FN Thomson Reuters Web of Science™ VR 1.0 PT J AU Hosokawa, T Yoshida, N Omukai, K Yorke, HW AF Hosokawa, Takashi Yoshida, Naoki Omukai, Kazuyuki Yorke, Harold W. TI PROTOSTELLAR FEEDBACK AND FINAL MASS OF THE SECOND-GENERATION PRIMORDIAL STARS SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE accretion, accretion disks; cosmology: theory; early universe; H II regions; stars: evolution; stars: formation ID FOSSIL HII-REGIONS; 1ST STARS; EARLY UNIVERSE; ACCRETION RATES; DISK ACCRETION; GAS CLOUDS; EVOLUTION; BINARIES; IMPACT; HD AB The first stars in the universe ionized the ambient primordial gas through various feedback processes. "Second-generation" primordial stars potentially form from this disturbed gas after its recombination. In this Letter, we study the late formation stage of such second-generation stars, where a large amount of gas accretes onto the protostar and the final stellar mass is determined when the accretion terminates. We directly compute the complex interplay between the accretion flow and stellar ultraviolet (UV) radiation, performing radiation-hydrodynamic simulations coupled with stellar evolution calculations. Because of more efficient H-2 and HD cooling in the prestellar stage, the accretion rates onto the star are 10 times lower than in the case of the formation of the first stars. The lower accretion rates and envelope density result in the occurrence of an expanding bipolar H II region at a lower protostellar mass M-* similar or equal to 10 M-circle dot, which blows out the circumstellar material, thereby quenching the mass supply from the envelope to the accretion disk. At the same time the disk loses mass due to photoevaporation by the growing star. In our fiducial case the stellar UV feedback terminates mass accretion onto the star at M-* similar or equal to 17 M-circle dot. Although the derived masses of the second-generation primordial stars are systematically lower than those of the first generation, the difference is within a factor of only a few. Our results suggest a new scenario, whereby the majority of the primordial stars are born as massive stars with tens of solar masses, regardless of their generations. C1 [Hosokawa, Takashi; Yoshida, Naoki] Univ Tokyo, Dept Phys, Tokyo 1130033, Japan. [Hosokawa, Takashi; Yorke, Harold W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Yoshida, Naoki] Univ Tokyo, Kavli Inst Phys & Math Universe, Kashiwa, Chiba 2778583, Japan. [Omukai, Kazuyuki] Kyoto Univ, Dept Phys, Kyoto 6068502, Japan. RP Hosokawa, T (reprint author), Univ Tokyo, Dept Phys, Tokyo 1130033, Japan. EM takashi.hosokawa@phys.s.u-tokyo.ac.jp FU Fellowship of the Japan Society for the Promotion of Science for Research Abroad; Ministry of Education, Science and Culture of Japan [2168407, 21244021]; National Aeronautics and Space Administration (NASA) FX The authors thank Neal Turner and Rolf Kuiper for fruitful discussions and comments. T.H. appreciates the support by the Fellowship of the Japan Society for the Promotion of Science for Research Abroad. K.O. is supported by the Grants-in-Aid by the Ministry of Education, Science and Culture of Japan (2168407 and 21244021). Portions of this work were conducted at the Jet Propulsion Laboratory, California Institute of Technology, operating under a contract with the National Aeronautics and Space Administration (NASA). NR 42 TC 37 Z9 37 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD DEC 1 PY 2012 VL 760 IS 2 AR L37 DI 10.1088/2041-8205/760/2/L37 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 037KM UT WOS:000311103000018 ER PT J AU Mayama, S Hashimoto, J Muto, T Tsukagoshi, T Kusakabe, N Kuzuhara, M Takahashi, Y Kudo, T Dong, R Fukagawa, M Takami, M Momose, M Wisniewski, JP Follette, K Abe, L Akiyama, E Brandner, W Brandt, T Carson, J Egner, S Feldt, M Goto, M Grady, CA Guyon, O Hayano, Y Hayashi, M Hayashi, S Henning, T Hodapp, KW Ishii, M Iye, M Janson, M Kandori, R Kwon, J Knapp, GR Matsuo, T McElwain, MW Miyama, S Morino, JI Moro-Martin, A Nishimura, T Pyo, TS Serabyn, E Suto, H Suzuki, R Takato, N Terada, H Thalmann, C Tomono, D Turner, EL Watanabe, M Yamada, T Takami, H Usuda, T Tamura, M AF Mayama, S. Hashimoto, J. Muto, T. Tsukagoshi, T. Kusakabe, N. Kuzuhara, M. Takahashi, Y. Kudo, T. Dong, R. Fukagawa, M. Takami, M. Momose, M. Wisniewski, J. P. Follette, K. Abe, L. Akiyama, E. Brandner, W. Brandt, T. Carson, J. Egner, S. Feldt, M. Goto, M. Grady, C. A. Guyon, O. Hayano, Y. Hayashi, M. Hayashi, S. Henning, T. Hodapp, K. W. Ishii, M. Iye, M. Janson, M. Kandori, R. Kwon, J. Knapp, G. R. Matsuo, T. McElwain, M. W. Miyama, S. Morino, J. -I. Moro-Martin, A. Nishimura, T. Pyo, T. -S. Serabyn, E. Suto, H. Suzuki, R. Takato, N. Terada, H. Thalmann, C. Tomono, D. Turner, E. L. Watanabe, M. Yamada, T. Takami, H. Usuda, T. Tamura, M. TI SUBARU IMAGING OF ASYMMETRIC FEATURES IN A TRANSITIONAL DISK IN UPPER SCORPIUS SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE planetary systems; protoplanetary disks; stars: pre-main sequence; techniques: polarimetric ID T-TAURI STARS; PROTOPLANETARY DISK; OB ASSOCIATION; PRETRANSITIONAL DISKS; INFRARED VARIABILITY; CIRCUMSTELLAR DISK; PLANET FORMATION; MOLECULAR CLOUD; FORMING REGIONS; SCATTERED-LIGHT AB We report high-resolution (0.07 arcsec) near-infrared polarized intensity images of the circumstellar disk around the star 2MASS J16042165-2130284 obtained with HiCIAO mounted on the Subaru 8.2 m telescope. We present our H-band data, which clearly exhibit a resolved, face-on disk with a large inner hole for the first time at infrared wavelengths. We detect the centrosymmetric polarization pattern in the circumstellar material as has been observed in other disks. Elliptical fitting gives the semimajor axis, semiminor axis, and position angle (P.A.) of the disk as 63 AU, 62 AU, and -14 degrees, respectively. The disk is asymmetric, with one dip located at P.A.s of similar to 85 degrees. Our observed disk size agrees well with a previous study of dust and CO emission at submillimeter wavelength with Submillimeter Array. Hence, the near-infrared light is interpreted as scattered light reflected from the inner edge of the disk. Our observations also detect an elongated arc (50 AU) extending over the disk inner hole. It emanates at the inner edge of the western side of the disk, extending inward first, then curving to the northeast. We discuss the possibility that the inner hole, the dip, and the arc that we have observed may be related to the existence of unseen bodies within the disk. C1 [Mayama, S.] Grad Univ Adv Studies SOKENDAI, Ctr Promot Integrated Sci, Hayama, Kanagawa 2400193, Japan. [Mayama, S.; Hayano, Y.; Hayashi, M.; Hayashi, S.; Iye, M.; Kwon, J.; Takato, N.; Takami, H.; Usuda, T.; Tamura, M.] Grad Univ Adv Studies SOKENDAI, Dept Astron Sci, Mitaka, Tokyo 1818588, Japan. [Hashimoto, J.; Kusakabe, N.; Kuzuhara, M.; Takahashi, Y.; Akiyama, E.; Hayashi, M.; Iye, M.; Kandori, R.; Morino, J. -I.; Suto, H.; Suzuki, R.; Tamura, M.] Natl Inst Nat Sci, Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan. [Muto, T.] Kogakuin Univ, Div Liberal Arts, Shinjuku Ku, Tokyo 1638677, Japan. [Tsukagoshi, T.; Momose, M.] Ibaraki Univ, Coll Sci, Mito, Ibaraki 3108512, Japan. [Kuzuhara, M.] Univ Tokyo, Dept Earth & Planetary Sci, Bunkyo Ku, Tokyo 1130033, Japan. [Takahashi, Y.] Univ Tokyo, Dept Astron, Bunkyo Ku, Tokyo 1130033, Japan. [Kudo, T.; Egner, S.; Guyon, O.; Hayano, Y.; Hayashi, S.; Ishii, M.; Nishimura, T.; Pyo, T. -S.; Takato, N.; Terada, H.; Tomono, D.; Takami, H.; Usuda, T.] Natl Inst Nat Sci, Natl Astron Observ Japan, Subaru Telescope, Hilo, HI 96720 USA. [Dong, R.; Brandt, T.; Janson, M.; Knapp, G. R.; Moro-Martin, A.; Turner, E. L.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Fukagawa, M.] Osaka Univ, Grad Sch Sci, Dept Earth & Space Sci, Toyonaka, Osaka 5600043, Japan. [Takami, M.] Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan. [Wisniewski, J. P.] Univ Oklahoma, HL Dodge Dept Phys & Astron, Norman, OK 73019 USA. [Follette, K.] Univ Arizona, Dept Astron, Tucson, AZ 85721 USA. [Follette, K.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Abe, L.] Univ Nice Sophia Antipolis, UMR6525, Lab Hippolyte Fizeau, F-06108 Nice 02, France. [Brandner, W.; Feldt, M.; Henning, T.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Carson, J.] Coll Charleston, Dept Phys & Astron, Charleston, SC 29424 USA. [Goto, M.] Univ Sternwarte Munchen, D-81679 Munich, Germany. [Grady, C. A.] NASA, Goddard Space Flight Ctr, Goddard Ctr Astrobiol, Greenbelt, MD 20771 USA. [Grady, C. A.] Eureka Sci, Oakland, CA 96002 USA. [Grady, C. A.; McElwain, M. W.] NASA, Goddard Space Flight Ctr, ExoPlanets & Stellar Astrophys Lab, Greenbelt, MD 20771 USA. [Hodapp, K. W.] Univ Hawaii, Inst Astron, Hilo, HI 96720 USA. [Matsuo, T.] Kyoto Univ, Dept Astron, Sakyo Ku, Kyoto 6068502, Japan. [Miyama, S.] Hiroshima Univ, Off President, Hiroshima 7398511, Japan. [Moro-Martin, A.] CSIC, INTA, CAB, Dept Astrofis, E-28850 Madrid, Spain. [Serabyn, E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Thalmann, C.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 XH Amsterdam, Netherlands. [Turner, E. L.] Univ Tokyo, Inst Phys & Math Universe, Kashiwa, Chiba 2278568, Japan. [Watanabe, M.] Hokkaido Univ, Dept Cosmosci, Sapporo, Hokkaido 0600810, Japan. [Yamada, T.] Tohoku Univ, Astron Inst, Aoba Ku, Sendai, Miyagi 9808578, Japan. RP Mayama, S (reprint author), Grad Univ Adv Studies SOKENDAI, Ctr Promot Integrated Sci, Hayama, Kanagawa 2400193, Japan. EM mayama_satoshi@soken.ac.jp RI Turner, Edwin/A-4295-2011; MIYAMA, Shoken/A-3598-2015 FU MEXT [22000005]; KAKENHI [23103004, 24103504, 24840037]; US NSF grant [1009314, 1009203]; Center for the Promotion of Integrated Sciences (CPIS) of The Graduate University for Advanced Studies (SOKENDAI) FX We thank the telescope staff and operators at the Subaru Telescope for their assistance. We also thank our referee for the constructive comments that have helped to improve this manuscript. Part of this research was carried out at the JPL, under a contract with NASA. This work is partially supported by a Grant-in-Aid for Science Research in a Priority Area from MEXT 22000005 (M.T.), KAKENHI 23103004 (M.M. and M.F.), 24103504 (T.T.), 24840037 (T.M.), US NSF grant 1009314 (J.P.W.), and 1009203 (J.C.). This work was supported in part by the Center for the Promotion of Integrated Sciences (CPIS) of The Graduate University for Advanced Studies (SOKENDAI). NR 41 TC 55 Z9 55 U1 0 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD DEC 1 PY 2012 VL 760 IS 2 AR L26 DI 10.1088/2041-8205/760/2/L26 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 037KM UT WOS:000311103000007 ER PT J AU Chatfield, RB Esswein, RF AF Chatfield, Robert B. Esswein, Robert F. TI Estimation of surface O-3 from lower-troposphere partial-column information: Vertical correlations and covariances in ozonesonde profiles SO ATMOSPHERIC ENVIRONMENT LA English DT Article DE Remote retrieval; Smog ozone; Surface ozone; Statistical structure of atmosphere; Ozonesonde; Boundary layer structure; Pollution layering ID SATELLITE MEASUREMENTS; POLLUTION AB Analysis of the spatial correlation of ozone mixing ratio in the vertical provides information useful for several purposes: (a) it aids description of the degree of regionality of the ozone transport-transformation processes, (b) the information provided in the form of a priori covariance matrices for remote retrieval algorithms can simplify and sharpen accuracy of the resulting estimates, and most importantly, (c) it allows a first evaluation of the improvement that remote retrievals can give over boundary-layer climatology. Vertical profiles of mean, variance, and vertical autocovariance, and vertical autocorrelation of ozone mixing ratios were estimated and given parameterizations. The WOUDC ozonesonde network database was used. During the years 2004-2006, these were considerably augmented by sondes taken by NASA, NOAA, and Canadian agencies during recent summertime intensive periods in North America. There are large differences across the North American continent in the patterns and magnitudes of correlation, especially in the lowest 2-3 km of the troposphere. This is especially significant for the near-surface layers (100's of meters deep) which determine actual surface O-3 smog exposure and phytotoxicity, since satellite retrievals typically characterize at best a thick layer extending 3 km or more from the surface. The relative variation of O-3 decreases in the vertical, particularly for the somewhat polluted launch stations, and this affects inference of surface O-3 significantly. We outline a simple synthesis of mixed-layer and ozone-chemistry behavior to aid discussion of this and similar phenomena. Regional differences suggest broad if qualitative explanations in terms of larger-scale (interstate-transport) and local-scale phenomena (lake and sea breezes, degree/frequency of subsidence), inviting future study. The character of near-surface-to-full-layer covariance suggests that remote retrieval can describe surface ozone surprisingly well using 0-3 km partial-column ozone... for many situations. This indicates that there is substantial utility for new remote-retrieval methods that exploit ozone absorption in multiple wavelength regions, e.g., UV + Vis, UV + IR, or UV + Vis + IR. In summary, we find considerable value in interpreting retrievable O-3 columns to estimate O-3 quantities that are closely relevant to air pollution mitigation. Published by Elsevier Ltd. C1 [Chatfield, Robert B.; Esswein, Robert F.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Esswein, Robert F.] Bay Area Environm Res, Sonoma, CA 95476 USA. RP Chatfield, RB (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM Robert.B.Chatfield@nasa.gov FU Environment Canada; NOAA; NASA; Earth Science Division of the NASA Science Mission Directorate FX We particularly appreciate the contributions of the many ozonesonde operators and the industry of the organizers (especially D.W. Tarasick, S.J. Oltmans, and A.M. Thompson) of the sonde networks, funded by Environment Canada and allied organizations, NOAA, and NASA. Funding for this effort was provided by the Earth Science Division of the NASA Science Mission Directorate. Thanks to Laura Iraci and Michael Newchurch who reviewed an earlier draft. NR 35 TC 7 Z9 7 U1 3 U2 15 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1352-2310 J9 ATMOS ENVIRON JI Atmos. Environ. PD DEC PY 2012 VL 61 BP 103 EP 113 DI 10.1016/j.atmosenv.2012.06.033 PG 11 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA 038QA UT WOS:000311188000012 ER PT J AU Beyersdorf, AJ Thornhill, KL Winstead, EL Ziemba, LD Blake, DR Timko, MT Anderson, BE AF Beyersdorf, Andreas J. Thornhill, K. Lee Winstead, Edward L. Ziemba, Luke D. Blake, Donald R. Timko, Michael T. Anderson, Bruce E. TI Power-dependent speciation of volatile organic compounds in aircraft exhaust SO ATMOSPHERIC ENVIRONMENT LA English DT Article DE Aircraft emissions; Turbine engine; Hydrocarbon emission indices; Oxygenated hydrocarbons ID HYDROCARBON EMISSION INDEXES; IN-FLIGHT MEASUREMENT; COMMERCIAL AIRCRAFT; CHEMICAL-COMPOSITION; TURBINE-ENGINES; AIRPORT; AIR; REACTIVITY; CO AB As part of the third NASA Aircraft Particle Emissions Experiment (APEX-3, November 2005), whole air samples were collected to determine the emission rates of volatile organic compounds (VOCs) from aircraft equipped with three different gas-turbine engines (an Allison Engine 3007-A1E, a Pratt-Whitney 4158, and a Rolls-Royce RB211-535E4B). Samples were collected 1 m behind the engine exhaust plane of the engines while they were operated at powers ranging from idle up to 30% of maximum rated thrust. Exhaust emission indices (mass emitted per kilogram of fuel used) for CO and non-methane hydrocarbons (NMHCs) were calculated based on enhancements over background relative to CO2. Emissions of all NMHCs were greatest at low power with values decreasing by an order of magnitude with increasing power. Previous studies have shown that scaling idle hydrocarbon emissions to formaldehyde or ethene (which are typically emitted at a ratio of 1-to-1 at idle) reduces variability amongst engine types. NMHC emissions were found to scale at low power, with alkenes contributing over 50% of measured NMHCs. However, as the power increases hydrocarbon emissions no longer scale to ethene, as the aromatics become the dominant species emitted. This may be due in part to a shift in combustion processes from thermal cracking (producing predominantly alkenes) to production of new molecules (producing proportionally more aromatics) as power increases. The formation of these aromatics is an intermediate step in the production of soot, which also increases with increasing power. The increase in aromatics relative to alkenes additionally results in a decrease in the hydroxyl radical reactivity and ozone formation potential of aircraft exhaust. Samples collected 30 m downwind of the engine were also analyzed for NMHCs and carbonyl compounds (acetone, 2-butanone and C-1-C-9 aldehydes). Formaldehyde was the predominant carbonyl emitted; however, the ratio of ethene-to-formaldehyde varied between the aircraft, possibly due to the sampling of transient emissions such as engine start-up and power changes. A large portion of the measured emissions (27-42% by mass) in the plume samples was made up of hazardous air pollutants (HAPs) with oxygenated compounds being most significant. Published by Elsevier Ltd. C1 [Beyersdorf, Andreas J.; Thornhill, K. Lee; Winstead, Edward L.; Ziemba, Luke D.; Anderson, Bruce E.] NASA Langley Res Ctr, Hampton, VA 23662 USA. [Thornhill, K. Lee; Winstead, Edward L.] Sci Syst & Applicat Inc, Hampton, VA 23666 USA. [Blake, Donald R.] Univ Calif Irvine, Irvine, CA 92697 USA. [Timko, Michael T.] Aerodyne Res Inc, Billerica, MA 01821 USA. RP Beyersdorf, AJ (reprint author), NASA Langley Res Ctr, Hampton, VA 23662 USA. EM andreas.j.beyersdorf@nasa.gov RI Beyersdorf, Andreas/N-1247-2013 FU NASA Aeronautics Research Mission Directorate FX This research was supported by the NASA Aeronautics Research Mission Directorate. Assistance during the field campaign was provided by Charles Hudgins (NASA Langley) and was facilitated by Southwest Airlines, Continental Airlines, Fed Ex and NASA Glenn Research Center. Analytical assistance was provided by Changlie Wey at NASA Glenn (CO2 data) and Gloria Liu, Brent Love and Simone Meinardi at UC Irvine. John Kinsey at the EPA provided the APEX report and helpful suggestions during manuscript preparation. Assistance with manuscript preparation was also provided by Scott Herndon at Aerodyne Research, Inc. and Angela Baker at the Max Planck Institute for Chemistry. NR 33 TC 5 Z9 5 U1 2 U2 25 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1352-2310 J9 ATMOS ENVIRON JI Atmos. Environ. PD DEC PY 2012 VL 61 BP 275 EP 282 DI 10.1016/j.atmosenv.2012.07.027 PG 8 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA 038QA UT WOS:000311188000029 ER PT J AU Jackson, WA Davila, AF Estrada, N Lyons, WB Coates, JD Priscu, JC AF Jackson, W. Andrew Davila, Alfonso F. Estrada, Nubia Lyons, W. Berry Coates, John D. Priscu, John C. TI Perchlorate and chlorate biogeochemistry in ice-covered lakes of the McMurdo Dry Valleys, Antarctica SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Article ID TAYLOR VALLEY; NATURAL PERCHLORATE; OXIDIZING BACTERIA; NITROUS-OXIDE; FRYXELL BASIN; SALINE LAKES; EVOLUTION; BONNEY; GEOCHEMISTRY; REDUCTION AB We measured chlorate (ClO3-) and perchlorate (ClO4-) concentrations in ice covered lakes of the McMurdo Dry Valleys (MDVs) of Antarctica, to evaluate their role in the ecology and geochemical evolution of the lakes. ClO3- and ClO4- are present throughout the MDV Lakes, streams, and other surface water bodies. ClO3- and ClO4- originate in the atmosphere and are transported to the lakes by surface inflow of glacier melt that has been differentially impacted by interaction with soils and aeolian matter. Concentrations of ClO3- and ClO4- in the lakes and between lakes vary based on both total evaporative concentration, as well as biological activity within each lake. All of the lakes except the East lobe of Lake Bonney support biological reduction of ClO3- and ClO4- either in the anoxic bottom waters or sediment. The younger less saline lakes (Miers and Hoare), have surface ClO3- and ClO4- concentrations, and ratios of ClO3-/Cl- and ClO4-/Cl-, similar to source streams, while Lake Fryxell has concentrations similar to input streams but much lower ClO3-/Cl- and ClO4-/Cl- ratios, reflecting the influence of a large Cl- source in bottom sediments. ClO3- and ClO4- in Lake Bonney are the highest of all the lakes reflecting the lake's greater age and higher concentration of Cl-. ClO4- appears to be stable in the East Lobe and its concentration is highly correlated with Cl- concentration suggesting that some ClO4- at depth is a remnant of the initial seawater that formed Lake Bonney. ClO3- and ClO4- concentrations provide a simple and sensitive means to evaluate microbial activity in these lakes due to their relatively low concentrations and lack of biological sources, unlike NO3-, NO2-, and SO42-. (C) 2012 Elsevier Ltd. All rights reserved. C1 [Jackson, W. Andrew; Estrada, Nubia] Texas Tech Univ, Dept Civil & Environm Engn, Lubbock, TX 79409 USA. [Davila, Alfonso F.] NASA, Ames Res Ctr, Moffett Field, CA 95136 USA. [Davila, Alfonso F.] SETI Inst, Mountain View, CA 94043 USA. [Lyons, W. Berry] Ohio State Univ, Byrd Polar Res Ctr, Columbus, OH 43210 USA. [Coates, John D.] Univ Calif Berkeley, Dept Plant & Microbial Biol, Berkeley, CA 94720 USA. [Priscu, John C.] Montana State Univ, Dept Land Resources & Environm Sci, Bozeman, MT 59717 USA. RP Jackson, WA (reprint author), Texas Tech Univ, Dept Civil & Environm Engn, Lubbock, TX 79409 USA. EM andrew.jackson@ttu.edu RI Jackson, William/B-8999-2009; Davila, Alfonso/A-2198-2013 OI Davila, Alfonso/0000-0002-0977-9909 FU Strategic Environmental Research and Development Program (SERDP) [ER-1435]; NSF OPP [0432595, 0631494]; Energy Biosciences Institute, UC Berkeley, CA; NASA Exobiology program [NNX12AD61G] FX This work was supported by the Strategic Environmental Research and Development Program (SERDP Project ER-1435) and by NSF OPP grants 0432595 and 0631494. We are grateful to the McMurdo Long Term Ecological Research Program for providing water samples from the MDV and would especially like to acknowledge Kathy Welch and Amy Chiuchiolo for their time and efforts. Work in the lab of J.D.C was supported by the Energy Biosciences Institute, UC Berkeley, CA. A. F. D is supported by the NASA Exobiology program (Grant Number NNX12AD61G). NR 44 TC 10 Z9 10 U1 1 U2 40 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD DEC 1 PY 2012 VL 98 BP 19 EP 30 DI 10.1016/j.gca.2012.09.014 PG 12 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 038ZB UT WOS:000311211500002 ER PT J AU Cheng, SW Garlan, D AF Cheng, Shang-Wen Garlan, David TI Stitch: A language for architecture-based self-adaptation SO JOURNAL OF SYSTEMS AND SOFTWARE LA English DT Article DE Rainbow; Self-adaptation; Strategy; Tactic; Uncertainty; Utility ID SYSTEMS AB Requirements for high availability in computing systems today demand that systems be self-adaptive to maintain expected qualities-of-service in the presence of system faults, variable environmental conditions, and changing user requirements. Autonomic computing tackles the challenge of automating tasks that humans would otherwise have to perform to achieve this goal. However, existing approaches to autonomic computing lack the ability to capture routine human repair tasks in a way that takes into account the business context humans use in selecting an appropriate form of adaptation, while dealing with timing delays and uncertainties in outcome of repair actions. In this article, we present Stitch, a language for representing repair strategies within the context of an architecture-based self-adaptation framework. Stitch supports the explicit representation of repair decision trees together with the ability to express business objectives, allowing a self-adaptive system to select a strategy that has optimal utility in a given context, even in the presence of potential timing delays and outcome uncertainty. (C) 2012 Elsevier Inc. All rights reserved. C1 [Cheng, Shang-Wen; Garlan, David] Carnegie Mellon Univ, Sch Comp Sci, Pittsburgh, PA 15213 USA. RP Cheng, SW (reprint author), NASA, Jet Prop Lab, Washington, DC 20546 USA. EM chengs@cmu.edu; garlan@cs.cmu.edu FU DARPA [N66001-99-2-8918, F30602-00-2-0616]; US Army Research Office (ARO) [DAAD19-01-1-0485, DAAD19-02-1-0389]; NASA High Dependability Computing Program [NCC-2-1298]; Foundation for Science and Technology [CMU-PT/ELE/0030/2009]; FEDER via the "Programa Operacional Factores de Competitividade" of QREN; COMPETE [FCOMP-01-0124-FEDER-012983]; IBM Eclipse Innovation Grant FX This research was sponsored by DARPA under grants N66001-99-2-8918 and F30602-00-2-0616, the US Army Research Office (ARO) under grants DAAD19-01-1-0485 and DAAD19-02-1-0389 ("Perpetually Available and Secure Information Systems") to Carnegie Mellon University's CyLab, the NASA High Dependability Computing Program under cooperative agreement NCC-2-1298, a 2004 IBM Eclipse Innovation Grant, the Foundation for Science and Technology via project CMU-PT/ELE/0030/2009, and by FEDER via the "Programa Operacional Factores de Competitividade" of QREN with COMPETE reference: FCOMP-01-0124-FEDER-012983. The views and conclusions contained in this document are those of the author and should not be interpreted as representing the official policies, either expressed or implied, of DARPA, the ARO, the U.S. Government, NASA, IBM, or any other entity. NR 62 TC 29 Z9 29 U1 1 U2 4 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0164-1212 EI 1873-1228 J9 J SYST SOFTWARE JI J. Syst. Softw. PD DEC PY 2012 VL 85 IS 12 SI SI BP 2860 EP 2875 DI 10.1016/j.jss.2012.02.060 PG 16 WC Computer Science, Software Engineering; Computer Science, Theory & Methods SC Computer Science GA 031VB UT WOS:000310669500014 ER PT J AU Bates, SD Bailes, M Barsdell, BR Bhat, NDR Burgay, M Burke-Spolaor, S Champion, DJ Coster, P D'Amico, N Jameson, A Johnston, S Keith, MJ Kramer, M Levin, L Lyne, A Milia, S Ng, C Nietner, C Possenti, A Stappers, B Thornton, D van Straten, W AF Bates, S. D. Bailes, M. Barsdell, B. R. Bhat, N. D. R. Burgay, M. Burke-Spolaor, S. Champion, D. J. Coster, P. D'Amico, N. Jameson, A. Johnston, S. Keith, M. J. Kramer, M. Levin, L. Lyne, A. Milia, S. Ng, C. Nietner, C. Possenti, A. Stappers, B. Thornton, D. van Straten, W. TI The High Time Resolution Universe Pulsar Survey - VI. An artificial neural network and timing of 75 pulsars SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE methods: data analysis; stars: neutron; pulsars: general ID MILLISECOND PULSARS; RADIO TELESCOPE; NEUTRON-STARS; DISCOVERY; SEARCHES; CANDIDATES; CATALOG; LOFAR; ARRAY AB We present 75 pulsars discovered in the mid-latitude portion of the High Time Resolution Universe survey, 54 of which have full timing solutions. All the pulsars have spin periods greater than 100 ms, and none of those with timing solutions is in binaries. Two display particularly interesting behaviour; PSR J1054-5944 is found to be an intermittent pulsar, and PSR J1809-0119 has glitched twice since its discovery. In the second half of the paper we discuss the development and application of an artificial neural network in the data-processing pipeline for the survey. We discuss the tests that were used to generate scores and find that our neural network was able to reject over 99 per cent of the candidates produced in the data processing, and able to blindly detect 85 per cent of pulsars. We suggest that improvements to the accuracy should be possible if further care is taken when training an artificial neural network; for example, ensuring that a representative sample of the pulsar population is used during the training process, or the use of different artificial neural networks for the detection of different types of pulsars. C1 [Bates, S. D.; Nietner, C.; Stappers, B.; Thornton, D.] Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England. [Bates, S. D.; Kramer, M.; Lyne, A.] W Virginia Univ, Dept Phys, Morgantown, WV 26506 USA. [Bailes, M.; Barsdell, B. R.; Bhat, N. D. R.; Coster, P.; Jameson, A.; Levin, L.; van Straten, W.] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia. [Burgay, M.; D'Amico, N.; Milia, S.; Possenti, A.] INAF Osservatorio Astron Cagliari, I-09012 Caopterra, Italy. [Burke-Spolaor, S.] NASA Jet Prop Lab, Pasadena, CA 91106 USA. [Champion, D. J.; Kramer, M.; Ng, C.] MPI Radioastron, D-53121 Bonn, Germany. [Johnston, S.; Keith, M. J.; Levin, L.] CSIRO, Australia Telescope Natl Facil, Epping, NSW 1710, Australia. [Milia, S.] Univ Cagliari, Dipartimento Fis, I-09042 Monserrato, CA, Italy. RP Bates, SD (reprint author), Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England. EM sam.d.bates@gmail.com RI Bhat, Ramesh/B-7396-2013; OI Champion, David/0000-0003-1361-7723; Burgay, Marta/0000-0002-8265-4344; van Straten, Willem/0000-0003-2519-7375 FU Commonwealth of Australia FX The authors thank Cristobal Espinoza for his helpful comments and expertise on pulsar glitches. The Parkes Observatory is part of the Australia Telescope which is funded by the Commonwealth of Australia for operation as a National Facility managed by CSIRO. We thank the anonymous referee for their helpful comment. NR 48 TC 11 Z9 12 U1 0 U2 0 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD DEC PY 2012 VL 427 IS 2 BP 1052 EP 1065 DI 10.1111/j.1365-2966.2012.22042.x PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 041PK UT WOS:000311413500016 ER PT J AU Carvalho, P Rocha, G Hobson, MP Lasenby, A AF Carvalho, Pedro Rocha, Graca Hobson, M. P. Lasenby, A. TI PowellSnakes II: a fast Bayesian approach to discrete object detection in multi-frequency astronomical data sets SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE methods: data analysis; cosmology: observations ID EXTRAGALACTIC RADIO-SOURCES; SUNYAEV-ZELDOVICH CLUSTERS; MICROWAVE BACKGROUND MAPS; POINT SOURCES; PLANCK; CATALOG; FILTERS; PREDICTIONS; EXTRACTION; EFFICIENT AB PowellSnakes (PwS) is a Bayesian algorithm for detecting compact objects embedded in a diffuse background, and was selected and successfully employed by the Planck consortium in the production of its first public deliverable: the Early Release Compact Source Catalogue (ERCSC). We present the critical foundations and main directions of further development of PwS, which extend it in terms of formal correctness and the optimal use of all the available information in a consistent unified framework, where no distinction is made between point sources (unresolved objects), Sunyaev-Zel'dovich (SZ) clusters, single-or multi-channel detection. An emphasis is placed on the necessity of a multi-frequency, multi-model detection algorithm in order to achieve optimality. C1 [Carvalho, Pedro; Hobson, M. P.; Lasenby, A.] Univ Cambridge, Cavendish Lab, Astrophys Grp, Cambridge CB3 0HE, England. [Rocha, Graca] CALTECH, Pasadena, CA 91125 USA. [Rocha, Graca] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Lasenby, A.] Kavli Inst Cosmol Cambridge, Cambridge CB3 0HA, England. RP Carvalho, P (reprint author), Univ Cambridge, Cavendish Lab, Astrophys Grp, JJ Thomson Ave, Cambridge CB3 0HE, England. EM carvalho@mrao.cam.ac.uk; graca@caltech.edu; mph@mrao.cam.ac.uk; a.n.lasenby@mrao.cam.ac.uk FU Fundacao para a Ciencia e Tecnologia (FCT) [SFRH/BD/42366/2007]; NASA Science Mission Directorate via the US Planck Project FX PC thanks all his colleagues at the Astrophysics Group of Cavendish laboratory and the KICC, and his fellow members of the Planck consortium for their help in completing PwS. In particular, special thanks go to Paulo Marques (code porting), Farhan Feroz and Philip Graff for their insightful contributions and discussions. PC is supported by a Portuguese fellowship (ref: SFRH/BD/42366/2007) from the Fundacao para a Ciencia e Tecnologia (FCT).; GR gratefully acknowledges support by the NASA Science Mission Directorate via the US Planck Project. The research described in this paper was partially carried out at the Jet propulsion Laboratory, California Institute of Technology, under a contract with NASA. NR 50 TC 19 Z9 19 U1 0 U2 5 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD DEC PY 2012 VL 427 IS 2 BP 1384 EP 1400 DI 10.1111/j.1365-2966.2012.22033.x PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 041PK UT WOS:000311413500041 ER PT J AU Camera, S Santos, MG Bacon, DJ Jarvis, MJ McAlpine, K Norris, RP Raccanelli, A Rottgering, H AF Camera, Stefano Santos, Mario G. Bacon, David J. Jarvis, Matt J. McAlpine, Kim Norris, Ray P. Raccanelli, Alvise Roettgering, Huub TI Impact of redshift information on cosmological applications with next-generation radio surveys SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE cosmological parameters; cosmology: observations; large-scale structure of universe; radio continuum: galaxies ID ESTIMATING PHOTOMETRIC REDSHIFTS; ARTIFICIAL NEURAL-NETWORKS; VLA SKY SURVEY; DEEP FIELD; TELESCOPE; GALAXIES; COSMOS; SIMULATION; UNIVERSE; CATALOG AB In this paper, we explore how the forthcoming generation of large-scale radio continuum surveys, with the inclusion of some degree of redshift information, can constrain cosmological parameters. By cross-matching these radio surveys with shallow optical to near-infrared surveys, we can essentially separate the source distribution into a low- and a high-redshift sample, thus providing a constraint on the evolution of cosmological parameters such as those related to dark energy. We examine two radio surveys, the Evolutionary Map of the Universe (EMU) and the Westerbork Observations of the Deep APERTIF Northern sky (WODAN). A crucial advantage is their combined potential to provide a deep, full-sky survey. The surveys used for the cross-identifications are SkyMapper and Sloan Digital Sky Survey, for the southern and northern skies, respectively. We concentrate on the galaxy clustering angular power spectrum as our benchmark observable, and find that the possibility of including such low-redshift information yields major improvements in the determination of cosmological parameters. With this approach, and provided a good knowledge of the galaxy bias evolution, we are able to put strict constraints on the dark energy parameters, i.e. w0 = -0.9 +/- 0.041 and wa = -0.24 +/- 0.13, with Type Ia supernovae and cosmic microwave background priors (with a one-parameter bias in this case); this corresponds to a Figure of Merit (FoM) >600, which is twice better than what is obtained by using only the cross-identified sources and greater than four time better than the case without any redshift information at all. C1 [Camera, Stefano; Santos, Mario G.] Univ Tecn Lisboa, CENTRA, Inst Super Tecn, P-1049001 Lisbon, Portugal. [Bacon, David J.] Univ Portsmouth, Inst Cosmol & Gravitat, Portsmouth P01 3FX, Hants, England. [Jarvis, Matt J.] Univ Hertfordshire, STRI, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England. [Jarvis, Matt J.] Univ Western Cape, Dept Phys, ZA-7535 Bellville, South Africa. [McAlpine, Kim] Rhodes Univ, Dept Phys & Elect, ZA-6139 Grahamstown, South Africa. [Norris, Ray P.] Australia Telescope Natl Facil, CSIRO Astron & Space Sci, Epping, NSW 1710, Australia. [Raccanelli, Alvise] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Raccanelli, Alvise] CALTECH, Pasadena, CA 91125 USA. [Roettgering, Huub] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. RP Camera, S (reprint author), Univ Tecn Lisboa, CENTRA, Inst Super Tecn, Av Rovisco Pais 1, P-1049001 Lisbon, Portugal. EM stefano.camera@ist.utl.pt; mgrsantos@ist.utl.pt; david.bacon@port.ac.uk RI Camera, Stefano/N-2456-2013; Norris, Ray/A-1316-2008; Santos, Mario/F-2484-2011; OI Camera, Stefano/0000-0003-3399-3574; Norris, Ray/0000-0002-4597-1906; Santos, Mario/0000-0003-3892-3073; Raccanelli, Alvise/0000-0001-6726-0438 FU FCT-Portugal [PTDC/FIS/100170/2008, SFRH/BPD/80274/2011] FX We thank the referee for a careful reading of our manuscript and very insightful comments. SC and MGS acknowledge support from FCT-Portugal under grant PTDC/FIS/100170/2008. SC's work is funded by FCT-Portugal under Post-Doctoral Grant SFRH/BPD/80274/2011. Part of the research described in this paper was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. The authors would also like to thank Gong-Bo Zhao for his friendly and gratuitous contribution. NR 50 TC 10 Z9 10 U1 0 U2 5 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD DEC PY 2012 VL 427 IS 3 BP 2079 EP 2088 DI 10.1111/j.1365-2966.2012.22073.x PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 041PX UT WOS:000311414800018 ER PT J AU Lakew, B Aslam, S Brasunas, J Cao, N Costen, N La, A Nguyen, L Stevenson, T Waczynski, A AF Lakew, B. Aslam, S. Brasunas, J. Cao, N. Costen, N. La, A. Nguyen, L. Stevenson, T. Waczynski, A. TI MgB2 thin-film bolometer for applications in far-infrared instruments on future planetary missions SO PHYSICA C-SUPERCONDUCTIVITY AND ITS APPLICATIONS LA English DT Article DE MgB2 thin-film; Bolometer; Thermal detector; D*; NEP ID HIGH-T-C; SILICON-NITRIDE FILMS; SUPERCONDUCTING BOLOMETER; MEMBRANE; PERFORMANCE; FABRICATION; RADIATION; TRANSPORT; SAPPHIRE; DETECTOR AB A SiN membrane based MgB2 thin-film bolometer, with a non-optimized absorber, has been fabricated that shows an electrical noise equivalent power of 2.56 x 10 (13) W/root Hz operating at 30 Hz and a responsivity of 702 kV/W. It is predicted that with the inclusion of a gold black absorber that an optical specific detectivity of 8.3 x 10(10) cm/root Hz/W at an operational frequency of 10 Hz, can be realized for integration into future planetary exploration instrumentation where high sensitivity is required in the 17-250 mu m spectral wavelength range. (C) 2012 Published by Elsevier B.V. C1 [Lakew, B.; Aslam, S.; Brasunas, J.] NASA, Goddard Space Flight Ctr, Planetary Syst Lab, Greenbelt, MD 20771 USA. [Cao, N.; Costen, N.; La, A.; Nguyen, L.; Stevenson, T.; Waczynski, A.] NASA, Goddard Space Flight Ctr, Detector Syst Branch, Greenbelt, MD 20771 USA. [Cao, N.; Costen, N.] MEI Technol Inc, Houston, TX 77058 USA. RP Aslam, S (reprint author), NASA, Goddard Space Flight Ctr, Planetary Syst Lab, Code 693, Greenbelt, MD 20771 USA. EM shahid.aslam-1@nasa.gov RI brasunas, john/I-2798-2013; Aslam, Shahid/D-1099-2012 FU NASA GSFC Internal Research and Development (IRAD) program; NASA HQ Planetary Instrument Definition and Development (PIDD) program FX The authors wish to thank Dr. Simon Bandler (University of Maryland) for enlightening conversations regarding ac impedance measurements on superconducting films. The NASA GSFC Internal Research and Development (IRAD) and the NASA HQ Planetary Instrument Definition and Development (PIDD) programs supported this work. NR 42 TC 0 Z9 0 U1 1 U2 16 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0921-4534 J9 PHYSICA C JI Physica C PD DEC PY 2012 VL 483 BP 119 EP 126 DI 10.1016/j.physc.2012.08.007 PG 8 WC Physics, Applied SC Physics GA 040UC UT WOS:000311348800026 ER PT J AU Aliu, E Archambault, S Arlen, T Aune, T Beilicke, M Benbow, W Bouvier, A Buckley, JH Bugaev, V Byrum, K Cesarini, A Ciupik, L Collins-Hughes, E Connolly, MP Cui, W Dickherber, R Duke, C Dumm, J Falcone, A Federici, S Feng, Q Finley, JP Finnegan, G Fortson, L Furniss, A Galante, N Gall, D Gillanders, GH Godambe, S Griffin, S Grube, J Gyuk, G Hanna, D Holder, J Huan, H Hughes, G Humensky, TB Kaaret, P Karlsson, N Khassen, Y Kieda, D Krawczynski, H Krennrich, F Lang, MJ LeBohec, S Lee, K Lyutikov, M Madhavan, AS Maier, G Majumdar, P McArthur, S McCann, A Moriarty, P Mukherjee, R Nelson, T de Bhroithe, AO Ong, RA Orr, M Otte, AN Park, N Perkins, JS Pohl, M Prokoph, H Quinn, J Ragan, K Reyes, LC Reynolds, PT Roache, E Saxon, DB Schroedter, M Sembroski, GH Senturk, GD Smith, AW Staszak, D Telezhinsky, I Tesic, G Theiling, M Thibadeau, S Tsurusaki, K Varlotta, A Vincent, S Vivier, M Wagner, RG Wakely, SP Weekes, TC Weinstein, A Welsing, R Williams, DA Zitzer, B Kondratiev, V AF Aliu, E. Archambault, S. Arlen, T. Aune, T. Beilicke, M. Benbow, W. Bouvier, A. Buckley, J. H. Bugaev, V. Byrum, K. Cesarini, A. Ciupik, L. Collins-Hughes, E. Connolly, M. P. Cui, W. Dickherber, R. Duke, C. Dumm, J. Falcone, A. Federici, S. Feng, Q. Finley, J. P. Finnegan, G. Fortson, L. Furniss, A. Galante, N. Gall, D. Gillanders, G. H. Godambe, S. Griffin, S. Grube, J. Gyuk, G. Hanna, D. Holder, J. Huan, H. Hughes, G. Humensky, T. B. Kaaret, P. Karlsson, N. Khassen, Y. Kieda, D. Krawczynski, H. Krennrich, F. Lang, M. J. LeBohec, S. Lee, K. Lyutikov, M. Madhavan, A. S. Maier, G. Majumdar, P. McArthur, S. McCann, A. Moriarty, P. Mukherjee, R. Nelson, T. de Bhroithe, A. O'Faolain Ong, R. A. Orr, M. Otte, A. N. Park, N. Perkins, J. S. Pohl, M. Prokoph, H. Quinn, J. Ragan, K. Reyes, L. C. Reynolds, P. T. Roache, E. Saxon, D. B. Schroedter, M. Sembroski, G. H. Sentuerk, G. D. Smith, A. W. Staszak, D. Telezhinsky, I. Tesic, G. Theiling, M. Thibadeau, S. Tsurusaki, K. Varlotta, A. Vincent, S. Vivier, M. Wagner, R. G. Wakely, S. P. Weekes, T. C. Weinstein, A. Welsing, R. Williams, D. A. Zitzer, B. Kondratiev, V. TI SEARCH FOR A CORRELATION BETWEEN VERY-HIGH-ENERGY GAMMA RAYS AND GIANT RADIO PULSES IN THE CRAB PULSAR SO ASTROPHYSICAL JOURNAL LA English DT Article DE rays: stars; pulsars: individual: B0531+21 ID EMISSION; TELESCOPES; UNIVERSE; PHOTONS; GEMINGA; NEBULA; RANGE; MODEL AB We present the results of a joint observational campaign between the Green Bank radio telescope and the VERITAS gamma-ray telescope, which searched for a correlation between the emission of very-high-energy (VHE) gamma rays (E-gamma > 150 GeV) and giant radio pulses (GRPs) from the Crab pulsar at 8.9 GHz. A total of 15,366 GRPs were recorded during 11.6 hr of simultaneous observations, which were made across four nights in 2008 December and in 2009 November and December. We searched for an enhancement of the pulsed gamma-ray emission within time windows placed around the arrival time of the GRP events. In total, eight different time windows with durations ranging from 0.033 ms to 72 s were positioned at three different locations relative to the GRP to search for enhanced gamma-ray emission which lagged, led, or was concurrent with, the GRP event. Furthermore, we performed separate searches on main pulse GRPs and interpulse GRPs and on the most energetic GRPs in our data sample. No significant enhancement of pulsed VHE emission was found in any of the preformed searches. We set upper limits of 5-10 times the average VHE flux of the Crab pulsar on the flux simultaneous with interpulse GRPs on single-rotation-period timescales. On similar to 8 s timescales around interpulse GRPs, we set an upper limit of 2-3 times the average VHE flux. Within the framework of recent models for pulsed VHE emission from the Crab pulsar, the expected VHE-GRP emission correlations are below the derived limits. C1 [Aliu, E.; Mukherjee, R.] Columbia Univ, Barnard Coll, Dept Phys & Astron, New York, NY 10027 USA. [Archambault, S.; Griffin, S.; Hanna, D.; Ragan, K.; Staszak, D.; Tesic, G.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Arlen, T.; Majumdar, P.; Ong, R. A.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Aune, T.; Bouvier, A.; Furniss, A.; Williams, D. A.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA. [Aune, T.; Bouvier, A.; Furniss, A.; Williams, D. A.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA. [Beilicke, M.; Buckley, J. H.; Bugaev, V.; Dickherber, R.; Krawczynski, H.; Lee, K.; McArthur, S.; Thibadeau, S.] Washington Univ, Dept Phys, St Louis, MO 63130 USA. [Benbow, W.; Galante, N.; Roache, E.; Schroedter, M.; Weekes, T. C.] Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA. [Byrum, K.; Wagner, R. G.; Zitzer, B.] Argonne Natl Lab, Argonne, IL 60439 USA. [Cesarini, A.; Connolly, M. P.; Gillanders, G. H.; Lang, M. J.] Natl Univ Ireland Galway, Sch Phys, Galway, Ireland. [Ciupik, L.; Grube, J.; Gyuk, G.] Adler Planetarium & Astron Museum, Dept Astron, Chicago, IL 60605 USA. [Collins-Hughes, E.; Khassen, Y.; de Bhroithe, A. O'Faolain; Quinn, J.] Univ Coll Dublin, Sch Phys, Dublin 4, Ireland. [Cui, W.; Feng, Q.; Finley, J. P.; Lyutikov, M.; Sembroski, G. H.; Theiling, M.; Varlotta, A.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. [Duke, C.] Grinnell Coll, Dept Phys, Grinnell, IA 50112 USA. [Dumm, J.; Fortson, L.; Karlsson, N.; Nelson, T.] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA. [Falcone, A.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA. [Federici, S.; Hughes, G.; Maier, G.; Pohl, M.; Prokoph, H.; Telezhinsky, I.; Vincent, S.; Welsing, R.] DESY, D-15738 Zeuthen, Germany. [Federici, S.; Pohl, M.; Telezhinsky, I.] Univ Potsdam, Inst Phys & Astron, D-14476 Potsdam, Germany. [Finnegan, G.; Godambe, S.; Kieda, D.; LeBohec, S.; Smith, A. W.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA. [Gall, D.; Kaaret, P.; Tsurusaki, K.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. [Holder, J.; Saxon, D. B.; Vivier, M.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA. [Holder, J.; Saxon, D. B.; Vivier, M.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA. [Huan, H.; Park, N.; Wakely, S. P.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [Humensky, T. B.; Sentuerk, G. D.] Columbia Univ, Dept Phys, New York, NY 10027 USA. [Krennrich, F.; Madhavan, A. S.; Orr, M.; Weinstein, A.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. [McCann, A.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Moriarty, P.] Galway Mayo Inst Technol, Dept Life & Phys Sci, Galway, Ireland. [Otte, A. N.] Georgia Inst Technol, Sch Phys, Atlanta, GA 30332 USA. [Otte, A. N.] Georgia Inst Technol, Ctr Relativist Astrophys, Atlanta, GA 30332 USA. [Perkins, J. S.] CRESST, Greenbelt, MD 20771 USA. [Perkins, J. S.] NASA, GSFC, Astroparticle Phys Lab, Greenbelt, MD 20771 USA. [Perkins, J. S.] Univ Maryland, Baltimore, MD 21250 USA. [Reyes, L. C.] Calif Polytech State Univ San Luis Obispo, Dept Phys, San Luis Obispo, CA 94307 USA. [Reynolds, P. T.] Cork Inst Technol, Dept Appl Phys & Instrumentat, Cork, Ireland. [Kondratiev, V.] Netherlands Inst Radio Astron, ASTRON, NL-7990 AA Dwingeloo, Netherlands. [Kondratiev, V.] PN Lebedev Phys Inst, Ctr Astro Space, Moscow 117997, Russia. RP Aliu, E (reprint author), Columbia Univ, Barnard Coll, Dept Phys & Astron, New York, NY 10027 USA. EM mccann@kicp.uchicago.edu; nepomuk.otte@gmail.com; schroedter@veritas.sao.arizona.edu RI Khassen, Yerbol/I-3806-2015; Kondratiev, Vladislav/N-1105-2015; OI Cesarini, Andrea/0000-0002-8611-8610; Khassen, Yerbol/0000-0002-7296-3100; Lang, Mark/0000-0003-4641-4201; Kondratiev, Vladislav/0000-0001-8864-7471; Cui, Wei/0000-0002-6324-5772 FU U.S. Department of Energy Office of Science; U.S. National Science Foundation; Smithsonian Institution; NSERC in Canada; Science Foundation Ireland [SFI 10/RFP/AST2748]; STFC in the UK FX This research is supported by grants from the U.S. Department of Energy Office of Science, the U.S. National Science Foundation, and the Smithsonian Institution, by NSERC in Canada, by Science Foundation Ireland (SFI 10/RFP/AST2748), and by STFC in the UK. We acknowledge the excellent work of the technical support staff at the Fred Lawrence Whipple Observatory and at the collaborating institutions in the construction and operation of the instrument. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. NR 35 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 J9 ASTROPHYS J JI Astrophys. J. PD DEC 1 PY 2012 VL 760 IS 2 AR 136 DI 10.1088/0004-637X/760/2/136 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 039BE UT WOS:000311217000040 ER PT J AU Araujo, D Bischoff, C Brizius, A Buder, I Chinone, Y Cleary, K Dumoulin, RN Kusaka, A Monsalve, R Kaess, S Newburgh, LB Reeves, R Wehus, IK Zwart, JTL Bronfman, L Bustos, R Church, SE Dickinson, C Eriksen, HK Gaier, T Gundersen, JO Hasegawa, M Hazumi, M Huffenberger, KM Ishidoshiro, K Jones, ME Kangaslahti, P Kapner, DJ Kubik, D Lawrence, CR Limon, M McMahon, JJ Miller, AD Nagai, M Nguyen, H Nixon, G Pearson, TJ Piccirillo, L Radford, SJE Readhead, ACS Richards, JL Samtleben, D Seiffert, M Shepherd, MC Smith, KM Staggs, ST Tajima, O Thompson, KL Vanderlinde, K Williamson, R AF Araujo, D. Bischoff, C. Brizius, A. Buder, I. Chinone, Y. Cleary, K. Dumoulin, R. N. Kusaka, A. Monsalve, R. Kaess, S. Newburgh, L. B. Reeves, R. Wehus, I. K. Zwart, J. T. L. Bronfman, L. Bustos, R. Church, S. E. Dickinson, C. Eriksen, H. K. Gaier, T. Gundersen, J. O. Hasegawa, M. Hazumi, M. Huffenberger, K. M. Ishidoshiro, K. Jones, M. E. Kangaslahti, P. Kapner, D. J. Kubik, D. Lawrence, C. R. Limon, M. McMahon, J. J. Miller, A. D. Nagai, M. Nguyen, H. Nixon, G. Pearson, T. J. Piccirillo, L. Radford, S. J. E. Readhead, A. C. S. Richards, J. L. Samtleben, D. Seiffert, M. Shepherd, M. C. Smith, K. M. Staggs, S. T. Tajima, O. Thompson, K. L. Vanderlinde, K. Williamson, R. CA QUIET Collaboration TI SECOND SEASON QUIET OBSERVATIONS: MEASUREMENTS OF THE COSMIC MICROWAVE BACKGROUND POLARIZATION POWER SPECTRUM AT 95 GHz SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmic background radiation; cosmology: observations; gravitational waves; inflation; polarization ID CMB POLARIZATION; COSMOLOGICAL PARAMETERS; GRAVITY-WAVES; PROBE; CONSTRAINTS; TEMPERATURE; TELESCOPE; IMAGER AB The Q/U Imaging ExperimenT (QUIET) has observed the cosmic microwave background (CMB) at 43 and 95 GHz. The 43 GHz results have been published in a previous paper, and here we report the measurement of CMB polarization power spectra using the 95 GHz data. This data set comprises 5337 hr of observations recorded by an array of 84 polarized coherent receivers with a total array sensitivity of 87 mu K root s. Four low-foreground fields were observed, covering a total of similar to 1000 deg(2) with an effective angular resolution of 12.'8, allowing for constraints on primordial gravitational waves and high signal-to-noise measurements of the E-modes across three acoustic peaks. The data reduction was performed using two independent analysis pipelines, one based on a pseudo-C-l (PCL) cross-correlation approach, and the other on a maximum-likelihood (ML) approach. All data selection criteria and filters were modified until a predefined set of null tests had been satisfied before inspecting any non-null power spectrum. The results derived by the two pipelines are in good agreement. We characterize the EE, EB, and BB power spectra between l = 25 and 975 and find that the EE spectrum is consistent with Lambda CDM, while the BB power spectrum is consistent with zero. Based on these measurements, we constrain the tensor-to-scalar ratio to r = 1.1(-0.8)(+0.9) (r < 2.8 at 95% C. L.) as derived by the ML pipeline, and r = 1.2(-0.8)(+0.9) (r < 2.7 at 95% C. L.) as derived by the PCL pipeline. In one of the fields, we find a correlation with the dust component of the Planck Sky Model, though the corresponding excess power is small compared to statistical errors. Finally, we derive limits on all known systematic errors, and demonstrate that these correspond to a tensor-to-scalar ratio smaller than r = 0.01, the lowest level yet reported in the literature. C1 [Araujo, D.; Dumoulin, R. N.; Newburgh, L. B.; Zwart, J. T. L.; Limon, M.; Miller, A. D.; Williamson, R.] Columbia Univ, Dept Phys, New York, NY 10027 USA. [Dumoulin, R. N.; Newburgh, L. B.; Zwart, J. T. L.; Limon, M.; Miller, A. D.; Williamson, R.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Bischoff, C.; Brizius, A.; Buder, I.; Kusaka, A.; Kapner, D. J.; Smith, K. M.; Tajima, O.; Vanderlinde, K.; Williamson, R.] Univ Chicago, Dept Phys, Kavli Inst Cosmol Phys, Enrico Fermi Inst, Chicago, IL 60637 USA. [Bischoff, C.; Buder, I.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Brizius, A.; Samtleben, D.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Chinone, Y.; Hasegawa, M.; Hazumi, M.; Ishidoshiro, K.; Nagai, M.; Tajima, O.] High Energy Accelerator Res Org KEK, Tsukuba, Ibaraki 3050801, Japan. [Chinone, Y.] Tohoku Univ, Grad Sch Sci, Astron Inst, Aoba Ku, Sendai, Miyagi 9808578, Japan. [Cleary, K.; Reeves, R.; Pearson, T. J.; Radford, S. J. E.; Readhead, A. C. S.; Richards, J. L.; Shepherd, M. C.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Kusaka, A.; Newburgh, L. B.; Nixon, G.; Smith, K. M.; Staggs, S. T.] Princeton Univ, Joseph Henry Labs Phys, Princeton, NJ 08544 USA. [Monsalve, R.; Bustos, R.; Gundersen, J. O.; Huffenberger, K. M.] Univ Miami, Dept Phys, Coral Gables, FL 33146 USA. [Monsalve, R.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [Kaess, S.; Eriksen, H. K.] Univ Oslo, Inst Theoret Astrophys, NO-0315 Oslo, Norway. [Wehus, I. K.; Jones, M. E.] Univ Oxford, Dept Astrophys, Oxford OX1 3RH, England. [Wehus, I. K.] Univ Oslo, Dept Phys, NO-0316 Oslo, Norway. [Zwart, J. T. L.] Univ Western Cape, Dept Phys, ZA-7535 Bellville, South Africa. [Bronfman, L.; Bustos, R.] Univ Chile, Dept Astron, Santiago, Chile. [Bustos, R.] Univ Concepcion, Dept Astron, Concepcion, Chile. [Church, S. E.; Thompson, K. L.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA. [Church, S. E.; Thompson, K. L.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA. [Dickinson, C.; Piccirillo, L.] Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England. [Eriksen, H. K.] Univ Oslo, Ctr Math Applicat, NO-0316 Oslo, Norway. [Gaier, T.; Kangaslahti, P.; Lawrence, C. R.; Seiffert, M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Kapner, D. J.] Micro Encoder Inc, Kirkland, WA 98034 USA. [Kubik, D.; Nguyen, H.] Fermilab Natl Accelerator Lab, Batavia, IL 60510 USA. [McMahon, J. J.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA. [Nixon, G.] Tradeworx Inc, Red Bank, NJ 07701 USA. [Samtleben, D.] Nikhef, Amsterdam, Netherlands. [Vanderlinde, K.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. RP Araujo, D (reprint author), Columbia Univ, Dept Phys, 538 W 120th St, New York, NY 10027 USA. EM ibuder@uchicago.edu RI Bronfman, Leonardo/H-9544-2013; Reeves, Rodrigo/H-2812-2014; Williamson, Ross/H-1734-2015; Pearson, Timothy/N-2376-2015; OI Huffenberger, Kevin/0000-0001-7109-0099; Bronfman, Leonardo/0000-0002-9574-8454; Bischoff, Colin/0000-0001-9185-6514; Reeves, Rodrigo/0000-0001-5704-271X; Williamson, Ross/0000-0002-6945-2975; Pearson, Timothy/0000-0001-5213-6231; Limon, Michele/0000-0002-5900-2698; radford, simon/0000-0001-9113-1660; Zwart, Jonathan/0000-0002-4967-946X FU NSF [AST-0506648, PHY-0355328, AST-0448909, PHY-0551142, PHY-0855887, AST-1010016]; KAKENHI [20244041, 20740158, 21111002]; PRODEX [C90284]; KIPAC Enterprise grant; Strategic Alliance for the Implementation of New Technologies (SAINT); Fermilab; Kavli Institute for Cosmological Physics; University of Chicago; Office of Science of the U.S. Department of Energy [DE-AC02-05CH11231]; JPL RTD program; STFC; ERC IRG grant under FP7; CONICYT [Basal PFB-06]; ALMA-Conicyt [31070015]; Sloan foundation; ERC FX Support for the QUIET instrument and operation comes through the NSF cooperative agreement AST-0506648. Support was also provided by NSF awards PHY-0355328, AST-0448909, PHY-0551142, PHY-0855887, and AST-1010016; KAKENHI 20244041, 20740158, and 21111002; PRODEX C90284; a KIPAC Enterprise grant; and by the Strategic Alliance for the Implementation of New Technologies (SAINT).; Some work was performed on the Joint Fermilab-KICP Supercomputing Cluster, supported by grants from Fermilab, the Kavli Institute for Cosmological Physics, and the University of Chicago. Some work was performed on the Titan Cluster, owned and maintained by the University of Oslo and NOTUR (the Norwegian High Performance Computing Consortium), and on the Central Computing System, owned and operated by the Computing Research Center at KEK. This research used resources of the National Energy Research Scientific Computing Center, which is supported by the Office of Science of the U.S. Department of Energy under Contract No. DE-AC02-05CH11231. Portions of this work were performed at the Jet Propulsion Laboratory (JPL) and California Institute of Technology, operating under a contract with the National Aeronautics and Space Administration. The Q-band modules were developed using funding from the JPL R&TD program. We acknowledge the Northrop Grumman Corporation for collaboration in the development and fabrication of HEMT-based cryogenic temperature-compatible MMICs. We acknowledge the use of the Planck Sky Model, developed by the Component Separation Working Group (WG2) of the Planck Collaboration. Some of the results in this paper have been derived using the HEALPix (Gorski et al. 2005) software and analysis package.; C.D. acknowledges an STFC Advanced Fellowship and an ERC IRG grant under FP7. R.B. acknowledges support from CONICYT project Basal PFB-06 and ALMA-Conicyt 31070015. A.D.M. acknowledges a Sloan foundation fellowship. H.K.E. acknowledges an ERC Starting Grant under FP7. NR 60 TC 37 Z9 37 U1 1 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 1 PY 2012 VL 760 IS 2 AR 145 DI 10.1088/0004-637X/760/2/145 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 039BE UT WOS:000311217000049 ER PT J AU Bampasidis, G Coustenis, A Achterberg, RK Vinatier, S Lavvas, P Nixon, CA Jennings, DE Teanby, NA Flasar, FM Carlson, RC Moussas, X Preka-Papadema, P Romani, PN Guandique, EA Stamogiorgos, S AF Bampasidis, Georgios Coustenis, A. Achterberg, R. K. Vinatier, S. Lavvas, P. Nixon, C. A. Jennings, D. E. Teanby, N. A. Flasar, F. M. Carlson, R. C. Moussas, X. Preka-Papadema, P. Romani, P. N. Guandique, E. A. Stamogiorgos, S. TI THERMAL AND CHEMICAL STRUCTURE VARIATIONS IN TITAN'S STRATOSPHERE DURING THE CASSINI MISSION SO ASTROPHYSICAL JOURNAL LA English DT Article DE infrared: planetary systems; planets and satellites: atmospheres; planets and satellites: composition; planets and satellites: individual (Titan); radiation mechanisms: thermal; radiative transfer ID COMPOSITE INFRARED SPECTROMETER; ATMOSPHERIC TEMPERATURES; SPECTROSCOPIC DATABASE; LATITUDINAL VARIATIONS; ISOTOPIC-RATIOS; HYDROCARBONS; SPECTRA; CIRS; HC3N; PROFILES AB We have developed a line-by-line Atmospheric Radiative Transfer for Titan code that includes the most recent laboratory spectroscopic data and haze descriptions relative to Titan's stratosphere. We use this code to model Cassini Composite Infrared Spectrometer data taken during the numerous Titan flybys from 2006 to 2012 at surface-intercepting geometry in the 600-1500 cm(-1) range for latitudes from 50 degrees S to 50 degrees N. We report variations in temperature and chemical composition in the stratosphere during the Cassini mission, before and after the Northern Spring Equinox (NSE). We find indication for a weakening of the temperature gradient with warming of the stratosphere and cooling of the lower mesosphere. In addition, we infer precise concentrations for the trace gases and their main isotopologues and find that the chemical composition in Titan's stratosphere varies significantly with latitude during the 6 years investigated here, with increased mixing ratios toward the northern latitudes. In particular, we monitor and quantify the amplitude of a maximum enhancement of several gases observed at northern latitudes up to 50 degrees N around mid-2009, at the time of the NSE. We find that this rise is followed by a rapid decrease in chemical inventory in 2010 probably due to a weakening north polar vortex with reduced lateral mixing across the vortex boundary. C1 [Bampasidis, Georgios; Coustenis, A.; Vinatier, S.] Univ Paris Diderot, UPMC Univ Paris 06, CNRS, LESIA,Observ Paris, F-92195 Meudon, France. [Bampasidis, Georgios; Moussas, X.; Preka-Papadema, P.; Stamogiorgos, S.] Univ Athens, Fac Phys, GR-15783 Athens, Greece. [Achterberg, R. K.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Lavvas, P.] Univ Reims, GSMA, F-51687 Reims 2, France. [Nixon, C. A.; Jennings, D. E.; Flasar, F. M.; Carlson, R. C.; Romani, P. N.; Guandique, E. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Teanby, N. A.] Univ Bristol, Sch Earth Sci, Bristol BS8 1RJ, Avon, England. [Carlson, R. C.] Catholic Univ Amer, IACS, Washington, DC 20064 USA. [Guandique, E. A.] Adnet Syst Inc, Rockville, MD USA. RP Bampasidis, G (reprint author), Univ Paris Diderot, UPMC Univ Paris 06, CNRS, LESIA,Observ Paris, 5 Pl Jules Janssen, F-92195 Meudon, France. EM gbabasid@phys.uoa.gr RI Nixon, Conor/A-8531-2009; Flasar, F Michael/C-8509-2012; OI Nixon, Conor/0000-0001-9540-9121; Teanby, Nicholas/0000-0003-3108-5775 FU CNES Cassini program FX We thank Nicolas Gorius, Marcia Segura, and Florence Henry for help with the data acquisition and processing during this project. We also acknowledge support from the CNES Cassini program. NR 33 TC 11 Z9 11 U1 0 U2 16 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 1 PY 2012 VL 760 IS 2 AR 144 DI 10.1088/0004-637X/760/2/144 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 039BE UT WOS:000311217000048 ER PT J AU Cheung, E Faber, SM Koo, DC Dutton, AA Simard, L McGrath, EJ Huang, JS Bell, EF Dekel, A Fang, JJ Salim, S Barro, G Bundy, K Coil, AL Cooper, MC Conselice, CJ Davis, M Dominguez, A Kassin, SA Kocevski, DD Koekemoer, AM Lin, LW Lotz, JM Newman, JA Phillips, AC Rosario, DJ Weiner, BJ Willmer, CNA AF Cheung, Edmond Faber, S. M. Koo, David C. Dutton, Aaron A. Simard, Luc McGrath, Elizabeth J. Huang, J. -S. Bell, Eric F. Dekel, Avishai Fang, Jerome J. Salim, Samir Barro, G. Bundy, K. Coil, A. L. Cooper, Michael C. Conselice, C. J. Davis, M. Dominguez, A. Kassin, Susan A. Kocevski, Dale D. Koekemoer, Anton M. Lin, Lihwai Lotz, Jennifer M. Newman, J. A. Phillips, Andrew C. Rosario, D. J. Weiner, Benjamin J. Willmer, C. N. A. TI THE DEPENDENCE OF QUENCHING UPON THE INNER STRUCTURE OF GALAXIES AT 0.5 <= z < 0.8 IN THE DEEP2/AEGIS SURVEY SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: bulges; galaxies: evolution; galaxies: formation; galaxies: fundamental parameters; galaxies: structure ID DEEP GROTH STRIP; ACTIVE GALACTIC NUCLEI; STAR-FORMING GALAXIES; DIGITAL SKY SURVEY; COLOR-MAGNITUDE DIAGRAM; HIGH-REDSHIFT GALAXIES; CENTRAL BLACK-HOLES; ARECIBO SDSS SURVEY; MASSIVE GALAXIES; STELLAR MASS AB The shutdown of star formation in galaxies is generally termed "quenching." Quenching may occur through a variety of processes, e.g., active galactic nucleus (AGN) feedback, stellar feedback, or the shock heating of gas in the dark matter halo. However, which mechanism(s) is, in fact, responsible for quenching is still in question. This paper addresses quenching by searching for traces of possible quenching processes through their effects on galaxy structural parameters such as stellar mass (M-*), M-*/r(e), surface stellar mass density (similar to M-*/r(e)(2)), and Sersic index (n). We analyze the rest-frame U - B color correlations versus these structural parameters using a sample of galaxies in the redshift range 0.5 <= z < 0.8 from the DEEP2/AEGIS survey. In addition to global radii, stellar masses, and Sersic parameters, we also use "bulge" and "disk" photometric measurements from GIM2D fits to HST/ACS V and I images. We assess the tightness of the color relationships by measuring their "overlap regions," defined as the area in color-parameter space in which red and blue galaxies overlap; the parameter that minimizes these overlap regions is considered to be the most effective color discriminator. We find that Sersic index (n) has the smallest overlap region among all tested parameters and resembles a step function with a threshold value of n = 2.3. There exists, however, a significant population of outliers with blue colors yet high n values that seem to contradict this behavior; they make up approximate to 40% of n > 2.3 galaxies. We hypothesize that their Sersic values may be distorted by bursts of star formation, AGNs, and/or poor fits, leading us to consider central surface stellar mass density, Sigma*(1) (kpc), as an alternative to Sersic index. Not only does Sigma*(1) (kpc) correct the outliers, but it also forms a tight relationship with color, suggesting that the innermost structure of galaxies is most physically linked with quenching. Furthermore, at z similar to 0.65, the majority of the blue cloud galaxies cannot simply fade onto the red sequence since their GIM2D bulge masses are only half as large on average as the bulge masses of similar red sequence galaxies, thus demonstrating that stellar mass must absolutely increase at the centers of galaxies as they quench. We discuss a two-stage model for quenching in which galaxy star formation rates are controlled by their dark halos while they are still in the blue cloud and a second quenching process sets in later, associated with the central stellar mass buildup. The mass buildup is naturally explained by any non-axisymmetric features in the potential, such as those induced by mergers and/or disk instabilities. However, the identity of the second quenching agent is still unknown. We have placed our data catalog online. C1 [Cheung, Edmond; Faber, S. M.; Koo, David C.; McGrath, Elizabeth J.; Fang, Jerome J.; Barro, G.; Kocevski, Dale D.; Phillips, Andrew C.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Faber, S. M.; Koo, David C.] Univ Calif Santa Cruz, UCO Lick Observ, Santa Cruz, CA 95064 USA. [Dutton, Aaron A.] Univ Victoria, Dept Phys & Astron, Victoria, BC V8P 5C2, Canada. [Simard, Luc] Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada. [Huang, J. -S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bell, Eric F.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Dekel, Avishai] Hebrew Univ Jerusalem, Racah Inst Phys, IL-91904 Jerusalem, Israel. [Salim, Samir; Lotz, Jennifer M.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Bundy, K.] Univ Tokyo, Kavli Inst Phys & Math Universe, Kashiwa, Chiba 2778582, Japan. [Coil, A. L.] Univ Calif San Diego, Ctr Astrophys & Space Sci, Dept Phys, San Diego, CA 92093 USA. [Cooper, Michael C.] Univ Calif Irvine, Ctr Galaxy Evolut, Dept Phys & Astron, Irvine, CA 92697 USA. [Conselice, C. J.] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England. [Davis, M.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Dominguez, A.] Univ Calif Riverside, Dept Phys & Astron, Riverside, CA 92521 USA. [Kassin, Susan A.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Koekemoer, Anton M.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Lin, Lihwai] Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan. [Newman, J. A.] Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA. [Rosario, D. J.] Max Planck Inst Extraterr Phys, D-85741 Garching, Germany. [Weiner, Benjamin J.; Willmer, C. N. A.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. RP Cheung, E (reprint author), Univ Calif Santa Cruz, Dept Astron & Astrophys, 1156 High St, Santa Cruz, CA 95064 USA. EM ec2250@gmail.com RI Conselice, Christopher/B-4348-2013; OI Conselice, Christopher/0000-0003-1949-7638; Cheung, Edmond/0000-0001-8546-1428; Koekemoer, Anton/0000-0002-6610-2048; Bell, Eric/0000-0002-5564-9873 FU National Science Foundation [AST 95-29098, 00-711098, 05-07483, 08-08133, AST 00-71048, 05-07428, 08-07630]; NASA [HST-AR-01947] FX The DEEP2 survey was initiated under the auspices of the NSF Center for Particle Astrophysics. Major grant support was provided by National Science Foundation grants AST 95-29098, 00-711098, 05-07483, and 08-08133 to UCSC and AST 00-71048, 05-07428, and 08-07630 to UCB. The DEEP2 survey has been made possible through the dedicated efforts of the DEIMOS instrument team at UC Santa Cruz and support of the staff at Keck Observatory. The HST ACS mosaic in EGS was constructed by Anton Koekemoer and Jennifer Lotz and was funded by grant HST-AR-01947 from NASA. Finally, we recognize and acknowledge the highly significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community; it has been a privilege to be given the opportunity to conduct observations from this mountain. NR 179 TC 67 Z9 68 U1 0 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 1 PY 2012 VL 760 IS 2 AR 131 DI 10.1088/0004-637X/760/2/131 PG 25 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 039BE UT WOS:000311217000035 ER PT J AU Dong, RB Hashimoto, J Rafikov, R Zhu, ZH Whitney, B Kudo, T Muto, T Brandt, T McClure, MK Wisniewski, J Abe, L Brandner, W Carson, J Egner, S Feldt, M Goto, M Grady, C Guyon, O Hayano, Y Hayashi, M Hayashi, S Henning, T Hodapp, KW Ishii, M Iye, M Janson, M Kandori, R Knapp, GR Kusakabe, N Kuzuhara, M Kwon, J Matsuo, T McElwain, M Miyama, S Morino, JI Moro-Martin, A Nishimura, T Pyo, TS Serabyn, E Suto, H Suzuki, R Takami, M Takato, N Terada, H Thalmann, C Tomono, D Turner, E Watanabe, M Yamada, T Takami, H Usuda, T Tamura, M AF Dong, Ruobing Hashimoto, Jun Rafikov, Roman Zhu, Zhaohuan Whitney, Barbara Kudo, Tomoyuki Muto, Takayuki Brandt, Timothy McClure, Melissa K. Wisniewski, John Abe, L. Brandner, W. Carson, J. Egner, S. Feldt, M. Goto, M. Grady, C. Guyon, O. Hayano, Y. Hayashi, M. Hayashi, S. Henning, T. Hodapp, K. W. Ishii, M. Iye, M. Janson, M. Kandori, R. Knapp, G. R. Kusakabe, N. Kuzuhara, M. Kwon, J. Matsuo, T. McElwain, M. Miyama, S. Morino, J. -I. Moro-Martin, A. Nishimura, T. Pyo, T. -S. Serabyn, E. Suto, H. Suzuki, R. Takami, M. Takato, N. Terada, H. Thalmann, C. Tomono, D. Turner, E. Watanabe, M. Yamada, T. Takami, H. Usuda, T. Tamura, M. TI THE STRUCTURE OF PRE-TRANSITIONAL PROTOPLANETARY DISKS. I. RADIATIVE TRANSFER MODELING OF THE DISK plus CAVITY IN THE PDS 70 SYSTEM SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; protoplanetary disks; radiative transfer; stars: individual (PDS 70); stars: pre-main sequence ID T-TAURI STARS; SPECTRAL ENERGY-DISTRIBUTIONS; YOUNG STELLAR OBJECTS; MAIN-SEQUENCE STARS; HERBIG AE/BE STARS; TRANSITIONAL DISKS; GG TAURI; PROTOSTELLAR ENVELOPES; IMAGING POLARIMETRY; SIZE DISTRIBUTION AB Through detailed radiative transfer modeling, we present a disk+cavity model to simultaneously explain both the spectral energy distribution (SED) and SubaruH-band polarized light imaging for the pre-transitional protoplanetary disk PDS 70. In particular, we are able to match not only the radial dependence but also the absolute scale of the surface brightness of the scattered light. Our disk model has a cavity 65AU in radius, which is heavily depleted of sub-micron-sized dust grains, and a small residual inner disk that produces a weak but still optically thick near-IR excess in the SED. To explain the contrast of the cavity's edge in the Subaru image, a factor of similar to 1000 depletion for the sub-micron-sized dust inside the cavity is required. The total dust mass of the disk may be on the order of 10(-4) M-circle dot, only weakly constrained due to the lack of long-wavelength observations and the uncertainties in the dust model. The scale height of the sub-micron-sized dust is similar to 6AU at the cavity edge, and the cavity wall is optically thick in the vertical direction at H-band. PDS 70 is not a member of the class of (pre-) transitional disks identified by Dong et al., whose members only show evidence of the cavity in the millimeter-size dust but not the sub-micron-sized dust in resolved images. The two classes of (pre-) transitional disks may form through different mechanisms, or they may simply be at different evolution stages in the disk-clearing process. C1 [Dong, Ruobing; Rafikov, Roman; Zhu, Zhaohuan; Brandt, Timothy; Janson, M.; Knapp, G. R.; Turner, E.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Hashimoto, Jun; Iye, M.; Kandori, R.; Kusakabe, N.; Kuzuhara, M.; Kwon, J.; Morino, J. -I.; Suto, H.; Tamura, M.] Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan. [Whitney, Barbara] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. [Kudo, Tomoyuki; Egner, S.; Guyon, O.; Hayano, Y.; Hayashi, S.; Ishii, M.; Nishimura, T.; Pyo, T. -S.; Takato, N.; Terada, H.; Tomono, D.; Takami, H.; Usuda, T.] Subaru Telescope, Hilo, HI 96720 USA. [Muto, Takayuki] Kogakuin Univ, Div Liberal Arts, Shinjuku Ku, Tokyo 1638677, Japan. [McClure, Melissa K.] Univ Michigan, Dept Astron, Ann Arbor, MI 48105 USA. [Wisniewski, John] Univ Oklahoma, HL Dodge Dept Phys & Astron, Norman, OK 73019 USA. [Abe, L.] Univ Nice Sophia Antipolis, CNRS, UMR7293, Lab Lagrange,Observ Cote Azur, F-06300 Nice, France. [Brandner, W.; Feldt, M.; Goto, M.; Henning, T.; Thalmann, C.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Carson, J.] Coll Charleston, Dept Phys & Astron, Charleston, SC 29424 USA. [Grady, C.; McElwain, M.] Goddard Space Flight Ctr, ExoPlanets & Stellar Astrophys Lab, Greenbelt, MD 20771 USA. [Grady, C.] Eureka Sci, Oakland, CA 96002 USA. [Hayashi, M.] Univ Tokyo, Dept Astron, Bunkyo Ku, Tokyo 1130033, Japan. [Hodapp, K. W.] Univ Hawaii, Inst Astron, Hilo, HI 96720 USA. [Matsuo, T.] Kyoto Univ, Dept Astron, Sakyo Ku, Kyoto 6068502, Japan. [Miyama, S.] Hiroshima Univ, Off President, Higashihiroshima 7398511, Japan. [Moro-Martin, A.] CAB INTA CSIC, Dept Astrofis, E-28850 Madrid, Spain. CALTECH, Jet Prop Lab, Pasadena, CA USA. [Suzuki, R.] TMT Observ Corp, Pasadena, CA 91105 USA. [Takami, M.] Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan. [Turner, E.] Univ Tokyo, Kavli Inst Phys & Math Univ, Kashiwa, Chiba 2278568, Japan. [Watanabe, M.] Hokkaido Univ, Dept Cosmosci, Sapporo, Hokkaido 0600810, Japan. [Yamada, T.] Tohoku Univ, Astron Inst, Sendai, Miyagi 9808578, Japan. RP Dong, RB (reprint author), Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. EM rdong@astro.princeton.edu RI Turner, Edwin/A-4295-2011; MIYAMA, Shoken/A-3598-2015 FU NSF [AST 0908269, AST 1008440, AST 1009314, AST 1009203]; NASA [NNX22SK53G]; Sloan Fellowship; World Premier International Research Center Initiative (WPI Initiative), MEXT, Japan FX R.D. thanks Edwin Bergin, Tilman Birnstiel, Brendan Bowler, Nuria Calvet, L. Ilsedore Cleeves, Bruce Draine, Catherine Espaillat, Lee Hartmann, Shu-ichiro Inutsuka, Andrea Isella, James Owen, Thomas P. Robitaille, Fredrik Windmark, and Yanqin Wu for useful discussions. The authors are also grateful to the anonymous referee who helped improve the manuscript. This work is partially supported by NSF grant AST 0908269 (R.D., Z.Z., and R.R.), AST 1008440 (C.G.), AST 1009314 (J.W.), AST 1009203 (J.C.), NASA grant NNX22SK53G (L.H.), Sloan Fellowship (R.R.), and World Premier International Research Center Initiative (WPI Initiative), MEXT, Japan (E.L.T.). 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 61 TC 25 Z9 25 U1 1 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 1 PY 2012 VL 760 IS 2 AR 111 DI 10.1088/0004-637X/760/2/111 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 039BE UT WOS:000311217000015 ER PT J AU Frisch, PC Andersson, BG Berdyugin, A Piirola, V DeMajistre, R Funsten, HO Magalhaes, AM Seriacopi, DB McComas, DJ Schwadron, NA Slavin, JD Wiktorowicz, SJ AF Frisch, P. C. Andersson, B-G Berdyugin, A. Piirola, V. DeMajistre, R. Funsten, H. O. Magalhaes, A. M. Seriacopi, D. B. McComas, D. J. Schwadron, N. A. Slavin, J. D. Wiktorowicz, S. J. TI THE INTERSTELLAR MAGNETIC FIELD CLOSE TO THE SUN. II. SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: bubbles; ISM: magnetic fields; local interstellar matter; methods: data analysis; polarization; Sun: heliosphere ID BOUNDARY-EXPLORER RIBBON; NEUTRAL ATOM MAPS; LOCAL BUBBLE; IBEX RIBBON; LINEAR-POLARIZATION; OUTER HELIOSHEATH; GRAIN ALIGNMENT; COSMIC-RAYS; OPTICAL POLARIZATION; STELLAR POLARIZATION AB The magnetic field in the local interstellar medium (ISM) provides a key indicator of the galactic environment of the Sun and influences the shape of the heliosphere. We have studied the interstellar magnetic field (ISMF) in the solar vicinity using polarized starlight for stars within 40 pc of the Sun and 90 degrees of the heliosphere nose. In Frisch et al. (Paper I), we developed a method for determining the local ISMF direction by finding the best match to a group of interstellar polarization position angles obtained toward nearby stars, based on the assumption that the polarization is parallel to the ISMF. In this paper, we extend the analysis by utilizing weighted fits to the position angles and by including new observations acquired for this study. We find that the local ISMF is pointed toward the galactic coordinates l, b = 47 degrees +/- 20 degrees, 25 degrees +/- 20 degrees. This direction is close to the direction of the ISMF that shapes the heliosphere, l, b = 33 degrees +/- 4 degrees, 55 degrees +/- 4 degrees, as traced by the center of the "Ribbon" of energetic neutral atoms discovered by the Interstellar Boundary Explorer (IBEX) mission. Both the magnetic field direction and the kinematics of the local ISM are consistent with a scenario where the local ISM is a fragment of the Loop I superbubble. A nearby ordered component of the local ISMF has been identified in the region l approximate to 0 degrees -> 80 degrees and b approximate to 0 degrees -> 30 degrees, where PlanetPol data show a distance-dependent increase of polarization strength. The ordered component extends to within 8 pc of the Sun and implies a weak curvature in the nearby ISMF of +/- 0 degrees.25 pc(-1). This conclusion is conditioned on the small sample of stars available for defining this rotation. Variations from the ordered component suggest a turbulent component of +/- 23 degrees. The ordered component and standard relations between polarization, color excess, and H-o column density predict a reasonable increase of N(H) with distance in the local ISM. The similarity of the ISMF directions traced by the polarizations, the IBEX Ribbon, and pulsars inside the Local Bubble in the third galactic quadrant suggest that the ISMF is relatively uniform over spatial scales of 8-200 pc and is more similar to interarm than spiral-arm magnetic fields. The ISMF direction from the polarization data is also consistent with small-scale spatial asymmetries detected in GeV-TeV cosmic rays with a galactic origin. The peculiar geometrical relation found earlier between the cosmic microwave background dipole moment, the heliosphere nose, and the ISMF direction is supported by this study. The interstellar radiation field at +/- 975 angstrom does not appear to play a role in grain alignment for the low-density ISM studied here. C1 [Frisch, P. C.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Andersson, B-G] NASA, Ames Res Ctr, Univ Space Res Assoc, SOFIA Sci Ctr, Moffett Field, CA 94035 USA. [Berdyugin, A.; Piirola, V.] Univ Turku, Finnish Ctr Astron ESO, SF-20500 Turku, Finland. [DeMajistre, R.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA. [Funsten, H. O.] Los Alamos Natl Lab, Los Alamos, NM USA. [Magalhaes, A. M.; Seriacopi, D. B.] Univ Sao Paulo, Inst Astron Geofis & Ciencias Atmosfer, BR-05508 Sao Paulo, Brazil. [McComas, D. J.] SW Res Inst, San Antonio, TX USA. [Schwadron, N. A.] Univ New Hampshire, Ctr Space Sci, Durham, NH 03824 USA. [Slavin, J. D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Wiktorowicz, S. J.] Univ Calif Santa Cruz, Dept Astron, Santa Cruz, CA 95064 USA. [McComas, D. J.] Univ Texas San Antonio, San Antonio, TX USA. RP Frisch, PC (reprint author), Univ Chicago, Dept Astron & Astrophys, 5640 S Ellis Ave, Chicago, IL 60637 USA. RI 7, INCT/H-6207-2013; Astrofisica, Inct/H-9455-2013; Magalhaes, Antonio Mario/K-9532-2013; Funsten, Herbert/A-5702-2015; OI Funsten, Herbert/0000-0002-6817-1039; Andersson, B-G/0000-0001-6717-0686 FU IBEX mission; NASA's Explorer Program; NASA [NNX09AH50G, NNX08AJ33G] FX This work was supported by the IBEX mission as part of NASA's Explorer Program, and by NASA grants NNX09AH50G and NNX08AJ33G to the University of Chicago. We are grateful for observations made with the Nordic Optical Telescope, operated on the island of La Palma jointly by Denmark, Finland, Iceland, Norway, and Sweden, in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias. We are also grateful for observations made with telescopes at the Observatorio do Pico dos Dias of the Laboratorio Nacional de Astrofisica of Brazil. NR 112 TC 30 Z9 30 U1 0 U2 8 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 1 PY 2012 VL 760 IS 2 AR 106 DI 10.1088/0004-637X/760/2/106 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 039BE UT WOS:000311217000010 ER PT J AU Linares, M Connaughton, V Jenke, P van der Horst, AJ Camero-Arranz, A Kouveliotou, C Chakrabarty, D Beklen, E Bhat, PN Briggs, MS Finger, M Paciesas, WS Preece, R von Kienlin, A Wilson-Hodge, CA AF Linares, M. Connaughton, V. Jenke, P. van der Horst, A. J. Camero-Arranz, A. Kouveliotou, C. Chakrabarty, D. Beklen, E. Bhat, P. N. Briggs, M. S. Finger, M. Paciesas, W. S. Preece, R. von Kienlin, A. Wilson-Hodge, C. A. TI THE FERMI-GBM X-RAY BURST MONITOR: THERMONUCLEAR BURSTS FROM 4U 0614+09 SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; binaries: close; stars: neutron; X-rays: binaries; X-rays: bursts; X-rays: individual (4U 0614+09) ID NEUTRON-STAR; BINARY 4U-0614+091; TIMING-EXPLORER; 2S-0918-549 AB Thermonuclear bursts from slowly accreting neutron stars (NSs) have proven difficult to detect, yet they are potential probes of the thermal properties of the NS interior. During the first year of a systematic all-sky search for X-ray bursts using the Gamma-ray Burst Monitor aboard the Fermi Gamma-ray Space Telescope we have detected 15 thermonuclear bursts from the NS low-mass X-ray binary 4U 0614+09 when it was accreting at nearly 1% of the Eddington limit. We measured an average burst recurrence time of 12 +/- 3 days (68% confidence interval) between 2010 March and 2011 March, classified all bursts as normal duration bursts and placed a lower limit on the recurrence time of long/intermediate bursts of 62 days (95% confidence level). We discuss how observations of thermonuclear bursts in the hard X-ray band compare to pointed soft X-ray observations and quantify such bandpass effects on measurements of burst radiated energy and duration. We put our results for 4U 0614+09 in the context of other bursters and briefly discuss the constraints on ignition models. Interestingly, we find that the burst energies in 4U 0614+09 are on average between those of normal duration bursts and those measured in long/intermediate bursts. Such a continuous distribution in burst energy provides a new observational link between normal and long/intermediate bursts. We suggest that the apparent bimodal distribution that defined normal and long/intermediate duration bursts during the last decade could be due to an observational bias toward detecting only the longest and most energetic bursts from slowly accreting NSs. C1 [Linares, M.; Chakrabarty, D.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Connaughton, V.; Bhat, P. N.; Briggs, M. S.; Preece, R.] Univ Alabama, CSPAR, Huntsville, AL 35899 USA. [Jenke, P.; Kouveliotou, C.; Wilson-Hodge, C. A.] NASA, Space Sci Off, VP62, Marshall Space Flight Ctr, Huntsville, AL 35812 USA. [van der Horst, A. J.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1090 GE Amsterdam, Netherlands. [Camero-Arranz, A.; Finger, M.; Paciesas, W. S.] Univ Space Res Assoc, Huntsville, AL 35805 USA. [Beklen, E.] Suleyman Demirel Univ, Dept Phys, TR-32260 Isparta, Turkey. [von Kienlin, A.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Connaughton, V.; Bhat, P. N.; Briggs, M. S.; Preece, R.] Univ Alabama, Dept Phys, Huntsville, AL 35899 USA. RP Linares, M (reprint author), MIT, Kavli Inst Astrophys & Space Res, 77 Massachusetts Ave, Cambridge, MA 02139 USA. OI Preece, Robert/0000-0003-1626-7335 FU NWO; NASA [NNX11AO19G] FX Quick-look ASM results were provided by the RXTE/ASM team. Swift/BAT transient monitor results were provided by the Swift/BAT team. This paper utilizes preliminary analysis results from the Multi-INstrument Burst ARchive (MINBAR; http://users.monash.edu.au/similar to dgallow/minbar). Data from previous bursts were kindly provided by E. Kuulkers. We thank A. Cumming for providing ignition models and for stimulating discussions and V. Chaplin for clarifications on detector geometries during some of the bursts. We also thank the anonymous referee for constructive comments. M.L. is grateful to the International Space Science Institute in Bern, where part of this work was completed, and acknowledges support from the NWO Rubicon fellowship. This research was partly funded by NASA's Fermi Guest Investigation program under grant NNX11AO19G. NR 41 TC 3 Z9 3 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 DEC 1 PY 2012 VL 760 IS 2 AR 133 DI 10.1088/0004-637X/760/2/133 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 039BE UT WOS:000311217000037 ER PT J AU Mallery, RP Mobasher, B Capak, P Kakazu, Y Masters, D Ilbert, O Hemmati, S Scarlata, C Salvato, M McCracken, H LeFevre, O Scoville, N AF Mallery, Ryan P. Mobasher, Bahram Capak, Peter Kakazu, Yuko Masters, Dan Ilbert, Olivier Hemmati, Shoubaneh Scarlata, Claudia Salvato, Mara McCracken, Henry LeFevre, Olivier Scoville, Nick TI Ly alpha EMISSION FROM HIGH-REDSHIFT SOURCES IN COSMOS SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: evolution; galaxies: high-redshift; galaxies: ISM ID LYMAN-BREAK GALAXIES; STAR-FORMING GALAXIES; SUBARU DEEP FIELD; SIMILAR-TO 3; LUMINOSITY FUNCTION; STELLAR POPULATIONS; EMITTING GALAXIES; SPECTROSCOPIC CONFIRMATION; PHOTOMETRIC PROPERTIES; BUILDING-BLOCKS AB We investigate spectroscopically measured Ly alpha equivalent widths (EWs) and escape fractions of 244 sources of which 95 are Lyman break galaxies (LBGs) and 106 Lyman alpha emitters (LAEs) at z similar to 4.2, z similar to 4.8, and z similar to 5.6 selected from intermediate and narrowband observations. The sources were selected from the Cosmic Evolution Survey and observed with the DEIMOS spectrograph. We find that the distribution of EWs shows no evolution with redshift for both the LBG selected sources and the intermediate/narrowband LAEs. We also find that the Ly alpha escape fraction of intermediate/narrowband LAEs is on average higher and has a larger variation than the escape fraction of LBG selected sources. The escape fraction does not show a dependence with redshift. Similar to what has been found for LAEs at low redshifts, the sources with the highest extinctions show the lowest escape fractions. The range of escape fractions increases with decreasing extinction. This is evidence that the dust extinction is the most important factor affecting the escape of Ly alpha photons, but at low extinctions other factors, such as the H I covering fraction and gas kinematics, can be just as effective at inhibiting the escape of Ly alpha photons. C1 [Mallery, Ryan P.; Mobasher, Bahram; Hemmati, Shoubaneh] Univ Calif Riverside, Dept Phys & Astron, Riverside, CA 92507 USA. [Capak, Peter; Kakazu, Yuko; Masters, Dan; Scoville, Nick] CALTECH, NASA, JPL Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Ilbert, Olivier; LeFevre, Olivier] Univ Aix Marseille 1, CNRS, Lab Astrophys Marseille, F-13388 Marseille 13, France. [Scarlata, Claudia] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA. [Salvato, Mara] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [McCracken, Henry] Univ Paris 06, CNRS UMR7095, Inst Astrophys Paris, F-75014 Paris, France. RP Mallery, RP (reprint author), Univ Calif Riverside, Dept Phys & Astron, 900 Univ Ave, Riverside, CA 92507 USA. FU W. M. Keck Foundation FX Based in part on data 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 and was made possible by the generous financial support of the W. M. Keck Foundation. NR 78 TC 21 Z9 21 U1 0 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 1 PY 2012 VL 760 IS 2 AR 128 DI 10.1088/0004-637X/760/2/128 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 039BE UT WOS:000311217000032 ER PT J AU Muinonen, K Mishchenko, MI Dlugach, JM Zubko, E Penttila, A Videen, G AF Muinonen, K. Mishchenko, M. I. Dlugach, J. M. Zubko, E. Penttila, A. Videen, G. TI COHERENT BACKSCATTERING VERIFIED NUMERICALLY FOR A FINITE VOLUME OF SPHERICAL PARTICLES SO ASTROPHYSICAL JOURNAL LA English DT Article DE minor planets, asteroids: general; planets and satellites: surfaces; polarization radiative transfer; scattering ID MULTIPLE-SCATTERING; RADIATIVE-TRANSFER; LIGHT-SCATTERING; T-MATRIX; INTERFACE; OBJECT; SYSTEM; SPHERES; MEDIA AB We consider electromagnetic scattering by a spherical volume sparsely and randomly populated by spherical particles of equal size and optical properties. The far-field scattering matrix of the entire volume is computed using an exact method and an approximate method. The former is a direct computer solver of the Maxwell equations called the superposition T-matrix method (STMM). The latter is a solver based on numerical Monte Carlo integration of the ladder and cyclical diagrams appearing in the microphysical theory of radiative transfer and coherent backscattering (RT-CB). The quantitative agreement between the STMM and RT-CB computations provides verification of the RT-CB theory. Prominent backscattering features exhibited by the STMM data cannot be reproduced by keeping only the ladder diagrams of RT. Our results strongly support the CB explanation of opposition brightness and polarization phenomena observed for a class of atmosphereless solar-system objects. Further research is necessary to determine the range of quantitative applicability of the RT-CB theory to densely packed particulate media. C1 [Muinonen, K.; Zubko, E.; Penttila, A.] Univ Helsinki, Dept Phys, FI-00014 U Helsinki, Finland. [Mishchenko, M. I.] NASA Goddard Inst Space Studies, New York, NY 10025 USA. [Dlugach, J. M.] Natl Acad Sci Ukraine, Main Astron Observ, UA-03680 Kiev, Ukraine. [Videen, G.] Army Res Lab, Adelphi, MD 20783 USA. [Muinonen, K.] Finnish Geodet Inst, FI-02431 Masala, Finland. [Zubko, E.] Kharkov Natl Univ, Inst Astron, UA-61022 Kharkov, Ukraine. RP Muinonen, K (reprint author), Univ Helsinki, Dept Phys, Gustaf Hallstromin Katu 2A, FI-00014 U Helsinki, Finland. EM karri.muinonen@helsinki.fi; michael.i.mishchenko@nasa.gov; dl@mao.kiev.ua; evgenij.zubko@helsinki.fi; antti.i.penttila@helsinki.fi; gorden.videen@gmail.com RI Penttila, Antti/C-4886-2012; Mishchenko, Michael/D-4426-2012 OI Penttila, Antti/0000-0001-7403-1721; FU Academy of Finland [127461]; NASA Outer Planets Research Program [NNX10AP93G]; NASA Lunar Advanced Science and Exploration Research Program [NNX11AB25G]; NASA Radiation Sciences Program; NASA Remote Sensing Theory Program; National Academy of Sciences of Ukraine under the Main Astronomical Observatory GRAPE/GPU/GRID Computing Cluster Project FX This research has been partially funded by the Academy of Finland (contract 127461), NASA Outer Planets Research Program (contract NNX10AP93G), and NASA Lunar Advanced Science and Exploration Research Program (contract NNX11AB25G), as well as by the NASA Radiation Sciences Program managed by Hal Maring and by the NASA Remote Sensing Theory Program managed by Lucia Tsaoussi. M.I.M. and J.M.D. also acknowledge support from the National Academy of Sciences of Ukraine under the Main Astronomical Observatory GRAPE/GPU/GRID Computing Cluster Project. NR 42 TC 35 Z9 36 U1 0 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 1 PY 2012 VL 760 IS 2 AR 118 DI 10.1088/0004-637X/760/2/118 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 039BE UT WOS:000311217000022 ER PT J AU Qian, L Li, D Goldsmith, PF AF Qian, Lei Li, Di Goldsmith, Paul F. TI (CO)-C-13 CORES IN THE TAURUS MOLECULAR CLOUD SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: clouds; ISM: individual objects (Taurus); ISM: molecules; turbulence ID INITIAL MASS FUNCTION; STAR-FORMATION; DENSE CORES; CLUMP DISTRIBUTION; SUBMILLIMETER CLUMPS; 850 MICRONS; ORION; PERSEUS; ORIGIN; EXTINCTION AB Young stars form in molecular cores, which are dense condensations within molecular clouds. We have searched for molecular cores traced by (CO)-C-13 J = 1 -> 0 emission in the Taurus molecular cloud and studied their properties. Our data set has a spatial dynamic range (the ratio of linear map size to the pixel size) of about 1000 and spectrally resolved velocity information, which together allow a systematic examination of the distribution and dynamic state of (CO)-C-13 cores in a large contiguous region. We use empirical fit to the CO and CO2 ice to correct for depletion of gas-phase CO. The (CO)-C-13 core mass function ((CO)-C-13 CMF) can be fitted better with a log-normal function than with a power-law function. We also extract cores and calculate the (CO)-C-13 CMF based on the integrated intensity of (CO)-C-13 and the CMF from Two Micron All Sky Survey. We demonstrate that core blending exists, i.e., combined structures that are incoherent in velocity but continuous in column density. The core velocity dispersion (CVD), which is the variance of the core velocity difference delta nu, exhibits a power-law behavior as a function of the apparent separation L: CVD (km s(-1)) proportional to L(pc)(0.7). This is similar to Larson's law for the velocity dispersion of the gas. The peak velocities of (CO)-C-13 cores do not deviate from the centroid velocities of the ambient (CO)-C-12 gas by more than half of the line width. The low velocity dispersion among cores, the close similarity between CVD and Larson's law, and the small separation between core centroid velocities and the ambient gas all suggest that molecular cores condense out of the diffuse gas without additional energy from star formation or significant impact from converging flows. C1 [Qian, Lei; Li, Di] Chinese Acad Sci, Natl Astron Observ, Beijing 100012, Peoples R China. [Li, Di] CALTECH, Dept Astron, Pasadena, CA 91125 USA. [Goldsmith, Paul F.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Li, Di] Space Sci Inst, Boulder, CO USA. RP Qian, L (reprint author), Chinese Acad Sci, Natl Astron Observ, Beijing 100012, Peoples R China. EM lqian@nao.cas.cn; ithaca.li@gmail.com RI Goldsmith, Paul/H-3159-2016 FU China Ministry of Science and Technology [2012CB821800]; General Program of National Natural Science Foundation of China [11073028]; Young Researcher Grant of National Astronomical Observatories, Chinese Academy of Sciences; Chinese Academy of Sciences FX This work is partly supported by the China Ministry of Science and Technology under State Key Development Program for Basic Research (2012CB821800) and partly supported by the General Program of National Natural Science Foundation of China (11073028). L. Q. is partly supported by the Young Researcher Grant of National Astronomical Observatories, Chinese Academy of Sciences and partly supported by M. Zhu with his funding from the One Hundred Person Project of the Chinese Academy of Sciences. This work was carried out in part at the Jet Propulsion Laboratory, operated by the California Institute of Technology. NR 58 TC 16 Z9 17 U1 1 U2 8 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 1 PY 2012 VL 760 IS 2 AR 147 DI 10.1088/0004-637X/760/2/147 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 039BE UT WOS:000311217000051 ER PT J AU Smail, I Blundell, KM Lehmer, BD Alexander, DM AF Smail, Ian Blundell, Katherine M. Lehmer, B. D. Alexander, D. M. TI INVERSE COMPTON X-RAY HALOS AROUND HIGH-z RADIO GALAXIES: A FEEDBACK MECHANISM POWERED BY FAR-INFRARED STARBURSTS OR THE COSMIC MICROWAVE BACKGROUND? SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology: observations; galaxies: evolution; galaxies: formation; galaxies: individual (4C03.24, 4C19.71) ID JET-CLOUD INTERACTIONS; DEEP-FIELD-NORTH; STAR-FORMATION; ELLIPTIC GALAXIES; AGN FEEDBACK; 4C 60.07; HDF 130; EMISSION; CHANDRA; EVOLUTION AB We report the detection of extended X-ray emission around two powerful radio galaxies at z similar to 3.6 (4C 03.24 and 4C 19.71) and use these to investigate the origin of extended, inverse Compton (IC) powered X-ray halos at high redshifts. The halos have X-ray luminosities of L-X similar to 3 x 10(44) erg s(-1) and sizes of similar to 60 kpc. Their morphologies are broadly similar to the similar to 60 kpc long radio lobes around these galaxies suggesting they are formed from IC scattering by relativistic electrons in the radio lobes, of either cosmic microwave background (CMB) photons or far-infrared photons from the dust-obscured starbursts in these galaxies. These observations double the number of z > 3 radio galaxies with X-ray-detected IC halos. We compare the IC X-ray-to-radio luminosity ratios for the two new detections to the two previously detected z similar to 3.8 radio galaxies. Given the similar redshifts, we would expect comparable X-ray IC luminosities if millimeter photons from the CMB are the dominant seed field for the IC emission (assuming all four galaxies have similar ages and jet powers). Instead we see that the two z similar to 3.6 radio galaxies, which are similar to 4x fainter in the far-infrared than those at z similar to 3.8, also have similar to 4x fainter X-ray IC emission. Including data for a further six z greater than or similar to 2 radio sources with detected IC X-ray halos from the literature, we suggest that in the more compact, majority of radio sources, those with lobe sizes less than or similar to 100-200 kpc, the bulk of the IC emission may be driven by scattering of locally produced far-infrared photons from luminous, dust-obscured starbursts within these galaxies, rather than millimeter photons from the CMB. The resulting X-ray emission appears sufficient to ionize the gas on similar to 100-200 kpc scales around these systems and thus helps form the extended, kinematically quiescent Ly alpha emission line halos found around some of these systems. The starburst and active galactic nucleus activity in these galaxies are thus combining to produce an even more effective and widespread "feedback" process, acting on the long-term gas reservoir for the galaxy, than either individually could achieve. If episodic radio activity and coeval starbursts are common in massive, high-redshift galaxies, then this IC-feedback mechanism may play a role in affecting the star formation histories of the most massive galaxies at the present day. C1 [Smail, Ian] Univ Durham, Inst Computat Cosmol, Durham DH1 3LE, England. [Blundell, Katherine M.] Univ Oxford, Dept Astrophys, Oxford OX1 3RH, England. [Lehmer, B. D.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Lehmer, B. D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Alexander, D. M.] Univ Durham, Dept Phys, Durham DH1 3LE, England. RP Smail, I (reprint author), Univ Durham, Inst Computat Cosmol, South Rd, Durham DH1 3LE, England. RI Smail, Ian/M-5161-2013; OI Smail, Ian/0000-0003-3037-257X; Alexander, David/0000-0002-5896-6313 FU Leverhulme Trust; STFC; Einstein Fellowship; CXC [G01-12173X] FX We thank for Nick Seymour for generously checking his data prior to publication and Rob Ivison, Richard Bower, Caleb Scharf, Wil van Breugel, Mark Dickinson, Arjun Dey, Hy Spinrad, and Dan Stern for help and useful conversations. I. R. S. acknowledges a Leverhulme Trust Fellowship and I. R. S., K. M. B., and D. M. A. acknowledge support from the STFC. B. D. L. acknowledges support from an Einstein Fellowship and CXC grant G01-12173X. This work has used data from the NASA Extragalactic Database (NED), and from the NRAO VLA, Hubble Space Telescope, and Spitzer Space Telescope data archives. NR 49 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 J9 ASTROPHYS J JI Astrophys. J. PD DEC 1 PY 2012 VL 760 IS 2 AR 132 DI 10.1088/0004-637X/760/2/132 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 039BE UT WOS:000311217000036 ER PT J AU Goosse, H Crespin, E Dubinkina, S Loutre, MF Mann, ME Renssen, H Sallaz-Damaz, Y Shindell, D AF Goosse, Hugues Crespin, Elisabeth Dubinkina, Svetlana Loutre, Marie-France Mann, Michael E. Renssen, Hans Sallaz-Damaz, Yoann Shindell, Drew TI The role of forcing and internal dynamics in explaining the "Medieval Climate Anomaly" SO CLIMATE DYNAMICS LA English DT Article DE Paleoclimate; Last millennium; Medieval Climate Anomaly; Climate modelling; Data assimilation; Atmospheric and ocean dynamics; Radiative forcing ID NORTH-ATLANTIC OSCILLATION; LAST MILLENNIUM; PAST MILLENNIUM; CARBON-CYCLE; GULF-STREAM; RADIONUCLIDE RECORDS; SOLAR-ACTIVITY; SYSTEM MODEL; WARM PERIOD; VARIABILITY AB Proxy reconstructions suggest that peak global temperature during the past warm interval known as the Medieval Climate Anomaly (MCA, roughly 950-1250 AD) has been exceeded only during the most recent decades. To better understand the origin of this warm period, we use model simulations constrained by data assimilation establishing the spatial pattern of temperature changes that is most consistent with forcing estimates, model physics and the empirical information contained in paleoclimate proxy records. These numerical experiments demonstrate that the reconstructed spatial temperature pattern of the MCA can be explained by a simple thermodynamical response of the climate system to relatively weak changes in radiative forcing combined with a modification of the atmospheric circulation, displaying some similarities with the positive phase of the so-called Arctic Oscillation, and with northward shifts in the position of the Gulf Stream and Kuroshio currents. The mechanisms underlying the MCA are thus quite different from anthropogenic mechanisms responsible for modern global warming. C1 [Goosse, Hugues; Crespin, Elisabeth; Dubinkina, Svetlana; Loutre, Marie-France; Sallaz-Damaz, Yoann] Catholic Univ Louvain, Earth & Life Inst, Georges Lemaitre Ctr Earth & Climate Res, B-1348 Louvain, Belgium. [Mann, Michael E.] Penn State Univ, Dept Meteorol, University Pk, PA 16802 USA. [Mann, Michael E.] Penn State Univ, Earth & Environm Syst Inst, University Pk, PA 16802 USA. [Renssen, Hans] Vrije Univ Amsterdam, Dept Earth Sci, Sect Climate Change & Landscape Dynam, Amsterdam, Netherlands. [Shindell, Drew] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. RP Goosse, H (reprint author), Catholic Univ Louvain, Earth & Life Inst, Georges Lemaitre Ctr Earth & Climate Res, Chemin Cyclotron 2, B-1348 Louvain, Belgium. EM hugues.goosse@uclouvain.be RI Shindell, Drew/D-4636-2012; Mann, Michael/B-8472-2017; OI Mann, Michael/0000-0003-3067-296X; Loutre, Marie-France/0000-0001-6944-4038 FU FRS-FNRS; Belgian Federal Science Policy Office; EU; NSF [ATM-0902133]; Fond de la Recherche Scientifique de Belgique (FRS-FNRS) FX We thank E. Zorita and R. Wilson for comments and all the scientists that collected and analysed the proxy data used in this work. H. G. is Senior Research Associate with the Fonds National de la Recherche Scientifique (FRS-FNRS-Belgium). This work is supported by the FRS-FNRS and by the Belgian Federal Science Policy Office (Research Program on Science for a Sustainable Development) and by EU (project Past4future). M. E. M. acknowledges support from the NSF Paleoclimate program (grant number ATM-0902133). Aurelien Mairesse helped in the design of Fig. 1. Computational resources have been provided by the super-computing facilities of the Universite Catholique de Louvain (CISM/UCL) and the Consortium des Equipements de Calcul Intensif en Federation Wallonie Bruxelles (CECI) funded by the Fond de la Recherche Scientifique de Belgique (FRS-FNRS). NR 60 TC 43 Z9 43 U1 1 U2 48 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0930-7575 J9 CLIM DYNAM JI Clim. Dyn. PD DEC PY 2012 VL 39 IS 12 BP 2847 EP 2866 DI 10.1007/s00382-012-1297-0 PG 20 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 038VV UT WOS:000311203100007 ER PT J AU Torres-Perez, JL Armstrong, RA AF Torres-Perez, J. L. Armstrong, R. A. TI Effects of UV radiation on the growth, photosynthetic and photoprotective components, and reproduction of the Caribbean shallow-water coral Porites furcata SO CORAL REEFS LA English DT Article DE Ultraviolet radiation; Coral growth; Mycosporine-like amino acids; Coral reproduction; Porites furcata ID AMINO-ACIDS MAAS; REEF-BUILDING CORAL; SOLAR ULTRAVIOLET-RADIATION; GREAT-BARRIER-REEF; POCILLOPORA-DAMICORNIS; STYLOPHORA-PISTILLATA; ABSORBING COMPOUNDS; ACROPORA-CERVICORNIS; SEXUAL REPRODUCTION; CLIMATE-CHANGE AB Shallow reef corals can frequently be subjected to high doses of ultraviolet radiation [280-400 nm (UVR)] and have developed mechanisms to cope with this. Nevertheless, slight changes in this stressor may impact their physiology and ultimately their survival. Here, we present results on the effects of artificially enhanced UVR on the growth, reproduction, production of photosynthetic pigments and photoprotective compounds of the Caribbean shallow-water branching coral Porites furcata. Corals were randomly located in one of the three different treatments: normal photosynthetically active radiation (PAR) + UVR; normal PAR+ enhanced UVR; normal PAR+ depleted UVR. Growth rates were measured using the Alizarin red staining method, photosynthetic pigments as well as mycosporine-like amino acids (MAAs) were quantified through high-performance liquid chromatography, and fecundity was estimated after histological analyses. Growth and photosynthetic pigment concentration were negatively correlated with increased UVR, compared to controls exposed to normal UVR. A significant increase in MAAs was also found in colonies under enhanced UVR. Based on their respective concentrations, the primary mycosporine-glycine (lambda(max) = 310 nm) and shinorine (lambda(max) = 333 nm) are the main contributors to UVR absorption in this species, while the levels of the secondary MAA palythine (lambda(max) = 320 nm) tripled toward the end of the 128 days of the experimental period. While several physical factors may influence reef coral physiology, the results suggest that slight increases in UVR can debilitate the skeletal constitution and severely reduce the fecundity of corals living in shallow waters. C1 [Torres-Perez, J. L.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Torres-Perez, J. L.; Armstrong, R. A.] Univ Puerto Rico, Dept Marine Sci, Mayaguez, PR 00708 USA. RP Torres-Perez, JL (reprint author), NASA, Ames Res Ctr, MS 245-4,Bldg 245 Rm 120,POB 1, Moffett Field, CA 94035 USA. EM juanltorresperez@gmail.com FU Department of Marine Sciences, University of Puerto Rico; Alliance for Graduate Education Professoriate (AGEP); National Science Foundation; NASA [NCCW-0088] FX We would like to acknowledge the help and support from the Department of Marine Sciences, University of Puerto Rico. This research was supported by fellowships from the Alliance for Graduate Education Professoriate (AGEP) and from the National Science Foundation's Puerto Rico Graduate Teaching Fellows in K-12 Education to the corresponding author, and a NASA grant (NCCW-0088) to RAA. We are grateful to the Puerto Rico Department of Natural and Environmental Resources particularly the Marine Fisheries Laboratory for facilitating their histology laboratory. This manuscript was greatly improved by the comments of two anonymous reviewers. NR 84 TC 7 Z9 7 U1 3 U2 46 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0722-4028 J9 CORAL REEFS JI Coral Reefs PD DEC PY 2012 VL 31 IS 4 BP 1077 EP 1091 DI 10.1007/s00338-012-0927-7 PG 15 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 036AS UT WOS:000310999300018 ER PT J AU Sheard, BS Heinzel, G Danzmann, K Shaddock, DA Klipstein, WM Folkner, WM AF Sheard, B. S. Heinzel, G. Danzmann, K. Shaddock, D. A. Klipstein, W. M. Folkner, W. M. TI Intersatellite laser ranging instrument for the GRACE follow-on mission SO JOURNAL OF GEODESY LA English DT Article DE GRACE; Intersatellite ranging; Laser interferometry ID FREQUENCY STABILIZATION; OPTICAL INTERFEROMETERS; AUTOMATIC ALIGNMENT; GRAVITY RECOVERY; MASS VARIABILITY; PHASEMETER; SYSTEM; IMPACT AB The Gravity Recovery and Climate Experiment (GRACE) has demonstrated that low-low satellite-to-satellite tracking enables monitoring the time variations of the Earth's gravity field on a global scale, in particular those caused by mass-transport within the hydrosphere. Due to the importance of long-term continued monitoring of the variations of the Earth's gravitational field and the limited lifetime of GRACE, a follow-on mission is currently planned to be launched in 2017. In order to minimise risk and the time to launch, the follow-on mission will be basically a rebuild of GRACE with microwave ranging as the primary instrument for measuring changes of the intersatellite distance. Laser interferometry has been proposed as a method to achieve improved ranging precision for future GRACE-like missions and is therefore foreseen to be included as demonstrator experiment in the follow-on mission now under development. This paper presents the top-level architecture of an interferometric laser ranging system designed to demonstrate the technology which can also operate in parallel with the microwave ranging system of the GRACE follow-on mission. C1 [Sheard, B. S.; Heinzel, G.; Danzmann, K.] Leibniz Univ Hannover, Albert Einstein Inst, Max Planck Inst Gravitat Phys, D-30167 Hannover, Germany. [Sheard, B. S.; Heinzel, G.; Danzmann, K.] Leibniz Univ Hannover, Inst Gravitat Phys, D-30167 Hannover, Germany. [Shaddock, D. A.] Australian Natl Univ, Dept Quantum Sci, Acton, ACT 0200, Australia. [Klipstein, W. M.; Folkner, W. M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Sheard, BS (reprint author), Leibniz Univ Hannover, Albert Einstein Inst, Max Planck Inst Gravitat Phys, Callinstr 38, D-30167 Hannover, Germany. EM benjamin.sheard@aei.mpg.de; gerhard.heinzel@aei.mpg.de; karsten.danzmann@aei.mpg.de; daniel.shaddock@anu.edu.au RI Shaddock, Daniel/A-7534-2011 OI Shaddock, Daniel/0000-0002-6885-3494 FU "Deutsche Forschungsgemeinschaft" (DFG) within the Cluster of Excellence QUEST (Centre for Quantum Engineering and Space-Time Research); Australian Government's Australian Space Research Program FX This work was partly funded by the "Deutsche Forschungsgemeinschaft" (DFG) within the Cluster of Excellence QUEST (Centre for Quantum Engineering and Space-Time Research). Parts of the research described in this publication were carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. This work was also supported under the Australian Government's Australian Space Research Program. NR 48 TC 84 Z9 87 U1 4 U2 20 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0949-7714 EI 1432-1394 J9 J GEODESY JI J. Geodesy PD DEC PY 2012 VL 86 IS 12 BP 1083 EP 1095 DI 10.1007/s00190-012-0566-3 PG 13 WC Geochemistry & Geophysics; Remote Sensing SC Geochemistry & Geophysics; Remote Sensing GA 035RG UT WOS:000310964800001 ER PT J AU Li, YF Wang, ML Carra, C Cucinotta, FA AF Li, Yongfeng Wang, Minli Carra, Claudio Cucinotta, Francis A. TI Modularized Smad-regulated TGF beta signaling pathway SO MATHEMATICAL BIOSCIENCES LA English DT Article DE Ionizing radiation; Transforming growth factor beta (TGF beta); Smad; Signaling pathway; Modularization; Stability ID GROWTH-FACTOR-BETA; UBIQUITIN-DEPENDENT DEGRADATION; KINETIC-ANALYSIS; CELL-MEMBRANE; RECEPTOR; DYNAMICS; FIBROSIS; NUCLEUS; FIBROBLASTS; INHIBITION AB The transforming Growth Factor beta (TGF beta) signaling pathway is a prominent regulatory signaling pathway controlling various important cellular processes. TGF beta signaling can be induced by several factors including ionizing radiation. The pathway is regulated in a negative feedback loop through promoting the nuclear import of the regulatory Smads and a subsequent expression of inhibitory Smad7, that forms ubiquitin ligase with Smurf2, targeting active TGF beta receptors for degradation. In this work, we proposed a mathematical model to study the Smad-regulated TGF beta signaling pathway. By modularization, we are able to analyze mathematically each component subsystem and recover the nonlinear dynamics of the entire network system. Meanwhile the excitability, a common feature observed in the biological systems, in the TGF beta signaling pathway is discussed and supported as well by numerical simulation, indicating the robustness of the model. Published by Elsevier Inc. C1 [Cucinotta, Francis A.