FN Thomson Reuters Web of Science™ VR 1.0 PT J AU Ferraz, A Saatchi, S Mallet, C Jacquemoud, S Goncalves, G Silva, CA Soares, P Tome, M Pereira, L AF Ferraz, Antonio Saatchi, Sassan Mallet, Clement Jacquemoud, Stephane Goncalves, Gil Silva, Carlos Alberto Soares, Paula Tome, Margarida Pereira, Luisa TI Airborne Lidar Estimation of Aboveground Forest Biomass in the Absence of Field Inventory SO REMOTE SENSING LA English DT Article DE airborne laser scanning; lidar; 3D point cloud clustering; multi-layered forest structure; biomass; carbon; individual tree extraction; crown delineation; vegetation cover ID CARBON STOCKS; TREES; COVER; MODEL AB The scientific community involved in the UN-REDD program is still reporting large uncertainties about the amount and spatial variability of CO2 stored in forests. The main limitation has been the lack of field samplings over space and time needed to calibrate and convert remote sensing measurements into aboveground biomass (AGB). As an alternative to costly field inventories, we examine the reliability of state-of-the-art lidar methods to provide direct retrieval of many forest metrics that are commonly collected through field sampling techniques (e.g., tree density, individual tree height, crown cover). AGB is estimated using existing allometric equations that are fed by lidar-derived metrics at either the individual tree-or forest layer-level (for the overstory or underneath layers, respectively). Results over 40 plots of a multilayered forest located in northwest Portugal show that the lidar method provides AGB estimates with a relatively small random error (RMSE = of 17.1%) and bias (of 4.6%). It provides local AGB baselines that meet the requirements in terms of accuracy to calibrate satellite remote sensing measurements (e.g., the upcoming lidar GEDI (Global Ecosystem Dynamics Investigation), and the Synthetic Aperture Radar (SAR) missions NISAR (National Aeronautics and Space Administration and Indian Space Research Organization SAR) and BIOMASS from the European Space Agency, ESA) for AGB mapping purposes. The development of similar techniques over a variety of forest types would be a significant improvement in quantifying CO2 stocks and changes to comply with the UN-REDD policies. C1 [Ferraz, Antonio; Saatchi, Sassan] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Mallet, Clement] Univ Paris Est, MATIS, Inst Natl Informat Geog & Forestiere IGN LaSTIG, F-94160 St Mande, France. [Jacquemoud, Stephane] Univ Paris Diderot, Sorbonne Paris Cite, CNRS, Inst Phys Globe Paris,UMR 7154, F-75013 Paris, France. [Goncalves, Gil] Univ Coimbra, INESC Coimbra, P-3001501 Coimbra, Portugal. [Goncalves, Gil] Univ Coimbra, Dept Math, P-3001501 Coimbra, Portugal. [Silva, Carlos Alberto] Univ Idaho, Coll Nat Resources, Dept Nat Resources & Soc, Moscow, ID 83843 USA. [Soares, Paula; Tome, Margarida] Univ Lisbon, Sch Agron, Forest Res Ctr, P-1349017 Lisbon, Portugal. [Pereira, Luisa] Univ Aveiro, Escola Super Tecnol & Gestao Agueda, P-3754909 Agueda, Portugal. RP Ferraz, A (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Antonio.A.Ferraz@jpl.nasa.gov; Sasan.S.Saatchi@jpl.nasa.gov; clement.mallet@ign.fr; jacquemoud@ipgp.fr; gil@mat.uc.pt; csilva@uidaho.edu; paulasoares@isa.ulisboa.pt; magatome@isa.ulisboa.pt; luisapereira@ua.pt RI Soares, Paula/F-8251-2010; Jacquemoud, Stephane/F-8842-2010; Tome, Margarida/F-5776-2010; Ferraz, Antonio/D-9662-2017; OI Soares, Paula/0000-0002-7603-5467; Tome, Margarida/0000-0002-6242-8593; Ferraz, Antonio/0000-0002-5328-5471; Mallet, Clement/0000-0002-2675-165X FU Portuguese Foundation for Science and Technology - European Fund of Regional Development (FEDER) through COMPETE-Operational Factors of Competitiveness Program (POFC) [PTDC/AGR-CFL/72380/2006]; Jet Propulsion Laboratory through the NASA; NASA; [Pest-OE/EEI/UI308/2014] FX This work was supported in part by the Portuguese Foundation for Science and Technology under Grant PTDC/AGR-CFL/72380/2006, co-financed by the European Fund of Regional Development (FEDER) through COMPETE-Operational Factors of Competitiveness Program (POFC) and the Grant Pest-OE/EEI/UI308/2014. The work of Antonio Ferraz was supported in part by the Jet Propulsion Laboratory through the NASA Postdoctoral Program, which was administrated by the Oak Ridge Associated Universities through a contract with NASA. NR 43 TC 0 Z9 0 U1 25 U2 25 PU MDPI AG PI BASEL PA ST ALBAN-ANLAGE 66, CH-4052 BASEL, SWITZERLAND SN 2072-4292 J9 REMOTE SENS-BASEL JI Remote Sens. PD AUG PY 2016 VL 8 IS 8 AR 653 DI 10.3390/rs8080653 PG 18 WC Remote Sensing SC Remote Sensing GA DU8JI UT WOS:000382458700040 ER PT J AU Hannon, A Lu, YJ Li, J Meyyappan, M AF Hannon, Ami Lu, Yijiang Li, Jing Meyyappan, M. TI A Sensor Array for the Detection and Discrimination of Methane and Other Environmental Pollutant Gases SO SENSORS LA English DT Article DE gas sensor; room temperature gas sensing; functionalized nanotubes; principal component analysis; electronic nose; selective methane sensor; smartphone based sensor ID WALLED CARBON NANOTUBES; CONDUCTING POLYMER; CHEMICAL SENSORS; MECHANOCHEMICAL REACTION; ACID CATALYST; THIN-FILMS; POLYANILINE; FABRICATION; ADSORPTION; OXIDATION AB We address the sensitive detection and discrimination of gases impacting the environment, such as CH4, NH3, SO2, and CO, using a sensor array and aided by principal component analysis (PCA). A 32-element chemiresistive sensor array consisting of nine different sensor materials including seven types of modified single-walled carbon nanotubes and two types of polymers has been constructed. PCA results demonstrate excellent discriminating ability of the chemiresistor sensor chip in the 1-30 ppm concentration range. The accuracy of the sensor was verified against data collected using cavity ring down spectroscopy. The sensor chip has also been integrated with a smartphone and has been shown to reproduce the sensing performance obtained with the laboratory measurement system. C1 [Hannon, Ami; Lu, Yijiang; Li, Jing; Meyyappan, M.] NASA Ames Res Ctr, Moffett Field, CA 94035 USA. [Hannon, Ami] NASA Ames Res Ctr, Analty Mech Associates Inc, Moffett Field, CA 94035 USA. [Lu, Yijiang] NASA Ames Res Ctr, ELORET Corp, Moffett Field, CA 94035 USA. RP Meyyappan, M (reprint author), NASA Ames Res Ctr, Moffett Field, CA 94035 USA. EM ami.m.hannon@nasa.gov; yijiang.lu-1@nasa.gov; jing.li-1@nasa.gov; m.meyyappan@nasa.gov FU US Department of Homeland Security, HSARPA Cell-All program via NASA-DHS [IAA: HSHQDC-08-X-00870]; AMA and ELORET Corporation FX The smartphone development was funded by the US Department of Homeland Security, HSARPA Cell-All program via a NASA-DHS interagency agreement (IAA: HSHQDC-08-X-00870). The work conducted by the employees of AMA and ELORET Corporation was supported through subcontracts to the respective organizations. The authors acknowledge George Yu and Chang Hsiung for their help with the smartphone sensor and Matt Fladeland for providing the Picarro Instrument. NR 52 TC 1 Z9 1 U1 31 U2 31 PU MDPI AG PI BASEL PA ST ALBAN-ANLAGE 66, CH-4052 BASEL, SWITZERLAND SN 1424-8220 J9 SENSORS-BASEL JI Sensors PD AUG PY 2016 VL 16 IS 8 AR 1163 DI 10.3390/s16081163 PG 11 WC Chemistry, Analytical; Electrochemistry; Instruments & Instrumentation SC Chemistry; Electrochemistry; Instruments & Instrumentation GA DU6KJ UT WOS:000382323200151 ER PT J AU Molter, EM Nixon, CA Cordiner, MA Serigano, J Irwin, PGJ Teanby, NA Charnley, SB Lindberg, JE AF Molter, Edward M. Nixon, C. A. Cordiner, M. A. Serigano, J. Irwin, P. G. J. Teanby, N. A. Charnley, S. B. Lindberg, J. E. TI ALMA OBSERVATIONS OF HCN AND ITS ISOTOPOLOGUES ON TITAN SO ASTRONOMICAL JOURNAL LA English DT Article DE planets and satellites: atmospheres; planets and satellites: individual (Titan) ID ISOTOPIC-RATIOS; HETERODYNE OBSERVATIONS; VERTICAL DISTRIBUTIONS; SUB-DOPPLER; ATMOSPHERE; SPECTROSCOPY; HC3N; ISOTOPOMERS; C-12/C-13; NITRILES AB We present sub-millimeter spectra of HCN isotopologues on Titan, derived from publicly available ALMA flux calibration observations of Titan taken in early 2014. We report the detection of a new HCN isotopologue on Titan, (HCN)-C-13-N-15, and confirm an earlier report of detection of DCN. We model high signal-to-noise observations of HCN, (HCN)-C-13, (HCN)-N-15, DCN, and (HCN)-C-13-N-15 to derive abundances and infer the following isotopic ratios: C-12/C-13 = 89.8 +/- 2.8, N-14/N-15 = 72.3 +/- 2.2, D/H = (2.5 +/- 0.2) x 10(-4), and HCN/(HCN)-C-13-N-15 = 5800 +/- 270 (1 sigma errors). The carbon and nitrogen ratios are consistent with and improve on the precision of previous results, confirming a factor of similar to 2.3 elevation in N-14/N-15 in HCN compared to N-2 and a lack of fractionation in C-12/C-13 from the protosolar value. This is the first published measurement of D/H in a nitrile species on Titan, and we find evidence for a factor of similar to 2 deuterium enrichment in hydrogen cyanide compared to methane. The isotopic ratios we derive may be used as constraints for future models to better understand the fractionation processes occurring in Titan's atmosphere. C1 [Molter, Edward M.; Nixon, C. A.; Cordiner, M. A.; Charnley, S. B.; Lindberg, J. E.] NASA, Goddard Space Flight Ctr, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA. [Molter, Edward M.; Cordiner, M. A.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA. [Serigano, J.] Johns Hopkins Univ, Dept Earth & Planetary Sci, Baltimore, MD 21218 USA. [Irwin, P. G. J.] Univ Oxford, Clarendon Lab, Atmospher Ocean & Planetary Phys, Parks Rd, Oxford OX1 3PU, England. [Teanby, N. A.] Univ Bristol, Sch Earth Sci, Wills Mem Bldg,Queens Rd, Bristol BS8 1RJ, Avon, England. RP Molter, EM (reprint author), NASA, Goddard Space Flight Ctr, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA.; Molter, EM (reprint author), Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA. EM edward.m.molter@nasa.gov RI Nixon, Conor/A-8531-2009; OI Nixon, Conor/0000-0001-9540-9121; Irwin, Patrick/0000-0002-6772-384X FU NASA's Planetary Atmospheres program; NASA's Planetary Astronomy program FX This research was supported by NASA's Planetary Atmospheres and Planetary Astronomy programs. NR 43 TC 0 Z9 0 U1 5 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD AUG PY 2016 VL 152 IS 2 AR 42 DI 10.3847/0004-6256/152/2/42 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DT9KG UT WOS:000381817500015 ER PT J AU Prsa, A Harmanec, P Torres, G Mamajek, E Asplund, M Capitaine, N Christensen-Dalsgaard, J Depagne, E Haberreiter, M Hekker, S Hilton, J Kopp, G Kostov, V Kurtz, DW Laskar, J Mason, BD Milone, EF Montgomery, M Richards, M Schmutz, W Schou, J Stewart, SG AF Prsa, Andrej Harmanec, Petr Torres, Guillermo Mamajek, Eric Asplund, Martin Capitaine, Nicole Christensen-Dalsgaard, Jorgen Depagne, Eric Haberreiter, Margit Hekker, Saskia Hilton, James Kopp, Greg Kostov, Veselin Kurtz, Donald W. Laskar, Jacques Mason, Brian D. Milone, Eugene F. Montgomery, Michele Richards, Mercedes Schmutz, Werner Schou, Jesper Stewart, Susan G. TI NOMINAL VALUES FOR SELECTED SOLAR AND PLANETARY QUANTITIES: IAU 2015 RESOLUTION B3 SO ASTRONOMICAL JOURNAL LA English DT Article DE planets and satellites: fundamental parameters; standards; stars: fundamental parameters; stars: general; Sun: fundamental parameters ID STELLAR ASTROPHYSICS MESA; STARS; CONSTANTS; MODULES; PARAMETERS; ACCURACY; BINARIES; SET AB In this brief communication we provide the rationale for. and the outcome of the International Astronomical Union (IAU) resolution vote at the XXIXth General Assembly in Honolulu, Hawaii, in 2015, on recommended nominal conversion constants for selected solar and planetary properties. The problem addressed by the resolution is a lack of established conversion constants between solar and planetary values and SI units: a missing standard has caused a proliferation of solar values (e.g., solar radius, solar irradiance, solar luminosity, solar effective temperature, and solar mass parameter) in the literature, with cited solar values typically based on best estimates at the time of paper writing. As precision of observations increases, a set of consistent values becomes increasingly important. To address this, an IAU Working Group on Nominal Units for Stellar and Planetary Astronomy formed in 2011, uniting experts from the solar, stellar, planetary, exoplanetary, and fundamental astronomy, as well as from general standards. fields to converge on optimal values for nominal conversion constants. The effort resulted in the IAU 2015 Resolution B3, passed at the IAU General Assembly by a large majority. The resolution recommends the use of nominal solar and planetary values, which are by definition exact and are expressed in SI units. These nominal values should be understood as conversion factors only, not as the true solar/planetary properties or current best estimates. Authors and journal editors are urged to join in using the standard values set forth by this resolution in future work and publications to help minimize further confusion. C1 [Prsa, Andrej] Villanova Univ, Dept Astrophys & Planetary Sci, 800 Lancaster Ave, Villanova, PA 19085 USA. [Harmanec, Petr] Charles Univ Prague, Fac Math & Phys, Astron Inst, V Holesovickach 2, CZ-18000 Prague 8, Czech Republic. [Torres, Guillermo] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Mamajek, Eric] Univ Rochester, Dept Phys & Astron, Rochester, NY 14627 USA. [Asplund, Martin] Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT 2611, Australia. [Capitaine, Nicole] Univ Paris 04, PSL Res Univ, Observ Paris, SYRTE,CNRS,UPMC,LNE, 61 Ave Observ, F-75014 Paris, France. [Christensen-Dalsgaard, Jorgen] Aarhus Univ, Dept Phys & Astron, Stellar Astrophys Ctr, Ny Munkegade 120, DK-8000 Aarhus C, Denmark. [Depagne, Eric] South African Astron Observ, POB 9 Observ, Cape Town, South Africa. [Depagne, Eric] Southern African Large Telescope, POB 9 Observ, Cape Town, South Africa. [Haberreiter, Margit; Schmutz, Werner] World Radiat Ctr, Phys Meteorol Observ Davos, Dorfstr 33, Davos, Switzerland. [Hekker, Saskia] Max Planck Inst Sonnensyst Forsch, Justus von Liebig Weg 3, D-37077 Gottingen, Germany. [Hekker, Saskia] Aarhus Univ, Dept Phys & Astron, Stellar Astrophys Ctr, Ny Munkegade 120, DK-8000 Aarhus C, Denmark. [Hilton, James; Mason, Brian D.; Stewart, Susan G.] US Naval Observ, 3450 Massachusetts Ave NW, Washington, DC 20392 USA. [Kopp, Greg] Lab Atmospher & Space Phys, 1234 Innovat Dr, Boulder, CO 80303 USA. [Kostov, Veselin] NASA, Goddard Space Flight Ctr, Mail Code 665, Greenbelt, MD 20771 USA. [Kurtz, Donald W.] Univ Cent Lancashire, Jeremiah Horrocks Inst, Preston PR1 2HE, Lancs, England. [Laskar, Jacques] UPMC, Observ Paris, CNRS, ASD IMCCE,PSL,UMR8028, 77 Ave Denfert Rochereau, F-75014 Paris, France. [Milone, Eugene F.] Univ Calgary, Dept Phys & Astron, 2500 Univ Dr NW, Calgary, AB T2N 1N4, Canada. [Montgomery, Michele] Univ Cent Florida, Dept Phys, 4000 Cent Florida Blvd, Orlando, FL 32816 USA. [Richards, Mercedes] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Schou, Jesper] Max Planck Inst Solar Syst Res, Justus von Liebig Weg 3, D-37077 Gottingen, Germany. RP Prsa, A (reprint author), Villanova Univ, Dept Astrophys & Planetary Sci, 800 Lancaster Ave, Villanova, PA 19085 USA. RI Schmutz, Werner/B-4153-2014; OI Schmutz, Werner/0000-0003-1159-5639; Christensen-Dalsgaard, Jorgen/0000-0001-5137-0966 FU Villanova University; Czech Science Foundation [P209/10/0715, GA15-02112S]; NSF [AST-1509375]; NSF AST award [1313029]; NASA's NExSS program; Danish National Research Foundation [DNRF106]; European Research Council under the European Community's Seventh Framework Programme (FP7)/ERC [338251]; European Community [313188] FX We kindly acknowledge discussions with Philip Bennett, Wolfgang Finsterle, William Folkner, and Hugh Hudson. We further acknowledge remarkable work by Dr. Allen, Dr. Cox, and collaborators on "Astrophysical Quantities." A.P. acknowledges support by Villanova University's Summer Fellowship grant. The research of P.H. was supported by grants P209/10/0715 and GA15-02112S of the Czech Science Foundation. G. T. acknowledges partial support from NSF award AST-1509375. E.M. acknowledges support from NSF AST award 1313029 and NASA's NExSS program. J.C.-D. acknowledges funding for the Stellar Astrophysics Centre that is provided by The Danish National Research Foundation (Grant DNRF106). S.H. acknowledges funding from the European Research Council under the European Community's Seventh Framework Programme (FP7/2007-2013)/ERC grant agreement no. 338251 (StellarAges). The research leading to these results has received funding from the European Community's Seventh Framework Programme (FP7/2007-2013) under Grant Agreement no. 313188 (SOLID, http://projects.pmodwrc.ch/solid/). NR 29 TC 9 Z9 9 U1 3 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD AUG PY 2016 VL 152 IS 2 AR 41 DI 10.3847/0004-6256/152/2/41 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DT9KG UT WOS:000381817500014 ER PT J AU Rebull, LM Carlberg, JK Gibbs, JC Deeb, JE Larsen, E Black, DV Altepeter, S Bucksbee, E Cashen, S Clarke, M Datta, A Hodgson, E Lince, M AF Rebull, Luisa M. Carlberg, Joleen K. Gibbs, John C. Deeb, J. Elin Larsen, Estefania Black, David V. Altepeter, Shailyn Bucksbee, Ethan Cashen, Sarah Clarke, Matthew Datta, Ashwin Hodgson, Emily Lince, Megan TI ON INFRARED EXCESSES ASSOCIATED WITH LI-RICH K GIANTS (vol 150, 123, 2015) SO ASTRONOMICAL JOURNAL LA English DT Correction C1 [Rebull, Luisa M.] CALTECH, SSC, 1200 E Calif Blvd, Pasadena, CA 91125 USA. [Rebull, Luisa M.] CALTECH, Infrared Sci Arch IRSA, IPAC, 1200 E Calif Blvd, Pasadena, CA 91125 USA. [Carlberg, Joleen K.] NASA, Goddard Space Flight Ctr, Code 667, Greenbelt, MD 20771 USA. [Gibbs, John C.; Cashen, Sarah; Datta, Ashwin; Hodgson, Emily; Lince, Megan] Glencoe High Sch, 2700 NW Glencoe Rd, Hillsboro, OR 97124 USA. [Deeb, J. Elin] Bear Creek High Sch, 9800 W Dartmouth Pl, Lakewood, CO 80227 USA. [Larsen, Estefania; Altepeter, Shailyn; Bucksbee, Ethan; Clarke, Matthew] Millard South High Sch, 14905 Q St, Omaha, NE 68137 USA. [Black, David V.] Walden Sch Liberal Arts, 4230 N Univ Ave, Provo, UT 84604 USA. RP Rebull, LM (reprint author), CALTECH, SSC, 1200 E Calif Blvd, Pasadena, CA 91125 USA.; Rebull, LM (reprint author), CALTECH, Infrared Sci Arch IRSA, IPAC, 1200 E Calif Blvd, Pasadena, CA 91125 USA. EM rebull@ipac.caltech.edu OI Rebull, Luisa/0000-0001-6381-515X NR 1 TC 0 Z9 0 U1 1 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD AUG PY 2016 VL 152 IS 2 AR 52 DI 10.3847/0004-6256/152/2/52 PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DT9KG UT WOS:000381817500025 ER PT J AU Benner, DC Devi, VM Sung, K Brown, LR Miller, CE Payne, VH Drouin, BJ Yu, SS Crawford, TJ Mantz, AW Smith, MAH Gamache, RR AF Benner, D. Chris Devi, V. Malathy Sung, Keeyoon Brown, Linda R. Miller, Charles E. Payne, Vivienne H. Drouin, Brian J. Yu, Shanshan Crawford, Timothy J. Mantz, Arlan W. Smith, Mary Ann H. Gamache, Robert R. TI Line parameters including temperature dependences of air- and self-broadened line shapes of (CO2)-C-12-O-16: 2.06-mu m region SO JOURNAL OF MOLECULAR SPECTROSCOPY LA English DT Article DE CO2; Lorentz widths; Pressure shifts; Temperature dependences; Spectral line shapes; Relaxation matrix element coefficients; Speed dependence ID MOLECULAR SPECTROSCOPIC DATABASE; PRESSURE SHIFT COEFFICIENTS; CO2 RETRIEVAL ALGORITHM; MU-M REGIONS; ATMOSPHERIC APPLICATIONS; SPEED DEPENDENCE; 4750-7000 CM(-1); HALF-WIDTH; DATA-BANK; INTENSITIES AB This study reports the results from analyzing a number of high resolution, high signal-to-noise ratio (S/N) spectra in the 2.06-mu m spectral region for pure CO2 and mixtures of CO2 in dry air. A multispectrum non-linear least squares curve fitting technique has been used to retrieve the various spectral line parameters. The dataset includes 27 spectra: ten pure CO2, two 99% C-13-enriched CO2 and fifteen spectra of mixtures of C-12-enriched CO2 in dry air. The spectra were recorded at various gas sample temperatures between 170 and 297 K. The absorption path lengths range from 0.347 to 49 m. The sample pressures for the pure CO2 spectra varied from 1.1 to 594 Torr; for the two (CO2)-C-13 spectra the pressures were similar to 10 and 146 Torr. For the air-broadened spectra, the pressures of the gas mixtures varied between 200 and 711 Torr with CO2 volume mixing ratios ranging from 0.014% to 0.203%. The multispectrum fitting technique was applied to fit simultaneously all these spectra to retrieve consistent set of line positions, intensities, and line shape parameters including their temperature dependences; for this, the Voigt line shape was modified to include line mixing (via the relaxation matrix formalism) and quadratic speed dependence. The new results are compared to select published values, including recent ab initio calculations. These results are required to retrieve the column averaged dry air mole fraction (X-co2) from space-based observations, such as the Orbiting Carbon Observatory-2 (OCO-2) satellite mission that NASA launched in July 2014. (C) 2016 Elsevier Inc. All rights reserved. C1 [Benner, D. Chris; Devi, V. Malathy] Coll William & Mary, Dept Phys, Box 8795, Williamsburg, VA 23187 USA. [Sung, Keeyoon; Brown, Linda R.; Miller, Charles E.; Payne, Vivienne H.; Drouin, Brian J.; Yu, Shanshan; Crawford, Timothy J.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Mantz, Arlan W.] Connecticut Coll, Dept Phys Astron & Geophys, New London, CT 06320 USA. [Smith, Mary Ann H.] NASA, Sci Directorate, Langley Res Ctr, Hampton, VA 23681 USA. [Gamache, Robert R.] Univ Massachusetts, Off Acad Affairs, Student Affairs, Int Relat, One Beacon St, Boston, MA 02108 USA. RP Devi, VM (reprint author), Coll William & Mary, Dept Phys, Box 8795, Williamsburg, VA 23187 USA. EM Malathy.d.venkataraman@nasa.gov RI Yu, Shanshan/D-8733-2016; Sung, Keeyoon/I-6533-2015 FU National Science Foundation [ATM-0338475, AGS-1156862]; JPL FX Part of the material related to Kitt Peak measurements applied in this investigation was based upon work supported by the National Science Foundation under Grant # ATM-0338475 to the College of William and Mary. The recent study involving the low temperature measurements was supported by a Research Grant to the College of William and Mary for the OCO-2 mission through JPL. The research at the Jet Propulsion Laboratory (JPL), California Institute of Technology, Connecticut College and NASA Langley Research Center was performed under contracts and cooperative agreements with the National Aeronautics and Space Administration.; One of the authors, RRG, was supported by the National Science Foundation through Grant # AGS-1156862. DCB and VMD acknowledge the help provided by Emily M. Nugent, a former student of the College of William and Mary. NR 70 TC 6 Z9 6 U1 5 U2 6 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0022-2852 EI 1096-083X J9 J MOL SPECTROSC JI J. Mol. Spectrosc. PD AUG PY 2016 VL 326 BP 21 EP 47 DI 10.1016/j.jms.2016.02.012 PG 27 WC Physics, Atomic, Molecular & Chemical; Spectroscopy SC Physics; Spectroscopy GA DT4KH UT WOS:000381448100005 ER PT J AU Chamberlin, PC AF Chamberlin, P. C. TI Measuring Solar Doppler Velocities in the He II 30.38 nm Emission Using the EUV Variability Experiment (EVE) SO SOLAR PHYSICS LA English DT Article DE Flares, dynamics; Flares, spectrum; Instrumentation and data management; Solar irradiance; Spectrum, ultraviolet ID IRRADIANCE; FLARES; MODELS; PLASMA; MARS AB The EUV Variability Experiment (EVE) onboard the Solar Dynamics Observatory has provided unprecedented measurements of the solar EUV irradiance at high temporal cadence with good spectral resolution and range since May 2010. The main purpose of EVE was to connect the Sun to the Earth by providing measurements of the EUV irradiance as a driver for space weather and Living With a Star studies, but after launch the instrument has demonstrated the significance of its measurements in contributing to studies looking at the sources of solar variability for pure solar physics purposes. This paper expands upon previous findings that EVE can in fact measure wavelength shifts during solar eruptive events and therefore provide Doppler velocities for plasma at all temperatures throughout the solar atmosphere from the chromosphere to hot flaring temperatures. This process is not straightforward as EVE was not designed or optimized for these types of measurements. In this paper we describe the many detailed instrumental characterizations needed to eliminate the optical effects in order to provide an absolute baseline for the Doppler shift studies. An example is given of a solar eruption on 7 September 2011 (SOL2011-09-07), associated with an X1.2 flare, where EVE Doppler analysis shows plasma ejected from the Sun in the He II 30.38 nm emission at a velocity of almost 120 kms(-1) along the line-of-sight. C1 [Chamberlin, P. C.] NASA, Goddard Space Flight Ctr, Solar Phys Lab, Heliophys Div, Greenbelt, MD 20771 USA. RP Chamberlin, PC (reprint author), NASA, Goddard Space Flight Ctr, Solar Phys Lab, Heliophys Div, Greenbelt, MD 20771 USA. EM phillip.c.chamberlin@nasa.gov RI Chamberlin, Phillip/C-9531-2012 OI Chamberlin, Phillip/0000-0003-4372-7405 FU Solar Dynamics Observatory project at NASA's Goddard Space Flight Center FX This work is supported through Solar Dynamics Observatory project funding at NASA's Goddard Space Flight Center. The author would like to acknowledge the SDO and EVE operations teams that provided the maneuvers and calibration support necessary for this analysis. NR 22 TC 0 Z9 0 U1 1 U2 1 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-0938 EI 1573-093X J9 SOL PHYS JI Sol. Phys. PD AUG PY 2016 VL 291 IS 6 BP 1665 EP 1679 DI 10.1007/s11207-016-0931-0 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DU3EP UT WOS:000382093900006 ER PT J AU Balakumar, P Kegerise, M AF Balakumar, P. Kegerise, Michael TI Roughness-Induced Transition in a Supersonic Boundary Layer SO AIAA JOURNAL LA English DT Article ID TOLLMIEN-SCHLICHTING WAVES; ELEMENT; INSTABILITY; EVOLUTION AB Direct numerical simulation is used to investigate the transition induced by three-dimensional isolated roughness elements in a supersonic boundary layer at a freestream Mach number of 3.5. Simulations are performed for two different configurations: one is a square planform roughness element, and the other is a diamond planform roughness element. The mean flow calculations show that the roughness element induces counter-rotating streamwise vortices downstream of the roughness element. These vortices persist for a long distance downstream, lift the low-momentum fluid from the near-wall region, and place it near the outer part of the boundary layer. This forms highly inflectional boundary-layer profiles. These observations agree with recent experimental observations. The receptivity calculations show that the amplitudes of the mass-flux fluctuations near the neutral point for the diamond-shaped roughness element are the same as the amplitude of the acoustic disturbances. They are three times smaller for the square-shaped roughness element. C1 [Balakumar, P.; Kegerise, Michael] NASA, Langley Res Ctr, Flow Phys & Control Branch, Hampton, VA 23681 USA. RP Balakumar, P (reprint author), NASA, Langley Res Ctr, Flow Phys & Control Branch, Hampton, VA 23681 USA. NR 34 TC 0 Z9 0 U1 1 U2 1 PU AMER INST AERONAUTICS ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0001-1452 EI 1533-385X J9 AIAA J JI AIAA J. PD AUG PY 2016 VL 54 IS 8 BP 2322 EP 2337 DI 10.2514/1.J054632 PG 16 WC Engineering, Aerospace SC Engineering GA DT2EI UT WOS:000381293200011 ER PT J AU Busa, KM Rice, BE McDaniel, JC Goyne, CP Rockwell, RD Fulton, JA Edwards, JR Diskin, GS AF Busa, Kristin M. Rice, Brian E. McDaniel, James C. Goyne, Christopher P. Rockwell, Robert D. Fulton, Jesse A. Edwards, Jack R. Diskin, Glenn S. TI Scramjet Combustion Efficiency Measurement via Tomographic Absorption Spectroscopy and Particle Image Velocimetry SO AIAA JOURNAL LA English DT Article ID DUAL-MODE SCRAMJET; DIODE-LASER ABSORPTION; PERFORMANCE AB The combustion efficiency of a scramjet is a metric that evaluates the overall performance of the engine. Until recently, combustion efficiency was measured using indirect approaches such as a one-dimensional control volume calculation or a calorimeter and wall pressure tap measurements. A novel nonintrusive direct approach for the measurement of combustion efficiency is presented that combines the optical diagnostic techniques tunable diode laser absorption tomography and stereoscopic particle image velocimetry. Experimental results are presented for measurements of the University of Virginia's Supersonic Combustion Facility in both the scram and ram-modes of operation. The tunablediode-laser-absorption-tomography/stereoscopic-particle-image-velocimetry method directly measures the converted hydrogen (via water vapor) mass flow rate exiting the dual-mode scramjet and compares this to the facility-measured injected hydrogen fuel mass flow rate. A complementary computational fluid dynamics study was performed and results are available for the scram-mode operating condition. The results reported show excellent agreement between the tunable-diode-laser-absorption-tomography/stereoscopic-particle-image-velocimetry-measured combustion efficiency and the computational-fluid-dynamics-predicted combustion efficiency for the scram-mode of operation, which are both near 99%. The tunable-diode-laser-absorption-tomography/stereoscopic-particle-image-velocimetry-measured combustion efficiency for the ram-mode of operation is shown to be lower than that of the scram-mode operation: at 79%. C1 [Busa, Kristin M.] US Air Force, Res Lab, High Speed Syst Div, AFRL RQHF, 2130 Eighth Street, Wright Patterson AFB, OH 45433 USA. [Rice, Brian E.] US Air Force, Res Lab, AFRL RQHX, High Speed Syst Div, 676 Second Street, Arnold AFB, TN 37389 USA. [McDaniel, James C.; Goyne, Christopher P.; Rockwell, Robert D.] Univ Virginia, Mech & Aerosp Engn, Charlottesville, VA 22904 USA. [Fulton, Jesse A.] Sandia Natl Labs, Aerosp Syst Anal, Mail Stop 1162,1515 Eubank, Albuquerque, NM 87185 USA. [Edwards, Jack R.] North Carolina State Univ, Mech & Aerosp Engn, Raleigh, NC 27695 USA. [Diskin, Glenn S.] NASA, Langley Res Ctr, Chem & Dynam Branch, Mail Stop 483, Hampton, VA 23681 USA. RP Busa, KM (reprint author), US Air Force, Res Lab, High Speed Syst Div, AFRL RQHF, 2130 Eighth Street, Wright Patterson AFB, OH 45433 USA. FU National Center for Hypersonic Combined Cycle Propulsion grant [FA9550-09-1-0611]; U.S. Air Force Office of Scientific Research; NASA [NNL11AB32P]; National Science Foundation FX This research was supported by the National Center for Hypersonic Combined Cycle Propulsion grant FA9550-09-1-0611, which was supported by NASA and the U.S. Air Force Office of Scientific Research (Richard Gaffney, Aaron Auslender, and Chiping Li as Technical Monitors); and by NASA contract NNL11AB32P (Richard Gaffney as Technical Monitor). K.M. Busa would like to acknowledge fellowship support from the National Science Foundation. The authors also thank Roger Reynolds for operation of the University of Virginia's Supersonic Combustion Facility and fabrication of the tunable diode laser absorption tomography hardware. NR 24 TC 1 Z9 1 U1 3 U2 3 PU AMER INST AERONAUTICS ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0001-1452 EI 1533-385X J9 AIAA J JI AIAA J. PD AUG PY 2016 VL 54 IS 8 BP 2463 EP 2471 DI 10.2514/1.J054662 PG 9 WC Engineering, Aerospace SC Engineering GA DT2EI UT WOS:000381293200021 ER PT J AU Sirbu, D Kim, Y Kasdin, NJ Vanderbei, RJ AF Sirbu, Dan Kim, Yunjong Kasdin, N. Jeremy Vanderbei, Robert J. TI Diffraction-based sensitivity analysis for an external occulter laboratory demonstration SO APPLIED OPTICS LA English DT Article ID DENSITY-FUNCTION; PLANETS AB An external flower-shaped occulter flying in formation with a space telescope can theoretically provide sufficient starlight suppression to enable direct imaging of an Earth-like planet. Occulter shapes are scaled to enable experimental validation of their performance at laboratory dimensions. Previous experimental results have shown promising performance but have not realized the full theoretical potential of occulter designs. Here, we develop a two-dimensional diffraction model for optical propagations for occulters incorporating experimental errors. We perform a sensitivity analysis, and comparison with experimental results from a scaled-occulter testbed validates the optical model to the 10(-10) contrast level. The manufacturing accuracy along the edge of the occulter shape is identified as the limiting factor to achieving the theoretical potential of the occulter design. This hypothesis is experimentally validated using a second occulter mask manufactured with increased edge feature accuracy and resulting in a measured contrast level approaching the 10(-12) level-a better than one order of magnitude improvement in performance. (C) 2016 Optical Society of America. C1 [Sirbu, Dan; Kim, Yunjong; Kasdin, N. Jeremy; Vanderbei, Robert J.] Princeton Univ, High Contrast Imaging Lab, Mech & Aerosp Engn, Princeton, NJ 08544 USA. [Sirbu, Dan] NASA, Ames Res Ctr, Mountain View, CA 94035 USA. RP Sirbu, D (reprint author), Princeton Univ, High Contrast Imaging Lab, Mech & Aerosp Engn, Princeton, NJ 08544 USA.; Sirbu, D (reprint author), NASA, Ames Res Ctr, Mountain View, CA 94035 USA. EM dan.sirbu@nasa.gov FU National Aeronautics and Space Administration (NASA) [NNX09AB97G]; Technology Demonstration for Exoplanet Missions grant [NNX14AQ63G]; NASA Postdoctoral Program Fellowship; California Institute of Technology (Caltech) [1430187]; Natural Sciences and Engineering Research Council of Canada (NSERC); U.S. Office of Naval Research (ONR) [N000141612162] FX National Aeronautics and Space Administration (NASA) (NNX09AB97G, Earth & Space Science Fellowship), a Technology Demonstration for Exoplanet Missions grant (NNX14AQ63G), and a NASA Postdoctoral Program Fellowship; California Institute of Technology (Caltech) (1430187); Natural Sciences and Engineering Research Council of Canada (NSERC); U.S. Office of Naval Research (ONR) (N000141612162). NR 31 TC 0 Z9 0 U1 0 U2 0 PU OPTICAL SOC AMER PI WASHINGTON PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA SN 1559-128X EI 2155-3165 J9 APPL OPTICS JI Appl. Optics PD AUG 1 PY 2016 VL 55 IS 22 BP 6083 EP 6094 DI 10.1364/AO.55.006083 PG 12 WC Optics SC Optics GA DS4HP UT WOS:000380742300036 PM 27505392 ER PT J AU Leon, JJD Norris, KJ Hartnett, RJ Garrett, MP Tompa, GS Kobayashi, NP AF Leon, Juan J. Diaz Norris, Kate J. Hartnett, Ryan J. Garrett, Matthew P. Tompa, Gary S. Kobayashi, Nobuhiko P. TI Nonlinear current-voltage characteristics based on semiconductor nanowire networks enable a new concept in thermoelectric device optimization SO APPLIED PHYSICS A-MATERIALS SCIENCE & PROCESSING LA English DT Article ID INDIUM-PHOSPHIDE NANOWIRES; SILICON NANOWIRES; THERMAL-CONDUCTIVITY; SOLAR-CELLS; GROWTH; PERFORMANCE; EFFICIENCY; TRANSPORT; SHELL; CORE AB Thermoelectric (TE) devices that produce electric power from heat are driven by a temperature gradient (Delta T - T-hot - T-cold, T-hot: hot side temperature, T-cold: cold side temperature) with respect to the average temperature (T). While the resistance of TE devices changes as Delta T and/or T change, the current-voltage (I-V) characteristics have consistently been shown to remain linear, which clips generated electric power (P-gen) within the given open-circuit voltage (V-OC) and short-circuit current (I-SC). This P-gen clipping is altered when an appropriate nonlinearity is introduced to the I-V characteristics-increasing P-gen. By analogy, photovoltaic cells with a large fill factor exhibit nonlinear I-V characteristics. In this paper, the concept of a unique TE device with nonlinear I-V characteristics is proposed and experimentally demonstrated. A single TE device with nonlinear I-V characteristics is fabricated by combining indium phosphide (InP) and silicon (Si) semiconductor nanowire networks. These TE devices show P-gen that is more than 25 times larger than those of comparable devices with linear I-V characteristics. The plausible causes of the nonlinear I-V characteristics are discussed. The demonstrated concept suggests that there exists a new pathway to increase P-gen of TE devices made of semiconductors. C1 [Leon, Juan J. Diaz; Norris, Kate J.; Hartnett, Ryan J.; Garrett, Matthew P.; Kobayashi, Nobuhiko P.] Univ Calif Santa Cruz, Baskin Sch Engn, Santa Cruz, CA 95064 USA. [Leon, Juan J. Diaz; Norris, Kate J.; Hartnett, Ryan J.; Garrett, Matthew P.; Kobayashi, Nobuhiko P.] Univ Calif Santa Cruz, NASA Ames Res Ctr, Nanostruct Energy Convers Technol & Res NECTAR, Adv Studies Labs, Moffett Field, CA 94035 USA. [Tompa, Gary S.] Struct Mat Ind Inc, Piscataway, NJ USA. RP Leon, JJD (reprint author), Univ Calif Santa Cruz, Baskin Sch Engn, Santa Cruz, CA 95064 USA.; Leon, JJD (reprint author), Univ Calif Santa Cruz, NASA Ames Res Ctr, Nanostruct Energy Convers Technol & Res NECTAR, Adv Studies Labs, Moffett Field, CA 94035 USA. EM jdiazleo@ucsc.edu FU NASA [SBIR NNX11CE14P]; National Science Foundation Graduate Research Fellowship [DGE-0809125]; Semiconductor Research Corporation CSR fund FX This work was supported by NASA SBIR NNX11CE14P. The authors are grateful to HP laboratories and the MACS facility (Moffett Field, California) at Advanced Studies Laboratories, University of California Santa Cruz, and NASA Ames Research Center for continuous support on analytical equipment. This material is based on work supported by the National Science Foundation Graduate Research Fellowship under Grant No. DGE-0809125. Support by Semiconductor Research Corporation CSR fund (Dr. Victor Zhirnov) is also highly appreciated. NR 47 TC 0 Z9 0 U1 9 U2 10 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0947-8396 EI 1432-0630 J9 APPL PHYS A-MATER JI Appl. Phys. A-Mater. Sci. Process. PD AUG PY 2016 VL 122 IS 8 AR 741 DI 10.1007/s00339-016-0260-z PG 9 WC Materials Science, Multidisciplinary; Physics, Applied SC Materials Science; Physics GA DS3FC UT WOS:000380667500027 ER PT J AU Cowperthwaite, PS Berger, E Soares-Santos, M Annis, J Brout, D Brown, DA Buckley-Geer, E Cenko, SB Chen, HY Chornock, R Diehl, HT Doctor, Z Drlica-Wagner, A Drout, MR Farr, B Finley, DA Foley, RJ Fong, W Fox, DB Frieman, J Garcia-Bellido, J Gill, MSS Gruendl, RA Herner, K Holz, DE Kasen, D Kessler, R Lin, H Margutti, R Marriner, J Matheson, T Metzger, BD Neilsen, EH Quataert, E Rest, A Sako, M Scolnic, D Smith, N Sobreira, F Strampelli, GM Villar, VA Walker, AR Wester, W Williams, PKG Yanny, B Abbott, TMC Abdalla, FB Allam, S Armstrong, R Bechtol, K Benoit-Levy, A Bertin, E Brooks, D Burke, DL Rosell, AC Kind, MC Carretero, J Castander, FJ Cunha, CE D'Andrea, CB da Costa, LN Desai, S Dietrich, JP Evrard, AE Neto, AF Fosalba, P Gerdes, DW Giannantonio, T Goldstein, DA Gruen, D Gutierrez, G Honscheid, K James, DJ Johnson, MWG Johnson, MD Krause, E Kuehn, K Kuropatkin, N Lima, M Maia, MAG Marshall, JL Menanteau, F Miquel, R Mohr, JJ Nichol, RC Nord, B Ogando, R Plazas, AA Reil, K Romer, AK Sanchez, E Scarpine, V Sevilla-Noarbe, I Smith, RC Suchyta, E Tarle, G Thomas, D Thomas, RC Tucker, DL Weller, J AF Cowperthwaite, P. S. Berger, E. Soares-Santos, M. Annis, J. Brout, D. Brown, D. A. Buckley-Geer, E. Cenko, S. B. Chen, H. Y. Chornock, R. Diehl, H. T. Doctor, Z. Drlica-Wagner, A. Drout, M. R. Farr, B. Finley, D. A. Foley, R. J. Fong, W. Fox, D. B. Frieman, J. Garcia-Bellido, J. Gill, M. S. S. Gruendl, R. A. Herner, K. Holz, D. E. Kasen, D. Kessler, R. Lin, H. Margutti, R. Marriner, J. Matheson, T. Metzger, B. D. Neilsen, E. H., Jr. Quataert, E. Rest, A. Sako, M. Scolnic, D. Smith, N. Sobreira, F. Strampelli, G. M. Villar, V. A. Walker, A. R. Wester, W. Williams, P. K. G. Yanny, B. Abbott, T. M. C. Abdalla, F. B. Allam, S. Armstrong, R. Bechtol, K. Benoit-Levy, A. Bertin, E. Brooks, D. Burke, D. L. Carnero Rosell, A. Kind, M. Carrasco Carretero, J. Castander, F. J. Cunha, C. E. D'Andrea, C. B. da Costa, L. N. Desai, S. Dietrich, J. P. Evrard, A. E. Fausti Neto, A. Fosalba, P. Gerdes, D. W. Giannantonio, T. Goldstein, D. A. Gruen, D. Gutierrez, G. Honscheid, K. James, D. J. Johnson, M. W. G. Johnson, M. D. Krause, E. Kuehn, K. Kuropatkin, N. Lima, M. Maia, M. A. G. Marshall, J. L. Menanteau, F. Miquel, R. Mohr, J. J. Nichol, R. C. Nord, B. Ogando, R. Plazas, A. A. Reil, K. Romer, A. K. Sanchez, E. Scarpine, V. Sevilla-Noarbe, I. Smith, R. C. Suchyta, E. Tarle, G. Thomas, D. Thomas, R. C. Tucker, D. L. Weller, J. CA DES Collaboration TI A DECAM SEARCH FOR AN OPTICAL COUNTERPART TO THE LIGO GRAVITATIONAL-WAVE EVENT GW151226 SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE binaries: close; catalogs; gravitational waves; stars: neutron; surveys ID ENERGY CAMERA SEARCH; FOLLOW-UP; SUPERNOVA RATES; IA SUPERNOVAE; GW150914; CURVES; PHOTOMETRY; PAN-STARRS1; AFTERGLOWS; LMC AB We report the results of a Dark Energy Camera optical follow-up of the gravitational-wave (GW) event GW151226, discovered by the Advanced Laser Interferometer Gravitational-wave Observatory detectors. Our observations cover 28.8 deg(2) of the localization region in the i and z bands (containing 3% of the BAYESTAR localization probability), starting 10 hr after the event was announced and spanning four epochs at 2-24 days after the GW detection. We achieve 5 sigma point-source limiting magnitudes of i approximate to 21.7 and z approximate to 21.5, with a scatter of 0.4 mag, in our difference images. Given the two-day delay, we search this area for a rapidly declining optical counterpart with greater than or similar to 3 sigma significance steady decline between the first and final observations. We recover four sources that pass our selection criteria, of which three are cataloged active galactic nuclei. The fourth source is offset by 5.8 arcsec from the center of a galaxy at a distance of 187 Mpc, exhibits a rapid decline by 0.5 mag over 4 days, and has a red color of i - z approximate to 0.3 mag. These properties could satisfy a set of cuts designed to identify kilonovae. However, this source was detected several times, starting 94 days prior to GW151226, in the Pan-STARRS Survey for Transients (dubbed as PS15cdi) and is therefore unrelated to the GW event. Given its long-term behavior, PS15cdi is likely a Type IIP supernova that transitioned out of its plateau phase during our observations, mimicking a kilonova-like behavior. We comment on the implications of this detection for contamination in future optical follow-up observations. C1 [Cowperthwaite, P. S.; Berger, E.; Drout, M. R.; Villar, V. A.; Williams, P. K. G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Soares-Santos, M.; Annis, J.; Buckley-Geer, E.; Diehl, H. T.; Drlica-Wagner, A.; Finley, D. A.; Frieman, J.; Herner, K.; Lin, H.; Marriner, J.; Neilsen, E. H., Jr.; Wester, W.; Yanny, B.; Allam, S.; Gutierrez, G.; Kuropatkin, N.; Nord, B.; Scarpine, V.; Tucker, D. L.] Fermilab Natl Accelerator Lab, POB 500, Batavia, IL 60510 USA. [Brout, D.; Sako, M.; Suchyta, E.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. [Brown, D. A.] Syracuse Univ, Dept Phys, Syracuse, NY 13244 USA. [Cenko, S. B.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA. [Cenko, S. B.] Univ Maryland, Joint Space Sci Inst, College Pk, MD 20742 USA. [Chen, H. Y.; Doctor, Z.; Frieman, J.; Kessler, R.; Scolnic, D.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Chornock, R.] Ohio Univ, Dept Phys & Astron, Inst Astrophys, Clippinger Lab 251B, Athens, OH 45701 USA. [Farr, B.; Holz, D. E.] Univ Chicago, Dept Astron & Astrophys, Dept Phys, Enrico Fermi Inst, Chicago, IL 60637 USA. [Farr, B.; Holz, D. E.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Foley, R. J.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Foley, R. J.; Gruendl, R. A.; Kind, M. Carrasco; Menanteau, F.] Univ Illinois, Dept Astron, 1002 W Green St, Urbana, IL 61801 USA. [Foley, R. J.] Univ Illinois, Dept Phys, 1110 W Green St, Urbana, IL 61801 USA. [Fong, W.; Smith, N.] Univ Arizona, Steward Observ, 933 N Cherry Ave, Tucson, AZ 85721 USA. [Fox, D. B.] Penn State Univ, Ctr Gravitat Wave & Particle Astrophys, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA. [Fox, D. B.] Penn State Univ, Ctr Theoret & Observat Cosmol, 525 Davey Lab, University Pk, PA 16802 USA. [Garcia-Bellido, J.] Univ Autonoma Madrid, CSIC, Inst Fis Teor UAM, E-28049 Madrid, Spain. [Burke, D. L.; Cunha, C. E.; Gruen, D.; Krause, E.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, POB 2450, Stanford, CA 94305 USA. [Gill, M. S. S.; Burke, D. L.; Gruen, D.; Reil, K.] SLAC Natl Accelerator Lab, Menlo Pk, CA 94025 USA. [Gruendl, R. A.; Kind, M. Carrasco; Johnson, M. W. G.; Johnson, M. D.; Menanteau, F.] Natl Ctr Supercomputing Applicat, 1205 West Clark St, Urbana, IL 61801 USA. [Kasen, D.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94704 USA. [Kasen, D.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94704 USA. [Kasen, D.; Goldstein, D. A.; Thomas, R. C.] Lawrence Berkeley Natl Lab, 1 Cyclotron Rd, Berkeley, CA 94720 USA. [Margutti, R.] NYU, Ctr Cosmol & Particle Phys, 4 Washington Pl, New York, NY 10003 USA. [Matheson, T.] Natl Opt Astron Observ, 950 North Cherry Ave, Tucson, AZ 85719 USA. [Metzger, B. D.] Columbia Univ, Columbia Astrophys Lab, Pupin Hall, New York, NY 10027 USA. [Quataert, E.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Quataert, E.] Univ Calif Berkeley, Theoret Astrophys Ctr, Berkeley, CA 94720 USA. [Rest, A.; Strampelli, G. M.] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA. [Sobreira, F.] Univ Estadual Paulista, Fundamental Res Inst Fis Teor, ICTP South Amer Inst, Sao Paulo, Brazil. [Sobreira, F.; Carnero Rosell, A.; da Costa, L. N.; Fausti Neto, A.; Lima, M.] Lab Interinst E Astron LIneA, Rua Gal Jose Cristino 77, Rio De Janeiro, RJ, Brazil. [Walker, A. R.; Abbott, T. M. C.; Brooks, D.; James, D. J.; Smith, R. C.] Natl Opt Astron Observ, Cerro Tololo Inter Amer Observ, Casilla 603, La Serena, Chile. [Benoit-Levy, A.; Carnero Rosell, A.] UCL, Dept Phys & Astron, Gower St, London WC1E 6BT, England. [Abdalla, F. B.] Rhodes Univ, Dept Phys & Elect, POB 94, ZA-6140 Grahamstown, South Africa. [Armstrong, R.] Princeton Univ, Dept Astrophys Sci, Peyton Hall, Princeton, NJ 08544 USA. [Bechtol, K.] Univ Wisconsin, Dept Phys, Madison, WI 53706 USA. [Bechtol, K.] Univ Wisconsin, Wisconsin IceCube Particle Astrophys Ctr, Madison, WI 53706 USA. [Benoit-Levy, A.; Bertin, E.] CNRS, Inst Astrophys Paris, UMR 7095, F-75014 Paris, France. [Benoit-Levy, A.; Bertin, E.] Univ Paris 06, Sorbonne Univ, Inst Astrophys Paris, UMR 7095, F-75014 Paris, France. [Carnero Rosell, A.; da Costa, L. N.; Maia, M. A. G.; Ogando, R.] Observ Nacl, Rua Gal Jose Cristino 77, BR-20921400 Rio De Janeiro, RJ, Brazil. [Carretero, J.; Castander, F. J.; Fosalba, P.] IEEC CSIC, Inst Ciencies Espai, Campus UAB,Carrer Can Magrans S-N, E-08193 Barcelona, Spain. [Carretero, J.; Miquel, R.] Barcelona Inst Sci & Technol, IFAE, Campus UAB, E-08193 Barcelona, Spain. [D'Andrea, C. B.; Nichol, R. C.; Thomas, D.] Univ Portsmouth, Inst Cosmol & Gravitat, Portsmouth PO1 3FX, Hants, England. [D'Andrea, C. B.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Desai, S.; Dietrich, J. P.; Mohr, J. J.] Univ Munich, Fac Phys, Scheinerstr 1, D-81679 Munich, Germany. [Desai, S.; Dietrich, J. P.; Mohr, J. J.; Weller, J.] Excellence Cluster Universe, Boltzmannstr 2, D-85748 Garching, Germany. [Evrard, A. E.; Gerdes, D. W.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Evrard, A. E.; Gerdes, D. W.; Suchyta, E.; Tarle, G.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA. [Giannantonio, T.] Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England. [Giannantonio, T.] Univ Cambridge, Kavli Inst Cosmol, Madingley Rd, Cambridge CB3 0HA, England. [Goldstein, D. A.] Univ Calif Berkeley, Dept Astron, 501 Campbell Hall, Berkeley, CA 94720 USA. [Honscheid, K.] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA. [Honscheid, K.] Ohio State Univ, Dept Phys, 174 W 18th Ave, Columbus, OH 43210 USA. [Kuehn, K.] Australian Astron Observ, N Ryde, NSW 2113, Australia. [Lima, M.] Univ Sao Paulo, Inst Fis, Dept Fis Matemat, CP 66318, BR-05314970 Sao Paulo, SP, Brazil. [Marshall, J. L.] Texas A&M Univ, George P & Cynthia Woods Mitchell Inst Fundamenta, College Stn, TX 77843 USA. [Marshall, J. L.] Texas A&M Univ, Dept Phys & Astron, College Stn, TX 77843 USA. [Miquel, R.] Inst Catalana Recerca & Estudis Avancats, E-08010 Barcelona, Spain. [Mohr, J. J.; Weller, J.] Max Planck Inst Extraterr Phys, Giessenbachstr, D-85748 Garching, Germany. [Plazas, A. A.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Romer, A. K.] Univ Sussex, Dept Phys & Astron, Pevensey Bldg, Brighton BN1 9QH, E Sussex, England. [Sanchez, E.; Sevilla-Noarbe, I.] Ctr Invest Energet Medioambientales & Tecnol CIEM, Madrid, Spain. [Cowperthwaite, P. S.; Weller, J.] Univ Munich, Univ Sternwarte, Fak Phys, Scheinerstr 1, D-81679 Munich, Germany. RP Cowperthwaite, PS (reprint author), Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.; Cowperthwaite, PS (reprint author), Univ Munich, Univ Sternwarte, Fak Phys, Scheinerstr 1, D-81679 Munich, Germany. EM pcowpert@cfa.harvard.edu RI Lima, Marcos/E-8378-2010; Ogando, Ricardo/A-1747-2010; OI Ogando, Ricardo/0000-0003-2120-1154; Cowperthwaite, Philip/0000-0002-2478-6939; Garcia-Bellido, Juan/0000-0002-9370-8360; Abdalla, Filipe/0000-0003-2063-4345; Sobreira, Flavia/0000-0002-7822-0658; Neilsen, Eric/0000-0002-7357-0317 FU NSF through the Graduate Research Fellowship Program [DGE1144152]; NSF [AST-1518052, AST-1138766]; Alfred P. Sloan Foundation; NSF CAREER [PHY-1151836]; Kavli Institute for Cosmological Physics at the University of Chicago through NSF [PHY-1125897]; FAS Division of Science, Research Computing Group at Harvard University; National Aeronautics and Space Administration; DOE; NSF (USA); MEC/MICINN/MINECO (Spain); STFC (UK); HEFCE (UK); MINECO [AYA2012-39559, ESP2013-48274, FPA2013-47986]; Centro de Excelencia Severo Ochoa [SEV-2012-0234]; ERC under the EU's 7th Framework Programme [ERC 240672, 291329, 306478] FX P.S.C. is grateful for support provided by the NSF through the Graduate Research Fellowship Program, grant DGE1144152. R. J.F. gratefully acknowledges support from NSF grant AST-1518052 and the Alfred P. Sloan Foundation. D.E.H. was supported by NSF CAREER grant PHY-1151836. He also acknowledges support from the Kavli Institute for Cosmological Physics at the University of Chicago through NSF grant PHY-1125897 as well as an endowment from the Kavli Foundation.r This research uses services or data provided by the NOAO Science Archive. NOAO is operated by the Association of Universities for Research in Astronomy (AURA), Inc. under a cooperative agreement with the National Science Foundation. The computations in this Letter were run on the Odyssey cluster supported by the FAS Division of Science, Research Computing Group at Harvard University. 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. Light curve data for PS15cdi were obtained from The Open Supernova Catalog (Guillochon et al. 2016). Some of the results in this Letter have been derived using the HEALPix package (Gorski et al. 2005).r Funding for the DES Projects has been provided by the DOE and NSF (USA), MEC/MICINN/MINECO (Spain), STFC (UK), HEFCE (UK). NCSA (UIUC), KICP (U. Chicago), CCAPP (Ohio State), MIFPA (Texas A&M), CNPQ, FAPERJ, FINEP (Brazil), DFG (Germany) and the Collaborating Institutions in the Dark Energy Survey.r The DES Data Management System is supported by the NSF under grant number AST-1138766. The DES participants from Spanish institutions are partially supported by MINECO under grants AYA2012-39559, ESP2013-48274, FPA2013-47986, and Centro de Excelencia Severo Ochoa SEV-2012-0234. Research leading to these results has received funding from the ERC under the EU's 7th Framework Programme including grants ERC 240672, 291329, and 306478. NR 45 TC 3 Z9 3 U1 5 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD AUG 1 PY 2016 VL 826 IS 2 AR L29 DI 10.3847/2041-8205/826/2/L29 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DT2TN UT WOS:000381334800013 ER PT J AU Skemer, AJ Morley, CV Allers, KN Geballe, TR Marley, MS Fortney, JJ Faherty, JK Bjoraker, GL Lupu, R AF Skemer, Andrew J. Morley, Caroline V. Allers, Katelyn N. Geballe, Thomas R. Marley, Mark S. Fortney, Jonathan J. Faherty, Jacqueline K. Bjoraker, Gordon L. Lupu, Roxana TI THE FIRST SPECTRUM OF THE COLDEST BROWN DWARF SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE brown dwarfs ID EXTRASOLAR GIANT PLANETS; T-DWARFS; THERMAL STRUCTURE; WATER CLOUDS; ATMOSPHERES; JUPITERS; CHEMISTRY; DISCOVERY; DEUTERIUM; COLORS AB The recently discovered brown dwarf WISE 0855 presents the first opportunity to directly study an object outside the solar system that is nearly as cold as our own gas giant planets. However, the traditional methodology for characterizing brown dwarfs-near-infrared spectroscopy-is not currently feasible, as WISE 0855 is too cold and faint. To characterize this frozen extrasolar world we obtained a 4.5-5.2 mu m spectrum, the same bandpass long used to study Jupiter's deep thermal emission. Our spectrum reveals the presence of atmospheric water vapor and clouds, with an absorption profile that is strikingly similar to Jupiter's. The spectrum quality is high enough to allow for the investigation of dynamical and chemical processes that have long been studied in Jupiter's atmosphere, but now on an extrasolar world. C1 [Skemer, Andrew J.; Morley, Caroline V.; Fortney, Jonathan J.] Univ Calif Santa Cruz, 1156 High St, Santa Cruz, CA 95064 USA. [Allers, Katelyn N.] Bucknell Univ, 701 Moore Ave, Lewisburg, PA 17837 USA. [Geballe, Thomas R.] Gemini Observ, 670 North Aohoku Pl, Hilo, HI 96720 USA. [Marley, Mark S.; Lupu, Roxana] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Faherty, Jacqueline K.] Carnegie Inst Sci, Dept Terr Magnetism, 5241 Broad Branch Rd NW, Washington, DC 20015 USA. [Faherty, Jacqueline K.] Natl Museum Amer Hist, Cent Pk West & 79th St, New York, NY 10024 USA. [Bjoraker, Gordon L.] NASA, Goddard Space Flight Ctr, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA. RP Skemer, AJ (reprint author), Univ Calif Santa Cruz, 1156 High St, Santa Cruz, CA 95064 USA. OI Marley, Mark/0000-0002-5251-2943 NR 37 TC 2 Z9 2 U1 3 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD AUG 1 PY 2016 VL 826 IS 2 AR L17 DI 10.3847/2041-8205/826/2/L17 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DT2TN UT WOS:000381334800001 ER PT J AU Walton, DJ Middleton, MJ Pinto, C Fabian, AC Bachetti, M Barret, D Brightman, M Fuerst, F Harrison, FA Miller, JM Stern, D AF Walton, D. J. Middleton, M. J. Pinto, C. Fabian, A. C. Bachetti, M. Barret, D. Brightman, M. Fuerst, F. Harrison, F. A. Miller, J. M. Stern, D. TI AN IRON K COMPONENT TO THE ULTRAFAST OUTFLOW IN NGC 1313 X-1 SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE black hole physics; X-rays: binaries; X-rays: individual (NGC 1313 X-1) ID X-RAY SOURCES; XMM-NEWTON OBSERVATIONS; MASS BLACK-HOLES; HOLMBERG IX X-1; BROAD-BAND; DISK WIND; ACCRETION DISKS; EMISSION-LINE; NEUTRON-STAR; NUSTAR AB We present the detection of an absorption feature at E = 8.77(+0.06)(+0.05) keV in the combined X-ray spectrum of the ultraluminous X-ray source NGC 1313 X-1 observed with XMM-Newton and NuSTAR, significant at the 3 sigma level. If associated with blueshifted ionized iron, the implied outflow velocity is similar to 0.2c for Fe XXVI, or similar to 0.25c for Fe XXV. These velocities are similar to the ultrafast outflow seen in absorption recently discovered in this source at lower energies by XMM-Newton, and we therefore conclude that this is an iron component to the same outflow. Photoionization modeling marginally prefers the Fe XXV solution, but in either case the outflow properties appear to be extreme, potentially supporting a super-Eddington hypothesis for NGC 1313 X-1. C1 [Walton, D. J.; Stern, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Walton, D. J.; Brightman, M.; Fuerst, F.; Harrison, F. A.] CALTECH, Space Radiat Lab, Pasadena, CA 91125 USA. [Middleton, M. J.; Pinto, C.; Fabian, A. C.] Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England. [Bachetti, M.] INAF, Osservatorio Astron Cagliari, Via Sci 5, I-09047 Selargius, CA, Italy. [Barret, D.] Univ Toulouse, UPS OMP, IRAP, Toulouse, France. [Barret, D.] CNRS, IRAP, 9 Av Colonel Roche,BP 44346, F-31028 Toulouse 4, France. [Miller, J. M.] Univ Michigan, Dept Astron, 1085 S Univ Ave, Ann Arbor, MI 49109 USA. RP Walton, DJ (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.; Walton, DJ (reprint author), CALTECH, Space Radiat Lab, Pasadena, CA 91125 USA. OI Pinto, Ciro/0000-0003-2532-7379 FU STFC Ernest Rutherford fellowship; ERC Advanced Grant [340442]; French Space Agency (CNES); NASA; ESA Member States FX The authors would like to thank the anonymous referee for their extremely timely and positive feedback, which helped improve the final manuscript. M.J.M. acknowledges support from an STFC Ernest Rutherford fellowship, C.P. and A.C.F. acknowledge support from ERC Advanced Grant 340442, and D.B. acknowledges financial support from the French Space Agency (CNES). This research has made use of data obtained with NuSTAR, a project led by Caltech, funded by NASA, and managed by NASA/JPL, and has utilized the NUSTARDAS software package, jointly developed by the ASDC (Italy) and Caltech (USA). This research has also made use of data obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States. NR 43 TC 2 Z9 2 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD AUG 1 PY 2016 VL 826 IS 2 AR L26 DI 10.3847/2041-8205/826/2/L26 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DT2TN UT WOS:000381334800010 ER PT J AU Chang, KE Hsiao, TC Hsu, NC Lin, NH Wang, SH Liu, GR Liu, CY Lin, TH AF Chang, Kuo-En Hsiao, Ta-Chih Hsu, N. Christina Lin, Neng-Huei Wang, Sheng-Hsiang Liu, Gin-Rong Liu, Chian-Yi Lin, Tang-Huang TI Mixing weight determination for retrieving optical properties of polluted dust with MODIS and AERONET data SO ENVIRONMENTAL RESEARCH LETTERS LA English DT Article DE mixing weight; dust-soot aerosols; MODIS; AOD; SSA; AERONET; spatial distribution ID AEROSOL PROPERTIES; SCATTERING PROPERTIES; SURFACE REFLECTIVITY; MISR AEROSOL; PARTICLES; EMISSIONS; PRODUCTS; EGYPT; RANGE; DEPTH AB In this study, an approach in determining effective mixing weight of soot aggregates from dust-soot aerosols is proposed to improve the accuracy of retrieving properties of polluted dusts by means of satellite remote sensing. Based on a pre-computed database containing several variables (such as wavelength, refractive index, soot mixing weight, surface reflectivity, observation geometries and aerosol optical depth (AOD)), the fan-shaped look-up tables can be drawn out accordingly for determining the mixing weights, AOD and single scattering albedo (SSA) of polluted dusts simultaneously with auxiliary regional dust properties and surface reflectivity. To validate the performance of the approach in this study, 6 cases study of polluted dusts (dust-soot aerosols) in Lower Egypt and Israel were examined with the ground-based measurements through AErosol RObotic NETwork (AERONET). The results show that the mean absolute differences could be reduced from 32.95% to 6.56% in AOD and from 2.67% to 0.83% in SSA retrievals for MODIS aerosol products when referenced to AERONET measurements, demonstrating the soundness of the proposed approach under different levels of dust loading, mixing weight and surface reflectivity. Furthermore, the developed algorithm is capable of providing the spatial distribution of the mixing weights and removing the requirement to assume that the dust plume properties are uniform. The case study further shows the spatially variant dust-soot mixing weight would improve the retrieval accuracy in AOD(mixture) and SSA(mixture) about 10.0% and 1.4% respectively. C1 [Chang, Kuo-En; Lin, Tang-Huang] Natl Cent Univ, Grad Inst Space Sci, Taoyuan 32001, Taiwan. [Hsiao, Ta-Chih] Natl Cent Univ, Grad Inst Environm Engn, Taoyuan 32001, Taiwan. [Hsu, N. Christina] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA. [Lin, Neng-Huei; Wang, Sheng-Hsiang; Liu, Gin-Rong; Liu, Chian-Yi] Natl Cent Univ, Dept Atmospher Sci, Taoyuan 32001, Taiwan. [Liu, Gin-Rong; Liu, Chian-Yi; Lin, Tang-Huang] Natl Cent Univ, Ctr Space & Remote Sensing Res, Taoyuan 32001, Taiwan. RP Lin, TH (reprint author), Natl Cent Univ, Grad Inst Space Sci, Taoyuan 32001, Taiwan.; Lin, TH (reprint author), Natl Cent Univ, Ctr Space & Remote Sensing Res, Taoyuan 32001, Taiwan. EM thlin@csrsr.ncu.edu.tw OI Liu, Chian-Yi/0000-0003-1725-4405; Hsiao, Ta-Chih/0000-0003-4103-6272 FU Taiwan Ministry of Science and Technology [MOST 103-2111-M-008-002, MOST 104-2111-M-008-007]; College of Geosciences at Texas AM University; NSF [ATM-0803779] FX This work was financially supported by the Taiwan Ministry of Science and Technology Grant MOST 103-2111-M-008-002 and MOST 104-2111-M-008-007. We are grateful to being partially supported by the College of Geosciences at Texas A&M University and NSF Grant ATM-0803779, as well as to Professor Ping Yang at Texas A&M University for providing the single-scattering properties of triaxial-ellipsoidal mineral dust in this study. NR 45 TC 0 Z9 0 U1 9 U2 9 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 1748-9326 J9 ENVIRON RES LETT JI Environ. Res. Lett. PD AUG PY 2016 VL 11 IS 8 AR 085002 DI 10.1088/1748-9326/11/8/085002 PG 11 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA DT9NH UT WOS:000381828300019 ER PT J AU Park, T Ganguly, S Tommervik, H Euskirchen, ES Hogda, KA Karlsen, SR Brovkin, V Nemani, RR Myneni, RB AF Park, Taejin Ganguly, Sangram Tommervik, Hans Euskirchen, Eugenie S. Hogda, Kjell-Arild Karlsen, Stein Rune Brovkin, Victor Nemani, Ramakrishna R. Myneni, Ranga B. TI Changes in growing season duration and productivity of northern vegetation inferred from long-term remote sensing data SO ENVIRONMENTAL RESEARCH LETTERS LA English DT Article DE photosynthetically active growing season; gross primary productivity; boreal and arctic; remote sensing; climate change; AVHRR; MODIS ID GROSS PRIMARY PRODUCTIVITY; CLIMATE-CHANGE; MONITORING VEGETATION; HIGH-LATITUDES; ECOLOGICAL RESPONSES; ARCTIC VEGETATION; DATA SET; PHENOLOGY; NDVI; AMERICA AB Monitoring and understanding climate-induced changes in the boreal and arctic vegetation is critical to aid in prognosticating their future. Weused a 33 year (1982-2014) long record of satellite observations to robustly assess changes in metrics of growing season (onset: SOS, end: EOS and length: LOS) and seasonal total gross primary productivity. Particular attention was paid to evaluating the accuracy of these metrics by comparing them to multiple independent direct and indirect growing season and productivity measures. These comparisons reveal that the derived metrics capture the spatio-temporal variations and trends with acceptable significance level (generally p < 0.05). We find that LOS has lengthened by 2.60 d dec(-1) (p < 0.05) due to an earlier onset of SOS (-1.61 d dec(-1), p < 0.05) and a delayed EOS (0.67 d dec(-1), p < 0.1) at the circumpolar scale over the past three decades. Relatively greater rates of changes in growing season were observed in Eurasia (EA) and in boreal regions than in North America (NA) and the arctic regions. However, this tendency of earlier SOS and delayed EOS was prominent only during the earlier part of the data record (1982-1999). During the later part (2000-2014), this tendency was reversed, i.e. delayed SOS and earlier EOS. As for seasonal total productivity, we find that 42.0% of northern vegetation shows a statistically significant (p < 0.1) greening trend over the last three decades. This greening translates to a 20.9% gain in productivity since 1982. In contrast, only 2.5% of northern vegetation shows browning, or a 1.2% loss of productivity. These trends in productivity were continuous through the period of record, unlike changes in growing season metrics. Similarly, we find relatively greater increasing rates of productivity in EA and in arctic regions than in NA and the boreal regions. These results highlight spatially and temporally varying vegetation dynamics and are reflective of biome-specific responses of northern vegetation during last three decades. C1 [Park, Taejin; Myneni, Ranga B.] Boston Univ, Dept Earth & Environm, Boston, MA 02215 USA. [Ganguly, Sangram] NASA, Ames Res Ctr, Bay Area Environm Res Inst, Moffett Field, CA 94035 USA. [Tommervik, Hans] Norwegian Inst Nat Res, FRAM High North Ctr Climate & Environm, POB 6606, N-9296 Tromso, Norway. [Euskirchen, Eugenie S.] Univ Alaska Fairbanks, Inst Arctic Biol, Fairbanks, AK USA. [Hogda, Kjell-Arild; Karlsen, Stein Rune] Norut, POB 6434, N-9294 Tromso, Norway. [Brovkin, Victor] Max Planck Inst Meteorol, Hamburg, Germany. [Nemani, Ramakrishna R.] NASA, Ames Res Ctr, Adv Supercomp Div, Moffett Field, CA 94035 USA. RP Park, T (reprint author), Boston Univ, Dept Earth & Environm, Boston, MA 02215 USA. EM parktj@bu.edu RI Brovkin, Victor/C-2803-2016; Myneni, Ranga/F-5129-2012 OI Brovkin, Victor/0000-0001-6420-3198; FU NASA Earth Science Division [NNX14AP80A]; ArcticBiomass Project (Norway-USA network project - Research Council of Norway) [RCN 227064] FX This work was funded by the NASA Earth Science Division (Grant No. NNX14AP80A) and the ArcticBiomass (Grant No. RCN 227064) Project (Norway-USA network project funded by the Research Council of Norway). We gratefully acknowledge the NASA GIMMS group and FLUXNET community for sharing the invaluable datasets (i.e., NDVI3g and fair-use eddy covariance datasets, respectively) and thank Sungho Choi and Jian Bi for helpful comments and guides. NR 56 TC 1 Z9 1 U1 33 U2 42 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 1748-9326 J9 ENVIRON RES LETT JI Environ. Res. Lett. PD AUG PY 2016 VL 11 IS 8 AR 084001 DI 10.1088/1748-9326/11/8/084001 PG 11 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA DT9NH UT WOS:000381828300002 ER PT J AU Sung, MK Kim, BM Baek, EH Lim, YK Kim, SJ AF Sung, Mi-Kyung Kim, Baek-Min Baek, Eun-Hyuk Lim, Young-Kwon Kim, Seong-Joong TI Arctic-North Pacific coupled impacts on the late autumn cold in North America SO ENVIRONMENTAL RESEARCH LETTERS LA English DT Article DE Pacific decadal oscillation; arctic warming; Arctic-midlatitude interaction ID EXTRATROPICAL SST ANOMALIES; DECADAL OSCILLATION; ATMOSPHERIC CIRCULATION; CLIMATE-CHANGE; UNITED-STATES; SEA-ICE; WINTER; HEMISPHERE; TEMPERATURE; VARIABILITY AB The Pacific decadal oscillation (PDO) is known to bring an anomalously cold (warm) period to southeastern (northwestern) North America during the cold season of its positive phase through a Rossby wave linkage. This study provides evidence that the remote connection between the North Pacific and the downstream temperature over central North America is strengthened by the warm arctic conditions over the Chukchi and East Siberian Sea, especially in the late autumn season. The modulation effect of the Arctic manifests itself as an altered Rossby wave response to a transient vorticity forcing that results from an equatorward storm track shift, which is induced collaboratively by the PDO and the warm Arctic. This observational finding is supported by two independent modeling experiments: (1) an idealized coupled GCM experiment being nudged toward the warm arctic surface condition and (2) a simple stationary wave model experiment forced by transient eddy forcing. C1 [Sung, Mi-Kyung; Kim, Baek-Min; Baek, Eun-Hyuk; Kim, Seong-Joong] Korea Polar Res Inst, Inchon, South Korea. [Lim, Young-Kwon] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Goddard Earth Sci Technol & Res,IM Syst Grp, Greenbelt, MD USA. RP Kim, BM (reprint author), Korea Polar Res Inst, Inchon, South Korea. EM bmkim@kopri.re.kr FU Korean government [KMIPA2015-2093 (PN16040)]; 'Development and Application of the Korea Polar Prediction System (KPOPS) for Climate Change and Weather Disaster' project [PE16100] FX This study was supported by KMIPA2015-2093 (PN16040) of the Korean government and 'Development and Application of the Korea Polar Prediction System (KPOPS) for Climate Change and Weather Disaster (PE16100)' project. NR 49 TC 0 Z9 0 U1 10 U2 11 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 1748-9326 J9 ENVIRON RES LETT JI Environ. Res. Lett. PD AUG PY 2016 VL 11 IS 8 AR 084016 DI 10.1088/1748-9326/11/8/084016 PG 8 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA DT9NH UT WOS:000381828300017 ER PT J AU Jungbluth, SP Bowers, RM Lin, HT Cowen, JP Rappe, MS AF Jungbluth, Sean P. Bowers, Robert M. Lin, Huei-Ting Cowen, James P. Rappe, Michael S. TI Novel microbial assemblages inhabiting crustal fluids within mid-ocean ridge flank subsurface basalt SO ISME JOURNAL LA English DT Article ID DE-FUCA RIDGE; HYDROTHERMAL CIRCULATION; OCEANIC-CRUST; SEA-FLOOR; BASEMENT FLUIDS; EASTERN FLANK; BIOSPHERE; DIVERSITY; SEDIMENT; SUBSEAFLOOR AB Although little is known regarding microbial life within our planet's rock-hosted deep subseafloor biosphere, boreholes drilled through deep ocean sediment and into the underlying basaltic crust provide invaluable windows of access that have been used previously to document the presence of microorganisms within fluids percolating through the deep ocean crust. In this study, the analysis of 1.7 million small subunit ribosomal RNA genes amplified and sequenced from marine sediment, bottom seawater and basalt-hosted deep subseafloor fluids that span multiple years and locations on the Juan de Fuca Ridge flank was used to quantitatively delineate a subseafloor microbiome comprised of distinct bacteria and archaea. Hot, anoxic crustal fluids tapped by newly installed seafloor sampling observatories at boreholes U1362A and U1362B contained abundant bacterial lineages of phylogenetically unique Nitrospirae, Aminicenantes, Calescamantes and Chloroflexi. Although less abundant, the domain Archaea was dominated by unique, uncultivated lineages of marine benthic group E, the Terrestrial Hot Spring Crenarchaeotic Group, the Bathyarchaeota and relatives of cultivated, sulfate-reducing Archaeoglobi. Consistent with recent geochemical measurements and bioenergetic predictions, the potential importance of methane cycling and sulfate reduction were imprinted within the basalt-hosted deep subseafloor crustal fluid microbial community. This unique window of access to the deep ocean subsurface basement reveals a microbial landscape that exhibits previously undetected spatial heterogeneity. C1 [Jungbluth, Sean P.; Rappe, Michael S.] Univ Hawaii, Hawaii Inst Marine Biol, SOEST, POB 1346, Kaneohe, HI 96744 USA. [Jungbluth, Sean P.; Lin, Huei-Ting; Cowen, James P.] Univ Hawaii, Dept Oceanog, SOEST, Honolulu, HI 96822 USA. [Bowers, Robert M.] Univ Hawaii, NASA, Astrobiol Inst, IfA, Honolulu, HI 96822 USA. [Bowers, Robert M.] DOE Joint Genome Inst, 2800 Mitchell Dr, Walnut Creek, CA 94598 USA. RP Rappe, MS (reprint author), Univ Hawaii, Hawaii Inst Marine Biol, SOEST, POB 1346, Kaneohe, HI 96744 USA. EM rappe@hawaii.edu RI Jungbluth, Sean/A-9054-2012 OI Jungbluth, Sean/0000-0001-9265-8341 FU National Science Foundation Microbial Observatories [MCB06-04014]; Schlanger Ocean Drilling Fellowship; National Science Foundation-funded Science and Technology Centers of Excellence; UH NASA Astrobiology Institute; Center for Dark Energy Biosphere Investigations (C-DEBI) [OCE-0939564]; NSF FX This study is dedicated to the memory of our friend, colleague, mentor and co-author, James P Cowen, whose determination and enthusiasm were driving forces in the adaptation of seafloor borehole observatories for microbiology. We thank the captain and crew, A Fisher, K Becker, CG Wheat and other members of the science teams on board R/V Atlantis cruises AT15-35, AT15-51, AT15-66 and AT18-07. We also thank the pilots and crew of human-occupied vehicle Alvin and remote-operated vehicle Jason II and Brian Glazer, Ryan Matsumoto, Michael Matzinger, Michelle Jungbluth, Alberto Robador, Jennifer Murphy, Chih-Chiang Hseih, Natalie Hamada, Karen Meech and Joshua Bninski for sampling, technical and other assistance. This research was supported by funding from National Science Foundation Microbial Observatories grant MCB06-04014 (to JC and MSR), a Schlanger Ocean Drilling Fellowship (to SPJ), which is part of the NSF-sponsored US Science Support Program for IODP that is administered by the Consortium for Ocean Leadership, the UH NASA Astrobiology Institute and the Center for Dark Energy Biosphere Investigations (C-DEBI) (OCE-0939564), a National Science Foundation-funded Science and Technology Centers of Excellence. This study used samples and data provided by the Integrated Ocean Drilling Program. This is SOEST contribution 9539, HIMB contribution 1636 and C-DEBI contribution 289. NR 57 TC 1 Z9 1 U1 7 U2 7 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 1751-7362 EI 1751-7370 J9 ISME J JI ISME J. PD AUG PY 2016 VL 10 IS 8 BP 2033 EP 2047 DI 10.1038/ismej.2015.248 PG 15 WC Ecology; Microbiology SC Environmental Sciences & Ecology; Microbiology GA DS7JN UT WOS:000380959800020 PM 26872042 ER PT J AU Crucian, B Johnston, S Mehta, S Stowe, R Uchakin, P Quiriarte, H Pierson, D Laudenslager, ML Sams, C AF Crucian, Brian Johnston, Smith Mehta, Satish Stowe, Raymond Uchakin, Peter Quiriarte, Heather Pierson, Duane Laudenslager, Mark L. Sams, Clarence TI Acaseofpersistent skinrashandrhinitis with immune system dysregulation onboard the International Space Station SO JOURNAL OF ALLERGY AND CLINICAL IMMUNOLOGY-IN PRACTICE LA English DT Letter ID VARICELLA-ZOSTER-VIRUS; LONG-DURATION SPACEFLIGHT; EPSTEIN-BARR-VIRUS; CHRONIC STRESS; HERPES-ZOSTER; REACTIVATION; ASTRONAUTS; SALIVA; RESPONSES; FLIGHT C1 [Crucian, Brian; Pierson, Duane] NASA, Johnson Space Ctr, Biomed Res & Environm Sci, Houston, TX USA. [Johnston, Smith; Sams, Clarence] NASA, Johnson Space Ctr, Space & Clin Operat, Houston, TX USA. [Mehta, Satish; Quiriarte, Heather] JES Tech, Biomed Res & Environm Sci, Houston, TX USA. [Stowe, Raymond] Microgen Labs, Immunol Res, La Marque, TX USA. [Uchakin, Peter] Mercer Univ, Dept Internal Med, Macon, GA 31207 USA. [Laudenslager, Mark L.] Univ Colorado, Denver Anschutz Med Campus, Behav Immunol & Endocrinol Lab, Denver, CO 80202 USA. RP Crucian, B (reprint author), NASA, Johnson Space Ctr, 2101 NASA Pkwy, Houston, TX 77058 USA. EM brian.crucian-1@nasa.gov OI Laudenslager, Mark/0000-0002-9815-3026 NR 23 TC 1 Z9 1 U1 2 U2 2 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 2213-2198 EI 2213-2201 J9 J ALLER CL IMM-PRACT JI J. Allergy Clin. Immunol.-Pract. PD AUG PY 2016 VL 4 IS 4 BP 759 EP + DI 10.1016/j.jaip.2015.12.021 PG 12 WC Allergy; Immunology SC Allergy; Immunology GA DU0SZ UT WOS:000381916100033 PM 27036643 ER PT J AU Datiles, MB Ferris, F Ansari, RR Zigler, JS AF Datiles, Manuel B., III Ferris, Frederick, III Ansari, Rafat R. Zigler, J. Samuel, Jr. TI Re: Datiles et al.: Longitudinal study of age-related cataract using dynamic light scattering: loss of alpha-crystallin leads to nuclear cataract development (Ophthalmology 2016;123:248-54) REPLY SO OPHTHALMOLOGY LA English DT Letter C1 [Datiles, Manuel B., III; Ferris, Frederick, III] NEI, Off Clin Director, NIH, 10 Ctr Dr,Bldg 10,Room 1, Bethesda, MD 20892 USA. [Ansari, Rafat R.] NASA, Glenn Res Ctr, Cleveland, OH USA. [Zigler, J. Samuel, Jr.] Johns Hopkins Univ Hosp, Wilmer Eye Inst, Baltimore, MD 21287 USA. RP Datiles, MB (reprint author), NEI, Off Clin Director, NIH, 10 Ctr Dr,Bldg 10,Room 1, Bethesda, MD 20892 USA. EM Datilesm@nei.nih.gov NR 1 TC 0 Z9 0 U1 3 U2 3 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0161-6420 EI 1549-4713 J9 OPHTHALMOLOGY JI Ophthalmology PD AUG PY 2016 VL 123 IS 8 BP E48 EP E48 PG 1 WC Ophthalmology SC Ophthalmology GA DS4MC UT WOS:000380754200005 PM 27450826 ER PT J AU Naghipour, P Pineda, EJ Arnold, SM AF Naghipour, P. Pineda, E. J. Arnold, S. M. TI Simulation of Lightning-Induced Delamination in Un-protected CFRP Laminates SO APPLIED COMPOSITE MATERIALS LA English DT Article DE Lightning damage; Temperature-dependent delamination; Interlaminar damage ID COMPOSITES; MODELS AB Lightning is a major cause of damage in laminated composite aerospace structures during flight. The most significant failure mode induced by lightning is delamination, which might extend well beyond the visible damage zone, and requires sophisticated techniques and equipment to detect. Therefore, it is crucial to develop a numerical tool capable of predicting the damage zone induced from a lightning strike to minimize costly repair acreage and supplement extremely expensive lightning experiments. Herein, a detailed numerical study consisting of a multidirectional composite with user-defined, temperature-dependent, interlaminar elements subjected to a lightning strike is designed, and delamination/damage expansion is studied under specified conditions. It is observed both the size and shape of the delamination zone are strongly dependent on the assumed temperature-dependent fracture toughness; the primary parameter controlling lightning-induced delamination propagation. An accurate estimation of the fracture toughness profile is crucial in order to have a reliable prediction of the delamination zone and avoid sub-critical structural failures. C1 [Naghipour, P.] Ohio Aerosp Inst, 22800 Cedar Point Rd, Cleveland, OH 44142 USA. [Pineda, E. J.; Arnold, S. M.] NASA, Glenn Res Ctr, 21000 Brookpark Rd, Cleveland, OH 44135 USA. RP Naghipour, P (reprint author), Ohio Aerosp Inst, 22800 Cedar Point Rd, Cleveland, OH 44142 USA. EM paria.naghipourghezeljeh@nasa.gov FU NASA Atmospheric Environment Safety Technologies (AEST) Project FX The authors would like to thank George Szatkowski and Kenneth Dudley from NASA LaRC for providing the experimental data used in this manuscript. This work was funded under the NASA Atmospheric Environment Safety Technologies (AEST) Project. NR 22 TC 0 Z9 0 U1 6 U2 8 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0929-189X EI 1573-4897 J9 APPL COMPOS MATER JI Appl. Compos. Mater. PD AUG PY 2016 VL 23 IS 4 BP 523 EP 535 DI 10.1007/s10443-016-9472-9 PG 13 WC Materials Science, Composites SC Materials Science GA DS3DV UT WOS:000380664100001 ER PT J AU Galazka, JM Klocko, AD Uesaka, M Honda, S Selker, EU Freitag, M AF Galazka, Jonathan M. Klocko, Andrew D. Uesaka, Miki Honda, Shinji Selker, Eric U. Freitag, Michael TI Neurospora chromosomes are organized by blocks of importin alpha-dependent heterochromatin that are largely independent of H3K9me3 SO GENOME RESEARCH LA English DT Article ID DNA METHYLATION; HISTONE H3; DROSOPHILA GENOME; FACULTATIVE HETEROCHROMATIN; NUCLEAR ARCHITECTURE; X-CHROMOSOME; CRASSA; CHROMATIN; GENE; YEAST AB Eukaryotic genomes are organized into chromatin domains with three-dimensional arrangements that presumably result from interactions between the chromatin constituents-proteins, DNA, and RNA-within the physical constraints of the nucleus. We used chromosome conformation capture (3C) followed by high-throughput sequencing (Hi-C) with wild-type and mutant strains of Neurospora crassa to gain insight into the role of heterochromatin in the organization and function of the genome. We tested the role of three proteins thought to be important for establishment of heterochromatin, namely, the histone H3 lysine 9 methyltransferase DIM-5, Heterochromatin Protein 1 (HP1), which specifically binds to the product of DIM-5 (trimethylated H3 lysine 9 [H3K9me3]), and DIM-3 (importin alpha), which is involved in DIM-5 localization. The average genome configuration of the wild-type strain revealed strong intra-and inter-chromosomal associations between both constitutive and facultative heterochromatic domains, with the strongest interactions among the centromeres, subtelomeres, and interspersed heterochromatin. Surprisingly, loss of either H3K9me3 or HP1 had only mild effects on heterochromatin compaction, whereas dim-3 caused more drastic changes, specifically decreasing interactions between constitutive heterochromatic domains. Thus, associations between heterochromatic regions are a major component of the chromosome conformation in Neurospora, but two widely studied key heterochromatin proteins are not necessary, implying that undefined protein factors play key roles in maintaining overall chromosome organization. C1 [Galazka, Jonathan M.; Freitag, Michael] Oregon State Univ, Dept Biochem & Biophys, Corvallis, OR 97331 USA. [Klocko, Andrew D.; Selker, Eric U.] Univ Oregon, Inst Mol Biol, Eugene, OR 97403 USA. [Uesaka, Miki; Honda, Shinji] Univ Fukui, Fac Med Sci, Dept Biochem & Bioinformat Sci, Fukui 9101193, Japan. [Galazka, Jonathan M.] NASA, Ames Res Ctr, Space Biosci Div, Moffett Field, CA 94035 USA. RP Freitag, M (reprint author), Oregon State Univ, Dept Biochem & Biophys, Corvallis, OR 97331 USA. EM freitagm@cgrb.oregonstate.edu FU National Institute of General Medical Sciences (NIH) [GM097637, GM035690, GM093061, GM097821]; Competitive Funds in Program to Disseminate Tenure Tracking System grant, MEXT, Japan; NASA Postdoctoral Program fellowship FX We thank Tereza Ormsby for validating the Delta hpo::hph strain obtained from the Fungal Genetics Stock Center; Diana Libuda and Jackie Helm for assistance with deconvolution microscopy; Jordan Gessaman for assistance with nuclear membrane diameter statistics; and Ayumi Yokoyama for technical support. We also thank members of the Freitag and Selker laboratories for helpful comments and discussions. Funding was provided by grants from the National Institute of General Medical Sciences (NIH) to M.F. (GM097637), E.U.S. (GM035690 and GM093061), and A.D.K. (GM097821), and a Competitive Funds in Program to Disseminate Tenure Tracking System grant, MEXT, Japan, to S.H. J.M.G. was partly supported by a NASA Postdoctoral Program fellowship. NR 56 TC 3 Z9 3 U1 2 U2 3 PU COLD SPRING HARBOR LAB PRESS, PUBLICATIONS DEPT PI COLD SPRING HARBOR PA 1 BUNGTOWN RD, COLD SPRING HARBOR, NY 11724 USA SN 1088-9051 EI 1549-5469 J9 GENOME RES JI Genome Res. PD AUG PY 2016 VL 26 IS 8 BP 1069 EP 1080 DI 10.1101/gr.203182.115 PG 12 WC Biochemistry & Molecular Biology; Biotechnology & Applied Microbiology; Genetics & Heredity SC Biochemistry & Molecular Biology; Biotechnology & Applied Microbiology; Genetics & Heredity GA DT8IH UT WOS:000381733000006 PM 27260477 ER PT J AU Williams, CA Gu, H MacLean, R Masek, JG Collatz, GJ AF Williams, Christopher A. Gu, Huan MacLean, Richard Masek, Jeffrey G. Collatz, G. James TI Disturbance and the carbon balance of US forests: A quantitative review of impacts from harvests, fires, insects, and droughts SO GLOBAL AND PLANETARY CHANGE LA English DT Review DE Forest ecology and management; Carbon sequestration; Climate change; Global environmental change; Carbon balance and management ID MOUNTAIN PINE-BEETLE; WESTERN UNITED-STATES; CANADA BOREAL FORESTS; OLD-GROWTH FORESTS; CLIMATE-CHANGE; TREE MORTALITY; MANAGING FORESTS; LODGEPOLE PINE; INVENTORY DATA; HURRICANE IMPACTS AB Disturbances are a major determinant of forest carbon stocks and uptake. They generally reduce land carbon stocks but also initiate a regrowth legacy that contributes substantially to the contemporary rate of carbon stock increase in US forestlands. As managers and policy makers increasingly look to forests for climate protection and mitigation, and because of increasing concern about changes in disturbance intensity and frequency, there is a need for synthesis and integration of current understanding about the role of disturbances and other processes in governing forest carbon cycle dynamics, and the likely future of this and other sinks for atmospheric carbon. This paper aims to address that need by providing a quantitative review of the distribution, extent and carbon impacts of the major disturbances active in the US. We also review recent trends in disturbances, climate, and other global environmental changes and consider their individual and collective contributions to the US carbon budget now and in the likely future. Lastly, we identify some key challenges and opportunities for future research needed to improve current understanding, advance predictive capabilities, and inform forest management in the face of these pressures. Harvest is found to be the most extensive disturbance both in terms of area and carbon impacts, followed by fire, windthrow and bark beetles, and lastly droughts. Collectively these lead to the gross loss of about 200 Tg C y(-1) in live biomass annually across the conterminous US. At the same time, the net change in forest carbon stocks is positive (190 Tg C y(-1)), indicating not only forest resilience but also an apparently large response to growth enhancements such as fertilization by CO2 and nitrogen. Uncertainty about disturbance legacies, disturbance interactions, likely trends, and global change factors make the future of the US forest carbon sink unclear. While there is scope for management to enhance carbon sinks in US forests, tradeoffs with other values and uses are likely to significantly limit practical implementation. Continued and expanded remote sensing and field-based monitoring capabilities and manipulative experimentation are needed to improve understanding of the US forest carbon sink, and assess how disturbance processes are responding to the pressures of global environmental change. In addition, continued development and application of holistic, decision support tools that consider a range of forest values are needed to enable managers and policy makers to use the best available information for guiding forest resources now and into the future. (C) 2016 Elsevier B.V. All rights reserved. C1 [Williams, Christopher A.; Gu, Huan; MacLean, Richard] Clark Univ, Grad Sch Geog, Worcester, MA 01610 USA. [Masek, Jeffrey G.; Collatz, G. James] NASA, Goddard Space Flight Ctr, Biospher Sci Lab, Greenbelt, MD USA. RP Williams, CA (reprint author), Clark Univ, Grad Sch Geog, Worcester, MA 01610 USA. RI collatz, george/D-5381-2012 FU NASA's Carbon Monitoring System program [NNH14ZDA001N-CMS, NNX14AR39G] FX We thank Timothy Horscroft and the editors of Global and Planetary Change for inviting this review. We also thank two anonymous reviewers for providing helpful critique that resulted in substantial improvements. This study was supported by NASA's Carbon Monitoring System program (NNH14ZDA001N-CMS) under award NNX14AR39G. NR 157 TC 2 Z9 2 U1 62 U2 82 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0921-8181 EI 1872-6364 J9 GLOBAL PLANET CHANGE JI Glob. Planet. Change PD AUG PY 2016 VL 143 BP 66 EP 80 DI 10.1016/j.gloplacha.2016.06.002 PG 15 WC Geography, Physical; Geosciences, Multidisciplinary SC Physical Geography; Geology GA DS2IU UT WOS:000380594000007 ER PT J AU Hobbs, WR Massom, R Stammerjohn, S Reid, P Williams, G Meier, W AF Hobbs, William R. Massom, Rob Stammerjohn, Sharon Reid, Phillip Williams, Guy Meier, Walter TI A review of recent changes in Southern Ocean sea ice, their drivers and forcings SO GLOBAL AND PLANETARY CHANGE LA English DT Review ID WESTERN ANTARCTIC PENINSULA; LOW-FREQUENCY VARIABILITY; SURFACE MASS-BALANCE; NCEP-NCAR REANALYSES; EARTH SYSTEM MODEL; FRESH-WATER FLUX; CLIMATE-CHANGE; CMIP5 MODELS; ANNULAR MODE; WHALING RECORDS AB Over the past 37 years, satellite records show an increase in Antarctic sea ice cover that is most pronounced in the period of sea ice growth. This trend is dominated by increased sea ice coverage in the western Ross Sea, and is mitigated by a strong decrease in the Bellingshausen and Amundsen seas. The trends in sea ice areal coverage are accompanied by related trends in yearly duration. These changes have implications for ecosystems, as well as global and regional climate. In this review, we summarise the research to date on observing these trends, identifying their drivers, and assessing the role of anthropogenic climate change. Whilst the atmosphere is thought to be the primary driver, the ocean is also essential in explaining the seasonality of the trend patterns. Detecting an anthropogenic signal in Antarctic sea ice is particularly challenging for a number of reasons: the expected response is small compared to the very high natural variability of the system; the observational record is relatively short; and the ability of global coupled climate models to faithfully represent the complex Antarctic climate system is in doubt. (C) 2016 Elsevier B.V. All rights reserved. C1 [Hobbs, William R.; Massom, Rob; Reid, Phillip] Univ Tasmania, Antarctic Climate & Ecosyst Cooperat Res Ctr, Private Bag 80, Hobart, Tas 7001, Australia. [Hobbs, William R.] Univ Tasmania, ARC Ctr Excellence Climate Syst Sci, IMAS, Private Bag 129, Hobart, Tas 7001, Australia. [Massom, Rob] Australian Antarctic Div, 203 Channel Highway, Kingston, Tas 7050, Australia. [Stammerjohn, Sharon] Univ Colorado, Inst Arctic & Alpine Res, Boulder, CO 80309 USA. [Reid, Phillip] Australian Bur Meteorol, Ctr Australian Weather & Climate Res, Hobart, Tas, Australia. [Williams, Guy] Univ Tasmania, Inst Marine & Antarctic Studies, Private Bag 129, Hobart, Tas 7001, Australia. [Meier, Walter] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA. RP Hobbs, WR (reprint author), Univ Tasmania, Antarctic Climate & Ecosyst Cooperat Res Ctr, Private Bag 80, Hobart, Tas 7001, Australia. EM whobbs@utas.edu.au RI Hobbs, Will/G-5116-2014; OI Hobbs, Will/0000-0002-2061-0899; STAMMERJOHN, SHARON/0000-0002-1697-8244; Meier, Walter/0000-0003-2857-0550 FU Australian Government's Cooperative Research Centres Programme through the Antarctic Climate and Ecosystems Cooperative Research Center (ACE CRC); National Science Foundation Office of Polar Programs Palmer Long-Term Ecological Project [ANT-1440435]; [4116] FX The authors are indebted to William de la Mare for providing his whale catch data, Kate Sinclair for the Whitehall Glacier excess deuterium record, and Holly Titchner for providing the HadISST2.2 sea ice concentration data. The authors express their gratitude to Paul Holland and an anonymous reviewer for their invaluable comments and help in improving this manuscript. Data analysis and visualisation was performed using NCL (http://dx.doi.org/10.5065/D6WD3XH5). We acknowledge the World Climate Research Programme's Working Group on Coupled Modeling, which is responsible for CMIP, and we thank the climate modeling groups (listed in Appendix A) for producing and making available their model output. For CMIP the U.S. Department of Energy's Programme 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. This work was supported by the Australian Government's Cooperative Research Centres Programme through the Antarctic Climate and Ecosystems Cooperative Research Center (ACE CRC), and contributes to AAS Project 4116. SS acknowledges support and contributions from the National Science Foundation Office of Polar Programs Palmer Long-Term Ecological Project (ANT-1440435). NR 265 TC 7 Z9 7 U1 19 U2 30 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0921-8181 EI 1872-6364 J9 GLOBAL PLANET CHANGE JI Glob. Planet. Change PD AUG PY 2016 VL 143 BP 228 EP 250 DI 10.1016/j.gloplacha.2016.06.008 PG 23 WC Geography, Physical; Geosciences, Multidisciplinary SC Physical Geography; Geology GA DS2IU UT WOS:000380594000018 ER PT J AU Abbott, T Abdalla, FB Aleksic, J Allam, S Amara, A Bacon, D Balbinot, E Banerji, M Bechtol, K Benoit-Levy, A Bernstein, GM Bertin, E Blazek, J Bonnett, C Bridle, S Brooks, D Brunner, RJ Buckley-Geer, E Burke, DL Caminha, GB Capozzi, D Carlsen, J Carnero-Rosell, A Carollo, M Carrasco-Kind, M Carretero, J Castander, FJ Clerkin, L Collett, T Conselice, C Crocce, M Cunha, CE D'Andrea, CB da Costa, LN Davis, TM Desai, S Diehl, HT Dietrich, JP Dodelson, S Doel, P Drlica-Wagner, A Estrada, J Etherington, J Evrard, AE Fabbri, J Finley, DA Flaugher, B Foley, RJ Fosalba, P Frieman, J Garcia-Bellido, J Gaztanaga, E Gerdes, DW Giannantonio, T Goldstein, DA Gruen, D Gruendl, RA Guarnieri, P Gutierrez, G Hartley, W Honscheid, K Jain, B James, DJ Jeltema, T Jouvel, S Kessler, R King, A Kirk, D Kron, R Kuehn, K Kuropatkin, N Lahav, O Li, TS Lima, M Lin, H Maia, MAG Makler, M Manera, M Maraston, C Marshall, JL Martini, P McMahon, RG Melchior, P Merson, A Miller, CJ Miquel, R Mohr, JJ Morice-Atkinson, X Naidoo, K Neilsen, E Nichol, RC Nord, B Ogando, R Ostrovski, F Palmese, A Papadopoulos, A Peiris, HV Peoples, J Percival, WJ Plazas, AA Reed, SL Refregier, A Romer, AK Roodman, A Ross, A Rozo, E Rykoff, ES Sadeh, I Sako, M Sanchez, C Sanchez, E Santiago, B Scarpine, V Schubnell, M Sevilla-Noarbe, I Sheldon, E Smith, M Smith, RC Soares-Santos, M Sobreira, F Soumagnac, M Suchyta, E Sullivan, M Swanson, M Tarle, G Thaler, J Thomas, D Thomas, RC Tucker, D Vieira, JD Vikram, V Walker, AR Wechsler, RH Weller, J Wester, W Whiteway, L Wilcox, H Yanny, B Zhang, Y Zuntz, J AF Abbott, T. Abdalla, F. B. Aleksic, J. Allam, S. Amara, A. Bacon, D. Balbinot, E. Banerji, M. Bechtol, K. Benoit-Levy, A. Bernstein, G. M. Bertin, E. Blazek, J. Bonnett, C. Bridle, S. Brooks, D. Brunner, R. J. Buckley-Geer, E. Burke, D. L. Caminha, G. B. Capozzi, D. Carlsen, J. Carnero-Rosell, A. Carollo, M. Carrasco-Kind, M. Carretero, J. Castander, F. J. Clerkin, L. Collett, T. Conselice, C. Crocce, M. Cunha, C. E. D'Andrea, C. B. da Costa, L. N. Davis, T. M. Desai, S. Diehl, H. T. Dietrich, J. P. Dodelson, S. Doel, P. Drlica-Wagner, A. Estrada, J. Etherington, J. Evrard, A. E. Fabbri, J. Finley, D. A. Flaugher, B. Foley, R. J. Fosalba, P. Frieman, J. Garcia-Bellido, J. Gaztanaga, E. Gerdes, D. W. Giannantonio, T. Goldstein, D. A. Gruen, D. Gruendl, R. A. Guarnieri, P. Gutierrez, G. Hartley, W. Honscheid, K. Jain, B. James, D. J. Jeltema, T. Jouvel, S. Kessler, R. King, A. Kirk, D. Kron, R. Kuehn, K. Kuropatkin, N. Lahav, O. Li, T. S. Lima, M. Lin, H. Maia, M. A. G. Makler, M. Manera, M. Maraston, C. Marshall, J. L. Martini, P. McMahon, R. G. Melchior, P. Merson, A. Miller, C. J. Miquel, R. Mohr, J. J. Morice-Atkinson, X. Naidoo, K. Neilsen, E. Nichol, R. C. Nord, B. Ogando, R. Ostrovski, F. Palmese, A. Papadopoulos, A. Peiris, H. V. Peoples, J. Percival, W. J. Plazas, A. A. Reed, S. L. Refregier, A. Romer, A. K. Roodman, A. Ross, A. Rozo, E. Rykoff, E. S. Sadeh, I. Sako, M. Sanchez, C. Sanchez, E. Santiago, B. Scarpine, V. Schubnell, M. Sevilla-Noarbe, I. Sheldon, E. Smith, M. Smith, R. C. Soares-Santos, M. Sobreira, F. Soumagnac, M. Suchyta, E. Sullivan, M. Swanson, M. Tarle, G. Thaler, J. Thomas, D. Thomas, R. C. Tucker, D. Vieira, J. D. Vikram, V. Walker, A. R. Wechsler, R. H. Weller, J. Wester, W. Whiteway, L. Wilcox, H. Yanny, B. Zhang, Y. Zuntz, J. CA Dark Energy Survey Collaboration TI The Dark Energy Survey: more than dark energy - an overview SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE surveys; minor planets, asteroids: general; supernovae: general; Galaxy: general; galaxies: general; quasars: general ID LARGE-MAGELLANIC-CLOUD; DIGITAL-SKY-SURVEY; BRIGHTEST CLUSTER GALAXIES; ACTIVE GALACTIC NUCLEI; SUPERMASSIVE BLACK-HOLES; GRAVITATIONALLY LENSED QUASARS; SCIENCE VERIFICATION DATA; STAR-FORMING GALAXIES; STELLAR MASS FUNCTION; MILKY-WAY SATELLITES AB This overview paper describes the legacy prospect and discovery potential of the Dark Energy Survey (DES) beyond cosmological studies, illustrating it with examples from the DES early data. DES is using a wide-field camera (DECam) on the 4 m Blanco Telescope in Chile to image 5000 sq deg of the sky in five filters (grizY). By its completion, the survey is expected to have generated a catalogue of 300 million galaxies with photometric redshifts and 100 million stars. In addition, a time-domain survey search over 27 sq deg is expected to yield a sample of thousands of Type Ia supernovae and other transients. The main goals of DES are to characterize dark energy and dark matter, and to test alternative models of gravity; these goals will be pursued by studying large-scale structure, cluster counts, weak gravitational lensing and Type Ia supernovae. However, DES also provides a rich data set which allows us to study many other aspects of astrophysics. In this paper, we focus on additional science with DES, emphasizing areas where the survey makes a difference with respect to other current surveys. The paper illustrates, using early data (from 'Science Verification', and from the first, second and third seasons of observations), what DES can tell us about the Solar system, the Milky Way, galaxy evolution, quasars and other topics. In addition, we show that if the cosmological model is assumed to be I >+cold dark matter, then important astrophysics can be deduced from the primary DES probes. Highlights from DES early data include the discovery of 34 trans-Neptunian objects, 17 dwarf satellites of the Milky Way, one published z > 6 quasar (and more confirmed) and two published superluminous supernovae (and more confirmed). C1 [Abbott, T.; James, D. J.; Smith, R. C.; Walker, A. R.] Cerro Tololo Interamer Observ, Natl Opt Astron Observ, La Serena, Chile. [Abdalla, F. B.; Benoit-Levy, A.; Brooks, D.; Clerkin, L.; Doel, P.; Fabbri, J.; Jouvel, S.; Kirk, D.; Lahav, O.; Manera, M.; Merson, A.; Naidoo, K.; Palmese, A.; Peiris, H. V.; Sadeh, I.; Soumagnac, M.; Whiteway, L.] UCL, Dept Phys & Astron, Gower St, London WC1E 6BT, England. [Aleksic, J.; Carretero, J.; Miquel, R.; Sanchez, C.] Barcelona Inst Sci & Technol, IFAE, Campus UAB, E-08193 Bellaterra, Barcelona, Spain. [Allam, S.; Buckley-Geer, E.; Diehl, H. T.; Dodelson, S.; Drlica-Wagner, A.; Estrada, J.; Finley, D. A.; Flaugher, B.; Frieman, J.; Gutierrez, G.; Kuropatkin, N.; Lin, H.; Neilsen, E.; Nord, B.; Peoples, J.; Scarpine, V.; Soares-Santos, M.; Sobreira, F.; Tucker, D.; Wester, W.; Yanny, B.] Fermilab Natl Accelerator Lab, POB 500, Batavia, IL 60510 USA. [Amara, A.; Hartley, W.; Refregier, A.] Swiss Fed Inst Technol, Dept Phys, Wolfgang Pauli Str 16, CH-8093 Zurich, Switzerland. [Bacon, D.; Capozzi, D.; Carlsen, J.; Collett, T.; D'Andrea, C. B.; Etherington, J.; Guarnieri, P.; Maraston, C.; Morice-Atkinson, X.; Nichol, R. C.; Papadopoulos, A.; Percival, W. J.; Thomas, D.; Wilcox, H.] Univ Portsmouth, Inst Cosmol & Gravitat, Portsmouth PO1 3FX, Hants, England. [Balbinot, E.] Univ Surrey, Dept Phys, Guildford GU2 7XH, Surrey, England. [Banerji, M.; Giannantonio, T.; McMahon, R. G.; Ostrovski, F.; Reed, S. L.] Univ Cambridge, Kavli Inst Cosmol, Madingley Rd, Cambridge CB3 0HA, England. [Banerji, M.; Giannantonio, T.; McMahon, R. G.; Ostrovski, F.; Reed, S. L.] Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England. [Bechtol, K.] Wisconsin IceCube Particle Astrophys Ctr WIPAC, Madison, WI 53703 USA. [Bechtol, K.] Univ Wisconsin, Dept Phys, 1150 Univ Ave, Madison, WI 53706 USA. [Benoit-Levy, A.; Bertin, E.] Univ Paris 06, Sorbonne Univ, UMR 7095, Inst Astrophys Paris, F-75014 Paris, France. [Benoit-Levy, A.; Bertin, E.] CNRS, Inst Astrophys Paris, UMR 7095, F-75014 Paris, France. [Bernstein, G. M.; Jain, B.; Sako, M.; Suchyta, E.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. [Blazek, J.; Honscheid, K.; Martini, P.; Ross, A.] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA. [Bonnett, C.] Univ Autonoma Barcelona, Inst Fis Altes Energies, E-08193 Barcelona, Spain. [Bridle, S.; Zuntz, J.] Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, Oxford Rd, Manchester M13 9PL, Lancs, England. [Brunner, R. J.; Foley, R. J.; Thaler, J.; Vieira, J. D.] Univ Illinois, Dept Phys, 1110 W Green St, Urbana, IL 61801 USA. [Brunner, R. J.; Carrasco-Kind, M.; Gruendl, R. A.; Vieira, J. D.] Natl Ctr Supercomp Applicat, 1205 West Clark St, Figure, IL 61801 USA. [Burke, D. L.; Cunha, C. E.; Gruen, D.; Roodman, A.; Rykoff, E. S.; Wechsler, R. H.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, POB 2450, Stanford, CA 94305 USA. [Burke, D. L.; Gruen, D.; Roodman, A.; Rykoff, E. S.; Wechsler, R. H.] SLAC Natl Accelerator Lab, Menlo Pk, CA 94025 USA. [Caminha, G. B.; Makler, M.] Ctr Brasileiro Pesquisas Fis, ICRA, Rua Dr Xavier Sigaud 150, BR-22290180 Rio De Janeiro, RJ, Brazil. [Caminha, G. B.] Univ Ferrara, Dipartimento Fis & Sci Terra, Via Saragat 1, I-44122 Ferrara, Italy. [Carnero-Rosell, A.; da Costa, L. N.; Maia, M. A. G.; Ogando, R.] Observ Nacl, Rua Gal Jose Cristino 77, BR-20921400 Rio De Janeiro, RJ, Brazil. [Carnero-Rosell, A.; da Costa, L. N.; Lima, M.; Maia, M. A. G.; Ogando, R.; Santiago, B.; Sobreira, F.] Lab Interinst & Astron LIneA, Rua Gal Jose Cristino 77, BR-20921400 Rio De Janeiro, RJ, Brazil. [Carollo, M.] Swiss Fed Inst Technol, Inst Astron, CH-8093 Zurich, Switzerland. [Carrasco-Kind, M.; Foley, R. J.; Gruendl, R. A.; Sevilla-Noarbe, I.; Vieira, J. D.] Univ Illinois, Dept Astron, 1002 W Green St, Urbana, IL 61801 USA. [Carretero, J.; Castander, F. J.; Crocce, M.; Fosalba, P.; Gaztanaga, E.] CSIC, IEEC, Inst Ciencies Espai, Campus UAB,Carrer Can Magrans S-N, E-08193 Barcelona, Spain. [Conselice, C.] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England. [Davis, T. M.; King, A.] Univ Queensland, Sch Math & Phys, Brisbane, Qld 4072, Australia. [Desai, S.; Dietrich, J. P.; Mohr, J. J.; Weller, J.] Excellence Cluster Universe, Boltzmannstr 2, D-85748 Garching, Germany. [Desai, S.; Dietrich, J. P.; Mohr, J. J.] Univ Munich, Fac Phys, Scheinerstr 1, D-81679 Munich, Germany. [Dodelson, S.; Kessler, R.; Kron, R.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Dodelson, S.; Frieman, J.; Kessler, R.] Univ Chicago, Dept Astron & Astrophys, 5640 S Ellis Ave, Chicago, IL 60637 USA. [Evrard, A. E.; Gerdes, D. W.; Miller, C. J.; Schubnell, M.; Tarle, G.; Zhang, Y.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA. [Evrard, A. E.; Miller, C. J.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Garcia-Bellido, J.] Univ Autonoma Madrid, CSIC, IFT, E-28049 Madrid, Spain. [Goldstein, D. A.; Miquel, R.] Univ Calif Berkeley, Dept Astron, 501 Campbell Hall, Berkeley, CA 94720 USA. [Goldstein, D. A.] Inst Catalana Recerca & Estudis Avancats, E-08010 Barcelona, Spain. [Honscheid, K.] Ohio State Univ, Dept Phys, 174 W 18th Ave, Columbus, OH 43210 USA. [Jeltema, T.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA. [Jeltema, T.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA. [Kuehn, K.] Australian Astron Observ, N Ryde, NSW 2113, Australia. [Li, T. S.; Marshall, J. L.] Texas A&M Univ, George P & Cynthia Woods Mitchell Inst Fundamenta, College Stn, TX 77843 USA. [Li, T. S.; Marshall, J. L.] Texas A&M Univ, Dept Phys & Astron, College Stn, TX 77843 USA. [Lima, M.] Univ Sao Paulo, Inst Fis, Dipartimento Fis Matemat, CP 66318, BR-05314970 Sao Paulo, Brazil. [Martini, P.] Ohio State Univ, Dept Astron, 174 W 18Th Ave, Columbus, OH 43210 USA. [Melchior, P.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Mohr, J. J.; Weller, J.] Max Planck Inst Extraterr Phys, Giessenbachstr, D-85748 Garching, Germany. [Papadopoulos, A.] European Univ Cyprus, Sch Sci, 6 Diogenis Str, CY-1516 Nicosia, Cyprus. [Plazas, A. A.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Romer, A. K.] Univ Sussex, Dept Phys & Astron, Pevensey Bldg, Brighton BN1 9QH, E Sussex, England. [Rozo, E.] Univ Arizona, Dept Phys, 1118 E 4th St, Tucson, AZ 85721 USA. [Sanchez, E.; Sevilla-Noarbe, I.] Ctr Invest Energet Medioambientales & Tecnol CIEM, Madrid, Spain. [Santiago, B.] Univ Fed Rio Grande do Sul, Inst Fis, Caixa Postal 15051, BR-91501970 Porto Alegre, RS, Brazil. [Sheldon, E.] Brookhaven Natl Lab, Bldg 510, Upton, NY 11973 USA. [Smith, M.; Sullivan, M.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Swanson, M.] Natl Ctr Supercomp Applicat, 1205 West Clark St, Urbana, IL 61801 USA. [Thomas, D.] South East Phys Network Www Sepnet Ac Uk, London, England. [Thomas, R. C.] Lawrence Berkeley Natl Lab, 1 Cyclotron Rd, Berkeley, CA 94720 USA. [Vikram, V.] Argonne Natl Lab, 9700 S Cass Ave, Lemont, IL 60439 USA. [Weller, J.] Univ Munich, Univ Sternwarte, Fak Phys, Scheinerstr 1, D-81679 Munich, Germany. RP Abbott, T (reprint author), Cerro Tololo Interamer Observ, Natl Opt Astron Observ, La Serena, Chile.; Lahav, O (reprint author), UCL, Dept Phys & Astron, Gower St, London WC1E 6BT, England. EM o.lahav@ucl.ac.uk RI Sobreira, Flavia/F-4168-2015; Lima, Marcos/E-8378-2010; Natarajan, Meena/J-9167-2012; Bartosch Caminha, Gabriel/C-8952-2013; Ogando, Ricardo/A-1747-2010; Davis, Tamara/A-4280-2008; Gaztanaga, Enrique/L-4894-2014; OI Sullivan, Mark/0000-0001-9053-4820; Garcia-Bellido, Juan/0000-0002-9370-8360; Sobreira, Flavia/0000-0002-7822-0658; Natarajan, Meena/0000-0001-5652-9681; Bartosch Caminha, Gabriel/0000-0001-6052-3274; Ogando, Ricardo/0000-0003-2120-1154; Davis, Tamara/0000-0002-4213-8783; Gaztanaga, Enrique/0000-0001-9632-0815; Tucker, Douglas/0000-0001-7211-5729; Weller, Jochen/0000-0002-8282-2010; Abdalla, Filipe/0000-0003-2063-4345 FU US Department of Energy; US National Science Foundation; Ministry of Science and Education of Spain; Science and Technology Facilities Council of the United Kingdom; Higher Education Funding Council for England; National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign; Kavli Institute of Cosmological Physics at the University of Chicago; Center for Cosmology and Astro-Particle Physics at the Ohio State University; Mitchell Institute for Fundamental Physics and Astronomy at Texas AM University; Financiadora de Estudos e Projetos; Fundacao Carlos Chagas Filho de Amparo a Pesquisa do Estado do Rio de Janeiro; Conselho Nacional de Desenvolvimento Cientifico e Tecnologico and the Ministerio da Ciencia; Tecnologia e Inovacao; Deutsche Forschungsgemeinschaft; Collaborating Institutions in the Dark Energy Survey; National Science Foundation [AST-1138766]; University of California at Santa Cruz; University of Cambridge, Centro de Investigaciones Energeticas, Medioambientales y Tecnologicas-Madrid; University of Chicago, University College London; DES-Brazil Consortium; University of Edinburgh; Eidgenossische Technische Hochschule (ETH) Zurich, Fermi National Accelerator Laboratory; University of Illinois at Urbana-Champaign; Institut de Ciencies de l'Espai (IEEC/CSIC); Institut de Fisica d'Altes Energies, Lawrence Berkeley National Laboratory; Ludwig-Maximilians Universitat Munchen; European Research Council [FP7/291329]; MINECO [AYA2012-39559, ESP2013-48274, FPA2013-47986]; Centro de Excelencia Severo Ochoa [SEV-2012-0234]; European Research Council under the European Union [240672, 291329, 306478] FX Funding for the DES Projects has been provided by the US Department of Energy, the US National Science Foundation, the Ministry of Science and Education of Spain, the Science and Technology Facilities Council of the United Kingdom, the Higher Education Funding Council for England, the National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign, the Kavli Institute of Cosmological Physics at the University of Chicago, the Center for Cosmology and Astro-Particle Physics at the Ohio State University, the Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M University, Financiadora de Estudos e Projetos, Fundacao Carlos Chagas Filho de Amparo a Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Cientifico e Tecnologico and the Ministerio da Ciencia, Tecnologia e Inovacao, the Deutsche Forschungsgemeinschaft and the Collaborating Institutions in the Dark Energy Survey. The DES Data Management system is supported by the National Science Foundation under Grant Number AST-1138766.r The Collaborating Institutions are Argonne National Laboratory, the University of California at Santa Cruz, the University of Cambridge, Centro de Investigaciones Energeticas, Medioambientales y Tecnologicas-Madrid, the University of Chicago, University College London, the DES-Brazil Consortium, the University of Edinburgh, the Eidgenossische Technische Hochschule (ETH) Zurich, Fermi National Accelerator Laboratory, the University of Illinois at Urbana-Champaign, the Institut de Ciencies de l'Espai (IEEC/CSIC), the Institut de Fisica d'Altes Energies, Lawrence Berkeley National Laboratory, the Ludwig-Maximilians Universitat Munchen and the associated Excellence Cluster Universe, the University of Michigan, the National Optical Astronomy Observatory, the University of Nottingham, the Ohio State University, the University of Pennsylvania, the University of Portsmouth, SLAC National Accelerator Laboratory, Stanford University, the University of Sussex and Texas A&M University.r OL acknowledges support from a European Research Council Advanced Grant FP7/291329. The DES participants from Spanish institutions are partially supported by MINECO under grants AYA2012-39559, ESP2013-48274, FPA2013-47986 and Centro de Excelencia Severo Ochoa SEV-2012-0234. Research leading to these results has received funding from the European Research Council under the European Union's Seventh Framework Programme (FP7/2007-2013) including ERC grant agreements 240672, 291329 and 306478.r We are grateful for the extraordinary contributions of our CTIO colleagues and the DECam Construction, Commissioning and Science Verification teams in achieving the excellent instrument and telescope conditions that have made this work possible. The success of this project also relies critically on the expertise and dedication of the DES Data Management group.r The VISTA Hemisphere Survey (VHS) is based on observations obtained as part of ESO Programme 179.A-2010 (PI: McMahon).r This paper has gone through internal review by the DES Collaboration. NR 358 TC 19 Z9 19 U1 9 U2 18 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD AUG 1 PY 2016 VL 460 IS 2 BP 1270 EP 1299 DI 10.1093/mnras/stw641 PG 30 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DR3WH UT WOS:000379832800009 ER PT J AU Merson, AI Jasche, J Abdalla, FB Lahav, O Wandelt, B Jones, DH Colless, M AF Merson, Alexander I. Jasche, Jens Abdalla, Filipe B. Lahav, Ofer Wandelt, Benjamin Jones, D. Heath Colless, Matthew TI Halo detection via large-scale Bayesian inference SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE methods: numerical; methods: statistical; galaxies: haloes; galaxies: clusters: general; dark matter; large-scale structure of Universe ID DIGITAL SKY SURVEY; 6DF GALAXY SURVEY; POWER-SPECTRUM INFERENCE; MASS ASSEMBLY GAMA; X-RAY-CLUSTERS; DATA RELEASE; DARK-MATTER; WIENER RECONSTRUCTION; LUMINOSITY FUNCTIONS; SPECTROSCOPY SYSTEM AB We present a proof-of-concept of a novel and fully Bayesian methodology designed to detect haloes of different masses in cosmological observations subject to noise and systematic uncertainties. Our methodology combines the previously published Bayesian large-scale structure inference algorithm, HAmiltonian Density Estimation and Sampling algorithm (hades), and a Bayesian chain rule (the Blackwell-Rao estimator), which we use to connect the inferred density field to the properties of dark matter haloes. To demonstrate the capability of our approach, we construct a realistic galaxy mock catalogue emulating the wide-area 6-degree Field Galaxy Survey, which has a median redshift of approximately 0.05. Application of hades to the catalogue provides us with accurately inferred three-dimensional density fields and corresponding quantification of uncertainties inherent to any cosmological observation. We then use a cosmological simulation to relate the amplitude of the density field to the probability of detecting a halo with mass above a specified threshold. With this information, we can sum over the hades density field realisations to construct maps of detection probabilities and demonstrate the validity of this approach within our mock scenario. We find that the probability of successful detection of haloes in the mock catalogue increases as a function of the signal to noise of the local galaxy observations. Our proposed methodology can easily be extended to account for more complex scientific questions and is a promising novel tool to analyse the cosmic large-scale structure in observations. C1 [Merson, Alexander I.; Abdalla, Filipe B.; Lahav, Ofer] UCL, Dept Phys & Astron, Gower St, London WC1E 6BT, England. [Merson, Alexander I.] Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Jasche, Jens] Tech Univ Munich, Excellence Cluster Universe, Boltzmannstr 2, D-85748 Garching, Germany. [Abdalla, Filipe B.] Rhodes Univ, Dept Phys & Elect, POB 94, ZA-6140 Grahamstown, South Africa. [Wandelt, Benjamin] Univ Paris 06, CNRS, UMR 7095, IAP, 98Bis Blvd Arago, F-75014 Paris, France. [Wandelt, Benjamin] Sorbonne Univ, ILP, 98Bis Blvd Arago, F-75014 Paris, France. [Wandelt, Benjamin] Univ Illinois, Dept Phys, Urbana, IL 61801 USA. [Wandelt, Benjamin] Univ Illinois, Dept Astron, Urbana, IL 61801 USA. [Jones, D. Heath] Macquarie Univ, Dept Phys & Astron, N Ryde, NSW 2109, Australia. [Colless, Matthew] Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT 2611, Australia. RP Merson, AI (reprint author), UCL, Dept Phys & Astron, Gower St, London WC1E 6BT, England.; Merson, AI (reprint author), Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM alex.i.merson@jpl.nasa.gov OI Abdalla, Filipe/0000-0003-2063-4345; Colless, Matthew/0000-0001-9552-8075 FU Royal Society; European Research Council [FP7/291329]; NSF [AST 07-08849, AST 09-08693 ARRA]; Chaire d'Excellence from the Agence Nationale de Recherche; DFG cluster of excellence 'Origin and Structure of the Universe' FX We thank the anonymous referee for many thorough and constructive comments. In addition, we also thank Sreekumar Thaithara Balan, Boris Leistedt, Michelle Lochner and Hiranya Peiris for several productive and insightful discussions and suggestions. FBA acknowledges the support of the Royal Society for a University Research Fellowship. OL acknowledges support from a European Research Council Advanced Grant FP7/291329. BDW acknowledges support from NSF grants AST 07-08849 and AST 09-08693 ARRA, and a Chaire d'Excellence from the Agence Nationale de Recherche. This research was supported by the DFG cluster of excellence 'Origin and Structure of the Universe' (www.universe-cluster.de). NR 87 TC 0 Z9 0 U1 3 U2 3 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD AUG 1 PY 2016 VL 460 IS 2 BP 1340 EP 1355 DI 10.1093/mnras/stw948 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DR3WH UT WOS:000379832800014 ER PT J AU Ruchayskiy, O Boyarsky, A Iakubovskyi, D Bulbul, E Eckert, D Franse, J Malyshev, D Markevitch, M Neronov, A AF Ruchayskiy, Oleg Boyarsky, Alexey Iakubovskyi, Dmytro Bulbul, Esra Eckert, Dominique Franse, Jeroen Malyshev, Denys Markevitch, Maxim Neronov, Andrii TI Searching for decaying dark matter in deep XMM-Newton observation of the Draco dwarf spheroidal SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE line: identification; galaxies: dwarf; dark matter; X-rays: general ID PHOTON IMAGING CAMERA; 3.5 KEV LINE; GALAXY CLUSTERS; EMISSION-LINE; MILKY-WAY; ORIGIN; HALO; CONSTRAINTS; SPECTRA; SUZAKU AB We present results of a search for the 3.5 keV emission line in our recent very long (similar to 1.4 Ms) XMM-Newton observation of the Draco dwarf spheroidal galaxy. The astrophysical X-ray emission from such dark matter-dominated galaxies is faint, thus they provide a test for the dark matter origin of the 3.5 keV line previously detected in other massive, but X-ray bright objects, such as galaxies and galaxy clusters. We do not detect a statistically significant emission line from Draco; this constrains the lifetime of a decaying dark matter particle to tau > (7-9) x 10(27) s at 95 per cent CL (combining all three XMM-Newton cameras; the interval corresponds to the uncertainty of the dark matter column density in the direction of Draco). The PN camera, which has the highest sensitivity of the three, does show a positive spectral residual (above the carefully modelled continuum) at E = 3.54 +/- A 0.06 keV with a 2.3 sigma significance. The two MOS cameras show less-significant or no positive deviations, consistently within 1 sigma with PN. Our Draco limit on tau is consistent with previous detections in the stacked galaxy clusters, M31 and the Galactic Centre within their 1 - 2 sigma uncertainties, but is inconsistent with the high signal from the core of the Perseus cluster (which has itself been inconsistent with the rest of the detections). We conclude that this Draco observation does not exclude the dark matter interpretation of the 3.5 keV line in those objects. C1 [Ruchayskiy, Oleg] Ecole Polytech Fed Lausanne, FSB ITP LPPC, BSP 720, CH-1015 Lausanne, Switzerland. [Ruchayskiy, Oleg; Iakubovskyi, Dmytro] Niels Bohr Inst & Discovery Ctr, Blegdamsvej 17, DK-2100 Copenhagen, Denmark. [Boyarsky, Alexey; Franse, Jeroen] Leiden Univ, Inst Lorentz Theoret Phys, Niels Bohrweg 2, Leiden, Netherlands. [Iakubovskyi, Dmytro] Bogolyubov Inst Theoret Phys, Metrologichna Str 14-b, UA-03680 Kiev, Ukraine. [Bulbul, Esra] MIT, Kavli Inst Astrophys & Space Res, 77 Massachusetts Ave, Cambridge, MA 02139 USA. [Eckert, Dominique; Malyshev, Denys; Neronov, Andrii] Univ Geneva, Dept Astron, Ch Ecogia 16, CH-1290 Versoix, Switzerland. [Franse, Jeroen] Leiden Univ, Leiden Observ, Niels Bohrweg 2, Leiden, Netherlands. [Markevitch, Maxim] NASA, Goddard Space Flight Ctr, Code 662,8800 Greenbelt Rd, Greenbelt, MD 20771 USA. RP Ruchayskiy, O (reprint author), Ecole Polytech Fed Lausanne, FSB ITP LPPC, BSP 720, CH-1015 Lausanne, Switzerland.; Ruchayskiy, O (reprint author), Niels Bohr Inst & Discovery Ctr, Blegdamsvej 17, DK-2100 Copenhagen, Denmark. EM oleg.ruchayskiy@epfl.ch RI Iakubovskyi, Dmytro/D-6418-2012; OI Iakubovskyi, Dmytro/0000-0002-6969-0738; Eckert, Dominique/0000-0001-7917-3892 FU NASA [NNX123AE77G]; Swiss National Science Foundation grant SCOPE [IZ7370-152581]; State Fund for Fundamental Research of Ukraine [F64/42-2015]; Program of Cosmic Research of the National Academy of Sciences of Ukraine; State Programme of Implementation of Grid Technology in Ukraine; ESA Member States; NASA FX We would like to thank K. Abazajian, G. Bertone, A. Geringer-Sameth, M. Lovell, M. Walker, C. Weniger for collaboration, discussion and useful comments. EB acknowledges support by NASA through grant no. NNX123AE77G. The work of DI has been partially supported from the Swiss National Science Foundation grant SCOPE IZ7370-152581, the grant no. F64/42-2015 of the State Fund for Fundamental Research of Ukraine, the Program of Cosmic Research of the National Academy of Sciences of Ukraine, and the State Programme of Implementation of Grid Technology in Ukraine. The Draco dSph observations were performed as a part of AO-14 Very Large Programme obtained with XMM Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA. NR 49 TC 7 Z9 7 U1 0 U2 1 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD AUG 1 PY 2016 VL 460 IS 2 BP 1390 EP 1398 DI 10.1093/mnras/stw1026 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DR3WH UT WOS:000379832800018 ER PT J AU Guainazzi, M Risaliti, G Awaki, H Arevalo, P Bauer, FE Bianchi, S Boggs, SE Brandt, WN Brightman, M Christensen, FE Craig, WW Forster, K Hailey, CJ Harrison, F Koss, M Longinotti, A Markwardt, C Marinucci, A Matt, G Reynolds, CS Ricci, C Stern, D Svoboda, J Walton, D Zhang, W AF Guainazzi, M. Risaliti, G. Awaki, H. Arevalo, P. Bauer, F. E. Bianchi, S. Boggs, S. E. Brandt, W. N. Brightman, M. Christensen, F. E. Craig, W. W. Forster, K. Hailey, C. J. Harrison, F. Koss, M. Longinotti, A. Markwardt, C. Marinucci, A. Matt, G. Reynolds, C. S. Ricci, C. Stern, D. Svoboda, J. Walton, D. Zhang, W. TI The nature of the torus in the heavily obscured AGN Markarian 3: an X-ray study SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: active; galaxies: Seyfert; X-rays: galaxies; X-rays: individual: Markarian 3 ID ACTIVE GALACTIC NUCLEI; SEYFERT 2 GALAXY; XMM-NEWTON; NGC 1068; REVERBERATION MEASUREMENTS; ENERGY-DISTRIBUTIONS; CIRCINUS GALAXY; WARM ABSORBERS; INNER RADIUS; LINE REGION AB In this paper, we report the results of an X-ray monitoring campaign on the heavily obscured Seyfert galaxy, Markarian 3, carried out between the fall of 2014 and the spring of 2015 with NuSTAR, Suzaku and XMM-Newton. The hard X-ray spectrum of Markarian 3 is variable on all the time-scales probed by our campaign, down to a few days. The observed continuum variability is due to an intrinsically variable primary continuum seen in transmission through a large, but still Compton-thin column density (N-H similar to 0.8-1.1 x 10(24) cm(-2)). If arranged in a spherical-toroidal geometry, the Compton scattering matter has an opening angle a parts per thousand integral 66A degrees, and is seen at a grazing angle through its upper rim (inclination angle a parts per thousand integral 70A degrees). We report a possible occultation event during the 2014 campaign. If the torus is constituted by a system of clouds sharing the same column density, this event allows us to constrain their number (17 +/- 5) and individual column density, [a parts per thousand integral (4.9 +/- 1.5) x 10(22) cm(-2)]. The comparison of IR and X-ray spectroscopic results with state-of-the art 'torus' models suggests that at least two-thirds of the X-ray obscuring gas volume might be located within the dust sublimation radius. We report also the discovery of an ionized absorber, characterized by variable resonant absorption lines due to He- and H-like iron. This discovery lends support to the idea that moderate column density absorbers could be due to clouds evaporated at the outer surface of the torus, possibly accelerated by the radiation pressure due to the central AGN emission leaking through the patchy absorber. C1 [Guainazzi, M.] Inst Space & Astronat Sci JAXA, 3-1-1 Yoshinodai, Sagamihara, Kanagawa 2525252, Japan. [Guainazzi, M.] ESA, European Space Astron Ctr, POB 78, E-28691 Madrid, Spain. [Risaliti, G.] Osservatorio Arcetri, INAF, Largo E Fermi 5, I-50125 Florence, Italy. [Risaliti, G.] Univ Florence, Dipartimento Fis & Astron, Via G Sansone 1, I-50019 Florence, Italy. [Awaki, H.] Ehime Univ, Dept Phys, Matsuyama, Ehime 7908577, Japan. [Arevalo, P.] Univ Valparaiso, Fac Ciencias, Inst Fis & Astron, Gran Bretana N 1111, Valparaiso, Chile. [Bauer, F. E.; Ricci, C.] Pontificia Univ Catolica Chile, Fac Fis, Inst Astrofis, Casilla 306, Santiago 22, Chile. [Bauer, F. E.] Millennium Inst Astrophys MAS, Nuncio Monsenor Sotero Sanz 100, Santiago, Chile. [Bauer, F. E.] Space Sci Inst, 4750 Walnut St,Suite 205, Boulder, CO 80301 USA. [Bianchi, S.; Marinucci, A.; Matt, G.] Univ Roma Tre, Dipartimento Matemat & Fis, Via Vasca Navale 84, I-00146 Rome, Italy. [Boggs, S. E.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Brandt, W. N.] Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA. [Brandt, W. N.] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA. [Brandt, W. N.] Penn State Univ, Dept Phys, Davey Lab 104, University Pk, PA 16802 USA. [Brightman, M.; Forster, K.; Harrison, F.; Walton, D.] CALTECH, Cahill Ctr Astrophys, 1216 East Calif Blvd, Pasadena, CA 91125 USA. [Christensen, F. E.] Tech Univ Denmark, DTU Space Natl Space Inst, Elektrovej 327, DK-2800 Lyngby, Denmark. [Craig, W. W.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA. [Hailey, C. J.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Koss, M.] ETH, Dept Phys, Inst Astron, Wolfgang Pauli Str 27, CH-8093 Zurich, Switzerland. [Longinotti, A.] Inst Nacl Astrofis Opt & Electr, Catedrat CONACYT, Luis E Erro 1, Puebla 72840, Mexico. [Markwardt, C.; Zhang, W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Reynolds, C. S.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Stern, D.; Walton, D.] NASA, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Svoboda, J.] Acad Sci Czech Republic, Astron Inst, Bocni 2 1401, CZ-14100 Prague, Czech Republic. RP Guainazzi, M (reprint author), Inst Space & Astronat Sci JAXA, 3-1-1 Yoshinodai, Sagamihara, Kanagawa 2525252, Japan.; Guainazzi, M (reprint author), ESA, European Space Astron Ctr, POB 78, E-28691 Madrid, Spain. EM Matteo.Guainazzi@sciops.esa.int RI Bianchi, Stefano/B-4804-2010; Svoboda, Jiri/G-9045-2014 OI Bianchi, Stefano/0000-0002-4622-4240; NR 87 TC 0 Z9 0 U1 2 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 AUG 1 PY 2016 VL 460 IS 2 BP 1954 EP 1969 DI 10.1093/mnras/stw1033 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DR3WH UT WOS:000379832800064 ER PT J AU Jarvis, M Sheldon, E Zuntz, J Kacprzak, T Bridle, SL Amara, A Armstrong, R Becker, MR Bernstein, GM Bonnett, C Chang, C Das, R Dietrich, JP Drlica-Wagner, A Eifler, TF Gangkofner, C Gruen, D Hirsch, M Huff, EM Jain, B Kent, S Kirk, D MacCrann, N Melchior, P Plazas, AA Refregier, A Rowe, B Rykoff, ES Samuroff, S Sanchez, C Suchyta, E Troxel, MA Vikram, V Abbott, T Abdalla, FB Allam, S Annis, J Benoit-Levy, A Bertin, E Brooks, D Buckley-Geer, E Burke, DL Capozzi, D Rosell, AC Kind, MC Carretero, J Castander, FJ Clampitt, J Crocce, M Cunha, CE D'Andrea, CB da Costa, LN DePoy, DL Desai, S Diehl, HT Doel, P Neto, AF Flaugher, B Fosalba, P Frieman, J Gaztanaga, E Gerdes, DW Gruendl, RA Gutierrez, G Honscheid, K James, DJ Kuehn, K Kuropatkin, N Lahav, O Li, TS Lima, M March, M Martini, P Miquel, R Mohr, JJ Neilsen, E Nord, B Ogando, R Reil, K Romer, AK Roodman, A Sako, M Sanchez, E Scarpine, V Schubnell, M Sevilla-Noarbe, I Smith, RC Soares-Santos, M Sobreira, F Swanson, MEC Tarle, G Thaler, J Thomas, D Walker, AR Wechsler, RH AF Jarvis, M. Sheldon, E. Zuntz, J. Kacprzak, T. Bridle, S. L. Amara, A. Armstrong, R. Becker, M. R. Bernstein, G. M. Bonnett, C. Chang, C. Das, R. Dietrich, J. P. Drlica-Wagner, A. Eifler, T. F. Gangkofner, C. Gruen, D. Hirsch, M. Huff, E. M. Jain, B. Kent, S. Kirk, D. MacCrann, N. Melchior, P. Plazas, A. A. Refregier, A. Rowe, B. Rykoff, E. S. Samuroff, S. Sanchez, C. Suchyta, E. Troxel, M. A. Vikram, V. Abbott, T. Abdalla, F. B. Allam, S. Annis, J. Benoit-Levy, A. Bertin, E. Brooks, D. Buckley-Geer, E. Burke, D. L. Capozzi, D. Rosell, A. Carnero Kind, M. Carrasco Carretero, J. Castander, F. J. Clampitt, J. Crocce, M. Cunha, C. E. D'Andrea, C. B. da Costa, L. N. DePoy, D. L. Desai, S. Diehl, H. T. Doel, P. Neto, A. Fausti Flaugher, B. Fosalba, P. Frieman, J. Gaztanaga, E. Gerdes, D. W. Gruendl, R. A. Gutierrez, G. Honscheid, K. James, D. J. Kuehn, K. Kuropatkin, N. Lahav, O. Li, T. S. Lima, M. March, M. Martini, P. Miquel, R. Mohr, J. J. Neilsen, E. Nord, B. Ogando, R. Reil, K. Romer, A. K. Roodman, A. Sako, M. Sanchez, E. Scarpine, V. Schubnell, M. Sevilla-Noarbe, I. Smith, R. C. Soares-Santos, M. Sobreira, F. Swanson, M. E. C. Tarle, G. Thaler, J. Thomas, D. Walker, A. R. Wechsler, R. H. TI The DES Science Verification weak lensing shear catalogues SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE gravitational lensing: weak; methods: data analysis; techniques: image processing; catalogues; surveys; cosmology: observations ID IMAGE-ANALYSIS COMPETITION; GALAXY SHAPE MEASUREMENT; DARK ENERGY CAMERA; DIGITAL SKY SURVEY; COSMIC SHEAR; NOISE BIAS; CHALLENGE HANDBOOK; MAXIMUM-LIKELIHOOD; GREAT08 CHALLENGE; SYSTEMATIC-ERRORS AB We present weak lensing shear catalogues for 139 square degrees of data taken during the Science Verification (SV) time for the new Dark Energy Camera (DECam) being used for the Dark Energy Survey (DES). We describe our object selection, point spread function estimation and shear measurement procedures using two independent shear pipelines, im3shape and ngmix, which produce catalogues of 2.12 million and 3.44 million galaxies, respectively. We detail a set of null tests for the shear measurements and find that they pass the requirements for systematic errors at the level necessary for weak lensing science applications using the SV data. We also discuss some of the planned algorithmic improvements that will be necessary to produce sufficiently accurate shear catalogues for the full 5-yr DES, which is expected to cover 5000 square degrees. C1 [Jarvis, M.; Bernstein, G. M.; Eifler, T. F.; Jain, B.; Clampitt, J.; March, M.; Sako, M.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. [Sheldon, E.] Brookhaven Natl Lab, Bldg 510, Upton, NY 11973 USA. [Zuntz, J.; Bridle, S. L.; MacCrann, N.; Samuroff, S.; Troxel, M. A.] Univ Manchester, Jodrell Bank, Ctr Astrophys, Sch Phys & Astron, Manchester M13 9PL, Lancs, England. [Kacprzak, T.; Amara, A.; Chang, C.; Refregier, A.] ETH, Dept Phys, Wolfgang Pauli Str 16, CH-8093 Zurich, Switzerland. [Armstrong, R.] Princeton Univ, Dept Astrophys Sci, Peyton Hall, Princeton, NJ 08544 USA. [Becker, M. R.; Wechsler, R. H.] Stanford Univ, Dept Phys, 382 Via Pueblo Mall, Stanford, CA 94305 USA. [Becker, M. R.; Rykoff, E. S.; Burke, D. L.; Cunha, C. E.; Roodman, A.; Wechsler, R. H.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, POB 2450, Stanford, CA 94305 USA. [Bonnett, C.; Sanchez, C.; Carretero, J.; Miquel, R.] Univ Autonoma Barcelona, Inst Fis Altes Energies, E-08193 Barcelona, Spain. Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA. [Dietrich, J. P.; Gangkofner, C.; Desai, S.; Mohr, J. J.] Excellence Cluster Universe, Boltzmannstr 2, D-85748 Garching, Germany. [Dietrich, J. P.; Gangkofner, C.; Desai, S.; Mohr, J. J.] Univ Munich, Fac Phys, Scheinerstr 1, D-81679 Munich, Germany. [Amara, A.; Drlica-Wagner, A.; Kent, S.; Allam, S.; Annis, J.; Buckley-Geer, E.; Diehl, H. T.; Flaugher, B.; Frieman, J.; Gutierrez, G.; Kuropatkin, N.; Neilsen, E.; Nord, B.; Scarpine, V.; Soares-Santos, M.; Sobreira, F.] Fermilab Natl Accelerator Lab, POB 500, Batavia, IL 60510 USA. [Eifler, T. F.; Plazas, A. A.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Gruen, D.; Mohr, J. J.] Max Planck Inst Extraterr Phys, Giessenbachstr, D-85748 Garching, Germany. [Gruen, D.] Univ Munich, Univ Sternwarte, Fak Phys, Scheinerstr 1, D-81679 Munich, Germany. [Hirsch, M.; Kirk, D.; Rowe, B.; Abdalla, F. B.; Benoit-Levy, A.; Brooks, D.; Doel, P.; Lahav, O.] UCL, Dept Phys & Astron, Gower St, London WC1E 6BT, England. [Huff, E. M.; Melchior, P.; Suchyta, E.; Honscheid, K.; Martini, P.] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA. [Huff, E. M.; Melchior, P.; Suchyta, E.; Honscheid, K.] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA. [Rykoff, E. S.; Burke, D. L.; Reil, K.; Roodman, A.; Wechsler, R. H.] SLAC Natl Accelerator Lab, Menlo Pk, CA 94025 USA. [Vikram, V.] Argonne Natl Lab, 9700 South Cass Ave, Lemont, IL 60439 USA. [Abbott, T.; James, D. J.; Smith, R. C.; Walker, A. R.] Natl Opt Astron Observ, Cerro Tololo Interamer Observ, Casilla 603, La Serena, Chile. [Abdalla, F. B.] Rhodes Univ, Dept Phys & Elect, POB 94, ZA-6140 Grahamstown, South Africa. [Bertin, E.] CNRS, Inst Astrophys Paris, UMR 7095, F-75014 Paris, France. [Bertin, E.] Univ Paris 06, Sorbonne Univ, UMR 7095, Inst Astrophys, F-75014 Paris, France. [Capozzi, D.; D'Andrea, C. B.; Thomas, D.] Univ Portsmouth, Inst Cosmol & Gravitat, Portsmouth PO1 3FX, Hants, England. [Rosell, A. Carnero; da Costa, L. N.; Neto, A. Fausti; Lima, M.; Ogando, R.; Sobreira, F.] Lab Interinst E Astron LIneA, Rua Gal Jose Cristino 77, BR-20921400 Rio De Janeiro, RJ, Brazil. [Rosell, A. Carnero; da Costa, L. N.; Ogando, R.] Observ Nacl, Jose Cristino 77, BR-20921400 Rio De Janeiro, RJ, Brazil. [Kind, M. Carrasco; Gruendl, R. A.; Sevilla-Noarbe, I.] Univ Illinois, Dept Astron, 1002 W Green St, Urbana, IL 61801 USA. [Kind, M. Carrasco; Gruendl, R. A.; Swanson, M. E. C.] Natl Ctr Supercomp Applicat, 1205 West Clark St, Urbana, IL 61801 USA. [Carretero, J.; Castander, F. J.; Crocce, M.; Fosalba, P.; Gaztanaga, E.] IEEC CSIC, Inst Ciencies Espai, Campus UAB,Carrer Can Magrans,S-N, E-08193 Barcelona, Spain. [DePoy, D. L.; Li, T. S.] Texas A&M Univ, George P & Cynthia Woods Mitchell Inst Fundamenal, College Stn, TX 77843 USA. [DePoy, D. L.; Li, T. S.] Texas A&M Univ, Dept Phys & Astron, College Stn, TX 77843 USA. [Frieman, J.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Kuehn, K.] Australian Astron Observ, N Ryde, NSW 2113, Australia. [Lima, M.] Univ Sao Paulo, Dept Fis Matemat, Inst Fis, CP 66318, BR-05314970 Sao Paulo, Brazil. [Martini, P.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Miquel, R.] Inst Catalana Recerca & Estudis Avancats, E-08010 Barcelona, Spain. [Romer, A. K.] Univ Sussex, Dept Phys & Astron, Pevensey Bldg, Brighton BN1 9QH, E Sussex, England. [Sanchez, E.; Sevilla-Noarbe, I.] CIEMAT, E-28040 Madrid, Spain. [Thaler, J.] Univ Illinois, Dept Phys, 1110 W Green St, Urbana, IL 61801 USA. RP Jarvis, M (reprint author), Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. EM michael@jarvis.net RI Sobreira, Flavia/F-4168-2015; Lima, Marcos/E-8378-2010; Ogando, Ricardo/A-1747-2010; Gaztanaga, Enrique/L-4894-2014; OI Sobreira, Flavia/0000-0002-7822-0658; Ogando, Ricardo/0000-0003-2120-1154; Gaztanaga, Enrique/0000-0001-9632-0815; Stern, Corvin/0000-0003-4406-6127; Rowe, Barnaby/0000-0002-7042-9174; Abdalla, Filipe/0000-0003-2063-4345 FU NSF [AST-0812790, AST-1138729]; DoE [DE-SC0007901, DE-AC02-98CH10886, DE-SC0007859, DE-FG02-91ER40690]; European Research Council [240672]; Deutsche Forschungsgemeinschaft (DFG) [SFB-Transregio 33]; DFG cluster of excellence 'Origin and Structure of the Universe'; JPL; FAPESP; CNPq; US Department of Energy; US National Science Foundation; Ministry of Science and Education of Spain; Science and Technology Facilities Council of the United Kingdom; Higher Education Funding Council for England; National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign; Kavli Institute of Cosmological Physics at the University of Chicago; Center for Cosmology and Astro-Particle Physics at the Ohio State University; Mitchell Institute for Fundamental Physics and Astronomy at Texas AM University; Financiadora de Estudos e Projetos; Fundacao Carlos Chagas Filho de Amparo a Pesquisa do Estado do Rio de Janeiro; Conselho Nacional de Desenvolvimento Cientifico e Tecnologico; Ministerio da Ciencia e Tecnologia; Deutsche Forschungsgemeinschaft; Collaborating Institutions in the DES; National Science Foundation [AST-1138766]; MINECO [AYA2012-39559, ESP2013-48274, FPA2013-47986]; Centro de Excelencia Severo Ochoa [SEV-2012-0234]; European Union; Argonne National Laboratory; University of California at Santa Cruz; University of Cambridge; Centro de Investigaciones Energeticas, Medioambientales y Tecnologicas-Madrid; University of Chicago; University College London; DES-Brazil Consortium; Eidgenossische Technische Hochschule (ETH) Zurich; Fermi National Accelerator Laboratory; University of Edinburgh; University of Illinois at Urbana-Champaign; Institut de Ciencies de l'Espai (IEEC/CSIC); Institut de Fisica d'Altes Energies; LBNL; Ludwig-Maximilians Universitat; associated Excellence Cluster Universe, the University of Michigan; National Optical Astronomy Observatory; University of Nottingham; Ohio State University; University of Pennsylvania; University of Portsmouth; SLAC National Accelerator Laboratory; Stanford University; University of Sussex; Texas AM University FX Jarvis has been supported on this project by NSF grants AST-0812790 and AST-1138729. Jarvis, Bernstein, Clampitt, and Jain are partially supported by DoE grant DE-SC0007901. Sheldon is supported by DoE grant DE-AC02-98CH10886. Zuntz, Kacprzak, Bridle, and Troxel acknowledge support from the European Research Council in the form of a Starting Grant with number 240672. Das was funded by DoE Grant DE-SC0007859. Gruen was supported by SFB-Transregio 33 'The Dark Universe' by the Deutsche Forschungsgemeinschaft (DFG) and the DFG cluster of excellence 'Origin and Structure of the Universe'. Gangkofner acknowledges the support by the DFG Cluster of Excellence 'Origin and Structure of the Universe'. Melchior was supported by DoE grant DE-FG02-91ER40690. Plazas was supported by DoE grant DE-AC02-98CH10886 and by JPL, run by Caltech under a contract for NASA. Lima is partially supported by FAPESP and CNPq.r Funding for the DES Projects has been provided by the US Department of Energy, the US National Science Foundation, the Ministry of Science and Education of Spain, the Science and Technology Facilities Council of the United Kingdom, the Higher Education Funding Council for England, the National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign, the Kavli Institute of Cosmological Physics at the University of Chicago, the Center for Cosmology and Astro-Particle Physics at the Ohio State University, the Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M University, Financiadora de Estudos e Projetos, Fundacao Carlos Chagas Filho de Amparo a Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Cientifico e Tecnologico and the Ministerio da Ciencia e Tecnologia, the Deutsche Forschungsgemeinschaft and the Collaborating Institutions in the DES.r The DES data management system is supported by the National Science Foundation under Grant Number AST-1138766. The DES participants from Spanish institutions are partially supported by MINECO under grants AYA2012-39559, ESP2013-48274, FPA2013-47986, and Centro de Excelencia Severo Ochoa SEV-2012-0234, some of which include ERDF funds from the European Union.r The Collaborating Institutions are Argonne National Laboratory, the University of California at Santa Cruz, the University of Cambridge, Centro de Investigaciones Energeticas, Medioambientales y Tecnologicas-Madrid, the University of Chicago, University College London, the DES-Brazil Consortium, the Eidgenossische Technische Hochschule (ETH) Zurich, Fermi National Accelerator Laboratory, the University of Edinburgh, the University of Illinois at Urbana-Champaign, the Institut de Ciencies de l'Espai (IEEC/CSIC), the Institut de Fisica d'Altes Energies, LBNL, the Ludwig-Maximilians Universitat and the associated Excellence Cluster Universe, the University of Michigan, the National Optical Astronomy Observatory, the University of Nottingham, The Ohio State University, the University of Pennsylvania, the University of Portsmouth, SLAC National Accelerator Laboratory, Stanford University, the University of Sussex, and Texas A&M University. NR 120 TC 17 Z9 17 U1 1 U2 2 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD AUG 1 PY 2016 VL 460 IS 2 BP 2245 EP 2281 DI 10.1093/mnras/stw990 PG 37 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DR3WH UT WOS:000379832800087 ER PT J AU Leppert, KD Cecil, DJ AF Leppert, Kenneth D., II Cecil, Daniel J. TI Tropical Cyclone Diurnal Cycle as Observed by TRMM SO MONTHLY WEATHER REVIEW LA English DT Article ID PRECIPITATION RADAR; ICE SCATTERING; SATELLITE; RAINFALL; INTENSITY; RAINBANDS; OSCILLATION; IMAGERY; CLOUD AB Previous work has indicated a clear, consistent diurnal cycle in rainfall and cold cloudiness coverage around tropical cyclones. This cycle may have important implications for structure and intensity changes of these storms and the forecasting of such changes. The goal of this paper is to use passive and active microwave measurements from the Tropical Rainfall Measuring Mission (TRMM) Microwave Imager (TMI) and Precipitation Radar (PR), respectively, to better understand the tropical cyclone diurnal cycle throughout a deep layer of a tropical cyclone's clouds. The composite coverage by PR reflectivity >= 20 dBZ at various heights as a function of local standard time (LST) and radius suggests the presence of a diurnal signal for radii <500 km through a deep layer (2-10-km height) of the troposphere using 1998-2011 Atlantic tropical cyclones of at least tropical storm strength. The area covered by reflectivity >= 20 dBZ at radii 100-500 km peaks in the morning (0130-1030 LST) and reaches a minimum 1030-1930 LST. Radii between 300 and 500 km tend to reach a minimum in coverage closer to 1200 LST before reaching another peak at 2100 LST. The inner core (0-100 km) appears to be associated with a single-peaked diurnal cycle only at upper levels (8-10 km) with a maximumat 2230-0430 LST. The TMI rainfall composites suggest a clear diurnal cycle at all radii between 200 and 1000 km with peak rainfall coverage and rain rate occurring in the morning (0130-0730 LST). C1 [Leppert, Kenneth D., II] Univ Alabama, Ctr Earth Syst Sci, Huntsville, AL 35899 USA. [Cecil, Daniel J.] NASA Marshall Space Flight Ctr, Huntsville, AL USA. [Leppert, Kenneth D., II] Univ Louisiana Monroe, Monroe, LA USA. RP Leppert, KD (reprint author), Univ Louisiana Monroe, Sch Sci, Hanna Rm 306,700 Univ Ave, Monroe, LA 71209 USA. EM leppert@ulm.edu FU NASA [NNX12AK70G, NNM11AA01A] FX Funding for this research was generously provided through NASA Grants NNX12AK70G and NNM11AA01A. The authors thank Dr. Haiyan Jiang for her help in identifying TRMM orbits that passed over tropical cyclones and Dr. Jason Dunion for his helpful suggestions for conducting this work. The authors are also grateful to the University of Utah for providing the TRMM data, Colorado State University for providing the radius of maximum wind and wind shear data, and the helpful suggestions from Jon Zawislak and another anonymous reviewer that led to the improvement of the manuscript. NR 31 TC 0 Z9 0 U1 2 U2 5 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0027-0644 EI 1520-0493 J9 MON WEATHER REV JI Mon. Weather Rev. PD AUG PY 2016 VL 144 IS 8 BP 2793 EP 2808 DI 10.1175/MWR-D-15-0358.1 PG 16 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA DS5BT UT WOS:000380796200002 ER PT J AU Carletta, ND Mullendore, GL Starzec, M Xi, BK Feng, Z Dong, XQ AF Carletta, Nicholas D. Mullendore, Gretchen L. Starzec, Mariusz Xi, Baike Feng, Zhe Dong, Xiquan TI Determining the Best Method for Estimating the Observed Level of Maximum Detrainment Based on Radar Reflectivity SO MONTHLY WEATHER REVIEW LA English DT Article ID LIGHTNING OBSERVATIONS; DEEP CONVECTION; STORM; STEPS; PRECIPITATION; KINEMATICS; TRANSPORT AB Convective mass transport is the transport of mass from near the surface up to the upper troposphere and lower stratosphere (UTLS) by a deep convective updraft. This transport can alter the chemical makeup and water vapor balance of the UTLS, which affects cloud formation and the radiative properties of the atmosphere. It is, therefore, important to understand the exact altitudes at which mass is detrained from convection. The purpose of this study was to improve upon previously published methodologies for estimating the level of maximum detrainment (LMD) within convection using data from a single ground-based radar. Four methods were used to identify the LMD and validated against dual-Doppler-derived vertical mass divergence fields for six cases with a variety of storm types. The best method for locating the LMD was determined to be the method that used a reflectivity texture technique to determine convective cores and a multilayer echo identification to determine anvil locations. Although an improvement over previously published methods, the new methodology still produced unreliable results in certain regimes. The methodology worked best when applied to mature updrafts, as the anvil needs time to grow to a detectable size. Thus, radar reflectivity is found to be valuable in estimating the LMD, but storm maturity must also be considered for best results. C1 [Carletta, Nicholas D.; Mullendore, Gretchen L.; Starzec, Mariusz; Xi, Baike; Dong, Xiquan] Univ North Dakota, Dept Atmospher Sci, Grand Forks, ND 58201 USA. [Carletta, Nicholas D.] NASA Goddard Space Flight Ctr, Greenbelt, MD USA. [Carletta, Nicholas D.] Sci Syst & Applicat Inc, Lanham, MD USA. [Feng, Zhe] Pacific Northwest Natl Lab, Richland, WA 99352 USA. RP Mullendore, GL (reprint author), Univ North Dakota, Clifford Hall,Room 400,4149 Univ Ave,Stop 9006, Grand Forks, ND 58202 USA. EM gretchen@atmos.und.edu FU NSF [ATM-0918010, ATM-1432930]; U.S. Department of Energy (DOE), Office of Science, Biological and Environmental Research; DOE [DE-AC05-76RL01830] FX The authors would like to acknowledge the support from NSF Grants ATM-0918010 and ATM-1432930. The authors thank Timothy Lang for providing access to the STEPS and CHILL dual-Doppler data. The authors would also like to thank Mark Askelson for his advice as a graduate committee member. The authors also thank the three anonymous reviewers for taking the time to provide thoughtful and constructive feedback. Dr. Zhe Feng at the Pacific Northwest National Laboratory is supported by the U.S. Department of Energy (DOE), Office of Science, Biological and Environmental Research as part of the Atmospheric System Research Program and the Regional and Global Climate Modeling Program. The Pacific Northwest National Laboratory is operated for DOE by the Battelle Memorial Institute under Contract DE-AC05-76RL01830. NR 22 TC 0 Z9 0 U1 3 U2 3 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0027-0644 EI 1520-0493 J9 MON WEATHER REV JI Mon. Weather Rev. PD AUG PY 2016 VL 144 IS 8 BP 2915 EP 2926 DI 10.1175/MWR-D-15-0427.1 PG 12 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA DS5BT UT WOS:000380796200008 ER PT J AU Lavraud, B Liu, Y Segura, K He, J Qin, G Temmer, M Vial, JC Xiong, M Davies, JA Rouillard, AP Pinto, R Auchere, F Harrison, RA Eyles, C Gan, W Lamy, P Xia, L Eastwood, JP Kong, L Wang, J Wimmer-Schweingruber, RF Zhang, S Zong, Q Soucek, J An, J Prech, L Zhang, A Rochus, P Bothmer, V Janvier, M Maksimovic, M Escoubet, CP Kilpua, EKJ Tappin, J Vainio, R Poedts, S Dunlop, MW Savani, N Gopalswamy, N Bale, SD Li, G Howard, T DeForest, C Webb, D Lugaz, N Fuselier, SA Dalmasse, K Tallineau, J Vranken, D Fernandez, JG AF Lavraud, B. Liu, Y. Segura, K. He, J. Qin, G. Temmer, M. Vial, J-C Xiong, M. Davies, J. A. Rouillard, A. P. Pinto, R. Auchere, F. Harrison, R. A. Eyles, C. Gan, W. Lamy, P. Xia, L. Eastwood, J. P. Kong, L. Wang, J. Wimmer-Schweingruber, R. F. Zhang, S. Zong, Q. Soucek, J. An, J. Prech, L. Zhang, A. Rochus, P. Bothmer, V. Janvier, M. Maksimovic, M. Escoubet, C. P. Kilpua, E. K. J. Tappin, J. Vainio, R. Poedts, S. Dunlop, M. W. Savani, N. Gopalswamy, N. Bale, S. D. Li, G. Howard, T. DeForest, C. Webb, D. Lugaz, N. Fuselier, S. A. Dalmasse, K. Tallineau, J. Vranken, D. Fernandez, J. G. TI A small mission concept to the Sun-Earth Lagrangian L5 point for innovative solar, heliospheric and space weather science SO JOURNAL OF ATMOSPHERIC AND SOLAR-TERRESTRIAL PHYSICS LA English DT Article DE Space mission; Coronal mass ejections; Instrumentation; Space weather ID CORONAL MASS EJECTIONS; IN-SITU OBSERVATIONS; L-ALPHA-LINE; MAGNETIC-FIELD; STEREO MISSION; 1 AU; INTERPLANETARY SHOCKS; ENERGETIC PARTICLES; RADIATION BELT; DRIVEN SHOCK AB We present a concept for a small mission to the Sun-Earth Lagrangian L5 point for innovative solar, heliospheric and space weather science. The proposed INvestigation of Solar-Terrestrial Activity aNd Transients (INSTANT) mission is designed to identify how solar coronal magnetic fields drive eruptions, mass transport and particle acceleration that impact the Earth and the heliosphere. INSTANT is the first mission designed to (1) obtain measurements of coronal magnetic fields from space and (2) determine coronal mass ejection (CME) kinematics with unparalleled accuracy. Thanks to innovative instrumentation at a vantage point that provides the most suitable perspective view of the Sun-Earth system, INSTANT would uniquely track the whole chain of fundamental processes driving space weather at Earth. We present the science requirements, payload and mission profile that fulfill ambitious science objectives within small mission programmatic boundary conditions. (C) 2016 Elsevier Ltd. All rights reserved. C1 [Lavraud, B.; Segura, K.; Rouillard, A. P.; Pinto, R.] Univ Toulouse 3, Inst Rech Astrophys & Planetol, Toulouse, France. [Lavraud, B.; Segura, K.; Rouillard, A. P.; Pinto, R.] CNRS, UMR 5277, Toulouse, France. [Liu, Y.; Qin, G.; Xiong, M.; Kong, L.; Wang, J.; Zhang, S.; An, J.; Zhang, A.] Chinese Acad Sci, Natl Space Sci Ctr, Beijing, Peoples R China. [He, J.; Zong, Q.] Peking Univ, Beijing 100871, Peoples R China. [Temmer, M.] Graz Univ, Inst Phys, Graz, Austria. [Vial, J-C; Auchere, F.; Janvier, M.] Inst Astrophys Spatiale, Orsay, France. [Davies, J. A.; Harrison, R. A.; Eyles, C.; Tappin, J.; Dunlop, M. W.] RAL Space, Didcot, Oxon, England. [Gan, W.] Purple Mt Observ, Nanjing, Jiangsu, Peoples R China. [Lamy, P.] CNRS, Lab Astrophys Marseille, Marseille, France. [Lamy, P.] Aix Marseille Univ, Marseille, France. [Xia, L.] Shandong Univ, Weihai, Peoples R China. [Eastwood, J. P.] Univ London Imperial Coll Sci Technol & Med, London, England. [Wimmer-Schweingruber, R. F.] Univ Kiel, Kiel, Germany. [Soucek, J.] Inst Atmospher Phys, Prague, Czech Republic. [Prech, L.] Charles Univ Prague, Prague, Czech Republic. [Rochus, P.] Ctr Spatial Liege, Liege, Belgium. [Bothmer, V.] Univ Gottingen, Gottingen, Germany. [Janvier, M.] Univ Paris Saclay, Univ Paris Sud, CNRS, Inst Astrophys Spatiale, Paris, France. [Maksimovic, M.] Observ Paris, Meudon, France. [Escoubet, C. P.] European Space Agcy, Noordwijk, Netherlands. [Kilpua, E. K. J.] Univ Helsinki, Helsinki, Finland. [Vainio, R.] Univ Turku, Turku, Finland. [Poedts, S.] Katholieke Univ Leuven, Leuven, Belgium. [Dunlop, M. W.] Beihang Univ, Beijing, Peoples R China. [Savani, N.] Univ Maryland, UMBC, GPHI, Baltimore, MD USA. [Savani, N.; Gopalswamy, N.