieve convergence in the sense of least-squares. The underlying distribution can then be extrapolated to a region of interest, here the terrestrial habitable-zone range. In this regime (small radii, long periods), the instrument noise makes such detections essentially impossible below a fairly sharply defined threshold signal level. This threshold can be estimated from the existing data. By taking this cutoff into account, the distribution of planets, as a function of radius and period, can be estimated with minimal bias. Extending this distribution to terrestrial planets in habitable-zone orbits can yield an estimate of eta-sub-Earth. C1 [Traub, Wesley A.] Jet Prop Lab, M S 321 100, Pasadena, CA 91109 USA. [Traub, Wesley A.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Traub, Wesley A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Traub, Wesley A.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. RP Traub, WA (reprint author), CALTECH, Jet Prop Lab, M-S 321-100,4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM wtraub@jpl.nasa.gov FU National Aeronautics and Space Administration under the Exoplanet Exploration Programme; NASA [NAS5-26555]; NASA Office of Space Science [NNX13AC07G]; NASA Science Mission directorate FX This research has made use of the NASA Exoplanet Archive, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Programme. Some of the data presented in this paper were obtained from the Mikulski Archive for Space Telescopes (MAST). STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. Support for MAST for non-HST data is provided by the NASA Office of Space Science via grant NNX13AC07G and by other grants and contracts. This paper includes data collected by the Kepler mission. Funding for the Kepler mission is provided by the NASA Science Mission directorate. Copyright 2014, California Institute of Technology. NR 6 TC 1 Z9 1 U1 1 U2 6 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 1473-5504 EI 1475-3006 J9 INT J ASTROBIOL JI Int. J. Astrobiol. PD JUL PY 2015 VL 14 IS 3 SI SI BP 359 EP 363 DI 10.1017/S1473550414000457 PG 5 WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics; Geology GA CI7TJ UT WOS:000354967400002 ER PT J AU Kuhn, JR Berdyugina, SV AF Kuhn, Jeff R. Berdyugina, Svetlana V. TI Global warming as a detectable thermodynamic marker of Earth-like extrasolar civilizations: the case for a telescope like Colossus SO INTERNATIONAL JOURNAL OF ASTROBIOLOGY LA English DT Article DE civilization biomarker; extraterrestrial civilizations; global warming; Kardashev Type I civilizations ID URBAN HEAT-ISLAND; HABITABLE ZONE; HARPS SEARCH; SUPER-EARTH; PLANETARY SYSTEM; FUTURE; 667C; LIFE AB Earth-like civilizations generate heat from the energy that they utilize. The thermal radiation from this heat can be a thermodynamic marker for civilizations. Here we model such planetary radiation on Earth-like planets and propose a strategy for detecting such an alien unintentional thermodynamic electromagnetic biomarker. We show that astronomical infrared (IR) civilization biomarkers may be detected within an interestingly large cosmic volume using a 70 m-class or larger telescope. In particular, the Colossus telescope with achievable coronagraphic and adaptive optics performance may reveal Earth-like civilizations from visible and IR photometry timeseries' taken during an exoplanetary orbit period. The detection of an alien heat signature will have far-ranging implications, but even a null result, given 70 m aperture sensitivity, could also have broad social implications. C1 [Kuhn, Jeff R.] Univ Hawaii, Inst Astron, Maui, HI 96768 USA. [Berdyugina, Svetlana V.] Univ Hawaii, NASA Astrobiol Inst, Inst Astron, Honolulu, HI 96822 USA. [Berdyugina, Svetlana V.] Kiepenheuer Inst Sonnenphys, D-79104 Freiburg, Germany. RP Kuhn, JR (reprint author), Univ Hawaii, Inst Astron, 34 Ohia Ku St, Maui, HI 96768 USA. EM kuhn@ifa.hawaii.edu FU Alexander von Humboldt Foundation at the Kiepenheuer Institut fuer Sonnenphysik, Freiburg, Germany; NASA Astrobiology Institute senior fellowship at the University of Hawaii, Honolulu, USA; ERC Advance Grant HotMol; Searchlight Observatory Network; Colossus Corporation; Dynamic Structures Ltd. FX JRK was supported by a senior