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Li, Yongfeng; Wang, Minli; Carra, Claudio] USRA, Div Space Life Sci, Houston, TX 77058 USA. RP Cucinotta, FA (reprint author), NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. EM francis.a.cucinotta@nasa.gov NR 42 TC 2 Z9 3 U1 0 U2 6 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0025-5564 EI 1879-3134 J9 MATH BIOSCI JI Math. Biosci. PD DEC PY 2012 VL 240 IS 2 BP 187 EP 200 DI 10.1016/j.mbs.2012.07.005 PG 14 WC Biology; Mathematical & Computational Biology SC Life Sciences & Biomedicine - Other Topics; Mathematical & Computational Biology GA 036ZK UT WOS:000311070600011 PM 22892478 ER PT J AU Yu, Y van Dyk, DA Kashyap, VL Young, CA AF Yu, Y. van Dyk, D. A. Kashyap, V. L. Young, C. A. TI A Bayesian Analysis of the Correlations Among Sunspot Cycles SO SOLAR PHYSICS LA English DT Article ID SOLAR-CYCLE; STOCHASTIC FLUCTUATIONS; PREDICTION; MAXIMUM; NUMBERS; RESTORATION; AMPLITUDE; SPECTRA; DYNAMO; MODEL AB Sunspot numbers form a comprehensive, long-duration proxy of solar activity and have been used numerous times to empirically investigate the properties of the solar cycle. A number of correlations have been discovered over the 24 cycles for which observational records are available. Here we carry out a sophisticated statistical analysis of the sunspot record that reaffirms these correlations, and sets up an empirical predictive framework for future cycles. An advantage of our approach is that it allows for rigorous assessment of both the statistical significance of various cycle features and the uncertainty associated with predictions. We summarize the data into three sequential relations that estimate the amplitude, duration, and time of rise to maximum for any cycle, given the values from the previous cycle. We find that there is no indication of a persistence in predictive power beyond one cycle, and we conclude that the dynamo does not retain memory beyond one cycle. Based on sunspot records up to October 2011, we obtain, for Cycle 24, an estimated maximum smoothed monthly sunspot number of 97 +/- 15, to occur in January-February 2014 +/- six months. C1 [Yu, Y.] Univ Calif Irvine, Irvine, CA 92717 USA. [van Dyk, D. A.] Univ London Imperial Coll Sci Technol & Med, London, England. [Kashyap, V. L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Young, C. A.] NASA, ADNET Syst Inc, GSFC, Greenbelt, MD USA. RP Yu, Y (reprint author), Univ Calif Irvine, Irvine, CA 92717 USA. EM yamingy@uci.edu; dvandyk@imperial.ac.uk; vkashyap@cfa.harvard.edu; c.alex.young@gsfc.nasa.gov OI Van Dyk, David/0000-0002-0816-331X FU CXC NASA [NAS 8-39073]; NSF [DMS 04-06085, DMS 09-07522] FX This work was supported by CXC NASA contract NAS 8-39073 (VLK) and NSF grants DMS 04-06085 and DMS 09-07522 (DvD, YY). NR 42 TC 3 Z9 3 U1 0 U2 1 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-0938 J9 SOL PHYS JI Sol. Phys. PD DEC PY 2012 VL 281 IS 2 BP 847 EP 862 DI 10.1007/s11207-012-0090-x PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 035UD UT WOS:000310974000020 ER PT J AU Johnson, L Young, R Barnes, N Friedman, L Lappas, V McInnes, C AF Johnson, Les Young, Roy Barnes, Nathan Friedman, Louis Lappas, Vaios McInnes, Colin TI Solar Sails: Technology And Demonstration Status SO INTERNATIONAL JOURNAL OF AERONAUTICAL AND SPACE SCIENCES LA English DT Review DE Solar Sail; In-Space Propulsion; IKAROS; Sunjammer; NanoSail-D; CubeSail; LightSail-1 AB Solar Sail propulsion has been validated in space (IKAROS, 2010) and soon several more solar-sail propelled spacecraft will be flown. Using sunlight for spacecraft propulsion is not a new idea. First proposed by Frederick Tsander and Konstantin Tsiolkovsky in the 1920' s, NASA's Echo 1 balloon, launched in 1960, was the first spacecraft for which the effects of solar photon pressure were measured. Solar sails reflect sunlight to achieve thrust, thus eliminating the need for costly and often very-heavy fuel. Such "propellantless" propulsion will enable whole new classes of space science and exploration missions previously not considered possible due to the propulsive-intense maneuvers and operations required. C1 [Johnson, Les; Young, Roy] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. [Barnes, Nathan] LGarde Inc, Tustin, CA 92780 USA. [Friedman, Louis] Planetary Soc, Execut Director Emeritus, Pasadena, CA 91107 USA. [Lappas, Vaios] Univ Surrey, Space Vehicle Control, Guildford GU2 5XH, Surrey, England. [McInnes, Colin] Univ Strathclyde, Dept Mech & Aerosp Engn, Adv Space Concepts Lab, Glasgow G1 1XJ, Lanark, Scotland. RP Johnson, L (reprint author), NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. EM charles.l.johnson-1@nasa.gov NR 16 TC 6 Z9 6 U1 6 U2 12 PU KOREAN SOC AERONAUTICAL & SPACE SCIENCES PI SEOULD PA 635-4, YEOGSAM-DONG, KANGNAM-KU, SEOULD, 135-703, SOUTH KOREA SN 2093-274X EI 2093-2480 J9 INT J AERONAUT SPACE JI Int. J. Aeronaut. Space Sci. PD DEC PY 2012 VL 13 IS 4 BP 421 EP 427 DI 10.5139/IJASS.2012.13.4.421 PG 7 WC Engineering, Aerospace SC Engineering GA V35WZ UT WOS:000209177200002 ER PT J AU Lillibridge, J Bonekamp, H Willis, J Bonnefond, P AF Lillibridge, John Bonekamp, Hans Willis, Josh Bonnefond, Pascal TI Special Issue: OSTM/Jason-2 Applications-Part 3 Preface SO MARINE GEODESY LA English DT Editorial Material C1 [Lillibridge, John] NOAA, Lab Satellite Altimetry, College Pk, MD USA. [Bonekamp, Hans] EUMETSAT, Darmstadt, Germany. [Willis, Josh] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Bonnefond, Pascal] Geoazur Observ Cote Azur, Grasse, France. RP Lillibridge, J (reprint author), NOAA, Lab Satellite Altimetry, College Pk, MD USA. RI Lillibridge, John/F-5606-2010 OI Lillibridge, John/0000-0001-9102-171X NR 0 TC 0 Z9 0 U1 0 U2 4 PU TAYLOR & FRANCIS INC PI PHILADELPHIA PA 520 CHESTNUT STREET, STE 850, PHILADELPHIA, PA 19106 USA SN 0149-0419 EI 1521-060X J9 MAR GEOD JI Mar. Geod. PD DEC 1 PY 2012 VL 35 SU 1 SI SI BP 1 EP 2 DI 10.1080/01490419.2012.721634 PG 2 WC Geochemistry & Geophysics; Oceanography; Remote Sensing SC Geochemistry & Geophysics; Oceanography; Remote Sensing GA 066RT UT WOS:000313238600001 ER PT J AU Masters, D Nerem, RS Choe, C Leuliette, E Beckley, B White, N Ablain, M AF Masters, D. Nerem, R. S. Choe, C. Leuliette, E. Beckley, B. White, N. Ablain, M. TI Comparison of Global Mean Sea Level Time Series from TOPEX/Poseidon, Jason-1, and Jason-2 SO MARINE GEODESY LA English DT Article DE Global mean sea level; climate data record; altimetry; interannual variability ID ALTIMETER DATA; TOPEX; BUDGET; TIDES; RISE; MISSIONS AB In the interest of improving the sea level climate data record, we compare the 19-year global mean sea level (GMSL) time series derived from TOPEX-Poseidon, Jason-1, and Jason-2 and produced by different research institutions. The GMSL time series are each produced using varying techniques and different applied corrections, and subsequently, the time series exhibit unique characteristics and sensitivity to seasonal and interannual signals. We find that the different applied corrections affect the time series variability much less than the technique for computing the GMSL from along-track versus gridded sea surface height anomalies and the choice of a minimum depth criteria. C1 [Masters, D.; Nerem, R. S.; Choe, C.] Univ Colorado, Colorado Ctr Astrodynam Res, Boulder, CO 80309 USA. [Leuliette, E.] NOAA, Lab Satellite Altimetry, Silver Spring, MD USA. [Beckley, B.] NASA, Goddard Space Flight Ctr, SGT Inc, Greenbelt, MD 20771 USA. [White, N.] CSIRO Marine & Atmospher Res, Ctr Australian Weather & Climate Res & Wealth Oce, Hobart, Tas, Australia. [Ablain, M.] CLS, Ramonville St Agne, France. RP Masters, D (reprint author), Univ Colorado, Colorado Ctr Astrodynam Res, 431UCB, Boulder, CO 80309 USA. EM dallas.masters@colorado.edu RI Leuliette, Eric/D-1527-2010 OI Leuliette, Eric/0000-0002-3425-4039 FU NASA; GSFC; NOAA; CNES; CLS; CSIRO FX This work was supported by two grants from NASA (Ocean Surface Topography Science Team and the MEaSUREs Project). Additional support from GSFC, NOAA, CNES, CLS, and CSIRO is also acknowledged. NR 45 TC 22 Z9 22 U1 0 U2 15 PU TAYLOR & FRANCIS INC PI PHILADELPHIA PA 520 CHESTNUT STREET, STE 850, PHILADELPHIA, PA 19106 USA SN 0149-0419 EI 1521-060X J9 MAR GEOD JI Mar. Geod. PD DEC 1 PY 2012 VL 35 SU 1 SI SI BP 20 EP 41 DI 10.1080/01490419.2012.717862 PG 22 WC Geochemistry & Geophysics; Oceanography; Remote Sensing SC Geochemistry & Geophysics; Oceanography; Remote Sensing GA 066RT UT WOS:000313238600003 ER PT J AU Cazenave, A Henry, O Munier, S Delcroix, T Gordon, AL Meyssignac, B Llovel, W Palanisamy, H Becker, M AF Cazenave, A. Henry, O. Munier, S. Delcroix, T. Gordon, A. L. Meyssignac, B. Llovel, W. Palanisamy, H. Becker, M. TI Estimating ENSO Influence on the Global Mean Sea Level, 1993-2010 SO MARINE GEODESY LA English DT Article DE Sea level; ENSO; land waters; steric sea level; ocean mass ID INDONESIAN THROUGHFLOW; MAKASSAR STRAIT; PRECIPITATION; PROJECT; OCEAN; VARIABILITY; EVOLUTION; TRANSPORT; MODEL; WATER AB Interannual global mean sea level (GMSL) variations and El Nino-Southern Oscillation (ENSO) are highly correlated, with positive/negative GMSL anomalies during El Nino/La Nina events. In a previous study, we showed that interannual GMSL and total land water storage variations are inversely correlated, with lower-than-average total water storage on land and higher-than-average GMSL during El Nino. This result is in agreement with the observed rainfall deficit/excess over land/oceans during El Nino (and vice versa during La Nina). It suggests that the positive GMSL anomaly observed during El Nino is likely due to an ocean mass rather than thermal expansion increase. Here, we analyze the respective contribution of the Atlantic, Indian, and Pacific oceans to the interannual (ENSO-related) GMSL anomalies observed during the altimetry era (i.e., since 1993) with an emphasis on the 1997/1998 El Nino event. For each oceanic region, we compute the steric contribution, and remove it from the altimetry-based mean sea level to estimate the ocean mass component. We find that mass changes of the tropical Pacific Ocean, mainly in the region within 025 degrees N, are mostly responsible for the observed 1997/1998 ENSO-related GMSL anomaly. The ocean mass excess of this region almost perfectly compensates the total land water deficit during the 1997/1998 El Nino. An estimate of the ocean-atmosphere water balance of this region shows that the time derivative of the ocean mass component is well correlated with net P-E (precipitation minus evaporation) over most of the study period, except during the 1997/1998 ENSO event, where there is a temporary ocean mass increase, not compensated by the net P-E. We thus propose that the 1997/1998 ocean mass increase of this north tropical Pacific area be linked to an imbalance between the inflow/outflow entering/leaving the north tropical Pacific. A preliminary qualitative analysis indicates that a significant reduction of the Makassar Strait transport, (about 80% of the total Indonesian throughflow), as previously reported in the literature during the strong 1997/1998 El Nino event, could explain the north tropical Pacific Ocean mass excess reported in this study, hence the observed positive GMSL anomaly. C1 [Cazenave, A.; Henry, O.; Munier, S.; Delcroix, T.; Meyssignac, B.; Palanisamy, H.] LEGOS, OMP, F-31401 Toulouse 9, France. [Llovel, W.] JPL, Pasadena, CA USA. [Gordon, A. L.] Columbia Univ, LDEO, New York, NY USA. [Becker, M.] UMR Espace DEV UAG, Cayenne, French Guiana. RP Cazenave, A (reprint author), LEGOS, OMP, 18 Ave Edouard Belin, F-31401 Toulouse 9, France. EM anny.cazenave@legos.obs-mip.fr RI Delcroix, Thierry/I-6103-2016; Munier, Simon/D-3849-2011; BECKER, Melanie/B-3658-2012; Gordon, Arnold/H-1049-2011; Meyssignac, Benoit/O-1910-2015; LLOVEL, William/G-6930-2016 OI Delcroix, Thierry/0000-0002-8850-4865; BECKER, Melanie/0000-0002-0263-5558; Gordon, Arnold/0000-0001-6480-6095; FU European grant in the context of the Monarch Project; CNES; JPL/NASA; French ANR CECILE project; National Science Foundation [OCE-0725935] FX O. Henry, S. Munier, W. Llovel, and H. Palanisamy are supported, respectively, by a European grant in the context of the Monarch Project, a postdoctoral grant from CNES, a postdoctoral grant from JPL/NASA, and the French ANR CECILE project. A. L. Gordon research is supported by the National Science Foundation grant OCE-0725935. This is Lamont-Doherty contribution number 7545. NR 37 TC 26 Z9 27 U1 4 U2 35 PU TAYLOR & FRANCIS INC PI PHILADELPHIA PA 520 CHESTNUT STREET, STE 850, PHILADELPHIA, PA 19106 USA SN 0149-0419 EI 1521-060X J9 MAR GEOD JI Mar. Geod. PD DEC 1 PY 2012 VL 35 SU 1 SI SI BP 82 EP 97 DI 10.1080/01490419.2012.718209 PG 16 WC Geochemistry & Geophysics; Oceanography; Remote Sensing SC Geochemistry & Geophysics; Oceanography; Remote Sensing GA 066RT UT WOS:000313238600006 ER PT J AU Ray, RD Beckley, BD AF Ray, R. D. Beckley, B. D. TI Calibration of Ocean Wave Measurements by the TOPEX, Jason-1, and Jason-2 Satellites SO MARINE GEODESY LA English DT Article DE Ocean waves; satellite altimetry; significant wave height; Jason-2 validation ID WIND-SPEED; ALTIMETER; HEIGHT; BUOY; VALIDATION; ERROR AB The calibration and validation of ocean wave height measurements by the TOPEX, Jason-1, and Jason-2 satellite altimeters are addressed by comparing the measurements internally among themselves and against independent wave measurements at moored buoys. The two six-month verification campaigns, when two of the satellites made near-simultaneous measurements along the same ground track, show the two Jason satellites to be remarkably consistent, while Topex reports waves generally 12% larger. External calibration is complicated by some systematic errors in the buoy data. We confirm that Canadian buoys underestimate significant wave heights by about 10% relative to U.S. buoys. Wave heights from all three altimetric satellites require scaling upwards by 56% to be consistent with U.S. buoys. C1 [Ray, R. D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Beckley, B. D.] SGT Inc, Greenbelt, MD USA. RP Ray, RD (reprint author), NASA, Goddard Space Flight Ctr, Code 698, Greenbelt, MD 20771 USA. EM richard.ray@nasa.gov RI Ray, Richard/D-1034-2012 FU U. S. National Aeronautics and Space Administration FX This work was funded by the U. S. National Aeronautics and Space Administration under the Ocean Surface Topography program and the MEaSUREs program. Buoy data were obtained from the National Data Buoy Center, a part of the National Oceanic and Atmospheric Administration, and from Fisheries and Oceans Canada. NR 35 TC 9 Z9 11 U1 0 U2 9 PU TAYLOR & FRANCIS INC PI PHILADELPHIA PA 520 CHESTNUT STREET, STE 850, PHILADELPHIA, PA 19106 USA SN 0149-0419 EI 1521-060X J9 MAR GEOD JI Mar. Geod. PD DEC 1 PY 2012 VL 35 SU 1 SI SI BP 238 EP 257 DI 10.1080/01490419.2012.718611 PG 20 WC Geochemistry & Geophysics; Oceanography; Remote Sensing SC Geochemistry & Geophysics; Oceanography; Remote Sensing GA 066RT UT WOS:000313238600014 ER PT J AU Crago, RD Okello, W Jasinski, MF AF Crago, Richard D. Okello, Winnie Jasinski, Michael F. TI Equations for the Drag Force and Aerodynamic Roughness Length of Urban Areas with Random Building Heights SO BOUNDARY-LAYER METEOROLOGY LA English DT Article DE Buildings; Aerodynamic roughness length; Shear stress; Urban ID VEGETATION; CANOPY; ARRAYS; MODEL; FLOW; DISPERSION; TURBULENCE; OBSTACLES; SURFACES; FIELDS AB We use a conceptual model to investigate how randomly varying building heights within a city affect the atmospheric drag forces and the aerodynamic roughness length of the city. The model is based on the assumptions regarding wake spreading and mutual sheltering effects proposed by Raupach (Boundary-Layer Meteorol 60:375-395, 1992). It is applied both to canopies having uniform building heights and to those having the same building density and mean height, but with variability about the mean. For each simulated urban area, a correction is determined, due to height variability, to the shear stress predicted for the uniform building height case. It is found that u (*)/u (*R) , where u (*) is the friction velocity and u (*R) is the friction velocity from the uniform building height case, is expressed well as an algebraic function of lambda and sigma (h) /h (m) , where lambda is the frontal area index, sigma (h) is the standard deviation of the building height, and h (m) is the mean building height. The simulations also resulted in a simple algebraic relation for z (0)/z (0R) as a function of lambda and sigma (h) /h (m) , where z (0) is the aerodynamic roughness length and z (0R) is z (0) found from the original Raupach formulation for a uniform canopy. Model results are in keeping with those of several previous studies. C1 [Crago, Richard D.; Okello, Winnie] Bucknell Univ, Dept Civil & Environm Engn, Lewisburg, PA 17837 USA. [Jasinski, Michael F.] NASA, Goddard Space Flight Ctr, Hydrol Sci Branch, Greenbelt, MD 20771 USA. RP Crago, RD (reprint author), Bucknell Univ, Dept Civil & Environm Engn, Lewisburg, PA 17837 USA. EM rcrago@bucknell.edu FU National Aeronautics and Space Administration [NNX08AY39G] FX This work was funded in part by the National Aeronautics and Space Administration through grant number NNX08AY39G. NR 32 TC 4 Z9 5 U1 1 U2 18 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0006-8314 J9 BOUND-LAY METEOROL JI Bound.-Layer Meteor. PD DEC PY 2012 VL 145 IS 3 BP 423 EP 437 DI 10.1007/s10546-012-9747-0 PG 15 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 027UA UT WOS:000310378100002 ER PT J AU Fereres, S Lautenberger, C Fernandez-Pello, AC Urban, DL Ruff, GA AF Fereres, Sonia Lautenberger, Chris Fernandez-Pello, A. Carlos Urban, David L. Ruff, Gary A. TI Understanding ambient pressure effects on piloted ignition through numerical modeling SO COMBUSTION AND FLAME LA English DT Article DE Piloted ignition; Reduced pressure; Ignition delay; Critical mass flux; FDS ID POLYMERIC MATERIALS; MASS FLUX AB This work presents a numerical modeling investigation of the mechanisms controlling the dependence on ambient pressure of the piloted ignition of a solid fuel under external radiant heating. The focus is to confirm the hypotheses and phenomenological arguments generated by previous experimental studies of the problem. For this purpose, the effect of ambient pressure on the piloted ignition of thermally irradiated samples of PMMA is modeled using the Fire Dynamics Simulator (FDS5) code. Two-dimensional simulations were performed using finite-rate single-step combustion kinetics in the gas-phase and a single-step Arrhenius reaction rate for the solid phase decomposition. Oxidative pyrolysis is not considered and the in-depth formed pyrolyzate is assumed to flow unrestricted through the PMMA. The objective is to understand the thermo-physical mechanisms leading to ignition and how they may be affected by a reduction in ambient pressure. The model is able to reproduce the main physical aspects of the piloted ignition of a solid fuel and confirms previous phenomenological explanations developed to describe recent experimental results at a range of ambient pressures. Reduced pressure environments result in: (1) shorter ignition times mainly due to reduced convective heat losses from the heated material to the surroundings, allowing for the material to heat more rapidly and pyrolyze faster; (2) a lower fuel mass flux at ignition, due primarily to a thicker thermal boundary layer and a thicker fuel species profile. The appearance of a premixed flame at the pilot, its propagation through the combustible mixture above the solid surface, and the subsequent sustained burning conditions are also explored in this work. The calculated ignition times and mass loss rates at ignition are compared to those measured experimentally in a laboratory-scale combustion wind tunnel. It is shown that with appropriate kinetic parameters the model qualitatively agrees with the experimental data. (C) 2012 The Combustion Institute. Published by Elsevier Inc. All rights reserved. C1 [Fereres, Sonia] Abengoa Res, Seville 41014, Spain. [Lautenberger, Chris; Fernandez-Pello, A. Carlos] Univ Calif Berkeley, Dept Mech Engn, Berkeley, CA 94720 USA. [Urban, David L.; Ruff, Gary A.] NASA John H Glenn Res Ctr, Cleveland, OH 44256 USA. RP Fereres, S (reprint author), Abengoa Res, C Energia Solar 1, Seville 41014, Spain. EM sonia.fereres@research.abengoa.com FU NASA [NNX08BA77A, NNX10AE01G] FX The authors would like to thank David Rich, Andres Osorio and Amanda Dodd for their comments and insightful discussions. This work was supported by NASA Grants NNX08BA77A and NNX10AE01G. NR 28 TC 7 Z9 7 U1 3 U2 31 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0010-2180 J9 COMBUST FLAME JI Combust. Flame PD DEC PY 2012 VL 159 IS 12 BP 3544 EP 3553 DI 10.1016/j.combustflame.2012.08.006 PG 10 WC Thermodynamics; Energy & Fuels; Engineering, Multidisciplinary; Engineering, Chemical; Engineering, Mechanical SC Thermodynamics; Energy & Fuels; Engineering GA 031QI UT WOS:000310656600009 ER PT J AU Nayagam, V Dietrich, DL Ferkul, PV Hicks, MC Williams, FA AF Nayagam, Vedha Dietrich, Daniel L. Ferkul, Paul V. Hicks, Michael C. Williams, Forman A. TI Can cool flames support quasi-steady alkane droplet burning? SO COMBUSTION AND FLAME LA English DT Article DE Droplet combustion; Cool flames; Alkane chemistry; Microgravity; Extinction ID N-HEPTANE OXIDATION; ATMOSPHERIC-PRESSURE; FUEL DROPLETS; COMBUSTION; IGNITION; MICROGRAVITY; CONVECTION; EXTINCTION; MIXTURES AB Experimental observations of anomalous combustion of n-heptane droplets burning in microgravity are reported. Following ignition, a relatively large n-heptane droplet first undergoes radiative extinction, that is, the visible flame ceases to exist because of radiant energy loss. But the droplet continues to experience vigorous vaporization for an extended period according to a quasi-steady droplet-burning law, ending in a secondary extinction at a finite droplet diameter, after which a vapor cloud rapidly appears surrounding the droplet. We hypothesize that the second-stage vaporization is sustained by low-temperature, soot-free, "cool-flame" chemical heat release. Measured droplet burning rates and extinction diameters are used to extract an effective heat release, overall activation energy, and pre-exponential factor for this low-temperature chemistry, and the values of the resulting parameters are found to be closer to those of "cool-flame" overall reaction-rate parameters, found in the literature, than to corresponding hot-flame parameters. (C) 2012 The Combustion Institute. Published by Elsevier Inc. All rights reserved. C1 [Nayagam, Vedha; Ferkul, Paul V.] Natl Ctr Space Explorat Res, Cleveland, OH 44135 USA. [Dietrich, Daniel L.; Hicks, Michael C.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. [Williams, Forman A.] Univ Calif San Diego, Dept Mech & Aerosp Engn, La Jolla, CA 92093 USA. RP Nayagam, V (reprint author), Natl Ctr Space Explorat Res, Cleveland, OH 44135 USA. EM v.nayagam@grc.nasa.gov FU NASA; International Space Station FX This work was supported by the NASA Space Life and Physical Sciences Research and Applications Program and the International Space Station Program. We would like to thank our other FLEX team members, C.T. Avedisian, M.Y. Choi, F.L. Dryer, and B.D. Shaw, as well as the reviewers for their very critical comments and N. Peters for recent insights. NR 27 TC 33 Z9 35 U1 3 U2 18 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0010-2180 J9 COMBUST FLAME JI Combust. Flame PD DEC PY 2012 VL 159 IS 12 BP 3583 EP 3588 DI 10.1016/j.combustflame.2012.07.012 PG 6 WC Thermodynamics; Energy & Fuels; Engineering, Multidisciplinary; Engineering, Chemical; Engineering, Mechanical SC Thermodynamics; Energy & Fuels; Engineering GA 031QI UT WOS:000310656600013 ER PT J AU Benafan, O Noebe, RD Padula, SA Vaidyanathan, R AF Benafan, O. Noebe, R. D. Padula, S. A., II Vaidyanathan, R. TI Microstructural Response During Isothermal and Isobaric Loading of a Precipitation-Strengthened Ni-29.7Ti-20Hf High-Temperature Shape Memory Alloy SO METALLURGICAL AND MATERIALS TRANSACTIONS A-PHYSICAL METALLURGY AND MATERIALS SCIENCE LA English DT Article ID SEVERE PLASTIC-DEFORMATION; ACQUIRED IN-SITU; DIFFRACTION SPECTRA; RIETVELD REFINEMENT; CYCLIC REVERSIBILITY; TRANSFORMATION; MARTENSITE; PHASE; BEHAVIOR; STRAIN AB A stable Ni-rich Ni-29.7Ti-20Hf (at. pct) shape memory alloy, with relatively high transformation temperatures, was shown to exhibit promising properties at lower raw material cost when compared to typical NiTi-X (X = Pt, Pd, Au) high-temperature shape memory alloys (HTSMAs). The excellent dimensional stability and high work output for this alloy were attributed to a coherent, nanometer size precipitate phase observed using transmission electron microscopy. To establish an understanding of the role of these precipitates on the microstructure and ensuing stability of the NiTiHf alloy, a detailed study of the micromechanical and microstructural behaviors was performed. In-situ neutron diffraction at stress and temperature was used to obtain quantitative information on phase-specific internal strain, texture, and phase volume fractions during both isothermal and isobaric testing of the alloy. During isothermal testing, the alloy exhibited low isothermal strains due to limited detwinning, consistent with direct measurements of the bulk texture through neutron diffraction. This limited detwinning was attributed to the pinning of twin and variant boundaries by the dispersion of fine precipitates. During isobaric thermal cycling at 400 MPa, the high work output and near-perfect dimensional stability was attributed to the presence of the precipitates that act as homogeneous sources for the nucleation of martensite throughout the material, while providing resistance to irrecoverable processes such as plastic deformation. C1 [Vaidyanathan, R.] Univ Cent Florida, Mech Mat & Aerosp Engn Dept, Adv Mat Proc & Anal Ctr AMPAC, Orlando, FL 32816 USA. [Noebe, R. D.; Padula, S. A., II] Univ Cent Florida, Mech Mat & Aerosp Engn Dept, Adv Mat Proc & Anal Ctr AMPAC, Orlando, FL 32816 USA. RP Benafan, O (reprint author), NASA Glenn Res Ctr, Struct & Mat Div, Cleveland, OH 44135 USA. EM raj@ucf.edu FU NASA Fundamental Aeronautics Program, Supersonics Project [NNX08A-B51A]; Office of Basic Energy Sciences, United States Department of Energy; Los Alamos National Security LLC under the United States Department of Energy [DE-AC52-06NA25396] FX Funding from the NASA Fundamental Aeronautics Program, Supersonics Project (Grant No. NNX08A-B51A), is gratefully acknowledged. The authors thank D. W. Brown, B. Clausen, and T. Sisneros (LANL) and D. Gaydosh, G. Bigelow, and A. Garg (NASA GRC) for technical support and helpful discussions. D. E. Nicholson's help in performing the neutron diffraction experiments is gratefully acknowledged. This work benefited from the use of the Lujan Neutron Scattering Center, LANSCE, which is funded by the Office of Basic Energy Sciences, United States Department of Energy. LANL is operated by Los Alamos National Security LLC under the United States Department of Energy Contract No. DE-AC52-06NA25396. NR 63 TC 29 Z9 29 U1 2 U2 30 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 1073-5623 J9 METALL MATER TRANS A JI Metall. Mater. Trans. A-Phys. Metall. Mater. Sci. PD DEC PY 2012 VL 43A IS 12 BP 4539 EP 4552 DI 10.1007/s11661-012-1297-z PG 14 WC Materials Science, Multidisciplinary; Metallurgy & Metallurgical Engineering SC Materials Science; Metallurgy & Metallurgical Engineering GA 022FH UT WOS:000309940500013 ER PT J AU Padula, S Qiu, SP Gaydosh, D Noebe, R Bigelow, G Garg, A Vaidyanathan, R AF Padula, Santo, II Qiu, Shipeng Gaydosh, Darrell Noebe, Ronald Bigelow, Glen Garg, Anita Vaidyanathan, Raj TI Effect of Upper-Cycle Temperature on the Load-Biased, Strain-Temperature Response of NiTi SO METALLURGICAL AND MATERIALS TRANSACTIONS A-PHYSICAL METALLURGY AND MATERIALS SCIENCE LA English DT Article ID SHAPE-MEMORY ALLOY; NEUTRON-DIFFRACTION; SUPERELASTIC NITI; IN-SITU; STRESS; TRANSFORMATION; TEXTURE AB Over the past decade, interest in shape-memory-alloy based actuators has increased as the primary benefits of these solid-state devices have become more apparent. However, much is still unknown about the characteristic behavior of these materials when used in actuator applications. Recently, we showed that the maximum temperature reached during thermal cycling under isobaric conditions could significantly affect the observed mechanical response of NiTi (55 wt pct Ni), especially the amount of transformation strain available for actuation and thus work output. The investigation we report here extends that original work to (1) ascertain whether increases in the upper-cycle temperature would produce additional changes in the work output of the material, which has a stress-free austenite finish temperature of 386 K (113 A degrees C), and (2) determine the optimum cyclic conditions. Thus, isobaric, thermal-cycle experiments were conducted on the aforementioned alloy at various stresses from 50 to 300 MPa using upper-cycle temperatures of 438 K, 473 K, 503 K, 533 K, 563 K, 593 K, and 623 K (165 A degrees C, 200 A degrees C, 230 A degrees C, 260 A degrees C, 290 A degrees C, 320 A degrees C, and 350 A degrees C). The data indicated that the amount of applied stress influenced the transformation strain, as would be expected. However, the maximum temperature reached during the thermal excursion also plays an equally significant role in determining the transformation strain, with the maximum transformation strain observed during thermal cycling to 563 K (290 A degrees C). In situ neutron diffraction at stress and temperature showed that the differences in transformation strain were mostly related to changes in martensite texture when cycling to different upper-cycle temperatures. Hence, understanding this effect is important to optimizing the operation of SMA-based actuators and could lead to new methods for processing and training shape-memory alloys for optimal performance. C1 [Padula, Santo, II; Noebe, Ronald; Bigelow, Glen] NASA Glenn Res Ctr, Cleveland, OH 44135 USA. [Qiu, Shipeng; Vaidyanathan, Raj] Univ Cent Florida, Orlanda, FL 32816 USA. [Gaydosh, Darrell] Ohio Aerosp Inst, Cleveland, OH 44142 USA. [Garg, Anita] Univ Toledo, Toledo, OH 43606 USA. RP Padula, S (reprint author), NASA Glenn Res Ctr, Cleveland, OH 44135 USA. EM Santo.A.Padula@nasa.gov FU Fundamental Aeronautics Program, Supersonics Project,; Office of Basic Energy Sciences (DOE); Los Alamos National Security LLC under DOE [DE-AC52-06NA25396] FX This work was supported by the Fundamental Aeronautics Program, Supersonics Project, API: Dale Hopkins. The authors thank B. Clausen, D. Brown, and T. Sisneros at Los Alamos National Laboratory for experimental assistance. This work has benefited from the use of the Lujan Neutron Scattering Center at LANSCE, which is funded by the Office of Basic Energy Sciences (DOE). LANL is operated by Los Alamos National Security LLC under DOE Contract DE-AC52-06NA25396. NR 20 TC 23 Z9 23 U1 0 U2 6 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 1073-5623 J9 METALL MATER TRANS A JI Metall. Mater. Trans. A-Phys. Metall. Mater. Sci. PD DEC PY 2012 VL 43A IS 12 BP 4610 EP 4621 DI 10.1007/s11661-012-1267-5 PG 12 WC Materials Science, Multidisciplinary; Metallurgy & Metallurgical Engineering SC Materials Science; Metallurgy & Metallurgical Engineering GA 022FH UT WOS:000309940500018 ER PT J AU Van Hoose, JR Grugel, RN Tewari, SN Brush, LN Erdmann, RG Poirier, DR AF Van Hoose, J. R. Grugel, R. N. Tewari, S. N. Brush, L. N. Erdmann, R. G. Poirier, D. R. TI Observation of Misoriented Tertiary Dendrite Arms During Controlled Directional Solidification in Aluminum-7 Wt pct Silicon Alloys SO METALLURGICAL AND MATERIALS TRANSACTIONS A-PHYSICAL METALLURGY AND MATERIALS SCIENCE LA English DT Article ID SINGLE-CRYSTAL SUPERALLOYS; CELLULAR ARRAY GROWTH; ZONE RAYLEIGH NUMBER; AL-SI ALLOYS; PB-SN ALLOYS; IN-SITU; NUMERICAL-ANALYSIS; METALLIC ALLOYS; MACROSEGREGATION; CU AB Electron backscattered diffraction (EBSD) examination of transverse cross sections from a directionally solidified aluminum-7 wt pct silicon alloy revealed tertiary dendrite arms that appeared in place but in reality had orientations that significantly differed from their parent arm. The maximum extent of spuriously orientated arms occurred at an intermediate growth velocity and was more pronounced at subgrain boundaries that separated uniquely oriented dendritic arrays. Mechanisms for tertiary arm misorientations are discussed, and attention is called to the practical consequences of these in-situ defects. C1 [Van Hoose, J. R.] Qualis Corp, Huntsville, AL 35806 USA. [Grugel, R. N.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. [Tewari, S. N.] Cleveland State Univ, Chem & Biomed Engn Dept, Cleveland, OH 44115 USA. [Brush, L. N.] Univ Washington, Dept Mat Sci & Engn, Seattle, WA 98195 USA. [Erdmann, R. G.; Poirier, D. R.] Univ Arizona, Dept Mat Sci & Engn, Tucson, AZ 85721 USA. RP Van Hoose, JR (reprint author), Siemens Corp, Orlando, FL 32826 USA. EM Richard.N.Grugel@nasa.gov FU NASA [NNX08AN49G]; Marshall Space Flight Center's Materials and Processing Laboratory FX The authors are grateful to Dr. Men G. Chu, Technical Fellow-Solidification Technology, Alcoa Technical Center, for providing the Al-7 wt pct Si as-cast feed bars. This research was supported, in part, by NASA Grant No. NNX08AN49G. The support of the Marshall Space Flight Center's Materials and Processing Laboratory is also gratefully acknowledged. NR 35 TC 1 Z9 1 U1 4 U2 26 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 1073-5623 J9 METALL MATER TRANS A JI Metall. Mater. Trans. A-Phys. Metall. Mater. Sci. PD DEC PY 2012 VL 43A IS 12 BP 4724 EP 4731 DI 10.1007/s11661-012-1260-z PG 8 WC Materials Science, Multidisciplinary; Metallurgy & Metallurgical Engineering SC Materials Science; Metallurgy & Metallurgical Engineering GA 022FH UT WOS:000309940500028 ER PT J AU Knight, GA Hou, TH Belcher, MA Palmieri, FL Wohl, CJ Connell, JW AF Knight, G. A. Hou, T. H. Belcher, M. A. Palmieri, F. L. Wohl, C. J. Connell, J. W. TI Hygrothermal aging of composite single lap shear specimens comprised of AF-555M adhesive and T800H/3900-2 adherends SO INTERNATIONAL JOURNAL OF ADHESION AND ADHESIVES LA English DT Article DE AF-555M adhesive; T800H/3900-2 adherends; Temperature/humidity aging; Composite lap shear specimens; Peel-ply surface treatment; Adhesion failure mode analysis AB Fiber reinforced resin matrix composites and structural adhesives have found increased usage on commercial and military aircraft. These structural materials offer weight savings without sacrificing strength and mechanical performance. Since service history and long-term aging performance of these relatively new material systems are not well established, a long-term environmental aging study was undertaken. Adhesive bonds were prepared by secondary bonding of 3M(TM) Scotch-Weld(TM) AF-555M between pre-cured, unidirectional composite adherends comprised of Toray(TM) T800H/3900-2 prepreg. Single lap shear specimens (SLS) were fabricated and subsequently aged in an unstressed configuration at 82 degrees C (180 degrees F) and 85% relative humidity for up to 772 days. The aging conditions are more severe than those expected to occur in service and were selected in order to observe some changes within a reasonable exposure time. The apparent shear strengths were measured periodically at both room temperature and 82 degrees C (180 degrees F), and failure modes were determined and compared to control specimens that had been stored for equal periods of time at room temperature under low humidity. With hygrothermal aging, apparent shear strengths decreased and some changes in the failure mode were observed relative to those of the control specimens. However, in spite of the severe aging conditions, no adhesive failures indicative of interfacial failures were observed. SLS specimens that were hygrothermally aged, subsequently dried, and then tested did not exhibit complete recovery of unaged apparent shear strengths indicating some irreversible changes. Published by Elsevier Ltd. C1 [Knight, G. A.; Hou, T. H.; Wohl, C. J.; Connell, J. W.] NASA, Langley Res Ctr, Hampton, VA 23681 USA. [Belcher, M. A.] Boeing Co, Seattle, WA 98124 USA. [Belcher, M. A.; Palmieri, F. L.] Natl Inst Aerosp, Hampton, VA 23666 USA. RP Connell, JW (reprint author), NASA, Langley Res Ctr, 6 W Taylor St,MS 226, Hampton, VA 23681 USA. EM john.w.connell@nasa.gov NR 10 TC 8 Z9 8 U1 1 U2 22 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0143-7496 J9 INT J ADHES ADHES JI Int. J. Adhes. Adhes. PD DEC PY 2012 VL 39 BP 1 EP 7 DI 10.1016/j.ijadhadh.2012.06.009 PG 7 WC Engineering, Chemical; Materials Science, Multidisciplinary SC Engineering; Materials Science GA 018EW UT WOS:000309643900001 ER PT J AU Lloyd, CW AF Lloyd, Charles W. TI IAC-11.E1-7.-A1.8.5 The Mission X: Train Like an Astronaut pilot study SO ACTA ASTRONAUTICA LA English DT Article DE Education; Astronaut training; Health; Fitness; Obesity; Mission X ID BODY-MASS INDEX; EARLY PHYSICAL-ACTIVITY; CHILDHOOD OBESITY; US CHILDREN; ADOLESCENTS; PREVENTION; PREVALENCE AB Mission X: Train Like an Astronaut is an international educational challenge focusing on fitness and nutrition as we encourage students to "train like an astronaut." Teams of students (aged 8-12) learn principles of healthy eating and exercise, compete for points by finishing training modules, and get excited about their future as "fit explorers." The 18 core exercises (targeting strength, endurance, coordination, balance, spatial awareness, and more) involve the same types of skills that astronauts learn in their training and use in spaceflight. This first-of-its-kind cooperative outreach program has allowed 11 space agencies and various partner institutions to work together to address quality health/fitness education, challenge students to be more physically active, increase awareness of the importance of lifelong health and fitness, teach students how fitness plays a vital role in human performance for exploration, and to inspire and motivate students to pursue careers in science, technology, engineering and math (STEM) fields. The project was initiated in 2009 in response to a request by the International Space Life Sciences Working Group. USA, Netherlands, Italy, France, Germany, Austria, Colombia, Spain, Belgium, Czech Republic and United Kingdom hosted teams for the pilot in the spring of 2010, and Japan held a modified version of the challenge. Several more agencies provided input into the preparations. Competing in 137 teams, more than 4000 students from over 40 cities worldwide participated in the first round of Mission X. Published by Elsevier Ltd. C1 NASA, Houston, TX 77058 USA. RP Lloyd, CW (reprint author), NASA, Houston, TX 77058 USA. EM charles.w.lloyd@nasa.gov NR 17 TC 3 Z9 3 U1 3 U2 23 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0094-5765 J9 ACTA ASTRONAUT JI Acta Astronaut. PD DEC PY 2012 VL 81 BP 77 EP 82 DI 10.1016/j.actaastro.2012.07.010 PG 6 WC Engineering, Aerospace SC Engineering GA 017CY UT WOS:000309568900010 ER PT J AU Gehrels, N Cannizzo, JK AF Gehrels, N. Cannizzo, J. K. TI IAC-11.A7.2.1: Gamma-ray astronomy technology needs SO ACTA ASTRONAUTICA LA English DT Article DE Gamma rays; General; Telescopes; Bursts; Blazars; Galactic transients ID EXPERIMENT TELESCOPE EGRET; ACTIVE GALACTIC NUCLEI; LARGE-AREA TELESCOPE; MISSION; CATALOG AB In recent decades gamma-ray observations have become a valuable tool for studying the universe. Progress made in diverse areas such as gamma-ray bursts (GRBs), nucleosynthesis, and active galactic nuclei (AGNs) has complemented and enriched our astrophysical understanding in many ways. We present an overview of current and future planned space gamma-ray missions and discuss technology needs for the next generation of space gamma-ray instruments. (c) 2012 Elsevier Ltd. All rights reserved. C1 [Cannizzo, J. K.] NASA, Goddard Space Flight Ctr, Astroparticle Phys Lab, JCA,CRESST,UMBC, Greenbelt, MD 20771 USA. RP Cannizzo, JK (reprint author), NASA, Goddard Space Flight Ctr, Astroparticle Phys Lab, JCA,CRESST,UMBC, Greenbelt, MD 20771 USA. EM neil.gehrels@nasa.gov; john.k.cannizzo@nasa.gov NR 21 TC 0 Z9 0 U1 0 U2 0 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0094-5765 EI 1879-2030 J9 ACTA ASTRONAUT JI Acta Astronaut. PD DEC PY 2012 VL 81 BP 83 EP 91 DI 10.1016/j.actaastro.2012.06.005 PG 9 WC Engineering, Aerospace SC Engineering GA 017CY UT WOS:000309568900011 ER PT J AU Lee, D Tippur, H Bogert, P AF Lee, Dongyeon Tippur, Hareesh Bogert, Phillip TI Dynamic fracture of graphite/epoxy composites stiffened by buffer strips: An experimental study SO COMPOSITE STRUCTURES LA English DT Article DE Graphite/epoxy; PETI-5/IM7; Stiffener; Dynamic fracture; Impact loading; Digital image correlation ID INDUCED LAMINATE FAILURE; IMAGE CORRELATION METHOD; HIGH-SPEED PHOTOGRAPHY; CRACK AB Fracture responses of unidirectional graphite/epoxy composite coupons enhanced by buffer strips are investigated under impact loading conditions using digital image correlation technique and high-speed photography. Composite coupons made of phenylethynyl terminated imide oligomer (PETI-5) as matrix and IM7 graphite fiber as reinforcement are studied. Buffer strips are made of the same material but with a different stacking sequence to attain quasi-isotropy. Edge-notched coupons are subjected to impact loading along the axis of symmetry. The effectiveness of methods used for attaching the buffer strip, namely, co-curing at elevated temperatures and adhesive bonding at room temperature, are also examined. The optically measured stress intensity factor histories reveal that both methods provide nearly identical fracture responses. However, the crack initiates much later in coupons stiffened using adhesive bonding method than its co-cured counterpart and thus shows higher stress intensity factor at initiation. The residual stresses are shown to be responsible for the difference in the fracture responses. (C) 2012 Elsevier Ltd. All rights reserved. C1 [Lee, Dongyeon; Tippur, Hareesh] Auburn Univ, Dept Mech Engn, Auburn, AL 36849 USA. [Bogert, Phillip] NASA, Langley Res Ctr, Hampton, VA USA. RP Tippur, H (reprint author), Auburn Univ, Dept Mech Engn, Auburn, AL 36849 USA. EM htippur@eng.auburn.edu FU NASA-LaRC [NNX07AC64B] FX This research was sponsored by the NASA-LaRC under cooperative agreement No. NNX07AC64B. NR 22 TC 2 Z9 5 U1 0 U2 9 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0263-8223 J9 COMPOS STRUCT JI Compos. Struct. PD DEC PY 2012 VL 94 IS 12 BP 3538 EP 3545 DI 10.1016/j.compstruct.2012.05.032 PG 8 WC Materials Science, Composites SC Materials Science GA 995XZ UT WOS:000308049900012 ER PT J AU Delcourt, DC Seki, K Terada, N Moore, TE AF Delcourt, D. C. Seki, K. Terada, N. Moore, T. E. TI Centrifugally stimulated exospheric ion escape at Mercury SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID MESSENGER OBSERVATIONS; ACCELERATION; FIELD; MODEL; MAGNETOSPHERE; IONOSPHERE AB We investigate the transport of ions in the low-altitude magnetosphere of Mercury. We show that, because of small spatial scales, the centrifugal effect due to curvature of the E X B drift paths can lead to significant particle energization in the parallel direction. We demonstrate that because of this effect, ions with initial speed smaller than the escape speed such as those produced via thermal desorption can overcome gravity and escape into the magnetosphere. The escape route of this low-energy exosphere originating material is largely controlled by the magnetospheric convection rate. This escape route spreads over a narrower range of altitudes when the convection rate increases. Bulk transport of low-energy planetary material thus occurs within a limited region of space once moderate magnetospheric convection is established. These results suggest that, via release of material otherwise gravitationally trapped, the E X B related centrifugal acceleration is an important mechanism for the net supply of plasma to the magnetosphere of Mercury. Citation: Delcourt, D. C., K. Seki, N. Terada, and T. E. Moore (2012), Centrifugally stimulated exospheric ion escape at Mercury, Geophys. Res. Lett., 39, L22105, doi:10.1029/2012GL054085. C1 [Delcourt, D. C.] CNRS, LPP, FR-94107 St Maur Des Fosses, France. [Seki, K.] Nagoya Univ, STELAB, Nagoya, Aichi 4648601, Japan. [Terada, N.] Tohoku Univ, Dept Geophys, Sendai, Miyagi 980, Japan. [Moore, T. E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Delcourt, DC (reprint author), CNRS, LPP, 4 Ave Neptune, FR-94107 St Maur Des Fosses, France. EM dominique.delcourt@lpp.polytechnique.fr RI Moore, Thomas/D-4675-2012 OI Moore, Thomas/0000-0002-3150-1137 NR 20 TC 4 Z9 4 U1 0 U2 7 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD NOV 30 PY 2012 VL 39 AR L22105 DI 10.1029/2012GL054085 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 047LH UT WOS:000311841800007 ER PT J AU Rodriguez, JAP Bourke, M Tanaka, KL Miyamoto, H Kargel, J Baker, V Fairen, AG Davies, RJ Bridget, L Santiago, RL Hernandez, MZ Berman, DC AF Rodriguez, J. A. P. Bourke, Mary Tanaka, Kenneth L. Miyamoto, Hideaki Kargel, Jeffrey Baker, Victor Fairen, Alberto G. Davies, Richard J. Bridget, Lynne Linares Santiago, Rogelio Zarroca Hernandez, Mario Berman, Daniel C. TI Infiltration of Martian outflow channel floodwaters into lowland cavernous systems SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID SOUTH CASPIAN BASIN; NORTHERN PLAINS; MUD VOLCANISM; MARS; GEOMORPHOLOGY; EMPLACEMENT; RELEASE; HISTORY; OCEAN; WATER AB The hydrosphere of Mars has remained mostly concealed within the subsurface for the past similar to 3.5 Gyr. Localized rupturing of the permafrost-capped crust led to voluminous groundwater discharges that carved some of the largest known channels in the solar system. However, our knowledge of the nature of the flows and their ultimate fate remains incomplete, partly because diagnostic landforms at outflow channel termini have been largely destroyed or buried. The Hebrus Valles outflow channels were excavated by fluid discharges that emanated from two point sources, and they mostly terminate in systems of fractures and depressions within the northern plains. Our investigation indicates that outflow channel floodwaters were captured and reabsorbed into the subsurface in zones where caverns developed within the northern plains. These findings imply that the study region comprises the only known location in the Martian northern lowlands where the fate of outflow channel discharges can be assessed with confidence. We propose that evacuation of subsurface materials via mud volcanism was an important process in cavern formation. Our conceptual model provides a hypothesis to account for the fate of sediments and fluids from some of the Martian outflow channels. It also reveals a mechanism for lowland cavern formation and upper crustal volatile enrichment after the development of the Martian global cryosphere. Citation: Rodriguez, J. A. P., et al. (2012), Infiltration of Martian outflow channel floodwaters into lowland cavernous systems, Geophys. Res. Lett., 39, L22201, doi: 10.1029/2012GL053225. C1 [Rodriguez, J. A. P.; Bourke, Mary; Berman, Daniel C.] Planetary Sci Inst, Tucson, AZ 85719 USA. [Bourke, Mary] Trinity Coll Dublin, Dept Geog, Dublin, Ireland. [Tanaka, Kenneth L.] US Geol Survey, Astrogeol Sci Ctr, Flagstaff, AZ 86001 USA. [Miyamoto, Hideaki] Univ Tokyo, Univ Museum, Tokyo 1138654, Japan. [Kargel, Jeffrey; Baker, Victor] Univ Arizona, Dept Hydrol & Water Resources, Tucson, AZ 85721 USA. [Fairen, Alberto G.] NASA, Ames Res Ctr, Space Sci & Astrobiol Div, Moffett Field, CA 94035 USA. [Davies, Richard J.] Univ Durham, Dept Earth Sci, Ctr Res Earth Energy Syst, Durham, England. [Bridget, Lynne] Univ Auckland, Inst Earth Sci & Engn, Auckland 1, New Zealand. [Linares Santiago, Rogelio; Zarroca Hernandez, Mario] Univ Autonoma Barcelona, Dept Geol, Unitat Geodinam Externa & Hidrogeol, E-08193 Barcelona, Spain. RP Rodriguez, JAP (reprint author), Planetary Sci Inst, 1700 E Ft Lowell Rd,Ste 106, Tucson, AZ 85719 USA. EM alexis@psi.edu RI Miyamoto, Hideaki/B-9666-2008; Bourke, Mary/I-4387-2012; OI Bourke, Mary/0000-0002-0424-0322; Zarroca, Mario/0000-0001-6907-1892 NR 47 TC 3 Z9 3 U1 0 U2 17 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD NOV 30 PY 2012 VL 39 AR L22201 DI 10.1029/2012GL053225 PG 6 WC Geosciences, Multidisciplinary SC Geology GA 047LH UT WOS:000311841800001 ER PT J AU Shepherd, A Ivins, ER Geruo, A Barletta, VR Bentley, MJ Bettadpur, S Briggs, KH Bromwich, DH Forsberg, R Galin, N Horwath, M Jacobs, S Joughin, I King, MA Lenaerts, JTM Li, JL Ligtenberg, SRM Luckman, A Luthcke, SB McMillan, M Meister, R Milne, G Mouginot, J Muir, A Nicolas, JP Paden, J Payne, AJ Pritchard, H Rignot, E Rott, H Sorensen, LS Scambos, TA Scheuchl, B Schrama, EJO Smith, B Sundal, AV van Angelen, JH van de Berg, WJ van den Broeke, MR Vaughan, DG Velicogna, I Wahr, J Whitehouse, PL Wingham, DJ Yi, DH Young, D Zwally, HJ AF Shepherd, Andrew Ivins, Erik R. Geruo, A. Barletta, Valentina R. Bentley, Mike J. Bettadpur, Srinivas Briggs, Kate H. Bromwich, David H. Forsberg, Rene Galin, Natalia Horwath, Martin Jacobs, Stan Joughin, Ian King, Matt A. Lenaerts, Jan T. M. Li, Jilu Ligtenberg, Stefan R. M. Luckman, Adrian Luthcke, Scott B. McMillan, Malcolm Meister, Rakia Milne, Glenn Mouginot, Jeremie Muir, Alan Nicolas, Julien P. Paden, John Payne, Antony J. Pritchard, Hamish Rignot, Eric Rott, Helmut Sorensen, Louise Sandberg Scambos, Ted A. Scheuchl, Bernd Schrama, Ernst J. O. Smith, Ben Sundal, Aud V. van Angelen, Jan H. van de Berg, Willem J. van den Broeke, Michiel R. Vaughan, David G. Velicogna, Isabella Wahr, John Whitehouse, Pippa L. Wingham, Duncan J. Yi, Donghui Young, Duncan Zwally, H. Jay TI A Reconciled Estimate of Ice-Sheet Mass Balance SO SCIENCE LA English DT Article ID PINE ISLAND GLACIER; RELATIVE SEA-LEVEL; ANTARCTIC PENINSULA; WEST ANTARCTICA; ISOSTATIC-ADJUSTMENT; OCEAN CIRCULATION; ELEVATION CHANGE; GREENLAND; MODEL; SHELF AB We combined an ensemble of satellite altimetry, interferometry, and gravimetry data sets using common geographical regions, time intervals, and models of surface mass balance and glacial isostatic adjustment to estimate the mass balance of Earth's polar ice sheets. We find that there is good agreement between different satellite methods-especially in Greenland and West Antarctica-and that combining satellite data sets leads to greater certainty. Between 1992 and 2011, the ice sheets of Greenland, East Antarctica, West Antarctica, and the Antarctic Peninsula changed in mass by -142 +/- 49, +14 +/- 43, -65 +/- 26, and -20 +/- 14 gigatonnes year(-1), respectively. Since 1992, the polar ice sheets have contributed, on average, 0.59 +/- 0.20 millimeter year(-1) to the rate of global sea-level rise. C1 [Shepherd, Andrew; Briggs, Kate H.; Sundal, Aud V.] Univ Leeds, Sch Earth & Environm, Leeds LS2 9JT, W Yorkshire, England. [Ivins, Erik R.; Velicogna, Isabella] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Geruo, A.; Wahr, John] Univ Colorado, Dept Phys, Boulder, CO 80309 USA. [Barletta, Valentina R.; Forsberg, Rene; Sorensen, Louise Sandberg] Tech Univ Denmark, DTU SPACE, Geodynam Dept, Natl Space Inst, DK-2880 Lyngby, Denmark. [Bentley, Mike J.; Whitehouse, Pippa L.] Univ Durham, Dept Geog, Durham DH1 3LE, England. [Bettadpur, Srinivas] Univ Texas Austin, Ctr Space Res, Austin, TX 78759 USA. [Bromwich, David H.; Nicolas, Julien P.] Ohio State Univ, Byrd Polar Res Ctr, Polar Meteorol Grp, Columbus, OH 43210 USA. [Bromwich, David H.; Nicolas, Julien P.] Ohio State Univ, Dept Geog, Atmospher Sci Program, Columbus, OH 43210 USA. [Galin, Natalia; Meister, Rakia; Muir, Alan; Wingham, Duncan J.] UCL, Dept Earth Sci, Ctr Polar Observat & Modelling, London WC1E 6BT, England. [Horwath, Martin] Tech Univ Munich, Inst Astron & Phys Geodasie, D-80333 Munich, Germany. [Jacobs, Stan] Lamont Doherty Earth Observ, Palisades, NY 10964 USA. [Joughin, Ian; Smith, Ben] Univ Washington, Appl Phys Lab, Polar Sci Ctr, Seattle, WA 98105 USA. [King, Matt A.] Newcastle Univ, Sch Civil Engn & Geosci, Newcastle Upon Tyne NE1 7RU, Tyne & Wear, England. [Lenaerts, Jan T. M.; Ligtenberg, Stefan R. M.; van Angelen, Jan H.; van de Berg, Willem J.; van den Broeke, Michiel R.] Univ Utrecht, Inst Marine & Atmospher Res, Utrecht, Netherlands. [Li, Jilu; Paden, John] Univ Kansas, Ctr Remote Sensing Ice Sheets, Lawrence, KS 66045 USA. [Luckman, Adrian] Swansea Univ, Coll Sci, Dept Geog, Swansea SA2 8PP, W Glam, Wales. [Luthcke, Scott B.] NASA, Goddard Space Flight Ctr, Planetary Geodynam Lab, Greenbelt, MD 20771 USA. [Milne, Glenn] Univ Ottawa, Dept Earth Sci, Ottawa, ON K1N 6N5, Canada. [Mouginot, Jeremie; Rignot, Eric; Velicogna, Isabella] Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA 92697 USA. [Payne, Antony J.] Univ Bristol, Sch Geog Sci, Bristol BS8 1SS, Avon, England. [Pritchard, Hamish; Vaughan, David G.] British Antarctic Survey, Cambridge CB3 0ET, England. [Rott, Helmut] Univ Innsbruck, Inst Meteorol & Geophys, A-6020 Innsbruck, Austria. [Scambos, Ted A.] Univ Colorado, Natl Snow & Ice Data Ctr, Boulder, CO 80309 USA. [Schrama, Ernst J. O.] Delft Univ Technol, Fac Aerosp Engn, NL-2629 HS Delft, Netherlands. [Yi, Donghui] NASA, Goddard Space Flight Ctr, Cryospher Sci Lab, SGT Inc, Greenbelt, MD 20771 USA. [Young, Duncan] Univ Texas Austin, Inst Geophys, Austin, TX 78759 USA. [Zwally, H. Jay] NASA, Goddard Space Flight Ctr, Cryospher Sci Lab, Greenbelt, MD 20771 USA. [King, Matt A.] Univ Tasmania, Sch Geog & Environm Studies, Hobart, Tas 7001, Australia. RP Shepherd, A (reprint author), Univ Leeds, Sch Earth & Environm, Leeds LS2 9JT, W Yorkshire, England. EM ashepherd@leeds.ac.uk; erik.r.ivins@jpl.nasa.gov RI Bentley, Michael/F-7386-2011; King, Matt/B-4622-2008; payne, antony/A-8916-2008; Horwath, Martin/F-9239-2011; van de Berg, Willem Jan/H-4385-2011; Vaughan, David/C-8348-2011; Joughin, Ian/A-2998-2008; Rignot, Eric/A-4560-2014; Van den Broeke, Michiel/F-7867-2011; Sorensen, Louise/E-5282-2014; Young, Duncan/G-6256-2010; McMillan, Malcolm/K-7712-2014; Bettadpur, Srinivas/M-3744-2014; Lenaerts, Jan/D-9423-2012; Mouginot, Jeremie/G-7045-2015; Bromwich, David/C-9225-2016 OI Bentley, Michael/0000-0002-2048-0019; King, Matt/0000-0001-5611-9498; Luckman, Adrian/0000-0002-9618-5905; Whitehouse, Pippa/0000-0002-9092-3444; payne, antony/0000-0001-8825-8425; Horwath, Martin/0000-0001-5797-244X; Joughin, Ian/0000-0001-6229-679X; Rignot, Eric/0000-0002-3366-0481; Van den Broeke, Michiel/0000-0003-4662-7565; Sorensen, Louise/0000-0002-3771-4061; Young, Duncan/0000-0002-6866-8176; Lenaerts, Jan/0000-0003-4309-4011; FU Phillip Leverhulme Prize award; European Union [125]; NASA [NNX09AE47G, NNX08AD64G]; Netherlands Organization for Scientific Research; Netherlands Polar Program; UK Natural Environment Research Council; NSF; Lamont Doherty Earth Observatory FX This Ice Sheet Mass Balance Exercise (IMBIE) was facilitated by the European Space Agency and NASA and by a Phillip Leverhulme Prize awarded to A. S. The work was additionally supported by the European Union Framework Programme 7 ice2sea program (ice2sea publication 125), the Lamont Doherty Earth Observatory, NASA (grants NNX09AE47G and NNX08AD64G), the Netherlands Organization for Scientific Research, the Netherlands Polar Program, the UK Natural Environment Research Council, and the NSF. Antarctic glacier ice thickness data used in the IOM calculations were acquired by NASA IceBridge and the Centro de Estudios Cientifico Chile, and additional estimates were provided by J. Bamber and J. Griggs. E. van Meijgaard provided assistance with the RACMO model. NR 93 TC 475 Z9 479 U1 29 U2 410 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 J9 SCIENCE JI Science PD NOV 30 PY 2012 VL 338 IS 6111 BP 1183 EP 1189 DI 10.1126/science.1228102 PG 7 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 045AL UT WOS:000311666200039 PM 23197528 ER PT J AU Ackermann, M Ajello, M Allafort, A Schady, P Baldini, L Ballet, J Barbiellini, G Bastieri, D Bellazzini, R Blandford, RD Bloom, ED Borgland, AW Bottacini, E Bouvier, A Bregeon, J Brigida, M Bruel, P Buehler, R Buson, S Caliandro, GA Cameron, RA Caraveo, PA Cavazzuti, E Cecchi, C Charles, E Chaves, RCG Chekhtman, A Cheung, CC Chiang, J Chiaro, G Ciprini, S Claus, R Cohen-Tanugi, J Conrad, J Cutini, S D'Ammando, F de Palma, F Dermer, CD Digel, SW Silva, EDE Domnguez, A Drell, PS Drlica-Wagner, A Favuzzi, C Fegan, SJ Focke, WB Franckowiak, A Fukazawa, Y Funk, S Fusco, P Gargano, F Gasparrini, D Gehrels, N Germani, S Giglietto, N Giordano, F Giroletti, M Glanzman, T Godfrey, G Grenier, IA Grove, JE Guiriec, S Gustafsson, M Hadasch, D Hayashida, M Hays, E Jackson, MS Jogler, T Kataoka, J Knodlseder, J Kuss, M Lande, J Larsson, S Latronico, L Longo, F Loparco, F Lovellette, MN Lubrano, P Mazziotta, MN McEnery, JE Mehault, J Michelson, PF Mizuno, T Monte, C Monzani, ME Morselli, A Moskalenko, IV Murgia, S Tramacere, A Nuss, E Greiner, J Ohno, M Ohsugi, T Omodei, N Orienti, M Orlando, E Ormes, JF Paneque, D Perkins, JS Pesce-Rollins, M Piron, F Pivato, G Porter, TA Raino, S Rando, R Razzano, M Razzaque, S Reimer, A Reimer, O Reyes, LC Ritz, S Rau, A Romoli, C Roth, M Sanchez-Conde, M Sanchez, DA Scargle, JD Sgro, C Siskind, EJ Spandre, G Spinelli, P Stawarz, L Suson, DJ Takahashi, H Tanaka, T Thayer, JG Thompson, DJ Tibaldo, L Tinivella, M Torres, DF Tosti, G Troja, E Usher, TL Vandenbroucke, J Vasileiou, V Vianello, G Vitale, V Waite, AP Winer, BL Wood, KS Wood, M AF Ackermann, M. Ajello, M. Allafort, A. Schady, P. Baldini, L. Ballet, J. Barbiellini, G. Bastieri, D. Bellazzini, R. Blandford, R. D. Bloom, E. D. Borgland, A. W. Bottacini, E. Bouvier, A. Bregeon, J. Brigida, M. Bruel, P. Buehler, R. Buson, S. Caliandro, G. A. Cameron, R. A. Caraveo, P. A. Cavazzuti, E. Cecchi, C. Charles, E. Chaves, R. C. G. Chekhtman, A. Cheung, C. C. Chiang, J. Chiaro, G. Ciprini, S. Claus, R. Cohen-Tanugi, J. Conrad, J. Cutini, S. D'Ammando, F. de Palma, F. Dermer, C. D. Digel, S. W. do Couto e Silva, E. Domnguez, A. Drell, P. S. Drlica-Wagner, A. Favuzzi, C. Fegan, S. J. Focke, W. B. Franckowiak, A. Fukazawa, Y. Funk, S. Fusco, P. Gargano, F. Gasparrini, D. Gehrels, N. Germani, S. Giglietto, N. Giordano, F. Giroletti, M. Glanzman, T. Godfrey, G. Grenier, I. A. Grove, J. E. Guiriec, S. Gustafsson, M. Hadasch, D. Hayashida, M. Hays, E. Jackson, M. S. Jogler, T. Kataoka, J. Knoedlseder, J. Kuss, M. Lande, J. Larsson, S. Latronico, L. Longo, F. Loparco, F. Lovellette, M. N. Lubrano, P. Mazziotta, M. N. McEnery, J. E. Mehault, J. Michelson, P. F. Mizuno, T. Monte, C. Monzani, M. E. Morselli, A. Moskalenko, I. V. Murgia, S. Tramacere, A. Nuss, E. Greiner, J. Ohno, M. Ohsugi, T. Omodei, N. Orienti, M. Orlando, E. Ormes, J. F. Paneque, D. Perkins, J. S. Pesce-Rollins, M. Piron, F. Pivato, G. Porter, T. A. Raino, S. Rando, R. Razzano, M. Razzaque, S. Reimer, A. Reimer, O. Reyes, L. C. Ritz, S. Rau, A. Romoli, C. Roth, M. Sanchez-Conde, M. Sanchez, D. A. Scargle, J. D. Sgro, C. Siskind, E. J. Spandre, G. Spinelli, P. Stawarz, Lukasz Suson, D. J. Takahashi, H. Tanaka, T. Thayer, J. G. Thompson, D. J. Tibaldo, L. Tinivella, M. Torres, D. F. Tosti, G. Troja, E. Usher, T. L. Vandenbroucke, J. Vasileiou, V. Vianello, G. Vitale, V. Waite, A. P. Winer, B. L. Wood, K. S. Wood, M. TI The Imprint of the Extragalactic Background Light in the Gamma-Ray Spectra of Blazars SO SCIENCE LA English DT Article ID ACTIVE GALACTIC NUCLEI; LARGE-AREA TELESCOPE; 1ST STARS; RADIATIVE-TRANSFER; UNIVERSE; ABSORPTION; REDSHIFT; OPACITY; FIELDS; GLAST AB The light emitted by stars and accreting compact objects through the history of the universe is encoded in the intensity of the extragalactic background light (EBL). Knowledge of the EBL is important to understand the nature of star formation and galaxy evolution, but direct measurements of the EBL are limited by galactic and other foreground emissions. Here, we report an absorption feature seen in the combined spectra of a sample of gamma-ray blazars out to a redshift of z similar to 1.6. This feature is caused by attenuation of gamma rays by the EBL at optical to ultraviolet frequencies and allowed us to measure the EBL flux density in this frequency band. C1 [Ajello, M.; Allafort, A.; Blandford, R. D.; Bloom, E. D.; Borgland, A. W.; Bottacini, E.; Buehler, R.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; Digel, S. W.; do Couto e Silva, E.; Drell, P. S.; Drlica-Wagner, A.; Focke, W. B.; Franckowiak, A.; Funk, S.; Glanzman, T.; Godfrey, G.; Hayashida, M.; Jogler, T.; Lande, J.; Michelson, P. F.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Omodei, N.; Orlando, E.; Paneque, D.; Porter, T. A.; Reimer, A.; Reimer, O.; Sanchez-Conde, M.; Tanaka, T.; Thayer, J. G.; Usher, T. L.; Vandenbroucke, J.; Vianello, G.; Waite, A. P.; Wood, M.] Stanford Univ, Dept Phys, Kavli Inst Particle Astrophys & Cosmol, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA. [Ajello, M.; Allafort, A.; Blandford, R. D.; Bloom, E. D.; Borgland, A. W.; Bottacini, E.; Buehler, R.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; Digel, S. W.; do Couto e Silva, E.; Drell, P. S.; Drlica-Wagner, A.; Focke, W. B.; Franckowiak, A.; Funk, S.; Glanzman, T.; Godfrey, G.; Hayashida, M.; Jogler, T.; Lande, J.; Michelson, P. F.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Omodei, N.; Orlando, E.; Paneque, D.; Porter, T. A.; Reimer, A.; Reimer, O.; Sanchez-Conde, M.; Tanaka, T.; Thayer, J. G.; Usher, T. L.; Vandenbroucke, J.; Vianello, G.; Waite, A. P.; Wood, M.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA. [Ackermann, M.] Deutsch Elektronen Synchrotron DESY, D-15738 Zeuthen, Germany. [Ajello, M.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Schady, P.; Greiner, J.; Rau, A.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Baldini, L.] Univ Pisa, I-56127 Pisa, Italy. [Baldini, L.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy. [Ballet, J.; Chaves, R. C. G.; Grenier, I. A.] Univ Paris Diderot, CNRS, CEA IRFU, Lab AIM,Serv Astrophys,CEA Saclay, 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, Dipartmento Fis, I-34127 Trieste, Italy. 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[Cecchi, C.; Ciprini, S.; Germani, S.; Lubrano, P.; Tosti, G.] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy. [Chekhtman, A.; Razzaque, S.] George Mason Univ, Coll Sci, Ctr Earth Observing & Space Res, Fairfax, VA 22030 USA. [Cheung, C. C.] Natl Acad Sci, Natl Res Council, Washington, DC 20001 USA. [Chiaro, G.] Univ Padua, Ist Nazl Fis Nucl, I-35131 Padua, Italy. [Chiaro, G.] Univ Padua, Dipartimento Fis & Astron G Galilei, I-35131 Padua, Italy. [Ciprini, S.] ASI Sci Data Ctr, I-00044 Rome, Italy. [Cohen-Tanugi, J.; Mehault, J.; Nuss, E.; Piron, F.; Vasileiou, V.] Univ Montpellier 2, CNRS, IN2P3, Lab Universe & Particules Montpellier, Montpellier, France. [Conrad, J.; Larsson, S.] Stockholm Univ, Dept Phys, AlbaNova, SE-10691 Stockholm, Sweden. [Conrad, J.; Jackson, M. S.; Larsson, S.] Oskar Klein Ctr Cosmoparticle Phys, AlbaNova, SE-10691 Stockholm, Sweden. [Conrad, J.] Royal Swedish Acad Sci Res, SE-10691 Stockholm, Sweden. [D'Ammando, F.] IASF Palermo, I-90146 Palermo, Italy. [D'Ammando, F.] INAF Ist Astrofis Spaziale & Fis Cosm, I-00133 Rome, Italy. [Dermer, C. D.; Grove, J. E.; Lovellette, M. N.; Wood, K. S.] USN, Res Lab, Div Space Sci, Washington, DC 20375 USA. [Fukazawa, Y.; Takahashi, H.] Hiroshima Univ, Dept Phys Sci, Hiroshima 7398526, Japan. [Gehrels, N.; Guiriec, S.; Hays, E.; McEnery, J. E.; Perkins, J. S.; Thompson, D. J.; Troja, E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Giroletti, M.; Orienti, M.] INAF Ist Radioastron, I-40129 Bologna, Italy. [Hayashida, M.] Kyoto Univ, Grad Sch Sci, Dept Astron, Sakyo Ku, Kyoto 6068502, Japan. [Jackson, M. S.] Royal Inst Technol KTH, Dept Phys, AlbaNova, SE-10691 Stockholm, Sweden. [Kataoka, J.] Waseda Univ, Res Inst Sci & Engn, Shinjuku Ku, Tokyo 1698555, Japan. [Knoedlseder, J.] IRAP, CNRS, F-31028 Toulouse 4, France. [Knoedlseder, J.] Univ Toulouse, UPS OMP, IRAP, GAHEC, Toulouse, France. [Larsson, S.] Stockholm Univ, Dept Astron, SE-10691 Stockholm, Sweden. [Latronico, L.] Ist Nazl Fis Nucl, Sez Torino, I-10125 Turin, Italy. [McEnery, J. E.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA. [McEnery, J. E.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Mizuno, T.; Ohsugi, T.] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Hiroshima 7398526, Japan. [Morselli, A.; Vitale, V.] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, I-00133 Rome, Italy. [Tramacere, A.] INTEGRAL Sci Data Ctr, CH-1290 Versoix, Switzerland. [Ohno, M.; Stawarz, Lukasz] JAXA, Inst Space & Astronaut Sci, Chuo Ku, Sagamihara, Kanagawa 2525210, Japan. [Ormes, J. F.] Univ Denver, Dept Phys & Astron, Denver, CO 80208 USA. [Paneque, D.] Max Planck Inst Phys & Astrophys, D-80805 Munich, Germany. [Perkins, J. S.] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA. [Perkins, J. S.] Univ Maryland Baltimore Cty, Ctr Space Sci & Technol, Baltimore, MD 21250 USA. [Perkins, J. S.] CRESST, Greenbelt, MD 20771 USA. [Perkins, J. S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Perkins, J. S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Reimer, A.; Reimer, O.] Leopold Franzens Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria. [Reimer, A.; Reimer, O.] Leopold Franzens Univ Innsbruck, Inst Theoret Phys, A-6020 Innsbruck, Austria. [Reyes, L. C.] Calif Polytech State Univ San Luis Obispo, Dept Phys, San Luis Obispo, CA 93401 USA. [Roth, M.] Univ Washington, Dept Phys, Seattle, WA 98195 USA. [Sanchez, D. A.] Max Planck Inst Kernphys, D-69029 Heidelberg, Germany. [Scargle, J. D.] NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA. [Siskind, E. J.] NYCB Real Time Comp Inc, Lattingtown, NY 11560 USA. [Stawarz, Lukasz] Jagiellonian Univ, Astron Observ, PL-30244 Krakow, Poland. [Suson, D. J.] Purdue Univ Calumet, Dept Chem & Phys, Hammond, IN 46323 USA. [Torres, D. F.] ICREA, Barcelona, Spain. [Vianello, G.] CIFS, I-10133 Turin, Italy. [Vitale, V.] Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy. [Winer, B. L.] Ohio State Univ, Dept Phys, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA. RP Ajello, M (reprint author), Stanford Univ, Dept Phys, Kavli Inst Particle Astrophys & Cosmol, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA. EM majello@slac.stanford.edu; buehler@stanford.edu; anita.reimer@uibk.ac.at RI Reimer, Olaf/A-3117-2013; Tosti, Gino/E-9976-2013; Rando, Riccardo/M-7179-2013; Hays, Elizabeth/D-3257-2012; Funk, Stefan/B-7629-2015; Loparco, Francesco/O-8847-2015; Gargano, Fabio/O-8934-2015; giglietto, nicola/I-8951-2012; Moskalenko, Igor/A-1301-2007; Mazziotta, Mario /O-8867-2015; Sgro, Carmelo/K-3395-2016; Torres, Diego/O-9422-2016; Orlando, E/R-5594-2016; OI Gasparrini, Dario/0000-0002-5064-9495; Tramacere, Andrea/0000-0002-8186-3793; Baldini, Luca/0000-0002-9785-7726; Sgro', Carmelo/0000-0001-5676-6214; SPINELLI, Paolo/0000-0001-6688-8864; Dominguez, Alberto/0000-0002-3433-4610; Bastieri, Denis/0000-0002-6954-8862; Omodei, Nicola/0000-0002-5448-7577; Pesce-Rollins, Melissa/0000-0003-1790-8018; orienti, monica/0000-0003-4470-7094; Giroletti, Marcello/0000-0002-8657-8852; Cutini, Sara/0000-0002-1271-2924; Reimer, Olaf/0000-0001-6953-1385; Funk, Stefan/0000-0002-2012-0080; Loparco, Francesco/0000-0002-1173-5673; Gargano, Fabio/0000-0002-5055-6395; giglietto, nicola/0000-0002-9021-2888; Moskalenko, Igor/0000-0001-6141-458X; Mazziotta, Mario /0000-0001-9325-4672; Torres, Diego/0000-0002-1522-9065; Caraveo, Patrizia/0000-0003-2478-8018 FU K. A. Wallenberg Foundation; Fermi guest investigator program [31117, 51258] FX M. A. acknowledges generous support from the Fermi guest investigator program (proposals ID 31117 and 51258) and the Swift and the Gamma-Ray Burst Optical/Near-Infrared Detector (GROND) teams for observing similar to 100 Fermi blazars in an effort to constrain their redshifts. 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. J. Conrad is funded by a grant from the K. A. Wallenberg Foundation. E. Troja is a NASA Postdoctoral Program Fellow. NR 45 TC 103 Z9 103 U1 1 U2 24 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 J9 SCIENCE JI Science PD NOV 30 PY 2012 VL 338 IS 6111 BP 1190 EP 1192 DI 10.1126/science.1227160 PG 3 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 045AL UT WOS:000311666200040 PM 23118013 ER PT J AU Bowman, K Henze, DK AF Bowman, K. Henze, D. K. TI Attribution of direct ozone radiative forcing to spatially resolved emissions SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID SATELLITE MEASUREMENTS; TROPOSPHERIC OZONE; TRANSPORT; CHEMISTRY; POLLUTION; SECTORS AB Quantifying the dependence of ozone direct radiative forcing (DRF) on the mixture and spatial distribution of precursor emissions is a key step towards understanding the impact of air quality standards on climate. We use here a combination of satellite observations of ozone and its radiative effect in conjunction with an adjoint chemical transport model to determine the ozone DRF due to global, anthropogenic NOx, CO, and non-methane hydrocarbons (NMHC) emissions regionally at 2 degrees x 2.5 degrees regions resolution. We show that 8% of the ozone DRF from the sum of all these emissions can be attributed to 15 regions, which are predominantly located in China and the United States (US). To achieve an equivalent reduction in ozone DRF, necessary emission reductions for each precursor vary intra-continentally by a factor of 3-10 and globally by over an order of magnitude. The contribution of NOx emissions to ozone DRF relative to CO and NMHC emissions within individual regions varies globally by nearly a factor of two. Citation: Bowman, K., and D. K. Henze (2012), Attribution of direct ozone radiative forcing to spatially resolved emissions, Geophys. Res. Lett., 39, L22704, doi: 10.1029/2012GL053274. C1 [Bowman, K.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Henze, D. K.] Univ Colorado, Dept Mech Engn, Boulder, CO 80309 USA. RP Bowman, K (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM kevin.w.bowman@jpl.nasa.gov FU NASA; NASA AQAST [NNX11AI54G]; AURA [NNH07ZDA001N]; New Investigator Program [NNX10AR06G]; HEC FX This research was carried out in part at the Jet Propulsion Laboratory, California Institute of Technology, under contract from NASA. We would like thank Helen Worden (NCAR) and the TES team for the IRK products. We acknowledge sponsorship from NASA AQAST (NNX11AI54G), AURA (NNH07ZDA001N), New Investigator Program (NNX10AR06G) and HEC computing facilities. NR 32 TC 15 Z9 15 U1 0 U2 31 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD NOV 29 PY 2012 VL 39 AR L22704 DI 10.1029/2012GL053274 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 047LG UT WOS:000311841500001 ER PT J AU Wu, H Kimball, JS Elsner, MM Mantua, N Adler, RF Stanford, J AF Wu, Huan Kimball, John S. Elsner, Marketa M. Mantua, Nate Adler, Robert F. Stanford, Jack TI Projected climate change impacts on the hydrology and temperature of Pacific Northwest rivers SO WATER RESOURCES RESEARCH LA English DT Article ID STREAM TEMPERATURE; WATER TEMPERATURE; GLOBAL OPTIMIZATION; UNITED-STATES; MODEL; BASIN; FLOW; PRECIPITATION; VARIABILITY; RESOURCES AB A dominant river-tracing-based streamflow and temperature (DRTT) model was developed by coupling stream thermal dynamics with a source-sink routing model. The DRTT model was applied using 1/16 degree (similar to 6 km) resolution gridded daily surface meteorology inputs over a similar to 988,000 km(2) Pacific Northwest (PNW) domain to produce regional daily streamflow and temperature simulations from 1996 to 2005. The DRTT results showed favorable performance for simulation of daily stream temperature (mean R-2 = 0.72 and root-mean-square error = 2.35 degrees C) and discharge (mean R-2 = 0.52 and annual relative error 14%) against observations from 12 PNW streams. The DRTT was then applied with a macroscale hydrologic model to predict streamflow and temperature changes under historical (1980s) and future (2020s, 2040s, and 2080s) climate change scenarios (IPCC AR4) as they may affect current and future patterns of freshwater salmon habitat and associated productivity of PNW streams. The model projected a 3.5% decrease in mean annual streamflow for the 2020s and 0.6% and 5.5% increases for the 2040s and 2080s, respectively, with projected increase in mean annual stream temperatures from 0.55 degrees C (2020s) to 1.68 degrees C (2080s). However, summer streamflow decreased from 19.3% (2020s) to 30.3% (2080s), while mean summer stream temperatures warmed from 0.92 degrees C to 2.10 degrees C. The simulations indicate that projected climate change will have greater impacts on snow dominant streams, with lower summer streamflows and warmer summer stream temperature changes relative to transient and rain dominant regimes. Lower summer flows combined with warmer stream temperatures suggest a future with widespread increased summertime thermal stress for coldwater fish in the PNW region. C1 [Wu, Huan; Adler, Robert F.] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20704 USA. [Wu, Huan; Adler, Robert F.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Kimball, John S.] Univ Montana, Flathead Lake Biol Stn, Polson, MT 59860 USA. [Kimball, John S.] Univ Montana, Coll Forestry & Conservat, Numer Terradynam Simulat Grp, Missoula, MT 59812 USA. [Elsner, Marketa M.; Mantua, Nate] Univ Washington, Climate Impacts Grp, Joint Inst Study Atmosphere & Ocean, Seattle, WA 98195 USA. [Mantua, Nate] Univ Washington, Sch Aquat & Fisheries Sci, Seattle, WA 98195 USA. RP Wu, H (reprint author), Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, 5825 Univ Ct,Ste 4001, College Pk, MD 20704 USA. EM huanwu@umd.edu RI Wu, Huan/K-1003-2013 OI Wu, Huan/0000-0003-2920-8860 FU Gordon and Betty Moore Foundation FX This work was conducted at the University of Montana (UMT) with financial support from the Gordon and Betty Moore Foundation. The authors would like to thank Wilfred Wollheim and the two anonymous reviewers for their very constructive comments and suggestions for improving the paper. The authors would also like to thank John Lucotch and Niels Maumenee for assistance in data processing. NR 63 TC 28 Z9 28 U1 2 U2 75 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0043-1397 J9 WATER RESOUR RES JI Water Resour. Res. PD NOV 29 PY 2012 VL 48 AR W11530 DI 10.1029/2012WR012082 PG 23 WC Environmental Sciences; Limnology; Water Resources SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Water Resources GA 047OQ UT WOS:000311850700001 ER PT J AU Rohling, EJ Sluijs, A Dijkstra, HA Kohler, P de Wal, RSWV von der Heydt, AS Beerling, DJ Berger, A Bijl, PK Crucifix, M DeConto, R Drijfhout, SS Fedorov, A Foster, GL Ganopolski, A Hansen, J Honisch, B Hooghiemstra, H Huber, M Huybers, P Knutti, R Lea, DW Lourens, LJ Lunt, D Masson-Demotte, V Medina-Elizalde, M Otto-Bliesner, B Pagani, M Palike, H Renssen, H Royer, DL Siddall, M Valdes, P Zachos, JC Zeebe, RE AF Rohling, E. J. Sluijs, A. Dijkstra, H. A. Koehler, P. de Wal, R. S. W. van von der Heydt, A. S. Beerling, D. J. Berger, A. Bijl, P. K. Crucifix, M. DeConto, R. Drijfhout, S. S. Fedorov, A. Foster, G. L. Ganopolski, A. Hansen, J. Hoenisch, B. Hooghiemstra, H. Huber, M. Huybers, P. Knutti, R. Lea, D. W. Lourens, L. J. Lunt, D. Masson-Demotte, V. Medina-Elizalde, M. Otto-Bliesner, B. Pagani, M. Paelike, H. Renssen, H. Royer, D. L. Siddall, M. Valdes, P. Zachos, J. C. Zeebe, R. E. CA PALAEOSENS Project Members TI Making sense of palaeoclimate sensitivity SO NATURE LA English DT Article ID CARBON-DIOXIDE CONCENTRATION; GLOBAL CLIMATE SENSITIVITY; EOCENE ATMOSPHERIC CO2; LAST GLACIAL MAXIMUM; PAST 800,000 YEARS; ICE-CORE; TEMPERATURE-VARIATIONS; ANTARCTIC TEMPERATURE; POLAR AMPLIFICATION; EARTHS TEMPERATURE AB Many palaeoclimate studies have quantified pre-anthropogenic climate change to calculate climate sensitivity (equilibrium temperature change in response to radiative forcing change), but a lack of consistent methodologies produces a wide range of estimates and hinders comparability of results. Here we present a stricter approach, to improve intercomparison of palaeoclimate sensitivity estimates in a manner compatible with equilibrium projections for future climatechange. Over the past 65 million years, this reveals a climate sensitivity (in KW-1 m(2)) of 0.3-1.9 or 0.6-1.3 at 95% or 68% probability, respectively. The latter implies a warming of 2.2-4.8 K per doubling of atmospheric CO2, which agrees with IPCC estimates. C1 [Rohling, E. J.; Foster, G. L.] Univ Southampton, Sch Ocean & Earth Sci, Natl Oceanog Ctr, Southampton SO14 3ZH, Hants, England. [Rohling, E. J.] Australian Natl Univ, Res Sch Earth Sci, Canberra, ACT 0200, Australia. [Sluijs, A.; Bijl, P. K.; Lourens, L. J.] Univ Utrecht, Dept Earth Sci, Fac Geosci, NL-3584 CD Utrecht, Netherlands. [Dijkstra, H. A.; de Wal, R. S. W. van; von der Heydt, A. S.] Univ Utrecht, Inst Marine & Atmospher Res Utrecht, NL-3584 CC Utrecht, Netherlands. [Koehler, P.] Alfred Wegener Inst Polar & Marine Res AWI, D-27515 Bremerhaven, Germany. [Beerling, D. J.] Univ Sheffield, Dept Anim & Plant Sci, Sheffield S10 2TN, S Yorkshire, England. [Berger, A.; Crucifix, M.] Catholic Univ Louvain, Georges Lemaitre Ctr Earth & Climate Res, Earth & Life Inst, B-1348 Louvain, Belgium. [DeConto, R.] Univ Massachusetts, Dept Geosci, Morrill Sci Ctr 233, Amherst, MA 01003 USA. [Drijfhout, S. S.] Royal Netherlands Meteorol Inst, NL-3730 AE De Bilt, Netherlands. [Fedorov, A.] Yale Univ, Dept Geol & Geophys, New Haven, CT 06520 USA. [Ganopolski, A.] Potsdam Inst Climate Impact Res PIK, D-14412 Potsdam, Germany. [Hansen, J.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Hoenisch, B.] Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY 10964 USA. [Hooghiemstra, H.] Univ Amsterdam, Inst Biodivers & Ecosyst Dynam, NL-1098 XH Amsterdam, Netherlands. [Huber, M.] Purdue Univ, Dept Earth & Atmospher Sci, W Lafayette, IN 47907 USA. [Huybers, P.] Harvard Univ, Dept Earth & Planetary Sci, Cambridge, MA 02138 USA. [Knutti, R.] ETH, Inst Atmospher andClimate Sci, CH-8092 Zurich, Switzerland. [Lea, D. W.] Univ Calif Santa Barbara, Dept Earth Sci, Santa Barbara, CA 93106 USA. [Lunt, D.; Valdes, P.] Univ Bristol, Sch Geog Sci, Bristol BS8 1SS, Avon, England. [Masson-Demotte, V.] LCEA Saclay, LSCE IPSL CEA CNRS UVSQ, UMR 8212, F-91191 Gif Sur Yvette, France. [Medina-Elizalde, M.] Ctr Invest Cient Yucatan, Unidad Ciencias Agua, Cancun 77500, Quintana Roo, Mexico. [Otto-Bliesner, B.] Natl Ctr Atmospher Res, Boulder, CO 80307 USA. [Paelike, H.] Univ Bremen, MARUM, D-28359 Bremen, Germany. [Renssen, H.] Free Univ Amsterdam, Dept Earth Sci, Fac Earth & Life Sci, NL-1081 HV Amsterdam, Netherlands. [Royer, D. L.] Wesleyan Univ, Dept Earth & Environm Sci, Middletown, CT 06459 USA. [Siddall, M.] Univ Bristol, Dept Earth Sci, Bristol BS8 1RJ, Avon, England. [Zeebe, R. E.] Univ Hawaii Manoa, Sch Ocean & Earth Sci & Technol, Dept Oceanog, Honolulu, HI 96822 USA. RP Rohling, EJ (reprint author), Univ Southampton, Sch Ocean & Earth Sci, Natl Oceanog Ctr, Southampton SO14 3ZH, Hants, England. EM e.rohling@noc.soton.ac.uk RI Palike, Heiko/A-6560-2008; Beerling, David/C-2840-2009; Drijfhout, Sybren/I-4230-2016; Dijkstra , Henk /H-2559-2016; Sluijs, Appy/B-3726-2009; Huber, Matthew/A-7677-2008; Kohler, Peter/F-7293-2010; Masson-Delmotte, Valerie/G-1995-2011; van de wal, roderik/D-1705-2011; Knutti, Reto/B-8763-2008; Lunt, Daniel/G-9451-2011; Pagani, Mark/B-3233-2008; Valdes, Paul/C-4129-2013; Hoenisch, Baerbel/C-7530-2013; Ganopolski, Andrey/F-6811-2013; Rohling, Eelco/B-9736-2008; von der Heydt, Anna/B-9250-2008 OI Palike, Heiko/0000-0003-3386-0923; Beerling, David/0000-0003-1869-4314; Sluijs, Appy/0000-0003-2382-0215; Royer, Dana/0000-0003-0976-953X; Huber, Matthew/0000-0002-2771-9977; Kohler, Peter/0000-0003-0904-8484; Masson-Delmotte, Valerie/0000-0001-8296-381X; Knutti, Reto/0000-0001-8303-6700; Lunt, Daniel/0000-0003-3585-6928; Hoenisch, Baerbel/0000-0001-5844-3398; Rohling, Eelco/0000-0001-5349-2158; von der Heydt, Anna/0000-0002-5557-3282 FU Royal Netherlands Academy of Arts and Sciences (KNAW); UK-NERC consortium iGlass [NE/I009906/1]; Australian Laureate Fellowship [FL120100050]; Royal Society Wolfson Research Merit Awards; European Research Council for ERC [259627]; NSF [0902882]; EU [243908] FX This Perspective arose from the first PALAEOSENS workshop in March 2011. We thank the Royal Netherlands Academy of Arts and Sciences (KNAW) for funding and hosting this workshop in Amsterdam, PAGES for their support, and J. Gregory for discussions. This study was supported by the UK-NERC consortium iGlass (NE/I009906/1), and 2012 Australian Laureate Fellowship FL120100050. D.J.B., E.J.R. and P.V. were supported by Royal Society Wolfson Research Merit Awards. A.S. thanks the European Research Council for ERC starting grant 259627, and M.H. acknowledges NSF P2C2 grant 0902882. Some of the work was supported by grant 243908 'Past4Future' of the EU's seventh framework programme; this is Past4Future contribution number 30. NR 99 TC 81 Z9 82 U1 21 U2 278 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 NOV 29 PY 2012 VL 491 IS 7426 BP 683 EP 691 DI 10.1038/nature11574 PG 9 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 044FY UT WOS:000311606000031 ER PT J AU Teanby, NA Irwin, PGJ Nixon, CA de Kok, R Vinatier, S Coustenis, A Sefton-Nash, E Calcutt, SB Flasar, FM AF Teanby, Nicholas A. Irwin, Patrick G. J. Nixon, Conor A. de Kok, Remco Vinatier, Sandrine Coustenis, Athena Sefton-Nash, Elliot Calcutt, Simon B. Flasar, F. Michael TI Active upper-atmosphere chemistry and dynamics from polar circulation reversal on Titan SO NATURE LA English DT Article ID COMPOSITE INFRARED SPECTROMETER; CASSINI/CIRS DATA; TEMPERATURES; MODEL; MESOSPHERE AB Saturn's moon Titan has a nitrogen atmosphere comparable to Earth's, with a surface pressure of 1.4 bar. Numerical models reproduce the tropospheric conditions very well but have trouble explaining the observed middle-atmosphere temperatures, composition and winds(1,2). The top of the middle-atmosphere circulation has been thought to lie at an altitude of 450 to 500 kilometres, where there is a layer of haze that appears to be separated from the main haze deck(3). This 'detached' haze was previously explained as being due to the co-location of peak haze production and the limit of dynamical transport by the circulation's upper branch(4). Here we report a build-up of trace gases over the south pole approximately two years after observing the 2009 post-equinox circulation reversal, from which we conclude that middle-atmosphere circulation must extend to an altitude of at least 600 kilometres. The primary drivers of this circulation are summer-hemisphere heating of haze by absorption of solar radiation and winter-hemisphere cooling due to infrared emission by haze and trace gases(5); our results therefore imply that these effects are important well into the thermosphere (altitudes higher than 500 kilometres). This requires both active upper-atmosphere chemistry, consistent with the detection of high-complexity molecules and ions at altitudes greater than 950 kilometres(6,7), and an alternative explanation for the detached haze, such as a transition in haze particle growth from monomers to fractal structures(8). C1 [Teanby, Nicholas A.; Sefton-Nash, Elliot] Univ Bristol, Sch Earth Sci, Bristol BS8 1RJ, Avon, England. [Irwin, Patrick G. J.; Calcutt, Simon B.] Univ Oxford, Dept Phys, Clarendon Lab, Oxford OX1 3PU, England. [Nixon, Conor A.; Flasar, F. Michael] NASA, Planetary Syst Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [de Kok, Remco] SRON, Netherlands Inst Space Res, NL-3584 CA Utrecht, Netherlands. [Vinatier, Sandrine; Coustenis, Athena] Univ Paris Diderot, LESIA Observ Paris, CNRS, Univ Paris 06, F-92195 Meudon, France. [Sefton-Nash, Elliot] Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90095 USA. RP Teanby, NA (reprint author), Univ Bristol, Sch Earth Sci, Wills Mem Bldg,Queens Rd, Bristol BS8 1RJ, Avon, England. EM n.teanby@bristol.ac.uk RI Nixon, Conor/A-8531-2009; Flasar, F Michael/C-8509-2012; OI Nixon, Conor/0000-0001-9540-9121; Calcutt, Simon/0000-0002-0102-3170; Teanby, Nicholas/0000-0003-3108-5775; Irwin, Patrick/0000-0002-6772-384X FU UK Science and Technology Facilities Council; Leverhulme Trust; NASA Cassini mission FX This work was funded by the UK Science and Technology Facilities Council, the Leverhulme Trust and the NASA Cassini mission. NR 30 TC 23 Z9 23 U1 1 U2 30 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 NOV 29 PY 2012 VL 491 IS 7426 BP 732 EP 735 DI 10.1038/nature11611 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 044FY UT WOS:000311606000039 PM 23192150 ER PT J AU Cooper, OR Gao, RS Tarasick, D Leblanc, T Sweeney, C AF Cooper, Owen R. Gao, Ru-Shan Tarasick, David Leblanc, Thierry Sweeney, Colm TI Long-term ozone trends at rural ozone monitoring sites across the United States, 1990-2010 SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID STRATOSPHERE-TROPOSPHERE EXCHANGE; GROUND-LEVEL OZONE; TRANSPORTED BACKGROUND OZONE; PARTICLE DISPERSION MODEL; ASIAN AIR-POLLUTION; NORTH-AMERICA; SURFACE OZONE; WEST-COAST; METEOROLOGICAL CONTROLS; 15-YEAR CLIMATOLOGY AB This analysis provides an up-to-date assessment of long-term (1990-2010) rural ozone trends using all available data in the western (12 sites) and eastern (41 sites) USA. Rather than focus solely on average ozone values or air quality standard violations, we consider the full range of ozone values, reporting trends for the 5th, 50th and 95th percentiles. Domestic ozone precursor emissions decreased strongly during 1990-2010. Accordingly 83%, 66% and 20% of summertime eastern U.S. sites experienced statistically significant ozone decreases in the 95th, 50th and 5th percentiles, respectively. During spring 43% of the eastern sites have statistically significant ozone decreases for the 95th percentile with no sites showing a significant increase. At the 50th percentile there is little overall change in the eastern U.S. In contrast, only 17% (2 sites) and 8% (1 site) of summertime western U.S. sites have statistically significant ozone decreases in the 95th and 50th percentiles, respectively. During spring no western site has a significant decrease, while 50% have a significant median increase. This dichotomy in U.S. ozone trends is discussed in terms of changing anthropogenic and biomass burning emissions. Consideration is given to the concept that increasing baseline ozone flowing into the western U.S. is counteracting ozone reductions due to domestic emission reductions. An update to the springtime free tropospheric ozone trend above western North America shows that ozone has increased significantly from 1995 to 2011 at the rate of 0.41 +/- 0.27 ppbv yr(-1). Finally, the ozone changes are examined in relation to regional temperature trends. C1 [Cooper, Owen R.; Gao, Ru-Shan; Sweeney, Colm] NOAA, Earth Syst Res Lab, Boulder, CO 80305 USA. [Cooper, Owen R.; Sweeney, Colm] Univ Colorado, NOAA, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA. [Tarasick, David] Environm Canada, Expt Studies Res Div, Meteorol Serv Canada, Ottawa, ON K1A 0H3, Canada. [Leblanc, Thierry] CALTECH, Jet Prop Lab, Table Mt Facil, Pasadena, CA USA. RP Cooper, OR (reprint author), NOAA, Earth Syst Res Lab, CSD04,325 Broadway, Boulder, CO 80305 USA. EM owen.r.cooper@noaa.gov RI Cooper, Owen/H-4875-2013; Gao, Ru-Shan/H-7455-2013; Manager, CSD Publications/B-2789-2015; OI Tarasick, David/0000-0001-9869-0692 FU European Communities; EADS; Airbus; airlines (Lufthansa, Austrian, Air France) FX Ozone data from the National Park Service Gaseous Pollutant Monitoring Program were collected by the National Park Service and downloaded from the NPS Gaseous Pollutant and Meteorological Data Access Page: http://ard-request.air-resource.com. Assistance in retrieving the data was provided by Jessica Ward, Air Resource Specialists, Inc. and John Ray, National Park Service Air Resources Division. Whiteface Mountain Summit ozone data were collected by the University of Albany with instrumentation provided by the New York State Department of Environmental Conservation, and provided by James J. Schwab, Atmospheric Sciences Research Center, University at Albany. Surface CO measurements from Niwot Ridge measured and made available by the NOAA Earth System Research Laboratory Carbon Cycle Group. We gratefully acknowledge the strong support of the MOZAIC program by the European Communities, EADS, Airbus and the airlines (Lufthansa, Austrian, Air France) who have carried the MOZAIC equipment free of charge since 1994. Jean-Pierre Cammas and Philippe Nedelec at CNRS - Laboratoire d'Aerologie, France, provided access to the MOZAIC data. The EDGARv4.1 global NOx emissions inventory was provided by European Commission, Joint Research Centre (JRC)/Netherlands Environmental Assessment Agency (PBL): Emission Database for Global Atmospheric Research (EDGAR), release version 4.1 http://edgar.jrc.ec.europa.eu, 2010. We acknowledge the free use of tropospheric NO2 column data from the GOME and SCIAMACHY sensors from www.temis.nl. The global topography data at 4 min resolution were downloaded from: NOAA National Geophysical Data Center, Boulder, www.ngdc.noaa.gov/mgg/global/global.html. Finally, we thank three anonymous referees whose comments and suggestions improved the analysis. Funding for the Trinidad Head ozonesondes was provided by the NOAA ESRL Health of the Atmosphere Program. NR 98 TC 74 Z9 74 U1 13 U2 144 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD NOV 28 PY 2012 VL 117 AR D22307 DI 10.1029/2012JD018261 PG 24 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 047MH UT WOS:000311844500005 ER PT J AU Martin, MV Kahn, RA Logan, JA Paugam, R Wooster, M Ichoku, C AF Martin, Maria Val Kahn, Ralph A. Logan, Jennifer A. Paugam, Ronan Wooster, Martin Ichoku, Charles TI Space-based observational constraints for 1-D fire smoke plume-rise models SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID REMOTE-SENSING DATA; INJECTION HEIGHT; FOREST-FIRES; WRF-CHEM; EMISSIONS; SATELLITE; TRANSPORT; SENSITIVITY; SIMULATION; WILDFIRES AB We use a plume height climatology derived from space-based Multiangle Imaging Spectroradiometer (MISR) observations to evaluate the performance of a widely used plume-rise model. We initialize the model with assimilated meteorological fields from the NASA Goddard Earth Observing System and estimated fuel moisture content at the location and time of the MISR measurements. Fire properties that drive the plume-rise model are difficult to constrain, and we test the model with four estimates each of active fire area and total heat flux, obtained from Moderate Resolution Imaging Spectroradiometer (MODIS) fire radiative power (FRP) thermal anomalies available for each MISR plume and other empirical data. We demonstrate the degree to which the fire dynamical heat flux (related to active fire area and sensible heat flux) and atmospheric stability structure influence plume rise, although entrainment and possibly other less well constrained factors are also likely to be significant. Using atmospheric stability conditions, MODIS FRP, and MISR plume heights, we find that smoke plumes reaching high altitudes are characterized by higher FRP and weaker atmospheric stability conditions than those at low altitude, which tend to remain confined below the boundary layer, consistent with earlier results. However, over the diversity of conditions studied, the model simulations generally underestimate the plume height dynamic range observed by MISR and do not reliably identify plumes injected into the free troposphere, key information needed for atmospheric models to simulate smoke dispersion. We conclude that embedding in large-scale atmospheric studies an advanced plume-rise model using currently available fire constraints remains a difficult proposition, and we propose a simplified model that crudely constrains plume injection height based on two main physical factors for which some observational constraints often exist. Field experiments aimed at directly measuring fire and smoke plume properties in detail are likely to produce the next major advances in plume-rise modeling. C1 [Martin, Maria Val; Logan, Jennifer A.] Harvard Univ, Sch Engn & Appl Sci, Cambridge, MA 02138 USA. [Kahn, Ralph A.; Ichoku, Charles] NASA, Climate & Radiat Lab, Goddard Space Flight Ctr, Greenbelt, MD USA. [Paugam, Ronan; Wooster, Martin] Kings Coll London, Dept Geog, London WC2R 2LS, England. RP Martin, MV (reprint author), Colorado State Univ, Dept Atmospher Sci, 3915 W Laporte Ave, Ft Collins, CO 80521 USA. EM mval@atmos.colostate.edu RI Val Martin, Maria/D-6955-2011; Ichoku, Charles/E-1857-2012; Kahn, Ralph/D-5371-2012 OI Ichoku, Charles/0000-0003-3244-4549; Kahn, Ralph/0000-0002-5234-6359 FU National Science Foundation [ATM0554804]; NASA [NNX09AC51G]; NASA's Climate and Radiation Research and Analysis Program; NASA's Atmospheric Composition Program; NASA Earth Observing System MISR instrument project FX This work was supported by grants from the National Science Foundation (ATM0554804) and NASA (NNX09AC51G) to Harvard University (M.V.M. and J.A.L.). The work of R.A.K. is supported in part by NASA's Climate and Radiation Research and Analysis Program under H. Maring, NASA's Atmospheric Composition Program under R. Eckman, and the NASA Earth Observing System MISR instrument project. We thank Saulo Freitas for providing and helping implement the 1-D plume-rise model, Nancy French for helpful discussions about North American fuel beds, Alan Cantin for access to the surface observations over Canada used to run CFWI. and Martin Parker for providing the Alaska fuel bed map. The work of David Nelson on the MISR plume climatology is gratefully acknowledged. NR 75 TC 18 Z9 18 U1 2 U2 33 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 NOV 28 PY 2012 VL 117 AR D22204 DI 10.1029/2012JD018370 PG 18 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 047MH UT WOS:000311844500006 ER PT J AU Hsu, TS McPherron, RL Angelopoulos, V Ge, YS Zhang, H Russell, C Chu, XN Kissinger, J AF Hsu, Tung-Shin McPherron, R. L. Angelopoulos, Vassilis Ge, Yasong Zhang, Hui Russell, Christopher Chu, Xiangning Kissinger, Jennifer TI A statistical analysis of the association between fast plasma flows and Pi2 pulsations SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID BURSTY BULK FLOWS; MAGNETOSPHERIC SUBSTORM; PI-2 PULSATIONS; LOW LATITUDES; MAGNETOTAIL; MECHANISM; BRAKING; TRIGGER; EVENT; SHEET AB What is the energy source for Pi2 pulsations? Some researchers have suggested that Pi2 pulsations are caused by plasma flows. Others have suggested that Pi2s are caused by a plasma instability initiated in the near-Earth region. In this study we use Time History of Events and Macroscale Interactions during Substorms (THEMIS) data to examine the relationship between plasma flows and Pi2s. We first identify plasma flows in the tail and then associate these flows with Pi2s. We find that the overall probability of association is nearly 70%. If we further examine the spatial distribution of association we find that in the near-Earth region (8-15 R-E) 90% of the flows are associated with Pi2s. This suggests either that plasma flow in the tail is the cause of Pi2 on the ground or that both are caused by the same process. More importantly, as the flows approach the Earth, the increasing magnetic field causes the flow speed to decrease, that is, the flows are decelerated. In this process of flow braking, the local magnetic field becomes more dipolar. The region of strongest flow braking corresponds to the region of strongest association between flows and Pi2s (8-15 R-E). The GSM X component of plasma flows become zero at around 8 R-E where the most significant magnetic dipolarization occurs. We also find that most plasma flows are associated with a sudden enhancement of the westward electrojet. These results suggest that plasma flows, Pi2 pulsations, and magnetic field dipolarization are essential components of the substorm expansion onset. C1 [Hsu, Tung-Shin; McPherron, R. L.; Angelopoulos, Vassilis; Russell, Christopher; Chu, Xiangning] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90095 USA. [Hsu, Tung-Shin; McPherron, R. L.; Angelopoulos, Vassilis; Russell, Christopher; Chu, Xiangning] Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90095 USA. [Ge, Yasong] Univ New Hampshire, Ctr Space Sci, Durham, NH 03824 USA. [Zhang, Hui] Chinese Acad Sci, Inst Geol & Geophys, Beijing Natl Observ Space Environm, Beijing, Peoples R China. [Kissinger, Jennifer] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Hsu, TS (reprint author), Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90095 USA. EM thsu@igpp.ucla.edu RI Zhang, Hui/G-6600-2014 FU NSF [ATM-1003854, AGS-0720422]; [NASA-NNX07AG47G]; [NASA-NNX07AG16G]; [NASA-NNX07AF60G] FX The authors would like to acknowledge support for this work from the following grants: NASA-NNX07AG47G, NASA-NNX07AG16G, NASA-NNX07AF60G, NSF ATM-1003854 and NSF AGS-0720422. We also thank the Principal Investigators of the THEMIS spacecraft and ground stations for making data from their instruments available for this study. Finally we thank the Data Center for Geomagnetism at Kyoto, Japan for creation and distribution of the AE indices. NR 40 TC 11 Z9 11 U1 0 U2 10 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD NOV 28 PY 2012 VL 117 AR A11221 DI 10.1029/2012JA018173 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 047LY UT WOS:000311843600003 ER PT J AU Bhatia, AK Sinha, C AF Bhatia, A. K. Sinha, C. TI Free-free transitions of the e-H system inside a dense plasma irradiated by a laser field at very low incident-electron energies SO PHYSICAL REVIEW A LA English DT Article ID ION-SCATTERING; EXCITATION; COLLISIONS; HYDROGEN AB The free-free transition is studied for an electron-hydrogen atom in ground state when a low-energy electron (external) is injected into hydrogenic plasma in the presence of an external homogenous, monochromatic, and linearly polarized laser field. The effect of plasma screening is considered in the Debye-Huckel approximation. The calculations are performed in the soft photon limit. The incident electron is considered to be dressed by the laser field in a nonperturbative manner by choosing the Volkov solutions in both the initial and final channels. The space part of the scattering wave function for the electron is solved numerically by taking into account the electron exchange. The laser-assisted differential and total cross sections are calculated for single-photon absorption or emission and no-photon exchange in the soft photon limit, the laser intensity being much less than the atomic field intensity. The calculations have been carried out for various values of Debye parameter, ranging from 0.005 to 0.12. A strong suppression is noted in the laser-assisted cross sections as compared to the field-free situation. A significant difference is noted for the singlet and triplet cross sections. The suppression is much more in the triplet states. C1 [Bhatia, A. K.] NASA, Goddard Space Flight Ctr, Solar Phys Lab, Greenbelt, MD 20771 USA. [Sinha, C.] Indian Assoc Cultivat Sci, Dept Theoret Phys, Kolkata 700032, India. RP Bhatia, AK (reprint author), NASA, Goddard Space Flight Ctr, Solar Phys Lab, Greenbelt, MD 20771 USA. NR 29 TC 6 Z9 6 U1 2 U2 5 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 2469-9926 EI 2469-9934 J9 PHYS REV A JI Phys. Rev. A PD NOV 28 PY 2012 VL 86 IS 5 AR 053421 DI 10.1103/PhysRevA.86.053421 PG 9 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 044FD UT WOS:000311603900005 ER PT J AU Fuchs, EC Cherukupally, A Paulitsch-Fuchs, AH Agostinho, LLF Wexler, AD Woisetschlager, J Freund, FT AF Fuchs, Elmar C. Cherukupally, Anvesh Paulitsch-Fuchs, Astrid H. Agostinho, Luewton L. F. Wexler, Adam D. Woisetschlaeger, Jakob Freund, Friedemann T. TI Investigation of the mid-infrared emission of a floating water bridge SO JOURNAL OF PHYSICS D-APPLIED PHYSICS LA English DT Article ID SIMPLE IONIC HYDROXIDES; PROTON CONDUCTIVITY; ELECTRIC-FIELD; TEMPERATURE-DEPENDENCE; INFRARED-SPECTROSCOPY; CARBON-DIOXIDE; LIQUID WATER; TRANSMITTANCE; DYNAMICS; MG(OH)2 AB We report on the infrared emission of aqueous bridges under the application of high dc voltage (;'floating water bridge') over the range between 400 and 2500 cm(-1) (4.0-10.3 mu m). Comparison with bulk water of the same temperature reveals an additional broad peak at similar to 2200 cm(-1) as well as water vapour emission lines. Two complementary explanations are presented for the broad peak: first, a cooperative proton transfer comprising an orientational motion along the direction of conduction is suggested. Second, the electrolysis-less current flow is explained by a proton/defect-proton band mechanism, which is in line with the cooperative proton transfer. The water vapour emissions occur due to collision ionization of space charges with micro-and nano-droplets which are electrosprayed from the liquid/gas interface. C1 [Fuchs, Elmar C.; Paulitsch-Fuchs, Astrid H.; Agostinho, Luewton L. F.; Wexler, Adam D.] Wetsus Ctr Excellence Sustainable Water Technol, Leeuwarden, Netherlands. [Cherukupally, Anvesh] Univ Arizona, Dept Min & Geol Engn, Tucson, AZ 85721 USA. [Woisetschlaeger, Jakob] Graz Univ Technol, Inst Thermal Turbomachinery & Machine Dynam, A-8010 Graz, Austria. [Woisetschlaeger, Jakob] Carl Sagan Ctr, SETI Inst, Mountain View, CA USA. [Freund, Friedemann T.] NASA, Ames Res Ctr, Div Earth Sci, Moffett Field, CA 94035 USA. RP Fuchs, EC (reprint author), Wetsus Ctr Excellence Sustainable Water Technol, Leeuwarden, Netherlands. EM elmar.fuchs@wetsus.nl OI Woisetschlaeger, Jakob/0000-0002-7057-761X FU Dutch Ministry of Economic Affairs; NASA Earth Surface and Interior program FX This work was performed in the TTIW-cooperation framework of Wetsus, centre of excellence for sustainable water technology (www.wetsus.nl). Wetsus is funded by the Dutch Ministry of Economic Affairs. The authors like to thank the participants of the research theme 'Applied Water Physics' for the fruitful discussions and their financial support. The IR emission spectra were recorded at the NASA Ames Research Center, Moffett Field, CA, USA, using an IR emission spectrometer provided by a grant from the NASA Earth Surface and Interior program. The authors thank Dr Dana Lynch for providing premier laboratory space for conducting these experiments. The authors also would like to thank Professors Huib Bakker (AMOLF Amsterdam), Cees Buisman (Wetsus), Karl Gatterer (Graz University of Technology), Emilio Del Giudice (Universita di Milano), Franz Heitmeir (Graz University of Technology), Jose Teixeira (Laboratoire Leon Brillouin, CEA-CNRS/IRAMIS, CEA/Saclay), as well as Cees Kamp (Wetsus), Lukasz Piatkowski (AMOLF) and Martina Sammer (Wetsus) for ongoing discussions about the water bridge phenomenon (in alphabetic order). NR 52 TC 11 Z9 11 U1 0 U2 14 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0022-3727 J9 J PHYS D APPL PHYS JI J. Phys. D-Appl. Phys. PD NOV 28 PY 2012 VL 45 IS 47 AR 475401 DI 10.1088/0022-3727/45/47/475401 PG 10 WC Physics, Applied SC Physics GA 033ZK UT WOS:000310839700016 ER PT J AU Elsila, JE Glavin, DP Dworkin, JP Martins, Z Bada, JL AF Elsila, Jamie E. Glavin, Daniel P. Dworkin, Jason P. Martins, Zita Bada, Jeffrey L. TI Inconclusive evidence for nonterrestrial isoleucine enantiomeric excesses in primitive meteorites SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Letter ID AMINO-ACIDS C1 [Elsila, Jamie E.; Glavin, Daniel P.; Dworkin, Jason P.] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA. [Martins, Zita] Univ London Imperial Coll Sci Technol & Med, Dept Earth Sci & Engn, London SW7 2AZ, England. [Bada, Jeffrey L.] Univ Calif San Diego, Scripps Inst Oceanog, Geosci Res Div, La Jolla, CA 92093 USA. RP Elsila, JE (reprint author), NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA. EM jamie.elsila@nasa.gov RI Elsila, Jamie/C-9952-2012; Glavin, Daniel/D-6194-2012; Martins, Zita/H-4860-2015; Dworkin, Jason/C-9417-2012 OI Glavin, Daniel/0000-0001-7779-7765; Martins, Zita/0000-0002-5420-1081; Dworkin, Jason/0000-0002-3961-8997 NR 5 TC 7 Z9 7 U1 0 U2 11 PU NATL ACAD SCIENCES PI WASHINGTON PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA SN 0027-8424 J9 P NATL ACAD SCI USA JI Proc. Natl. Acad. Sci. U. S. A. PD NOV 27 PY 2012 VL 109 IS 48 BP E3288 EP E3288 DI 10.1073/pnas.1213261109 PG 1 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 053ZN UT WOS:000312313900001 PM 23064644 ER PT J AU Gluscevic, V Hanson, D Kamionkowski, M Hirata, CM AF Gluscevic, Vera Hanson, Duncan Kamionkowski, Marc Hirata, Christopher M. TI First CMB constraints on direction-dependent cosmological birefringence from WMAP-7 SO PHYSICAL REVIEW D LA English DT Article ID DISTANT RADIO-SOURCES; TESTING CPT SYMMETRY; POWER SPECTRA; GRAVITY-WAVES; POLARIZATION; ANISOTROPY; PROBE; LIMITS; SIGNATURE; GALAXIES AB A Chern-Simons coupling of a new scalar field to electromagnetism may give rise to cosmological birefringence, a rotation of the linear polarization of electromagnetic waves as they propagate over cosmological distances. Prior work has sought this rotation, assuming the rotation angle to be uniform across the sky, by looking for the parity-violating TB and EB correlations that a uniform rotation produces in the cosmic microwave background temperature/polarization. However, if the scalar field that gives rise to cosmological birefringence has spatial fluctuations, then the rotation angle may vary across the sky. Here we search for direction-dependent cosmological birefringence in the WMAP-7 data. We report the first cosmic microwave background constraint on the rotation-angle power spectrum C-L(alpha alpha) for multipoles between L = 0 and L = 512. We also obtain a 68% confidence-level upper limit of root C-2(alpha alpha)/(4 pi) less than or similar to 1 degrees on the quadrupole of a scale-invariant rotation-angle power spectrum. C1 [Gluscevic, Vera; Hanson, Duncan; Kamionkowski, Marc; Hirata, Christopher M.] CALTECH, Pasadena, CA 91125 USA. [Kamionkowski, Marc] Johns Hopkins Univ Hosp, Dept Phys & Astron, Baltimore, MD 21218 USA. [Hanson, Duncan] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Gluscevic, V (reprint author), CALTECH, Mail Code 350-17, Pasadena, CA 91125 USA. OI Kamionkowski, Marc/0000-0001-7018-2055 FU DOE [DE-FG03-92-ER40701, DOE.DE-SC0006624]; NASADavid and Lucile Packard Foundation [NNX12AE86G] FX This work was supported by DOE DE-FG03-92-ER40701, NASA NNX12AE86G, DOE (DOE.DE-SC0006624), and the David and Lucile Packard Foundation. Part of 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. Some of the results in this paper have been derived using the HEALPix package [31]. NR 49 TC 22 Z9 22 U1 0 U2 3 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1550-7998 J9 PHYS REV D JI Phys. Rev. D PD NOV 26 PY 2012 VL 86 IS 10 AR 103529 DI 10.1103/PhysRevD.86.103529 PG 14 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 043NA UT WOS:000311549300005 ER PT J AU Sibeck, DG Korotova, G Turner, DL Angelopoulos, V Glassmeier, KH McFadden, JP AF Sibeck, D. G. Korotova, G. Turner, D. L. Angelopoulos, V. Glassmeier, K. -H. McFadden, J. P. TI Frequency doubling and field-aligned ion streaming in a long-period poloidal pulsation SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID HIGH-BETA PLASMA; COMPRESSIONAL PC5 PULSATIONS; PITCH-ANGLE DISTRIBUTIONS; MIRROR INSTABILITY; GEOMAGNETIC-PULSATIONS; ENERGETIC PARTICLES; ULF PULSATIONS; RING CURRENT; PC-5 WAVES; MAGNETOSPHERE AB We reexamine a long-period (10-18 min) poloidal pulsation observed by THEMIS-A in the outer dawn magnetosphere from 10: 00 to 12: 30 UT on 7 November 2007. The interval was originally reported by Korotova et al. (2009). Although the nonlinear compressional plasma and magnetic field perturbations observed by THEMIS-A during this interval agree well with model predictions for the linear perturbations associated with antisymmetric waves generated by the ballooning-mirror mode instability, the phase relationships between these perturbations indicates a complex frequency rather than the purely imaginary frequency that theory predicts for the outer dawnside magnetosphere. Variations in the radial plasma velocity confirm that a phase-locked north/south oscillation in the equatorial line of nodes associated with the ballooning-mirror mode waves doubles the frequency of the compressional component of the magnetic field during these pulsations. The same velocity and magnetic field perturbations exclude explanations for the frequency doubling in terms of spatial gradients sweeping back and forth across the spacecraft or drift-bounce resonances. Azimuthal electric fields associated with the pulsations generate field-aligned anisotropies in the pitch angle distributions that become more prominent with increasing ion energy due to the presence of drift-shell splitting and radial flux gradients that steepen with increasing energy. Although there was no evidence for drift-bounce interactions during this event, the role of such events in ion energization in other events and at other locations remains to be evaluated. C1 [Sibeck, D. G.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Korotova, G.] IZMIRAN, Troitsk 142092, Russia. [Korotova, G.] Univ Maryland, IPST, College Pk, MD 20742 USA. [Turner, D. L.; Angelopoulos, V.] Univ Calif Los Angeles, ESS, Los Angeles, CA USA. [Glassmeier, K. -H.] TUB, Inst Geophys & Extraterr Phys, Braunschweig, Germany. [McFadden, J. P.] Univ Calif Berkeley, SSL, Berkeley, CA 94720 USA. RP Sibeck, DG (reprint author), NASA, Goddard Space Flight Ctr, Code 674, Greenbelt, MD 20771 USA. EM david.g.sibeck@nasa.gov RI Turner, Drew/G-3224-2012 FU NASA's THEMIS Program; NASA GSFC [NNX09AV52G] FX Research at GSFC was funded by NASA's THEMIS Program. Research at the University of Maryland was supported by NASA GSFC grant NNX09AV52G. D. G. S. thanks both referees, C. Z. Cheng, and K. Takahashi for many helpful suggestions and boundless patience. V. Kondratovich aided in analyzing the pulsations. NR 48 TC 7 Z9 7 U1 0 U2 8 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD NOV 21 PY 2012 VL 117 AR A11215 DI 10.1029/2011JA017473 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 043SD UT WOS:000311567000001 ER PT J AU Jaramillo-Botero, A An, Q Cheng, MJ Goddard, WA Beegle, LW Hodyss, R AF Jaramillo-Botero, Andres An, Qi Cheng, Mu-Jeng Goddard, William A., III Beegle, Luther W. Hodyss, Robert TI Hypervelocity Impact Effect of Molecules from Enceladus' Plume and Titan's Upper Atmosphere on NASA's Cassini Spectrometer from Reactive Dynamics Simulation SO PHYSICAL REVIEW LETTERS LA English DT Article ID FORCE-FIELD; REAXFF; IONS AB The NASA/ESA Cassini probe of Saturn analyzed the molecular composition of plumes emanating from one of its moons, Enceladus, and the upper atmosphere of another, Titan. However, interpretation of this data is complicated by the hypervelocity (HV) flybys of up to similar to 18 km/sec that cause substantial molecular fragmentation. To interpret this data we use quantum mechanical based reactive force fields to simulate the HV impact of various molecular species and ice clathrates on oxidized titanium surfaces mimicking those in Cassini's neutral and ion mass spectrometer (INMS). The predicted velocity dependent fragmentation patterns and composition mixing ratios agree with INMS data providing the means for identifying the molecules in the plume. We used our simulations to predict the surface damage from the HV impacts on the INMS interior walls, which we suggest acts as a titanium sublimation pump that could alter the instrument's readings. These results show how the theory can identify chemical events from hypervelocity impacts in space plumes and atmospheres, providing in turn clues to the internal structure of the corresponding sources (e.g., Enceladus). This may be valuable in steering modifications in future missions. C1 [Jaramillo-Botero, Andres; An, Qi; Cheng, Mu-Jeng; Goddard, William A., III] CALTECH, Mat & Proc Simulat Ctr, Pasadena, CA 91125 USA. [Beegle, Luther W.; Hodyss, Robert] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Jaramillo-Botero, A (reprint author), CALTECH, Mat & Proc Simulat Ctr, 1200 E Calif Blvd, Pasadena, CA 91125 USA. EM ajaramil@caltech.edu; wag@wag.caltech.edu RI An, Qi/I-6985-2012; Cheng, Mu-Jeng/I-7316-2012 FU Department of Energy National Nuclear Security Administration [DE-FC52-08NA28613] FX Thanks to Adri van Duin and colleagues for providing the basic TiO2-H2O ReaxFF force field, Patrick L. Theofanis for his suggestions on the manuscript, and Chi Feng (SURF Fellow at Caltech) for his contributions to hexane simulations. This work was performed at Caltech and JPL under a contract with the National Aeronautics and Space Administration (NASA). Partial support was provided by the Department of Energy National Nuclear Security Administration under Contract No. DE-FC52-08NA28613 (Caltech PSAAP). NR 17 TC 4 Z9 4 U1 2 U2 43 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 0031-9007 J9 PHYS REV LETT JI Phys. Rev. Lett. PD NOV 21 PY 2012 VL 109 IS 21 AR 213201 DI 10.1103/PhysRevLett.109.213201 PG 5 WC Physics, Multidisciplinary SC Physics GA 041CT UT WOS:000311374500003 PM 23215593 ER PT J AU Garry, WB Robinson, MS Zimbelman, JR Bleacher, JE Hawke, BR Crumpler, LS Braden, SE Sato, H AF Garry, W. B. Robinson, M. S. Zimbelman, J. R. Bleacher, J. E. Hawke, B. R. Crumpler, L. S. Braden, S. E. Sato, H. TI The origin of Ina: Evidence for inflated lava flows on the Moon SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID MARTIAN FLOOD LAVAS; SNAKE RIVER PLAIN; STEEP-SIDED DOMES; BASALTIC LAVA; LABORATORY SIMULATIONS; KILAUEA VOLCANO; THERMAL MODELS; MAGELLAN DATA; PAHOEHOE; EMPLACEMENT AB Ina is an enigmatic volcanic feature on the Moon known for its irregularly shaped mounds, the origin of which has been debated since the Apollo Missions. Three main units are observed on the floor of the depression (2.9 km across, <= 64 m deep) located at the summit of a low-shield volcano: irregularly shaped mounds up to 20 m tall, a lower unit 1 to 5 m in relief that surrounds the mounds, and blocky material. Analyses of Lunar Reconnaissance Orbiter Camera images and topography show that features in Ina are morphologically similar to terrestrial inflated lava flows. Comparison of these unusual lunar mounds and possible terrestrial analogs leads us to hypothesize that features in Ina were formed through lava flow inflation processes. While the source of the lava remains unclear, this new model suggests that as the mounds inflated, breakouts along their margins served as sources for surface flows that created the lower morphologic unit. Over time, mass wasting of both morphologic units has exposed fresh surfaces observed in the blocky unit. Ina is different than the terrestrial analogs presented in this study in that the lunar features formed within a depression, no vent sources are observed, and no cracks are observed on the mounds. However, lava flow inflation processes explain many of the morphologic relationships observed in Ina and are proposed to be analogous with inflated lava flows on Earth. C1 [Garry, W. B.; Bleacher, J. E.] NASA, Planetary Geodynam Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Garry, W. B.] Planetary Sci Inst, Tucson, AZ USA. [Robinson, M. S.; Braden, S. E.; Sato, H.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ USA. [Zimbelman, J. R.] Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. [Hawke, B. R.] Univ Hawaii Manoa, SOEST, Inst Geophys & Planetol, Honolulu, HI 96822 USA. [Crumpler, L. S.] New Mexico Museum Nat Hist & Sci, Albuquerque, NM USA. RP Garry, WB (reprint author), NASA, Planetary Geodynam Lab, Goddard Space Flight Ctr, Code 698, Greenbelt, MD 20771 USA. EM william.b.garry@nasa.gov RI Garry, Brent/I-5920-2013; Bleacher, Jacob/D-1051-2012 OI Bleacher, Jacob/0000-0002-8499-4828 FU NASA [NNX11AG90G, NNX08AM77G]; LROC Science Operations; NASA Moon and Mars Analog Mission Activities (MMAMA) [NNX08AR76G, NNX09AW15G, 08-MMAMA08-016]; NASA Planetary Geology and Geophysics (PGG) [NNX09AD88G]; Smithsonian Scholarly Studies Program [FY11] FX Lunar research was supported by the NASA Lunar Reconnaissance Orbiter Participating Scientist Program grants NNX11AG90G (PI: Garry), NNX08AM77G (PI: Hawke), and LROC Science Operations (PI: Robinson). Field work in Hawai'i, Idaho, and New Mexico was supported by the following grants: NASA Moon and Mars Analog Mission Activities (MMAMA) NNX08AR76G and NNX09AW15G (PI: Garry), 08-MMAMA08-016 (PI: Bleacher), NASA Planetary Geology and Geophysics (PGG) NNX09AD88G (PI: Zimbelman), Smithsonian Scholarly Studies Program FY11 (PI: Zimbelman). The authors would like to thank the Lunar Reconnaissance Orbiter Project Office at NASA Goddard Space Flight Center, the LROC Science Operations Center at Arizona State University, El Malpais National Monument in New Mexico, Craters of the Moon National Monument in Idaho, plus William J. Clancey and Maarten Sierhuis for their assistance with field work in Idaho and New Mexico. Thank you to Lazlo Keszthelyi, Peter H. Schultz, and an anonymous reviewer for their time and thorough reviews of the manuscript. NR 74 TC 6 Z9 7 U1 0 U2 8 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD NOV 20 PY 2012 VL 117 AR E00H31 DI 10.1029/2011JE003981 PG 15 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 043RR UT WOS:000311565100001 ER PT J AU Abadie, J Abbott, BP Abbott, R Abbott, TD Abernathy, M Accadia, T Acernese, F Adams, C Adhikari, RX Affeldt, C Agathos, M Agatsuma, K Ajith, P Allen, B Ceron, EA Amariutei, D Anderson, SB Anderson, WG Arai, K Arain, MA Araya, MC Aston, SM Astone, P Atkinson, D Aufmuth, P Aulbert, C Aylott, BE Babak, S Baker, P Ballardin, G Ballmer, S Barayoga, JCB Barker, D Barone, F Barr, B Barsotti, L Barsuglia, M Barton, MA Bartos, I Bassiri, R Bastarrika, M Basti, A Batch, J Bauchrowitz, J Bauer, TS Bebronne, M Beck, D Behnke, B Bejger, M Beker, MG Bell, AS Belopolski, I Benacquista, M Berliner, JM Bertolini, A Betzwieser, J Beveridge, N Beyersdorf, PT Bilenko, IA Billingsley, G Birch, J Biswas, R Bitossi, M Bizouard, MA Black, E Blackburn, JK Blackburn, L Blair, D Bland, B Blom, M Bock, O Bodiya, TP Bogan, C Bondarescu, R Bondu, F Bonelli, L Bonnand, R Bork, R Born, M Boschi, V Bose, S Bosi, L Bouhou, B Braccini, S Bradaschia, C Brady, PR Braginsky, VB Branchesi, M Brau, JE Breyer, J Briant, T Bridges, DO Brillet, A Brinkmann, M Brisson, V Britzger, M Brooks, AF Brown, DA Bulik, T Bulten, HJ Buonanno, A Burguet-Castell, J Buskulic, D Buy, C Byer, RL Cadonati, L Calloni, E Camp, JB Campsie, P Cannizzo, J Cannon, K Canuel, B Cao, J Capano, CD Carbognani, F Carbone, L Caride, S Caudill, S Cavaglia, M Cavalier, F Cavalieri, R Cella, G Cepeda, C Cesarini, E Chaibi, O Chalermsongsak, T Charlton, P Chassande-Mottin, E Chelkowski, S Chen, W Chen, X Chen, Y Chincarini, A Chiummo, A Cho, HS Chow, J Christensen, N Chua, SSY Chung, CTY Chung, S Ciani, G Clara, F Clark, DE Clark, J Clayton, JH Cleva, F Coccia, E Cohadon, PF Colacino, CN Colas, J Colla, A Colombini, M Conte, A Conte, R Cook, D Corbitt, TR Cordier, M Cornish, N Corsi, A Costa, CA Coughlin, M Coulon, JP Couvares, P Coward, DM Cowart, M Coyne, DC Creighton, JDE Creighton, TD Cruise, AM Cumming, A Cunningham, L Cuoco, E Cutler, RM Dahl, K Danilishin, SL Dannenberg, R D'Antonio, S Danzmann, K Dattilo, V Daudert, B Daveloza, H Davier, M Daw, EJ Day, R Dayanga, T De Rosa, R Debra, D Debreczeni, G Degallaix, J Del Pozzo, W del Prete, M Dent, T Dergachev, V DeRosa, R DeSalvo, R Dhurandhar, S Di Fiore, L Di Lieto, A Di Palma, I Emilio, MD Di Virgilio, A Diaz, M Dietz, A Donovan, F Dooley, KL Drago, M Drever, RWP Driggers, JC Du, Z Dumas, JC Dwyer, S Eberle, T Edgar, M Edwards, M Effler, A Ehrens, P Endroczi, G Engel, R Etzel, T Evans, K Evans, M Evans, T Factourovich, M Fafone, V Fairhurst, S Fan, Y Farr, BF Fazi, D Fehrmann, H Feldbaum, D Feroz, F Ferrante, I Fidecaro, F Finn, LS Fiori, I Fisher, RP Flaminio, R Flanigan, M Foley, S Forsi, E Forte, LA Fotopoulos, N Fournier, JD Franc, J Franco, S Frasca, S Frasconi, F Frede, M Frei, M Frei, Z Freise, A Frey, R Fricke, TT Friedrich, D Fritschel, P Frolov, VV Fujimoto, MK Fulda, PJ Fyffe, M Gair, J Galimberti, M Gammaitoni, L Garcia, J Garufi, F Gaspar, ME Gehrels, N Gemme, G Geng, R Genin, E Gennai, A Gergely, LA Ghosh, S Giaime, JA Giampanis, S Giardina, KD Giazotto, A Gil-Casanova, S Gill, C Gleason, J Goetz, E Goggin, LM Gonzalez, G Gorodetsky, ML Gossler, S Gouaty, R Graef, C Graff, PB Granata, M Grant, A Gras, S Gray, C Gray, N Greenhalgh, RJS Gretarsson, AM Greverie, C Grosso, R Grote, H Grunewald, S Guidi, GM Guido, C Gupta, R Gustafson, EK Gustafson, R Ha, T Hallam, JM Hammer, D Hammond, G Hanks, J Hanna, C Hanson, J Hardt, A Harms, J Harry, GM Harry, IW Harstad, ED Hartman, MT Haughian, K Hayama, K Hayau, JF Heefner, J Heidmann, A Heintze, MC Heitmann, H Hello, P Hendry, MA Heng, IS Heptonstall, AW Herrera, V Hewitson, M Hild, S Hoak, D Hodge, KA Holt, K Holtrop, M Hong, T Hooper, S Hosken, DJ Hough, J Howell, EJ Hughey, B Husa, S Huttner, SH Huynh-Dinh, T Ingram, DR Inta, R Isogai, T Ivanov, A Izumi, K Jacobson, M James, E Jang, YJ Jaranowski, P Jesse, E Johnson, WW Jones, DI Jones, G Jones, R Jonker, RJG Ju, L Kalmus, P Kalogera, V Kandhasamy, S Kang, G Kanner, JB Kasturi, R Katsavounidis, E Katzman, W Kaufer, H Kawabe, K Kawamura, S Kawazoe, F Kelley, D Kells, W Keppel, DG Keresztes, Z Khalaidovski, A Khalili, FY Khazanov, EA Kim, BK Kim, C Kim, H Kim, K Kim, N Kim, YM King, PJ Kinzel, DL Kissel, JS Klimenko, S Kokeyama, K Kondrashov, V Koranda, S Korth, WZ Kowalska, I Kozak, D Kranz, O Kringel, V Krishnamurthy, S Krishnan, B Krolak, A Kuehn, G Kumar, P Kumar, R Kwee, P Lam, PK Landry, M Lantz, B Lastzka, N Lawrie, C Lazzarini, A Leaci, P Lee, CH Lee, HK Lee, HM Leong, JR Leonor, I Leroy, N Letendre, N Li, J Li, TGF Liguori, N Lindquist, PE Liu, Y Liu, Z Lockerbie, NA Lodhia, D Lorenzini, M Loriette, V Lormand, M Losurdo, G Lough, J Luan, J Lubinski, M Luck, H Lundgren, AP Macdonald, E Machenschalk, B MacInnis, M Macleod, DM Mageswaran, M Mailand, K Majorana, E Maksimovic, I Malvezzi, V Man, N Mandel, I Mandic, V Mantovani, M Marandi, A Marchesoni, F Marion, F Marka, S Marka, Z Markosyan, A Maros, E Marque, J Martelli, F Martin, IW Martin, RM Marx, JN Mason, K Masserot, A Matichard, F Matone, L Matzner, RA Mavalvala, N Mazzolo, G McCarthy, R McClelland, DE McGuire, SC McIntyre, G McIver, J McKechan, DJA McWilliams, S Meadors, GD Mehmet, M Meier, T Melatos, A Melissinos, AC Mendell, G Mercer, RA Meshkov, S Messenger, C Meyer, MS Miao, H Michel, C Milano, L Miller, J Minenkov, Y Mitrofanov, VP Mitselmakher, G Mittleman, R Miyakawa, O Moe, B Mohan, M Mohanty, SD Mohapatra, SRP Moraru, D Moreno, G Morgado, N Morgia, A Mori, T Morriss, SR Mosca, S Mossavi, K Mours, B Mow-Lowry, CM Mueller, CL Mueller, G Mukherjee, S Mullavey, A Muller-Ebhardt, H Munch, J Murphy, D Murray, PG Mytidis, A Nash, T Naticchioni, L Necula, V Nelson, J Neri, I Newton, G Nguyen, T Nishizawa, A Nitz, A Nocera, F Nolting, D Normandin, ME Nuttall, L Ochsner, E O'Dell, J Oelker, E Ogin, GH Oh, JJ Oh, SH O'Reilly, B O'Shaughnessy, R Osthelder, C Ott, CD Ottaway, DJ Ottens, RS Overmier, H Owen, BJ Page, A Palladino, L Palomba, C Pan, Y Pankow, C Paoletti, F Paoletti, R Papa, MA Parisi, M Pasqualetti, A Passaquieti, R Passuello, D Patel, P Pedraza, M Peiris, P Pekowsky, L Penn, S Perreca, A Persichetti, G Phelps, M Pichot, M Pickenpack, M Piergiovanni, F Pietka, M Pinard, L Pinto, IM Pitkin, M Pletsch, HJ Plissi, MV Poggiani, R Pold, J Postiglione, F Prato, M Predoi, V Prestegard, T Price, LR Prijatelj, M Principe, M Privitera, S Prix, R Prodi, GA Prokhorov, LG Puncken, O Punturo, M Puppo, P Quetschke, V Quitzow-James, R Raab, FJ Rabeling, DS Racz, I Radkins, H Raffai, P Rakhmanov, M Rankins, B Rapagnani, P Raymond, V Re, V Redwine, K Reed, CM Reed, T Regimbau, T Reid, S Reitze, DH Ricci, F Riesen, R Riles, K Robertson, NA Robinet, F Robinson, C Robinson, EL Rocchi, A Roddy, S Rodriguez, C Rodruck, M Rolland, L Rollins, JG Romano, JD Romano, R Romie, JH Rosinska, D Rover, C Rowan, S Rudiger, A Ruggi, P Ryan, K Sainathan, P Salemi, F Sammut, L Sandberg, V Sannibale, V Santamaria, L Santiago-Prieto, I Santostasi, G Sassolas, B Sathyaprakash, BS Sato, S Saulson, PR Savage, RL Schilling, R Schnabel, R Schofield, RMS Schreiber, E Schulz, B Schutz, BF Schwinberg, P Scott, J Scott, SM Seifert, F Sellers, D Sentenac, D Sergeev, A Shaddock, DA Shaltev, M Shapiro, B Shawhan, P Shoemaker, DH Sibley, A Siemens, X Sigg, D Singer, A Singer, L Sintes, AM Skelton, GR Slagmolen, BJJ Slutsky, J Smith, JR Smith, MR Smith, RJE Smith-Lefebvre, ND Somiya, K Sorazu, B Soto, J Speirits, FC Sperandio, L Stefszky, M Stein, AJ Stein, LC Steinert, E Steinlechner, J Steinlechner, S Steplewski, S Stochino, A Stone, R Strain, KA Strigin, SE Stroeer, AS Sturani, R Stuver, AL Summerscales, TZ Sung, M Susmithan, S Sutton, PJ Swinkels, B Tacca, M Taffarello, L Talukder, D Tanner, DB Tarabrin, SP Taylor, JR Taylor, R ter Braack, APM Thomas, P Thorne, KA Thorne, KS Thrane, E Thuring, A Tokmakov, KV Tomlinson, C Toncelli, A Tonelli, M Torre, O Torres, C Torrie, CI Tournefier, E Tucker, E Travasso, F Traylor, G Tseng, K Ugolini, D Vahlbruch, H Vajente, G van den Brand, JFJ Van den Broeck, C van der Putten, S van Veggel, AA Vass, S Vasuth, M Vaulin, R Vavoulidis, M Vecchio, A Vedovato, G Veitch, J Veitch, PJ Veltkamp, C Verkindt, D Vetrano, F Vicere, A Villar, AE Vinet, JY Vitale, S Vocca, H Vorvick, C Vyatchanin, SP Wade, A Wade, L Wade, M Waldman, SJ Wallace, L Wan, Y Wang, M Wang, X Wang, Z Wanner, A Ward, RL Was, M Weinert, M Weinstein, AJ Weiss, R Wen, L Wessels, P West, M Westphal, T Wette, K Whelan, JT Whitcomb, SE White, DJ Whiting, BF Wilkinson, C Willems, PA Williams, L Williams, R Willke, B Winkelmann, L Winkler, W Wipf, CC Wiseman, AG Wittel, H Woan, G Wooley, R Worden, J Yakushin, I Yamamoto, H Yamamoto, K Yancey, CC Yang, H Yeaton-Massey, D Yoshida, S Yu, P Yvert, M Zadrozny, A Zanolin, M Zendri, JP Zhang, F Zhang, L Zhang, W Zhao, C Zotov, N Zucker, ME Zweizig, J Briggs, MS Connaughton, V Hurley, KC Jenke, PA von Kienlin, A Rau, A Zhang, XL AF Abadie, J. Abbott, B. P. Abbott, R. Abbott, T. D. Abernathy, M. Accadia, T. Acernese, F. Adams, C. Adhikari, R. X. Affeldt, C. Agathos, M. Agatsuma, K. Ajith, P. Allen, B. Ceron, E. Amador Amariutei, D. Anderson, S. B. Anderson, W. G. Arai, K. Arain, M. A. Araya, M. C. Aston, S. M. Astone, P. Atkinson, D. Aufmuth, P. Aulbert, C. Aylott, B. E. Babak, S. Baker, P. Ballardin, G. Ballmer, S. Barayoga, J. C. B. Barker, D. Barone, F. Barr, B. Barsotti, L. Barsuglia, M. Barton, M. A. Bartos, I. Bassiri, R. Bastarrika, M. Basti, A. Batch, J. Bauchrowitz, J. Bauer, Th. S. Bebronne, M. Beck, D. Behnke, B. Bejger, M. Beker, M. G. Bell, A. S. Belopolski, I. Benacquista, M. Berliner, J. M. Bertolini, A. Betzwieser, J. Beveridge, N. Beyersdorf, P. T. Bilenko, I. A. Billingsley, G. Birch, J. Biswas, R. Bitossi, M. Bizouard, M. A. Black, E. Blackburn, J. K. Blackburn, L. Blair, D. Bland, B. Blom, M. Bock, O. Bodiya, T. P. Bogan, C. Bondarescu, R. Bondu, F. Bonelli, L. Bonnand, R. Bork, R. Born, M. Boschi, V. 