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA. [Bale, S. D.] Univ Calif Berkeley, Berkeley, CA 94720 USA. [Li, G.] Univ Alabama, Huntsville, AL 35899 USA. [Howard, T.; DeForest, C.] Southwest Res Inst, Boulder, CO USA. [Webb, D.] Boston Coll, ISR, Chestnut Hill, MA USA. [Lugaz, N.] Univ New Hampshire, Durham, NH 03824 USA. [Fuselier, S. A.] Southwest Res Inst, San Antonio, TX USA. [Dalmasse, K.] Natl Ctr Atmospher Res, POB 3000, Boulder, CO 80307 USA. [Tallineau, J.; Vranken, D.] Qinetiq Space, Kruibeke, Belgium. [Fernandez, J. G.] GMV, Tres Cantos, Spain. RP Lavraud, B (reprint author), Univ Toulouse 3, Inst Rech Astrophys & Planetol, Toulouse, France. RI Bale, Stuart/E-7533-2011; Vainio, Rami/A-5590-2009; Soucek, Jan/G-3424-2014; Kilpua, Emilia/G-8994-2012; Qin, Gang/B-2250-2009; Lugaz, Noe/C-1284-2008 OI Bale, Stuart/0000-0002-1989-3596; Vainio, Rami/0000-0002-3298-2067; Soucek, Jan/0000-0003-0462-6804; Qin, Gang/0000-0002-3437-3716; Lugaz, Noe/0000-0002-1890-6156 FU CNES; CNRS FX The authors acknowledge the inputs and support from more than 180 collaborators to the INSTANT mission proposal submitted to the ESA and CAS call for small missions in 2015. Although INSTANT was not selected in that call, the concept will be proposed in future opportunities at ESA or other agencies. Work at IRAP was supported by CNES and CNRS. BL wishes to thank D. Lario for providing the figure from which Fig. 5 is adapted. NR 79 TC 0 Z9 0 U1 4 U2 6 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1364-6826 EI 1879-1824 J9 J ATMOS SOL-TERR PHY JI J. Atmos. Sol.-Terr. Phys. PD AUG PY 2016 VL 146 BP 171 EP 185 DI 10.1016/j.jastp.2016.06.004 PG 15 WC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences SC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences GA DS2IN UT WOS:000380593300017 ER PT J AU Knysh, S AF Knysh, Sergey TI Zero-temperature quantum annealing bottlenecks in the spin-glass phase SO Nature Communications LA English DT Article ID CRITICAL-BEHAVIOR; TRANSVERSE-FIELD; NEURAL-NETWORKS; MODEL; COMPUTATION; ROTORS AB A promising approach to solving hard binary optimization problems is quantum adiabatic annealing in a transverse magnetic field. An instantaneous ground state-initially a symmetric superposition of all possible assignments of N qubits-is closely tracked as it becomes more and more localized near the global minimum of the classical energy. Regions where the energy gap to excited states is small (for instance at the phase transition) are the algorithm's bottlenecks. Here I show how for large problems the complexity becomes dominated by O(log N) bottlenecks inside the spin-glass phase, where the gap scales as a stretched exponential. For smaller N, only the gap at the critical point is relevant, where it scales polynomially, as long as the phase transition is second order. This phenomenon is demonstrated rigorously for the two-pattern Gaussian Hopfield model. Qualitative comparison with the Sherrington-Kirkpatrick model leads to similar conclusions. C1 [Knysh, Sergey] NASA, Ames Res Ctr, QuAIL, Moffett Field, CA 94035 USA. [Knysh, Sergey] SGT Inc, 7701 Greenbelt Rd,Suite 400, Greenbelt, MD 20770 USA. RP Knysh, S (reprint author), NASA, Ames Res Ctr, QuAIL, Moffett Field, CA 94035 USA.; Knysh, S (reprint author), SGT Inc, 7701 Greenbelt Rd,Suite 400, Greenbelt, MD 20770 USA. EM Sergey.I.Knysh@nasa.gov FU Office of the Director of National Intelligence (ODNI); Intelligence Advanced Research Projects Activity (IARPA) [IAA 145483]; Air Force Research Laboratory (AFRL) Information Directorate [F4HBKC4162G001] FX I would like to thank Vadim Smelyanskiy for useful discussions. This work was supported in part by the Office of the Director of National Intelligence (ODNI), Intelligence Advanced Research Projects Activity (IARPA), via IAA 145483, and by the Air Force Research Laboratory (AFRL) Information Directorate under grant F4HBKC4162G001. The views and conclusions contained herein are those of the author and should not be interpreted as necessarily representing the official policies or endorsements, either expressed or implied, of ODNI, IARPA, AFRL or the U.S. Government. The U.S. Government is authorized to reproduce and distribute reprints for Governmental purpose notwithstanding any copyright annotation thereon. NR 51 TC 2 Z9 2 U1 8 U2 8 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 2041-1723 J9 NAT COMMUN JI Nat. Commun. PD AUG PY 2016 VL 7 AR 12370 DI 10.1038/ncomms12370 PG 9 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA DS5ZA UT WOS:000380860300001 PM 27491338 ER PT J AU Harvey, N AF Harvey, Nate TI GRACE star camera noise SO ADVANCES IN SPACE RESEARCH LA English DT Article DE Low Earth orbit satellites; Attitude; Star cameras; GRACE AB Extending results from previous work by Bandikova et al. (2012) and Inacio et al. (2015), this paper analyzes Gravity Recovery and Climate Experiment (GRACE) star camera attitude measurement noise by processing inter-camera quaternions from 2003 to 2015. We describe a correction to star camera data, which will eliminate a several-arcsec twice-per-rev error with daily modulation, currently visible in the auto-covariance function of the inter-camera quaternion, from future GRACE Level-1B product releases. We also present evidence supporting the argument that thermal conditions/settings affect long-term inter-camera attitude biases by at least tens-of-arcsecs, and that several-to-tens-of-arcsecs per-rev star camera errors depend largely on field-of-view. (C) 2016 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 [Harvey, Nate] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Harvey, Nate] Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. RP Harvey, N (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.; Harvey, N (reprint author), Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM nathaniel.e.harvey@jpl.nasa.gov FU National Aeronautics and Space Administration FX This research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. NR 9 TC 1 Z9 1 U1 2 U2 2 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0273-1177 EI 1879-1948 J9 ADV SPACE RES JI Adv. Space Res. PD AUG 1 PY 2016 VL 58 IS 3 BP 408 EP 414 DI 10.1016/j.asr.2016.04.025 PG 7 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA DQ9WW UT WOS:000379561000012 ER PT J AU Armellin, R Di Lizia, P Zanetti, R AF Armellin, Roberto Di Lizia, Pierluigi Zanetti, Renato TI Dealing with uncertainties in angles-only initial orbit determination SO CELESTIAL MECHANICS & DYNAMICAL ASTRONOMY LA English DT Article DE Initial orbit determination (IOD); Optical observations; Uncertainties mapping; Differential algebra (DA) ID DOMAIN AB A method to deal with uncertainties in initial orbit determination (IOD) is presented. This is based on the use of Taylor differential algebra (DA) to nonlinearly map uncertainties from the observation space to the state space. When a minimum set of observations is available, DA is used to expand the solution of the IOD problem in Taylor series with respect to measurement errors. When more observations are available, high order inversion tools are exploited to obtain full state pseudo-observations at a common epoch. The mean and covariance of these pseudo-observations are nonlinearly computed by evaluating the expectation of high order Taylor polynomials. Finally, a linear scheme is employed to update the current knowledge of the orbit. Angles-only observations are considered and simplified Keplerian dynamics adopted to ease the explanation. Three test cases of orbit determination of artificial satellites in different orbital regimes are presented to discuss the feature and performances of the proposed methodology. C1 [Armellin, Roberto] Univ La Rioja, Dept Matemat & Comp, Logrono 26006, Spain. [Di Lizia, Pierluigi] Politecn Milan, Dept Aerosp Sci & Technol, I-20156 Milan, Italy. [Zanetti, Renato] NASA, Johnson Space Ctr, 2101 NASA Rd 1, Houston, TX 77058 USA. RP Armellin, R (reprint author), Univ La Rioja, Dept Matemat & Comp, Logrono 26006, Spain. EM roberto.armellin@unirioja.es; pierluigi.dilizia@polimi.it; renato.zanetti@nasa.gov OI Armellin, Roberto/0000-0002-3516-6428 FU Sklodowska-Curie Grant [627111] FX R. Armellin acknowledges the support received by the Sklodowska-Curie Grant 627111 (HOPT -Merging Lie perturbation theory and Taylor Differential algebra to address space debris challenges). The authors are grateful to Monica Valli, who implemented a preliminary version of the DA-based IOD update. R. Armellin is thankful to Cristina Parigini for her help in the visualization of the results. NR 22 TC 0 Z9 0 U1 1 U2 1 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0923-2958 EI 1572-9478 J9 CELEST MECH DYN ASTR JI Celest. Mech. Dyn. Astron. PD AUG PY 2016 VL 125 IS 4 BP 435 EP 450 DI 10.1007/s10569-016-9694-z PG 16 WC Astronomy & Astrophysics; Mathematics, Interdisciplinary Applications SC Astronomy & Astrophysics; Mathematics GA DR0VJ UT WOS:000379624700003 ER PT J AU Potter, C AF Potter, Christopher TI Measurements of fog water interception by shrubs on the California central coast SO JOURNAL OF COASTAL CONSERVATION LA English DT Article DE Fog; Deposition; Coastal shrub; Central California; Water budget ID STOMATAL CONDUCTANCE; ESTABLISHMENT; AVAILABILITY; VEGETATION; GRASSLAND; STRATUS; DRIP AB Fog water deposition may be an important component of the water budget of herbaceous-shrub ecosystems on the central and southern coastal regions of California. This paper presents the first analysis of measured fog water drip rates and meteorological controls in shrublands of Big Sur, California. Seasonal totals of 1255 mm and 306 mm of fog water drip were recorded in 2014 and 2015 (respectively), for averaged fog deposition rates of 0.02-0.08 l m(2) hr.(-1) to the soil under shrub canopy cover. The diurnal patterns of fog water drip showed that the majority of all trough water collected under shrubs on no-rain days occurred between the hours of 11 PM and 9 AM. During the study period from June 1 to October 31 of both 2014 and 2015, soil water content decreased significantly from average levels of 4-6 % at the shrub canopy center and middle locations, through 2-3 % VWC at the shrub edge locations, to levels at or below 2 % at 2-m distance locations from the shrub edge in open grass cover. Based on these results, we conclude that detectable rates of shrub canopy fog interception help sustain elevated soil water levels under shrubs and aid woody vegetation survival through periods of low rainfall. C1 [Potter, Christopher] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Potter, C (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM chris.potter@nasa.gov NR 26 TC 0 Z9 0 U1 10 U2 10 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 1400-0350 EI 1874-7841 J9 J COAST CONSERV JI J. Coast. Conserv. PD AUG PY 2016 VL 20 IS 4 BP 315 EP 325 DI 10.1007/s11852-016-0443-y PG 11 WC Biodiversity Conservation; Environmental Sciences; Marine & Freshwater Biology; Water Resources SC Biodiversity & Conservation; Environmental Sciences & Ecology; Marine & Freshwater Biology; Water Resources GA DR0FW UT WOS:000379584400006 ER PT J AU Haddad, EE Tuite, ML Martinez, AM Williford, K Boyer, DL Droser, ML Love, GD AF Haddad, Emily E. Tuite, Michael L. Martinez, Aaron M. Williford, Kenneth Boyer, Diana L. Droser, Mary L. Love, Gordon D. TI Lipid biomarker stratigraphic records through the Late Devonian Frasnian/Famennian boundary: Comparison of high-and low-latitude epicontinental marine settings SO ORGANIC GEOCHEMISTRY LA English DT Article DE Upper Kellwasser; Black shale; Mass extinctions; Appalachian Basin; Madre de Dios Basin; Lipid biomarkers; Redox; Nitrogen isotopes ID HOLY-CROSS MOUNTAINS; SEDIMENTARY ORGANIC-MATTER; OCEANIC ANOXIC EVENT; PHOTIC ZONE EUXINIA; BLACK SHALES; MASS EXTINCTION; BIOGEOCHEMICAL CYCLES; NITROGEN LIMITATION; BIOLOGICAL MARKERS; APPALACHIAN BASIN AB The pervasiveness of black shale preservation in association with Late Devonian biological crises suggests marine anoxia played a major role in driving ecological perturbations. However, Devonian black shale deposition is still mechanistically poorly understood. We have compiled detailed biomarker lipid chemostratigraphic records for 83 different rock samples using molecular constituents of bitumens of Upper Kellwasser equivalent black shales from two foreland basins: from the low paleolatitude Appalachian Basin (New York State) and from the high paleolatitude Madre de Dios Basin (Bolivia), in order to better understand local environmental conditions and organic source inputs during this depositional event. Despite strong indications from stable nitrogen isotopic signatures for fixed nitrogen nutrient limitation, the biomarker assemblages with consistently low-moderate hopane/sterane ratios (< 0.8) indicate that algae were major marine primary producers in both basins throughout the Frasnian/Famennian (F/F) stratigraphic coverage. Consistently higher C-28/C-29 sterane ratios at higher paleolatitude in the more nutrient-replete Madre de Dios Basin suggest prasinophyte microalgae flourished in this setting in accordance with palynological evidence for high contributions of Tasmanites cysts in these strata. All samples contain only very low absolute amounts of aryl isoprenoids (with 2,3,6-trimethyl substitution) and other aromatic carotenoids, up to several orders of magnitude lower than concentrations reported from other Phanerozoic euxinic basins. These data are consistent with local marine paleoredox models for both basins lacking a persistently shallow sulfidic aquatic zone and demonstrate that temporally persistent or spatially pervasive photic zone euxinia is not necessarily associated with all black shale sequences in the Late Devonian. (C) 2016 Published by Elsevier Ltd. C1 [Haddad, Emily E.; Martinez, Aaron M.; Droser, Mary L.; Love, Gordon D.] Univ Calif Riverside, Dept Earth Sci, 900 Univ Ave, Riverside, CA 92521 USA. [Tuite, Michael L.; Williford, Kenneth] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Boyer, Diana L.] SUNY Coll Oswego, Shineman Sci Ctr 241, Dept Earth Sci, Oswego, NY 13126 USA. RP Haddad, EE (reprint author), Univ Calif Riverside, Dept Earth Sci, 900 Univ Ave, Riverside, CA 92521 USA. EM emily.haddad@email.ucr.edu FU National Science Foundation Earth Sciences Program [NSF-EAR 1348988, NSF-EAR 1348981]; Agouron Institute; NSF GRFP; AAPG; SEPM; Gulf Coast Section of SEPM; Paleontological Society FX This work was funded principally by a National Science Foundation Earth Sciences Program grants to GDL (NSF-EAR 1348988) and DLB (NSF-EAR 1348981). GDL also thanks the Agouron Institute for grant support. EEH acknowledges graduate student support from the NSF GRFP, AAPG, SEPM, the Gulf Coast Section of SEPM, and the Paleontological Society. The authors are indebted to Sarah de la Rue for providing Pando X-1 core samples for geochemical analysis. NR 107 TC 0 Z9 0 U1 5 U2 8 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0146-6380 J9 ORG GEOCHEM JI Org. Geochem. PD AUG PY 2016 VL 98 BP 38 EP 53 DI 10.1016/j.orggeochem.2016.05.007 PG 16 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA DR3DH UT WOS:000379782300004 ER PT J AU Chen, TL Primiero, G Raimondi, F Rungta, N AF Chen, Taolue Primiero, Giuseppe Raimondi, Franco Rungta, Neha TI A Computationally Grounded, Weighted Doxastic Logic SO STUDIA LOGICA LA English DT Article; Proceedings Paper CT 7th Workshop on Logical Aspects of Multi-Agent Systems (LAMAS) Co-Located with 15th International Conference on Autonomous Agents and Multi-Agent Systems (AAMAS) CY 2014 CL Paris, FRANCE DE Multi-agent systems; Doxastic logic; Model checking ID MODEL CHECKING; VERIFICATION; SYSTEMS AB Modelling, reasoning and verifying complex situations involving a system of agents is crucial in all phases of the development of a number of safety-critical systems. In particular, it is of fundamental importance to have tools and techniques to reason about the doxastic and epistemic states of agents, to make sure that the agents behave as intended. In this paper we introduce a computationally grounded logic called COGWED and we present two types of semantics that support a range of practical situations. We provide model checking algorithms, complexity characterisations and a prototype implementation. We validate our proposal against a case study from the avionic domain: we assess and verify the situational awareness of pilots flying an aircraft with several automated components in off-nominal conditions. C1 [Chen, Taolue; Primiero, Giuseppe; Raimondi, Franco] Middlesex Univ, Dept Comp Sci, London, England. [Rungta, Neha] NASA Ames Res Ctr, Moffett Field, CA 94035 USA. RP Chen, TL (reprint author), Middlesex Univ, Dept Comp Sci, London, England. EM t.chen@mdx.ac.uk; g.primiero@mdx.ac.uk; f.raimondi@mdx.ac.uk; neha.s.rungta@nasa.gov OI Primiero, Giuseppe/0000-0003-3264-7100 NR 27 TC 0 Z9 0 U1 0 U2 0 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0039-3215 J9 STUD LOGICA JI Stud. Log. PD AUG PY 2016 VL 104 IS 4 SI SI BP 679 EP 703 DI 10.1007/s11225-015-9621-4 PG 25 WC Mathematics; Logic; Philosophy SC Mathematics; Science & Technology - Other Topics; Philosophy GA DQ9KW UT WOS:000379529800004 ER PT J AU Ho, SP Pappas, CG Austermann, J Beall, JA Becker, D Choi, SK Datta, R Duff, SM Gallardo, PA Grace, E Hasselfield, M Henderson, SW Hilton, GC Hubmayr, J Koopman, BJ Lanen, JV Li, D McMahon, J Nati, F Niemack, MD Niraula, P Salatino, M Schillaci, A Schmitt, BL Simon, SM Staggs, ST Stevens, JR Ward, JT Wollack, EJ Vavagiakis, EM AF Ho, S. P. Pappas, C. G. Austermann, J. Beall, J. A. Becker, D. Choi, S. K. Datta, R. Duff, S. M. Gallardo, P. A. Grace, E. Hasselfield, M. Henderson, S. W. Hilton, G. C. Hubmayr, J. Koopman, B. J. Lanen, J. V. Li, D. McMahon, J. Nati, F. Niemack, M. D. Niraula, P. Salatino, M. Schillaci, A. Schmitt, B. L. Simon, S. M. Staggs, S. T. Stevens, J. R. Ward, J. T. Wollack, E. J. Vavagiakis, E. M. TI The First Multichroic Polarimeter Array on the Atacama Cosmology Telescope: Characterization and Performance SO JOURNAL OF LOW TEMPERATURE PHYSICS LA English DT Article DE ACTPol; Cosmic microwave background; Multichroic; Polarization; Transition edge sensors; SQUID AB The Atacama Cosmology Telescope Polarimeter (ACTPol) is a polarization sensitive receiver for the 6-m Atacama Cosmology Telescope (ACT) and measures the small angular scale polarization anisotropies in the cosmic microwave background (CMB). The full focal plane is composed of three detector arrays, containing over 3000 transition edge sensors (TES detectors) in total. The first two detector arrays, observing at 146 GHz, were deployed in 2013 and 2014, respectively. The third and final array is composed of multichroic pixels sensitive to both 90 and 146 GHz and saw first light in February 2015. Fabricated at NIST, this dichroic array consists of 255 pixels, with a total of 1020 polarization sensitive bolometers and is coupled to the telescope with a monolithic array of broad-band silicon feedhorns. The detectors are read out using time-division SQUID multiplexing and cooled by a dilution refrigerator at 110 mK. We present an overview of the assembly and characterization of this multichroic array in the lab, and the initial detector performance in Chile. The detector array has a TES detector electrical yield of 85 %, a total array sensitivity of less than 10 K, and detector time constants and saturation powers suitable for ACT CMB observations. C1 [Ho, S. P.; Pappas, C. G.; Choi, S. K.; Grace, E.; Hasselfield, M.; Niraula, P.; Salatino, M.; Schillaci, A.; Simon, S. M.; Staggs, S. T.] Princeton Univ, Dept Phys, Princeton, NJ 08540 USA. [Austermann, J.; Beall, J. A.; Becker, D.; Duff, S. M.; Hilton, G. C.; Hubmayr, J.; Lanen, J. V.; Li, D.] NIST Quantum Devices Grp, 325 Broadway,Mailcode 817-03, Boulder, CO 80305 USA. [Datta, R.; McMahon, J.] Univ Michigan, Dept Phys, Ann Arbor, MI 48103 USA. [Gallardo, P. A.; Henderson, S. W.; Koopman, B. J.; Niemack, M. D.; Stevens, J. R.; Vavagiakis, E. M.] Cornell Univ, Dept Phys, Ithaca, NY 14853 USA. [Nati, F.; Schmitt, B. L.; Ward, J. T.] Univ Penn, Dept Phys & Astron, 209 South 33rd St, Philadelphia, PA 19104 USA. [Wollack, E. J.] Natl Aeronaut & Space Adm, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Ho, SP (reprint author), Princeton Univ, Dept Phys, Princeton, NJ 08540 USA. EM spho@princeton.edu RI Wollack, Edward/D-4467-2012; Nati, Federico/I-4469-2016 OI Wollack, Edward/0000-0002-7567-4451; Nati, Federico/0000-0002-8307-5088 FU U.S. National Science Foundation [AST-0965625, PHY-1214379]; NIST Quantum Initiative; NASA [NNX13AE56G, NNX14AB58G]; NASA Space Technology Research Fellowship awards FX This work was supported by the U.S. National Science Foundation through awards AST-0965625 and PHY-1214379. The NIST authors would like to acknowledge the support of the NIST Quantum Initiative. The development of multichroic detectors and lenses was supported by NASA Grants s NNX13AE56G and NNX14AB58G. The work of KPC, KTC, EG, BJK, CM, BLS, JTW, and SMS was supported by NASA Space Technology Research Fellowship awards. NR 11 TC 2 Z9 2 U1 4 U2 9 PU SPRINGER/PLENUM PUBLISHERS PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0022-2291 EI 1573-7357 J9 J LOW TEMP PHYS JI J. Low Temp. Phys. PD AUG PY 2016 VL 184 IS 3-4 BP 559 EP 567 DI 10.1007/s10909-016-1573-1 PG 9 WC Physics, Applied; Physics, Condensed Matter SC Physics GA DQ2HF UT WOS:000379022700006 ER PT J AU Datta, R Austermann, J Beall, JA Becker, D Coughlin, KP Duff, SM Gallardo, PA Grace, E Hasselfield, M Henderson, SW Hilton, GC Ho, SP Hubmayr, J Koopman, BJ Lanen, JV Li, D McMahon, J Munson, CD Nati, F Niemack, MD Page, L Pappas, CG Salatino, M Schmitt, BL Schillaci, A Simon, SM Staggs, ST Stevens, JR Vavagiakis, EM Ward, JT Wollack, EJ AF Datta, R. Austermann, J. Beall, J. A. Becker, D. Coughlin, K. P. Duff, S. M. Gallardo, P. A. Grace, E. Hasselfield, M. Henderson, S. W. Hilton, G. C. Ho, S. P. Hubmayr, J. Koopman, B. J. Lanen, J. V. Li, D. McMahon, J. Munson, C. D. Nati, F. Niemack, M. D. Page, L. Pappas, C. G. Salatino, M. Schmitt, B. L. Schillaci, A. Simon, S. M. Staggs, S. T. Stevens, J. R. Vavagiakis, E. M. Ward, J. T. Wollack, E. J. TI Design and Deployment of a Multichroic Polarimeter Array on the Atacama Cosmology Telescope SO JOURNAL OF LOW TEMPERATURE PHYSICS LA English DT Article DE Anti-reflection coating; Cosmic microwave background; Feedhorn; Millimeter wave; Polarimeter; Silicon lenses; Superconducting detectors; TES ID OPTICAL DESIGN; POLARIZATION AB We present the design and the preliminary on-sky performance with respect to beams and passbands of a multichroic polarimeter array covering the 90 and 146 GHz cosmic microwave background bands and its enabling broad-band optical system recently deployed on the Atacama Cosmology Telescope (ACT). The constituent pixels are feedhorn-coupled multichroic polarimeters fabricated at NIST. This array is coupled to the ACT telescope via a set of three silicon lenses incorporating novel broad-band metamaterial anti-reflection coatings. This receiver represents the first multichroic detector array deployed for a CMB experiment and paves the way for the extensive use of multichroic detectors and broad-band optical systems in the next generation of CMB experiments. C1 [Datta, R.; Coughlin, K. P.; McMahon, J.; Munson, C. D.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA. [Austermann, J.; Beall, J. A.; Becker, D.; Duff, S. M.; Hilton, G. C.; Hubmayr, J.; Lanen, J. V.; Li, D.] NIST, Quantum Devices Grp, 325 Broadway Mailcode 817-03, Boulder, CO 80305 USA. [Gallardo, P. A.; Henderson, S. W.; Koopman, B. J.; Niemack, M. D.; Stevens, J. R.; Vavagiakis, E. M.] Cornell Univ, Dept Phys, Ithaca, NY 14853 USA. [Grace, E.; Ho, S. P.; Page, L.; Pappas, C. G.; Salatino, M.; Schillaci, A.; Simon, S. M.; Staggs, S. T.] Princeton Univ, Joseph Henry Labs Phys, Jadwin Hall, Princeton, NJ 08544 USA. [Hasselfield, M.] Princeton Univ, Dept Astrophys Sci, Peyton Hall, Princeton, NJ 08544 USA. [Li, D.] SLAC Natl Accelerator Lab, 2575 Sandy Hill Rd, Menlo Pk, CA 94025 USA. [Nati, F.; Schmitt, B. L.; Ward, J. T.] Univ Penn, Dept Phys & Astron, 209 South 33rd St, Philadelphia, PA 19104 USA. [Schillaci, A.] Soc Radiosky Asesorias Ingn Ltd, Dept 805, Lincoya 54, Concepcion, Chile. [Wollack, E. J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Datta, R (reprint author), Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA. EM dattar@umich.edu RI Wollack, Edward/D-4467-2012; Nati, Federico/I-4469-2016 OI Wollack, Edward/0000-0002-7567-4451; Nati, Federico/0000-0002-8307-5088 FU NASA [NNX13AE56G, NNX14AB58G]; U.S. National Science Foundation [AST-0965625, PHY-1214379]; NIST Quantum Initiative; NASA Office of the Chief Technologists Space Technology Research Fellowship awards FX This work was supported by NASA through awards NNX13AE56G and NNX14AB58G and by the U.S. National Science Foundation through awards AST-0965625 and PHY-1214379. The NIST authors would like to acknowledge the support of the NIST Quantum Initiative. The work of KPC, EG, BJK, BLS, CDM, JTW, and SMS were supported by NASA Office of the Chief Technologists Space Technology Research Fellowship awards. NR 25 TC 3 Z9 3 U1 2 U2 4 PU SPRINGER/PLENUM PUBLISHERS PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0022-2291 EI 1573-7357 J9 J LOW TEMP PHYS JI J. Low Temp. Phys. PD AUG PY 2016 VL 184 IS 3-4 BP 568 EP 575 DI 10.1007/s10909-016-1553-5 PG 8 WC Physics, Applied; Physics, Condensed Matter SC Physics GA DQ2HF UT WOS:000379022700007 ER PT J AU Jhabvala, CA Benford, DJ Brekosky, RP Costen, NP Datesman, AM Hilton, GC Irwin, KD Maher, SF Manos, G Miller, TM Moseley, SH Sharp, EH Staguhn, JG Wang, F Wollack, EJ AF Jhabvala, C. A. Benford, D. J. Brekosky, R. P. Costen, N. P. Datesman, A. M. Hilton, G. C. Irwin, K. D. Maher, S. F. Manos, G. Miller, T. M. Moseley, S. H. Sharp, E. H. Staguhn, J. G. Wang, F. Wollack, E. J. TI Superconducting Pathways Through Kilopixel Backshort-Under-Grid Arrays SO JOURNAL OF LOW TEMPERATURE PHYSICS LA English DT Article DE Backshort-Under-Grid; Bolometer; HAWC; Through wafer via; Transition edge sensor; Indium bump bonding; Atomic layer deposition ID INFRARED ASTRONOMY; BOLOMETER ARRAYS AB We have demonstrated in the laboratory multiple, fully functional, kilopixel, bolometer arrays for the upgraded instrument, the High-resolution airborne wideband camera plus (HAWC+), for the stratospheric observatory for infrared astronomy (SOFIA). Each kilopixel array consists of three individual components assembled into a single working unit: (1) a filled, Transition Edge Sensor (TES) bolometer array, (2) an infrared, back-termination, and (3) an integrated, two-dimensional superconducting quantum interference device (SQUID) multiplexer readout. Kilopixel TES arrays are directly indium-bump-bonded to a 32 40 SQUID multiplexer (MUX) circuit. In order to provide a fully superconducting pathway from the TES to the SQUID readout, numerous superconductor-to-superconductor interfaces must be made. This paper focuses on the fabrication techniques needed to create the superconducting path from the TES, out of the detector membrane, through the wafer, and to the SQUID readout. C1 [Jhabvala, C. A.; Benford, D. J.; Manos, G.; Miller, T. M.; Moseley, S. H.; Wollack, E. J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Brekosky, R. P.; Costen, N. P.; Datesman, A. M.] Stinger Ghaffarian Technol Inc, Seabrook, MD USA. [Hilton, G. C.] NIST, Boulder, CO USA. [Irwin, K. D.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA. [Sharp, E. H.] Global Sci & Technol Inc, Greenbelt, MD USA. [Maher, S. F.] Sci Syst & Applicat Inc, Greenbelt, MD USA. [Staguhn, J. G.] Johns Hopkins Univ, Baltimore, MD USA. [Wang, F.] ASRC Fed Space & Def, Greenbelt, MD USA. RP Jhabvala, CA (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM christine.a.jhabvala@nasa.gov RI Wollack, Edward/D-4467-2012; Benford, Dominic/D-4760-2012 OI Wollack, Edward/0000-0002-7567-4451; Benford, Dominic/0000-0002-9884-4206 FU NASA FX This work was supported through a series of NASA awards, including the High resolution Airborne Wideband Camera Plus (HAWC+/SOFIA, Dr. Darren Dowell, Principal Investigator) and the Primordial Inflation Polarization Explorer (PIPER, Dr. Alan Kogut, Principal Investigator). The authors also wish to thank the work of Dr. James A. Chervenak, NASA Goddard Space Flight Center, Detector Systems Branch, for cryogenic test support. NR 10 TC 0 Z9 0 U1 0 U2 1 PU SPRINGER/PLENUM PUBLISHERS PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0022-2291 EI 1573-7357 J9 J LOW TEMP PHYS JI J. Low Temp. Phys. PD AUG PY 2016 VL 184 IS 3-4 BP 615 EP 620 DI 10.1007/s10909-016-1487-y PG 6 WC Physics, Applied; Physics, Condensed Matter SC Physics GA DQ2HF UT WOS:000379022700014 ER PT J AU Lowitz, AE Brown, AD Mikula, V Stevenson, TR Timbie, PT Wollack, EJ AF Lowitz, A. E. Brown, A. D. Mikula, V. Stevenson, T. R. Timbie, P. T. Wollack, E. J. TI Design, Fabrication, and Testing of a TiN/Ti/TiN Trilayer KID Array for 3 mm CMB Observations SO JOURNAL OF LOW TEMPERATURE PHYSICS LA English DT Article DE Kinetic inductance detector; CMB; Titanium nitride; Trilayer AB Kinetic inductance detectors (KIDs) are a promising technology for astronomical observations over a wide range of wavelengths in the mm and sub-mm regime. Simple fabrication, in as little as one lithographic layer, and passive frequency-domain multiplexing, with readout of up to 1000 pixels on a single line with a single cold amplifier, make KIDs an attractive solution for high-pixel-count detector arrays. We are developing an array that optimizes KIDs for optical frequencies near 100 GHz to expand their usefulness in mm-wave applications, with a particular focus on CMB B-mode measurement efforts in association with the QUBIC telescope. We have designed, fabricated, and tested a 20-pixel prototype array using a simple quasi-lumped microstrip design and pulsed DC reactive magnetron-sputtered TiN/Ti/TiN trilayer resonators, optimized for detecting 100 GHz (3 mm) signals. Here we present a discussion of design considerations for the array, as well as preliminary detector characterization measurements and results from a study of TiN trilayer properties. C1 [Lowitz, A. E.; Timbie, P. T.] Univ Wisconsin, Madison, WI 53706 USA. [Brown, A. D.; Stevenson, T. R.; Wollack, E. J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA. [Mikula, V.] Catholic Univ Amer, Washington, DC 20064 USA. RP Lowitz, AE (reprint author), Univ Wisconsin, Madison, WI 53706 USA. EM lowitz@wisc.edu RI Wollack, Edward/D-4467-2012 OI Wollack, Edward/0000-0002-7567-4451 FU NASA Space Technology Research Fellowship FX This work was supported by a NASA Space Technology Research Fellowship. NR 6 TC 0 Z9 0 U1 4 U2 7 PU SPRINGER/PLENUM PUBLISHERS PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0022-2291 EI 1573-7357 J9 J LOW TEMP PHYS JI J. Low Temp. Phys. PD AUG PY 2016 VL 184 IS 3-4 BP 627 EP 633 DI 10.1007/s10909-016-1584-y PG 7 WC Physics, Applied; Physics, Condensed Matter SC Physics GA DQ2HF UT WOS:000379022700016 ER PT J AU Duff, SM Austermann, J Beall, JA Becker, D Datta, R Gallardo, PA Henderson, SW Hilton, GC Ho, SP Hubmayr, J Koopman, BJ Li, D McMahon, J Nati, F Niemack, MD Pappas, CG Salatino, M Schmitt, BL Simon, SM Staggs, ST Stevens, JR Van Lanen, J Vavagiakis, EM Ward, JT Wollack, EJ AF Duff, S. M. Austermann, J. Beall, J. A. Becker, D. Datta, R. Gallardo, P. A. Henderson, S. W. Hilton, G. C. Ho, S. P. Hubmayr, J. Koopman, B. J. Li, D. McMahon, J. Nati, F. Niemack, M. D. Pappas, C. G. Salatino, M. Schmitt, B. L. Simon, S. M. Staggs, S. T. Stevens, J. R. Van Lanen, J. Vavagiakis, E. M. Ward, J. T. Wollack, E. J. TI Advanced ACTPol Multichroic Polarimeter Array Fabrication Process for 150 mm Wafers SO JOURNAL OF LOW TEMPERATURE PHYSICS LA English DT Article DE AlMn; Multichroic; Polarimeter; SiNx; Transition-edge sensor ID POLARIZATION AB Advanced ACTPol (AdvACT) is a third-generation cosmic microwave background receiver to be deployed in 2016 on the Atacama Cosmology Telescope (ACT). Spanning five frequency bands from 25 to 280 GHz and having just over 5600 transition-edge sensor (TES) bolometers, this receiver will exhibit increased sensitivity and mapping speed compared to previously fielded ACT instruments. This paper presents the fabrication processes developed by NIST to scale to large arrays of feedhorn-coupled multichroic AlMn-based TES polarimeters on 150-mm diameter wafers. In addition to describing the streamlined fabrication process which enables high yields of densely packed detectors across larger wafers, we report the details of process improvements for sensor (AlMn) and insulator (SiN) materials and microwave structures, and the resulting performance improvements. C1 [Duff, S. M.; Austermann, J.; Beall, J. A.; Becker, D.; Hilton, G. C.; Hubmayr, J.; Van Lanen, J.] NIST, 325 Broadway, Boulder, CO 80305 USA. [Datta, R.; McMahon, J.] Univ Michigan, Dept Phys, Ann Arbor, MI 48103 USA. [Gallardo, P. A.; Henderson, S. W.; Koopman, B. J.; Niemack, M. D.; Stevens, J. R.; Vavagiakis, E. M.] Cornell Univ, Dept Phys, Ithaca, NY 14853 USA. [Ho, S. P.; Pappas, C. G.; Salatino, M.; Simon, S. M.; Staggs, S. T.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Li, D.] SLAC Natl Accelerator Lab, 2575 Sandy Hill Rd, Menlo Pk, CA 94025 USA. [Nati, F.; Schmitt, B. L.; Ward, J. T.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. [Wollack, E. J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Duff, SM (reprint author), NIST, 325 Broadway, Boulder, CO 80305 USA. EM shannon.duff@nist.gov RI Wollack, Edward/D-4467-2012; Nati, Federico/I-4469-2016 OI Wollack, Edward/0000-0002-7567-4451; Nati, Federico/0000-0002-8307-5088 FU U.S. National Science Foundation [1440226]; NIST Quantum Initiative; NASA [NNX13AE56G, NNX14AB58G]; NASA Space Technology Research Fellowship awards FX This work was supported by the U.S. National Science Foundation through award 1440226. The NIST authors would like to acknowledge the support of the NIST Quantum Initiative. The development of multichroic detectors and lenses was supported by NASA grants NNX13AE56G and NNX14AB58G. The work of BJK, BLS, JTW, and SMS was supported by NASA Space Technology Research Fellowship awards. NR 15 TC 2 Z9 2 U1 1 U2 4 PU SPRINGER/PLENUM PUBLISHERS PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0022-2291 EI 1573-7357 J9 J LOW TEMP PHYS JI J. Low Temp. Phys. PD AUG PY 2016 VL 184 IS 3-4 BP 634 EP 641 DI 10.1007/s10909-016-1576-y PG 8 WC Physics, Applied; Physics, Condensed Matter SC Physics GA DQ2HF UT WOS:000379022700017 ER PT J AU Denis, KL Ali, A Appel, J Bennett, CL Chang, MP Chuss, DT Colazo, FA Costen, N Essinger-Hileman, T Hu, R Marriage, T Rostem, K U-Yen, K Wollack, EJ AF Denis, K. L. Ali, A. Appel, J. Bennett, C. L. Chang, M. P. Chuss, D. T. Colazo, F. A. Costen, N. Essinger-Hileman, T. Hu, R. Marriage, T. Rostem, K. U-Yen, K. Wollack, E. J. TI Fabrication of Feedhorn-Coupled Transition Edge Sensor Arrays for Measurement of the Cosmic Microwave Background Polarization SO JOURNAL OF LOW TEMPERATURE PHYSICS LA English DT Article DE TES; CMB; Wafer bonding; Micro-machining; Polarization ID BOLOMETER AB Characterization of the minute cosmic microwave background polarization signature requires multi-frequency, high-throughput precision instrument systems. We have previously described the detector fabrication of a 40 GHz focal plane and now describe the fabrication of detector modules for measurement of the CMB at 90 GHz. The 90 GHz detectors are a scaled version of the 40 GHz architecture where, due to smaller size detectors, we have implemented a modular (wafer level) rather than the chip-level architecture. The new fabrication process utilizes the same design rules with the added challenge of increased wiring density to the 74 TES's as well as a new wafer level hybridization procedure. The hexagonally shaped modules are tile-able, and as such can be used to form the large focal planes required for a space-based CMB polarimeter. The detectors described here will be deployed in two focal planes with seven modules each in the Johns Hopkins University led ground-based Cosmology Large Angular Scale Surveyor (CLASS) telescope. C1 [Denis, K. L.; Chang, M. P.; Colazo, F. A.; Costen, N.; Hu, R.; U-Yen, K.; Wollack, E. J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Ali, A.; Appel, J.; Bennett, C. L.; Essinger-Hileman, T.; Marriage, T.; Rostem, K.] Johns Hopkins Univ, Baltimore, MD 21218 USA. [Chang, M. P.; Costen, N.; Hu, R.] Stinger Ghaffarian Technol Greenbelt, Greenbelt, MD 20770 USA. [Chuss, D. T.] Villanova Univ, Villanova, PA 19085 USA. RP Denis, KL (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM kevin.l.denis@nasa.gov RI Wollack, Edward/D-4467-2012; OI Wollack, Edward/0000-0002-7567-4451; Denis, Kevin/0000-0002-3592-5703 FU NASA ROSES/APRA grant; National Science Foundation [0959349, 1429236] FX NASA ROSES/APRA grant provided support for the detector technology development. We acknowledge the National Science Foundation for their support of CLASS under Grants numbered 0959349 and 1429236. NR 10 TC 1 Z9 1 U1 2 U2 3 PU SPRINGER/PLENUM PUBLISHERS PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0022-2291 EI 1573-7357 J9 J LOW TEMP PHYS JI J. Low Temp. Phys. PD AUG PY 2016 VL 184 IS 3-4 BP 668 EP 673 DI 10.1007/s10909-015-1366-y PG 6 WC Physics, Applied; Physics, Condensed Matter SC Physics GA DQ2HF UT WOS:000379022700022 ER PT J AU Fyhrie, A Glenn, J Wheeler, J Day, P Eom, BH Leduc, H Skrutskie, M AF Fyhrie, A. Glenn, J. Wheeler, J. Day, P. Eom, B. H. Leduc, H. Skrutskie, M. TI Towards Background-Limited Kinetic Inductance Detectors for a Cryogenic Far-Infrared Space Telescope SO JOURNAL OF LOW TEMPERATURE PHYSICS LA English DT Article DE Kinetic inductance detector; Far-infrared; Low NEP AB Arrays of tens of thousands of sensitive far-infrared detectors coupled to a cryogenic 4-6 m class orbital telescope are needed to trace the assembly of galaxies over cosmic time. The sensitivity of a 4 Kelvin telescope observing in the far-infrared (30-300 m) would be limited by zodiacal light and Galactic interstellar dust emission, and require broadband detector noise equivalent powers (NEPs) in the range of 3 W/. We are fabricating and testing 96 element arrays of lumped-element kinetic inductance detectors (LEKIDs) designed to reach NEPs near this level in a low-background laboratory environment. The LEKIDs are fabricated with aluminum: the low normal-state resistivity of Al permits the use of very thin wire-grid absorber lines (150 nm) for efficient absorption of radiation, while the small volumes enable high sensitivities because quasiparticle densities are high. Such narrow absorption lines present a fabrication challenge, but we deposit TiN atop the Al to increase the robustness of the detectors and achieve a 95 yield. We present the design of these Al/TiN bilayer LEKIDs and preliminary sensitivity measurements at 350 m optically loaded by cold blackbody radiation. C1 [Fyhrie, A.; Glenn, J.; Wheeler, J.] Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA. [Day, P.; Eom, B. H.; Leduc, H.] Jet Prop Lab, Pasadena, CA USA. [Skrutskie, M.] Univ Virginia, Charlottesville, VA USA. RP Fyhrie, A (reprint author), Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA. EM adalyn.fyhrie@colorado.edu NR 10 TC 1 Z9 1 U1 3 U2 3 PU SPRINGER/PLENUM PUBLISHERS PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0022-2291 EI 1573-7357 J9 J LOW TEMP PHYS JI J. Low Temp. Phys. PD AUG PY 2016 VL 184 IS 3-4 BP 712 EP 717 DI 10.1007/s10909-016-1539-3 PG 6 WC Physics, Applied; Physics, Condensed Matter SC Physics GA DQ2HF UT WOS:000379022700029 ER PT J AU Hunacek, J Bock, J Bradford, CM Bumble, B Chang, TC Cheng, YT Cooray, A Crites, A Hailey-Dunsheath, S Gong, Y Kenyon, M Koch, P Li, CT O'Brient, R Shirokoff, E Shiu, C Staniszewski, Z Uzgil, B Zemcov, M AF Hunacek, J. Bock, J. Bradford, C. M. Bumble, B. Chang, T-C. Cheng, Y-T. Cooray, A. Crites, A. Hailey-Dunsheath, S. Gong, Y. Kenyon, M. Koch, P. Li, C-T. O'Brient, R. Shirokoff, E. Shiu, C. Staniszewski, Z. Uzgil, B. Zemcov, M. TI Design and Fabrication of TES Detector Modules for the TIME-Pilot [CII] Intensity Mapping Experiment SO JOURNAL OF LOW TEMPERATURE PHYSICS LA English DT Article DE Reionization; Intensity mapping; Bolometers; Transition edge sensors ID POWER SPECTRUM; REIONIZATION; SPECTROMETER; CONSTRAINTS; GALAXIES; UNIVERSE; EPOCH AB We are developing a series of close-packed modular detector arrays for TIME-Pilot, a new mm-wavelength grating spectrometer array that will map the intensity fluctuations of the redshifted 157.7 m emission line of singly ionized carbon ([CII]) from redshift to 9. TIME-Pilot's two banks of 16 parallel-plate waveguide spectrometers (one bank per polarization) will have a spectral range of 183-326 GHz and a resolving power of . The spectrometers use a curved diffraction grating to disperse and focus the light on a series of output arcs, each sampled by 60 transition edge sensor (TES) bolometers with gold micro-mesh absorbers. These low-noise detectors will be operated from a 250 mK base temperature and are designed to have a background-limited NEP of . This proceeding presents an overview of the detector design in the context of the TIME-Pilot instrument. Additionally, a prototype detector module produced at the Microdevices Laboratory at JPL is shown. C1 [Hunacek, J.; Bock, J.; Bradford, C. M.; Cheng, Y-T.; Crites, A.; Hailey-Dunsheath, S.; O'Brient, R.; Shiu, C.] CALTECH, Pasadena, CA 91125 USA. [Bock, J.; Bradford, C. M.; Bumble, B.; Kenyon, M.; O'Brient, R.; Staniszewski, Z.] Jet Prop Lab, Pasadena, CA USA. [Chang, T-C.; Koch, P.; Li, C-T.] Acad Sinica, Inst Astron & Astrophys, Taipei, Taiwan. [Cooray, A.] Univ Calif Irvine, Irvine, CA USA. [Shirokoff, E.] Univ Chicago, Chicago, IL 60637 USA. [Uzgil, B.] Univ Penn, Philadelphia, PA 19104 USA. [Gong, Y.] Natl Astron Observ China, Beijing, Peoples R China. [Zemcov, M.] Rochester Inst Technol, Rochester, NY 14623 USA. RP Hunacek, J (reprint author), CALTECH, Pasadena, CA 91125 USA. EM jhunacek@caltech.edu FU National Science Foundation Graduate Research Fellowship [DGE1144469] FX This material is based upon work supported by the National Science Foundation Graduate Research Fellowship under Grant No. DGE1144469. NR 14 TC 0 Z9 0 U1 1 U2 2 PU SPRINGER/PLENUM PUBLISHERS PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0022-2291 EI 1573-7357 J9 J LOW TEMP PHYS JI J. Low Temp. Phys. PD AUG PY 2016 VL 184 IS 3-4 BP 733 EP 738 DI 10.1007/s10909-015-1359-x PG 6 WC Physics, Applied; Physics, Condensed Matter SC Physics GA DQ2HF UT WOS:000379022700032 ER PT J AU Chuss, DT Ali, A Amiri, M Appel, J Bennett, CL Colazo, F Denis, KL Dunner, R Essinger-Hileman, T Eimer, J Fluxa, P Gothe, D Halpern, M Harrington, K Hilton, G Hinshaw, G Hubmayr, J Iuliano, J Marriage, TA Miller, N Moseley, SH Mumby, G Petroff, M Reintsema, C Rostem, K U-Yen, K Watts, D Wagner, E Wollack, EJ Xu, Z Zeng, L AF Chuss, D. T. Ali, A. Amiri, M. Appel, J. Bennett, C. L. Colazo, F. Denis, K. L. Dunner, R. Essinger-Hileman, T. Eimer, J. Fluxa, P. Gothe, D. Halpern, M. Harrington, K. Hilton, G. Hinshaw, G. Hubmayr, J. Iuliano, J. Marriage, T. A. Miller, N. Moseley, S. H. Mumby, G. Petroff, M. Reintsema, C. Rostem, K. U-Yen, K. Watts, D. Wagner, E. Wollack, E. J. Xu, Z. Zeng, L. TI Cosmology Large Angular Scale Surveyor (CLASS) Focal Plane Development SO JOURNAL OF LOW TEMPERATURE PHYSICS LA English DT Article DE CMB; TES ID MICROWAVE BACKGROUND POLARIMETRY; BANDWIDTH AB The Cosmology Large Angular Scale Surveyor (CLASS) will measure the polarization of the Cosmic Microwave Background to search for and characterize the polarized signature of inflation. CLASS will operate from the Atacama Desert and observe 70 % of the sky. A variable-delay polarization modulator provides modulation of the polarization at 10 Hz to suppress the 1/f noise of the atmosphere and enable the measurement of the large angular scale polarization modes. The measurement of the inflationary signal across angular scales that spans both the recombination and reionization features allows a test of the predicted shape of the polarized angular power spectra in addition to a measurement of the energy scale of inflation. CLASS is an array of telescopes covering frequencies of 38, 93, 148, and 217 GHz. These frequencies straddle the foreground minimum and thus allow the extraction of foregrounds from the primordial signal. Each focal plane contains feedhorn-coupled transition-edge sensors that simultaneously detect two orthogonal linear polarizations. The use of single-crystal silicon as the dielectric for the on-chip transmission lines enables both high efficiency and uniformity in fabrication. Integrated band definition has been implemented that both controls the bandpass of the single-mode transmission on the chip and prevents stray light from coupling to the detectors. C1 [Chuss, D. T.] Villanova Univ, Dept Phys, Villanova, PA 19085 USA. [Ali, A.; Appel, J.; Bennett, C. L.; Essinger-Hileman, T.; Eimer, J.; Gothe, D.; Harrington, K.; Iuliano, J.; Marriage, T. A.; Miller, N.; Mumby, G.; Petroff, M.; Rostem, K.; Watts, D.; Wagner, E.; Xu, Z.] Johns Hopkins Univ, Dept Phys & Astron, 3400 N Charles St, Baltimore, MD 21218 USA. [Colazo, F.; Miller, N.; Moseley, S. H.; Rostem, K.; Wollack, E. J.] NASA, Goddard Space Flight Ctr, Code 665, Greenbelt, MD 20771 USA. [Denis, K. L.] NASA, Goddard Space Flight Ctr, Code 553, Greenbelt, MD 20771 USA. [U-Yen, K.] NASA, Goddard Space Flight Ctr, Code 555, Greenbelt, MD 20771 USA. [Amiri, M.; Halpern, M.; Hinshaw, G.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z4, Canada. [Hilton, G.; Hubmayr, J.; Reintsema, C.] NIST, 325 Broadway, Boulder, CO 80305 USA. [Zeng, L.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Dunner, R.; Fluxa, P.] Pontificia Univ Catolica Chile, Inst Astrofis, Santiago, Chile. RP Chuss, DT (reprint author), Villanova Univ, Dept Phys, Villanova, PA 19085 USA. EM david.chuss@villanova.edu RI Wollack, Edward/D-4467-2012; OI Wollack, Edward/0000-0002-7567-4451; Watts, Duncan/0000-0002-5437-6121 FU National Science Foundation [0959349, 1429236]; NASA ROSES/APRA program; NASA Space Technology Research Fellowship [NNX14AM49H]; Maryland Space Grant Consortium FX Support for CLASS has been provided by the National Science Foundation through Grant Numbers 0959349 and 1429236. The NASA ROSES/APRA program has provided funding for the development of the detectors. K. Harrington was supported by a NASA Space Technology Research Fellowship (NNX14AM49H). D Watts is funded by the Maryland Space Grant Consortium. NR 18 TC 0 Z9 0 U1 0 U2 4 PU SPRINGER/PLENUM PUBLISHERS PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0022-2291 EI 1573-7357 J9 J LOW TEMP PHYS JI J. Low Temp. Phys. PD AUG PY 2016 VL 184 IS 3-4 BP 759 EP 764 DI 10.1007/s10909-015-1368-9 PG 6 WC Physics, Applied; Physics, Condensed Matter SC Physics GA DQ2HF UT WOS:000379022700036 ER PT J AU Wu, WLK Ade, PAR Ahmed, Z Alexander, KD Amiri, M Barkats, D Benton, SJ Bischoff, CA Bock, JJ Bowens-Rubin, R Buder, I Bullock, E Buza, V Connors, JA Filippini, JP Fliescher, S Grayson, JA Halpern, M Harrison, SA Hilton, GC Hristov, VV Hui, H Irwin, KD Kang, J Karkare, KS Karpel, E Kefeli, S Kernasovskiy, SA Kovac, JM Kuo, CL Megerian, KG Netterfield, CB Nguyen, HT O'Brient, R Ogburn, RW Pryke, C Reintsema, CD Richter, S Sorensen, C Staniszewski, ZK Steinbach, B Sudiwala, RV Teply, GP Thompson, KL Tolan, JE Tucker, CE Turner, AD Vieregg, AG Weber, AC Wiebe, DV Willmert, J Yoon, KW AF Wu, W. L. K. Ade, P. A. R. Ahmed, Z. Alexander, K. D. Amiri, M. Barkats, D. Benton, S. J. Bischoff, C. A. Bock, J. J. Bowens-Rubin, R. Buder, I. Bullock, E. Buza, V. Connors, J. A. Filippini, J. P. Fliescher, S. Grayson, J. A. Halpern, M. Harrison, S. A. Hilton, G. C. Hristov, V. V. Hui, H. Irwin, K. D. Kang, J. Karkare, K. S. Karpel, E. Kefeli, S. Kernasovskiy, S. A. Kovac, J. M. Kuo, C. L. Megerian, K. G. Netterfield, C. B. Nguyen, H. T. O'Brient, R. Ogburn, R. W. Pryke, C. Reintsema, C. D. Richter, S. Sorensen, C. Staniszewski, Z. K. Steinbach, B. Sudiwala, R. V. Teply, G. P. Thompson, K. L. Tolan, J. E. Tucker, C. E. Turner, A. D. Vieregg, A. G. Weber, A. C. Wiebe, D. V. Willmert, J. Yoon, K. W. TI Initial Performance of Bicep3: A Degree Angular Scale 95 GHz Band Polarimeter SO JOURNAL OF LOW TEMPERATURE PHYSICS LA English DT Article DE Cosmic microwave background; Primordial gravitational waves; Inflation; Instrumentation: polarimetry; Telescopes AB Bicep3 is a 550-mm aperture telescope with cold, on-axis, refractive optics designed to observe at the 95-GHz band from the South Pole. It is the newest member of the Bicep/Keck family of inflationary probes specifically designed to measure the polarization of the cosmic microwave background (CMB) at degree angular scales. Bicep3 is designed to house 1280 dual-polarization pixels, which, when fully populated, totals to 9 the number of pixels in a single Keck 95-GHz receiver, thus further advancing the Bicep/Keck program's 95 GHz mapping speed. Bicep3 was deployed during the austral summer of 2014-2015 with nine detector tiles, to be increased to its full capacity of 20 in the second season. After instrument characterization, measurements were taken, and CMB observation commenced in April 2015. Together with multi-frequency observation data from Planck, Bicep2, and the Keck Array, Bicep3 is projected to set upper limits on the tensor-to-scalar ratio to at 95 % C.L. C1 [Wu, W. L. K.; Ahmed, Z.; Grayson, J. A.; Irwin, K. D.; Kang, J.; Karpel, E.; Kernasovskiy, S. A.; Kuo, C. L.; Ogburn, R. W.; Thompson, K. L.; Tolan, J. E.; Yoon, K. W.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA. [Wu, W. L. K.; Ahmed, Z.; Grayson, J. A.; Irwin, K. D.; Kang, J.; Karpel, E.; Kernasovskiy, S. A.; Kuo, C. L.; Ogburn, R. W.; Thompson, K. L.; Tolan, J. E.; Yoon, K. W.] Kavli Inst Particle Astrophys & Cosmol, SLAC Natl Accelerator Lab, Menlo Pk, CA 94025 USA. [Ade, P. A. R.; Sudiwala, R. V.; Tucker, C. E.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Alexander, K. D.; Barkats, D.; Bischoff, C. A.; Bowens-Rubin, R.; Buder, I.; Buza, V.; Connors, J. A.; Harrison, S. A.; Karkare, K. S.; Kovac, J. M.; Richter, S.; Sorensen, C.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Amiri, M.; Halpern, M.] Univ Toronto, Dept Phys, Toronto, ON, Canada. [Benton, S. J.; Netterfield, C. B.; Wiebe, D. V.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC, Canada. [Bock, J. J.; Hristov, V. V.; Hui, H.; Kefeli, S.; O'Brient, R.; Staniszewski, Z. K.; Steinbach, B.; Teply, G. P.] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA. [Bock, J. J.; Megerian, K. G.; Nguyen, H. T.; O'Brient, R.; Staniszewski, Z. K.; Turner, A. D.; Weber, A. C.] Jet Prop Lab, Pasadena, CA 91109 USA. [Bullock, E.; Fliescher, S.; Pryke, C.; Willmert, J.] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA. [Filippini, J. P.] Univ Illinois, Dept Phys, Urbana, IL 61820 USA. [Hilton, G. C.; Reintsema, C. D.] NIST, Boulder, CO 80305 USA. [Vieregg, A. G.] Univ Chicago, Enrico Fermi Inst, Dept Phys, Chicago, IL 60637 USA. RP Wu, WLK (reprint author), Stanford Univ, Dept Phys, Stanford, CA 94305 USA. EM wlwu@stanford.edu OI Barkats, Denis/0000-0002-8971-1954 FU National Science Foundation [1313158, 1313010, 1313062, 1313287, 1056465, 0960243]; SLAC Laboratory Directed Research and Development Fund; Canada Foundation for Innovation, Science and Technology Facilities Council Consolidated Grant [ST/K000926/1]; British Columbia Development Fund; JPL Research and Technology Development Fund; NASA APRA program [06-ARPA206-0040, 10-SAT10-0017, 12-SAT12-0031]; NASA SAT program [06-ARPA206-0040, 10-SAT10-0017, 12-SAT12-0031] FX This work is supported by the National Science Foundation (Grant Nos. 1313158, 1313010, 1313062, 1313287, 1056465, 0960243), the SLAC Laboratory Directed Research and Development Fund, the Canada Foundation for Innovation, Science and Technology Facilities Council Consolidated Grant (ST/K000926/1), and the British Columbia Development Fund. The development of detector technology was supported by the JPL Research and Technology Development Fund and Grants 06-ARPA206-0040, 10-SAT10-0017, and 12-SAT12-0031 from the NASA APRA and SAT programs. The development and testing of detector modules were supported by the Gordon and Betty Moore Foundation. NR 12 TC 1 Z9 1 U1 4 U2 5 PU SPRINGER/PLENUM PUBLISHERS PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0022-2291 EI 1573-7357 J9 J LOW TEMP PHYS JI J. Low Temp. Phys. PD AUG PY 2016 VL 184 IS 3-4 BP 765 EP 771 DI 10.1007/s10909-015-1403-x PG 7 WC Physics, Applied; Physics, Condensed Matter SC Physics GA DQ2HF UT WOS:000379022700037 ER PT J AU Henderson, SW Allison, R Austermann, J Baildon, T Battaglia, N Beall, JA Becker, D De Bernardis, F Bond, JR Calabrese, E Choi, SK Coughlin, KP Crowley, KT Datta, R Devlin, MJ Duff, SM Dunkley, J Dunner, R van Engelen, A Gallardo, PA Grace, E Hasselfield, M Hills, F Hilton, GC Hincks, AD Hlozek, R Ho, SP Hubmayr, J Huffenberger, K Hughes, JP Irwin, KD Koopman, BJ Kosowsky, AB Li, D McMahon, J Munson, C Nati, F Newburgh, L Niemack, M Niraula, P Page, LA Pappas, CG Salatino, M Schillaci, A Schmitt, BL Sehgal, N Sherwin, BD Sievers, JL Simon, SM Spergel, DN Staggs, ST Stevens, JR Thornton, R Van Lanen, J Vavagiakis, EM Ward, JT Wollack, EJ AF Henderson, S. W. Allison, R. Austermann, J. Baildon, T. Battaglia, N. Beall, J. A. Becker, D. De Bernardis, F. Bond, J. R. Calabrese, E. Choi, S. K. Coughlin, K. P. Crowley, K. T. Datta, R. Devlin, M. J. Duff, S. M. Dunkley, J. Dunner, R. van Engelen, A. Gallardo, P. A. Grace, E. Hasselfield, M. Hills, F. Hilton, G. C. Hincks, A. D. Hlozek, R. Ho, S. P. Hubmayr, J. Huffenberger, K. Hughes, J. P. Irwin, K. D. Koopman, B. J. Kosowsky, A. B. Li, D. McMahon, J. Munson, C. Nati, F. Newburgh, L. Niemack, M. D. Niraula, P. Page, L. A. Pappas, C. G. Salatino, M. Schillaci, A. Schmitt, B. L. Sehgal, N. Sherwin, B. D. Sievers, J. L. Simon, S. M. Spergel, D. N. Staggs, S. T. Stevens, J. R. Thornton, R. Van Lanen, J. Vavagiakis, E. M. Ward, J. T. Wollack, E. J. TI Advanced ACTPol Cryogenic Detector Arrays and Readout SO JOURNAL OF LOW TEMPERATURE PHYSICS LA English DT Article DE Bolometers; Cosmic microwave background; Millimeter-wave; Polarimetry; Superconducting detectors; Transition edge sensors ID TELESCOPE; COSMOLOGY; MILLIMETER; CAMERA AB Advanced ACTPol is a polarization-sensitive upgrade for the 6 m aperture Atacama Cosmology Telescope, adding new frequencies and increasing sensitivity over the previous ACTPol receiver. In 2016, Advanced ACTPol will begin to map approximately half the sky in five frequency bands (28-230 GHz). Its maps of primary and secondary cosmic microwave background anisotropies-imaged in intensity and polarization at few arcminute-scale resolution-will enable precision cosmological constraints and also a wide array of cross-correlation science that probes the expansion history of the universe and the growth of structure via gravitational collapse. To accomplish these scientific goals, the Advanced ACTPol receiver will be a significant upgrade to the ACTPol receiver, including four new multichroic arrays of cryogenic, feedhorn-coupled AlMn transition edge sensor polarimeters (fabricated on 150 mm diameter wafers); a system of continuously rotating meta-material silicon half-wave plates; and a new multiplexing readout architecture which uses superconducting quantum interference devices and time division to achieve a 64-row multiplexing factor. Here we present the status and scientific goals of the Advanced ACTPol instrument, emphasizing the design and implementation of the Advanced ACTPol cryogenic detector arrays. C1 [Henderson, S. W.; De Bernardis, F.; Gallardo, P. A.; Koopman, B. J.; Niemack, M. D.; Stevens, J. R.; Vavagiakis, E. M.] Cornell Univ, Dept Phys, Keble Rd, Ithaca, NY 14853 USA. [Allison, R.; Dunkley, J.] Univ Oxford, Subdept Astrophys, Keble Rd, Oxford OX1 3RH, England. [Austermann, J.; Beall, J. A.; Becker, D.; Duff, S. M.; Hilton, G. C.; Hubmayr, J.; Li, D.; Van Lanen, J.] NIST, Quantum Devices Grp, 325 Broadway Mailcode 817-03, Boulder, CO 80305 USA. [Baildon, T.; Coughlin, K. P.; Datta, R.; Hills, F.; McMahon, J.; Munson, C.] Univ Michigan, Dept Phys, Ann Arbor, MI 48103 USA. [Battaglia, N.; Calabrese, E.; Hasselfield, M.; Hlozek, R.; Spergel, D. N.] Princeton Univ, Dept Astrophys Sci, Peyton Hall, Princeton, NJ 08544 USA. [Bond, J. R.; van Engelen, A.] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada. [Choi, S. K.; Crowley, K. T.; Grace, E.; Ho, S. P.; Niraula, P.; Page, L. A.; Pappas, C. G.; Salatino, M.; Schillaci, A.; Simon, S. M.; Staggs, S. T.] Princeton Univ, Joseph Henry Labs Phys, Jadwin Hall, Princeton, NJ 08544 USA. [Devlin, M. J.; Nati, F.; Schmitt, B. L.; Ward, J. T.] Univ Penn, Dept Phys & Astron, 209 South 33rd St, Philadelphia, PA 19104 USA. [Dunner, R.] Ponticia Univ Catolica, Dept Astron & Astrofis, Casilla 306, Santiago 22, Chile. [Hincks, A. D.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z4, Canada. [Huffenberger, K.] Florida State Univ, Dept Phys, Tallahassee, FL 32306 USA. [Hughes, J. P.] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. [Irwin, K. D.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA. [Kosowsky, A. B.] Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA. [Li, D.] SLAC Natl Accelerator Lab, 2575 Sandy Hill Rd, Menlo Pk, CA 94025 USA. [Newburgh, L.] Univ Toronto, Dunlap Inst, 50 St George St, Toronto, ON M5S 3H4, Canada. [Sehgal, N.] SUNY Stony Brook, Dept Phys & Astron, Stony Brook, NY 11794 USA. [Sherwin, B. D.] Univ Calif Berkeley, Berkeley Ctr Cosmol Phys, Berkeley, CA 94720 USA. [Sievers, J. L.] Univ KwaZulu Natal, Astrophys & Cosmol Res Unit, Sch Math Stat & Comp Sci, ZA-4041 Durban, South Africa. [Thornton, R.] West Chester Univ Penns, Dept Phys, W Chester, PA 19383 USA. [Wollack, E. J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Schillaci, A.] Soc Radiosky Asesorias Ingn Ltd, Lincoyan 54, Concepcion, Chile. RP Henderson, SW (reprint author), Cornell Univ, Dept Phys, Keble Rd, Ithaca, NY 14853 USA. EM swh76@cornell.edu RI Wollack, Edward/D-4467-2012; Nati, Federico/I-4469-2016; OI Wollack, Edward/0000-0002-7567-4451; Nati, Federico/0000-0002-8307-5088; Huffenberger, Kevin/0000-0001-7109-0099 FU U.S. National Science Foundation [1312380, 1440226]; NIST Quantum Initiative; NASA [NNX13AE56G, NNX14AB58G]; NASA Space Technology Research Fellowship awards FX This work was supported by the U.S. National Science Foundation through Awards 1312380 and 1440226. The NIST authors would like to acknowledge the support of the NIST Quantum Initiative. The development of multichroic detectors and lenses was supported by NASA Grants NNX13AE56G and NNX14AB58G. The work of KPC, KTC, EG, BJK, CM, BLS, JTW, and SMS was supported by NASA Space Technology Research Fellowship awards. NR 37 TC 14 Z9 14 U1 2 U2 7 PU SPRINGER/PLENUM PUBLISHERS PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0022-2291 EI 1573-7357 J9 J LOW TEMP PHYS JI J. Low Temp. Phys. PD AUG PY 2016 VL 184 IS 3-4 BP 772 EP 779 DI 10.1007/s10909-016-1575-z PG 8 WC Physics, Applied; Physics, Condensed Matter SC Physics GA DQ2HF UT WOS:000379022700038 ER PT J AU Suzuki, A Ade, P Akiba, Y Aleman, C Arnold, K Baccigalupi, C Barch, B Barron, D Bender, A Boettger, D Borrill, J Chapman, S Chinone, Y Cukierman, A Dobbs, M Ducout, A Dunner, R Elleflot, T Errard, J Fabbian, G Feeney, S Feng, C Fujino, T Fuller, G Gilbert, A Goeckner-Wald, N Groh, J Haan, T Hall, G Halverson, N Hamada, T Hasegawa, M Hattori, K Hazumi, M Hill, C Holzapfel, W Hori, Y Howe, L Inoue, Y Irie, F Jaehnig, G Jaffe, A Jeong, O Katayama, N Kaufman, J Kazemzadeh, K Keating, B Kermish, Z Keskitalo, R Kisner, T Kusaka, A Jeune, M Lee, A Leon, D Linder, E Lowry, L Matsuda, F Matsumura, T Miller, N Mizukami, K Montgomery, J Navaroli, M Nishino, H Peloton, J Poletti, D Puglisi, G Rebeiz, G Raum, C Reichardt, C Richards, P Ross, C Rotermund, K Segawa, Y Sherwin, B Shirley, I Siritanasak, P Stebor, N Stompor, R Suzuki, J Tajima, O Takada, S Takakura, S Takatori, S Tikhomirov, A Tomaru, T Westbrook, B Whitehorn, N Yamashita, T Zahn, A Zahn, O AF Suzuki, A. Ade, P. Akiba, Y. Aleman, C. Arnold, K. Baccigalupi, C. Barch, B. Barron, D. Bender, A. Boettger, D. Borrill, J. Chapman, S. Chinone, Y. Cukierman, A. Dobbs, M. Ducout, A. Dunner, R. Elleflot, T. Errard, J. Fabbian, G. Feeney, S. Feng, C. Fujino, T. Fuller, G. Gilbert, A. Goeckner-Wald, N. Groh, J. Haan, T. De Hall, G. Halverson, N. Hamada, T. Hasegawa, M. Hattori, K. Hazumi, M. Hill, C. Holzapfel, W. Hori, Y. Howe, L. Inoue, Y. Irie, F. Jaehnig, G. Jaffe, A. Jeong, O. Katayama, N. Kaufman, J. Kazemzadeh, K. Keating, B. Kermish, Z. Keskitalo, R. Kisner, T. Kusaka, A. Jeune, M. Le Lee, A. Leon, D. Linder, E. Lowry, L. Matsuda, F. Matsumura, T. Miller, N. Mizukami, K. Montgomery, J. Navaroli, M. Nishino, H. Peloton, J. Poletti, D. Puglisi, G. Rebeiz, G. Raum, C. Reichardt, C. Richards, P. Ross, C. Rotermund, K. Segawa, Y. Sherwin, B. Shirley, I. Siritanasak, P. Stebor, N. Stompor, R. Suzuki, J. Tajima, O. Takada, S. Takakura, S. Takatori, S. Tikhomirov, A. Tomaru, T. Westbrook, B. Whitehorn, N. Yamashita, T. Zahn, A. Zahn, O. TI The POLARBEAR-2 and the Simons Array Experiments SO JOURNAL OF LOW TEMPERATURE PHYSICS LA English DT Article DE Cosmic microwave background; Inflation; Gravitational weak lensing; Polarization; B-mode ID B-MODE POLARIZATION; SCALES AB We present an overview of the design and status of the Polarbear-2 and the Simons Array experiments. Polarbear-2 is a cosmic microwave background polarimetry experiment which aims to characterize the arc-minute angular scale B-mode signal from weak gravitational lensing and search for the degree angular scale B-mode signal from inflationary gravitational waves. The receiver has a 365 mm diameter focal plane cooled to 270 mK. The focal plane is filled with 7588 dichroic lenslet-antenna-coupled polarization sensitive transition edge sensor (TES) bolometric pixels that are sensitive to 95 and 150 GHz bands simultaneously. The TES bolometers are read-out by SQUIDs with 40 channel frequency domain multiplexing. Refractive optical elements are made with high-purity alumina to achieve high optical throughput. The receiver is designed to achieve noise equivalent temperature of 5.8 K in each frequency band. Polarbear-2 will deploy in 2016 in the Atacama desert in Chile. The Simons Array is a project to further increase sensitivity by deploying three Polarbear-2 type receivers. The Simons Array will cover 95, 150, and 220 GHz frequency bands for foreground control. The Simons Array will be able to constrain tensor-to-scalar ratio and sum of neutrino masses to at and to 40 meV. C1 [Barch, B.; Barron, D.; Chinone, Y.; Cukierman, A.; Goeckner-Wald, N.; Groh, J.; Haan, T. De; Hall, G.; Hill, C.; Holzapfel, W.; Hori, Y.; Jeong, O.; Lee, A.; Raum, C.; Richards, P.; Shirley, I.; Westbrook, B.; Whitehorn, N.; Zahn, O.] Univ Calif, Dept Phys, Berkeley, CA 94720 USA. [Suzuki, A.] Univ Calif, Radio Astron Lab, Berkeley, CA 94720 USA. [Fujino, T.; Irie, F.; Katayama, N.; Mizukami, K.; Yamashita, T.] Univ Tokyo, Kavli IPMU WPI, UTIAS, Chiba 2778583, Japan. [Ade, P.] Cardiff Univ, Sch Phys & Astron, Cardiff CF10 3XQ, Wales. [Hamada, T.; Hasegawa, M.; Hattori, K.; Nishino, H.; Segawa, Y.; Suzuki, J.; Tajima, O.; Takatori, S.; Tomaru, T.] High Energy Accelerator Res Org KEK, Tsukuba, Ibaraki 3050801, Japan. [Aleman, C.; Elleflot, T.; Fuller, G.; Howe, L.; Kaufman, J.; Kazemzadeh, K.; Keating, B.; Leon, D.; Lowry, L.; Matsuda, F.; Navaroli, M.; Siritanasak, P.; Stebor, N.; Zahn, A.] Univ Calif, Dept Phys, San Diego, CA 92093 USA. [Baccigalupi, C.; Fabbian, G.; Puglisi, G.] Int Sch Adv Studies SISSA, I-34136 Trieste, Italy. [Bender, A.] Argonne Natl Lab, Argonne, IL 60439 USA. [Borrill, J.; Keskitalo, R.; Kisner, T.] Lawrence Berkeley Natl Lab, Computat Cosmol Ctr, Berkeley, CA 94720 USA. [Chapman, S.; Ross, C.; Rotermund, K.; Tikhomirov, A.] Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS B3H 4R2, Canada. [Dobbs, M.; Gilbert, A.; Montgomery, J.] McGill Univ, Dept Phys, Montreal, PQ H3A 0G4, Canada. [Ducout, A.; Feeney, S.; Jaffe, A.] Imperial Coll London, Dept Phys, Blackett Lab, London SW7 2AZ, England. [Boettger, D.; Dunner, R.] Pontif Univ Catol, Dept Astron, Santiago, Chile. [Feng, C.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. [Halverson, N.; Jaehnig, G.] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA. [Kermish, Z.] Princeton Univ, Dept Phys, Princeton, NJ 08544 USA. [Kusaka, A.; Linder, E.; Sherwin, B.] Lawrence Berkeley Natl Lab, Div Phys, Berkeley, CA 94720 USA. [Jeune, M. Le; Peloton, J.; Poletti, D.; Stompor, R.] Univ Paris Diderot, AstroParticule & Cosmol, CEA Irfu, Obs Paris, Paris, France. [Matsumura, T.] Inst Space & Astronaut Studies ISAS, Tokyo, Japan. [Miller, N.] NASA Goddard Space Flight Ctr, Observat Cosmol Lab, Code 665, Greenbelt, MD 20771 USA. [Rebeiz, G.] Univ Calif, Dept Elect & Comp Engn, San Diego, CA 92093 USA. [Reichardt, C.] Univ Melbourne, Sch Phys, Parkville, Vic 3010, Australia. [Takada, S.] Natl Inst Fusion Sci, Toki, Gifu, Japan. [Akiba, Y.; Hazumi, M.; Inoue, Y.] SOKENDAI Kamiyamaguchi, Hayama, Miura, Kanagawa 2400115, Japan. [Arnold, K.] Univ Wisconsin, Dept Phys, Madison, WI 53706 USA. [Takakura, S.] Osaka Univ, Dept Phys, Osaka, Japan. [Errard, J.] Inst Lagrange Paris ILP, Univ Sorbonne, F-75014 Paris, France. EM asuzuki@berkeley.edu OI Fabbian, Giulio/0000-0002-3255-4695; Reichardt, Christian/0000-0003-2226-9169 FU MEXT Kahenhi [21111002]; NSF [AST-0618398]; NASA [NNG06GJ08G]; Simons Foundation; Natural Sciences and Engineering Research Council; Canadian Institute for Advanced Research; Japan Society for the Promotion of Science; CONICYT FX We acknowledge the support from the MEXT Kahenhi Grant 21111002, NSF Grant AST-0618398, NASA Grant NNG06GJ08G, The Simons Foundation, Natural Sciences and Engineering Research Council, Canadian Institute for Advanced Research, and Japan Society for the Promotion of Science, and the CONICYT provided invaluable funding and support. Detectors were fabricated at the Berkeley Marvell Nanofabrication laboratory. NR 22 TC 7 Z9 7 U1 7 U2 12 PU SPRINGER/PLENUM PUBLISHERS PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0022-2291 EI 1573-7357 J9 J LOW TEMP PHYS JI J. Low Temp. Phys. PD AUG PY 2016 VL 184 IS 3-4 BP 805 EP 810 DI 10.1007/s10909-015-1425-4 PG 6 WC Physics, Applied; Physics, Condensed Matter SC Physics GA DQ2HF UT WOS:000379022700043 ER PT J AU Staguhn, JG Benford, DJ Dowell, CD Fixsen, DJ Hilton, GC Irwin, KD Jhabvala, CA Maher, SF Miller, TM Moseley, SH Sharp, EH Runyan, MC Wollack, EJ AF Staguhn, J. G. Benford, D. J. Dowell, C. D. Fixsen, D. J. Hilton, G. C. Irwin, K. D. Jhabvala, C. A. Maher, S. F. Miller, T. M. Moseley, S. H. Sharp, E. H. Runyan, M. C. Wollack, E. J. TI Performance of Backshort-Under-Grid Kilopixel TES Arrays for HAWC SO JOURNAL OF LOW TEMPERATURE PHYSICS LA English DT Article DE Transition edge sensor; Backshort-Under-Grid; Bolometer; HAWC; Far-infrared astronomy; Polarimetry AB We present results from laboratory detector characterizations of the first kilopixel BUG arrays for the High- resolution Wideband Camera Plus (HAWC+) which is the imaging far-infrared polarimeter camera for the Stratospheric Observatory for Infrared Astronomy (SOFIA). Our tests demonstrate that the array performance is consistent with the predicted properties. Here, we highlight results obtained for the thermal conductivity, noise performance, detector speed, and first optical results demonstrating the pixel yield of the arrays. C1 [Staguhn, J. G.] Johns Hopkins Univ, 3400 N Charles St, Baltimore, MD 21218 USA. [Staguhn, J. G.; Benford, D. J.; Fixsen, D. J.; Jhabvala, C. A.; Maher, S. F.; Miller, T. M.; Moseley, S. H.; Sharp, E. H.; Wollack, E. J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Dowell, C. D.; Runyan, M. C.] Jet Prop Lab, Pasadena, CA 91109 USA. [Hilton, G. C.] NIST, Boulder, CO 80305 USA. [Irwin, K. D.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA. [Maher, S. F.] Sci Syst & Applicat Inc, Greenbelt, MD 20770 USA. [Sharp, E. H.] Global Sci & Technol Inc, Greenbelt, MD 20770 USA. RP Staguhn, JG (reprint author), Johns Hopkins Univ, 3400 N Charles St, Baltimore, MD 21218 USA. EM johannes.staguhn@nasa.gov RI Wollack, Edward/D-4467-2012; Benford, Dominic/D-4760-2012 OI Wollack, Edward/0000-0002-7567-4451; Benford, Dominic/0000-0002-9884-4206 NR 3 TC 0 Z9 0 U1 2 U2 3 PU SPRINGER/PLENUM PUBLISHERS PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0022-2291 EI 1573-7357 J9 J LOW TEMP PHYS JI J. Low Temp. Phys. PD AUG PY 2016 VL 184 IS 3-4 BP 811 EP 815 DI 10.1007/s10909-016-1509-9 PG 5 WC Physics, Applied; Physics, Condensed Matter SC Physics GA DQ2HF UT WOS:000379022700044 ER PT J AU Faverzani, M Alpert, B Backer, D Bennet, D Biasotti, M Brofferio, C Ceriale, V Ceruti, G Corsini, D Day, PK De Gerone, M Dressler, R Ferri, E Fowler, J Fumagalli, E Gard, J Gatti, F Giachero, A Hays-Wehle, J Heinitz, S Hilton, G Koster, U Lusignoli, M Maino, M Mates, J Nisi, S Nizzolo, R Nucciotti, A Orlando, A Parodi, L Pessina, G Pizzigoni, G Puiu, A Ragazzi, S Reintsema, C Ribeiro-Gomez, M Schmidt, D Schuman, D Siccardi, F Sisti, M Swetz, D Terranova, F Ullom, J Vale, L AF Faverzani, M. Alpert, B. Backer, D. Bennet, D. Biasotti, M. Brofferio, C. Ceriale, V. Ceruti, G. Corsini, D. Day, P. K. De Gerone, M. Dressler, R. Ferri, E. Fowler, J. Fumagalli, E. Gard, J. Gatti, F. Giachero, A. Hays-Wehle, J. Heinitz, S. Hilton, G. Koster, U. Lusignoli, M. Maino, M. Mates, J. Nisi, S. Nizzolo, R. Nucciotti, A. Orlando, A. Parodi, L. Pessina, G. Pizzigoni, G. Puiu, A. Ragazzi, S. Reintsema, C. Ribeiro-Gomez, M. Schmidt, D. Schuman, D. Siccardi, F. Sisti, M. Swetz, D. Terranova, F. Ullom, J. Vale, L. TI The HOLMES Experiment SO JOURNAL OF LOW TEMPERATURE PHYSICS LA English DT Article DE Neutrino mass measurement; Electron capture; Holmium; Transition edge sensors ID ELECTRON NEUTRINO MASS; CAPTURE; HO-163 AB The determination of the neutrino mass is an open issue in modern particle physics and astrophysics. The direct mass measurement is the only theory-unrelated experimental tool capable to probe such quantity. The HOLMES experiment will measure the end-point energy of the electron capture decay of Ho, aiming at a statistical sensitivity on the neutrino mass around 1 eV/c. In order to acquire the large needed statistics by keeping the pile-up contribution as low as possible, 1000 transition edge sensors will be readout simultaneously with the frequency domain readout, a multiplexing technique where the multiplex factor is only limited by the bandwidth of the available commercial fast digitizers. We outline here the HOLMES project with its technical challenges, and its status and perspectives. C1 [Alpert, B.; Backer, D.; Bennet, D.; Fowler, J.; Gard, J.; Hays-Wehle, J.; Hilton, G.; Mates, J.; Reintsema, C.; Schmidt, D.; Schuman, D.; Swetz, D.; Ullom, J.; Vale, L.] NIST, Boulder, CO USA. [Biasotti, M.; Ceriale, V.; Corsini, D.; De Gerone, M.; Fumagalli, E.; Gatti, F.; Orlando, A.; Parodi, L.; Pizzigoni, G.; Siccardi, F.] Univ Genoa, Dipartimento Fis, Genoa, Italy. [Biasotti, M.; Ceriale, V.; Corsini, D.; De Gerone, M.; Fumagalli, E.; Gatti, F.; Orlando, A.; Parodi, L.; Pizzigoni, G.; Siccardi, F.] Ist Nazl Fis Nuc, Sez Genova, Genoa, Italy. [Faverzani, M.; Brofferio, C.; Ferri, E.; Nizzolo, R.; Nucciotti, A.; Puiu, A.; Ragazzi, S.; Sisti, M.; Terranova, F.] Univ Milano Bicocca, Dipartimento Fis, Milan, Italy. [Faverzani, M.; Brofferio, C.; Ceruti, G.; Ferri, E.; Giachero, A.; Maino, M.; Nizzolo, R.; Nucciotti, A.; Pessina, G.; Puiu, A.; Ragazzi, S.; Sisti, M.; Terranova, F.] Ist Nazl Fis Nucl, Sez Milano Bicocca, Milan, Italy. [Day, P. K.] Jet Prop Lab, Pasadena, CA USA. [Dressler, R.; Heinitz, S.] Paul Scherrer Inst, Villigen, Switzerland. [Koster, U.] Inst Laue Langeving, Grenoble, France. [Lusignoli, M.] Ist Nazl Fis Nucl, Sez Roma 1, Rome, Italy. [Nisi, S.] INFN, Lab Nazl Gran Sasso, Assergi, AQ, Italy. [Ribeiro-Gomez, M.] Univ Lisbon, Multidisciplinary Ctr Astrophys CENTRA IST, Lisbon, Portugal. RP Nucciotti, A (reprint author), Univ Milano Bicocca, Dipartimento Fis, Milan, Italy.; Nucciotti, A (reprint author), Ist Nazl Fis Nucl, Sez Milano Bicocca, Milan, Italy. EM angelo.nucciotti@mib.infn.it RI Ferri, Elena/L-8531-2014; Biasotti, Michele/C-7890-2017; Giachero, Andrea/I-1081-2013; OI Ferri, Elena/0000-0003-1425-3669; Biasotti, Michele/0000-0002-7241-8479; Giachero, Andrea/0000-0003-0493-695X; De Gerone, Matteo/0000-0002-5489-6581; Pessina, Gianluigi Ezio/0000-0003-3700-9757 FU European Research Council under the European Union/ERC [340321]; INFN; Fundacao para a Ciencia e a Tecnologia [PTDC/FIS/116719/2010] FX The HOLMES experiment is funded by the European Research Council under the European Union Seventh Framework Programme (FP7/2007-2013)/ERC Grant Agreement no. 340321. We also acknowledge support from INFN for the MARE project, from the NIST Innovations in Measurement Science program for the TES detector development, and from Fundacao para a Ciencia e a Tecnologia (PTDC/FIS/116719/2010) for providing the enriched Er2O3 used in preliminary 163Ho production by means of neutron irradiation. NR 15 TC 1 Z9 1 U1 0 U2 3 PU SPRINGER/PLENUM PUBLISHERS PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0022-2291 EI 1573-7357 J9 J LOW TEMP PHYS JI J. Low Temp. Phys. PD AUG PY 2016 VL 184 IS 3-4 BP 922 EP 929 DI 10.1007/s10909-016-1540-x PG 8 WC Physics, Applied; Physics, Condensed Matter SC Physics GA DQ2HF UT WOS:000379022700060 ER PT J AU Simon, JI Matzel, JEP Simon, SB Hutcheon, ID Ross, DK Weber, PK Grossman, L AF Simon, Justin I. Matzel, Jennifer E. P. Simon, Steven B. Hutcheon, Ian D. Ross, D. Kent Weber, Peter K. Grossman, Lawrence TI Oxygen isotopic variations in the outer margins and Wark-Lovering rims of refractory inclusions SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Article DE Oxygen isotopes; CAIs; Wark-Lovering rims; NanoSIMS; Protoplanetary disk ID AL-RICH INCLUSIONS; EARLY SOLAR-SYSTEM; COARSE-GRAINED CA; CARBONACEOUS CHONDRITES; PROTOPLANETARY DISK; ALLENDE METEORITE; CV3 CHONDRITES; INITIAL AL-26/AL-27; SELF-DIFFUSION; NEBULA GAS AB Oxygen isotopic variations across the outer margins and Wark-Lovering (WL) rims of a diverse suite of six coarse-grained Types A and B refractory inclusions from both oxidized and reduced CV3 chondrites suggest that CAIs originated from a O-16-rich protosolar gas reservoir and were later exposed to both relatively O-17,O-18-rich and O-16-rich reservoirs. The O-isotope profiles of CAIs can be explained by changes in the composition of gas near the protoSun or the migration of CAIs through a heterogeneous nebula. Variability within the inclusion interiors appears to have been set prior to WL rim growth. Modeling the isotopic zoning profiles as diffusion gradients between inclusion interiors and edges establishes a range of permissible time-temperature combinations for their exposure in the nebula. At mean temperatures of 1400 K, models that match the isotope gradients in the inclusions yield timescales ranging from 5 x 10(3) to 3 x 10(5) years. Assuming CAIs originated with a relatively O-16-rich (protosolar) isotopic composition, differences among the melilite interiors and the isotopic gradients in their margins imply the existence of a number of isotopically distinct reservoirs. Evidence at the edges of some CAIs for subsequent isotopic exchange may relate to the beginning of rim formation. In the WL rim layers surrounding the interiors, spinel is relatively O-16-rich but subtly distinct among different CAIs. Melilite is often relatively O-16-poor, but rare relatively O-16-rich grains also exist. Pyroxene generally exhibits intermediate O-isotope compositions and isotopic zoning. Olivine in both WL and accretionary rims, when present, is isotopically heterogeneous. The extreme isotopic heterogeneity among and within individual WL rim layers and in particular, the observed trends of outward O-16-enrichments, suggest that rims surrounding CAIs contained in CV3 chondrites, like the inclusions themselves, formed from a number of isotopically distinct gas reservoirs. Collectively, these results support numerical protoplanetary disk models in which CAIs were transported between several distinct nebular reservoirs multiple times prior to accretion onto a parent body. Published by Elsevier Ltd. C1 [Simon, Justin I.; Ross, D. Kent] NASA, Ctr Isotope Cosmochem & Geochronol, Astromat Res & Explorat Sci Div Explorat Integrat, Johnson Space Ctr, Houston, TX 77058 USA. [Matzel, Jennifer E. P.; Hutcheon, Ian D.; Weber, Peter K.] Lawrence Livermore Natl Lab, Livermore, CA 94451 USA. [Simon, Steven B.; Grossman, Lawrence] Univ Chicago, Dept Geophys Sci, 5734 S Ellis Ave, Chicago, IL 60637 USA. [Ross, D. Kent] Univ Texas El Paso, Jacobs Technol, Houston, TX 77058 USA. [Grossman, Lawrence] Univ Chicago, Enrico Fermi Inst, 5640 S Ellis Ave, Chicago, IL 60637 USA. RP Simon, JI (reprint author), NASA, Ctr Isotope Cosmochem & Geochronol, Astromat Res & Explorat Sci Div Explorat Integrat, Johnson Space Ctr, Houston, TX 77058 USA. EM justin.i.simon@nasa.gov FU NASA Cosmochemistry and Origins Programs [NNH11ZDA66N, NNH10AO48I, NNH10AO05I, NNX13AE73G]; U.S. Department of Energy at Lawrence Livermore National Laboratory [DE-AC52-07NA27344] FX This work is dedicated to Dr. Ian Douglass Hutcheon (1947-2015), an exceptional scientist, mentor, and friend. He made significant contributions to this work, masterfully integrating intuition, open-mindedness, and skepticism. The remaining authors and many others in our community will sorely miss him. We are grateful to Journal Editor D. Papanastassiou and three anonymous reviewers for their careful and constructive reviews of this paper. The work was supported by NASA Cosmochemistry and Origins Programs: Grants NNH11ZDA66N to JIS, NNH10AO48I and NNH10AO05I to IDH, and NNX13AE73G to LG. Repolishing of several 'well-used' samples by Roger Harrington is gratefully appreciated. This work was performed under the auspices of the U.S. Department of Energy at Lawrence Livermore National Laboratory under Contract DE-AC52-07NA27344. NR 92 TC 2 Z9 2 U1 5 U2 10 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 EI 1872-9533 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD AUG 1 PY 2016 VL 186 BP 242 EP 276 DI 10.1016/j.gca.2016.04.025 PG 35 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA DP9SF UT WOS:000378836600015 ER PT J AU Barnes, JJ Tartese, R Anand, M McCubbin, FM Neal, CR Franchi, IA AF Barnes, Jessica J. Tartese, Romain Anand, Mahesh McCubbin, Francis M. Neal, Clive R. Franchi, Ian A. TI Early degassing of lunar urKREEP by crust-breaching impact(s) SO EARTH AND PLANETARY SCIENCE LETTERS LA English DT Article DE Moon; apatite; volatiles; NanoSIMS; chlorine; magma ocean ID CHLORINE ISOTOPE COMPOSITION; FORMING GIANT IMPACT; NOBLE-GAS-ANALYSES; MAGMATIC VOLATILES; VOLCANIC GLASSES; MARE BASALTS; MG-SUITE; MOON; WATER; HYDROGEN AB Current models for the Moon's formation have yet to fully account for the thermal evolution of the Moon in the presence of H2O and other volatiles. Of particular importance is chlorine, since most lunar samples are characterised by unique heavy delta Cl-37 values, significantly deviating from those of other planetary materials, including Earth, for which delta Cl-37 values cluster around similar to 0 parts per thousand. In order to unravel the cause(s) of the Moon's unique chlorine isotope signature, we performed a comprehensive study of high-precision in situ Cl isotope measurements of apatite from a suite of Apollo samples with a range of geochemical characteristics and petrologic types. The Cl-isotopic compositions measured in lunar apatite in the studied samples display a wide range of delta Cl-37 values (reaching a maximum value of +36 parts per thousand), which are positively correlated with the amount of potassium (K), Rare Earth Element (REE) and phosphorous (P) (CREEP) component in each sample. Using these new data, integrated with existing H-isotope data obtained for the same samples, we are able to place these findings in the context of the canonical lunar magma ocean (LMO) model. The results are consistent with the urKREEP reservoir being characterised by a delta Cl-37 similar to+30%o. Such a heavy Cl isotope signature requires metal-chloride degassing from a Cl-enriched urKREEP LMO residue, a process likely to have been triggered by at least one large crust-breaching impact event that facilitated the transport and exposure of urKREEP liquid to the lunar surface. (C) 2016 The Authors. Published by Elsevier B.V. C1 [Barnes, Jessica J.; Tartese, Romain; Anand, Mahesh; Franchi, Ian A.] Open Univ, Planetary & Space Sci, Walton Hall, Milton Keynes MK7 6AA, Bucks, England. [Tartese, Romain] UPMC, Univ Paris 04, Museum Natl Hist Nat, Inst Mineral Phys Mat & Cosmochim,CNRS, F-75005 Paris, France. [Tartese, Romain] IRD, F-75005 Paris, France. [Anand, Mahesh] Nat Hist Museum, Dept Earth Sci, Cromwell Rd, London SW7 5BD, England. [McCubbin, Francis M.] NASA, Johnson Space Ctr, Mailcode X12,2101 NASA Pkwy, Houston, TX 77058 USA. [Neal, Clive R.] Univ Notre Dame, Dept Civil & Environm Engn & Earth Sci, Notre Dame, IN 46556 USA. RP Barnes, JJ (reprint author), Open Univ, Planetary & Space Sci, Walton Hall, Milton Keynes MK7 6AA, Bucks, England. EM jessica.bames@open.ac.uk OI Tartese, Romain/0000-0002-3490-9875 FU UK Science and Technology Facilities Council [ST/L000776/1]; NASA's LASER program [NNX13AK32G] FX We thank NASA CAPTEM for allocation of lunar samples (to MA and CRN). This research was supported by a grant from the UK Science and Technology Facilities Council (grant # ST/L000776/1 to M.A. and I.A.F.). FMM acknowledges support from NASA's LASER program during this study through grant NNX13AK32G. We thank Erik Hauri and Evelyn Furl for their insightful reviews which helped to improve this manuscript, and we thank the editor Bernard Marty for his handling of this manuscript. NR 59 TC 3 Z9 3 U1 6 U2 12 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0012-821X EI 1385-013X J9 EARTH PLANET SC LETT JI Earth Planet. Sci. Lett. PD AUG 1 PY 2016 VL 447 BP 84 EP 94 DI 10.1016/j.epsl.2016.04.036 PG 11 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA DP4AS UT WOS:000378438400008 ER PT J AU Daigle, MJ Bregon, A Koutsoukos, X Biswas, G Pulido, B AF Daigle, Matthew J. Bregon, Anibal Koutsoukos, Xenofon Biswas, Gautam Pulido, Belarmino TI A qualitative event-based approach to multiple fault diagnosis in continuous systems using structural model decomposition SO ENGINEERING APPLICATIONS OF ARTIFICIAL INTELLIGENCE LA English DT Article DE Fault diagnosis; Model-based diagnosis; Multiple faults; Diagnosability; Structural model decomposition; Discrete-event systems ID ANALYTICAL REDUNDANCY RELATIONS; DIAGNOSABILITY; CONFLICTS AB Multiple fault diagnosis is a difficult problem for dynamic systems, and, as a result, most multiple fault diagnosis approaches are restricted to static systems, and most dynamic system diagnosis approaches make the single fault assumption. Within the framework of consistency-based diagnosis, the challenge is to generate conflicts from dynamic signals. For multiple faults, this becomes difficult due to the possibility of fault masking and different relative times of fault occurrence, resulting in many different ways that any given combination of faults can manifest in the observations. In order to address these challenges, we develop a novel multiple fault diagnosis framework for continuous dynamic systems. We construct a qualitative event-based framework, in which discrete qualitative symbols are generated from residual signals. Within this framework, we formulate an online diagnosis approach and establish definitions of multiple fault diagnosability. Residual generators are constructed based on structural model decomposition, which, as we demonstrate, has the effect of reducing the impact of fault masking by decoupling faults from residuals, thus improving diagnosability and fault isolation performance. Through simulation-based multiple fault diagnosis experiments, we demonstrate and validate the concepts developed here, using a multi-tank system as a case study. Published by Elsevier Ltd. C1 [Daigle, Matthew J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Bregon, Anibal; Pulido, Belarmino] Univ Valladolid, Dept Informat, E-47011 Valladolid, Spain. [Koutsoukos, Xenofon; Biswas, Gautam] Vanderbilt Univ, Dept Elect Engn & Comp Sci, Inst Software Integrated Syst, Nashville, TN 37235 USA. RP Daigle, MJ (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM matthew.j.daigle@nasa.gov; anibal@infor.uva.es; xenofon.koutsoukos@vanderbilt.edu; gautam.biswas@vanderbilt.edu; belar@infor.uva.es OI Daigle, Matthew/0000-0002-4616-3302 FU NASA System-Wide Safety and Assurance Technologies (SSAT) project; Spanish MINECO Grant [DPI2013-45414-R] FX The author's work has been partially supported by the NASA System-Wide Safety and Assurance Technologies (SSAT) project.; The authors work has been supported by the Spanish MINECO Grant DPI2013-45414-R. NR 40 TC 1 Z9 1 U1 2 U2 4 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0952-1976 EI 1873-6769 J9 ENG APPL ARTIF INTEL JI Eng. Appl. Artif. Intell. PD AUG PY 2016 VL 53 BP 190 EP 206 DI 10.1016/j.engappai.2016.04.002 PG 17 WC Automation & Control Systems; Computer Science, Artificial Intelligence; Engineering, Multidisciplinary; Engineering, Electrical & Electronic SC Automation & Control Systems; Computer Science; Engineering GA DP0LH UT WOS:000378180800014 ER PT J AU Gwenzi, D Lefsky, MA Suchdeo, VP Harding, DJ AF Gwenzi, David Lefsky, Michael A. Suchdeo, Vijay P. Harding, David J. TI Prospects of the ICESat-2 laser altimetry mission for savanna ecosystem structural studies based on airborne simulation data SO ISPRS JOURNAL OF PHOTOGRAMMETRY AND REMOTE SENSING LA English DT Article DE Photon counting lidar; ICESat-2; MABEL; MATLAS; Savanna; Canopy height ID LIDAR; VEGETATION; FOREST AB The next planned spaceborne lidar mission is the Ice, Cloud and land Elevation Satellite 2 (ICESat-2), which will use the Advanced Topographic Laser Altimeter System (ATLAS) sensor, a photon counting technique. To pre-validate the capability of this mission for studying three dimensional vegetation structure in savannas, we assessed the potential of the measurement approach to estimate canopy height in an oak savanna landscape. We used data from the Multiple Altimeter Beam Experimental Lidar (MABEL), an airborne photon counting lidar sensor developed by NASA's Goddard Space Flight Center. ATLAS-like data was generated using the MATLAS simulator, which adjusts MABEL data's detected number of signal and noise photons to that expected from the ATLAS instrument. Transects flown over the Tejon ranch conservancy in Kern County, California, USA were used for this work. For each transect we chose to use data from the near infrared channel that had the highest number of photons. We segmented each transect into 50 m, 25 m and 14 m long blocks and aggregated the photons in each block into a histogram based on their elevation values. We then used an automated algorithm to identify cut off points where the cumulative density of photons from the highest elevation indicates the presence of the canopy top and likewise where such cumulative density from the lowest elevation indicates the mean terrain elevation. MABEL derived height metrics were moderately correlated to discrete return lidar (DRL) derived height metrics (r(2) and RMSE values ranging from 0.60 to 0.73 and 2.9 m to 4.4 m respectively) but MATLAS simulation resulted in more modest correlations with DRL indices (r(2) ranging from 0.5 to 0.64 and RMSE from 3.6 m to 4.6 m). Simulations also indicated that the expected number of signal photons from ATLAS will be substantially lower, a situation that reduces canopy height estimation precision especially in areas of low density vegetation cover. On the basis of the simulated data, there is reason to believe that the ability of ICESat-2 to estimate height in savannas will be comparable to the original ICESat mission although the respective sensors have different measurement principles. Published by Elsevier B.V. on behalf of International Society for Photogrammetry and Remote Sensing, Inc. (ISPRS). C1 [Gwenzi, David; Lefsky, Michael A.] Colorado State Univ, Dept Ecosyst Sci & Sustainabil, Nat Resource Ecol Lab, NESB 108,1499 Campus Delivery, Ft Collins, CO 80523 USA. [Suchdeo, Vijay P.; Harding, David J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Gwenzi, D (reprint author), Colorado State Univ, Dept Ecosyst Sci & Sustainabil, Nat Resource Ecol Lab, NESB 108,1499 Campus Delivery, Ft Collins, CO 80523 USA. EM dgwenzi@rams.colostate.edu RI Harding, David/F-5913-2012 FU NASA [NNH11ZDA001N-ICESAT2] FX We are grateful to NASA, Grant number NNH11ZDA001N-ICESAT2 for funding this project. Anita Brenner (Sigma Space Corporation) is thanked for providing the MABEL photons classification algorithm. We also thank the 2 anonymous reviewers whose valuable criticism of our first draft greatly improved the manuscript. NR 20 TC 1 Z9 1 U1 9 U2 18 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0924-2716 EI 1872-8235 J9 ISPRS J PHOTOGRAMM JI ISPRS-J. Photogramm. Remote Sens. PD AUG PY 2016 VL 118 BP 68 EP 82 DI 10.1016/j.isprsjprs.2016.04.009 PG 15 WC Geography, Physical; Geosciences, Multidisciplinary; Remote Sensing; Imaging Science & Photographic Technology SC Physical Geography; Geology; Remote Sensing; Imaging Science & Photographic Technology GA DP4FI UT WOS:000378451300006 ER PT J AU Patzold, M Hausler, B Tyler, GL Andert, T Asmar, SW Bird, MK Dehant, V Hinson, DP Rosenblatt, P Simpson, RA Tellmann, S Withers, P Beuthe, M Efimov, AI Hahn, M Kahan, D Le Maistre, S Oschlisniok, J Peter, K Remus, S AF Paetzold, M. Haeusler, B. Tyler, G. L. Andert, T. Asmar, S. W. Bird, M. K. Dehant, V. Hinson, D. P. Rosenblatt, P. Simpson, R. A. Tellmann, S. Withers, P. Beuthe, M. Efimov, A. I. Hahn, M. Kahan, D. Le Maistre, S. Oschlisniok, J. Peter, K. Remus, S. TI Mars Express 10 years at Mars: Observations by the Mars Express Radio Science Experiment (MaRS) SO PLANETARY AND SPACE SCIENCE LA English DT Review DE Mars Express; Mars; Atmosphere; Ionosphere; Radio science; Radio occultation ID MARTIAN DAYSIDE IONOSPHERE; CONVECTIVE BOUNDARY-LAYER; ORBITER LASER ALTIMETER; GLOBAL SURVEYOR; OCCULTATION MEASUREMENTS; BISTATIC RADAR; ATMOSPHERIC PROFILES; SOLAR CONJUNCTION; VENUS-EXPRESS; SCATTERING OBSERVATIONS AB The Mars Express spacecraft is operating in Mars orbit since early 2004. The Mars Express Radio Science Experiment (MaRS) employs the spacecraft and ground station radio systems (i) to conduct radio occultations of the atmosphere and ionosphere to obtain vertical profiles of temperature, pressure, neutral number densities and electron density, (ii) to conduct bistatic radar experiments to obtain information on the dielectric and scattering properties of the surface, (iii) to investigate the structure and variation of the crust and lithosphere in selected target areas, (iv) to determine the mass, bulk and internal structure of the moon Phobos, and (v) to track the MEX radio signals during superior solar conjunction to study the morphology of coronal mass ejections (CMEs). Here we report observations, results and discoveries made in the Mars environment between 2004 and 2014 over almost an entire solar cycle. (C) 2016 Elsevier Ltd. All rights reserved. C1 [Paetzold, M.; Bird, M. K.; Tellmann, S.; Hahn, M.; Oschlisniok, J.; Peter, K.] Univ Cologne, Abt Planetenforsch, Rhein Inst Umweltforsch, D-50931 Cologne, Germany. [Haeusler, B.; Andert, T.] Univ Bundeswehr Munchen, Inst Raumfahrttech & Weltraumnutzung, Neubiberg, Germany. [Tyler, G. L.; Hinson, D. P.; Simpson, R. A.] Stanford Univ, Dept Elect Engn, Stanford, CA 94305 USA. [Asmar, S. W.; Kahan, D.