research award from the Alexander von Humboldt Foundation at the Kiepenheuer Institut fuer Sonnenphysik, Freiburg, Germany. SVB was supported by the NASA Astrobiology Institute senior fellowship at the University of Hawaii, Honolulu, USA and the ERC Advance Grant HotMol. We acknowledge the Searchlight Observatory Network, the Colossus Corporation and Dynamic Structures Ltd. for their support of the large telescope design and engineering efforts that would enable this search for extraterrestrial intelligence. NR 43 TC 2 Z9 2 U1 0 U2 4 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 1473-5504 EI 1475-3006 J9 INT J ASTROBIOL JI Int. J. Astrobiol. PD JUL PY 2015 VL 14 IS 3 SI SI BP 401 EP 410 DI 10.1017/S1473550414000585 PG 10 WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics; Geology GA CI7TJ UT WOS:000354967400007 ER PT J AU Douglas, S Perry, ME Abbey, WJ Tanaka, Z Chen, B McKay, CP AF Douglas, Susanne Perry, Meredith E. Abbey, William J. Tanaka, Zuki Chen, Bin McKay, Christopher P. TI The structure and chemical layering of Proterozoic stromatolites in the Mojave Desert SO INTERNATIONAL JOURNAL OF ASTROBIOLOGY LA English DT Article DE stromatolite; Mars; elemental analysis ID WESTERN-AUSTRALIA; EARTH; LIFE; OLD AB The Proterozoic carbonate stromatolites of the Pahrump Group from the Crystal Spring formation exhibit interesting layering patterns. In continuous vertical formations, there are sections of chevron-shaped stromatolites alternating with sections of simple horizontal layering. This apparent cycle of stromatolite formation and lack of formation repeats several times over a vertical distance of at least 30 m at the locality investigated. Small representative samples from each layer were taken and analysed using X-ray diffraction (XRD), X-ray fluorescence (XRF), environmental scanning electron microscopy - energy dispersive X-ray spectrometry, and were optically analysed in thin section. Optical and spectroscopic analyses of stromatolite and of non-stromatolite samples were undertaken with the objective of determining the differences between them. Elemental analysis of samples from within each of the four stromatolite layers and the four intervening layers shows that the two types of layers are chemically and mineralogically distinct. In the layers that contain stromatolites the Ca/Si ratio is high; in layers without stromatolites the Ca/Si ratio is low. In the high Si layers, both K and Al are positively correlated with the presence and levels of Si. This, together with XRD analysis, suggested a high K-feldspar (microcline) content in the non-stromatolitic layers. This variation between these two types of rocks could be due to changes in biological growth rates in an otherwise uniform environment or variations in detrital influx and the resultant impact on biology. The current analysis does not allow us to choose between these two alternatives. A Mars rover would have adequate resolution to image these structures and instrumentation capable of conducting a similar elemental analysis. C1 [Douglas, Susanne] Planetary Sci Inst, Tucson, AZ 85719 USA. [Douglas, Susanne] East Los Angeles Coll, Monterey Pk, CA 91754 USA. [Perry, Meredith E.] Univ Penn, Dept Earth & Environm Sci, Philadelphia, PA 19104 USA. [Perry, Meredith E.; Tanaka, Zuki; Chen, Bin; McKay, Christopher P.] NASA, Ames Res Ctr, Moffett Field, CA USA. [Abbey, William J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Tanaka, Zuki; Chen, Bin] Univ Calif Santa Cruz, Dept Elect Engn, Santa Cruz, CA 95060 USA. RP Douglas, S (reprint author), Planetary Sci Inst, Tucson, AZ 85719 USA. EM chris.mckay@nasa.gov FU NASA Astrobiology Institute; NASA Pennsylvania Space Grant Consortium; Greg and Susan Walker Endowment FX The authors would like to thank Hermann Pfefferkorn for help with thin section analyses, David Vann for help with handheld XRF analyses and thin section preparation, Gomaa Omar for help with XRD analyses and XRD equipment, and University of Pennsylvania Earth and Environmental Science Department, particularly Jane Dmochowski and Robert Giegengack. We would like to thank Drs Robert Anderson, Rohit Bhartia & Yang Liu of NASA's Jet Propulsion Laboratory for access to, respectively, the X-ray diffractometer, Raman