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Schofield, R. M. S. Schreiber, E. Schulz, B. Schutz, B. F. Schwinberg, P. Scott, J. Scott, S. M. Seifert, F. Sellers, D. Sentenac, D. Sergeev, A. Shaddock, D. A. Shaltev, M. Shapiro, B. Shawhan, P. Shoemaker, D. H. Sibley, A. Siemens, X. Sigg, D. Singer, A. Singer, L. Sintes, A. M. Skelton, G. R. Slagmolen, B. J. J. Slutsky, J. Smith, J. R. Smith, M. R. Smith, R. J. E. Smith-Lefebvre, N. D. Somiya, K. Sorazu, B. Soto, J. Speirits, F. C. Sperandio, L. Stefszky, M. Stein, A. J. Stein, L. C. Steinert, E. Steinlechner, J. Steinlechner, S. Steplewski, S. Stochino, A. Stone, R. Strain, K. A. Strigin, S. E. Stroeer, A. S. Sturani, R. Stuver, A. L. Summerscales, T. Z. Sung, M. Susmithan, S. Sutton, P. J. Swinkels, B. Tacca, M. Taffarello, L. Talukder, D. Tanner, D. B. Tarabrin, S. P. Taylor, J. R. Taylor, R. ter Braack, A. P. M. Thomas, P. Thorne, K. A. Thorne, K. S. Thrane, E. Thuering, A. Tokmakov, K. V. Tomlinson, C. Toncelli, A. Tonelli, M. Torre, O. Torres, C. Torrie, C. I. Tournefier, E. Tucker, E. Travasso, F. Traylor, G. Tseng, K. Ugolini, D. Vahlbruch, H. Vajente, G. van den Brand, J. F. J. Van den Broeck, C. van der Putten, S. van Veggel, A. A. Vass, S. Vasuth, M. Vaulin, R. Vavoulidis, M. Vecchio, A. Vedovato, G. Veitch, J. Veitch, P. J. Veltkamp, C. Verkindt, D. Vetrano, F. Vicere, A. Villar, A. E. Vinet, J. -Y. Vitale, S. Vocca, H. Vorvick, C. Vyatchanin, S. P. Wade, A. Wade, L. Wade, M. Waldman, S. J. Wallace, L. Wan, Y. Wang, M. Wang, X. Wang, Z. Wanner, A. Ward, R. L. Was, M. Weinert, M. Weinstein, A. J. Weiss, R. Wen, L. Wessels, P. West, M. Westphal, T. Wette, K. Whelan, J. T. Whitcomb, S. E. White, D. J. Whiting, B. F. Wilkinson, C. Willems, P. A. Williams, L. Williams, R. Willke, B. Winkelmann, L. Winkler, W. Wipf, C. C. Wiseman, A. G. Wittel, H. Woan, G. Wooley, R. Worden, J. Yakushin, I. Yamamoto, H. Yamamoto, K. Yancey, C. C. Yang, H. Yeaton-Massey, D. Yoshida, S. Yu, P. Yvert, M. Zadrozny, A. Zanolin, M. Zendri, J. -P. Zhang, F. Zhang, L. Zhang, W. Zhao, C. Zotov, N. Zucker, M. E. Zweizig, J. Briggs, M. S. Connaughton, V. Hurley, K. C. Jenke, P. A. von Kienlin, A. Rau, A. Zhang, X. -L. CA LIGO Sci Collaboration Virgo Colla TI SEARCH FOR GRAVITATIONAL WAVES ASSOCIATED WITH GAMMA-RAY BURSTS DURING LIGO SCIENCE RUN 6 AND VIRGO SCIENCE RUNS 2 AND 3 SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: close; gamma-ray burst: general; gravitational waves ID NEUTRON STAR BINARIES; GIANT FLARE; JET BREAKS; APRIL 1998; REDSHIFT DISTRIBUTION; PRECURSOR ACTIVITY; RELATIVISTIC JETS; UNUSUAL SUPERNOVA; COMPACT BINARIES; LOCAL UNIVERSE AB We present the results of a search for gravitational waves associated with 154 gamma-ray bursts (GRBs) that were detected by satellite-based gamma-ray experiments in 2009-2010, during the sixth LIGO science run and the second and third Virgo science runs. We perform two distinct searches: a modeled search for coalescences of either two neutron stars or a neutron star and black hole, and a search for generic, unmodeled gravitational-wave bursts. We find no evidence for gravitational-wave counterparts, either with any individual GRB in this sample or with the population as a whole. For all GRBs we place lower bounds on the distance to the progenitor, under the optimistic assumption of a gravitational-wave emission energy of 10(-2) M-circle dot c(2) at 150 Hz, with a median limit of 17 Mpc. For short-hard GRBs we place exclusion distances on binary neutron star and neutron-star-black-hole progenitors, using astrophysically motivated priors on the source parameters, with median values of 16 Mpc and 28 Mpc, respectively. These distance limits, while significantly larger than for a search that is not aided by GRB satellite observations, are not large enough to expect a coincidence with a GRB. 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H.; Osthelder, C.; Patel, P.; Pedraza, M.; Phelps, M.; Price, L. R.; Privitera, S.; Reitze, D. H.; Robertson, N. A.; Rollins, J. G.; Sannibale, V.; Santamaria, L.; Seifert, F.; Singer, A.; Singer, L.; Smith, M. R.; Stochino, A.; Taylor, R.; Torrie, C. I.; Vass, S.; Villar, A. E.; Wallace, L.; Weinstein, A. J.; Whitcomb, S. E.; Willems, P. A.; Williams, R.; Yamamoto, H.; Yeaton-Massey, D.; Zhang, L.; Zweizig, J.] CALTECH, LIGO, Pasadena, CA 91125 USA. [Abbott, T. D.; Smith, J. R.] Calif State Univ Fullerton, Fullerton, CA 92831 USA. [Abernathy, M.; Barr, B.; Bassiri, R.; Bastarrika, M.; Bell, A. S.; Beveridge, N.; Campsie, P.; Cumming, A.; Cunningham, L.; Edgar, M.; Evans, K.; Gill, C.; Grant, A.; Gray, N.; Hammond, G.; Haughian, K.; Hendry, M. A.; Heng, I. S.; Hild, S.; Hough, J.; Huttner, S. H.; Jones, R.; Kumar, R.; Lawrie, C.; Macdonald, E.; Martin, I. W.; Murray, P. G.; Nelson, J.; Newton, G.; Pitkin, M.; Plissi, M. V.; Reid, S.; Robertson, N. A.; Rowan, S.; Santiago-Prieto, I.; Scott, J.; Sorazu, B.; Speirits, F. C.; Strain, K. A.; Torrie, C. I.; van Veggel, A. A.; Woan, G.] Univ Glasgow, SUPA, Glasgow G12 8QQ, Lanark, Scotland. [Accadia, T.; Bebronne, M.; Buskulic, D.; Dietz, A.; Gouaty, R.; Letendre, N.; Marion, F.; Masserot, A.; Mours, B.; Rolland, L.; Tournefier, E.; Verkindt, D.; Yvert, M.] Univ Savoie, CNRS, Lab Annecy le Vieux Phys Particules LAPP, IN2P3, F-74941 Annecy Le Vieux, France. [Acernese, F.; Barone, F.; Calloni, E.; De Rosa, R.; Di Fiore, L.; Forte, L. A.; Garufi, F.; Milano, L.; Mosca, S.; Parisi, M.; Persichetti, G.; Romano, R.] Complesso Univ Monte S Angelo, INFN, Sez Napoli, I-80126 Naples, Italy. [Acernese, F.; Barone, F.; Romano, R.] Univ Salerno, I-84084 Salerno, Italy. [Adams, C.; Birch, J.; Bridges, D. O.; Cowart, M.; Evans, T.; Forsi, E.; Frolov, V. V.; Fyffe, M.; Giaime, J. A.; Giardina, K. D.; Guido, C.; Hanson, J.; Holt, K.; Huynh-Dinh, T.; Katzman, W.; Kinzel, D. L.; Lormand, M.; Meyer, M. 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J.; Poeld, J.; Prijatelj, M.; Prix, R.; Puncken, O.; Roever, C.; Ruediger, A.; Salemi, F.; Schilling, R.; Schnabel, R.; Schreiber, E.; Schulz, B.; Shaltev, M.; Steinlechner, J.; Steinlechner, S.; Tarabrin, S. P.; Taylor, J. R.; Thuering, A.; Vahlbruch, H.; Veltkamp, C.; Wanner, A.; Was, M.; Weinert, M.; Wessels, P.; Westphal, T.; Wette, K.; Willke, B.; Winkelmann, L.; Winkler, W.; Wittel, H.; Yamamoto, K.] Max Planck Inst Gravitat Phys, Albert Einstein Inst, D-30167 Hannover, Germany. [Affeldt, C.; Allen, B.; Aufmuth, P.; Aulbert, C.; Bauchrowitz, J.; Bertolini, A.; Bock, O.; Bogan, C.; Born, M.; Breyer, J.; Brinkmann, M.; Britzger, M.; Dahl, K.; Danzmann, K.; Di Palma, I.; Eberle, T.; Fehrmann, H.; Frede, M.; Friedrich, D.; Goetz, E.; Gossler, S.; Graef, C.; Grote, H.; Hewitson, M.; Kaufer, H.; Kawazoe, F.; Khalaidovski, A.; Kim, H.; Kranz, O.; Kringel, V.; Kuehn, G.; Kwee, P.; Lastzka, N.; Leong, J. R.; Lueck, H.; Machenschalk, B.; Mazzolo, G.; Mehmet, M.; Meier, T.; Mossavi, K.; Mueller-Ebhardt, H.; Pickenpack, M.; Pletsch, H. J.; Poeld, J.; Prijatelj, M.; Prix, R.; Puncken, O.; Roever, C.; Ruediger, A.; Salemi, F.; Schilling, R.; Schnabel, R.; Schreiber, E.; Schulz, B.; Shaltev, M.; Steinlechner, J.; Steinlechner, S.; Tarabrin, S. P.; Taylor, J. R.; Thuering, A.; Vahlbruch, H.; Veltkamp, C.; Wanner, A.; Was, M.; Weinert, M.; Wessels, P.; Westphal, T.; Wette, K.; Willke, B.; Winkelmann, L.; Winkler, W.; Wittel, H.; Yamamoto, K.] Leibniz Univ Hannover, D-30167 Hannover, Germany. [Agathos, M.; Bauer, Th. S.; Beker, M. G.; Blom, M.; Bulten, H. J.; Del Pozzo, W.; Jonker, R. J. G.; Li, T. G. F.; Maksimovic, I.; Rabeling, D. S.; ter Braack, A. P. M.; van den Brand, J. F. J.; Van den Broeck, C.; van der Putten, S.; Vitale, S.] NIKHEF H, NL-1009 DB Amsterdam, Netherlands. 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J.; Hallam, J. M.; Kokeyama, K.; Lodhia, D.; Mandel, I.; Page, A.; Smith, R. J. E.; Vecchio, A.; Wang, M.] Univ Birmingham, Birmingham B15 2TT, W Midlands, England. [Astone, P.; Colla, A.; Conte, A.; Frasca, S.; Majorana, E.; Naticchioni, L.; Palomba, C.; Puppo, P.; Rapagnani, P.; Ricci, F.] Ist Nazl Fis Nucl, Sez Roma, I-00185 Rome, Italy. [Atkinson, D.; Barker, D.; Barton, M. A.; Batch, J.; Berliner, J. M.; Bland, B.; Clara, F.; Cook, D.; Flanigan, M.; Garcia, J.; Gray, C.; Hanks, J.; Ingram, D. R.; Kawabe, K.; Landry, M.; Lubinski, M.; McCarthy, R.; Mendell, G.; Moraru, D.; Moreno, G.; Raab, F. J.; Radkins, H.; Reed, C. M.; Rodruck, M.; Ryan, K.; Sandberg, V.; Savage, R. L.; Schwinberg, P.; Sigg, D.; Steinert, E.; Thomas, P.; Vorvick, C.; Wilkinson, C.; Worden, J.] Hanford Observ, LIGO, Richland, WA 99352 USA. [Babak, S.; Behnke, B.; Grunewald, S.; Krishnan, B.; Leaci, P.; Papa, M. A.; Robinson, E. L.; Schutz, B. 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RI Mow-Lowry, Conor/F-8843-2015; Finn, Lee Samuel/A-3452-2009; Sigg, Daniel/I-4308-2015; Puppo, Paola/J-4250-2012; Tacca, Matteo/J-1599-2015; Graef, Christian/J-3167-2015; Ottaway, David/J-5908-2015; Garufi, Fabio/K-3263-2015; Neri, Igor/F-1482-2010; Shaddock, Daniel/A-7534-2011; Postiglione, Fabio/O-4744-2015; Rocchi, Alessio/O-9499-2015; Martelli, Filippo/P-4041-2015; Miao, Haixing/O-1300-2013; Khazanov, Efim/B-6643-2014; Mitrofanov, Valery/D-8501-2012; Bilenko, Igor/D-5172-2012; Nelson, John/H-7215-2014; Losurdo, Giovanni/K-1241-2014; Danilishin, Stefan/K-7262-2012; Canuel, Benjamin/C-7459-2014; Lee, Chang-Hwan/B-3096-2015; Khalili, Farit/D-8113-2012; McClelland, David/E-6765-2010; Vecchio, Alberto/F-8310-2015; Parisi, Maria/D-2817-2013; Steinlechner, Sebastian/D-5781-2013; Strigin, Sergey/I-8337-2012; Colla, Alberto/J-4694-2012; Drago, Marco/E-7134-2013; Vyatchanin, Sergey/J-2238-2012; Re, Virginia /F-6403-2013; Gorodetsky, Michael/C-5938-2008; Bell, Angus/E-7312-2011; Hild, Stefan/A-3864-2010; Martin, Iain/A-2445-2010; Pitkin, Matthew/I-3802-2013; Prokhorov, Leonid/I-2953-2012; Gammaitoni, Luca/B-5375-2009; Zhao, Chunnong/C-2403-2013; Ju, Li/C-2623-2013; Lam, Ping Koy/A-5276-2008; Marchesoni, Fabio/A-1920-2008; Allen, Bruce/K-2327-2012; prodi, giovanni/B-4398-2010; Chen, Yanbei/A-2604-2013; Costa, Cesar/G-7588-2012; CONTE, ANDREA/J-6667-2012; Vicere, Andrea/J-1742-2012; Gemme, Gianluca/C-7233-2008; Punturo, Michele/I-3995-2012; Strain, Kenneth/D-5236-2011; Ward, Robert/I-8032-2014; Cesarini, Elisabetta/C-4507-2017; Chow, Jong/A-3183-2008; Frey, Raymond/E-2830-2016; Ciani, Giacomo/G-1036-2011; Di Virgilio, Angela Dora Vittoria/E-9078-2015; Sergeev, Alexander/F-3027-2017; Harms, Jan/J-4359-2012; Branchesi, Marica/P-2296-2015; Gehring, Tobias/A-8596-2016; Howell, Eric/H-5072-2014; Heidmann, Antoine/G-4295-2016; Ott, Christian/G-2651-2011; mosca, simona/I-7116-2012; Frasconi, Franco/K-1068-2016; Pinto, Innocenzo/L-3520-2016; Ferrante, Isidoro/F-1017-2012; Prato, Mirko/D-8531-2012; Travasso, Flavio/J-9595-2016; Bartos, Imre/A-2592-2017; Cella, Giancarlo/A-9946-2012 OI Finn, Lee Samuel/0000-0002-3937-0688; Sigg, Daniel/0000-0003-4606-6526; Puppo, Paola/0000-0003-4677-5015; Tacca, Matteo/0000-0003-1353-0441; Graef, Christian/0000-0002-4535-2603; Garufi, Fabio/0000-0003-1391-6168; Neri, Igor/0000-0002-9047-9822; Shaddock, Daniel/0000-0002-6885-3494; Postiglione, Fabio/0000-0003-0628-3796; Rocchi, Alessio/0000-0002-1382-9016; Martelli, Filippo/0000-0003-3761-8616; Miao, Haixing/0000-0003-4101-9958; Nelson, John/0000-0002-6928-617X; Losurdo, Giovanni/0000-0003-0452-746X; Danilishin, Stefan/0000-0001-7758-7493; Lee, Chang-Hwan/0000-0003-3221-1171; McClelland, David/0000-0001-6210-5842; Vecchio, Alberto/0000-0002-6254-1617; Steinlechner, Sebastian/0000-0003-4710-8548; Gorodetsky, Michael/0000-0002-5159-2742; Bell, Angus/0000-0003-1523-0821; Pitkin, Matthew/0000-0003-4548-526X; Gammaitoni, Luca/0000-0002-4972-7062; Veitch, John/0000-0002-6508-0713; Principe, Maria/0000-0002-6327-0628; Kanner, Jonah/0000-0001-8115-0577; Zhao, Chunnong/0000-0001-5825-2401; Lam, Ping Koy/0000-0002-4421-601X; Marchesoni, Fabio/0000-0001-9240-6793; Allen, Bruce/0000-0003-4285-6256; prodi, giovanni/0000-0001-5256-915X; Vicere, Andrea/0000-0003-0624-6231; Gemme, Gianluca/0000-0002-1127-7406; Punturo, Michele/0000-0001-8722-4485; Strain, Kenneth/0000-0002-2066-5355; Vitale, Salvatore/0000-0003-2700-0767; PERSICHETTI, GIANLUCA/0000-0001-8424-9791; Freise, Andreas/0000-0001-6586-9901; Nitz, Alexander/0000-0002-1850-4587; Mandel, Ilya/0000-0002-6134-8946; Whiting, Bernard F/0000-0002-8501-8669; Murphy, David/0000-0002-8538-815X; Zweizig, John/0000-0002-1521-3397; Del Pozzo, Walter/0000-0003-3978-2030; O'Shaughnessy, Richard/0000-0001-5832-8517; Gray, Norman/0000-0002-1941-9202; Granata, Massimo/0000-0003-3275-1186; Di Paolo Emilio, Maurizio/0000-0002-9558-3610; Naticchioni, Luca/0000-0003-2918-0730; Nishizawa, Atsushi/0000-0003-3562-0990; calloni, enrico/0000-0003-4819-3297; Scott, Jamie/0000-0001-6701-6515; Sorazu, Borja/0000-0002-6178-3198; Bondu, Francois/0000-0001-6487-5197; Boschi, Valerio/0000-0001-8665-2293; Papa, M.Alessandra/0000-0002-1007-5298; Vocca, Helios/0000-0002-1200-3917; Pinto, Innocenzo M./0000-0002-2679-4457; Farr, Ben/0000-0002-2916-9200; Coccia, Eugenio/0000-0002-6669-5787; Vetrano, Flavio/0000-0002-7523-4296; Husa, Sascha/0000-0002-0445-1971; Milano, Leopoldo/0000-0001-9487-5876; Swinkels, Bas/0000-0002-3066-3601; Guidi, Gianluca/0000-0002-3061-9870; Drago, Marco/0000-0002-3738-2431; Hallam, Jonathan Mark/0000-0002-7087-0461; Ward, Robert/0000-0001-5503-5241; Ricci, Fulvio/0000-0001-5475-4447; Vedovato, Gabriele/0000-0001-7226-1320; Cesarini, Elisabetta/0000-0001-9127-3167; Chow, Jong/0000-0002-2414-5402; Frey, Raymond/0000-0003-0341-2636; Ciani, Giacomo/0000-0003-4258-9338; Di Virgilio, Angela Dora Vittoria/0000-0002-2237-7533; Jaranowski, Piotr/0000-0001-8085-3414; Fairhurst, Stephen/0000-0001-8480-1961; Whelan, John/0000-0001-5710-6576; Aulbert, Carsten/0000-0002-1481-8319; Stein, Leo/0000-0001-7559-9597; Matichard, Fabrice/0000-0001-8982-8418; Gehring, Tobias/0000-0002-4311-2593; Howell, Eric/0000-0001-7891-2817; Heidmann, Antoine/0000-0002-0784-5175; Ott, Christian/0000-0003-4993-2055; mosca, simona/0000-0001-7869-8275; Frasconi, Franco/0000-0003-4204-6587; Ferrante, Isidoro/0000-0002-0083-7228; Prato, Mirko/0000-0002-2188-8059; Travasso, Flavio/0000-0002-4653-6156; Cella, Giancarlo/0000-0002-0752-0338 FU United States National Science Foundation; Science and Technology Facilities Council of the United Kingdom; Max-Planck-Society; State of Niedersachsen/Germany; Australian Research Council; International Science Linkages program of the Commonwealth of Australia; Council of Scientific and Industrial Research of India; Istituto Nazionale di Fisica Nucleare of Italy; Spanish Ministerio de Economia y Competitividad; Conselleria d'Economia Hisenda i Innovacio of the Govern de les Illes Balears; Foundation for Fundamental Research on Matter; Polish Ministry of Science and Higher Education; FOCUS Programme of Foundation for Polish Science; Royal Society; Scottish Funding Council; Scottish Universities Physics Alliance; National Aeronautics and Space Administration; Carnegie Trust; Leverhulme Trust; David and Lucile Packard Foundation; Research Corporation; Alfred P. Sloan Foundation; Netherlands Organisation for Scientific Research FX We are indebted to the observers of the electromagnetic events and the Gamma-ray burst Coordinates Network for providing us with valuable data. The authors gratefully acknowledge the support of the United States National Science Foundation for the construction and operation of the LIGO Laboratory, the Science and Technology Facilities Council of the United Kingdom, the Max-Planck-Society, and the State of Niedersachsen/Germany for support of the construction and operation of the GEO600 detector, and the Italian Istituto Nazionale di Fisica Nucleare and the French Centre National de la Recherche Scientifique for the construction and operation of the Virgo detector. The authors also gratefully acknowledge the support of the research by these agencies and by the Australian Research Council, the International Science Linkages program of the Commonwealth of Australia, the Council of Scientific and Industrial Research of India, the Istituto Nazionale di Fisica Nucleare of Italy, the Spanish Ministerio de Economia y Competitividad, the Conselleria d'Economia Hisenda i Innovacio of the Govern de les Illes Balears, the Foundation for Fundamental Research on Matter supported by the Netherlands Organisation for Scientific Research, the Polish Ministry of Science and Higher Education, the FOCUS Programme of Foundation for Polish Science, the Royal Society, the Scottish Funding Council, the Scottish Universities Physics Alliance, the National Aeronautics and Space Administration, the Carnegie Trust, the Leverhulme Trust, the David and Lucile Packard Foundation, the Research Corporation, and the Alfred P. Sloan Foundation. This document has been assigned LIGO Laboratory document number LIGO-P1000121-v10. NR 144 TC 66 Z9 66 U1 7 U2 99 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD NOV 20 PY 2012 VL 760 IS 1 AR 12 DI 10.1088/0004-637X/760/1/12 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 035DD UT WOS:000310922200012 ER PT J AU Barry, RK Demory, BO Segransan, D Forveille, T Danchi, WC Di Folco, E Queloz, D Spooner, HR Torres, G Traub, WA Delfosse, X Mayor, M Perrier, C Udry, S AF Barry, R. K. Demory, B. -O. Segransan, D. Forveille, T. Danchi, W. C. Di Folco, E. Queloz, D. Spooner, H. R. Torres, G. Traub, W. A. Delfosse, X. Mayor, M. Perrier, C. Udry, S. TI A PRECISE PHYSICAL ORBIT FOR THE M-DWARF BINARY GLIESE 268 SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars: general; stars: individual (Gliese 268); techniques: interferometric; techniques: radial velocities ID LOW-MASS STARS; ECLIPSING BINARY; ACCURATE MASSES; SPECTROSCOPIC BINARIES; EVOLUTIONARY MODELS; LAMBDA-VIRGINIS; MAIN-SEQUENCE; INTERFEROMETER; SYSTEM AB We report high-precision interferometric and radial velocity (RV) observations of the M-dwarf binary Gl 268. Combining measurements conducted using the IOTA interferometer and the ELODIE and Harvard Center for Astrophysics RV instruments leads to a mass of 0.22596 +/- 0.00084 M-circle dot for component A and 0.19230 +/- 0.00071 M-circle dot for component B. The system parallax as determined by these observations is 0.1560 +/- 0.0030 arcsec-a measurement with 1.9% uncertainty in excellent agreement with Hipparcos (0.1572 +/- 0.0033). The absolute H-band magnitudes of the component stars are not well constrained by these measurements; however, we can place an approximate upper limit of 7.95 and 8.1 for Gl 268A and B, respectively. We test these physical parameters against the predictions of theoretical models that combine stellar evolution with high fidelity, non-gray atmospheric models. Measured and predicted values are compatible within 2 sigma. These results are among the most precise masses measured for visual binaries and compete with the best adaptive optics and eclipsing binary results. C1 [Barry, R. K.; Danchi, W. C.] NASA, Goddard Space Flight Ctr, Lab Exoplanets & Stellar Astrophys, Greenbelt, MD 20771 USA. [Demory, B. -O.; Segransan, D.; Di Folco, E.; Queloz, D.; Udry, S.] MIT, Cambridge, MA 02139 USA. [Forveille, T.; Delfosse, X.; Mayor, M.; Perrier, C.] Univ Geneva, Observ Geneva, CH-1290 Versoix, Switzerland. [Spooner, H. R.] Univ Maryland, College Pk, MD 20742 USA. [Torres, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02136 USA. [Traub, W. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Barry, RK (reprint author), NASA, Goddard Space Flight Ctr, Lab Exoplanets & Stellar Astrophys, Code 667, Greenbelt, MD 20771 USA. EM Richard.K.Barry@nasa.gov OI Demory, Brice-Olivier/0000-0002-9355-5165 FU National Aeronautics and Space Administration; University of Grenoble Observatory; Jet Propulsion Laboratory; California Association for Research in Astronomy; Harvard-Smithsonian Center for Astrophysics; Fonds National Suisse de la Recherche Scientifique FX We are grateful to the National Aeronautics and Space Administration, the University of Grenoble Observatory, Jet Propulsion Laboratory, the California Association for Research in Astronomy, and to the Harvard-Smithsonian Center for Astrophysics for support of this research. We are also grateful for the work on software to reduce the interferometric data from IOTA by J. Monnier. B.O.D. acknowledges the support of the Fonds National Suisse de la Recherche Scientifique. R.K.B. acknowledges the technical editing assistance of C. M. Morales Sabogal. NR 46 TC 1 Z9 1 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD NOV 20 PY 2012 VL 760 IS 1 AR 55 DI 10.1088/0004-637X/760/1/55 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 035DD UT WOS:000310922200055 ER PT J AU Bryans, P Pesnell, WD AF Bryans, P. Pesnell, W. D. TI THE EXTREME-ULTRAVIOLET EMISSION FROM SUN-GRAZING COMETS SO ASTROPHYSICAL JOURNAL LA English DT Article DE comets: general; comets: individual (C/2011 N3, C/2011 W3); Sun: corona; Sun: general ID PHOTOIONIZATION CROSS-SECTIONS; IONIZATION RATE COEFFICIENTS; X-RAY; SUNGRAZING COMETS; ELEMENTS HYDROGEN; ATOMIC DATABASE; CHARGE-TRANSFER; ANALYTIC FITS; SOLAR; SPECTRUM AB The Atmospheric Imaging Assembly (AIA) on the Solar Dynamics Observatory has observed two Sun-grazing comets as they passed through the solar atmosphere. Both passages resulted in a measurable enhancement of extreme-ultraviolet (EUV) radiance in several of the AIA bandpasses. We explain this EUV emission by considering the evolution of the cometary atmosphere as it interacts with the ambient solar atmosphere. Molecules in the comet rapidly sublimate as it approaches the Sun. They are then photodissociated by the solar radiation field to create atomic species. Subsequent ionization of these atoms produces a higher abundance of ions than normally present in the corona and results in EUV emission in the wavelength ranges of the AIA telescope passbands. C1 [Bryans, P.] NASA, ADNET Syst Inc, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Bryans, P (reprint author), NASA, ADNET Syst Inc, Goddard Space Flight Ctr, Code 671, Greenbelt, MD 20771 USA. RI Pesnell, William/D-1062-2012 OI Pesnell, William/0000-0002-8306-2500 FU Solar Dynamics Observatory FX Research was supported by the Solar Dynamics Observatory. We acknowledge many helpful comments and suggestions from K. Battams, J.C. Brown, H.S. Hudson, W. Liu, P. Saint-Hilaire, and C.J. Schrijver. NR 39 TC 14 Z9 14 U1 0 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD NOV 20 PY 2012 VL 760 IS 1 AR 18 DI 10.1088/0004-637X/760/1/18 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 035DD UT WOS:000310922200018 ER PT J AU Gomez, HL Krause, O Barlow, MJ Swinyard, BM Owen, PJ Clark, CJR Matsuura, M Gomez, EL Rho, J Besel, MA Bouwman, J Gear, WK Henning, T Ivison, RJ Polehampton, ET Sibthorpe, B AF Gomez, H. L. Krause, O. Barlow, M. J. Swinyard, B. M. Owen, P. J. Clark, C. J. R. Matsuura, M. Gomez, E. L. Rho, J. Besel, M. -A. Bouwman, J. Gear, W. K. Henning, Th. Ivison, R. J. Polehampton, E. T. Sibthorpe, B. TI A COOL DUST FACTORY IN THE CRAB NEBULA: A HERSCHEL STUDY OF THE FILAMENTS SO ASTROPHYSICAL JOURNAL LA English DT Article DE dust, extinction; ISM: individual objects (Crab Nebula); ISM: supernova remnants; submillimeter: ISM ID LASER MAGNETIC-RESONANCE; CORE-COLLAPSE SUPERNOVAE; SPITZER-SPACE-TELESCOPE; LARGE-MAGELLANIC-CLOUD; CHEMICAL EVOLUTION; OPTICAL-PROPERTIES; SPIRE INSTRUMENT; EARLY UNIVERSE; II SUPERNOVAE; COLD DUST AB Whether supernovae are major sources of dust in galaxies is a long-standing debate. We present infrared and submillimeter photometry and spectroscopy from the Herschel Space Observatory of the Crab Nebula between 51 and 670 mu m as part of the Mass Loss from Evolved StarS program. We compare the emission detected with Herschel with multiwavelength data including millimeter, radio, mid-infrared, and archive optical images. We carefully remove the synchrotron component using the Herschel and Planck fluxes measured in the same epoch. The contribution from line emission is removed using Herschel spectroscopy combined with Infrared Space Observatory archive data. Several forbidden lines of carbon, oxygen, and nitrogen are detected where multiple velocity components are resolved, deduced to be from the nitrogen-depleted, carbon-rich ejecta. No spectral lines are detected in the SPIRE wavebands; in the PACS bands, the line contribution is 5% and 10% at 70 and 100 mu m and negligible at 160 mu m. After subtracting the synchrotron and line emission, the remaining far-infrared continuum can be fit with two dust components. Assuming standard interstellar silicates, the mass of the cooler component is 0.24(-0.08)(+0.32)M(circle dot) for T = 28.1(-3.2)(+5.5)K. Amorphous carbon grains require 0.11 +/- 0.01M(circle dot) of dust with T = 33.8(-1.8)(+2.3)K. A single temperature modified blackbody with 0.14M(circle dot) and 0.08M(circle dot) for silicate and carbon dust, respectively, provides an adequate fit to the far-infrared region of the spectral energy distribution but is a poor fit at 24-500 mu m. The Crab Nebula has condensed most of the relevant refractory elements into dust, suggesting the formation of dust in core-collapse supernova ejecta is efficient. C1 [Gomez, H. L.; Clark, C. J. R.; Gomez, E. L.; Gear, W. K.] Cardiff Univ, Sch Phys & Astron, The Parade, Cardiff CF24 3AA, S Glam, Wales. [Krause, O.; Besel, M. -A.; Bouwman, J.; Henning, Th.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Barlow, M. J.; Swinyard, B. M.; Owen, P. J.; Matsuura, M.] UCL, Dept Phys & Astron, London WC1E 6BT, England. [Swinyard, B. M.; Polehampton, E. T.] Rutherford Appleton Lab, Space Sci & Technol Dept, Didcot OX11 0QX, Oxon, England. [Gomez, E. L.] Las Cumbres Obsevratory Global Telescope Network, Goleta, CA 93117 USA. [Rho, J.] NASA, Ames Res Ctr, Univ Space Res Assoc, SOFIA Sci Ctr, Moffett Field, CA 94035 USA. [Ivison, R. J.; Sibthorpe, B.] Royal Observ Edinburgh, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland. [Ivison, R. J.] Univ Edinburgh, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland. [Polehampton, E. T.] Univ Lethbridge, Inst Space Imaging Sci, Lethbridge, AB T1J 1B1, Canada. RP Gomez, HL (reprint author), Cardiff Univ, Sch Phys & Astron, The Parade, Cardiff CF24 3AA, S Glam, Wales. RI Barlow, Michael/A-5638-2009; Ivison, R./G-4450-2011 OI Barlow, Michael/0000-0002-3875-1171; Ivison, R./0000-0001-5118-1313 FU Las Cumbres Observatory; National Aeronautics and Space Administration; BMVIT (Austria); ESA-PRODEX (Belgium); CEA/CNES (France); DLR (Germany); ASI/INAF (Italy); CICYT/MCYT(Spain); CSA (Canada); NAOC (China); CEA (France); CNES (France); CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC (UK); UKSA (UK); NASA (USA) FX We thank the referee Tea Temim for her constructive and helpful referee report. This research made use of APLpy, an open-source plotting package for Python hosted at http://aplpy.github.com. We thank Robbie Auld, Eli Dwek, Stuart Lowe, Takaya Nozawa, and Matt Smith for informative discussions and J D Armstrong for support with the Faulkes Telescope North. H. L. G. acknowledges the support of Las Cumbres Observatory. 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. PACS has been developed by a consortium of institutes led by MPE (Germany) and including UVIE (Austria); KU Leuven, CSL, IMEC (Belgium); CEA, LAM (France); MPIA (Germany); INAF-IFSI/OAA/OAP/OAT, LENS, SISSA (Italy); IAC (Spain). This development has been supported by the funding agencies BMVIT (Austria), ESA-PRODEX (Belgium), CEA/CNES (France), DLR (Germany), ASI/INAF (Italy), and CICYT/MCYT(Spain). SPIRE has been developed by a consortium of institutes led by Cardiff Univ. (UK) and including: Univ. Lethbridge (Canada); NAOC (China); CEA, LAM (France); IFSI, Univ. Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, Univ. Sussex (UK); and Caltech, JPL, NHSC, Univ. Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC, UKSA (UK); and NASA (USA). HIPE is a joint development by the Herschel Science Ground Segment Consortium, consisting of ESA, the NASA Herschel Science Center and the HIFI, PACS and SPIRE consortia. NR 95 TC 59 Z9 59 U1 0 U2 9 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD NOV 20 PY 2012 VL 760 IS 1 AR 96 DI 10.1088/0004-637X/760/1/96 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 035DD UT WOS:000310922200096 ER PT J AU Hathaway, DH AF Hathaway, David H. TI SUPERGRANULES AS PROBES OF THE SUN'S MERIDIONAL CIRCULATION SO ASTROPHYSICAL JOURNAL LA English DT Article DE convection; Sun: rotation ID MICHELSON DOPPLER IMAGER; WAVE-LIKE PROPERTIES; DIFFERENTIAL ROTATION; MAGNETIC-FIELDS; SOLAR CONVECTION; LOCAL HELIOSEISMOLOGY; VELOCITY FIELDS; FLOW; EVOLUTION; TRANSPORT AB Recent analysis revealed that supergranules (convection cells seen at the Sun's surface) are advected by the zonal flows at depths equal to the widths of the cells themselves. Here we probe the structure of the meridional circulation by cross-correlating maps of the Doppler velocity signal using a series of successively longer time lags between maps. We find that the poleward meridional flow decreases in amplitude with time lag and reverses direction to become an equatorward return flow at time lags >24 hr. These cross-correlation results are dominated by larger and deeper cells at longer time lags. (The smaller cells have shorter lifetimes and do not contribute to the correlated signal at longer time lags.) We determine the characteristic cell size associated with each time lag by comparing the equatorial zonal flows measured at different time lags with the zonal flows associated with different cell sizes from a Fourier analysis. This association gives a characteristic cell size of similar to 50 Mm at a 24 hr time lag. This indicates that the poleward meridional flow returns equatorward at depths >50 Mm-just below the base of the surface shear layer. A substantial and highly significant equatorward flow (4.6 +/- 0.4 m s(-1)) is found at a time lag of 28 hr corresponding to a depth of similar to 70 Mm. This represents one of the first positive detections of the Sun's meridional return flow and illustrates the power of using supergranules to probe the Sun's internal dynamics. C1 NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. RP Hathaway, DH (reprint author), NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. EM david.hathaway@nasa.gov FU Heliophysics Causes and Consequences of the Minimum of Solar Cycle 23/24 Program; Living With a Star Program to NASA Marshall Space Flight Center FX The author thanks NASA for its support of this research through grants from the Heliophysics Causes and Consequences of the Minimum of Solar Cycle 23/24 Program and the Living With a Star Program to NASA Marshall Space Flight Center. He is indebted to Ron Moore and Lisa (Rightmire) Upton and an anonymous referee whose comments greatly improved the manuscript and to John Beck who produced the temporally filtered data from the original MDI Doppler data. He also thanks the American taxpayers who support scientific research in general and this research in particular. SOHO is a project of international cooperation between ESA and NASA. NR 47 TC 40 Z9 41 U1 1 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD NOV 20 PY 2012 VL 760 IS 1 AR 84 DI 10.1088/0004-637X/760/1/84 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 035DD UT WOS:000310922200084 ER PT J AU Hesman, BE Bjoraker, GL Sada, PV Achterberg, RK Jennings, DE Romani, PN Lunsford, AW Fletcher, LN Boyle, RJ Simon-Miller, AA Nixon, CA Irwin, PGJ AF Hesman, B. E. Bjoraker, G. L. Sada, P. V. Achterberg, R. K. Jennings, D. E. Romani, P. N. Lunsford, A. W. Fletcher, L. N. Boyle, R. J. Simon-Miller, A. A. Nixon, C. A. Irwin, P. G. J. TI ELUSIVE ETHYLENE DETECTED IN SATURN'S NORTHERN STORM REGION SO ASTROPHYSICAL JOURNAL LA English DT Article DE planets and satellites: atmospheres; planets and satellites: individual (Saturn) ID ROTOTRANSLATIONAL ABSORPTION-SPECTRA; OUTER PLANETS; THERMAL STRUCTURE; TEMPERATURES; ATMOSPHERE; PAIRS; STRATOSPHERE; DISTURBANCE; ABUNDANCE; EMISSION AB The massive eruption at 40 degrees N (planetographic latitude) on Saturn in 2010 December has produced significant and lasting effects in the northern hemisphere on temperature and species abundances. The northern storm region was observed on many occasions in 2011 by Cassini's Composite Infrared Spectrometer (CIRS). In 2011 May, temperatures in the stratosphere greater than 200 K were derived from CIRS spectra in the regions referred to as "beacons" (warm regions in the stratosphere). Ethylene has been detected in the beacon region in Saturn's northern storm region using CIRS. Ground-based observations using the high-resolution spectrometer Celeste on the McMath-Pierce Telescope on 2011 May 15 were used to confirm the detection and improve the altitude resolution in the retrieved profile. The derived ethylene profile from the CIRS data gives a C2H4 mole fraction of 5.9 +/- 4.5 x 10(-7) at 0.5 mbar, and from Celeste data it gives 2.7 +/- 0.45 x 10(-6) at 0.1 mbar. This is two orders of magnitude higher than the amount measured in the ultraviolet at other latitudes prior to the storm. It is also much higher than predicted by photochemical models, indicating that perhaps another production mechanism is required or a loss mechanism is being inhibited. C1 [Hesman, B. E.; Achterberg, R. K.; Nixon, C. A.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Hesman, B. E.; Bjoraker, G. L.; Achterberg, R. K.; Jennings, D. E.; Romani, P. N.; Simon-Miller, A. A.; Nixon, C. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Sada, P. V.] Univ Monterrey, Dept Fis & Matemat, Garza Garcia 66238, NL, Mexico. [Lunsford, A. W.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA. [Fletcher, L. N.] Clarendon Lab, Oxford OX1 3PU, England. [Boyle, R. J.] Dickinson Coll, Dept Phys & Astron, Carlisle, PA 17013 USA. [Hesman, B. E.; Achterberg, R. K.; Nixon, C. A.] CRESST, Greenbelt, MD 20771 USA. RP Hesman, BE (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA. EM brigette.e.hesman@nasa.gov RI Nixon, Conor/A-8531-2009; Fletcher, Leigh/D-6093-2011; Simon, Amy/C-8020-2012; OI Nixon, Conor/0000-0001-9540-9121; Fletcher, Leigh/0000-0001-5834-9588; Simon, Amy/0000-0003-4641-6186; Irwin, Patrick/0000-0002-6772-384X FU NASA Cassini/CIRS project; NASA Planetary Astronomy (PAST) Program [NNX11AJ47G]; NASA Cassini Data Analysis Participating Scientists (CDAPS) Program [NNX12AC24G] FX The authors thank the Cassini/CIRS calibration team for their assistance in the calibration of these data sets. The authors also thank the McMath-Pierce Telescope staff for their assistance during these observations. This research was supported by the NASA Cassini/CIRS project, by the NASA Planetary Astronomy (PAST) Program grant number NNX11AJ47G, and the NASA Cassini Data Analysis Participating Scientists (CDAPS) Program grant number NNX12AC24G. The National Solar Observatory is operated by the Association of Universities for Research in Astronomy under contract for the National Science Foundation. NR 25 TC 8 Z9 8 U1 0 U2 24 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD NOV 20 PY 2012 VL 760 IS 1 AR 24 DI 10.1088/0004-637X/760/1/24 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 035DD UT WOS:000310922200024 ER PT J AU Huber, D Ireland, MJ Bedding, TR Brandao, IM Piau, L Maestro, V White, TR Bruntt, H Casagrande, L Molenda-Zakowicz, J Aguirre, VS Sousa, SG Barclay, T Burke, CJ Chaplin, WJ Christensen-Dalsgaard, J Cunha, MS De Ridder, J Farrington, CD Frasca, A Garcia, RA Gilliland, RL Goldfinger, PJ Hekker, S Kawaler, SD Kjeldsen, H McAlister, HA Metcalfe, TS Miglio, A Monteiro, MJPFG Pinsonneault, MH Schaefer, GH Stello, D Stumpe, MC Sturmann, J Sturmann, L ten Brummelaar, TA Thompson, MJ Turner, N Uytterhoeven, K AF Huber, D. Ireland, M. J. Bedding, T. R. Brandao, I. M. Piau, L. Maestro, V. White, T. R. Bruntt, H. Casagrande, L. Molenda-Zakowicz, J. Aguirre, V. Silva Sousa, S. G. Barclay, T. Burke, C. J. Chaplin, W. J. Christensen-Dalsgaard, J. Cunha, M. S. De Ridder, J. Farrington, C. D. Frasca, A. Garcia, R. A. Gilliland, R. L. Goldfinger, P. J. Hekker, S. Kawaler, S. D. Kjeldsen, H. McAlister, H. A. Metcalfe, T. S. Miglio, A. Monteiro, M. J. P. F. G. Pinsonneault, M. H. Schaefer, G. H. Stello, D. Stumpe, M. C. Sturmann, J. Sturmann, L. ten Brummelaar, T. A. Thompson, M. J. Turner, N. Uytterhoeven, K. TI FUNDAMENTAL PROPERTIES OF STARS USING ASTEROSEISMOLOGY FROM KEPLER AND CoRoT AND INTERFEROMETRY FROM THE CHARA ARRAY SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars: late-type; stars: oscillations (including pulsations); techniques: interferometric; techniques: photometric ID SOLAR-LIKE OSCILLATIONS; RED GIANT STARS; EFFECTIVE TEMPERATURE SCALE; EXOPLANET HOST STARS; ALPHA-CENTAURI-B; 1ST 4 MONTHS; BOLOMETRIC CORRECTIONS; MAIN-SEQUENCE; SPECTROSCOPIC PARAMETERS; PHOTOMETRIC SYSTEM AB We present results of a long-baseline interferometry campaign using the PAVO beam combiner at the CHARA Array to measure the angular sizes of five main-sequence stars, one subgiant and four red giant stars for which solar-like oscillations have been detected by either Kepler or CoRoT. By combining interferometric angular diameters, Hipparcos parallaxes, asteroseismic densities, bolometric fluxes, and high-resolution spectroscopy, we derive a full set of near-model-independent fundamental properties for the sample. We first use these properties to test asteroseismic scaling relations for the frequency of maximum power (nu(max)) and the large frequency separation (Delta nu). We find excellent agreement within the observational uncertainties, and empirically show that simple estimates of asteroseismic radii for main-sequence stars are accurate to less than or similar to 4%. We furthermore find good agreement of our measured effective temperatures with spectroscopic and photometric estimates with mean deviations for stars between T-eff = 4600-6200 K of -22 +/- 32 K (with a scatter of 97 K) and -58 +/- 31 K (with a scatter of 93 K), respectively. Finally, we present a first comparison with evolutionarymodels, and find differences between observed and theoretical properties for the metal-rich main-sequence star HD 173701. We conclude that the constraints presented in this study will have strong potential for testing stellar model physics, in particular when combined with detailed modeling of individual oscillation frequencies. C1 [Huber, D.; Ireland, M. J.; Bedding, T. R.; Maestro, V.; White, T. R.; Stello, D.] Univ Sydney, Sch Phys, SIfA, Sydney, NSW 2006, Australia. [Huber, D.; Barclay, T.] NASA, Bay Area Environm Res Inst, Ames Res Ctr, Moffett Field, CA 94035 USA. [Ireland, M. J.] Macquarie Univ, Dept Phys & Astron, N Ryde, NSW 2109, Australia. [Ireland, M. J.] Australian Astron Observ, Epping, NSW 1710, Australia. [Brandao, I. M.; Sousa, S. G.; Cunha, M. S.; Monteiro, M. J. P. F. G.] Univ Porto, Ctr Astrofis, P-4150762 Oporto, Portugal. [Brandao, I. M.; Sousa, S. G.; Cunha, M. S.; Monteiro, M. J. P. F. G.] Univ Porto, Fac Ciencias, P-4150762 Oporto, Portugal. [Piau, L.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48823 USA. [Bruntt, H.; Aguirre, V. Silva; Chaplin, W. J.; Christensen-Dalsgaard, J.; Kjeldsen, H.] Aarhus Univ, Dept Phys & Astron, Stellar Astrophys Ctr, DK-8000 Aarhus C, Denmark. [Casagrande, L.] Australian Natl Univ, Mt Stromlo Observ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia. [Molenda-Zakowicz, J.] Univ Wroclaw, Astron Inst, PL-51622 Wroclaw, Poland. [Burke, C. J.; Stumpe, M. C.] NASA, SETI Inst, Ames Res Ctr, Moffett Field, CA 94035 USA. [Chaplin, W. J.; Miglio, A.] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. [De Ridder, J.] Katholieke Univ Leuven, Inst Sterrenkunde, B-3001 Louvain, Belgium. [Farrington, C. D.; Goldfinger, P. J.; McAlister, H. A.; Schaefer, G. H.; Sturmann, J.; Sturmann, L.; ten Brummelaar, T. A.; Turner, N.] Georgia State Univ, Ctr High Angular Resolut Astron, Atlanta, GA 30302 USA. [Frasca, A.] INAF Osservatorio Astrofis Catania, I-95123 Catania, Italy. [Garcia, R. A.] Univ Paris 07, CEA DSM CNRS, Lab AIM, Ctr Saclay,IRFU SAp, F-91191 Gif Sur Yvette, France. [Gilliland, R. L.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Hekker, S.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 XH Amsterdam, Netherlands. [Kawaler, S. D.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. [Metcalfe, T. S.] Space Sci Inst, Boulder, CO 80301 USA. [Pinsonneault, M. H.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Thompson, M. J.] NCAR, High Altitude Observ, Boulder, CO 80307 USA. [Uytterhoeven, K.] Inst Astrofis Canarias, E-38205 Tenerife, Spain. [Uytterhoeven, K.] Univ La Laguna, Dept Astrofis, E-38205 Tenerife, Spain. RP Huber, D (reprint author), Univ Sydney, Sch Phys, SIfA, Sydney, NSW 2006, Australia. EM daniel.huber@nasa.gov RI Sousa, Sergio/I-7466-2013; Brandao, Isa/M-5172-2013; Monteiro, Mario J.P.F.G./B-4715-2008; OI Garcia, Rafael/0000-0002-8854-3776; Kawaler, Steven/0000-0002-6536-6367; Sousa, Sergio/0000-0001-9047-2965; Brandao, Isa/0000-0002-1153-0942; Monteiro, Mario J.P.F.G./0000-0003-0513-8116; Cunha, Margarida/0000-0001-8237-7343; Frasca, Antonio/0000-0002-0474-0896; Ireland, Michael/0000-0002-6194-043X; Bedding, Timothy/0000-0001-5943-1460; Metcalfe, Travis/0000-0003-4034-0416; Bedding, Tim/0000-0001-5222-4661 FU National Science Foundation through NSF [AST-0606958]; Georgia State University through the College of Arts and Sciences; W. M. Keck Foundation; FCT/MCTES, Portugal [SFRH/BD/41213/2007]; Polish Ministry [N N203 405139]; Fundacao para a Ciencia e Tecnologia [SFRH/BPD/47611/2008]; European Research Council [ERC-2009-StG-239953, 267864]; UK Science and Technology Facilities Council (STFC); FCT (Portugal); POPH/FSE (EC); PTDC/CTE [AST/098754/2008]; Netherlands Organisation for Scientific Research (NWO); Spanish National Plan of RD [AYA2010-17803]; ASTERISK project; National Aeronautics and Space Administration; National Science Foundation FX The authors gratefully acknowledge the Kepler Science Office and everyone involved in the Kepler mission for making this paper possible. Funding for the Kepler mission is provided by NASA's Science Mission Directorate. The CHARA Array is funded by the National Science Foundation through NSF grant AST-0606958, by Georgia State University through the College of Arts and Sciences, and by the W. M. Keck Foundation. The CoRoT space mission, launched on 2006 December 27, has been developed and is operated by CNES, with the contribution of Austria, Belgium, Brazil, ESA (RSSD and Science Programme), Germany, and Spain. D. H. is thankful to Karsten Brogaard, Pieter Degroote, and Benoit Mosser for interesting discussions and comments on the paper. D. H., T. R. B., and V. M. acknowledge support from the Access to Major Research Facilities Program, administered by the Australian Nuclear Science and Technology Organisation (ANSTO). D. H. is supported by an appointment to the NASA Postdoctoral Program at Ames Research Center, administered by Oak Ridge Associated Universities through a contract with NASA. I. M. B. is supported by the grant SFRH/BD/41213/2007 from FCT/MCTES, Portugal. J.M.-.Z. acknowledges the Polish Ministry grant number N N203 405139. S. G. S. acknowledges the support from the Fundacao para a Ciencia e Tecnologia (grant ref. SFRH/BPD/47611/2008) and the European Research Council (grant ref. ERC-2009-StG-239953). W.J.C. acknowledges financial support from the UK Science and Technology Facilities Council (STFC). M. C. acknowledges funding from FCT (Portugal) and POPH/FSE (EC), for funding through a Contrato Cincia 2007 and the project PTDC/CTE-AST/098754/2008. S. H. acknowledges financial support from the Netherlands Organisation for Scientific Research (NWO). K. U. acknowledges financial support by the Spanish National Plan of R&D for 2010, project AYA2010-17803. Funding for the Stellar Astrophysics Centre is provided by The Danish National Research Foundation. The research is supported by the ASTERISK project (ASTERoseismic Investigations with SONG and Kepler) funded by the European Research Council (grant agreement No. 267864). This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. NR 162 TC 93 Z9 93 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 NOV 20 PY 2012 VL 760 IS 1 AR 32 DI 10.1088/0004-637X/760/1/32 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 035DD UT WOS:000310922200032 ER PT J AU Karpen, JT Antiochos, SK DeVore, CR AF Karpen, J. T. Antiochos, S. K. DeVore, C. R. TI THE MECHANISMS FOR THE ONSET AND EXPLOSIVE ERUPTION OF CORONAL MASS EJECTIONS AND ERUPTIVE FLARES SO ASTROPHYSICAL JOURNAL LA English DT Article DE magnetic fields; magnetohydrodynamics (MHD); Sun: coronal mass ejections (CMEs); Sun: flares ID HOMOLOGOUS SOLAR-FLARES; MAGNETIC RECONNECTION; BREAKOUT MODEL; CURRENT SHEETS; INTERNAL RECONNECTION; PARTICLE-ACCELERATION; EXTERNAL RECONNECTION; QUIESCENT FILAMENT; 2-RIBBON FLARES; FLUX EMERGENCE AB We have investigated the onset and acceleration of coronal mass ejections (CMEs) and eruptive flares. To isolate the eruption physics, our study uses the breakout model, which is insensitive to the energy buildup process leading to the eruption. We performed 2.5D simulations with adaptive mesh refinement that achieved the highest overall spatial resolution to date in a CME/eruptive flare simulation. The ultra-high resolution allows us to separate clearly the timing of the various phases of the eruption. Using new computational tools, we have determined the number and evolution of all X- and O-type nulls in the system, thereby tracking both the progress and the products of reconnection throughout the computational domain. Our results show definitively that CME onset is due to the start of fast reconnection at the breakout current sheet. Once this reconnection begins, eruption is inevitable; if this is the only reconnection in the system, however, the eruption will be slow. The explosive CME acceleration is triggered by fast reconnection at the flare current sheet. Our results indicate that the explosive eruption is caused by a resistive instability, not an ideal process. Moreover, both breakout and flare reconnections begin first as a form of weak tearing characterized by slowly evolving plasmoids, but eventually transition to a fast form with well-defined Alfvenic reconnection jets and rapid flux transfer. This transition to fast reconnection is required for both CME onset and explosive acceleration. We discuss the key implications of our results for CME/flare observations and for theories of magnetic reconnection. C1 [Karpen, J. T.; Antiochos, S. K.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [DeVore, C. R.] NRL, Washington, DC 20375 USA. RP Karpen, JT (reprint author), NASA, Goddard Space Flight Ctr, Code 674, Greenbelt, MD 20771 USA. RI Antiochos, Spiro/D-4668-2012; DeVore, C/A-6067-2015 OI Antiochos, Spiro/0000-0003-0176-4312; DeVore, C/0000-0002-4668-591X FU NASA's LWS research program; Heliophysics SR&T research program FX We thank B. Dennis, D. Falconer, and K. D. Leka for helpful discussions, and the referee for suggestions that have improved this paper. This work was supported in part by NASA's LWS and Heliophysics SR&T research programs. The computer resources were provided by the DoD HPCMP. NR 98 TC 54 Z9 54 U1 2 U2 13 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD NOV 20 PY 2012 VL 760 IS 1 AR 81 DI 10.1088/0004-637X/760/1/81 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 035DD UT WOS:000310922200081 ER PT J AU Tassis, K Hezareh, T Willacy, K AF Tassis, Konstantinos Hezareh, Talayeh Willacy, Karen TI A SEARCH FOR CO-EVOLVING ION AND NEUTRAL GAS SPECIES IN PRESTELLAR MOLECULAR CLOUD CORES SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: abundances; ISM: clouds; ISM: magnetic fields; ISM: molecules; magnetohydrodynamics (MHD); stars: formation ID TURBULENT AMBIPOLAR DIFFUSION; MAGNETIC-FIELD; CHEMISTRY; SPECTRA; DISSIPATION; 21(OH) AB A comparison between the widths of ion and neutral molecule spectral lines has been recently used to estimate the strength of the magnetic field in turbulent star-forming regions. However, the ion (HCO+) and neutral (HCN) species used in such studies may not be necessarily co-evolving at every scale and density, and thus, may not trace the same regions. Here, we use coupled chemical/dynamical models of evolving prestellar molecular cloud cores including non-equilibrium chemistry, with and without magnetic fields, to study the spatial distribution of HCO+ and HCN, which have been used in observations of spectral line width differences to date. In addition, we seek new ion-neutral pairs that are good candidates for such observations, because they have similar evolution and are approximately co-spatial in our models. We identify three such good candidate pairs: HCO+/NO, HCO+/CO, and NO+/NO. C1 [Tassis, Konstantinos; Hezareh, Talayeh] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Willacy, Karen] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Tassis, K (reprint author), Max Planck Inst Radioastron, D-53121 Bonn, Germany. RI Tassis, Konstantinos/C-3155-2011; OI Tassis, Konstantinos/0000-0002-8831-2038 FU Alexander von Humboldt foundation; NASA FX We thank Harold Yorke and Helmut Wiesemeyer for insightful and constructive comments that improved this paper. T.H. is funded by the Alexander von Humboldt foundation. The project was supported in part by the NASA Origins of Solar Systems program. Part of this work was carried out at the Jet Propulsion Laboratory, California Institute of Technology under contract with the National Aeronautics and Space Administration. NR 26 TC 2 Z9 2 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD NOV 20 PY 2012 VL 760 IS 1 AR 57 DI 10.1088/0004-637X/760/1/57 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 035DD UT WOS:000310922200057 ER PT J AU Teets, WK Weintraub, DA Kastner, JH Grosso, N Hamaguchi, K Richmond, M AF Teets, William K. Weintraub, David A. Kastner, Joel H. Grosso, Nicolas Hamaguchi, Kenji Richmond, Michael TI DETECTION OF A COOL, ACCRETION-SHOCK-GENERATED X-RAY PLASMA IN EX LUPI DURING THE 2008 OPTICAL ERUPTION SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars: formation; stars: individual (EX Lupi); stars: pre-main sequence; X-rays: stars ID T-TAURI STARS; ILLUMINATING MCNEIL-NEBULA; FU-ORIONIS STARS; YOUNG STAR; V1647 ORI; SPECTRAL VARIABILITY; EXTREME OUTBURST; SPACED DATA; XMM-NEWTON; EMISSION AB EX Lupi is the prototype for a class of young, pre-main-sequence stars which are observed to undergo irregular, presumably accretion-generated, optical outbursts that result in a several magnitude rise of the optical flux. EX Lupi was observed to optically erupt in 2008 January, triggering Chandra ACIS Target of Opportunity observations shortly thereafter. We find very strong evidence that most of the X-ray emission in the first few months after the optical outburst is generated by accretion of circumstellar material onto the stellar photosphere. Specifically, we find a strong correlation between the decreasing optical and X-ray fluxes following the peak of the outburst in the optical, which suggests that these observed declines in both the optical and X-ray fluxes are the result of declining accretion rate. In addition, in our models of the X-ray spectrum, we find strong evidence for a similar to 0.4 keV plasma component, as expected for accretion shocks on low-mass, pre-main-sequence stars. From 2008 March through October, this cool plasma component appeared to fade as EX Lupi returned to its quiescent level in the optical, consistent with a decrease in the overall emission measure of accretion-shock-generated plasma. The overall small increase of the X-ray flux during the optical outburst of EX Lupi is similar to what was observed in previous X-ray observations of the 2005 optical outburst of the EX Lupi-type star V1118 Ori but contrasts with the large increase of the X-ray flux from the erupting young star V1647 Ori during its 2003 and 2008 optical outbursts. C1 [Teets, William K.; Weintraub, David A.] Vanderbilt Univ, Dept Phys & Astron, Nashville, TN 37235 USA. [Grosso, Nicolas] Univ Strasbourg, Observ Astron Strasbourg, CNRS, UMR 7550, F-67000 Strasbourg, France. [Hamaguchi, Kenji] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Kastner, Joel H.; Richmond, Michael] Rochester Inst Technol, Rochester, NY 14623 USA. RP Teets, WK (reprint author), Vanderbilt Univ, Dept Phys & Astron, Nashville, TN 37235 USA. NR 38 TC 3 Z9 3 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD NOV 20 PY 2012 VL 760 IS 1 AR 89 DI 10.1088/0004-637X/760/1/89 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 035DD UT WOS:000310922200089 ER PT J AU Wang, FY Bromm, V Greif, TH Stacy, A Dai, ZG Loeb, A Cheng, KS AF Wang, F. Y. Bromm, Volker Greif, Thomas H. Stacy, Athena Dai, Z. G. Loeb, Abraham Cheng, K. S. TI PROBING PRE-GALACTIC METAL ENRICHMENT WITH HIGH-REDSHIFT GAMMA-RAY BURSTS SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology: observations; cosmology: theory; galaxies: high-redshift; gamma-ray burst: general; quasars: absorption lines ID INITIAL MASS FUNCTION; POPULATION-III STARS; ATOMIC-ABSORPTION LINES; 1ST STARS; INTERGALACTIC MEDIUM; PRIMORDIAL GAS; EARLY UNIVERSE; LIGHT CURVES; HII-REGIONS; PROTOSTELLAR FEEDBACK AB We explore high-redshift gamma-ray bursts (GRBs) as promising tools to probe pre-galactic metal enrichment. We utilize the bright afterglow of a Population III (Pop III) GRB exploding in a primordial dwarf galaxy as a luminous background source, and calculate the strength of metal absorption lines that are imprinted by the first heavy elements in the intergalactic medium (IGM). To derive the GRB absorption line diagnostics, we use an existing highly resolved simulation of the formation of a first galaxy which is characterized by the onset of atomic hydrogen cooling in a halo with virial temperature greater than or similar to 10(4) K. We explore the unusual circumburst environment inside the systems that hosted Pop III stars, modeling the density evolution with the self-similar solution for a champagne flow. For minihalos close to the cooling threshold, the circumburst density is roughly proportional to (1 + z) with values of about a few cm(-3). In more massive halos, corresponding to the first galaxies, the density may be larger, n greater than or similar to 100 cm(-3). The resulting afterglow fluxes are weakly dependent on redshift at a fixed observed time, and may be detectable with the James Webb Space Telescope and Very Large Array in the near-IR and radio wavebands, respectively, out to redshift z greater than or similar to 20. We predict that the maximum of the afterglow emission shifts from near-IR to millimeter bands with peak fluxes from mJy to Jy at different observed times. The metal absorption line signature is expected to be detectable in the near future. GRBs are ideal tools for probing the metal enrichment in the early IGM, due to their high luminosities and featureless power-law spectra. The metals in the first galaxies produced by the first supernova (SN) explosions are likely to reside in low-ionization stages (C II, OI, Si II and Fe II). We show that, if the afterglow can be observed sufficiently early, analysis of the metal lines may distinguish whether the first heavy elements were produced in a pair-instability supernova or a core-collapse (Type II) SN, thus constraining the initial mass function of the first stars. C1 [Wang, F. Y.; Dai, Z. G.] Nanjing Univ, Sch Astron & Space Sci, Nanjing 210093, Peoples R China. [Wang, F. Y.; Bromm, Volker] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Bromm, Volker] Univ Texas Austin, Texas Cosmol Ctr, Austin, TX 78712 USA. [Greif, Thomas H.] Max Planck Inst Astrophys, D-85740 Garching, Germany. [Stacy, Athena] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Loeb, Abraham] Harvard Univ, Dept Astron, Cambridge, MA 02138 USA. [Cheng, K. S.] Univ Hong Kong, Dept Phys, Hong Kong, Hong Kong, Peoples R China. RP Wang, FY (reprint author), Nanjing Univ, Sch Astron & Space Sci, Nanjing 210093, Peoples R China. RI Wang, Fayin/B-1479-2009; Cheng, Kwong Sang/D-3073-2009 OI Wang, Fayin/0000-0003-4157-7714; FU National Natural Science Foundation of China [11103007, 11033002]; NSF [AST-1009928]; NASA [NNX09AJ33G]; Government of the Hong Kong SAR [HKU 7011/09p] FX We are indebted to Anna Frebel and Steve Finkelstein for helpful discussions. This work is supported by the National Natural Science Foundation of China (grants 11103007 and 11033002). V.B. acknowledges support from NSF grant AST-1009928 and NASA ATFP grant NNX09AJ33G. K.S.C. is supported by the GRF grants of the Government of the Hong Kong SAR under HKU 7011/09p. The simulations presented here were carried out at the Texas Advanced Computing Center (TACC). NR 131 TC 35 Z9 35 U1 0 U2 10 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD NOV 20 PY 2012 VL 760 IS 1 AR 27 DI 10.1088/0004-637X/760/1/27 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 035DD UT WOS:000310922200027 ER PT J AU Xu, CK Shupe, DL Bethermin, M Aussel, H Berta, S Bock, J Bridge, C Conley, A Cooray, A Elbaz, D Franceschini, A Le Floc'h, E Lu, N Lutz, D Magnelli, B Marsden, G Oliver, SJ Pozzi, F Riguccini, L Schulz, B Scoville, N Vaccari, M Vieira, JD Wang, L Zemcov, M AF Xu, C. K. Shupe, D. L. Bethermin, M. Aussel, H. Berta, S. Bock, J. Bridge, C. Conley, A. Cooray, A. Elbaz, D. Franceschini, A. Le Floc'h, E. Lu, N. Lutz, D. Magnelli, B. Marsden, G. Oliver, S. J. Pozzi, F. Riguccini, L. Schulz, B. Scoville, N. Vaccari, M. Vieira, J. D. Wang, L. Zemcov, M. TI COSMIC EVOLUTION OF STAR FORMATION ENHANCEMENT IN CLOSE MAJOR-MERGER GALAXY PAIRS SINCE z=1 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: evolution; galaxies: general; galaxies: interactions; galaxies: starburst ID DIGITAL SKY SURVEY; LUMINOUS INFRARED GALAXIES; HERSCHEL-SPIRE INSTRUMENT; HIGH-REDSHIFT GALAXIES; SUBMILLIMETER GALAXIES; FIELD GALAXIES; STELLAR MASS; EXTRAGALACTIC SURVEY; FORMING GALAXIES; S-COSMOS AB The infrared (IR) emission of "M-* galaxies" (10(10.4) <= M-star <= 10(11.0) M-circle dot) in galaxy pairs, derived using data obtained in Herschel (PEP/HerMES) and Spitzer (S-COSMOS) surveys, is compared to that of single-disk galaxies in well-matched control samples to study the cosmic evolution of the star formation enhancement induced by galaxy-galaxy interaction. Both the mean IR spectral energy distribution and mean IR luminosity of star-forming galaxies (SFGs) in SFG+SFG (S+S) pairs in the redshift bin of 0.6 < z < 1 are consistent with no star formation enhancement. SFGs in S+S pairs in a lower redshift bin of 0.2 < z < 0.6 show marginal evidence for a weak star formation enhancement. Together with the significant and strong sSFR enhancement shown by SFGs in a local sample of S+S pairs (obtained using previously published Spitzer observations), our results reveal a trend for the star formation enhancement in S+S pairs to decrease with increasing redshift. Between z = 0 and z = 1, this decline of interaction-induced star formation enhancement occurs in parallel with the dramatic increase (by a factor of similar to 10) of the sSFR of single SFGs, both of which can be explained by the higher gas fraction in higher-z disks. SFGs in mixed pairs (S+E pairs) do not show any significant star formation enhancement at any redshift. The difference between SFGs in S+S pairs and in S+E pairs suggests a modulation of the sSFR by the intergalactic medium (IGM) in the dark matter halos hosting these pairs. C1 [Xu, C. K.; Shupe, D. L.; Lu, N.; Schulz, B.; Zemcov, M.] CALTECH, Infrared Proc & Anal Ctr, JPL, Pasadena, CA 91125 USA. [Bethermin, M.; Aussel, H.; Elbaz, D.; Le Floc'h, E.; Riguccini, L.] Univ Paris Diderot, Lab AIM Paris Saclay, CEA DSM Irfu, CNRS,CE Saclay, F-91191 Gif Sur Yvette, France. [Bethermin, M.] Univ Paris 11, IAS, F-91405 Orsay, France. [Bethermin, M.] CNRS, UMR 8617, F-91405 Orsay, France. [Berta, S.; Lutz, D.; Magnelli, B.] Max Planck Inst Extraterr Phys MPE, D-85741 Garching, Germany. [Conley, A.] Univ Colorado, Ctr Astrophys & Space Astron UCB 389, Boulder, CO 80309 USA. [Cooray, A.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. [Franceschini, A.; Vaccari, M.] Univ Padua, Dipartimento Astron, I-35122 Padua, Italy. [Marsden, G.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. [Oliver, S. J.; Wang, L.] Univ Sussex, Ctr Astron, Dept Phys & Astron, Brighton BN1 9QH, E Sussex, England. [Pozzi, F.] INAF Osservatorio Astron Roma, I-00040 Monte Porzio Catone, Italy. [Vaccari, M.] Univ Western Cape, Astrophys Grp, Dept Phys, ZA-7535 Bellville, Cape Town, South Africa. RP Xu, CK (reprint author), CALTECH, Infrared Proc & Anal Ctr, JPL, 1200 E Calif Blvd, Pasadena, CA 91125 USA. RI Oliver, Seb/A-2479-2013; Vaccari, Mattia/R-3431-2016; OI Oliver, Seb/0000-0001-7862-1032; Vaccari, Mattia/0000-0002-6748-0577; Bethermin, Matthieu/0000-0002-3915-2015 FU Science and Technology Facilities Council [ST/I000976/1]; BMVIT (Austria); ESA-PRODEX (Belgium); CEA/CNES (France); DLR (Germany); ASI/INAF (Italy); CICYT/MCYT (Spain); CSA (Canada); NAOC (China); CEA (France); CNES (France); CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC (UK); UKSA (UK); NASA (USA) FX Dr. Xianzhong Zheng is thanked for kindly providing the software and instructions for the "clean stacking." We acknowledge support from the Science and Technology Facilities Council (grant No. ST/I000976/1). PACS has been developed by a consortium of institutes led by MPE (Germany) and including UVIE (Austria); KU Leuven, CSL, IMEC (Belgium); CEA, LAM (France); MPIA (Germany); INAF-IFSI/OAA/OAP/OAT, LENS, SISSA (Italy); IAC (Spain). This development has been supported by the funding agencies BMVIT (Austria), ESA-PRODEX (Belgium), CEA/CNES (France), DLR (Germany), ASI/INAF (Italy), and CICYT/MCYT (Spain). SPIRE has been developed by a consortium of institutes led by Cardiff University (UK) and including: the University of Lethbridge (Canada); NAOC (China); CEA, LAM (France); IFSI, the University of Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, the University of Sussex (UK); and Caltech, JPL, NHSC, the University of Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC, UKSA (UK); and NASA (USA). The data presented in this paper will be released through the Herschel Database in Marseille (HeDaM, http://hedam.oamp.fr/HerMES). NR 79 TC 16 Z9 17 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD NOV 20 PY 2012 VL 760 IS 1 AR 72 DI 10.1088/0004-637X/760/1/72 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 035DD UT WOS:000310922200072 ER PT J AU Mainzer, A Grav, T Masiero, J Bauer, J Cutri, RM McMillan, RS Nugent, CR Tholen, D Walker, R Wright, EL AF Mainzer, A. Grav, T. Masiero, J. Bauer, J. Cutri, R. M. McMillan, R. S. Nugent, C. R. Tholen, D. Walker, R. Wright, E. L. TI PHYSICAL PARAMETERS OF ASTEROIDS ESTIMATED FROM THE WISE 3-BAND DATA AND NEOWISE POST-CRYOGENIC SURVEY SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE atlases; catalogs; minor planets, asteroids: general; surveys ID THERMAL-MODEL CALIBRATION; EARTH; DIAMETERS; ALBEDOS; OBJECTS AB Enhancements to the science data processing pipeline of NASA's Wide-field Infrared Survey Explorer (WISE) mission, collectively known as NEOWISE, resulted in the detection of >158,000 minor planets in four infrared wavelengths during the fully cryogenic portion of the mission. Following the depletion of its cryogen, NASA's Planetary Science Directorate funded a four-month extension to complete the survey of the inner edge of the Main Asteroid Belt and to detect and discover near-Earth objects (NEOs). This extended survey phase, known as the NEOWISE Post-Cryogenic Survey, resulted in the detection of similar to 6500 large Main Belt asteroids and 86 NEOs in its 3.4 and 4.6 mu m channels. During the Post-Cryogenic Survey, NEOWISE discovered and detected a number of asteroids co-orbital with the Earth and Mars, including the first known Earth Trojan. We present preliminary thermal fits for these and other NEOs detected during the 3-Band Cryogenic and Post-Cryogenic Surveys. C1 [Mainzer, A.; Masiero, J.; Bauer, J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Grav, T.] Planetary Sci Inst, Tucson, AZ 85719 USA. [Bauer, J.; Cutri, R. M.] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA. [McMillan, R. S.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Nugent, C. R.] Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90095 USA. [Tholen, D.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Walker, R.] Monterey Inst Res Astron, Monterey, CA 93933 USA. [Wright, E. L.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. RP Mainzer, A (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM amainzer@jpl.nasa.gov OI Masiero, Joseph/0000-0003-2638-720X FU National Aeronautics and Space Administration; NSF [AST 1109940] FX This publication makes use of data products from the Widefield Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, and NEOWISE, which is a project of the Jet Propulsion Laboratory/California Institute of Technology. WISE and NEOWISE are funded by the National Aeronautics and Space Administration. We gratefully acknowledge the extraordinary services specific to NEOWISE contributed by the International Astronomical Union's Minor Planet Center, operated by the Harvard-Smithsonian Center for Astrophysics. We thank the worldwide community of dedicated amateur and professional astronomers devoted to minor planet follow-up observations. We thank our referee for thoughtful comments. This research has made use of the NASA/IPAC Infrared Science Archive, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. D.J.T. acknowledges support from NSF Grant AST 1109940. NR 13 TC 17 Z9 17 U1 0 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD NOV 20 PY 2012 VL 760 IS 1 AR L12 DI 10.1088/2041-8205/760/1/L12 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 033ZE UT WOS:000310839100012 ER PT J AU Ofman, L Thompson, BJ AF Ofman, L. Thompson, B. J. TI SDO/AIA OBSERVATION OF KELVIN-HELMHOLTZ INSTABILITY IN THE SOLAR CORONA (vol 734, pg L11, 2011) SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Correction C1 [Ofman, L.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA. [Ofman, L.; Thompson, B. J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Ofman, L (reprint author), Tel Aviv Univ, Dept Geophys & Planetary Sci, IL-69978 Tel Aviv, Israel. RI Thompson, Barbara/C-9429-2012 NR 3 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 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD NOV 20 PY 2012 VL 760 IS 1 AR L19 DI 10.1088/2041-8205/760/1/L19 PG 1 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 033ZE UT WOS:000310839100019 ER PT J AU Perez, LM Carpenter, JM Chandler, CJ Isella, A Andrews, SM Ricci, L Calvet, N Corder, SA Deller, AT Dullemond, CP Greaves, JS Harris, RJ Henning, T Kwon, W Lazio, J Linz, H Mundy, LG Sargent, AI Storm, S Testi, L Wilner, DJ AF Perez, Laura M. Carpenter, John M. Chandler, Claire J. Isella, Andrea Andrews, Sean M. Ricci, Luca Calvet, Nuria Corder, Stuartt A. Deller, Adam T. Dullemond, Cornelis P. Greaves, Jane S. Harris, Robert J. Henning, Thomas Kwon, Woojin Lazio, Joseph Linz, Hendrik Mundy, Lee G. Sargent, Anneila I. Storm, Shaye Testi, Leonardo Wilner, David J. TI CONSTRAINTS ON THE RADIAL VARIATION OF GRAIN GROWTH IN THE AS 209 CIRCUMSTELLAR DISK SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE protoplanetary disks; stars: individual (AS 209) ID T-TAURI STARS; PROTOPLANETARY DISKS; ACCRETION DISKS; OPTICAL-CONSTANTS; CQ TAURI; EVOLUTION; OPACITIES; SIZE AB We present dust continuum observations of the protoplanetary disk surrounding the pre-main-sequence star AS 209, spanning more than an order of magnitude in wavelength from 0.88 to 9.8 mm. The disk was observed with subarcsecond angular resolution (0 ''.2-0 ''.5) to investigate radial variations in its dust properties. At longer wavelengths, the disk emission structure is notably more compact, providing model-independent evidence for changes in the grain properties across the disk. We find that physical models which reproduce the disk emission require a radial dependence of the dust opacity kappa(nu) Assuming that the observed wavelength-dependent structure can be attributed to radial variations in the dust opacity spectral index (beta), we find that beta(R) increases from beta < 0.5 at similar to 20 AU to beta > 1.5 for R greater than or similar to 80 AU, inconsistent with a constant value of beta across the disk (at the 10 sigma level). Furthermore, if radial variations of kappa(nu) are caused by particle growth, we find that the maximum size of the particle-size distribution (a(max)) increases from submillimeter-sized grains in the outer disk (R greater than or similar to 70 AU) to millimeter- and centimeter-sized grains in the inner disk regions (R less than or similar to 70 AU). We compare our observational constraint on a(max)(R) with predictions from physical models of dust evolution in protoplanetary disks. For the dust composition and particle-size distribution investigated here, our observational constraints on a(max)(R) are consistent with models where the maximum grain size is limited by radial drift. C1 [Perez, Laura M.; Carpenter, John M.; Isella, Andrea; Ricci, Luca; Sargent, Anneila I.] CALTECH, Dept Astron, Pasadena, CA 91125 USA. [Chandler, Claire J.] Natl Radio Astron Observ, Socorro, NM 87801 USA. [Andrews, Sean M.; Harris, Robert J.; Wilner, David J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Calvet, Nuria] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Corder, Stuartt A.] Joint ALMA Observ, Santiago, Chile. [Deller, Adam T.] Netherlands Inst Radio Astron ASTRON, NL-7990 AA Dwingeloo, Netherlands. [Dullemond, Cornelis P.; Linz, Hendrik] Univ Heidelberg, Ctr Astron, D-69120 Heidelberg, Germany. [Greaves, Jane S.] Univ St Andrews, Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland. [Henning, Thomas] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Kwon, Woojin] Univ Illinois, Dept Astron, Urbana, IL 61801 USA. [Lazio, Joseph] CALTECH, Jet Prop Lab, Pasadena, CA 91106 USA. [Mundy, Lee G.; Storm, Shaye] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Testi, Leonardo] European So Observ, D-85748 Garching, Germany. [Testi, Leonardo] INAF Osservatorio Astrofis Arcetri, I-50125 Florence, Italy. RP Perez, LM (reprint author), CALTECH, Dept Astron, 1200 E Calif Blvd, Pasadena, CA 91125 USA. OI Dullemond, Cornelis/0000-0002-7078-5910; Deller, Adam/0000-0001-9434-3837 FU NSF [AST-1109334]; Smithsonian Institution; Academia Sinica FX We acknowledge T. Birnstiel for useful discussions. A.I., J.M.C., L.M.P acknowledge support from NSF award AST-1109334. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. Ongoing CARMA development and operations are supported by the National Science Foundation under a cooperative agreement, and by the CARMA partner universities. The SMA is a joint project between the Smithsonian Astrophysical Observatory and the Academia Sinica Institute of Astronomy and Astrophysics, funded by the Smithsonian Institution and Academia Sinica. Part of this research was carried out at the Jet Propulsion Laboratory, Caltech, under a contract with the National Aeronautics and Space Administration. NR 35 TC 74 Z9 74 U1 0 U2 8 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD NOV 20 PY 2012 VL 760 IS 1 AR L17 DI 10.1088/2041-8205/760/1/L17 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 033ZE UT WOS:000310839100017 ER PT J AU Miyashita, Y Machida, S Nose, M Liou, K Saito, Y Paterson, WR AF Miyashita, Y. Machida, S. Nose, M. Liou, K. Saito, Y. Paterson, W. R. TI A statistical study of energy release and transport midway between the magnetic reconnection and initial dipolarization regions in the near-Earth magnetotail associated with substorm expansion onsets SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID CENTRAL PLASMA SHEET; GEOTAIL OBSERVATIONS; MIDDISTANT MAGNETOTAIL; AURORAL BREAKUPS; FLUX TRANSPORT; BULK FLOWS; EVOLUTION; ION; MAGNETOSPHERE; SPACECRAFT AB Our previous study showed that the energy release associated with substorm expansion onsets is the most significant midway between the magnetic reconnection and initial dipolarization regions (- 12 > X > - 18 R-E in the premidnight sector) in the magnetotail. In the present paper, we have statistically studied the substorm-associated energy balance and transport in the magnetotail, focusing on the midway region as well as the near-Earth initial dipolarization region (X > similar to- 12 R-E). We find that a large amount of energy is released in the midway region, associated with onsets, but only a part of this energy is transported to the near-Earth initial dipolarization region mainly in the form of the thermal flux and the wave Poynting flux. It is possible that the energy carried by fast earthward flows and waves from the reconnection region is not sufficient for the thermal energy increase and the outward transported energy in the initial dipolarization region, although the magnetic flux may be sufficiently carried. A considerably large amount of the magnetic energy comes from the lobes in the form of the Poynting flux also in the initial dipolarization region. C1 [Miyashita, Y.] Nagoya Univ, Solar Terr Environm Lab, Chikusa Ku, Nagoya, Aichi 4648601, Japan. [Machida, S.] Kyoto Univ, Dept Geophys, Kyoto, Japan. [Nose, M.] Kyoto Univ, Grad Sch Sci, Data Anal Ctr Geomagnetism & Space Magnetism, Kyoto, Japan. [Liou, K.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA. [Saito, Y.] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2298510, Japan. [Paterson, W. R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Miyashita, Y (reprint author), Nagoya Univ, Solar Terr Environm Lab, Chikusa Ku, Furo Cho, Nagoya, Aichi 4648601, Japan. EM miyasita@stelab.nagoya-u.ac.jp RI Nose, Masahito/B-1900-2015; Liou, Kan/C-2089-2016 OI Nose, Masahito/0000-0002-2789-3588; Liou, Kan/0000-0001-5277-7688 FU Japan Society for the Promotion of Science [22340145]; [22740321] FX The Geotail MGF magnetic field data were provided by T. Nagai and S. Kokubun. The Geotail EPIC-STICS high-energy particle data were provided by A. T. Y. Lui, R. W. McEntire, and S. P. Christon. We also thank D. Nagata for processing the EPIC-STICS data. This work was supported by a Grant-in-Aid for Young Scientists (22740321) and a Grant-in-Aid for Scientific Research (22340145) of Japan Society for the Promotion of Science. NR 42 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 NOV 17 PY 2012 VL 117 AR A11214 DI 10.1029/2012JA017925 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 039NK UT WOS:000311253100002 ER PT J AU Leahy, LV Wood, R Charlson, RJ Hostetler, CA Rogers, RR Vaughan, MA Winker, DM AF Leahy, L. V. Wood, R. Charlson, R. J. Hostetler, C. A. Rogers, R. R. Vaughan, M. A. Winker, D. M. TI On the nature and extent of optically thin marine low clouds SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID SPECTRAL-RESOLUTION LIDAR; LIQUID WATER PATH; TRADE-WIND CUMULI; STRATIFORM CLOUDS; CALIPSO LIDAR; SATELLITE-OBSERVATIONS; INSTRUMENT SIMULATORS; RADIATION BUDGET; BOUNDARY-LAYER; SEA-SALT AB Macrophysical properties of optically thin marine low clouds over the nonpolar oceans (60 degrees S-60 degrees N) are measured using 2 years of full-resolution nighttime data from the Cloud-Aerosol Lidar with Orthogonal Polarization (CALIOP). Optically thin clouds, defined as the subset of marine low clouds that do not fully attenuate the lidar signal, comprise almost half of the low clouds over the marine domain. Regionally, the fraction of low clouds that are optically thin (f(thin,cld)) exhibits a strong inverse relationship with the low-cloud cover, with maxima in the tropical trades (f(thin,cld) > 0.8) and minima in regions of persistent marine stratocumulus and in midlatitudes (f(thin,cld) < 0.3). Domain-wide, a power law fit describes the cloud length distribution, with exponent beta = 2.03 +/- 0.06 (+/- 95% confidence interval). On average, the fraction of a cloud that is optically thin decreases from similar to 1 for clouds smaller than 2 km to <0.3 for clouds larger than 30 km. This relationship is found to be independent of region, so that geographical variations in the cloud length distribution explain three quarters of the variance in f(thin,cld). Comparing collocated trade cumulus observations from CALIOP and the airborne High Spectral Resolution Lidar reveals that clouds with lengths smaller than are resolvable with CALIOP contribute approximately half of the low clouds in the region sampled. A bounded cascade model is constructed to match the observations from the trades. The model shows that the observed optically thin cloud behavior is consistent with a power law scaling of cloud optical depth and suggests that most optically thin clouds only partially fill the CALIOP footprint. C1 [Leahy, L. V.; Wood, R.; Charlson, R. J.] Univ Washington, Dept Atmospher Sci, Seattle, WA 98195 USA. [Hostetler, C. A.; Rogers, R. R.; Vaughan, M. A.; Winker, D. M.] NASA, Langley Res Ctr, Hampton, VA 23665 USA. RP Leahy, LV (reprint author), Univ Washington, Dept Atmospher Sci, Box 351640, Seattle, WA 98195 USA. EM lleahy@atmos.washington.edu RI Wood, Robert/A-2989-2008 OI Wood, Robert/0000-0002-1401-3828 FU NASA [NNX10AE59G, NNX10AN78G] FX This work was supported by NASA award numbers NNX10AE59G and NNX10AN78G. We wish to thank Sarah Doherty for insightful comments which contributed greatly to the quality of this work and Roger Marchand for pointing out an important flaw in our original application of the bounded cascade model. NR 67 TC 8 Z9 8 U1 1 U2 20 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD NOV 16 PY 2012 VL 117 AR D22201 DI 10.1029/2012JD017929 PG 20 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 039LS UT WOS:000311247900003 ER PT J AU Larour, E Morlighem, M Seroussi, H Schiermeier, J Rignot, E AF Larour, E. Morlighem, M. Seroussi, H. Schiermeier, J. Rignot, E. TI Ice flow sensitivity to geothermal heat flux of Pine Island Glacier, Antarctica SO JOURNAL OF GEOPHYSICAL RESEARCH-EARTH SURFACE LA English DT Article ID WEST ANTARCTICA; SATELLITE RADAR; SHEET MODEL; PART 1; SHELF; BASAL; VELOCITY; RHEOLOGY; SURFACE AB Model projections of ice flow in a changing climate are dependent on model inputs such as surface elevation, bedrock position or surface temperatures, among others. Of all these inputs, geothermal heat flux is the one for which uncertainty is greatest. In the area of Pine Island Glacier, Antarctica, available data sets differ by up to a factor of 2.5. Here, we evaluate the impact of such uncertainty on ice flow, using sampling analyses based on the Latin-Hypercube method. First, we quantify the impact of geothermal heat flux errors on ice hardness, a thermal parameter that critically controls the magnitude of ice flow. Second, we quantify the impact of the same errors on mass balance, specifically on the mass flux advecting through thirteen fluxgates distributed across Pine Island Glacier. We contrast our results with similar uncertainties generated by errors in the specification of ice thickness. Model outputs indicate that geothermal heat flux errors yield uncertainties on ice hardness on the order of 5-7%, with maximum uncertainty reaching 15%. Resulting uncertainties in mass balance remain however below 1%. We discuss the uncertainty distribution and its relationship to the amount of heat available at the base of the ice sheet from friction, viscous and geothermal heating. We also show that comparatively, errors in ice thickness contribute more to model uncertainty than errors in geothermal heat flux, especially for fast-flowing ice streams. C1 [Larour, E.; Seroussi, H.; Schiermeier, J.; Rignot, E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Morlighem, M.; Rignot, E.] Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA USA. RP Larour, E (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM eric.larour@jpl.nasa.gov RI Rignot, Eric/A-4560-2014; Morlighem, Mathieu/O-9942-2014 OI Rignot, Eric/0000-0002-3366-0481; Morlighem, Mathieu/0000-0001-5219-1310 FU National Aeronautics and Space Administration; Cryospheric Sciences Program; MAP Program; NSF [ANT-0424589]; NASA [NNX10AT68G]; NASA Postdoctoral Program at the Jet Propulsion Laboratory, California Institute of Technology FX This work was performed at the Jet Propulsion Laboratory, California Institute of Technology, and the Department of Earth System Science, University of California Irvine, under a contract with the National Aeronautics and Space Administration, Cryospheric Sciences Program and MAP Program. The authors would like to acknowledge Operation IceBridge data used in the study, as well as CReSIS data generated from NSF grant ANT-0424589 and NASA grant NNX10AT68G. Helene Seroussi was supported by an appointment to the NASA Postdoctoral Program at the Jet Propulsion Laboratory, California Institute of Technology, administered by Oak Ridge Associated Universities through a contract with NASA. We would also like to acknowledge R. Gladstone, the Associate Editor Poul Christoffersen and the other anonymous reviewers for their review and insights into the manuscript. NR 56 TC 18 Z9 18 U1 1 U2 23 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 NOV 16 PY 2012 VL 117 AR F04023 DI 10.1029/2012JF002371 PG 12 WC Geosciences, Multidisciplinary SC Geology GA 039OE UT WOS:000311255400001 ER PT J AU Kitamura, N Nishimura, Y Chandler, MO Moore, TE Terada, N Ono, T Shinbori, A Kumamoto, A AF Kitamura, N. Nishimura, Y. Chandler, M. O. Moore, T. E. Terada, N. Ono, T. Shinbori, A. Kumamoto, A. TI Storm-time electron density enhancement in the cleft ion fountain SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID INTERPLANETARY MAGNETIC-FIELD; POLAR WIND; PLASMA SHEET; EARTHS MAGNETOSPHERE; GEOMAGNETIC STORM; SOLAR-WIND; IONOSPHERIC OUTFLOWS; COORDINATE SYSTEM; AURORAL-ZONE; OXYGEN IONS AB To determine the characteristics and origin of observed storm-time electron density enhancements in the polar cap, and to investigate the spatial extent (noon-midnight direction) of associated O+ ion outflows, we analyzed nearly simultaneous observations of such electron density enhancements from the Akebono satellite and ion upflows from the Polar satellite during a geomagnetic storm occurring on 6 April 2000. The Akebono satellite observed substantial electron density enhancements by a factor of similar to 10-90 with a long duration of similar to 15 h at similar to 2 R-E in the southern polar region. The Polar satellite outflow measurements in the northern polar cap at similar to 7-4 R-E exhibited velocity filtering of the similar to 100 eV to similar to 0 eV (from the spacecraft potential) ion outflow from the cleft ion fountain, with resultant temperatures declining from similar to 3 eV to 0.03 eV with increasing distance from the cusp. Similar velocity filtering was detected in the southern polar cap at similar to 1.8-3.5 RE. The region of O+ ion outflows with fluxes exceeding 5 x 10(8) /cm(2)/s (mapped to 1000 km altitude) extended similar to 10 degrees MLAT (similar to 1000 km) at the ionosphere from the cusp/cleft into the dayside polar cap at similar to 2.5 RE. These coordinated Akebono-Polar observations are consistent with the development of storm-time electron density enhancements in the polar cap as a result of the bulk outflow of low-energy plasma as part of the cleft ion fountain. The large spatial scale, large ion fluxes, and the long duration indicate significant supply of very-low-energy O+ ions to the magnetosphere through this region. C1 [Kitamura, N.] Nagoya Univ, Solar Terr Environm Lab, Nagoya, Aichi 4648601, Japan. [Nishimura, Y.] Univ Calif Los Angeles, Dept Atmospher & Ocean Sci, Los Angeles, CA USA. [Chandler, M. O.] NASA, Nat Environm EV44, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. [Moore, T. E.] NASA, Heliophys Sci Div, Goddard Space Flight Ctr, Greenbelt, MD USA. [Terada, N.; Ono, T.; Kumamoto, A.] Tohoku Univ, Dept Geophys, Sendai, Miyagi 980, Japan. [Shinbori, A.] Kyoto Univ, Res Inst Sustainable Humanosphere, Uji, Kyoto, Japan. RP Kitamura, N (reprint author), Nagoya Univ, Solar Terr Environm Lab, Nagoya, Aichi 4648601, Japan. EM kitamura@stelab.nagoya-u.ac.jp RI Moore, Thomas/D-4675-2012 OI Moore, Thomas/0000-0002-3150-1137 FU Global COE program "Global Education and Research Center for Earth and Planetary Dynamics" at Tohoku University; Research Fellowship of the Japan Society for the Promotion of Science (JSPS); JSPS KAKENHI [22.1671]; Inter-university Upper atmosphere Global Observation NETwork (IUGONET); Ministry of Education, Culture, Sports, Science and Technology (MEXT), Japan FX The Akebono satellite project has been managed by Institute of Space and Astronautical Science (ISAS), Japan Aerospace Exploration Agency (JAXA). The SYM-H index was provided by WDC for Geomagnetism, Kyoto. The OMNI data set were obtained from the GSFC/SPDF OMNIWeb interface at http://omniweb.gsfc.nasa.gov. This work was supported by the Global COE program "Global Education and Research Center for Earth and Planetary Dynamics" at Tohoku University, a Research Fellowship of the Japan Society for the Promotion of Science (JSPS), and JSPS KAKENHI grant 22.1671. The Hydra data set were obtained from the Coordinated Data Analysis Web at http://cdaweb.gsfc.nasa.gov. The authors would like to thank J. Scudder and Hydra team for use of the data. A. Shinbori is supported by the Inter-university Upper atmosphere Global Observation NETwork (IUGONET) project funded by the Ministry of Education, Culture, Sports, Science and Technology (MEXT), Japan. NR 112 TC 4 Z9 4 U1 1 U2 8 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD NOV 16 PY 2012 VL 117 AR A11212 DI 10.1029/2012JA017900 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 039NF UT WOS:000311252500003 ER PT J AU Biaggi-Labiosa, A Sola, F Lebron-Colon, M Evans, LJ Xu, JC Hunter, GW Berger, GM Gonzalez, JM AF Biaggi-Labiosa, A. Sola, F. Lebron-Colon, M. Evans, L. J. Xu, J. C. Hunter, G. W. Berger, G. M. Gonzalez, J. M. TI A novel methane sensor based on porous SnO2 nanorods: room temperature to high temperature detection SO NANOTECHNOLOGY LA English DT Article ID GAS SENSORS; OXIDE NANOSTRUCTURES; CARBON NANOTUBES; METAL-OXIDES; TIN OXIDE; NANOWIRES; RESISTANCE; DEVICES AB We report for the first time a novel room temperature methane (CH4) sensor fabricated using porous tin oxide (SnO2) nanorods as the sensing material. The porous SnO2 nanorods were synthesized by using multiwall carbon nanotubes (MWCNTs) as templates. Current versus time curves were obtained demonstrating the room temperature sensing capabilities of the sensor system when exposed to 0.25% CH4 in air. The sensor also exhibited a wide temperature range for different concentrations of CH4 (25-500 degrees C), making it useful in harsh environments as well. C1 [Biaggi-Labiosa, A.; Berger, G. M.] NASA, Glenn Res Ctr, Natl Ctr Space Explorat Res, Cleveland, OH 44135 USA. [Gonzalez, J. M.] NASA, Glenn Res Ctr, Gilcrest, Cleveland, OH 44135 USA. RP Biaggi-Labiosa, A (reprint author), NASA, Glenn Res Ctr, Natl Ctr Space Explorat Res, 21000 Brookpark Rd, Cleveland, OH 44135 USA. EM azlin.m.biaggi-labiosa@nasa.gov FU Vehicle Systems Safety Technologies Project FX The authors would like to acknowledge the contributions of Drs L Matus, M Zeller, and C W Chang for discussions and critical review of the manuscript. We also acknowledge the technical assistance of C Hampton, P Lampard, and M Artale. This research is supported by the Vehicle Systems Safety Technologies Project. NR 35 TC 20 Z9 20 U1 2 U2 69 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0957-4484 J9 NANOTECHNOLOGY JI Nanotechnology PD NOV 16 PY 2012 VL 23 IS 45 AR 455501 DI 10.1088/0957-4484/23/45/455501 PG 8 WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary; Physics, Applied SC Science & Technology - Other Topics; Materials Science; Physics GA 030OE UT WOS:000310579200015 PM 23064120 ER PT J AU Roberts, JC Harrigan, TP Ward, EE Taylor, TM Annett, MS Merkle, AC AF Roberts, J. C. Harrigan, T. P. Ward, E. E. Taylor, T. M. Annett, M. S. Merkle, A. C. TI Human head-neck computational model for assessing blast injury SO JOURNAL OF BIOMECHANICS LA English DT Article DE Brain injury; Finite element models (FEM); Surrogate models; Blast; Human models ID IMPACT AB A human head finite element model (HHFEM) was developed to study the effects of a blast to the head. To study both the kinetic and kinematic effects of a blast wave, the HHFEM was attached to a finite element model of a Hybrid III ATD neck. A physical human head surrogate model (HSHM) was developed from solid model files of the HHFEM, which was then attached to a physical Hybrid III ATD neck and exposed to shock tube overpressures. This allowed direct comparison between the HSHM and HHFEM. To develop the temporal and spatial pressures on the HHFEM that would simulate loading to the HSHM, a computational fluid dynamics (CFD) model of the HHFEM in front of a shock tube was generated. CFD simulations were made using loads equivalent to those seen in experimental studies of the HSHM for shock tube driver pressures of 517, 690 and 862 kPa. Using the selected brain material properties, the peak intracranial pressures, temporal and spatial histories of relative brain-skull displacements and the peak relative brain-skull displacements in the brain of the HHFEM compared favorably with results from the HSHM. The HSHM sensors measured the rotations of local areas of the brain as well as displacements, and the rotations of the sensors in the sagittal plane of the HSHM were, in general, correctly predicted from the HHFEM. Peak intracranial pressures were between 70 and 120 kPa, while the peak relative brain-skull displacements were between 0.5 and 3.0 mm. (C) 2012 Elsevier Ltd. All rights reserved. C1 [Roberts, J. C.; Harrigan, T. P.; Ward, E. E.; Taylor, T. M.; Merkle, A. C.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Annett, M. S.] NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Roberts, JC (reprint author), Johns Hopkins Univ, Appl Phys Lab, 10020 Johns Hopkins Rd, Laurel, MD 20723 USA. EM jack.roberts@jhuapl.edu FU Office of Naval Research (ONR) [N0001407PD20006]; Department of Defense Congressionally Directed Medical Research Programs (CDMRP) [W81XVVH-09-2-0168] FX The authors would like to express their appreciation to the Office of Naval Research (ONR) and the Department of Defense Congressionally Directed Medical Research Programs (CDMRP) under contracts N0001407PD20006 and W81XVVH-09-2-0168, respectively, for supporting this work. The content included in this work does not necessarily reflect the position or policy of the US Government. NR 24 TC 11 Z9 12 U1 4 U2 26 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0021-9290 J9 J BIOMECH JI J. Biomech. PD NOV 15 PY 2012 VL 45 IS 16 BP 2899 EP 2906 DI 10.1016/j.jbiomech.2012.07.027 PG 8 WC Biophysics; Engineering, Biomedical SC Biophysics; Engineering GA 050FS UT WOS:000312039100026 PM 23010219 ER PT J AU Fazal, IM Ahmed, N Wang, J Yang, JY Yan, Y Shamee, B Huang, H Yue, Y Dolinar, S Tur, M Willner, AE AF Fazal, Irfan M. Ahmed, Nisar Wang, Jian Yang, Jeng-Yuan Yan, Yan Shamee, Bishara Huang, Hao Yue, Yang Dolinar, Sam Tur, Moshe Willner, Alan E. TI 2 Tbit/s free-space data transmission on two orthogonal orbital-angular-momentum beams each carrying 25 WDM channels SO OPTICS LETTERS LA English DT Article ID DIVISION; SYSTEMS; LIGHT AB We demonstrate a 2 Tbit/s free-space data link using two orthogonal orbital angular momentum beams each carrying 25 different wavelength-division-multiplexing channels. We measure the performance for different modulation formats, including directly detected 40 Gbit/s nonreturn-to-zero (NRZ) differential phase-shift keying, 40 Gbit/s NRZ on-off keying, and coherently-detected 10 Gbaud NRZ quadrature phase-shift keying, and achieve low bit error rates with penalties less than 5 dB. (C) 2012 Optical Society of America C1 [Fazal, Irfan M.; Ahmed, Nisar; Wang, Jian; Yang, Jeng-Yuan; Yan, Yan; Shamee, Bishara; Huang, Hao; Yue, Yang; Willner, Alan E.] Univ So Calif, Dept Elect Engn, Los Angeles, CA 90089 USA. [Dolinar, Sam] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Tur, Moshe] Tel Aviv Univ, Sch Elect Engn, IL-69978 Tel Aviv, Israel. RP Ahmed, N (reprint author), Univ So Calif, Dept Elect Engn, Los Angeles, CA 90089 USA. EM nisarahm@usc.edu RI Yue, Yang/A-3357-2012 FU DARPA under the InPho (Information in Photon) program FX We acknowledge the support of DARPA under the InPho (Information in Photon) program. NR 14 TC 8 Z9 10 U1 0 U2 19 PU OPTICAL SOC AMER PI WASHINGTON PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA SN 0146-9592 J9 OPT LETT JI Opt. Lett. PD NOV 15 PY 2012 VL 37 IS 22 BP 4753 EP 4755 PG 3 WC Optics SC Optics GA 038JA UT WOS:000311169800063 PM 23164902 ER PT J AU Jozwiak, LM Head, JW Zuber, MT Smith, DE Neumann, GA AF Jozwiak, Lauren M. Head, James W. Zuber, Maria T. Smith, David E. Neumann, Gregory A. TI Lunar floor-fractured craters: Classification, distribution, origin and implications for magmatism and shallow crustal structure SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID IMPACT CRATERS; VISCOUS RELAXATION; EVOLUTION; GRAVITY; BASINS; INTRUSIONS; VOLCANISM; ERUPTION; MERCURY; DEPTH AB Floor-Fractured Craters (FFCs) are a class of lunar craters characterized by anomalously shallow floors cut by radial, concentric, and/or polygonal fractures; additional interior features are moats, ridges, and patches of mare material. Two formation mechanisms have been hypothesized-floor uplift in response to shallow magmatic intrusion and sill formation, and floor shallowing in response to thermally driven viscous relaxation. This study combines new Lunar Orbiter Laser Altimeter (LOLA) and Lunar Reconnaissance Orbiter Camera (LROC) data to characterize and categorize the population of FFCs and map their distribution on the Moon, and uses variations in floor-fractured crater morphology and regional distribution to investigate the proposed formation mechanisms. The population of FFCs was categorized according to the classes outlined by Schultz (1976). The distribution of these FFC categories shows an evolution of crater morphology from areas adjacent to lunar impact basins to areas in the lunar highlands. We propose that this trend is supportive of formation by shallow magmatic intrusion and sill formation-crustal thickness determines the magnitude of magmatic driving pressure, and thus either piston-like floor uplift for high magnitude, or a convex floor profile for low magnitude. Predictions from previous studies modeling viscous relaxation are inconsistent with the observed altimetric profiles of FFCs. Hence our analysis favors FFC formation by shallow magmatic intrusion, with the variety of FFC morphologies being intimately linked with location and crustal thickness, and the driving pressure of the intrusion. Data from the GRAIL (Gravity Recovery and Interior Laboratory) mission will help to test these conclusions. C1 [Jozwiak, Lauren M.; Head, James W.] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA. [Zuber, Maria T.; Smith, David E.] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA USA. [Neumann, Gregory A.] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA. RP Jozwiak, LM (reprint author), Brown Univ, Dept Geol Sci, Providence, RI 02912 USA. EM lauren_jozwiak@brown.edu RI Neumann, Gregory/I-5591-2013; Jozwiak, Lauren/N-2474-2016 OI Neumann, Gregory/0000-0003-0644-9944; Jozwiak, Lauren/0000-0001-7946-5633 FU LRO LOLA [NNX09AM54G] FX Thanks are extended to the Lunar Reconnaissance Orbiter (LRO) mission personnel and to the planning and operations teams for both LOLA and LROC. This work was supported by the LRO LOLA team through grant NNX09AM54G to JWH. NR 43 TC 23 Z9 23 U1 0 U2 16 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9097 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD NOV 15 PY 2012 VL 117 AR E11005 DI 10.1029/2012JE004134 PG 23 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 039OJ UT WOS:000311256000001 ER PT J AU Zhang, FF Xu, HF Konishi, H Kemp, JM Roden, EE Shen, ZZ AF Zhang, Fangfu Xu, Huifang Konishi, Hiromi Kemp, Joshua M. Roden, Eric E. Shen, Zhizhang TI Dissolved sulfide-catalyzed precipitation of disordered dolomite: Implications for the formation mechanism of sedimentary dolomite SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Article ID SULFATE-REDUCING BACTERIA; CONTINENTAL-MARGIN SEDIMENTS; ANAEROBIC METHANE OXIDATION; LATEMAR CARBONATE BUILDUP; ORGANIC-RICH SEDIMENTS; GULF-OF-CALIFORNIA; CALCIUM-CARBONATE; ORGANOGENIC DOLOMITIZATION; ISOTOPE FRACTIONATION; MICROBIAL MEDIATION AB Dolomite is a common mineral in the rock record. However, the rarity of modern dolomite and the notorious difficulty in synthesizing dolomite abiotically under normal Earth-surface conditions result in the long-standing "dolomite problem" in sedimentary geology. Some modern dolomites are associated with sediments where microbial sulfate reduction is active; however, the role of sulfate-reducing bacteria in dolomite formation is still under debate. In this study, we tested the effect of dissolved sulfide on the precipitation of Ca-Mg carbonates, which has been never explored before although dissolved sulfide is one of the major products of microbial sulfate reduction. Our results demonstrated that dissolved sulfide with a concentration of as low as several millimoles can enhance the Mg2+ incorporation into the calcitic structure, and promote the crystallization of high magnesian calcite and disordered dolomite. We also conducted seeded precipitation in experimental solutions containing dissolved sulfide, which showed that calcite seeds can inhibit the precipitation of aragonite and monohydrocalcite (CaCO3 center dot H2O), and induce more Mg2+ incorporation. We propose that accumulated dissolved sulfide in pore waters in organic-rich sediments may trigger the precipitation of disordered dolomite which can be considered as a precursor of some sedimentary dolomite. Our adsorption experiments revealed a strong adsorption of dissolved sulfide onto calcite faces. We suggest that adsorbed dissolved sulfide can lower the energy barrier to the dehydration of Mg2+-water complexes on the growing carbonate surfaces. This study sheds new light on understanding the role of sulfate-reducing bacteria in dolomite formation and the formation mechanism of sedimentary dolomite. (C) 2012 Published by Elsevier Ltd. C1 [Zhang, Fangfu; Xu, Huifang; Konishi, Hiromi; Kemp, Joshua M.; Roden, Eric E.; Shen, Zhizhang] Univ Wisconsin, Dept Geosci, NASA Astrobiol Inst, Madison, WI 53706 USA. RP Xu, HF (reprint author), Univ Wisconsin, Dept Geosci, NASA Astrobiol Inst, 1215 W Dayton St,A352 Weeks Hall, Madison, WI 53706 USA. EM hfxu@geology.wisc.edu RI Zhang, Fangfu/B-4295-2014 OI Zhang, Fangfu/0000-0001-7550-9483 FU NASA Astrobiology Institute [N07-5489]; NSF [EAR-095800]; U.S. Department of Energy [DE-SC0001929]; Department of Geoscience, University of Wisconsin-Madison; ExxonMobil; Geological Society of America FX This work is supported by NASA Astrobiology Institute (N07-5489), NSF (EAR-095800), and U.S. Department of Energy (DE-SC0001929). We thank Prof. Timothy W. Lyons for handling this paper and the three anonymous reviewers for their fruitful suggestions which greatly improved this paper. We thank Dr. John Fournelle for providing the dolomite standard. Zhang thanks Department of Geoscience, University of Wisconsin-Madison and ExxonMobil for 2008 Summer Research Grant, and Geological Society of America for 2009 Graduate Research Grant. NR 116 TC 29 Z9 33 U1 1 U2 61 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD NOV 15 PY 2012 VL 97 BP 148 EP 165 DI 10.1016/j.gca.2012.09.008 PG 18 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 028MW UT WOS:000310427400010 ER PT J AU Peslier, AH Woodland, AB Bell, DR Lazarov, M Lapen, TJ AF Peslier, A. H. Woodland, A. B. Bell, D. R. Lazarov, M. Lapen, T. J. TI Metasomatic control of water contents in the Kaapvaal cratonic mantle SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Article ID NOMINALLY ANHYDROUS MINERALS; SOUTHERN AFRICAN KIMBERLITES; ARCHEAN LITHOSPHERIC MANTLE; EARTHS UPPER-MANTLE; MELT-ROCK REACTION; RE-OS ISOTOPE; TRACE-ELEMENT; PERIDOTITE XENOLITHS; ORTHO-PYROXENE; HYDROGEN DIFFUSION AB Water and trace element contents were measured by FTIR and laser ablation-ICPMS on minerals from peridotite xenoliths in kimberlites of the Kaapvaal craton from Finsch, Kimberley, Jagersfontein (South Africa), Letseng-La-Terae, and Liqhobong (Lesotho) mines. The peridotites record a wide range of pressure, temperature, oxygen fugacity, and metasomatic events. Correlations between water content or OH vibration bands with major, minor and trace elements in pyroxene and garnet precludes disturbance during xenolith entrainment by the host kimberlite magma and indicate preservation of mantle water contents. Clinopyroxene water contents (150-400 ppm H2O, by weight) correlate with those of orthopyroxene (40-250 ppm). Olivines (Peslier et al., 2008, 2010) and garnets have 0-86 and 0-20 ppm H2O, respectively. Relations in individual xenolith suites between the amount of water and that of incompatible elements Ti, Na, Fe3+ and rare earths in minerals suggests that metasomatism by oxidizing melts controls the water content of olivine, pyroxene and garnet. At pressures <= 5.5 GPa, hydrous, alkaline, siliceous fluids or melts metasomatized Liqhobong and Kimberley peridotites, producing high water contents in their olivine, pyroxenes and garnet. At higher pressures, the percolation of ultramafic melts reacting with peridotite resulted in co-variation of Ca, Ti and water at the edge of garnets at Jagersfontein, and the overall crystallization of garnet with lower water contents than those in the original peridotites. The upward migration of these ultramafic melts through the lithospheric mantle also increased the water content of olivines with decreasing pressure at Finsch Mine. H2O/Ce ratios of melts in equilibrium with Kaapvaal peridotites range from 100 to 20,000 and the larger values may indicate metasomatism in subduction zone settings. Metasomatic events in Kaapvaal peridotites are thought to have occurred from the Archean to the Mesozoic. However, circumstantial evidence suggest that the metasomatic events responsible for setting the water contents may date from the Archean at Kimberley and from the Proterozoic at Jagersfontein. Combined water with Lu-Hf and Sm-Nd isotopic data at Finsch (Lazarov et al., in press-a) and with Ar-Ar phlogopite ages at Liqhobong (Hopp et al., 2008) indicates that water addition by metasomatic melts occurred in the Proterozoic. Water contents of mantle minerals in Kaapvaal xenoliths measured here have been preserved since that time and can consequently be used in modelling viscosity and longevity of cratonic roots since at least the mid-Proterozoic. (C) 2012 Elsevier Ltd. All rights reserved. C1 [Peslier, A. H.] Jacobs Technol, ESCG, Houston, TX 77058 USA. [Peslier, A. H.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Woodland, A. B.] Goethe Univ Frankfurt, Inst Geosci, D-60438 Frankfurt, Germany. [Bell, D. R.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [Lazarov, M.] Leibniz Univ Hannover, Inst Mineral, D-30167 Hannover, Germany. [Lapen, T. J.] Univ Houston, Houston, TX 77204 USA. RP Peslier, AH (reprint author), Jacobs Technol, ESCG, Mail Code JE23,2224 Bay Area Blvd, Houston, TX 77058 USA. EM anne.h.peslier@nasa.gov; woodland@em.uni-frankfurt.de; David.R.Bell@asu.edu; m.lazarov@mineralogie.uni-hannover.de; tjlapen@uh.edu FU NSF [EAR-1118335, EAR-1129072, EAR-0743377] FX This work was supported by NSF (Grants EAR-1118335, EAR-1129072, and EAR-0743377). Thank you to L. Keller for letting AHP use his Nicolet FTIR. We are very grateful to M. Gregoire and two anonymous reviewers for their constructive comments which greatly improved this manuscript and to M. Norman for his work as editor. NR 213 TC 32 Z9 35 U1 3 U2 66 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD NOV 15 PY 2012 VL 97 BP 213 EP 246 DI 10.1016/j.gca.2012.08.028 PG 34 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 028MW UT WOS:000310427400014 ER PT J AU Garcia-Soto, C Vazquez-Cuervo, J Clemente-Colon, P Hernandez, F AF Garcia-Soto, Carlos Vazquez-Cuervo, Jorge Clemente-Colon, Pablo Hernandez, Fabrice TI Satellite oceanography and climate change SO DEEP-SEA RESEARCH PART II-TOPICAL STUDIES IN OCEANOGRAPHY LA English DT Article DE Climate change; Satellite oceanography; Global warming; Sea level rise; Polar regions; Natural climate variability ID SEA-SURFACE TEMPERATURE; LEVEL RISE; VARIABILITY; ICE; CHLOROPHYLL; OSCILLATION; PATTERNS; COLLAPSE; TRENDS; BUDGET AB Satellites are essential tools in the present monitoring of climate change as they provide frequent measurements of the Earth over decades with significantly high spatial resolution. Satellite measurements of sea surface temperature are a key component in the analyses of global warming and its effects. Altimeters and gravity missions such as GRACE are used to measure sea level rise at global and regional scales. A variety of satellite sensors (microwave and visible radiometers, scatterometers, SAR, gravity sensors, altimeters, etc.) are used for tracking the melting of sea ice and continental ice over the Polar Regions and Greenland. Satellite techniques are used to monitor large scale natural climate oscillations such as El Nino and the influence of atmospheric teleconexions such as NAO. The present issue is the first one of a series of issues updating our knowledge of the satellite-observed variability related to climate change. A short introduction to the topic is presented. (c) 2012 Elsevier Ltd. All rights reserved. C1 [Garcia-Soto, Carlos] IEO, Santander 39004, Spain. [Garcia-Soto, Carlos] Plentziako Itsas Estazioa Euskalherriko Unibertsi, Plentzia 48620, Spain. [Vazquez-Cuervo, Jorge] CALTECH, NASA Jet Prop Lab JPL, Pasadena, CA 91109 USA. [Clemente-Colon, Pablo] NOAA NSOF, Natl Naval Ice Ctr, Washington, DC 20395 USA. [Hernandez, Fabrice] MERCATOR Ocean IRD, F-31520 Ramonville St Agne, France. RP Garcia-Soto, C (reprint author), IEO, Promontorio S Martin S-N, Santander 39004, Spain. EM carlos.soto@st.ieo.es RI Clemente-Colon, Pablo/F-5581-2010; Hernandez, Fabrice/F-6642-2013 OI Hernandez, Fabrice/0000-0003-2152-0657 NR 38 TC 4 Z9 4 U1 0 U2 45 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 NOV 15 PY 2012 VL 77-80 SI SI BP 1 EP 9 DI 10.1016/j.dsr2.2012.07.004 PG 9 WC Oceanography SC Oceanography GA 006TS UT WOS:000308842500001 ER PT J AU Nghiem, SV Clemente-Colon, P Rigor, IG Hall, DK Neumann, G AF Nghiem, S. V. Clemente-Colon, P. Rigor, I. G. Hall, D. K. Neumann, G. TI Seafloor control on sea ice SO DEEP-SEA RESEARCH PART II-TOPICAL STUDIES IN OCEANOGRAPHY LA English DT Article DE Sea ice; Bathymetry; Arctic; Scatterometer; IBCAO ID GREENLAND SEA; POLAR FRONT; BARENTS SEA; OCEAN AB The seafloor has a profound role in Arctic Sea ice formation and seasonal evolution. Ocean bathymetry controls the distribution and mixing of warm and cold waters, which may originate from different sources, thereby dictating the pattern of sea ice on the ocean surface. Sea ice dynamics, forced by surface winds, are also guided by seafloor features in preferential directions. Here, satellite mapping of sea ice together with buoy measurements are used to reveal the bathymetric control on sea ice growth and dynamics. Bathymetric effects on sea ice formation are clearly observed in the conformity between sea ice patterns and bathymetric characteristics in the peripheral seas. Beyond local features, bathymetric control appears over extensive regions of the sea ice cover across the Arctic Ocean. The large-scale conformity between bathymetry and patterns of different synoptic sea ice classes, including seasonal and perennial sea ice, is identified. An implication of the bathymetric influence is that the maximum extent of the total sea ice cover is relatively stable, as observed by scatterometer data in the decade of the 2000s, while the minimum ice extent has decreased drastically. Because of the geologic control, the sea ice cover can expand only as far as it reaches the seashore, the continental shelf break, or other pronounced bathymetric features in the peripheral seas. Since the seafloor does not change significantly for decades or centuries, sea ice patterns can be recurrent around certain bathymetric features, which, once identified, may help improve short-term forecast, seasonal outlook, and decadal prediction of the sea ice cover. Moreover, the seafloor can indirectly influence the cloud cover by its control on sea ice distribution, which differentially modulates the latent heat flux through ice covered and open water areas. (c) 2012 Elsevier Ltd. All rights reserved. C1 [Nghiem, S. V.; Neumann, G.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Clemente-Colon, P.] Natl Naval Ice Ctr, Washington, DC 20395 USA. [Rigor, I. G.] Univ Washington, Appl Phys Lab, Seattle, WA 98105 USA. [Hall, D. K.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Nghiem, SV (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM son.v.nghiem@jpl.nasa.gov RI Clemente-Colon, Pablo/F-5581-2010 FU National Aeronautics and Space Administration (NASA) Cryospheric Sciences Program (CSP); NASA CSP; NASA FX The research carried out at the Jet Propulsion Laboratory, California Institute of Technology, was supported by the National Aeronautics and Space Administration (NASA) Cryospheric Sciences Program (CSP). The research at the Goddard Space Flight Center is also supported by NASA CSP. Rigor is funded by NASA, and the contributors to the International Arctic Buoy Programme (IABP), which include the International Arctic Research Center, NASA, NAVO, NIC, NOAA, NSF, ONR, and U.S. Coast Guard. The views, opinions, and findings contained in this report are those of the authors and should not be construed as an official National Oceanic and Atmospheric Administration, or any other U.S. government position, policy, or decision. NR 40 TC 11 Z9 13 U1 0 U2 18 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 NOV 15 PY 2012 VL 77-80 SI SI BP 52 EP 61 DI 10.1016/j.dsr2.2012.04.004 PG 10 WC Oceanography SC Oceanography GA 006TS UT WOS:000308842500006 ER PT J AU Dewitte, B Vazquez-Cuervo, J Goubanova, K Illig, S Takahashi, K Cambon, G Purca, S Correa, D Gutierrez, D Sifeddine, A Ortlieb, L AF Dewitte, B. Vazquez-Cuervo, J. Goubanova, K. Illig, S. Takahashi, K. Cambon, G. Purca, S. Correa, D. Gutierrez, D. Sifeddine, A. Ortlieb, L. TI Change in El Nino flavours over 1958-2008: Implications for the long-term trend of the upwelling off Peru SO DEEP-SEA RESEARCH PART II-TOPICAL STUDIES IN OCEANOGRAPHY LA English DT Article DE El Nino Modoki; Equatorial Kelvin wave; Climate change; Coastal upwelling; Peru undercurrent ID SEA-SURFACE TEMPERATURE; HIGH-RESOLUTION; CURRENT SYSTEM; PACIFIC RIM; WARM POOL; OCEAN; MODEL; CLIMATE; ENSO; REANALYSIS AB The tropical Pacific variability has experienced changes in its characteristics over the last decades. In particular, there is some evidence of an increased occurrence of El Nino events in the central Pacific (a.k.a. 'Central Pacific El Nino' (CP El Nino) or 'El Nino Modoki'), in contrast with the cold tongue or Eastern Pacific (EP) El Nino which develops in the eastern Pacific. Here we show that the different flavours of El Nino imply a contrasted Equatorial Kelvin Wave (EKW) characteristic and that their rectification on the mean upwelling condition off Peru through oceanic teleconnection is changed when the CP El Nino frequency of occurrence increases. The Simple Ocean Data Assimilation (SODA) reanalysis product is first used to document the seasonal evolution of the EKW during CP and EP El Nino. It is shown that the strong positive asymmetry of ENSO (El Nino Southern Oscillation) is mostly reflected into the EKW activity of the EP El Nino whereas during CP El Nino, the EKW is negatively skewed in the eastern Pacific. Along with slightly cooler conditions off Peru (shallow thermocline) during CP El Nino, this is favourable for the accumulation of cooler SST anomalies along the coast by the remotely forced coastal Kelvin wave. Such a process is observed in a high-resolution regional model of the Humboldt Current system using the SODA outputs as boundary conditions. In particular the model simulates a cooling trend of the SST off Peru although the wind stress forcing has no trend. The model is further used to document the vertical structure along the coast during the two types of El Nino. It is suggested that the increased occurrence of the CP El Nino may also lead to a reduction of mesoscale activity off Peru. (c) 2012 Elsevier Ltd. All rights reserved. C1 [Dewitte, B.; Goubanova, K.; Illig, S.; Cambon, G.] IRD, LEGOS, Toulouse, France. [Vazquez-Cuervo, J.] NASA, JPL, CALTECH, Pasadena, CA USA. [Goubanova, K.] CNES, Toulouse, France. [Illig, S.; Purca, S.; Gutierrez, D.] Inst Mar Peru, Callao, Peru. [Takahashi, K.] Inst Geofis Peru, Lima, Peru. [Correa, D.] Serv Nacl Meteorol & Hidrol Peru, Lima, Peru. [Gutierrez, D.] Univ Peruana Cayetano Heredia, Programa Maestria Ciencias Mar, Lima, Peru. [Sifeddine, A.; Ortlieb, L.] IRD, LOCEAN, Paris, France. [Sifeddine, A.; Ortlieb, L.] IRD, LOCEAN, Bondy, France. [Sifeddine, A.] Univ Fed Fluminense, LMI PALEOTRACES, Dept Geoquim, Niteroi, RJ, Brazil. RP Dewitte, B (reprint author), IRD, LEGOS, Toulouse, France. EM bxd@legos.obs-mip.fr RI ORTLIEB, Luc/A-8801-2011; Takahashi, Ken/G-5321-2010; Cambon, Gildas/A-1882-2016; OI Takahashi, Ken/0000-0003-3670-2939; Cambon, Gildas/0000-0002-3899-1204; Purca, Sara/0000-0001-8751-1476 FU National Aeronautics and Space Administration; CNES (Centre National d'Etudes Spatiales, France); Peru Chile Climate Change (PCCC) program of the Agence Nationale de la Recherche (ANR); CALMIP [2011-[1044]] FX Most parts of this work were initiated while Boris Dewitte was at CIMOBP (modelling centre at IMARPE, Peru). Katerina Goubanova was supported by CNES (Centre National d'Etudes Spatiales, France). Jorge Vazquez-Cuervo was supported under contract with the National Aeronautics and Space Administration. We would like to thank the Peru Chile Climate Change (PCCC) program of the Agence Nationale de la Recherche (ANR) for financial support. This work was performed using HPC resources from CALMIP (Grant 2011-[1044]). We are grateful to Dr. Ben Giese from Texas A&M University for providing the SODA data. Pr. D. Gushchina (University of Moscow) is also acknowledged for fruitful discussions on a previous version of this manuscript. NR 61 TC 24 Z9 24 U1 5 U2 83 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 NOV 15 PY 2012 VL 77-80 SI SI BP 143 EP 156 DI 10.1016/j.dsr2.2012.04.011 PG 14 WC Oceanography SC Oceanography GA 006TS UT WOS:000308842500014 ER PT J AU Singh, G West, WC Soler, J Katiyar, RS AF Singh, Gurpreet West, W. C. Soler, J. Katiyar, Ram S. TI In situ Raman spectroscopy of layered solid solution Li2MnO3-LiMO2 (M = Ni, Mn, Co) SO JOURNAL OF POWER SOURCES LA English DT Article DE Cathode; Solid solution; Lithium ion battery; Raman spectroscopy ID ELECTROCHEMICAL ACTIVITY; IRREVERSIBLE CAPACITY; OXYGEN LOSS; ELECTRODES; CATHODES; BATTERIES; OXIDE; LI AB Lithium rich manganese oxide based materials are emerging as possible high energy density cathode materials for lithium ion batteries. In the present research, we have investigated the first charge/discharge profile behavior of Li1.2Ni0.175Co0.1Mn0.52O2 via in situ Raman spectroscopy. X-ray diffraction studies confirm the presence of cation ordering in the transition metal layers. Scanning electron microscopy shows the homogeneous distribution of highly dense spherical agglomerates of similar to 5 mu m size. Steady decrease in impedance up to similar to 4.5 V followed by a less steep increase as the cell voltage traversed the first charge cycle has been confirmed by electrochemical impedance spectroscopy. Raman spectroscopy shows that the extraction of lithium takes place from both the transition metal layers as well as lithium layers in the voltage range of 4.1-4.4 V. The oxygen removal becomes severe in the voltage range of 4.55-4.6 V, after which the diffusion of the transition metal ions to the vacant sites takes place. (C) 2012 Elsevier B.V. All rights reserved. C1 [Singh, Gurpreet; Katiyar, Ram S.] Univ Puerto Rico, Dept Phys, Inst Funct Nanomat, San Juan, PR 00936 USA. [West, W. C.; Soler, J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Singh, G (reprint author), Univ Puerto Rico, Dept Phys, Inst Funct Nanomat, San Juan, PR 00936 USA. EM singhgurpreet268@yahoo.com RI Singh, Gurpreet/B-5293-2012 OI Singh, Gurpreet/0000-0001-5496-6992 FU NASA-URC [NNX08BA48A]; NASA FX The financial support from NASA-URC (NNX08BA48A) grant to University of Puerto Rico is gratefully acknowledged.; This work was partially carried out at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. The authors acknowledge the funding support of NASA's Space Power Systems Program. NR 21 TC 23 Z9 25 U1 7 U2 159 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0378-7753 EI 1873-2755 J9 J POWER SOURCES JI J. Power Sources PD NOV 15 PY 2012 VL 218 BP 34 EP 38 DI 10.1016/j.jpowsour.2012.06.083 PG 5 WC Chemistry, Physical; Electrochemistry; Energy & Fuels; Materials Science, Multidisciplinary SC Chemistry; Electrochemistry; Energy & Fuels; Materials Science GA 009PQ UT WOS:000309038100007 ER PT J AU Bell, SW Thomson, BJ Dyar, MD Neish, CD Cahill, JTS Bussey, DBJ AF Bell, Samuel W. Thomson, Bradley J. Dyar, M. Darby Neish, Catherine D. Cahill, Joshua T. S. Bussey, D. B. J. TI Dating small fresh lunar craters with Mini-RF radar observations of ejecta blankets SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID IMPACT CRATERS; AGE; MATURITY; FARSIDE; SURFACE; EARTH; MOON AB The ages of large impact craters on the Moon can be estimated by measuring the size-frequency distribution of smaller craters superimposed on their ejecta, but applying this method to individual craters under similar to 3 km in diameter remains difficult due to their limited areal extent. The ejecta blankets of fresh lunar impact craters are expressed as halos of optical and radar bright material that gradually fade with time. Although compositional differences make inferring crater ages from optical albedo problematic, radar is less sensitive to composition and thus may provide a more reliable means of estimating age. In this work, we use radar data from the Miniature Radio Frequency (Mini-RF) instrument on the Lunar Reconnaissance Orbiter (LRO) to characterize the radar backscatter of large numbers of ejecta blankets. By analyzing the size-frequency distribution of these craters, we show that the lifetime of the radar-bright discontinuous ejecta blanket varies with crater diameter in a predictable way for craters with diameters between 0.45 and 5 km. Absolute ages of individual craters can then be estimated by combining this empirically derived model with estimates of the relative degradation state of each individual crater. The lifetimes of radar-bright discontinuous ejecta blankets are significantly shorter in the highlands than the maria, although this is likely due to local topography, creating difficulties in applying the method to the highlands. The cosmic ray exposure age of South Ray Crater, a fresh crater visited by Apollo 16, provides confirmation of these results. This method therefore provides a new way to accurately date small, fresh craters using the Mini-RF data set. C1 [Bell, Samuel W.] Brown Univ, Providence, RI 02912 USA. [Thomson, Bradley J.] Boston Univ, Ctr Remote Sensing, Boston, MA 02215 USA. [Dyar, M. Darby] Mt Holyoke Coll, Dept Astron, S Hadley, MA 01075 USA. [Neish, Catherine D.] NASA, Goddard Space Flight Ctr, Planetary Geodynam Lab, Greenbelt, MD 20771 USA. [Cahill, Joshua T. S.; Bussey, D. B. J.