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Dehant, V.; Rosenblatt, P.; Beuthe, M.; Le Maistre, S.] Observ Royal Belgique, B-1180 Brussels, Belgium. [Withers, P.] Boston Univ, Dept Astron, 725 Commonwealth Ave, Boston, MA 02215 USA. [Efimov, A. I.] Russian Acad Sci, Kotelnikov Inst Radio Engn & Elect, Moscow 125009, Russia. [Remus, S.] ESA ESTEC, Noordwijk, Netherlands. RP Patzold, M (reprint author), Univ Cologne, Abt Planetenforsch, Rhein Inst Umweltforsch, D-50931 Cologne, Germany. EM martin.paetzold@uni-koeln.de FU Bundesministerium fur Wirtschaft BMWi, Berlin via German Space Agency DLR, Bonn [50QM1004, 50QM1401, 50QM1002]; NASA [1217744]; NASA/JPL FX The Mars Express Radio Science experiment (MaRS) is funded by the Bundesministerium fur Wirtschaft BMWi, Berlin, via the German Space Agency DLR, Bonn, under grants 50QM1004, 50QM1401 and 50QM1002 (UniBw). Support for MaRS at Stanford University is provided by NASA through JPL contract 1217744. Support for the Multimission Radio Science Support Team is provided by NASA/JPL. We thank everyone involved with the Mars Express mission at ESTEC, ESOC, ESAC, JPL and in particular at the ESTRACK and DSN ground stations. The MaRS team expresses deep appreciation for the critical support provided by the MEX SGS at ESAC during the planning and the data acquisition periods. We are deeply indebted to Padma Varanasi and Tommy Thompson, both at JPL, for their dedicated support. NR 164 TC 3 Z9 3 U1 11 U2 21 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0032-0633 J9 PLANET SPACE SCI JI Planet Space Sci. PD AUG PY 2016 VL 127 BP 44 EP 90 DI 10.1016/j.pss.2016.02.013 PG 47 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DP0MS UT WOS:000378184500004 ER PT J AU Mokhtarishirazabad, M Lopez-Crespo, P Moreno, B -Moreno, AL Zanganeh, M AF Mokhtarishirazabad, M. Lopez-Crespo, P. Moreno, B. -Moreno, A. Lopez Zanganeh, M. TI Evaluation of crack-tip fields from DIC data: A parametric study SO INTERNATIONAL JOURNAL OF FATIGUE LA English DT Article; Proceedings Paper CT 3rd International Conference on Characterisation of Crack Tip Fields CY APR 20-22, 2015 CL Urbino, ITALY SP Italian Grp Fracture DE Linear elastic fracture mechanics; Digital image correlation; Stress intensity factor; K-dominance; Crack-tip displacement field ID DIGITAL IMAGE CORRELATION; STRESS INTENSITY FACTORS; DISPLACEMENT-FIELDS; SYSTEMATIC-ERRORS; FATIGUE; CLOSURE; PATTERNS; SIZE AB In the past two decades, crack-tip mechanics has been studied increasingly using full-field techniques. Within these techniques, Digital Image Correlation (DIC) has been most widely used due to its many advantages, to extract important crack-tip information, including Stress Intensity Factor (SIF), crack opening displacement, J-integral, T-stress, closure level, plastic zone size, etc. However, little information is given in the literature about the experimental setup that provides best estimations for the different parameters. The current work aims at understanding how the experimental conditions used in DIC influence the crack-tip information extracted experimentally. The influence of parameters such as magnification factor, the position of the images with respect the crack-tip and size of the subset used in the correlation is studied. The influence is studied in terms of SIF by using Williams' model. In this regard, cyclic loading on a fatigue crack in a compact tension (CT) specimen, made of aluminium 2024-T351 alloy, has been applied and the surface deformation around the crack-tip has been examined. The comparison between nominal and experimental values of K-I showed that the effect of subset size on the measured K-I is negligible compared to the effect of the field of view and the position of the area of interest. (C) 2016 Published by Elsevier Ltd. C1 [Mokhtarishirazabad, M.; Lopez-Crespo, P.; Moreno, B.] Univ Malaga, Dept Civil & Mat Engn, C Dr Ortiz Ramos S-N, E-29071 Malaga, Spain. [-Moreno, A. Lopez] Univ Jaen, Dept Mat Sci & Met Engn, Campus Las Lagunillas, Jaen 23071, Spain. [Zanganeh, M.] NASA, Lyndon B Johnson Space Ctr, Jacobs Technol, Houston, TX 77058 USA. RP Lopez-Crespo, P (reprint author), Univ Malaga, Dept Civil & Mat Engn, C Dr Ortiz Ramos S-N, E-29071 Malaga, Spain. EM plopezcrespo@uma.es NR 49 TC 3 Z9 3 U1 12 U2 23 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0142-1123 EI 1879-3452 J9 INT J FATIGUE JI Int. J. Fatigue PD AUG PY 2016 VL 89 SI SI BP 11 EP 19 DI 10.1016/j.ijfatigue.2016.03.006 PG 9 WC Engineering, Mechanical; Materials Science, Multidisciplinary SC Engineering; Materials Science GA DO5QY UT WOS:000377839100003 ER PT J AU Pahlevan, N Sarkar, S Franz, BA AF Pahlevan, Nima Sarkar, Sudipta Franz, Bryan A. TI Uncertainties in coastal ocean color products: Impacts of spatial sampling SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE Coastal ocean color; Spatial sampling; Uncertainty; Intercomparison ID RESOLUTION IMAGING SPECTRORADIOMETER; INHERENT OPTICAL-PROPERTIES; REMOTE-SENSING REFLECTANCE; ATMOSPHERIC CORRECTION; CLIMATE-CHANGE; VICARIOUS CALIBRATION; SATELLITE DATA; BIOOPTICAL MODEL; LANDSAT 8; DATA SETS AB With increasing demands for ocean color (OC) products with improved accuracy and well characterizdd, per retrieval uncertainty budgets, it is vital to decompose overall estimated errors into their primary components. Amongst various contributing elements (e.g., instrument calibration, atmospheric correction, inversion algorithms) in the uncertainty of an OC observation, less attention has been paid to uncertainties associated with spatial sampling. In this paper, we simulate MODIS (aboard both Aqua and Terra) and VIIRS OC products using 30 m resolution OC products derived from the Operational Land Imager (OLI) aboard Landsat-8, to examine impacts of spatial sampling on both cross-sensor product intercomparisons and in-situ validations of R-rs products in coastal waters. Various OLI OC products representing different productivity levels and in-water spatial features were scanned for one full orbital-repeat cycle of each ocean color satellite. While some view-angle dependent differences in simulated Aqua-MODIS and VIIRS were observed, the average uncertainties (absolute) in product intercomparisons (due to differences in spatial sampling) at regional scales are found to be 1.8%, 1.9%, 2.4%, 4.3%, 2.7%, 1.8%, and 4% for the R-rs(443), R-rs(482), R-rs(561), R-rs(655), Chla, K-d (482), and b(bp)(655) products, respectively. It is also found that, depending on in-water spatial variability and the sensor's footprint size, the errors for an in-situ validation station in coastal areas can reach as high as +/- 18%. We conclude that a) expected biases induced by the spatial sampling in product intercomparisons are mitigated when products are averaged over at least 7 km x 7 km areas, b) VIIRS observations, with improved consistency in cross-track spatial sampling, yield more precise calibration/validation statistics than that of MODIS, and c) use of a single pixel centered on in situ coastal stations provides an optimal sampling size for validation efforts. These findings will have implications for enhancing our understanding of uncertainties in ocean color retrievals and for planning of future ocean color missions and the associated calibration/validation exercises. (C) 2016 Elsevier Inc. All rights reserved. C1 [Pahlevan, Nima; Sarkar, Sudipta; Franz, Bryan A.] NASA, Goddard Space Flight Ctr, Code 619 8800 Greenbelt Rd,Greenbelt Bldg 32, Greenbelt, MD 20771 USA. [Pahlevan, Nima; Sarkar, Sudipta] Sci Syst & Applicat Inc, 10210 Greenbelt Rd,Suite 600, Lanham, MD 20706 USA. RP Pahlevan, N (reprint author), NASA, Goddard Space Flight Ctr, Code 619 8800 Greenbelt Rd,Greenbelt Bldg 32, Greenbelt, MD 20771 USA. RI Franz, Bryan/D-6284-2012; OI Franz, Bryan/0000-0003-0293-2082; Pahlevan, Nima/0000-0002-5454-5212 FU NASA [NNG15HQ01C]; Geo-CAPE mission pre-fomulation studies FX Financial support by the NASA contract (award # NNG15HQ01C) and the Geo-CAPE mission pre-fomulation studies is acknowledged. We are also grateful to Robert E. Wolfe and Gary Lin with NASA GSFC's Terrestrial Information Systems Lab for the discussions of spatial performance of VIIRS and MODIS instruments. The computing support at the Terrestrial Information Systems Lab by Miguel O. Roman and Ed Masuoka is acknowledged. We are also grateful to the anonymous reviewers for their thoughtful comments that help improve this manuscript. NR 77 TC 2 Z9 2 U1 7 U2 21 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0034-4257 EI 1879-0704 J9 REMOTE SENS ENVIRON JI Remote Sens. Environ. PD AUG PY 2016 VL 181 BP 14 EP 26 DI 10.1016/j.rse.2016.03.022 PG 13 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA DO4CU UT WOS:000377730200002 ER PT J AU Alexandrov, MD Cairns, B van Diedenhoven, B Ackerman, AS Wasilewski, AP McGill, MJ Yorks, JE Hlavka, DL Platnick, SE Arnold, GT AF Alexandrov, Mikhail D. Cairns, Brian van Diedenhoven, Bastiaan Ackerman, Andrew S. Wasilewski, Andrzej P. McGill, Matthew J. Yorks, John E. Hlavka, Dennis L. Platnick, Steven E. Arnold, G. Thomas TI Polarized view of supercooled liquid water clouds SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE Clouds; Supercooled water; Electromagnetic scattering; Polarization; Mie theory; Rainbow; Remote sensing ID RESEARCH SCANNING POLARIMETER; AIRCRAFT ICING ENVIRONMENTS; THERMODYNAMIC PHASE; SOUTHERN-OCEAN; LARGE DROPS; AEROSOLS; SIMULATIONS; INSTRUMENT; MISSION; PHYSICS AB Supercooled liquid water (SLW) clouds, where liquid droplets exist at temperatures below 0 degrees C present a wellknown aviation hazard through aircraft icing, in which SLW accretes on the airframe. SLW clouds are common over the Southern Ocean, and climate-induced changes in their occurrence is thought to constitute a strong cloud feedback on global climate. The two recent NASA field campaigns POlarimeter Definition EXperiment (PODEX, based in Palmdale, California, January-February 2013) and Studies of Emissions and Atmospheric Composition, Clouds and Climate Coupling by Regional Surveys (SEAC4RS, based in Houston, Texas in August September 2013) provided a unique opportunity to observe SLW clouds from the high-altitude airborne platform of NASA's ER-2 aircraft. We present an analysis of measurements made by the Research Scanning Polarimeter (RSP) during these experiments accompanied by correlative retrievals from other sensors. The RSP measures both polarized and total reflectance in 9 spectral channels with wavelengths ranging from 410 to 2250 nm. It is a scanning sensor taking samples at 0.8 degrees intervals within 60 degrees from nadir in both forward and backward directions. This unique angular resolution allows for characterization of liquid water droplet size using the rainbow structure observed in the polarized reflectances in the scattering angle range between 135 degrees and 165 degrees. Simple parametric fitting algorithms applied to the polarized reflectance provide retrievals of the droplet effective radius and variance assuming a prescribed size distribution shape (gamma distribution). In addition to this, we use a non-parametric method, Rainbow Fourier Transform (RFT), which allows retrieval of the droplet size distribution without assuming a size distribution shape. We present an overview of the RSP campaign datasets available from the NASA GISS website, as well as two detailed examples of the retrievals. In these case studies we focus on cloud fields with spatial features varying between glaciated and liquid phases at altitudes as high as 10 km, which correspond to temperatures close to the homogeneous freezing temperature of pure water drops (about-35 degrees C or colder). The multimodal droplet size distributions retrieved from RSP data in these cases are consistent with the multi-layer cloud structure observed by correlative Cloud Physics Lidar (CPL) measurements. (C) 2016 Elsevier Inc. All rights reserved. C1 [Alexandrov, Mikhail D.] Columbia Univ, Dept Appl Phys & Appl Math, 2880 Broadway, New York, NY 10025 USA. [Alexandrov, Mikhail D.; Cairns, Brian; van Diedenhoven, Bastiaan; Ackerman, Andrew S.; Wasilewski, Andrzej P.] NASA Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA. [van Diedenhoven, Bastiaan] Columbia Univ, Ctr Climate Syst Res, 2880 Broadway, New York, NY 10025 USA. [Wasilewski, Andrzej P.] Trinnovim LLC, 2880 Broadway, New York, NY 10025 USA. [Hlavka, Dennis L.; Arnold, G. Thomas] Sci Syst & Applicat Inc, Lanham, MD USA. [McGill, Matthew J.; Yorks, John E.; Hlavka, Dennis L.; Platnick, Steven E.; Arnold, G. Thomas] NASA Goddard Space Flight Ctr, Greenbelt, MD USA. RP Alexandrov, MD (reprint author), NASA Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA. EM mda14@columbia.edu RI Platnick, Steven/J-9982-2014; OI Platnick, Steven/0000-0003-3964-3567; Cairns, Brian/0000-0002-1980-1022 FU NASA Radiation Sciences Program; NASA Earth Science Division; NASA ROSES program [NNX15AD44G] FX This research was funded by the NASA Radiation Sciences Program managed by Hal Maring and by the NASA ROSES program under grant NNX15AD44G. This work was also funded by the NASA Earth Science Division as part of the pre-formulation study for the Aerosol, Cloud, and ocean Ecosystem (ACE) Mission. We would like to thank David Starr, Richard Ferrare and Jens Redeman for providing the leadership needed to get the best possible observations from the available flight hours during PODEX. We are tremendously grateful to the SEAC4RS leadership team that allowed us to obtain such a comprehensive cloud remote sensing dataset. The NASA ER-2 pilots, crew and management were immensely supportive and we thank them for all the help they so generously provided. NR 55 TC 0 Z9 0 U1 12 U2 21 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0034-4257 EI 1879-0704 J9 REMOTE SENS ENVIRON JI Remote Sens. Environ. PD AUG PY 2016 VL 181 BP 96 EP 110 DI 10.1016/j.rse.2016.04.002 PG 15 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA DO4CU UT WOS:000377730200008 ER PT J AU Sharma, P Jones, CE Dudas, J Bawden, GW Deverel, S AF Sharma, Priyanka Jones, Cathleen E. Dudas, Joel Bawden, Gerald W. Deverel, Steven TI Monitoring of subsidence with UAVSAR on Sherman Island in California's Sacramento-San Joaquin Delta SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE Deltas; Subsidence; Synthetic aperture radar; Interferometry; InSAR; Land use; UAVSAR ID RADAR INTERFEROMETRY; SOILS; FAULT AB Sherman Island, the westernmost island in the Sacramento-San Joaquin Delta in California, plays a crucial role in maintaining the water flux between saline ocean water from the San Francisco Bay to its west and the rest of the Delta to its east. Land elevation below mean sea level and continuous subsidence over the past century has made this island a high priority area for investigations of subsidence and restoration in the Delta. This study reports the results of successful application of Interferometric Synthetic Aperture Radar (InSAR) data and technique to measure subsidence in the Delta, which is a coherence-challenged non-urban area. We carried out a time series interferometric analysis of Uninhabited Aerial Vehicle Synthetic Aperture Radar (UAVSAR) L-band (23.8 cm) data, collected from July 2009-August 2014, to assess both the spatial and temporal variation of subsidence on Sherman Island. We report both large-scale (island-wide) subsidence trends and small-scale (levee/ farm scale) subsidence features in Sherman Island. Assuming the subsidence is linear during the five years of UAVSAR data acquisition, subsidence rates across the island range from 0-5 cm/yr, with an average of 1.3 +/- 0.2 cm/yr. We estimate our systematic uncertainty to be 03 cm/yr. Overall, the central region in the island has subsided at a faster rate than the rest of the island. We find our results to be consistent with previous measurements of subsidence rates at electric transmission line towers scattered throughout the island. The results of this study provide insights into several factors influencing subsidence, including soil type, water table depth, land use, land elevation and the location and time of levee repairs. Subsidence monitoring on Sherman Island is essential for maintaining a reliable water supply for the state of California and for protecting the Delta ecosystem. (C) 2016 Elsevier Inc. All rights reserved. C1 [Sharma, Priyanka; Jones, Cathleen E.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,M-S T1721-220, Pasadena, CA 91109 USA. [Dudas, Joel] Calif Dept Water Resources, 1416 9th St, Sacramento, CA 95814 USA. [Bawden, Gerald W.] NASA Headquarters, 300 E St SW, Washington, DC 20546 USA. [Deverel, Steven] HydroFocus Inc, 2827 Spafford St, Davis, CA 95618 USA. RP Sharma, P (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,M-S T1721-220, Pasadena, CA 91109 USA. EM Priyanka.Sharma@jpl.nasa.gov; Cathleen.E.Jones@jpl.nasa.gov; Joel.Dudas@water.ca.gov; Gerald.W.Bawden@nasa.gov; sdeverel@hydrofocus.com FU Delta Science Program; California Sea Grant; NASA [NASA DEC08-0019]; Department of Homeland Security (DHS) [HSHPM-15-X-00023]; Department of Land, Air and Water Resources at UC Davis (NIFA) [2011-67003-30371]; US Department of Agriculture [201015552-06]; National Aeronautics and Space Administration FX The authors gratefully acknowledge those who designed, developed and operate the Uninhabited Aerial Vehicle Synthetic Aperture Radar (UAVSAR). We are grateful to the Delta Science Program and the California Sea Grant for awarding the Delta Science Sea Grant Postdoctoral Fellowship to the lead author of this study, which enabled the research described here to be conducted. We thank Mike Gunson and Duane Waliser for their mentorship and financial support during this study. This work was also supported through grants from NASA (NASA DEC08-0019), Department of Homeland Security (DHS HSHPM-15-X-00023), Department of Land, Air and Water Resources at UC Davis (NIFA # 2011-67003-30371) and US Department of Agriculture (Sub award No. 201015552-06). The research described here was carried out in part at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. The UAVSAR data are provided courtesy of NASA/JPL-Caltech. Copyright 2015. All rights reserved. NR 62 TC 0 Z9 0 U1 6 U2 14 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0034-4257 EI 1879-0704 J9 REMOTE SENS ENVIRON JI Remote Sens. Environ. PD AUG PY 2016 VL 181 BP 218 EP 236 DI 10.1016/j.rse.2016.04.012 PG 19 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA DO4CU UT WOS:000377730200018 ER PT J AU Nghiem, SV Rigor, IG Clemente-Colon, P Neumann, G Li, PP AF Nghiem, S. V. Rigor, I. G. Clemente-Colon, P. Neumann, G. Li, P. P. TI Geophysical constraints on the Antarctic sea ice cover SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE Antarctic sea ice; Passive and active microwave remote sensing; Frontal ice zone; Wind patterns; Antarctic Circumpolar Current front; GEBCO bathymetry ID SOUTHERN-OCEAN FRONTS; THICKNESS DISTRIBUTION; CIRCUMPOLAR CURRENT; SHIP OBSERVATIONS; CLIMATE-CHANGE; SATELLITE DATA; AMUNDSEN SEAS; SNOW COVER; VARIABILITY; MICROWAVE AB The contrast between the slight increase of Antarctic sea ice and the drastic reduction of Arctic sea ice since the 1970s has been a conundrum to be resolved. Sea ice trajectory tracking with satellite scatterometer data in 2008 shows that ice around Antarctica is pushed offshore by katabatic winds influenced by the continental topography. The ice trajectories reveal that sea ice, grown earlier in the ice season, drifts northward away from the Antarctic continent forming a circumpolar frontal ice zone (FIZ) behind the ice edge. The FIZ thereby consists of sea ice that becomes rougher due to a longer exposure to wind and wave actions, and thicker over time by more ice growth and greater snow accumulation. In the Antarctic circumpolar sea ice zone adjacent to the sea ice edge, satellite data in 1999-2009 exhibit a band of strong radar backscatter, which is consistent with the signature of older, thicker, and rougher sea ice with more snow in the FIZ. This sea ice band, as wide as 1000 km, serves as a 'Great Shield,' encapsulating and protecting younger and thinner ice in the internal ice pack. In the young and thin ice region behind the FIZ, ice can grow rapidly as winds continue opening interior areas thereby creating effective "ice factories." In addition, ridging can enhance ice thickness by convergence toward the circumpolar FIZ that is recirculated by westerly winds and currents. During the ice growth season, the FIZ advances until reaching lower-latitude warm waters at a boundary determined by the southern Antarctic Circumpolar Current front that is constrained by seafloor features. These persistent topographical and bathymetric geological factors help sustain the Antarctic sea ice cover. As such, the behavior of Antarctic sea ice is not a paradox as some have suggested, but instead is consistent with the geophysical characteristics in the southern polar region that starkly contrast to those in the Arctic. (C) 2016 Elsevier Inc. All rights reserved. C1 [Nghiem, S. V.; Neumann, G.; Li, P. P.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Nghiem, S. V.] Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA 90095 USA. [Rigor, I. G.] Univ Washington, Appl Phys Lab, 1013 NE 40th St,Box 355640, Seattle, WA 98105 USA. [Clemente-Colon, P.] NOAA Satellite Operat Facil, US Natl Naval Ice Ctr, 4251 Suitland Rd, Washington, DC 20395 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; National Oceanic and Atmospheric Administration (NOAA); National Science Foundation 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. This research was also carried out in part under the support of the National Oceanic and Atmospheric Administration (NOAA) via a subcontract to the Joint Institute for Regional Earth System Science and Engineering of the University of California at Los Angeles. Rigor is funded by NASA, National Science Foundation, and NOAA. The statements, findings, conclusions, and recommendations in this paper are those of the authors and do not necessarily reflect the views of NOAA or the Department of Commerce. We thank S. Helfrich of NIC for preparing NIC SIE data, L. Kaleschke of the University of Hamburg for helping in the ICDC SIE data access, D.T. Nguyen of JPL for assisting in GEBCO bathymetry representation, and J. Vazquez and T.M. Chin of JPL for the MUR SST data access and documentation. We thank the reviewers, all having positive and constructive comments and suggestions in the review process by Remote Sensing of Environment. In particular, we highly appreciate the excellent and thorough review by Claire Parkinson of the NASA Goddard Space Flight Center. NR 76 TC 3 Z9 3 U1 12 U2 31 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0034-4257 EI 1879-0704 J9 REMOTE SENS ENVIRON JI Remote Sens. Environ. PD AUG PY 2016 VL 181 BP 281 EP 292 DI 10.1016/j.rse.2016.04.005 PG 12 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA DO4CU UT WOS:000377730200022 ER PT J AU Yao, WG Liou, MS AF Yao, Weigang Liou, Meng-Sing TI A nonlinear modeling approach using weighted piecewise series and its applications to predict unsteady flows SO JOURNAL OF COMPUTATIONAL PHYSICS LA English DT Article DE Modeling of nonlinear dynamics with parametric inputs; Weighted piecewise linear (WPL) model; Unsteady flow; Limited cycle oscillations ID PROPER ORTHOGONAL DECOMPOSITION; REDUCTION; COMPUTATION; SIMULATION; DYNAMICS; SYSTEMS AB To preserve nonlinearity of a full-order system over a range of parameters of interest, we propose an accurate and robust nonlinear modeling approach by assembling a set of piecewise linear local solutions expanded about some sampling states. The work by Rewienski and White [1] on micromachined devices inspired our use of piecewise linear local solutions to study nonlinear unsteady aerodynamics. These local approximations are assembled via nonlinear weights of radial basis functions. The efficacy of the proposed procedure is validated for a two-dimensional airfoil moving with different pitching motions, specifically AGARD's CT2 and CT5 problems [27], in which the flows exhibit different nonlinear behaviors. Furthermore, application of the developed aerodynamic model to a two-dimensional aero-elastic system proves the approach is capable of predicting limit cycle oscillations (LCOs) by using AGARD's CT6 [28] as a benchmark test. All results, based on inviscid solutions, confirm that our nonlinear model is stable and accurate, against the full model solutions and measurements, and for predicting not only aerodynamic forces but also detailed flowfields. Moreover, the model is robust for inputs that considerably depart from the base trajectory in form and magnitude. This modeling provides a very efficient way for predicting unsteady flowfields with varying parameters because it needs only a tiny fraction of the cost of a full-order modeling for each new condition-the more cases studied, the more savings rendered. Hence, the present approach is especially useful for parametric studies, such as in the case of design optimization and exploration of flow phenomena. Published by Elsevier Inc. C1 [Yao, Weigang; Liou, Meng-Sing] NASA, John H Glenn Res Ctr Lewis Field, Cleveland, OH 44135 USA. [Yao, Weigang] NASA Postdoc Program, Washington, DC USA. [Yao, Weigang] Queens Univ Belfast, Sch Mech & Aerosp Engn, Belfast, Antrim, North Ireland. RP Liou, MS (reprint author), NASA, John H Glenn Res Ctr Lewis Field, Cleveland, OH 44135 USA. EM meng-sing.liou@nasa.gov FU Subsonic Fixed Wing Project under NASA's Fundamental Aeronautics Program; Aero Sciences Project under NASA's Fundamental Aeronautics Program FX Weigang Yao was a NASA Postdoc Fellow supported by the Subsonic Fixed Wing Project, under NASA's Fundamental Aeronautics Program; Mr. William Haller is the Technical Lead of the task. Meng-Sing Liou has been supported by the Subsonic Fixed Wing and Aero Sciences Projects, under NASA's Fundamental Aeronautics Program and Dr. Jeffery Moder is the task Technical Lead for the Aero Sciences Project. The authors thank the reviewers for several useful suggestions and comments that have contributed to improvement of the paper. NR 36 TC 1 Z9 1 U1 3 U2 6 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0021-9991 EI 1090-2716 J9 J COMPUT PHYS JI J. Comput. Phys. PD AUG 1 PY 2016 VL 318 BP 58 EP 84 DI 10.1016/j.jcp.2016.04.052 PG 27 WC Computer Science, Interdisciplinary Applications; Physics, Mathematical SC Computer Science; Physics GA DN4NF UT WOS:000377043400004 ER PT J AU Laguna, AA Lani, A Deconinck, H Mansour, NN Poedts, S AF Laguna, A. Alvarez Lani, A. Deconinck, H. Mansour, N. N. Poedts, S. TI A fully-implicit finite-volume method for multi-fluid reactive and collisional magnetized plasmas on unstructured meshes SO JOURNAL OF COMPUTATIONAL PHYSICS LA English DT Article DE Plasma; Finite volume method; Magnetohydrodynamics (MHD); Multi-fluid ID IDEAL MAGNETOHYDRODYNAMICS; RIEMANN SOLVER; EQUATIONS; MODEL; SIMULATIONS; SCHEME; RECONNECTION; MAXWELL; SEQUEL; AUSM AB We present a Finite Volume scheme for solving Maxwell's equations coupled to magnetized multi-fluid plasma equations for reactive and collisional partially ionized flows on unstructured meshes. The inclusion of the displacement current allows for studying electromagnetic wave propagation in a plasma as well as charge separation effects beyond the standard magnetohydrodynamics (MHD) description, however, it leads to a very stiff system with characteristic velocities ranging from the speed of sound of the fluids up to the speed of light. In order to control the fulfillment of the elliptical constraints of the Maxwell's equations, we use the hyperbolic divergence cleaning method. In this paper, we extend the latter method applying the CIR scheme with scaled numerical diffusion in order to balance those terms with the Maxwell flux vectors. For the fluids, we generalize the AUSM+-up to multiple fluids of different species within the plasma. The fully implicit second-order method is first verified on the Hartmann flow (including comparison with its analytical solution), two ideal MHD cases with strong shocks, namely, Orszag-Tang and the MHD rotor, then validated on a much more challenging case, representing a two-fluid magnetic reconnection under solar chromospheric conditions. For the latter case, a comparison with pioneering results available in literature is provided. (C) 2016 Elsevier Inc. All rights reserved. C1 [Laguna, A. Alvarez; Lani, A.; Deconinck, H.] Von Karman Inst Fluid Dynam, Waterloosesteenweg 72, B-1640 Rhode St Genese, Belgium. [Laguna, A. Alvarez; Poedts, S.] Katholieke Univ Leuven, Ctr Math Plasma Astrophys, Celestijnenlaan 200B, B-3001 Leuven, Belgium. [Mansour, N. N.] NASA, Ames Res Ctr, MS 230-3, Moffett Field, CA 94035 USA. RP Laguna, AA (reprint author), Von Karman Inst Fluid Dynam, Waterloosesteenweg 72, B-1640 Rhode St Genese, Belgium.; Laguna, AA (reprint author), Katholieke Univ Leuven, Ctr Math Plasma Astrophys, Celestijnenlaan 200B, B-3001 Leuven, Belgium. EM alejandro.alvarez.laguna@vki.ac.be; alani@vki.ac.be; deconinck@vki.ac.be; Nagi.N.Mansour@nasa.gov; Stefaan.Poedts@wis.kuleuven.be RI Poedts, Stefaan/C-9775-2012; OI Poedts, Stefaan/0000-0002-1743-0651; Lani, Andrea/0000-0003-4017-215X FU Agency for Innovation by Science and Technology in Flanders (IWT); Research Foundation of Flanders [FWO G.0729.11N]; KU Leuven [GOA/2015-014]; FWO-Vlaanderen [G.0A23.16N]; ESA Prodex [C90347] FX The first author's contribution was supported by a Ph.D. grant from the Agency for Innovation by Science and Technology in Flanders (IWT). The second author's contribution was supported by the FWO G.0729.11N grant from the Research Foundation of Flanders. Some magnetic reconnection simulations whose results have been discussed in this work were run on Pleiades, NASA's supercomputer at the NASA Ames Research Center. These results were obtained in the framework of the projects GOA/2015-014 (KU Leuven), G.0A23.16N (FWO-Vlaanderen) and C90347 (ESA Prodex). NR 61 TC 2 Z9 2 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 0021-9991 EI 1090-2716 J9 J COMPUT PHYS JI J. Comput. Phys. PD AUG 1 PY 2016 VL 318 BP 252 EP 276 DI 10.1016/j.jcp.2016.04.058 PG 25 WC Computer Science, Interdisciplinary Applications; Physics, Mathematical SC Computer Science; Physics GA DN4NF UT WOS:000377043400012 ER PT J AU Tsafack, T Alred, JM Wise, KE Jensen, B Siochi, E Yakobson, BI AF Tsafack, Thierry Alred, John M. Wise, Kristopher E. Jensen, Benjamin Siochi, Emilie Yakobson, Boris I. TI Exploring the interface between single-walled carbon nanotubes and epoxy resin SO CARBON LA English DT Article ID MOLECULAR-DYNAMICS; MECHANICAL-PROPERTIES; NANOCOMPOSITES; COMPOSITES; RUBBER; STATES AB A significant mechanical reinforcement of epoxy matrices with carbon nanotubes (CNTs) requires a very strong covalent interfacial bonding between the tube and the resin, diglycidylether of bisphenol A (DGEBA). Using classical molecular dynamics (MD) and density functional theory (DFT), various methods of improving covalent binding to CNTs are applied on four major categories: CNT diameters, dopants, defects, and functional groups. The diameter category includes (n, 0) CNTs with n = 5, 7, 9,11, 13, 15; the dopant category includes B-, N-, and Si-doped CNTs; the defect category includes CNTs with monovacancies, Stone-Wales, and more complex nitrogen terminated monovacancies and divacancies; the functional group category includes CNTs with atomic oxygen, hydroxyl, amine, carboxyl, and a combination of oxygen and hydroxyl. The computation of binding energies (BE), affinity indices (AI), and shear fracture forces on all configurations converged to the conclusion that smaller tubes, Si-doped CNTs, CNTs functionalized with a combination of oxygen and hydroxyl, and CNTs with monovacancies show the strongest indication for mechanical reinforcement in their respective categories. (C) 2016 Elsevier Ltd. All rights reserved. C1 [Tsafack, Thierry; Alred, John M.; Yakobson, Boris I.] Rice Univ, Dept Mat Sci & Nanoengn, 6100 Main St MS-325, Houston, TX USA. [Wise, Kristopher E.; Jensen, Benjamin; Siochi, Emilie] NASA, Langley Res Ctr, Adv Mat & Proc Branch, Hampton, VA 23665 USA. RP Yakobson, BI (reprint author), Rice Univ, Dept Mat Sci & Nanoengn, 6100 Main St MS-325, Houston, TX USA.; Wise, KE (reprint author), NASA, Langley Res Ctr, Adv Mat & Proc Branch, Hampton, VA 23665 USA. EM Kristopher.E.Wise@nasa.gov; biy@rice.edu RI Jensen, Benjamin/B-1297-2013 OI Jensen, Benjamin/0000-0002-7982-0663 FU NASA under the NASA Langley Research Center Nano Incubator Project [NNX13AN37G] FX The authors appreciate the useful discussions with Dr. Adri van Duin. This research was funded by NASA under the NASA Langley Research Center Nano Incubator Project (Grant NNX13AN37G). NR 44 TC 0 Z9 0 U1 23 U2 58 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0008-6223 EI 1873-3891 J9 CARBON JI Carbon PD AUG PY 2016 VL 105 BP 600 EP 606 DI 10.1016/j.carbon.2016.04.066 PG 7 WC Chemistry, Physical; Materials Science, Multidisciplinary SC Chemistry; Materials Science GA DM8JB UT WOS:000376607200069 ER PT J AU Stephan, K Wagner, R Jaumann, R Clark, RN Cruikshank, DP Brown, RH Giese, B Roatsch, T Filacchione, G Matson, D Ore, CD Capaccioni, F Baines, KH Rodriguez, S Krupp, N Buratti, BJ Nicholson, PD AF Stephan, Katrin Wagner, Roland Jaumann, Ralf Clark, Roger N. Cruikshank, Dale P. Brown, Robert H. Giese, Bernd Roatsch, Thomas Filacchione, Gianrico Matson, Dennis Ore, Cristina Dalle Capaccioni, Fabrizio Baines, Kevin H. Rodriguez, Sebastien Krupp, Norbert Buratti, Bonnie J. Nicholson, Phil D. TI Cassini's geological and compositional view of Tethys SO ICARUS LA English DT Article DE Saturn; Satellites surfaces; Geological processes; Ices; IR spectroscopy ID SATURNS ICY SATELLITES; SURFACE-COMPOSITION; CRATERING HISTORY; IMAGING SCIENCE; VIMS; MIMAS; RHEA; ENCELADUS; DIONE; SYSTEM AB The Saturnian satellite Tethys exhibits geological and spectral properties, whose appearance, nature and spatial distribution partly mirror those identified on the neighboring satellites Dione and Rhea or fit to the picture how spectral surface properties are expected to change from one satellite to the other within the inner Saturnian system. However, we also identified spectral variations that are unique in the Saturnian system. Whereas geologically young surface features are characterized by pure H2O-ice composition with relatively large particles, which match the particle sizes measured for fresh surface features also on Dione and Rhea, geologically old weathered regions are dominated by submicron-sized ice particles. Our investigations confirm that the Odysseus impact event did not cause the formation of Tethys' extended graben system Ithaca Chasma. On the contrary, Odysseus might be responsible for the N-S trending 'icy' bands that mark Tethys' surface in the center of its leading and trailing hemisphere. (C) 2016 Elsevier Inc. All rights reserved. C1 [Stephan, Katrin; Wagner, Roland; Jaumann, Ralf; Giese, Bernd; Roatsch, Thomas] DLR, Inst Planetary Res, D-12489 Berlin, Germany. [Jaumann, Ralf] Free Univ Berlin, Dept Earth Sci, Inst Geosci, Berlin, Germany. [Clark, Roger N.] US Geol Survey, Denver Fed Ctr, Denver, CO 80225 USA. [Cruikshank, Dale P.; Ore, Cristina Dalle] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Brown, Robert H.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Filacchione, Gianrico; Capaccioni, Fabrizio; Buratti, Bonnie J.] INAF IAPS, I-00133 Rome, Italy. [Matson, Dennis] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Baines, Kevin H.] Univ Wisconsin, Space Sci & Engn Ctr, Madison, WI 53706 USA. [Rodriguez, Sebastien] Univ Paris 07, CEA Saclay, Lab AIM, CNRS,DSM,IRFU,SAp, F-91191 Gif Sur Yvette, France. [Krupp, Norbert] Max Planck Inst Sonnensyst Forsch, D-37077 Gottingen, Germany. [Nicholson, Phil D.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. RP Stephan, K (reprint author), DLR, Inst Planetary Res, D-12489 Berlin, Germany. EM Katrin.Stephan@dlr.de RI Rodriguez, Sebastien/H-5902-2016; OI Rodriguez, Sebastien/0000-0003-1219-0641; Filacchione, Gianrico/0000-0001-9567-0055 NR 64 TC 0 Z9 0 U1 3 U2 12 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD AUG PY 2016 VL 274 BP 1 EP 22 DI 10.1016/j.icarus.2016.03.002 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DL8IM UT WOS:000375885700001 ER PT J AU Davies, AG Sotin, C Choukroun, M Matson, DL Johnson, TV AF Davies, Ashley Gerard Sotin, Christophe Choukroun, Mathieu Matson, Dennis L. Johnson, Torrence V. TI Cryolava flow destabilization of crustal methane clathrate hydrate on Titan SO ICARUS LA English DT Article DE Titan; Volcanism; Titan, atmosphere; Titan, surface ID POSSIBLE ORIGIN; ICY SATELLITES; CRYOVOLCANISM; ENCELADUS; FEATURES; SURFACE; ETHANE; SYSTEM; RADAR; SPOT AB To date, there has been no conclusive observation of ongoing endogenous volcanic activity on Saturn's moon Titan. However, with time, Titan's atmospheric methane is lost and must be replenished. We have modeled one possible mechanism for the replenishment of Titan's methane loss. Cryolavas can supply enough heat to release large amounts of methane from methane clathrate hydrates (MCH). The volume of methane released is controlled by the flow thickness and its areal extent. The depth of the destabilisation layer is typically approximate to 30% of the thickness of the lava flow (approximate to 3 m for a 10-m thick flow). For this flow example, a maximum of 372 kg of methane is released per m(2) of flow area. Such an event would release methane for nearly a year. One or two events per year covering similar to 20 km(2) would be sufficient to resupply atmospheric methane. A much larger effusive event covering an area of approximate to 9000 km(2) with flows 200 m thick would release enough methane to sustain current methane concentrations for 10,000 years. The minimum size of "cryo-flows" sufficient to maintain the current atmospheric methane is small enough that their detection with current instruments (e.g., Cassini) could be challenging. We do not suggest that Titan's original atmosphere was generated by this mechanism. It is unlikely that small-scale surface MCH destabilisation is solely responsible for long-term (> a few Myr) sustenance of Titan's atmospheric methane, but rather we present it as a possible contributor to Titan's past and current atmospheric methane. (C) 2016 Published by Elsevier Inc. C1 [Davies, Ashley Gerard; Sotin, Christophe; Choukroun, Mathieu; Johnson, Torrence V.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Matson, Dennis L.] Bear Fight Inst, Winthrop, WA 98862 USA. RP Davies, AG (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Ashley.Davies@jpl.nasa.gov RI Choukroun, Mathieu/F-3146-2017 OI Choukroun, Mathieu/0000-0001-7447-9139 FU NASA Outer Planets Research Program [NMO710931] FX This work was performed at the Jet Propulsion Laboratory, California Institute of Technology, under contract to NASA. (c) 2016 Caltech. We thank the NASA Outer Planets Research Program for support through award NMO710931. We thank a number of reviewers, including Christopher McKay and Ralph Lorenz, for their input. NR 56 TC 1 Z9 1 U1 7 U2 19 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD AUG PY 2016 VL 274 BP 23 EP 32 DI 10.1016/j.icarus.2016.02.046 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DL8IM UT WOS:000375885700002 ER PT J AU Craddock, RA Golombek, MP AF Craddock, Robert A. Golombek, Matthew P. TI Characteristics of terrestrial basaltic rock populations: Implications for Mars lander and rover science and safety SO ICARUS LA English DT Article DE Mars; Mars, surface; Terrestrial planets ID PATHFINDER LANDING SITE; MARTIAN SURFACE; GROUND ICE; SOUTHWEST ICELAND; VIKING LANDERS; BRITTLE SOLIDS; FRAGMENT SIZE; DEBRIS FLOWS; GRAIN SHAPE; GALE CRATER AB We analyzed the morphometry of basaltic rock populations that have been emplaced or affected by a variety of geologic processes, including explosive volcanic eruptions (as a proxy for impact cratering), catastrophic flooding, frost shattering, salt weathering, alluvial deposition, and chemical weathering. Morphometric indices for these rock populations were compared to an unmodified population of rocks that had broken off a solidified lava flow to understand how different geologic processes change rock shape. We found that a majority of rocks have an sphericity described as either a disc or sphere in the Zingg classification system and posit that this is a function of cooling fractures in the basalt (Zingg [1935] Schweiz. Miner. Petrogr. Mitt., 15, 39-140). Angularity (roundness) is the most diagnostic morphometric index, but the Corey Shape Factor (CSF), Oblate-Prolate Index (OPI) and deviation from compactness (D) also sometimes distinguished weathering processes. Comparison of our results to prior analyses of rock populations found at the Mars Pathfinder, Spirit, and Curiosity landing sites support previous conclusions. The observation that the size-frequency distribution of terrestrial rock populations follow exponential functions similar to lander and orbital measurements of rocks on Mars, which is expected from fracture and fragmentation theory, indicates that these distributions are being dominantly controlled by the initial fracture and fragmentation of the basalt. Published by Elsevier Inc. C1 [Craddock, Robert A.] Smithsonian Inst, Ctr Earth & Planetary Studies, Natl Air & Space Museum, Washington, DC 20560 USA. [Golombek, Matthew P.] CALTECH, Jet Prop Lab, Div Earth & Space Sci, Pasadena, CA 91109 USA. RP Craddock, RA (reprint author), Smithsonian Inst, Ctr Earth & Planetary Studies, Natl Air & Space Museum, Washington, DC 20560 USA. EM craddockb@si.edu FU Smithsonian Institution's George F. Becker endowment fund; Smithsonian Institution's George F. Becker Endowment FX This research was supported by the Smithsonian Institution's George F. Becker endowment fund. We thank Scott Eaton, Carolyn Russo, and Alan Howard for assistance in the field. We also thank Aileen Yingst for her constructive comments on the initial draft of this manuscript. Scott Rowland and an anonymous reviewer provided many valuable and insightful comments that improved the final version of the manuscript. This research was partially supported by a grant from the Smithsonian Institution's George F. Becker Endowment. Part of the research in this paper was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA. NR 156 TC 0 Z9 0 U1 7 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 EI 1090-2643 J9 ICARUS JI Icarus PD AUG PY 2016 VL 274 BP 50 EP 72 DI 10.1016/j.icarus.2016.02.042 PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DL8IM UT WOS:000375885700005 ER PT J AU Kollmann, P Brandt, PC Collinson, G Rong, ZJ Futaana, Y Zhang, TL AF Kollmann, P. Brandt, P. C. Collinson, G. Rong, Z. J. Futaana, Y. Zhang, T. L. TI Properties of planetward ion flows in Venus' magnetotail SO ICARUS LA English DT Article DE Venus; Magnetospheres; Reconnection; Venus Express; Plasma ID EXPRESS OBSERVATIONS; MAGNETIC-FIELD; SOLAR-WIND; PLASMA ENVIRONMENT; FLAPPING MOTIONS; MARS-EXPRESS; ESCAPE RATE; PRECIPITATION; DISTRIBUTIONS; CONSEQUENCES AB Venus is gradually losing some of its atmosphere in the form of ions through its induced magnetotail. Some of these ions have been reported previously to flow back to the planet. Proposed drivers are magnetic reconnection and deflection of pickup ions in the magnetic field. We analyze protons and oxygen ions with eV to keV energies acquired by the ASPERA-4/IMA instrument throughout the entire Venus Express mission. We find that venusward flowing ions are important in the sense that their density and deposition rate into the atmosphere is of the same order of magnitude as the density and escape rate of downtail flowing ions. Our analysis shows that during strong EUV irradiance, which occurs during solar maximum, the flux of venusward flowing protons is weaker and of oxygen ions is stronger than during weak irradiance. Since such a behavior was observed when tracing oxygen ions through a MHD model, the ultimate driver of the venusward flowing ions may simply be the magnetic field configuration around Venus. Although the pure downtail oxygen flux stays mostly unchanged for all observed EUV conditions, the increase in venusward oxygen flux for high irradiance results in a lower net atmospheric escape rate. Venusward bulk flows are mostly found in locations where the magnetic field is weak relative to the interplanetary conditions. Although a weak field is generally an indicator of proximity to the magnetotail current sheet, these flows do not cluster around current sheet crossings, as one may expect if they would be driven by magnetic reconnection. (C) 2016 The Authors. Published by Elsevier Inc. C1 [Kollmann, P.; Brandt, P. C.] Johns Hopkins Univ, Appl Phys Lab, Johns Hopkins Rd, Laurel, MD 20723 USA. [Collinson, G.] NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Greenbelt, MD 20771 USA. [Futaana, Y.] Swedish Inst Space Phys IRF, S-98128 Kiruna, Sweden. [Rong, Z. J.] Chinese Acad Sci, Inst Geol & Geophys, Key Lab Earth & Planetary Phys, Beijing 100029, Peoples R China. [Zhang, T. L.] Austrian Acad Sci, Space Res Inst IWF, A-8042 Graz, Austria. RP Kollmann, P (reprint author), Johns Hopkins Univ, Appl Phys Lab, Johns Hopkins Rd, Laurel, MD 20723 USA. EM peter.kollmann@jhuapl.edu RI Kollmann, Peter/C-2583-2016; Brandt, Pontus/N-1218-2016; OI Kollmann, Peter/0000-0002-4274-9760; Brandt, Pontus/0000-0002-4644-0306; Futaana, Yoshifumi/0000-0002-7056-3517 FU NASA [NNX10AI17G] FX Venus Express/ASPERA-4 and MAG data are available online through ESA's planetary science archive (PSA). Timed/SEE data is available through the LASP Interactive Solar Irradiance Data Center (LISIRD) at lasp.colorado.edu/lisird. JHU/APL authors were supported by NASA grant NNX10AI17G for Venus Express Participating Scientists. The authors like to thank M. Fraenz (MPS) and A. Fedorov (IRAP) for analysis software and data processing. NR 50 TC 0 Z9 0 U1 4 U2 9 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD AUG PY 2016 VL 274 BP 73 EP 82 DI 10.1016/j.icarus.2016.02.053 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DL8IM UT WOS:000375885700006 ER PT J AU Carlson, RW Baines, KH Anderson, MS Filacchione, G Simon, AA AF Carlson, R. W. Baines, K. H. Anderson, M. S. Filacchione, G. Simon, A. A. TI Chromophores from photolyzed ammonia reacting with acetylene: Application to Jupiter's Great Red Spot SO ICARUS LA English DT Article DE Jupiter, atmosphere; Photochemistry; Atmospheres, chemistry; Atmospheres, composition; Organic chemistry ID INFRARED MAPPING SPECTROMETER; SIMULATED JOVIAN ATMOSPHERE; ORGANIC SYNTHESIS; PHOSPHINE PHOTOLYSIS; MASS-SPECTROMETER; UPPER TROPOSPHERE; CROSS-SECTIONS; IMAGING DATA; NH3; PHOTOCHEMISTRY AB The high altitude of Jupiter's Great Red Spot (GRS) may enhance the upward flux of gaseous ammonia (NH3) into the high troposphere, where NH3 molecules can be photodissociated and initiate a chain of chemical reactions with downwelling acetylene molecules (C2H2). These reactions, experimentally studied earlier by (Ferris and Ishikawa [1987] Nature 326, 777-778) and (Ferris and Ishikawa [1988] J. Amer. Chem. Soc. 110, 4306-4312), produce chromophores that absorb in the visible and ultraviolet regions. In this work we photolyzed mixtures of NH3 and C2H2 using. ultraviolet radiation with a wavelength of 214 nm and measured the spectral transmission of the deposited films in the visible region (400-740 nm). From these transmission data we estimated the imaginary indices of refraction. Assuming that ammonia grains at the top of the GRS clouds are coated with this material, we performed layered sphere and radiative transfer calculations to predict GRS reflection spectra. Comparison of those results with observed and previously unreported Cassini visible spectra and with true-color images of the GRS show that the unknown GRS chromophore is spectrally consistent with the coupled NH3-C2H2 photochemical products produced in our laboratory experiments. Using high-resolution mass spectrometry and infrared spectroscopy we infer that the chromophore-containing residue is composed of aliphatic azine, azo, and diazo compounds. (C) 2016 Elsevier Inc. All rights reserved. C1 [Carlson, R. W.; Baines, K. H.; Anderson, M. S.] CALTECH, Jet Prop Lab, Mail Stop 183-601,4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Filacchione, G.] Ist Astrofis & Planetol Spaziali, Rome, Italy. [Simon, A. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA. RP Carlson, RW (reprint author), CALTECH, Jet Prop Lab, Mail Stop 183-601,4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Robert.W.Carlson@jpl.nasa.gov RI Simon, Amy/C-8020-2012; OI Simon, Amy/0000-0003-4641-6186; Filacchione, Gianrico/0000-0001-9567-0055 FU NASA's Planetary Atmospheres Program; Association of Universities for Research in Astronomy, Inc., under NASA [NAS 5-26555]; [GO6009]; [GO6452]; [GO11498]; [GO13937] FX We thank the two anonymous reviewers for their careful reading and thoughtful comments that have greatly improved the paper. RWC and KHB gratefully acknowledge funding from NASA's Planetary Atmospheres Program. Portions of this work were performed at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Space and Aeronautics Administration. Some results were based on observations made with the NASA/ESA Cassini spacecraft and the Hubble Space Telescope. Data from the latter were obtained from the Data Archive at the Space Telescope Science Institute, operated by the Association of Universities for Research in Astronomy, Inc., under NASA Contract NAS 5-26555. These observations are associated with programs GO6009, GO6452, GO11498 and GO13937. NR 78 TC 0 Z9 0 U1 7 U2 15 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD AUG PY 2016 VL 274 BP 106 EP 115 DI 10.1016/j.icarus.2016.03.008 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DL8IM UT WOS:000375885700009 ER PT J AU Konopliv, AS Park, RS Folkner, WM AF Konopliv, Alex S. Park, Ryan S. Folkner, William M. TI An improved JPL Mars gravity field and orientation from Mars orbiter and lander tracking data SO ICARUS LA English DT Article DE Mars, interior; Rotational dynamics; Mars ID GLOBAL SURVEYOR; ORDER MODEL; PHOBOS AB The Mars gravity field resolution is mostly determined by the lower altitude Mars Reconnaissance Orbiter (MRO) tracking data. With nearly four years of additional MRO and Mars Odyssey tracking data since the last JPL released gravity field MRO110C and lander tracking from the MER Opportunity Rover, the gravity field and orientation of Mars have been improved. The new field, MRO120D, extends the maximum spherical harmonic degree slightly to 120, improves the determination of the higher degree coefficients as demonstrated by improved correlation with topography and reduces the uncertainty in the corresponding Mars orientation parameters by up to a factor of two versus previously combined gravity and orientation solutions. The new precession solution is (psi) over dot = -7608.3 +/- 2.1 mas/yr and is consistent with previous results but with a reduced uncertainty by 40%. The Love number solution, k(2) = 0.169 +/- 0.006, also shows a similar result to previous studies. (C) 2016 Elsevier Inc. All rights reserved. C1 [Konopliv, Alex S.; Park, Ryan S.; Folkner, William M.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. RP Konopliv, AS (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Alex.Konopliv@jpl.nasa.gov NR 28 TC 1 Z9 1 U1 10 U2 18 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD AUG PY 2016 VL 274 BP 253 EP 260 DI 10.1016/j.icarus.2016.02.052 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DL8IM UT WOS:000375885700018 ER PT J AU de Pater, I Davies, AG Marchis, F AF de Pater, Imke Davies, Ashley Gerard Marchis, Franck TI Keck observations of eruptions on Io in 2003-2005 SO ICARUS LA English DT Article DE Io; Infrared observations; Volcanism ID GALILEO NIMS DATA; VOLCANIC ACTIVITY; HEAT-FLOW; THERMAL SIGNATURE; STANDARD STARS; LOKI PATERA; MU-M; MISSION; TELESCOPE; EVOLUTION AB We report observations of four energetic volcanic eruptions on Io: at Tupan Patera on UT 8 March 2003; Tung Yo Patera on UT 28 May 2004; Sui Jen Patera on UT 30 May 2004; and south of Babbar Patera on UT 31 May 2005. The Tung Yo, Sui Jen and south of Babbar Paterae eruptions are in locations where no activity had been seen before. Our observations were obtained at near-infrared wavelengths (1.2-4.7 mu m) with the 10-m Keck telescope equipped with adaptive optics. We report single and two-temperature blackbody fits, as well as single-component and dual-component Io Flow Model (IFM) fits (Davies, 1996, Icarus, 124, 45-61) to all four eruptions where applicable. We use 2-mu m and 5-mu m radiant fluxes, the 2:5-mu m radiant flux ratio, and radiant flux density of each thermal source to constrain the likely style of volcanic eruption. All eruptions are characterized by a high temperature IFM component (ranging from 1475 to similar to 900 K) from a relatively small area (<1 km(2) to several tens of km(2)), and a lower temperature component with a more extensive surface area. The relationship of the areas at the highest temperatures to the cooler, more extensive area is of particular importance in deriving eruption style. Model fits to the Sui Jen Patera data are strongly suggestive of lava fountaining, although not at a level consistent with a large "outburst" eruption. Activity at Tupan Patera suggests that the entire floor of the patera may have been resurfaced with silicate lava in 2003. (C) 2016 Elsevier Inc. All rights reserved. C1 [de Pater, Imke] Univ Calif Berkeley, Dept Astron, 501 Campbell Hall, Berkeley, CA 94720 USA. [de Pater, Imke] Delft Univ Technol, Fac Aerosp Engn, NL-2629 HS Delft, Netherlands. [de Pater, Imke] SRON Netherlands Inst Space Res, NL-3584 CA Utrecht, Netherlands. [Davies, Ashley Gerard] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Marchis, Franck] SETI Inst, Carl Sagan Ctr, Mountain View, CA 94043 USA. [Marchis, Franck] IMCCE Obs Paris, F-75014 Paris, France. RP de Pater, I (reprint author), Univ Calif Berkeley, Dept Astron, 501 Campbell Hall, Berkeley, CA 94720 USA. EM imke@berkeley.edu FU W.M. Keck Foundation; National Science Foundation, NSF [AST-1313485]; NASA Outer Planets Research and Planetary Geology and Geophysics Program FX We thank Alfred McEwen and an anonymous referee for valuable comments on the paper, which helped improve the paper substantially. The data presented in this paper were obtained at the W.M. Keck Observatories. The Keck Telescopes are 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. Our research was partially supported by the National Science Foundation, NSF grant AST-1313485 to UC Berkeley. Ashley Davies thanks the NASA Outer Planets Research and Planetary Geology and Geophysics Program for support. The authors recognize and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations of Ionian volcanoes from this Hawaiian volcano. NR 42 TC 1 Z9 1 U1 4 U2 8 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD AUG PY 2016 VL 274 BP 284 EP 296 DI 10.1016/j.icarus.2015.12.054 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DL8IM UT WOS:000375885700021 ER PT J AU Farnocchia, D Chesley, SR Brown, PG Chodas, PW AF Farnocchia, Davide Chesley, Steven R. Brown, Peter G. Chodas, Paul W. TI The trajectory and atmospheric impact of asteroid 2014 AA SO ICARUS LA English DT Article DE Asteroids; Asteroids; Dynamics; Astrometry; Near-Earth objects; Orbit determination AB Near-Earth asteroid 2014 AA entered the Earth's atmosphere on 2014 January 2, only 21 h after being discovered by the Catalina Sky Survey. In this paper we compute the trajectory of 2014 AA by combining the available optical astrometry, seven ground-based observations over 69 min, and the International Monitoring System detection of the atmospheric impact infrasonic airwaves in a least-squares orbit estimation filter. The combination of these two sources of observations results in a tremendous improvement in the orbit uncertainties. The impact time is 3:05 UT with a 1 sigma uncertainty of 6 min, while the impact location corresponds to a west longitude of 44.2 degrees and a latitude of 13.1 degrees with a 1 sigma uncertainty of 140 km. The minimum impact energy estimated from the infrasound data and the impact velocity result in an estimated minimum mass of 22.6 t. By propagating the trajectory of 2014 AA backwards we find that the only window for finding precovery observations is for the three days before its discovery. (C) 2016 Elsevier Inc. All rights reserved. C1 [Farnocchia, Davide; Chesley, Steven R.; Chodas, Paul W.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Brown, Peter G.] Univ Western Ontario, London, ON N6A 3K7, Canada. RP Farnocchia, D (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Davide.Farnocchia@jpl.nasa.gov FU NASA [NNX11AB76A] FX We thank J. D. Giorgini and the reviewers, P. Jenniskens and an anonymous one, for useful comments that helped improve the paper. D. Farnocchia, S. R., Chesley, and P. W. Chodas conducted this research at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. P. G. Brown received support for this study from NASA Cooperative agreement NNX11AB76A. P. G. Brown thanks the Canadian Hazard Information Service of Natural Resources Canada for technical support and IDC access as part of the Canadian National Data Center. NR 25 TC 1 Z9 1 U1 4 U2 4 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD AUG PY 2016 VL 274 BP 327 EP 333 DI 10.1016/j.icarus.2016.02.056 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DL8IM UT WOS:000375885700024 ER PT J AU Filacchione, G Capaccioni, F Ciarniello, M Raponi, A Tosi, F De Sanctis, MC Erard, S Morvan, DB Leyrat, C Arnold, G Schmitt, B Quirico, E Piccioni, G Migliorini, A Capria, MT Palomba, E Cerroni, P Longobardo, A Barucci, A Fornasier, S Carlson, RW Jaumann, R Stephan, K Moroz, LV Kappel, D Rousseau, B Fonti, S Mancarella, F Despan, D Faure, M AF Filacchione, Gianrico Capaccioni, Fabrizio Ciarniello, Mauro Raponi, Andrea Tosi, Federico De Sanctis, Maria Cristina Erard, Stephane Morvan, Dominique Bockelee Leyrat, Cedric Arnold, Gabriele Schmitt, Bernard Quirico, Eric Piccioni, Giuseppe Migliorini, Alessandra Capria, Maria Teresa Palomba, Ernesto Cerroni, Priscilla Longobardo, Andrea Barucci, Antonella Fornasier, Sonia Carlson, Robert W. Jaumann, Ralf Stephan, Katrin Moroz, Lyuba V. Kappel, David Rousseau, Batiste Fonti, Sergio Mancarella, Francesca Despan, Daniela Faure, Mathilde TI The global surface composition of 67P/CG nucleus by Rosetta/VIRTIS. (I) Prelanding mission phase SO ICARUS LA English DT Article DE Comets, composition; Comets, nucleus; Spectroscopy ID EXPOSED WATER ICE; COMET 67P/CHURYUMOV-GERASIMENKO; PHOTOMETRIC PROPERTIES; IMAGING SPECTROMETER; OSIRIS OBSERVATIONS; ONBOARD ROSETTA; IMHOTEP REGION; VIRTIS; SHAPE; H2O AB From August to November 2014 the Rosetta orbiter has performed an extensive observation campaign aimed at the characterization of 67P/CG nucleus properties and to the selection of the Philae landing site. The campaign led to the production of a global map of the illuminated portion of 67P/CG nucleus. During this prelanding phase the comet's heliocentric distance decreased from 3.62 to 2.93 AU while Rosetta was orbiting around the nucleus at distances between 100 to 10 km. VIRTIS-M, the Visible and InfraRed Thermal Imaging Spectrometer - Mapping channel (Coradini et al., [2007] Space Sci. Rev., 128, 529-559) onboard the orbiter, has acquired 0.25-5.1 mu m hyperspectral data of the entire illuminated surface, e.g. the north hemisphere and the equatorial regions, with spatial resolution between 2.5 and 25 m/pixel. I/F spectra have been corrected for thermal emission removal in the 3.5-5.1 mu m range and for surface's photometric response. The resulting reflectance spectra have been used to compute several Cometary Spectral Indicators (CSI): single scattering albedo at 0.55 mu m, 0.5-0.8 mu m and 1.0-2.5 mu m spectral slopes, 3.2 mu m organic material and 2.0 mu m water ice band parameters (center, depth) with the aim to map their spatial distribution on the surface and to study their temporal variability as the nucleus moved towards the Sun. Indeed, throughout the investigated period, the nucleus surface shows a significant increase of the single scattering albedo along with a decrease of the 0.5-0.8 and 1.0-2.5 mu m spectral slopes, indicating a flattening of the reflectance. We attribute the origin of this effect to the partial removal of the dust layer caused by the increased contribution of water sublimation to the gaseous activity as comet crossed the frost-line. The regions more active at the time of these observations, like Hapi in the neck/north pole area, appear brighter, bluer and richer in organic material than the rest of the large and small lobe of the nucleus. The parallel coordinates method (Inselberg [1985] Vis. Comput., 1, 69-91) has been used to identify associations between average values of the spectral indicators and the properties of the geomorphological units as defined by (Thomas et al., [2015] Science, 347, 6220) and (El-Maarr et al., [2015] Astron. Astrophys., 583, A26). Three classes have been identified (smooth/active areas, dust covered areas and depressions), which can be clustered on the basis of the 3.2 mu m organic material's band depth, while consolidated terrains show a high variability of the spectral properties resulting being distributed across all three classes. These results show how the spectral variability of the nucleus surface is more variegated than the morphological classes and that 67P/CG surface properties are dynamical, changing with the heliocentric distance and with activity processes. (C) 2016 Elsevier Inc. All rights reserved. C1 [Filacchione, Gianrico; Capaccioni, Fabrizio; Ciarniello, Mauro; Raponi, Andrea; Tosi, Federico; De Sanctis, Maria Cristina; Piccioni, Giuseppe; Migliorini, Alessandra; Capria, Maria Teresa; Palomba, Ernesto; Cerroni, Priscilla; Longobardo, Andrea] Ist Astrofis & Planetol Spaziali, INAF IAPS, Area Ric Tor Vergata, Via Fosso del Cavaliere 100, I-00133 Rome, Italy. [Erard, Stephane; Morvan, Dominique Bockelee; Leyrat, Cedric; Barucci, Antonella; Fornasier, Sonia; Rousseau, Batiste; Despan, Daniela] Univ Paris Diderot, UPMC, Observ Paris, LESIA,CNRS, F-92195 Meudon, France. [Arnold, Gabriele; Jaumann, Ralf; Stephan, Katrin; Moroz, Lyuba V.; Kappel, David] Deutsch Zentrum Luft & Raumfahrt DLR, Inst Planetary Res, Berlin, Germany. [Schmitt, Bernard; Quirico, Eric; Faure, Mathilde] Univ Grenoble Alpes, CNRS, IPAG, Grenoble, France. [Carlson, Robert W.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Fonti, Sergio; Mancarella, Francesca] Univ Salento, Dipartimento Matemat & Fis Ennio De Giorgi, Lecce, Italy. RP Filacchione, G (reprint author), Ist Astrofis & Planetol Spaziali, INAF IAPS, Area Ric Tor Vergata, Via Fosso del Cavaliere 100, I-00133 Rome, Italy. EM gianrico.filacchione@iaps.inaf.it RI Schmitt, Bernard/A-1064-2009; quirico, eric/K-9650-2013; OI Schmitt, Bernard/0000-0002-1230-6627; quirico, eric/0000-0003-2768-0694; Migliorini, Alessandra/0000-0001-7386-9215; Filacchione, Gianrico/0000-0001-9567-0055; Rousseau, Batiste/0000-0001-9247-7890; Palomba, Ernesto/0000-0002-9101-6774; Tosi, Federico/0000-0003-4002-2434 FU Italian Space Agency (ASI - Italy); Centre National d'Etudes Spatiales (CNES- France); Deutsches Zentrum fur Luft- and Raumfahrt (DLR-Germany); National Aeronautic and Space Administration (NASA-USA); ASI; CNES; DLR FX The authors would like to thank the following institutions and agencies, which supported this work: Italian Space Agency (ASI - Italy), Centre National d'Etudes Spatiales (CNES- France), Deutsches Zentrum fur Luft- and Raumfahrt (DLR-Germany), National Aeronautic and Space Administration (NASA-USA). VIRTIS was built by a consortium from Italy, France and Germany, under the scientific responsibility of IAPS, Istituto di Astrofisica e Planetologia Spaziali of INAF, Rome (IT), which lead also the scientific operations. The VIRTIS instrument development for ESA has been funded and managed by ASI, with contributions from Observatoire de Meudon financed by CNES and from DLR. The VIRTIS instrument industrial prime contractor was former Officine Galileo, now Selex ES (Finmeccanica Group) in Campi Bisenzio, Florence, IT. The authors wish to thank the Rosetta Liaison Scientists, the Rosetta Science Ground Segment and the Rosetta Mission Operations Centre for their support in planning the VIRTIS observations. The VIRTIS calibrated data will be available through the ESA's Planetary Science Archive (PSA) web site. This research has made use of NASA's Astrophysics Data System. NR 42 TC 5 Z9 5 U1 5 U2 12 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD AUG PY 2016 VL 274 BP 334 EP 349 DI 10.1016/j.icarus.2016.02.055 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DL8IM UT WOS:000375885700025 ER PT J AU Chyba, CF Hand, KP AF Chyba, Christopher F. Hand, Kevin P. TI Electric Power Generation from Earth's Rotation through its Own Magnetic Field SO PHYSICAL REVIEW APPLIED LA English DT Article ID AT-A-DISTANCE; UNIPOLAR INDUCTION; STATIC SITUATION; LINES; GAUGE; SHIELDS; COULOMB; THEOREM; MOTION AB We examine electric power generation from Earth's rotation through its own nonrotating magnetic field (that component of the field symmetric about Earth's rotation axis). There is a simple general proof that this is impossible. However, we identify a loophole in that proof and show that voltage can be continuously generated in a low-magnetic-Reynolds-number conductor rotating with Earth, provided magnetically permeable material is used to ensure curl (v x B-0) not equal 0 within the conductor, where B-0 derives from the axially symmetric component of Earth's magnetic flux density, and v is Earth's rotation velocity at the conductor's location. We solve the relevant equations for one laboratory realization, and from this solution, we predict the voltage magnitude and sign dependence on system dimensions and orientation relative to Earth's rotation. The effect, which would be available nearly globally with no intermittency, requires testing and further examination to see if it can be scaled to practical emission-free power generation. C1 [Chyba, Christopher F.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Chyba, Christopher F.] Princeton Univ, Woodrow Wilson Sch Publ & Int Affairs, Princeton, NJ 08544 USA. [Hand, Kevin P.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. RP Chyba, CF (reprint author), Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.; Chyba, CF (reprint author), Princeton Univ, Woodrow Wilson Sch Publ & Int Affairs, Princeton, NJ 08544 USA. EM cchyba@princeton.edu; Kevin.P.Hand@jpl.nasa.gov FU Woodrow Wilson School; Department of Astrophysical Sciences at Princeton University; Jet Propulsion Laboratory, California Institute of Technology; National Aeronautics and Space Administration; National Aeronautics and Space Administration Exobiology Program [NNH09ZDA001N] FX We thank three anonymous referees for their reviews, and we are grateful for helpful discussions with T. H. Chyba, R. L. Garwin, M. J. Rees, P. J. Thomas, E. L. Turner, and three anonymous colleagues. We thank G. Z. McDermott and G. Cooper for administrative support, B. A. Lin for reference assistance, and M. Northrup of National Magnetics Group Inc. for help with materials. C. F. C. acknowledges research funds from the Woodrow Wilson School and the Department of Astrophysical Sciences at Princeton University. K. P. H. acknowledges support through the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration, and through the National Aeronautics and Space Administration Exobiology Program (Grant No. NNH09ZDA001N). NR 67 TC 0 Z9 0 U1 2 U2 2 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 2331-7019 J9 PHYS REV APPL JI Phys. Rev. Appl. PD JUL 29 PY 2016 VL 6 IS 1 AR 014017 DI 10.1103/PhysRevApplied.6.014017 PG 18 WC Physics, Applied SC Physics GA DT5CV UT WOS:000381499200002 ER PT J AU Breuillard, H Le Contel, O Retino, A Chasapis, A Chust, T Mirioni, L Graham, DB Wilder, FD Cohen, I Vaivads, A Khotyaintsev, YV Lindqvist, PA Marklund, GT Burch, JL Torbert, RB Ergun, RE Goodrich, KA Macri, J Needell, J Chutter, M Rau, D Dors, I Russell, CT Magnes, W Strangeway, RJ Bromund, KR Plaschke, F Fischer, D Leinweber, HK Anderson, BJ Le, G Slavin, JA Kepko, EL Baumjohann, W Mauk, B Fuselier, SA Nakamura, R AF Breuillard, H. Le Contel, O. Retino, A. Chasapis, A. Chust, T. Mirioni, L. Graham, D. B. Wilder, F. D. Cohen, I. Vaivads, A. Khotyaintsev, Yu V. Lindqvist, P. -A. Marklund, G. T. Burch, J. L. Torbert, R. B. Ergun, R. E. Goodrich, K. A. Macri, J. Needell, J. Chutter, M. Rau, D. Dors, I. Russell, C. T. Magnes, W. Strangeway, R. J. Bromund, K. R. Plaschke, F. Fischer, D. Leinweber, H. K. Anderson, B. J. Le, G. Slavin, J. A. Kepko, E. L. Baumjohann, W. Mauk, B. Fuselier, S. A. Nakamura, R. TI Multispacecraft analysis of dipolarization fronts and associated whistler wave emissions using MMS data SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE Earth magnetotail; dipolarization fronts ID KINETIC BALLOONING/INTERCHANGE INSTABILITY; ELECTROMAGNETIC ENERGY-CONVERSION; PLASMA SHEET; RECONNECTION; MAGNETOTAIL; SIMULATIONS; TURBULENCE; DRIVEN; FLOW AB Dipolarization fronts (DFs), embedded in bursty bulk flows, play a crucial role in Earth's plasma sheet dynamics because the energy input from the solar wind is partly dissipated in their vicinity. This dissipation is in the form of strong low-frequency waves that can heat and accelerate energetic electrons up to the high-latitude plasma sheet. However, the dynamics of DF propagation and associated low-frequency waves in the magnetotail are still under debate due to instrumental limitations and spacecraft separation distances. In May 2015 the Magnetospheric Multiscale (MMS) mission was in a string-of-pearls configuration with an average intersatellite distance of 160km, which allows us to study in detail the microphysics of DFs. Thus, in this letter we employ MMS data to investigate the properties of dipolarization fronts propagating earthward and associated whistler mode wave emissions. We show that the spatial dynamics of DFs are below the ion gyroradius scale in this region (approximate to 500km), which can modify the dynamics of ions in the vicinity of the DF (e.g., making their motion nonadiabatic). We also show that whistler wave dynamics have a temporal scale of the order of the ion gyroperiod (a few seconds), indicating that the perpendicular temperature anisotropy can vary on such time scales. C1 [Breuillard, H.; Le Contel, O.; Retino, A.; Chust, T.; Mirioni, L.] CNRS, LPP, UMR, Paris, France. [Chasapis, A.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA. [Graham, D. B.; Vaivads, A.; Khotyaintsev, Yu V.; Mauk, B.] Swedish Inst Space Phys, Uppsala, Sweden. [Wilder, F. D.; Ergun, R. E.; Goodrich, K. A.] Univ Colorado, LASP, Boulder, CO 80309 USA. [Cohen, I.; Anderson, B. J.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA. [Lindqvist, P. -A.; Marklund, G. T.] Royal Inst Technol, Alfven Lab, Stockholm, Sweden. [Burch, J. L.] Southwest Res Inst, San Antonio, TX USA. [Torbert, R. B.; Macri, J.; Needell, J.; Chutter, M.; Rau, D.; Dors, I.] Univ New Hampshire, Ctr Space Sci, Durham, NH 03824 USA. [Torbert, R. B.; Macri, J.; Needell, J.; Chutter, M.; Rau, D.; Dors, I.] Univ New Hampshire, Dept Phys, Durham, NH 03824 USA. [Russell, C. T.; Strangeway, R. J.; Leinweber, H. K.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90024 USA. [Magnes, W.; Plaschke, F.; Fischer, D.; Baumjohann, W.; Nakamura, R.] Austrian Acad Sci, Space Res Inst IWF, Graz, Austria. [Bromund, K. R.; Le, G.; Kepko, E. L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA. [Slavin, J. A.] Univ Michigan, Dept Climate & Space Sci & Engn, Ann Arbor, MI 48109 USA. [Fuselier, S. A.] Univ Texas San Antonio, Dept Phys & Astron, San Antonio, TX USA. RP Breuillard, H (reprint author), CNRS, LPP, UMR, Paris, France. EM hugo.breuillard@lpp.polytechnique.fr RI NASA MMS, Science Team/J-5393-2013; Cohen, Ian/K-3038-2015; Le, Guan/C-9524-2012; Slavin, James/H-3170-2012; Mauk, Barry/E-8420-2017 OI NASA MMS, Science Team/0000-0002-9504-5214; Cohen, Ian/0000-0002-9163-6009; Le, Guan/0000-0002-9504-5214; Slavin, James/0000-0002-9206-724X; Mauk, Barry/0000-0001-9789-3797 FU CNES; CNRS-INSIS; CNRS-INSU FX H.B.'s work has been supported by CNES through the grant "Allocations de recherche post-doctorale." The French involment (SCM) on MMS is supported by CNES, CNRS-INSIS, and CNRS-INSU. Used data are available at https://lasp.colorado.edu/mms/sdc. NR 56 TC 4 Z9 4 U1 8 U2 8 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD JUL 28 PY 2016 VL 43 IS 14 BP 7279 EP 7286 DI 10.1002/2016GL069188 PG 8 WC Geosciences, Multidisciplinary SC Geology GA DV9VL UT WOS:000383290200001 ER PT J AU Lee, SH Sibeck, DG Hwang, KJ Wang, Y Silveira, MVD Fok, MC Mauk, BH Cohen, IJ Ruohoniemi, JM Kitamura, N Burch, JL Giles, BL Torbert, RB Russell, CT Lester, M AF Lee, S. H. Sibeck, D. G. Hwang, K. -J. Wang, Y. Silveira, M. V. D. Fok, M. -C. Mauk, B. H. Cohen, I. J. Ruohoniemi, J. M. Kitamura, N. Burch, J. L. Giles, B. L. Torbert, R. B. Russell, C. T. Lester, M. TI Inverse energy dispersion of energetic ions observed in the magnetosheath SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE particle escape; energetic ions; magnetosheath; magnetic reconnection; solar wind-magnetosphere interaction ID UPSTREAM PRESSURE VARIATIONS; OXYGEN IONS; DAYSIDE MAGNETOPAUSE; MAGNETOSPHERIC IONS; BOW SHOCK; ACCELERATION; SIGNATURES; RECONNECTION; LATITUDES; LEAKAGE AB We present a case study of energetic ions observed by the Energetic Particle Detector (EPD) on the Magnetospheric Multiscale spacecraft in the magnetosheath just outside the subsolar magnetopause that occurred at 1000UT on 8 December 2015. As the magnetopause receded inward, the EPD observed a burst of energetic (approximate to 50-1000keV) proton, helium, and oxygen ions that exhibited an inverse dispersion, with the lowest energy ions appearing first. The prolonged interval of fast antisunward flow observed in the magnetosheath and transient increases in the H components of global ground magnetograms demonstrate that the burst appeared at a time when the magnetosphere was rapidly compressed. We attribute the inverse energy dispersion to the leakage along reconnected magnetic field lines of betatron-accelerated energetic ions in the magnetosheath, and a burst of reconnection has an extent of about 1.5R(E) using combined Super Dual Auroral Radar Network radar and EPD observations. C1 [Lee, S. H.; Sibeck, D. G.; Hwang, K. -J.; Silveira, M. V. D.; Fok, M. -C.; Giles, B. L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Hwang, K. -J.] Univ Maryland, Goddard Planetary & Heliophys Inst, Baltimore, MD 21201 USA. [Wang, Y.] Peking Univ, Sch Earth & Space Sci, Inst Space Phys & Appl Technol, Beijing 100871, Peoples R China. [Mauk, B. H.; Cohen, I. J.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA. [Ruohoniemi, J. M.] Virginia Polytech Inst & State Univ, Bradley Dept Elect & Comp Engn, Blacksburg, VA 24061 USA. [Kitamura, N.] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Sagamihara, Kanagawa, Japan. [Burch, J. L.] Southwest Res Inst, San Antonio, TX USA. [Torbert, R. B.] Univ New Hampshire, Ctr Space Sci, Durham, NH 03824 USA. [Russell, C. T.] Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90024 USA. [Lester, M.] Univ Leicester, Dept Phys & Astron, Leicester, Leics, England. RP Lee, SH (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM sun.h.lee@nasa.gov RI NASA MMS, Science Team/J-5393-2013; Cohen, Ian/K-3038-2015; Lester, Mark/C-9657-2016; Mauk, Barry/E-8420-2017 OI NASA MMS, Science Team/0000-0002-9504-5214; Cohen, Ian/0000-0002-9163-6009; Lester, Mark/0000-0001-7353-5549; Mauk, Barry/0000-0001-9789-3797 FU NASA; MMS project; NSF [AGS-1341918]; NERC [NE/K011766/1]; national scientific agency of Australia; national scientific agency of Canada; national scientific agency of China; national scientific agency of France; national scientific agency of Japan; national scientific agency of South Africa; national scientific agency of United Kingdom; national scientific agency of United States; AFOSR FX We thank the FGM, FPI, and EPD instrument teams of MMS mission and ARTEMIS mission for the successful spacecraft operation and for providing plasma and magnetic field data. This research was supported by an appointment to the NASA Postdoctoral Program appointment at the NASA/GSFC, administered by Universities Space Research Association through a contract with NASA. Some of the work conducted at NASA/GSFC was supported by the MMS project. J.M.R. acknowledges the support of NSF under AGS-1341918. M.L. is supported by NERC grant NE/K011766/1. The SuperDARN radars are funded by the national scientific agencies of Australia, Canada, China, France, Japan, South Africa, United Kingdom, and the United States. We thank the team of Katie Herlingshaw, Suzie Imber, Hammed Lawal, Tim Yeoman, Jasmine Sandhu, Rosie Johnson, and Timothy David at the University of Leicester who collected the Hankasalmi radar data used in this paper which supported the CAPER rocket campaign. We thank the national institutes that support them and INTERMAGNET for promoting high standards of magnetic observatory practice. We also thank E. Yizengaw, E. Zesta, M.B. Moldwin, and the rest of the AMBER team for the data. AMBER is operated by Boston College and funded by NASA and AFOSR. The Kp and Dst indices were provided by the website (http://wdc.kugi.kyoto-u.ac.jp/). NR 31 TC 0 Z9 0 U1 0 U2 0 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD JUL 28 PY 2016 VL 43 IS 14 BP 7338 EP 7347 DI 10.1002/2016GL069840 PG 10 WC Geosciences, Multidisciplinary SC Geology GA DV9VL UT WOS:000383290200008 ER PT J AU Jaynes, AN Turner, DL Wilder, FD Osmane, A Baker, DN Blake, JB Fennell, JF Cohen, IJ Mauk, BH Reeves, GD Ergun, RE Giles, BL Gershman, DJ Torbert, RB Burch, JL AF Jaynes, A. N. Turner, D. L. Wilder, F. D. Osmane, A. Baker, D. N. Blake, J. B. Fennell, J. F. Cohen, I. J. Mauk, B. H. Reeves, G. D. Ergun, R. E. Giles, B. L. Gershman, D. J. Torbert, R. B. Burch, J. L. TI Energetic electron acceleration observed by MMS in the vicinity of an X-line crossing SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE electron acceleration; wave-particle interactions; VLF waves; magnetopause; dayside reconnection; MMS ID MAGNETIC RECONNECTION; LATITUDE MAGNETOPAUSE; WAVES; LAYER AB During the first months of observations, the Magnetospheric Multiscale Fly's Eye Energetic Particle Spectrometer instrument has observed several instances of electron acceleration up to >100keV while in the vicinity of the dayside reconnection region. While particle acceleration associated with magnetic reconnection has been seen to occur up to these energies in the tail region, it had not yet been reported at the magnetopause. This study reports on observations of electron acceleration up to hundreds of keV that were recorded on 19 September 2015 around 1000 UT, in the midst of an X-line crossing. In the region surrounding the X-line, whistler-mode and broadband electrostatic waves were observed simultaneously with the appearance of highly energetic electrons which exhibited significant energization in the perpendicular direction. The mechanisms by which particles may be accelerated via reconnection-related processes are intrinsic to understanding particle dynamics among a wide range of spatial scales and plasma environments. C1 [Jaynes, A. N.; Wilder, F. D.; Baker, D. N.; Ergun, R. E.] Univ Colorado, Lab Atmospher & Space Phys, Boulder, CO 80309 USA. [Turner, D. L.; Blake, J. B.; Fennell, J. F.] Aerosp Corp, Dept Space Sci, El Segundo, CA 90245 USA. [Osmane, A.] Aalto Univ, Dept Radio Sci & Engn, Helsinki, Finland. [Cohen, I. J.; Mauk, B. H.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA. [Reeves, G. D.] Los Alamos Natl Lab, Los Alamos, NM USA. [Giles, B. L.; Gershman, D. J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA. [Torbert, R. B.] Univ New Hampshire, Ctr Space Sci, Durham, NH 03824 USA. [Burch, J. L.] Southwest Res Inst, San Antonio, TX USA. RP Jaynes, AN (reprint author), Univ Colorado, Lab Atmospher & Space Phys, Boulder, CO 80309 USA. EM allison.jaynes@lasp.colorado.edu RI NASA MMS, Science Team/J-5393-2013; Cohen, Ian/K-3038-2015; Mauk, Barry/E-8420-2017; OI NASA MMS, Science Team/0000-0002-9504-5214; Cohen, Ian/0000-0002-9163-6009; Mauk, Barry/0000-0001-9789-3797; Reeves, Geoffrey/0000-0002-7985-8098 FU MMS mission, under NASA [NNG04EB99C] FX This work was supported by funding from the MMS mission, under NASA contract NNG04EB99C. The data presented here are publicly available on the MMS Science Data Center website: https://lasp.colorado.edu/mms/sdc/ or by request for dates earlier than 1 September 2015. Solar wind OMNI data from ACE and Wind are available via the Space Physics Data Facility at http://cdaweb.gsfc.nasa.gov/istp_public/. NR 32 TC 2 Z9 2 U1 4 U2 4 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD JUL 28 PY 2016 VL 43 IS 14 BP 7356 EP 7363 DI 10.1002/2016GL069206 PG 8 WC Geosciences, Multidisciplinary SC Geology GA DV9VL UT WOS:000383290200010 ER PT J AU Yizengaw, E Moldwin, MB Zesta, E Magoun, M Pradipta, R Biouele, CM Rabiu, AB Obrou, OK Bamba, Z de Paula, ER AF Yizengaw, E. Moldwin, M. B. Zesta, E. Magoun, M. Pradipta, R. Biouele, C. M. Rabiu, A. B. Obrou, O. K. Bamba, Z. de Paula, E. R. TI Response of the equatorial ionosphere to the geomagnetic DP 2 current system SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE DP 2 current; equatorial electrodynamics ID ELECTRIC-FIELD; PENETRATION; SUBSTORMS AB The response of equatorial ionosphere to the magnetospheric origin DP 2 current system fluctuations is examined using ground-based multiinstrument observations. The interaction between the solar wind and magnetosphere generates a convection electric field that can penetrate to the ionosphere and cause the DP 2 current system. The quasiperiodic DP 2 current system, which fluctuates coherently with fluctuations of the interplanetary magnetic field (IMF) B-z, penetrates nearly instantaneously to the dayside equatorial region at all longitudes and modulates the electrodynamics that governs the equatorial density distributions. In this paper, using magnetometers at high and equatorial latitudes, we demonstrate that the quasiperiodic DP 2 current system penetrates to the equator and causes the dayside equatorial electrojet (EEJ) and the independently measured ionospheric drift velocity to fluctuate coherently with the high-latitude DP 2 current as well as with the IMF B-z component. At the same time, radar observations show that the ionospheric density layers move up and down, causing the density to fluctuate up and down coherently with the EEJ and IMF B-z. C1 [Yizengaw, E.; Magoun, M.; Pradipta, R.] Boston Coll, Inst Sci Res, Boston, MA USA. [Moldwin, M. B.] Univ Michigan, Dept Climate Space Sci & Engn, Ann Arbor, MI 48109 USA. [Zesta, E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA. [Biouele, C. M.] Univ Yaounde, Dept Phys, Yaounde, Cameroon. [Rabiu, A. B.] Natl Space Res & Dev Agcy, Abuja, Nigeria. [Obrou, O. K.] Univ Felix Houphouet Boigny FHB, Lab Phys Atmosphere, Abidjan, Cote Ivoire. [Bamba, Z.] Ctr Rech Sci Conakry Rogbane, Conakry, Guinea. [de Paula, E. R.] Inst Nacl Pesquisas Espaciais, Sao Jose Dos Campos, Brazil. RP Yizengaw, E (reprint author), Boston Coll, Inst Sci Res, Boston, MA USA. EM Kassie@bc.edu FU AFOSR [FA9550-12-1-0437, FA9550-15-1-0399]; NSF [AGS145136, AGS1450512] FX This work has been partially supported by AFOSR (FA9550-12-1-0437 and FA9550-15-1-0399) and NSF (AGS145136 and AGS1450512) grants. The authors are indebted to the Jicamarca Radio Observatory and INTERMAGNET team for the magnetometer data resources they made available to the public. We also thank the Global Ionospheric Radio Observatory team for the ionosonde data. The solar wind data were obtained from the CDAWeb database. NR 18 TC 0 Z9 0 U1 0 U2 0 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD JUL 28 PY 2016 VL 43 IS 14 BP 7364 EP 7372 DI 10.1002/2016GL070090 PG 9 WC Geosciences, Multidisciplinary SC Geology GA DV9VL UT WOS:000383290200011 ER PT J AU Plaschke, F Kahr, N Fischer, D Nakamura, R Baumjohann, W Magnes, W Burch, JL Torbert, RB Russell, CT Giles, BL Strangeway, RJ Leinweber, HK Bromund, KR Anderson, BJ Le, G Chutter, M Slavin, JA Kepko, EL AF Plaschke, F. Kahr, N. Fischer, D. Nakamura, R. Baumjohann, W. Magnes, W. Burch, J. L. Torbert, R. B. Russell, C. T. Giles, B. L. Strangeway, R. J. Leinweber, H. K. Bromund, K. R. Anderson, B. J. Le, G. Chutter, M. Slavin, J. A. Kepko, E. L. TI Steepening of waves at the duskside magnetopause SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE magnetopause; surface wave; steepening; Kelvin-Helmholtz instability; plasma depletion layer; Magnetospheric Multiscale ID INTERPLANETARY MAGNETIC-FIELD; KELVIN-HELMHOLTZ INSTABILITY; SOLAR-WIND; MAGNETOSPHERE; BOUNDARY; PLASMA; LAYER; SHAPE; FLOW AB Surface waves at the magnetopause flanks typically feature steeper, i.e., more inclined leading (antisunward facing) than trailing (sunward facing) edges. This is expected for Kelvin-Helmholtz instability (KHI) amplified waves. Very rarely, during northward interplanetary magnetic field (IMF) conditions, anomalous/inverse steepening has been observed. The small-scale tetrahedral configuration of the Magnetospheric Multiscale spacecraft and their high time resolution measurements enable us to routinely ascertain magnetopause boundary inclinations during surface wave passage with high accuracy by four-spacecraft timing analysis. At the dusk flank magnetopause, 77%/23% of the analyzed wave intervals exhibit regular/inverse steepening. Inverse steepening happens during northward IMF conditions, as previously reported and, in addition, during intervals of dominant equatorial IMF. Inverse steepening observed under the latter conditions may be due to the absence of KHI or due to instabilities arising from the alignment of flow and magnetic fields in the magnetosheath. C1 [Plaschke, F.; Kahr, N.; Fischer, D.; Nakamura, R.; Baumjohann, W.; Magnes, W.] Austrian Acad Sci, Space Res Inst, Graz, Austria. [Burch, J. L.; Torbert, R. B.] Southwest Res Inst, San Antonio, TX USA. [Torbert, R. B.; Chutter, M.] Univ New Hampshire, Inst Study Earth Oceans & Space, Durham, NH 03824 USA. [Russell, C. T.; Strangeway, R. J.; Leinweber, H. K.] Univ Calif Los Angeles, Dept Earth Planetary & Space Sci, Los Angeles, CA USA. [Giles, B. L.; Bromund, K. R.; Le, G.; Kepko, E. L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA. [Anderson, B. J.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA. [Slavin, J. A.] Univ Michigan, Dept Climate & Space Sci & Engn, Ann Arbor, MI 48109 USA. RP Plaschke, F (reprint author), Austrian Acad Sci, Space Res Inst, Graz, Austria. EM Ferdinand.Plaschke@oeaw.ac.at RI NASA MMS, Science Team/J-5393-2013; Le, Guan/C-9524-2012; Slavin, James/H-3170-2012 OI NASA MMS, Science Team/0000-0002-9504-5214; Le, Guan/0000-0002-9504-5214; Slavin, James/0000-0002-9206-724X FU NASA [NNG04EB99C]; Austrian Academy of Sciences; Austrian Space Applications Programme [FFG/ASAP-844377] FX The dedication and expertise of the Magnetopheric MultiScale (MMS) development and operations teams are greatly appreciated. Work at JHU/APL, UCLA, UNH, and SwRI was supported by NASA contract NNG04EB99C. We acknowledge the use of merged magnetic field measurements that are based on burst FluxGate Magnetometer (FGM) data from the Digital Flux-Gate (DFG) magnetometers and burst Search Coil Magnetometer (SCM) data. Furthermore, we acknowledge the use of fast survey Fast Plasma Investigation (FPI) data. The FPI data are stored at the MMS Science Data Center https://lasp.colorado.edu/mms/sdc/ and are publicly available. The merged magnetic field data are available upon request. The Austrian part of the development, operation, and calibration of the DFG was financially supported by rolling grant of the Austrian Academy of Sciences and the Austrian Space Applications Programme with the contract FFG/ASAP-844377. NR 33 TC 0 Z9 0 U1 2 U2 2 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD JUL 28 PY 2016 VL 43 IS 14 BP 7373 EP 7380 DI 10.1002/2016GL070003 PG 8 WC Geosciences, Multidisciplinary SC Geology GA DV9VL UT WOS:000383290200012 ER PT J AU Lanza, NL Wiens, RC Arvidson, RE Clark, BC Fischer, WW Gellert, R Grotzinger, JP Hurowitz, JA McLennan, SM Morris, RV Rice, MS Bell, JF Berger, JA Blaney, DL Bridges, NT Calef, F Campbell, JL Clegg, SM Cousin, A Edgett, KS Fabre, C Fisk, MR Forni, O Frydenvang, J Hardy, KR Hardgrove, C Johnson, JR Lasue, J Le Mouelic, S Malin, MC Mangold, N Martin-Torres, J Maurice, S McBride, MJ Ming, DW Newsom, HE Ollila, AM Sautter, V Schroder, S Thompson, LM Treiman, AH VanBommel, S Vaniman, DT Zorzano, MP AF Lanza, Nina L. Wiens, Roger C. Arvidson, Raymond E. Clark, Benton C. Fischer, Woodward W. Gellert, Ralf Grotzinger, John P. Hurowitz, Joel A. McLennan, Scott M. Morris, Richard V. Rice, Melissa S. Bell, James F., III Berger, Jeffrey A. Blaney, Diana L. Bridges, Nathan T. Calef, Fred, III Campbell, John L. Clegg, Samuel M. Cousin, Agnes Edgett, Kenneth S. Fabre, Cecile Fisk, Martin R. Forni, Olivier Frydenvang, Jens Hardy, Keian R. Hardgrove, Craig Johnson, Jeffrey R. Lasue, Jeremie Le Mouelic, Stephane Malin, Michael C. Mangold, Nicolas Martin-Torres, Javier Maurice, Sylvestre McBride, Marie J. Ming, Douglas W. Newsom, Horton E. Ollila, Ann M. Sautter, Violaine Schroder, Susanne Thompson, Lucy M. Treiman, Allan H. VanBommel, Scott Vaniman, David T. Zorzano, Maria-Paz TI Oxidation of manganese in an ancient aquifer, Kimberley formation, Gale crater, Mars SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE Mars; manganese; oxidation; MSL; ChemCam ID ATMOSPHERE; MINERALOGY; CHEMISTRY; EVOLUTION; ORIGIN; DIFFRACTION; DIAGENESIS; ROCKNEST; COATINGS; SULFUR AB The Curiosity rover observed high Mn abundances (>25wt % MnO) in fracture-filling materials that crosscut sandstones in the Kimberley region of Gale crater, Mars. The correlation between Mn and trace metal abundances plus the lack of correlation between Mn and elements such as S, Cl, and C, reveals that these deposits are Mn oxides rather than evaporites or other salts. On Earth, environments that concentrate Mn and deposit Mn minerals require water and highly oxidizing conditions; hence, these findings suggest that similar processes occurred on Mars. Based on the strong association between Mn-oxide deposition and evolving atmospheric dioxygen levels on Earth, the presence of these Mn phases on Mars suggests that there was more abundant molecular oxygen within the atmosphere and some groundwaters of ancient Mars than in the present day. C1 [Lanza, Nina L.; Wiens, Roger C.; Clegg, Samuel M.; Ollila, Ann M.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA. [Arvidson, Raymond E.] Washington Univ, Dept Earth & Planetary Sci, St Louis, MO 63130 USA. [Clark, Benton C.] Space Sci Inst, Boulder, CO USA. [Fischer, Woodward W.; Grotzinger, John P.] CALTECH, Pasadena, CA 91125 USA. [Gellert, Ralf; Campbell, John L.; VanBommel, Scott] Univ Guelph, Guelph, ON, Canada. [Hurowitz, Joel A.; McLennan, Scott M.] SUNY Stony Brook, Dept Geosci, Stony Brook, NY 11794 USA. [Morris, Richard V.; Ming, Douglas W.] NASA, Johnson Space Ctr, Houston, TX USA. [Rice, Melissa S.] Western Washington Univ, Dept Geol, Bellingham, WA 98225 USA. [Bell, James F., III; Hardgrove, Craig] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ USA. [Berger, Jeffrey A.] Univ Western Ontario, Dept Earth Sci, London, ON, Canada. [Blaney, Diana L.; Calef, Fred, III] Jet Prop Lab, Pasadena, CA USA. [Bridges, Nathan T.; Johnson, Jeffrey R.