spectrometer and petrographic microscope. Also, the authors would like to thank Ann Copin of JPL Library Services for timely help in gathering reference material. The authors would also like to thank the NASA Spaceward Bound for the field activities. The NASA Astrobiology Institute for funding to support travel and analysis. The NASA Pennsylvania Space Grant Consortium and The Greg and Susan Walker Endowment for funding. We thank the reviewers for specific and useful comments that greatly improved the paper. NR 20 TC 0 Z9 0 U1 3 U2 11 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 1473-5504 EI 1475-3006 J9 INT J ASTROBIOL JI Int. J. Astrobiol. PD JUL PY 2015 VL 14 IS 3 SI SI BP 517 EP 526 DI 10.1017/S1473550415000026 PG 10 WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics; Geology GA CI7TJ UT WOS:000354967400019 ER PT J AU Hyun, HJ Anderson, T Angelaszek, D Baek, SJ Copley, M Coutu, S Han, JH Huh, HG Hwang, YS Im, S Jeon, HB Kah, DH Kang, KH Kim, HJ Kim, KC Kwashnak, K Lee, J Lee, MH Link, JT Lutz, L Mitchell, JW Nutter, S Ofoha, O Park, H Park, IH Park, JM Patterson, P Seo, ES Wu, J Yoon, YS AF Hyun, H. J. Anderson, T. Angelaszek, D. Baek, S. J. Copley, M. Coutu, S. Han, J. H. Huh, H. G. Hwang, Y. S. Im, S. Jeon, H. B. Kah, D. H. Kang, K. H. Kim, H. J. Kim, K. C. Kwashnak, K. Lee, J. Lee, M. H. Link, J. T. Lutz, L. Mitchell, J. W. Nutter, S. Ofoha, O. Park, H. Park, I. H. Park, J. M. Patterson, P. Seo, E. S. Wu, J. Yoon, Y. S. TI Performances of photodiode detectors for top and bottom counting detectors of ISS-CREAM experiment SO NUCLEAR INSTRUMENTS & METHODS IN PHYSICS RESEARCH SECTION A-ACCELERATORS SPECTROMETERS DETECTORS AND ASSOCIATED EQUIPMENT LA English DT Article; Proceedings Paper CT 7th International Conference on New Developments in Photodetection (NDIP) CY JUL, 2014 CL Tours, FRANCE SP Inst Res Fundamental Laws Universe, CEA Tech LIST, Univ Lyon, Univ Claude Bernard Lyon, Inst Natl Physique Nucleaire Physique Particules, French Space Agcy DE Cosmic ray; ISS-CREAM; Photodiode; Plastic scintillator; Thermal-vacuum; Vibration ID COSMIC-RAYS; RADIATION; FABRICATION AB The Cosmic Ray Energetics and Mass (CREAM) experiment at the International Space Station (ISS) aims to elucidate the source and acceleration mechanisms of high-energy cosmic rays by measuring the energy spectra from protons to iron. The instalment is planned for launch in 2015 at the ISS, and it comprises a silicon charge detector, a carbon target, top and bottom counting detectors, a calorimeter, and a boronated scintillator detector. The top and bottom counting detectors are developed for separating the electrons from the protons, and each of them comprises a plastic scintillator and a 20 x 20 silicon photocliocle array. Each photodiocle is 2.3 cm x 2.3 cm in size and exhibits good electrical characteristics. The leakage current is measured to be less than 20 nA/cm(2) at an operating voltage. The signal-to-noise ratio is measured to be better than 70 using commercial electronics, and the radiation hardness is tested using a proton beam. A signal from the photodiode is amplified by VLSI (very-largescale integration) charge amp/hold circuits, the VA-TA viking chip. Environmental tests are performed using whole assembled photodiode detectors of a flight version. Herein, we present the characteristics of the developed photocliode along with the results of the environmental tests. (C) 2014 Elsevier B.V. All rights reserved. C1 [Hyun, H. J.; Jeon, H. B.; Kah, D. H.; Kang, K. H.; Kim, H. J.; Park, H.; Park, J. M.] Kyungpook Natl Univ, Taegu 702701, South Korea. [Anderson, T.; Coutu, S.] Penn State Univ, University Pk, PA 16802 USA. [Angelaszek, D.; Copley, M.; Han, J. H.; Huh, H. G.; Kim, K. C.; Kwashnak, K.; Lee, M. H.; Lutz, L.; Ofoha, O.; Patterson, P.; Seo, E. S.; Wu, J.; Yoon, Y. S.] Univ Maryland, College Pk, MD 20740 USA. [Baek, S. J.; Lee, J.; Park, I. H.] Sungkyunkwan Univ, Suwon 440746, South Korea. [Link, J. T.; Mitchell, J. W.] NASA GSFC, Greenbelt, MD 20771 USA. [Link, J. T.] CRESST USRA, Columbia, MD 21044 USA. [Nutter, S.] No Kentucky Univ, Highland Hts, KY 41099 USA. RP Park, H (reprint author), Kyungpook Natl Univ, Taegu 702701, South Korea. EM sunshine@knu.ac.kr RI Yoon, Young