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA. RP Bell, SW (reprint author), Brown Univ, 45 Prospect St, Providence, RI 02912 USA. EM samuel_bell@brown.edu RI Neish, Catherine/G-6321-2012; Cahill, Joshua/I-3656-2012; OI Cahill, Joshua/0000-0001-6874-5533; Thomson, Bradley/0000-0001-8635-8932 NR 60 TC 11 Z9 11 U1 0 U2 7 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9097 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD NOV 14 PY 2012 VL 117 AR E00H30 DI 10.1029/2011JE004007 PG 14 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 039OG UT WOS:000311255600001 ER PT J AU Harrison, KW Kumar, SV Peters-Lidard, CD Santanello, JA AF Harrison, Kenneth W. Kumar, Sujay V. Peters-Lidard, Christa D. Santanello, Joseph A. TI Quantifying the change in soil moisture modeling uncertainty from remote sensing observations using Bayesian inference techniques SO WATER RESOURCES RESEARCH LA English DT Article ID CHAIN MONTE-CARLO; SATURATED HYDRAULIC CONDUCTIVITY; LAND INFORMATION-SYSTEM; MESOSCALE ETA-MODEL; BOUNDARY-LAYER; UNITED-STATES; DIFFERENTIAL EVOLUTION; PEDOTRANSFER FUNCTIONS; HETEROGENEOUS SOILS; MAXIMUM-LIKELIHOOD AB Operational land surface models (LSMs) compute hydrologic states such as soil moisture that are needed for a range of important applications (e. g., drought, flood, and weather prediction). The uncertainty in LSM parameters is sufficiently great that several researchers have proposed conducting parameter estimation using globally available remote sensing data to identify best fit local parameter sets. However, even with in situ data at fine modeling scales, there can be significant remaining uncertainty in LSM parameters and outputs. Here, using a new uncertainty estimation subsystem of the NASA Land Information System (LIS) (described herein), a Markov chain Monte Carlo (MCMC) technique is applied to conduct Bayesian analysis for the accounting of parameter uncertainties. The Differential Evolution Markov Chain (DE-MC) MCMC algorithm was applied, for which a new parallel implementation was developed. A case study is examined that builds on previous work in which the Noah LSM was calibrated to passive (L-band) microwave remote sensing estimates of soil moisture for the Walnut Gulch Experimental Watershed. In keeping with prior related studies, the parameters subjected to the analysis were restricted to the soil hydraulic properties (SHPs). The main goal is to estimate SHPs and soil moisture simulation uncertainty before and after consideration of the remote sensing data. The prior SHP uncertainty is based on the original source of the standard SHP lookup tables for the Noah LSM. Conclusions are drawn regarding the value and viability of Bayesian analysis over alternative approaches (e. g., parameter estimation, lookup tables) and further research needs are identified. C1 [Harrison, Kenneth W.; Kumar, Sujay V.; Peters-Lidard, Christa D.; Santanello, Joseph A.] NASA, Hydrol Sci Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Kumar, Sujay V.] Sci Applicat Int Corp, Beltsville, MD USA. [Harrison, Kenneth W.] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. RP Harrison, KW (reprint author), NASA, Hydrol Sci Lab, Goddard Space Flight Ctr, Code 617,8800 Greenbelt Rd, Greenbelt, MD 20771 USA. EM ken.harrison@nasa.gov RI Santanello, Joseph/D-4438-2012; Kumar, Sujay/B-8142-2015; Peters-Lidard, Christa/E-1429-2012 OI Santanello, Joseph/0000-0002-0807-6590; Peters-Lidard, Christa/0000-0003-1255-2876 FU NASA Earth Science Technology Office (ESTO) [AIST-08-077] FX We gratefully acknowledge the financial support from the NASA Earth Science Technology Office (ESTO) (Advanced Information System Technology program award AIST-08-077). Thanks to David Mocko and Scott Rheingrover for helpful comments. Also, we thank the anonymous reviewers who suggestions improved the manuscript. Computing was supported by the resources at the NASA Center for Climate Simulation. NR 132 TC 14 Z9 14 U1 2 U2 34 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 NOV 13 PY 2012 VL 48 AR W11514 DI 10.1029/2012WR012337 PG 22 WC Environmental Sciences; Limnology; Water Resources SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Water Resources GA 039AW UT WOS:000311216200003 ER PT J AU Gerin, M Levrier, F Falgarone, E Godard, B Hennebelle, P Le Petit, F De Luca, M Neufeld, D Sonnentrucker, P Goldsmith, P Flagey, N Lis, DC Persson, CM Black, JH Goicoechea, JR Menten, KM AF Gerin, M. Levrier, F. Falgarone, E. Godard, B. Hennebelle, P. Le Petit, F. De Luca, M. Neufeld, D. Sonnentrucker, P. Goldsmith, P. Flagey, N. Lis, D. C. Persson, C. M. Black, J. H. Goicoechea, J. R. Menten, K. M. TI Hydride spectroscopy of the diffuse interstellar medium: new clues on the gas fraction in molecular form and cosmic ray ionization rate in relation to H-3(+) SO PHILOSOPHICAL TRANSACTIONS OF THE ROYAL SOCIETY A-MATHEMATICAL PHYSICAL AND ENGINEERING SCIENCES LA English DT Article DE diffuse interstellar medium; W49N; W51 ID MEUDON PDR CODE; HERSCHEL/HIFI OBSERVATIONS; G10.6-0.4 W31C; NITROGEN HYDRIDES; ABSORPTION-LINES; SIGHT-LINE; CLOUDS; REGIONS; W49N; CHLORONIUM AB The Herschel-guaranteed time key programme PRobing InterStellar Molecules with Absorption line Studies (PRISMAS)(1) is providing a survey of the interstellar hydrides containing the elements C, O, N, F and Cl. As the building blocks of interstellar molecules, hydrides provide key information on their formation pathways. They can also be used as tracers of important physical and chemical properties of the interstellar gas that are difficult to measure otherwise. This paper presents an analysis of two sight-lines investigated by the PRISMAS project, towards the star-forming regions W49N and W51. By combining the information extracted from the detected spectral lines, we present an analysis of the physical properties of the diffuse interstellar gas, including the electron abundance, the fraction of gas in molecular form, and constraints on the cosmic ray ionization rate and the gas density. C1 [Gerin, M.; Levrier, F.; Falgarone, E.; Hennebelle, P.; De Luca, M.] Observ Paris, LERMA, CNRS UMR8112, F-75014 Paris, France. [Gerin, M.; Levrier, F.; Falgarone, E.; Hennebelle, P.; De Luca, M.] ENS, F-75230 Paris 05, France. [Godard, B.; Goicoechea, J. R.] Ctr Astrobiol CAB, Madrid 28850, Spain. [Le Petit, F.] Observ Paris, LUTh, CNRS UMR8102, Meudon, France. [Neufeld, D.] Johns Hopkins Univ, Baltimore, MD 21218 USA. [Sonnentrucker, P.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Goldsmith, P.; Flagey, N.] Jet Prop Lab, Pasadena, CA 91011 USA. [Lis, D. C.] CALTECH, Pasadena, CA 91125 USA. [Persson, C. M.; Black, J. H.] Chalmers, SE-43992 Onsala, Sweden. [Menten, K. M.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. RP Gerin, M (reprint author), Observ Paris, LERMA, CNRS UMR8112, F-75014 Paris, France. EM maryvonne.gerin@lra.ens.fr FU CNES; CNRS/INSU program PCMI; French Agence Nationale de la Recherche [ANR-09-BLAN-0231-01] FX HIFI has been designed and built by a consortium of institutes and university departments from across Europe, Canada and the USA under the leadership of the SRON Netherlands Institute for Space Research, Groningen, The Netherlands, and with major contributions from Germany, France and the USA. 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. The 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. M.G., F.L., E.F., P.H. and M.D.L. acknowledge support from CNES and from the CNRS/INSU program PCMI. The chemical modelling is partly funded by grant no. ANR-09-BLAN-0231-01 from the French Agence Nationale de la Recherche as part of the SCHISM project. NR 32 TC 13 Z9 13 U1 0 U2 5 PU ROYAL SOC PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 1364-503X J9 PHILOS T R SOC A JI Philos. Trans. R. Soc. A-Math. Phys. Eng. Sci. PD NOV 13 PY 2012 VL 370 IS 1978 BP 5174 EP 5185 DI 10.1098/rsta.2012.0023 PG 12 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 016MN UT WOS:000309522800017 PM 23028164 ER PT J AU Beilicke, M Baring, MG Barthelmy, S Binns, WR Buckley, J Cowsik, R Dowkontt, P Garson, A Guo, Q Haba, Y Israel, MH Kunieda, H Lee, K Matsumoto, H Miyazawa, T Okajima, T Schnittman, J Tamura, K Tueller, J Krawczynski, H AF Beilicke, M. Baring, M. G. Barthelmy, S. Binns, W. R. Buckley, J. Cowsik, R. Dowkontt, P. Garson, A. Guo, Q. Haba, Y. Israel, M. H. Kunieda, H. Lee, K. Matsumoto, H. Miyazawa, T. Okajima, T. Schnittman, J. Tamura, K. Tueller, J. Krawczynski, H. TI Design and tests of the hard X-ray polarimeter X-Calibur SO NUCLEAR INSTRUMENTS & METHODS IN PHYSICS RESEARCH SECTION A-ACCELERATORS SPECTROMETERS DETECTORS AND ASSOCIATED EQUIPMENT LA English DT Article; Proceedings Paper CT 3rd Roma International Conference on Astroparticle Physics (RICAP) CY MAY 24-27, 2011 CL Roma Tre Univ, Roma, ITALY SP Univ Sapienza, Univ Tor Vergata HO Roma Tre Univ DE X-rays; Polarization; Black hole; InFOC mu S; X-Calibur ID EMISSION; CRAB AB X-ray polarimetry will give qualitatively new information about high-energy astrophysical sources. We designed, built and tested a hard X-ray polarimeter X-Calibur to be used in the focal plane of the InFOC mu S grazing incidence hard X-ray telescope. X-Calibur combines a low-Z Compton scatterer with a CZT detector assembly to measure the polarization of 10-80 keV X-rays making use of the fact that polarized photons Compton scatter preferentially perpendicular to the electric field orientation. X-Calibur achieves a high detection efficiency of order unity. (C) 2012 Elsevier B.V. All rights reserved. C1 [Beilicke, M.; Binns, W. R.; Buckley, J.; Cowsik, R.; Dowkontt, P.; Garson, A.; Guo, Q.; Israel, M. H.; Lee, K.; Krawczynski, H.] Washington Univ, St Louis, MO 63130 USA. [Baring, M. G.] Rice Univ, Houston, TX 77251 USA. [Barthelmy, S.; Okajima, T.; Schnittman, J.; Tueller, J.] Goddard Space Flight Ctr, Greenbelt, MD USA. [Haba, Y.; Kunieda, H.; Matsumoto, H.; Miyazawa, T.; Tamura, K.] Nagoya Univ, Nagoya, Aichi 4648601, Japan. RP Beilicke, M (reprint author), Washington Univ, St Louis, MO 63130 USA. EM beilicke@physics.wustl.edu NR 8 TC 1 Z9 1 U1 1 U2 2 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0168-9002 J9 NUCL INSTRUM METH A JI Nucl. Instrum. Methods Phys. Res. Sect. A-Accel. Spectrom. Dect. Assoc. Equip. PD NOV 11 PY 2012 VL 692 BP 283 EP 284 DI 10.1016/j.nima.2011.12.111 PG 2 WC Instruments & Instrumentation; Nuclear Science & Technology; Physics, Nuclear; Physics, Particles & Fields SC Instruments & Instrumentation; Nuclear Science & Technology; Physics GA 020CJ UT WOS:000309786000058 ER PT J AU Aliu, E Archambault, S Arlen, T Aune, T Beilicke, M Benbow, W Bottcher, M Bouvier, A Buckley, JH Bugaev, V Cesarini, A Ciupik, L Collins-Hughes, E Connolly, MP Cui, W Dickherber, R Duke, C Dumm, J Errando, M Falcone, A Federici, S Feng, Q Finley, JP Finnegan, G Fortson, L Furniss, A Galante, N Gall, D Godambe, S Griffin, S Grube, J Gyuk, G Hanna, D Holder, J Huan, H Kaaret, P Karlsson, N Khassen, Y Kieda, D Krawczynski, H Krennrich, F Lee, K Madhavan, AS Maier, G Majumdar, P McArthur, S McCann, A Moriarty, P Mukherjee, R Nelson, T de Bhroithe, AO Ong, RA Orr, M Otte, AN Park, N Perkins, JS Pichel, A Pohl, M Prokoph, H Quinn, J Ragan, K Reyes, LC Reynolds, PT Roache, E Saxon, DB Sembroski, GH Staszak, D Telezhinsky, I Tesic, G Theiling, M Thibadeau, S Tsurusaki, K Varlotta, A Vassiliev, VV Vincent, S Vivier, M Wakely, SP Weekes, TC Weinstein, A Welsing, R Williams, DA Zitzer, B Fortin, P Horan, D Fumagalli, M Kaplan, K Prochaska, JX AF Aliu, E. Archambault, S. Arlen, T. Aune, T. Beilicke, M. Benbow, W. Boettcher, M. Bouvier, A. Buckley, J. H. Bugaev, V. Cesarini, A. Ciupik, L. Collins-Hughes, E. Connolly, M. P. Cui, W. Dickherber, R. Duke, C. Dumm, J. Errando, M. Falcone, A. Federici, S. Feng, Q. Finley, J. P. Finnegan, G. Fortson, L. Furniss, A. Galante, N. Gall, D. Godambe, S. Griffin, S. Grube, J. Gyuk, G. Hanna, D. Holder, J. Huan, H. Kaaret, P. Karlsson, N. Khassen, Y. Kieda, D. Krawczynski, H. Krennrich, F. Lee, K. Madhavan, A. S. Maier, G. Majumdar, P. McArthur, S. McCann, A. Moriarty, P. Mukherjee, R. Nelson, T. de Bhroithe, A. O'Faolain Ong, R. A. Orr, M. Otte, A. N. Park, N. Perkins, J. S. Pichel, A. Pohl, M. Prokoph, H. Quinn, J. Ragan, K. Reyes, L. C. Reynolds, P. T. Roache, E. Saxon, D. B. Sembroski, G. H. Staszak, D. Telezhinsky, I. Tesic, G. Theiling, M. Thibadeau, S. Tsurusaki, K. Varlotta, A. Vassiliev, V. V. Vincent, S. Vivier, M. Wakely, S. P. Weekes, T. C. Weinstein, A. Welsing, R. Williams, D. A. Zitzer, B. Fortin, P. Horan, D. Fumagalli, M. Kaplan, K. Prochaska, J. X. CA VERITAS Collaboration TI VERITAS OBSERVATIONS OF SIX BRIGHT, HARD-SPECTRUM FERMI-LAT BLAZARS SO ASTROPHYSICAL JOURNAL LA English DT Article DE BL Lacertae objects: general; gamma rays: galaxies ID EXTRAGALACTIC BACKGROUND LIGHT; BL-LACERTAE OBJECTS; ALL-SKY SURVEY; LARGE-AREA TELESCOPE; ACTIVE GALACTIC NUCLEI; ENERGY GAMMA-RAYS; MULTIWAVELENGTH OBSERVATIONS; RELATIVISTIC JET; COMPLETE SAMPLE; SOURCE CATALOG AB We report on VERITAS very high energy (VHE; E >= 100 GeV) observations of six blazars selected from the Fermi Large Area Telescope First Source Catalog (1FGL). The gamma-ray emission from 1FGL sources was extrapolated up to the VHE band, taking gamma-ray absorption by the extragalactic background light into account. This allowed the selection of six bright, hard-spectrum blazars that were good candidate TeV emitters. Spectroscopic redshift measurements were attempted with the Keck Telescope for the targets without Sloan Digital Sky Survey spectroscopic data. No VHE emission is detected during the observations of the six sources described here. Corresponding TeV upper limits are presented, along with contemporaneous Fermi observations and non-concurrent Swift UVOT and X-Ray Telescope data. The blazar broadband spectral energy distributions (SEDs) are assembled and modeled with a single-zone synchrotron self-Compton model. The SED built for each of the six blazars shows a synchrotron peak bordering between the intermediate-and high-spectrum-peak classifications, with four of the six resulting in particle-dominated emission regions. C1 [Aune, T.; Bouvier, A.; Furniss, A.; Williams, D. A.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA. [Aune, T.; Bouvier, A.; Furniss, A.; Williams, D. A.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA. [Aliu, E.; Errando, M.; Mukherjee, R.] Columbia Univ, Dept Phys & Astron, Barnard Coll, New York, NY 10027 USA. [Archambault, S.; Griffin, S.; Hanna, D.; Ragan, K.; Staszak, D.; Tesic, G.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Arlen, T.; Majumdar, P.; Ong, R. A.; Vassiliev, V. V.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Beilicke, M.; Buckley, J. H.; Bugaev, V.; Dickherber, R.; Krawczynski, H.; Lee, K.; McArthur, S.; Thibadeau, S.] Washington Univ, Dept Phys, St Louis, MO 63130 USA. [Benbow, W.; Galante, N.; Roache, E.; Weekes, T. C.; Fortin, P.] Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA. [Boettcher, M.] Ohio Univ, Dept Phys & Astron, Inst Astrophys, Athens, OH 45701 USA. [Cesarini, A.; Connolly, M. P.] Natl Univ Ireland Galway, Sch Phys, Galway, Ireland. [Ciupik, L.; Grube, J.; Gyuk, G.] Adler Planetarium & Astron Museum, Dept Astron, Chicago, IL 60605 USA. [Collins-Hughes, E.; Khassen, Y.; de Bhroithe, A. O'Faolain; Quinn, J.] Natl Univ Ireland Univ Coll Dublin, Sch Phys, Dublin 4, Ireland. [Cui, W.; Feng, Q.; Finley, J. P.; Sembroski, G. H.; Theiling, M.; Varlotta, A.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. [Duke, C.] Grinnell Coll, Dept Phys, Grinnell, IA 50112 USA. [Dumm, J.; Fortson, L.; Karlsson, N.; Nelson, T.] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA. [Falcone, A.] Penn State Univ, Davey Lab 525, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Federici, S.; Maier, G.; Pohl, M.; Prokoph, H.; Telezhinsky, I.; Vincent, S.; Welsing, R.] DESY, D-15738 Zeuthen, Germany. [Federici, S.; Pohl, M.; Telezhinsky, I.] Univ Potsdam, Inst Phys & Astron, D-14476 Potsdam, Germany. [Finnegan, G.; Godambe, S.; Kieda, D.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA. [Gall, D.; Kaaret, P.; Tsurusaki, K.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. [Holder, J.; Saxon, D. B.; Vivier, M.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA. [Holder, J.; Saxon, D. B.; Vivier, M.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA. [Huan, H.; Park, N.; Wakely, S. P.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [Krennrich, F.; Madhavan, A. S.; Orr, M.; Weinstein, A.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. [McCann, A.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Moriarty, P.] Galway Mayo Inst Technol, Dept Life & Phys Sci, Galway, Ireland. [Otte, A. N.] Georgia Inst Technol, Sch Phys, Atlanta, GA 30332 USA. [Otte, A. N.] Georgia Inst Technol, Ctr Relativist Astrophys, Atlanta, GA 30332 USA. [Perkins, J. S.] CRESST, Greenbelt, MD 20771 USA. [Perkins, J. S.] NASA, Astroparticle Phys Lab, GSFC, Greenbelt, MD 20771 USA. [Perkins, J. S.] Univ Maryland Baltimore Cty, Baltimore, MD 21250 USA. [Pichel, A.] Inst Astron & Fis Espacio, RA-1428 Buenos Aires, DF, Argentina. [Reyes, L. C.] Calif Polytech State Univ San Luis Obispo, Dept Phys, San Luis Obispo, CA 94307 USA. [Reynolds, P. T.] Cork Inst Technol, Dept Appl Phys & Instrumentat, Cork, Ireland. [Zitzer, B.] Argonne Natl Lab, Argonne, IL 60439 USA. [Horan, D.] Ecole Polytech, CNRS, IN2P3, Lab Leprince Ringuet, F-91128 Palaiseau, France. [Prochaska, J. X.] Univ Calif Santa Cruz, Dept Astron & Astrophys, UCO Lick Observ, Santa Cruz, CA 95064 USA. [Boettcher, M.] North West Univ, Ctr Space Res, ZA-2531 Potchefstroom, South Africa. RP Furniss, A (reprint author), Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA. EM afurniss@ucsc.edu; pafortin@cfa.harvard.edu; deirdre@llr.in2p3.fr RI Khassen, Yerbol/I-3806-2015; Fumagalli, Michele/K-9510-2015; OI Khassen, Yerbol/0000-0002-7296-3100; Fumagalli, Michele/0000-0001-6676-3842; Cui, Wei/0000-0002-6324-5772; Cesarini, Andrea/0000-0002-8611-8610 FU U.S. Department of Energy Office of Science; U.S. National Science Foundation; Smithsonian Institution; NSERC in Canada; Science Foundation Ireland [SFI 10/RFP/AST2748]; STFC in the U.K; NSF [AST-0548180]; Alfred P. Sloan Foundation; U.S. Department of Energy; National Aeronautics and Space Administration; Japanese Monbukagakusho; Max Planck Society; Higher Education Funding Council for England; Istituto Nazionale di Astrofisica in Italy; Centre National d'Etudes Spatiales in France FX This research is supported by grants from the U.S. Department of Energy Office of Science, the U.S. National Science Foundation, and the Smithsonian Institution, by NSERC in Canada, by Science Foundation Ireland (SFI 10/RFP/AST2748), and by STFC in the U.K. We acknowledge the excellent work of the technical support staff at the Fred Lawrence Whipple Observatory and at the collaborating institutions in the construction and operation of the instrument. The Fermi-LAT Collaboration acknowledges generous support from a number of agencies and institutes that have supported 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 acknowledged from the Istituto Nazionale di Astrofisica in Italy and the Centre National d'Etudes Spatiales in France. J.X.P. acknowledges funding through an NSF CAREER grant (AST-0548180). Funding for the SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, the U.S. Department of Energy, the National Aeronautics and Space Administration, the Japanese Monbukagakusho, the Max Planck Society, and the Higher Education Funding Council for England. The SDSS Web site is http://www.sdss.org/. 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. NR 91 TC 2 Z9 2 U1 1 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD NOV 10 PY 2012 VL 759 IS 2 AR 102 DI 10.1088/0004-637X/759/2/102 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 034ZL UT WOS:000310911300025 ER PT J AU Hewitt, JW Grondin, MH Lemoine-Goumard, M Reposeur, T Ballet, J Tanaka, T AF Hewitt, J. W. Grondin, M. -H. Lemoine-Goumard, M. Reposeur, T. Ballet, J. Tanaka, T. TI FERMI-LAT AND WMAP OBSERVATIONS OF THE PUPPIS A SUPERNOVA REMNANT SO ASTROPHYSICAL JOURNAL LA English DT Article DE acceleration of particles; cosmic rays; ISM: individual objects (Puppis A); radiation mechanisms: non-thermal ID LARGE-AREA TELESCOPE; GAMMA-RAY EMISSION; MOLECULAR CLOUDS; NEUTRAL HYDROGEN; VLA OBSERVATIONS; EMITTING EJECTA; DISCOVERY; PULSAR; CASSIOPEIA; DIRECTION AB We report the detection of GeV gamma-ray emission from the supernova remnant (SNR) Puppis A with the Fermi Gamma-Ray Space Telescope. Puppis A is among the faintest SNRs yet detected at GeV energies, with a luminosity of only 2.7 x 10(34) (D/2.2 kpc)(2) erg s(-1) between 1 and 100 GeV. The gamma-ray emission from the remnant is spatially extended, with a morphology matching that of the radio and X-ray emission, and is well described by a simple power law with an index of 2.1. We attempt to model the broadband spectral energy distribution (SED), from radio to gamma-rays, using standard nonthermal emission mechanisms. To constrain the relativistic electron population we use 7 years of Wilkinson Microwave Anisotropy Probe data to extend the radio spectrum up to 93 GHz. Both leptonic- and hadronic-dominated models can reproduce the nonthermal SED, requiring a total content of cosmic-ray electrons and protons accelerated in Puppis A of at least W-CR approximate to (1-5) x 10(49) erg. C1 [Hewitt, J. W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Grondin, M. -H.] Max Planck Inst Kernphys, D-69029 Heidelberg, Germany. [Grondin, M. -H.] Univ Heidelberg, Landessternwarte, D-69117 Heidelberg, Germany. [Lemoine-Goumard, M.; Reposeur, T.] Univ Bordeaux 1, CNRS, IN2P3, Ctr Etud Nucl Bordeaux Gradignan, F-33175 Gradignan, France. [Ballet, J.] Univ Paris Diderot, CEA Saclay, Serv Astrophys, Lab AIM,CEA IRFU,CNRS, F-91191 Gif Sur Yvette, France. [Tanaka, T.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, WW Hansen Expt Phys Lab, Dept Phys, Stanford, CA 94305 USA. [Tanaka, T.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA. RP Hewitt, JW (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM john.w.hewitt@nasa.gov; marie-helene.grondin@mpi-hd.mpg.de; lemoine@cenbg.in2p3.fr FU Istituto Nazionale di Astrofisica in Italy; Centre National d' Etudes Spatiales in France; Commonwealth Government; Science Mission Directorate Office at NASA Headquarters; NASA Postdoctoral Program at the Goddard Space Flight Center; NASA; Fermi Guest Investigator Program; Alexander von Humboldt Foundation; European Community [ERC-StG-259391] FX 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.; The Parkes radio telescope is part of the Australia Telescope which is funded by the Commonwealth Government for operation as a National Facility managed by CSIRO. We thank our colleagues for their assistance with the radio timing observations.; The WMAP mission is made possible by the support of the Science Mission Directorate Office at NASA Headquarters. This research has made use of NASA's Astrophysics Data System Bibliographic Services, and data obtained from the High Energy Astrophysics Science Archive Research Center (HEASARC), provided by NASA's Goddard Space Flight Center. We thank Nils Odegard for assisting us with analysis of WMAP data, and Gloria Dubner for providing us with the 1.4 GHz radio image of Puppis A. J.W.H. acknowledges support 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, and also by a grant from the Fermi Guest Investigator Program. M.H.G. acknowledges support from the Alexander von Humboldt Foundation. M.L.G. acknowledges funding by contract ERC-StG-259391 from the European Community. NR 46 TC 19 Z9 19 U1 0 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD NOV 10 PY 2012 VL 759 IS 2 AR 89 DI 10.1088/0004-637X/759/2/89 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 034ZL UT WOS:000310911300012 ER PT J AU Jenke, PA Finger, MH Wilson-Hodge, CA Camero-Arranz, A AF Jenke, P. A. Finger, M. H. Wilson-Hodge, C. A. Camero-Arranz, A. TI ORBITAL DECAY AND EVIDENCE OF DISK FORMATION IN THE X-RAY BINARY PULSAR OAO 1657-415 SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; pulsars: individual (OAO 1657-415); stars: neutron; stars: winds, outflows; X-rays: binaries ID NEUTRON STAR STRUCTURE; ACCRETION TORQUES; BURST MONITOR; OAO-1657-415; OAO1657-415; EVOLUTION; COMPANION AB OAO 1657-415 is an eclipsing X-ray binary wind-fed pulsar that has exhibited smooth spin-up/spin-down episodes and has undergone several torque reversals throughout its long history of observation. We present a frequency history spanning nearly 19 years of observations from the Burst and Transient Source Experiment and from the Gamma-Ray Burst Monitor (Fermi/GBM). Our analysis suggests two modes of accretion: one resulting in steady spin-up correlated with flux during which we believe a stable accretion disk is present and one in which the neutron star is spinning down at a lesser rate which is uncorrelated with flux. Orbital elements of the pulsar system are determined at several intervals throughout this history. With these ephemerides, statistically significant orbital decay with a P-orb = (-9.74 +/- 0.78) x 10(-8) is established. C1 [Jenke, P. A.] MSFC NPP, Huntsville, AL 35812 USA. [Finger, M. H.] Univ Space Res Assoc, Huntsville, AL 35806 USA. [Wilson-Hodge, C. A.] NASA, George C Marshall Space Flight Ctr, Space Sci Off, Huntsville, AL 35812 USA. [Camero-Arranz, A.] Fac Ciencies, Inst Ciencies Espai CSIC IEEC, E-08193 Barcelona, Spain. RP Jenke, PA (reprint author), MSFC NPP, Huntsville, AL 35812 USA. FU NASA [NNX08AW06G, NNX11AE24G]; NASA Postdoctoral Program at the Marshall Space Flight Center; Fermi Guest Investigator program; Astrophysics Data Analysis Program (ADAP) FX We acknowledge Slawomir Suchy for the use of his results from his observations of OAO 1657-415 by RXTE. M.F. and A.C. acknowledge support from NASA grants NNX08AW06G and NNX11AE24G. P. Jenke was supported by an appointment to the NASA Postdoctoral Program at the Marshall Space Flight Center, administered by Oak Ridge Associated Universities through a contract with NASA. This work was supported by the Fermi Guest Investigator program and by the Astrophysics Data Analysis Program (ADAP). NR 30 TC 10 Z9 10 U1 0 U2 8 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD NOV 10 PY 2012 VL 759 IS 2 AR 124 DI 10.1088/0004-637X/759/2/124 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 034ZL UT WOS:000310911300047 ER PT J AU Monson, AJ Freedman, WL Madore, BF Persson, SE Scowcroft, V Seibert, M Rigby, JR AF Monson, Andrew J. Freedman, Wendy L. Madore, Barry F. Persson, S. E. Scowcroft, Victoria Seibert, Mark Rigby, Jane R. TI THE CARNEGIE HUBBLE PROGRAM: THE LEAVITT LAW AT 3.6 AND 4.5 mu m IN THE MILKY WAY SO ASTROPHYSICAL JOURNAL LA English DT Article DE infrared: stars; stars: variables: Cepheids ID CEPHEID PERIOD-LUMINOSITY; LARGE-MAGELLANIC-CLOUD; SPITZER-SPACE-TELESCOPE; INFRARED ARRAY CAMERA; CLASSICAL CEPHEIDS; GALACTIC CEPHEIDS; TRIGONOMETRIC PARALLAXES; INTERSTELLAR EXTINCTION; SUPERNOVA PROJECT; COLOR RELATIONS AB The Carnegie Hubble Program (CHP) is designed to calibrate the extragalactic distance scale using data from the post-cryogenic era of the Spitzer Space Telescope. The ultimate goal of the CHP is a systematic improvement in the distance scale leading to a determination of the Hubble constant to within an accuracy of 2%. This paper focuses on the measurement and calibration of the Galactic Cepheid period-luminosity (PL, Leavitt) relation using the warm Spitzer/IRAC 1 and 2 bands at 3.6 and 4.5 mu m. We present photometric measurements covering the period range 4-70 days for 37 Galactic Cepheids. Data at 24 phase points were collected for each star. Three PL relations of the form M = a(log(P)- 1)+b are derived. The method adopted here takes the slope a to be -3.31, as determined from the Spitzer Large Magellanic Cloud (LMC) data of Scowcroft et al. Using the geometric Hubble Space Telescope guide-star distances to 10 Galactic Cepheids, we find a calibrated 3.6 mu m PL zero point of -5.80 +/- 0.03. Together with our value for the LMC zero point, we determine a reddening-corrected distance modulus of 18.48 +/- 0.04 mag to the LMC. The mid-IR period-color diagram and the [3.6]-[4.5] color variation with phase are interpreted in terms of CO absorption at 4.5 mu m. This situation compromises the use of the 4.5 mu m data for distance determinations. C1 [Monson, Andrew J.; Freedman, Wendy L.; Madore, Barry F.; Persson, S. E.; Scowcroft, Victoria; Seibert, Mark] Observ Carnegie Inst Washington, Pasadena, CA 91101 USA. [Rigby, Jane R.] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA. RP Monson, AJ (reprint author), Observ Carnegie Inst Washington, 813 Santa Barbara St, Pasadena, CA 91101 USA. EM amonson@obs.carnegiescience.edu; wendy@obs.carnegiescience.edu; barry@obs.carnegiescience.edu; persson@obs.carnegiescience.edu; vs@obs.carnegiescience.edu; mseibert@obs.carnegiescience.edu; Jane.R.Rigby@nasa.gov RI Rigby, Jane/D-4588-2012 OI Rigby, Jane/0000-0002-7627-6551 FU Jet Propulsion Laboratory, California Institute of Technology; NASA FX We thank the staff of the Spitzer Science Center for their assistance with scheduling such a large and complex project as well as the support received to make these analyses. This work is based (in part) on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech. We also thank the anonymous referee for constructive comments regarding the form and content of this work. NR 51 TC 32 Z9 32 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD NOV 10 PY 2012 VL 759 IS 2 AR 146 DI 10.1088/0004-637X/759/2/146 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 034ZL UT WOS:000310911300069 ER PT J AU Nakauchi, D Suwa, Y Sakamoto, T Kashiyama, K Nakamura, T AF Nakauchi, Daisuke Suwa, Yudai Sakamoto, Takanori Kashiyama, Kazumi Nakamura, Takashi TI LONG-DURATION X-RAY FLASH AND X-RAY-RICH GAMMA-RAY BURSTS FROM LOW-MASS POPULATION III STARS SO ASTROPHYSICAL JOURNAL LA English DT Article DE early universe; gamma rays: general; stars: Population III ID 1ST STARS; LUMINOSITY RELATION; EVOLUTION; JETS; CONSTRAINTS; SUPERNOVAE; COLLAPSARS; ACCRETION; REDSHIFT; TRANSIENTS AB Recent numerical simulations suggest that Population III (Pop III) stars were born with masses not larger than similar to 100 M-circle dot and typically similar to 40 M-circle dot. By self-consistently considering the jet generation and propagation in the envelope of these low-mass Pop III stars, we find that a Pop III blue supergiant star has the possibility of giving rise to a gamma-ray burst (GRB) even though it keeps a massive hydrogen envelope. We evaluate observational characteristics of Pop III GRBs and predict that Pop III GRBs have a duration of similar to 10(5) s in the observer frame and a peak luminosity of similar to 5 x 10(50) erg s(-1). Assuming that the E-p-L-p (or E-p-E-gamma,E-iso) correlation holds for Pop III GRBs, we find that the spectrum peak energy falls at approximately a few keV (or similar to 100 keV) in the observer frame. We discuss the detectability of Pop III GRBs by future satellite missions such as EXIST and Lobster. If the E-p-E-gamma,E-iso correlation holds, we have the possibility to detect Pop III GRBs at z similar to 9 as long-duration X-ray-rich GRBs by EXIST. Conversely, if the E-p-L-p correlation holds, we have the possibility to detect Pop III GRBs up to z similar to 19 as long-duration X-ray flashes by Lobster. C1 [Nakauchi, Daisuke; Kashiyama, Kazumi; Nakamura, Takashi] Kyoto Univ, Dept Phys, Sakyo Ku, Kyoto 6068502, Japan. [Suwa, Yudai] Kyoto Univ, Yukawa Inst Theoret Phys, Sakyo Ku, Kyoto 6068502, Japan. [Sakamoto, Takanori] NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA. [Sakamoto, Takanori] Univ Maryland, Joint Ctr Astrophys, Baltimore, MD 21250 USA. [Kashiyama, Kazumi] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. RP Nakauchi, D (reprint author), Kyoto Univ, Dept Phys, Sakyo Ku, Oiwake Cho, Kyoto 6068502, Japan. RI Suwa, Yudai/G-9711-2012 FU Ministry of Education, Culture, Sports, Science and Technology (MEXT) of Japan [23540305, 24103006, 23840023]; Universality and Emergence at Kyoto University FX We thank A. Heger for kindly providing us his stellar model data. We thank D. Yonetoku and R. Yamazaki for fruitful discussion and suggestions about GRB observations. We also thank K. Omukai for fruitful discussions about Population III stars and the anonymous referee for fruitful comments. This work is supported in part by the Grant-in-Aid from the Ministry of Education, Culture, Sports, Science and Technology (MEXT) of Japan, Nos. 23540305 (T.N.), 24103006 (T.N.), 23840023 (Y.S.) and by the Grant-in-Aid for the global COE program The Next Generation of Physics, Spun from Universality and Emergence at Kyoto University. NR 43 TC 22 Z9 22 U1 1 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD NOV 10 PY 2012 VL 759 IS 2 AR 128 DI 10.1088/0004-637X/759/2/128 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 034ZL UT WOS:000310911300051 ER PT J AU Peacock, MB Zepf, SE Kundu, A Maccarone, TJ Rhode, KL Salzer, JJ Waters, CZ Ciardullo, R Gronwall, C Stern, D AF Peacock, Mark B. Zepf, Stephen E. Kundu, Arunav Maccarone, Thomas J. Rhode, Katherine L. Salzer, John J. Waters, Christopher Z. Ciardullo, Robin Gronwall, Caryl Stern, Daniel TI SPATIALLY RESOLVED SPECTROSCOPY OF THE GLOBULAR CLUSTER RZ 2109 AND THE NATURE OF ITS BLACK HOLE SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: individual (NGC 4472); galaxies: star clusters: general; galaxies: star clusters: individual: RZ 2109; globular clusters: general; X-rays: binaries; X-rays: galaxies: clusters ID X-RAY BINARIES; HUBBLE-SPACE-TELESCOPE; EARLY-TYPE GALAXIES; LUMINOUS O III; ELLIPTIC GALAXIES; STAR-CLUSTERS; NGC 4472; N II; MASS; EMISSION AB We present optical Hubble Space Telescope/Space Telescope Imaging Spectrograph (HST/STIS) spectroscopy of RZ 2109, a globular cluster (GC) in the elliptical galaxy NGC 4472. This GC is notable for hosting an ultraluminous X-ray source as well as associated strong and broad [O III] lambda lambda 4959, 5007 emission. We show that the HST/STIS spectroscopy spatially resolves the [O III] emission in RZ 2109. While we are unable to make a precise determination of the morphology of the emission-line nebula, the best-fitting models all require that the [O III] lambda 5007 emission has a half-light radius in the range 3-7 pc. The extended nature of the [O III] lambda 5007 emission is inconsistent with published models that invoke an intermediate-mass black hole origin. It is also inconsistent with the ionization of ejecta from a nova in the cluster. The spatial scale of the nebula could be produced via the photoionization of a strong wind driven from a stellar mass black hole accreting at roughly its Eddington rate. C1 [Peacock, Mark B.; Zepf, Stephen E.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. [Kundu, Arunav] Eureka Sci Inc, Oakland, CA 94602 USA. [Maccarone, Thomas J.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Rhode, Katherine L.; Salzer, John J.] Indiana Univ, Dept Astron, Bloomington, IN 47405 USA. [Waters, Christopher Z.] Univ Hawaii Manoa, Inst Astron, Honolulu, HI 96822 USA. [Ciardullo, Robin; Gronwall, Caryl] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Ciardullo, Robin; Gronwall, Caryl] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA. [Stern, Daniel] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Peacock, MB (reprint author), Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. EM mpeacock@msu.edu FU NASA from the Space Telescope Science Institute [HST-GO-11703, HST-GO-11029]; AURA, Inc., under NASA [NAS 5-26555]; NASA through Chandra [GO1-12112X, GO0-11111A]; NASA [NAS8-03060]; NSF Faculty Early Career Development (CAREER) award [AST-0847109] FX We thank the anonymous referee for considering this paper and for helpful comments. We are grateful for the assistance of the HST STIS helpdesk team, who provided very useful answers and suggestions in relation to the analysis of these data. Support for this work was provided by NASA through grant numbers HST-GO-11703 (M.B.P. and S.E.Z.) and HST-GO-11029 (S.E.Z. and C.Z.W.) from the Space Telescope Science Institute, which is operated by AURA, Inc., under NASA contract NAS 5-26555. Support for A.K.'s work was provided by NASA through Chandra grant Numbers GO1-12112X and GO0-11111A issued by the Chandra X-ray Observatory Center, which is operated by the SAO for and on behalf of the NASA under contract NAS8-03060. K.L.R. is supported by an NSF Faculty Early Career Development (CAREER) award (AST-0847109). The work of D.S. was carried out at Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA.; STScI is operated by the Association of Universities for Research in Astronomy, Inc. under NASA contract NAS 5-26555. NR 40 TC 4 Z9 4 U1 0 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD NOV 10 PY 2012 VL 759 IS 2 AR 126 DI 10.1088/0004-637X/759/2/126 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 034ZL UT WOS:000310911300049 ER PT J AU Savani, NP Shiota, D Kusano, K Vourlidas, A Lugaz, N AF Savani, N. P. Shiota, D. Kusano, K. Vourlidas, A. Lugaz, N. TI A STUDY OF THE HELIOCENTRIC DEPENDENCE OF SHOCK STANDOFF DISTANCE AND GEOMETRY USING 2.5D MAGNETOHYDRODYNAMIC SIMULATIONS OF CORONAL MASS EJECTION DRIVEN SHOCKS SO ASTROPHYSICAL JOURNAL LA English DT Article DE magnetohydrodynamics (MHD); solar-terrestrial relations; Sun: coronal mass ejections (CMEs); Sun: heliosphere ID MAGNETIC-FIELD; SOLAR-WIND; FLUX ROPE; LASCO OBSERVATIONS; TRIGGER MECHANISM; STEREO MISSION; IMAGER SMEI; BOW SHOCKS; 1 AU; EVOLUTION AB We perform four numerical magnetohydrodynamic simulations in 2.5 dimensions ( 2.5D) of fast coronal mass ejections (CMEs) and their associated shock fronts between 10 Rs and 300 Rs. We investigate the relative change in the shock standoff distance, Delta, as a fraction of the CME radial half-width, D-OB (i.e., Delta/D-OB). Previous hydrodynamic studies have related the shock standoff distance for Earth's magnetosphere to the density compression ratio (DR; rho(u)/rho(d)) measured across the bow shock. The DR coefficient, k(dr), which is the proportionality constant between the relative standoff distance (Delta/D-OB) and the compression ratio, was semi-empirically estimated as 1.1. For CMEs, we show that this value varies linearly as a function of heliocentric distance and changes significantly for different radii of curvature of the CME's leading edge. We find that a value of 0.8 +/- 0.1 is more appropriate for small heliocentric distances (<30 Rs) which corresponds to the spherical geometry of a magnetosphere presented by Seiff. As the CME propagates its cross section becomes more oblate and the k(dr) value increases linearly with heliocentric distance, such that k(dr) = 1.1 is most appropriate at a heliocentric distance of about 80 Rs. For terrestrial distances (215 Rs) we estimate k(dr) = 1.8 +/- 0.3, which also indicates that the CME cross-sectional structure is generally more oblate than that of Earth's magnetosphere. These alterations to the proportionality coefficients may serve to improve investigations into the estimates of the magnetic field in the corona upstream of a CME as well as the aspect ratio of CMEs as measured in situ. C1 [Savani, N. P.] UCAR, Boulder, CO 80307 USA. [Savani, N. P.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Shiota, D.] RIKEN, Computat Astrophys Lab, Adv Sci Inst, Wako, Saitama 3510198, Japan. [Kusano, K.] Nagoya Univ, Solar Terr Environm Lab, Nagoya, Aichi 4648601, Japan. [Kusano, K.] Japan Agcy Marine Earth Sci & Technol, Yokohama, Kanagawa 2360001, Japan. [Vourlidas, A.] USN, Res Lab, Div Space Sci, Washington, DC 20375 USA. [Lugaz, N.] Univ New Hampshire, Expt Space Plasma Grp, Durham, NH 03824 USA. RP Savani, NP (reprint author), UCAR, Boulder, CO 80307 USA. EM neel.savani02@imperial.ac.uk RI Lugaz, Noe/C-1284-2008; Savani, Neel/G-4066-2014; Vourlidas, Angelos/C-8231-2009; OI Lugaz, Noe/0000-0002-1890-6156; Savani, Neel/0000-0002-1916-7877; Vourlidas, Angelos/0000-0002-8164-5948; Shiota, Daikou/0000-0002-9032-8792 FU NASA Living With a Star Jack Eddy Postdoctoral Fellowship Program; NASA; office of Naval Research; JSPS fellowship at Nagoya University FX N.P.S. was supported by the NASA Living With a Star Jack Eddy Postdoctoral Fellowship Program, administered by the UCAR Visiting Scientist Programs and hosted by the Naval Research Laboratory. N.P.S. and A.V. were supported by NASA and the office of Naval Research. The numerical calculations were made using the supercomputing cluster at the Solar-Terrestrial Environment Laboratory, Nagoya University. This work of N.P.S. was in part performed during a JSPS fellowship at Nagoya University. NR 75 TC 9 Z9 9 U1 0 U2 14 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD NOV 10 PY 2012 VL 759 IS 2 AR 103 DI 10.1088/0004-637X/759/2/103 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 034ZL UT WOS:000310911300026 ER PT J AU Stevenson, R Kramer, EA Bauer, JM Masiero, JR Mainzer, AK AF Stevenson, R. Kramer, E. A. Bauer, J. M. Masiero, J. R. Mainzer, A. K. TI CHARACTERIZATION OF ACTIVE MAIN BELT OBJECT P/2012 F5 (GIBBS): A POSSIBLE IMPACTED ASTEROID SO ASTROPHYSICAL JOURNAL LA English DT Article DE comets: individual (P/2012 F5 (Gibbs)); minor planets, asteroids: individual (P/2012 F5) ID INFRARED-SURVEY-EXPLORER; NEAR-EARTH ASTEROIDS; R2 LA SAGRA; 596 SCHEILA; THERMAL-MODEL; PHYSICAL-PROPERTIES; SOLAR-SYSTEM; 1999 KW4; COMET; 133P/ELST-PIZARRO AB In this work, we characterize the recently discovered active main belt object P/2012 F5 (Gibbs), which was discovered with a dust trail > 7' in length in the outer main belt, 7 months prior to aphelion. We use optical imaging obtained on UT 2012 March 27 to analyze the central condensation and the long trail. We find B-band and R-band apparent magnitudes of 20.96 +/- 0.04 mag and 19.93 +/- 0.02 mag, respectively, which give an upper limit on the radius of the nucleus of 2.1 km. The geometric scattering cross-section of material in the trail was similar to 4 x 10(8) m(2), corresponding to a mass of similar to 5 x 10(7) kg. Analysis of infrared images taken by the Wide-field Infrared Survey Explorer in 2010 September reveals that the object was below the detection limit, suggesting that it was less active than it was during 2012, or possibly inactive, just six months after it passed through perihelion. We set a 1 sigma upper limit on its radius during this time of 2.9 km. P/2012 F5 (Gibbs) is dynamically stable in the outer main belt on timescales of similar to 1 Gyr, pointing toward an asteroidal origin. We find that the morphology of the ejected dust is consistent with it being produced by a single event that occurred on UT 2011 July 7 +/- 20 days, possibly as the result of a collision with a small impactor. C1 [Stevenson, R.; Kramer, E. A.; Bauer, J. M.; Masiero, J. R.; Mainzer, A. K.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Kramer, E. A.] Univ Cent Florida, Dept Phys, Orlando, FL 32816 USA. RP Stevenson, R (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Rachel.A.Stevenson@jpl.nasa.gov OI Masiero, Joseph/0000-0003-2638-720X FU National Aeronautics and Space Administration; NASA Postdoctoral Fellowship Program; JPL Graduate Fellowship Program; NASA through the Near Earth Object observing programs; JPL Office of the Chief Information Officer FX This publication makes use of data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration. This work was based on observations obtained at the Hale Telescope, Palomar Observatory as part of a continuing collaboration between the California Institute of Technology, NASA/JPL, and Cornell University. The authors thank Henry Hsieh for bringing the discovery of P/2012 F5 to their attention. They also thank Kevin Rykoski, Carolyn Heffner, and Jean Mueller for assistance with the observations at Palomar Observatory. R.S. and J.M. acknowledge support from the NASA Postdoctoral Fellowship Program. E.K. was supported by the JPL Graduate Fellowship Program. This research was funded in part by a grant from NASA through the Near Earth Object observing programs, for the NEOWISE project. The supercomputer used in this investigation was provided by funding from the JPL Office of the Chief Information Officer. NR 53 TC 19 Z9 19 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD NOV 10 PY 2012 VL 759 IS 2 AR 142 DI 10.1088/0004-637X/759/2/142 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 034ZL UT WOS:000310911300065 ER PT J AU Tian, H McIntosh, SW Wang, TJ Ofman, L De Pontieu, B Innes, DE Peter, H AF Tian, Hui McIntosh, Scott W. Wang, Tongjiang Ofman, Leon De Pontieu, Bart Innes, Davina E. Peter, Hardi TI PERSISTENT DOPPLER SHIFT OSCILLATIONS OBSERVED WITH HINODE/EIS IN THE SOLAR CORONA: SPECTROSCOPIC SIGNATURES OF ALFVENIC WAVES AND RECURRING UPFLOWS SO ASTROPHYSICAL JOURNAL LA English DT Article DE line: profiles; solar wind; Sun: corona; Sun: oscillations; waves ID SLOW MAGNETOACOUSTIC WAVES; ACTIVE-REGION LOOPS; EUV IMAGING SPECTROMETER; TRANSITION-REGION; TRANSVERSE OSCILLATIONS; PROPAGATING WAVES; MAGNETIC-FIELD; KINK WAVES; INTENSITY OSCILLATIONS; EMISSION-LINES AB Using data obtained by the EUV Imaging Spectrometer on board Hinode, we have performed a survey of obvious and persistent (without significant damping) Doppler shift oscillations in the corona. We have found mainly two types of oscillations from February to April in 2007. One type is found at loop footpoint regions, with a dominant period around 10 minutes. They are characterized by coherent behavior of all line parameters (line intensity, Doppler shift, line width, and profile asymmetry), and apparent blueshift and blueward asymmetry throughout almost the entire duration. Such oscillations are likely to be signatures of quasi-periodic upflows (small-scale jets, or coronal counterpart of type-II spicules), which may play an important role in the supply of mass and energy to the hot corona. The other type of oscillation is usually associated with the upper part of loops. They are most clearly seen in the Doppler shift of coronal lines with formation temperatures between one and two million degrees. The global wavelets of these oscillations usually peak sharply around a period in the range of three to six minutes. No obvious profile asymmetry is found and the variation of the line width is typically very small. The intensity variation is often less than 2%. These oscillations are more likely to be signatures of kink/Alfven waves rather than flows. In a few cases, there seems to be a pi/2 phase shift between the intensity and Doppler shift oscillations, which may suggest the presence of slow-mode standing waves according to wave theories. However, we demonstrate that such a phase shift could also be produced by loops moving into and out of a spatial pixel as a result of Alfvenic oscillations. In this scenario, the intensity oscillations associated with Alfvenic waves are caused by loop displacement rather than density change. These coronal waves may be used to investigate properties of the coronal plasma and magnetic field. C1 [Tian, Hui; McIntosh, Scott W.] Natl Ctr Atmospher Res, High Altitude Observ, Boulder, CO 80307 USA. [Wang, Tongjiang; Ofman, Leon] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA. [Wang, Tongjiang; Ofman, Leon] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [De Pontieu, Bart] Lockheed Martin Solar & Astrophys Lab, Org ADBS, Palo Alto, CA 94304 USA. [Innes, Davina E.; Peter, Hardi] Max Planck Inst Solar Syst Res, D-37191 Katlenburg Lindau, Germany. RP Tian, H (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM htian@ucar.edu FU NASA [NNX08AL22G, NNX08BA99G, NNX10AN10G, NNX12AB34G]; NSF [ATM-0541567, ATM-0925177]; ASP Postdoctoral Fellowship Program of National Center for Atmospheric Research; National Science Foundation FX EIS is an instrument on board Hinode, a Japanese mission developed and launched by ISAS/JAXA, with NAOJ as domestic partner and NASA and STFC (UK) as international partners. It is operated by these agencies in cooperation with ESA and NSC (Norway). S. W. McIntosh is supported by NASA (NNX08AL22G and NNX08BA99G) and NSF (ATM-0541567, ATM-0925177). T. Wang and L. Ofman acknowledge supports by NASA grants NNX10AN10G and NNX12AB34G. H. Tian is supported by the ASP Postdoctoral Fellowship Program of National Center for Atmospheric Research, which is sponsored by the National Science Foundation. H. Tian thanks I. De Moortel, G. R. Gupta, and L. Teriaca for helpful discussions. NR 188 TC 36 Z9 36 U1 12 U2 29 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD NOV 10 PY 2012 VL 759 IS 2 AR 144 DI 10.1088/0004-637X/759/2/144 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 034ZL UT WOS:000310911300067 ER PT J AU Warren, HP Winebarger, AR Brooks, DH AF Warren, Harry P. Winebarger, Amy R. Brooks, David H. TI A SYSTEMATIC SURVEY OF HIGH-TEMPERATURE EMISSION IN SOLAR ACTIVE REGIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun: corona ID ULTRAVIOLET IMAGING SPECTROMETER; TRANSITION-REGION; ATOMIC DATA; X-RAY; FUNDAMENTAL LIMITATIONS; PLASMA TEMPERATURE; HINODE EIS; HOT PLASMA; FE-XVIII; CORONA AB The recent analysis of observations taken with the EUV Imaging Spectrometer and X-Ray Telescope instruments on Hinode suggests that well-constrained measurements of the temperature distribution in solar active regions can finally be made. Such measurements are critical for constraining theories of coronal heating. Past analysis, however, has suffered from limited sample sizes and large uncertainties at temperatures between 5 and 10 MK. Here we present a systematic study of the differential emission measure distribution in 15 active region cores. We focus on measurements in the "inter-moss" region, that is, the region between the loop footpoints, where the observations are easier to interpret. To reduce the uncertainties at the highest temperatures we present a new method for isolating the Fe XVIII emission in the AIA/SDO 94 angstrom channel. The resulting differential emission measure distributions confirm our previous analysis showing that the temperature distribution in an active region core is often strongly peaked near 4 MK. We characterize the properties of the emission distribution as a function of the total unsigned magnetic flux. We find that the amount of high-temperature emission in the active region core is correlated with the total unsigned magnetic flux, while the emission at lower temperatures, in contrast, is inversely related. These results provide compelling evidence that high-temperature active region emission is often close to equilibrium, although weaker active regions may be dominated by evolving million degree loops in the core. C1 [Warren, Harry P.] USN, Res Lab, Div Space Sci, Washington, DC 20375 USA. [Winebarger, Amy R.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. [Brooks, David H.] George Mason Univ, Coll Sci, Fairfax, VA 22030 USA. RP Warren, HP (reprint author), USN, Res Lab, Div Space Sci, Washington, DC 20375 USA. FU NASA FX This research was supported by NASA. Hinode is a Japanese mission developed and launched by ISAS/JAXA, with NAOJ as domestic partner and NASA and STFC (UK) as international partners. It is operated by these agencies in co-operation with ESA and NSC (Norway). H.P.W. benefited greatly from discussions at an International Space Science Institute meeting on coronal heating led by Steve Bradshaw and Helen Mason. NR 51 TC 65 Z9 65 U1 1 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD NOV 10 PY 2012 VL 759 IS 2 AR 141 DI 10.1088/0004-637X/759/2/141 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 034ZL UT WOS:000310911300064 ER PT J AU Werner, MW Murphy, DW Livingston, JH Gorjian, V Jones, DL Meier, DL Lawrence, CR AF Werner, Michael W. Murphy, David W. Livingston, John H. Gorjian, Varoujan Jones, Dayton L. Meier, David L. Lawrence, Charles R. TI SPITZER OBSERVATIONS OF HOTSPOTS IN RADIO LOBES SO ASTROPHYSICAL JOURNAL LA English DT Article DE acceleration of particles; radiation mechanisms: non-thermal ID X-RAY-EMISSION; HOT-SPOTS; CYGNUS-A; CHANDRA OBSERVATIONS; SPACE-TELESCOPE; COSMIC-RAYS; GALAXIES; RESOLUTION; JETS; ACCELERATION AB We have carried out a systematic search with Spitzer Warm Mission and archival data for infrared emission from the hotspots in radio lobes that have been described by Hardcastle et al. These hotspots have been detected with both radio and X-ray observations, but an observation at an intermediate frequency in the infrared can be critical to distinguish between competing models for particle acceleration and radiation processes in these objects. Between the archival and warm mission data, we report detections of 18 hotspots; the archival data generally include detections at all four IRAC bands, the Warm Mission data only at 3.6 mu m. Using a theoretical formalism adopted from Godfrey et al., we fit both archival and warm mission spectral energy distributions (SEDs)-including radio, X-ray, and optical data from Hardcastle as well as the Spitzer data-with a synchrotron self-Compton (SSC) model, in which the X-rays are produced by Compton scattering of the radio frequency photons by the energetic electrons which radiate them. With one exception, an SSC model requires that the magnetic field be less or much less than the equipartition value which minimizes total energy and has comparable amounts of energy in the magnetic field and in the energetic particles. This conclusion agrees with those of comparable recent studies of hotspots, and with the analysis presented by Hardcastle et al. We also show that the infrared data rule out the simplest synchrotron-only models for the SEDs. We briefly discuss the implications of these results and of alternate interpretations of the data. C1 [Werner, Michael W.; Murphy, David W.; Livingston, John H.; Gorjian, Varoujan; Jones, Dayton L.; Meier, David L.; Lawrence, Charles R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Werner, MW (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. FU Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA; NASA FX We thank the referee and Martin Hardcastle for their thoughtful commentswhich improved the paper significantly. This work is based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech. NR 23 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 J9 ASTROPHYS J JI Astrophys. J. PD NOV 10 PY 2012 VL 759 IS 2 AR 86 DI 10.1088/0004-637X/759/2/86 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 034ZL UT WOS:000310911300009 ER PT J AU Gebregiorgis, AS Tian, YD Peters-Lidard, CD Hossain, F AF Gebregiorgis, Abebe S. Tian, Yudong Peters-Lidard, Christa D. Hossain, Faisal TI Tracing hydrologic model simulation error as a function of satellite rainfall estimation bias components and land use and land cover conditions SO WATER RESOURCES RESEARCH LA English DT Article ID PRECIPITATION ANALYSIS TMPA; GLOBAL PRECIPITATION; PASSIVE MICROWAVE; UNITED-STATES; PRODUCTS; SYSTEM; RESOLUTION; SCALES; DATASET; FLUXES AB The key question that is asked in this study is "how are the three independent bias components of satellite rainfall estimation, comprising hit bias, missed, and false precipitation, physically related to the estimation uncertainty of soil moisture and runoff for a physically based hydrologic model?" The study also investigated the performance of different satellite rainfall products as a function of land use and land cover (LULC) type. Using the entire Mississippi river basin as the study region and the variable infiltration capacity (VIC)-3L as the distributed hydrologic model, the study of the satellite products (CMORPH, 3B42RT, and PERSIANN-CCS) yielded two key findings. First, during the winter season, more than 40% of the rainfall total bias is dominated by missed precipitation in forest and woodland regions (southeast of Mississippi). During the summer season, 51% of the total bias is governed by the hit bias, and about 42% by the false precipitation in grassland-savanna region (western part of Mississippi basin). Second, a strong dependence is observed between hit bias and runoff error, and missed precipitation and soil moisture error. High correlation with runoff error is observed with hit bias (similar to 0.85), indicating the need for improving the satellite rainfall product's ability to detect rainfall more consistently for flood prediction. For soil moisture error, it is the total bias that correlated significantly (similar to 0.78), indicating that a satellite product needed to be minimized of total bias for long-term monitoring of watershed conditions for drought through continuous simulation. C1 [Gebregiorgis, Abebe S.; Hossain, Faisal] Tennessee Technol Univ, Dept Civil & Environm Engn, Cookeville, TN 38505 USA. [Tian, Yudong; Peters-Lidard, Christa D.] NASA, Goddard Space Flight Ctr, Hydrol Sci Lab, Greenbelt, MD 20771 USA. [Tian, Yudong] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. RP Hossain, F (reprint author), Tennessee Technol Univ, Dept Civil & Environm Engn, 1020 Stadium Dr,Box 5015, Cookeville, TN 38505 USA. EM fhossain@tntech.edu RI Gebregiorgis, Abebe/C-7947-2016; Peters-Lidard, Christa/E-1429-2012; Measurement, Global/C-4698-2015 OI Gebregiorgis, Abebe/0000-0002-2975-9104; Peters-Lidard, Christa/0000-0003-1255-2876; FU NASA New Investigator Program (NIP) [NNX08AR32G]; Center for Management, Utilization and Protection of Water Resources at TN Technological University FX The study and the first author (Gebregiorgis) were supported by NASA New Investigator Program (NIP) grant NNX08AR32G of Faisal Hossain and the Center for Management, Utilization and Protection of Water Resources at TN Technological University. A major component of the research was also generously supported by the Goddard Earth Sciences and Technology (GEST) Center of University of MD Baltimore County through its Graduate Student Summer Program (GSSP) during summer 2011 awarded to the first author under the able supervision of Dr. Christa Peters-Lidard and Dr. Yudong Tian. The authors are also grateful for the guidance received from the associate editor and the three anonymous reviewers that helped to improve the quality of the study and manuscript considerably. NR 38 TC 17 Z9 17 U1 0 U2 21 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0043-1397 J9 WATER RESOUR RES JI Water Resour. Res. PD NOV 10 PY 2012 VL 48 AR W11509 DI 10.1029/2011WR011643 PG 17 WC Environmental Sciences; Limnology; Water Resources SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Water Resources GA 035QI UT WOS:000310962200001 ER PT J AU Dragomir, D Matthews, JM Howard, AW Antoci, V Henry, GW Guenther, DB Johnson, JA Kuschnig, R Marcy, GW Moffat, AFJ Rowe, JF Rucinski, SM Sasselov, D Weiss, WW AF Dragomir, Diana Matthews, Jaymie M. Howard, Andrew W. Antoci, Victoria Henry, Gregory W. Guenther, David B. Johnson, John A. Kuschnig, Rainer Marcy, Geoffrey W. Moffat, Anthony F. J. Rowe, Jason F. Rucinski, Slavek M. Sasselov, Dimitar Weiss, Werner W. TI NON-DETECTION OF PREVIOUSLY REPORTED TRANSITS OF HD 97658b WITH MOST PHOTOMETRY SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE planetary systems; stars: individual (HD 97658); techniques: photometric ID EXTRASOLAR PLANETS; SPACED DATA; ORBITS AB The radial velocity-discovered exoplanet HD 97658b was recently announced to transit, with a derived planetary radius of 2.93 +/- 0.28 R-circle plus. As a transiting super-Earth orbiting a bright star, this planet would make an attractive candidate for additional observations, including studies of its atmospheric properties. We present and analyze follow-up photometric observations of the HD 97658 system acquired with the Microvariability and Oscillations of STars space telescope. Our results show no transit with the depth and ephemeris reported in the announcement paper. For the same ephemeris, we rule out transits for a planet with radius larger than 2.09 R-circle plus, corresponding to the reported 3 sigma lower limit. We also report new radial velocity measurements which continue to support the existence of an exoplanet with a period of 9.5 days, and obtain improved orbital parameters. C1 [Dragomir, Diana; Matthews, Jaymie M.; Antoci, Victoria] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. [Howard, Andrew W.; Marcy, Geoffrey W.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Howard, Andrew W.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Antoci, Victoria] Aarhus Univ, Dept Phys & Astron, Stellar Astrophys Ctr SAC, DK-8000 Aarhus C, Denmark. [Antoci, Victoria; Kuschnig, Rainer; Weiss, Werner W.] Univ Vienna, Inst Astron, A-1180 Vienna, Austria. [Henry, Gregory W.] Tennessee State Univ, Ctr Excellence Informat Syst, Nashville, TN 37209 USA. [Guenther, David B.] St Marys Univ, Dept Phys & Astron, Halifax, NS B3H 3C3, Canada. [Johnson, John A.] CALTECH, Dept Astron, Pasadena, CA 91125 USA. [Johnson, John A.] NASA, Exoplanet Sci Inst NExScI, Pasadena, CA 91125 USA. [Moffat, Anthony F. J.] Univ Montreal, Dept Phys, Montreal, PQ H3C 3J7, Canada. [Rowe, Jason F.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Rucinski, Slavek M.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada. [Sasselov, Dimitar] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Dragomir, D (reprint author), Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. EM diana@phas.ubc.ca RI Howard, Andrew/D-4148-2015; OI Howard, Andrew/0000-0001-8638-0320; Dragomir, Diana/0000-0003-2313-467X; Antoci, Victoria/0000-0002-0865-3650 FU University of British Columbia Four Year Fellowship; Danish National Research Foundation; ASTERISK project; European Research Council [267864]; Natural Sciences and Engineering Research Council of Canada; FQRNT (Quebec); Austrian Science Fund [P22691-N16]; Austrian Research Promotion Agency-ALR FX D.D. is supported by a University of British Columbia Four Year Fellowship. Funding for the Stellar Astrophysics Centre (SAC) is provided by The Danish National Research Foundation and research is supported by the ASTERISK project (ASTERoseismic Investigations with SONG and Kepler) funded by the European Research Council (grant agreement No. 267864). The Natural Sciences and Engineering Research Council of Canada supports the research of D. B. G., J.M.M., A.F.J.M., and S. M. R. Additional support for A.F.J.M. comes from FQRNT (Quebec). R. K. and W. W. W. were supported by the Austrian Science Fund (P22691-N16) and by the Austrian Research Promotion Agency-ALR. NR 19 TC 3 Z9 3 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD NOV 10 PY 2012 VL 759 IS 2 AR L41 DI 10.1088/2041-8205/759/2/L41 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 030PC UT WOS:000310581600015 ER PT J AU Redford, JA Castro, IP Coleman, GN AF Redford, John A. Castro, Ian P. Coleman, Gary N. TI On the universality of turbulent axisymmetric wakes SO JOURNAL OF FLUID MECHANICS LA English DT Article DE shear layer turbulence; turbulence simulation; wakes ID DIRECT NUMERICAL-SIMULATION; EVOLVING PLANE WAKES; INITIAL CONDITIONS; REYNOLDS-NUMBER; EQUILIBRIUM; SIMILARITY; FLOW; EVOLUTION; MEMORY AB Direct numerical simulations (DNS) of two time-dependent, axially homogeneous, axisymmetric turbulent wakes having very different initial conditions are presented in order to assess whether they reach a universal self-similar state as classically hypothesized by Townsend. It is shown that an extensive early-time period exists during which the two wakes are individually self-similar with wake widths growing like delta proportional to t(1/3), as predicted by classical dimensional analysis, but have very different growth rates and are thus not universal. Subsequently, however, the turbulence adjusts to yield, eventually, wakes that are structurally identical and have the same growth rate (also with delta proportional to t(1/3)) so provide clear evidence of a universal, self-similar state. The former non-universal but self-similar state extends, in terms of a spatially equivalent flow behind a spherical body of diameter d, to a distance of O(3000d) whereas the final universal state does not appear before O(5000d) (and exists despite relatively low values of the Reynolds number and no evidence of a spectral kappa (5/3) inertial subrange). Universal wake evolution is therefore likely to be rare in practice. Despite its low Reynolds number, the flow does not exhibit the sometime-suggested alternative self-similar behaviour with delta proportional to t(1/2) (as for the genuinely laminar case) at large times (or, equivalently, distances), since the eddy viscosity remains large compared to the molecular viscosity and its temporal variations are not negligible. C1 [Redford, John A.; Castro, Ian P.; Coleman, Gary N.] Univ Southampton, Aerodynam & Flight Mech Res Grp, Southampton SO17 1BJ, Hants, England. RP Coleman, GN (reprint author), NASA Langley Res Ctr, Computat Aerosci Branch, Hampton, VA 23681 USA. EM Gary.N.Coleman@nasa.gov FU UK Ministry of Defence [RD027-02854]; UK Turbulence Consortium; EPSRC [EP/D044073/1, EP/G069581/1]; Office of Science and Technology through EPSRC FX This work was supported by the UK Ministry of Defence (Dstl project RD027-02854, managed by Dr R. P. Hornby), and the UK Turbulence Consortium, funded by the EPSRC under Grants EP/D044073/1 and EP/G069581/1. It made use of the facilities of HPCx and HECToR, the UK's national high-performance computing service, which is provided by UoE HPCx Ltd at the University of Edinburgh, Cray Inc and NAG Ltd, and funded by the Office of Science and Technology through EPSRC's High End Computing Programme. We are indebted to Drs P. J. Archer, T. S. Lund, E. Rind, K. Shariff and T. G. Thomas, and Professors S. Chernyshenko, B. Ganapathisumbramani, R. D. Sandberg and N. D. Sandham for their advice and encouragement along the way. Professors P. Bradshaw and R. Narasimha made useful comments on the manuscript. Thanks are due Dr C. P. Yorke for the substantial role he played in developing the vortex-ring initialization strategy, and to Dr Lund for proposing the procedure used to expand the lateral domain. The explanation in 3 regarding the relationship between the radius of the vortex rings and the half-width of the initial mean profile was provided by Dr Shariff. We have also benefited from timely discussions with Professor W. K. George, Professor J. C. R. Hunt, Dr M. M. Rogers and especially Dr P. R. Spalart. NR 29 TC 15 Z9 15 U1 0 U2 8 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 0022-1120 J9 J FLUID MECH JI J. Fluid Mech. PD NOV 10 PY 2012 VL 710 BP 419 EP 452 DI 10.1017/jfm.2012.371 PG 34 WC Mechanics; Physics, Fluids & Plasmas SC Mechanics; Physics GA 029AJ UT WOS:000310466900017 ER PT J AU Hanna, KLD Thomas, IR Bowles, NE Greenhagen, BT Pieters, CM Mustard, JF Jackson, CRM Wyatt, MB AF Hanna, K. L. Donaldson Thomas, I. R. Bowles, N. E. Greenhagen, B. T. Pieters, C. M. Mustard, J. F. Jackson, C. R. M. Wyatt, M. B. TI Laboratory emissivity measurements of the plagioclase solid solution series under varying environmental conditions SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID SPECTROSCOPY; ANORTHOSITE; FELDSPARS; MINERALS; SPECTRA; MOON; MARS AB New laboratory thermal infrared emissivity measurements of the plagioclase solid solution series over the 1700 similar to 400 cm(-1) (6-25 mu m) spectral range are presented. Thermal infrared (TIR) spectral changes for fine-particulate samples (0-25 mu m) are characterized for the first time under different laboratory environmental conditions: ambient (terrestrial-like), half-vacuum (Mars-like), vacuum, and vacuum with cooled chamber (lunar-like). Under all environmental conditions the Christiansen Feature (CF) is observed to vary in a systematic way with Na-rich end-member (albite) having a CF position at the highest wave number (shortest wavelength) and the Ca-rich end-member (anorthite) having a CF position with the lowest wave number (longest wavelength). As pressure decreases to <10(-3) mbar four observations are made: (1) the CF position shifts to higher wave numbers, (2) the spectral contrast of the CF increases relative to the RB, (3) the spectral contrast of the RB in the similar to 1200-900 spectral range decreases while the spectral contrast of the RB in the similar to 800-400 spectral range either increases or remains the same and (4) the TF disappears. A relationship between the wavelength position of the CF measured under simulated lunar conditions and plagioclase composition (An#) is developed. Although its exact form may evolve with additional data, this linear relationship should be applied to current and future TIR data sets of the Moon. Our new spectral measurements demonstrate how sensitive thermal infrared emissivity spectra of plagioclase feldspars are to the environmental conditions under which they are measured and provide important constraints for interpreting current and future thermal infrared data sets. C1 [Hanna, K. L. Donaldson; Pieters, C. M.; Mustard, J. F.; Jackson, C. R. M.; Wyatt, M. B.] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA. [Thomas, I. R.; Bowles, N. E.] Univ Oxford, Clarendon Lab, Oxford OX1 3PU, England. [Greenhagen, B. T.] CALTECH, Jet Prop Lab, Geophys & Planetary Geosci Grp, Pasadena, CA USA. RP Hanna, KLD (reprint author), Brown Univ, Dept Geol Sci, Box 1846, Providence, RI 02912 USA. EM ri_donaldson_hanna@brown.edu RI Greenhagen, Benjamin/C-3760-2016 FU NASA [NNX08AM75G]; NLSI [NNA09DB34A] FX We would like to extend our appreciation to Phil Christensen and Arizona State University for donating samples used in this study. A special thanks to Nilanjan Chatterjee at the MIT Electron Microprobe Facility for sample analyses. The authors would also like to thank Steve Ruff and the other anonymous reviewers for the thorough comments and suggestions that greatly improved this manuscript. K. L. Donaldson Hanna was supported by NASA grant ID NNX08AM75G. This research was supported in part by NLSI grant ID NNA09DB34A. NR 28 TC 10 Z9 10 U1 0 U2 6 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD NOV 8 PY 2012 VL 117 AR E11004 DI 10.1029/2012JE004184 PG 7 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 035PP UT WOS:000310960100001 ER PT J AU Lindsay, R Haas, C Hendricks, S Hunkeler, P Kurtz, N Paden, J Panzer, B Sonntag, J Yungel, J Zhang, J AF Lindsay, R. Haas, C. Hendricks, S. Hunkeler, P. Kurtz, N. Paden, J. Panzer, B. Sonntag, J. Yungel, J. Zhang, J. TI Seasonal forecasts of Arctic sea ice initialized with observations of ice thickness SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID MODEL AB Seasonal forecasts of the September 2012 Arctic sea ice thickness and extent are conducted starting from 1 June 2012. An ensemble of forecasts is made with a coupled ice-ocean model. For the first time, observations of the ice thickness are used to correct the initial ice thickness distribution to improve the initial conditions. Data from two airborne campaigns are used: NASA Operation IceBridge and SIZONet. The model was advanced through April and May using reanalysis data from 2012 and for June-September it was forced with reanalysis data from the previous seven summers. The ice extent in the corrected runs averaged lower in the Pacific sector and higher in the Atlantic sector compared to control runs with no corrections. The predicted total ice extent is 4.4 +/- 0.5 M km(2), 0.2 M km(2) less than that made with the control runs but 0.8 M km(2) higher than the observed September extent. Citation: Lindsay, R., C. Haas, S. Hendricks, P. Hunkeler, N. Kurtz, J. Paden, B. Panzer, J. Sonntag, J. Yungel, and J. Zhang (2012), Seasonal forecasts of Arctic sea ice initialized with observations of ice thickness, Geophys. Res. Lett., 39, L21502, doi:10.1029/2012GL053576. C1 [Lindsay, R.; Zhang, J.] Univ Washington, Polar Sci Ctr, Appl Phys Lab, Seattle, WA 98105 USA. [Haas, C.] York Univ, Dept Earth & Space Sci & Engn, Toronto, ON M3J 2R7, Canada. [Hendricks, S.; Hunkeler, P.] Alfred Wegener Inst Polar & Marine Res, Bremerhaven, Germany. [Kurtz, N.] NASA, Cryospher Sci Program, Goddard Space Flight Ctr, Greenbelt, MD USA. [Paden, J.; Panzer, B.] Univ Kansas, Ctr Remote Sensing Ice Sheets, Lawrence, KS 66045 USA. [Sonntag, J.; Yungel, J.] NASA, Wallops Flight Facil, Goddard Space Flight Ctr, Wallops Isl, VA USA. RP Lindsay, R (reprint author), Univ Washington, Polar Sci Ctr, Appl Phys Lab, 1013 NE 40th St, Seattle, WA 98105 USA. EM lindsay@apl.washington.edu RI Hendricks, Stefan/D-5168-2011; Haas, Christian/L-5279-2016; Lindsay, Ron/S-9083-2016 OI Hendricks, Stefan/0000-0002-1412-3146; Haas, Christian/0000-0002-7674-3500; FU National Science Foundation Office of Polar Programs; National Aeronautics and Space Administration Cryosphere Program and Operation IceBridge; Office of Naval Research; Center for Remote Sensing of Ice Sheets FX This study was conducted with support from the National Science Foundation Office of Polar Programs, the National Aeronautics and Space Administration Cryosphere Program and Operation IceBridge, the Office of Naval Research, and the Center for Remote Sensing of Ice Sheets. NR 17 TC 21 Z9 21 U1 0 U2 28 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD NOV 8 PY 2012 VL 39 AR L21502 DI 10.1029/2012GL053576 PG 6 WC Geosciences, Multidisciplinary SC Geology GA 035QQ UT WOS:000310963000002 ER PT J AU Jin, D Murtugudde, R Waliser, DE AF Jin, Daeho Murtugudde, Raghu Waliser, Duane E. TI Tropical Indo-Pacific Ocean chlorophyll response to MJO forcing SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS LA English DT Article ID ATMOSPHERIC INTRASEASONAL VARIABILITY; MADDEN-JULIAN OSCILLATION; GENERAL-CIRCULATION MODEL; MIXED-LAYER MODEL; ARABIAN SEA; PENETRATIVE RADIATION; SOLAR-RADIATION; INDIAN-OCEAN; CLIMATE; PHYTOPLANKTON AB Previous studies that analyzed ocean color satellite data have suggested that the primary mechanism of surface chlorophyll (Chl) response to the MJO is wind-induced turbulent mixing and the corresponding mixed layer entrainment. In this study, this notion is examined with an ocean biophysical model in an ensemble framework, focusing on upper ocean processes (z < 200 m). As a whole, the model's mean Chl state is lower than observations except in the tropical Pacific basin, but its seasonal variation is acceptable, particularly in the tropical Indian Ocean. In this basin, the model can simulate surface Chl responses to the MJO consistent with the observations in terms of the phase-by-phase anomaly evolution patterns. These Chl responses are mostly induced by surface wind forcing, which is consistent with previous studies. Further investigation of subsurface variations is performed at select grid points, and it is revealed that (1) entrained nutrients are the primary source of enhancement for surface Chl concentration and detrainment blooms are relatively less common; (2) in limited regions, Ekman pumping can effectively reduce Chl concentration; and (3) both entrainment/detrainment and Ekman pumping mechanisms rely on background states of nutrient availability, so the same forcing can result in completely different Chl responses depending on the background state. C1 [Jin, Daeho; Murtugudde, Raghu] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20740 USA. [Waliser, Duane E.] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Jin, D (reprint author), Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, 5825 Univ Res Ct,Ste 4001, College Pk, MD 20740 USA. EM daehojin@umd.edu FU NASA PO grant [NNX09AF43G]; Divecha Center for Climate Change; IITM-Pune; National Aeronautics and Space Administration FX D.J., R. M., and D. W. acknowledge support from NASA PO grant NNX09AF43G. R. M. acknowledges the support by the Divecha Center for Climate Change and IITM-Pune for their support and hospitality. R. M. also acknowledges the ONR DYNAMO grant. D.W.'s contribution to this study was carried out on behalf of the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. Associated with the observations data, CMAP Precipitation data provided by the NOAA/OAR/ESRL PSD, Boulder, Colorado, USA, from their Web site at http://www.esrl.noaa.gov/psd/.ECMWF ERA-Interim data used in this study have been obtained from the ECMWF data server. The CFSR data was developed by NOAA's NCEP. The data for this study are from NOAA's National Operational Model Archive and Distribution System (NOMADS), which is maintained at NOAA's National Climate Data Center (NCDC). NR 58 TC 5 Z9 5 U1 0 U2 16 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 NOV 8 PY 2012 VL 117 AR C11008 DI 10.1029/2012JC008015 PG 20 WC Oceanography SC Oceanography GA 035RS UT WOS:000310966300001 ER PT J AU Sibanda, P Moldwin, MB Galvan, DA Sandel, BR Forrester, T AF Sibanda, Patrick Moldwin, Mark B. Galvan, David A. Sandel, Bill R. Forrester, Terry TI Quantifying the azimuthal plasmaspheric density structure and dynamics inferred from IMAGE EUV SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID EXTREME-ULTRAVIOLET IMAGER; 17 APRIL 2002; INNER MAGNETOSPHERE; CRRES OBSERVATIONS; PLASMAPAUSE; CONVECTION; EVOLUTION; FEATURES; PLUMES; STORMS AB The extreme ultraviolet (EUV) imager on the IMAGE satellite provided the first global images of the plasmasphere leading to enhanced understanding of plasmapause structure and dynamics. However, few studies have investigated the structure and dynamics of the inner plasmasphere (regions interior to the plasmapause), which previous in situ observations have shown to often be highly structured. This study is the first to systematically analyze global images of the density structure of the inner plasmasphere by using data from the EUV imager on the IMAGE satellite. We find that the inner plasmasphere exhibits both fine and meso-scale structure characterized by rapid density fluctuations and density enhancements of varying amplitudes (factors of similar to 2-5) and spatial scales (from 10 s of minutes to 6 hours MLT) that occur regularly in the aftermath of geomagnetic storms. The level of variability within the azimuthal structure was found to increase with increasing geomagnetic activity. The observations suggest that some meso-scale azimuthal density structure observed in the inner plasmasphere is from "fossil" plasmapause features entrained inside the expanding and refilling plasmasphere. C1 [Sibanda, Patrick; Moldwin, Mark B.] Univ Michigan, Ann Arbor, MI 48109 USA. [Sibanda, Patrick] Univ Zambia, Dept Phys, Lusaka, Zambia. [Galvan, David A.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Sandel, Bill R.; Forrester, Terry] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. RP Sibanda, P (reprint author), Univ Michigan, Ann Arbor, MI 48109 USA. EM sibandapatrick.ps@gmail.com RI Moldwin, Mark/F-8785-2011 OI Moldwin, Mark/0000-0003-0954-1770 FU NASA [NNX09AI62G, NNX10AC82G, NNH09ZDA001-LWSSTRT, NNX07AG46G] FX This work was done while Patrick Sibanda worked as a Post-doc under the guidance of Mark Moldwin at the University of Michigan and was supported by NASA grants NNX09AI62G, NNX10AC82G and NNH09ZDA001-LWSSTRT. The IDL EUV analysis tools developed by the University of Arizona are available at http://euv.lpl.arizona.edu/euv/index. Work at the University of Arizona was supported under NASA Grant NNX07AG46G from the Heliospheric Guest Investigator Program. NR 31 TC 2 Z9 2 U1 0 U2 9 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD NOV 8 PY 2012 VL 117 AR A11204 DI 10.1029/2012JA017522 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 035RX UT WOS:000310967000001 ER PT J AU Simoes, F Klenzing, J Ivanov, S Pfaff, R Freudenreich, H Bilitza, D Rowland, D Bromund, K Liebrecht, MC Martin, S Schuck, P Uribe, P Yokoyama, T AF Simoes, Fernando Klenzing, Jeffrey Ivanov, Stoyan Pfaff, Robert Freudenreich, Henry Bilitza, Dieter Rowland, Douglas Bromund, Kenneth Liebrecht, Maria Carmen Martin, Steven Schuck, Peter Uribe, Paulo Yokoyama, Tatsuhiro TI Detection of ionospheric Alfven resonator signatures in the equatorial ionosphere SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID SCHUMANN RESONANCE; BACKGROUND-NOISE; PROPAGATION; MODEL; GENERATION; EXCITATION; ATMOSPHERE; WAVES; RANGE; FIELD AB The ionosphere response resulting from minimum solar activity during cycle 23/24 was unusual and offered unique opportunities for investigating space weather in the near-Earth environment. We report ultra low frequency electric field signatures related to the ionospheric Alfven resonator detected by the Communications/Navigation Outage Forecasting System (C/NOFS) satellite in the equatorial region. These signatures are used to constrain ionospheric empirical models and offer a new approach for monitoring ionosphere dynamics and space weather phenomena, namely aeronomy processes, Alfven wave propagation, and troposphere-ionosphere-magnetosphere coupling mechanisms. C1 [Simoes, Fernando; Klenzing, Jeffrey; Pfaff, Robert; Freudenreich, Henry; Rowland, Douglas; Bromund, Kenneth; Liebrecht, Maria Carmen; Martin, Steven; Schuck, Peter; Uribe, Paulo; Yokoyama, Tatsuhiro] NASA, Goddard Space Flight Ctr, Space Weather Lab, Heliophys Sci Div, Greenbelt, MD 20771 USA. [Ivanov, Stoyan] Georgia Inst Technol, Dept Phys, Atlanta, GA 30332 USA. [Bilitza, Dieter] NASA, Goddard Space Flight Ctr, Heliospher Phys Lab, Heliophys Sci Div, Greenbelt, MD 20771 USA. [Bilitza, Dieter] George Mason Univ, Space Weather Lab, Fairfax, VA 22030 USA. RP Simoes, F (reprint author), NASA, Goddard Space Flight Ctr, Space Weather Lab, Heliophys Sci Div, Greenbelt, MD 20771 USA. EM fernando.a.simoes@nasa.gov RI Klenzing, Jeff/E-2406-2011; Pfaff, Robert/F-5703-2012; Rowland, Douglas/F-5589-2012 OI Klenzing, Jeff/0000-0001-8321-6074; Pfaff, Robert/0000-0002-4881-9715; Rowland, Douglas/0000-0003-0948-6257 FU USAF; Air Force Office of Scientific Research; NASA FX The Communication/Navigation Outage Forecast System (C/NOFS) mission, conceived and developed by the U.S. Air Force Research Laboratory, is sponsored and executed by the USAF Space Test Program. We acknowledge support from the Air Force Office of Scientific Research. FS and JK are supported by an appointment to the NASA Postdoctoral Program at the Goddard Space Flight Center, administered by Oak Ridge Associated Universities through a contract with NASA. The work performed by SI at Goddard Space Flight Center was made possible by the NASA Education Office through the Undergraduate Student Research Program managed by the Universities Space Research Association. NR 42 TC 8 Z9 8 U1 0 U2 4 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD NOV 8 PY 2012 VL 117 AR A11305 DI 10.1029/2012JA017709 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 035RX UT WOS:000310967000002 ER PT J AU Perri, S Goldstein, ML Dorelli, JC Sahraoui, F AF Perri, S. Goldstein, M. L. Dorelli, J. C. Sahraoui, F. TI Detection of Small-Scale Structures in the Dissipation Regime of Solar-Wind Turbulence SO PHYSICAL REVIEW LETTERS LA English DT Article ID MAGNETOHYDRODYNAMIC TURBULENCE; MAGNETIC RECONNECTION; RANGE SPECTRUM; FLUCTUATIONS; CASCADES; DYNAMICS; WAVES; AU AB Recent observations of the solar wind have pointed out the existence of a cascade of magnetic energy from the scale of the proton Larmor radius rho(p) down to the electron Larmor radius rho(e) scale. In this Letter we study the spatial properties of magnetic field fluctuations in the solar wind and find that at small scales the magnetic field does not resemble a sea of homogeneous fluctuations, but rather a two-dimensional plane containing thin current sheets and discontinuities with spatial sizes ranging from l greater than or similar to rho(p) down to rho(e) and below. These isolated structures may be manifestations of intermittency that localize sites of turbulent dissipation. Studying the relationship between turbulent dissipation, reconnection, and intermittency is crucial for understanding the dynamics of laboratory and astrophysical plasmas. C1 [Perri, S.] Univ Calabria, Dipartmento Fis, I-87036 Arcavacata Di Rende, CS, Italy. [Goldstein, M. L.; Dorelli, J. C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Sahraoui, F.] UPMC, Lab Phys Plasmas, CNRS, Ecole Polytech,Observ St Maur, F-94107 St Maur Des Fosses, France. RP Perri, S (reprint author), Univ Calabria, Dipartmento Fis, I-87036 Arcavacata Di Rende, CS, Italy. RI Dorelli, John/C-9488-2012 FU Borsa Post-doc POR Calabria FSE Asse IV Capitale Umano-Obiettivo Operativo M.2; ISSI team "Dispersive cascade and dissipation in collisionless space plasma turbulence-observations and simulations" [185]; Marie Curie Project FP7 [PIRSES-2010-269297-"Turboplasmas'']; Magnetospheric Multiscale Mission Interdisciplinary Science program at the Goddard Space Flight Center; French ANR project, THESOW FX S. P.'s research was supported by "Borsa Post-doc POR Calabria FSE 2007/2013 Asse IV Capitale Umano-Obiettivo Operativo M.2''. S. P. and F. S. acknowledge their participation in the ISSI team 185 "Dispersive cascade and dissipation in collisionless space plasma turbulence-observations and simulations.'' S. P. further acknowledges the Marie Curie Project FP7 PIRSES-2010-269297-"Turboplasmas''. M. L. G. and J. C. D. acknowledge support from the Magnetospheric Multiscale Mission Interdisciplinary Science program at the Goddard Space Flight Center. F. S. acknowledges support from the French ANR project, THESOW. NR 35 TC 46 Z9 46 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 NOV 8 PY 2012 VL 109 IS 19 AR 191101 DI 10.1103/PhysRevLett.109.191101 PG 5 WC Physics, Multidisciplinary SC Physics GA 034EL UT WOS:000310853100004 PM 23215371 ER PT J AU Jordan, PM Saccomandi, G AF Jordan, P. M. Saccomandi, G. TI Compact acoustic travelling waves in a class of fluids with nonlinear material dispersion SO PROCEEDINGS OF THE ROYAL SOCIETY A-MATHEMATICAL PHYSICAL AND ENGINEERING SCIENCES LA English DT Article DE nonlinear acoustics; compact travelling waves; nonlinear dispersion ID EQUATIONS; MODEL; FLOW; SOLIDS; GREEN AB We apply a phenomenological theory of continua put forth by Rubin, Rosenau and Gottlieb in 1995 to an important class of compressible media. Regarding the material characteristic length coefficient, a, not as constant, but instead as a quadratic function of the velocity gradient, we carry out an in-depth analysis of one-dimensional acoustic travelling waves in inviscid, non-thermally conducting fluids. Analytical and numerical methods are employed to study the resulting waveforms, a special case of which exhibits compact support. In particular, a phase plane analysis is performed; simplified approximate/asymptotic expressions are presented; and a weakly nonlinear, KdV-like model that admits compact travelling wave solutions (TWSs), but which is not of the class K(m, n), is derived and analysed. Most significantly, our formulation allows for compact, pulse-type, acoustic waveforms in both gases and liquids. C1 [Jordan, P. M.] USN, Acoust Div, Res Lab, Stennis Space Ctr, Stennis Space Ctr, MS 39529 USA. [Saccomandi, G.] Univ Perugia, Dipartimento Ingn Ind, I-06125 Perugia, Italy. RP Jordan, PM (reprint author), USN, Acoust Div, Res Lab, Stennis Space Ctr, Stennis Space Ctr, MS 39529 USA. EM pjordan@nrlssc.navy.mil RI Saccomandi, Giuseppe/F-8690-2010 OI Saccomandi, Giuseppe/0000-0001-7987-8892 FU ONR FX The authors thank Dr Len G. Margolin for his constructive comments and suggestions, and Dr Josette P. Fabre for her careful proofreading of an earlier version of this article. P.M.J. was supported by ONR funding. G. S. acknowledges GNFM of INdAM and by PRIN 2009 'Matematica e meccanica dei sistemi biologici e dei tessuti molli.' All figures were generated using the software package MATHEMATICA (v. 5.2). NR 31 TC 8 Z9 8 U1 2 U2 10 PU ROYAL SOC PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 1364-5021 J9 P ROY SOC A-MATH PHY JI Proc. R. Soc. A-Math. Phys. Eng. Sci. PD NOV 8 PY 2012 VL 468 IS 2147 BP 3441 EP 3457 DI 10.1098/rspa.2012.0321 PG 17 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 016XA UT WOS:000309551900011 ER PT J AU Khazanov, GV Khabibrakhmanov, IK Glocer, A AF Khazanov, George V. Khabibrakhmanov, Ildar K. Glocer, Alex TI Kinetic description of ionospheric outflows based on the exact form of Fokker-Planck collision operator: Electrons SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID POLAR WIND; MONTE-CARLO; TRANSPORT-EQUATIONS; SUPERTHERMAL ELECTRONS; TEMPERATURE ANISOTROPY; VELOCITY DISTRIBUTION; MODEL; PLASMA; ION; SIMULATION AB We present the results of a finite difference implementation of the kinetic Fokker-Planck model with an exact form of the nonlinear collisional operator. The model is time dependent and three-dimensional; one spatial dimension and two in velocity space. The spatial dimension is aligned with the local magnetic field, and the velocity space is defined by the magnitude of the velocity and the cosine of pitch angle. An important new feature of model, the concept of integration along the particle trajectories, is discussed in detail. Integration along the trajectories combined with the operator time splitting technique results in a solution scheme which accurately accounts for both the fast convection of the particles along the magnetic field lines and relatively slow collisional process. We present several tests of the model's performance and also discuss simulation results of the evolution of the plasma distribution for realistic conditions in Earth's plasmasphere under different scenarios. C1 [Glocer, Alex] NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Greenbelt, MD 20771 USA. [Khabibrakhmanov, Ildar K.] IBM Corp, Thomas J Watson Res Ctr, Yorktown Hts, NY 10598 USA. RP Glocer, A (reprint author), NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Mail Code 673, Greenbelt, MD 20771 USA. EM alex.glocer-1@nasa.gov RI Glocer, Alex/C-9512-2012; feggans, john/F-5370-2012 OI Glocer, Alex/0000-0001-9843-9094; FU NASA [UPN 370 16 10]; NASA HQ POLAR Project; NASA LWS Program FX Funding in support of this study was provided by NASA grant UPN 370 16 10, NASA HQ POLAR Project, and the NASA LWS Program. We are grateful to the reviewers for their helpful comments. NR 59 TC 2 Z9 2 U1 0 U2 3 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD NOV 7 PY 2012 VL 117 AR A11203 DI 10.1029/2012JA018082 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 035RW UT WOS:000310966800002 ER PT J AU Velez, JCR Blanco-Cano, X Aguilar-Rodriguez, E Russell, CT Kajdic, P Jian, LK Luhmann, JG AF Ramirez Velez, J. C. Blanco-Cano, X. Aguilar-Rodriguez, E. Russell, C. T. Kajdic, P. Jian, L. K. Luhmann, J. G. TI Whistler waves associated with weak interplanetary shocks SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID QUASI-PARALLEL SHOCKS; EARTHS BOW SHOCK; MACH NUMBER; ISEE-2 OBSERVATIONS; OBSERVED UPSTREAM; SOLAR-WIND; PLASMA; IONS; INSTABILITY; BETA AB We analyze the properties of 98 weak interplanetary shocks measured by the dual STEREO spacecraft over approximately 3 years during the past solar minimum. We study the occurrence of whistler waves associated with these shocks, which on average are high beta shocks (0.2 < beta < 10). We have compared the waves properties upstream and downstream of the shocks. In the upstream region the waves are mainly circularly polarized, and in most of the cases (similar to 75%) they propagate almost parallel to the ambient magnetic field (<30 degrees). In contrast, the propagation angle with respect to the shock normal varies in a broad range of values (20 degrees to 90 degrees), suggesting that they are not phase standing. We find that the whistler waves can extend up to 100,000 km in the upstream region but in most cases (88%) are contained in a distance within 30,000 km from the shock. This corresponds to a larger region with upstream whistlers associated with IP shocks than previously reported in the literature. The maximum amplitudes of the waves are observed next to the shock interface, and they decrease as the distance to the shock increases. In most cases the wave propagation direction becomes more aligned with the magnetic field as the distance to the shock increases. These two facts suggest that most of the waves in the upstream region are Landau damping as they move away from the shock. From the analysis we also conclude that it is likely that the generation mechanism of the upstream whistler waves is taking place at the shock interface. In the downstream region, the waves are irregularly polarized, and the fluctuations are very compressive; that is, the compressive component of the wave clearly dominates over the transverse one. The majority of waves in the downstream region (95%) propagate at oblique angles with respect to the ambient magnetic field (>60 degrees). The wave propagation with respect to the shock-normal direction has no preferred direction and varies similarly to the upstream case. It is possible that downstream fluctuations are generated by ion relaxation as suggested in previous hybrid simulation shocks. C1 [Ramirez Velez, J. C.] Univ Nacl Autonoma Mexico, Inst Astron, Unidad Ensenada, Ensenada, Baja California, Mexico. [Blanco-Cano, X.; Kajdic, P.] Univ Nacl Autonoma Mexico, Inst Geofis, Mexico City 04510, DF, Mexico. [Aguilar-Rodriguez, E.] Univ Nacl Autonoma Mexico, Inst Geofis, Unidad Michoacan, Morelia, Michoacan, Mexico. [Russell, C. T.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90024 USA. [Jian, L. K.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Jian, L. K.] NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Greenbelt, MD 20771 USA. [Luhmann, J. G.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. RP Velez, JCR (reprint author), Univ Nacl Autonoma Mexico, Inst Astron, Unidad Ensenada, Ensenada, Baja California, Mexico. EM julio@astrosen.unam.mx RI Russell, Christopher/E-7745-2012; Jian, Lan/B-4053-2010; Ramirez-Velez, Robinson/D-5311-2016 OI Russell, Christopher/0000-0003-1639-8298; Jian, Lan/0000-0002-6849-5527; Ramirez-Velez, Robinson/0000-0003-3075-6960 FU PAPIIT [IN109112]; CONACyT [101625, 81154]; NASA STEREO program [NAS5-03131]; DGAPA [110511-3]; PAPIT [IN-110511-3] FX J. C. Ramirez Velez and E. Aguilar-Rodriguez thank PAPIIT project grant IN109112 and CONACyT project grant 101625. L. K. Jian is supported by the NASA STEREO program through grant NAS5-03131 administered by UC Berkeley. X. Blanco-Cano thanks CONACyT project grant 81154 and DGAPA grant 110511-3. P. Kajdic thanks CONACyT project grants 101625 and 81154 and PAPIT grant IN-110511-3. NR 31 TC 4 Z9 4 U1 0 U2 13 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD NOV 6 PY 2012 VL 117 AR A11103 DI 10.1029/2012JA017573 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 035RV UT WOS:000310966600001 ER PT J AU Eckermann, SD Wu, DL AF Eckermann, S. D. Wu, D. L. TI Satellite detection of orographic gravity-wave activity in the winter subtropical stratosphere over Australia and Africa SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID MOUNTAIN WAVES; RADIANCES; VARIANCES; LIMB AB Orographic gravity-wave (OGW) parameterizations in models produce waves over subtropical mountain ranges in Australia and Africa that propagate into the stratosphere during austral winter and deposit momentum, affecting weather and climate. Satellite sensors have measured stratospheric GWs for over a decade, yet find no evidence of these waves. So are parameterizations failing here? Here we argue that the short wavelengths of subtropical OGWs place them near or below the detection limits of satellite sensors. To test this hypothesis, we reanalyze nine years of stratospheric radiances from the Atmospheric Infrared Sounder (AIRS) on NASA's Aqua satellite during austral winter, applying new averaging techniques to maximize signal-to-noise and improve thresholds for OGW detection. Deep climatological enhancements in stratospheric OGW variance over specific mountain ranges in Australia and southern Africa are revealed for the first time, which exhibit temporal and vertical variations consistent with predicted OGW responses to varying background winds. Citation: Eckermann, S. D., and D. L. Wu (2012), Satellite detection of orographic gravity-wave activity in the winter subtropical stratosphere over Australia and Africa, Geophys. Res. Lett., 39, L21807, doi:10.1029/2012GL053791. C1 [Eckermann, S. D.] USN, Div Space Sci, Res Lab, Washington, DC 20375 USA. [Wu, D. L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Eckermann, SD (reprint author), USN, Div Space Sci, Res Lab, Code 7631,4555 Overlook Ave SW, Washington, DC 20375 USA. EM stephen.eckermann@nrl.navy.mil FU NASA through the NRA [NNH09ZDA001N-TERRAQUA, NNH11AQ99I] FX This work was partially supported by NASA through the NRA NNH09ZDA001N-TERRAQUA (The Science of Terra and Aqua), grant NNH11AQ99I. NR 14 TC 9 Z9 9 U1 0 U2 12 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD NOV 6 PY 2012 VL 39 AR L21807 DI 10.1029/2012GL053791 PG 6 WC Geosciences, Multidisciplinary SC Geology GA 035QK UT WOS:000310962400005 ER PT J AU Baars, H Ansmann, A Althausen, D Engelmann, R Heese, B Muller, D Artaxo, P Paixao, M Pauliquevis, T Souza, R AF Baars, H. Ansmann, A. Althausen, D. Engelmann, R. Heese, B. Mueller, D. Artaxo, P. Paixao, M. Pauliquevis, T. Souza, R. TI Aerosol profiling with lidar in the Amazon Basin during the wet and dry season SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID MICROPHYSICAL PARTICLE PARAMETERS; FOREST-FIRE SMOKE; OPTICAL-PROPERTIES; PHYSICAL-PROPERTIES; BACKSCATTER LIDAR; RAMAN-LIDAR; RAIN-FOREST; SUBMICROMETER AEROSOL; SIZE DISTRIBUTION; FREE TROPOSPHERE AB For the first time, multiwavelength polarization Raman lidar observations of optical and microphysical particle properties over the Amazon Basin are presented. The fully automated advanced Raman lidar was deployed 60 km north of Manaus, Brazil (2.5 degrees S, 60 degrees W) in the Amazon rain forest from January to November 2008. The measurements thus cover both the wet season (Dec-June) and the dry or burning season (July-Nov). Two cases studies of young and aged smoke plumes are discussed in terms of spectrally resolved optical properties (355, 532, and 1064 nm) and further lidar products such as particle effective radius and single-scattering albedo. These measurement examples confirm that biomass burning aerosols show a broad spectrum of optical, microphysical, and chemical properties. The statistical analysis of the entire measurement period revealed strong differences between the pristine wet and the polluted dry season. African smoke and dust advection frequently interrupt the pristine phases during the wet season. Compared to pristine wet season conditions, the particle scattering coefficients in the lowermost 2 km of the atmosphere were found to be enhanced, on average, by a factor of 4 during periods of African aerosol intrusion and by a factor of 6 during the dry (burning) season. Under pristine conditions, the particle extinction coefficients and optical depth for 532 nm wavelength were frequently as low as 10-30 Mm(-1) and <0.05, respectively. During the dry season, biomass burning smoke plumes reached to 3-5 km height and caused a mean optical depth at 532 nm of 0.26. On average during that season, particle extinction coefficients (532 nm) were of the order of 100 Mm(-1) in the main pollution layer (up to 2 km height). Angstrom exponents were mainly between 1.0 and 1.5, and the majority of the observed lidar ratios were between 50-80 sr. C1 [Baars, H.; Ansmann, A.; Althausen, D.; Engelmann, R.; Heese, B.; Mueller, D.; Paixao, M.] Leibniz Inst Tropospher Res, DE-04318 Leipzig, Germany. [Mueller, D.] NASA, Langley Res Ctr, Sci Syst & Applicat Inc, Hampton, VA 23665 USA. [Artaxo, P.; Paixao, M.] Univ Sao Paulo, Inst Phys, Sao Paulo, Brazil. [Pauliquevis, T.] Univ Fed Sao Paulo, Dept Earth & Nat Sci, Diadema, Brazil. [Souza, R.] Univ State Amazonas, Manaus, Amazonas, Brazil. RP Baars, H (reprint author), Leibniz Inst Tropospher Res, Permoserstr 15, DE-04318 Leipzig, Germany. EM baars@tropos.de RI MUELLER, DETLEF/F-1010-2015; Baars, Holger/I-3308-2015; Pauliquevis, Theotonio/B-9408-2012; Artaxo, Paulo/E-8874-2010 OI MUELLER, DETLEF/0000-0002-0203-7654; Baars, Holger/0000-0002-2316-8960; Artaxo, Paulo/0000-0001-7754-3036 FU National Institute for Amazonia Research (INPA); AMAZE-08 team; European Union (FP7) [036833-2]; CNPq; FAPESP Thematic Project AEROCLIMA [2008/58100-2]; EU FP6 project EUCAARI [34684] FX We thank the National Institute for Amazonia Research (INPA) and the AMAZE-08 team, especially Scot Martin, for their support. EUCAARI was funded by the European Union (FP7, grant 036833-2). Paulo Artaxo acknowledges CNPq and FAPESP Thematic Project AEROCLIMA 2008/58100-2. This project was also funded by the EU FP6 project EUCAARI (contract 34684). Some analyses and visualizations used in this paper were produced with the Giovanni online data system, developed and maintained by the NASA GES DISC. We also acknowledge the MODIS mission scientists and associated NASA personnel for the production of the data used in this research effort. We thank Mika Komppula for providing ECMWF data. NR 68 TC 29 Z9 29 U1 1 U2 42 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD NOV 3 PY 2012 VL 117 AR D21201 DI 10.1029/2012JD018338 PG 16 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 032BE UT WOS:000310686000001 ER PT J AU Li, LM Baines, KH Smith, MA West, RA Perez-Hoyos, S Trammell, HJ Simon-Miller, AA Conrath, BJ Gierasch, PJ Orton, GS Nixon, CA Filacchione, G Fry, PM Momary, TW AF Li, Liming Baines, Kevin H. Smith, Mark A. West, Robert A. Perez-Hoyos, Santiago Trammell, Harold J. Simon-Miller, Amy A. Conrath, Barney J. Gierasch, Peter J. Orton, Glenn S. Nixon, Conor A. Filacchione, Gianrico Fry, Patrick M. Momary, Thomas W. TI Emitted power of Jupiter based on Cassini CIRS and VIMS observations SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID QUASI-BIENNIAL OSCILLATION; MERIDIONAL ENERGY-BALANCE; INFRARED SPECTROMETER; SPATIAL-ORGANIZATION; MOIST CONVECTION; TIME-DEPENDENCE; INTERNAL HEAT; ATMOSPHERE; STRATOSPHERE; TEMPERATURES AB The emitted power of Jupiter and its meridional distribution are determined from observations by the Composite Infrared Spectrometer and Visual and Infrared Mapping Spectrometer onboard Cassini during its flyby en route to Saturn in late 2000 and early 2001. Jupiter's global-average emitted power and effective temperature are measured to be 14.10 +/- 0.03 Wm(-2) and 125.57 +/- 0.07 K, respectively. Jupiter's 5 mm thermal emission contributes 0.7 +/- 0.1% to the total emitted power at the global scale, but it can reach 1.9 +/- 0.6% at 15 degrees N. The meridional distribution of emitted power shows a significant asymmetry between the two hemispheres with the emitted power in the northern hemisphere 3.0 +/- 0.3% larger than that in the southern hemisphere. Such an asymmetry shown in the Cassini epoch (2000-2001) is not present in the Voyager epoch (1979). In addition, the global-average emitted power increased 3.8 +/- 1.0% between the two epochs. The temporal variation of Jupiter's total emitted power is mainly due to the warming of atmospheric layers around the pressure level of 200 mbar. The temporal variation of emitted power was also discovered on Saturn. Therefore, we suggest that the varying emitted power is a common phenomenon on the giant planets. C1 [Li, Liming; Smith, Mark A.; Trammell, Harold J.] Univ Houston, Coll Nat Sci & Math, Houston, TX 77004 USA. [Baines, Kevin H.; West, Robert A.; Orton, Glenn S.; Momary, Thomas W.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Perez-Hoyos, Santiago] Univ Basque Country, ETS Ingn, Dept Fis Aplicada 1, Bilbao, Spain. [Simon-Miller, Amy A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Conrath, Barney J.; Gierasch, Peter J.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. [Nixon, Conor A.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Filacchione, Gianrico] Area Ric Tor Vergata, Ist Astrofis & Planetol Spaziali, INAF IAPS, Rome, Italy. [Fry, Patrick M.] Univ Wisconsin Madison, Ctr Space Sci & Engn, Madison, WI USA. RP Li, LM (reprint author), Univ Houston, Coll Nat Sci & Math, 4800 Calhoun Rd, Houston, TX 77004 USA. EM lli13@uh.edu RI Nixon, Conor/A-8531-2009; Perez-Hoyos, Santiago/L-7543-2014; Simon, Amy/C-8020-2012; OI Nixon, Conor/0000-0001-9540-9121; Perez-Hoyos, Santiago/0000-0002-2587-4682; Simon, Amy/0000-0003-4641-6186; Filacchione, Gianrico/0000-0001-9567-0055 NR 43 TC 7 Z9 7 U1 0 U2 15 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD NOV 3 PY 2012 VL 117 AR E11002 DI 10.1029/2012JE004191 PG 17 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 032CU UT WOS:000310690400001 ER PT J AU Norvig, P AF Norvig, Peter TI THE COMING SUPERINTELLIGENCE SO NEW SCIENTIST LA English DT Editorial Material C1 [Norvig, Peter] Stanford Univ, Stanford, CA 94305 USA. [Norvig, Peter] NASA, Ames Res Ctr, Computat Sci Div, Washington, DC USA. NR 0 TC 0 Z9 0 U1 2 U2 10 PU REED BUSINESS INFORMATION LTD PI SUTTON PA QUADRANT HOUSE THE QUADRANT, SUTTON SM2 5AS, SURREY, ENGLAND SN 0262-4079 J9 NEW SCI JI New Sci. PD NOV 3 PY 2012 VL 216 IS 2889 BP VIII EP VIII PG 1 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 034HI UT WOS:000310863100036 ER PT J AU Boening, C Lebsock, M Landerer, F Stephens, G AF Boening, Carmen Lebsock, Matthew Landerer, Felix Stephens, Graeme TI Snowfall-driven mass change on the East Antarctic ice sheet SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID GRACE; VARIABILITY; REANALYSIS; BALANCE; SYSTEM AB An improved understanding of processes dominating the sensitive balance between mass loss primarily due to glacial discharge and mass gain through precipitation is essential for determining the future behavior of the Antarctic ice sheet and its contribution to sea level rise. While satellite observations of Antarctica indicate that West Antarctica experiences dramatic mass loss along the Antarctic Peninsula and Pine Island Glacier, East Antarctica has remained comparably stable. In this study, we describe the causes and magnitude of recent extreme precipitation events along the East Antarctic coast that led to significant regional mass accumulations that partially compensate for some of the recent global ice mass losses that contribute to global sea level rise. The gain of almost 350 Gt from 2009 to 2011 is equivalent to a decrease in global mean sea level at a rate of 0.32 mm/yr over this three-year period. Citation: Boening, C., M. Lebsock, F. Landerer, and G. Stephens (2012), Snowfall-driven mass change on the East Antarctic ice sheet, Geophys. Res. Lett., 39, L21501, doi:10.1029/2012GL053316. C1 [Boening, Carmen; Lebsock, Matthew; Landerer, Felix; Stephens, Graeme] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Boening, C (reprint author), CALTECH, Jet Prop Lab, MS 300-323,4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM carmen.boening@jpl.nasa.gov OI Landerer, Felix/0000-0003-2678-095X FU NASA [NMO710771] FX We would like to thank two anonymous reviewers for their helpful comments and suggestions. The work was performed at the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA and is partially supported through NASA contract NMO710771 to JPL. We thank the GRACE analysis centers at University of Texas, JPL, and Geoforschungszentrum Potsdam, and the German Space Operations Center (GSOC) of the German Aerospace Center (DLR). NR 31 TC 39 Z9 40 U1 2 U2 47 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD NOV 2 PY 2012 VL 39 AR L21501 DI 10.1029/2012GL053316 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 032DA UT WOS:000310691000001 ER PT J AU Siegel, PH AF Siegel, Peter H. TI Untitled SO IEEE TRANSACTIONS ON TERAHERTZ SCIENCE AND TECHNOLOGY LA English DT Editorial Material C1 [Siegel, Peter H.] CALTECH, Pasadena, CA 91125 USA. [Siegel, Peter H.] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Siegel, PH (reprint author), CALTECH, Pasadena, CA 91125 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 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 NOV PY 2012 VL 2 IS 6 BP 573 EP 574 DI 10.1109/TTHZ.2012.2224234 PG 2 WC Engineering, Electrical & Electronic; Optics; Physics, Applied SC Engineering; Optics; Physics GA 142AU UT WOS:000318769000001 ER PT J AU Siegel, PH AF Siegel, Peter H. TI Terahertz Pioneers A Series of Interviews With Significant Contributors to Terahertz Science and Technology SO IEEE TRANSACTIONS ON TERAHERTZ SCIENCE AND TECHNOLOGY LA English DT Editorial Material C1 [Siegel, Peter H.] CALTECH, Pasadena, CA 91125 USA. [Siegel, Peter H.] JPL, Pasadena, CA 91125 USA. RP Siegel, PH (reprint author), CALTECH, Pasadena, CA 91125 USA. NR 12 TC 1 Z9 1 U1 1 U2 4 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 NOV PY 2012 VL 2 IS 6 BP 577 EP 577 DI 10.1109/TTHZ.2012.2222637 PG 1 WC Engineering, Electrical & Electronic; Optics; Physics, Applied SC Engineering; Optics; Physics GA 142AU UT WOS:000318769000002 ER PT J AU Siegel, PH AF Siegel, Peter H. TI Terahertz Pioneer: Frank C. De Lucia "The Numbers Count" SO IEEE TRANSACTIONS ON TERAHERTZ SCIENCE AND TECHNOLOGY LA English DT Editorial Material ID MILLIMETER-WAVE; ROTATIONAL SPECTRUM; HYDROGEN-PEROXIDE; INDIUM ANTIMONIDE; ANALYTICAL TOOL; BEAM MASER; GAS-PHASE; SPECTROSCOPY; REGION; PRESSURE C1 [Siegel, Peter H.] CALTECH, Dept Biol, Pasadena, CA 91125 USA. [Siegel, Peter H.] CALTECH, Dept Elect Engn, Pasadena, CA 91125 USA. [Siegel, Peter H.] NASA, Jet Prop Lab, Pasadena, CA 91109 USA. RP Siegel, PH (reprint author), CALTECH, Dept Biol, Pasadena, CA 91125 USA. EM phs@cal-tech.edu NR 62 TC 0 Z9 0 U1 0 U2 5 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 NOV PY 2012 VL 2 IS 6 BP 578 EP 583 DI 10.1109/TTHZ.2012.2222638 PG 6 WC Engineering, Electrical & Electronic; Optics; Physics, Applied SC Engineering; Optics; Physics GA 142AU UT WOS:000318769000003 ER PT J AU Morales, W Street, KW Richard, RM Valco, DJ AF Morales, Wilfredo Street, Kenneth W. Richard, Ryan M. Valco, Daniel J. TI Tribological Testing and Thermal Analysis of an Alkyl Sulfate Series of Ionic Liquids for Use as Aerospace Lubricants SO TRIBOLOGY TRANSACTIONS LA English DT Article DE Ionic Liquids; Spiral Orbit Tribometry; Vapor Pressure; Thermogravimetric Analysis ID MELTING-POINT DEPRESSION; SPIRAL ORBIT TRIBOMETRY; VACUUM; PRESSURE AB Due to their low vapor pressures, low melting points, high boiling points, high radiation resistance, and high thermal stability, room-temperature ionic liquids (ILs) appear to be suitable candidates as new aerospace lubricants for the upcoming return to the Moon and eventual Mars missions and for air and rotorcraft applications. In this study, three ILs with the same cation, 1-butyl-3-methylimidazolium, but different sulfate anions were tested using an ultra-high vacuum spiral orbit tribometer (SOT) and their thermal properties were determined by thermogravimetric analysis (TGA). Specifically, 1-butyl-3-methylimidazolium methyl sulfate, 1-butyl-3-methylimidazolium ethyl sulfate, and 1-butyl-3-methylimidazolium octyl sulfate were tested. The SOT experiments revealed that the lifetimes of the three ILs decreased with increasing alkyl substituent length on the sulfate anion. Infrared and Raman spectra were taken to detect unused ILs and graphitic degradation products, respectively, on worn parts. Post-run spectroscopic analysis indicated residual degraded, but still usable, ILs in all runs, coupled with varying amounts of amorphous graphitic material produced as the final degradation product of all ILs. SOT testing indicated that these ILs have lower friction coefficients and lifetimes greater than those of two commonly used perfluoropolyalkylether (PFPE) space lubricants. TGA showed that the methyl sulfate IL had the highest thermal stability in air and nitrogen. The vapor pressure of the methyl sulfate IL is as at least as low as Fomblin 815Z at 20 degrees C. C1 [Morales, Wilfredo; Street, Kenneth W.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. [Richard, Ryan M.] Cleveland State Univ, Cleveland, OH 44115 USA. [Valco, Daniel J.] Ohio State Univ, Columbus, OH 43210 USA. RP Morales, W (reprint author), NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. NR 16 TC 14 Z9 14 U1 3 U2 24 PU TAYLOR & FRANCIS INC PI PHILADELPHIA PA 325 CHESTNUT ST, SUITE 800, PHILADELPHIA, PA 19106 USA SN 1040-2004 J9 TRIBOL T JI Tribol. Trans. PD NOV 1 PY 2012 VL 55 IS 6 BP 815 EP 821 DI 10.1080/10402004.2012.715322 PG 7 WC Engineering, Mechanical SC Engineering GA 089LS UT WOS:000314912600012 ER PT J AU Kudryavtsev, VA Spooner, NJC Gluyas, J Fung, C Coleman, M AF Kudryavtsev, Vitaly A. Spooner, Neil J. C. Gluyas, Jon Fung, Cora Coleman, Max TI Monitoring subsurface CO2 emplacement and security of storage using muon tomography SO INTERNATIONAL JOURNAL OF GREENHOUSE GAS CONTROL LA English DT Article DE Carbon capture; Carbon storage monitoring; Muon tomography; Cosmic-ray muons ID CARBON-DIOXIDE; MUSIC; JAPAN AB Storage of supercritical carbon dioxide in the deep subsurface is arguably the most viable industrial scale process available to stop increase of atmospheric CO2. Today, monitoring CO2 emplacement and possible leakage is a major challenge; methods are episodic and expensive. Cosmic-ray muon tomography has been used to investigate hidden archaeological and geological features. We developed a model to test if this approach would work for monitoring CO2 storage and show that muon detection is a viable method. Our results indicate that we could detect as little as 0.4% change in the mean reservoir density at about 1 km depth (equivalent to 7% of pore volume). Hence, cosmic ray muon detection could monitor migration of injected CO2 continuously and inexpensively and help rapid introduction of this essential technology. (c) 2012 Elsevier Ltd. All rights reserved. C1 [Kudryavtsev, Vitaly A.; Spooner, Neil J. C.; Fung, Cora] Univ Sheffield, Dept Phys & Astron, Sheffield S3 7RH, S Yorkshire, England. [Gluyas, Jon] Univ Durham, Dept Earth Sci, Ctr Res Earth Energy Syst, Durham DH1 3LE, England. [Coleman, Max] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Kudryavtsev, VA (reprint author), Univ Sheffield, Dept Phys & Astron, Hounsfield Rd, Sheffield S3 7RH, S Yorkshire, England. EM v.kudryavtsev@sheffield.ac.uk RI Gluyas, Jon/B-8808-2014 OI Gluyas, Jon/0000-0002-9386-7206 FU University of Sheffield; EPSRC through the E-Futures Doctoral Training Centre at the University of Sheffield; National Aeronautics and Space Administration (NASA) FX We are grateful to S. M. Paling, L. F. Thompson, J. Cripps, T. Bennett, D. Lerner, C. Shelbourn, D. A. French and I. Phillips for useful discussions, and to D. H. Rodgers, who alerted MC to the existence of muon tomography. VAK and NJCS are grateful to the University of Sheffield for the financial support of the Ph.D. network related to muon tomography. CF's project work was funded by EPSRC through the E-Futures Doctoral Training Centre at the University of Sheffield. JG thanks DONG and Ikon Science for supporting carbon capture and storage research at Durham University. The contribution of MC was carried out at the Jet Propulsion Laboratory (JPL), California Institute of Technology, under contract with the National Aeronautics and Space Administration (NASA). NR 22 TC 14 Z9 14 U1 0 U2 17 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 1750-5836 J9 INT J GREENH GAS CON JI Int. J. Greenh. Gas Control PD NOV PY 2012 VL 11 BP 21 EP 24 DI 10.1016/j.ijggc.2012.07.023 PG 4 WC GREEN & SUSTAINABLE SCIENCE & TECHNOLOGY; Energy & Fuels; Engineering, Environmental SC Science & Technology - Other Topics; Energy & Fuels; Engineering GA 070AW UT WOS:000313479200003 ER PT J AU Rickman, D Immer, C Metzger, P Dixon, E Pendleton, M Edmunson, J AF Rickman, Doug Immer, Christopher Metzger, Philip Dixon, Emily Pendleton, Matthew Edmunson, Jennifer TI PARTICLE SHAPE IN SIMULANTS OF THE LUNAR REGOLITH SO JOURNAL OF SEDIMENTARY RESEARCH LA English DT Article AB Shape is an important property of lunar regolith particles. It substantially affects the regolith's strength, the angle of repose, the packing density, and the ability of regolith particles to attach to and abrade spacecraft materials or clog air filters. For these reasons, simulants are needed to reproduce regolith particle shapes for testing spacecraft that interacts with the lunar surface. Difficulties in assessing "how good" a simulant reproduces the shape of lunar particles stem from the lack of shape measurements obtained on lunar particles, compounded by the lack of a strict definition of shape or a way to quantifiably measure shape. This paper presents a general method for measuring and comparing particle shapes, and provides shape measurements for six lunar-regolith simulants. The method of evaluating particle shape presented here involves Fine Particle Analysis and corresponding image analysis to extract the maximum Feret diameter, Feret diameter of the minor axis of the inertial ellipse, mean diameter, sieve diameter, area, and perimeter length from images with an approximately 4.4 mu m pixel resolution. From those, aspect ratio and Heywood factor are computed. Data processing involves calculating the frequency distributions of particle shapes according to their sieve diameter, aspect ratio, and Heywood factor. The resulting graphical representations indicate that the majority of the lunar regolith simulant particles, in two-dimensional projection, can be well represented by a mixture of ellipses and rectangles of varying aspect ratios. The differences between simulant particle shapes, and lunar regolith particle shapes measured in the future, can be quantified by differencing the accumulated distributions. Thus, this paper presents a new method of particle shape analysis and a new way to quantifiably compare particle shapes. C1 [Rickman, Doug] NASA, George C Marshall Space Flight Ctr, Earth Sci Off, Huntsville, AL 35812 USA. [Immer, Christopher] GE Global Res, Electromagnet & Superconduct Lab, Niskayuna, NY 12309 USA. [Metzger, Philip] NASA, Granular Mech & Regolith Operat Lab, Kennedy Space Ctr, FL 32899 USA. [Dixon, Emily] Univ Oklahoma, Dept Geol, Norman, OK 73019 USA. [Pendleton, Matthew] Univ Minnesota, Dept Geol & Geophys, Minneapolis, MN 55440 USA. [Edmunson, Jennifer] BAE Syst, Huntsville, AL 35806 USA. RP Rickman, D (reprint author), NASA, George C Marshall Space Flight Ctr, Earth Sci Off, Huntsville, AL 35812 USA. RI Metzger, Philip/R-3136-2016; OI Metzger, Philip/0000-0002-6871-5358; Rickman, Doug/0000-0003-3409-2882 NR 18 TC 3 Z9 3 U1 0 U2 7 PU SEPM-SOC SEDIMENTARY GEOLOGY PI TULSA PA 6128 EAST 38TH ST, STE 308, TULSA, OK 74135-5814 USA SN 1527-1404 J9 J SEDIMENT RES JI J. Sediment. Res. PD NOV-DEC PY 2012 VL 82 IS 11-12 BP 823 EP 832 DI 10.2110/jsr.2012.69 PG 10 WC Geology SC Geology GA 078FZ UT WOS:000314085400002 ER PT J AU Gietzen, KM Lacy, CHS Ostrowski, DR Sears, DWG AF Gietzen, Katherine M. Lacy, Claud H. S. Ostrowski, Daniel R. Sears, Derek W. G. TI IRTF observations of S complex and other asteroids: Implications for surface compositions, the presence of clinopyroxenes, and their relationship to meteorites SO METEORITICS & PLANETARY SCIENCE LA English DT Article ID MODIFIED GAUSSIAN MODEL; NEAR-EARTH OBJECTS; SPECTROSCOPIC SURVEY; SPECTRAL PROPERTIES; ORDINARY CHONDRITES; PYROXENE MIXTURES; THERMAL HISTORIES; INFRARED-SPECTRA; VESTA; CONNECTION AB We have obtained near-infrared spectra for near-Earth asteroids (NEA) and Main Belt asteroids by using NASA's Infrared Telescope Facility. Most of the S complex classes of the Tholen-Bus-DeMeo scheme and the S(I)-S(VII) classes are represented. To help interpret the results, we examined visible/near-IR spectra for ordinary chondrites. The unequilibrated ordinary chondrites (UOC) spectra contain a 2.3 mu m feature which is absent in the spectra of the equilibrated ordinary chondrites (EOC). On the basis of literature data and new spectra low-Ca clinopyroxenes, we suggest that the 2.3 mu m in UOC is due to the presence of low-Ca clinopyroxene in the UOC which is absent in EOC. While this difference can be seen in the raw spectra, we confirmed this observation using a modified Gaussian model (MGM) for spectral analysis. Both the UOC and the EOC plot in the S(IV) field of the band area ratio plot for asteroids. We suggest that many or most S(IV) asteroids have material resembling UOC on their surfaces. An internally heated ordinary chondrite parent object would have EOC material at depth and UOC material on the surface. Cosmic ray exposure ages, and K-Ar ages for L chondrites, indicate that most EOC came from relatively few objects; however, the age distributions for UOC are unlike those of EOC. We suggest that while EOC come from the interiors of a limited number of S(IV) asteroids, the UOC come from the surfaces of a large number of S(IV) asteroids. C1 [Gietzen, Katherine M.; Lacy, Claud H. S.; Ostrowski, Daniel R.; Sears, Derek W. G.] Univ Arkansas, Arkansas Ctr Space & Planetary Sci, Fayetteville, AR 72701 USA. [Lacy, Claud H. S.] Univ Arkansas, Dept Phys, Fayetteville, AR 72701 USA. [Sears, Derek W. G.] Univ Arkansas, Dept Chem & Biochem, Fayetteville, AR 72701 USA. RP Sears, DWG (reprint author), NASA, Space Sci & Astrobiol Div, Ames Res Ctr, MS245-3, Mountain View, CA 94035 USA. EM derek.sears@nasa.gov FU NASA FX Without implying endorsement of our views, we gratefully acknowledge the many colleagues who have commented on our work over the last few years or otherwise helped as we evolved our thoughts and ideas: Paul Abell, Rick Binzel, Vincent Chevrier, Mike Gaffey, Paul Hardersen, Tim McCoy, Andy Rivkin, Ludolf Schultz, and Jessica Sunshine. We are also grateful to NASA for access to the IRTF and for funding, to Bobby Bus for hospitality and help in obtaining the data, Dan Britt for advice using the facility, Takahiro Hiroi for obtaining spectra for terrestrial clinopyroxenes, and Tom Burbine, Beth Clark Joseph, and Hazel Sears for very helpful reviews, and Hazel Sears for proofing the paper. NR 74 TC 5 Z9 5 U1 0 U2 3 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD NOV PY 2012 VL 47 IS 11 BP 1789 EP 1808 DI 10.1111/maps.12013 PG 20 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 076UW UT WOS:000313985100008 ER PT J AU Clark, BE AF Clark, Beth Ellen TI ASTEROIDS Dark and stormy weather SO NATURE LA English DT Editorial Material ID SPACE; SURFACE C1 [Clark, Beth Ellen] Ithaca Coll, Dept Phys, Ithaca, NY 14850 USA. [Clark, Beth Ellen] Univ Arizona, NASA, OSIRIS REx Asteroid Sample Return Mission, Tucson, AZ 85721 USA. RP Clark, BE (reprint author), Ithaca Coll, Dept Phys, Ithaca, NY 14850 USA. EM bclark@ithaca.edu NR 14 TC 0 Z9 0 U1 0 U2 0 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD NOV 1 PY 2012 VL 491 IS 7422 BP 45 EP 46 PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 028PM UT WOS:000310434500025 PM 23128222 ER PT J AU Pieters, CM Ammannito, E Blewett, DT Denevi, BW De Sanctis, MC Gaffey, MJ Le Corre, L Li, JY Marchi, S McCord, TB McFadden, LA Mittlefehldt, DW Nathues, A Palmer, E Reddy, V Raymond, CA Russell, CT AF Pieters, C. M. Ammannito, E. Blewett, D. T. Denevi, B. W. De Sanctis, M. C. Gaffey, M. J. Le Corre, L. Li, J. -Y. Marchi, S. McCord, T. B. McFadden, L. A. Mittlefehldt, D. W. Nathues, A. Palmer, E. Reddy, V. Raymond, C. A. Russell, C. T. TI Distinctive space weathering on Vesta from regolith mixing processes SO NATURE LA English DT Article ID ITOKAWA DUST PARTICLES; ASTEROID 4 VESTA; ORDINARY CHONDRITES; IRRADIATION; MORPHOLOGY; MINERALOGY; SURFACE; ALBEDO; BELT; DAWN AB The surface of the asteroid Vesta has prominent near-infrared absorption bands characteristic of a range of pyroxenes, confirming a direct link to the basaltic howardite-eucrite-diogenite class of meteorites(1,2,3). Processes active in the space environment produce 'space weathering' products that substantially weaken or mask such diagnostic absorption on airless bodies observed elsewhere(4,5), and it has long been a mystery why Vesta's absorption bands are so strong. Analyses of soil samples from both the Moon(6) and the asteroid Itokawa(7) determined that nanophase metallic particles (commonly nanophase iron) accumulate on the rims of regolith grains with time, accounting for an observed optical degradation. These nanophase particles, believed to be related to solar wind and micrometeoroid bombardment processes, leave unique spectroscopic signatures that can be measured remotely(8-10) but require sufficient spatial resolution to discern the geologic context and history of the surface, which has not been achieved for Vesta until now. Here we report that Vesta shows its own form of space weathering, which is quite different from that of other airless bodies visited. No evidence is detected on Vesta for accumulation of lunar-like nanophase iron on regolith particles, even though distinct material exposed at several fresh craters becomes gradually masked and fades into the background as the craters age. Instead, spectroscopic data reveal that on Vesta a locally homogenized upper regolith is generated with time through small-scale mixing of diverse surface components. C1 [Pieters, C. M.] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA. [Ammannito, E.; De Sanctis, M. C.] ARTOV, INAF, Ist Astrofis & Planetol Spaziali, I-00133 Rome, Italy. [Blewett, D. T.; Denevi, B. W.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Gaffey, M. J.] Univ N Dakota, Dept Space Studies, Grand Forks, ND 58202 USA. [Le Corre, L.; Nathues, A.; Reddy, V.] Max Planck Inst Solar Syst Res, D-37191 Katlenburg Lindau, Germany. [Li, J. -Y.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Marchi, S.] NASA, Lunar Sci Inst, Boulder, CO 80302 USA. [McCord, T. B.] Bear Fight Inst, Winthrop, WA 98862 USA. [McFadden, L. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Mittlefehldt, D. W.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Palmer, E.] Planetary Sci Inst, Tucson, AZ 85719 USA. [Raymond, C. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Russell, C. T.] Univ Calif Los Angeles, Los Angeles, CA 90095 USA. RP Pieters, CM (reprint author), Brown Univ, Dept Geol Sci, Providence, RI 02912 USA. EM carle_pieters@brown.edu RI Russell, Christopher/E-7745-2012; McFadden, Lucy-Ann/I-4902-2013; De Sanctis, Maria Cristina/G-5232-2013; Denevi, Brett/I-6502-2012; Blewett, David/I-4904-2012; OI Le Corre, Lucille/0000-0003-0349-7932; Russell, Christopher/0000-0003-1639-8298; McFadden, Lucy-Ann/0000-0002-0537-9975; De Sanctis, Maria Cristina/0000-0002-3463-4437; Denevi, Brett/0000-0001-7837-6663; Blewett, David/0000-0002-9241-6358; Reddy, Vishnu/0000-0002-7743-3491 FU NASA [NNM05AA86C]; NASA Dawn participating scientist programme FX We acknowledge the Dawn Instrument, Flight and Operations teams for the successful development, cruise, orbital insertion and operations of the Dawn spacecraft at Vesta. US team members are supported by the NASA Discovery Program through contract NNM05AA86C to the University of California, Los Angeles and by the NASA Dawn participating scientist programme. NR 31 TC 71 Z9 71 U1 4 U2 25 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD NOV 1 PY 2012 VL 491 IS 7422 BP 79 EP 82 DI 10.1038/nature11534 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 028PM UT WOS:000310434500033 PM 23128227 ER PT J AU McCord, TB Li, JY Combe, JP McSween, HY Jaumann, R Reddy, V Tosi, F Williams, DA Blewett, DT Turrini, D Palomba, E Pieters, CM De Sanctis, MC Ammannito, E Capria, MT Le Corre, L Longobardo, A Nathues, A Mittlefehldt, DW Schroder, SE Hiesinger, H Beck, AW Capaccioni, F Carsenty, U Keller, HU Denevi, BW Sunshine, JM Raymond, CA Russell, CT AF McCord, T. B. Li, J. -Y. Combe, J. -P. McSween, H. Y. Jaumann, R. Reddy, V. Tosi, F. Williams, D. A. Blewett, D. T. Turrini, D. Palomba, E. Pieters, C. M. De Sanctis, M. C. Ammannito, E. Capria, M. T. Le Corre, L. Longobardo, A. Nathues, A. Mittlefehldt, D. W. Schroeder, S. E. Hiesinger, H. Beck, A. W. Capaccioni, F. Carsenty, U. Keller, H. U. Denevi, B. W. Sunshine, J. M. Raymond, C. A. Russell, C. T. TI Dark material on Vesta from the infall of carbonaceous volatile-rich material SO NATURE LA English DT Article ID DAWN MISSION; HETEROGENEITY; MINERALOGY; SURFACE; ALBEDO; COLOR; WATER; MOON AB Localized dark and bright materials, often with extremely different albedos, were recently found on Vesta's surface(1,2). The range of albedos is among the largest observed on Solar System rocky bodies. These dark materials, often associated with craters, appear in ejecta and crater walls, and their pyroxene absorption strengths are correlated with material brightness. It was tentatively suggested that the dark material on Vesta could be either exogenic, from carbon-rich, low-velocity impactors, or endogenic, from freshly exposed mafic material or impact melt, created or exposed by impacts. Here we report Vesta spectra and images and use them to derive and interpret the properties of the 'pure' dark and bright materials. We argue that the dark material is mainly from infall of hydrated carbonaceous material (like that found in a major class of meteorites and some comet surfaces(3-5)), whereas the bright material is the uncontaminated indigenous Vesta basaltic soil. Dark material from low-albedo impactors is diffused over time through the Vestan regolith by impact mixing, creating broader, diffuse darker regions and finally Vesta's background surface material. This is consistent with howardite-eucrite-diogenite meteorites coming from Vesta. C1 [McCord, T. B.; Combe, J. -P.] Bear Fight Inst, Winthrop, WA 98862 USA. [Li, J. -Y.] Planetary Sci Inst, Tucson, AZ 85719 USA. [McSween, H. Y.] Univ Tennessee, Knoxville, TN 37996 USA. [Jaumann, R.; Carsenty, U.] Inst Planetary Res, DLR, D-80302 Berlin, Germany. [Reddy, V.; Le Corre, L.; Nathues, A.; Schroeder, S. E.] Max Planck Inst Solar Syst Res, D-37191 Katlenburg, Germany. [Reddy, V.] Univ N Dakota, Grand Forks, ND 58202 USA. [Tosi, F.; Turrini, D.; Palomba, E.; De Sanctis, M. C.; Ammannito, E.; Capria, M. T.; Longobardo, A.; Capaccioni, F.] Ist Nazl Astrofis IASF, I-00133 Rome, Italy. [Williams, D. A.] Arizona State Univ, Tempe, AZ 85287 USA. [Blewett, D. T.; Denevi, B. W.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Pieters, C. M.] Brown Univ, Providence, RI 02912 USA. [Mittlefehldt, D. W.] NASA, Lyndon B Johnson Space Ctr, Astromat Res Off, Houston, TX 77058 USA. [Hiesinger, H.] Univ Munster, Inst Planetol, D-48149 Munster, Germany. [Beck, A. W.] Smithsonian Natl Museum Nat Hist, Dept Mineral Sci, Washington, DC 20024 USA. [Keller, H. U.] Inst Geophys & Extraterr Phys, D-38106 Braunschweig, Germany. [Sunshine, J. M.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Raymond, C. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Russell, C. T.] Univ Calif Los Angeles, Los Angeles, CA 90095 USA. RP McCord, TB (reprint author), Bear Fight Inst, 22 Fiddlers Rd,Box 667, Winthrop, WA 98862 USA. EM tmccord@bearfightinstitute.com; jean-philippe_combe@bearfightinstitutute.com RI Russell, Christopher/E-7745-2012; Schroder, Stefan/D-9709-2013; De Sanctis, Maria Cristina/G-5232-2013; Denevi, Brett/I-6502-2012; Blewett, David/I-4904-2012; Beck, Andrew/J-7215-2015; OI Le Corre, Lucille/0000-0003-0349-7932; Palomba, Ernesto/0000-0002-9101-6774; Tosi, Federico/0000-0003-4002-2434; Russell, Christopher/0000-0003-1639-8298; Capaccioni, Fabrizio/0000-0003-1631-4314; Schroder, Stefan/0000-0003-0323-8324; De Sanctis, Maria Cristina/0000-0002-3463-4437; Denevi, Brett/0000-0001-7837-6663; Blewett, David/0000-0002-9241-6358; Beck, Andrew/0000-0003-4455-2299; capria, maria teresa/0000-0002-9814-9588; Reddy, Vishnu/0000-0002-7743-3491; Turrini, Diego/0000-0002-1923-7740 FU NASA Dawn Project under UCLA; NASA Dawn at Vesta Participating Scientist program; Italian Space Agency; Max Planck Institute for Solar System Research; Germany Aerospace Agency (DLR) FX This research was supported by the NASA Dawn Project under contract from UCLA, by the NASA Dawn at Vesta Participating Scientist program, the Italian Space Agency, the Max Planck Institute for Solar System Research, and the Germany Aerospace Agency (DLR). We acknowledge the support of the Dawn Science, Instrument and Operations Teams. NR 23 TC 87 Z9 88 U1 4 U2 37 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD NOV 1 PY 2012 VL 491 IS 7422 BP 83 EP U93 DI 10.1038/nature11561 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 028PM UT WOS:000310434500034 PM 23128228 ER PT J AU Vicroy, DD Loeser, TD Schutte, A AF Vicroy, Dan D. Loeser, Thomas D. Schuette, Andreas TI Static and Forced-Oscillation Tests of a Generic Unmanned Combat Air Vehicle SO JOURNAL OF AIRCRAFT LA English DT Article AB A series of three wind-tunnel static and forced-oscillation tests were conducted on a model of a generic unmanned combat air vehicle. These tests are part of an international research effort to assess the state of the art of computational fluid dynamics methods to predict the static and dynamic stability and control characteristics. The experimental data set includes not only force and moment time histories, but also surface pressure and offbody particle image velocimetry measurements. The extent of the data precludes a full examination within the scope of this paper. This paper provides a general description and selected examples of the available static and dynamic data, as well as some of the observed trends. C1 [Vicroy, Dan D.] NASA, Langley Res Ctr, Flight Dynam Branch, Hampton, VA 23681 USA. [Loeser, Thomas D.] German Dutch Wind Tunnels, Low Speed Wind Tunnel Brunswick, D-38108 Braunschweig, Germany. [Schuette, Andreas] German Dutch Wind Tunnels, DLR, Inst Aerodynam & Flow Technol, D-38108 Braunschweig, Germany. RP Vicroy, DD (reprint author), NASA, Langley Res Ctr, Flight Dynam Branch, Mail Stop 308, Hampton, VA 23681 USA. FU German Federal Office of Defense Technology and Procurement; NASA FX The authors wish to thank the German Federal Office of Defense Technology and Procurement (BWB), which supported the work by funding the DLR, German Aerospace Center, project "UCAV 2010" and the NASA Fundamental Aeronautics Program's Subsonic Fixed Wing Project, which provided funding for the stability and control configuration (SACCON) model and NASA wind-tunnel testing. NR 21 TC 2 Z9 3 U1 1 U2 1 PU AMER INST AERONAUT ASTRONAUT PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0021-8669 J9 J AIRCRAFT JI J. Aircr. PD NOV-DEC PY 2012 VL 49 IS 6 BP 1558 EP 1583 DI 10.2514/1.C031501 PG 26 WC Engineering, Aerospace SC Engineering GA 060GH UT WOS:000312764000003 ER PT J AU Frink, NT Tormalm, M Schmidt, S AF Frink, Neal T. Tormalm, Magnus Schmidt, Stefan TI Three Unstructured Computational Fluid Dynamics Studies on Generic Uninhabited Combat Air Vehicle SO JOURNAL OF AIRCRAFT LA English DT Article ID TURBULENT FLOWS; MODEL AB Three independent studies from the United States (NASA), Sweden (Swedish Defense Research Agency), and Australia (Defense Science and Technology Organization) are analyzed to assess the state of current unstructured grid computational fluid dynamic tools and practices for predicting the complex static and dynamic aerodynamic and stability characteristics of a generic 53-deg swept, round-leading-edge uninhabited combat air vehicle configuration, called SACCON (which stands for "stability and control configuration"). NASA exercised the USM3D tetrahedral cell-centered flow solver, while the Swedish Defense Research Agency and the Defense Science and Technology Organization applied the Swedish Defense Research Agency/EDGE general-cell vertex-based solver. The authors primarily employ the Reynolds-averaged Navier-Stokes assumption, with a limited assessment of the EDGE detached eddy simulation extension, to explore sensitivities to grids and turbulence models. Correlations with experimental data are provided for force and moments, surface pressure, and off-body flow measurements. The vortical flowfield over SACCON proved extremely difficult to model adequately. As a general rule, the prospect of obtaining reasonable correlations of SACCON pitching moment characteristics with the Reynolds-averaged Navier-Stokes formulation is not promising, even for static cases. However, dynamic pitch oscillation results seem to produce a promising characterization of shapes for the lift and pitching moment hysteresis curves. Future studies of this configuration should include more investigation with higher-fidelity turbulence models such as detached eddy simulation. C1 [Frink, Neal T.] NASA, Langley Res Ctr, Configurat Aerodynam Branch, Res Directorate, Hampton, VA 23681 USA. [Tormalm, Magnus] Swedish Def Res Agcy, Dept Aeronaut & Syst Integrat, S-16490 Stockholm, Sweden. [Schmidt, Stefan] Def Sci & Technol Org, Air Vehicles Div, Fishermans Bend, Vic 3207, Australia. RP Frink, NT (reprint author), NASA, Langley Res Ctr, Configurat Aerodynam Branch, Res Directorate, MS 499, Hampton, VA 23681 USA. EM Neal.T.Frink@nasa.gov; Magnus.Tormalm@foi.se; Stefan.Schmidt@dsto.defence.gov.au FU Swedish Armed Forces FX The first author gratefully acknowledges the generous support for this work from the NASA Aviation Safety Program, Integrated Resilient Aircraft Controls project, and the Fundamental Aerodynamics Program, Subsonic Fixed Wing project, for the opportunity to participate in the NATO/RTO AVT-161 task group. The second author would like to thank the Swedish Armed Forces for financing the FOI research in this task group. The third author would like to thank NATO for allowing DSTO to make active contributions to research in AVT-161. NR 24 TC 1 Z9 1 U1 2 U2 6 PU AMER INST AERONAUT ASTRONAUT PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0021-8669 J9 J AIRCRAFT JI J. Aircr. PD NOV-DEC PY 2012 VL 49 IS 6 BP 1619 EP 1637 DI 10.2514/1.C031383 PG 19 WC Engineering, Aerospace SC Engineering GA 060GH UT WOS:000312764000007 ER PT J AU Kaul, UK Ahmad, J AF Kaul, Upender K. Ahmad, Jasim TI Skin-Friction Predictions on a Hovering Tilt-Rotor Blade SO JOURNAL OF AIRCRAFT LA English DT Article ID COMPUTATIONAL FLUID-DYNAMICS AB Skin-friction predictions on hovering XV-15 helicopter blades have been made with the OVERFLOW2 flow solver using the Spalart-Allmaras one-equation turbulence model. The figure of merit for the 10 deg collective pitch is predicted reasonably, and for the 3 deg collective pitch it is underpredicted in comparison with experimental data. The trend in the skin-friction predictions at the 10 deg collective pitch in the fully turbulent region is in good agreement with the experimental data at radial stations away from the hub. For the 3 deg collective pitch, the agreement in the fully turbulent region is not as good as for the 10 deg case. In the transition region, the predictions deviate significantly from the experimental data for both the cases. By modulating the turbulence viscosity a priori in the experimentally known transition zone in various ways, a measurable change was predicted in the behavior of skin friction over the blade. This change was observed to be significant for the 3 deg collective pitch. Skin-friction results corresponding to the fully laminar calculations are in good agreement with experimental skin friction in the laminar region for both of the collective pitch angles. C1 [Kaul, Upender K.; Ahmad, Jasim] NASA, Ames Res Ctr, Appl Modeling & Simulat Branch, Adv Supercomp Div, Moffett Field, CA 94035 USA. RP Kaul, UK (reprint author), NASA, Ames Res Ctr, Appl Modeling & Simulat Branch, Adv Supercomp Div, Moffett Field, CA 94035 USA. FU Subsonic Rotary Wing Project of the NASA Fundamental Aeronautics Program FX This work was funded by the Subsonic Rotary Wing Project of the NASA Fundamental Aeronautics Program. The authors would like to acknowledge helpful information on the experimental results provided by Gloria Yamauchi throughout the course of this study. The authors would also like to thank Alan Wadcock for providing reference experimental data and the image of the 80 by 120 ft wind-tunnel experiment setup. Finally, a critical review of the paper by Cetin Kiris, Mark Potsdam, and Alan Wadcock is gratefully acknowledged. NR 29 TC 1 Z9 2 U1 0 U2 2 PU AMER INST AERONAUT ASTRONAUT PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0021-8669 J9 J AIRCRAFT JI J. Aircr. PD NOV-DEC PY 2012 VL 49 IS 6 BP 1726 EP 1738 DI 10.2514/1.C031401 PG 13 WC Engineering, Aerospace SC Engineering GA 060GH UT WOS:000312764000015 ER PT J AU Morelli, EA AF Morelli, Eugene A. TI Flight Test Maneuvers for Efficient Aerodynamic Modeling SO JOURNAL OF AIRCRAFT LA English DT Article AB Novel flight test maneuvers for efficient aerodynamic modeling were developed and demonstrated in flight. Orthogonal optimized multisine inputs were applied to aircraft control surfaces to excite aircraft dynamic response in all six degrees of freedom simultaneously, while keeping the aircraft close to chosen reference flight conditions. Each maneuver was designed for a specific modeling task that cannot be adequately or efficiently accomplished using conventional flight test maneuvers. The maneuvers are described and explained, then demonstrated on a subscale jet transport aircraft in flight. Real-time and post-flight modeling results from equation-error parameter estimation in the frequency domain were used to show the effectiveness and efficiency of the maneuvers, as well as the quality of the aerodynamic models that can be identified from the resultant flight data. C1 NASA, Langley Res Ctr, Dynam Syst & Control Branch, Hampton, VA 23681 USA. RP Morelli, EA (reprint author), NASA, Langley Res Ctr, Dynam Syst & Control Branch, Mail Stop 308, Hampton, VA 23681 USA. FU NASA Aviation Safety Program, Integrated Resilient Aircraft Control project; NASA Aviation Safety Program, Vehicle Safety Systems Technology project FX Research in dynamic modeling is funded by the NASA Aviation Safety Program, Integrated Resilient Aircraft Control and Vehicle Safety Systems Technology projects. The efforts of the Airborne Subscale Transport Aircraft Research (AirSTAR) flight-test team at NASA Langley Research Center in building and testing the aircraft and associated systems, carefully calibrating the instrumentation, and carrying out the flight operations to collect the high-quality flight data used in this study, are gratefully acknowledged. NR 17 TC 4 Z9 5 U1 2 U2 6 PU AMER INST AERONAUT ASTRONAUT PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0021-8669 J9 J AIRCRAFT JI J. Aircr. PD NOV-DEC PY 2012 VL 49 IS 6 BP 1857 EP 1867 DI 10.2514/1.C031699 PG 11 WC Engineering, Aerospace SC Engineering GA 060GH UT WOS:000312764000027 ER PT J AU Ku, JT Ottenstein, L Douglas, D Hoang, T AF Ku, Jentung Ottenstein, Laura Douglas, Donya Hoang, Triem TI Technology Overview of a Multi-Evaporator Miniature Loop Heat Pipe for Spacecraft Applications SO JOURNAL OF SPACECRAFT AND ROCKETS LA English DT Article; Proceedings Paper CT 48th AIAA Aerospace Sciences Meeting and Exhibit / New Horizons Forum and Aerospace Exposition CY JAN 04-08, 2010 CL Orlando, FL SP AIAA AB A miniature loop heat pipe with multiple evaporators and multiple condensers was developed for thermal control of small spacecraft and instruments requiring low mass, low power, and compactness. Multiple evaporators afford flexible placement of instruments inside the spacecraft and facilitate heat-load sharing among instruments. Multiple condensers allow the radiators to be placed at various locations on the spacecraft surface and exposed to different thermal environments. Thermoelectric converters are used to provide heating and cooling to the reservoir for loop operating temperature control. A breadboard and a protoflight unit of the miniature loop heat pipe with two evaporators and two condensers were built and tested in a thermal vacuum chamber to demonstrate the thermal performance. In addition, an analytical model was developed to simulate the steady-state and transient behaviors of the miniature loop heat pipe during thermal performance tests. C1 [Ku, Jentung; Ottenstein, Laura] NASA, Goddard Space Flight Ctr, Thermal Engn Branch, Greenbelt, MD 20771 USA. [Douglas, Donya] NASA, Goddard Space Flight Ctr, Instrument Syst Branch, Greenbelt, MD 20771 USA. [Hoang, Triem] TTH Res Inc, Clifton, VA 20124 USA. RP Ku, JT (reprint author), NASA, Goddard Space Flight Ctr, Thermal Engn Branch, Greenbelt, MD 20771 USA. NR 30 TC 2 Z9 2 U1 2 U2 19 PU AMER INST AERONAUT ASTRONAUT PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0022-4650 J9 J SPACECRAFT ROCKETS JI J. Spacecr. Rockets PD NOV-DEC PY 2012 VL 49 IS 6 BP 999 EP 1007 DI 10.2514/1.51348 PG 9 WC Engineering, Aerospace SC Engineering GA 064NS UT WOS:000313082900005 ER PT J AU Ku, JT Ottenstein, L Douglas, D Hoang, T AF Ku, Jentung Ottenstein, Laura Douglas, Donya Hoang, Triem TI Validation Design for a Multi-Evaporator Miniature Loop Heat Pipe for Spacecraft Applications SO JOURNAL OF SPACECRAFT AND ROCKETS LA English DT Article; Proceedings Paper CT 48th AIAA Aerospace Sciences Meeting and Exhibit / New Horizons Forum and Aerospace Exposition CY JAN 04-08, 2010 CL Orlando, FL SP AIAA AB A miniature loop heat pipe with multiple evaporators and multiple condensers for thermal control of small spacecraft and instruments was successfully developed. The miniature loop heat pipe had a 6.35 mm primary wick and used thermoelectric converters to control its operating temperature. A breadboard and a protoflight unit were built and tested under laboratory and thermal vacuum environments. Both loops demonstrated excellent thermal performance, including 100% startup success, tight temperature control under various heat loads and sink conditions, and heat-load sharing between evaporators. An analytical model designed to simulate steady-state and transient behaviors of the miniature loop heat pipe was also developed, and the model predictions agreed very well with experimental data. The maturity of this technology has been advanced from "proof of concept" to "prototype demonstration in a relevant environment." C1 [Ku, Jentung; Ottenstein, Laura] NASA, Goddard Space Flight Ctr, Thermal Engn Branch, Greenbelt, MD 20771 USA. [Douglas, Donya] NASA, Goddard Space Flight Ctr, Syst Engn Serv, Greenbelt, MD 20771 USA. [Douglas, Donya] NASA, Goddard Space Flight Ctr, Adv Concepts Branch, Greenbelt, MD 20771 USA. [Hoang, Triem] TTH Res Inc, Clifton, VA 20124 USA. RP Ku, JT (reprint author), NASA, Goddard Space Flight Ctr, Thermal Engn Branch, Greenbelt, MD 20771 USA. NR 34 TC 0 Z9 0 U1 2 U2 10 PU AMER INST AERONAUT ASTRONAUT PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0022-4650 J9 J SPACECRAFT ROCKETS JI J. Spacecr. Rockets PD NOV-DEC PY 2012 VL 49 IS 6 BP 1008 EP 1018 DI 10.2514/1.51349 PG 11 WC Engineering, Aerospace SC Engineering GA 064NS UT WOS:000313082900006 ER PT J AU Everline, CJ AF Everline, Chester J. TI Bayesian Approach to Quantifying Epistemic Uncertainty in a Processor Availability Model SO JOURNAL OF SPACECRAFT AND ROCKETS LA English DT Article ID PROBABILISTIC RISK-ASSESSMENT; SYSTEMS; RELIABILITY; COMPONENTS AB It is often necessary to use a combination of testing and analysis to demonstrate compliance with quantitative performance requirements. Increasingly, the demonstration must establish that requirements are satisfied with a certain level of confidence. As an example, a processor intended for space applications may be required to have a certain reliability or availability (e.g., at least 99.9%) with high confidence (e.g., 95%). This paper examines the application of Bayesian statistics and Monte Carlo simulation to such situations, focusing on quantifying epistemic uncertainty associated with the quantity of available data, the validity of alternative models, probabilistically combining alternative models when appropriate, and estimating epistemic uncertainty associated with certain aspects of model completeness. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Everline, CJ (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,Mail Stop 156-206, Pasadena, CA 91109 USA. EM Chester.J.Everline@jpl.nasa.gov FU NASA FX The research described in this paper was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. I especially thank John F. Stocky and Raphael R. Some of the Jet Propulsion Laboratory for their support of this effort. NR 31 TC 0 Z9 0 U1 0 U2 2 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 NOV-DEC PY 2012 VL 49 IS 6 BP 1019 EP 1031 DI 10.2514/1.51352 PG 13 WC Engineering, Aerospace SC Engineering GA 064NS UT WOS:000313082900007 ER PT J AU Mishra, K Trivedi, KS Some, RR AF Mishra, Kesari Trivedi, Kishor S. Some, Raphael R. TI Uncertainty Analysis of the Remote Exploration and Experimentation System SO JOURNAL OF SPACECRAFT AND ROCKETS LA English DT Article ID APPROXIMATE CONFIDENCE LIMITS; INPUT VARIABLES; COMPLEX-SYSTEMS; RELIABILITY; SERIES; COMPONENT; RISK AB This paper discusses a method for computing the uncertainty in output metrics of stochastic models due to epistemic uncertainties in the model-input parameters. The method is illustrated by applying it to compute the distribution and confidence interval of the reliability of the Remote Exploration and Experimentation system. This method makes use of Monte Carlo sampling and propagates the epistemic uncertainty in the model parameters through the system reliability model. It acts as a wrapper to already-existing models as well as their solution tools/techniques and has a wide range of applicability. Although it is a sampling-based method, no simulation is carried out when performing uncertainty propagation through analytic models, but analytic or analytic numeric solution of the underlying stochastic model is performed for each set of input-parameter values, sampled from their distributions. Using the input epistemic uncertainty, in the form of 95% confidence intervals of input parameters of the stochastic model, the two-sided 95% confidence interval of reliability of the Remote Exploration and Experimentation system at a time t = 5 years is computed to be (0.949485, 0.981994). C1 [Mishra, Kesari; Trivedi, Kishor S.] Duke Univ, Dept Elect & Comp Engn, Durham, NC 27708 USA. [Some, Raphael R.] CALTECH, Jet Prop Lab, Autonomous Syst Div, Pasadena, CA 91109 USA. RP Mishra, K (reprint author), Duke Univ, Dept Elect & Comp Engn, Durham, NC 27708 USA. EM km@ee.duke.edu; kst@ee.duke.edu; Raphael.R.Some@jpl.nasa.gov FU National Aeronautics and Space Administration FX 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 44 TC 0 Z9 0 U1 0 U2 1 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 NOV-DEC PY 2012 VL 49 IS 6 BP 1032 EP 1042 DI 10.2514/1.51380 PG 11 WC Engineering, Aerospace SC Engineering GA 064NS UT WOS:000313082900008 ER PT J AU Cruden, BA Prabhu, D Martinez, R AF Cruden, Brett A. Prabhu, Dinesh Martinez, Ramon TI Absolute Radiation Measurement in Venus and Mars Entry Conditions SO JOURNAL OF SPACECRAFT AND ROCKETS LA English DT Article; Proceedings Paper CT 10th AIAA/ASME Joint Thermophysics and Heat Transfer Conference CY JUN 28-JUL 01, 2010 CL Chicago, IL SP AIAA, ASME ID CO2-N-2 PLASMAS AB Comparisons of experimental characterization and model predictions of entry radiation relevant to Mars and Venus exploration are presented. Characterization is performed in the recently upgraded Electric Arc Shock Tube facility at NASA Ames Research Center. Tests are performed in simulated Mars (96% CO2, 4% N-2) and Venus (96.5% CO2, 3.5% N-2) atmospheres at downstream pressures and incident velocities spanning from 0.1 to 2.0 torr and 3-12 km/s. Velocity and pressure conditions were chosen based on expected flight conditions (direct entry or aerocapture) for Mars and Venus atmospheres. The absolute radiance data are spatially and spectrally resolved and span the vacuum ultraviolet through midinfrared (120-1650 nm, 3-5 mu m). Resolved spectra of the CO fourth positive band in the vacuum ultraviolet are reported for the first time. Measurements of CO2 molecular vibrational radiation are also attempted at low-velocity conditions. Radiation modeled using an equilibrium assumption with the NEQAIR code compares favorably to measured radiation under some, but not all, conditions. C1 [Cruden, Brett A.; Prabhu, Dinesh; Martinez, Ramon] NASA, ERC Inc, Ames Res Ctr, Aerothermodynam Branch, Moffett Field, CA 94035 USA. RP Cruden, BA (reprint author), NASA, ERC Inc, Ames Res Ctr, Aerothermodynam Branch, Mail Stop 230-3, Moffett Field, CA 94035 USA. EM Brett.A.Cruden@nasa.gov NR 20 TC 7 Z9 7 U1 0 U2 3 PU AMER INST AERONAUT ASTRONAUT PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0022-4650 J9 J SPACECRAFT ROCKETS JI J. Spacecr. Rockets PD NOV-DEC PY 2012 VL 49 IS 6 BP 1069 EP 1079 DI 10.2514/1.A32204 PG 11 WC Engineering, Aerospace SC Engineering GA 064NS UT WOS:000313082900011 ER PT J AU Yap, KC Macias, J Kaouk, M Gafka, TL Kerr, JH AF Yap, Keng C. Macias, Jesus Kaouk, Mohamed Gafka, Tammy L. Kerr, Justin H. TI Structural Health Monitoring and Risk Management of a Reusable Launch Vehicle SO JOURNAL OF SPACECRAFT AND ROCKETS LA English DT Article; Proceedings Paper CT 19th AIAA/ASME/AHS Adaptive Structures Conference CY APR 04-07, 2011 CL Denver, CO SP AIAA, ASME, AHS ID RANK PERTURBATION-THEORY AB A structural-health-monitoring system can contribute to the risk management of a structure operating under hazardous conditions. An example is the wing leading-edge impact-detection system that monitors the debris hazards to the Space Shuttle Orbiter's reinforced carbon carbon panels. Since return to flight after the Columbia accident, the system was developed and subsequently deployed on board the orbiter to detect ascent and on-orbit debris impacts, so as to support the assessment of wing leading edge structural integrity before orbiter reentry. As structural health monitoring is inherently an inverse problem, the analyses involved, including those performed for this system, tend to be associated with significant uncertainty. The use of probabilistic approaches to handle the uncertainty has resulted in the successful implementation of many development and application milestones. C1 [Yap, Keng C.] Boeing Space Explorat, Loads & Dynam, Boeing Def Space & Secur, Houston, TX 77059 USA. [Macias, Jesus] United Space Alliance, Vehicle & Syst Anal, USA Orbiter Element, Houston, TX 77058 USA. [Kaouk, Mohamed] NASA, Struct & Dynam ES6, NASA JSC, Houston, TX 77058 USA. [Kerr, Justin H.] NASA, Space Shuttle Orbiter Project Off MV6, NASA JSC, Houston, TX 77058 USA. RP Yap, KC (reprint author), Boeing Space Explorat, Loads & Dynam, Boeing Def Space & Secur, Houston, TX 77059 USA. EM Keng.C.Yap@Boeing.com; Jesus.Macias@USA-SpaceOps.com; Mohamed.Kaouk@NASA.com; Tammy.L.Gafka@NASA.com; Justin.H.Kerr@NASA.gov NR 40 TC 1 Z9 1 U1 1 U2 9 PU AMER INST AERONAUT ASTRONAUT PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0022-4650 J9 J SPACECRAFT ROCKETS JI J. Spacecr. Rockets PD NOV-DEC PY 2012 VL 49 IS 6 BP 1099 EP 1108 DI 10.2514/1.A32156 PG 10 WC Engineering, Aerospace SC Engineering GA 064NS UT WOS:000313082900014 ER PT J AU Schuerger, AC Golden, DC Ming, DW AF Schuerger, Andrew C. Golden, D. C. Ming, Doug W. TI Biotoxicity of Mars soils: 1. Dry deposition of analog soils on microbial colonies and survival under Martian conditions SO PLANETARY AND SPACE SCIENCE LA English DT Article DE Biotoxic soils; Mars geochemistry; Biocidal soils; Regolith; Exobiology ID PHOENIX LANDING SITE; X-RAY SPECTROMETER; SPACECRAFT SURFACES; GUSEV CRATER; MOSSBAUER SPECTROMETER; CHEMICAL-COMPOSITION; TERRESTRIAL ANALOGS; BACILLUS-SUBTILIS; PATHFINDER SITE; SPIRIT ROVER AB Six Mars analog soils were created to simulate a range of potentially biotoxic geochemistries relevant to the survival of terrestrial microorganisms on Mars, and included basalt-only (non-toxic control), salt, acidic, alkaline, aeolian, and perchlorate rich geochemistries. Experiments were designed to simulate the dry-deposition of Mars soils onto spacecraft surfaces during an active descent landing scenario with propellant engines. Six eubacteria were initially tested for tolerance to desiccation, and the spore-former Bacillus subtilis HA101 and non-spore former Enterococcus faecalis ATCC 29212 were identified to be strongly resistant (HA101) and moderately resistant (29212) to desiccation at 24 degrees C. Furthermore, tests with B. subtilis and E. faecalis demonstrated that at least 1 mm of Mars analog soil was required to fully attenuate the biocidal effects of a simulated Mars-normal equatorial UV flux. Biotoxicity experiments were conducted under simulated Martian conditions of 6.9 mbar, - 10 degrees C, CO2-enriched anoxic atmosphere, and a simulated equatorial solar spectrum (200-1100 nm) with an optical depth of 0.1. For B. subtilis, the six analog soils were found, in general, to be of low biotoxicity with only the high salt and acidic soils exhibiting the capacity to inactivate a moderate number of spores ( < 1 log reductions) exposed 7 days to the soils under simulated Martian conditions. In contrast, the overall response of E. faecalis to the analog soils was more dramatic with between two and three orders of magnitude reductions in viable cells for most soils, and between six and seven orders of magnitude reductions observed for the high-salt soil. Results suggest that Mars soils are likely not to be overtly biotoxic to terrestrial microorganisms, and suggest that the soil geochemistries on Mars will not preclude the habitability of the Martian surface. (C) 2012 Elsevier Ltd. All rights reserved, C1 [Schuerger, Andrew C.] Univ Florida, Dept Plant Pathol, Space Life Sci Lab, Kennedy Space Ctr, FL 32899 USA. [Golden, D. C.] ESCG, Houston, TX 77058 USA. [Ming, Doug W.] NASA, Lyndon B Johnson Space Ctr, Astromat Res & Explorat Sci Off, Mail Code 7X, Houston, TX 77058 USA. RP Schuerger, AC (reprint author), Univ Florida, Dept Plant Pathol, Space Life Sci Lab, Bldg M6-1025, Kennedy Space Ctr, FL 32899 USA. EM schuerg@ufl.edu; d.c.golden@nasa.gov; douglas.w.ming@nasa.gov FU Planetary Protection grant [NNX08AQ81A] FX The research was supported by a Planetary Protection grant (NNX08AQ81A). NR 60 TC 6 Z9 6 U1 2 U2 28 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0032-0633 J9 PLANET SPACE SCI JI Planet Space Sci. PD NOV PY 2012 VL 72 IS 1 SI SI BP 91 EP 101 DI 10.1016/j.pss.2012.07.026 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 058DZ UT WOS:000312615600010 ER PT J AU Ciufolini, I Paolozzi, A Pavlis, E Ries, J Gurzadyan, V Koenig, R Matzner, R Penrose, R Sindoni, G AF Ciufolini, Ignazio Paolozzi, Antonio Pavlis, Erricos Ries, John Gurzadyan, Vahe Koenig, Rolf Matzner, Richard Penrose, Roger Sindoni, Giampiero TI Testing General Relativity and gravitational physics using the LARES satellite SO EUROPEAN PHYSICAL JOURNAL PLUS LA English DT Article ID ACCELERATING UNIVERSE; DARK ENERGY; SUPERNOVAE; LAGEOS; ORBIT; CONFIRMATION; GRAVITY; MOTION; SPACE; DRAG AB The discovery of the accelerating expansion of the Universe, thought to be driven by a mysterious form of "dark energy" constituting most of the Universe, has further revived the interest in testing Einstein's theory of General Relativity. At the very foundation of Einstein's theory is the geodesic motion of a small, structureless test-particle. Depending on the physical context, a star, planet or satellite can behave very nearly like a test-particle, so geodesic motion is used to calculate the advance of the perihelion of a planet's orbit, the dynamics of a binary pulsar system and of an Earth-orbiting satellite. Verifying geodesic motion is then a test of paramount importance to General Relativity and other theories of fundamental physics. On the basis of the first few months of observations of the recently launched satellite LARES, its orbit shows the best agreement of any satellite with the test-particle motion predicted by General Relativity. That is, after modelling its known non-gravitational perturbations, the LARES orbit shows the smallest deviations from geodesic motion of any artificial satellite: its residual mean acceleration away from geodesic motion is less than 0.5 x 10(-12) m/s(2). LARES-type satellites can thus be used for accurate measurements and for tests of gravitational and fundamental physics. Already with only a few months of observation, LARES provides smaller scatter in the determination of several low-degree geopotential coefficients (Earth gravitational deviations from sphericity) than available from observations of any other satellite or combination of satellites. C1 [Ciufolini, Ignazio] Univ Salento, Dipartimento Ingn Innovaz, Lecce, Italy. [Ciufolini, Ignazio] Ist Nazl Fis Nucl, I-73100 Lecce, Italy. [Paolozzi, Antonio; Sindoni, Giampiero] Univ Roma La Sapienza, Scuola Ingn Aerosp, Rome, Italy. [Paolozzi, Antonio; Sindoni, Giampiero] Univ Roma La Sapienza, DIAEE, Rome, Italy. [Pavlis, Erricos] NASA, Goddard Space Flight Ctr, Planetary Geodynam Lab, Greenbelt, MD 20771 USA. [Ries, John] Univ Texas Austin, Ctr Space Res, Austin, TX 78712 USA. [Gurzadyan, Vahe] Alikhanian Natl Lab, Ctr Cosmol & Astrophys, Yerevan, Armenia. [Koenig, Rolf] GFZ German Res Ctr Geosci, Helmholtz Ctr Potsdam, Potsdam, Germany. [Matzner, Richard] Univ Texas Austin, Ctr Relat, Austin, TX 78712 USA. [Penrose, Roger] Univ Oxford, Math Inst, Oxford OX1 2JD, England. RP Ciufolini, I (reprint author), Univ Salento, Dipartimento Ingn Innovaz, Lecce, Italy. EM ignazio.ciufolini@gmail.com FU Italian Space Agency [I/043/08/0, I/043/08/1]; NASA [NNG06DA07C, NNX09AU86G] FX The authors gratefully acknowledge the International Laser Ranging Service for providing high-quality laser ranging tracking of the LARES satellites. I. Ciufolini and A. Paolozzi gratefully acknowledge the support of the Italian Space Agency, Grants I/043/08/0 and I/043/08/1, J.C. Ries the support of NASA Contract NNG06DA07C, and E. C. Pavlis and R. A. Matzner the support of NASA Grant NNX09AU86G. NR 34 TC 38 Z9 38 U1 0 U2 6 PU SPRINGER HEIDELBERG PI HEIDELBERG PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY SN 2190-5444 J9 EUR PHYS J PLUS JI Eur. Phys. J. Plus PD NOV PY 2012 VL 127 IS 11 AR 133 DI 10.1140/epjp/i2012-12133-8 PG 7 WC Physics, Multidisciplinary SC Physics GA 056ZU UT WOS:000312532100002 ER PT J AU Reddy, V Le Corre, L O'Brien, DP Nathues, A Cloutis, EA Durda, DD Bottke, WF Bhatt, MU Nesvorny, D Buczkowski, D Scully, JEC Palmer, EM Sierks, H Mann, PJ Becker, KJ Beck, AW Mittlefehldt, D Li, JY Gaskell, R Russell, CT Gaffey, MJ McSween, HY McCord, TB Combe, JP Blewett, D AF Reddy, Vishnu Le Corre, Lucille O'Brien, David P. Nathues, Andreas Cloutis, Edward A. Durda, Daniel D. Bottke, William F. Bhatt, Megha U. Nesvorny, David Buczkowski, Debra Scully, Jennifer E. C. Palmer, Elizabeth M. Sierks, Holger Mann, Paul J. Becker, Kris J. Beck, Andrew W. Mittlefehldt, David Li, Jian-Yang Gaskell, Robert Russell, Christopher T. Gaffey, Michael J. McSween, Harry Y. McCord, Thomas B. Combe, Jean-Philippe Blewett, David TI Delivery of dark material to Vesta via carbonaceous chondritic impacts SO ICARUS LA English DT Article DE Asteroid Vesta; Asteroids, Composition; Mineralogy; Spectroscopy ID ASTEROID 4 VESTA; SOLAR-SYSTEM; EXPLOSIVE ERUPTIONS; PARENT BODY; ORIGIN; SURFACE; HETEROGENEITY; MINERALOGY; 4-VESTA; CLASTS AB NASA's Dawn spacecraft observations of Asteroid (4) Vesta reveal a surface with the highest albedo and color variation of any asteroid we have observed so far. Terrains rich in low albedo dark material (DM) have been identified using Dawn Framing Camera (FC) 0.75 mu m filter images in several geologic settings: associated with impact craters (in the ejecta blanket material and/or on the crater walls and rims); as flow-like deposits or rays commonly associated with topographic highs; and as dark spots (likely secondary impacts) nearby impact craters. This DM could be a relic of ancient volcanic activity or exogenic in origin. We report that the majority of the spectra of DM are similar to carbonaceous chondrite meteorites mixed with materials indigenous to Vesta. Using high-resolution seven color images we compared DM color properties (albedo, band depth) with laboratory measurements of possible analog materials. Band depth and albedo of DM are identical to those of carbonaceous chondrite xenolith-rich howardite Mt. Pratt (PRA) 04401: Laboratory mixtures of Murchison CM2 carbonaceous chondrite and basaltic eucrite Millbillillie also show band depth and albedo affinity to DM. Modeling of carbonaceous chondrite abundance in DM (1-6 vol.%) is consistent with howardite meteorites. We find no evidence for large-scale volcanism (exposed dikes/pyroclastic falls) as the source of DM. Our modeling efforts using impact crater scaling laws and numerical models of ejecta reaccretion suggest the delivery and emplacement of this DM on Vesta during the formation of the similar to 400 km Veneneia basin by a low-velocity (<2 km/s) carbonaceous impactor. This discovery is important because it strengthens the long-held idea that primitive bodies are the source of carbon and probably volatiles in the early Solar System. (C) 2012 Elsevier Inc. All rights reserved. C1 [Reddy, Vishnu; Le Corre, Lucille; Nathues, Andreas; Bhatt, Megha U.; Sierks, Holger] Max Planck Inst Solar Syst Res, D-37191 Katlenburg Lindau, Germany. [Reddy, Vishnu; Gaffey, Michael J.] Univ N Dakota, Dept Space Studies, Grand Forks, ND 58201 USA. [O'Brien, David P.; Gaskell, Robert] Planetary Sci Inst, Tucson, AZ USA. [Cloutis, Edward A.; Mann, Paul J.] Univ Winnipeg, Dept Geog, Winnipeg, MB R3B 2E9, Canada. [Durda, Daniel D.; Bottke, William F.; Nesvorny, David] SW Res Inst, Boulder, CO USA. [Buczkowski, Debra; Blewett, David] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA. [Scully, Jennifer E. C.; Palmer, Elizabeth M.; Russell, Christopher T.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90024 USA. [Becker, Kris J.] US Geol Survey, Astrogeol Sci Ctr, Flagstaff, AZ 86001 USA. [Beck, Andrew W.] Smithsonian Natl Museum Nat Hist, Dept Mineral Sci, Washington, DC USA. [Mittlefehldt, David] NASA Johnson Space Ctr, Astromat Res Off, Houston, TX USA. [Li, Jian-Yang] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [McSween, Harry Y.] Univ Tennessee, Dept Earth & Planetary Sci, Knoxville, TN USA. [McCord, Thomas B.; Combe, Jean-Philippe] Bear Fight Inst, Winthrop, WA USA. RP Reddy, V (reprint author), Max Planck Inst Solar Syst Res, D-37191 Katlenburg Lindau, Germany. EM reddy@mps.mpg.de RI Blewett, David/I-4904-2012; Beck, Andrew/J-7215-2015; OI Le Corre, Lucille/0000-0003-0349-7932; Blewett, David/0000-0002-9241-6358; Beck, Andrew/0000-0003-4455-2299; Reddy, Vishnu/0000-0002-7743-3491 FU Max Planck Society; German Space Agency, DLR; Dawn at Vesta Participating Scientist Program [NNX10AR22G]; CFI; MRIF; CSA; University of Winnipeg FX We thank the Dawn team for the development, cruise, orbital insertion, and operations of the Dawn spacecraft at Vesta. The Framing Camera project is financially supported by the Max Planck Society and the German Space Agency, DLR. We also thank the Dawn at Vesta Participating Scientist Program (NNX10AR22G) for funding the research. Dawn data is archived with the NASA Planetary Data System. EAC thanks CFI, MRIF, CSA, and the University of Winnipeg for support of this project and the necessary infrastructure. We thank Paul Buchanan (Kilgore College) and Tom Burbine (Mt Holyoke College) for their helpful reviews to improve the manuscript. VR would like to thank Richard Binzel (MIT), Rhiannon Mayne (TCU), and Guneshwar Thangjam (MPS) for their helpful suggestions to improve the manuscript. NR 61 TC 89 Z9 90 U1 2 U2 23 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 J9 ICARUS JI Icarus PD NOV-DEC PY 2012 VL 221 IS 2 BP 544 EP 559 DI 10.1016/j.icarus.2012.08.011 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 055RL UT WOS:000312434300007 ER PT J AU Fletcher, LN Hesman, BE Achterberg, RK Irwin, PGJ Bjoraker, G Gorius, N Hurley, J Sinclair, J Orton, GS Legarreta, J Garcia-Melendo, E Sanchez-Lavega, A Read, PL Simon-Miller, AA Flasar, FM AF Fletcher, Leigh N. Hesman, B. E. Achterberg, R. K. Irwin, P. G. J. Bjoraker, G. Gorius, N. Hurley, J. Sinclair, J. Orton, G. S. Legarreta, J. Garcia-Melendo, E. Sanchez-Lavega, A. Read, P. L. Simon-Miller, A. A. Flasar, F. M. TI The origin and evolution of Saturn's 2011-2012 stratospheric vortex SO ICARUS LA English DT Article DE Saturn; Atmospheres, Composition; Atmospheres, Structure ID ROTOTRANSLATIONAL ABSORPTION-SPECTRA; GREAT WHITE SPOT; INFRARED MEASUREMENTS; UPPER TROPOSPHERE; THERMAL STRUCTURE; MOIST CONVECTION; LINE PARAMETERS; OUTER PLANETS; ATMOSPHERE; TEMPERATURES AB The planet-encircling springtime storm in Saturn's troposphere (December 2010-July 2011, Fletcher, L.N. et al. [2011]. Science 332, 1413-1414; Sanchez-Lavega, A. et al. [2011]. Nature 475, 71-74; Fischer, G. et al. [2011]. Nature 475, 75-77) produced dramatic perturbations to stratospheric temperatures, winds and composition at mbar pressures that persisted long after the tropospheric disturbance had abated. Thermal infrared (IR) spectroscopy from the Cassini Composite Infrared Spectrometer (CIRS), supported by ground-based IR imaging from the VISIR instrument on the Very Large Telescope and the MIRSI instrument on NASA's IRTF, is used to track the evolution of a large, hot stratospheric anticyclone between January 2011 and March 2012. The evolutionary sequence can be divided into three phases: (I) the formation and intensification of two distinct warm airmasses near 0.5 mbar between 25 and 35 degrees N (B1 and B2) between January-April 2011, moving westward with different zonal velocities, B1 residing directly above the convective tropospheric storm head; (II) the merging of the warm airmasses to form the large single 'stratospheric beacon' near 40 degrees N (BO) between April and June 2011, disassociated from the storm head and at a higher pressure (2 mbar) than the original beacons, a downward shift of 1.4 scale heights (approximately 85 km) post-merger; and (III) the mature phase characterised by slow cooling (0.11 +/- 0.01 K/day) and longitudinal shrinkage of the anticyclone since July 2011. Peak temperatures of 221.6 +/- 1.4 K at 2 mbar were measured on May 5th 2011 immediately after the merger, some 80 K warmer than the quiescent surroundings. From July 2011 to the time of writing, BO remained as a long-lived stable stratospheric phenomenon at 2 mbar, moving west with a near-constant velocity of 2.70 +/- 0.04 deg/day (-24.5 +/- 0.4 m/s at 40 degrees N relative to System III longitudes). No perturbations to visible clouds and hazes were detected during this period. With no direct tracers of motion in the stratosphere, we use thermal windshear calculations to estimate clockwise peripheral velocities of 200-400 m/s at 2 mbar around BO. The peripheral velocities of the two original airmasses were smaller (70-140 m/s). In August 2011, the size of the vortex as defined by the peripheral collar was 65 degrees longitude (50,000 km in diameter) and 25 degrees latitude. Stratospheric acetylene (C2H2) was uniformly enhanced by a factor of three within the vortex, whereas ethane (C2H6) remained unaffected. The passage of BO generated a new band of warm stratospheric emission at 0.5 mbar at its northern edge, and there are hints of warm stratospheric structures associated with the beacons at higher altitudes (p < 0.1 mbar) than can be reliably observed by CIRS nadir spectroscopy. Analysis of the zonal windshear suggests that Rossby wave perturbations from the convective storm could have propagated vertically into the stratosphere at this point in Saturn's seasonal cycle, one possible source of energy for the formation of these stratospheric anticyclones. (C) 2012 Elsevier Inc. All rights reserved. C1 [Fletcher, Leigh N.; Irwin, P. G. J.; Hurley, J.; Sinclair, J.; Read, P. L.] Univ Oxford, Dept Phys, Clarendon Lab, Oxford OX1 3PU, England. [Hesman, B. E.; Achterberg, R. K.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Bjoraker, G.; Simon-Miller, A. A.; Flasar, F. M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Gorius, N.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA. [Orton, G. S.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Legarreta, J.] Univ Pas Vasco UPV EHU, Dept Ingn Sistemas & Automt, EUITI, Bilbao, Spain. [Garcia-Melendo, E.] Esteve Duran Observ Fdn, Seva 08553, Spain. [Garcia-Melendo, E.] Inst Cincies Espai CSIC IEEC, Fac Cincies, E-08193 Bellaterra, Spain. [Sanchez-Lavega, A.] Univ Pas Vasco, ETS Ingn, Dept Fs Aplicada, Bilbao 48013, Spain. RP Fletcher, LN (reprint author), Univ Oxford, Dept Phys, Clarendon Lab, Parks Rd, Oxford OX1 3PU, England. EM fletcher@atm.ox.ac.uk RI Flasar, F Michael/C-8509-2012; Fletcher, Leigh/D-6093-2011; Simon, Amy/C-8020-2012; OI Fletcher, Leigh/0000-0001-5834-9588; Irwin, Patrick/0000-0002-6772-384X; Simon, Amy/0000-0003-4641-6186; LEGARRETA ETXAGIBEL, JON JOSU/0000-0001-6501-2705; Sanchez-Lavega, Agustin/0000-0001-7355-1522 FU Glasstone Science Fellowship at the University of Oxford; NASA/Infrared Telescope Facility [NCC 5-538]; Science and Technology Facilities Council (STFC); NASA Cassini Data Analysis Participating Scientists (CDAPS) Program [NNX12AC24G]; NASA; Spanish MICIIN [AYA2009-10701]; FEDER; Grupos Gobierno Vasco [IT-464-07]; Universidad Pas Vasco UPV/EHU [UFI11/55]; [386.C-0096(A)] FX Fletcher was supported by a Glasstone Science Fellowship at the University of Oxford. We thank the members of the Cassini/CIRS investigation team who have assisted in the design of the imaging sequences, instrument commands and other vital operational tasks, and the Ground Systems Operations for the Cassini Project. We wish to thank the directors and staff of the ESO Very Large Telescope and the NASA Infrared Telescope Facility for their assistance with the execution of these observations. This investigation was partially based on observations acquired at the Paranal UT3/Melipal Observatory under ID 386.C-0096 and 287.C-5032. Program 386.C-0096(A) had been awarded time to study Saturn's slow seasonal evolution in April 2011, but we are grateful to ESO for granting our request to obtain these images of Saturn's storm as soon as the planet became available after solar conjunction (which occurred in October 2010).; We are grateful to the operators at the NASA/Infrared Telescope Facility (operated by the University of Hawaii under Cooperative Agreement No. NCC 5-538 with the National Aeronautics and Space Administration, Science Mission Directorate, Planetary Astronomy Program). The UK authors acknowledge the support of the Science and Technology Facilities Council (STFC). B.E.H., G.L.B., and R.K.A. were supported by the NASA Cassini Data Analysis Participating Scientists (CDAPS) Program Grant No. NNX12AC24G. GSO is supported by Grants from NASA to the Jet Propulsion Laboratory, California Institute of Technology. J.L., E.G.M. and A.S.L. were supported by the Spanish MICIIN Project AYA2009-10701 with FEDER funds, by Grupos Gobierno Vasco IT-464-07 and by Universidad Pas Vasco UPV/EHU through program UFI11/55. We thank T. Greathouse and J. Moses for helpful discussions of the beacon results. NR 70 TC 31 Z9 31 U1 0 U2 23 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD NOV-DEC PY 2012 VL 221 IS 2 BP 560 EP 586 DI 10.1016/j.icarus.2012.08.024 PG 27 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 055RL UT WOS:000312434300008 ER PT J AU Reddy, V Le Corre, L Hicks, M Lawrence, K Buratti, BJ Abell, PA Gaffey, MJ Hardersen, PS AF Reddy, Vishnu Le Corre, Lucille Hicks, Michael Lawrence, Kenneth Buratti, Bonnie J. Abell, Paul A. Gaffey, Michael J. Hardersen, Paul S. TI Composition of near-Earth Asteroid 2008 EV5: Potential target for robotic and human exploration SO ICARUS LA English DT Article DE Asteroids, Surfaces; Spectroscopy; Asteroids, Composition; Radar observations ID SPECTROGRAPH; POPULATION; RESOLUTION; TELESCOPE; CHONDRITE; ALBEDO; METAL; SPEX AB We observed Potentially Hazardous Asteroid (PHA) 2008 EV5 in the visible (0.30-0.92 mu m) and near-IR (0.75-2.5 mu m) wavelengths to determine its surface composition. This asteroid is especially interesting because it is a potential target for two sample return mission proposals (Marco Polo-R and Hayabusa-2) and human exploration due to its low delta-v for rendezvous. The spectrum of 2008 EV5 is essentially featureless with exception of a weak 0.48-mu m spin-forbidden Fe3+ absorption band. The spectrum also has an overall blue slope. The albedo of 2008 EV5 remains uncertain with a lower limit at 0.05 and a higher end at 0.20 based on thermal modeling. The Busch et al. (Busch et al. [2011]. Icarus 212, 649-660) albedo estimate of 0.12 +/- 0.04 is consistent with our thermal modeling results. The albedo and composition of 2008 EV5 are also consistent with a C-type taxonomic classification (Somers, J.M., Hicks, M.D., Lawrence, K.J. [2008]. Bull. Am. Astron. Soc. 40, 440). The best spectral match is with CI carbonaceous chondrites similar to Orgueil, which also have a weak 0.48-mu m feature and an overall blue slope. This 0.48-mu m feature is also seen in the spectrum of magnetite. The albedo of Cl chondrites is at the lower limit of our estimated range for the albedo of 2008 EV5. (C) 2012 Elsevier Inc. All rights reserved. C1 [Reddy, Vishnu; Le Corre, Lucille] Max Planck Inst Solar Syst Res, Katlenburg Lindau, Germany. [Reddy, Vishnu; Gaffey, Michael J.; Hardersen, Paul S.] Univ N Dakota, Dept Space Studies, Grand Forks, ND 58202 USA. [Hicks, Michael; Lawrence, Kenneth; Buratti, Bonnie J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Abell, Paul A.] NASA Johnson Space Ctr, Astromat Res & Explorat Sci Directorate, Houston, TX 77058 USA. RP Reddy, V (reprint author), Max Planck Inst Solar Syst Res, Katlenburg Lindau, Germany. EM reddy@mps.mpg.de RI Hardersen, Paul/N-9343-2014; OI Hardersen, Paul/0000-0002-0440-9095; Reddy, Vishnu/0000-0002-7743-3491; Le Corre, Lucille/0000-0003-0349-7932 FU NASA NEOO Program Grant [NNX07AL29G]; NASA Planetary Geology and Geophysics Grant [NNX07AP73G]; IRTF TAC FX This research was supported by NASA NEOO Program Grant NNX07AL29G, and NASA Planetary Geology and Geophysics Grant NNX07AP73G. V.R. would like to thank Javier Licandro for his helpful comments. We thank the IRTF TAC for awarding time to this project, and to the IRTF TOs and MKSS staff for their support. NR 26 TC 10 Z9 10 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 J9 ICARUS JI Icarus PD NOV-DEC PY 2012 VL 221 IS 2 BP 678 EP 681 DI 10.1016/j.icarus.2012.08.035 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 055RL UT WOS:000312434300018 ER PT J AU Ore, CMD Cruikshank, DP Clark, RN AF Ore, Cristina Morea Dalle Cruikshank, Dale P. Clark, Roger N. TI Infrared spectroscopic characterization of the low-albedo materials on Iapetus SO ICARUS LA English DT Article DE Iapetus; Satellites, Composition; Satellites, Surfaces; Saturn, Satellites; Spectroscopy ID SATURNS MOON PHOEBE; MAPPING SPECTROMETER; IRREGULAR SATELLITES; SURFACE-COMPOSITION; DARK MATERIAL; SOLAR-SYSTEM; CASSINI VIMS; MU-M; HYPERION; SPECTRA AB Iapetus, one of the large satellites of Saturn, has been studied over the centuries for its signature brightness contrast, light on one side and dark on the opposite. It has recently been suggested that the dark material is a combination of native and exogenous materials with distinct histories. We present an analysis of parts of the Cassini Regio, the darkest region on the leading hemisphere of Iapetus, focusing on the hydrocarbon signature with a view to detect and investigate differences in the material(s). We find variations in the hydrocarbon bands with geographic location, one type predominantly located on the leading hemisphere. A comparison with the equivalent spectral features on Phoebe and -Iyperion reveals a predictable resemblance between the leading hemisphere material and Phoebe and an unexpected likeness between Hyperion's darkest material and Iapetus trailing hemisphere surface. An analysis of the slope in the visible part of the spectrum is strongly affected by a rise in the continuum (similar to 0.35-0.65 mu m) attributed to Rayleigh scattering from nano-size particles on the surface. The continuum rise varies in strength with the albedo and H2O ice content, and when it is properly accounted for, the overall slope in all the identified spectral units is the same over the interval 0.35-2.3 mu m, independent of albedo or ice abundance. The interpretation of current and previous results offers two different scenarios illustrated by the presence of one vs. two dark materials distributed over the Iapetus surface. We describe the scenarios and their implications. The appearance of the aromatic and aliphatic absorption bands together in their measured relative strengths makes this spectral signature unique, and thus enables the comparison among the three satellites. (C) 2012 Elsevier Inc. All rights reserved. C1 [Ore, Cristina Morea Dalle; Cruikshank, Dale P.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Ore, Cristina Morea Dalle] SETI Inst, Mountain View, CA 94043 USA. [Clark, Roger N.] US Geol Survey, Denver Fed Ctr, Denver, CO 80225 USA. RP Ore, CMD (reprint author), NASA, Ames Res Ctr, MS 245-6, Moffett Field, CA 94035 USA. EM Cristina.M.DalleOre@nasa.gov FU Cassini Science Team funding; NASA [NNX11AN90G] FX We thank Drs. J.A. Mosher and Bonnie J. Buratti for making available the Phoebe mosaic. D.P.C. acknowledges support from Cassini Science Team funding.; C.D.O. acknowledges support from NASA Grant NNX11AN90G. NR 36 TC 5 Z9 5 U1 2 U2 7 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 J9 ICARUS JI Icarus PD NOV-DEC PY 2012 VL 221 IS 2 BP 735 EP 743 DI 10.1016/j.icarus.2012.09.010 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 055RL UT WOS:000312434300023 ER PT J AU Sotin, C Lawrence, KJ Reinhardt, B Barnes, JW Brown, RH Hayes, AG Le Mouelic, S Rodriguez, S Soderblom, JM Soderblom, LA Baines, KH Buratti, BJ Clark, RN Jaumann, R Nicholson, PD Stephan, K AF Sotin, C. Lawrence, K. J. Reinhardt, B. Barnes, J. W. Brown, R. H. Hayes, A. G. Le Mouelic, S. Rodriguez, S. Soderblom, J. M. Soderblom, L. A. Baines, K. H. Buratti, B. J. Clark, R. N. Jaumann, R. Nicholson, P. D. Stephan, K. TI Observations of Titan's Northern lakes at 5 mu m: Implications for the organic cycle and geology SO ICARUS LA English DT Article DE Titan; Titan hydrology; Titan atmosphere; Organic chemistry; Exobiology ID HUYGENS LANDING SITE; HYDROCARBON LAKES; METHANE CYCLE; CASSINI VIMS; ATMOSPHERE; SURFACE; RADAR; ETHANE; MODEL; HAZE AB Since Titan entered Northern spring in August 2009, the North Pole has been illuminated allowing observations at optical wavelengths. On June 5, 2010 the Visual and Infrared Mapping Spectrometer (VIMS) onboard the Cassini spacecraft observed the Northern Pole area with a pixel size from 3 to 7 km. Since, as we demonstrate, little of the solar flux at 5 pm is scattered by the atmosphere, these observations were obtained at relatively large incidence angles and allowed us to build a mosaic covering an area of more than 500,000 km(2) that overlaps and complements observations made by the Synthetic Aperture Radar (SAR) in 2007. We find that there is an excellent correlation between the shape of the radar dark area, known as Ligeia Mare and the VIMS 5-mu m dark unit. Matching most of the radar shoreline, the 2010 VIMS observations suggest that the 125,000-km(2) surface area of Ligeia Mare measured by RADAR in 2007 has not significantly changed. The VIMS observations complement the radar observations to the west of Ligeia Mare and suggest that Ligeia Mare is connected to Kraken Mare by either a diffuse network similar to a swamp area, or by well-defined, sub-pixel rivers. Considering the results of recent evaporation models of methane, our preferred interpretation of the relative constancy in surface area of Ligeia is that it is principally composed of ethane although we cannot rule out the possibility that methane evaporation is balanced with replenishment by either precipitation or underground seepage. There is also strong correlation between the location of the small radar lakes and the small VIMS 5-mu m dark patches. The geographic location of the small lakes are within a VIMS pixel of the SAR location, suggesting that the non-synchronous component of Titan's spin rate, if it exists, was less than 2.3 x 10(-4) deg/day between 2007 and 2010 in agreement with the recent T64 radar observations. These observations question the existence of non-synchronous rotation. Two radar-bright features appear dark at 5-mu m. The simplest interpretation is that these are very shallow lakes, less than one meter deep. Three new small lakes, named Freeman, Cardiel, and Towada by the IAU, are found outside of the area mapped with the SAR. A single-scattering model describing reflection of sunlight at 5-mu m suggests that the lake surface is mirror-like and that the albedo of the solid surfaces surrounding the lakes is about 8%. These observations together with information of the haze aerosols allow us to show that Titan's lakes, atmospheric ethane and aerosol haze are smaller carbon reservoirs than Titan's sand dunes and atmospheric methane. A simple model involving an outburst of methane a few hundreds of Myr ago followed by the dissociation of methane in the atmosphere leading to the formation of the haze particles that constitute the dune fields would be consistent with both the present observations and recent measurements of isotopic ratios in atmospheric methane (Mandt, K.E. et al. [2012]. Astrophys. J. 749(160), 14). (C) 2012 Elsevier Inc. All rights reserved. C1 [Sotin, C.; Lawrence, K. J.; Reinhardt, B.; Hayes, A. G.; Baines, K. H.; Buratti, B. J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Barnes, J. W.] Univ Idaho, Dept Phys, Moscow, ID 83844 USA. [Brown, R. H.; Soderblom, J. M.] Univ Arizona, Lunar & Planetary Lab, Dept Planetary Sci, Tucson, AZ 85721 USA. [Le Mouelic, S.] Univ Nantes, CNRS, Lab Planetol & Geodynam, UMR 6112, F-44322 Nantes, France. [Rodriguez, S.] Univ Paris 07, CNRS, CEA Saclay, DSM,IRFU,SAp,Lab AIM, F-75221 Paris 05, France. [Soderblom, L. A.] US Geol Survey, Flagstaff, AZ 86001 USA. [Clark, R. N.] US Geol Survey, Denver Fed Ctr, Denver, CO 80225 USA. [Jaumann, R.; Stephan, K.] Inst Planetary Res, DLR, D-12489 Berlin, Germany. [Nicholson, P. D.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. RP Sotin, C (reprint author), CALTECH, Jet Prop Lab, M-S 183-301,4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Christophe.sotin@jpl.nasa.gov RI Barnes, Jason/B-1284-2009; Hayes, Alexander/P-2024-2014; Rodriguez, Sebastien/H-5902-2016 OI Barnes, Jason/0000-0002-7755-3530; Hayes, Alexander/0000-0001-6397-2630; Rodriguez, Sebastien/0000-0003-1219-0641 FU NASA Astrobiology Institute; JPL RTD program; NASA FX We thank the VIMS Operations and Science Teams for their dedication in implementing the observations. Reviews by Ellen Stofan and an anonymous reviewer are acknowledged. CS acknowledges support by the NASA Astrobiology Institute and the JPL R&TD program. This work has been performed at the Jet Propulsion Laboratory, California Institute of Technology under contract with NASA. NR 64 TC 29 Z9 30 U1 1 U2 36 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD NOV-DEC PY 2012 VL 221 IS 2 BP 768 EP 786 DI 10.1016/j.icarus.2012.08.017 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 055RL UT WOS:000312434300026 ER PT J AU Johnson, PV Hodyss, R Chernow, VF Lipscomb, DM Goguen, JD AF Johnson, Paul V. Hodyss, Robert Chernow, Victoria F. Lipscomb, Dawn M. Goguen, Jay D. TI Ultraviolet photolysis of amino acids on the surface of icy Solar System bodies SO ICARUS LA English DT Article DE Ices; Ices, IR spectroscopy; Photochemistry; Exobiology; Satellites, Surfaces ID MONOCARBOXYLIC ACIDS; PHOTOCHEMISTRY; EUROPA; SPACE; ICES AB The icy worlds of the outer Solar System are of significant astrobiological interests due, in large part, to the evidence of liquid water beneath the surfaces of a number of jovian and saturnian satellites. Many of these surfaces are subject to various levels of particle and photon radiation. If molecular compounds of biological origin are present in the surface ice layer (originating either in situ or delivered from a subsurface aqueous environment), can they be detected as evidence of biological activity, or do they decompose too rapidly in the surface radiation environment? We present a wavelength resolved study of the ultraviolet photolysis of glycine and phenylalanine to address this question. Studying these reactions at multiple discreet wavelengths distinguishes the present work from previous matrix isolation studies using hydrogen flow lamps and continuum sources by resolving the important contribution of photons with energies much lower than Lyman-alpha (121.6 nm). We find that although the half-lives of glycine and phenylalanine are essentially identical at 147 nm, they diverge at 206 nm and diverge significantly at 254 nm with glycine having longer half-lives at these longer wavelengths. Scaling the results to account for the wavelength dependent variation in solar irradiance shows that despite the reduction of photon energies in the 200-250 nm range, versus 147 nm, it is the longer wavelengths that will dominate the destruction of amino acids in icy surfaces. It seems unlikely that organics can survive long enough on the surface of an icy planetary body to be detected without being frequently replenished from a shielded source such as a subsurface ocean. (C) 2012 Elsevier Inc. All rights reserved. C1 [Johnson, Paul V.; Hodyss, Robert; Chernow, Victoria F.; Lipscomb, Dawn M.; Goguen, Jay D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Johnson, PV (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,Mail Stop 183-601, Pasadena, CA 91109 USA. EM Paul.V.Johnson@jpl.nasa.gov FU National Aeronautics and Space Administration (NASA); NASA's Astrobiology: Exobiology and Evolutionary Biology program; NASA Astrobiology Institute (Icy Worlds); NASA Undergraduate Research Program FX This research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration (NASA). Funding from NASA's Astrobiology: Exobiology and Evolutionary Biology program and the NASA Astrobiology Institute (Icy Worlds) is gratefully acknowledged. VFC and DML participated in this work as undergraduate interns sponsored by the NASA Undergraduate Research Program. We would like to thank Dr. Arthur L. Lane for his insights into the importance of monochromatic ice photolysis studies. Finally, we thank two anonymous reviewers for their constructive comments. NR 28 TC 6 Z9 6 U1 4 U2 30 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 J9 ICARUS JI Icarus PD NOV-DEC PY 2012 VL 221 IS 2 BP 800 EP 805 DI 10.1016/j.icarus.2012.09.005 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 055RL UT WOS:000312434300028 ER PT J AU Morishima, R Edgington, SG Spilker, L AF Morishima, Ryuji Edgington, Scott G. Spilker, Linda TI Regolith grain sizes of Saturn's rings inferred from Cassini-CIRS far-infrared spectra SO ICARUS LA English DT Article DE Saturn, Rings; Infrared observations; Radiative transfer; Regoliths ID SELF-GRAVITY WAKES; MU-M; THERMAL OBSERVATIONS; REFLECTANCE SPECTRA; MULTILAYER MODEL; MAIN RINGS; IN-SITU; SNOW; EMISSION; PHASE AB We analyze far-infrared (10-650 cm(-1)) emissivity spectra of Saturn's main rings obtained by the Cassini Composite Infrared Spectrometer (CIRS). In modeling of the spectra, the single scattering albedos of regolith grains are calculated using the Mie theory, diffraction is removed with the delta-Eddington approximation, and the hemispherical emissivities of macroscopic free-floating ring particles are calculated using the Hapke's isotropic scattering model. Only pure crystalline water ice is considered and the size distribution of regolith grains is estimated. We find that good fits are obtained if the size distribution is broad ranging from 1 mu m to 1-10 cm with a power law index of similar to 3. This means that the largest regolith grains are comparable to the smallest free-floating particles in size and that the power law indices for both free-floating particles and regolith grains are similar to each other. The apparent relative abundance of small grains increases with decreasing solar phase angle (or increasing mean temperature). This trend is particularly strong for the C ring and is probably caused by eclipse cooling in Saturn's shadow, which relatively suppresses warming up of grains larger than the thermal skin depth (similar to 1 mm) under subsequent solar illumination. (C) 2012 Elsevier Inc. All rights reserved. C1 [Morishima, Ryuji; Edgington, Scott G.; Spilker, Linda] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Morishima, Ryuji] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90095 USA. RP Morishima, R (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Ryuji.Morishima@jpl.nasa.gov FU NASA; NASA's Cassini Data Analysis Program FX We are grateful to Bruce Hapke and an anonymous reviewer for their thorough reviews. We thank Jeffrey Cuzzi, Matthew Hedman, John Spenser, Deau Estelle, and Donald Jennings for fruitful discussions and helpful comments on this work, and Stu Pilorz, Shawn Brooks, and Mark Showalter for designing of CIRS observations. This research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA. Government sponsorship acknowledged. This work was also supported in part by NASA's Cassini Data Analysis Program. NR 56 TC 6 Z9 6 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 NOV-DEC PY 2012 VL 221 IS 2 BP 888 EP 899 DI 10.1016/j.icarus.2012.09.012 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 055RL UT WOS:000312434300036 ER PT J AU Cloutis, EA Hudon, P Hiroi, T Gaffey, MJ AF Cloutis, E. A. Hudon, P. Hiroi, T. Gaffey, M. J. TI Spectral reflectance properties of carbonaceous chondrites: 7. CK chondrites SO ICARUS LA English DT Article DE Asteroids, Surfaces; Asteroids, Composition; Meteorites; Spectroscopy ID THERMAL METAMORPHISM; ELEMENT ABUNDANCES; CV-CHONDRITES; METEORITE; ASTEROIDS; OLIVINE; CLASSIFICATION; PLAGIOCLASE; INCLUSIONS; MINERALOGY AB The reflectance spectra of 15 CK chondrites have been measured as part of an ongoing study of carbonaceous chondrite reflectance spectra. The available sample suite includes multiple grain sizes and samples with petrologic grades varying from CK4 to CK6. CK reflectance spectra are all characterized by an olivine-associated absorption band in the 1.05 mu m region. Compared to pure olivine, CK spectra are darker, have a more subdued olivine absorption band, and are often more blue-sloped. Reflectance at 0.56 mu m varies from 9.6% to 22.5%, and olivine band depth varies from 6.7% to 31.0%, for powder; that include the finest fraction. With increasing grain size, and exclusion of the finest fraction, CK spectra become darker and more blue sloped, while the olivine absorption band initially becomes deeper and then shallower. The presence of calcium-aluminum inclusions (CAIs), whose abundance varies widely in CKs, does not normally lead to the appearance of a well-defined absorption band in the 2.1 mu m region, although the overall blue slope of many CKs is likely attributable to Fe-bearing spinel in CK CAIs. The only consistent spectral feature that relates to metamorphic grade is that CK6 spectra have uniformly deeper olivine absorption band than CK4-5.5 spectra. This could be related to various factors such as loss/aggregation of opaques that may accompany metamorphism. Comparison of CV and thermally metamorphosed carbonaceous chondrite to CK spectra suggests that metamorphism to between similar to 1000 and 1200 degrees C is required for CV spectra to match CK spectra; CV spectra are uniformly darker and have shallower olivine absorption bands than CK spectra. (C) 2012 Elsevier :nc. All rights reserved. C1 [Cloutis, E. A.] Univ Winnipeg, Dept Geog, Winnipeg, MB R3B 2E9, Canada. [Hudon, P.] NASA Johnson Space Ctr, Astromat Res & Explorat Sci Off, Mail Code KR, Houston, TX 77058 USA. [Hiroi, T.] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA. [Gaffey, M. J.] Univ N Dakota, Dept Space Studies, Grand Forks, ND 58202 USA. RP Cloutis, EA (reprint author), Univ Winnipeg, Dept Geog, 515 Portage Ave, Winnipeg, MB R3B 2E9, Canada. EM e.cloutis@uwinnipeg.ca; pierre.hudon@mcgill.ca; takahiro_hiroi@brown.edu; gaffey@space.edu FU NASA [NNG06GJ31G]; NSERC FX We wish to thank the invaluable and generous assistance provided by many individuals which made this study possible. In particular we thank the US and Japanese Antarctic meteorite programs for recovering the majority of the samples included in this study. The RELAB facility at Brown University is a multi-user facility operated with support from NASA Planetary Geology and Geophysics Grant NNG06GJ31G, whose support is gratefully acknowledged. This study was supported by an NSERC Discovery grant to EAC. We also wish to thank Alan Rubin and Beth Clark for their cogent and valuable comments which improved the accuracy and readability of this manuscript. NR 92 TC 10 Z9 10 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 J9 ICARUS JI Icarus PD NOV-DEC PY 2012 VL 221 IS 2 BP 911 EP 924 DI 10.1016/j.icarus.2012.09.017 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 055RL UT WOS:000312434300038 ER PT J AU Heggy, E Palmer, EM Kofman, W Clifford, SM Righter, K Herique, A AF Heggy, Essam Palmer, Elizabeth M. Kofman, Wlodek Clifford, Stephen M. Righter, Kevin Herique, Alain TI Radar properties of comets: Parametric dielectric modeling of Comet 67P/Churyumov-Gerasimenko SO ICARUS LA English DT Article DE Comets, Composition; Comets, Dust; Ices; Radar observations; Experimental techniques ID SPACE-TELESCOPE OBSERVATIONS; NUCLEUS SOUNDING EXPERIMENT; DEEP IMPACT; RADIOWAVE TRANSMISSION; INNER COMA; CONSERT; MARS; COMET-9P/TEMPEL-1; PERMITTIVITY; FREQUENCIES AB In 2014, the European Space Agency's Rosetta mission is scheduled to rendezvous with Comet 67P/Churyumov-Gerasimenko (Comet 67P). Rosetta's CONSERT experiment aims to explore the cometary nucleus' geophysical properties using radar tomography. The expected scientific return and inversion algorithms are mainly dependent on our understanding of the dielectric properties of the comet nucleus and how they vary with the spatial distribution of geophysical parameters. Using observations of Comets 9P/Tempel 1 and 81P/Wild 2 in combination with dielectric laboratory measurements of temperature, porosity, and dust-to-ice mass ratio dependencies for cometary analog material, we have constructed two hypothetical three-dimensional parametric dielectric models of Comet 67P's nucleus to assess different dielectric scenarios of the inner structure. Our models suggest that dust-to-ice mass ratios and porosity variations generate the most significant measurable dielectric contrast inside the comet nucleus, making it possible to explore the structural and compositional hypotheses of cometary nuclei. Surface dielectric variations, resulting from temperature changes induced by solar illumination of the comet's faces, have also been modeled and suggest that the real part of the dielectric constant varies from 1.9 to 3.0, hence changing the surface radar reflectivity. For CONSERT, this variation could be significant at low incidence angles, when the signal propagates through a length of dust mantle comparable to the wavelength. The overall modeled dielectric permittivity spatial and temporal variations are therefore consistent with the expected deep penetration of CONSERT's transmitted wave through the nucleus. It is also clear that changes in the physical properties of the nucleus induce sufficient variation in the dielectric properties of cometary material to allow their inversion from radar tomography. (C) 2012 Elsevier Inc. All rights reserved. C1 [Heggy, Essam] CALTECH, NASA Jet Prop Lab, Pasadena, CA 91109 USA. [Palmer, Elizabeth M.] Univ Calif Los Angeles, Los Angeles, CA 90095 USA. [Kofman, Wlodek; Herique, Alain] UJF Grenoble 1 CNRS INSU, Inst Planetol & Astrophys Grenoble IPAG UMR 5274, F-38041 Grenoble, France. [Kofman, Wlodek] Polish Acad Sci, Space Res Ctr, PL-01237 Warsaw, Poland. [Clifford, Stephen M.] Lunar & Planetary Inst, Houston, TX 77058 USA. [Righter, Kevin] NASA Johnson Space Ctr, Mail Code KT, Houston, TX 77058 USA. RP Heggy, E (reprint author), CALTECH, NASA Jet Prop Lab, 4800 Oak Grove Dr,Mail Stop 300-227, Pasadena, CA 91109 USA. EM essam.heggy@jpl.nasa.gov; empalmer@ucla.edu; wlodek.kofman@obs.ujf-grenoble.fr; clifford@lpi.usra.e-du; kevin.righter-1@nasa.gov; alain.herique@obs.ujf-grenoble.fr RI Heggy, Essam/E-8250-2013; Kofman, Wlodek/C-4556-2008; Herique, Alain/E-7210-2017 OI Heggy, Essam/0000-0001-7476-2735; Herique, Alain/0000-0003-3699-883X FU NASA Planetary Geology and Geophysics Program [NNXZ08AKA2G, NNG05GL11G]; French Space Agency (CNES); National Aeronautics and Space Administration FX The authors would like to thank Drs. Claudia Alexander and Artur Chmielewski from the Jet Propulsion Laboratory and Prof. Christopher Russell from UCLA for their helpful comments and discussions. We also thank the Meteorite Working Group and NASA Johnson Space Center Curation office for providing samples from the U.S. Antarctic Meteorite Collection. This work was supported in part by NASA Planetary Geology and Geophysics Program under Grants NNXZ08AKA2G and NNG05GL11G. The authors would like to acknowledge the French Space Agency (CNES) for its support to the part of this study performed in the Institut de Planetologie et d'Astrophysique de Grenoble. 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 50 TC 24 Z9 24 U1 2 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 J9 ICARUS JI Icarus PD NOV-DEC PY 2012 VL 221 IS 2 BP 925 EP 939 DI 10.1016/j.icarus.2012.09.023 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 055RL UT WOS:000312434300039 ER PT J AU Feofilov, AG Kutepov, AA Rezac, L Smith, MD AF Feofilov, A. G. Kutepov, A. A. Rezac, L. Smith, M. D. TI Extending MGS-TES temperature retrievals in the martian atmosphere up to 90 km: Retrieval approach and results SO ICARUS LA English DT Article DE Mars, Atmosphere; Atmospheres, Structure; Infrared observations; Radiative transfer ID THERMAL EMISSION SPECTROMETER; ACCELERATED LAMBDA ITERATION; MIDDLE ATMOSPHERE; PLANETARY-ATMOSPHERES; LOWER THERMOSPHERE; ATOMIC OXYGEN; RATE-CONSTANT; WATER-VAPOR; MARS; VARIABILITY AB This paper describes a methodology for performing temperature retrievals in the martian atmosphere in the 60-90 km altitude range using spectrally integrated 15 mu m CO2 limb emissions measured by the Thermal Emission Spectrometer (TES), the infrared spectrometer on-board the Mars Global Surveyor (MGS). We show that a limited number of limb-geometry sequences observed by this instrument are characterized by a high enough signal-to-noise ratio (SNR) to extend the upper limit of the retrievals to 90 km. Using the methodology described in the paper, we have retrieved similar to 200 individual temperature profiles from the MGS TES limb observations in the altitude range between 30 and 90 km. The set of retrieved temperature profiles is available for download in supplemental materials of this paper. The temperature retrieval uncertainties are mainly caused by noise in the observed radiance, and are estimated to be about +/- 2 K at 60 km, +/- 3 K at 70 km, 5 +/- K at 80 km, and +/- 13 K at 90 km. We compare the retrieved profiles to the martian Year 24 (MY 24) dataset of the Mars Climate Database (MCD) and SPI-CAM measured temperature profiles for MY 27 and find good qualitative agreement. Quantitatively, our retrieved profiles are in general warmer and demonstrate strong profile-to-profile variability. The warm bias is partially explained by the selection of high SNR limb scans and can be estimated and taken into account. Overall, the average difference between the TES-retrieved temperatures corrected for warm bias and the MCD MY 24 dataset is 4 K at 60 km, 4 K at 70 km, -2 K at 80 km, and 2 K at 90 km. The root-mean-square of the temperature variability caused by gravity waves estimated in this work is 7 K at 60 km, 11 K at 70 km, 18 K at 80 km, and 25 K at 90 km. (C) 2012 Elsevier Inc. All rights reserved. C1 [Feofilov, A. G.; Kutepov, A. A.] Catholic Univ Amer, Washington, DC 20064 USA. [Feofilov, A. G.; Kutepov, A. A.; Smith, M. D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Rezac, L.] Hampton Univ, Hampton, VA 23668 USA. RP Feofilov, AG (reprint author), Ecole Polytech, Lab Dynam Meteorol, Palaiseau, France. EM artem-feofilov@cua-nasa-gsfc.info RI Feofilov, Artem/A-2271-2015 OI Feofilov, Artem/0000-0001-9924-4846 FU NASA [NNX08AL12G] FX The work of A. Feofilov and A. Kutepov was supported by NASA Grant NNX08AL12G. The authors are grateful to two anonymous reviewers for their thorough analysis of the manuscript and their helpful comments and recommendations. We also thank Dr. Francois Forget for providing the SPICAM data and consultations regarding usage of the MCD data. NR 47 TC 3 Z9 3 U1 0 U2 3 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 J9 ICARUS JI Icarus PD NOV-DEC PY 2012 VL 221 IS 2 BP 949 EP 959 DI 10.1016/j.icarus.2012.09.033 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 055RL UT WOS:000312434300041 ER PT J AU Cloutis, EA Hudon, P Hiroi, T Gaffey, MJ Mann, P AF Cloutis, E. A. Hudon, P. Hiroi, T. Gaffey, M. J. Mann, P. TI Spectral reflectance properties of carbonaceous chondrites: 8. "Other" carbonaceous chondrites: CH, ungrouped, polymict, xenolithic inclusions, and R chondrites SO ICARUS LA English DT Article DE Asteroids, Surfaces; Meteorites; Spectroscopy ID TAGISH LAKE METEORITE; EARLY SOLAR-SYSTEM; X-RAY-DIFFRACTION; ORGANIC-MATTER; MOSSBAUER-SPECTROSCOPY; ISOTOPIC COMPOSITIONS; MINERAL CHEMISTRY; CV-CHONDRITES; CM CHONDRITES; EARTH AB We have analyzed reflectance spectra (0.3-2.5 mu m) of a number of ungrouped or tentatively grouped carbonaceous chondrites (CCs), possible CC-type xenoliths in an aubrite (Cumberland Falls) and a howardite (PRA 04401), a CH chondrite (PCA 91467), a CC polymict breccia (Kaidun), and some R chondrites. The best approach to analysis relies largely on characterizing spectrally active phases - i.e., those phases that contribute diagnostic absorption features, involving absorption band wavelength position, band depth, shape of absorption features, combined with albedo and spectral slope. Mafic silicate (hydrous and/or anhydrous) absorption features are ubiquitous in the CCs and R chondrites we have examined. Combining information on these features along with albedo and spectral slopes allows reasonable inferences to be made concerning their uniqueness. Reflectance spectra of Coolidge show contributions from both olivine and Fe oxyhydroxides (from terrestrial weathering), and its high reflectance and mafic silicate band depths are consistent with a petrologic grade >3 and inconsistent with CVs. The CC nature of the Cumberland Falls inclusions from spectral analysis is inconclusive, but they do exhibit spectral features consistent with their overall mineralogy. DaG 430, which has petrologic characteristics of both CV and CK chondrites, has a spectrum that is not fully consistent with either group. The spectrum of EET 96029 is consistent with some, but not all CM2 chondrites. GRO 95566, a meteorite with some affinities to CM2s, most resembles the Renazzo CR2 chondrite, consistent with their similar mineralogies, and its spectral properties can be related to its major mineralogic characteristics. Spectra of Kaidun are most consistent with CR chondrites, which form the bulk of this meteorite. The reflectance spectrum of MCY 92005 is consistent with its recent classification as a CM2 chondrite. The R3 chondrite MET 01149 shares many characteristics with CKs, but differs in terms of its slightly red slope and 2 mu m region absorption feature. The combination of high reflectance, deep 1 mu m band and, to a lesser extent, slightly red slope and weak 2 mu m region absorption band, distinguishes PRE 95404 from CV3s, to which it was initially assigned. The LAP 04840 R6 spectrum is dominated by olivine, consistent with a petrologic grade >3. Its reflectance is somewhat lower than for the R3 chondrites, and falls within the range of many CCs. Its most characteristic feature is the metal-OH absorption bands in the 2.3 mu m region. Analysis and assignment of PCA 91467 (CH3) is complicated by the presence of terrestrial weathering products. Its red spectral slope is consistent with its high metal content. Reflectance spectra of the howardite PRA 04401, which contains similar to 40% CM2-like inclusions, is dominated by the howardite's pyroxene absorption bands, and expected CM2-type absorption bands near 0.7 and 1.1 mu m are not seen. The CC xenoliths do reduce overall reflectance and pyroxene absorption band depths significantly, and probably add an overall red slope, when compared to inclusion-free howardites. QUE 99038, which has been linked to CM2, CO, or CR chondrites is not spectrally consistent with any of these groups. The 2 mu m band, high overall reflectance, and dominant olivine absorption band are all generally inconsistent with CM2 and CR2-3 chondrites. It resembles the CO3 chondrite ALH 77003 in the 1 mu m region, but differs in the 2 mu m region. The red-sloped, nearly featureless spectrum of Tagish Lake is unique among carbonaceous chondrites. It probably arises from the highly aromatic nature of the organic component and its intimate association with the phyllosilicate-rich matrix, which makes up a high proportion of this meteorite. Our results suggest that the meteorites included in this study can usually be determined to be either unique or to be placed with a reasonable degree of confidence into established CC groups. Our analysis has also provided insights into the degree to which spectral analysis can be used for characterization, the spectral features that can be used for characterization, and their limitations. (C) 2012 Elsevier Inc. All rights reserved. C1 [Cloutis, E. A.; Mann, P.] Univ Winnipeg, Dept Geog, Winnipeg, MB R3B 2E9, Canada. [Hudon, P.] NASA Johnson Space Ctr, Astromat Res & Explorat Sci Off, Mail Code KR, Houston, TX 77058 USA. [Hiroi, T.] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA. [Gaffey, M. J.] Univ N Dakota, Dept Space Studies, Grand Forks, ND 58202 USA. RP Cloutis, EA (reprint author), Univ Winnipeg, Dept Geog, 515 Portage Ave, Winnipeg, MB R3B 2E9, Canada. EM e.cloutis@uwinnipeg.ca; pierre.hudon@mcgill.ca; takahiro_hiroi@brown.edu; gaffey@space.edu FU NASA [NNG06GJ31G]; NSERC FX We wish to thank the invaluable and generous assistance provided by many individuals which made this study possible. In particular we thank the US and Japanese Antarctic meteorite programs for recovering many of the samples included in this study. We also wish to thank Dr. Andreas Nathues from the Max Planck Institute for providing samples of PRA 04401 and a number of other howardites, Mike Zolensky and Andrei Ivanov for the sample of Kaidun, and Katsuhito Ohtsuka for DaG 430. The RELAB facility at Brown University is a multi-user facility operated with support from NASA Planetary Geology and Geophysics Grant NNG06GJ31G, whose support is gratefully acknowledged. This study was supported by an NSERC Discovery grant to EAC. We also wish to thank Josep Trigo-Rodriguez and an anonymous reviewer for their valuable and thoughtful comments and suggestions. NR 127 TC 11 Z9 11 U1 0 U2 7 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 J9 ICARUS JI Icarus PD NOV-DEC PY 2012 VL 221 IS 2 BP 984 EP 1001 DI 10.1016/j.icarus.2012.10.008 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 055RL UT WOS:000312434300044 ER PT J AU Schinder, PJ Flasar, FM Marouf, EA French, RG McGhee, CA Kliore, AJ Rappaport, NJ Barbinis, E Fleischman, D Anabtawi, A AF Schinder, Paul J. Flasar, F. Michael Marouf, Essam A. French, Richard G. McGhee, Colleen A. Kliore, Arvydas J. Rappaport, Nicole J. Barbinis, Elias Fleischman, Don Anabtawi, Aseel TI The structure of Titan's atmosphere from Cassini radio occultations: Occultations from the Prime and Equinox missions SO ICARUS LA English DT Article DE Titan; Atmospheres, Structure; Occultations ID SURFACE TEMPERATURES; STRATOSPHERIC COMPOSITION; PLANETARY-ATMOSPHERES; INFRARED-SPECTRA; DYNAMICS; MODEL; EQUILIBRIA; PROFILES; METHANE; CLOUDS AB We present the results of six soundings of the atmosphere of Titan by the radio occultation technique using the Cassini spacecraft currently in orbit around Saturn. These occultations occurred during four separate targeted Titan encounters in both the Prime and Equinox missions of Cassini over 3 years. They cover a wide range of latitude from 75 degrees S to 79 degrees N, split so that three soundings are in the northern hemisphere and three are in the southern hemisphere. Techniques and error analysis are similar to Schinder et al. (2011). The six temperature-altitude profiles presented here are compared to those earlier results. Of special interest is the sudden cooling observed at altitudes of similar to 80-100 km in the two high northern (winter) soundings at 74 degrees N and 80 degrees N, where the temperature drops by about 10 K over the course of 20 km. The northern profiles also exhibit a transition between the troposphere and stratosphere that is much more abrupt than in the south, and the northern tropopause temperatures are much cooler. (C) 2012 Elsevier Inc. All rights reserved. C1 [Schinder, Paul J.] Cornell Univ, Ctr Radiophys & Space Res, Ithaca, NY 14853 USA. [Flasar, F. Michael] NASA Goddard Space Flight Ctr, Greenbelt, MD 20770 USA. [Marouf, Essam A.] San Jose State Univ, Dept Elect Engn, San Jose, CA 95192 USA. [French, Richard G.; McGhee, Colleen A.] Wellesley Coll, Dept Astron, Wellesley, MA 02481 USA. [Kliore, Arvydas J.; Rappaport, Nicole J.; Barbinis, Elias; Fleischman, Don; Anabtawi, Aseel] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Schinder, PJ (reprint author), Cornell Univ, Ctr Radiophys & Space Res, Ithaca, NY 14853 USA. EM schinder@astro.cornell.edu; f.m.flasar@nasa.gov; emarouf@email.sjsu.edu; rfrench@wellesley.edu; cmcghee@wellesley.edu; akliore@jpl.nasa.gov; Nicole.J.Rappaport@jpl.nasa.gov; elias.barbinis@jpl.nasa.gov; don.u.fleischman@jpl.nasa.gov; Aseel.Anabtawi@jpl.na-sa.gov RI Flasar, F Michael/C-8509-2012; OI Schinder, Paul/0000-0002-4571-7895 NR 43 TC 20 Z9 20 U1 0 U2 17 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 J9 ICARUS JI Icarus PD NOV-DEC PY 2012 VL 221 IS 2 BP 1020 EP 1031 DI 10.1016/j.icarus.2012.10.021 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 055RL UT WOS:000312434300046 ER PT J AU White, DW Mastrapa, RME Sandford, SA AF White, Douglas W. Mastrapa, Rachel M. E. Sandford, Scott A. TI Laboratory spectra of CO2 vibrational modes in planetary ice analogs SO ICARUS LA English DT Article DE Ices, IR spectroscopy; Experimental techniques; Organic chemistry; Satellites, Surfaces ID NEAR-INFRARED SPECTROSCOPY; AMORPHOUS SOLID WATER; CARBON-DIOXIDE; OPTICAL-CONSTANTS; SOLAR-SYSTEM; MOLECULAR-COMPLEXES; GLASS-TRANSITION; GRAIN MANTLES; MU-M; INTERSTELLAR AB Laboratory spectra have shown that CO2 is a powerful diagnostic tool for analyzing infrared data from remote observations, as it has been detected on icy moons in the outer Solar System as well as dust grain surfaces in the interstellar medium (ISM). IR absorption band profiles of CO2 within ice mixtures containing H2O and CH3OH change with respect to temperature and mixture ratios. In this particular study, the nu(3) CO2 asymmetric stretch mode near 4.3 mu m (2350 cm(-1)), overtone mode near 1.97 mu m (5080 cm(-1)), and the combination bands near 2.7 mu m (3700 cm(-1)), 2.8 mu m (3600 cm(-1)), and 2.02 mu m (4960 cm(-1)), are systematically observed in different mixtures with H2O and CH3OH in temperature ranges from 15 K to 150 K. Additionally, some high-temperature deposits (T > 50 K) of H2O, CH3OH, and CO2 ice mixtures were performed and it was discovered that CO2 may deposit out at higher temperatures than previously recorded. These data may then be used to interpret infrared observational data obtained from icy surfaces in the outer Solar System and beyond. (C) 2012 Elsevier Inc. All rights reserved. C1 [White, Douglas W.; Sandford, Scott A.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Mastrapa, Rachel M. E.] SETI Inst, Mountain View, CA 94035 USA. RP White, DW (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM douglas.white@nasa.gov FU NASA; Oak Ridge Associated Universities; NASA's Origins of Solar Systems and Planetary Geology and Geophysics Programs FX The authors thank NASA and Oak Ridge Associated Universities for sponsoring the NASA Postdoctoral Program (NPP) and NASA's Origins of Solar Systems and Planetary Geology and Geophysics Programs for support. We also thank Perry Gerakines and the University of Alabama at Birmingham (UAB) for use of some of the data in this study. NR 72 TC 3 Z9 3 U1 0 U2 17 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 J9 ICARUS JI Icarus PD NOV-DEC PY 2012 VL 221 IS 2 BP 1032 EP 1042 DI 10.1016/j.icarus.2012.10.024 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 055RL UT WOS:000312434300047 ER PT J AU Perez-Hoyos, S Sanz-Requena, JF Sanchez-Lavega, A Wong, MH Hammel, HB Orton, GS de Pater, I Simon-Miller, AA Clarke, JT Noll, K AF Perez-Hoyos, S. Sanz-Requena, J. F. Sanchez-Lavega, A. Wong, M. H. Hammel, H. B. Orton, G. S. de Pater, I. Simon-Miller, A. A. Clarke, J. T. Noll, K. TI Vertical cloud structure of the 2009 Jupiter impact based on HST/WFC3 observations SO ICARUS LA English DT Article DE Jupiter; Atmospheres, Structure; Jupiter, Atmosphere; Impact processes ID LEVY 9 H; COMET SHOEMAKER-LEVY-9; PLANETARY ATMOSPHERES; TEMPORAL EVOLUTION; AEROSOL DEBRIS; CALAR-ALTO; HST; ULTRAVIOLET; EQUATORIAL; TELESCOPE AB The impact of a body of unknown origin with Jupiter in July 2009 produced ar intense perturbation of the planet's atmosphere at the visible cloud levels. The vertical cloud structure was deeply affected by the presence of a strongly absorbing dense aerosol layer that was expanded steadily by advection in the local winds. We observed this phenomenon at high spatial resolution with the Hubble Space Telescope in July, August, September and November 2009 using the Wide Field Camera 3. In this work, we present radiative transfer modeling of the observed reflectivity in the wavelength range from the near UV (200 nm) to near IR (950 nm) range. The geometric and spectral variations of reflectivity give information on the main particle properties (optical thickness, size, and imaginary refractive index). The observations can be fitted by introducing small particles into the stratosphere with an optical thickness, at a wavelength of 400 nm, ranging from 0.5 +/- 0.2 (center of the Impact Cloud) to 0.17 +/- 0.03 (impact periphery). Similar effects are detected in the troposphere: the disturbance increases the particle density at all detectable atmospheric levels, with a total aerosol column density of 5 +/- 2 x 10(9) cm(-2). The imaginary refractive indices of the aerosol were also substantially altered, with values of m(i) similar to 0.015 at UV wavelengths, resembling the absorption spectrum of absorber candidates previously proposed for SL9. We find a typical e-folding temporal scale of 10 +/- 3 days in the most rapidly evolving region of the Impact Cloud. (C) 2012 Elsevier Inc. All rights reserved. C1 [Perez-Hoyos, S.; Sanchez-Lavega, A.] Univ Basque Country, Escuela T Super Ingn, Dept Fis Aplicada 1, Bilbao 48013, Spain. [Sanz-Requena, J. F.] Univ Europea Miguel de Cervantes, Valladolid, Spain. [Wong, M. H.; de Pater, I.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Hammel, H. B.] AURA Inc, Washington, DC 20005 USA. [Hammel, H. B.] Space Sci Inst, Boulder, CO 80301 USA. [Orton, G. S.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Simon-Miller, A. A.; Noll, K.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Clarke, J. T.] Boston Univ, Ctr Space Phys, Boston, MA 02215 USA. RP Perez-Hoyos, S (reprint author), Univ Basque Country, Escuela T Super Ingn, Dept Fis Aplicada 1, Alameda Urquijo S-N, Bilbao 48013, Spain. EM santiago.perez@ehu.es RI Clarke, John/C-8644-2013; Noll, Keith/C-8447-2012; Perez-Hoyos, Santiago/L-7543-2014; Simon, Amy/C-8020-2012; OI Perez-Hoyos, Santiago/0000-0002-2587-4682; Simon, Amy/0000-0003-4641-6186; Sanchez-Lavega, Agustin/0000-0001-7355-1522 FU Spanish MICIIN [AYA2009-10701]; FEDER funds; Grupos Gobierno Vasco [IT-464-07]; Universidad Pais Vasco UPV/EHU [UFI11/55]; HST Programs [GO/DD-12045, GO/DD-12003, GO-11559]; NASA through Space Telescope Science Institute; NASA [NAS 5-26555] FX This work was supported by the Spanish MICIIN Project AYA2009-10701 with FEDER funds and Grupos Gobierno Vasco IT-464-07, and by Universidad Pais Vasco UPV/EHU through Program UFI11/55. The observations were supported by HST Programs GO/DD-12045, GO/DD-12003 and GO-11559, with support 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. NR 49 TC 3 Z9 3 U1 0 U2 9 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 J9 ICARUS JI Icarus PD NOV-DEC PY 2012 VL 221 IS 2 BP 1061 EP 1078 DI 10.1016/j.icarus.2012.10.012 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 055RL UT WOS:000312434300049 ER PT J AU Howett, CJA Spencer, JR Hurford, T Verbiscer, A Segura, M AF Howett, C. J. A. Spencer, J. R. Hurford, T. Verbiscer, A. Segura, M. TI PacMan returns: An electron-generated thermal anomaly on Tethys SO ICARUS LA English DT Article DE Saturn, Satellites; Satellites, Surfaces; Satellites, Composition ID SYSTEM AB New Cassini observations show that Saturn's moon Tethys, like Mimas, has a region of anomalously high thermal inertia at low latitudes centered on its leading hemisphere. Derivation of the thermophysical properties of the surface across three representative regions indicate that the bolometric Bond albedo across Tethys' leading hemisphere remains constant, within error, whilst the thermal inertia increases from 5 +/- 1 J s(-1) m(-1) K-1 outside of the anomalous region to 25 +/- 3 J s(-1) m(-1) K-1 inside. The thermally anomalous region is spatially correlated with a decrease in the IR/UV surface coloration. The discovery greatly strengthens the hypothesis that high-energy electrons, which preferentially bombard the leading hemispheres on both satellites, produce dramatic alterations in surface texture. (C) 2012 Elsevier Inc. All rights reserved. C1 [Howett, C. J. A.; Spencer, J. R.] SW Res Inst, Boulder, CO 80403 USA. [Hurford, T.; Segura, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Verbiscer, A.] Univ Virginia, Charlottesville, VA 22904 USA. RP Howett, CJA (reprint author), 1050 Walnut St,Suite 300, Boulder, CO 80302 USA. EM howett@boulder.swri.edu RI Hurford, Terry/F-2625-2012 FU Cassini Project; Cassini Data Analysis Program [NNX12AC23G] FX The authors would like to thank the Cassini Project and the Cassini Data Analysis Program (NNX12AC23G) for funding this work. Thanks are also extended to Chris Paranicas, who supplied data on the energy flux bombarding Tethys, and Paul Schenk, who provided the IR/UV color ratio maps of Tethys. NR 11 TC 17 Z9 17 U1 0 U2 2 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 J9 ICARUS JI Icarus PD NOV-DEC PY 2012 VL 221 IS 2 BP 1084 EP 1088 DI 10.1016/j.icarus.2012.10.013 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 055RL UT WOS:000312434300051 ER PT J AU Marchis, F Enriquez, JE Emery, JP Mueller, M Baek, M Pollock, J Assafin, M Martins, RV Berthier, J Vachier, F Cruikshank, DP Lim, LF Reichart, DE Ivarsen, KM Haislip, JB LaCluyze, AP AF Marchis, F. Enriquez, J. E. Emery, J. P. Mueller, M. Baek, M. Pollock, J. Assafin, M. Vieira Martins, R. Berthier, J. Vachier, F. Cruikshank, D. P. Lim, L. F. Reichart, D. E. Ivarsen, K. M. Haislip, J. B. LaCluyze, A. P. TI Multiple asteroid systems: Dimensions and thermal properties from Spitzer Space Telescope and ground-based observations SO ICARUS LA English DT Article DE Asteroids; Satellites of asteroids; Asteroids, Composition; Infrared observations ID NEAR-EARTH ASTEROIDS; MAIN-BELT ASTEROIDS; BINARY MINOR PLANETS; 33342 1998 WT24; INFRARED OBSERVATIONS; 21 LUTETIA; ROTATIONAL PROPERTIES; SPECTROSCOPIC SURVEY; SURFACE-COMPOSITION; ANGULAR-MOMENTUM AB We collected mid-IR spectra from 5.2 to 38 mu m using the Spitzer Space Telescope Infrared Spectrograph of 28 asteroids representative of all established types of binary groups. Photometric lightcurves were also obtained for 14 of them during the Spitzer observations to provide the context of the observations and reliable estimates of their absolute magnitudes. The extracted mid-IR spectra were analyzed using a modified standard thermal model (STM) and a thermophysical model (TPM) that takes into account the shape and geometry of the large primary at the time of the Spitzer observation. We derived a reliable estimate of the size, albedo, and beaming factor for each of these asteroids, representing three main taxonomic groups: C, S. and X. For large (volume-equivalent system diameter D-eq > 130 km) binary asteroids, the TPM analysis indicates a low thermal inertia (Gamma <= similar to 100 J s(-1/2) K-1 m(-2)) and their emissivity spectra display strong mineral features, implying that they are covered with a thick layer of thermally insulating regolith. The smaller (surface-equivalent system diameter D-eff < 17 km) asteroids also show some emission lines of minerals, but they are significantly weaker, consistent with regoliths with coarser grains, than those of the large binary asteroids. The average bulk densities of these multiple asteroids vary from 0.7-1.7 g/cm(3) (P-, C-type) to similar to 2 g/cm(3) (S-type). The highest density is estimated for the M-type (22) Kalliope (3.2 +/- 0.9 g/cm(3)). The spectral energy distributions (SEDs) and emissivity spectra, made available as a supplement document, could help to constrain the surface compositions of these asteroids. (C) 2012 Elsevier Inc. All rights reserved. C1 [Marchis, F.; Enriquez, J. E.; Baek, M.] SETI Inst, Carl Sagan Ctr, Mountain View, CA 94043 USA. [Emery, J. P.] Univ Tennessee, Knoxville, TN 37996 USA. [Mueller, M.] Univ Groningen, SRON, Netherlands Inst Space Res, NL-9700 AV Groningen, Netherlands. [Pollock, J.] Appalachian State Univ, Dept Phys & Astron, Boone, NC 28608 USA. [Assafin, M.] Univ Fed Rio de Janeiro, Observ Valongo, Rio de Janeiro, Brazil. [Vieira Martins, R.] MCT, Observ Nacl, BR-20921400 Rio De Janeiro, RJ, Brazil. [Marchis, F.; Berthier, J.; Vachier, F.] Observ Paris, Inst Mecan Celeste & Calcul Ephemerides, F-75014 Paris, France. [Cruikshank, D. P.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Lim, L. F.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Reichart, D. E.; Ivarsen, K. M.; Haislip, J. B.; LaCluyze, A. P.] Univ N Carolina, Dept Phys & Astron, Chapel Hill, NC 27514 USA. RP Marchis, F (reprint author), SETI Inst, Carl Sagan Ctr, 189 Bernardo Ave, Mountain View, CA 94043 USA. EM fmarchis@seti.org RI Assafin, Marcelo/C-3188-2013; Tecnologias espaciai, Inct/I-2415-2013; Lim, Lucy/C-9557-2012; Baek, Minjin/L-4425-2016; OI Lim, Lucy/0000-0002-9696-9654; Baek, Minjin/0000-0002-9698-2525; Mueller, Michael/0000-0003-3217-5385 FU California Institute of Technology; NASA through JPL/Caltech; National Science Foundation [AAG-0807468]; NAS FX The authors would like to thank Prof. Alan Harris from DLR and an anonymous referee for their valuable comments which improved significantly the quality of this article. This work is based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory. California Institute of Technology under a Contract with NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech. FMA, JEN & MBA were supported by the National Science Foundation under Award Number AAG-0807468. NR 121 TC 16 Z9 16 U1 0 U2 4 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 J9 ICARUS JI Icarus PD NOV-DEC PY 2012 VL 221 IS 2 BP 1130 EP 1161 DI 10.1016/j.icarus.2012.09.013 PG 32 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 055RL UT WOS:000312434300055 ER PT J AU Reddy, V Sanchez, JA Gaffey, MJ Abell, PA Le Corre, L Hardersen, PS AF Reddy, Vishnu Sanchez, Juan A. Gaffey, Michael J. Abell, Paul A. Le Corre, Lucille Hardersen, Paul S. TI Composition of near-Earth Asteroid (4179) Toutatis SO ICARUS LA English DT Article DE Asteroids; Asteroids, Composition; Spectroscopy; Meteorites; Infrared observations ID SPECTROSCOPIC SURVEY; REFLECTANCE SPECTRA; ORDINARY CHONDRITES; COMPLEX ROTATION; PHASE-II; METEORITES; BELT; 4179-TOUTATIS; SPECTROGRAPH; LIGHTCURVE AB Surface composition of near-Earth Asteroid (4179) Toutatis is consistent with an undiffeientiated L-chondrite composition. This is inconsistent with early observations that suggested high pyroxene iron content and a differentiated body. (C) 2012 Elsevier Inc. All rights reserved. C1 [Reddy, Vishnu; Gaffey, Michael J.; Hardersen, Paul S.] Univ N Dakota, Dept Space Studies, Grand Forks, ND 58202 USA. [Reddy, Vishnu; Le Corre, Lucille] Max Planck Inst Solar Syst Res, D-37191 Katlenburg Lindau, Germany. [Sanchez, Juan A.] Univ Munster, Inst Planetol, D-48149 Munster, Germany. [Abell, Paul A.] NASA, Lyndon B Johnson Space Ctr, Astromat Res & Explorat Sci Directorate, Houston, TX 77058 USA. RP Reddy, V (reprint author), Univ N Dakota, Dept Space Studies, Grand Forks, ND 58202 USA. EM reddy@space.edu RI Hardersen, Paul/N-9343-2014; OI Hardersen, Paul/0000-0002-0440-9095; Reddy, Vishnu/0000-0002-7743-3491; Le Corre, Lucille/0000-0003-0349-7932 FU NASA NEOO Program [NNX12AG12G]; NASA Planetary Geology and Geophysics [NNX11AN84G] FX This research was supported by NASA NEOO Program Grant NNX12AG12G, and NASA Planetary Geology and Geophysics Grant NNX11AN84G. We thank the IRTF TAC for awarding time to this project, and to the IRTF TOs and MKSS staff for their support. The authors would like to thank Tasha Dunn and an anonymous reviewer for their helpful reviews to improve the manuscript. NR 29 TC 11 Z9 12 U1 1 U2 16 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 J9 ICARUS JI Icarus PD NOV-DEC PY 2012 VL 221 IS 2 BP 1177 EP 1179 DI 10.1016/j.icarus.2012.10.005 PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 055RL UT WOS:000312434300058 ER PT J AU Hurwitz, FI Guo, HQ Rogers, RB Sheets, EJ Miller, DR Newlin, KN Shave, MK Palczer, AR Cox, MT AF Hurwitz, Frances I. Guo, Haiquan Rogers, Richard B. Sheets, Erik J. Miller, Derek R. Newlin, Katy N. Shave, Molly K. Palczer, Anna R. Cox, Michael T. TI Influence of Ti addition on boehmite-derived aluminum silicate aerogels: structure and properties SO JOURNAL OF SOL-GEL SCIENCE AND TECHNOLOGY LA English DT Article DE Aerogel; Boehmite; Aluminum silicate; Titanium isopropoxide; Al2TiO5; Mullite ID SOL-GEL PROCESS; SYSTEMS; OXIDES; ROUTE; PHASE AB Aluminosilicate aerogels offer potential for extremely low thermal conductivities at temperatures greater than 900 A degrees C, beyond where silica aerogels reach their upper temperature use limits. Aerogels have been synthesized at two Al:Si ratios, a 3Al:1Si mullite composition, and an 8Al:1Si alumina rich composition. Boehmite (AlOOH) is used as the Al source, and tetraethoxysilane as the Si precursor. The influence of Ti as a ternary constituent, introduced through the addition of titanium isopropoxide in the sol-gel synthesis, on aerogel morphology and thermal properties is evaluated. Four different boehmite precursor powders are evaluated. Morphology, surface area and pore size, and thermal transformation vary with the crystallite size of the starting boehmite powder, as does incorporation of titanium and evolution of Ti-containing crystalline phases. The addition of Ti influences sol viscosity, gelation time, surface area and pore size distribution, as well as phase formation on heat treatment. C1 [Hurwitz, Frances I.; Rogers, Richard B.; Palczer, Anna R.