Soo/O-8580-2014 OI Yoon, Young Soo/0000-0001-7023-699X FU U.S. by NASA [NNX11AC52G, NNX08AC15G, NNX08AC16G]; Korea by the Creative Research Initiatives of MEST/NRF; National Research Foundation (NRF) of Korea [NRF-2014R1A1A2006456, NRF-2014R1A2A2A01002734] FX The authors thank the NASA Goddard Space Flight Center (GSFC) Wallops Flight Facility for project management and engineering support and NASA Johnson Space Center ISS Program Office for the launch support and the ISS accommodation. This work was supported in the U.S. by NASA Grant Nos. NNX11AC52G, NNX08AC15G, NNX08AC16G and their predecessor grants, as well as by directed RTOP funds to the NASA GSFC. It is supported in Korea by the Creative Research Initiatives of MEST/NRF and funded by a National Research Foundation (NRF) of Korea Grant Nos. (NRF-2014R1A1A2006456, NRF-2014R1A2A2A01002734). NR 10 TC 0 Z9 0 U1 0 U2 4 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0168-9002 EI 1872-9576 J9 NUCL INSTRUM METH A JI Nucl. Instrum. Methods Phys. Res. Sect. A-Accel. Spectrom. Dect. Assoc. Equip. PD JUL 1 PY 2015 VL 787 BP 134 EP 139 DI 10.1016/j.nima.2014.11.075 PG 6 WC Instruments & Instrumentation; Nuclear Science & Technology; Physics, Nuclear; Physics, Particles & Fields SC Instruments & Instrumentation; Nuclear Science & Technology; Physics GA CI6LE UT WOS:000354869900030 ER PT J AU Zhang, JC Wei, M Fryauf, DM Leon, JJD Norris, KJ Deng, H Kobayashi, NP AF Zhang, Junce Wei, Min Fryauf, David M. Leon, Juan J. Diaz Norris, Kate J. Deng, Hong Kobayashi, Nobuhiko P. TI Single-crystal indium phosphide nanowires grown on polycrystalline copper foils with an aluminum-doped zinc oxide template SO JOURNAL OF MATERIALS SCIENCE LA English DT Article ID ZNO THIN-FILMS; INP NANOWIRES; PHOTOLUMINESCENCE; SILICON; GAAS; SPECTROSCOPY; DEPOSITION; NETWORKS; CORE AB The growth of indium phosphide (InP) nanowires on transparent conductive aluminum-doped zinc oxide (AZO) thin films on polycrystalline copper (Cu) foils was proposed and demonstrated. AZO thin films and zinc oxide (ZnO) thin films, as comparison, were deposited on Cu foils by radio frequency magnetron sputtering. Subsequently, InP was grown by metal organic chemical vapor deposition with gold catalysts. InP nanowire networks formed on the AZO thin films, while no InP nanowires grew on the ZnO thin films. Morphological, crystalline, and optical properties of the InP nanowires on AZO thin films were compared with those of InP nanowires grown on silicon (Si) substrates. Zinc diffusion from AZO thin films into InP nanowire networks was suggested as the cause of substantial modifications on the optical properties of the InP nanowires on AZO thin films; redshift in photoluminescence spectra and a larger relative TO/LO intensity ratio in Raman spectra were observed, in comparison to those of the InP nanowires grown on Si substrates. In this paper, we proposed and demonstrated a new route to grow semiconductor nanowires on metals that potentially provide low-cost and mechanically flexible substrates and establish a reliable electrical contact by utilizing conductive oxide thin films as a template, which could offer a new material platform for such applications as sensors and thermoelectric devices. C1 [Zhang, Junce; Wei, Min; Fryauf, David M.; Leon, Juan J. Diaz; Norris, Kate J.; Kobayashi, Nobuhiko P.] Univ Calif Santa Cruz, Baskin Sch Engn, Santa Cruz, CA 95064 USA. [Zhang, Junce; Wei, Min; Fryauf, David M.; Leon, Juan J. Diaz; Norris, Kate J.; Kobayashi, Nobuhiko P.] Univ Calif Santa Cruz, Adv Studies Labs, Nanostruct Energy Convers Technol & Res NECTAR, NASA,Ames Res Ctr, Moffett Field, CA 94035 USA. [Deng, Hong] Univ Elect Sci & Technol China, Sch Microelect & Solid Elect, Chengdu 610054, Peoples R China. RP Zhang, JC (reprint author), Univ Calif Santa Cruz, Baskin Sch Engn, Santa Cruz, CA 95064 USA. EM juncezhang@gmail.com FU NASA SBIR [NNX11CE14P]; Semiconductor Research Corporation; University of California Santa Cruz; NASA Ames Research Center FX This work was partially supported by NASA SBIR NNX11CE14P and Semiconductor Research Corporation (Global Research Collaboration, Program Officer: Dr. Victor Zhirnov). We would like to thank Quantum Systems Laboratory at Hewlett-Packard Laboratories (Palo Alto, California) and the MACS facility (Moffett Field, California) at the Advanced Studies Laboratories, a strategic partnership between the University of California Santa Cruz and NASA Ames Research Center, for their continuous support on analytical equipment. NR 34 TC 0 Z9 0 U1 4 U2 52 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0022-2461 EI 1573-4803 J9 J MATER SCI JI J. Mater. Sci. PD JUL PY 2015 VL 50 IS 14 BP 4926 EP 4932 DI 10.1007/s10853-015-9038-5 PG 7 WC Materials Science, Multidisciplinary SC Materials Science GA CH7IM UT WOS:000354209400011 ER PT J AU Franco, B Bader, W Toon, GC Bray, C Perrin, A Fischer, EV Sudo, K Boone, CD Bovy, B Lejeune, B Servais, C Mahieu, E AF Franco, B. Bader, W. Toon, G. C. Bray, C. Perrin, A. Fischer, E. V. Sudo, K. Boone, C. D. Bovy, B. Lejeune, B. Servais, C. Mahieu, E. TI Retrieval of ethane from ground-based FTIR solar spectra using improved spectroscopy: Recent burden increase above Jungfraujoch SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Article DE Ethane; FTIR; Jungfraujoch; Pseudo-lines; Trend; Shale gas ID FREE TROPOSPHERIC CO; MODEL DESCRIPTION; CARBON-MONOXIDE; ATMOSPHERIC CHEMISTRY; SEASONAL-VARIATIONS; COLUMN ABUNDANCES; METHYL-CHLORIDE; HIGH-RESOLUTION; C2H6; HCN AB An improved spectroscopy is used to implement and optimize the retrieval strategy of ethane (C2H6) from ground-based Fourier Transform Infrared (FTIR) solar spectra recorded at the high-altitude station of Jungfraujoch (Swiss Alps, 46.5 degrees N, 8.0 degrees E, 3580 m a.s.l.). The improved spectroscopic parameters include C2H6 pseudo-lines in the 2720-3100 cm(-1) range and updated line parameters for methyl chloride and ozone. These improved spectroscopic parameters allow for substantial reduction of the fitting residuals as well as enhanced information content. They also contribute to limiting oscillations responsible for ungeophysical negative mixing ratio profiles. This strategy has been successfully applied to the Jungfraujoch solar spectra available from 1994 onwards. The resulting time series is compared with C2H6 total columns simulated by the state-of-the-art chemical transport model GEOS-Chem. Despite very consistent seasonal cycles between both data sets, a negative systematic bias relative to the FTIR observations suggests that C2H6 emissions are underestimated in the current inventories implemented in GEOS-Chem. Finally, C2H6 trends are derived from the FTIR time series, revealing a statistically-significant sharp increase of the C2H6 burden in the remote atmosphere above Jungfraujoch since 2009. Evaluating cause of this change in the C2H6 burden, which may be related to the recent massive growth of shale gas exploitation in North America, is of primary importance for atmospheric composition and air quality in the Northern Hemisphere. (c) 2015 Elsevier Ltd. All rights reserved. C1 [Franco, B.; Bader, W.; Bovy, B.; Lejeune, B.; Servais, C.; Mahieu, E.] Univ Liege, Inst Astrophys & Geophys, B-4000 Sart Tilman Par Liege, Belgium. [Toon, G. C.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Bray, C.] CEA, DEN, DPC, F-91191 Gif Sur Yvette, France. [Perrin, A.] Univ Paris Est Creteil, CNRS, LISA, UMR7583,IPSL, F-94010 Creteil, France. [Perrin, A.] Univ Paris 07, CNRS, LISA, UMR7583,IPSL, F-94010 Creteil, France. [Fischer, E. V.] Colorado State Univ, Dept Atmospher Sci, Ft Collins, CO 80523 USA. [Sudo, K.] Nagoya Univ, Grad Sch Environm Studies, Nagoya, Aichi 4648601, Japan. [Sudo, K.] Japan Agcy Marine Earth Sci & Technol, Dept Environm Geochem Cycle Res, Yokohama, Kanagawa, Japan. [Boone, C. D.] Univ Waterloo, Dept Chem, Waterloo, ON N2L 3G1, Canada. RP Franco, B (reprint author), Univ Liege, Inst Astrophys & Geophys, B-4000 Sart Tilman Par Liege, Belgium. EM bruno.franco@ulg.ac.be RI Fischer, Emily/K-7330-2015; Chem, GEOS/C-5595-2014; OI Fischer, Emily/0000-0001-8298-3669; Mahieu, Emmanuel/0000-0002-5251-0286; Bader, Whitney/0000-0003-0766-8460 FU AGACC-II project of the Science for Sustainable Development (SSD) program of the Belgian Science Policy Office (BELSPO, Brussels); MeteoSwiss (Global Atmospheric Watch); Federation Wallonie-Bruxelles; F.R.S. - FNRS; French program LEFE-CHAT (Les Enveloppes Fluides et l'Environnement - Chimie Atmospherique) of INSU (Institut des Sciences de l'Univers) from CNRS; U.S. National Oceanographic and Atmospheric Administration [NA14OAR4310148]; Global Environment Research Fund by Ministry of the Environment (MOE), Japan [S-7/12]; Research Program on Climate Change Adaptation (RECCA) by Ministry of Education, Culture, Sports, Science and Technology (MEXT), Japan; Canadian Space Agency FX The University of Liege contribution to the present work has mainly been supported by the AGACC-II project of the Science for Sustainable Development (SSD) program of the Belgian Science Policy Office (BELSPO, Brussels). Additional support was provided by MeteoSwiss (Global Atmospheric Watch), the Federation Wallonie-Bruxelles and the F.R.S. - FNRS. We thank the International Foundation High Altitude Research Stations Jungfraujoch and Gornergrat (HFSJG, Bern). E. Mahieu is Research Associate with F.R.S. - FNRS. We are grateful to the many colleagues who have contributed to FTIR data acquisition at the Jungfraujoch station. We thank Jeremy Harrison and colleagues for their high quality lab measurements of C2H6. Part of this work was performed at the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA. Agnes Perrin would like to thank for financial support the French program LEFE-CHAT (Les Enveloppes Fluides et l'Environnement - Chimie Atmospherique) of INSU (Institut des Sciences de l'Univers) from CNRS. Funding for Emily V. Fischer was provided by the U.S. National Oceanographic and Atmospheric Administration through award number NA14OAR4310148. This research was partly supported by the Global Environment Research Fund (S-7/12) by the Ministry of the Environment (MOE), Japan, and the Research Program on Climate Change Adaptation (RECCA) by the Ministry of Education, Culture, Sports, Science and Technology (MEXT), Japan. Funding for the Atmospheric Chemistry Experiment comes from the Canadian Space Agency. NR 74 TC 8 Z9 8 U1 1 U2 17 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0022-4073 EI 1879-1352 J9 J QUANT SPECTROSC RA JI J. Quant. Spectrosc. Radiat. Transf. PD JUL PY 2015 VL 160 BP 36 EP 49 DI 10.1016/j.jqsrt.2015.03.017 PG 14 WC Optics; Spectroscopy SC Optics; Spectroscopy GA CH6MN UT WOS:000354150800006 ER PT J AU Parsons, GR Foster, DG AF Parsons, Glenn R. Foster, Daniel G. TI Reducing bycatch in the United States Gulf of Mexico shrimp trawl fishery with an emphasis on red snapper bycatch reduction SO FISHERIES RESEARCH LA English DT Article DE Bycatch reduction device; Shrimp trawl; Red snapper ID LUTJANUS-CAMPECHANUS; WATER-FLOW; PERFORMANCE; HABITATS; BEHAVIOR; DEVICES AB Bycatch, the capture of non-targeted species during commercial fishing, is a global problem that may require novel solutions. The nested cylinder bycatch reduction device (NCBRD), developed using laboratory behavioral studies (Parsons and Foster, 2007; Parsons et al., 2012), was herein evaluated for reducing bycatch in shrimp trawl fisheries and fonts application in the U.S. Gulf of Mexico (GOM) fishery. We examined the efficacy of the NCBRD for retaining shrimp, for reducing total bycatch, and for reducing bycatch of juvenile red snapper (Lutjanus campechanus), a species that is presently over-fished in the GOM. Using paired trawling on-board leased, commercial fishing vessels, shrimp catch, total bycatch, and the catch of red snapper juveniles were compared from trawls equipped with an NCBRD and control trawls without. Depending upon configuration, trawls with an NCBRD captured about 46-100% of shrimp taken in controls, reduced total bycatch by 26-60% and, of particular note, reduced red snapper bycatch by about 50%. When catch rates were compared, 2.29 (+/- 0.38 s.e.) snapper/h/trawl were taken with an NCBRD and 6.11 (+/- 0.93 s.e.) snapper/h/trawl without, a highly significant (ANOVA, P = 0.0032, F = 9.39, d.f. = 1, 64) effect. Finally, using only red snapper captured in control trawls, we observed a significant effect of depth on red snapper capture with decreasing numbers of red snapper captured with increasing depth. In waters south of Galveston shallower than about 55 m, catch rates ranged from 4.5 to 23.4 snapper/h/trawl and in deeper water ranged from 0.3 to 2.4 snapper/h/trawl. We