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. [Guo, Haiquan] Ohio Aerosp Inst, Cleveland, OH USA. [Sheets, Erik J.] Purdue Univ, W Lafayette, IN 47907 USA. [Miller, Derek R.] Michigan State Univ, E Lansing, MI 48824 USA. [Newlin, Katy N.] Univ Louisville, Louisville, KY 40292 USA. [Shave, Molly K.] Colorado Sch Mines, Golden, CO 80401 USA. [Cox, Michael T.] Arctic Slope Reg Corp, Cleveland, OH USA. RP Hurwitz, FI (reprint author), NASA, Glenn Res Ctr, 21000 Brookpark Rd, Cleveland, OH 44135 USA. EM frances.hurwitz@nasa.gov NR 20 TC 3 Z9 3 U1 2 U2 28 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0928-0707 EI 1573-4846 J9 J SOL-GEL SCI TECHN JI J. Sol-Gel Sci. Technol. PD NOV PY 2012 VL 64 IS 2 BP 367 EP 374 DI 10.1007/s10971-012-2866-8 PG 8 WC Materials Science, Ceramics SC Materials Science GA 057SN UT WOS:000312584400014 ER PT J AU Lopez, J Boyd, D Ylitalo, GM Littnan, C Pearce, R AF Lopez, Jessica Boyd, Daryle Ylitalo, Gina M. Littnan, Charles Pearce, Ronald TI Persistent organic pollutants in the endangered Hawaiian monk seal (Monachus schauinslandi) from the main Hawaiian Islands SO MARINE POLLUTION BULLETIN LA English DT Article DE Hawaiian monk seal; Monachus schauinslandi; Persistent organic pollutants; Endangered species; Hawaii; Contaminants ID LIONS ZALOPHUS-CALIFORNIANUS; ORGANOCHLORINE PESTICIDES; HARBOR SEALS; POLYCHLORINATED-BIPHENYLS; CALLORHINUS-URSINUS; GLOBAL TRANSPORT; FLAME RETARDANTS; PHOCA-VITULINA; ELEPHANT SEALS; GREY SEALS AB Little is known about levels or effects of persistent organic pollutants (POPs) in Hawaiian monk seals (HMS) from the main Hawaiian Islands (MHI) subpopulation. This study examined concentrations of a large suite of POPs in blubber and serum of juvenile and adult HMS from the MHI. Adult females have the lowest blubber levels of most POPs, whereas adult males have highest levels. POPs in serum were significantly different in adult males compared with adult females for chlordanes and summed dichlorodiphenyltrichloroethanes (DDTs). Lipid-normalized concentrations of chlordanes, DDTs, polychlorinated biphenyls, and mirex in paired blubber and serum samples were significantly correlated. Contaminant levels from the MHI were at similar or lower levels than those from remote Northwestern Hawaiian Island populations. Determining initial ranges of POPs is an important step towards assessing one of the many potential health threats to this critically endangered species. (C) 2012 Elsevier Ltd. All rights reserved. C1 [Lopez, Jessica] Univ Hawaii, Joint Inst Marine & Atmospher Res, Honolulu, HI 96814 USA. [Lopez, Jessica] Hawaii Pacific Univ, Kaneohe, HI 96744 USA. [Boyd, Daryle; Ylitalo, Gina M.; Pearce, Ronald] NOAA, Natl Marine Fisheries Serv, NW Fisheries Sci Ctr, Seattle, WA 98112 USA. [Littnan, Charles] NOAA, Natl Marine Fisheries Serv, Pacific Isl Fisheries Sci Ctr, Honolulu, HI 96814 USA. RP Lopez, J (reprint author), Univ Hawaii, Joint Inst Marine & Atmospher Res, JBPHH, 1025 Quincy Ave,Ste 5010, Manoa, HI 96860 USA. EM Jessica.Lopez@noaa.gov; Daryle.Boyd@noaa.gov; Gina.Ylitalo@noaa.gov; Charles.Litnnan@noaa.gov; Ronald.W.Pearce@noaa.gov FU NOAA's PIFSC; NOAA's Nancy Foster Scholarship program FX The NOAA Pacific Islands Fisheries Science Center (PIFSC) Hawaiian Monk Seal Research Program staff provided samples and life history information. We especially thank Lizabeth Kashinsky and Angie Kaufman for assistance with samples; Tracy Wurth, and Thea Johanos for individual seal information; Chad Yoshinaga, Kenady Wilson, and Jason Baker, for field assistance. Thanks to Bernadita Anulacion, Jennie Bolton, Catherine Sloan, Karen Tilbury and their colleagues at the Northwest Fisheries Science Center Environmental Assessment program for sample analysis and guidance. A special thank you to David Hyrenbach, Jason Baker, and Brenda Jensen for helping with manuscript edits. Funding was provided by NOAA's PIFSC and NOAA's Nancy Foster Scholarship program. All sample collection and research was conducted under the Marine Mammal Protection Act Scientific Research Permit Numbers 848-1335, 848-1695 and 10137 and safe handling and capture protocols of NOAA Fisheries. NR 67 TC 10 Z9 10 U1 3 U2 76 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0025-326X EI 1879-3363 J9 MAR POLLUT BULL JI Mar. Pollut. Bull. PD NOV PY 2012 VL 64 IS 11 BP 2588 EP 2598 DI 10.1016/j.marpolbul.2012.07.012 PG 11 WC Environmental Sciences; Marine & Freshwater Biology SC Environmental Sciences & Ecology; Marine & Freshwater Biology GA 055LP UT WOS:000312418100052 PM 22884537 ER PT J AU Scott, P Savage, C Edsjo, J Collaboration, I Abbasi, R Abdou, Y Ackermann, M Adams, J Aguilar, JA Ahlers, M Altmann, D Andeen, K Enberg, JAF Bai, X Baker, M Barwick, SW Baum, V Bay, R Beattie, K Beatty, JJ Bechet, S Tjus, JB Becker, KH Bell, M Benabderrahmane, ML BenZvi, S Berdermann, J Berghaus, P Berley, D Bernardini, E Bertrand, D Besson, DZ Bindig, D Bissok, M Blaufuss, E Blumenthal, J Boersma, DJ Bohm, C Bose, D Boser, S Botner, O Brayeur, L Brown, AM Bruijn, R Brunner, J Buitink, S Caballero-Mora, KS Carson, M Casey, J Casier, M Chirkin, D Christy, B Clevermann, F Cohen, S Cowen, DF Silva, AHC Danninger, M Daughhetee, J Davis, JC De Clercq, C Descamps, F Desiati, P de Vries-Uiterweerd, G DeYoung, T Diaz-Velez, JC Dreyer, J Dumm, JP Dunkman, M Eagan, R Eisch, J Ellsworth, RW Engdegard, O Euler, S Evenson, PA Fadiran, O Fazely, AR Fedynitch, A Feintzeig, J Feusels, T Filimonov, K Finley, C Fischer-Wasels, T Flis, S Franckowiak, A Franke, R Frantzen, K Fuchs, T Gaisser, TK Gallagher, J Gerhardt, L Gladstone, L Glusenkamp, T Goldschmidt, A Goodman, JA Gora, D Grant, D Gross, A Grullon, S Gurtner, M Ha, C Ismail, AH Hallgren, A Halzen, F Hanson, K Heereman, D Heimann, P Heinen, D Helbing, K Hellauer, R Hickford, S Hill, GC Hoffman, KD Hoffmann, R Homeier, A Hoshina, K Huelsnitz, W Hulth, PO Hultqvist, K Hussain, S Ishihara, A Jacobi, E Jacobsen, J Japaridze, GS Jlelati, O Johansson, H Kappes, A Karg, T Karle, A Kiryluk, J Kislat, F Klas, J Klein, SR Kohne, JH Kohnen, G Kolanoski, H Kopke, L Kopper, C Kopper, S Koskinen, DJ Kowalski, M Krasberg, M Kroll, G Kunnen, J Kurahashi, N Kuwabara, T Labare, M Laihem, K Landsman, H Larson, MJ Lauer, R Lesiak-Bzdak, M Lunemann, J Madsen, J Maruyama, R Mase, K Matis, HS McNally, F Meagher, K Merck, M Meszaros, P Meures, T Miarecki, S Middell, E Milke, N Miller, J Mohrmann, L Montaruli, T Morse, R Movit, SM Nahnhauer, R Naumann, U Nowicki, SC Nygren, DR Obertacke, A Odrowski, S Olivas, A Olivo, M O'Murchadha, A Panknin, S Paul, L Pepper, JA de los Heros, CP Pieloth, D Pirk, N Posselt, J Price, PB Przybylski, GT Raedel, L Rawlins, K Redl, P Resconi, E Rhode, W Ribordy, M Richman, M Riedel, B Rodrigues, JP Rothmaier, F Rott, C Ruhe, T Rutledge, D Ruzybayev, B Ryckbosch, D Saba, SM Salameh, T Sander, HG Santander, M Sarkar, S Schatto, K Scheel, M Scheriau, F Schmidt, T Schmitz, M Schoenen, S Schoneberg, S Schonherr, L Schonwald, A Schukraft, A Schulte, L Schulz, O Seckel, D Seo, SH Sestayo, Y Seunarine, S Smith, MWE Soiron, M Soldin, D Spiczak, GM Spiering, C Stamatikos, M Stanev, T Stasik, A Stezelberger, T Stokstad, RG Stoessl, A Strahler, EA Strom, R Sullivan, GW Taavola, H Taboada, I Tamburro, A Ter-Antonyan, S Tilav, S Toale, PA Toscano, S Usner, M van Eijndhoven, N van der Drift, D Van Overloop, A van Santen, J Vehring, M Voge, M Walck, C Waldenmaier, T Wallraff, M Walter, M Wasserman, R Weaver, C Wendt, C Westerhoff, S Whitehorn, N Wiebe, K Wiebusch, CH Williams, DR Wissing, H Wolf, M Wood, TR Woschnagg, K Xu, C Xu, DL Xu, XW Yanez, JP Yodh, G Yoshida, S Zarzhitsky, P Ziemann, J Zilles, A Zoll, M AF Scott, P. Savage, C. Edsjo, J. Collaboration, IceCube Abbasi, R. Abdou, Y. Ackermann, M. Adams, J. Aguilar, J. A. Ahlers, M. Altmann, D. Andeen, K. Enberg, J. Au Ff Bai, X. Baker, M. Barwick, S. W. Baum, V. Bay, R. Beattie, K. Beatty, J. J. Bechet, S. Tjus, J. Becker Becker, K. -H. Bell, M. Benabderrahmane, M. L. BenZvi, S. Berdermann, J. Berghaus, P. Berley, D. Bernardini, E. Bertrand, D. Besson, D. Z. Bindig, D. Bissok, M. Blaufuss, E. Blumenthal, J. Boersma, D. J. Bohm, C. Bose, D. Boeser, S. Botner, O. Brayeur, L. Brown, A. M. Bruijn, R. Brunner, J. Buitink, S. Caballero-Mora, K. S. Carson, M. Casey, J. Casier, M. Chirkin, D. Christy, B. Clevermann, F. Cohen, S. Cowen, D. F. Silva, A. H. Cruz Danninger, M. Daughhetee, J. Davis, J. C. De Clercq, C. Descamps, F. Desiati, P. de Vries-Uiterweerd, G. DeYoung, T. Diaz-Velez, J. C. Dreyer, J. Dumm, J. P. Dunkman, M. Eagan, R. Eisch, J. Ellsworth, R. W. Engdegard, O. Euler, S. Evenson, P. A. Fadiran, O. Fazely, A. R. Fedynitch, A. Feintzeig, J. Feusels, T. Filimonov, K. Finley, C. Fischer-Wasels, T. Flis, S. Franckowiak, A. Franke, R. Frantzen, K. Fuchs, T. Gaisser, T. K. Gallagher, J. Gerhardt, L. Gladstone, L. Gluesenkamp, T. Goldschmidt, A. Goodman, J. A. Gora, D. Grant, D. Gross, A. Grullon, S. Gurtner, M. Ha, C. Ismail, A. Haj Hallgren, A. Halzen, F. Hanson, K. Heereman, D. Heimann, P. Heinen, D. Helbing, K. Hellauer, R. Hickford, S. Hill, G. C. Hoffman, K. D. Hoffmann, R. Homeier, A. Hoshina, K. Huelsnitz, W. Hulth, P. O. Hultqvist, K. Hussain, S. Ishihara, A. Jacobi, E. Jacobsen, J. Japaridze, G. S. Jlelati, O. Johansson, H. Kappes, A. Karg, T. Karle, A. Kiryluk, J. Kislat, F. Klaes, J. Klein, S. R. Koehne, J. -H. Kohnen, G. Kolanoski, H. Koepke, L. Kopper, C. Kopper, S. Koskinen, D. J. Kowalski, M. Krasberg, M. Kroll, G. Kunnen, J. Kurahashi, N. Kuwabara, T. Labare, M. Laihem, K. Landsman, H. Larson, M. J. Lauer, R. Lesiak-Bzdak, M. Luenemann, J. Madsen, J. Maruyama, R. Mase, K. Matis, H. S. McNally, F. Meagher, K. Merck, M. Meszaros, P. Meures, T. Miarecki, S. Middell, E. Milke, N. Miller, J. Mohrmann, L. Montaruli, T. Morse, R. Movit, S. M. Nahnhauer, R. Naumann, U. Nowicki, S. C. Nygren, D. R. Obertacke, A. Odrowski, S. Olivas, A. Olivo, M. O'Murchadha, A. Panknin, S. Paul, L. Pepper, J. A. de los Heros, C. Perez Pieloth, D. Pirk, N. Posselt, J. Price, P. B. Przybylski, G. T. Raedel, L. Rawlins, K. Redl, P. Resconi, E. Rhode, W. Ribordy, M. Richman, M. Riedel, B. Rodrigues, J. P. Rothmaier, F. Rott, C. Ruhe, T. Rutledge, D. Ruzybayev, B. Ryckbosch, D. Saba, S. M. Salameh, T. Sander, H. -G. Santander, M. Sarkar, S. Schatto, K. Scheel, M. Scheriau, F. Schmidt, T. Schmitz, M. Schoenen, S. Schoeneberg, S. Schoenherr, L. Schoenwald, A. Schukraft, A. Schulte, L. Schulz, O. Seckel, D. Seo, S. H. Sestayo, Y. Seunarine, S. Smith, M. W. E. Soiron, M. Soldin, D. Spiczak, G. M. Spiering, C. Stamatikos, M. Stanev, T. Stasik, A. Stezelberger, T. Stokstad, R. G. Stoessl, A. Strahler, E. A. Strom, R. Sullivan, G. W. Taavola, H. Taboada, I. Tamburro, A. Ter-Antonyan, S. Tilav, S. Toale, P. A. Toscano, S. Usner, M. van Eijndhoven, N. van der Drift, D. Van Overloop, A. van Santen, J. Vehring, M. Voge, M. Walck, C. Waldenmaier, T. Wallraff, M. Walter, M. Wasserman, R. Weaver, Ch. Wendt, C. Westerhoff, S. Whitehorn, N. Wiebe, K. Wiebusch, C. H. Williams, D. R. Wissing, H. Wolf, M. Wood, T. R. Woschnagg, K. Xu, C. Xu, D. L. Xu, X. W. Yanez, J. P. Yodh, G. Yoshida, S. Zarzhitsky, P. Ziemann, J. Zilles, A. Zoll, M. TI Use of event-level neutrino telescope data in global fits for theories of new physics SO JOURNAL OF COSMOLOGY AND ASTROPARTICLE PHYSICS LA English DT Article DE dark matter theory; neutrino astronomy; dark matter experiments; cosmology of theories beyond the SM ID DARK-MATTER CANDIDATES; OBSERVATIONS COSMOLOGICAL INTERPRETATION; CONSTRAINTS; SUPERSYMMETRY; LIMITS; LHC; CAPTURE; SEARCH; LIGHT AB We present a fast likelihood method for including event-level neutrino telescope data in parameter explorations of theories for new physics, and announce its public release as part of DarkSUSY 5.0.6. Our construction includes both angular and spectral information about neutrino events, as well as their total number. We also present a corresponding measure for simple model exclusion, which can be used for single models without reference to the rest of a parameter space. We perform a number of supersymmetric parameter scans with IceCube data to illustrate the utility of the method: example global fits and a signal recovery in the constrained minimal supersymmetric standard model (CMSSM), and a model exclusion exercise in a 7-parameter phenomenological version of the MSSM. The final IceCube detector con figuration will probe almost the entire focus-point region of the CMSSM, as well as a number of MSSM-7 models that will not otherwise be accessible to e. g. direct detection. Our method accurately recovers the mock signal, and provides tight constraints on model parameters and derived quantities. We show that the inclusion of spectral information significantly improves the accuracy of the recovery, providing motivation for its use in future IceCube analyses. C1 [Scott, P.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Savage, C.; Edsjo, J.; Bohm, C.; Danninger, M.; Finley, C.; Flis, S.; Hulth, P. O.; Hultqvist, K.; Johansson, H.; Seo, S. H.; Walck, C.; Wolf, M.; Zoll, M.] Stockholm Univ, Oskar Klein Ctr Cosmoparticle Phys, SE-10691 Stockholm, Sweden. [Savage, C.; Edsjo, J.; Bohm, C.; Danninger, M.; Finley, C.; Flis, S.; Hulth, P. O.; Hultqvist, K.; Johansson, H.; Seo, S. H.; Walck, C.; Wolf, M.; Zoll, M.] Stockholm Univ, Dept Phys, SE-10691 Stockholm, Sweden. [Abbasi, R.; Ahlers, M.; Andeen, K.; Enberg, J. Au Ff; Baker, M.; BenZvi, S.; Chirkin, D.; Descamps, F.; Desiati, P.; Diaz-Velez, J. C.; Dumm, J. P.; Eisch, J.; Fadiran, O.; Feintzeig, J.; Gladstone, L.; Grullon, S.; Halzen, F.; Hoshina, K.; Jacobsen, J.; Karle, A.; Kopper, C.; Krasberg, M.; Kurahashi, N.; Landsman, H.; Maruyama, R.; McNally, F.; Merck, M.; Morse, R.; Riedel, B.; Rodrigues, J. P.; Santander, M.; Toscano, S.; van Santen, J.; Weaver, Ch.; Wendt, C.; Westerhoff, S.; Whitehorn, N.] Univ Wisconsin, Dept Phys, Madison, WI 53706 USA. [Abbasi, R.; Ahlers, M.; Andeen, K.; Enberg, J. Au Ff; Baker, M.; BenZvi, S.; Chirkin, D.; Descamps, F.; Desiati, P.; Diaz-Velez, J. C.; Dumm, J. P.; Eisch, J.; Fadiran, O.; Feintzeig, J.; Gladstone, L.; Grullon, S.; Halzen, F.; Hoshina, K.; Jacobsen, J.; Karle, A.; Kopper, C.; Krasberg, M.; Kurahashi, N.; Landsman, H.; Maruyama, R.; McNally, F.; Merck, M.; Morse, R.; Riedel, B.; Rodrigues, J. P.; Santander, M.; Toscano, S.; van Santen, J.; Weaver, Ch.; Wendt, C.; Westerhoff, S.; Whitehorn, N.] Univ Wisconsin, Wisconsin IceCube Particle Astrophys Ctr, Madison, WI 53706 USA. [Abdou, Y.; Carson, M.; de Vries-Uiterweerd, G.; Feusels, T.; Ismail, A. Haj; Jlelati, O.; Ryckbosch, D.; Van Overloop, A.] Univ Ghent, Dept Phys & Astron, B-9000 Ghent, Belgium. [Ackermann, M.; Benabderrahmane, M. L.; Berdermann, J.; Berghaus, P.; Bernardini, E.; Brunner, J.; Silva, A. H. Cruz; Franke, R.; Gluesenkamp, T.; Gora, D.; Jacobi, E.; Karg, T.; Kislat, F.; Lauer, R.; Middell, E.; Mohrmann, L.; Nahnhauer, R.; Pirk, N.; Schoenwald, A.; Spiering, C.; Stoessl, A.; Walter, M.; Yanez, J. P.] DESY, D-15735 Zeuthen, Germany. [Adams, J.; Brown, A. M.; Hickford, S.] Univ Canterbury, Dept Phys & Astron, Christchurch 1, New Zealand. [Aguilar, J. A.; Montaruli, T.] Univ Geneva, Dept Phys Nucl & Corpusculaire, CH-1211 Geneva, Switzerland. [Altmann, D.; Kappes, A.; Kolanoski, H.; Waldenmaier, T.] Humboldt Univ, Inst Phys, D-12489 Berlin, Germany. [Bai, X.; Evenson, P. A.; Gaisser, T. K.; Hussain, S.; Kuwabara, T.; Ruzybayev, B.; Seckel, D.; Stanev, T.; Tamburro, A.; Tilav, S.; Xu, C.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA. [Bai, X.; Evenson, P. A.; Gaisser, T. K.; Hussain, S.; Kuwabara, T.; Ruzybayev, B.; Seckel, D.; Stanev, T.; Tamburro, A.; Tilav, S.; Xu, C.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA. [Bai, X.] S 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. [Baum, V.; Koepke, L.; Kroll, G.; Luenemann, J.; Sander, H. -G.; Schatto, K.; Wiebe, K.] Johannes Gutenberg Univ Mainz, Inst Phys, D-55099 Mainz, Germany. [Bay, R.; Filimonov, K.; Gerhardt, L.; Ha, C.; Klein, S. R.; Miarecki, S.; Price, P. B.; Rothmaier, F.; van der Drift, D.; Woschnagg, K.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Beattie, K.; 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.; van der Drift, D.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. [Beatty, J. J.; Davis, J. C.; Rott, C.; Stamatikos, M.] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA. [Beatty, J. J.; Davis, J. C.; Rott, C.; Stamatikos, M.] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA. [Beatty, J. J.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Bechet, S.; Bertrand, D.; Hanson, K.; Heereman, D.; Meures, T.; O'Murchadha, A.] Univ Libre Bruxelles, Fac Sci, B-1050 Brussels, Belgium. [Tjus, J. Becker; Dreyer, J.; Fedynitch, A.; Olivo, M.; Saba, S. M.; Schoeneberg, S.] Ruhr Univ Bochum, Fak Phys & Astron, D-44780 Bochum, Germany. [Becker, K. -H.; Bindig, D.; Fischer-Wasels, T.; Gurtner, M.; Helbing, K.; Hoffmann, R.; Klaes, J.; Kopper, S.; Naumann, U.; Obertacke, A.; Posselt, J.; Soldin, D.] Univ Wuppertal, Dept Phys, D-42119 Wuppertal, Germany. [Bell, M.; Caballero-Mora, K. S.; Cowen, D. F.; DeYoung, T.; Dunkman, M.; Eagan, R.; Koskinen, D. J.; Meszaros, P.; Rutledge, D.; Salameh, T.; Smith, M. W. E.; Wasserman, R.] Penn State Univ, Dept Phys, University Pk, PA 16802 USA. [Berley, D.; Blaufuss, E.; Christy, B.; Ellsworth, R. W.; Goodman, J. A.; Hellauer, R.; Hoffman, K. D.; Huelsnitz, W.; Meagher, K.; Olivas, A.; Redl, P.; Richman, M.; Schmidt, T.; Sullivan, G. W.; Wissing, H.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA. [Besson, D. Z.] Univ Kansas, Dept Phys & Astron, Lawrence, KS 66045 USA. [Bissok, M.; Blumenthal, J.; Boersma, D. J.; Euler, S.; Heimann, P.; Heinen, D.; Laihem, K.; Paul, L.; Raedel, L.; Scheel, M.; Schoenen, S.; Schoenherr, L.; Schukraft, A.; Soiron, M.; Vehring, M.; Wallraff, M.; Wiebusch, C. H.; Zilles, A.] Rhein Westfal TH Aachen, Inst Phys 3, D-52056 Aachen, Germany. [Bose, D.; Brayeur, L.; Buitink, S.; Casier, M.; De Clercq, C.; Kunnen, J.; Labare, M.; Miller, J.; Strahler, E. A.; van Eijndhoven, N.] Vrije Univ Brussel, Dienst ELEM, B-1050 Brussels, Belgium. [Boeser, S.; Franckowiak, A.; Homeier, A.; Kowalski, M.; Panknin, S.; Schulte, L.; Stasik, A.; Usner, M.; Voge, M.] Univ Bonn, Inst Phys, D-53115 Bonn, Germany. [Botner, O.; Engdegard, O.; Hallgren, A.; de los Heros, C. Perez; Strom, R.; Taavola, H.] Uppsala Univ, Dept Phys & Astron, S-75120 Uppsala, Sweden. [Bruijn, R.; Cohen, S.; Ribordy, M.] Ecole Polytech Fed Lausanne, High Energy Phys Lab, CH-1015 Lausanne, Switzerland. [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. [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.; Meszaros, P.; Movit, S. M.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Fazely, A. R.; Ter-Antonyan, S.; Xu, X. W.] Southern Univ, Dept Phys, Baton Rouge, LA 70813 USA. [Gallagher, J.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. [Grant, D.; Nowicki, S. C.; Wood, T. R.] Univ Alberta, Dept Phys, Edmonton, AB T6G 2G7, Canada. [Gross, A.; Odrowski, S.; Resconi, E.; Schulz, O.; Sestayo, Y.] Tech Univ Munich, D-85748 Garching, Germany. [Hill, G. C.] Univ Adelaide, Sch Chem & Phys, Adelaide, SA 5005, Australia. [Huelsnitz, W.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA. [Ishihara, A.; Mase, K.; Yoshida, S.] Chiba Univ, Dept Phys, Chiba 2638522, Japan. [Japaridze, G. S.] Clark Atlanta Univ, CTSPS, Atlanta, GA 30314 USA. [Kiryluk, J.; Lesiak-Bzdak, M.] SUNY Stony Brook, Dept Phys & Astron, Stony Brook, NY 11794 USA. [Kohnen, G.] Univ Mons, B-7000 Mons, Belgium. [Larson, M. J.; Pepper, J. A.; Toale, P. A.; Williams, D. R.; Xu, D. L.; Zarzhitsky, P.] Univ Alabama, Dept Phys & Astron, Tuscaloosa, AL 35487 USA. [Madsen, J.; Spiczak, G. M.] Univ Wisconsin, Dept Phys, River Falls, WI 54022 USA. [Montaruli, T.] Univ Bari, Dipartmento Fis, Sez INFN, I-70126 Bari, Italy. [Rawlins, K.] Univ Alaska Anchorage, Dept Phys & Astron, Anchorage, AK 99508 USA. [Sarkar, S.] Univ Oxford, Dept Phys, Oxford OX1 3NP, England. [Seunarine, S.] Univ W Indies, Dept Phys, BB-11000 Bridgetown, Barbados. [Stamatikos, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Scott, P (reprint author), McGill Univ, Dept Phys, 3600 Rue Univ, Montreal, PQ H3A 2T8, Canada. EM patscott@physics.mcgill.ca; savage@fysik.su.se; danning@fysik.su.se RI Wiebusch, Christopher/G-6490-2012; Koskinen, David/G-3236-2014; Brunner, Juergen/G-3540-2015; Maruyama, Reina/A-1064-2013; Sarkar, Subir/G-5978-2011; Beatty, James/D-9310-2011; Tamburro, Alessio/A-5703-2013; Botner, Olga/A-9110-2013; Hallgren, Allan/A-8963-2013; Tjus, Julia/G-8145-2012 OI Aguilar Sanchez, Juan Antonio/0000-0003-2252-9514; Wiebusch, Christopher/0000-0002-6418-3008; Koskinen, David/0000-0002-0514-5917; Brunner, Juergen/0000-0002-5052-7236; Maruyama, Reina/0000-0003-2794-512X; Sarkar, Subir/0000-0002-3542-858X; Beatty, James/0000-0003-0481-4952; Rott, Carsten/0000-0002-6958-6033; Ter-Antonyan, Samvel/0000-0002-5788-1369; Schukraft, Anne/0000-0002-9112-5479; FU Lorne Trottier Chair in Astrophysics; Canadian Institute for Particle Physics Theory Fellowship; Swedish Research Council [621-2010-3705, 621-2010-3301]; 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); U.S. Department of Energy; National Energy Research Scientific Computing Center; Louisiana Optical Network Initiative (LONI); National Science and Engineering Research Council of Canada; Swedish Research Council; Swedish Polar Research Secretariat; Swedish National Infrastructure for Computing (SNIC); Knut and Alice Wallenberg Foundation, Sweden; German Ministry for Education and Research (BMBF); Deutsche Forschungsgemeinschaft (DFG); Research Department of Plasmas with Complex Interactions (Bochum), Germany; Fund for Scientific Research (FNRS-FWO); FWO Odysseus programme; Flanders Institute to encourage scientific and technological research in industry (IWT); Belgian Federal Science Policy - Office (Belspo); University of Oxford, United Kingdom; Marsden Fund, New Zealand; Australian Research Council; Japan Society for Promotion of Science (JSPS); Swiss National Science Foundation (SNSF), Switzerland FX We are grateful to Hamish Silverwood for helpful comments and discussions. P. S. is supported by the Lorne Trottier Chair in Astrophysics and a Canadian Institute for Particle Physics Theory Fellowship. M. D. and K. H. acknowledge support from the Swedish Research Council (Contract No. 621-2010-3705), as does J.E. (Contract No. 621-2010-3301).; We acknowledge the support from the following agencies: U.S. National Science Foundation - Office of Polar Programs, U.S. National Science Foundation - Physics Division, University of Wisconsin Alumni Research Foundation, the Grid Laboratory Of Wisconsin (GLOW) grid infrastructure at the University of Wisconsin {Madison, the Open Science Grid (OSG) grid infrastructure; U.S. Department of Energy, and National Energy Research Scientific Computing Center, the Louisiana Optical Network Initiative (LONI) grid computing resources; National Science and Engineering Research Council of Canada; Swedish Research Council, Swedish Polar Research Secretariat, Swedish National Infrastructure for Computing (SNIC), and Knut and Alice Wallenberg Foundation, Sweden; German Ministry for Education and Research (BMBF), Deutsche Forschungsgemeinschaft (DFG), Research Department of Plasmas with Complex Interactions (Bochum), Germany; Fund for Scientific Research (FNRS-FWO), FWO Odysseus programme, Flanders Institute to encourage scientific and technological research in industry (IWT), Belgian Federal Science Policy - Office (Belspo); University of Oxford, United Kingdom; Marsden Fund, New Zealand; Australian Research Council; Japan Society for Promotion of Science (JSPS); the Swiss National Science Foundation (SNSF), Switzerland. NR 102 TC 18 Z9 18 U1 0 U2 8 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 NOV PY 2012 IS 11 AR 057 DI 10.1088/1475-7516/2012/11/057 PG 33 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 053IA UT WOS:000312263500040 ER PT J AU Klenzing, J Rowland, D AF Klenzing, J. Rowland, D. TI The fixed-bias Langmuir probe on the Communication/Navigation Outage Forecast System satellite: Calibration and validation SO REVIEW OF SCIENTIFIC INSTRUMENTS LA English DT Article ID FLOWING PLASMA; ION COLLECTION; SPHERE AB A fixed-bias spherical Langmuir probe is included as part of the Vector Electric Field Instrument (VEFI) suite on the Communication/Navigation Outage Forecast System (C/NOFS) satellite. C/NOFS gathers data in the equatorial ionosphere between 400 and 860 km, where the primary constituent ions are H+ and O+. The ion current collected by the probe surface per unit plasma density is found to be a strong function of ion composition. The calibration of the collected current to an absolute density is discussed, and the performance of the spherical probe is compared to other in situ instruments on board the C/NOFS satellite. The application of the calibration is discussed with respect to future fixed-bias probes; in particular, it is demonstrated that some density fluctuations will be suppressed in the collected current if the plasma composition rapidly changes along with density. This is illustrated in the observation of plasma density enhancements on C/NOFS. [http://dx.doi.org/10.1063/1.4766333] C1 [Klenzing, J.; Rowland, D.] NASA, Goddard Space Flight Ctr, Space Weather Lab, Greenbelt, MD 20771 USA. RP Klenzing, J (reprint author), NASA, Goddard Space Flight Ctr, Space Weather Lab, Code 674, Greenbelt, MD 20771 USA. EM jeffrey.klenzing@nasa.gov RI Klenzing, Jeff/E-2406-2011; Rowland, Douglas/F-5589-2012 OI Klenzing, Jeff/0000-0001-8321-6074; Rowland, Douglas/0000-0003-0948-6257 FU USAF Space Test Program FX The Communication/Navigation Outage Forecast System (C/NOFS) mission, conceived and developed by the Air Force Research Laboratory (AFRL), is sponsored and executed by the USAF Space Test Program. Thanks to F. Simoes for useful comments on this manuscript and P. A. Roddy of AFRL and R. A. Heelis of UT Dallas for providing data for the calibration procedure. NR 23 TC 0 Z9 0 U1 0 U2 3 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 0034-6748 J9 REV SCI INSTRUM JI Rev. Sci. Instrum. PD NOV PY 2012 VL 83 IS 11 AR 114501 DI 10.1063/1.4766333 PG 5 WC Instruments & Instrumentation; Physics, Applied SC Instruments & Instrumentation; Physics GA 050DY UT WOS:000312034400034 PM 23206077 ER PT J AU Sanjuan, J Korytov, D Mueller, G Spannagel, R Braxmaier, C Preston, A Livas, J AF Sanjuan, J. Korytov, D. Mueller, G. Spannagel, R. Braxmaier, C. Preston, A. Livas, J. TI Note: Silicon carbide telescope dimensional stability for space-based gravitational wave detectors SO REVIEW OF SCIENTIFIC INSTRUMENTS LA English DT Article AB Space-based gravitational wave detectors are conceived to detect gravitational waves in the low frequency range by measuring the distance between proof masses in spacecraft separated by millions of kilometers. One of the key elements is the telescope which has to have a dimensional stability better than 1 pm Hz(-1/2) at 3 mHz. In addition, the telescope structure must be light, strong, and stiff. For this reason a potential telescope structure consisting of a silicon carbide quadpod has been designed, constructed, and tested. We present dimensional stability results meeting the requirements at room temperature. Results at -60 degrees C are also shown although the requirements are not met due to temperature fluctuations in the setup. (C) 2012 American Institute of Physics. [http://dx.doi.org/10.1063/1.4767247] C1 [Sanjuan, J.; Korytov, D.; Mueller, G.] Univ Florida, Gainesville, FL 32611 USA. [Spannagel, R.; Braxmaier, C.] Univ Appl Sci Konstanz HTWG, D-78462 Constance, Germany. [Preston, A.; Livas, J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Sanjuan, J (reprint author), Univ Florida, Corner Gale Lemerand Dr & Museum Rd, Gainesville, FL 32611 USA. FU NASA [NNX10AJ38G, NNX11AO26G] FX The authors would like to thank J. I. Thorpe for fruitful discussions and I. Pucher, A. Cordes, and A. Spector for helping on the experimental setup. This work is supported by NASA Grant Nos. NNX10AJ38G and NNX11AO26G. NR 12 TC 7 Z9 7 U1 1 U2 1 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 0034-6748 J9 REV SCI INSTRUM JI Rev. Sci. Instrum. PD NOV PY 2012 VL 83 IS 11 AR 116107 DI 10.1063/1.4767247 PG 3 WC Instruments & Instrumentation; Physics, Applied SC Instruments & Instrumentation; Physics GA 050DY UT WOS:000312034400071 PM 23206114 ER PT J AU Feofilov, AG Kutepov, AA AF Feofilov, Artem G. Kutepov, Alexander A. TI Infrared Radiation in the Mesosphere and Lower Thermosphere: Energetic Effects and Remote Sensing SO SURVEYS IN GEOPHYSICS LA English DT Review DE Infrared energy; Radiative transfer; Mesosphere lower thermosphere ID ACCELERATED LAMBDA ITERATION; NONLOCAL THERMODYNAMIC-EQUILIBRIUM; SCHUMANN-RUNGE CONTINUUM; SPACELAB 3 OBSERVATIONS; CO2 15-MU-M EMISSION; HOT LUMINOUS STARS; NON-LTE PROBLEM; MIDDLE ATMOSPHERE; MU-M; WATER-VAPOR AB This paper discusses the formation mechanisms of infrared radiation in the mesosphere and lower thermosphere (MLT), the energetic effects of the radiative absorption/emission processes, and the retrieval of atmospheric parameters from infrared radiation measurements. In the MLT and above, the vibrational levels of the molecules involved in radiative transitions are not in local thermodynamic equilibrium (LTE) with the surrounding medium, and this then requires specific theoretical treatment. The non-LTE models for CO2, O-3, and H2O molecules are presented, and the radiative cooling/heating rates estimated for five typical atmospheric scenarios, from polar winter to polar summer, are shown. An optimization strategy for calculating the cooling/heating rates in general circulation models is proposed, and its accuracy is estimated for CO2. The sensitivity of the atmospheric quantities retrieved from infrared observations made from satellites to the non-LTE model parameters is shown. C1 [Feofilov, Artem G.] Ecole Polytech, Meteorol Dynam Lab, Palaiseau, France. [Kutepov, Alexander A.] Catholic Univ Amer, Washington, DC 20064 USA. [Kutepov, Alexander A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Feofilov, AG (reprint author), Ecole Polytech, Meteorol Dynam Lab, Palaiseau, France. EM artem.feofilov@lmd.polytechnique.fr RI Feofilov, Artem/A-2271-2015 OI Feofilov, Artem/0000-0001-9924-4846 NR 148 TC 9 Z9 10 U1 2 U2 18 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0169-3298 EI 1573-0956 J9 SURV GEOPHYS JI Surv. Geophys. PD NOV PY 2012 VL 33 IS 6 SI SI BP 1231 EP 1280 DI 10.1007/s10712-012-9204-0 PG 50 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 054SU UT WOS:000312364400003 ER PT J AU Bachelet, E Fouque, P Han, C Gould, A Albrow, MD Beaulieu, JP Bertin, E Bond, IA Christie, GW Heyrovsky, D Horne, K Jorgensen, UG Maoz, D Mathiasen, M Matsunaga, N McCormick, J Menzies, J Nataf, D Natusch, T Oi, N Renon, N Tsapras, Y Udalski, A Yee, JC Batista, V Bennett, DP Brillant, S Caldwell, JAR Cassan, A Cole, A Cook, KH Coutures, C Dieters, S Dominik, M Prester, DD Donatowicz, J Greenhill, J Kains, N Kane, SR Marquette, JB Martin, R Pollard, KR Sahu, KC Street, RA Wambsganss, J Williams, A Zub, M Bos, M Dong, SB Drummond, J Gaudi, BS Graff, D Janczak, J Kaspi, S Kozlowski, S Lee, CU Monard, LAG Munoz, JA Park, BG Pogge, RW Polishook, D Shporer, A Abe, F Botzler, CS Fukui, A Furusawa, K Hearnshaw, JB Itow, Y Korpela, AV Ling, CH Masuda, K Matsubara, Y Miyake, N Muraki, Y Ohnishi, K Rattenbury, NJ Saito, T Sullivan, D Sumi, T Suzuki, D Sweatman, WL Tristram, PJ Wada, K Allan, A Bode, MF Bramich, DM Clay, N Fraser, SN Hawkins, E Kerins, E Lister, TA Mottram, CJ Saunders, ES Snodgrass, C Steele, IA Wheatley, PJ Bozza, V Browne, P Burgdorf, MJ Novati, SC Dreizler, S Finet, F Glitrup, M Grundahl, F Harpsoe, K Hessman, FV Hinse, TC Hundertmark, M Liebig, C Maier, G Mancini, L Rahvar, S Ricci, D Scarpetta, G Skottfelt, J Southworth, J Surdej, J Zimmer, F AF Bachelet, E. Fouque, P. Han, C. Gould, A. Albrow, M. D. Beaulieu, J. -P. Bertin, E. Bond, I. A. Christie, G. W. Heyrovsky, D. Horne, K. Jorgensen, U. G. Maoz, D. Mathiasen, M. Matsunaga, N. McCormick, J. Menzies, J. Nataf, D. Natusch, T. Oi, N. Renon, N. Tsapras, Y. Udalski, A. Yee, J. C. Batista, V. Bennett, D. P. Brillant, S. Caldwell, J. A. R. Cassan, A. Cole, A. Cook, K. H. Coutures, C. Dieters, S. Dominik, M. Prester, D. Dominis Donatowicz, J. Greenhill, J. Kains, N. Kane, S. R. Marquette, J. -B. Martin, R. Pollard, K. R. Sahu, K. C. Street, R. A. Wambsganss, J. Williams, A. Zub, M. Bos, M. Dong, Subo Drummond, J. Gaudi, B. S. Graff, D. Janczak, J. Kaspi, S. Kozlowski, S. Lee, C. -U. Monard, L. A. G. Munoz, J. A. Park, B. -G. Pogge, R. W. Polishook, D. Shporer, A. Abe, F. Botzler, C. S. Fukui, A. Furusawa, K. Hearnshaw, J. B. Itow, Y. Korpela, A. V. Ling, C. H. Masuda, K. Matsubara, Y. Miyake, N. Muraki, Y. Ohnishi, K. Rattenbury, N. J. Saito, To. Sullivan, D. Sumi, T. Suzuki, D. Sweatman, W. L. Tristram, P. J. Wada, K. Allan, A. Bode, M. F. Bramich, D. M. Clay, N. Fraser, S. N. Hawkins, E. Kerins, E. Lister, T. A. Mottram, C. J. Saunders, E. S. Snodgrass, C. Steele, I. A. Wheatley, P. J. Bozza, V. Browne, P. Burgdorf, M. J. Novati, S. Calchi Dreizler, S. Finet, F. Glitrup, M. Grundahl, F. Harpsoe, K. Hessman, F. V. Hinse, T. C. Hundertmark, M. Liebig, C. Maier, G. Mancini, L. Rahvar, S. Ricci, D. Scarpetta, G. Skottfelt, J. Southworth, J. Surdej, J. Zimmer, F. CA PLANET Collaboration FUN Collaboration MOA Collaboration RoboNet-II Collaboration MiNDSTEp Consortium TI A brown dwarf orbiting an M-dwarf: MOA 2009-BLG-411L SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE binaries: general; gravitational lensing: micro; stars: individual: MOA 2009-BLG-411L ID MAGNIFICATION MICROLENSING EVENTS; SURFACE BRIGHTNESS RELATIONS; DIFFERENCE IMAGE-ANALYSIS; CLUMP ABSOLUTE MAGNITUDE; GALACTIC BULGE FIELDS; INTERSTELLAR EXTINCTION; BINARY INTERPRETATIONS; CENTRAL PERTURBATIONS; PLANETARY SYSTEMS; MASS PLANET AB Context. Caustic crossing is the clearest signature of binary lenses in microlensing. In the present context, this signature is diluted by the large source star but a detailed analysis has allowed the companion signal to be extracted. Aims. MOA 2009-BLG-411 was detected on August 5, 2009 by the MOA-Collaboration. Alerted as a high-magnification event, it was sensitive to planets. Suspected anomalies in the light curve were not confirmed by a real-time model, but further analysis revealed small deviations from a single lens extended source fit. Methods. Thanks to observations by all the collaborations, this event was well monitored. We first decided to characterize the source star properties by using a more refined method than the classical one: we measure the interstellar absorption along the line of sight in five different passbands (VIJHK). Secondly, we model the lightcurve by using the standard technique: make (s, q, alpha) grids to look for local minima and refine the results by using a downhill method (Markov chain Monte Carlo). Finally, we use a Galactic model to estimate the physical properties of the lens components. Results. We find that the source star is a giant G star with radius 9 R-circle dot. The grid search gives two local minima, which correspond to the theoretical degeneracy s = s(-1). We find that the lens is composed of a brown dwarf secondary of mass M-S = 0.05 M-circle dot orbiting a primary M-star of mass M-P = 0.18 M-circle dot. We also reveal a new mass-ratio degeneracy for the central caustics of close binaries. Conclusions. As far as we are aware, this is the first detection using the microlensing technique of a binary system in our Galaxy composed of an M-star and a brown dwarf. C1 [Gould, A.; Nataf, D.; Yee, J. C.; Gaudi, B. S.; Janczak, J.; Kozlowski, S.; Pogge, R. W.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Albrow, M. D.; Pollard, K. R.; Hearnshaw, J. B.] Univ Canterbury, Dept Phys & Astron, Christchurch 8020, New Zealand. [Brillant, S.; Snodgrass, C.] European So Observ, Santiago 19, Chile. [Kains, N.; Bramich, D. M.] European So Observ, D-85748 Garching, Germany. [Beaulieu, J. -P.; Bertin, E.; Batista, V.; Cassan, A.; Coutures, C.; Dieters, S.; Marquette, J. -B.] Univ Paris 06, Inst Astrophys Paris, CNRS, F-75014 Paris, France. [Wambsganss, J.; Zub, M.; Liebig, C.; Maier, G.; Zimmer, F.] Heidelberg Univ, ARI, Zentrum Astron, D-69120 Heidelberg, Germany. [Horne, K.; Dominik, M.; Kains, N.; Browne, P.; Liebig, C.] Univ St Andrews, Sch Phys & Astron, Scottish Univ Phys Alliance, St Andrews KY16 9SS, Fife, Scotland. Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA. [Bennett, D. P.; Caldwell, J. A. R.] Univ Texas, McDonald Observ, Ft Davis, TX 79734 USA. [Cook, K. H.] Lawrence Livermore Natl Lab, IGPP, Livermore, CA 94551 USA. [Prester, D. Dominis] Univ Rijeka, Fac Arts & Sci, Dept Phys, Rijeka 51000, Croatia. [Donatowicz, J.] Vienna Univ Technol, Dept Comp, A-1060 Vienna, Austria. [Cole, A.; Greenhill, J.] Univ Tasmania, Sch Math & Phys, Hobart, Tas 7001, Australia. [Kane, S. R.] CALTECH, NASA Exoplanet Sci Inst, Pasadena, CA 91125 USA. [Martin, R.; Williams, A.] Perth Observ, Perth, WA 6076, Australia. [Menzies, J.] S African Astron Observ, ZA-7925 Observatory, South Africa. [Sahu, K. C.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Han, C.] Chonnam Natl Univ, Inst Basic Sci Res, Dept Phys, Chonju 361763, South Korea. [Lee, C. -U.; Park, B. -G.; Hinse, T. C.] Korea Astron & Space Sci Inst, Taejon 305348, South Korea. [Monard, L. A. G.] Bronberg Observ, Pretoria, South Africa. [Udalski, A.; Kozlowski, S.] Univ Warsaw Observ, Warsaw, Poland. Univ Concepcion, Dept Fis, Astron Grp, Concepcion, Chile. [Tristram, P. J.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Bond, I. A.; Ling, C. H.; Sweatman, W. L.] Massey Univ, Inst Informat & Math Sci, N Shore Mail Ctr, Auckland, New Zealand. [Abe, F.; Furusawa, K.; Itow, Y.; Masuda, K.; Matsubara, Y.; Miyake, N.; Sumi, T.; Suzuki, D.; Wada, K.] Osaka Univ, Dept Earth & Space Sci, Osaka 5600043, Japan. [Kerins, E.] Univ Manchester, Jodrell Bank, Ctr Astrophys, Manchester M13 9PL, Lancs, England. [Muraki, Y.] Konan Univ, Dept Phys, Kobe, Hyogo 6588501, Japan. [Ohnishi, K.] Nagano Natl Coll Technol, Nagano 3818550, Japan. [Botzler, C. S.; Rattenbury, N. J.] Univ Auckland, Dept Phys, Auckland 1142, New Zealand. [Saito, To.] Tokyo Metropolitan Coll Ind Technol, Tokyo 1160003, Japan. Nagoya Univ, Fac Sci, Dept Phys & Astrophys, Nagoya, Aichi 4648602, Japan. [Korpela, A. V.; Sullivan, D.] Mt John Observ, Lake Tekapo, New Zealand. [Tsapras, Y.; Street, R. A.; Hawkins, E.; Lister, T. A.; Saunders, E. S.] Las Cumbres Observ, Goleta, CA 93117 USA. [Bode, M. F.; Clay, N.; Fraser, S. N.; Mottram, C. J.; Steele, I. A.] Liverpool John Moores Univ, Astrophys Res Inst, Birkenhead CH41 1LD, Merseyside, England. [Allan, A.; Saunders, E. S.] Univ Exeter, Sch Phys, Exeter EX4 4QL, Devon, England. [Wheatley, P. J.] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. [Street, R. A.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Bachelet, E.; Fouque, P.] Univ Toulouse, IRAP, CNRS, F-31400 Toulouse, France. [Jorgensen, U. G.; Mathiasen, M.; Harpsoe, K.; Hinse, T. C.; Skottfelt, J.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark. [Jorgensen, U. G.; Mathiasen, M.; Harpsoe, K.; Hinse, T. C.; Skottfelt, J.] Univ Copenhagen, Ctr Star & Planet Format, DK-2100 Copenhagen, Denmark. Univ Observ Munich, D-81679 Munich, Germany. [Mancini, L.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Heyrovsky, D.] Charles Univ Prague, Inst Theoret Phys, CR-18000 Prague, Czech Republic. Bellatrix Observ, I-03023 Ceccano, Italy. [Bozza, V.; Novati, S. Calchi; Scarpetta, G.] IIASS, Sez Napoli, INFN, Vietri Sur Mare, Italy. [Botzler, C. S.; Bozza, V.; Novati, S. Calchi; Scarpetta, G.] Univ Salerno, Dipartimento Fis, Fisciano, Italy. [Hinse, T. C.] Armagh Observ, Armagh BT61 9DG, North Ireland. [Rahvar, S.] Sharif Univ Technol, Dept Phys, Tehran, Iran. [Dreizler, S.; Hessman, F. V.; Hundertmark, M.] Univ Gottingen, Inst Astrophys, D-37077 Gottingen, Germany. [Finet, F.; Ricci, D.; Surdej, J.] Inst Astrophys & Geophys, B-4000 Liege, Belgium. [Southworth, J.] Univ Keele, Astrophys Grp, Newcastle Under Lyme ST5 5BG, England. Osserv Astron Brera, INAF, I-23846 Merate, LC, Italy. [Burgdorf, M. J.] Univ Stuttgart, Deutsch SOFIA Inst, D-70569 Stuttgart, Germany. [Burgdorf, M. J.] NASA, SOFIA Sci Ctr, Ames Res Ctr, Moffett Field, CA 94035 USA. Kyoto Univ, Dept Astron, Kyoto 6068502, Japan. [Tsapras, Y.] Queen Mary Univ London, Sch Math Sci, London E1 4NS, England. [Drummond, J.] Possum Observ, Patutahi, Gisbourne, New Zealand. [Maoz, D.; Kaspi, S.; Polishook, D.; Shporer, A.] Tel Aviv Univ, Sch Phys & Astron, IL-69978 Tel Aviv, Israel. [Maoz, D.; Kaspi, S.; Polishook, D.; Shporer, A.] Tel Aviv Univ, Wise Observ, IL-69978 Tel Aviv, Israel. [Christie, G. W.; Natusch, T.] Auckland Observ, Auckland, New Zealand. [McCormick, J.] Ctr Backyard Astrophys, Farm Cove Observ, Auckland, New Zealand. [Matsunaga, N.] Univ Tokyo, Inst Astron, Kiso Observ, Nagano 3970101, Japan. [Oi, N.] Grad Univ Adv Studies Sokendai, Mitaka, Tokyo 1818588, Japan. [Renon, N.] Univ Toulouse, DTSI Univ Paul Sabatier, CALMIP, F-31062 Toulouse, France. [Rahvar, S.] Perimeter Inst Theoret Phys, Waterloo, ON N2L 2Y5, Canada. [Mancini, L.] Int Inst Adv Sci Studies, I-84019 Vietri Sul Mare, SA, Italy. [Mancini, L.] Univ Salerno, Dept Phys, I-84084 Fisciano, SA, Italy. [Glitrup, M.; Grundahl, F.] Aarhus Univ, Dept Phys & Astron, DK-8000 Aarhus C, Denmark. [Bos, M.] Molehill Astron Observ, Auckland, New Zealand. [Munoz, J. A.] Univ Valencia, Dept Astron & Astrofis, E-46100 Valencia, Spain. Texas A&M Univ, Dept Phys, College Stn, TX 77843 USA. [Dong, Subo] Inst Adv Study, Princeton, NJ 08540 USA. [Natusch, T.] AUT Univ, Auckland, New Zealand. [Fukui, A.] Natl Inst Nat Sci, Natl Astron Observ Japan, Okayama Astrophys Observ, Kamogatacho, Okayama 7190232, Japan. EM gwchristie@christie.org.nz; farmcoveobs@xtra.co.nz; john_drummond@xtra.co.nz; shai@wise.tau.ac.il; shporer@wise.tau.ac.il RI Kane, Stephen/B-4798-2013; Greenhill, John/C-8367-2013; Kozlowski, Szymon/G-4799-2013; Williams, Andrew/K-2931-2013; Zimmer, Fabian/M-4765-2014; Heyrovsky, David/A-2031-2015; Hundertmark, Markus/C-6190-2015; Rahvar, Sohrab/A-9350-2008; OI Ricci, Davide/0000-0002-9790-0552; Snodgrass, Colin/0000-0001-9328-2905; Wheatley, Peter/0000-0003-1452-2240; Kozlowski, Szymon/0000-0003-4084-880X; Williams, Andrew/0000-0001-9080-0105; Heyrovsky, David/0000-0002-5198-5343; Hundertmark, Markus/0000-0003-0961-5231; Rahvar, Sohrab/0000-0002-7084-5725; Dominik, Martin/0000-0002-3202-0343; Cole, Andrew/0000-0003-0303-3855 FU French Agence Nationale de la Recherche; Czech Science Foundation [GACR 205/07/0824]; Czech Ministry of Education [MSM0021620860]; National Research Foundation of Korea [2009-0081561]; Department for Culture, Arts and Leisure, Northern Ireland, UK; Korea Research Council for Fundamental Science and Technology (KRCF); Communaute francaise de Belgique - Actions de recherche concertees - Academie universitaire Wallonie-Europe; European Community [229517]; NSF [AST-1103471, 2009068160]; NASA [NNG04GL51G]; Qatar Foundation through QNRF [NPRP-09-476-1-78]; Korea Astronomy and Space Science Institute (KASI) [2012-1-410-02]; [JSPS18253002]; [JSPS20340052]; [JSPS20740104] FX We are very grateful to the observatories that support our science (Bronberg, Canopus, CTIO, ESO, IRSF, LCOGT, Liverpool, LOAO, MOA, OGLE, Perth, SAAO, Skinakas) via the generous allocation of time that makes this work possible. The operation of Canopus Observatory is in part supported by a financial contribution from David Warren. Allocation of the Holmes grant from the French Agence Nationale de la Recherche has been indispensable to finance observing trips and travel costs for meetings, and is gratefully acknowledged here. D. H. was supported by Czech Science Foundation grant GACR 205/07/0824 and by the Czech Ministry of Education project MSM0021620860. C. H. was supported by the grant 2009-0081561 of National Research Foundation of Korea. T. C. H. was financed for his astronomical research at the Armagh Observatory by the Department for Culture, Arts and Leisure, Northern Ireland, UK and is now supported by the Korea Research Council for Fundamental Science and Technology (KRCF) via the Young Scientist Research Fellowship Program. MOA project was funded by JSPS18253002 and JSPS20340052. T. S. was funded by JSPS20740104. D. R. and J.S. acknowledge support from the Communaute francaise de Belgique - Actions de recherche concertees - Academie universitaire Wallonie-Europe. P. F. wishes to thank Noriyuki Matsunaga for discussions about the interplay between adopted distance and derived extinction. The research leading to these results has received funding from the European Community's Seventh Framework Programme (/FP7/2007-2013/) under grant agreement No 229517. A. Gould acknowledges support from NSF AST-1103471. B. S. Gaudi, A. Gould, and R. W. Pogge acknowledge support from NASA grant NNG04GL51G. Work by J. C. Yee is supported by a National Science Foundation Graduate Research Fellowship under Grant No. 2009068160. Work by S. Dong was performed under contract with the California Institute of Technology (Caltech) funded by NASA through the Sagan Fellowship Program. The RoboNet team is supported by the Qatar Foundation through QNRF grant NPRP-09-476-1-78. CUL acknowledges support by Korea Astronomy and Space Science Institute (KASI) grant 2012-1-410-02. This publication makes use of data products from the 2MASS project, as well as the SIMBAD database, Aladin and Vizier catalogue operation tools (CDS Strasbourg, France). The Two Micron All Sky Survey is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. This work was granted access to the HPC resources of CALMIP under the allocation 2012-[1131]. NR 57 TC 10 Z9 10 U1 1 U2 14 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 NOV PY 2012 VL 547 AR A55 DI 10.1051/0004-6361/201219765 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 036MZ UT WOS:000311031700055 ER PT J AU Furst, F Pottschmidt, K Kreykenbohm, I Muller, S Kuhnel, M Wilms, J Rothschild, RE AF Fuerst, F. Pottschmidt, K. Kreykenbohm, I. Mueller, S. Kuehnel, M. Wilms, J. Rothschild, R. E. TI Staring at 4U 1909+07 with Suzaku SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE accretion, accretion disks; X-rays: binaries; stars: neutron ID X-RAY PULSARS; SPECTROSCOPY; X1908+075; ACCRETION; EMISSION; BINARY; PERIOD; LINES AB We present an analysis of the neutron star high mass X-ray binary (HMXB) 4U 1909+07 mainly based on Suzaku data. We extend the pulse period evolution, which behaves in a random-walk like manner, indicative of direct wind accretion. Studying the spectral properties of 4U 1909+07 between 0.5 to 90 keV we find that a power-law with an exponential cutoff can describe the data well, when additionally allowing for a blackbody or a partially covering absorber at low energies. We find no evidence for a cyclotron resonant scattering feature (CRSF), a feature seen in many other neutron star HMXBs sources. By performing pulse phase resolved spectroscopy we investigate the origin of the strong energy dependence of the pulse profile, which evolves from a broad two-peak profile at low energies to a profile with a single, narrow peak at energies above 20 keV. Our data show that it is very likely that a higher folding energy in the high energy peak is responsible for this behavior. This in turn leads to the assumption that we observe the two magnetic poles and their respective accretion columns at different phases, and that these accretion columns have slightly different physical conditions. C1 [Fuerst, F.; Kreykenbohm, I.; Mueller, S.; Kuehnel, M.; Wilms, J.] Univ Erlangen Nurnberg, Dr Karl Remeis Sternwarte, D-96049 Bamberg, Germany. [Fuerst, F.] CALTECH, Space Radiat Lab, Pasadena, CA 91125 USA. [Pottschmidt, K.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Pottschmidt, K.] CRESST, Greenbelt, MD 20771 USA. [Pottschmidt, K.] Univ Maryland Baltimore Cty, Ctr Space Sci & Technol, Baltimore, MD 21250 USA. [Rothschild, R. E.] Univ Calif San Diego, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA. [Fuerst, F.; Kreykenbohm, I.; Mueller, S.; Kuehnel, M.; Wilms, J.] Univ Erlangen Nurnberg, ECAP, D-96049 Bamberg, Germany. RP Furst, F (reprint author), Univ Erlangen Nurnberg, Dr Karl Remeis Sternwarte, Sternwartstr 7, D-96049 Bamberg, Germany. EM felix.fuerst@sternwarte.uni-erlangen.de RI Wilms, Joern/C-8116-2013; Kreykenbohm, Ingo/H-9659-2013; XRAY, SUZAKU/A-1808-2009 OI Wilms, Joern/0000-0003-2065-5410; Kreykenbohm, Ingo/0000-0001-7335-1803; FU Bundesministerium fur Wirtschaft und Technologie through DLR [50 OR 0808, 50 OR 0905, 50 OR 1113]; ESA member states FX This work was supported by the Bundesministerium fur Wirtschaft und Technologie through DLR grants 50 OR 0808, 50 OR 0905, and 50 OR 1113. F. F. thanks GSFC for the hospitality. 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). This work is furthermore based on observations with INTEGRAL, an ESA project with instruments and science data centre funded by ESA member states (especially the PI countries: Denmark, France, Germany, Italy, Switzerland, Spain), Czech Republic and Poland, and with the participation of Russia and the USA. We have made use of NASA's Astrophysics Data System. We like to thank J. E. Davis for the slxfig module which was used to create all plots throughout this paper. NR 26 TC 1 Z9 1 U1 0 U2 3 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD NOV PY 2012 VL 547 AR A2 DI 10.1051/0004-6361/201219845 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 036MZ UT WOS:000311031700002 ER PT J AU Lebzelter, T Heiter, U Abia, C Eriksson, K Ireland, M Neilson, H Nowotny, W Maldonado, J Merle, T Peterson, R Plez, B Short, CI Wahlgren, GM Worley, C Aringer, B Bladh, S de Laverny, P Goswami, A Mora, A Norris, RP Recio-Blanco, A Scholz, M Thevenin, F Tsuji, T Kordopatis, G Montesinos, B Wing, RF AF Lebzelter, T. Heiter, U. Abia, C. Eriksson, K. Ireland, M. Neilson, H. Nowotny, W. Maldonado, J. Merle, T. Peterson, R. Plez, B. Short, C. I. Wahlgren, G. M. Worley, C. Aringer, B. Bladh, S. de Laverny, P. Goswami, A. Mora, A. Norris, R. P. Recio-Blanco, A. Scholz, M. Thevenin, F. Tsuji, T. Kordopatis, G. Montesinos, B. Wing, R. F. TI Comparative modelling of the spectra of cool giants SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: atmospheres; stars: late-type; stars: abundances; stars: fundamental parameters ID HIGH-RESOLUTION SPECTROSCOPY; EFFECTIVE TEMPERATURE SCALE; SOLAR CHEMICAL-COMPOSITION; NEUTRAL HYDROGEN-ATOMS; METAL-POOR STARS; LINE-DATA-BASE; OPTICAL INTERFEROMETRY; ANGULAR DIAMETERS; INFRARED-SPECTRA; RICH GIANTS AB Context. Our ability to extract information from the spectra of stars depends on reliable models of stellar atmospheres and appropriate techniques for spectral synthesis. Various model codes and strategies for the analysis of stellar spectra are available today. Aims. We aim to compare the results of deriving stellar parameters using different atmosphere models and different analysis strategies. The focus is set on high-resolution spectroscopy of cool giant stars. Methods. Spectra representing four cool giant stars were made available to various groups and individuals working in the area of spectral synthesis, asking them to derive stellar parameters from the data provided. The results were discussed at a workshop in Vienna in 2010. Most of the major codes currently used in the astronomical community for analyses of stellar spectra were included in this experiment. Results. We present the results from the different groups, as well as an additional experiment comparing the synthetic spectra produced by various codes for a given set of stellar parameters. Similarities and differences of the results are discussed. Conclusions. Several valid approaches to analyze a given spectrum of a star result in quite a wide range of solutions. The main causes for the differences in parameters derived by different groups seem to lie in the physical input data and in the details of the analysis method. This clearly shows how far from a definitive abundance analysis we still are. C1 [Lebzelter, T.; Nowotny, W.] Univ Vienna, A-1180 Vienna, Austria. [Heiter, U.; Eriksson, K.; Bladh, S.] Uppsala Univ, Dept Phys & Astron, S-75120 Uppsala, Sweden. [Abia, C.] Univ Granada, Depto Fis Teor & Cosmos, E-18071 Granada, Spain. [Ireland, M.] Macquarie Univ, Dept Phys & Astron, N Ryde, NSW 2109, Australia. [Neilson, H.] Univ Bonn, Argelander Inst Astron, D-53121 Bonn, Germany. [Maldonado, J.] Univ Autonoma Madrid, Dpto Fis Teor, Fac Ciencias, E-28049 Madrid, Spain. [Merle, T.; Worley, C.; de Laverny, P.; Recio-Blanco, A.; Thevenin, F.; Kordopatis, G.] Univ Nice Sophia Antipolis, CNRS, UMR 6202, Observ Cote Azur, F-06304 Nice 04, France. [Peterson, R.] Astrophys Adv UCOLick, Palo Alto, CA 94301 USA. [Plez, B.] Univ Montpellier 2, CNRS, Lab Universe & Particules Montpellier, F-34095 Montpellier, France. [Short, C. I.] St Marys Univ, Dept Phys & Astron, Halifax, NS B3H 3C3, Canada. [Wahlgren, G. M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Aringer, B.] INAF OAPD, I-35122 Padua, Italy. [Goswami, A.] Indian Inst Astrophys, Bangalore 560034, Karnataka, India. [Mora, A.] ESA ESAC Gaia SOC, Madrid 28691, Spain. [Norris, R. P.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA. [Scholz, M.] Heidelberg Univ, Zentrum Astron, Inst Theoret Astrophys, D-69120 Heidelberg, Germany. [Tsuji, T.] Univ Tokyo, Inst Astron, Mitaka, Tokyo 1810015, Japan. [Montesinos, B.] ESAC, Ctr Astrobiol INTA CSIC, Madrid 28691, Spain. [Wing, R. F.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Ireland, M.] Australian Astron Observ, Epping, NSW 1710, Australia. [Scholz, M.] Univ Sydney, Sch Phys, SIfA, Sydney, NSW 2006, Australia. RP Lebzelter, T (reprint author), Univ Vienna, Turkenschanzstr 17, A-1180 Vienna, Austria. EM lebzelter@univie.ac.at RI Plez, Bertrand/G-6697-2011; Montesinos, Benjamin/C-3493-2017 OI Plez, Bertrand/0000-0002-0398-4434; Montesinos, Benjamin/0000-0002-7982-2095 FU ESF within the GREAT network initiative; ESF through the GREAT initiative; Robert F. Wing Support Fund at Ohio State University; Department of Astronomy at the University of Vienna; Austrian Science Fund FWF [P20046, P21988, P23737, P23006]; Swedish National Space Board; Spanish grant [AYA2008-08013-C03-03]; Alexander von Humboldt foundation; Swedish Research Council; CNES; OCA; ESO; CNRS FX Kindly funded by the ESF within the GREAT network initiative.; The workshop on which this paper is based was kindly supported by the ESF through the GREAT initiative, by the Robert F. Wing Support Fund at Ohio State University, and the Department of Astronomy at the University of Vienna. The work of T. L. was funded by the Austrian Science Fund FWF projects P20046, P21988, and P23737. U. H. acknowledges support from the Swedish National Space Board. C. A. acknowledges partial support by the Spanish grant AYA2008-08013-C03-03. H.N. acknowledges financial support from the Alexander von Humboldt foundation. K. E. gratefully acknowledges support from The Swedish Research Council. C. W. acknowledges the financial support of CNES, OCA and ESO. G. K. acknowledges the financial support of CNES and CNRS. U. H., K. E., T. M., and F. T. acknowledge the role of the SAM collaboration (http://www.anst.uu.se/ulhei450/GaiaSAM/) in stimulating this research through regular workshops. B. A. thanks for support by the Austrian Science Fund FWF under project number P23006. We thank all participants in the workshop for contributing to the fruitful discussions there. We thank B. Edvardsson and B. Gustafsson for comments on a draft version of the paper. Based on data obtained within the Gaia DPAC (Data Processing and Analysis Consortium) and coordinated by the GBOG (Ground-Based Observations for Gaia) working group. NR 142 TC 17 Z9 17 U1 2 U2 3 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD NOV PY 2012 VL 547 AR A108 DI 10.1051/0004-6361/201219142 PG 30 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 036MZ UT WOS:000311031700108 ER PT J AU Melandri, A Pian, E Ferrero, P D'Elia, V Walker, ES Ghirlanda, G Covino, S Amati, L D'Avanzo, P Mazzali, PA Della Valle, M Guidorzi, C Antonelli, LA Bernardini, MG Bersier, D Bufano, F Campana, S Castro-Tirado, AJ Chincarini, G Deng, J Filippenko, AV Fugazza, D Ghisellini, G Kouveliotou, C Maeda, K Marconi, G Masetti, N Nomoto, K Palazzi, E Patat, F Piranomonte, S Salvaterra, R Saviane, I Starling, RLC Tagliaferri, G Tanaka, M Vergani, SD AF Melandri, A. Pian, E. Ferrero, P. D'Elia, V. Walker, E. S. Ghirlanda, G. Covino, S. Amati, L. D'Avanzo, P. Mazzali, P. A. Della Valle, M. Guidorzi, C. Antonelli, L. A. Bernardini, M. G. Bersier, D. Bufano, F. Campana, S. Castro-Tirado, A. J. Chincarini, G. Deng, J. Filippenko, A. V. Fugazza, D. Ghisellini, G. Kouveliotou, C. Maeda, K. Marconi, G. Masetti, N. Nomoto, K. Palazzi, E. Patat, F. Piranomonte, S. Salvaterra, R. Saviane, I. Starling, R. L. C. Tagliaferri, G. Tanaka, M. Vergani, S. D. TI The optical SN2012bz associated with the long GRB120422A SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE gamma-ray burst: general; supernovae: individual: SN2012bz ID GAMMA-RAY BURST; 25 APRIL 1998; LIGHT-CURVE; SUPERNOVA CONNECTION; SPECTRAL MODELS; GRB 100316D; AFTERGLOW; GRB-030329; GRB-031203; GRB-980425 AB Aims. The association of Type Ic supernovae (SNe) with long-duration gamma-ray bursts (GRBs) is well established. We endeavor, through accurate ground-based observational campaigns, to characterize these SNe at increasingly high redshifts. Methods. We obtained a series of optical photometric and spectroscopic observations of the Type Ic SN2012bz associated with the Swift long-duration GRB120422A (redshift z = 0.283) using the 3.6-m TNG and the 8.2-m VLT telescopes during the time interval between 4 and 36 days after the burst. Results. The peak times of the light curves of SN2012bz in various optical filters differ, with the B-band and i'-band light curves reaching maximum at 9 +/- 4 and 23 +/- 3 rest-frame days, respectively. The bolometric light curve has been derived from individual bands photometric measurements, but no correction for the unknown contribution in the near-infrared (probably around 10-15%) has been applied. Therefore, the present light curve should be considered as a lower limit to the actual UV-optical-IR bolometric light curve. This pseudo-bolometric curve reaches its maximum (M-bol = -18.56 +/- 0.06) at 13 +/- 1 rest-frame days; it is similar in shape and luminosity to the bolometric light curves of the SNe associated with z < 0.2 GRBs and more luminous than those of SNe associated with X-ray flashes (XRFs). A comparison with the model generated for the bolometric light curve of SN2003dh suggests that SN2012bz produced only about 15% less Ni-56 than SN2003dh, about 0.35 M-circle dot. Similarly the VLT spectra of SN2012bz, after correction for Galactic extinction and for the contribution of the host galaxy, suggest comparable explosion parameters with those observed in SN2003dh (E-K similar to 3.5 x 10(52) erg, M-ej similar to 7 M-circle dot) and a similar progenitor mass (similar to 25-40 M-circle dot). GRB120422A is consistent with the E-peak -E-iso and the E-X,E-iso -E-gamma,E-iso -E-peak relations. GRB120422A / SN2012bz shows the GRB-SN connection at the highest redshift so far accurately monitored both photometrically and spectroscopically. C1 [Melandri, A.; Ghirlanda, G.; Covino, S.; D'Avanzo, P.; Bernardini, M. G.; Campana, S.; Chincarini, G.; Fugazza, D.; Ghisellini, G.; Tagliaferri, G.; Vergani, S. D.] INAF Brera Astron Observ, I-23807 Merate, LC, Italy. [Pian, E.; Walker, E. S.] Scuola Normale Super Pisa, I-56126 Pisa, Italy. [Pian, E.] INAF Trieste Astron Observ, I-34143 Trieste, Italy. [Pian, E.] INFN, Sez Pisa, I-56127 Pisa, Italy. [Ferrero, P.] Inst Astrofis Canarias, Tenerife 38200, Spain. [Ferrero, P.] Univ La Laguna, Dept Astrofis, E-38206 Tenerife, Spain. [D'Elia, V.] ASI, Sci Data Ctr, I-00044 Frascati, Italy. [D'Elia, V.; Antonelli, L. A.; Piranomonte, S.] INAF Roma Astron Observ, I-00040 Monte Porzio Catone, Italy. [Amati, L.; Masetti, N.; Palazzi, E.] IASF Bologna, INAF, I-40129 Bologna, Italy. [Mazzali, P. A.] Max Planck Inst Astrophys, D-85748 Garching, Germany. [Mazzali, P. A.] INAF Padova Astron Observ, I-35122 Padua, Italy. [Della Valle, M.] INAF Capodimonte Astron Observ, I-80131 Naples, Italy. [Della Valle, M.] ICRANET, I-65122 Pescara, Italy. [Guidorzi, C.] Univ Ferrara, Dept Phys, I-44122 Ferrara, Italy. [Bersier, D.] Liverpool John Moores Univ, ARI, Birkenhead CH41 1LD, Merseyside, England. [Bufano, F.] Univ Andres Bello, Dept Ciencias Fis, Santiago, Chile. [Castro-Tirado, A. J.] CSIC, Inst Astrofis Andalucia, E-18008 Granada, Spain. [Deng, J.] Chinese Acad Sci, Natl Astron Observ, Beijing 100012, Peoples R China. [Filippenko, A. V.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Kouveliotou, C.] NASA, Marshall Space Flight Ctr, Huntsville, AL 35805 USA. [Maeda, K.; Nomoto, K.; Saviane, I.] Univ Tokyo, Kavli Inst Phys & Math Universe, Kashiwa, Chiba 2778583, Japan. [Marconi, G.] European So Observ, Santiago 19, Chile. [Patat, F.] European So Observ, D-85748 Garching, Germany. [Salvaterra, R.] IASF Milano, INAF, I-20133 Milan, Italy. [Starling, R. L. C.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Tanaka, M.] Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan. [Vergani, S. D.] Univ Paris Diderot, CNRS, Observ Paris, GEPI, F-92190 Meudon, France. RP Melandri, A (reprint author), INAF Brera Astron Observ, Via E Bianchi 46, I-23807 Merate, LC, Italy. EM andrea.melandri@brera.inaf.it RI Nomoto, Ken'ichi/A-4393-2011; Palazzi, Eliana/N-4746-2015; Amati, Lorenzo/N-5586-2015; OI Ghisellini, Gabriele/0000-0002-0037-1974; Della Valle, Massimo/0000-0003-3142-5020; Patat, Ferdinando/0000-0002-0537-3573; Salvaterra, Ruben/0000-0002-9393-8078; Covino, Stefano/0000-0001-9078-5507; Masetti, Nicola/0000-0001-9487-7740; Tagliaferri, Gianpiero/0000-0003-0121-0723; Pian, Elena/0000-0001-8646-4858; Ghirlanda, Giancarlo/0000-0001-5876-9259; Castro-Tirado, A. J./0000-0003-2999-3563; Amati, Lorenzo/0000-0001-5355-7388; Palazzi, Eliana/0000-0002-8691-7666; Campana, Sergio/0000-0001-6278-1576; D'Elia, Valerio/0000-0002-7320-5862 FU VLT observation planning; PRIN INAF; PRIN-MIUR [2009ERC3HT]; ASI INAF [I/088/06/0, I/011/07/0]; FONDECYT [3120227]; Royal Society; US NSF [AST-0908886, AST-1211916]; TABASGO Foundation; Christopher R. Redlich Fund FX We thank the anonymous referee for valuable comments and suggestions that improved the paper. We thank the TNG staff, in particular W. Boschin, M. Cecconi, L. di Fabrizio, F. Ghinassi, A. Harutyunyan, and M. Pedani, for their valuable support with TNG observations, and the Paranal Science Operations Team, in particular H. Boffin, S. Brillant, D. Gadotti, D. Jones, M. Rodrigues, L. Schmidtobreick, and J. Smoker. We are grateful to D. Malesani, J. Fynbo, N. Tanvir, and K. Wiersema for their support with VLT observation planning. We acknowledge support from PRIN INAF 2009 and 2011, PRIN-MIUR grant 2009ERC3HT and from grants ASI INAF I/088/06/0 and I/011/07/0. E. Pian is grateful for hospitality at the ESO Headquarters in Santiago, where part of this work was developed. F.B. acknowledges support from FONDECYT through Postdoctoral grant 3120227. J.D. is supported by the 973 Program of China (Grant No. 2009CB824800). R.L.C.S. is supported by a Royal Society Fellowship. A. V. F. is grateful for the support of US NSF grants AST-0908886 and AST-1211916, the TABASGO Foundation, and the Christopher R. Redlich Fund. NR 92 TC 26 Z9 26 U1 0 U2 7 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD NOV PY 2012 VL 547 AR A82 DI 10.1051/0004-6361/201219879 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 036MZ UT WOS:000311031700082 ER PT J AU Valcarce, AAR Catelan, M Sweigart, AV AF Valcarce, A. A. R. Catelan, M. Sweigart, A. V. TI Effects of helium enrichment in globular clusters I. Theoretical plane with PGPUC stellar evolution code SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: evolution; stars: general; stars: horizontal-branch; globular clusters: general ID HORIZONTAL-BRANCH STARS; RED GIANT BRANCH; POPULATION-II STARS; METAL-POOR STARS; THERMONUCLEAR REACTION-RATES; COLOR-MAGNITUDE DIAGRAM; DOUBLE SUBGIANT BRANCH; 2ND PARAMETER PROBLEM; MAIN-SEQUENCE STARS; RELATIVE AGES AB Aims. Recently, the study of globular cluster (GC) color-magnitude diagrams (CMDs) has shown that some of them harbor multiple populations with different chemical compositions and/or ages. In the first case, the most common candidate is a spread in the initial helium abundance, but this quantity is difficult to determine spectroscopically due to the fact that helium absorption lines are not present in cooler stars, whereas for hotter GC stars gravitational settling of helium becomes important. As a consequence, indirect methods to determine the initial helium abundance among populations are necessary. For that reason, in this series of papers, we investigate the effects of a helium enrichment in populations covering the range of GC metallicities. Methods. In this first paper, we present the theoretical evolutionary tracks, isochrones, and zero-age horizontal branch (ZAHB) loci calculated with the Princeton-Goddard-PUC (PGPUC) stellar evolutionary code, which has been updated with the most recent input physics and compared with other theoretical databases. The chemical composition grid covers 9 metallicities ranging from Z = 1.60 x 10(-4) to 1.57 x 10(-2) (-2.25 less than or similar to [Fe/H] less than or similar to -0.25), 7 helium abundances from Y = 0.230 to 0.370, and an alpha-element enhancement of [alpha/Fe] = 0.3. Results. The effects of different helium abundances that can be observed in isochrones are: splits in the main sequence (MS), differences in the luminosity (L) and effective temperature (T-eff) of the turn off point, splits in the sub giant branch being more prominent for lower ages or higher metallicities, splits in the lower red giant branch (RGB) being more prominent for higher ages or higher metallicities, differences in L of the RGB bump (with small changes in T-eff), and differences in L at the RGB tip. At the ZAHB, when Y is increased there is an increase of L for low T-eff, which is affected in different degrees depending on the age of the GC being studied. Finally, the ZAHB morphology distribution depending on the age explains how for higher GC metallicities a population with higher helium abundance could be hidden at the red ZAHB locus. C1 [Valcarce, A. A. R.; Catelan, M.] Pontificia Univ Catolica Chile, Fac Fis, Dept Astron & Astrofis, Santiago 7820436, Chile. [Valcarce, A. A. R.] Univ Fed Rio Grande do Norte, Dept Fis, BR-59072970 Natal, RN, Brazil. [Valcarce, A. A. R.; Catelan, M.] Milky Way Millennium Nucleus, Santiago 7820436, Chile. [Valcarce, A. A. R.; Catelan, M.] Pontificia Univ Catolica Chile, Ctr Astroingn, Santiago 7820436, Chile. [Sweigart, A. V.] NASA, Goddard Space Flight Ctr, Explorat Universe Div, Greenbelt, MD 20771 USA. RP Valcarce, AAR (reprint author), Pontificia Univ Catolica Chile, Fac Fis, Dept Astron & Astrofis, Av Vicuna Mackena 4860, Santiago 7820436, Chile. EM avalcarc@astro.puc.cl; mcatelan@astro.puc.cl; allen.v.sweigart@nasa.gov FU Ministry for the Economy, Development, and Tourism's Programa Iniciativa Cientifica Milenio [P07-021-F]; Proyecto Basal [PFB-06/2007]; FONDAP Centro de Astrofisica [15010003]; Proyecto FONDECYT Regular [1110326]; Proyecto Anillo de Investigacion en Ciencia y Tecnologia PIA CONICYT-ACT [86]; CNPq; CAPES; Proyecto ALMA-Conicyt [31090002]; MECESUP2; SOCHIAS FX We thank the anonymous referee for her/his comments, which have helped improve the presentation of our results. A. A. R. V. thanks Santi Casissi for his useful comments during A.A.R.V.'s Ph.D. Thesis on this topic. Support for A. A. R. V. and M. C. is provided by the Ministry for the Economy, Development, and Tourism's Programa Iniciativa Cientifica Milenio through grant P07-021-F, awarded to The Milky Way Millennium Nucleus; by Proyecto Basal PFB-06/2007; by FONDAP Centro de Astrofisica 15010003; by Proyecto FONDECYT Regular #1110326; and by Proyecto Anillo de Investigacion en Ciencia y Tecnologia PIA CONICYT-ACT 86. A. A. R. V. acknowledges additional support from CNPq, CAPES, from Proyecto ALMA-Conicyt 31090002, MECESUP2, and SOCHIAS. NR 168 TC 26 Z9 26 U1 1 U2 3 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD NOV PY 2012 VL 547 AR A5 DI 10.1051/0004-6361/201219510 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 036MZ UT WOS:000311031700005 ER PT J AU Lohn, AJ Cormia, RD Fryauf, DM Zhang, JC Norris, KJ Kobayashi, NP AF Lohn, Andrew J. Cormia, Robert D. Fryauf, David M. Zhang, Junce Norris, Kate J. Kobayashi, Nobuhiko P. TI Morphological Effect of Doping Environment on Silicon Nanowires Grown by Plasma-Assisted Chemical Vapor Deposition SO JAPANESE JOURNAL OF APPLIED PHYSICS LA English DT Article ID SURFACE; PERFORMANCE; OXIDATION; MODEL; BORON; GOLD AB Physical properties of semiconductor nanowires are tied intimately to their specific morphologies such as length and diameter. We studied the growth of silicon nanowires and found their lengths and diameters to vary over orders of magnitude in different doping environments. In all cases we examined, doping resulted in increased diameters. In addition, boron doping was found to accelerate volume growth rate while arsenic and antimony both appeared to slow it down. We further studied the formation of the native oxides that cover the nanowires. X-ray photoelectron spectroscopy indicated that properties of the native oxides are also dependent on doping environment and correlated to doping-dependent shifts in apparent binding energy of the Si 2p(3/2) peak illustrating that the electronic contribution is the dominant mechanism for the oxide growth. (C) 2012 The Japan Society of Applied Physics C1 [Lohn, Andrew J.; Fryauf, David M.; Zhang, Junce; Norris, Kate J.; Kobayashi, Nobuhiko P.] Univ Calif Santa Cruz, Baskin Sch Engn, Santa Cruz, CA 95064 USA. [Lohn, Andrew J.; Fryauf, David M.; Zhang, Junce; Norris, Kate J.; Kobayashi, Nobuhiko P.] Univ Calif Santa Cruz, Nanostruct Energy Convers Technol & Res NECTAR, Adv Studies Labs, NASA Ames Res Ctr, Moffett Field, CA 94035 USA. [Cormia, Robert D.] Foothill Coll, Los Altos Hills, CA 94022 USA. RP Lohn, AJ (reprint author), Univ Calif Santa Cruz, Baskin Sch Engn, Santa Cruz, CA 95064 USA. RI Kobayashi, Nobuhiko/E-3834-2012 FU NASA [SBIR NNX11CE14P]; NSF [0903316, DGE-0809125-006] FX The authors would like to thank Elane Coleman and Gary S. Tompa at Structured Materials Industries, Inc for nanowire growth and Vince Crist at NanoLab Technologies and XPS International LLC for XPS measurements. The authors would also like to acknowledge the following funding sources: NASA SBIR NNX11CE14P, NSF grant number 0903316, and NSF grant number DGE-0809125-006. NR 32 TC 1 Z9 1 U1 0 U2 11 PU JAPAN SOC APPLIED PHYSICS PI TOKYO PA KUDAN-KITA BUILDING 5TH FLOOR, 1-12-3 KUDAN-KITA, CHIYODA-KU, TOKYO, 102-0073, JAPAN SN 0021-4922 J9 JPN J APPL PHYS JI Jpn. J. Appl. Phys. PD NOV PY 2012 VL 51 IS 11 SI SI AR 11PE04 DI 10.1143/JJAP.51.11PE04 PN 2 PG 6 WC Physics, Applied SC Physics GA 049RP UT WOS:000312001400019 ER PT J AU Meador, MAB Wright, S Sandberg, A Nguyen, BN Van Keuls, FW Mueller, CH Rodriguez-Solis, R Miranda, FA AF Meador, Mary Ann B. Wright, Sarah Sandberg, Anna Nguyen, Baochau N. Van Keuls, Frederick W. Mueller, Carl H. Rodriguez-Solis, Rafael Miranda, Felix A. TI Low Dielectric Polyimide Aerogels As Substrates for Lightweight Patch Antennas SO ACS APPLIED MATERIALS & INTERFACES LA English DT Article DE aerogels; polyimides; low dielectric; antennas; mesoporous ID POROUS POLYIMIDE; FILMS AB The dielectric properties and loss tangents of low-density polyimide aerogels have been characterized at various frequencies. Relative dielectric constants as low as 1.16 were measured for polyimide aerogels made from 2,2'-dimethylbenzidine (DMBZ) and biphenyl 3,3',4,4'-tetracarbozylic dianhydride (BPDA) cross-linked with 1,3,5-triamino-phenoxybenzene (TAB). This formulation was used as the substrate to fabricate and test prototype microstrip patch antennas and benchmark against state of practice commercial antenna substrates. The polyimide aerogel antennas exhibited broader bandwidth, higher gain, and lower mass than the antennas made using commercial substrates. These are very encouraging results, which support the potential advantages of the polyimide aerogel-based antennas for aerospace applications. C1 [Meador, Mary Ann B.; Wright, Sarah; Sandberg, Anna; Miranda, Felix A.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. [Nguyen, Baochau N.] Ohio Aerosp Inst, Cleveland, OH 44135 USA. [Van Keuls, Frederick W.] Vantage Partners LLC, Brookpark, OH 44142 USA. [Mueller, Carl H.] Qinetiq N Amer, Brookpark, OH 44142 USA. [Rodriguez-Solis, Rafael] Univ Puerto Rico, Mayaguez, PR USA. RP Meador, MAB (reprint author), NASA, Glenn Res Ctr, 21000 Brookpk Rd, Cleveland, OH 44135 USA. EM maryann.meador@nasa.gov OI Meador, Mary Ann/0000-0003-2513-7372; Rodriguez Solis, Rafael/0000-0001-5700-2021 FU NASA FX We thank the NASA Aeronautics Mission Directorate Seedling Fund for support of this work. We thank our NASA GRC colleagues Mr. Nicholas Varaljay and Ms. Elizabeth McQuaid for their support in the fabrication of the antennas, as well as Dr. Kevin Lambert for his support in antenna metrology. NR 19 TC 34 Z9 39 U1 18 U2 119 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 1944-8244 J9 ACS APPL MATER INTER JI ACS Appl. Mater. Interfaces PD NOV PY 2012 VL 4 IS 11 BP 6346 EP 6353 DI 10.1021/am301985s PG 8 WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary SC Science & Technology - Other Topics; Materials Science GA 043DA UT WOS:000311521900084 PM 23134844 ER PT J AU Ponchak, GE AF Ponchak, George E. TI Special Issue on Biomedical Applications of RF/Microwave Technologies SO IEEE TRANSACTIONS ON MICROWAVE THEORY AND TECHNIQUES LA English DT Editorial Material C1 NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Ponchak, GE (reprint author), NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. NR 0 TC 0 Z9 0 U1 0 U2 2 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0018-9480 J9 IEEE T MICROW THEORY JI IEEE Trans. Microw. Theory Tech. PD NOV PY 2012 VL 60 IS 11 BP 3345 EP 3345 DI 10.1109/TMTT.2012.2216811 PG 1 WC Engineering, Electrical & Electronic SC Engineering GA 035SO UT WOS:000310969100001 ER PT J AU Patterson, CE Khan, WT Ponchak, GE May, GS Papapolymerou, J AF Patterson, Chad E. Khan, Wasif Tanveer Ponchak, George E. May, Gary S. Papapolymerou, John TI A 60-GHz Active Receiving Switched-Beam Antenna Array With Integrated Butler Matrix and GaAs Amplifiers SO IEEE TRANSACTIONS ON MICROWAVE THEORY AND TECHNIQUES LA English DT Article DE Butler matrix; integrated circuit (IC) packaging; iquid crystal polymer (LCP); phased arrays; receiving antennas ID NETWORK; GAIN; BAND; GHZ; G/T AB This paper presents for the first time a 60-GHz receiving switched-beam antenna on organic liquid crystal polymer (LCP) platform. A 4 x 1 quasi-Yagi array is incorporated with a 4 x 4 Butler matrix beamforming network and GaAs low-noise amplifiers on an LCP substrate. The active beam is controlled by GaAs single-pole-double-throw switches to access the four output states of the Butler matrix. The entire 4 x 1 active array is 1.4 cm x 1.75 cm and consumes 1.1 W of dc power. Successful comparisons of the measured and simulated results verify a working phased array with a return loss better than 10 dB across the frequency band of 56.7-63.7 GHz. A comparison of radiation patterns demonstrate beam steering of +/- 40 degrees with a peak active gain of 27.5 dB. The combined antenna and receiver noise performance at 60 GHz exhibits an estimated merit G/T of -18.6 dB/K and noise figure of 5.4 dB. C1 [Patterson, Chad E.; Khan, Wasif Tanveer; May, Gary S.; Papapolymerou, John] Georgia Inst Technol, Sch Elect & Comp Engn, Atlanta, GA 30332 USA. [Ponchak, George E.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Patterson, CE (reprint author), Georgia Inst Technol, Sch Elect & Comp Engn, Atlanta, GA 30332 USA. EM cpatterson@gatech.edu; george.ponchak@sbcglobal.net; john.papa-polymerou@ece.gatech.edu NR 23 TC 23 Z9 23 U1 0 U2 9 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0018-9480 J9 IEEE T MICROW THEORY JI IEEE Trans. Microw. Theory Tech. PD NOV PY 2012 VL 60 IS 11 BP 3599 EP 3607 DI 10.1109/TMTT.2012.2213834 PG 9 WC Engineering, Electrical & Electronic SC Engineering GA 035SO UT WOS:000310969100028 ER PT J AU Zaretsky, E AF Zaretsky, Erwin TI Correspondence regarding the role of white etching cracks and related features in the failure processes of bearing steels, with responses from the authors response SO MATERIALS SCIENCE AND TECHNOLOGY LA English DT Letter C1 NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Zaretsky, E (reprint author), NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. EM ezaretsky@sbcglobal.net NR 0 TC 0 Z9 0 U1 1 U2 2 PU MANEY PUBLISHING PI LEEDS PA STE 1C, JOSEPHS WELL, HANOVER WALK, LEEDS LS3 1AB, W YORKS, ENGLAND SN 0267-0836 J9 MATER SCI TECH-LOND JI Mater. Sci. Technol. PD NOV PY 2012 VL 28 IS 11 BP 1360 EP 1364 PG 5 WC Materials Science, Multidisciplinary; Metallurgy & Metallurgical Engineering SC Materials Science; Metallurgy & Metallurgical Engineering GA 044LE UT WOS:000311619900023 ER PT J AU Hashmi, AJ Eftekhar, A Adibi, A Amoozegar, F AF Hashmi, Ali Javed Eftekhar, Ali Adibi, Ali Amoozegar, Farid TI A Kalman filter based synchronization scheme for telescope array receivers in deep-space optical communication links SO OPTICS COMMUNICATIONS LA English DT Article DE Deep-space optical communication; Kalman filter; Telescope array receiver; Clock synchronization ID SYSTEM AB In this paper, the impact of random synchronization errors on the performance of ground-based telescope array receivers for an inter-planetary optical deep-space communication (ODSC) link is investigated. An adaptive method based on Kalman filters is developed for the synchronization and combination of different telescope signals in the array. An end-to-end simulation platform for ODSC link between Earth and planet Mars is implemented that incorporates pulse-position modulation (PPM), direct-detection array receivers, and photon-counting detectors. The effects of atmospheric turbulence and background noise are also modeled. The performance of array receivers is evaluated in terms of probability of symbol error and achievable data rates. The simulation results show that the Kalman filter-based synchronization scheme keeps the synchronization induced power losses to less than 1 dB. The analysis also shows that in the worst-case operational scenario and presence of random synchronization errors, an array consisting of hundred, 1 m telescopes performs almost similar to a single 10 m telescope. Hence, the degradation in the combined signal due to synchronization errors places a minor limitation on the number of telescopes in a telescope array receiver consisting of up to 100 telescope elements. (C) 2012 Elsevier B.V. All rights reserved. C1 [Hashmi, Ali Javed] Natl Univ Sci & Technol, Islamabad, Pakistan. [Eftekhar, Ali; Adibi, Ali] Georgia Inst Technol, Sch Elect & Comp Engn, Atlanta, GA 30332 USA. [Amoozegar, Farid] CALTECH, Jet Prop Lab NASA, Pasadena, CA 91109 USA. RP Hashmi, AJ (reprint author), Natl Univ Sci & Technol, H-12, Islamabad, Pakistan. EM hashmi@gatech.edu NR 20 TC 5 Z9 6 U1 0 U2 8 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0030-4018 J9 OPT COMMUN JI Opt. Commun. PD NOV 1 PY 2012 VL 285 IS 24 BP 5037 EP 5043 DI 10.1016/j.optcom.2012.08.025 PG 7 WC Optics SC Optics GA 038TH UT WOS:000311196500052 ER PT J AU Maneesha, K Murty, VSN Ravichandran, M Lee, T Yu, WD McPhaden, MJ AF Maneesha, K. Murty, V. S. N. Ravichandran, M. Lee, T. Yu, Weidong McPhaden, M. J. TI Upper ocean variability in the Bay of Bengal during the tropical cyclones Nargis and Laila SO PROGRESS IN OCEANOGRAPHY LA English DT Review ID INDIAN-OCEAN; HURRICANE; INTENSITY; MONSOON; EDDY AB Upper ocean variability at different stages in the evolution of the tropical cyclones Nargis and Laila is evaluated over the Bay of Bengal (BoB) during May 2008 and May 2010 respectively. Nargis initially developed on 24 April 2008; intensified twice on 27-28 April and 1 May, and eventually made landfall at Myanmar on 2 May 2008. Laila developed over the western BoB in May 2010 and moved westward towards the east coast of India. Data from the Argo Profiling floats, the Research Moored Array for African-Asian-Australian Monsoon Analysis and prediction (RAMA), and various satellite products are analyzed to evaluate upper ocean variability due to Nargis and Laila. The analysis reveals pre-conditioning of the central BoB prior to Nargis with warm (>30 degrees C) Sea Surface Temperature (SST), low (<33 psu) Sea Surface Salinity (SSS) and shallow (<30 m) mixed layer depths during March-April 2008. Enhanced ocean response to the right of the storm track due to Nargis includes a large SST drop by similar to 1.76 degrees C, SSS increase up to 0.74 psu, mixed layer deepening of 32 m, shoaling of the 26 degrees C isotherm by 36 m and high net heat loss at the sea surface. During Nargis, strong inertial currents (up to 0.9 ms(-1)) were generated to the right of storm track as measured at a RAMA buoy located at 15 degrees N, 90 degrees E, producing strong turbulent mixing that lead to the deepening of mixed layer. This mixing facilitated entrainment of cold waters from as deep as 75 m and, together with net heat loss at sea surface and cyclone-induced subsurface upwelling, contributed to the observed SST cooling in the wake of the storm. A similar upper ocean response occurs during Laila. though it was a significantly weaker storm than Nargis. (C) 2012 Elsevier Ltd. All rights reserved. C1 [Maneesha, K.; Murty, V. S. N.] CSIR, Natl Inst Oceanog, Reg Ctr, Visakhapatnam 530017, Andhra Pradesh, India. [Ravichandran, M.] Indian Natl Ctr Ocean Informat Serv, Hyderabad, Andhra Pradesh, India. [Lee, T.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Yu, Weidong] SOA, Inst Oceanog 1, Lab Ocean Atmosphere Interact & Climate Change, Qingdao, Peoples R China. [McPhaden, M. J.] NOAA, Pacific Marine Environm Lab, Seattle, WA 98115 USA. RP Maneesha, K (reprint author), CSIR, Natl Inst Oceanog, Reg Ctr, 176 Lawsons Bay Colony, Visakhapatnam 530017, Andhra Pradesh, India. EM kkpalli_manisha@yahoo.com RI McPhaden, Michael/D-9799-2016 OI Ravichandran, Muthalagu/0000-0002-4602-0731; FU Council of Scientific & Industrial Research (CSIR); NASA Physical Oceanography Program FX The authors are thankful to the Director, NIO for his encouragement in the collaborative research with INCOIS, Hyderabad, PMEL, USA, JPL, USA and FIO, China through IOGOOS partnership. The lead author is thankful to the Council of Scientific & Industrial Research (CSIR) for funding support with Senior Research Fellowship. These data were collected and made freely available by the International Argo Program and the national programs that contribute to it (http://www.argo.ucsd.edu, http://argo.jcommops.org). The Argo Program is part of the Global Ocean Observing System. ODV software has been used to construct Argo temperature and salinity sections.; This has the NIO contribution No. 5200, INCOIS contribution No. 119 and the PMEL contribution No. 3622. The research is partially supported by NASA Physical Oceanography Program. NR 32 TC 9 Z9 11 U1 2 U2 21 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 NOV PY 2012 VL 106 BP 49 EP 61 DI 10.1016/j.pocean.2012.06.006 PG 13 WC Oceanography SC Oceanography GA 044ZO UT WOS:000311663900004 ER PT J AU Little, MP Azizova, TV Bazyka, D Bouffler, SD Cardis, E Chekin, S Chumak, VV Cucinotta, FA de Vathaire, F Hall, P Harrison, JD Hildebrandt, G Ivanov, V Kashcheev, VV Klymenko, SV Kreuzer, M Laurent, O Ozasa, K Schneider, T Tapio, S Taylor, AM Tzoulaki, I Vandoolaeghe, WL Wakeford, R Zablotska, LB Zhang, W Lipshultz, SE AF Little, Mark P. Azizova, Tamara V. Bazyka, Dimitry Bouffler, Simon D. Cardis, Elisabeth Chekin, Sergey Chumak, Vadim V. Cucinotta, Francis A. de Vathaire, Florent Hall, Per Harrison, John D. Hildebrandt, Guido Ivanov, Victor Kashcheev, Valeriy V. Klymenko, Sergiy V. Kreuzer, Michaela Laurent, Olivier Ozasa, Kotaro Schneider, Thierry Tapio, Soile Taylor, Andrew M. Tzoulaki, Ioanna Vandoolaeghe, Wendy L. Wakeford, Richard Zablotska, Lydia B. Zhang, Wei Lipshultz, Steven E. TI Systematic Review and Meta-analysis of Circulatory Disease from Exposure to Low-Level Ionizing Radiation and Estimates of Potential Population Mortality Risks SO ENVIRONMENTAL HEALTH PERSPECTIVES LA English DT Review DE cancer; circulatory disease; heart disease; radiation; stroke ID ATOMIC-BOMB SURVIVORS; CORONARY-HEART-DISEASE; POWER INDUSTRY WORKERS; NUCLEAR-FUELS PLC; LOW-DOSE EXPOSURE; CARDIOVASCULAR-DISEASE; EPIDEMIOLOGIC EVIDENCE; MAYAK PA; CANCER; COHORT AB BACKGROUND: Although high doses of ionizing radiation have long been linked to circulatory disease, evidence for an association at lower exposures remains controversial. However, recent analyses suggest excess relative risks at occupational exposure levels. OBJECTIVES: We performed a systematic review and meta-analysis to summarize information on circulatory disease risks associated with moderate- and low-level whole-body ionizing radiation exposures. METHODS: We conducted PubMed/ISI Thomson searches of peer-reviewed papers published since 1990 using the terms "radiation" AND "heart" AND "disease," OR "radiation" AND "stroke," OR "radiation" AND "circulatory" AND "disease." Radiation exposures had to be whole-body, with a cumulative mean dose of < 0.5 Sv, or at a low dose rate (< 10 mSv/day). We estimated population risks of circulatory disease from low-level radiation exposure using excess relative risk estimates from this meta-analysis and current mortality rates for nine major developed countries. RESULTS: Estimated excess population risks for all circulatory diseases combined ranged from 2.5%/Sv [95% confidence interval (Cl): 0.8, 4.2] for France to 8.5%/Sv (95% CI: 4.0, 13.0) for Russia. CONCLUSIONS: Our review supports an association between circulatory disease mortality and low and moderate doses of ionizing radiation. Our analysis was limited by heterogeneity among studies (particularly for noncardiac end points), the possibility of uncontrolled confounding in some occupational groups by lifestyle factors, and higher dose groups (> 0.5 Sv) generally driving the observed trends. If confirmed, our findings suggest that overall radiation-related mortality is about twice that currently estimated based on estimates for cancer end points alone (which range from 4.2% to 5.6%/Sv for these populations). C1 [Little, Mark P.] NCI, Radiat Epidemiol Branch, NIH, Dept Hlth & Human Serv, Rockville, MD 20852 USA. [Azizova, Tamara V.] So Urals Biophys Inst, Ozyorsk, Russia. [Bazyka, Dimitry; Chumak, Vadim V.] Res Ctr Radiat Med, Kiev, Ukraine. [Bouffler, Simon D.; Harrison, John D.; Zhang, Wei] Hlth Protect Agcy, Ctr Radiat Chem & Environm Hazards, Chilton, England. [Cardis, Elisabeth] Ctr Res Environm Epidemiol CREAL, Barcelona, Spain. [Chekin, Sergey; Ivanov, Victor; Kashcheev, Valeriy V.] Russian Acad Med Sci, Med Radiol Res Ctr, Obninsk, Russia. [Cucinotta, Francis A.] NASA, Lyndon B Johnson Space Ctr, Space Radiat Program, Houston, TX 77058 USA. [de Vathaire, Florent] Inst Gustave Roussy, INSERM, Radiat Epidemiol Grp, Unite U1018, F-94805 Villejuif, France. [Hall, Per] Karolinska Inst, Dept Med Epidemiol & Biostat, Stockholm, Sweden. [Hildebrandt, Guido] Univ Leipzig, Dept Radiotherapy & Radiat Oncol, Leipzig, Germany. [Hildebrandt, Guido] Univ Rostock, Dept Radiotherapy & Radiat Oncol, Rostock, Germany. [Kreuzer, Michaela] Fed Off Radiat Protect, Dept Radiat Protect & Hlth, Oberschleissheim, Germany. [Laurent, Olivier] Inst Radioprotect & Surete Nucl, Lab Epidemiol, Fontenay Aux Roses, France. [Ozasa, Kotaro] Radiat Effects Res Fdn, Dept Epidemiol, Hiroshima, Japan. [Schneider, Thierry] CEPN Nucl Evaluat Protect Ctr, Fontenay Aux Roses, France. [Tapio, Soile] Helmholtz Zentrum Munchen, German Res Ctr Environm Hlth, Inst Radiat Biol ISB, Oberschleissheim, Germany. [Taylor, Andrew M.] UCL, Inst Cardiovasc Sci, London, England. [Taylor, Andrew M.] Great Ormond St Hosp Sick Children, London WC1N 3JH, England. [Tzoulaki, Ioanna; Vandoolaeghe, Wendy L.] Univ London Imperial Coll Sci Technol & Med, Fac Med, Dept Epidemiol & Biostat, London, England. [Wakeford, Richard] Univ Manchester, Dalton Nucl Inst, Manchester, Lancs, England. [Zablotska, Lydia B.] Univ Calif San Francisco, Sch Med, Dept Epidemiol & Biostat, San Francisco, CA USA. [Lipshultz, Steven E.] Univ Miami, Dept Pediat, Leonard M Miller Sch Med, Miami, FL 33152 USA. RP Little, MP (reprint author), NCI, Radiat Epidemiol Branch, NIH, Dept Hlth & Human Serv, Execut Plaza S,6120 Execut Blvd,MSC 7238, Rockville, MD 20852 USA. EM mark.little@nih.gov RI Taylor, Andrew/C-4311-2008; Tapio, Soile/M-7358-2014; Kashcheev, Valeriy/L-7794-2015; Chumak, Vadim/N-6960-2015; de Vathaire, Florent/L-2983-2016; Ivanov, Victor/R-9385-2016; Cardis, Elisabeth/C-3904-2017; OI Little, Mark/0000-0003-0980-7567; Klymenko, Sergiy/0000-0002-9758-7316; Tapio, Soile/0000-0001-9860-3683; Kashcheev, Valeriy/0000-0003-4108-9761; Chumak, Vadim/0000-0001-6045-9356; Ivanov, Victor/0000-0003-1372-0018; Bazyka, Dimitry/0000-0001-9982-5990; Wakeford, Richard/0000-0002-2934-0987 FU European Commission (EC) [FP6-036465]; Intramural Research Program of the National Institutes of Health (NIH); National Cancer Institute; Japanese Ministry of Health, Labour and Welfare; U.S. Department of Energy through the National Academy of Sciences FX This work was funded partially by the European Commission (EC) under contract FP6-036465 [NOn-Targeted Effects of ionising radiation (NOTE) integrated project]. This research was also supported by the Intramural Research Program of the National Institutes of Health (NIH) and the National Cancer Institute. This report makes use of data obtained from the Radiation Effects Research Foundation (RERF), Hiroshima and Nagasaki, Japan. RERF is a private, nonprofit foundation funded by the Japanese Ministry of Health, Labour and Welfare and the U.S. Department of Energy, the latter through the National Academy of Sciences. NR 59 TC 83 Z9 93 U1 3 U2 27 PU US DEPT HEALTH HUMAN SCIENCES PUBLIC HEALTH SCIENCE PI RES TRIANGLE PK PA NATL INST HEALTH, NATL INST ENVIRONMENTAL HEALTH SCIENCES, PO BOX 12233, RES TRIANGLE PK, NC 27709-2233 USA SN 0091-6765 J9 ENVIRON HEALTH PERSP JI Environ. Health Perspect. PD NOV PY 2012 VL 120 IS 11 BP 1503 EP 1511 DI 10.1289/ehp.1204982 PG 9 WC Environmental Sciences; Public, Environmental & Occupational Health; Toxicology SC Environmental Sciences & Ecology; Public, Environmental & Occupational Health; Toxicology GA 036ZE UT WOS:000311070000017 PM 22728254 ER PT J AU Morgan, JLL Zwart, SR Heer, M Ploutz-Snyder, R Ericson, K Smith, SM AF Morgan, Jennifer L. L. Zwart, Sara R. Heer, Martina Ploutz-Snyder, Robert Ericson, Karen Smith, Scott M. TI Bone metabolism and nutritional status during 30-day head-down-tilt bed rest SO JOURNAL OF APPLIED PHYSIOLOGY LA English DT Article DE bed rest; bone metabolism; nutritional status; oxalate; parathyroid hormone ID BODY NEGATIVE-PRESSURE; DURATION SPACE-FLIGHT; RED-BLOOD-CELL; TREADMILL EXERCISE; RESISTANCE EXERCISE; ARTIFICIAL GRAVITY; CALCIUM-METABOLISM; IDENTICAL-TWINS; SPACEFLIGHT; COUNTERMEASURE AB Morgan JL, Zwart SR, Heer M, Ploutz-Snyder R, Ericson K, Smith SM. Bone metabolism and nutritional status during 30-day head-down-tilt bed rest. J Appl Physiol 113: 1519-1529, 2012. First published September 20, 2012; doi:10.1152/japplphysiol.01064.2012.-Bed rest studies provide an important tool for modeling physiological changes that occur during spaceflight. Markers of bone metabolism and nutritional status were evaluated in 12 subjects (8 men, 4 women; ages 25-49 yr) who participated in a 30-day -6 degrees head-down-tilt diet-controlled bed rest study. Blood and urine samples were collected twice before, once a week during, and twice after bed rest. Data were analyzed using a mixed-effects linear regression with a priori contrasts comparing all days to the second week of the pre-bed rest acclimation period. During bed rest, all urinary markers of bone resorption increased similar to 20% (P < 0.001), and serum parathyroid hormone decreased similar to 25% (P < 0.001). Unlike longer (>60 days) bed rest studies, neither markers of oxidative damage nor iron status indexes changed over the 30 days of bed rest. Urinary oxalate excretion decreased similar to 20% during bed rest (P < 0.001) and correlated inversely with urinary calcium (R = -0.18, P < 0.02). These data provide a broad overview of the biochemistry associated with short-duration bed rest studies and provide an impetus for using shorter studies to save time and costs wherever possible. For some effects related to bone biochemistry, short-duration bed rest will fulfill the scientific requirements to simulate spaceflight, but other effects (antioxidants/oxidative damage, iron status) do not manifest until subjects are in bed longer, in which case longer studies or other analogs may be needed. Regardless, maximizing research funding and opportunities will be critical to enable the next steps in space exploration. C1 [Morgan, Jennifer L. L.; Smith, Scott M.] NASA, Lyndon B Johnson Space Ctr, Oak Ridge Assoc Univ NASA, Houston, TX 77058 USA. [Zwart, Sara R.; Ploutz-Snyder, Robert] NASA, Lyndon B Johnson Space Ctr, Univ Space Res Assoc & NASA, Houston, TX 77058 USA. [Heer, Martina] Univ Bonn, Dept Nutr & Food Sci, Bonn, Germany. [Heer, Martina] Profil Inst Metab Res, Neuss, Germany. [Ericson, Karen] Indiana Univ Purdue Univ, Dept Chem, Ft Wayne, IN 46805 USA. RP Smith, SM (reprint author), NASA, Lyndon B Johnson Space Ctr, Oak Ridge Assoc Univ NASA, Attn Mail Code SK3,2101 NASA Pkwy, Houston, TX 77058 USA. EM scott.m.smith@nasa.gov FU NASA Flight Analogs Project of NASA's Human Research Program; National Center for Advancing Translational Sciences, National Institutes of Health [1UL1RR029876-01] FX This study was funded in part by the NASA Flight Analogs Project of NASA's Human Research Program, and in part by grant 1UL1RR029876-01 from the National Center for Advancing Translational Sciences, National Institutes of Health. NR 42 TC 15 Z9 16 U1 0 U2 12 PU AMER PHYSIOLOGICAL SOC PI BETHESDA PA 9650 ROCKVILLE PIKE, BETHESDA, MD 20814 USA SN 8750-7587 J9 J APPL PHYSIOL JI J. Appl. Physiol. PD NOV PY 2012 VL 113 IS 10 BP 1519 EP 1529 DI 10.1152/japplphysiol.01064.2012 PG 11 WC Physiology; Sport Sciences SC Physiology; Sport Sciences GA 038XZ UT WOS:000311208700003 PM 22995395 ER PT J AU Yeh, SW Ham, YG Lee, JY AF Yeh, Sang-Wook Ham, Yoo-Geun Lee, June-Yi TI Changes in the Tropical Pacific SST Trend from CMIP3 to CMIP5 and Its Implication of ENSO SO JOURNAL OF CLIMATE LA English DT Article ID SEA-SURFACE TEMPERATURE; EL-NINO-LIKE; CLIMATE-CHANGE; DECADAL VARIABILITY; OSCILLATION; AMPLITUDE; OCEAN; MODULATIONS; MODEL; ICE AB This study assesses the changes in the tropical Pacific Ocean sea surface temperature (SST) trend and ENSO amplitude by comparing a historical run of the World Climate Research Programme Coupled Model Intercomparison Project (CMIP) phase-5 multimodel ensemble dataset (CMIP5) and the CMIP phase-3 dataset (CMIP3). The results indicate that the magnitude of the SST trend in the tropical Pacific basin has been significantly reduced from CMIP3 to CMIP5, which may be associated with the overestimation of the response to natural forcing and aerosols by including Earth system models in CMIP5. Moreover, the patterns of tropical warming over the second half of the twentieth century have changed from a La Nina-like structure in CMIP3 to an El Nino-like structure in CMIP5. Further analysis indicates that such changes in the background state of the tropical Pacific and an increase in the sensitivity of the atmospheric response to the SST changes in the eastern tropical Pacific have influenced the ENSO properties. In particular, the ratio of the SST anomaly variance in the eastern and western tropical Pacific increased from CMIP3 to CMIP5, indicating that a center of action associated with the ENSO amplitude has shifted to the east. C1 [Ham, Yoo-Geun] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA. [Ham, Yoo-Geun] Univ Space Res Assoc, Goddard Earth Sci Technol & Res Studies & Investi, Columbia, MD USA. [Yeh, Sang-Wook] Hanyang Univ, Dept Environm Marine Sci, Ansan, South Korea. [Lee, June-Yi] Univ Hawaii Manoa, Dept Meteorol, Honolulu, HI 96822 USA. [Lee, June-Yi] Univ Hawaii Manoa, Int Pacific Res Ctr, Honolulu, HI 96822 USA. RP Ham, YG (reprint author), NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Mail Code 610-1, Greenbelt, MD 20771 USA. EM yoo-geun.ham@nasa.gov RI Lee, June-Yi/D-5752-2012; Yeh, Sang-Wook/G-3007-2014 OI Yeh, Sang-Wook/0000-0003-4549-1686 FU Korea Meteorological Administration Research and Development Program [CATER 2012-3041]; International Pacific Research Center (IPRC); JAMSTEC; NOAA; NASA FX We acknowledge the WCRP's Working Group on Coupled Modeling, which is responsible for CMIP, and we thank the climate modeling groups (listed in Table 2) for producing and making available their model output. For CMIP, the U.S. Department of Energy's Program for Climate Model Diagnosis and Intercomparison provides coordinating support and led development of software infrastructure in partnership with the Global Organization for Earth System Science Portals. S.-W. Yeh was funded by the Korea Meteorological Administration Research and Development Program under Grant CATER 2012-3041. J.-Y. Lee acknowledges support from the International Pacific Research Center (IPRC) which is funded jointly by JAMSTEC, NOAA, and NASA. NR 33 TC 44 Z9 46 U1 5 U2 51 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 NOV 1 PY 2012 VL 25 IS 21 BP 7764 EP 7771 DI 10.1175/JCLI-D-12-00304.1 PG 8 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 036BZ UT WOS:000311002700026 ER PT J AU Miller, RL AF Miller, R. L. TI Adjustment to Radiative Forcing in a Simple Coupled Ocean-Atmosphere Model SO JOURNAL OF CLIMATE LA English DT Article ID SAHARAN AIR LAYER; TROPICAL NORTH-ATLANTIC; SOIL DUST AEROSOLS; CLIMATE RESPONSE; TEMPERATURE; IMPACTS; AFRICA; ENSO AB This study calculates the adjustment to radiative forcing in a simple model of a mixed layer ocean coupled to the overlying atmosphere. One application of the model is to calculate how dust aerosols perturb the temperature of the atmosphere and ocean, which in turn influence tropical cyclone development. Forcing at the top of the atmosphere (TOA) is the primary control upon both the atmospheric and ocean temperature anomalies, both at equilibrium and during most of the adjustment to the forcing. Ocean temperature is directly influenced by forcing only at the surface, but is indirectly related to forcing at TOA due to heat exchange with the atmosphere. Within a few days of the forcing onset, the atmospheric temperature adjusts to heating within the aerosol layer, reducing the net transfer of heat from the ocean to the atmosphere. For realistic levels of aerosol radiative forcing, the perturbed net surface heating strongly opposes forcing at the surface. This means that surface forcing dominates the ocean response only within the first few days following a dust outbreak, before the atmosphere has responded. This suggests that, to calculate the effect of dust upon the ocean temperature, the atmospheric adjustment must be taken into account explicitly and forcing at TOA must be considered in addition to the surface forcing. The importance of TOA forcing should be investigated in a model where vertical and lateral mixing of heat are calculated with fewer assumptions than in the simple model presented here. Nonetheless, the fundamental influence of TOA forcing appears to be only weakly sensitive to the model assumptions. C1 [Miller, R. L.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Miller, R. L.] Columbia Univ, Dept Appl Phys & Appl Math, New York, NY USA. RP Miller, RL (reprint author), NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA. EM ron.l.miller@nasa.gov RI Miller, Ron/E-1902-2012 FU National Science Foundation [ATM-06-20066] FX I am grateful for the thoughtful comments of two anonymous reviewers and Amato Evan (who suggested representing dynamical transport as linear relaxation). I also benefited from discussions with Peter Knippertz, Natalie Mahowald, Carlos Perez, Adam Sobel, and Charlie Zender. Thanks also to Lilly Del Valle for drafting Fig. 1. This work was supported by the Climate Dynamics Program of the National Science Foundation under ATM-06-20066. NR 41 TC 3 Z9 3 U1 0 U2 2 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 NOV PY 2012 VL 25 IS 22 BP 7802 EP 7821 DI 10.1175/JCLI-D-11-00119.1 PG 20 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 036NO UT WOS:000311034300002 ER PT J AU Englander, JA Conway, BA Williams, T AF Englander, Jacob A. Conway, Bruce A. Williams, Trevor TI Automated Mission Planning via Evolutionary Algorithms SO JOURNAL OF GUIDANCE CONTROL AND DYNAMICS LA English DT Article; Proceedings Paper CT 21st AAS/AIAA Space Flight Mechanics Meeting CY FEB 13-17, 2011 CL New Orleans, LA SP AAS, AIAA ID ASSIST TRAJECTORIES OPTIMIZATION; DIFFERENTIAL EVOLUTION; GLOBAL OPTIMIZATION; GENETIC ALGORITHM; DESIGN AB Many space mission planning problems may be formulated as hybrid optimal control problems, that is, problems that include both real-valued variables and categorical variables. In orbital mechanics problems, the categorical variables will typically specify the sequence of events that qualitatively describe the trajectory or mission, and the real-valued variables will represent the launch date, flight times between planets, magnitudes and directions of rocket burns, flyby altitudes, etc. A current practice is to preprune the categorical state space to limit the number of possible missions to a number whose cost may reasonably be evaluated. Of course, this risks pruning away the optimal solution. The method to be developed here avoids the need for prepruning by incorporating a new solution approach. The new approach uses nested loops: an outer-loop problem solver that handles the finite dynamics and finds a solution sequence in terms of the categorical variables, and an inner-loop problem solver that finds the optimal trajectory for a given sequence A binary genetic algorithm is used to solve the outer-loop problem, and a cooperative algorithm based on particle swarm optimization and differential evolution is used to solve the inner-loop problem. The hybrid optimal control solver is successfully demonstrated here by reproducing the Galileo and Cassini missions. C1 [Englander, Jacob A.; Conway, Bruce A.] Univ Illinois, Dept Aerosp Engn, Urbana, IL 61801 USA. [Williams, Trevor] NASA, Goddard Space Flight Ctr, Nav & Mission Design Branch, Greenbelt, MD 20770 USA. RP Englander, JA (reprint author), Univ Illinois, Dept Aerosp Engn, 104 S Wright St,Mail Code 236, Urbana, IL 61801 USA. NR 22 TC 26 Z9 26 U1 1 U2 20 PU AMER INST AERONAUTICS ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0731-5090 EI 1533-3884 J9 J GUID CONTROL DYNAM JI J. Guid. Control Dyn. PD NOV-DEC PY 2012 VL 35 IS 6 BP 1878 EP 1887 DI 10.2514/1.54101 PG 10 WC Engineering, Aerospace; Instruments & Instrumentation SC Engineering; Instruments & Instrumentation GA 037TM UT WOS:000311129400017 ER PT J AU Zanetti, R D'Souza, C AF Zanetti, Renato D'Souza, Chris TI Dual Accelerometer Usage Strategy for Onboard Space Navigation SO JOURNAL OF GUIDANCE CONTROL AND DYNAMICS LA English DT Article; Proceedings Paper CT 22nd AAS/AIAA Space Flight Mechanics Meeting CY JAN 29-FEB 02, 2012 CL Charleston, SC SP AAS, Space Flight Mech Comm, AIAA, Astrodynam Techn Comm C1 [Zanetti, Renato] Charles Stark Draper Lab Inc, Houston, TX 77058 USA. [D'Souza, Chris] NASA, Lyndon B Johnson Space Ctr, Aerosci & Flight Mech Div, Houston, TX 77058 USA. RP Zanetti, R (reprint author), Charles Stark Draper Lab Inc, Houston, TX 77058 USA. EM rzanetti@draper.com; chris.dsouza@nasa.gov NR 6 TC 0 Z9 0 U1 1 U2 5 PU AMER INST AERONAUTICS ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0731-5090 J9 J GUID CONTROL DYNAM JI J. Guid. Control Dyn. PD NOV-DEC PY 2012 VL 35 IS 6 BP 1899 EP 1902 DI 10.2514/1.58154 PG 4 WC Engineering, Aerospace; Instruments & Instrumentation SC Engineering; Instruments & Instrumentation GA 037TM UT WOS:000311129400019 ER PT J AU Zaretsky, EV Litt, JS Hendricks, RC Soditus, SM AF Zaretsky, Erwin V. Litt, Jonathan S. Hendricks, Robert C. Soditus, Sherry M. TI Determination of Turbine Blade Life from Engine Field Data SO JOURNAL OF PROPULSION AND POWER LA English DT Article; Proceedings Paper CT AIAA/ASME/ASCE/AHS/ASC 49th Structures, Structural Dynamics, and Materials Conference CY APR 07-10, 2008 CL Schaumburg, IL SP Amer Inst Aeronaut & Astronaut (AIAA), ASME, ASCE, AHS, ASC ID WEIBULL STATISTICS AB It is probable that no two engine companies determine the life of their engines or their components in the same way or apply the same experience and safety factors to their designs. Available data regarding failure mode for aircraft engine blades, although favoring low-cycle thermal-mechanical fatigue as the controlling mode of failure, are not definitive. Sixteen high-pressure turbine T-1 blade sets were removed from commercial aircraft engines that had been commercially flown by a single airline and inspected for damage. Each set contained 82 blades. The damage was cataloged into three categories related to their mode of failure: 1) Thermal-mechanical fatigue, 2) Oxidation/Erosion, and 3) Other. From these field data the turbine blade life was determined as well as the lives related to individual blade failure modes. A simplified formula for calculating turbine blade life and reliability was formulated. The L-10 blade life was calculated to be 2427 cycles (11,077 h). The resulting blade life attributed to oxidation/erosion equaled that attributed to thermal-mechanical fatigue. The category that contributed most to blade failure was Other. If there were there no blade failures attributed to oxidation/erosion and thermal-mechanical fatigue, the overall blade L-10 life would increase approximately 11 to 17%. C1 [Zaretsky, Erwin V.; Litt, Jonathan S.; Hendricks, Robert C.] NASA, John H Glenn Res Ctr, Cleveland, OH 44135 USA. [Soditus, Sherry M.] United Airlines Maintenance, San Francisco, CA 94128 USA. NR 27 TC 1 Z9 2 U1 1 U2 5 PU AMER INST AERONAUTICS ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0748-4658 J9 J PROPUL POWER JI J. Propul. Power PD NOV-DEC PY 2012 VL 28 IS 6 BP 1156 EP 1167 DI 10.2514/1.B34375 PG 12 WC Engineering, Aerospace SC Engineering GA 037UQ UT WOS:000311132400002 ER PT J AU Heymans, C Van Waerbeke, L Miller, L Erben, T Hildebrandt, H Hoekstra, H Kitching, TD Mellier, Y Simon, P Bonnett, C Coupon, J Fu, LP Harnois-Deraps, J Hudson, MJ Kilbinger, M Kuijken, K Rowe, B Schrabback, T Semboloni, E van Uitert, E Vafaei, S Velander, M AF Heymans, Catherine Van Waerbeke, Ludovic Miller, Lance Erben, Thomas Hildebrandt, Hendrik Hoekstra, Henk Kitching, Thomas D. Mellier, Yannick Simon, Patrick Bonnett, Christopher Coupon, Jean Fu, Liping Harnois-Deraps, Joachim Hudson, Michael J. Kilbinger, Martin Kuijken, Koenraad Rowe, Barnaby Schrabback, Tim Semboloni, Elisabetta van Uitert, Edo Vafaei, Sanaz Velander, Malin TI CFHTLenS: the Canada-France-Hawaii Telescope Lensing Survey SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE gravitational lensing: weak; cosmology: observations ID SHEAR CORRELATION-FUNCTIONS; WEAK GRAVITATIONAL SHEAR; GALAXY SHAPE MEASUREMENT; POINT-SPREAD FUNCTION; COSMIC SHEAR; DARK-MATTER; PHOTOMETRIC REDSHIFTS; IMAGE-ANALYSIS; LEGACY SURVEY; LARGE SCALES AB We present the CanadaFranceHawaii Telescope Lensing Survey (CFHTLenS) that accurately determines a weak gravitational lensing signal from the full 154 deg(2) of deep multicolour data obtained by the CFHT Legacy Survey. Weak gravitational lensing by large-scale structure is widely recognized as one of the most powerful but technically challenging probes of cosmology. We outline the CFHTLenS analysis pipeline, describing how and why every step of the chain from the raw pixel data to the lensing shear and photometric redshift measurement has been revised and improved compared to previous analyses of a subset of the same data. We present a novel method to identify data which contributes a non-negligible contamination to our sample and quantify the required level of calibration for the survey. Through a series of cosmology-insensitive tests we demonstrate the robustness of the resulting cosmic shear signal, presenting a science-ready shear and photometric redshift catalogue for future exploitation. C1 [Heymans, Catherine] Univ Edinburgh, Scottish Univ Phys Alliance, Inst Astron, Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland. [Van Waerbeke, Ludovic; Hildebrandt, Hendrik; Vafaei, Sanaz] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. [Miller, Lance; Velander, Malin] Univ Oxford, Dept Phys, Oxford OX1 3RH, England. [Erben, Thomas; Hildebrandt, Hendrik; Schrabback, Tim; van Uitert, Edo] Univ Bonn, Argelander Inst Astron, D-53121 Bonn, Germany. [Hoekstra, Henk; Kuijken, Koenraad; Schrabback, Tim; Semboloni, Elisabetta; van Uitert, Edo; Velander, Malin] Leiden Univ, Leiden Observ, NL-2333 CA Leiden, Netherlands. [Hoekstra, Henk] Univ Victoria, Dept Phys & Astron, Victoria, BC V8P 5C2, Canada. [Mellier, Yannick] Univ Paris 06, Inst Astrophys Paris, F-75014 Paris, France. [Bonnett, Christopher] CSIC IEEC, Inst Ciencies Espai, Barcelona 08193, Spain. [Coupon, Jean] Acad Sinica, Ins Astron & Astrophys, Taipei 10617, Taiwan. [Fu, Liping] Shanghai Normal Univ, Key Lab Astrophys, Shanghai 200234, Peoples R China. [Harnois-Deraps, Joachim] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada. [Harnois-Deraps, Joachim] Univ Toronto, Dept Phys, Toronto, ON M5S 1A7, Canada. [Hudson, Michael J.] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada. [Hudson, Michael J.] Perimeter Inst Theoret Phys, Waterloo, ON N2L 1Y5, Canada. [Kilbinger, Martin] CEA Saclay, Serv Astrophys SAp, F-91191 Gif Sur Yvette, France. [Kilbinger, Martin] Excellence Cluster Univ, D-85748 Garching, Germany. [Kilbinger, Martin] Univ Munich, Univ Sternwarte, D-81679 Munich, Germany. [Rowe, Barnaby] UCL, Dept Phys & Astron, London WC1E 6BT, England. [Rowe, Barnaby] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Rowe, Barnaby] CALTECH, Pasadena, CA 91125 USA. [Schrabback, Tim] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA. RP Heymans, C (reprint author), Univ Edinburgh, Scottish Univ Phys Alliance, Inst Astron, Royal Observ, Blackford Hill, Edinburgh EH9 3HJ, Midlothian, Scotland. EM heymans@roe.ac.uk RI Hudson, Michael/H-3238-2012; OI Hudson, Michael/0000-0002-1437-3786; Kilbinger, Martin/0000-0001-9513-7138; Rowe, Barnaby/0000-0002-7042-9174; Hoekstra, Henk/0000-0002-0641-3231 FU Canadian Space Agency; NSERC Research Tools and Instruments grant programme; Canada Foundation for Innovation under Compute Canada; Government of Ontario; Ontario Research Fund - Research Excellence; University of Toronto; European Commissions Marie Curie Research Training Network DUEL [MRTN-CT-2006-036133]; European Research Council under the EC [240185, 279396, 240672]; Natural Sciences and Engineering Research Council of Canada; Canadian Institute for Advanced Research; Deutsche Forschungsgemeinschaft [ER 327/3-1]; Transregional Collaborative Research Centre [TR 33]; Marie Curie IOF [252760]; CITA; Marie Curie IRG grant [230924]; Netherlands Organisation for Scientific Research [639.042.814]; Royal Society; CNRS/INSU (Institut National des Sciences de l'Univers); Programme National Galaxies et Cosmologie (PNCG); NSFC [11103012, 10878003]; Innovation Program [12ZZ134]; Chen Guang project; SMEC [10CG46]; STCSM [11290706600]; NSF [AST-0444059-001]; SAO [GO0-11147A]; NWO; Beecroft Institute for Particle Astrophysics and Cosmology; Spanish Science Ministry [AYA2009-13936, CSD2007-00060]; Generalitat de Catalunya [2009SGR1398]; European Commissions Marie Curie Initial Training Network CosmoComp [PITN-GA-2009-238356] FX This work is based on observations obtained with MegaPrime/MegaCam, a joint project of CFHT and CEA/DAPNIA, at the CFHT which is operated by the National Research Council (NRC) of Canada, the Institut National des Sciences de l'Univers of the Centre National de la Recherche Scientifique (CNRS) of France, and the University of Hawaii. This research used the facilities of the Canadian Astronomy Data Centre operated by the National Research Council of Canada with the support of the Canadian Space Agency. We thank the CFHT staff for successfully conducting the CFHTLS observations and in particular Jean-Charles Cuillandre and Eugene Magnier for the continuous improvement of the instrument calibration and the ELIXIR detrended data that we used. We also thank TERAPIX for the quality assessment and validation of individual exposures during the CFHTLS data acquisition period, and Emmanuel Bertin for developing some of the software used in this study. CFHTLenS data processing was made possible thanks to significant computing support from the NSERC Research Tools and Instruments grant programme, and to HPC specialist Ovidiu Toader. The N-body simulations used in this analysis were performed on the TCS supercomputer at the SciNet HPC Consortium. SciNet is funded by: the Canada Foundation for Innovation under the auspices of Compute Canada; the Government of Ontario; the Ontario Research Fund - Research Excellence; and the University of Toronto. The early stages of the CFHTLenS project were made possible thanks to the support of the European Commissions Marie Curie Research Training Network DUEL (MRTN-CT-2006-036133) which directly supported six members of the CFHTLenS team (LF, HHi, PS, BR, CB, MV) between 2007 and 2011 in addition to providing travel support and expenses for team meetings.; CH, HHo and BR acknowledge support from the European Research Council under the EC FP7 grant numbers 240185 (CH), 279396 (HHo) and 240672 (BR). LVW acknowledges support from the Natural Sciences and Engineering Research Council of Canada and the Canadian Institute for Advanced Research (Cosmology and Gravity programme). TE is supported by the Deutsche Forschungsgemeinschaft through project ER 327/3-1 and, with PS, is supported by the Transregional Collaborative Research Centre TR 33 - 'The Dark Universe'. HHi is supported by the Marie Curie IOF 252760 and by a CITA National Fellowship. HHo also acknowledges support from Marie Curie IRG grant 230924 and the Netherlands Organisation for Scientific Research grant number 639.042.814. TDK acknowledges support from a Royal Society University Research Fellowship. YM acknowledges support from CNRS/INSU (Institut National des Sciences de l'Univers) and the Programme National Galaxies et Cosmologie (PNCG). LF acknowledges support from NSFC grants 11103012 and 10878003, Innovation Program 12ZZ134 and Chen Guang project 10CG46 of SMEC, and STCSM grant 11290706600. MJH acknowledges support from the Natural Sciences and Engineering Research Council of Canada. TS acknowledges support from NSF through grant AST-0444059-001, SAO through grant GO0-11147A, and NWO.; MV acknowledges support from the Netherlands Organisation for Scientific Research (NWO) and from the Beecroft Institute for Particle Astrophysics and Cosmology. CB is supported by the Spanish Science Ministry AYA2009-13936 Consolider-Ingenio CSD2007-00060, project 2009SGR1398 from Generalitat de Catalunya and by the European Commissions Marie Curie Initial Training Network CosmoComp (PITN-GA-2009-238356). Part of BR's work was done at the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA. NR 77 TC 227 Z9 228 U1 1 U2 2 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD NOV PY 2012 VL 427 IS 1 BP 146 EP 166 DI 10.1111/j.1365-2966.2012.21952.x PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 031XH UT WOS:000310675400013 ER PT J AU Cappelluti, N Ranalli, P Roncarelli, M Arevalo, P Zamorani, G Comastri, A Gilli, R Rovilos, E Vignali, C Allevato, V Finoguenov, A Miyaji, T Nicastro, F Georgantopoulos, I Kashlinsky, A AF Cappelluti, N. Ranalli, P. Roncarelli, M. Arevalo, P. Zamorani, G. Comastri, A. Gilli, R. Rovilos, E. Vignali, C. Allevato, V. Finoguenov, A. Miyaji, T. Nicastro, F. Georgantopoulos, I. Kashlinsky, A. TI The nature of the unresolved extragalactic cosmic soft X-ray background SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: active; dark matter; diffuse radiation; large-scale structure of Universe; X-rays: galaxies ID HOT INTERGALACTIC MEDIUM; ACTIVE GALACTIC NUCLEI; DEEP FIELD-SOUTH; MS SOURCE CATALOGS; STAR-FORMING GALAXIES; LYMAN-BREAK GALAXIES; DARK-MATTER HALOES; XMM-NEWTON; NUMBER COUNTS; MISSING BARYONS AB In this paper we investigate the power spectrum of the unresolved 0.5-2 keV cosmic X-ray background (CXB) with deep Chandra 4-Msec (Ms) observations in the Chandra Deep Field South (CDFS). We measured a signal that, on scales >30 arcsec, is significantly higher than the shot noise and is increasing with angular scale. We interpreted this signal as the joint contribution of clustered undetected sources like active galactic nuclei (AGN), galaxies and the intergalactic medium (IGM). The power of unresolved cosmic source fluctuations accounts for similar to 12 per cent of the 0.5-2 keV extragalactic CXB. Overall, our modelling predicts that similar to 20 per cent of the unresolved CXB flux is produced by low-luminosity AGN, similar to 25 per cent by galaxies and similar to 55 per cent by the IGM. We do not find any direct evidence of the so-called 'warm hot intergalactic medium' (i.e. matter with 10(5) < T < 10(7) K and density contrast delta < 1000), but we estimated that it could produce about 1/7 of the unresolved CXB. We placed an upper limit on the space density of postulated X-ray-emitting early black holes at z > 7.5 and compared it with supermassive black hole evolution models. C1 [Cappelluti, N.; Ranalli, P.; Zamorani, G.; Comastri, A.; Gilli, R.; Rovilos, E.; Vignali, C.; Georgantopoulos, I.] INAF, Osservatorio Astron Bologna, I-40127 Bologna, Italy. [Cappelluti, N.; Finoguenov, A.] Univ Maryland Baltimore Cty, Baltimore, MD 21250 USA. [Ranalli, P.; Georgantopoulos, I.] Natl Observ Athens, Inst Astron & Astrophys, Athens 15236, Greece. [Ranalli, P.; Roncarelli, M.; Vignali, C.] Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy. [Arevalo, P.] Univ Andres Bello, Dept Ciencias Fis, Santiago, Chile. [Allevato, V.] Max Planck Inst Plasmaphys & Excellence Cluster U, D-85748 Garching, Germany. [Finoguenov, A.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Miyaji, T.] Univ Nacl Autonoma Mexico, Inst Astron, Ensenada, Baja California, Mexico. [Nicastro, F.] INAF, Osservatorio Astron Roma, I-00040 Monte Porzio Catone, Italy. [Kashlinsky, A.] SSAI, Lanham, MD 20706 USA. [Kashlinsky, A.] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA. RP Cappelluti, N (reprint author), INAF, Osservatorio Astron Bologna, Via Ranzani 1, I-40127 Bologna, Italy. EM nico.cappelluti@oabo.inaf.it RI Vignali, Cristian/J-4974-2012; Ranalli, Piero/K-6363-2013; Georgantopoulos, Ioannis/L-3687-2013; Comastri, Andrea/O-9543-2015; Gilli, Roberto/P-1110-2015; OI Cappelluti, Nico/0000-0002-1697-186X; Zamorani, Giovanni/0000-0002-2318-301X; Vignali, Cristian/0000-0002-8853-9611; Ranalli, Piero/0000-0003-3956-755X; Comastri, Andrea/0000-0003-3451-9970; Gilli, Roberto/0000-0001-8121-6177; Nicastro, Fabrizio/0000-0002-6896-1364 FU INAF-Fellowship program; Fondecyt [11100449]; ASI-INAF [1/009/10/0]; NAS XMM [NNX08AX51G, NNX09AQ05G]; ASI [ASI-ADAE]; Greek General Secretariat of Research and Technology FX NC acknowledges the INAF-Fellowship program for support. PA acknowledges support from Fondecyt 11100449. We acknowledge financial contribution from the agreement ASI-INAF 1/009/10/0. FN acknowledges support from NAS XMM Grant NNX08AX51G, XMM Grant NNX09AQ05G and ASI Grant ASI-ADAE. PR acknowledges a grant from the Greek General Secretariat of Research and Technology in the framework of the programme Support of Postdoctoral Researchers. NC thanks the anonymous referee for the suggested improvements. NR 74 TC 21 Z9 21 U1 0 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 NOV PY 2012 VL 427 IS 1 BP 651 EP 663 DI 10.1111/j.1365-2966.2012.21867.x PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 031XH UT WOS:000310675400050 ER PT J AU Livermore, RC Jones, T Richard, J Bower, RG Ellis, RS Swinbank, AM Rigby, JR Smail, I Arribas, S Rodriguez-Zaurin, J Colina, L Ebeling, H Crain, RA AF Livermore, R. C. Jones, T. Richard, J. Bower, R. G. Ellis, R. S. Swinbank, A. M. Rigby, J. R. Smail, Ian Arribas, S. Rodriguez-Zaurin, J. Colina, L. Ebeling, H. Crain, R. A. TI Hubble Space Telescope H alpha imaging of star-forming galaxies at z similar or equal to 1-1.5: evolution in the size and luminosity of giant H II regions SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE gravitational lensing: strong; galaxies: high-redshift; galaxies: star formation ID INTEGRAL FIELD SPECTROSCOPY; ULTRA DEEP FIELD; HIGH-REDSHIFT; MOLECULAR CLOUDS; INTERSTELLAR-MEDIUM; RESOLVED SPECTROSCOPY; COMPACT SPHEROIDS; SCALING RELATIONS; SURFACE-DENSITY; BILLION YEARS AB We present Hubble Space Telescope/Wide Field Camera 3 narrow-band imaging of the H alpha emission in a sample of eight gravitationally lensed galaxies at z = 1-1.5. The magnification caused by the foreground clusters enables us to obtain a median source plane spatial resolution of 360 pc, as well as providing magnifications in flux ranging from similar to 10x to similar to 50x. This enables us to identify resolved star-forming H II regions at this epoch and therefore study their H alpha luminosity distributions for comparisons with equivalent samples at z similar to 2 and in the local Universe. We find evolution in the both luminosity and surface brightness of H II regions with redshift. The distribution of clump properties can be quantified with an H II region luminosity function, which can be fit by a power law with an exponential break at some cut-off, and we find that the cut-off evolves with redshift. We therefore conclude that clumpy galaxies are seen at high redshift because of the evolution of the cut-off mass; the galaxies themselves follow similar scaling relations to those at z = 0, but their H II regions are larger and brighter and thus appear as clumps which dominate the morphology of the galaxy. A simple theoretical argument based on gas collapsing on scales of the Jeans mass in a marginally unstable disc shows that the clumpy morphologies of high-z galaxies are driven by the competing effects of higher gas fractions causing perturbations on larger scales, partially compensated by higher epicyclic frequencies which stabilize the disc. C1 [Livermore, R. C.; Richard, J.; Bower, R. G.; Swinbank, A. M.; Smail, Ian] Univ Durham, Inst Computat Cosmol, Durham DH1 3LE, England. [Jones, T.; Ellis, R. S.] CALTECH, Dept Astron, Pasadena, CA 91125 USA. [Richard, J.] Observ Lyon, CRAL, F-69561 St Genis Laval, France. [Rigby, J. R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Arribas, S.; Colina, L.] CSIC INTA, Ctr Astrobiol, Dept Astrofis, Madrid 28850, Spain. [Rodriguez-Zaurin, J.] IAC, E-38205 Tenerife, Spain. [Ebeling, H.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Crain, R. A.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. RP Livermore, RC (reprint author), Univ Durham, Inst Computat Cosmol, South Rd, Durham DH1 3LE, England. EM r.c.livermore@durham.ac.uk RI Smail, Ian/M-5161-2013; Rigby, Jane/D-4588-2012; Arribas, Santiago/F-9277-2015 OI Smail, Ian/0000-0003-3037-257X; Rigby, Jane/0000-0002-7627-6551; Arribas, Santiago/0000-0001-7997-1640 FU STFC; Marie Curie Career Integration Grant [294074]; STScI [GO-09722, GO-10491, GO-10875, GO-12166]; NASA [NAS5-26555]; NASA through Space Telescope Science Institute [12197, 11678] FX The authors would like to thank Karl Glazebrook, Emily Wisnioski, Lisa Kewley and Norm Murray for useful discussions and Andrew Newman for providing an updated strong lensing model of the cluster Abell 611. RCL acknowledges a studentship from STFC, RGB and IS are supported by STFC and IS further acknowledges a Leverhulme Senior Fellowship. AMS acknowledges an STFC Advanced Fellowship, and JR is supported by the Marie Curie Career Integration Grant 294074. HE gratefully acknowledges financial support from STScI grants GO-09722, GO-10491, GO-10875 and GO-12166. This work is based on observations with the NASA/ESA Hubble Space Telescope obtained at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. Support for Program number 12197 and Program number 11678 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 NAS5-26555. NR 64 TC 34 Z9 34 U1 0 U2 3 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD NOV PY 2012 VL 427 IS 1 BP 688 EP 702 DI 10.1111/j.1365-2966.2012.21900.x PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 031XH UT WOS:000310675400053 ER PT J AU Smith, DJB Dunne, L da Cunha, E Rowlands, K Maddox, SJ Gomez, HL Bonfield, DG Charlot, S Driver, SP Popescu, CC Tuffs, RJ Dunlop, JS Jarvis, MJ Seymour, N Symeonidis, M Baes, M Bourne, N Clements, DL Cooray, A De Zotti, G Dye, S Eales, S Scott, D Verma, A van der Werf, P Andrae, E Auld, R Buttiglione, S Cava, A Dariush, A Fritz, J Hopwood, R Ibar, E Ivison, RJ Kelvin, L Madore, BF Pohlen, M Rigby, EE Robotham, A Seibert, M Temi, P AF Smith, D. J. B. Dunne, L. da Cunha, E. Rowlands, K. Maddox, S. J. Gomez, H. L. Bonfield, D. G. Charlot, S. Driver, S. P. Popescu, C. C. Tuffs, R. J. Dunlop, J. S. Jarvis, M. J. Seymour, N. Symeonidis, M. Baes, M. Bourne, N. Clements, D. L. Cooray, A. De Zotti, G. Dye, S. Eales, S. Scott, D. Verma, A. van der Werf, P. Andrae, E. Auld, R. Buttiglione, S. Cava, A. Dariush, A. Fritz, J. Hopwood, R. Ibar, E. Ivison, R. J. Kelvin, L. Madore, B. F. Pohlen, M. Rigby, E. E. Robotham, A. Seibert, M. Temi, P. TI Herschel-ATLAS: multi-wavelength SEDs and physical properties of 250 mu m selected galaxies at z < 0.5 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Review DE Galaxies: starburst ID SPECTRAL ENERGY-DISTRIBUTION; SCIENCE DEMONSTRATION PHASE; STAR-FORMING GALAXIES; DEEP FIELD-SOUTH; STELLAR POPULATIONS; COLD DUST; NEARBY GALAXIES; SKY SURVEY; SUBMILLIMETER WAVELENGTHS; PHOTOMETRIC REDSHIFTS AB We present a pan-chromatic analysis of an unprecedented sample of 1402 250 mu m selected galaxies at z < 0.5 (<(z)over bar> = 0.24) from the Herschel-ATLAS survey. We complement our Herschel 100-500 mu m data with UV-K-band photometry from the Galaxy And Mass Assembly (GAMA) survey and apply the magphys energy-balance technique to produce pan-chromatic spectral energy distributions (SEDs) for a representative sample of 250 mu m selected galaxies spanning the most recent 5 Gyr of cosmic history. We derive estimates of physical parameters, including star formation rates, stellar masses, dust masses and infrared (IR) luminosities. The typical H-ATLAS galaxy at z < 0.5 has a far-infrared luminosity in the range 10(10)-10(12) L-circle dot (SFR: 1-50 M-circle dot yr(-1)) and thus is broadly representative of normal star-forming galaxies over this redshift range. We show that 250 mu m selected galaxies contain a larger mass of dust at a given IR luminosity or star formation rate than previous samples selected at 60 mu m from the IRAS. We derive typical SEDs for H-ATLAS galaxies, and show that the emergent SED shape is most sensitive to specific star formation rate. The optical-UV SEDs also become more reddened due to dust at higher redshifts. Our template SEDs are significantly cooler than existing IR templates. They may therefore be most appropriate for inferring total IR luminosities from moderate redshift sub-millimetre selected samples and for inclusion in models of the lower redshift sub-millimetre galaxy populations. C1 [Smith, D. J. B.; Dunne, L.; Rowlands, K.; Maddox, S. J.; Bourne, N.; Dye, S.; Rigby, E. E.] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England. [Smith, D. J. B.; Bonfield, D. G.; Jarvis, M. J.] Univ Hertfordshire, Ctr Astrophys, Sci & Technol Res Inst, Hatfield AL10 9AB, Herts, England. [Dunne, L.; Maddox, S. J.] Univ Canterbury, Dept Phys & Astron, Christchurch 8140, New Zealand. [da Cunha, E.; Eales, S.] Max Planck Inst Astron, D-60115 Heidelberg, Germany. [Gomez, H. L.; Auld, R.; Dariush, A.; Pohlen, M.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Charlot, S.] Univ Paris 06, CNRS, Inst Astrophys Paris, UMR 7095, F-75014 Paris, France. [Driver, S. P.; Kelvin, L.; Robotham, A.] Univ St Andrews, Sch Phys & Astron, SUPA, St Andrews KY16 9SS, Fife, Scotland. [Driver, S. P.; Kelvin, L.; Robotham, A.] Univ Western Australia, Int Ctr Radio Astron Res, Perth, WA 6009, Australia. [Popescu, C. C.] Univ Cent Lancashire, Jeremiah Horrocks Inst, Preston PR1 2HE, Lancs, England. [Tuffs, R. J.; Andrae, E.] Max Planck Inst Kernphys, D-69117 Heidelberg, Germany. [Dunlop, J. S.; Ivison, R. J.] Univ Edinburgh, Royal Observ, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland. [Seymour, N.] CSIRO Astron & Space Sci, Epping, NSW 1710, Australia. [Seymour, N.; Symeonidis, M.] Univ Coll London, Mullard Space Sci Lab, Dept Space & Climate Phys, Dorking RH5 6NT, Surrey, England. [Baes, M.; Fritz, J.] Univ Ghent, Sterrenkundig Observ, B-9000 Ghent, Belgium. [Clements, D. L.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Astrophys Grp, London SW7 2AZ, England. [Cooray, A.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. [De Zotti, G.; Buttiglione, S.] Osserv Astron Padova, INAF, I-35122 Padua, Italy. [De Zotti, G.] SISSA, I-34136 Trieste, Italy. [Scott, D.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. [Verma, A.] Univ Oxford, Dept Phys, Oxford OX1 3RH, England. [van der Werf, P.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Cava, A.] Univ Complutense Madrid, Fac CC Fis, Dept Astrofis, E-28040 Madrid, Spain. [Dariush, A.; Hopwood, R.] Univ London Imperial Coll Sci Technol & Med, Dept Phys, London SW7 2AZ, England. [Ibar, E.; Ivison, R. J.] Royal Observ, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland. [Madore, B. F.; Seibert, M.] Observ Carnegie Inst, Pasadena, CA 91101 USA. [Temi, P.] NASA, Ames Res Ctr, Astrophys Branch, Moffett Field, CA 94035 USA. [Jarvis, M. J.] Univ Western Cape, Dept Phys, ZA-7535 Bellville, South Africa. RP Smith, DJB (reprint author), Univ Nottingham, Sch Phys & Astron, Univ Pk, Nottingham NG7 2RD, England. EM daniel.j.b.smith@gmail.com RI Baes, Maarten/I-6985-2013; Robotham, Aaron/H-5733-2014; Driver, Simon/H-9115-2014; Ivison, R./G-4450-2011; Cava, Antonio/C-5274-2017; OI Seymour, Nicholas/0000-0003-3506-5536; Baes, Maarten/0000-0002-3930-2757; Robotham, Aaron/0000-0003-0429-3579; Driver, Simon/0000-0001-9491-7327; Ivison, R./0000-0001-5118-1313; Cava, Antonio/0000-0002-4821-1275; Maddox, Stephen/0000-0001-5549-195X; Scott, Douglas/0000-0002-6878-9840 FU STFC (UK); ARC (Australia); AAO; Alfred P. Sloan Foundation; National Science Foundation; U.S. Department of Energy; National Aeronautics and Space Administration; Japanese Monbukagakusho; Max Planck Society; Higher Education Funding Council for England; ASI/INAF [I/009/10/0] FX The authors wish to thank the anonymous referee for his/her tireless work and insightful comments, which have substantially improved this paper. The Herschel-ATLAS is a project with Herschel, which is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA. The H-ATLAS website is http://www.hatlas.org/. GAMA is a joint European-Australasian project based around a spectroscopic campaign using the Anglo-Australian Telescope. The GAMA input catalogue is based on data taken from the Sloan Digital Sky Survey and the UKIRT Infrared Deep Sky Survey. Complementary imaging of the GAMA regions is being obtained by a number of independent survey programmes including GALEX MIS, VST KIDS, VISTA VIKING, WISE, GMRT and ASKAP providing UV to radio coverage. GAMA is funded by the STFC (UK), the ARC (Australia), the AAO, and the participating institutions. The GAMA website is http://www.gama-survey.org/. This work used data from the UKIDSS DR5 and the SDSS DR7. The UKIDSS project is defined in Lawrence et al. (2007) and uses the UKIRT Wide Field Camera (WFCAM; Casali et al. 2007). Funding for the SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, the U.S. Department of Energy, the National Aeronautics and Space Administration, the Japanese Monbukagakusho, the Max Planck Society and the Higher Education Funding Council for England. The Italian group acknowledges partial financial support from ASI/INAF agreement no. I/009/10/0. NR 106 TC 78 Z9 78 U1 0 U2 8 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD NOV PY 2012 VL 427 IS 1 BP 703 EP 727 DI 10.1111/j.1365-2966.2012.21930.x PG 25 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 031XH UT WOS:000310675400054 ER PT J AU D'Ammando, F Rau, A Schady, P Finke, J Orienti, M Greiner, J Kann, DA Ojha, R Foley, AR Stevens, J Blanchard, JM Edwards, PG Kadler, M Lovell, JEJ AF D'Ammando, F. Rau, A. Schady, P. Finke, J. Orienti, M. Greiner, J. Kann, D. A. Ojha, R. Foley, A. R. Stevens, J. Blanchard, J. M. Edwards, P. G. Kadler, M. Lovell, J. E. J. TI PKS 2123-463: a confirmed gamma-ray blazar at high redshift SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: active; galaxies: nuclei; quasars: general; quasars: individual: PKS 2123-463; gamma rays: general ID ACTIVE GALACTIC NUCLEI; LARGE-AREA TELESCOPE; ALL-SKY SURVEY; BL LACERTAE OBJECTS; PHOTOMETRIC REDSHIFT; RADIO-SOURCES; COMPTON ANALYSIS; SOURCE CATALOG; BLACK-HOLES; MISSION AB The flat spectrum radio quasar (FSRQ) PKS 2123-463 was associated in the first Fermi-Large Area Telescope (LAT) source catalogue with the gamma-ray source 1FGL J2126.1-4603, but when considering the full first two years of Fermi observations, no gamma-ray source at a position consistent with this FSRQ was detected, and thus PKS 2123-463 was not reported in the second Fermi-LAT source catalogue. On 2011 December 14 a gamma-ray source positionally consistent with PKS 2123-463 was detected in flaring activity by Fermi-LAT. This activity triggered radio-to-X-ray observations by the Swift, Gamma-ray Optical/Near-Infrared Detector (GROND), Australia Telescope Compact Array (ATCA), Ceduna and Seven Dishes Karoo Array Telescope (KAT-7) observatories. Results of the localization of the gamma-ray source over 41 months of Fermi-LAT operation are reported here in conjunction with the results of the analysis of radio, optical, ultraviolet (UV) and X-ray data collected soon after the gamma-ray flare. The strict spatial association with the lower energy counterpart together with a simultaneous increase of the activity in optical, UV, X-ray and gamma-ray bands led to a firm identification of the gamma-ray source with PKS 2123-463. A new photometric redshift has been estimated as z = 1.46 +/- 0.05 using GROND and Swift Ultraviolet/Optical Telescope (UVOT) observations, in rough agreement with the disputed spectroscopic redshift of z = 1.67. We fit the broad-band spectral energy distribution with a synchrotron/external Compton model. We find that a thermal disc component is necessary to explain the optical/UV emission detected by Swift/UVOT. This disc has a luminosity of similar to 1.8 x 10(46) erg s(-1), and a fit to the disc emission assuming a Schwarzschild (i.e. non-rotating) black hole gives a mass of similar to 2 x 10(9) M-circle dot. This is the first black hole mass estimate for this source. C1 [D'Ammando, F.] Univ Perugia, Dip Fis, I-06123 Perugia, Italy. [D'Ammando, F.] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy. [D'Ammando, F.; Orienti, M.] INAF, Ist Radioastron, I-40129 Bologna, Italy. [Rau, A.; Schady, P.; Greiner, J.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Finke, J.] USN, Res Lab, Washington, DC 20375 USA. [Orienti, M.] Univ Bologna, Dip Astron, I-40127 Bologna, Italy. [Kann, D. A.] Thuringer Landessternwarte Tautenburg, D-07778 Tautenburg, Germany. [Ojha, R.] Catholic Univ Amer, Dept Phys, IACS, Washington, DC 20064 USA. [Foley, A. R.] SKA SA, Cape Town, South Africa. [Stevens, J.] ATNF, CSIRO Astron & Space Sci, Narrabri, NSW 2390, Australia. [Blanchard, J. M.; Lovell, J. E. J.] Univ Tasmania, Sch Math & Phys, Hobart, Tas 7001, Australia. [Edwards, P. G.] ATNF, CSIRO Astron & Space Sci, Epping, NSW 1710, Australia. [Kadler, M.] Univ Wurzburg, Inst Theoret Phys & Astrophys, D-97074 Wurzburg, Germany. [Kadler, M.] NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA. RP D'Ammando, F (reprint author), Univ Perugia, Dip Fis, Via A Pascoli, I-06123 Perugia, Italy. EM filippo.dammando@fisica.unipg.it FU DFG [HA 1850/28-1, Kl 766/16-1]; MPE; Commonwealth of Australia; NASA [NNH09ZDA001N, 31263] FX Part of the funding for GROND (both hardware and personnel) was generously granted from the Leibniz-Prize to Professor G. Hasinger (DFG grant HA 1850/28-1). We thank the Swift team for making these observations possible, the duty scientists and science planners. DAK acknowledges support by DFG grant Kl 766/16-1, and is grateful for travel funding support through MPE. The Australia Telescope Compact 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 research was funded in part by NASA through Fermi Guest Investigator grant NNH09ZDA001N (proposal number 31263). This research was supported by an appointment to the NASA Postdoctoral Program at the Goddard Space Flight Center, administered by Oak Ridge Associated Universities through a contract with NASA. We thank Silvia Raino and the anonymous referee for useful comments and suggestions. NR 58 TC 5 Z9 5 U1 0 U2 1 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD NOV PY 2012 VL 427 IS 1 BP 893 EP 900 DI 10.1111/j.1365-2966.2012.22041.x PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 031XH UT WOS:000310675400069 ER PT J AU Burgess, D Drake, J Marsch, E Velli, M von Steiger, R Zurbuchen, TH AF Burgess, David Drake, James Marsch, Eckart Velli, Marco von Steiger, Rudolf Zurbuchen, Thomas H. TI Multi-Scale Physics in Coronal Heating and Solar Wind Acceleration Foreword SO SPACE SCIENCE REVIEWS LA English DT Editorial Material C1 [von Steiger, Rudolf] Int Space Sci Inst, CH-3012 Bern, Switzerland. [Burgess, David] Univ London, Sch Phys & Astron, London E1 4NS, England. [Drake, James] Univ Maryland, Dept Phys, Inst Phys Sci & Technol, College Pk, MD 20742 USA. [Marsch, Eckart] Univ Kiel, IEAP, D-24118 Kiel, Germany. [Velli, Marco] NASA, Jet Prop Lab, Pasadena, CA 91109 USA. [Zurbuchen, Thomas H.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. RP von Steiger, R (reprint author), Int Space Sci Inst, Hallerstr 6, CH-3012 Bern, Switzerland. EM d.burgess@qmul.ac.uk; drake@plasma.umd.edu; marsch@physik.uni-kiel.de; mvelli@mail.jpl.nasa.gov; vsteiger@issibern.ch; thomasz@umich.edu RI Von Steiger, Rudolf/F-6822-2011 OI Von Steiger, Rudolf/0000-0002-3350-0023 NR 0 TC 0 Z9 0 U1 0 U2 6 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-6308 J9 SPACE SCI REV JI Space Sci. Rev. PD NOV PY 2012 VL 172 IS 1-4 BP 1 EP 3 DI 10.1007/s11214-012-9939-4 PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 034MJ UT WOS:000310877300001 ER PT J AU Hansteen, VH Velli, M AF Hansteen, Viggo H. Velli, Marco TI Solar Wind Models from the Chromosphere to 1 AU SO SPACE SCIENCE REVIEWS LA English DT Review DE Solar wind acceleration; Energy conservation; Thermal force; Scaling laws; Solar wind origins ID ALFVEN WAVES; TRANSPORT-EQUATIONS; CORONAL HOLES; ACCELERATION; TURBULENCE; ATMOSPHERE; HELIUM; ENERGY; RECONNECTION; ANISOTROPY AB Recent models of the fast solar wind are characterized by low coronal electron temperatures while proton, alpha-particle, and minor ion temperatures are expected to be quite high and generally anisotropic, including large temperatures perpendicular to the magnetic field and parallel beams. This entails that the electric field should be relatively unimportant and that solar wind outflows with both high asymptotic flow speeds but maintaining a low mass flux should be a natural outcome of plasma expansion along open polar magnetic field lines. In this chapter we will explain why such changes with respect to the classical, electron thermally driven solar wind have come about and outline the most important remaining concerning the astrophysics of coronal winds. The progress we have seen in the last decade is largely due observations made with instruments onboard Ulysses (McComas et al. in Space Sci. Rev. 72:93, 1995) and SOHO (Fleck et al. in The SOHO Mission, Kluwer, Dordrecht, 1995). These observations have spawned a new understanding of solar wind energetics, and the consideration of the chromosphere, corona, and solar wind as a unified system. We will begin by giving our own, highly biased, "pocket history" of solar wind theory highlighting the problems that had to be resolved in order to make the original Parker formulation of thermally driven winds conform with observational results. Central to this discussion are questions of how the wind's asymptotic flow speed and mass flux are set, but we will also touch upon higher order moments such as the ion and electron temperatures and heat fluxes as well as the possible role of Alfv,n waves and particle effects in driving the solar wind outflow. Solar wind scaling laws will be discussed in the context of the origin of slow and fast wind streams. C1 [Hansteen, Viggo H.] Univ Oslo, Inst Theoret Astrophys, Oslo, Norway. [Velli, Marco] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Hansteen, VH (reprint author), Univ Oslo, Inst Theoret Astrophys, Oslo, Norway. EM viggoh@astro.uio.no; mvelli@jpl.nasa.gov NR 75 TC 10 Z9 10 U1 0 U2 12 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 NOV PY 2012 VL 172 IS 1-4 BP 89 EP 121 DI 10.1007/s11214-012-9887-z PG 33 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 034MJ UT WOS:000310877300007 ER PT J AU Antiochos, SK Linker, JA Lionello, R Mikic, Z Titov, V Zurbuchen, TH AF Antiochos, Spiro K. Linker, Jon A. Lionello, Roberto Mikic, Zoran Titov, Viacheslav Zurbuchen, Thomas H. TI The Structure and Dynamics of the Corona-Heliosphere Connection SO SPACE SCIENCE REVIEWS LA English DT Review DE Sun: corona; Sun: solar wind ID SLOW SOLAR-WIND; WHOLE SUN MONTH; MAGNETIC-FIELD; MASS EJECTIONS; RECONNECTION; STREAMERS; MODELS; FLUX; FLOW; DISCONNECTION AB Determining how the heliospheric magnetic field and plasma connect to the Sun's corona and photosphere is, perhaps, the central problem in solar and heliospheric physics. For much of the heliosphere, this connection appears to be well understood. It is now generally accepted that so-called coronal holes, which appear dark in X-rays and are predominantly unipolar at the photosphere, are the sources of quasi-steady wind that is generally fast, > 500 km/s, but can sometimes be slow. However, the connection to the Sun of the slow, non-steady wind is far from understood and remains a major mystery. We review the existing theories for the sources of the non-steady wind and demonstrate that they have difficulty accounting for both the observed composition of the wind and its large angular extent. A new theory is described in which this wind originates from the continuous opening and closing of narrow open field corridors in the corona, which give rise to a web of separatrices (the S-Web) in the heliosphere. Note that in this theory the corona-heliosphere connection is intrinsically dynamic, at least for this type of wind. Support for the S-Web model is derived from MHD solutions for the corona and wind during the time of the August 1, 2008 eclipse. Additionally, we perform fully dynamic numerical simulations of the corona and heliosphere in order to test the S-Web model as well as the interchange model proposed by Fisk and co-workers. We discuss the implications of our simulations for the competing theories and for understanding the corona-heliosphere connection, in general. C1 [Antiochos, Spiro K.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Linker, Jon A.; Lionello, Roberto; Mikic, Zoran; Titov, Viacheslav] Predict Sci Inc, San Diego, CA 92121 USA. [Zurbuchen, Thomas H.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Coll Engn, Ann Arbor, MI 48109 USA. RP Antiochos, SK (reprint author), NASA, Goddard Space Flight Ctr, Code 674, Greenbelt, MD 20771 USA. EM spiro.antiochos@nasa.gov RI Antiochos, Spiro/D-4668-2012 OI Antiochos, Spiro/0000-0003-0176-4312 FU NASA HTP Program; NASA GI Program; NASA SRT Program; NASA TRT Program; CISM (an NSF Science and Technology Center); Strategic Capabilities; NASA; NSF; AFOSR; ISSI FX This work originated from numerous discussions in a LWS Focus Team on open flux in the heliosphere. The work was funded, in part, by the NASA HTP, GI, SR&T, and TR&T Programs, by CISM (an NSF Science and Technology Center), and by Strategic Capabilities (jointly funded by NASA, NSF, and AFOSR). THZ acknowledges the support of ISSI where much of his work on this paper was performed. Computational resources were provided by the NSF supported Texas Advanced Computing Center (TACC) in Austin and the NASA Advanced Supercomputing Division (NAS) at Ames Research Center. NR 67 TC 24 Z9 24 U1 2 U2 9 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 NOV PY 2012 VL 172 IS 1-4 BP 169 EP 185 DI 10.1007/s11214-011-9795-7 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 034MJ UT WOS:000310877300011 ER PT J AU Edmondson, JK AF Edmondson, J. K. TI On the Role of Interchange Reconnection in the Generation of the Slow Solar Wind SO SPACE SCIENCE REVIEWS LA English DT Review DE Solar corona; Solar wind; MHD; Reconnection ID CORONAL-HOLE BOUNDARIES; OPEN MAGNETIC-FIELD; MASS EJECTIONS; STELLAR WINDS; EVOLUTION; DYNAMICS; MODELS; SUN; ROTATION; STABILITY AB The heating of the solar corona and therefore the generation of the solar wind, remain an active area of solar and heliophysics research. Several decades of in situ solar wind plasma observations have revealed a rich bimodal solar wind structure, well correlated with coronal magnetic field activity. Therefore, the reconnection processes associated with the large-scale dynamics of the corona likely play a major role in the generation of the slow solar wind flow regime. In order to elucidate the relationship between reconnection-driven coronal magnetic field structure and dynamics and the generation of the slow solar wind, this paper reviews the observations and phenomenology of the solar wind and coronal magnetic field structure. The geometry and topology of nested flux systems, and the (interchange) reconnection process, in the context of coronal physics is then explained. Once these foundations are laid out, the paper summarizes several fully dynamic, 3D MHD calculations of the global coronal system. Finally, the results of these calculations justify a number of important implications and conclusions on the role of reconnection in the structural dynamics of the coronal magnetic field and the generation of the solar wind. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Edmondson, JK (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,Mail Stop 169-506, Pasadena, CA 91109 USA. EM justin.k.edmondson@jpl.nasa.gov FU ISSI FX I would like to gratefully acknowledge S. K. Antiochos, C. R. DeVore, B.J. Lynch, and T. H. Zurbuchen for their involvement in the calculations (Edmondson et al. 2009, 2010a, 2010b) and subsequent discussions. In addition, I want to thank M. Velli, S. Lepri, and the two reviewers for their valuable insights and discussions regarding this paper. This review was supported in part by the ISSI workshop on the "Multi-scale physics in coronal heating and solar wind acceleration-from the Sun into the inner heliosphere", 25-29 January, 2010, as well as by an appointment to the NASA Postdoctoral Program at the Jet Propulsion Laboratory, California Institute of Technology, administered by Oak Ridge Associated Universities under a contract with the National Aeronautics and Space Administration. Copyright 2010 California Institute of Technology. Government sponsorship acknowledged. NR 61 TC 2 Z9 2 U1 2 U2 4 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-6308 J9 SPACE SCI REV JI Space Sci. Rev. PD NOV PY 2012 VL 172 IS 1-4 BP 209 EP 225 DI 10.1007/s11214-011-9767-y PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 034MJ UT WOS:000310877300014 ER PT J AU Matteini, L Hellinger, P Landi, S Travnicek, PM Velli, M AF Matteini, Lorenzo Hellinger, Petr Landi, Simone Travnicek, Pavel M. Velli, Marco TI Ion Kinetics in the Solar Wind: Coupling Global Expansion to Local Microphysics SO SPACE SCIENCE REVIEWS LA English DT Review DE Solar wind; Ion kinetics; Numerical simulations ID POLARIZED ALFVEN WAVES; ELECTROMAGNETIC PROTON/PROTON INSTABILITIES; PROTON TEMPERATURE ANISOTROPY; HYBRID SIMULATIONS; COULOMB COLLISIONS; VELOCITY DISTRIBUTIONS; PARAMETRIC DECAY; RADIAL EVOLUTION; CORONAL HOLES; FIRE HOSE AB We discuss selected ion kinetic processes relevant in the context of the expanding solar wind. We focus on the role of wave-wave and wave-particle interactions, plasma instabilities and Coulomb collisions on the overall kinetic evolution of ions. We review recent results from the hybrid expanding box model, which enables the coupling of the large scale effects of the solar wind expansion to the microscale kinetics of ions. We discuss how different plasma processes develop and influence each other during the expansion, as well their role in the shaping of ion distribution functions, and we compare the simulation results with the observed trends in the solar wind. C1 [Matteini, Lorenzo; Landi, Simone; Velli, Marco] Univ Florence, Dipartimento Fis & Astron, I-50125 Florence, Italy. [Hellinger, Petr; Travnicek, Pavel M.] AS CR, Astron Inst, Prague 14131, Czech Republic. [Hellinger, Petr; Travnicek, Pavel M.] AS CR, Inst Atmospher Phys, Prague 14131, Czech Republic. [Travnicek, Pavel M.] Univ Calif Berkeley, SSL, Berkeley, CA 94720 USA. [Velli, Marco] CALTECH, JPL, Pasadena, CA 91109 USA. RP Matteini, L (reprint author), Univ Florence, Dipartimento Fis & Astron, Largo Enrico Fermi 2, I-50125 Florence, Italy. EM matteini@arcetri.astro.it RI Hellinger, Petr/F-5267-2014; Travnicek, Pavel/G-8608-2014; Landi, Simone/G-7282-2015 OI Hellinger, Petr/0000-0002-5608-0834; Landi, Simone/0000-0002-1322-8712 FU Italian Space Agency [I/015/07/0]; PECS from European Space Agency [98068]; ISSI; Czech grant [GAAV IAA300420702] FX The research described in this paper was supported by the Italian Space Agency contract ASI No. I/015/07/0 "Solar System Exploration". It was also carried out in part at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. P. H. and P. M. T. acknowledge the Czech grant GAAV IAA300420702 and PECS contract No. 98068 from the European Space Agency. L. M., P. H. and S. L. thanks the ISSI staff for their kind hospitality and acknowledge ISSI financial support during the ISSI workshop on Coronal Heating and Solar Wind Acceleration. NR 97 TC 60 Z9 60 U1 2 U2 13 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 NOV PY 2012 VL 172 IS 1-4 BP 373 EP 396 DI 10.1007/s11214-011-9774-z PG 24 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 034MJ UT WOS:000310877300025 ER PT J AU Voytek, MA AF Voytek, Mary A. TI Where Will Curiosity Take Us? SO ASTROBIOLOGY LA English DT Editorial Material C1 NASA Headquarters, Washington, DC 20546 USA. RP Voytek, MA (reprint author), NASA Headquarters, Room 3Y56, Washington, DC 20546 USA. EM mary.voytek-1@nasa.gov NR 0 TC 0 Z9 0 U1 1 U2 4 PU MARY ANN LIEBERT INC PI NEW ROCHELLE PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA SN 1531-1074 J9 ASTROBIOLOGY JI Astrobiology PD NOV PY 2012 VL 12 IS 11 BP 1093 EP 1094 DI 10.1089/ast.2012.1022 PG 2 WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics; Geology GA 031NT UT WOS:000310649600009 PM 23121016 ER PT J AU Breger, M Fossati, L Balona, L Kurtz, DW Robertson, P Bohlender, D Lenz, P Mueller, I Lueftinger, T Clarke, BD Hall, JR Ibrahim, KA AF Breger, M. Fossati, L. Balona, L. Kurtz, D. W. Robertson, P. Bohlender, D. Lenz, P. Mueller, I. Lueftinger, Th. Clarke, Bruce D. Hall, Jennifer R. Ibrahim, Khadeejah A. TI RELATIONSHIP BETWEEN LOW AND HIGH FREQUENCIES IN delta SCUTI STARS: PHOTOMETRIC KEPLER AND SPECTROSCOPIC ANALYSES OF THE RAPID ROTATOR KIC 8054146 SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars: abundances; stars: individual (KIC 8054146); stars: oscillations; stars: rotation; stars: variables: delta Scuti ID LINE-DATA-BASE; A-TYPE STARS; PRAESEPE CLUSTER; TURBULENT CONVECTION; MODEL; ATMOSPHERES; ABUNDANCES AB Two years of Kepler data of KIC 8054146 (delta Sct/gamma Dor hybrid) revealed 349 statistically significant frequencies between 0.54 and 191.36 cycles day(-1) (6.3 mu Hz to 2.21 mHz). The 117 low frequencies cluster in specific frequency bands, but do not show the equidistant period spacings predicted for gravity modes of successive radial order, n, and reported for at least one other hybrid pulsator. The four dominant low frequencies in the 2.8-3.0 cycles day(-1) (32-35 mu Hz) range show strong amplitude variability with timescales of months and years. These four low frequencies also determine the spacing of the higher frequencies in and beyond the delta Sct pressure-mode frequency domain. In fact, most of the higher frequencies belong to one of three families with spacings linked to a specific dominant low frequency. In the Fourier spectrum, these family regularities show up as triplets, high-frequency sequences with absolutely equidistant frequency spacings, side lobes (amplitude modulations), and other regularities in frequency spacings. Furthermore, within two families the amplitude variations between the low and high frequencies are related. We conclude that the low frequencies (gravity modes, rotation) and observed high frequencies (mostly pressure modes) are physically connected. This unusual behavior may be related to the very rapid rotation of the star: from a combination of high-and low-resolution spectroscopy we determined that KIC 8054146 is a very fast rotator (upsilon sin i = 300 +/- 20 km s(-1)) with an effective temperature of 7600 +/- 200 K and a surface gravity log g of 3.9 +/- 0.3. Several astrophysical ideas explaining the origin of the relationship between the low and high frequencies are explored. C1 [Breger, M.; Robertson, P.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Breger, M.; Mueller, I.; Lueftinger, Th.] Univ Vienna, Inst Astronphys, A-1180 Vienna, Austria. [Fossati, L.] Open Univ, Dept Phys Sci, Milton Keynes MK7 6AA, Bucks, England. [Balona, L.] S African Astron Observ, ZA-7935 Cape Town, South Africa. [Kurtz, D. W.] Univ Cent Lancashire, Jeremiah Horrocks Inst, Preston PR1 2HE, Lancs, England. [Bohlender, D.] Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada. [Lenz, P.] Polish Acad Sci, N Copernicus Astron Ctr, PL-00716 Warsaw, Poland. [Clarke, Bruce D.] NASA, SETI Inst, Ames Res Ctr, Moffett Field, CA 94035 USA. [Hall, Jennifer R.; Ibrahim, Khadeejah A.] NASA, Orbital Sci Corp, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Breger, M (reprint author), Univ Texas Austin, Dept Astron, RLM 15308, Austin, TX 78712 USA. FU Austrian Fonds zur Forderung der wissenschaftlichen Forschung [P 21830-N16]; NASA's Science Mission Directorate FX M.B. is grateful to E. L. Robinson, K. Zwintz, and M. Montgomery for helpful discussions. This investigation has been supported by the Austrian Fonds zur Forderung der wissenschaftlichen Forschung through project P 21830-N16. The authors wish to thank the Kepler team for their generosity in allowing the data to be released to the Kepler Asteroseismic Science Consortium (KASC) ahead of public release and for their outstanding efforts which have made these results possible. Funding for the Kepler mission is provided by NASA's Science Mission Directorate. NR 26 TC 13 Z9 13 U1 0 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD NOV 1 PY 2012 VL 759 IS 1 AR 62 DI 10.1088/0004-637X/759/1/62 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 030JL UT WOS:000310566900062 ER PT J AU Debes, JH Hoard, DW Farihi, J Wachter, S Leisawitz, DT Cohen, M AF Debes, John H. Hoard, D. W. Farihi, Jay Wachter, Stefanie Leisawitz, David T. Cohen, Martin TI THE WIRED SURVEY. III. AN INFRARED EXCESS AROUND THE ECLIPSING POST-COMMON ENVELOPE BINARY SDSS J030308.35+005443.7 SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: eclipsing; circumstellar matter; white dwarfs ID DIGITAL-SKY-SURVEY; SPITZER-SPACE-TELESCOPE; MAIN-SEQUENCE BINARIES; WHITE-DWARF CATALOG; PLANETARY SYSTEMS; DUST; CALIBRATION; ACCRETION; STARS; I. AB We present the discovery with WISE of a significant infrared excess associated with the eclipsing post-common envelope binary SDSS J030308.35+005443.7, the first excess discovered around a non-interacting white dwarf+main-sequence M dwarf binary. The spectral energy distribution of the white dwarf+M dwarf companion shows significant excess longward of 3 mu m. A T-eff of 8940 K for the white dwarf is consistent with a cooling age >2 Gyr, implying that the excess may be due to a recently formed circumbinary dust disk of material that extends from the tidal truncation radius of the binary at 1.96 R-circle dot out to <0.8 AU, with a total mass of similar to 10(20) g. We also construct WISE and follow-up ground-based near-infrared light curves of the system and find variability in the K band that appears to be in phase with ellipsoidal variations observed in the visible. The presence of dust might be due to (1) material being generated by the destruction of small rocky bodies that are being perturbed by an unseen planetary system or (2) dust condensing from the companion's wind. The high inclination of this system and the presence of dust make it an attractive target for M dwarf transit surveys and long-term photometric monitoring. C1 [Debes, John H.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Hoard, D. W.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Farihi, Jay] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Wachter, Stefanie] CALTECH, IPAC, Pasadena, CA 91125 USA. [Leisawitz, David T.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Cohen, Martin] Monterey Inst Res Astron, Marina, CA 93933 USA. RP Debes, JH (reprint author), Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA. OI Hoard, Donald W./0000-0002-6800-6519; Farihi, Jay/0000-0003-1748-602X FU National Aeronautics and Space Administration (NASA); NASA; National Science Foundation; NASA [1000-S-MA756]; UCLA FAU [26311] FX This work is based on data obtained from: (1) the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory (JPL), California Institute of Technology (Caltech), funded by the National Aeronautics and Space Administration (NASA); (2) the Two Micron All Sky Survey (2MASS), a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center (IPAC)/Caltech, funded by NASA and the National Science Foundation; (3) the SIMBAD database, operated at CDS, Strasbourg, France; and (4) the NASA/IPAC Infrared Science Archive, which is operated by JPL, Caltech, under a contract with NASA. M. C. thanks NASA for supporting his participation in this work through UCLA Sub-Award 1000-S-MA756 with a UCLA FAU 26311 to MIRA. NR 33 TC 6 Z9 6 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD NOV 1 PY 2012 VL 759 IS 1 AR 37 DI 10.1088/0004-637X/759/1/37 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 030JL UT WOS:000310566900037 ER PT J AU Dominik, M Belczynski, K Fryer, C Holz, DE Berti, E Bulik, T Mandel, I O'Shaughnessy, R AF Dominik, Michal Belczynski, Krzysztof Fryer, Christopher Holz, Daniel E. Berti, Emanuele Bulik, Tomasz Mandel, Ilya O'Shaughnessy, Richard TI DOUBLE COMPACT OBJECTS. I. THE SIGNIFICANCE OF THE COMMON ENVELOPE ON MERGER RATES SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: general; black hole physics; stars: evolution; stars: neutron ID BLACK-HOLE BINARIES; GAMMA-RAY BURSTS; BINDING-ENERGY PARAMETER; MASSIVE CLOSE BINARIES; NEUTRON-STAR SYSTEMS; O-TYPE STARS; GLOBULAR-CLUSTERS; INSPIRALING BINARIES; EXPLOSION MECHANISM; GRAVITATIONAL-WAVES AB The last decade of observational and theoretical developments in stellar and binary evolution provides an opportunity to incorporate major improvements to the predictions from population synthesis models. We compute the Galactic merger rates for NS-NS, BH-NS, and BH-BH mergers with the StarTrack code. The most important revisions include updated wind mass-loss rates (allowing for stellar-mass black holes up to 80 M-circle dot), a realistic treatment of the common envelope phase (a process that can affect merger rates by 2-3 orders of magnitude), and a qualitatively new neutron star/black hole mass distribution (consistent with the observed "mass gap"). Our findings include the following. (1) The binding energy of the envelope plays a pivotal role in determining whether a binary merges within a Hubble time. (2) Our description of natal kicks from supernovae plays an important role, especially for the formation of BH-BH systems. (3) The masses of BH-BH systems can be substantially increased in the case of low metallicities or weak winds. (4) Certain combinations of parameters underpredict the Galactic NS-NS merger rate and can be ruled out. (5) Models incorporating delayed supernovae do not agree with the observed NS/BH "mass gap," in accordance with our previous work. This is the first in a series of three papers. The second paper will study the merger rates of double compact objects as a function of redshift, star formation rate, and metallicity. In the third paper, we will present the detection rates for gravitational-wave observatories, using up-to-date signal waveforms and sensitivity curves. C1 [Dominik, Michal; Belczynski, Krzysztof; Bulik, Tomasz] Univ Warsaw, Astron Observ, PL-00478 Warsaw, Poland. [Belczynski, Krzysztof] Univ Texas Brownsville, Ctr Gravitat Wave Astron, Brownsville, TX 78520 USA. [Holz, Daniel E.] Univ Chicago, Enrico Fermi Inst, Dept Phys, Chicago, IL 60637 USA. [Holz, Daniel E.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Holz, Daniel E.] Los Alamos Natl Lab, Div Theoret, Los Alamos, NM 87545 USA. [Berti, Emanuele] Univ Mississippi, Dept Phys & Astron, University, MS 38677 USA. [Berti, Emanuele] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Mandel, Ilya] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. [O'Shaughnessy, Richard] Univ Wisconsin, Ctr Gravitat & Cosmol, Milwaukee, WI 53211 USA. RP Dominik, M (reprint author), Univ Warsaw, Astron Observ, Al Ujazdowskie 4, PL-00478 Warsaw, Poland. RI Berti, Emanuele/C-9331-2016; OI Berti, Emanuele/0000-0003-0751-5130; O'Shaughnessy, Richard/0000-0001-5832-8517; Mandel, Ilya/0000-0002-6134-8946 FU National Nuclear Security Administration of the U.S. Department of Energy at Los Alamos National Laboratory [DE-AC52-06NA25396]; NSF [PHY-0900735, PHY-1055103, PHY-0970074]; Bradley Program Fellowship; UWM Research Growth Initiative; Polish grant [N N203 511238, DPN/N176/VIRGO/2009, N N203 302835, GR-4071] FX We thank Francesca Valsecchi for providing detailed calculations of specific mass transfer scenarios. We also thank the N. Copernicus Astronomical Centre in Warsaw, Poland, and the University of Texas at Brownsville, USA, for their courtesy in allowing us to use their computational resources. Work at LANL was done under the auspices of the National Nuclear Security Administration of the U.S. Department of Energy at Los Alamos National Laboratory under Contract No. DE-AC52-06NA25396. E.B. is supported by NSF grant PHY-0900735 and by NSF CAREER grant PHY-1055103. R.O.S. is currently supported by NSF award PHY-0970074, the Bradley Program Fellowship, and the UWM Research Growth Initiative. T.B. is supported by the Polish grants N N203 511238 and DPN/N176/VIRGO/2009. K.B. is supported by the Polish grant N N203 302835. M.D. is supported by the Polish grant GR-4071. NR 82 TC 148 Z9 148 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD NOV 1 PY 2012 VL 759 IS 1 AR 52 DI 10.1088/0004-637X/759/1/52 PG 28 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 030JL UT WOS:000310566900052 ER PT J AU Dragomir, D Matthews, JM Kuschnig, R Rowe, JF Gladman, BJ Guenther, DB Moffat, AFJ Rucinski, SM Sasselov, D Weiss, WW AF Dragomir, Diana Matthews, Jaymie M. Kuschnig, Rainer Rowe, Jason F. Gladman, Brett J. Guenther, David B. Moffat, Anthony F. J. Rucinski, Slavek M. Sasselov, Dimitar Weiss, Werner W. TI A SEARCH FOR TRANSITS OF GJ 581e AND CHARACTERIZATION OF THE HOST STAR VARIABILITY USING MOST SPACE TELESCOPE PHOTOMETRY SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems; stars: individual (GJ 581); techniques: photometric ID EXTRA-SOLAR PLANETS; M-CIRCLE-PLUS; SUPER-EARTHS; TRANSMISSION SPECTRUM; HABITABLE ZONE; TAU-BOOTIS; EXOPLANET SYSTEM; MAGNETIC CYCLES; HARPS SEARCH; LOW-MASS AB The GJ 581 system has been amply studied since its discovery in 2005: the number of known planets in the system has increased and their orbital parameters are among the most precisely determined for radial-velocity-detected exoplanets. We have acquired MOST space-based photometry during 2007 and 2009, with the aims of measuring the stellar variability and searching for transits of GJ 581e, respectively. We quantify our sensitivity to shallow transit signals using Monte Carlo simulations, and perform a transit search within the 3 sigma transit windows corresponding to both the circular and Keplerian orbit ephemerides. Our analysis rules out transits for a planet with an orbital period of 3.15 days (GJ 581e) having a radius larger than 1.62 R-circle plus (or a density lower than 2.39 g cm(-3) for an orbital inclination of 90 degrees) to 2 sigma confidence. Thus, if the planet transits, we can exclude hydrogen, helium, and water theoretical model compositions. The MOST photometry also allows us to rule out transits of GJ 581b within the Keplerian orbit-derived transit window for impact parameter values smaller than similar to 0.4 and confirm previous results which exclude transits for this planet within the circular orbit-derived transit window, for all plausible interior compositions. We find that the stellar brightness of GJ 581 is stable to within 1%, a characteristic which is favorable to the development of life in the habitable zone of the system. In the 2009 photometry, we detect a stellar signal with a period of 5.586 +/- 0.051 days, which is close to the orbital period of GJ 581b (P = 5.37 days). However, further monitoring of the system is necessary to verify the nature of this variation. C1 [Dragomir, Diana; Matthews, Jaymie M.; Gladman, Brett J.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. [Kuschnig, Rainer; Weiss, Werner W.] Univ Vienna, Inst Astron, A-1180 Vienna, Austria. [Rowe, Jason F.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Guenther, David B.] St Marys Univ, Dept Phys & Astron, Halifax, NS B3H 3C3, Canada. [Moffat, Anthony F. J.] Univ Montreal, Dept Phys & Obs Mt Megant, Montreal, PQ H3C 3J7, Canada. [Rucinski, Slavek M.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada. [Sasselov, Dimitar] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Dragomir, D (reprint author), Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. EM diana@phas.ubc.ca OI Dragomir, Diana/0000-0003-2313-467X FU University of British Columbia; Natural Sciences and Engineering Research Council of Canada; FQRNT (Qubec); Austrian Science Fund [P22691-N16]; Austrian Research Promotion Agency-ALR FX The authors thank Michael Gillon, Stephen Kane, and Bryce Croll for useful conversations. We are grateful to Xavier Bonfils and Thierry Forveille for providing additional information regarding their analysis of the GJ 581 system parameters. We also thank the anonymous referee for valuable comments and suggestions which have helped improve and clarify the manuscript. D.D. is supported by a University of British Columbia Four Year Fellowship. The Natural Sciences and Engineering Research Council of Canada supports the research of D.B.G., J.M.M., A.F.J.M., and S.M.R. Additional support for A.F.J.M. comes from FQRNT (Qubec). R.K. and W.W.W. were supported by the Austrian Science Fund (P22691-N16) and by the Austrian Research Promotion Agency-ALR. NR 48 TC 2 Z9 2 U1 0 U2 9 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD NOV 1 PY 2012 VL 759 IS 1 AR 2 DI 10.1088/0004-637X/759/1/2 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 030JL UT WOS:000310566900002 ER PT J AU Emslie, AG Dennis, BR Shih, AY Chamberlin, PC Mewaldt, RA Moore, CS Share, GH Vourlidas, A Welsch, BT AF Emslie, A. G. Dennis, B. R. Shih, A. Y. Chamberlin, P. C. Mewaldt, R. A. Moore, C. S. Share, G. H. Vourlidas, A. Welsch, B. T. TI GLOBAL ENERGETICS OF THIRTY-EIGHT LARGE SOLAR ERUPTIVE EVENTS SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun: activity; Sun: coronal mass ejections (CMEs); Sun: flares; Sun: particle emission; Sun: X-rays, gamma rays ID CORONAL MASS EJECTIONS; 20 JANUARY 2005; ADVANCED COMPOSITION EXPLORER; FREE FIELD EXTRAPOLATIONS; GROUND-LEVEL EVENTS; X-RAY IMAGER; FORCE-FREE; GAMMA-RAY; MAGNETIC-FIELDS; INTERPLANETARY MEDIUM AB We have evaluated the energetics of 38 solar eruptive events observed by a variety of spacecraft instruments between 2002 February and 2006 December, as accurately as the observations allow. The measured energetic components include: (1) the radiated energy in the Geostationary Operational Environmental Satellite 1-8 angstrom band, (2) the total energy radiated from the soft X-ray (SXR) emitting plasma, (3) the peak energy in the SXR-emitting plasma, (4) the bolometric radiated energy over the full duration of the event, (5) the energy in flare-accelerated electrons above 20 keV and in flare-accelerated ions above 1MeV, (6) the kinetic and potential energies of the coronal mass ejection (CME), (7) the energy in solar energetic particles (SEPs) observed in interplanetary space, and (8) the amount of free (non-potential) magnetic energy estimated to be available in the pertinent active region. Major conclusions include: (1) the energy radiated by the SXR-emitting plasma exceeds, by about half an order of magnitude, the peak energy content of the thermal plasma that produces this radiation; (2) the energy content in flare-accelerated electrons and ions is sufficient to supply the bolometric energy radiated across all wavelengths throughout the event; (3) the energy contents of flare-accelerated electrons and ions are comparable; (4) the energy in SEPs is typically a few percent of the CME kinetic energy (measured in the rest frame of the solar wind); and (5) the available magnetic energy is sufficient to power the CME, the flare-accelerated particles, and the hot thermal plasma. C1 [Emslie, A. G.] Western Kentucky Univ, Dept Phys & Astron, Bowling Green, KY 42101 USA. [Dennis, B. R.; Shih, A. Y.; Chamberlin, P. C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Mewaldt, R. A.] CALTECH, Space Radiat Lab, Pasadena, CA 91125 USA. [Moore, C. S.] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA. [Share, G. H.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Vourlidas, A.] USN, Res Lab, Washington, DC 20375 USA. [Welsch, B. T.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. RP Emslie, AG (reprint author), Western Kentucky Univ, Dept Phys & Astron, Bowling Green, KY 42101 USA. EM emslieg@wku.edu; brian.r.dennis@nasa.gov; albert.y.shih@nasa.gov; phillip.c.chamberlin@nasa.gov; rmewaldt@srl.caltech.edu; christopher.moore-1@colorado.edu; share@astro.umd.edu; vourlidas@nrl.navy.mil; welsch@ssl.berkeley.edu RI Chamberlin, Phillip/C-9531-2012; Vourlidas, Angelos/C-8231-2009 OI Chamberlin, Phillip/0000-0003-4372-7405; Vourlidas, Angelos/0000-0002-8164-5948 FU NASA [NNX10AT78J, NNX08AI11G, NNX11AO75G]; NASA FX We thank Gordon Holman, Richard Schwartz, and Kim Tolbert for help with analyzing the GOES and RHESSI data, and Anil Gopie for doing most of the GOES data analysis. We also thank the referee for an unusually comprehensive and thorough review of the originally submitted version of this manuscript, which resulted in a significantly improved paper. A.G.E. was supported by NASA Grant NNX10AT78J, R.A.M. by NASA Grants NNX08AI11G and NNX11AO75G, and A.V. by various NASA grants to the Naval Research Laboratory. SOHO is a joint ESA and NASA mission. CHIANTI is a collaborative project involving researchers at NRL (USA), RAL (UK), and the Universities of Cambridge (UK), George Mason (USA), and Florence (Italy). NR 97 TC 92 Z9 92 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 NOV 1 PY 2012 VL 759 IS 1 AR 71 DI 10.1088/0004-637X/759/1/71 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 030JL UT WOS:000310566900071 ER PT J AU Grav, T Mainzer, AK Bauer, JM Masiero, JR Nugent, CR AF Grav, T. Mainzer, A. K. Bauer, J. M. Masiero, J. R. Nugent, C. R. TI WISE/NEOWISE OBSERVATIONS OF THE JOVIAN TROJAN POPULATION: TAXONOMY SO ASTROPHYSICAL JOURNAL LA English DT Article DE infrared: planetary systems; minor planets, asteroids: general ID ASTEROID SPECTROSCOPIC SURVEY; THERMAL-MODEL CALIBRATION; INFRARED-SURVEY-EXPLORER; MAIN BELT ASTEROIDS; SOLAR-SYSTEM; DYNAMICAL FAMILIES; PHOTOMETRIC SURVEY; JUPITER TROJANS; MINOR PLANETS; IRREGULAR SATELLITES AB We present updated/new thermal model fits for 478 Jovian Trojan asteroids observed with the Wide-field Infrared Survey Explorer (WISE). Using the fact that the two shortest bands used by WISE, centered on 3.4 and 4.6 mu m, are dominated by reflected light, we derive albedos of a significant fraction of these objects in these bands. While the visible albedos of both the C-, P-, and D-type asteroids are strikingly similar, the WISE data reveal that the albedo at 3.4 mu m is different between C-/P- and D-types. The albedo at 3.4 mu m can thus be used to classify the objects, with C-/P-types having values less than 10% and D-types have values larger than 10%. Classifying all objects larger than 50 km shows that the D-type objects dominate both the leading cloud (L-4), with a fraction of 84%, and trailing cloud (L-5), with a fraction of 71%-80%. The two clouds thus have very similar taxonomic distribution for these large objects, but the leading cloud has a larger number of these large objects, L-4/L-5 = 1.34. The taxonomic distribution of the Jovian Trojans is found to be different from that of the large Hildas, which is dominated by C-and P-type objects. At smaller sizes, the fraction of D-type Hildas starts increasing, showing more similarities with the Jovian Trojans. If this similarity is confirmed through deeper surveys, it could hold important clues to the formation and evolution of the two populations. The Jovian Trojans does have similar taxonomic distribution to that of the Jovian irregular satellites, but lacks the ultra red surfaces found among the Saturnian irregular satellites and Centaur population. C1 [Grav, T.] Planetary Sci Inst, Tucson, AZ 85719 USA. [Mainzer, A. K.; Bauer, J. M.; Masiero, J. R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Nugent, C. R.] Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90095 USA. RP Grav, T (reprint author), Planetary Sci Inst, Tucson, AZ 85719 USA. EM tgrav@psi.edu OI Masiero, Joseph/0000-0003-2638-720X FU National Aeronautics and Space Administration; Planetary Science Division of the National Aeronautics and Space Administration FX This publication makes use of data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration. This publication also makes use of data products from NEOWISE, which is a project of the Jet Propulsion Laboratory/California Institute of Technology, funded by the Planetary Science Division of the National Aeronautics and Space Administration. We gratefully acknowledge the extraordinary services specific to NEOWISE contributed by the International Astronomical Union's Minor Planet Center, operated by the Harvard-Smithsonian Center for Astro-physics, and the Central Bureau for Astronomical Telegrams, operated by Harvard University. We also thank the worldwide community of dedicated amateur and professional astronomers devoted to minor planet follow-up observations. This research has made use the NASA/IPAC Infrared Science Archive, which is operated by the Jet Propulsion Laboratory/California Institute of Technology, under contract with the National Aeronautics and Space Administration. NR 58 TC 31 Z9 31 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 NOV 1 PY 2012 VL 759 IS 1 AR 49 DI 10.1088/0004-637X/759/1/49 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 030JL UT WOS:000310566900049 ER PT J AU Jia, JJ Ptak, A Heckman, TM Braito, V Reeves, J AF Jia, Jianjun Ptak, Andrew Heckman, Timothy M. Braito, Valentina Reeves, James TI A CHANDRA OBSERVATION OF THE ULTRALUMINOUS INFRARED GALAXY IRAS 19254-7245 (THE SUPERANTENNAE): X-RAY EMISSION FROM THE COMPTON-THICK ACTIVE GALACTIC NUCLEUS AND THE DIFFUSE STARBURST SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: individual (IRAS 19254-7245 (the Superantennae)); galaxies: starburst; X-rays: galaxies ID STAR-FORMING GALAXIES; LYMAN BREAK GALAXIES; FAR-ULTRAVIOLET; FEEDBACK; LINE; LUMINOSITY; MERGERS; SPECTROSCOPY; SUPERWINDS; ANALOG AB We present a Chandra observation of IRAS 19254-7245, a nearby ultraluminous infrared galaxy also known as the Superantennae. The high spatial resolution of Chandra allows us to disentangle for the first time the diffuse starburst (SB) emission from the embedded Compton-thick active galactic nucleus (AGN) in the southern nucleus. No AGN activity is detected in the northern nucleus. The 2-10 keV spectrum of the AGN emission is fitted by a flat power law (Gamma = 1.3) and an He-like Fe K alpha line with equivalent width similar to 1.5 keV, consistent with previous observations. The Fe K alpha line profile could be resolved as a blend of a neutral 6.4 keV line and an ionized 6.7 keV (He-like) or 6.9 keV (H-like) line. Variability of the neutral line is detected compared with the previous XMM-Newton and Suzaku observations, demonstrating the compact size of the iron line emission. The spectrum of the galaxy-scale extended emission excluding the AGN and other bright point sources is fitted with a thermal component with a best-fit kT of similar to 0.8 keV. The 2-10 keV luminosity of the extended emission is about one order of magnitude lower than that of the AGN. The basic physical and structural properties of the extended emission are fully consistent with a galactic wind being driven by the SB. A candidate ultraluminous X-ray source is detected 8 '' south of the southern nucleus. The 0.3-10 keV luminosity of this off-nuclear point source is similar to 6 x 10(40) erg s(-1) if the emission is isotropic and the source is associated with the Superantennae. C1 [Jia, Jianjun; Heckman, Timothy M.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Ptak, Andrew] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Braito, Valentina] INAF Osservatorio Astron Brera, I-20121 Milan, Italy. [Reeves, James] Univ Keele, Astrophys Grp, Sch Phys & Geog Sci, Keele ST5 5BG, Staffs, England. RP Jia, JJ (reprint author), Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. RI XRAY, SUZAKU/A-1808-2009; OI Braito, Valentina/0000-0002-2629-4989 FU Chandra grant [GO9-0091X] FX This work was supported by Chandra grant GO9-0091X. The authors thank the anonymous referee for helpful comments and suggestions. NR 51 TC 5 Z9 5 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD NOV 1 PY 2012 VL 759 IS 1 AR 41 DI 10.1088/0004-637X/759/1/41 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 030JL UT WOS:000310566900041 ER PT J AU Kanner, J Camp, J Racusin, J Gehrels, N White, D AF Kanner, Jonah Camp, Jordan Racusin, Judith Gehrels, Neil White, Darren TI SEEKING COUNTERPARTS TO ADVANCED LIGO/Virgo TRANSIENTS WITH SWIFT SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: statistics; gamma-ray burst: general; gravitational waves; X-rays: general ID GAMMA-RAY BURSTS; COMPACT OBJECT MERGERS; NEUTRON-STAR BINARIES; ALL-SKY SURVEY; ELECTROMAGNETIC COUNTERPARTS; LIGHT CURVES; SEARCH; TELESCOPE; RATES; FERMI AB Binary neutron star (NS) mergers are among the most promising astrophysical sources of gravitational wave (GW) emission for Advanced LIGO and Advanced Virgo, expected to be operational in 2015. Finding electromagnetic counterparts to these signals will be essential to placing them in an astronomical context. The Swift satellite carries a sensitive X-Ray Telescope (XRT), and can respond to target-of-opportunity requests within one to two hours, and so is uniquely poised to find the X-ray counterparts to LIGO/Virgo triggers. Assuming that NS mergers are the progenitors of short gamma-ray bursts (GRBs), some percentage of LIGO/Virgo triggers will be accompanied by X-ray band afterglows that are brighter than 10(-12) erg s(-1) cm(-2) in the XRT band one day after the trigger time. We find that a soft X-ray transient of this flux is bright enough to be extremely rare, and so could be confidently associated with even a moderately localized GW signal. We examine two possible search strategies with the Swift XRT to find bright transients in LIGO/Virgo error boxes. In the first strategy, XRT could search a volume of space with a similar to 100 Mpc radius by observing similar to 30 galaxies over the course of a day, with sufficient depth to observe the expected X-ray afterglow. For an extended LIGO/Virgo horizon distance, the XRT could employ 100 s exposures to cover an area of similar to 35 deg(2) in about a day and remain sensitive enough to image GW-discovered GRB afterglows. These strategies demonstrate that discovery of X-ray band counterparts to GW triggers will be possible, though challenging, with current facilities. C1 [Kanner, Jonah; Camp, Jordan; Racusin, Judith; Gehrels, Neil] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [White, Darren] Univ Sheffield, Dept Phys & Astron, Sheffield S3 7RH, S Yorkshire, England. RP Kanner, J (reprint author), NASA, Goddard Space Flight Ctr, Mail Code 663, Greenbelt, MD 20771 USA. EM jonah.b.kanner@nasa.gov RI Racusin, Judith/D-2935-2012; OI Kanner, Jonah/0000-0001-8115-0577 FU NASA Postdoctoral Program at Goddard Space Flight Center FX We are grateful for fruitful discussions and feedback from Lindy Blackburn, David Burrows, Thomas Dent, Brennan Hughey, Susan Kassin, Takanori Sakamoto, and Peter Shawhan. J.K. is supported by an appointment to the NASA Postdoctoral Program at Goddard Space Flight Center, administered by Oak Ridge Associated Universities through a contract with NASA. This work made use of data supplied by the UK Swift Science Data Centre at the University of Leicester and data obtained from the High Energy Astrophysics Science Archive Research Center (HEASARC), provided by NASA's Goddard Space Flight Center. NR 60 TC 23 Z9 23 U1 0 U2 12 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD NOV 1 PY 2012 VL 759 IS 1 AR 22 DI 10.1088/0004-637X/759/1/22 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 030JL UT WOS:000310566900022 ER PT J AU Masiero, JR Mainzer, AK Grav, T Bauer, JM Jedicke, R AF Masiero, Joseph R. Mainzer, A. K. Grav, T. Bauer, J. M. Jedicke, R. TI REVISING THE AGE FOR THE BAPTISTINA ASTEROID FAMILY USING WISE/NEOWISE DATA SO ASTROPHYSICAL JOURNAL LA English DT Article DE minor planets, asteroids: general ID MAIN-BELT ASTEROIDS; INFRARED-SURVEY-EXPLORER; SOLAR-SYSTEM; K/T IMPACTOR; YARKOVSKY; FRAGMENTS; EVOLUTION; CHRONOLOGY; PLANETS; NEOWISE AB We have used numerical routines to model the evolution of a simulated Baptistina family to constrain its age in light of new measurements of the diameters and albedos of family members from the Wide-field Infrared Survey Explorer. We also investigate the effect of varying the assumed physical and orbital parameters on the best-fitting age. We find that the physically allowed range of assumed values for the density and thermal conductivity induces a large uncertainty in the rate of evolution. When realistic uncertainties in the family members' physical parameters are taken into account, we find that the best-fitting age can fall anywhere in the range of 140-320 Myr. Without more information on the physical properties of the family members, it is difficult to place a more firm constraint on Baptistina's age. C1 [Masiero, Joseph R.; Mainzer, A. K.; Bauer, J. M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Grav, T.] Planetary Sci Inst, Tucson, AZ 85719 USA. [Bauer, J. M.] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA. [Jedicke, R.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. RP Masiero, JR (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,MS 321-520, Pasadena, CA 91109 USA. EM Joseph.Masiero@jpl.nasa.gov OI Masiero, Joseph/0000-0003-2638-720X FU NASA Postdoctoral Program at JPL; JPL Office of the Chief Information Officer; National Aeronautics and Space Administration; Planetary Science Division of the National Aeronautics and Space Administration FX We thank the referee, Bill Bottke, for his helpful and insightful comments that resulted in a critical reanalysis of the data, greatly improving our results and the manuscript in general. We also thank Bob McMillan for his editing of this manuscript. J.R.M. was supported by an appointment to the NASA Postdoctoral Program at JPL, administered by Oak Ridge Associated Universities through a contract with NASA. Computer simulations for this research were carried out on JPL's Zodiac supercomputer, which is administered by the JPL Supercomputing and Visualization Facility. The supercomputer used in this investigation was provided by funding from the JPL Office of the Chief Information Officer. This publication makes use of data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration. This publication also makes use of data products from NEOWISE, which is a project of the Jet Propulsion Laboratory/California Institute of Technology, funded by the Planetary Science Division of the National Aeronautics and Space Administration. This research has made use of the NASA/IPAC Infrared Science Archive, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. NR 42 TC 16 Z9 16 U1 0 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD NOV 1 PY 2012 VL 759 IS 1 AR 14 DI 10.1088/0004-637X/759/1/14 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 030JL UT WOS:000310566900014 ER PT J AU Pereira, TMD De Pontieu, B Carlsson, M AF Pereira, Tiago M. D. De Pontieu, Bart Carlsson, Mats TI QUANTIFYING SPICULES SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun: atmosphere; Sun: chromosphere; Sun: transition region ID HIGH-RESOLUTION OBSERVATIONS; SOLAR OPTICAL TELESCOPE; II SPICULES; MAGNETOACOUSTIC SHOCKS; MAGNETIC CHROMOSPHERE; DYNAMIC FIBRILS; HINODE; WAVES; SIMULATIONS; DRIVEN AB Understanding the dynamic solar chromosphere is fundamental in solar physics. Spicules are an important feature of the chromosphere, connecting the photosphere to the corona, potentially mediating the transfer of energy and mass. The aim of this work is to study the properties of spicules over different regions of the Sun. Our goal is to investigate if there is more than one type of spicule, and how spicules behave in the quiet Sun, coronal holes, and active regions. We make use of high cadence and high spatial resolution Ca II H observations taken by Hinode/Solar Optical Telescope. Making use of a semi-automated detection algorithm, we self-consistently track and measure the properties of 519 spicules over different regions. We find clear evidence of two types of spicules. Type I spicules show a rise and fall and have typical lifetimes of 150-400 s and maximum ascending velocities of 15-40 km s(-1), while type II spicules have shorter lifetimes of 50-150 s, faster velocities of 30-110 km s(-1), and are not seen to fall down, but rather fade at around their maximum length. Type II spicules are the most common, seen in the quiet Sun and coronal holes. Type I spicules are seen mostly in active regions. There are regional differences between quiet-Sun and coronal hole spicules, likely attributable to the different field configurations. The properties of type II spicules are consistent with published results of rapid blueshifted events (RBEs), supporting the hypothesis that RBEs are their disk counterparts. For type I spicules we find the relations between their properties to be consistent with a magnetoacoustic shock wave driver, and with dynamic fibrils as their disk counterpart. The driver of type II spicules remains unclear from limb observations. C1 [Pereira, Tiago M. D.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Pereira, Tiago M. D.; De Pontieu, Bart] Lockheed Martin Solar & Astrophys Lab, Palo Alto, CA 94304 USA. [Carlsson, Mats] Inst Theoret Astrophys, NO-0315 Oslo, Norway. [Carlsson, Mats] Univ Oslo, Ctr Math Applicat, NO-0316 Oslo, Norway. RP Pereira, TMD (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM tiago.pereira@nasa.gov RI Pereira, Tiago/G-4079-2014 OI Pereira, Tiago/0000-0003-4747-4329 FU NASA Postdoctoral Program at Ames Research Center [NNH06CC03B]; NASA [NNX08AH45G, NNX08BA99G, NNX11AN98G]; Research Council of Norway FX T.M.D.P.'s research was supported by the NASA Postdoctoral Program at Ames Research Center through Contract Number NNH06CC03B. B.D.P. gratefully acknowledges support by NASA grants NNX08AH45G, NNX08BA99G, and NNX11AN98G. This research was supported by the Research Council of Norway. Hinode is a Japanese mission developed by ISAS/JAXA, with the NAOJ as domestic partner and NASA and STFC (UK) as international partners. It is operated in cooperation with ESA and NSC (Norway). The authors thank Silje Bjolseth and Anne Fox for help with the data reduction and Alan Title, Rob Rutten, Luc Rouppe van der Voort, Viggo Hansteen, Scott McIntosh, and Ted Tarbell for interesting discussions. We thank the referee, whose comments were very helpful and improved the manuscript. NR 42 TC 44 Z9 45 U1 1 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 NOV 1 PY 2012 VL 759 IS 1 AR 18 DI 10.1088/0004-637X/759/1/18 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 030JL UT WOS:000310566900018 ER PT J AU Richey, CR Gerakines, PA AF Richey, C. R. Gerakines, P. A. TI NEAR-INFRARED BAND STRENGTHS OF MOLECULES DILUTED IN N-2 AND H2O ICE MIXTURES RELEVANT TO INTERSTELLAR AND PLANETARY ICES SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrochemistry; infrared: general; infrared: ISM; techniques: spectroscopic ID OUTER SOLAR-SYSTEM; LABORATORY SIMULATIONS; PHYSICAL STATE; WATER-ICE; CARBON-DIOXIDE; SOLID CH4; SURFACE; SPECTROSCOPY; CLOUDS; TRITON AB The relative abundances of ices in astrophysical environments rely on accurate laboratory measurements of physical parameters, such as band strengths (or absorption intensities), determined for the molecules of interest in relevant mixtures. In an extension of our previous study on pure-ice samples, here we focus on the near-infrared absorption features of molecules in mixtures with the dominant components of interstellar and planetary ices, H2O and N-2. We present experimentally measured near-infrared spectral information (peak positions, widths, and band strengths) for both H2O- and N-2-dominated mixtures of CO (carbon monoxide), CO2 (carbon dioxide), CH4 (methane), and NH3 (ammonia). Band strengths were determined during sample deposition by correlating the growth of near-infrared features (10,000-4000 cm(-1), 1-2.5 mu m) with better-known mid-infrared features (4000-400 cm(-1), 2.5-25 mu m) at longer wavelengths. C1 [Richey, C. R.; Gerakines, P. A.] Univ Alabama Birmingham, Astro & Solar Syst Phys Program, Dept Phys, Birmingham, AL 35294 USA. RP Richey, CR (reprint author), NASA, GSFC, Mail Code 665, Greenbelt, MD 20771 USA. EM christina.r.richey@nasa.gov; gerak@uab.edu RI Gerakines, Perry/D-2226-2012 OI Gerakines, Perry/0000-0002-9667-5904 FU National Aeronautics and Space Administration [NNG05GG95G]; U.S. Dept. of Education [P200A090143]; NASA Alabama Space Grant Consortium [NNG05GE80H] FX C.R.R. gratefully acknowledges support for this research from the National Aeronautics and Space Administration under Grant No. NNG05GG95G issued through the Outer Planets Research Program and the Graduate Assistance in Areas of National Need (GAANN) Fellowship (U.S. Dept. of Education Grant No. P200A090143), as well as in earlier years through the NASA Alabama Space Grant Consortium Fellowship through Grant No. NNG05GE80H. NR 46 TC 7 Z9 7 U1 1 U2 17 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD NOV 1 PY 2012 VL 759 IS 1 AR 74 DI 10.1088/0004-637X/759/1/74 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 030JL UT WOS:000310566900074 ER PT J AU Ackermann, M Ajello, M Albert, A Allafort, A Atwood, WB Axelsson, M Baldini, L Ballet, J Barbiellini, G Bastieri, D Bechtol, K Bellazzini, R Bissaldi, E Blandford, RD Bloom, ED Bogart, JR Bonamente, E Borgland, AW Bottacini, E Bouvier, A Brandt, TJ Bregeon, J Brigida, M Bruel, P Buehler, R Burnett, TH Buson, S Caliandro, GA Cameron, RA Caraveo, PA Casandjian, JM Cavazzuti, E Cecchi, C Celik, O Charles, E Chaves, RCG Chekhtman, A Cheung, CC Chiang, J Ciprini, S Claus, R Cohen-Tanugi, J Conrad, J Corbet, R Cutini, S D'Ammando, F Davis, DS de Angelis, A DeKlotz, M de Palma, F Dermer, CD Digel, SW Silva, EDE Drell, PS Drlica-Wagner, A Dubois, R Favuzzi, C Fegan, SJ Ferrara, EC Focke, WB Fortin, P Fukazawa, Y Funk, S Fusco, P Gargano, F Gasparrini, D Gehrels, N Giebels, B Giglietto, N Giordano, F Giroletti, M Glanzman, T Godfrey, G Grenier, IA Grove, JE Guiriec, S Hadasch, D Hayashida, M Hays, E Horan, D Hou, X Hughes, RE Jackson, MS Jogler, T Johannesson, G Johnson, RP Johnson, TJ Johnson, WN Kamae, T Katagiri, H Kataoka, J Kerr, M Knodlseder, J Kuss, M Lande, J Larsson, S Latronico, L Lavalley, C Lemoine-Goumard, M Longo, F Loparco, F Lott, B Lovellette, MN Lubrano, P Mazziotta, MN McConville, W McEnery, JE Mehault, J Michelson, PF Mitthumsiri, W Mizuno, T Moiseev, AA Monte, C Monzani, ME Morselli, A Moskalenko, IV Murgia, S Naumann-Godo, M Nemmen, R Nishino, S Norris, JP Nuss, E Ohno, M Ohsugi, T Okumura, A Omodei, N Orienti, M Orlando, E Ormes, JF Paneque, D Panetta, JH Perkins, JS Pesce-Rollins, M Pierbattista, M Piron, F Pivato, G Porter, TA Racusin, JL Raino, S Rando, R Razzano, M Razzaque, S Reimer, A Reimer, O Reposeur, T Reyes, LC Ritz, S Rochester, LS Romoli, C Roth, M Sadrozinski, HFW Sanchez, DA Parkinson, PMS Sbarra, C Scargle, JD Sgro, C Siegal-Gaskins, J Siskind, EJ Spandre, G Spinelli, P Stephens, TE Suson, DJ Tajima, H Takahashi, H Tanaka, T Thayer, JG Thayer, JB Thompson, DJ Tibaldo, L Tinivella, M Tosti, G Troja, E Usher, TL Vandenbroucke, J Van Klaveren, B Vasileiou, V Vianello, G Vitale, V Waite, AP Wallace, E Winer, BL Wood, DL Wood, KS Wood, M Yang, Z Zimmer, S AF Ackermann, M. Ajello, M. Albert, A. Allafort, A. Atwood, W. B. Axelsson, M. Baldini, L. Ballet, J. Barbiellini, G. Bastieri, D. Bechtol, K. Bellazzini, R. Bissaldi, E. Blandford, R. D. Bloom, E. D. Bogart, J. R. Bonamente, E. Borgland, A. W. Bottacini, E. Bouvier, A. Brandt, T. J. Bregeon, J. Brigida, M. Bruel, P. Buehler, R. Burnett, T. H. Buson, S. Caliandro, G. A. Cameron, R. A. Caraveo, P. A. Casandjian, J. M. Cavazzuti, E. Cecchi, C. Celik, O. Charles, E. Chaves, R. C. G. Chekhtman, A. Cheung, C. C. Chiang, J. Ciprini, S. Claus, R. Cohen-Tanugi, J. Conrad, J. Corbet, R. Cutini, S. D'Ammando, F. Davis, D. S. de Angelis, A. DeKlotz, M. de Palma, F. Dermer, C. D. Digel, S. W. do Couto e Silva, E. Drell, P. S. Drlica-Wagner, A. Dubois, R. Favuzzi, C. Fegan, S. J. Ferrara, E. C. Focke, W. B. Fortin, P. Fukazawa, Y. Funk, S. Fusco, P. Gargano, F. Gasparrini, D. Gehrels, N. Giebels, B. Giglietto, N. Giordano, F. Giroletti, M. Glanzman, T. Godfrey, G. Grenier, I. A. Grove, J. E. Guiriec, S. Hadasch, D. Hayashida, M. Hays, E. Horan, D. Hou, X. Hughes, R. E. Jackson, M. S. Jogler, T. Johannesson, G. Johnson, R. P. Johnson, T. J. Johnson, W. N. Kamae, T. Katagiri, H. Kataoka, J. Kerr, M. Knoedlseder, J. Kuss, M. Lande, J. Larsson, S. Latronico, L. Lavalley, C. Lemoine-Goumard, M. Longo, F. Loparco, F. Lott, B. Lovellette, M. N. Lubrano, P. Mazziotta, M. N. McConville, W. McEnery, J. E. Mehault, J. Michelson, P. F. Mitthumsiri, W. Mizuno, T. Moiseev, A. A. Monte, C. Monzani, M. E. Morselli, A. Moskalenko, I. V. Murgia, S. Naumann-Godo, M. Nemmen, R. Nishino, S. Norris, J. P. Nuss, E. Ohno, M. Ohsugi, T. Okumura, A. Omodei, N. Orienti, M. Orlando, E. Ormes, J. F. Paneque, D. Panetta, J. H. Perkins, J. S. Pesce-Rollins, M. Pierbattista, M. Piron, F. Pivato, G. Porter, T. A. Racusin, J. L. Raino, S. Rando, R. Razzano, M. Razzaque, S. Reimer, A. Reimer, O. Reposeur, T. Reyes, L. C. Ritz, S. Rochester, L. S. Romoli, C. Roth, M. Sadrozinski, H. F. -W. Sanchez, D. A. Parkinson, P. M. Saz Sbarra, C. Scargle, J. D. Sgro, C. Siegal-Gaskins, J. Siskind, E. J. Spandre, G. Spinelli, P. Stephens, T. E. Suson, D. J. Tajima, H. Takahashi, H. Tanaka, T. Thayer, J. G. Thayer, J. B. Thompson, D. J. Tibaldo, L. Tinivella, M. Tosti, G. Troja, E. Usher, T. L. Vandenbroucke, J. Van Klaveren, B. Vasileiou, V. Vianello, G. Vitale, V. Waite, A. P. Wallace, E. Winer, B. L. Wood, D. L. Wood, K. S. Wood, M. Yang, Z. Zimmer, S. TI THE FERMI LARGE AREA TELESCOPE ON ORBIT: EVENT CLASSIFICATION, INSTRUMENT RESPONSE FUNCTIONS, AND CALIBRATION SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE instrumentation: detectors; instrumentation: miscellaneous; methods: data analysis; methods: observational; telescopes ID GAMMA-RAY EMISSION; SPACE-TELESCOPE; LAT OBSERVATIONS; SOURCE CATALOG; VELA PULSAR; MISSION; TESTS; EGRET AB The Fermi Large Area Telescope (Fermi-LAT, hereafter LAT), the primary instrument on the Fermi Gamma-ray Space Telescope (Fermi) mission, is an imaging, wide field-of-view, high-energy gamma-ray telescope, covering the energy range from 20 MeV to more than 300 GeV. During the first years of the mission, the LAT team has gained considerable insight into the in-flight performance of the instrument. Accordingly, we have updated the analysis used to reduce LAT data for public release as well as the instrument response functions (IRFs), the description of the instrument performance provided for data analysis. In this paper, we describe the effects that motivated these updates. Furthermore, we discuss how we originally derived IRFs from Monte Carlo simulations and later corrected those IRFs for discrepancies observed between flight and simulated data. We also give details of the validations performed using flight data and quantify the residual uncertainties in the IRFs. Finally, we describe techniques the LAT team has developed to propagate those uncertainties into estimates of the systematic errors on common measurements such as fluxes and spectra of astrophysical sources. C1 [Ackermann, M.] Deutsch Elektronen Synchrotron DESY, D-15738 Zeuthen, Germany. [Ajello, M.; Allafort, A.; Bechtol, K.; Blandford, R. D.; Bloom, E. D.; Bogart, J. R.; Borgland, A. W.; Bottacini, E.; Buehler, R.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; Digel, S. W.; do Couto e Silva, E.; Drell, P. S.; Drlica-Wagner, A.; Dubois, R.; Focke, W. B.; Funk, S.; Glanzman, T.; Godfrey, G.; Hayashida, M.; Jogler, T.; Kamae, T.; Kerr, M.; Lande, J.; Michelson, P. F.; Mitthumsiri, W.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Okumura, A.; Omodei, N.; Orlando, E.; Paneque, D.; Panetta, J. H.; Porter, T. A.; Reimer, A.; Reimer, O.; Rochester, L. S.; Tajima, H.; Tanaka, T.; Thayer, J. G.; Thayer, J. B.; Usher, T. L.; Vandenbroucke, J.; Van Klaveren, B.; Vianello, G.; Waite, A. P.; Wood, M.] Stanford Univ, WW Hansen Expt Phys Lab, Kavli Inst Particle Astrophys & Cosmol, Dept Phys, Stanford, CA 94305 USA. [Ajello, M.; Allafort, A.; Bechtol, K.; Blandford, R. D.; Bloom, E. D.; Bogart, J. R.; Borgland, A. W.; Bottacini, E.; Buehler, R.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; Digel, S. W.; do Couto e Silva, E.; Drell, P. S.; Drlica-Wagner, A.; Dubois, R.; Focke, W. B.; Funk, S.; Glanzman, T.; Godfrey, G.; Hayashida, M.; Jogler, T.; Kamae, T.; Kerr, M.; Lande, J.; Michelson, P. F.; Mitthumsiri, W.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Okumura, A.; Omodei, N.; Orlando, E.; Paneque, D.; Panetta, J. H.; Porter, T. A.; Reimer, A.; Reimer, O.; Rochester, L. S.; Tajima, H.; Tanaka, T.; Thayer, J. G.; Thayer, J. B.; Usher, T. L.; Vandenbroucke, J.; Van Klaveren, B.; Vianello, G.; Waite, A. P.; Wood, M.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA. [Albert, A.; Hughes, R. E.; Winer, B. L.] Ohio State Univ, Dept Phys, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA. [Atwood, W. B.; Bouvier, A.; Johnson, R. P.; Razzano, M.; Ritz, S.; Sadrozinski, H. F. -W.; Parkinson, P. M. Saz] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Dept Phys, Santa Cruz, CA 95064 USA. [Atwood, W. B.; Bouvier, A.; Johnson, R. P.; Razzano, M.; Ritz, S.; Sadrozinski, H. F. -W.; Parkinson, P. M. Saz] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Axelsson, M.; Larsson, S.] Stockholm Univ, Dept Astron, SE-10691 Stockholm, Sweden. [Axelsson, M.; Conrad, J.; Jackson, M. S.; Larsson, S.; Yang, Z.; Zimmer, S.] AlbaNova, Oskar Klein Ctr Cosmoparticle Phys, SE-10691 Stockholm, Sweden. [Axelsson, M.; Jackson, M. S.] AlbaNova, Dept Phys, Royal Inst Technol KTH, SE-10691 Stockholm, Sweden. [Baldini, L.] Univ Pisa, I-56127 Pisa, Italy. [Baldini, L.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy. [Ballet, J.; Casandjian, J. M.; Chaves, R. C. G.; Grenier, I. A.; Naumann-Godo, M.; Pierbattista, M.] Univ Paris Diderot, Lab AIM, CNRS, CEA,IRFU,Serv Astrophys,CEA Saclay, 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.; Sbarra, C.; Tibaldo, L.] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy. [Bastieri, D.; Buson, S.; Pivato, G.; Rando, R.; Romoli, C.; Tibaldo, L.] Univ Padua, Dipartimento Fis & Astron G Galilei, I-35131 Padua, Italy. [Bellazzini, R.; Bregeon, J.; Kuss, M.; Pesce-Rollins, M.; Razzano, M.; Sgro, C.; Spandre, G.; Tinivella, M.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy. [Bissaldi, E.; Reimer, A.; Reimer, O.] Leopold Franzens Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria. [Bissaldi, E.; Reimer, A.; Reimer, O.] Leopold Franzens Univ Innsbruck, Inst Theoret Phys, A-6020 Innsbruck, Austria. [Bonamente, E.; Cecchi, C.; D'Ammando, F.; Lubrano, P.; Tosti, G.] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy. [Bonamente, E.; Cecchi, C.; Ciprini, S.; Lubrano, P.; Tosti, G.] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy. [Brandt, T. J.; Celik, O.; Corbet, R.; Davis, D. S.; Ferrara, E. C.; Gehrels, N.; Guiriec, S.; Hays, E.; McConville, W.; McEnery, J. E.; Moiseev, A. A.; Nemmen, R.; Perkins, J. S.; Racusin, J. L.; Stephens, T. E.; Thompson, D. J.; Troja, E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Brigida, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Giordano, F.; Loparco, F.; Monte, C.; Raino, S.; Spinelli, P.] Univ Bari, Dipartimento Fis M Merlin, I-70126 Bari, Italy. [Brigida, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Giordano, F.; Loparco, F.; Monte, C.; Raino, S.; Spinelli, P.] Politecn Bari, I-70126 Bari, Italy. [Brigida, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Gargano, F.; Giglietto, N.; Giordano, F.; Loparco, F.; Mazziotta, M. N.; Monte, C.; Raino, S.; Spinelli, P.] Ist Nazl Fis Nucl, Sez Bari, I-70126 Bari, Italy. [Bruel, P.; Fegan, S. J.; Fortin, P.; Giebels, B.; Horan, D.] Ecole Polytech, CNRS, IN2P3, Lab Leprince Ringuet, F-91128 Palaiseau, France. [Burnett, T. H.; Roth, M.; Wallace, E.] Univ Washington, Dept Phys, Seattle, WA 98195 USA. [Caliandro, G. A.; Hadasch, D.] CSIC, Inst Ciencies Espai IEEE, E-08193 Barcelona, Spain. [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-00044 Frascati, Roma, Italy. [Celik, O.; Moiseev, A. A.; Perkins, J. S.] CRESST, Greenbelt, MD 20771 USA. [Celik, O.; Corbet, R.; Davis, D. S.; Perkins, J. S.] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA. [Celik, O.; Corbet, R.; Davis, D. S.; Perkins, J. S.] Univ Maryland Baltimore Cty, Ctr Space Sci & Technol, Baltimore, MD 21250 USA. [Chekhtman, A.; Razzaque, S.] George Mason Univ, Coll Sci, Ctr Earth Observing & Space Res, Fairfax, VA 22030 USA. [Cheung, C. C.; Johnson, T. J.] Natl Acad Sci, Washington, DC 20001 USA. [Cohen-Tanugi, J.; Lavalley, C.; Mehault, J.; Nuss, E.; Piron, F.; Vasileiou, V.] Univ Montpellier 2, CNRS, IN2P3, Lab Univers & Particules Montpellier, F-34095 Montpellier, France. [Conrad, J.; Larsson, S.; Yang, Z.; Zimmer, S.] Stockholm Univ, AlbaNova, Dept Phys, SE-10691 Stockholm, Sweden. [D'Ammando, F.] IASF Palermo, I-90146 Palermo, Italy. [D'Ammando, F.] INAF Ist Astrofis Spaziale & Fis Cosm, I-00133 Rome, Italy. [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. [DeKlotz, M.] Stellar Solut Inc, Palo Alto, CA 94306 USA. [Dermer, C. D.; Grove, J. E.; Johnson, W. N.; Lovellette, M. N.; Wood, K. S.] USN, Div Space Sci, Res Lab, Washington, DC 20375 USA. [Fukazawa, Y.; Nishino, S.; Takahashi, H.] Hiroshima Univ, Dept Phys Sci, Hiroshima 7398526, Japan. [Giroletti, M.; Orienti, M.] INAF Ist Radioastron, I-40129 Bologna, Italy. [Hayashida, M.] Kyoto Univ, Grad Sch Sci, Dept Astron, Sakyo Ku, Kyoto 6068502, Japan. [Hou, X.; Lemoine-Goumard, M.; Lott, B.; Reposeur, T.] Univ Bordeaux 1, Ctr Etud Nucl Bordeaux Gradignan, IN2P3, CNRS, F-33175 Gradignan, France. [Johannesson, G.] Univ Iceland, Inst Sci, IS-107 Reykjavik, Iceland. [Katagiri, H.] Ibaraki Univ, Coll Sci, Mito, Ibaraki 3108512, Japan. [Kataoka, J.] Waseda Univ, Res Inst Sci & Engn, Shinjuku Ku, Tokyo 1698555, Japan. [Knoedlseder, J.] IRAP, CNRS, F-31028 Toulouse 4, France. [Knoedlseder, J.] Univ Toulouse, GAHEC, UPS OMP, IRAP, F-31028 Toulouse, France. [Latronico, L.] Ist Nazl Fis Nucl, Sez Torino, I-10125 Turin, Italy. [McConville, W.; McEnery, J. E.; Moiseev, A. A.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA. [McConville, W.; McEnery, J. E.; Moiseev, A. A.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Mizuno, T.; Ohsugi, T.] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Hiroshima 7398526, Japan. [Morselli, A.; Vitale, V.] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, I-00133 Rome, Italy. [Norris, J. P.] Boise State Univ, Dept Phys, Boise, ID 83725 USA. [Ohno, M.] JAXA, Inst Space & Astronaut Sci, Chuo Ku, Sagamihara, Kanagawa 2525210, Japan. [Okumura, A.; Tajima, H.] Nagoya Univ, Solar Terr Environm Lab, Nagoya, Aichi 4648601, Japan. [Ormes, J. F.] Univ Denver, Dept Phys & Astron, Denver, CO 80208 USA. [Paneque, D.] Max Planck Inst Phys & Astrophys, D-80805 Munich, Germany. [Perkins, J. S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Reyes, L. C.] Calif Polytech State Univ San Luis Obispo, Dept Phys, San Luis Obispo, CA 93401 USA. [Sanchez, D. A.] Max Planck Inst Kernphys, D-69029 Heidelberg, Germany. [Scargle, J. D.] NASA, Div Space Sci, Ames Res Ctr, Moffett Field, CA 94035 USA. [Siegal-Gaskins, J.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Siskind, E. J.] NYCB Real Time Comp Inc, Lattingtown, NY 11560 USA. [Stephens, T. E.] Wyle Labs, El Segundo, CA 90245 USA. [Suson, D. J.] Purdue Univ Calumet, Dept Chem & Phys, Hammond, IN 46323 USA. [Vianello, G.] CIFS, I-10133 Turin, Italy. [Vitale, V.] Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy. [Wood, D. L.] Praxis Inc, Alexandria, VA 22303 USA. RP Ackermann, M (reprint author), Deutsch Elektronen Synchrotron DESY, D-15738 Zeuthen, Germany. EM luca.baldini@pi.infn.it; echarles@slac.stanford.edu; rando@pd.infn.it RI Moskalenko, Igor/A-1301-2007; Mazziotta, Mario /O-8867-2015; Sgro, Carmelo/K-3395-2016; Bissaldi, Elisabetta/K-7911-2016; Orlando, E/R-5594-2016; Reimer, Olaf/A-3117-2013; Racusin, Judith/D-2935-2012; Loparco, Francesco/O-8847-2015; Gargano, Fabio/O-8934-2015; giglietto, nicola/I-8951-2012; Tosti, Gino/E-9976-2013; Saz Parkinson, Pablo Miguel/I-7980-2013; Rando, Riccardo/M-7179-2013; Hays, Elizabeth/D-3257-2012; Johnson, Neil/G-3309-2014; Nemmen, Rodrigo/O-6841-2014; Funk, Stefan/B-7629-2015; Johannesson, Gudlaugur/O-8741-2015; OI Moskalenko, Igor/0000-0001-6141-458X; Mazziotta, Mario /0000-0001-9325-4672; Bissaldi, Elisabetta/0000-0001-9935-8106; De Angelis, Alessandro/0000-0002-3288-2517; Caraveo, Patrizia/0000-0003-2478-8018; Stephens, Thomas/0000-0003-3065-6871; Sgro', Carmelo/0000-0001-5676-6214; SPINELLI, Paolo/0000-0001-6688-8864; Rando, Riccardo/0000-0001-6992-818X; Zimmer, Stephan/0000-0002-5735-0082; Bastieri, Denis/0000-0002-6954-8862; Omodei, Nicola/0000-0002-5448-7577; Reimer, Olaf/0000-0001-6953-1385; Loparco, Francesco/0000-0002-1173-5673; Gargano, Fabio/0000-0002-5055-6395; giglietto, nicola/0000-0002-9021-2888; Funk, Stefan/0000-0002-2012-0080; Johannesson, Gudlaugur/0000-0003-1458-7036; Pesce-Rollins, Melissa/0000-0003-1790-8018; orienti, monica/0000-0003-4470-7094; Axelsson, Magnus/0000-0003-4378-8785; Giroletti, Marcello/0000-0002-8657-8852; Cutini, Sara/0000-0002-1271-2924; Gasparrini, Dario/0000-0002-5064-9495; Baldini, Luca/0000-0002-9785-7726 FU K. A. Wallenberg Foundation; European Community [ERC-StG-259391]; Commonwealth Government FX Royal Swedish Academy of Sciences Research Fellow, funded by a grant from the K. A. Wallenberg Foundation.; Funded by contract ERC-StG-259391 from the European Community.; The Parkes radio telescope is part of the Australia Telescope, which is funded by the Commonwealth Government for operation as a National Facility managed by CSIRO. We thank our colleagues for their assistance with the radio timing observations. NR 52 TC 215 Z9 215 U1 5 U2 23 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD NOV PY 2012 VL 203 IS 1 AR 4 DI 10.1088/0067-0049/203/1/4 PG 70 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 034YH UT WOS:000310908300004 ER PT J AU Donato, D Angelini, L Padgett, CA Reichard, T Gehrels, N Marshall, FE Sakamoto, T AF Donato, D. Angelini, L. Padgett, C. A. Reichard, T. Gehrels, N. Marshall, F. E. Sakamoto, T. TI THE HEASARC Swift GAMMA-RAY BURST ARCHIVE: THE PIPELINE AND THE CATALOG SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE catalogs; methods: data analysis; X-rays: bursts ID ULTRAVIOLET/OPTICAL TELESCOPE; AFTERGLOW; CALIBRATION; MISSION; BAT AB Since its launch in late 2004, the Swift satellite triggered or observed an average of one gamma-ray burst (GRB) every 3 days, for a total of 771 GRBs by 2012 January. Here, we report the development of a pipeline that semiautomatically performs the data-reduction and data-analysis processes for the three instruments on board Swift (BAT, XRT, UVOT). The pipeline is written in Perl, and it uses only HEAsoft tools and can be used to perform the analysis of a majority of the point-like objects (e.g., GRBs, active galactic nuclei, pulsars) observed by Swift. We run the pipeline on the GRBs, and we present a database containing the screened data, the output products, and the results of our ongoing analysis. Furthermore, we created a catalog summarizing some GRB information, collected either by running the pipeline or from the literature. The Perl script, the database, and the catalog are available for downloading and querying at the HEASARC Web site. C1 [Donato, D.; Sakamoto, T.] CRESST, Greenbelt, MD 20771 USA. [Donato, D.; Angelini, L.; Gehrels, N.; Marshall, F. E.; Sakamoto, T.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Donato, D.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA. [Donato, D.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Padgett, C. A.] RS Informat Syst Inc, Mclean, VA 22102 USA. [Reichard, T.] ADNET Syst Inc, Rockville, MD 20852 USA. [Sakamoto, T.] Univ Maryland Baltimore Cty, Joint Ctr Astrophys, Baltimore, MD 21250 USA. RP Donato, D (reprint author), CRESST, Greenbelt, MD 20771 USA. EM davide.donato-1@nasa.gov NR 22 TC 4 Z9 4 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD NOV PY 2012 VL 203 IS 1 AR 2 DI 10.1088/0067-0049/203/1/2 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 034YH UT WOS:000310908300002 ER PT J AU Goldsmith, PF Langer, WD Pineda, JL Velusamy, T AF Goldsmith, Paul F. Langer, William D. Pineda, Jorge L. Velusamy, T. TI COLLISIONAL EXCITATION OF THE [C II] FINE STRUCTURE TRANSITION IN INTERSTELLAR CLOUDS SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE atomic processes; photon-dominated region (PDR); submillimeter: ISM ID 158 MU-M; FAR-INFRARED SPECTROSCOPY; STAR-FORMATION; MOLECULAR CLOUDS; IONIZED CARBON; GROUND-STATE; HETERODYNE INSTRUMENT; CII EMISSION; LINE SURVEY; HERSCHEL AB We analyze the collisional excitation of the 158 mu m (1900.5 GHz) fine structure transition of ionized carbon in terms of line intensities produced by simple cloud models. The single C+ fine structure transition is a very important coolant of the atomic interstellar medium (ISM) and of photon-dominated regions in which carbon is partially or completely in ionized form. The [C II] line is widely used as a tracer of star formation in the Milky Way and other galaxies. Excitation of the [C II] fine structure transition can be via collisions with hydrogen molecules, atoms, and electrons. Analysis of [C II] observations is complicated by the fact that it is difficult to determine the optical depth of the line. We discuss the excitation of the [C II] line, deriving analytic results for several limiting cases and carry out numerical solutions using a large velocity gradient model for a more inclusive analysis. For antenna temperatures up to 1/3 of the brightness temperature of the gas kinetic temperature, the antenna temperature is linearly proportional to the column density of C+ irrespective of the optical depth of the transition. This is appropriately referred to as the effectively optically thin approximation. We review the critical densities for excitation of the [C II] line by various collision partners, briefly analyze C+ absorption, and conclude with a discussion of C+ cooling and how the considerations for line intensities affect the behavior of this important coolant of the ISM. C1 [Goldsmith, Paul F.; Langer, William D.; Pineda, Jorge L.; Velusamy, T.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Goldsmith, PF (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Paul.F.Goldsmith@jpl.nasa.gov RI Goldsmith, Paul/H-3159-2016 FU National Aeronautics and Space Administration FX This work was largely carried out at the Jet Propulsion Laboratory, which is operated by the California Institute of Technology under contract with the National Aeronautics and Space Administration. It was supported by a Senior Research Scientist leave from JPL in conjunction with a stay as Professeur Invite at the Ecole Normale Superieure, Paris, both of which are gratefully acknowledged. We thank Maryvonne Gerin for allowing us to use PRISMAS data prior to publication and for extensive discussions about [C II] absorption, and Edith Falgarone for interesting discussions about the ISM and the role of ionized carbon. We greatly appreciate a critical reading of the manuscript by David Neufeld that led to clearing up a significant problem with an earlier version of Figure 1. NR 50 TC 38 Z9 38 U1 1 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD NOV PY 2012 VL 203 IS 1 AR 13 DI 10.1088/0067-0049/203/1/13 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 034YH UT WOS:000310908300013 ER PT J AU Contreras, CS Sahai, R AF Sanchez Contreras, C. Sahai, R. TI OPACOS: OVRO POST-AGB CO (1-0) EMISSION SURVEY. I. DATA AND DERIVED NEBULAR PARAMETERS SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE circumstellar matter; ISM: jets and outflows; planetary nebulae: general; stars: AGB and post-AGB; stars: mass-loss ID ASYMPTOTIC GIANT BRANCH; MASS-LOSS RATES; RICH CIRCUMSTELLAR ENVELOPES; YOUNG PLANETARY-NEBULAE; MORPHOLOGICAL CLASSIFICATION-SYSTEM; TELESCOPE SNAPSHOT SURVEY; EXTREME CARBON STARS; POINT-SOURCE CATALOG; PROTOPLANETARY NEBULA; OH/IR STARS AB We have performed interferometric observations of the (CO)-C-12 (J = 1-0) emission in a sample of 27 objects spanning different evolutionary stages from the late asymptotic giant branch (late-AGB), through the post-AGB (pAGB) phase, and to the planetary nebula (PN) stage, but dominated by pAGB objects and young PNs (>= 81%). In this paper (the first in a series) we present our maps and main nebular properties derived for the whole sample. Observations were performed with the Caltech Millimeter Array at the Owens Valley Radio Observatory. The angular resolution obtained in our survey ranges between 2 ''.3 and 10 ''.7. The (CO)-C-13 and (CO)-O-18 (J = 1-0) transitions as well as the 2.6 mm continuum emission have also been observed in several objects. The detection statistics in the (CO)-C-12, (CO)-C-13, (CO)-O-18 transitions and 2.6 mm continuum are 89%, 83%, 0%, and 37%, respectively. We report first detections of (CO)-C-12 (J = 1-0) emission in 13 targets and confirm emission from several previous marginal detections. The molecular envelope probed by (CO)-C-12 (J = 1-0) emission is extended for 18 (out of 24) sources; envelope asymmetries and/or velocity gradients are found in most extended objects. Our data have been used to derive accurate target coordinates and systemic velocities and to characterize the envelope size, morphology, and kinematics. We also provide an estimate of the total molecular mass and the fraction of it contained in fast flows, lower limits to the linear momentum and to the isotopic C-12/C-13 ratio, as well as the AGB mass-loss rate and timescale for sources with extended CO emission. C1 [Sanchez Contreras, C.] INTA CSIC, Ctr Astrobiol, E-28691 Madrid, Spain. [Sahai, R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Contreras, CS (reprint author), ESAC, POB 78, E-28691 Madrid, Spain. RI Sanchez-Contreras, Carmen/N-3718-2015 OI Sanchez-Contreras, Carmen/0000-0002-6341-592X FU Spanish MICINN [AYA2009-07304]; Spanish MICINN through CONSOLIDER INGENIO for the team "Molecular Astrophysics: The Herschel and Alma Era - ASTROMOL" [CSD2009-00038]; Spanish MEC [PIE 200750I028]; National Science Foundation [AST 08-38260]; NASA [NMO710651/399-20-40-06, 399-20-40-08]; HST/GO awards from the Space Telescope Science Institute [GO-09463.01, 09801.01, 10185.01, 10851.01]; Association of Universities for Research in Astronomy, under NASA [NAS5-26555] FX We thank the anonymous referees for their helpful comments and suggestions. This work has been partially performed at the Astrophysics Department of the Astrobiology Center (CAB, CSIC/INTA) and the California Institute of Technology and has been partially supported by the Spanish MICINN through grants AYA2009-07304 and CONSOLIDER INGENIO 2010 for the team "Molecular Astrophysics: The Herschel and Alma Era - ASTROMOL" (ref.: CSD2009-00038), and by the Spanish MEC under project PIE 200750I028. Ongoing development and operations for OVRO and CARMA are supported by the National Science Foundation under a cooperative agreement (grant AST 08-38260). R.S.'s contribution to the research described here was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contact with NASA. R.S. thanks NASA for partially funding this work by NASA LTSA and ADP awards (nos. NMO710651/399-20-40-06 and 399-20-40-08); R.S. also received partial support for this work from HST/GO awards (nos. GO-09463.01, 09801.01, 10185.01, and 10851.01) from the Space Telescope Science Institute (operated by the Association of Universities for Research in Astronomy, under NASA contract NAS5-26555). This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France, the NASA's Astrophysics Data System, and Aladin. This research has made use of observations with AKARI, a JAXA project with the participation of ESA. NR 166 TC 7 Z9 7 U1 3 U2 8 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 EI 1538-4365 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD NOV PY 2012 VL 203 IS 1 AR 16 DI 10.1088/0067-0049/203/1/16 PG 33 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 034YH UT WOS:000310908300016 ER PT J AU Vivian, U Sanders, DB Mazzarella, JM Evans, AS Howell, JH Surace, JA Armus, L Iwasawa, K Kim, DC Casey, CM Vavilkin, T Dufault, M Larson, KL Barnes, JE Chan, BHP Frayer, DT Haan, S Inami, H Ishida, CM Kartaltepe, JS Melbourne, JL Petric, AO AF Vivian, U. Sanders, D. B. Mazzarella, J. M. Evans, A. S. Howell, J. H. Surace, J. A. Armus, L. Iwasawa, K. Kim, D. -C. Casey, C. M. Vavilkin, T. Dufault, M. Larson, K. L. Barnes, J. E. Chan, B. H. P. Frayer, D. T. Haan, S. Inami, H. Ishida, C. M. Kartaltepe, J. S. Melbourne, J. L. Petric, A. O. TI SPECTRAL ENERGY DISTRIBUTIONS OF LOCAL LUMINOUS AND ULTRALUMINOUS INFRARED GALAXIES SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE galaxies: active; galaxies: interactions; galaxies: photometry; infrared: galaxies ID ACTIVE GALACTIC NUCLEI; SKY LIRG SURVEY; STAR-FORMATION; STARBURST GALAXIES; GHZ ATLAS; DUST; SAMPLE; STELLAR; ULTRAVIOLET; RESOLUTION AB Luminous (LIRGs; log (L-IR/L-circle dot) = 11.00-11.99) and ultraluminous infrared galaxies (ULIRGs; log (L-IR/L-circle dot) = 12.00-12.99) are the most extreme star-forming galaxies in the universe. The local (U)LIRGs provide a unique opportunity to study their multi-wavelength properties in detail for comparison with their more numerous counterparts at high redshifts. We present common large aperture photometry at radio through X-ray wavelengths and spectral energy distributions (SEDs) for a sample of 53 nearby (z < 0.083) LIRGs and 11 ULIRGs spanning log (L-IR/L-circle dot) = 11.14-12.57 from the flux-limited (f(60 mu m) > 5.24 Jy) Great Observatories All-sky LIRG Survey. The SEDs for all objects are similar in that they show a broad, thermal stellar peak (similar to 0.3-2 mu m), and a dominant FIR (similar to 40-200 mu m) thermal dust peak, where vL(v) (60 mu m)/vL(v) (V) increases from similar to 2 to 30 with increasing L-IR. When normalized at IRAS 60 mu m, the largest range in the luminosity ratio, R(lambda) = log[vL(v)(lambda)/vL(v) (60 mu m)], observed over the full sample is seen in the hard X-rays (HX = 2-10 keV), where Delta R-HX = 3.73 ((R) over bar (HX) = -3.10). A small range is found in the radio (1.4 GHz), Delta R-1.4 GHz = 1.75, where the mean ratio is largest, ((R) over bar (1.4 GHz) = -5.81). Total infrared luminosities, L-IR(8-1000 mu m), dust temperatures, and dust masses were computed from fitting thermal dust emission modified blackbodies to the mid-infrared (MIR) through submillimeter SEDs. The new results reflect an overall similar to 0.02 dex lower luminosity than the original IRAS values. Total stellar masses were computed by fitting stellar population synthesis models to the observed near-infrared (NIR) through ultraviolet (UV) SEDs. Mean stellar masses are found to be log(M-*/M-circle dot) = 10.79 +/- 0.40. Star formation rates have been determined from the infrared (SFRIR similar to 45M(circle dot) yr(-1)) and from the monochromatic UV luminosities (SFRUV similar to 1.3M(circle dot) yr(-1)), respectively. Multi-wavelength active galactic nucleus (AGN) indicators have be used to select putative AGNs: About 60% of the ULIRGs would have been classified as an AGN by at least one of the selection criteria. C1 [Vivian, U.; Sanders, D. B.; Casey, C. M.; Larson, K. L.; Barnes, J. E.; Ishida, C. M.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Vivian, U.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Mazzarella, J. M.; Howell, J. H.; Chan, B. H. P.] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA. [Evans, A. S.; Kim, D. -C.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. [Evans, A. S.; Kim, D. -C.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. [Howell, J. H.; Surace, J. A.; Armus, L.; Petric, A. O.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Iwasawa, K.] Univ Barcelona IEEC UB, ICREA, E-08028 Barcelona, Spain. [Iwasawa, K.] Univ Barcelona IEEC UB, Inst Ciencies Cosmos, E-08028 Barcelona, Spain. [Vavilkin, T.] SUNY Stony Brook, Dept Phys & Astron, Stony Brook, NY 11794 USA. [Dufault, M.] Yale Univ, Dept Astron, New Haven, CT 06511 USA. [Frayer, D. T.] Natl Radio Astron Observ, Green Bank, WV 24944 USA. [Haan, S.] CSIRO Astron & Space Sci, Marsfield, NSW 2122, Australia. [Inami, H.; Kartaltepe, J. S.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Melbourne, J. L.] CALTECH, Caltech Opt Observ, Div Phys Math & Astron, Pasadena, CA 91125 USA. RP Vivian, U (reprint author), NASA, Washington, DC 20546 USA. EM vivian@ifa.hawaii.edu OI Mazzarella, Joseph/0000-0002-8204-8619; Casey, Caitlin/0000-0002-0930-6466 FU National Aeronautics and Space Administration; National Science Foundation; NASA; JPL Contract/IRAC GTO Grant [1256790]; Giovanni Fazio via the Smithsonian Astrophysical Observatory Predoctoral Fellowship FX V. U. thanks O. Ilbert and S. Arnouts for their help with using the Le PHARE code, C. J. Ma for his help with UH 2.2 m data acquisition and reduction, T.-T. Yuan for her help with various scientific and technical contributions, and C. W. K. Chiang for statistical consult and technical help with Figures 1 and 3. V. U. also extends appreciation toward the UH TAC for their generous support of this project in awarding telescope time on Mauna Kea, as well as Colin Aspin and the UH 2.2 m Telescope staff for their help and support in the acquisition of the ground-based optical photometry. This research has made use of the NASA/IPAC Extragalactic Database (NED) and IPAC Infrared Science Archive, which are operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. This publication has also made use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. V. U. wishes to acknowledge funding support from the NASA Harriet G. Jenkins Predoctoral Fellowship Project and Giovanni Fazio via the Smithsonian Astrophysical Observatory Predoctoral Fellowship and JPL Contract/IRAC GTO Grant 1256790. This paper is dedicated to the memory of Michele Dufault, who led the effort to obtain accurate large aperature photometric optical and near-infrared data for our complete sample of objects, and whose early work was critical in our decision to publish this paper. NR 52 TC 5 Z9 5 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD NOV PY 2012 VL 203 IS 1 AR 9 DI 10.1088/0067-0049/203/1/9 PG 27 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 034YH UT WOS:000310908300009 ER PT J AU Zavodsky, BT Chou, SH Jedlovec, GJ AF Zavodsky, Bradley T. Chou, Shih-Hung Jedlovec, Gary J. TI Improved Regional Analyses and Heavy Precipitation Forecasts With Assimilation of Atmospheric Infrared Sounder Retrieved Thermodynamic Profiles SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE Atmosphere; hyperspectral sensors; meteorology; remote sensing; weather forecasting ID ANALYSIS SYSTEM; AIRS/AMSU/HSB; RADIANCES; MISSION; AIRS; AQUA AB This paper describes a procedure to assimilate Atmospheric Infrared Sounder (AIRS)-retrieved thermodynamic profiles into a regional configuration of the Weather Research and Forecasting (WRF) model and validates subsequent precipitation forecasts over the eastern half of the continental U. S. Quality indicators were used to select the highest quality temperature and moisture profiles for assimilation throughout the entire atmosphere in clear and partly cloudy regions and above cloud top in cloudy regions. Separate error characteristics for land and water profiles were also used in the assimilation process. Assimilation of AIRS profiles produced analyses with a better validation to in situ observations than the short-term WRF forecast first-guess field. The AIRS-enhanced initial conditions improved simulation of a severe weather event over Texas and Louisiana from February 12-13, 2007. For this event, assimilation of AIRS profiles produced a more unstable boundary-layer air mass in the warm sector ahead of an advancing midlatitude cyclone, resulting in enhanced convective available potential energy in the model. The simulated squall line and precipitation totals from a forecast initialized with AIRS-enhanced initial conditions more closely reflected ground-based observations than one initialized with a no-AIRS control forecast. The impact of the improved initial conditions through the assimilation of AIRS profiles was further demonstrated through an evaluation of a 37-day period from the winter of 2007. The unstable environment over the Gulf of Mexico and coastal region with the AIRS-enhanced initial conditions resulted in 20%+ improvements in the 6-h accumulated precipitation forecasts out to 48 h over that period. C1 [Zavodsky, Bradley T.; Chou, Shih-Hung; Jedlovec, Gary J.] NASA, Marshall Space Flight Ctr, Huntsville, AL 35805 USA. RP Zavodsky, BT (reprint author), NASA, Marshall Space Flight Ctr, Huntsville, AL 35805 USA. EM brad.zavodsky@nasa.gov; shih.h.chou@nasa.gov; gary.jedlovec@nasa.gov NR 29 TC 5 Z9 6 U1 0 U2 11 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0196-2892 EI 1558-0644 J9 IEEE T GEOSCI REMOTE JI IEEE Trans. Geosci. Remote Sensing PD NOV PY 2012 VL 50 IS 11 BP 4243 EP 4251 DI 10.1109/TGRS.2012.2194158 PN 1 PG 9 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA 034QM UT WOS:000310888000002 ER PT J AU Tilton, JC Tarabalka, Y Montesano, PM Gofman, E AF Tilton, James C. Tarabalka, Yuliya Montesano, Paul M. Gofman, Emanuel TI Best Merge Region-Growing Segmentation With Integrated Nonadjacent Region Object Aggregation SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE Image analysis; image classification; image region analysis; image segmentation; object detection ID IMAGE SEGMENTATION; CLASSIFICATION; SYSTEM AB Best merge region growing normally produces segmentations with closed connected region objects. Recognizing that spectrally similar objects often appear in spatially separate locations, we present an approach for tightly integrating best merge region growing with nonadjacent region object aggregation, which we call hierarchical segmentation or HSeg. However, the original implementation of nonadjacent region object aggregation in HSeg required excessive computing time even for moderately sized images because of the required intercomparison of each region with all other regions. This problem was previously addressed by a recursive approximation of HSeg, called RHSeg. In this paper, we introduce a refined implementation of nonadjacent region object aggregation in HSeg that reduces the computational requirements of HSeg without resorting to the recursive approximation. In this refinement, HSeg's region intercomparisons among nonadjacent regions are limited to regions of a dynamically determined minimum size. We show that this refined version of HSeg can process moderately sized images in about the same amount of time as RHSeg incorporating the original HSeg. Nonetheless, RHSeg is still required for processing very large images due to its lower computer memory requirements and amenability to parallel processing. We then note a limitation of RHSeg with the original HSeg for high spatial resolution images and show how incorporating the refined HSeg into RHSeg overcomes this limitation. The quality of the image segmentations produced by the refined HSeg is then compared with other available best merge segmentation approaches. Finally, we comment on the unique nature of the hierarchical segmentations produced by HSeg. C1 [Tilton, James C.; Tarabalka, Yuliya] NASA, Goddard Space Flight Ctr, Computat & Informat Sci & Technol Off, Greenbelt, MD 20771 USA. [Montesano, Paul M.] Sigma Space Corp, Lanham, MD 20706 USA. [Montesano, Paul M.] NASA, Goddard Space Flight Ctr, Biospher Sci Branch, Greenbelt, MD 20771 USA. [Gofman, Emanuel] IBM Haifa Res Labs, IL-31905 Haifa, Israel. RP Tilton, JC (reprint author), NASA, Goddard Space Flight Ctr, Computat & Informat Sci & Technol Off, Greenbelt, MD 20771 USA. EM James.C.Tilton@nasa.gov; yuliya.tarabalka@inria.fr; Paul.M.Montesano@nasa.gov; gofman@il.ibm.com FU U.S. National Aeronautics and Space Administration (NASA); Internal Research and Development program at NASA's Goddard Space Flight Center; Marie Curie Research Training Network "Hyper-I-Net" FX This work was supported in part by the Applied Information Systems Research program of the U.S. National Aeronautics and Space Administration (NASA), by the Internal Research and Development program at NASA's Goddard Space Flight Center, and by the Marie Curie Research Training Network "Hyper-I-Net." NR 35 TC 46 Z9 51 U1 1 U2 21 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0196-2892 EI 1558-0644 J9 IEEE T GEOSCI REMOTE JI IEEE Trans. Geosci. Remote Sensing PD NOV PY 2012 VL 50 IS 11 BP 4454 EP 4467 DI 10.1109/TGRS.2012.2190079 PN 1 PG 14 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA 034QM UT WOS:000310888000019 ER PT J AU Misra, S De Roo, RD Ruf, CS AF Misra, Sidharth De Roo, Roger D. Ruf, Christopher S. TI An Improved Radio Frequency Interference Model: Reevaluation of the Kurtosis Detection Algorithm Performance Under Central-Limit Conditions SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE Central limit; microwave radiometry; radio frequency interference (RFI) ID RADIOFREQUENCY INTERFERENCE; L-BAND; MICROWAVE RADIOMETERS; RFI DETECTION; MITIGATION; OCEAN; LAND AB Recent airborne field campaigns making passive microwave measurements have observed some radio frequency interference (RFI) that remained undetected by the kurtosis RFI-detection algorithm. The current pulsed-sinusoidal model for RFI does not explain this anomalous behavior of the detection algorithm. In this paper, a new RFI model is developed that takes into account multiple RFI sources within an antenna footprint. The performance of the kurtosis algorithm with the new model is evaluated. The behavior of the kurtosis detection algorithm under central-limit conditions due to multiple sources is experimentally verified. The new RFI model offers a plausible explanation for the lack of detection by the kurtosis algorithm of the RFI otherwise observed. C1 [Misra, Sidharth] CALTECH, Jet Prop Lab, Microwave Syst Technol Grp, Pasadena, CA 91109 USA. [De Roo, Roger D.; Ruf, Christopher S.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. [Ruf, Christopher S.] Univ Michigan, Space Phys Res Lab, Ann Arbor, MI 48109 USA. RP Misra, S (reprint author), CALTECH, Jet Prop Lab, Microwave Syst Technol Grp, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM sidharth.misra@jpl.nasa.gov; deroo@umich.edu; cruf@umich.edu RI De Roo, Roger/J-2208-2012; Ruf, Christopher/I-9463-2012 OI De Roo, Roger/0000-0001-8391-2950; FU National Aeronautics and Space Administration (NASA) under the NASA Earth and Space Science Fellowship [NNX08AU76H] FX This work was supported in part by the National Aeronautics and Space Administration (NASA) under the NASA Earth and Space Science Fellowship (NNX08AU76H). NR 31 TC 1 Z9 1 U1 0 U2 8 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0196-2892 J9 IEEE T GEOSCI REMOTE JI IEEE Trans. Geosci. Remote Sensing PD NOV PY 2012 VL 50 IS 11 BP 4565 EP 4574 DI 10.1109/TGRS.2012.2191972 PN 2 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 034QS UT WOS:000310888600002 ER PT J AU Brasunas, JC AF Brasunas, John C. TI Laser mode behavior of the Cassini CIRS Fourier transform spectrometer at Saturn SO INFRARED PHYSICS & TECHNOLOGY LA English DT Article DE Fourier transform spectrometer; Wavelength calibration; Laser mode; Mylar ID INFRARED SPECTROMETER; SYSTEM AB The CIRS Fourier transform spectrometer aboard the NASA/ESA/ASI Cassini orbiter has been acquiring spectra of the Saturnian system since 2004. The CIRS reference interferometer employs a laser diode to trigger the interferogram sampling. Although the control of laser diode drive current and operating temperature are stringent enough to restrict laser wavelength variation to a small fraction of CIRS finest resolution element, the CIRS instrument does need to be restarted every year or two, at which time it may start in a new laser mode. By monitoring the Mylar absorption features in un-calibrated spectra due to the beam splitter Mylar substrate, it can be shown that these jumps are to adjacent modes and that most of the 8-year operation so far is restricted to three adjacent modes. For a given mode, the wavelength stability appears consistent with the stability of the laser diode drive current and operating temperature. Published by Elsevier B.V. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Brasunas, JC (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM john.c.brasunas@nasa.gov RI brasunas, john/I-2798-2013 FU NASA's Cassini mission; Cassini CIRS calibration team FX The author acknowledges support from NASA's Cassini mission and from the Cassini CIRS calibration team. NR 3 TC 1 Z9 1 U1 2 U2 4 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 1350-4495 J9 INFRARED PHYS TECHN JI Infrared Phys. Technol. PD NOV PY 2012 VL 55 IS 6 BP 533 EP 537 DI 10.1016/j.infrared.2012.07.003 PG 5 WC Instruments & Instrumentation; Optics; Physics, Applied SC Instruments & Instrumentation; Optics; Physics GA 036JZ UT WOS:000311023500014 ER PT J AU Bringi, VN Huang, GJ Munchak, SJ Kummerow, CD Marks, DA Wolff, DB AF Bringi, V. N. Huang, Gwo-Jong Munchak, S. Joseph Kummerow, Christian D. Marks, David A. Wolff, David B. TI Comparison of Drop Size Distribution Parameter (D-0) and Rain Rate from S-Band Dual-Polarized Ground Radar, TRMM Precipitation Radar (PR), and Combined PR TMI: Two Events from Kwajalein Atoll SO JOURNAL OF ATMOSPHERIC AND OCEANIC TECHNOLOGY LA English DT Article ID PROFILING ALGORITHM; POLARIMETRIC RADAR; SPACEBORNE RADAR; GAUGE DATA; VALIDATION; SATELLITE; SPECTRA; DISDROMETER; RETRIEVAL; CLOUDS AB The estimation of the drop size distribution parameter [median volume diameter (D-0)] and rain rate (R) from the Tropical Rainfall Measuring Mission (TRMM) precipitation radar (PR) as well as from combined PR TRMM Microwave Imager (TMI) algorithms are considered in this study for two TRMM satellite overpasses near the Kwajalein Atoll. An operational dual-polarized S-band radar (KPOL) located in Kwajalein is central as the only TRMM ground validation site for measurement of precipitation over the open ocean. The accuracy of the TRMM PR in retrieving D-0 and R is better for precipitation over the ocean based on a more stable surface reference technique for estimating the path-integrated attenuation. Also, combined PR TMI methods are more accurate over the open ocean because of better knowledge of the surface microwave emissivity. Using Z(h) (horizontal polarized radar reflectivity) and Z(dr) (differential reflectivity) data for the two TRMM overpass events over Kwajalein, Do and R from KPOL arc retrieved. Herein, the main objective is to see if the D-0 retrieved from either PR or the combined PR TMI algorithms are in agreement with KPOL-derived values. Also, the variation of D-0 versus R is compared for convective rain pixels from KPOL, PR, and PR-TMI. It is shown that the PR-TMI optimal estimation scheme does indeed adjust the D-0 in the "correct" direction, on average, from the a priori state if the KPOL data are considered to be the ground truth. This correct adjustment may be considered as evidence of the value added by the TMI brightness temperatures in the combined PR-TMI variational scheme, at least for the two overpass events considered herein. C1 [Bringi, V. N.; Huang, Gwo-Jong] Colorado State Univ, Dept Elect & Comp Engn, Ft Collins, CO 80523 USA. [Munchak, S. Joseph] Univ Maryland, NASA, GSFC, Greenbelt & Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. [Kummerow, Christian D.] Colorado State Univ, Dept Atmospher Sci, Ft Collins, CO 80523 USA. [Marks, David A.; Wolff, David B.] NASA, GSFC, Greenbelt & Sci Syst Applicat Inc, Lanham, MD USA. RP Bringi, VN (reprint author), Colorado State Univ, Dept Elect & Comp Engn, Ft Collins, CO 80523 USA. EM bringi@engr.colostate.edu FU NASA PMM Science Grant [NNX10AG74G]; NASA Headquarters; NASA [NNG06HX18C] FX VNB and GJH were supported by the NASA PMM Science Grant NNX10AG74G. Development and use of the MK algorithm was supported by NASA Headquarters through the NASA Earth and Space Science Fellowship Program under Dr. Ming-Ying Wei and the Global Precipitation Science Program under Dr. Ramesh Kakar. DBW and DAM were supported by Drs. Arthur Hou and Matt Schwaller (TRMM Ground Validation) under NASA Grant NNG06HX18C. The Joss disdrometer data were provided by Dr. Ali Tokay of the University of Maryland, Baltimore County. NR 50 TC 3 Z9 3 U1 1 U2 11 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0739-0572 J9 J ATMOS OCEAN TECH JI J. Atmos. Ocean. Technol. PD NOV PY 2012 VL 29 IS 11 BP 1603 EP 1616 DI 10.1175/JTECH-D-11-00153.1 PG 14 WC Engineering, Ocean; Meteorology & Atmospheric Sciences SC Engineering; Meteorology & Atmospheric Sciences GA 036WZ UT WOS:000311064300002 ER PT J AU Wu, XB Yan, XH Jo, YH Liu, WT AF Wu, Xiangbai Yan, Xiao-Hai Jo, Young-Heon Liu, W. Timothy TI Estimation of Subsurface Temperature Anomaly in the North Atlantic Using a Self-Organizing Map Neural Network SO JOURNAL OF ATMOSPHERIC AND OCEANIC TECHNOLOGY LA English DT Article ID MIXED-LAYER DEPTH; MULTIDECADAL OSCILLATION; MEDITERRANEAN OUTFLOW; THERMAL STRUCTURE; ANALYTICAL MODEL; SEA; VARIABILITY; WATER; ARGO AB A self-organizing map (SOM) neural network was developed from Argo gridded datasets in order to estimate a subsurface temperature anomaly (STA) from remote sensing data. The SOM maps were trained using anomalies of sea surface temperature (SST), height (SSH), and salinity (SSS) data from Argo gridded monthly anomaly datasets, labeled with Argo STA data from 2005 through 2010, which were then used to estimate the STAs at different depths in the North Atlantic from the sea surface data. The estimated STA maps and time series were compared with Argo STAs including independent datasets for validation. In the Gulf Stream path areas, the STA estimations from the SOM algorithm show good agreement with in situ measurements taken from the surface down to 700-m depth, with a correlation coefficient larger than 0.8. Sensitivity of the SUM, when including salinity, shows that with SSS anomaly data in the SOM training process reveal the importance of SSS information, which can improve the estimation of STA in the subtropical ocean by up to 30%. In subpolar basins, the monthly climatology SST and SSH can also help to improve the estimation by as much as 40%. The STA time series for 1993-2004 in the midlatitude North Atlantic were estimated from remote sensing SST and altimetry time series using the SOM algorithm. Limitations for the SUM algorithm and possible error sources in the estimation are briefly discussed. C1 [Yan, Xiao-Hai] Univ Delaware, Coll Earth Ocean & Environm, Ctr Remote Sensing, Newark, DE 19716 USA. [Wu, Xiangbai; Yan, Xiao-Hai; Jo, Young-Heon] Univ Delaware, Joint Inst Coastal Res & Management, Newark, DE 19716 USA. [Wu, Xiangbai; Yan, Xiao-Hai] Xiamen Univ, State Key Lab Marine Environm Sci, Xiamen, Peoples R China. [Liu, W. Timothy] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Yan, XH (reprint author), Univ Delaware, Coll Earth Ocean & Environm, Ctr Remote Sensing, 209 Robinson Hall, Newark, DE 19716 USA. EM xiaohai@udel.edu FU NASA Physical Oceanography Program; NASA EPSCoR Program; NASA Space Grant; NOAA Sea Grant FX This research was partially supported by the NASA Physical Oceanography Program, NASA EPSCoR Program, NASA Space Grant, and NOAA Sea Grant. The authors thank Weiwei Zhang and Feili Li for the help in data analysis. We also thank Federico Ienna for editorial assistance with the English language. Argo gridded data used in this study provided by IPRC, University of Hawaii. NOAA_OI_SST_V2 data provided by the NOAA/OAR/ESRL PSD, Boulder, Colorado, from their website at http://www.esrl.noaa.gov/psd/. The altimeter products (MSLA data) were produced by Ssalto/Duacs and distributed by AVISO with support from CNES. We thank two anonymous reviewers whose comments have helped improve the manuscript. NR 38 TC 6 Z9 6 U1 0 U2 11 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0739-0572 J9 J ATMOS OCEAN TECH JI J. Atmos. Ocean. Technol. PD NOV PY 2012 VL 29 IS 11 BP 1675 EP 1688 DI 10.1175/JTECH-D-12-00013.1 PG 14 WC Engineering, Ocean; Meteorology & Atmospheric Sciences SC Engineering; Meteorology & Atmospheric Sciences GA 036WZ UT WOS:000311064300008 ER PT J AU Hirata, A Fujishima, K Yamagami, R Kawamura, T Banfield, JF Kanai, A Hori, H AF Hirata, Akira Fujishima, Kosuke Yamagami, Ryota Kawamura, Takuya Banfield, Jillian F. Kanai, Akio Hori, Hiroyuki TI X-ray structure of the fourth type of archaeal tRNA splicing endonuclease: insights into the evolution of a novel three-unit composition and a unique loop involved in broad substrate specificity SO NUCLEIC ACIDS RESEARCH LA English DT Article ID NANOARCHAEUM-EQUITANS; ORDER THERMOPROTEALES; INTRON; RECOGNITION; GENES; MOTIFS; SITE; CONSERVATION; ULTRASMALL; SOFTWARE AB Cleavage of introns from precursor transfer RNAs (tRNAs) by tRNA splicing endonuclease (EndA) is essential for tRNA maturation in Archaea and Eukarya. In the past, archaeal EndAs were classified into three types (alpha'(2), alpha(4) and alpha(2)beta(2)) according to subunit composition. Recently, we have identified a fourth type of archaeal EndA from an uncultivated archaeon Candidatus Micrarchaeum acidiphilum, referred to as ARMAN-2, which is deeply branched within Euryarchaea. The ARMAN-2 EndA forms an epsilon(2) homodimer and has broad substrate specificity like the alpha(2)beta(2) type EndAs found in Crenarchaea and Nanoarchaea. However, the precise architecture of ARMAN-2 EndA was unknown. Here, we report the crystal structure of the epsilon(2) homodimer of ARMAN-2 EndA. The structure reveals that the epsilon protomer is separated into three novel units (alpha(N), alpha and beta(C)) fused by two distinct linkers, although the overall structure of ARMAN-2 EndA is similar to those of the other three types of archaeal EndAs. Structural comparison and mutational analyses reveal that an ARMAN-2 type-specific loop (ASL) is involved in the broad substrate specificity and that K161 in the ASL functions as the RNA recognition site. These findings suggest that the broad substrate specificities of epsilon(2) and alpha(2)beta(2) EndAs were separately acquired through different evolutionary processes. C1 [Hirata, Akira; Yamagami, Ryota; Kawamura, Takuya; Hori, Hiroyuki] Ehime Univ, Grad Sch Sci & Engn, Dept Mat Sci & Biotechnol, Matsuyama, Ehime 7908577, Japan. [Fujishima, Kosuke; Kanai, Akio] Keio Univ, Inst Adv Biosci, Tsuruoka, Yamagata 9970017, Japan. [Fujishima, Kosuke] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Banfield, Jillian F.] Univ Calif Berkeley, Dept Earth & Planetary Sci, Berkeley, CA 94270 USA. [Hori, Hiroyuki] Ehime Univ, Venture Business Lab, Matsuyama, Ehime 7908577, Japan. RP Hori, H (reprint author), Ehime Univ, Grad Sch Sci & Engn, Dept Mat Sci & Biotechnol, 3 Bunkyo Cho, Matsuyama, Ehime 7908577, Japan. EM hori@eng.ehime-u.ac.jp OI Kanai, Akio/0000-0002-6362-2419; Fujishima, Kosuke/0000-0002-8844-812X FU Japan Society for the Promotion of Science; [24770125]; [23350081] FX Funding for open access charge: The Grant-in-Aid for Young Scientists (B) [No. 24770125 to A. H.]; Grant-in-Aid for Science Research (B) [No. 23350081 to H. H.]; Japan Society for the Promotion of Science. NR 42 TC 4 Z9 4 U1 0 U2 6 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0305-1048 J9 NUCLEIC ACIDS RES JI Nucleic Acids Res. PD NOV PY 2012 VL 40 IS 20 BP 10554 EP 10566 DI 10.1093/nar/gks826 PG 13 WC Biochemistry & Molecular Biology SC Biochemistry & Molecular Biology GA 035TC UT WOS:000310970700058 PM 22941657 ER PT J AU Thompson, DJ Digel, SW Racusin, JL AF Thompson, David J. Digel, Seth W. Racusin, Judith L. TI Exploring the extreme universe with the Fermi Gamma-Ray Space Telescope SO PHYSICS TODAY LA English DT Article ID LARGE-AREA TELESCOPE C1 [Thompson, David J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Digel, Seth W.] SLAC, Menlo Pk, CA USA. RP Thompson, DJ (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RI Racusin, Judith/D-2935-2012 NR 9 TC 0 Z9 0 U1 0 U2 1 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 0031-9228 J9 PHYS TODAY JI Phys. Today PD NOV PY 2012 VL 65 IS 11 BP 39 EP 45 PG 7 WC Physics, Multidisciplinary SC Physics GA 037UG UT WOS:000311131400020 ER PT J AU Bykov, A Gehrels, N Krawczynski, H Lemoine, M Pelletier, G Pohl, M AF Bykov, Andrei Gehrels, Neil Krawczynski, Henric Lemoine, Martin Pelletier, Guy Pohl, Martin TI Particle Acceleration in Relativistic Outflows SO SPACE SCIENCE REVIEWS LA English DT Review DE Cosmic rays; Particle acceleration; Shocks ID GAMMA-RAY BURSTS; ENERGY COSMIC-RAYS; ACTIVE GALACTIC NUCLEI; ULTRARELATIVISTIC SHOCK-WAVES; MAGNETIC-FIELD AMPLIFICATION; VERY-HIGH-ENERGY; 28 FEBRUARY 1997; X-RAY; FERMI ACCELERATION; PROMPT EMISSION AB In this review we confront the current theoretical understanding of particle acceleration at relativistic outflows with recent observational results on various source classes thought to involve such outflows, e.g. gamma-ray bursts, active galactic nuclei, and pulsar wind nebulae. We highlight the possible contributions of these sources to ultra-high-energy cosmic rays. C1 [Pohl, Martin] Univ Potsdam, Inst Phys & Astron, D-14476 Potsdam, Germany. [Bykov, Andrei] Ioffe Inst Phys & Technol, St Petersburg 194021, Russia. [Bykov, Andrei] St Petersburg State Politech Univ, St Petersburg 195251, Russia. [Gehrels, Neil] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Krawczynski, Henric] Washington Univ, Dept Phys, St Louis, MO 63130 USA. [Lemoine, Martin] UPMC, CNRS, Inst Astrophys Paris, F-75014 Paris, France. [Pelletier, Guy] Inst Planetol & Astrophys Grenoble, F-38041 Grenoble 9, France. [Pohl, Martin] DESY, D-15738 Zeuthen, Germany. RP Pohl, M (reprint author), Univ Potsdam, Inst Phys & Astron, D-14476 Potsdam, Germany. EM byk@astro.ioffe.ru; neil.gehrels@nasa.gov; krawcz@wuphys.wustl.edu; lemoine@iap.fr; Guy.Pelletier@obs.ujf-grenoble.fr; marpohl@uni-potsdam.de RI Bykov, Andrei/E-3131-2014; OI Lemoine, Martin/0000-0002-2395-7812 FU Russian government [11.G34.31.0001]; RAS; RAS Presidium; RFBR [11-02-12082]; Helmholtz Alliance for Astroparticle Phyics HAP; Initiative and Networking Fund of Helmholtz Association; PEPS/PTI program of CNRS-INP FX A.M.B. was supported in part by the Russian government grant 11.G34.31.0001 to Sankt-Petersburg State Politechnical University, and also by the RAS and RAS Presidium Programs and by the RFBR grant 11-02-12082. N.G. acknowledges scientific discussions and assistance by J. Cannizzo. M. P. is supported by the 'Helmholtz Alliance for Astroparticle Phyics HAP' funded by the Initiative and Networking Fund of the Helmholtz Association. M. L. and G. P. acknowledge financial support of the PEPS/PTI program of the CNRS-INP. NR 166 TC 20 Z9 20 U1 0 U2 6 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 NOV PY 2012 VL 173 IS 1-4 BP 309 EP 339 DI 10.1007/s11214-012-9896-y PG 31 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 034MR UT WOS:000310878100010 ER PT J AU Simon, M Bobskill, MR Wilhite, A AF Simon, M. Bobskill, M. R. Wilhite, A. TI Historical volume estimation and a structured method for calculating habitable volume for in-space and surface habitats SO ACTA ASTRONAUTICA LA English DT Article DE Habitable volume; Volume; Pressurized volume; Numerical method; Spacecraft design; Interior; Habitat; Requirements; Gravity environment; Mission duration; Habitability; Utility; Boolean test; Collision detection; Accessibility AB Habitable volume is an important spacecraft design figure of merit necessary to determine the required size of crewed space vehicles, or habitats. In order to design habitats for future missions and properly compare the habitable volumes of future habitat designs with historical spacecraft, consistent methods of both defining the required amount of habitable volume and estimating the habitable volume for a given layout are required. This paper provides a brief summary of historical habitable volume requirements and describes the appropriate application of requirements to various types of missions, particularly highlighting the appropriate application for various gravity environments. Then the proposed "Marching Grid Method", a structured automatic, numerical method to calculate habitable volume for a given habitat design, is described in detail. This method uses a set of geometric Boolean tests applied to a discrete set of points within the pressurized volume to numerically estimate the functionally usable and accessible space that comprises the habitable volume. The application of this method to zero gravity and nonzero gravity environments is also discussed. This proposed method is then demonstrated by calculating habitable volumes using two conceptual-level layouts of habitat designs, one for each type of gravity environment. These include the US Laboratory Module on ISS and the Scenario 12.0 Pressurized Core Module from the recent NASA Lunar Surface Systems studies. Results of this study include a description of the effectiveness of this method for various resolutions of the investigated grid, and commentary highlighting the use of this method to determine the overall utility of interior configurations for automatically evaluating interior layouts. Published by Elsevier Ltd. C1 [Simon, M.; Wilhite, A.] Georgia Inst Technol, Hampton, VA USA. [Bobskill, M. R.] NASA, Langley Res Ctr, Hampton, VA 23665 USA. RP Simon, M (reprint author), Georgia Inst Technol, Hampton, VA USA. EM msimon@gatech.edu; wilhite@nianet.org NR 19 TC 0 Z9 0 U1 0 U2 1 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0094-5765 J9 ACTA ASTRONAUT JI Acta Astronaut. PD NOV-DEC PY 2012 VL 80 BP 65 EP 81 DI 10.1016/j.actaastro.2012.04.041 PG 17 WC Engineering, Aerospace SC Engineering GA 005EN UT WOS:000308733400009 ER PT J AU Johnson, NL AF Johnson, Nicholas L. TI A new look at the GEO and near-GEO regimes: Operations, disposals, and debris SO ACTA ASTRONAUTICA LA English DT Article DE Geosynchronous; Operations; Debris; Disposal AB Since 1963 more than 900 spacecraft and more than 200 launch vehicle upper stages have been inserted into the vicinity of the geosynchronous regime. Equally important, more than 300 spacecraft have been maneuvered into disposal orbits at mission termination to alleviate unnecessary congestion in the finite GEO region. However, the number of GEO satellites continues to grow, and evidence exists of a substantial small debris population. In addition, the operational modes of an increasing number of GEO spacecraft differ from those of their predecessors of several decades ago, including more frequent utilization of inclined and eccentric geosynchronous orbits. Consequently, the nature of the GEO regime and its immediate surroundings is evolving from well-known classical characteristics. This paper takes a fresh look at the GEO satellite population and the near- and far-term environmental implications of the region, including the effects of national and international debris mitigation measures. Published by Elsevier Ltd. C1 NASA, Orbital Debris Program Off, Houston, TX USA. RP Johnson, NL (reprint author), NASA, Orbital Debris Program Off, Houston, TX USA. EM Nicholas.L.Johnson@nasa.gov NR 9 TC 4 Z9 4 U1 0 U2 1 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0094-5765 J9 ACTA ASTRONAUT JI Acta Astronaut. PD NOV-DEC PY 2012 VL 80 BP 82 EP 88 DI 10.1016/j.actaastro.2012.05.024 PG 7 WC Engineering, Aerospace SC Engineering GA 005EN UT WOS:000308733400010 ER PT J AU Schmidt, GR Landis, GA Oleson, SR AF Schmidt, George R. Landis, Geoffrey A. Oleson, Steven R. TI Human Exploration using Real-Time Robotic Operations (HERRO): A space exploration strategy for the 21st century SO ACTA ASTRONAUTICA LA English DT Article DE Space exploration; Human spaceflight; Space science; Planetary exploration; Telerobotics; Communications latency AB This paper presents an exploration strategy for human missions beyond Low Earth Orbit (LEO) and the Moon that combines the best features of human and robotic spaceflight. This "Human Exploration using Real-time Robotic Operations" (HERRO) strategy refrains from placing humans on the surfaces of the Moon and Mars in the near-term. Rather, it focuses on sending piloted spacecraft and crews into orbit around Mars and other exploration targets of interest, and conducting astronaut exploration of the surfaces using telerobots and remotely-controlled systems. By eliminating the significant communications delay or "latency" with Earth due to the speed of light limit, teleoperation provides scientists real-time control of rovers and other sophisticated instruments. This in effect gives them a "virtual presence" on planetary surfaces, and thus expands the scientific return at these destinations. HERRO mitigates several of the major issues that have hindered the progress of human spaceflight beyond Low Earth Orbit (LEO) by: (1) broadening the range of destinations for near-term human missions; (2) reducing cost and risk through less complexity and fewer man-rated elements; (3) offering benefits of human-equivalent in-situ cognition, decision-making and fieldwork on planetary bodies; (4) providing a simpler approach to returning samples from Mars and planetary surfaces; and (5) facilitating opportunities for international collaboration through contribution of diverse robotic systems. HERRO provides a firm justification for human spaceflight-one that expands the near-term capabilities of scientific exploration while providing the space transportation infrastructure needed for eventual human landings in the future. Published by Elsevier Ltd. C1 [Schmidt, George R.; Landis, Geoffrey A.; Oleson, Steven R.] NASA Glenn Res Ctr, Cleveland, OH USA. RP Schmidt, GR (reprint author), NASA Glenn Res Ctr, Cleveland, OH USA. EM George.Schmidt@nasa.gov; Geoffrey.Landis@nasa.gov; Steven.R.Oleson@nasa.gov NR 25 TC 1 Z9 1 U1 2 U2 17 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0094-5765 J9 ACTA ASTRONAUT JI Acta Astronaut. PD NOV-DEC PY 2012 VL 80 BP 105 EP 113 DI 10.1016/j.actaastro.2012.05.036 PG 9 WC Engineering, Aerospace SC Engineering GA 005EN UT WOS:000308733400012 ER PT J AU Lee, BJ Liou, MS AF Lee, Byung Joon Liou, Meng-Sing TI Unsteady Adjoint Approach for Design Optimization of Flapping Airfoils SO AIAA JOURNAL LA English DT Article ID PROPULSIVE EFFICIENCY; PERFORMANCE; FOIL AB This paper describes the work for optimizing the propulsive efficiency of flapping airfoils (i.e., improving the thrust under constraining aerodynamic work during the flapping flights by changing their shape and trajectory of motion with the unsteady discrete adjoint approach). For unsteady problems, it is essential that the time scales of motion under consideration should be properly resolved and must be compatible with the objective sought after. Both the instantaneous and time-averaged (periodic) formulations are included in this study. For the design optimization with shape parameters or motion parameters, the time-averaged objective function is found to be more useful, while the instantaneous one is more suitable for flow control. The instantaneous objective function is operationally straightforward. On the other hand, the time-averaged objective function requires additional steps in the adjoint approach; the adjoint vectors for the whole time domain must be solved in a reverse time manner. In the current study, applying the periodicity condition allows the unsteady discrete adjoint equations to be reformulated and the resulting system of equations for each sub-time-interval is solved iteratively. The design results from shape and trajectory optimizations are compared, and the physical relevance of design variables to the flapping motion at on- and off-design conditions is investigated. C1 [Lee, Byung Joon; Liou, Meng-Sing] NASA, John H Glenn Res Ctr, Lewis Field, Aeroprop Div, Cleveland, OH 44135 USA. RP Lee, BJ (reprint author), NASA, John H Glenn Res Ctr, Lewis Field, Aeroprop Div, Cleveland, OH 44135 USA. EM mdo.bjlee@gmail.com FU NASA FX The authors are grateful for the financial supports provided by NASA's Subsonic Fixed Wing Project. NR 25 TC 3 Z9 3 U1 1 U2 9 PU AMER INST AERONAUTICS ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0001-1452 EI 1533-385X J9 AIAA J JI AIAA J. PD NOV PY 2012 VL 50 IS 11 BP 2460 EP 2475 DI 10.2514/1.J051663 PG 16 WC Engineering, Aerospace SC Engineering GA 030GM UT WOS:000310559000014 ER PT J AU Feldman, Y Colonius, T Pauken, MT Hall, JL Jones, JA AF Feldman, Yuri Colonius, Tim Pauken, Michael T. Hall, Jeffrey L. Jones, Jack A. TI Simulation and Cryogenic Experiments of Natural Convection for the Titan Montgolfiere SO AIAA JOURNAL LA English DT Article ID BALLOONS; SPHERES AB Natural convection in a spherical geometry is considered for prediction of the buoyancy of single- and double-walled balloons in a cryogenic environment such as Titan's atmosphere. The steady-state flow characteristics obtained by solving the Reynolds-averaged Navier-Stokes equations with a standard turbulence model are used to determine the net buoyancy as a function of heat input. Thermal radiation effects are shown to have a minor impact on the buoyancy, as would he expected at cryogenic conditions. The predicted buoyancy and temperature fields compare favorably with experiments preformed on a 1-m-diameter Montgolfiere prototype in a cryogenic facility. In addition, both numerical and experimental results were compared with correlations for the heat transfer coefficients for free convection internal and external to the balloon as well as in the concentric gap of the double-walled balloons. Finally, scaling issues related to inferring the performance of the full-scale Montgolfiere from the model-scale results are examined. C1 [Feldman, Yuri; Colonius, Tim] CALTECH, Pasadena, CA 91125 USA. [Pauken, Michael T.; Hall, Jeffrey L.; Jones, Jack A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Feldman, Y (reprint author), CALTECH, Pasadena, CA 91125 USA. NR 15 TC 5 Z9 5 U1 2 U2 4 PU AMER INST AERONAUT ASTRONAUT PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0001-1452 J9 AIAA J JI AIAA J. PD NOV PY 2012 VL 50 IS 11 BP 2483 EP 2491 DI 10.2514/1.J051672 PG 9 WC Engineering, Aerospace SC Engineering GA 030GM UT WOS:000310559000016 ER PT J AU Yi, J Kim, C Lee, BJ AF Yi, JunSok Kim, Chongam Lee, Byung Joon TI Adjoint-Based Design Optimization of Vortex Generator in an S-Shaped Subsonic Inlet SO AIAA JOURNAL LA English DT Article ID NAVIER-STOKES EQUATIONS; TURBULENCE MODELS; FLOW-CONTROL; DISTORTION AB This paper deals with an adjoint-based design optimization of vortex generators for the performance improvement of an S-shaped subsonic inlet, the Royal Aircraft Establishment intake model 2129. To enhance the flow quality entering the engine face maximally, the vortex generators are independently optimized with five design parameters per each vortex generator (a total of 55 design variables). To increase the design efficiency, the source term model of the vortex generator is employed. The original source term model, which does not reflect a small change in position and thus has difficulties in differentiation for sensitivity analysis, is modified into a differentiable source term model. To deal with a large number of design variables, the gradient-based design optimization method using the discrete adjoint approach is employed to minimize the distortion coefficient while maintaining the baseline total pressure recovery ratio. A total of five design cases are conducted to validate the proposed design approach, to obtain the optimized vortex generators, and to confirm their enhanced performance. Through the proposed design process, the performance of the target inlet is remarkably improved, showing that the distortion coefficient decreases well over 70% while maintaining the total pressure recovery ratio. C1 [Kim, Chongam] Seoul Natl Univ, Dept Aerosp Engn, Inst Adv Aerosp Technol, Seoul 151744, South Korea. [Yi, JunSok] Seoul Natl Univ, Dept Aerosp Engn, Flight Vehicle Res Ctr, Seoul 151744, South Korea. [Lee, Byung Joon] NASA, John H Glenn Res Ctr, Lewis Field, Cleveland, OH 44135 USA. RP Kim, C (reprint author), Seoul Natl Univ, Dept Aerosp Engn, Inst Adv Aerosp Technol, Seoul 151744, South Korea. EM chongam@snu.ac.kr FU National Research Foundation of Korea; Korean government [2011-0027486]; National Space Lab program through the National Research Foundation of Korea; Ministry of Education, Science and Technology [2011-0029871]; Ministry of Education, Science, and Technology [2011-0020559] FX This work was supported by the National Research Foundation of Korea grant funded by the Korean government (no. 2011-0027486) and National Space Lab program through the National Research Foundation of Korea, funded by the Ministry of Education, Science and Technology (no. 2011-0029871). This research was also supported by the Ministry of Education, Science, and Technology, subject to the Education-Research Integration Through Simulation on the Net project (no. 2011-0020559). NR 33 TC 2 Z9 2 U1 2 U2 10 PU AMER INST AERONAUTICS ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0001-1452 J9 AIAA J JI AIAA J. PD NOV PY 2012 VL 50 IS 11 BP 2492 EP 2507 DI 10.2514/1.J051687 PG 16 WC Engineering, Aerospace SC Engineering GA 030GM UT WOS:000310559000017 ER PT J AU Schultz, MR Oremont, L Guzman, JC McCarville, D Rose, CA Hilburger, MW AF Schultz, Marc R. Oremont, Leonard Guzman, J. Carlos McCarville, Douglas Rose, Cheryl A. Hilburger, Mark W. TI Compression Response of Fluted-Core Composite Panels SO AIAA JOURNAL LA English DT Article ID SANDWICH; BEHAVIOR AB In recent years, fiber-reinforced composites have become more accepted for aerospace applications. For example, during NASA's recent efforts to develop new launch vehicles, composite materials were considered and baselined for a number of structures, including dry barrel sections, which are primarily loaded in longitudinal compression. Because of mass and stiffness requirements, sandwich composites are often selected for these applications. However, there are a number of manufacturing and in-service concerns associated with traditional honeycomb-core sandwich composites that in certain instances may be alleviated through the use of other core materials or construction methods. A fluted core, which consists of integral angled web members with structural radius fillers spaced between laminate facesheets, is one such construction alternative. In this paper, two different fluted-core composite designs were considered: a subscale design and a full-scale design sized for a heavy-lift-launch-vehicle interstage. In particular, the longitudinal compression behavior of fluted-core composites was evaluated with experiments and finite-element analyses. Detailed branched-shell finite-element models were developed, and geometrically nonlinear analyses were conducted to predict both buckling and material failures. Good agreement was obtained between test data and analysis predictions for both failure types. Though the local buckling events are not catastrophic, the resulting deformations contribute to material failures. Consequently, neither the local buckling behavior nor the material failure loads and modes can be predicted by either linear analyses or nonlinear smeared-shell analyses. Compression-after-impact performance of fluted-core composites was also investigated experimentally. Nondestructive inspection of the damage zones indicated that the detectable damage was limited to no more than one flute on either side of any given impact. More study is needed, but this may indicate that an inherent damage-arrest capability of fluted core could provide benefits over traditional sandwich designs in certain weight-critical applications. C1 [Schultz, Marc R.; Rose, Cheryl A.; Hilburger, Mark W.] NASA, Langley Res Ctr, Struct Mech & Concepts Branch, Hampton, VA 23681 USA. [Oremont, Leonard] Lockheed Martin Corp, Hampton, VA 23681 USA. [Guzman, J. Carlos; McCarville, Douglas] Boeing Co, Boeing Res & Technol, Seattle, WA 98124 USA. RP Schultz, MR (reprint author), NASA, Langley Res Ctr, Struct Mech & Concepts Branch, Mail Stop 190, Hampton, VA 23681 USA. NR 22 TC 2 Z9 2 U1 1 U2 8 PU AMER INST AERONAUTICS ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0001-1452 J9 AIAA J JI AIAA J. PD NOV PY 2012 VL 50 IS 11 BP 2546 EP 2557 DI 10.2514/1.J051728 PG 12 WC Engineering, Aerospace SC Engineering GA 030GM UT WOS:000310559000021 ER PT J AU Bhagwat, MJ Ramasamy, M AF Bhagwat, Mahendra J. Ramasamy, Manikandan TI Effect of tip vortex aperiodicity on measurement uncertainty SO EXPERIMENTS IN FLUIDS LA English DT Article ID HELICOPTER ROTOR; FLOW; WAKE; VORTICES AB Vortex aperiodicity introduces random uncertainty in the measured vortex center location. Unless corrected, this may lead to systematic uncertainty in the vortex properties derived from the measured velocity field. For example, the vortex core size derived from averaged or mean flow field appears larger because of aperiodicity. Several methodologies for aperiodicity correction have been developed over the past two decades to alleviate this systematic uncertainty. However, these do not always reduce the accompanying random uncertainty. The current work shows that the analysis methods used to derive the vortex properties from the measured velocity field play an important role in the resultant random uncertainty in these properties; perhaps, even more important role than the aperiodicity correction methodology itself. It is hypothesized that a class of methods called global methods, which use a large extent of measured data, yield a smaller measurement uncertainty compared to local methods. This hypothesis is verified using a newly proposed global method based on a planar least-squares fit. The general applicability of the method is demonstrated using previous particle image velocimetry measurements of rotor tip vortices. The results clearly demonstrate a reduced random uncertainty in the vortex core properties, even in the presence of secondary vortical structures. Furthermore, the results are independent of the choice of aperiodicity correction methodology. C1 [Bhagwat, Mahendra J.] USA, Aeroflightdynam Directorate AMRDEC, Ames Res Ctr, Moffett Field, CA 94035 USA. [Ramasamy, Manikandan] NASA, UARC AFDD, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Bhagwat, MJ (reprint author), USA, Aeroflightdynam Directorate AMRDEC, Ames Res Ctr, M-S 215-1, Moffett Field, CA 94035 USA. EM mahendra.bhagwat@us.army.mil NR 24 TC 8 Z9 8 U1 1 U2 6 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0723-4864 J9 EXP FLUIDS JI Exp. Fluids PD NOV PY 2012 VL 53 IS 5 BP 1191 EP 1202 DI 10.1007/s00348-012-1348-7 PG 12 WC Engineering, Mechanical; Mechanics SC Engineering; Mechanics GA 031MA UT WOS:000310643600002 ER PT J AU Rampe, EB Kraft, MD Sharp, TG Golden, DC Ming, DW Christensen, PR AF Rampe, E. B. Kraft, M. D. Sharp, T. G. Golden, D. C. Ming, D. W. Christensen, P. R. TI Allophane detection on Mars with Thermal Emission Spectrometer data and implications for regional-scale chemical weathering processes SO GEOLOGY LA English DT Article ID MARTIAN SURFACE; SYNTHETIC ALLOPHANE; MERIDIANI-PLANUM; ICE DEPOSITS; MINERALOGY; COMPONENT; SPECTRA; BASALT; TES AB Models of Thermal Emission Spectrometer (TES) data suggest that poorly-crystalline weathering products allophane and aluminosilicate gel occur in several low-albedo regions of Mars. The presence of allophane in TES models indicates that the martian surface experienced low-temperature chemical weathering at low water-to-rock ratios and mildly acidic to neutral pH on regional scales. The allophane and gel may be ancient and preserved by a persistently dry martian climate. Alternatively, evidence for recent ground ice in these regions suggests that pedogenic processes causing the formation of poorly-crystalline aluminosilicates could be late Amazonian in age and may be active today. While previous models have suggested that global-scale acidic weathering has occurred on Mars for the past 3.5 billion years, the presence of allophane indicates that acidic weathering was not occurring in these low-albedo regions and that mildly acidic to neutral weathering has been an important regional-scale weathering process on the martian surface. C1 [Rampe, E. B.; Ming, D. W.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Rampe, E. B.] Oak Ridge Associated Univ, Oak Ridge, TN 37831 USA. [Kraft, M. D.; Sharp, T. G.; Christensen, P. R.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [Golden, D. C.] Engn & Sci Contract Grp Hamilton Sundstrand, Houston, TX 77058 USA. RP Rampe, EB (reprint author), NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. EM elizabeth.b.rampe@nasa.gov FU NASA [NNX07AP11H] FX We thank A.D. Rogers for her input and insight. We thank J. Quinn for quantifying allophane compositions. We gratefully acknowledge the use of facilities within the LeRoy Eyring Center for Solid State Science at Arizona State University. This manuscript was improved by helpful reviews by M. McDowell and two anonymous reviewers. This research was supported by NASA Graduate Student Researchers Program grant NNX07AP11H. NR 29 TC 13 Z9 13 U1 0 U2 15 PU GEOLOGICAL SOC AMER, INC PI BOULDER PA PO BOX 9140, BOULDER, CO 80301-9140 USA SN 0091-7613 EI 1943-2682 J9 GEOLOGY JI Geology PD NOV PY 2012 VL 40 IS 11 BP 995 EP 998 DI 10.1130/G33215.1 PG 4 WC Geology SC Geology GA 028GO UT WOS:000310411000009 ER PT J AU Hui, FK Yim, J Spiotta, AM Hussain, MS Toth, G AF Hui, Ferdinand K. Yim, John Spiotta, Alejandro M. Hussain, M. Shazam Toth, Gabor TI Intermediate catheter injections in closed segments during acute stroke intervention: a cautionary note SO JOURNAL OF NEUROINTERVENTIONAL SURGERY LA English DT Article ID TRIAL AB Objective and importance In the setting of stroke intervention, there is typically an occlusion that limits angiographic visualization of patent vasculature distal to the embolus. Certain mechanical thrombectomy paradigms include angiography of the vasculature distal to the point of occlusion in preparation for thrombectomy, typically using a microcatheter. Injections using an intermediate catheter allows for higher volume of injection at a faster rate, resulting in radically different pressure gradients. Clinical presentations Two patients presenting with acute ischemic stroke were treated via mechanical thrombectomy using the Penumbra 054 system. The first was a tandem occlusion with a high grade narrowing and occlusion of the internal carotid artery (ICA) origin and an ICA terminus thrombus. The second was a long segment, high volume thrombus extending from the cavernous segment to the ICA terminus. Intervention Conventional access techniques were utilized to position the Penumbra 054 catheter in the ICA in both cases. Intraprocedurally, angiography through the 054 catheter within the closed segment resulted in contrast extravasation adjacent to the tentorium, originating from the communicating segment of the ICA, both of which cleared within 48 h. Due to the extravasation, the interventions were both terminated, and the infarcts went on to complete. Conclusion During an acute stroke, flow within large vessels is abnormal, and rapid changes in volume may result in drastic changes in pressure which may lead to extravasation. The authors recommend never performing a contrast injection through a large lumen catheter when flow may be impeded proximally and distally. Closed segment injections of large volumes at a high rate are probably at high risk for vessel injury. C1 [Hui, Ferdinand K.] Cleveland Clin, Cerebrovasc Ctr, Cleveland, OH 44195 USA. [Yim, John] NASA, Glenn Res Ctr, Cleveland, OH USA. [Spiotta, Alejandro M.] Cleveland Clin, Neurol Inst, Cleveland, OH 44195 USA. [Hussain, M. Shazam; Toth, Gabor] CCF, Cerebrovasc Ctr, Cleveland, OH USA. RP Hui, FK (reprint author), Cleveland Clin, Cerebrovasc Ctr, 9500 Euclid Ave S80 55, Cleveland, OH 44195 USA. EM huif@ccf.org NR 6 TC 4 Z9 4 U1 0 U2 0 PU BMJ PUBLISHING GROUP PI LONDON PA BRITISH MED ASSOC HOUSE, TAVISTOCK SQUARE, LONDON WC1H 9JR, ENGLAND SN 1759-8478 J9 J NEUROINTERV SURG JI J. NeuroInterventional Surg. PD NOV PY 2012 VL 4 IS 6 AR e39 DI 10.1136/neurintsurg-2011-010163 PG 5 WC Neuroimaging; Surgery SC Neurosciences & Neurology; Surgery GA 029MX UT WOS:000310501000009 PM 22234947 ER PT J AU Thompson, DR Benner, DC Brown, LR Crisp, D Devi, VM Jiang, YB Natraj, V Oyafuso, F Sung, K Wunch, D Castano, R Miller, CE AF Thompson, David R. Benner, D. Chris Brown, Linda R. Crisp, David Devi, V. Malathy Jiang, Yibo Natraj, Vijay Oyafuso, Fabiano Sung, Keeyoon Wunch, Debra Castano, Rebecca Miller, Charles E. TI Atmospheric validation of high accuracy CO2 absorption coefficients for the OCO-2 mission SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Article DE Fourier transform spectroscopy; Infrared CO2 spectroscopy; Atmospheric CO2 retrievals; Line shapes; Line mixing; Speed dependence ID COLUMN OBSERVING NETWORK; 20 MU-M; SPEED DEPENDENCE; SPECTROSCOPIC DATABASE; SATELLITE-OBSERVATIONS; INFRARED-SPECTRA; LINE PARAMETERS; WING REGIONS; A-BAND; RETRIEVALS AB We describe atmospheric validation of 1.61 mu m and 2.06 mu m CO2 absorption coefficient databases for use by the Orbiting Carbon Observatory (OCO-2). The OCO-2 mission will collect the measurements needed to estimate column-averaged CO2 similar to dry air mole fraction within 1 ppm accuracy without the region- or airmass-dependent biases that would significantly degrade efforts to understand carbon sources and sinks on a global scale. To accomplish this, the forward radiative transfer model used to generate synthetic atmospheric spectra for retrievals must achieve unprecedented spectroscopic fidelity within the short wave infrared CO2 bands sampled by the sensors. The failure of Voigt line shapes and conventional line mixing formulations for such objectives has motivated significant revisions to line shape models used to generate the gas absorption cross sections for the OCO-2 forward model. In this paper, we test line mixing and speed dependent line shapes combined with improved experimental line parameters. We evaluate pre-computed absorption coefficients in the two spectral regions of CO2 absorbtion using high resolution FT-IR laboratory spectra, atmospheric spectra from the Total Carbon Column Observing Network (TCCON), and medium resolution soundings from the space-based Greenhouse Gases Observing Satellite (GOSAT). (C) 2012 Elsevier Ltd. All rights reserved. C1 [Thompson, David R.; Brown, Linda R.; Crisp, David; Jiang, Yibo; Natraj, Vijay; Oyafuso, Fabiano; Sung, Keeyoon; Castano, Rebecca; Miller, Charles E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Benner, D. Chris; Devi, V. Malathy] Coll William & Mary, Dept Phys, Williamsburg, VA 23187 USA. [Wunch, Debra] CALTECH, Pasadena, CA 91125 USA. RP Thompson, DR (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM david.r.thompson@jpl.nasa.gov RI Sung, Keeyoon/I-6533-2015 FU U.S. NASA's Terrestrial Ecology Program [NNX11AG01G]; US Government FX We thank the OCO-2 ACOS Level 2 algorithm team including Annmarie Eldering, Vivienne Payne and Michael Gunson. We thank the members of the OCO-2 science team including Eli Mlawer and Iouli Gordon. We have also benefited from the counsel of Mitchio Okumura, Joseph Hodges, and David Long. GOSAT TANSO-FTS spectra were provided to the ACOS Team through a GOSAT Research Announcement (RA) agreement between the California Institute of Technology and the three parties, JAXA, NIES and the MOE. The European Centre for Medium-Range Weather Forecasts (ECMWF) provided meteorological data for initializing the retrievals. The Total Carbon Column Observing Network (TCCON) Archive, operated by the California Institute of Technology, supplied upward-looking measurements. U.S. funding for the Park Falls TCCON station comes from NASA's Terrestrial Ecology Program, grant number NNX11AG01G. A portion of the research described was carried out at the Jet Propulsion Laboratory, California Institute of Technology and The College of William and Mary under contracts with the National Aeronautics and Space Administration. Copyright 2012, California Institute of Technology. All Rights Reserved. US Government support acknowledged. NR 54 TC 28 Z9 29 U1 0 U2 36 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0022-4073 EI 1879-1352 J9 J QUANT SPECTROSC RA JI J. Quant. Spectrosc. Radiat. Transf. PD NOV PY 2012 VL 113 IS 17 BP 2265 EP 2276 DI 10.1016/j.jqsrt.2012.05.021 PG 12 WC Optics; Spectroscopy SC Optics; Spectroscopy GA 031RP UT WOS:000310660300013 ER PT J AU Moncada, AM Chattopadhyay, A Bednarcyk, BA Arnold, SM AF Moncada, Albert M. Chattopadhyay, Aditi Bednarcyk, Brett A. Arnold, Steven M. TI Micromechanics-based progressive failure analysis of composite laminates using different constituent failure theories SO JOURNAL OF REINFORCED PLASTICS AND COMPOSITES LA English DT Article DE Micromechanics; composite material; failure; Worldwide Failure Exercise ID PERIODIC MULTIPHASE MATERIALS; HIGHER-ORDER THEORY; GLASSY-POLYMERS; EPOXY-RESIN; GENERALIZED-METHOD; STRAIN; MODEL; DEFORMATION; STRENGTH; EXERCISE AB Predicting failure in a composite can be performed using ply level mechanisms and/or micro level mechanisms. This paper uses the generalized method of cells and high-fidelity generalized method of cells micromechanics theories, coupled with classical lamination theory, to study progressive damage in composites. Different failure theories, implemented at the fiber and matrix constituent level within a laminate, are investigated. A comparison is made among maximum stress, maximum strain, Tsai-Hill, and Tsai-Wu failure theories. To verify the failure theories, the Worldwide Failure Exercise experiments are used. The Worldwide Failure Exercise is a comprehensive study that covers a wide range of polymer matrix composite laminates. The objectives of this paper are to evaluate the current predictive capabilities of the generalized method of cells and high-fidelity generalized method of cells micromechanics theories for the progressive failure prediction of polymer matrix composite laminates and to evaluate the influence of four failure criteria applied at the fiber/matrix constituent scale. The numerical results demonstrate overall agreement with the experimental results for most of the composite layups examined, but also point to the need for more accurate resin damage progression models. C1 [Moncada, Albert M.; Chattopadhyay, Aditi] Arizona State Univ, Dept Mech & Aerosp Engn, Sch Engn Matter Transport & Energy, Tempe, AZ 85287 USA. [Bednarcyk, Brett A.; Arnold, Steven M.] NASA, Glenn Res Ctr, Cleveland, OH USA. RP Moncada, AM (reprint author), Arizona State Univ, Dept Mech & Aerosp Engn, Sch Engn Matter Transport & Energy, Tempe, AZ 85287 USA. EM amoncada@asu.edu FU NASA [NNX07AD70A] FX This work was supported by NASA [grant number NNX07AD70A]. NR 37 TC 5 Z9 6 U1 4 U2 23 PU SAGE PUBLICATIONS LTD PI LONDON PA 1 OLIVERS YARD, 55 CITY ROAD, LONDON EC1Y 1SP, ENGLAND SN 0731-6844 J9 J REINF PLAST COMP JI J. Reinf. Plast. Compos. PD NOV PY 2012 VL 31 IS 21 BP 1467 EP 1487 DI 10.1177/0731684412456330 PG 21 WC Materials Science, Composites; Polymer Science SC Materials Science; Polymer Science GA 033OR UT WOS:000310807900006 ER PT J AU Grudinin, IS Yu, N AF Grudinin, Ivan S. Yu, Nan TI Finite-element modeling of coupled optical microdisk resonators for displacement sensing SO JOURNAL OF THE OPTICAL SOCIETY OF AMERICA B-OPTICAL PHYSICS LA English DT Article ID WHISPERING-GALLERY MODES; SENSITIVITY; MICROCAVITIES; MICROSPHERES; LASER AB We analyze normal mode splitting in a pair of vertically coupled microdisk resonators. A full vectorial finite-element model is used to find the eigenfrequencies of the symmetric and antisymmetric composite modes as a function of coupling distance. We find that the coupled microdisks can compete with the best Fabry-Perot resonators in displacement sensing. We also show how we configured FreeFem++ for the sphere eigenvalue problem. (C) 2012 Optical Society of America C1 [Grudinin, Ivan S.; Yu, Nan] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Grudinin, IS (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM grudinin@jpl.nasa.gov FU National Aeronautics and Space Administration; NASA Center Innovation Fund; Jet Propulsion Laboratory (JPL) Research and Technology Development Program FX This work was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration, with partial support from the NASA Center Innovation Fund and Jet Propulsion Laboratory (JPL) Research and Technology Development Program. We are grateful to K. J. Vahala, M. L. Gorodetsky, R. Thompson, F. Hecht, and participants of the FreeFem mailing list for helpful discussions. NR 34 TC 9 Z9 9 U1 1 U2 27 PU OPTICAL SOC AMER PI WASHINGTON PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA SN 0740-3224 J9 J OPT SOC AM B JI J. Opt. Soc. Am. B-Opt. Phys. PD NOV PY 2012 VL 29 IS 11 BP 3010 EP 3014 PG 5 WC Optics SC Optics GA 032IG UT WOS:000310708700004 ER PT J AU Campana, S Immler, S AF Campana, Sergio Immler, Stefan TI XMM-Newton and Swift observations of the Type IIb supernova 2011dh in Messier 51 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE supernovae: individual: SN 2011dh; galaxies: ISM; X-rays: individual: SN 2011dh ID X-RAY-EMISSION; SUPERGIANT PROGENITOR; H-I; GALAXY; M51; EXPLOSION; EVOLUTION; COMPACT; 1993J AB The Type IIb supernova (SN) 2011dh exploded in the nearby galaxy M51 (the Whirlpool galaxy) and provides us with one of the best laboratories to study early high-energy emission from SNe. We give here a comprehensive view of the X-ray properties of SN 2011dh from the analyses of two pointed XMMNewton early observations as well as the full Swift X-ray Telescope (XRT) data set (163 ks). Due to the high XMMNewton throughput, we were able to satisfactorily fit the X-ray spectrum with two hot diffuse gas components including an additional absorption component to our Galaxy. A power-law model provided a worse description of the data. In addition, the early Swift XRT light curve hints of a flux excess at early times (less than or similar to 3 d), consistent with the adiabatic cooling of stellars photosphere a few days after the shock breakout. C1 [Campana, Sergio] INAF Osservatorio Astron Brera, I-23807 Merate, LC, Italy. [Immler, Stefan] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Immler, Stefan] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. RP Campana, S (reprint author), INAF Osservatorio Astron Brera, Via Bianchi 46, I-23807 Merate, LC, Italy. EM sergio.campana@brera.inaf.it OI Campana, Sergio/0000-0001-6278-1576 FU ASI [I/004/11/0]; PRIN-MIUR grant [2009ERC3HT] FX SC thanks Norbert Schartel for granting DDT XMM-Newton observations and Neil Gehrels and the Swift science operations team for approving and scheduling the Swift observational campaign. We thank the referee for comments that helped improve the manuscript. This work made use of data supplied by the UK Swift Science Data Centre at the University of Leicester. This work has been partially supported by the ASI grant I/004/11/0 and by the PRIN-MIUR grant 2009ERC3HT. NR 30 TC 5 Z9 5 U1 0 U2 0 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD NOV PY 2012 VL 427 IS 1 BP L70 EP L74 DI 10.1111/j.1745-3933.2012.01347.x PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 033MH UT WOS:000310800300015 ER PT J AU Mercury, M Green, R Hook, S Oaida, B Wu, W Gunderson, A Chodas, M AF Mercury, M. Green, R. Hook, S. Oaida, B. Wu, W. Gunderson, A. Chodas, M. TI Global cloud cover for assessment of optical satellite observation opportunities: A HyspIRI case study SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE Global clouds; Remote sensing; Viewing opportunities; HyspIRI; Cloudiness ID MODIS; MASK AB The number of cloud-free views by Earth-orbiting optical remote sensing instruments must be characterized to verify that the coverage is sufficient to address a mission's science objectives. This study determines the expected cloud-free coverage for the Hyperspectral Infra-red Imager (HyspIRI) mission concept using the Terra MODIS 5 km daytime cloud mask dataset covering the period 2001-2010. The HyspIRI mission concept has two instruments: a Visible Shortwave Infrared (VSWIR) imaging spectrometer and a Thermal Infrared (TIR) multispectral imager. The VSWIR and TIR instruments have equatorial revisit times of 19 and 5 days, respectively. Using the MODIS cloud mask data, we determined the percentage of the Earth's land and shallow water regions that would have been viewable with cloud-free acquisitions for each quarter and year in 2001 through 2010. For the VSWIR, the average cloud-free coverage was 83.0% quarterly and 99.6% annually. Average TIR monthly coverage was also evaluated to be 90.7%. The standard deviations for these statistics were all less than 1.2%, and the average coverages exceed HyspIRI's quarterly and annual requirements (listed in Table 6) by over twenty standard deviations. By the central limit theorem, it follows that in a typical year, HyspIRI will meet its coverage requirements (listed in Table 6) with extremely low uncertainty, acquiring a sufficient number of scenes to enable both monthly and quarterly assessments of the vast majority of the Earth's land and shallow water. This paper includes: yearly global statistics for cloud-free MODIS observations at 5 km resolution between 2001 and 2010; a one year global map representing percent cloud-free observations between 2001 and 2010; global maps representing percent cloud-free observations between 2001 and 2010 for each quarter; maps of the predicted number of views by each HyspIRI instrument quarterly and over the course of a year; and predicted global coverage quarterly and for one year for each HyspIRI instrument, with additional monthly statistics for TIR. (C) 2012 Elsevier Inc. All rights reserved. C1 [Mercury, M.; Green, R.; Hook, S.; Oaida, B.; Wu, W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Gunderson, A.] Montana State Univ, Bozeman, MT 59718 USA. [Chodas, M.] MIT, Cambridge, MA 02139 USA. RP Mercury, M (reprint author), 4800 Oak Grove Dr,Mail Stop 301-165, Pasadena, CA 91109 USA. EM michael.b.mercuty@jpl.nasa.gov FU NASA through the HyspIRI project FX The authors gratefully acknowledge the insightful contributions of David H. Atkinson and the anonymous peer reviewers. Figure 4's analyses and visualizations were produced with the Giovanni online data system, developed and maintained by the NASA GES DISC. This work was supported by NASA through the HyspIRI project under contract to JPL/Caltech. NR 22 TC 10 Z9 10 U1 0 U2 26 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 NOV PY 2012 VL 126 BP 62 EP 71 DI 10.1016/j.rse.2012.08.007 PG 10 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA 027XY UT WOS:000310388600006 ER PT J AU Brown, ME de Beurs, KM Marshall, M AF Brown, M. E. de Beurs, K. M. Marshall, M. TI Global phenological response to climate change in crop areas using satellite remote sensing of vegetation, humidity and temperature over 26 years SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE Phenology; NDVI; Agriculture; Cereal crops; Temperature; Humidity ID NET PRIMARY PRODUCTION; LAND-SURFACE PHENOLOGY; FOOD SECURITY; SPOT-VEGETATION; AVHRR; NDVI; VARIABILITY; RAINFALL; SEASON; CHINA AB The recent increase in food prices has revealed that climate, combined with an expanding population and a widespread change in diet, may result in an end to an era of predictable abundance of global cereal crops. The objective of this paper is to estimate changes of agriculturally-relevant growing season parameters, including the start of the season, length of the growing period and the position of the height or peak of the season, in the primary regions with rainfed agriculture during the past 26 years. Our analysis found that globally, 27% of cereal crop areas have experienced changes in the length of the growing season since 1981, the majority of which had seasons that were at least 2.3 days per year longer on average. We also found both negative and positive trends in the start of season globally, with different effects of changing temperature and humidity being isolated depending on the country and region. We investigated the correlation between the peak timing of the growing season and agricultural production statistics for rain fed agriculture. We found that two thirds of the countries investigated had at least 25% of pixels with crop production that behaved differently than expected from the null hypothesis of no correlation. The results show that variations in the peak of the growing season have a strong effect on global food production in these countries. We show that northern hemisphere countries and states appear to have improved model fit when using phenological models based on humidity while southern hemisphere countries and states have improved model fit by phenological models based on accumulated growing degree days, showing the impact of climate variability during the past two and a half decades. Published by Elsevier Inc. C1 [Brown, M. E.] NASA, Biospher Sci Branch, Goddard Space Flight Ctr, Greenbelt, MD 20171 USA. [de Beurs, K. M.] Univ Oklahoma, Dept Geog & Environm Sustainabil, Norman, OK 73019 USA. [Marshall, M.] Univ Calif Santa Barbara, Dept Geog, Santa Barbara, CA 93106 USA. RP Brown, ME (reprint author), NASA, Biospher Sci Branch, Goddard Space Flight Ctr, Code 614-4, Greenbelt, MD 20171 USA. EM molly.brown@nasa.gov RI Brown, Molly/M-5146-2013; Brown, Molly/E-2724-2010 OI Brown, Molly/0000-0001-7384-3314; Brown, Molly/0000-0001-7384-3314 NR 46 TC 35 Z9 40 U1 12 U2 119 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 NOV PY 2012 VL 126 BP 174 EP 183 DI 10.1016/j.rse.2012.08.009 PG 10 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA 027XY UT WOS:000310388600015 ER PT J AU Fleck, B Heber, B Vourlidas, A van Driel-Gesztelyi, L Mandrini, CH Leibacher, J AF Fleck, Bernhard Heber, Bernd Vourlidas, Angelos van Driel-Gesztelyi, Lidia Mandrini, Cristina H. Leibacher, John TI The Sun 360 Preface SO SOLAR PHYSICS LA English DT Editorial Material C1 [Fleck, Bernhard] NASA, Goddard Space Flight Ctr, ESA Sci Operat Dept, Greenbelt, MD 20771 USA. [Heber, Bernd] Univ Kiel, Inst Expt & Angew Phys, Kiel, Germany. [Vourlidas, Angelos] USN, Res Lab, Div Space Sci, Washington, DC 20375 USA. [van Driel-Gesztelyi, Lidia] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. [van Driel-Gesztelyi, Lidia] Univ Paris Diderot, Univ Paris 06, Observ Paris, CNRS,LESIA, Meudon, France. [van Driel-Gesztelyi, Lidia] Hungarian Acad Sci, Konkoly Observ, Budapest, Hungary. [Mandrini, Cristina H.] Int Space Sci Inst, Bern, Switzerland. [Mandrini, Cristina H.] Univ Buenos Aires, CONICET, Inst Astron & Fis Espacio, RA-1428 Buenos Aires, DF, Argentina. [Mandrini, Cristina H.] Univ Buenos Aires, Fac Ciencias Exactas & Nat, Buenos Aires, DF, Argentina. [Leibacher, John] Natl Opt Astron Observ, Natl Solar Observ, Tucson, AZ 85726 USA. [Leibacher, John] Inst Astrophys Spatiale, Orsay, France. RP Fleck, B (reprint author), NASA, Goddard Space Flight Ctr, ESA Sci Operat Dept, Greenbelt, MD 20771 USA. EM bfleck@esa.nascom.nasa.gov RI Vourlidas, Angelos/C-8231-2009 OI Vourlidas, Angelos/0000-0002-8164-5948 NR 0 TC 0 Z9 0 U1 0 U2 1 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-0938 J9 SOL PHYS JI Sol. Phys. PD NOV PY 2012 VL 281 IS 1 BP 1 EP 2 DI 10.1007/s11207-012-0120-8 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 033QB UT WOS:000310811900001 ER PT J AU Liewer, PC Hernandez, IG Hall, JR Thompson, WT Misrak, A AF Liewer, P. C. Hernandez, I. Gonzalez Hall, J. R. Thompson, W. T. Misrak, A. TI Comparison of Far-Side STEREO Observations of Solar Activity and Active Region Predictions from GONG SO SOLAR PHYSICS LA English DT Article DE Corona; Active regions; Helioseismology; Space weather ID SUNSPOT; SUN AB On 6 February 2011, the two Solar TErrestrial Relations Observatory (STEREO) spacecraft reached 180A degrees separation and began imaging the entire far-side hemisphere of the Sun in extreme ultraviolet light (EUV). Here, we compare STEREO's observations of far-side solar activity, as evidenced by bright regions in the EUV images, to predictions of far-side active regions from helioseismology using National Solar Observatory Global Oscilla-tion Network Group (GONG) observations. GONG produces seismic Carrington maps of strong magnetic field regions, labeling far-side regions with a probability >= 70%. By visual comparison of these GONG maps with STEREO EUV Carrington maps, we determine whether or not solar activity is observed at the locations of the predicted active regions. For data from February -June 2011, we find that for 139 of 157 comparisons activity is observed in EUV at the predicted site, yielding an 89% success rate. For 18 comparisons, no activity was seen at the predicted region (11% false predictions). We also investigated GONG's success at predicting large active regions before they appear at the east limb as viewed from Earth. Of 15 such east-limb active regions, eight were predicted by GONG at least once in the seven days preceding their Earth-side appearance. STEREO B observations of activity in the days preceding the appearance of the other seven large East-limb active regions indicated that, while three were possibly too small for GONG to make a prediction, four seemed as large and active as other active regions that had been predicted successfully by GONG. C1 [Liewer, P. C.; Hall, J. R.; Misrak, A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Hernandez, I. Gonzalez] Natl Solar Observ, Tucson, AZ 85719 USA. [Thompson, W. T.] Adnet Syst Inc, Lanham, MD 20706 USA. RP Liewer, PC (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Paulett.Liewer@jpl.nasa.gov FU NASA [NNG06EB68C]; Star Targeted Research and Technology program FX We would like to thank F. Hill, P. Scherrer and A. Kosovichev for informative discussions on the use of helioseismology to make far-side active region predictions. We also thank Eric De Jong, Marco Velli and Angelos Vourlidas for useful discussions of this research. The work of P. C. L., J.R.H. and A. M. was conducted at the Jet Propulsion Laboratory, California Institute of Technology under a contract from NASA. The work of I. G. H. was supported by the NASA Living with a Star Targeted Research and Technology program. The work of W. T. T. was supported by NASA grant NNG06EB68C. The STEREO/SECCHI data used here are produced by an international consortium of the Naval Research Laboratory (USA), Lockheed Martin Solar and Astrophysics Lab (USA), NASA Goddard Space Flight Center (USA) Rutherford Appleton Laboratory (UK), University of Birmingham (UK), Max-Planck-Institut fur Sonnensystemforschung (Germany), Centre Spatiale de Liege (Belgium), Institut d'Optique Theorique et Applique (France), Institut d'Astrophysique Spatiale (France). This work utilizes data obtained by the Global Oscillation Network Group (GONG) Program. GONG is managed by the National Solar Observatory, which is operated by AURA, Inc. under a cooperative agreement with the NSF. The GONG data were acquired by instruments operated by the Big Bear Solar Observatory, High Altitude Observatory, Learmonth Solar Observatory, Udaipur Solar Observatory, Instituto de Astrofisica de Canarias, and Cerro Tololo Interamerican Observatory. NR 15 TC 4 Z9 4 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 NOV PY 2012 VL 281 IS 1 BP 3 EP 20 DI 10.1007/s11207-012-9932-9 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 033QB UT WOS:000310811900002 ER PT J AU Watanabe, T Hara, H Sterling, AC Harra, LK AF Watanabe, T. Hara, H. Sterling, A. C. Harra, L. K. TI Production of High-Temperature Plasmas During the Early Phases of a C9.7 Flare. II. Bi-directional Flows Suggestive of Reconnection in a Pre-flare Brightening Region SO SOLAR PHYSICS LA English DT Article DE Flares, dynamics; Flares, spectrum; Heating, in flares ID ULTRAVIOLET IMAGING SPECTROMETER; LOOP RADIATIVE HYDRODYNAMICS; SOLAR-FLARES; CHROMOSPHERIC EVAPORATION; MAGNETIC RECONNECTION; FILAMENT ERUPTION; HINODE; EMISSION; ONSET; DYNAMICS AB The 6 June 2007 16:55 UT flare was well observed with high time-cadence sparse raster scans by the EUV Imaging Spectrometer (EIS) on board the Hinode spacecraft. The observation covers an active region area of 240 arcsec x 240 arcsec with the 1 arcsec slit in about 160 seconds. We describe here spectral properties of a "pre-flare brightening" to this flare, which started about nine minutes prior to flare-ribbon onset. This flare brightening looks like two small loops apparently having a cusp-shape structure about 40 -aEuro parts per thousand 50 arcsec west of the main flaring loops, which show dynamic behavior in velocity during the early phases of the flare: The He ii line at 256.32 shows the existence of a bi-directional flow along the Sun-Earth line of sight of about -70 and +100 km s(-1). On the other hand, the Fe xvi line at 262.98 formed at higher coronal temperatures shows only a slight increase in intensity at the location of these loops, and the Fe xxiii line at 263.76 barely appears. Electron density at the site derived from the intensity ratios of the Fe xiv line pair at 264.78 and 274.20 is lower than the average of 10(9.3) cm(-3) in other parts of the active-region outskirts. Combining a time series of STEREO-A/B SECCHI-EUVI 171 images, we conclude that the pre-flare-brightening region may be heated via magnetic reconnection taking place as a result of loop-loop interaction. C1 [Watanabe, T.; Hara, H.] Natl Inst Nat Sci, Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan. [Watanabe, T.; Hara, H.] Grad Sch Adv Studies, Hayama, Kanagawa 2400193, Japan. [Sterling, A. C.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. [Sterling, A. C.] JAXA, Inst Space & Astronaut Sci, Chuo Ku, Sagamihara, Kanagawa 2525210, Japan. [Harra, L. K.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. RP Watanabe, T (reprint author), Natl Inst Nat Sci, Natl Astron Observ Japan, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan. EM watanabe@uvlab.mtk.nao.ac.jp; hara@solar.mtk.nao.ac.jp; alphonse.sterling@nasa.gov; lkh@mssl.ucl.ac.uk OI Harra, Louise/0000-0001-9457-6200 FU MEXT, Japan; Sun Microsystems; NAOJ/NINS; NINS inter-institute collaborative program for Creation of New Research Area; NIFS/NINS under the project of Formation of International Network for Scientific Collaborations; NASA's Office of Space Science FX Hinode is a Japanese mission developed and launched by ISAS/JAXA, collaborating with NAOJ as domestic partner, NASA and STFC (UK) as international partners. Scientific operation of the Hinode mission is conducted by the Hinode science team organized at ISAS/JAXA. This team mainly consists of scientists from institutes in the partner countries. Support for the post-launch operation is provided by JAXA and NAOJ (Japan), STFC (UK), NASA (USA), ESA, and NSC (Norway). This work is partly carried out at the NAOJ Hinode Science Center, which was supported by the Grant-in-Aid for Creative Scientific Research: "The Basic Study of Space Weather Prediction" from MEXT, Japan (Head Investigator: K. Shibata), generous donations from Sun Microsystems, and NAOJ/NINS internal funding. It was also supported by NINS inter-institute collaborative program for Creation of New Research Area (Head Investigator: T. Watanabe), and by NIFS/NINS under the project of Formation of International Network for Scientific Collaborations (Head Investigator: H. Yamada). ACS was supported by funding from NASA's Office of Space Science through the Living with a Star and the Supporting Research and Technology programs. NR 27 TC 4 Z9 4 U1 0 U2 4 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-0938 J9 SOL PHYS JI Sol. Phys. PD NOV PY 2012 VL 281 IS 1 BP 87 EP 99 DI 10.1007/s11207-012-0079-5 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 033QB UT WOS:000310811900007 ER PT J AU Kliem, B Torok, T Thompson, WT AF Kliem, B. Toeroek, T. Thompson, W. T. TI A Parametric Study of Erupting Flux Rope Rotation Modeling the "Cartwheel CME" on 9 April 2008 SO SOLAR PHYSICS LA English DT Article DE Corona, active; Prominences, dynamics; Coronal mass ejections, initiation and propagation; Magnetic fields, corona; Magnetohydrodynamics ID CORONAL MASS EJECTIONS; SOLAR ACTIVE REGIONS; KINK INSTABILITY; MAGNETIC CLOUDS; PROMINENCES; FIELD; FILAMENT; SIGMOIDS; STEREO; LINE AB The rotation of erupting filaments in the solar corona is addressed through a parametric simulation study of unstable, rotating flux ropes in bipolar force-free initial equilibrium. The Lorentz force due to the external shear-field component and the relaxation of tension in the twisted field are the major contributors to the rotation in this model, while reconnection with the ambient field is of minor importance, due to the field's simple structure. In the low-beta corona, the rotation is not guided by the changing orientation of the vertical field component's polarity inversion line with height. The model yields strong initial rotations which saturate in the corona and differ qualitatively from the profile of rotation vs. height obtained in a recent simulation of an eruption without preexisting flux rope. Both major mechanisms writhe the flux rope axis, converting part of the initial twist helicity, and produce rotation profiles which, to a large part, are very similar within a range of shear-twist combinations. A difference lies in the tendency of twist-driven rotation to saturate at lower heights than shear-driven rotation. For parameters characteristic of the source regions of erupting filaments and coronal mass ejections, the shear field is found to be the dominant origin of rotations in the corona and to be required if the rotation reaches angles of order 90 degrees and higher; it dominates even if the twist exceeds the threshold of the helical kink instability. The contributions by shear and twist to the total rotation can be disentangled in the analysis of observations if the rotation and rise profiles are simultaneously compared with model calculations. The resulting twist estimate allows one to judge whether the helical kink instability occurred. This is demonstrated for the erupting prominence in the "Cartwheel CME" on 9 April 2008, which has shown a rotation of a parts per thousand aEuro parts per thousand 115(a similar to) up to a height of 1.5 R (aS (TM)) above the photosphere. Out of a range of initial equilibria which include strongly kink-unstable (twist I broken vertical bar=5 pi), weakly kink-unstable (I broken vertical bar=3.5 pi), and kink-stable (I broken vertical bar=2.5 pi) configurations, only the evolution of the weakly kink-unstable flux rope matches the observations in their entirety. C1 [Kliem, B.] Univ Potsdam, Inst Phys & Astron, D-14476 Potsdam, Germany. [Kliem, B.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. [Kliem, B.] George Mason Univ, Coll Sci, Fairfax, VA 22030 USA. [Toeroek, T.] Univ Paris Diderot, UPMC, Observ Paris, CNRS,LESIA, F-92195 Meudon, France. [Thompson, W. T.] NASA, Goddard Space Flight Ctr, Adnet Syst Inc, Greenbelt, MD 20771 USA. RP Kliem, B (reprint author), Univ Potsdam, Inst Phys & Astron, Karl Liebknecht Str 24-25, D-14476 Potsdam, Germany. EM bkliem@uni-potsdam.de FU DFG; STFC; NASA [NNX08AG44G, NNG06EB68C]; European Commission through the SOTERIA Network (EU) [218816]; NASA HTP program; NASA LWS program FX We acknowledge the careful reading of the manuscript and the constructive comments by the referee. BK acknowledges support by the DFG, the STFC, and by NASA through Grant NNX08AG44G. TT's work was partially supported by the European Commission through the SOTERIA Network (EU FP7 Space Science Project No. 218816) and by the NASA HTP and LWS programs. WTT's work was supported by NASA Grant NNG06EB68C. NR 56 TC 30 Z9 30 U1 0 U2 3 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-0938 EI 1573-093X J9 SOL PHYS JI Sol. Phys. PD NOV PY 2012 VL 281 IS 1 BP 137 EP 166 DI 10.1007/s11207-012-9990-z PG 30 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 033QB UT WOS:000310811900010 ER PT J AU Leske, RA Cohen, CMS Mewaldt, RA Christian, ER Cummings, AC Labrador, AW Stone, EC Wiedenbeck, ME von Rosenvinge, TT AF Leske, R. A. Cohen, C. M. S. Mewaldt, R. A. Christian, E. R. Cummings, A. C. Labrador, A. W. Stone, E. C. Wiedenbeck, M. E. von Rosenvinge, T. T. TI Large Proton Anisotropies in the 18 August 2010 Solar Particle Event SO SOLAR PHYSICS LA English DT Article DE Cosmic rays, solar; Energetic particles, propagation; Magnetic fields, interplanetary ID CORONAL MASS EJECTIONS; ENERGETIC PARTICLES; ELECTRON EVENTS; STEREO MISSION; MAGNETIC CLOUD; TELESCOPE; ONSET; TOPOLOGY; PLASMA; WAVES AB The solar particle event observed at STEREO Ahead on 18 August 2010 displayed a rich variety of behavior in the particle anisotropies. Sectored rates measured by the Low Energy Telescope (LET) on STEREO showed very large bidirectional anisotropies in 4-6 MeV protons for the first 17 hours of the event while inside a magnetic cloud, with intensities along the field direction several hundred to nearly 1000 times greater than those perpendicular to the field. At the trailing end of the cloud, the protons became isotropic and their spectrum hardened slightly, while the He/H abundance ratio plunged by a factor of approximately four for about four hours. Associated with the arrival of a shock on 20 August was a series of brief (< 10 minute duration) intensity increases (commonly called "shock spikes") with relatively narrow angular distributions (45(a) FWHM), followed by an abrupt decrease in particle intensities at the shock itself and a reversal of the proton flow to a direction toward the Sun and away from the receding shock. We discuss the STEREO/LET observations of this interesting event in the context of other observations reported in the literature. C1 [Leske, R. A.; Cohen, C. M. S.; Mewaldt, R. A.; Cummings, A. C.; Labrador, A. W.; Stone, E. C.] CALTECH, Pasadena, CA 91125 USA. [Christian, E. R.; von Rosenvinge, T. T.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Wiedenbeck, M. E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Leske, RA (reprint author), CALTECH, Mail Code 290-17, Pasadena, CA 91125 USA. EM ral@srl.caltech.edu RI Christian, Eric/D-4974-2012 OI Christian, Eric/0000-0003-2134-3937 FU National Aeronautics and Space Administration (NASA) at Caltech; JPL from the University of California at Berkeley under NASA [SA2715-26309, NAS5-03131]; NASA [NNX08AK87G, NAS5-00132] FX This work was supported by the National Aeronautics and Space Administration (NASA) at Caltech and JPL under subcontract SA2715-26309 from the University of California at Berkeley under NASA contract NAS5-03131, and by NASA award NNX08AK87G. We thank the PLASTIC (NASA contract NAS5-00132), MAG, and SWEA investigators on STEREO for making their data publicly available. This work benefited greatly from discussions at "The Sun-360 Workshop" held at the Christian-Albrechts-Universitat in Kiel, Germany in July 2011. We thank B. Dotson for help in analyzing the data and in preparing the figures. NR 37 TC 11 Z9 11 U1 0 U2 4 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-0938 J9 SOL PHYS JI Sol. Phys. PD NOV PY 2012 VL 281 IS 1 BP 301 EP 318 DI 10.1007/s11207-012-0018-5 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 033QB UT WOS:000310811900017 ER PT J AU Wood, BE Rouillard, AP Mostl, C Battams, K Savani, NP Marubashi, K Howard, RA Socker, DG AF Wood, B. E. Rouillard, A. P. Moestl, C. Battams, K. Savani, N. P. Marubashi, K. Howard, R. A. Socker, D. G. TI Connecting Coronal Mass Ejections and Magnetic Clouds: A Case Study Using an Event from 22 June 2009 SO SOLAR PHYSICS LA English DT Article DE Coronal mass ejections, initiation and propagation; Coronal mass ejections, interplanetary ID SOLAR-WIND; INNER HELIOSPHERE; WHITE-LIGHT; 1 AU; FLUX; EVOLUTION; RECONSTRUCTION; SIGNATURES; LASCO; CME AB On 27 June 2009 the Wind and Advanced Composition Explorer (ACE) spacecraft near Earth detected a magnetic cloud (MC). The MC can be traced back to a slow coronal mass ejection (CME) launched from the Sun on 22 June 2009 but this connection relies entirely on heliospheric imaging of the Sun-Earth line from the two STEREO spacecraft, illustrating the value of such imaging. The STEREO and SOHO/LASCO views of this event collectively suggest strongly that the CME has the shape of a magnetic flux rope. The arrival times of two density peaks at ACE are consistent with the expected arrival times of the front and back of the flux rope observed in the images, and the velocity of the CME seen by ACE is also consistent with the STEREO measurements. However, the complex nature of the MC signature of this event complicates attempts to compare the flux rope orientations inferred from the imaging and in situ data. Various analyses of the in situ data, performed using both force-free and Grad-Shafranov approaches to MC modeling, yield a wide range of flux rope orientations depending on the type of analysis and on the exact time interval used. The best reproduction of the image-inferred orientation occurs when the first third of the MC time interval is ignored. C1 [Wood, B. E.; Battams, K.; Howard, R. A.; Socker, D. G.] USN, Res Lab, Div Space Sci, Washington, DC 20375 USA. [Rouillard, A. P.] George Mason Univ, Fairfax, VA 22030 USA. [Rouillard, A. P.] IRAP, F-31028 Toulouse 4, France. [Moestl, C.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Moestl, C.] Graz Univ, Inst Phys, Kanzelhohe Observ IGAM, A-8010 Graz, Austria. [Moestl, C.] Austrian Acad Sci, Space Res Inst, A-8042 Graz, Austria. [Savani, N. P.] Nagoya Univ, Solar Terr Environm Lab, Nagoya, Aichi 4648601, Japan. [Savani, N. P.; Marubashi, K.] UCAR, Boulder, CO 80307 USA. [Savani, N. P.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Wood, BE (reprint author), USN, Res Lab, Div Space Sci, Washington, DC 20375 USA. EM brian.wood@nrl.navy.mil RI Savani, Neel/G-4066-2014; OI Savani, Neel/0000-0002-1916-7877; Moestl, Christian/0000-0001-6868-4152 FU NASA [NNH10AN83I]; NASA; NRL; USAF Space Test Program; ONR; Marie Curie International Outgoing Fellowship within European Community; Austrian Science Fund (FWF) [P20145-N16]; European Union [263252] FX This work has been supported by NASA award NNH10AN83I to the Naval Research Laboratory. The STEREO/SECCHI data are produced by a consortium of NRL (US), LMSAL (US), NASA/GSFC (US), RAL (UK), UBHAM (UK), MPS (Germany), CSL (Belgium), IOTA (France), and IAS (France). In addition to funding by NASA, NRL also received support from the USAF Space Test Program and ONR. C. M. was supported by a Marie Curie International Outgoing Fellowship within the 7th European Community Framework Programme, by the Austrian Science Fund (FWF): P20145-N16, and by funding from the European Union Seventh Framework Programme (FP7/2007-2013) under grant agreement no 263252 [COMESEP]. NR 52 TC 7 Z9 7 U1 0 U2 4 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-0938 EI 1573-093X J9 SOL PHYS JI Sol. Phys. PD NOV PY 2012 VL 281 IS 1 BP 369 EP 389 DI 10.1007/s11207-012-0036-3 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 033QB UT WOS:000310811900021 ER PT J AU Simunac, KDC Galvin, AB Farrugia, CJ Kistler, LM Kucharek, H Lavraud, B Liu, YCM Luhmann, JG Ogilvie, KW Opitz, A Popecki, MA Sauvaud, JA Wang, S AF Simunac, K. D. C. Galvin, A. B. Farrugia, C. J. Kistler, L. M. Kucharek, H. Lavraud, B. Liu, Y. C. -M. Luhmann, J. G. Ogilvie, K. W. Opitz, A. Popecki, M. A. Sauvaud, J. -A. Wang, S. TI The Heliospheric Plasma Sheet Observed in situ by Three Spacecraft over Four Solar Rotations SO SOLAR PHYSICS LA English DT Article ID ADVANCED COMPOSITION EXPLORER; CORONAL STREAMERS; MAGNETIC CLOUDS; 1 AU; WIND; INTERFACES; ORIGIN AB In this paper we present in situ observations of the heliospheric plasma sheet (HPS) from STEREO-A, Wind, and STEREO-B over four solar rotations in the declining phase of Solar Cycle 23, covering late March through late June 2007. During this time period the three spacecraft were located in the ecliptic plane, and were gradually separating in heliographic longitude from about 3 degrees to 14 degrees. Crossings of the HPS were identified using the following criteria: reversal of the interplanetary magnetic field sector, enhanced proton density, and local minima in both the proton specific entropy argument and in the alpha particle-to-proton number density ratio (N (a)/N (p)). Two interplanetary coronal mass ejections (ICMEs) were observed during the third solar rotation of our study period, which disrupted the HPS from its quasi-stationary state. We find differences in the in situ proton parameters at the HPS between the three spacecraft despite temporal separations of less than one day. We attribute these differences to both small separations in heliographic latitude and radial evolution of the solar wind leading to the development of compression regions associated with stream interaction regions (SIRs). We also observed a modest enhancement in the density of iron ions at the HPS. C1 [Simunac, K. D. C.; Galvin, A. B.; Farrugia, C. J.; Kistler, L. M.; Kucharek, H.; Liu, Y. C. -M.; Popecki, M. A.; Wang, S.] Univ New Hampshire, Durham, NH 03824 USA. [Luhmann, J. G.] Univ Calif Berkeley, Berkeley, CA 94720 USA. [Ogilvie, K. W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Lavraud, B.; Opitz, A.; Sauvaud, J. -A.] Univ Toulouse, IRAP CNRS UPS, Toulouse, France. [Liu, Y. C. -M.] Chinese Acad Sci, Ctr Space Sci & Appl Res, State Key Lab Space Weather, Beijing, Peoples R China. RP Simunac, KDC (reprint author), Univ New Hampshire, Durham, NH 03824 USA. EM K.Simunac@unh.edu RI Galvin, Antoinette/A-6114-2013; Yong, Liu/H-5333-2011 FU NASA [NAS5-00132, NNX10AQ29G] FX This work was supported at UNH under NASA contract NAS5-00132, and grant NNX10AQ29G. NR 42 TC 6 Z9 6 U1 0 U2 7 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-0938 J9 SOL PHYS JI Sol. Phys. PD NOV PY 2012 VL 281 IS 1 BP 423 EP 447 DI 10.1007/s11207-012-0156-9 PG 25 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 033QB UT WOS:000310811900024 ER PT J AU Farrugia, CJ Harris, B Leitner, M Mostl, C Galvin, AB Simunac, KDC Torbert, RB Temmer, MB Veronig, AM Erkaev, NV Szabo, A Ogilvie, KW Luhmann, JG Osherovich, VA AF Farrugia, C. J. Harris, B. Leitner, M. Moestl, C. Galvin, A. B. Simunac, K. D. C. Torbert, R. B. Temmer, M. B. Veronig, A. M. Erkaev, N. V. Szabo, A. Ogilvie, K. W. Luhmann, J. G. Osherovich, V. A. TI Deep Solar Activity Minimum 2007-2009: Solar Wind Properties and Major Effects on the Terrestrial Magnetosphere SO SOLAR PHYSICS LA English DT Article ID CORONAL MASS EJECTIONS; MAGNETIC-FIELD; QUASI-INVARIANT; BOW SHOCK; PLASMA INSTRUMENT; MAGNETOPAUSE; SATURATION; INDEX; DEPENDENCE; EVOLUTION AB We discuss the temporal variations and frequency distributions of solar wind and interplanetary magnetic field parameters during the solar minimum of 2007-2009 from measurements returned by the IMPACT and PLASTIC instruments on STEREO-A. We find that the density and total field strength were significantly weaker than in the previous minimum. The Alfv,n Mach number was higher than typical. This reflects the weakness of magnetohydrodynamic (MHD) forces, and has a direct effect on the solar wind-magnetosphere interactions. We then discuss two major aspects that this weak solar activity had on the magnetosphere, using data from Wind and ground-based observations: i) the dayside contribution to the cross-polar cap potential (CPCP), and ii) the shapes of the magnetopause and bow shock. For i) we find a low interplanetary electric field of 1.3 +/- 0.9 mV m(-1) and a CPCP of 37.3 +/- 20.2 kV. The auroral activity is closely correlated to the prevalent stream-stream interactions. We suggest that the Alfven wave trains in the fast streams and Kelvin-Helmholtz instability were the predominant agents mediating the transfer of solar wind momentum and energy to the magnetosphere during this three-year period. For ii) we determine 328 magnetopause and 271 bow shock crossings made by Geotail, Cluster 1, and the THEMIS B and C spacecraft during a three-month interval when the daily averages of the magnetic and kinetic energy densities attained their lowest value during the three years under survey. We use the same numerical approach as in Fairfield's (J. Geophys. Res. 76, 7600, 1971) empirical model and compare our findings with three magnetopause models. The stand-off distance of the subsolar magnetopause and bow shock were 11.8 R-E and 14.35 R-E, respectively. When comparing with Fairfield's (1971) classic result, we find that the subsolar magnetosheath is thinner by similar to 1 R-E. This is mainly due to the low dynamic pressure which results in a sunward shift of the magnetopause. The magnetopause is more flared than in Fairfield's model. By contrast the bow shock is less flared, and the latter is the result of weaker MHD forces. C1 [Farrugia, C. J.; Harris, B.; Leitner, M.; Galvin, A. B.; Simunac, K. D. C.; Torbert, R. B.] Univ New Hampshire, Ctr Space Sci, Durham, NH 03824 USA. [Farrugia, C. J.; Harris, B.; Leitner, M.; Galvin, A. B.; Simunac, K. D. C.; Torbert, R. B.] Univ New Hampshire, Dept Phys, Durham, NH 03824 USA. [Leitner, M.] Univ Innsbruck, Inst Astro & Particle Phys, A-6020 Innsbruck, Austria. [Moestl, C.; Temmer, M. B.; Veronig, A. M.] Graz Univ, Inst Phys, Kanzelhohe Observ IGAM, A-8010 Graz, Austria. [Moestl, C.; Temmer, M. B.] Austrian Acad Sci, Space Res Inst, A-8042 Graz, Austria. [Erkaev, N. V.] Russian Acad Sci, Inst Computat Modeling, Krasnoyarsk, Russia. [Erkaev, N. V.] Siberian Fed Univ, Krasnoyarsk, Russia. [Szabo, A.; Ogilvie, K. W.; Osherovich, V. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Moestl, C.; Luhmann, J. G.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. RP Farrugia, CJ (reprint author), Univ New Hampshire, Ctr Space Sci, Durham, NH 03824 USA. EM charlie.farrugia@unh.edu RI Galvin, Antoinette/A-6114-2013; Erkaev, Nikolai/M-1608-2013; Veronig, Astrid/B-8422-2009; OI Erkaev, Nikolai/0000-0001-8993-6400; Moestl, Christian/0000-0001-6868-4152; Temmer, Manuela/0000-0003-4867-7558 FU NASA [NNX10AQ29G, NAS5-03131, NNXO9AR80G]; European Commissions [263253]; Austrian Science Fund (FWF) [FWF V195-N16]; European Community FX We are grateful to the referee for many helpful suggestions. We thank Marc Hairston, Jana Safrankova and Zdenek Nemecek for helpful comments. For the data used in the geomagnetic response section, we thank the World Data Center for Geomagnetism at the Kyoto web site, Japan; the OMNI website at Goddard Space Flight Center, USA; and the Defense Meteorological Satellite Program (DMSP) program, NOAA. Work at UNH was supported by NASA grants NNX10AQ29G and NAS5-03131. This work has received funding from the European Commissions's Seventh Framework Programme (FP7/2007-2013) under the grant agreement No. 263253 [COMESEP]. V.O. was supported by NASA Grant NNXO9AR80G. M.T. greatly acknowledges the Austrian Science Fund (FWF): FWF V195-N16. This research was supported by a Marie Curie International Outgoing Fellowship within the 7th European Community Framework Program. NR 53 TC 7 Z9 7 U1 1 U2 12 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-0938 EI 1573-093X J9 SOL PHYS JI Sol. Phys. PD NOV PY 2012 VL 281 IS 1 BP 461 EP 489 DI 10.1007/s11207-012-0119-1 PG 29 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 033QB UT WOS:000310811900026 ER PT J AU Pesnell, WD AF Pesnell, W. Dean TI Solar Cycle Predictions (Invited Review) SO SOLAR PHYSICS LA English DT Article DE Solar cycle; Predictions ID SUNSPOT NUMBER; SPECTRAL COMPONENTS; MAXIMUM AMPLITUDE; ACTIVITY FORECAST; PRECURSOR METHOD; SOUTH ASYMMETRY; AVERAGE METHOD; SOLAR-CYCLE-24; MINIMUM; MODELS AB Solar cycle predictions are needed to plan long-term space missions, just as weather predictions are needed to plan the launch. Fleets of satellites circle the Earth collecting many types of science data, protecting astronauts, and relaying information. All of these satellites are sensitive at some level to solar cycle effects. Predictions of drag on low-Earth orbit spacecraft are one of the most important. Launching a satellite with less propellant can mean a higher orbit, but unanticipated solar activity and increased drag can make that a Pyrrhic victory as the reduced propellant load is consumed more rapidly. Energetic events at the Sun can produce crippling radiation storms that endanger all assets in space. Solar cycle predictions also anticipate the shortwave emissions that cause degradation of solar panels. Testing solar dynamo theories by quantitative predictions of what will happen in 5-20 years is the next arena for solar cycle predictions. A summary and analysis of 75 predictions of the amplitude of the upcoming Solar Cycle 24 is presented. The current state of solar cycle predictions and some anticipations of how those predictions could be made more accurate in the future are discussed. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Pesnell, WD (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM william.d.pesnell@nasa.gov RI Pesnell, William/D-1062-2012 OI Pesnell, William/0000-0002-8306-2500 FU NASA's Solar Dynamics Observatory at the Goddard Space Flight Center FX This work was supported by NASA's Solar Dynamics Observatory at the Goddard Space Flight Center. NR 128 TC 45 Z9 45 U1 2 U2 12 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-0938 EI 1573-093X J9 SOL PHYS JI Sol. Phys. PD NOV PY 2012 VL 281 IS 1 BP 507 EP 532 DI 10.1007/s11207-012-9997-5 PG 26 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 033QB UT WOS:000310811900029 ER PT J AU Berta, ZK Irwin, J Charbonneau, D Burke, CJ Falco, EE AF Berta, Zachory K. Irwin, Jonathan Charbonneau, David Burke, Christopher J. Falco, Emilio E. TI TRANSIT DETECTION IN THE MEarth SURVEY OF NEARBY M DWARFS: BRIDGING THE CLEAN-FIRST, SEARCH-LATER DIVIDE SO ASTRONOMICAL JOURNAL LA English DT Article DE eclipses; methods: data analysis; planetary systems; stars: low-mass; techniques: photometric ID EARTH GJ 1214B; SOLAR-LIKE VARIABILITY; PLANETARY TRANSITS; LIGHT CURVES; TRANSMISSION SPECTROSCOPY; MONITOR PROJECT; DETECTION ALGORITHMS; STELLAR VARIABILITY; ECLIPSING BINARIES; EXTRASOLAR PLANETS AB In the effort to characterize the masses, radii, and atmospheres of potentially habitable exoplanets, there is an urgent need to find examples of such planets transiting nearby M dwarfs. The MEarth Project is an ongoing effort to do so, as a ground-based photometric survey designed to detect exoplanets as small as 2 R-circle plus. transiting mid-to-late M dwarfs within 33 pc of the Sun. Unfortunately, identifying transits of such planets in photometric monitoring is complicated both by the intrinsic stellar variability that is common among these stars and by the nocturnal cadence, atmospheric variations, and instrumental systematics that often plague Earth-bound observatories. Here, we summarize the properties of MEarth data gathered so far, emphasizing the challenges they present for transit detection. We address these challenges with a new framework to detect shallow exoplanet transits in wiggly and irregularly spaced light curves. In contrast to previous methods that clean trends from light curves before searching for transits, this framework assesses the significance of individual transits simultaneously while modeling variability, systematics, and the photometric quality of individual nights. Our Method for Including Starspots and Systematics in the Marginalized Probability of a Lone Eclipse (MISS MarPLE) uses a computationally efficient semi-Bayesian approach to explore the vast probability space spanned by the many parameters of this model, naturally incorporating the uncertainties in these parameters into its evaluation of candidate events. We show how to combine individual transits processed by MISS MarPLE into periodic transiting planet candidates and compare our results to the popular box-fitting least-squares method with simulations. By applying MISS MarPLE to observations from the MEarth Project, we demonstrate the utility of this framework for robustly assessing the false alarm probability of transit signals in real data. C1 [Berta, Zachory K.; Irwin, Jonathan; Charbonneau, David] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Burke, Christopher J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Burke, Christopher J.] SETI Inst, Mountain View, CA 94043 USA. [Falco, Emilio E.] Smithsonian Astrophys Observ, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA. RP Berta, ZK (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM zberta@cfa.harvard.edu OI Berta-Thompson, Zachory/0000-0002-3321-4924; Charbonneau, David/0000-0002-9003-484X FU David and Lucile Packard Fellowship for Science and Engineering; National Science Foundation (NSF) [AST-0807690] FX We thank Philip Nutzman for inspirational conversations regarding this work; John Johnson, Diana Dragomir, Scott Gaudi, and Elisabeth Newton for discussions regarding the method and the paper; and the referee whose careful reading improved the manuscript considerably. We gratefully acknowledge funding for the MEarth Project from the David and Lucile Packard Fellowship for Science and Engineering and from the National Science Foundation (NSF) under grant No. AST-0807690. The MEarth team is greatly indebted to the staff at the Fred Lawrence Whipple Observatory for their efforts in construction and maintenance of the facility and would like to thank Wayne Peters, Ted Groner, Karen Erdman-Myres, Grace Alegria, Rodger Harris, Bob Hutchins, Dave Martina, Dennis Jankovsky, Tom Welsh, Robert Hyne, Mike Calkins, Perry Berlind, and Gil Esquerdo for their support. This research has made use of NASA's Astro-Physics Data System. NR 98 TC 34 Z9 34 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD NOV PY 2012 VL 144 IS 5 AR 145 DI 10.1088/0004-6256/144/5/145 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 029XI UT WOS:000310530400021 ER PT J AU Griffith, RL Kirkpatrick, JD Eisenhardt, PRM Gelino, CR Cushing, MC Benford, D Blain, A Bridge, CR Cohen, M Cutri, RM Donoso, E Jarrett, TH Lonsdale, C Mace, G Mainzer, A Marsh, K Padgett, D Petty, S Ressler, ME Skrutskie, MF Stanford, SA Stern, D Tsai, CW Wright, EL Wu, JW Yan, L AF Griffith, Roger L. Kirkpatrick, J. Davy Eisenhardt, Peter R. M. Gelino, Christopher R. Cushing, Michael C. Benford, Dominic Blain, Andrew Bridge, Carrie R. Cohen, Martin Cutri, Roc M. Donoso, Emilio Jarrett, Thomas H. Lonsdale, Carol Mace, Gregory Mainzer, A. Marsh, Ken Padgett, Deborah Petty, Sara Ressler, Michael E. Skrutskie, Michael F. Stanford, Spencer A. Stern, Daniel Tsai, Chao-Wei Wright, Edward L. Wu, Jingwen Yan, Lin TI SPITZER PHOTOMETRY OF WISE-SELECTED BROWN DWARF AND HYPER-LUMINOUS INFRARED GALAXY CANDIDATES SO ASTRONOMICAL JOURNAL LA English DT Article DE brown dwarfs; galaxies: evolution; galaxies: high-redshift; galaxies: photometry ID ARRAY CAMERA IRAC; SKY SURVEY 2MASS; SPECTRAL TYPE-L; SURVEY EXPLORER; T-DWARFS; LOW-MASS; SPACE DENSITY; FIELD; WIDE; STARS AB We present Spitzer 3.6 and 4.5 mu m photometry and positions for a sample of 1510 brown dwarf candidates identified by the Wide-field Infrared Survey Explorer (WISE) all-sky survey. Of these, 166 have been spectroscopically classified as objects with spectral types M(1), L(7), T(146), and Y(12). Sixteen other objects are non-(sub) stellar in nature. The remainder are most likely distant L and T dwarfs lacking spectroscopic verification, other Y dwarf candidates still awaiting follow-up, and assorted other objects whose Spitzer photometry reveals them to be background sources. We present a catalog of Spitzer photometry for all astrophysical sources identified in these fields and use this catalog to identify seven fainter (4.5 mu m similar to 17.0 mag) brown dwarf candidates, which are possibly wide-field companions to the original WISE sources. To test this hypothesis, we use a sample of 919 Spitzer observations around WISE-selected high-redshift hyper-luminous infrared galaxy candidates. For this control sample, we find another six brown dwarf candidates, suggesting that the seven companion candidates are not physically associated. In fact, only one of these seven Spitzer brown dwarf candidates has a photometric distance estimate consistent with being a companion to the WISE brown dwarf candidate. Other than this, there is no evidence for any widely separated (>20 AU) ultra-cool binaries. As an adjunct to this paper, we make available a source catalog of similar to 7.33 x 10(5) objects detected in all of these Spitzer follow-up fields for use by the astronomical community. The complete catalog includes the Spitzer 3.6 and 4.5 mu m photometry, along with positionally matched B and R photometry from USNO-B; J, H, and K-s photometry from Two Micron All-Sky Survey; and W1, W2, W3, and W4 photometry from the WISE all-sky catalog. C1 [Griffith, Roger L.; Kirkpatrick, J. Davy; Gelino, Christopher R.; Cutri, Roc M.; Donoso, Emilio; Jarrett, Thomas H.; Tsai, Chao-Wei; Yan, Lin] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA. [Eisenhardt, Peter R. M.; Mainzer, A.; Ressler, Michael E.; Stern, Daniel; Wu, Jingwen] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Cushing, Michael C.] Univ Toledo, Dept Phys & Astron, Toledo, OH 43606 USA. [Benford, Dominic; Padgett, Deborah] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Blain, Andrew] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Bridge, Carrie R.; Cohen, Martin] CALTECH, Dept Astrophys, Pasadena, CA 91125 USA. Monterey Inst Res Astron, Marina, CA 93933 USA. [Lonsdale, Carol] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. [Mace, Gregory; Petty, Sara; Wright, Edward L.] Univ Calif Los Angeles, Dept Astron, Los Angeles, CA USA. [Marsh, Ken] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Skrutskie, Michael F.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. [Stanford, Spencer A.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. RP Griffith, RL (reprint author), CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA. RI Benford, Dominic/D-4760-2012 OI Benford, Dominic/0000-0002-9884-4206 FU National Aeronautics and Space Administration (NASA); National Science Foundation FX 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 (NASA). This publication also makes use of observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. This work is also based in part on observations made with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. Some of the spectroscopic classifications 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. This publication also makes use of data products from 2MASS. 2MASS is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. This research has made use of the NASA/IPAC Infrared Science Archive (IRSA), which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA. NR 36 TC 11 Z9 11 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD NOV PY 2012 VL 144 IS 5 AR 148 DI 10.1088/0004-6256/144/5/148 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 029XI UT WOS:000310530400024 ER PT J AU Jacobson, R Brozovic, M Gladman, B Alexandersen, M Nicholson, PD Veillet, C AF Jacobson, R. Brozovic, M. Gladman, B. Alexandersen, M. Nicholson, P. D. Veillet, C. TI IRREGULAR SATELLITES OF THE OUTER PLANETS: ORBITAL UNCERTAINTIES AND ASTROMETRIC RECOVERIES IN 2009-2011 SO ASTRONOMICAL JOURNAL LA English DT Article DE planets and satellites: individual (Jupiter, Saturn, Uranus, Neptune) ID EPHEMERIDES; FACILITY AB More than 100 small satellites have been identified orbiting the giant planets in distant, inclined, eccentric orbits. Detailed study of these objects requires that their orbits be known well enough to permit routine observations both from the Earth and from spacecraft. Unfortunately, many of the satellites have very poorly known orbits due to a scarcity of astrometric measurements. We have developed a reliable method to estimate the future on-sky position uncertainties of the satellites and have verified that those uncertainties provide a correct measure of the true on-sky positional uncertainty. Based on the uncertainties, we identified a set of satellites that are effectively "lost" and another set that would be lost if additional observations were not obtained in the near future. We attempted recoveries of 26 of the latter group using the Hale 5 m and CFHT 3.6 m telescopes and found 23. This validated our method's predictions and led to significant improvements in our knowledge of the orbits of the recovered moons. There remains a handful of irregular moons which are recoverable and whose orbits will benefit from additional observations during the next decade, while 16 moons of Jupiter and Saturn are essentially lost and will require a re-survey to be located again. C1 [Jacobson, R.; Brozovic, M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Gladman, B.; Alexandersen, M.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. [Nicholson, P. D.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. [Veillet, C.] Canada France Hawaii Telescope Corp, Kameula, HI 96743 USA. RP Jacobson, R (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM robert.jacobson@jpl.nasa.gov OI Alexandersen, Mike/0000-0003-4143-8589 FU National Aeronautics and Space Administration FX Thanks to Palomar and CFHT staff for assisting us in the acquisition of the recovery observations. The research described in this publication was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. NR 19 TC 7 Z9 7 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD NOV PY 2012 VL 144 IS 5 AR 132 DI 10.1088/0004-6256/144/5/132 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 029XI UT WOS:000310530400008 ER PT J AU Mazzarella, JM Iwasawa, K Vavilkin, T Armus, L Kim, DC Bothun, G Evans, AS Spoon, HWW Haan, S Howell, JH Lord, S Marshall, JA Ishida, CM Xu, CK Petric, A Sanders, DB Surace, JA Appleton, P Chan, BHP Frayer, DT Inami, H Khachikian, EY Madore, BF Privon, GC Sturm, E Vivian, U Veilleux, S AF Mazzarella, J. M. Iwasawa, K. Vavilkin, T. Armus, L. Kim, D. -C. Bothun, G. Evans, A. S. Spoon, H. W. W. Haan, S. Howell, J. H. Lord, S. Marshall, J. A. Ishida, C. M. Xu, C. K. Petric, A. Sanders, D. B. Surace, J. A. Appleton, P. Chan, B. H. P. Frayer, D. T. Inami, H. Khachikian, E. Ye. Madore, B. F. Privon, G. C. Sturm, E. Vivian, U. Veilleux, S. TI INVESTIGATION OF DUAL ACTIVE NUCLEI, OUTFLOWS, SHOCK-HEATED GAS, AND YOUNG STAR CLUSTERS IN MARKARIAN 266 SO ASTRONOMICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: interactions; galaxies: nuclei; galaxies: Seyfert; galaxies: starburst; galaxies: star clusters: general ID ULTRALUMINOUS INFRARED GALAXIES; SPITZER-SPACE-TELESCOPE; SUPERMASSIVE BLACK-HOLES; DARK-MATTER HALOS; SKY LIRG SURVEY; X-RAY; GALACTIC NUCLEI; SEYFERT-GALAXIES; LUMINOSITY FUNCTION; ANTENNAE GALAXIES AB Results of observations with the Spitzer, Hubble, GALEX, Chandra, and XMM-Newton space telescopes are presented for the luminous infrared galaxy (LIRG) merger Markarian 266. The SW (Seyfert 2) and NE (LINER) nuclei reside in galaxies with Hubble types SBb (pec) and S0/a (pec), respectively. Both companions are more luminous than L* galaxies and they are inferred to each contain a approximate to 2.5 x 10(8) M-circle dot black hole. Although the nuclei have an observed hard X-ray flux ratio of f(X)(NE)/f(X)(SW) = 6.4, Mrk 266 SW is likely the primary source of a bright Fe K alpha line detected from the system, consistent with the reflection-dominated X-ray spectrum of a heavily obscured active galactic nucleus (AGN). Optical knots embedded in an arc with aligned radio continuum radiation, combined with luminous H-2 line emission, provide evidence for a radiative bow shock in an AGN-driven outflow surrounding the NE nucleus. A soft X-ray emission feature modeled as shock-heated plasma with T similar to 10(7) K is cospatial with radio continuum emission between the galaxies. Mid-infrared diagnostics provide mixed results, but overall suggest a composite system with roughly equal contributions of AGN and starburst radiation powering the bolometric luminosity. Approximately 120 star clusters have been detected, with most having estimated ages less than 50 Myr. Detection of 24 mu m emission aligned with soft X-rays, radio continuum, and ionized gas emission extending similar to 34 '' (20 kpc) north of the galaxies is interpreted as similar to 2 x 10(7) M-circle dot of dust entrained in an outflowing superwind. At optical wavelengths this Northern Loop region is resolved into a fragmented morphology indicative of Rayleigh-Taylor instabilities in an expanding shell of ionized gas. Mrk 266 demonstrates that the dust "blowout" phase can begin in a LIRG well before the galaxies fully coalesce during a subsequent ultraluminous infrared galaxy (ULIRG) phase, and rapid gas consumption in luminous dual AGNs with kiloparsec-scale separations early in the merger process may explain the paucity of detected binary QSOs (with parsec-scale orbital separations) in spectroscopic surveys. An evolutionary sequence is proposed representing a progression from dual to binary AGNs, accompanied by an increase in observed L-x/L-ir ratios by over two orders of magnitude. C1 [Mazzarella, J. M.; Chan, B. H. P.; Madore, B. F.] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA. [Iwasawa, K.] Univ Barcelona IEEC UB, ICREA, E-08028 Barcelona, Spain. [Iwasawa, K.] Univ Barcelona, IEEC UB, Inst Ciencies Cosmos, E-08028 Barcelona, Spain. [Vavilkin, T.] SUNY Stony Brook, Dept Phys & Astron, Stony Brook, NY 11794 USA. [Armus, L.; Haan, S.; Howell, J. H.; Marshall, J. A.; Petric, A.; Surace, J. A.; Inami, H.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Kim, D. -C.; Evans, A. S.; Privon, G. C.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. [Kim, D. -C.; Evans, A. S.; Frayer, D. T.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. [Bothun, G.] Univ Oregon, Dept Phys, Eugene, OR 97402 USA. [Spoon, H. W. W.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. [Haan, S.] ATNF, CSIRO Astron & Space Sci, Marsfield, NSW 2122, Australia. [Lord, S.; Xu, C. K.; Appleton, P.] CALTECH, NASA, Herschel Sci Ctr, Pasadena, CA 91125 USA. [Marshall, J. A.; Petric, A.] CALTECH, Dept Astron, Pasadena, CA 91125 USA. [Ishida, C. M.] Natl Astron Observ Japan, Hilo, HI 96720 USA. [Sanders, D. B.; Vivian, U.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Khachikian, E. Ye.] Natl Acad Sci Armenia, Byurakan Astrophys Observ, Byurakan 378433, Aragatsodn Prov, Armenia. [Madore, B. F.] Carnegie Inst Washington Observ, The Observ, Pasadena, CA 91101 USA. [Sturm, E.] Max Planck Inst Extraterr Phys, D-85741 Garching, Germany. [Veilleux, S.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. RP Mazzarella, JM (reprint author), CALTECH, Ctr Infrared Proc & Anal, MS 100-22, Pasadena, CA 91125 USA. EM mazz@ipac.caltech.edu; kazushi.iwasawa@icc.ub.edu; vavilkin@grad.physics.sunysb.edu; lee@ipac.caltech.edu; dkim@nrao.edu; nuts@bigmoo.uoregon.edu; aevans@virginia.edu; spoon@isc.astro.cornell.edu; haan@ipac.caltech.edu; jhhowell@ipac.caltech.edu; lord@ipac.caltech.edu; jason.mashall@caltech.edu; cmishida@mac.com; cxu@ipac.caltech.edu; ap@astro.caltech.edu; sanders@ifa.hawaii.edu; jason@ipac.caltech.edu; apple@ipac.caltech.edu; bchan@ipac.caltech.edu; dfrayer@nrao.edu; inami@ipac.caltech.edu; khache@bao.sci.am; barry@obs.carnegiescience.edu; gcp8y@virginia.edu; sturm@mpe.mpg.de; vivian@ifa.hawaii.edu; veilleux@astro.umd.edu OI Mazzarella, Joseph/0000-0002-8204-8619; Appleton, Philip/0000-0002-7607-8766; Privon, George/0000-0003-3474-1125 FU Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA; NASA/ESA Hubble Space Telescope; Association of Universities for Research in Astronomy, Inc. under NASA [NAS5-26555]; Chandra X-ray Observatory Center; Smithsonian Astrophysical Observatory for and on behalf of NASA [NAS8-03060]; Galaxy Evolution Explorer (GALEX); NASA by the California Institute of Technology under NASA [NAS5-98034]; JPL/Caltech [Spitzer PID 3672, HST-GO10592.01-A, 11235]; Spanish grant MICINN [AYA2010-21782-C03-01]; NASA FX This work is based on observations with the following facilities: the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA, the NASA/ESA Hubble Space Telescope, which is operated by the Association of Universities for Research in Astronomy, Inc. under NASA contract NAS5-26555, the Chandra X-ray Observatory Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of NASA under contract NAS8-03060, and the Galaxy Evolution Explorer (GALEX), which is operated for NASA by the California Institute of Technology under NASA contract NAS5-98034. The Aladin (CDS, Strasbourg) and SAOImage DS9 tools were used for image analysis. Support for this work was provided by the following NASA grants: an award issued by JPL/Caltech (Spitzer PID 3672, PI: J. Mazzarella); HST-GO10592.01-A (ACS imaging, PI: A. Evans) and program 11235 (NICMOS imaging, PI: J. Surace) issued by the STScI. K. Iwasawa acknowledges support from Spanish grant MICINN (AYA2010-21782-C03-01). This research made use of the NASA/IPAC Extragalactic Database (NED) and the Infrared Science Archive (IRSA), which are operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA. We thank Masa Imanishi for providing FITS files for the NobeyamaMillimeter Array observations and Tsuyoshi Ishigaki for supplying optical emission-line images. We thank ChrisMihos for helpful discussions regarding merger timescales. Finally, we thank the anonymous referee for very helpful comments that led to improvements to the manuscript. NR 176 TC 20 Z9 20 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD NOV PY 2012 VL 144 IS 5 AR 125 DI 10.1088/0004-6256/144/5/125 PG 43 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 029XI UT WOS:000310530400001 ER PT J AU Mizusawa, TF Rebull, LM Stauffer, JR Bryden, G Meyer, M Song, I AF Mizusawa, Trisha F. Rebull, Luisa M. Stauffer, John R. Bryden, Geoffrey Meyer, Michael Song, Inseok TI EXPLORING THE EFFECTS OF STELLAR ROTATION AND WIND CLEARING: DEBRIS DISKS AROUND F STARS SO ASTRONOMICAL JOURNAL LA English DT Article DE circumstellar matter; infrared: stars ID SPITZER-SPACE-TELESCOPE; SOLAR-TYPE STARS; GENEVA-COPENHAGEN SURVEY; LOW-MASS STARS; MULTIBAND IMAGING PHOTOMETER; ANGULAR-MOMENTUM EVOLUTION; MAIN-SEQUENCE STARS; SUN-LIKE STARS; ALL-SKY SURVEY; T-TAURI STARS AB We have conducted a study of debris disks around F stars in order to explore correlations between rotation, stellar winds, and circumstellar disks. We obtained new 24 mu m photometry from the Multiband Imaging Photometer for Spitzer (MIPS) camera for a sample of 188 relatively nearby F dwarfs with various rotation rates and optical colors, and combined it with archival MIPS data for 66 more F stars, as well as Wide-field Infrared Survey Explorer data for the entire sample, plus 9 more F stars. Based on the objects' K-s - [24] and [3.4] - [22] colors, we identify 22 stars in our sample as having 22 and/or 24 mu m excesses above our detection limit, 13 of which are new discoveries. Our overall disk detection rate is 22/263, or 8%, consistent with previous determinations of disk fractions in the solar neighborhood. While fast-rotating stars are expected to have strong winds capable of efficiently removing dust, we find no correlation between rotational velocity and infrared excess. Similarly, we find no significant difference in excess detection rate between late-type F stars, which have convective surfaces, and early-type F stars, which have fully radiative envelopes. However, the essentially unknown range of ages in this sample may be washing out any effects relating rotation, winds, and disks. C1 [Mizusawa, Trisha F.] Florida Inst Technol, Melbourne, FL 32901 USA. [Rebull, Luisa M.; Stauffer, John R.] CALTECH, SSC, Pasadena, CA 91125 USA. [Bryden, Geoffrey] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Meyer, Michael] ETH, Zurich, Switzerland. [Song, Inseok] Univ Georgia, Dept Phys & Astron, Athens, GA 30602 USA. [Mizusawa, Trisha F.; Bryden, Geoffrey] CALTECH, NASA Star & Exoplanet Database NStED, Pasadena, CA 91125 USA. RP Mizusawa, TF (reprint author), Florida Inst Technol, 150 W Univ Blvd, Melbourne, FL 32901 USA. EM trisha.mizusawa@gmail.com OI Rebull, Luisa/0000-0001-6381-515X FU NASA; National Aeronautics and Space Administration; National Science Foundation; U.S. Government [NAG W-2166] FX This work is based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech. The research described in this paper was partially carried out at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. This research has made use of what was then called the NASA/IPAC/NExScI Star and Exoplanet Database, which was operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration.; This research has made use of NASA's Astrophysics Data System (ADS) Abstract Service, and of the SIMBAD database, operated at CDS, Strasbourg, France. This research has made use of data products from the Two Micron All Sky Survey (2MASS), which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center, funded by the National Aeronautics and Space Administration and the National Science Foundation. 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 WISE and 2MASS data are served by the NASA/IPAC Infrared Science Archive, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. This research has made use of the Digitized Sky Surveys, which were produced at the Space Telescope Science Institute under U.S. Government grant NAG W-2166. NR 62 TC 10 Z9 10 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD NOV PY 2012 VL 144 IS 5 AR 135 DI 10.1088/0004-6256/144/5/135 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 029XI UT WOS:000310530400011 ER PT J AU Stevenson, R Jewitt, D AF Stevenson, Rachel Jewitt, David TI NEAR-NUCLEUS PHOTOMETRY OF OUTBURSTING COMET 17P/HOLMES SO ASTRONOMICAL JOURNAL LA English DT Article DE comets: general; comets: individual (17P/Holmes) ID FRANCE-HAWAII-TELESCOPE; BAND PHOTOMETRY; OBJECTS; COLORS; GRAINS; SYSTEM; RATES AB Comet 17P/Holmes underwent the largest cometary outburst in recorded history on UT 2007 October 23, releasing massive quantities of dust and gas. We used the Canada-France-Hawaii Telescope to obtain wide-field images of 17P/Holmes on 15 dates over a period of three months following the outburst and employ them here to examine the subsequent activity of the nucleus and the nature of the ejecta closest to the nucleus. Through aperture photometry we observed the inner coma (within 2500 km of the nucleus) to fade from an apparent magnitude of 11.7 mag to 17.6 mag, corresponding to absolute magnitudes of 8.1 mag and 12.4 mag, between UT 2007 November 6 and 2008 February 12. A second much smaller outburst occurred on UT 2007 November 12, three weeks after the original outburst, suggesting that the nucleus remained unstable. The surface brightness profile of the inner coma was consistently shallow relative to the expected steady-state profile, and showed a persistent brightness enhancement within similar to 5000 km of the nucleus. We propose that sublimating ice grains created an ice grain halo around the nucleus, while fragmenting grains were responsible for the shallow surface brightness profile. C1 [Jewitt, David] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Stevenson, Rachel; Jewitt, David] Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90095 USA. RP Stevenson, R (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Rachel.A.Stevenson@jpl.nasa.gov; jewitt@ucla.edu FU NASA Outer Planets Research Program; NASA Postdoctoral Fellowship Program; National Aeronautics and Space Administration FX Based on observations obtained with MegaPrime/MegaCam, a joint project of CFHT and CEA/DAPNIA, at the Canada-France-Hawaii Telescope (CFHT) which is operated by the National Research Council (NRC) of Canada, the Institut National des Science de l'Univers of the Centre National de la Recherche Scientifique (CNRS) of France, and the University of Hawaii. This work is based in part on data products produced at the TERAPIX data center located at the Institut d'Astrophysique de Paris. We appreciate grant support from the NASA Outer Planets Research Program to D.J. R.S. acknowledges support from the NASA Postdoctoral Fellowship Program. 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 33 TC 7 Z9 7 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD NOV PY 2012 VL 144 IS 5 AR 138 DI 10.1088/0004-6256/144/5/138 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 029XI UT WOS:000310530400014 ER PT J AU Gettings, DP Gonzalez, AH Stanford, SA Eisenhardt, PRM Brodwin, M Mancone, C Stern, D Zeimann, GR Masci, FJ Papovich, C Tanaka, I Wright, EL AF Gettings, Daniel P. Gonzalez, Anthony H. Stanford, S. Adam Eisenhardt, Peter R. M. Brodwin, Mark Mancone, Conor Stern, Daniel Zeimann, Gregory R. Masci, Frank J. Papovich, Casey Tanaka, Ichi Wright, Edward L. TI THE MASSIVE DISTANT CLUSTERS OF WISE SURVEY: THE FIRST DISTANT GALAXY CLUSTER DISCOVERED BY WISE SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE galaxies: clusters: individual (MOO J2342.0+1301); galaxies: distances and redshifts; galaxies: evolution ID STELLAR POPULATION SYNTHESIS; DIGITAL SKY SURVEY; DARK-MATTER; TELESCOPE; Z=1.75; RESOLUTION; EXISTENCE; UNIVERSE; CATALOG; MODELS AB We present spectroscopic confirmation of a z = 0.99 galaxy cluster discovered using data from the Wide-field Infrared Survey Explorer (WISE). This is the first z similar to 1 cluster candidate from the Massive Distant Clusters of WISE Survey to be confirmed. It was selected as an overdensity of probable z greater than or similar to 1 sources using a combination of WISE and Sloan Digital Sky Survey DR8 photometric catalogs. Deeper follow-up imaging data from Subaru and WIYN reveal the cluster to be a rich system of galaxies, and multi-object spectroscopic observations from Keck confirm five cluster members at z = 0.99. The detection and confirmation of this cluster represents a first step toward constructing a uniformly selected sample of distant, high-mass galaxy clusters over the full extragalactic sky using WISE data. C1 [Gettings, Daniel P.; Gonzalez, Anthony H.; Mancone, Conor] Univ Florida, Dept Astron, Bryant Space Ctr 211, Gainesville, FL 32611 USA. [Stanford, S. Adam] Lawrence Livermore Natl Lab, Inst Geophys & Planetary Phys, Livermore, CA 94550 USA. [Stanford, S. Adam; Zeimann, Gregory R.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. [Eisenhardt, Peter R. M.; Stern, Daniel] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Brodwin, Mark] Univ Missouri, Dept Phys & Astron, Kansas City, MO 64110 USA. [Masci, Frank J.] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA. [Papovich, Casey] Texas A&M Univ, Dept Phys & Astron, College Stn, TX 77843 USA. [Papovich, Casey] Texas A&M Univ, George P & Cynthia Woods Mitchell Inst Fundamenta, College Stn, TX 77843 USA. [Tanaka, Ichi] Natl Inst Nat Sci, Natl Astron Observ Japan, Subaru Telescope, Hilo, HI 96720 USA. [Wright, Edward L.] UCLA Astron, Los Angeles, CA 90095 USA. RP Gettings, DP (reprint author), Univ Florida, Dept Astron, Bryant Space Ctr 211, Gainesville, FL 32611 USA. FU National Aeronautics and Space Administration (NASA); NASA Astrophysics Data Analysis Program (ADAP) [NNX12AE15G]; W.M. Keck Foundation FX The authors thank the anonymous referee whose comments improved the quality of the manuscript. 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 (NASA). D. P. G. and A. H. G. acknowledge support for this research from the NASA Astrophysics Data Analysis Program (ADAP) through grant NNX12AE15G. 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. Based in part on data collected at Subaru Telescope, which is operated by the National Astronomical Observatory of Japan. D. P. G. was a Visiting Astronomer, Kitt Peak National Observatory, National Optical Astronomy Observatory, which is operated by the Association of Universities for Research in Astronomy (AURA) under cooperative agreement with the National Science Foundation. The WIY