identified a highly significant relationship (P < 0.001, R-2 = 0.685) between red snapper catch and depth. We estimate that use of the NCBRD would reduce juvenile red snapper bycatch in the northern Gulf of Mexico by about 50%. These results suggest that the NCBRD may find application in trawl fisheries worldwide. (C) 2015 Elsevier B.V. All rights reserved. C1 [Parsons, Glenn R.] Univ Mississippi, Dept Biol, University, MS 38677 USA. [Foster, Daniel G.] Natl Marine Fisheries Serv, Engn & Harvesting Branch, Pascagoula, MS 39567 USA. RP Parsons, GR (reprint author), Univ Mississippi, Dept Biol, University, MS 38677 USA. EM bygrp@olemiss.edu; Daniel.G.Foster@noaa.gov FU Walton Foundation for Marine Research; World Wildlife Fund; National Marine Fisheries Service; National Fish and Wildlife Foundations', Shell Marine Research Program FX We are most grateful for the help of J. Mitchell, C. Gledhill, A. Chester and S. Szedlmayer for reviewing drafts of the manuscript and J. Gearhart for assistance with the figures. The help of the Ole Miss Biological Research Team consisting of B. Crosby, M. Gaylord, K. Rice and D. Williams was invaluable. We are likewise grateful for the captains and crews of the F/V Isabel Maier, F/V Simple Man, F/V Fair Maiden and F/V Captain Wick. Many thanks are due to S. Bosarge, L. Bosarge, G. Graham, M. Osmond and S. Donovan for their assistance. This work was made possible by grants to G.R.P. from the Walton Foundation for Marine Research, the World Wildlife Fund, the National Marine Fisheries Service and the National Fish and Wildlife Foundations', Shell Marine Research Program, The National Marine Fisheries Service does not approve, recommend, or endorse any proprietary product or material mentioned in this publication. NR 23 TC 0 Z9 0 U1 6 U2 34 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0165-7836 EI 1872-6763 J9 FISH RES JI Fish Res. PD JUL PY 2015 VL 167 BP 210 EP 215 DI 10.1016/j.fishres.2015.02.009 PG 6 WC Fisheries SC Fisheries GA CH0VO UT WOS:000353740700024 ER PT J AU Sanghavi, S Stephens, G AF Sanghavi, Suniti Stephens, Graeme TI Adaptation of the delta-m and delta-fit truncation methods to vector radiative transfer: Effect of truncation on radiative transfer accuracy SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Article DE Vector radiative transfer; Delta-m truncation; delta-fit method; Phase matrix; Aerosol; Cloud; Hyperspectral retrievals ID GASES OBSERVING SATELLITE; TRANSFER MODEL; COUPLED ATMOSPHERE; AEROSOL PROPERTIES; FOURIER EXPANSION; POLARIZED-LIGHT; PHASE FUNCTIONS; MIE SCATTERING; RETRIEVAL; MATRIX AB In the presence of aerosol and/or clouds, the use of appropriate truncation methods becomes indispensable for accurate but cost-efficient radiative transfer computations. Truncation methods allow the reduction of the large number (usually several hundreds) of Fourier components associated with particulate scattering functions to a more manageable number, thereby making it possible to carry out radiative transfer computations with a modest number of streams. While several truncation methods have been discussed for scalar radiative transfer, few rigorous studies have been made of truncation methods for the vector case. Here, we formally derive the vector form of Wiscombe's delta-m truncation method. Two main sources of error associated with delta-m truncation are identified as the delta-separation error (DSE) and the phase-truncation error (PTE). The view angles most affected by truncation error occur in the vicinity of the direction of exact backscatter. This view geometry occurs commonly in satellite based remote sensing applications, and is hence of considerable importance. In order to deal with these errors, we adapt the delta-fit approach of Hu et al. (2000) [17] to vector radiative transfer. The resulting delta BGE-fit is compared with the vectorized delta-m method. For truncation at l=25 of an original phase matrix consisting of over 300 Fourier components, the use of the delta BGE-fit minimizes the error due to truncation at these view angles, while practically eliminating error at other angles. We also show how truncation errors have a distorting effect on hyperspectral absorption line shapes. The choice of the delta BGE-fit method over delta-m truncation minimizes errors in absorption line depths, thus affording greater accuracy for sensitive retrievals such as those of XCO2 from OCO-2 or GOSAT measurements. (C) 2015 Elsevier Ltd. All rights reserved. C1 [Sanghavi, Suniti; Stephens, Graeme] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Sanghavi, Suniti; Stephens, Graeme] Colorado State Univ, Ft Collins, CO 80523 USA. RP Sanghavi, S (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM sanghavi@jpl.nasa.gov OI Sanghavi, Suniti/0000-0003-0754-9154 FU NASA Aerosol-Cloud-Ecosystem (ACE) mission project FX Three anonymous reviewers are thanked, whose comments helped improve the overall quality of this paper. The authors also wish to thank Dr. Paul von Allmen of JPL, whose computing facility was used to run vSmartMOM. This work has been supported by the NASA Aerosol-Cloud-Ecosystem (ACE) mission project. This research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA. NR 35 TC 2 Z9 2 U1 1 U2 13 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0022-4073 EI 1879-1352 J9 J QUANT SPECTROSC RA JI J. Quant. Spectrosc. Radiat. Transf. PD JUL PY 2015 VL 159 BP 53 EP 68 DI 10.1016/j.jqsrt.2015.03.007 PG 16 WC Optics; Spectroscopy SC Optics; Spectroscopy GA CH2LZ UT WOS:000353858000007 ER PT J AU Parsani, M Carpenter, MH Nielsen, EJ AF Parsani, Matteo Carpenter, Mark H. Nielsen, Eric J. TI Entropy stable wall boundary conditions for the three-dimensional compressible Navier-Stokes equations SO JOURNAL OF COMPUTATIONAL PHYSICS LA English DT Article DE Entropy; Entropy stability; Compressible Navier-Stokes equations; Solid wall boundary conditions; SBP-SAT; High-order discontinuous methods ID LARGE-EDDY SIMULATION; CONSERVATION-LAWS; DISCONTINUOUS GALERKIN; SQUARE CYLINDER; SCHEMES; SYSTEMS; FLOW; OPERATORS; EULER; FORM AB Non-linear entropy stability and a summation-by-parts framework are used to derive entropy stable wall boundary conditions for the three-dimensional compressible Navier-Stokes equations. A semi-discrete entropy estimate for the entire domain is achieved when the new boundary conditions are coupled with an entropy stable discrete interior operator. The data at the boundary are weakly imposed using a penalty flux approach and a simultaneous-approximation-term penalty technique. Although discontinuous spectral collocation operators on unstructured grids are used herein for the purpose of demonstrating their robustness and efficacy, the new boundary conditions are compatible with any diagonal norm summation-by-parts spatial operator, including finite element, finite difference, finite volume, discontinuous Galerkin, and flux reconstruction/correction procedure via reconstruction schemes. The proposed boundary treatment is tested for three-dimensional subsonic and supersonic flows. The numerical computations corroborate the non-linear stability (entropy stability) and accuracy of the boundary conditions. (C) 2015 Elsevier Inc. All rights reserved. C1 [Parsani, Matteo; Carpenter, Mark H.; Nielsen, Eric J.] NASA, Langley Res Ctr LaRC, Computat AeroSci Branch, Hampton, VA 23681 USA. RP Parsani, M (reprint author), NASA, Langley Res Ctr LaRC, Computat AeroSci Branch, Hampton, VA 23681 USA. EM matteo.parsani@nasa.gov; mark.h.carpenter@nasa.gov; eric.j.nielsen@nasa.gov OI Parsani, Matteo/0000-0001-7300-1280 FU "Revolutionary Computational Aerosciences" project; NASA Postdoctoral Program at the Langley Research Center FX Special thanks are extended to Dr. Mujeeb Malik for funding this work as part of the "Revolutionary Computational Aerosciences" project. This research was also supported by an appointment to the NASA Postdoctoral Program at the Langley Research Center, administered by Oak Ridge Associated Universities through a contract with NASA. The authors are also grateful to Professor Magnus Svard for the fruitful discussions on entropy stability. NR 62 TC 9 Z9 9 U1 1 U2 14 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0021-9991 EI 1090-2716 J9 J COMPUT PHYS JI J. Comput. Phys. PD JUL 1 PY 2015 VL 292 BP 88 EP 113 DI 10.1016/j.jcp.2015.03.026 PG 26 WC Computer Science, Interdisciplinary Applications; Physics, Mathematical SC Computer Science; Physics GA CF8KD UT WOS:000352807100005 ER EF