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA. [Cousin, Agnes; Forni, Olivier; Lasue, Jeremie; Maurice, Sylvestre; Schroder, Susanne] Inst Rech Astrophys & Planetol, Toulouse, France. [Edgett, Kenneth S.; Malin, Michael C.] Malin Space Sci Syst, San Diego, CA USA. [Fabre, Cecile] Univ Lorraine, GeoRessources Lab, Nancy, France. [Fisk, Martin R.] Oregon State Univ, Coll Earth Ocean & Atmospher Sci, Corvallis, OR 97331 USA. [Frydenvang, Jens] Univ Copenhagen, Niels Bohr Inst, Copenhagen, Denmark. [Hardy, Keian R.] US Naval Acad, Aerosp Engn, Annapolis, MD 21402 USA. [Le Mouelic, Stephane; Mangold, Nicolas] Univ Nantes, CNRS, LPGNantes, UMR 6112, Nantes, France. [Martin-Torres, Javier; Zorzano, Maria-Paz] Lulea Univ Technol, Dept Comp Sci Elect & Space Engn, Kiruna, Sweden. [Martin-Torres, Javier] Inst Andaluz Ciencias Tierra CSIC UGR, Granada, Spain. [McBride, Marie J.] Purdue Univ, Earth Atmospher & Planetary Sci, W Lafayette, IN 47907 USA. [Newsom, Horton E.] Univ New Mexico, Inst Meteorit, Albuquerque, NM 87131 USA. [Sautter, Violaine] Museum Hist Nat, IMPMC, Paris, France. [Thompson, Lucy M.] Univ New Brunswick, Planetary & Space Sci Ctr, Fredericton, NB, Canada. [Treiman, Allan H.] Lunar & Planetary Inst, 3303 NASA Rd 1, Houston, TX 77058 USA. [Vaniman, David T.] Planetary Sci Inst, Tucson, AZ USA. [Zorzano, Maria-Paz] Ctr Astrobiol INTA CSIC, Madrid, Spain. RP Lanza, NL (reprint author), Los Alamos Natl Lab, Los Alamos, NM 87545 USA. EM nlanza@lanl.gov RI Frydenvang, Jens/D-4781-2013; Zorzano, Maria-Paz/F-2184-2015; OI Frydenvang, Jens/0000-0001-9294-1227; Zorzano, Maria-Paz/0000-0002-4492-9650; Clegg, Sam/0000-0002-0338-0948 FU NASA's Mars Program Office; Centre National d'Etude Spatiale; Canadian Space Agency FX We gratefully acknowledge the very helpful comments of M. Osterloo and N. Tosca. This research was carried out in the U.S. under contract from NASA's Mars Program Office. Work in France was carried out with funding from the Centre National d'Etude Spatiale and in Canada by the Canadian Space Agency. This team acknowledges the Jet Propulsion Laboratory for developing and leading the Mars Science Laboratory (MSL) Curiosity rover mission. The data reported in this paper are archived at the Planetary Data System, accessible at http://pds-geosciences.wustl.edu/missions/msl/index.htm. Additional data are available as supporting information. NR 50 TC 3 Z9 3 U1 17 U2 17 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD JUL 28 PY 2016 VL 43 IS 14 BP 7398 EP 7407 DI 10.1002/2016GL069109 PG 10 WC Geosciences, Multidisciplinary SC Geology GA DV9VL UT WOS:000383290200015 ER PT J AU Byrne, PK Ostrach, LR Fassett, CI Chapman, CR Denevi, BW Evans, AJ Klimczak, C Banks, ME Head, JW Solomon, SC AF Byrne, Paul K. Ostrach, Lillian R. Fassett, Caleb I. Chapman, Clark R. Denevi, Brett W. Evans, Alexander J. Klimczak, Christian Banks, Maria E. Head, James W. Solomon, Sean C. TI Widespread effusive volcanism on Mercury likely ended by about 3.5Ga SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE Mercury; volcanism; crater size-frequency distributions; global contraction; impact cratering ID 1ST MESSENGER FLYBY; INNER SOLAR-SYSTEM; SMOOTH PLAINS; GLOBAL CONTRACTION; CRATER CHRONOLOGY; EVOLUTION; ERUPTIONS; ORIGIN; STRATIGRAPHY; INTERIOR AB Crater size-frequency analyses have shown that the largest volcanic plains deposits on Mercury were emplaced around 3.7Ga, as determined with recent model production function chronologies for impact crater formation on that planet. To test the hypothesis that all major smooth plains on Mercury were emplaced by about that time, we determined crater size-frequency distributions for the nine next-largest deposits, which we interpret also as volcanic. Our crater density measurements are consistent with those of the largest areas of smooth plains on the planet. Model ages based on recent crater production rate estimates for Mercury imply that the main phase of plains volcanism on Mercury had ended by similar to 3.5Ga, with only small-scale volcanism enduring beyond that time. Cessation of widespread effusive volcanism is attributable to interior cooling and contraction of the innermost planet. C1 [Byrne, Paul K.] North Carolina State Univ, Dept Marine Earth & Atmospher Sci, Planetary Res Grp, Raleigh, NC 27695 USA. [Byrne, Paul K.; Klimczak, Christian; Solomon, Sean C.] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DE USA. [Ostrach, Lillian R.] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD USA. [Fassett, Caleb I.] Mt Holyoke Coll, Dept Astron, S Hadley, MA 01075 USA. [Chapman, Clark R.; Evans, Alexander J.] Southwest Res Inst, Dept Space Studies, Boulder, CO USA. [Denevi, Brett W.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA. [Evans, Alexander J.; Solomon, Sean C.] Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY USA. [Klimczak, Christian] Univ Georgia, Dept Geol, Athens, GA 30602 USA. [Banks, Maria E.] Smithsonian Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DE USA. [Banks, Maria E.] Planetary Sci Inst, Tucson, AZ USA. [Head, James W.] Brown Univ, Dept Earth Environm & Planetary Sci, Providence, RI 02912 USA. RP Byrne, PK (reprint author), North Carolina State Univ, Dept Marine Earth & Atmospher Sci, Planetary Res Grp, Raleigh, NC 27695 USA. EM paul.byrne@ncsu.edu RI Denevi, Brett/I-6502-2012 OI Denevi, Brett/0000-0001-7837-6663 FU NASA Discovery Program [NASW-00002, NAS5-97271]; North Carolina State University; NASA [NNX14AR88G] FX We thank David A. Rothery and an anonymous reviewer for their comments that helped improve the paper. We also thank Greg Michael for his help with the application of Poisson timing analysis with Craterstats to this study. The MESSENGER project is supported by the NASA Discovery Program under contracts NASW-00002 to the Carnegie Institution of Washington and NAS5-97271 to The Johns Hopkins University Applied Physics Laboratory. P.K.B. acknowledges support from North Carolina State University faculty start-up funds. C.I.F. is supported on this study by NASA grant NNX14AR88G. All MESSENGER data used in this paper are publicly available at the NASA Planetary Data System (PDS). This research made use of NASA's PDS and Astrophysics Data System. NR 61 TC 5 Z9 5 U1 4 U2 4 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD JUL 28 PY 2016 VL 43 IS 14 BP 7408 EP 7416 DI 10.1002/2016GL069412 PG 9 WC Geosciences, Multidisciplinary SC Geology GA DV9VL UT WOS:000383290200016 ER PT J AU Huang, MH Tung, H Fielding, EJ Huang, HH Liang, CR Huang, C Hu, JC AF Huang, Mong-Han Tung, Hsin Fielding, Eric J. Huang, Hsin-Hua Liang, Cunren Huang, Chung Hu, Jyr-Ching TI Multiple fault slip triggered above the 2016 M-w 6.4 MeiNong earthquake in Taiwan SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE coseismic deformation; finite source inversion; stress triggering; SW Taiwan tectonics ID JOINT INVERSION; WAVEFORM DATA; GEODETIC DATA; DEFORMATION; CALIFORNIA; RUPTURE; SEISMICITY; THRUST AB Rapid shortening in convergent mountain belts is often accommodated by slip on faults at multiple levels in upper crust, but no geodetic observation of slip at multiple levels within hours of a moderate earthquake has been shown before. Here we show clear evidence of fault slip within a shallower thrust at 5-10km depth in SW Taiwan triggered by the 2016 M-w 6.4 MeiNong earthquake at 15-20km depth. We constrain the primary coseismic fault slip with kinematic modeling of seismic and geodetic measurements and constrain the triggered slip and fault geometry using synthetic aperture radar interferometry. The shallower thrust coincides with a proposed duplex located in a region of high fluid pressure and high interseismic uplift rate, and may be sensitive to stress perturbations. Our results imply that under tectonic conditions such as high-background stress level and high fluid pressure, a moderate lower crustal earthquake can trigger faults at shallower depth. C1 [Huang, Mong-Han; Fielding, Eric J.; Liang, Cunren] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91125 USA. [Tung, Hsin; Huang, Chung; Hu, Jyr-Ching] Natl Taiwan Univ, Dept Geosci, Taipei, Taiwan. [Huang, Hsin-Hua] CALTECH, Seismol Lab, Pasadena, CA 91125 USA. [Huang, Hsin-Hua] Univ Utah, Dept Geol & Geophys, Salt Lake City, UT 84112 USA. RP Huang, MH (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91125 USA. EM mong@seismo.berkeley.edu RI Fielding, Eric/A-1288-2007; OI Fielding, Eric/0000-0002-6648-8067; Huang, Mong-Han/0000-0003-2331-3766 FU NASA Earth Surface and Interior focus area; NASA FX We thank D. Dreger for providing the codes for computing data weighting, smoothing, and inversions. The Central Weather Bureau, Taiwan and C.-H. Chang provided the aftershock relocations based on Shin et al. [2013]. We thank IRIS/DMC for data services and management. Discussion with M. Simons, Y.-R. Hsu, J. Suppe, R. Burgmann, C. Johnson, A. Freed, L.-H. Chung, M. Le Beon, and K.-M. Yang significantly improved this manuscript. K. Johnson and an anonymous reviewer gave insightful feedback that improved the original manuscript. Original ALOS-2 data are copyright by Japanese Aerospace Exploration Agency (JAXA) and were provided under JAXA ALOS RA-4 projects P1385 (S. Owen) and P1372 (E. Fielding). The Sentinel-1 interferograms contain Copernicus data. Part of this research was supported by the NASA Earth Surface and Interior focus area and performed at the Jet Propulsion Laboratory, California Institute of Technology. M.-H. Huang is supported by an appointment to the NASA Postdoctoral Programat the Jet Propulsion Laboratory, administered by the University of Space and Research Association through a contract with NASA. NR 37 TC 2 Z9 2 U1 2 U2 2 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD JUL 28 PY 2016 VL 43 IS 14 BP 7459 EP 7467 DI 10.1002/2016GL069351 PG 9 WC Geosciences, Multidisciplinary SC Geology GA DV9VL UT WOS:000383290200022 ER PT J AU Lehnert, H Stone, RP AF Lehnert, Helmut Stone, Robert P. TI A comprehensive inventory of the Gulf of Alaska sponge fauna with the description of two new species and geographic range extensions SO ZOOTAXA LA English DT Article DE new demosponges; Gulf of Alaska; North Pacific Ocean ID ALEUTIAN ISLANDS; BRITISH-COLUMBIA; ADJACENT WATERS; PORIFERA; DEMOSPONGIAE; NOV AB Two new species, Hamacantha (Vomerula) cassanoi n. sp. and Prosuberites salgadoi n. sp., are described from the eastern Gulf of Alaska in the North Pacific Ocean. These are the first records of the genera Hamacantha and Prosuberites from Alaska. We also report two geographic range extensions for the region. Geodia japonica Sollas, 1888 was previously known only from Japan and is now recorded from the Gulf of Alaska. We also document the first record of Rhizaxinella cervicornis Thiele, 1898 from the Gulf of Alaska. Our comprehensive inventory of the sponge fauna of the Gulf of Alaska confirms the presence of 52 taxa with an additional 38 taxa suspected of occurring in the region. This is a much lower number of species than that recorded from neighbouring regions like the Aleutian Islands and British Columbia. C1 [Lehnert, Helmut] Eichenstr 14, D-86507 Oberottmarshausen, Germany. [Lehnert, Helmut] GeoBioctr LMU Munchen, Richard Wagner Str 10, D-80333 Munich, Germany. [Stone, Robert P.] Natl Marine Fisheries Serv, Auke Bay Labs, Alaska Fisheries Sci Ctr, NOAA, 17109 Point Lena Loop, Juneau, AK 99801 USA. RP Lehnert, H (reprint author), Eichenstr 14, D-86507 Oberottmarshausen, Germany. EM Lehnert@spongetaxonomics.de FU Alaska Fisheries Science Center FX We thank Pelagic Research Services and the captain and crew of the RV Dorado Discovery for their assistance with the research cruise that made these collections possible. Special thanks to ROV team leader Edward Cassano for going the extra league. We thank Michele Masuda (Auke Bay Laboratories) for providing Figure 1 and Bruce Ott (Khoyatan Marine Laboratory) for providing distributional data for several species in the Gulf of Alaska. Thanks to the Zoologische Staatssammlung, Munchen, for providing access to the scanning electron microscope (SEM), especially to Enrico Schwabe for help operating the SEM. Thanks to Hjalmar Kunz for advice on Latin. Helmut Lehnert was supported by a contract from the Alaska Fisheries Science Center. The findings and conclusions in this paper are those of the authors and do not necessarily represent the views of the National Marine Fisheries Service, NOAA. NR 62 TC 0 Z9 0 U1 1 U2 1 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD JUL 28 PY 2016 VL 4144 IS 3 BP 365 EP 382 DI 10.11646/zootaxa.4144.3.5 PG 18 WC Zoology SC Zoology GA DS1LL UT WOS:000380357000005 PM 27470862 ER PT J AU Delp, MD Charvat, JM Limoli, CL Globus, RK Ghosh, P AF Delp, Michael D. Charvat, Jacqueline M. Limoli, Charles L. Globus, Ruth K. Ghosh, Payal TI Apollo Lunar Astronauts Show Higher Cardiovascular Disease Mortality: Possible Deep Space Radiation Effects on the Vascular Endothelium SO SCIENTIFIC REPORTS LA English DT Article ID IONIZING-RADIATION; CIRCULATORY DISEASE; CANCELLOUS BONE; RISK; EXPOSURE; HEALTH; MICE; CANCER; VASODILATION; EXPLORATION AB As multiple spacefaring nations contemplate extended manned missions to Mars and the Moon, health risks could be elevated as travel goes beyond the Earth's protective magnetosphere into the more intense deep space radiation environment. The primary purpose of this study was to determine whether mortality rates due to cardiovascular disease (CVD), cancer, accidents and all other causes of death differ in (1) astronauts who never flew orbital missions in space, (2) astronauts who flew only in low Earth orbit (LEO), and (3) Apollo lunar astronauts, the only humans to have traveled beyond Earth's magnetosphere. Results show there were no differences in CVD mortality rate between non-flight (9%) and LEO (11%) astronauts. However, the CVD mortality rate among Apollo lunar astronauts (43%) was 4-5 times higher than in non-flight and LEO astronauts. To test a possible mechanistic basis for these findings, a secondary purpose was to determine the long-term effects of simulated weightlessness and space-relevant total-body irradiation on vascular responsiveness in mice. The results demonstrate that space-relevant irradiation induces a sustained vascular endothelial cell dysfunction. Such impairment is known to lead to occlusive artery disease, and may be an important risk factor for CVD among astronauts exposed to deep space radiation. C1 [Delp, Michael D.; Ghosh, Payal] Florida State Univ, Dept Nutr Food & Exercise Sci, Tallahassee, FL 32306 USA. [Charvat, Jacqueline M.] Johnson Space Ctr, Wyle Sci Technol & Engn Grp, Houston, TX 77058 USA. [Limoli, Charles L.] Univ Calif Irvine, Dept Radiat Oncol, Irvine, CA 92697 USA. [Globus, Ruth K.] NASA Ames Res Ctr, Space Biosci Div, Moffett Field, CA 94035 USA. RP Delp, MD (reprint author), Florida State Univ, Dept Nutr Food & Exercise Sci, Tallahassee, FL 32306 USA. EM mdelp@fsu.edu FU National Space and Biomedical Research Institute under NASA [MA02501, NCC 9-58]; National Space and Biomedical Research Institute under NASA Space Biology [NNX14AQ57G, NNX16AC28G] FX We would like to thank Candice Tahimic, Yasaman Shirazi-Fard, Ann-Sofie Schreurs, Masahira Terada and Joshua Alwood for their help with the animal husbandry radiation exposures, Drs David Goukassian, Matthew Coleman and Leif Peterson for their assistance with the initial astronaut mortality analysis, and Dr. Judy Muller-Delp for her dissection of the mouse coronary arteries. This study was supported by grants from the National Space and Biomedical Research Institute (MA02501) under the NASA Cooperative Agreement NCC 9-58 and NASA Space Biology (NNX14AQ57G and NNX16AC28G). NR 42 TC 3 Z9 3 U1 17 U2 23 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 2045-2322 J9 SCI REP-UK JI Sci Rep PD JUL 28 PY 2016 VL 6 AR 29901 DI 10.1038/srep29901 PG 11 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA DS2YO UT WOS:000380650100001 PM 27467019 ER PT J AU Funatsu, BM Claud, C Keckhut, P Hauchecorne, A Leblanc, T AF Funatsu, Beatriz M. Claud, Chantal Keckhut, Philippe Hauchecorne, Alain Leblanc, Thierry TI Regional and seasonal stratospheric temperature trends in the last decade (2002-2014) from AMSU observations SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID UPPER TROPOSPHERE; CLIMATE-CHANGE; DATA RECORDS; OZONE; LIDAR; SYSTEM; SSU AB Stratospheric temperature trends for the period 2002-2014 have been estimated using NOAA's Integrated Microwave Inter-calibration Approach (IMICA) version of advanced microwave sounding unit (AMSU) on AQUA satellite. In this period the stratosphere continued cooling over most of the globe with a rate ranging from -0.4 0.3 to -0.5 0.4K/decade above 25km. Considering specific latitude bands, trends are highly variable with height. In the tropical region, trends vary from -0.5 0.3K/decade for channel 12 (approximate to 30km) to -0.7 0.3K/decade for higher channels and present small seasonal variability in the intensity of cooling. In the polar regions and in the midlatitudes, trends for all channels are negative but not significant; uncertainties are large due to the high dynamical variability particularly in high latitudes. There is also large seasonal variability, with southern midlatitudes seasonal trends significant during summer (December, January, February) and autumn (March, April, May) above approximate to 25km, with values ranging from -1.0 +/- 0.5 to -0.6 +/- 0.5K/decade. Regional trends estimated with AMSU and long-term lidar measurements (over two decades) confirm stratospheric cooling in the northern midlatitudes and tropical regions. The effect of the length of the short series on trends was found to be small outside polar regions. It was found to be large in polar regions with about 1K changes in trend depending on start dates of the time series. C1 [Funatsu, Beatriz M.] Univ Rennes 2, CNRS, LETG Rennes COSTEL UMR 6554, Rennes, France. [Claud, Chantal] Ecole Polytech, CNRS UMR 5839, LMD, IPSL, Palaiseau, France. [Keckhut, Philippe; Hauchecorne, Alain] Univ Versailles St Quentin, CNRS UMR 8190, LATMOS, IPSL, Guyancourt, France. [Leblanc, Thierry] CALTECH, Jet Prop Lab, Wrightwood, CA USA. RP Funatsu, BM (reprint author), Univ Rennes 2, CNRS, LETG Rennes COSTEL UMR 6554, Rennes, France. EM bmf.amit@gmail.com RI Hauchecorne, Alain/A-8489-2013; OI Claud, Chantal/0000-0001-7613-9525; Hauchecorne, Alain/0000-0001-9888-6994 FU Climserv-IPSL; French National Research Agency (ANR) through the StraDyVariUS project [ANR-13-BS06-0011]; EU H2020 project ARISE2 (Atmospheric dynamics Research InfraStructure in Europe) FX The AMSU-A Climate Data Record (CDR) used in this study was acquired from NOAA's National Climatic Data Center (http://www.ncdc.noaa.gov) with the support of Climserv-IPSL. This CDR was originally developed by Cheng-Zhi Zou and colleagues at NOAA through support from NOAA's CDR Program. The lidar data used in this publication were obtained through the Network for the Detection of Atmospheric Composition Change (NDACC) and are publicly available (see http://www.ndacc.org). This work was supported by the French National Research Agency (ANR) through the StraDyVariUS project (ANR-13-BS06-0011), by the EU H2020 project ARISE2 (Atmospheric dynamics Research InfraStructure in Europe), and is a contribution to the WCRP/SPARC Temperature Trends Group. We are grateful for the critical comments from three anonymous Reviewers that helped improve the manuscript. NR 43 TC 0 Z9 0 U1 5 U2 9 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD JUL 27 PY 2016 VL 121 IS 14 BP 8172 EP 8185 DI 10.1002/2015JD024305 PG 14 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA DT6YX UT WOS:000381632100003 ER PT J AU Boeke, RC Taylor, PC AF Boeke, Robyn C. Taylor, Patrick C. TI Evaluation of the Arctic surface radiation budget in CMIP5 models SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID CLIMATE MODEL; ATMOSPHERE RADIATION; POLAR AMPLIFICATION; PART I; CLOUD; FEEDBACKS; ALBEDO; CERES; PARAMETERIZATION; UNCERTAINTY AB The Arctic region is warming at a rate more than double the global average, a trend predicted to continue by all Coupled Model Intercomparison Project 5 (CMIP5) climate models. Despite this consistency, significant intermodel spread exists in the simulated Arctic climate related to differences in the Arctic surface radiation budget. Building upon previous work to characterize and understand surface radiation budget biases in climate models, the annual mean and seasonal cycle of the Arctic surface radiation budget in 17 CMIP5 models using the Historical-forcing scenario is evaluated against state-of-the-art Cloud and Earth's Radiant Energy System Surface Energy Balanced and Filled data. The CMIP5 multimodel ensemble is found to simulate longwave surface fluxes well during the sunlit months (similar to 1Wm(-2) differences in July) but exhibits significant wintertime biases (up to -19Wm(-2)). Shortwave fluxes show substantial across-model spread during summer; the model standard deviation approaches 20Wm(-2) in July. Applying a decomposition analysis to the cloud radiative effect (CRE) seasonal cycles, an unrealistic compensation is uncovered between the model-simulated seasonal cycles of cloud fraction, all-sky/clear-sky flux differences, and surface albedo that enables models to simulate realistic CRE seasonal cycles with unrealistic individual contributions. This unrealistic behavior in models must be constrained to improve Arctic climate simulation; observational uncertainty is sufficient to do so. Lastly, biases in all and clear-sky longwave downwelling fluxes positively correlate with model surface temperature in winter, while in summer surface temperature is most strongly related to clear-sky upwelling radiation biases from surface albedo errors. C1 [Boeke, Robyn C.] Sci Syst Applicat Inc, Hampton, VA 23666 USA. [Taylor, Patrick C.] NASA, Langley Res Ctr, Climate Sci Branch, Hampton, VA 23665 USA. RP Boeke, RC (reprint author), Sci Syst Applicat Inc, Hampton, VA 23666 USA. EM robyn.c.boeke@nasa.gov FU NASA Interdisciplinary Studies Program [NNH12ZDA001N-IDS]; NASA Energy and Water Cycle Studies program FX This work is funded by the NASA Interdisciplinary Studies Program grant NNH12ZDA001N-IDS. The processing of the C3M data used in this analysis was funded under the NASA Energy and Water Cycle Studies program. The C3M and CERES data are available from the Langley Atmospheric Science Data Center (http://eosweb.larc.nasa.gov). We acknowledge the World Climate Research Programme's Working Group on Coupled Modelling, which is responsible for CMIP, and we thank the climate modeling groups (listed in Table 1 of this paper) 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. NR 59 TC 0 Z9 0 U1 10 U2 10 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD JUL 27 PY 2016 VL 121 IS 14 BP 8525 EP 8548 DI 10.1002/2016JD025099 PG 24 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA DT6YX UT WOS:000381632100023 ER PT J AU Alfaro-Nunez, A Bojesen, AM Bertelsen, MF Wales, N Balazs, GH Gilbert, MTP AF Alfaro-Nunez, Alonzo Bojesen, Anders Miki Bertelsen, Mads F. Wales, Nathan Balazs, George H. Gilbert, M. Thomas P. TI Further evidence of Chelonid herpesvirus 5 (ChHV5) latency: high levels of ChHV5 DNA detected in clinically healthy marine turtles SO PEERJ LA English DT Article DE Chelonid herpesvirus 5 (ChHV5); Fibropapillomatosis (FP); Glycoprotein B; Clinically healthy; Quantitative PCR; Viral loads; Ubiquitous; Asymptomatic ID FIBROPAPILLOMA-ASSOCIATED HERPESVIRUS; SIMPLEX-VIRUS; GREEN TURTLES; SEA-TURTLES; MYDAS; ESTABLISHMENT; PROTEINS; EXPOSURE; ASSAY AB The Chelonid herpesvirus 5 (ChHV5) has been consistently associated with fibropapillomatosis (FP), a transmissible neoplastic disease of marine turtles. Whether ChHV5 plays a causal role remains debated, partly because while FP tumours have been clearly documented to contain high concentrations of ChHV5 DNA, recent PCR-based studies have demonstrated that large proportions of asymptomatic marine turtles are also carriers of ChHV5. We used a real-time PCR assay to quantify the levels of ChHV5 Glycoprotein B (gB) DNA in both tumour and non-tumour skin tissues, from clinically affected and healthy turtles drawn from distant ocean basins across four species. In agreement with previous studies, higher ratios of viral to host DNA were consistently observed in tumour versus non-tumour tissues in turtles with FP. Unexpectedly however, the levels of ChHV5 gB DNA in clinically healthy turtles were significantly higher than in non-tumour tissues from FP positive turtles. Thus, a large proportion of clinically healthy sea turtle populations worldwide across species carry ChHV5 gB DNA presumably through persistent latent infections. ChHV5 appears to be ubiquitous regardless of the animals' clinical conditions. Hence, these results support the theory that ChHV5 is a near ubiquitous virus with latency characteristics requiring co-factors, possibly environmental or immune related, to induce FP. C1 [Alfaro-Nunez, Alonzo; Wales, Nathan; Gilbert, M. Thomas P.] Univ Copenhagen, Nat Hist Museum Denmark, Ctr GeoGenet, Sect Evolutionary Genom, Copenhagen K, Denmark. [Alfaro-Nunez, Alonzo] Escuela Super Politecn Litoral, Biomed Labs, Fac Ciencias Vida, Guayaquil, Ecuador. [Bojesen, Anders Miki] Univ Copenhagen, Fac Hlth & Med Sci, Dept Vet Dis Biol, Vet Clin Microbiol, Copenhagen, Denmark. [Bertelsen, Mads F.] Copenhagen Zoo, Ctr Zoo & Wild Anim Hlth, Copenhagen, Denmark. [Balazs, George H.] Natl Marine Fisheries Serv, Pacific Isl Fisheries Sci Ctr, Honolulu, HI USA. [Gilbert, M. Thomas P.] Curtin Univ Technol, Sch Environm & Agr, Trace & Environm DNA Lab, Perth, WA, Australia. RP Alfaro-Nunez, A (reprint author), Univ Copenhagen, Nat Hist Museum Denmark, Ctr GeoGenet, Sect Evolutionary Genom, Copenhagen K, Denmark.; Alfaro-Nunez, A (reprint author), Escuela Super Politecn Litoral, Biomed Labs, Fac Ciencias Vida, Guayaquil, Ecuador. EM alonzoalfaro@gmail.com OI Bertelsen, Mads/0000-0001-9201-7499; Wales, Nathan/0000-0003-0359-8450 FU Lundbeck Foundation Grant [R52-A5062] FX This project study was funded by the Lundbeck Foundation Grant R52-A5062. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 32 TC 1 Z9 1 U1 9 U2 10 PU PEERJ INC PI LONDON PA 341-345 OLD ST, THIRD FLR, LONDON, EC1V 9LL, ENGLAND SN 2167-8359 J9 PEERJ JI PeerJ PD JUL 27 PY 2016 VL 4 AR e2274 DI 10.7717/peerj.2274 PG 16 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA DS4HU UT WOS:000380742900006 PM 27547576 ER PT J AU Richardson, DE Marancik, KE Guyon, JR Lutcavage, ME Galuardi, B Lam, CH Walsh, HJ Wildes, S Yates, DA Hare, JA AF Richardson, David E. Marancik, Katrin E. Guyon, Jeffrey R. Lutcavage, Molly E. Galuardi, Benjamin Lam, Chi Hin Walsh, Harvey J. Wildes, Sharon Yates, Douglas A. Hare, Jonathan A. TI REPLY TO SAFINA AND WALTER ET AL.: Multiple lines of evidence for size-structured spawning migrations in western Atlantic bluefin tuna SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Letter ID THUNNUS-THYNNUS; GULF C1 [Richardson, David E.; Marancik, Katrin E.; Walsh, Harvey J.; Hare, Jonathan A.] NOAA, Natl Marine Fisheries Serv, Northeast Fisheries Sci Ctr, Ecosyst Proc Div, Narragansett, RI 02882 USA. [Marancik, Katrin E.] Northeast Fisheries Sci Ctr, Integrated Stat, Narragansett, RI 02882 USA. [Guyon, Jeffrey R.; Wildes, Sharon; Yates, Douglas A.] NOAA, Natl Marine Fisheries Serv, Alaska Fisheries Sci Ctr, Genet Program, Juneau, AK 99801 USA. [Lutcavage, Molly E.; Lam, Chi Hin] Univ Massachusetts Boston, Sch Environm, Large Pelag Res Ctr, Gloucester, MA 01931 USA. [Galuardi, Benjamin] Univ Massachusetts Dartmouth, Sch Marine Sci & Technol, Fairhaven, MA 02719 USA. [Galuardi, Benjamin] NOAA, Natl Marine Fisheries Serv, Greater Atlantic Reg Fisheries Off, Gloucester, MA 01930 USA. RP Richardson, DE (reprint author), NOAA, Natl Marine Fisheries Serv, Northeast Fisheries Sci Ctr, Ecosyst Proc Div, Narragansett, RI 02882 USA. EM david.richardson@noaa.gov NR 14 TC 0 Z9 0 U1 7 U2 7 PU NATL ACAD SCIENCES PI WASHINGTON PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA SN 0027-8424 J9 P NATL ACAD SCI USA JI Proc. Natl. Acad. Sci. U. S. A. PD JUL 26 PY 2016 VL 113 IS 30 BP E4262 EP E4263 DI 10.1073/pnas.1607666113 PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA DS1HJ UT WOS:000380346200003 PM 27436889 ER PT J AU Kara, E Miller, JM Reynolds, C Dai, LX AF Kara, Erin Miller, Jon M. Reynolds, Chris Dai, Lixin TI Relativistic reverberation in the accretion flow of a tidal disruption event SO NATURE LA English DT Article ID ACTIVE GALACTIC NUCLEI; X-RAY REVERBERATION; MASSIVE BLACK-HOLE; BROAD-LINE REGION; RADIUS-LUMINOSITY RELATIONSHIP; K-ALPHA REVERBERATION; NARROW-LINE; XMM-NEWTON; IRON K; TIME LAGS AB Our current understanding of the curved space-time around supermassive black holes is based on actively accreting black holes, which make up only ten per cent or less of the overall population. X-ray observations of that small fraction reveal strong gravitational redshifts that indicate that many of these black holes are rapidly rotating(1); however, selection biases suggest that these results are not necessarily reflective of the majority of black holes in the Universe(2). Tidal disruption events, where a star orbiting an otherwise dormant black hole gets tidally shredded and accreted onto the black hole(3), can provide a short, unbiased glimpse at the space-time around the other ninety per cent of black holes. Observations of tidal disruptions have hitherto revealed the formation of an accretion disk and the onset of an accretion-powered jet(4-8), but have failed to reveal emission from the inner accretion flow, which enables the measurement of black hole spin. Here we report observations of reverberation(9-12) arising from gravitationally redshifted iron Ka photons reflected off the inner accretion flow in the tidal disruption event Swift J1644+57. From the reverberation timescale, we estimate the mass of the black hole to be a few million solar masses, suggesting an accretion rate of 100 times the Eddington limit or more(13). The detection of reverberation from the relativistic depths of this rare super-Eddington event demonstrates that the X-rays do not arise from the relativistically moving regions of a jet, as previously thought(5,14). C1 [Kara, Erin; Reynolds, Chris] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Kara, Erin] NASA, Xray Astrophys Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Kara, Erin; Reynolds, Chris; Dai, Lixin] Univ Maryland, Joint Space Sci Inst, College Pk, MD 20742 USA. [Miller, Jon M.] Univ Michigan, Dept Astron, Ann Arbor, MI 48103 USA. [Dai, Lixin] Univ Maryland, Dept Phys, College Pk, MD 20742 USA. RP Kara, E (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA.; Kara, E (reprint author), NASA, Xray Astrophys Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.; Kara, E (reprint author), Univ Maryland, Joint Space Sci Inst, College Pk, MD 20742 USA. EM ekara@astro.umd.edu FU Hubble Fellowship Program from Space Telescope Science Institute [HST-HF2-51360.001-A]; NASA [NAS5-26555, NNX14AF86G]; NASA/NSF/TCAN [NNX14AB46G]; NSF/XSEDE/TACC [TG-PHY120005]; NASA/Pleiades [SMD-14-5451]; ESA member states; US (NASA); Suzaku satellite FX E.K. thanks A. Zoghbi, M. C. Miller, F. Tombesi, E. Miller and L. Denby for discussions. E. K. also thanks the Hubble Fellowship Program for support under grant number HST-HF2-51360.001-A from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555. J.M.M. acknowledges N. Schartel and XMM-Newton for executing target-of-opportunity observations of Swift J1644+57. C.R. acknowledges support from NASA under grant number NNX14AF86G. L.D. thanks J. McKinney for discussions. L.D. acknowledges support from NASA/NSF/TCAN (NNX14AB46G), NSF/XSEDE/TACC (TG-PHY120005) and NASA/Pleiades (SMD-14-5451). This work is based on observations made with XMM-Newton, a European Space Agency (ESA) science mission with instruments and contributions directly funded by ESA member states and the US (NASA) and the Suzaku satellite, a collaborative mission between the space agencies of Japan (JAXA) and the US (NASA). NR 61 TC 3 Z9 3 U1 3 U2 4 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 EI 1476-4687 J9 NATURE JI Nature PD JUL 21 PY 2016 VL 535 IS 7612 BP 388 EP + DI 10.1038/nature18007 PG 16 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA DS1GQ UT WOS:000380344200033 PM 27338795 ER PT J AU Wright, AH Robotham, ASG Bourne, N Driver, SP Dunne, L Maddox, SJ Alpaslan, M Andrews, SK Bauer, AE Bland-Hawthorn, J Brough, S Brown, MJI Clarke, C Cluver, M Davies, LJM Grootes, MW Holwerda, BW Hopkins, AM Jarrett, TH Kafle, PR Lange, R Liske, J Loveday, J Moffett, AJ Norberg, P Popescu, CC Smith, M Taylor, EN Tuffs, RJ Wang, L Wilkins, SM AF Wright, A. H. Robotham, A. S. G. Bourne, N. Driver, S. P. Dunne, L. Maddox, S. J. Alpaslan, M. Andrews, S. K. Bauer, A. E. Bland-Hawthorn, J. Brough, S. Brown, M. J. I. Clarke, C. Cluver, M. Davies, L. J. M. Grootes, M. W. Holwerda, B. W. Hopkins, A. M. Jarrett, T. H. Kafle, P. R. Lange, R. Liske, J. Loveday, J. Moffett, A. J. Norberg, P. Popescu, C. C. Smith, M. Taylor, E. N. Tuffs, R. J. Wang, L. Wilkins, S. M. TI Galaxy And Mass Assembly: accurate panchromatic photometry from optical priors using lambdar SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE techniques: photometric; astronomical data bases: miscellaneous; galaxies: evolution; galaxies: general; galaxies: photometry ID DIGITAL SKY SURVEY; SPECTRAL ENERGY-DISTRIBUTIONS; EXTRAGALACTIC LEGACY SURVEY; DATA RELEASE; PRECISION PHOTOMETRY; MATCHED PHOTOMETRY; HERSCHEL ATLAS; STAR-FORMATION; DATA PRODUCTS; DATA SETS AB We present the Lambda Adaptive Multi-Band Deblending Algorithm in R (lambdar), a novel code for calculating matched aperture photometry across images that are neither pixel- nor PSF-matched, using prior aperture definitions derived from high-resolution optical imaging. The development of this program is motivated by the desire for consistent photometry and uncertainties across large ranges of photometric imaging, for use in calculating spectral energy distributions. We describe the program, specifically key features required for robust determination of panchromatic photometry: propagation of apertures to images with arbitrary resolution, local background estimation, aperture normalization, uncertainty determination and propagation, and object deblending. Using simulated images, we demonstrate that the program is able to recover accurate photometric measurements in both high-resolution, low-confusion, and low-resolution, high-confusion, regimes. We apply the program to the 21-band photometric data set from the Galaxy And Mass Assembly (GAMA) Panchromatic Data Release (PDR; Driver et al. 2016), which contains imaging spanning the far-UV to the far-IR. We compare photometry derived from lambdar with that presented in Driver et al. (2016), finding broad agreement between the data sets. None the less, we demonstrate that the photometry from lambdar is superior to that from the GAMA PDR, as determined by a reduction in the outlier rate and intrinsic scatter of colours in the lambdar data set. We similarly find a decrease in the outlier rate of stellar masses and star formation rates using lambdar photometry. Finally, we note an exceptional increase in the number of UV and mid-IR sources able to be constrained, which is accompanied by a significant increase in the mid-IR colour-colour parameter-space able to be explored. C1 [Wright, A. H.; Robotham, A. S. G.; Driver, S. P.; Andrews, S. K.; Kafle, P. R.; Lange, R.; Moffett, A. J.] Univ Western Australia, ICRAR, 35 Stirling Highway, Crawley, WA 6009, Australia. [Bourne, N.; Dunne, L.; Maddox, S. J.] Univ Edinburgh, Inst Astron, SUPA, Royal Observ, Blackford Hill, Edinburgh EH9 3HJ, Midlothian, Scotland. [Driver, S. P.] Univ St Andrews, Sch Phys & Astron, SUPA, St Andrews KY16 9SS, Fife, Scotland. [Dunne, L.; Maddox, S. J.; Smith, M.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Alpaslan, M.] NASA, Ames Res Ctr, N232, Mountain View, CA 94035 USA. [Bauer, A. E.; Brough, S.; Hopkins, A. M.] Australian Astron Observ, POB 915, N Ryde, NSW 1670, Australia. [Bland-Hawthorn, J.] Univ Sydney, Sch Phys A28, Sydney Inst Astron, Sydney, NSW 2006, Australia. [Brown, M. J. I.] Monash Univ, Sch Phys & Astron, Clayton, Vic 3800, Australia. [Clarke, C.; Loveday, J.; Wilkins, S. M.] Univ Sussex, Ctr Astron, Brighton BN1 9QH, E Sussex, England. [Cluver, M.] Univ Western Cape, Dept Phys & Astron, Robert Sobukwe Rd, ZA-7535 Bellville, South Africa. [Grootes, M. W.] ESA, Estec, Keplerlaan 1, NL-2201 AZ Noordwijk, Netherlands. [Holwerda, B. W.] Leiden Univ, Sterrenwacht Leiden, Niels Bohrweg 2, NL-2333 CA Leiden, Netherlands. [Jarrett, T. H.] Univ Cape Town, Dept Astron, ZA-7701 Rondebosch, South Africa. [Liske, J.] Univ Hamburg, Hamburger Sternwarte, Gojenbergsweg 112, D-21029 Hamburg, Germany. [Norberg, P.] Univ Durham, Dept Phys, ICC, South Rd, Durham DH1 3LE, England. [Norberg, P.] Univ Durham, Dept Phys, CEA, South Rd, Durham DH1 3LE, England. [Popescu, C. C.] Univ Cent Lancashire, Jeremiah Horrocks Inst, Preston PR1 2HE, Lancs, England. [Popescu, C. C.] Romanian Acad, Astron Inst, Str Cutitul Argint 5, Bucharest, Romania. [Taylor, E. N.] Univ Melbourne, Sch Phys, Melbourne, Vic 3010, Australia. [Tuffs, R. J.] Max Planck Inst Kernphys, Saupfercheckweg 1, D-69117 Heidelberg, Germany. [Wang, L.] SRON Netherlands Inst Space Res, Landleven 12, NL-9747 AD Groningen, Netherlands. RP Wright, AH (reprint author), Univ Western Australia, ICRAR, 35 Stirling Highway, Crawley, WA 6009, Australia. EM angus.wright@icrar.org RI Brown, Michael/B-1181-2015 OI Brown, Michael/0000-0002-1207-9137 FU Australian Government's Department of Industry Australian Postgraduate Award (APA); Australian Research Council [FT140101166]; ERC in the form of the Advanced Investigator Program; COS-MICISM; ERC Consolidator Grant CosmicDust; European Union [312725]; STFC (UK); ARC (Australia); AAO FX We thank the anonymous referee for a thorough reading of the paper and for their many constructive comments. AHW and SKA are supported by the Australian Government's Department of Industry Australian Postgraduate Award (APA). SB acknowledges funding support from the Australian Research Council through a Future Fellowship (FT140101166). LD and SJM acknowledge support from the ERC in the form of the Advanced Investigator Program, COS-MICISM, and the ERC Consolidator Grant CosmicDust. NB acknowledges funding from the European Union Seventh Framework Programme (FP7/2007-2013) under grant agreement no. 312725. GAMA is a joint European-Australasian project based around a spectroscopic campaign using the AAT. The GAMA IC is based on data taken from the SDSS 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, Herschel-ATLAS, 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/. The Herschel-ATLAS is a project with Herschel, which is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA. The H-ATLAS website is http://www.h-atlas.org/. We thank the Herschel Multitiered Extragalactic Survey (HERMES) collaboration for providing the mock FIR imaging used in Section 5. Figures in this paper have been prepared using the R package MAGICAXIS.2 This research has made use of NASA's Astrophysics Data System. NR 72 TC 9 Z9 9 U1 2 U2 3 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUL 21 PY 2016 VL 460 IS 1 BP 765 EP 801 DI 10.1093/mnras/stw832 PG 37 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DR3XE UT WOS:000379835200053 ER PT J AU Champion, DJ Petroff, E Kramer, M Keith, MJ Bailes, M Barr, ED Bates, SD Bhat, NDR Burgay, M Burke-Spolaor, S Flynn, CML Jameson, A Johnston, S Ng, C Levin, L Possenti, A Stappers, BW van Straten, W Thornton, D Tiburzi, C Lyne, AG AF Champion, D. J. Petroff, E. Kramer, M. Keith, M. J. Bailes, M. Barr, E. D. Bates, S. D. Bhat, N. D. R. Burgay, M. Burke-Spolaor, S. Flynn, C. M. L. Jameson, A. Johnston, S. Ng, C. Levin, L. Possenti, A. Stappers, B. W. van Straten, W. Thornton, D. Tiburzi, C. Lyne, A. G. TI Five new fast radio bursts from the HTRU high-latitude survey at Parkes: first evidence for two-component bursts SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE scattering; surveys; pulsars: general; intergalactic medium ID UNIVERSE PULSAR SURVEY; GAMMA-RAY BURSTS; NEUTRON-STARS; GIANT PULSES; COSMOLOGICAL DISTANCES; REIONIZATION HISTORY; INITIAL DISCOVERIES; GALACTIC LATITUDES; CRAB PULSAR; TRANSIENTS AB The detection of five new fast radio bursts (FRBs) found in the 1.4-GHz High Time Resolution Universe high-latitude survey at Parkes, is presented. The rate implied is 7(-3)(+5) x 10(3) (95 per cent) FRBs sky(-1) d(-1) above a fluence of 0.13 Jy ms for an FRB of 0.128 ms duration to 1.5 Jy ms for 16 ms duration. One of these FRBs has a two-component profile, in which each component is similar to the known population of single component FRBs and the two components are separated by 2.4 +/- 0.4 ms. All the FRB components appear to be unresolved following deconvolution with a scattering tail and accounting for intrachannel smearing. The two-component burst, FRB 121002, also has the highest dispersion measure (1629 pc cm(-3)) of any FRB to-date. Many of the proposed models to explain FRBs use a single high-energy event involving compact objects (such as neutron-star mergers) and therefore cannot easily explain a two-component FRB. Models that are based on extreme versions of flaring, pulsing, or orbital events, however, could produce multiple component profiles. The compatibility of these models and the FRB rate implied by these detections is discussed. C1 [Champion, D. J.; Kramer, M.; Ng, C.; Tiburzi, C.] Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany. [Petroff, E.; Bailes, M.; Barr, E. D.; Bhat, N. D. R.; Flynn, C. M. L.; Jameson, A.; van Straten, W.] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Mail H30,POB 218, Hawthorn, Vic 3122, Australia. [Petroff, E.; Bailes, M.; Barr, E. D.; Bhat, N. D. R.; Flynn, C. M. L.; Jameson, A.; van Straten, W.] Swinburne Univ Technol, ARC Ctr Excellence All Sky Astron CAASTRO, Mail H30,POB 218, Hawthorn, Vic 3122, Australia. [Petroff, E.; Johnston, S.; Thornton, D.] CSIRO Astron & Space Sci, Australia Telescope Natl Facil, POB 76, Epping, NSW 1710, Australia. [Kramer, M.; Keith, M. J.; Bates, S. D.; Levin, L.; Stappers, B. W.; Thornton, D.; Lyne, A. G.] Univ Manchester, Jodrell Bank, Ctr Astrophys, Alan Turing Bldg,Oxford Rd, Manchester M13 9PL, Lancs, England. [Bates, S. D.] Natl Radio Astron Observ, POB 2, Green Bank, WV 24944 USA. [Bhat, N. D. R.] Curtin Univ, Int Ctr Radio Astron Res, Bentley, WA 6102, Australia. [Burgay, M.; Possenti, A.] INAF Osservatorio Astron Cagliari, Via Sci 5, I-09047 Selargius, Italy. [Burke-Spolaor, S.] NASA, Jet Prop Lab, M-S 138-307, Pasadena, CA 91106 USA. [Tiburzi, C.] Univ Bielefeld, Fak Phys, Postfach 100131, D-33501 Bielefeld, Germany. RP Champion, DJ (reprint author), Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany. EM champion@mpifr-bonn.mpg.de FU Commonwealth of Australia; Australian Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO) [CE110001020]; Swinburne; Australian Government's Education Investment Fund FX The Parkes radio telescope is part of the Australia Telescope which is funded by the Commonwealth of Australia for operation as a National Facility managed by CSIRO. Parts of this research were conducted by the Australian Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO), through project number CE110001020. This work used the gSTAR national facility which is funded by Swinburne and the Australian Government's Education Investment Fund. NR 42 TC 24 Z9 24 U1 0 U2 1 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUL 21 PY 2016 VL 460 IS 1 BP L30 EP L34 DI 10.1093/mnrasl/slw069 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DR3VZ UT WOS:000379832000007 ER PT J AU Cusumano, G La Parola, V D' Ai, A Segreto, A Tagliaferri, G Barthelmy, SD Gehrels, N AF Cusumano, G. La Parola, V. D' Ai, A. Segreto, A. Tagliaferri, G. Barthelmy, S. D. Gehrels, N. TI An unexpected drop in the magnetic field of the X-ray pulsar V0332+53 after the bright outburst occurred in 2015 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE magnetic fields; pulsars: individual: V0332+53; X-rays: binaries ID ACCRETING NEUTRON-STARS; TRANSIENT V0332+53; CYCLOTRON LINES; DISCOVERY; EVOLUTION; MASS; LUMINOSITY; TELESCOPE; X0331+53; FEATURES AB How the accreted mass settling on the surface of a neutron star affects the topology of the magnetic field and how the secular evolution of the binary system depends on the magnetic field change is still an open issue. We report evidence for a clear drop in the observed magnetic field in the accreting pulsar V0332+53 after undergoing a bright 3-month long X-ray outburst. We determine the field from the position of the fundamental cyclotron line in its X-ray spectrum and relate it to the luminosity. For equal levels of luminosity, in the declining phase we measure a systematically lower value of the cyclotron line energy with respect to the rising phase. This results in a drop of similar to 1.7 x 10(11) G of the observed field between the onset and the end of the outburst. The settling of the accreted plasma on to the polar cap seems to induce a distortion of the magnetic field lines weakening their intensity along the accretion columns. Therefore, the dissipation rate of the magnetic field could be much faster than previously estimated, unless the field is able to restore its original configuration on a time-scale comparable with the outbursts recurrence time. C1 [Cusumano, G.; La Parola, V.; D' Ai, A.; Segreto, A.] INAF Ist Astrofis Spaziale & Fis Cosm, Via U La Malfa 153, I-90146 Palermo, Italy. [Tagliaferri, G.] INAF Brera Astron Observ, Via Bianchi 46, Merate, LC, Italy. [Barthelmy, S. D.; Gehrels, N.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Cusumano, G (reprint author), INAF Ist Astrofis Spaziale & Fis Cosm, Via U La Malfa 153, I-90146 Palermo, Italy. EM cusumano@ifc.inaf.it FU ASI [I/004/11/1] FX This work has been supported by ASI grant I/004/11/1. NR 27 TC 3 Z9 3 U1 0 U2 0 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUL 21 PY 2016 VL 460 IS 1 BP L99 EP L103 DI 10.1093/mnrasl/slw084 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DR3VZ UT WOS:000379832000021 ER PT J AU Evans, PA Kennea, JA Barthelmy, SD Beardmore, AP Burrows, DN Campana, S Cenko, SB Gehrels, N Giommi, P Gronwall, C Marshall, FE Malesani, D Markwardt, CB Mingo, B Nousek, JA O'Brien, PT Osborne, JP Pagani, C Page, KL Palmer, DM Perri, M Racusin, JL Siegel, MH Sbarufatti, B Tagliaferri, G AF Evans, P. A. Kennea, J. A. Barthelmy, S. D. Beardmore, A. P. Burrows, D. N. Campana, S. Cenko, S. B. Gehrels, N. Giommi, P. Gronwall, C. Marshall, F. E. Malesani, D. Markwardt, C. B. Mingo, B. Nousek, J. A. O'Brien, P. T. Osborne, J. P. Pagani, C. Page, K. L. Palmer, D. M. Perri, M. Racusin, J. L. Siegel, M. H. Sbarufatti, B. Tagliaferri, G. TI Swift follow-up of the gravitational wave source GW150914 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE gravitational waves; methods: data analysis; X-rays: general ID ALL-SKY SURVEY; X-RAY-TELESCOPE; SOURCE CATALOG; COUNTERPART; SEARCHES; MISSION AB The Advanced Laser Interferometer Gravitational-Wave Observatory (ALIGO) observatory recently reported the first direct detection of gravitational waves (GW) which triggered ALIGO on 2015 September 14. We report on observations taken with the Swift satellite two days after the trigger. No new X-ray, optical, UV or hard X-ray sources were detected in our observations, which were focused on nearby galaxies in the GW error region and covered 4.7 deg(2) similar to 2 per cent of the probability in the rapidly available GW error region; 0.3 per cent of the probability from the final GW error region, which was produced several months after the trigger). We describe the rapid Swift response and automated analysis of the X-ray telescope and UV/Optical telescope data, and note the importance to electromagnetic follow-up of early notification of the progenitor details inferred from GW analysis. C1 [Evans, P. A.; Beardmore, A. P.; Mingo, B.; O'Brien, P. T.; Osborne, J. P.; Pagani, C.; Page, K. L.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Kennea, J. A.; Burrows, D. N.; Gronwall, C.; Nousek, J. A.; Siegel, M. H.; Sbarufatti, B.] Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA. [Barthelmy, S. D.; Cenko, S. B.; Gehrels, N.; Marshall, F. E.; Markwardt, C. B.; Racusin, J. L.] NASA, Goddard Space Flight Ctr, Mail Code 661, Greenbelt, MD 20771 USA. [Campana, S.; Sbarufatti, B.; Tagliaferri, G.] Osserv Astron Brera, INAF, Via E Bianchi 46, I-23807 Merate, Italy. [Cenko, S. B.] Univ Maryland, Joint Space Sci Institude, College Pk, MD 20742 USA. [Giommi, P.; Perri, M.] Agenzia Spaziale Italiana ASI Sci Data Ctr, I-00133 Rome, Italy. [Gronwall, C.] Penn State Univ, Inst Gravitat & Cosmos, Inst Gravitat & Cosmos, University Pk, PA 16802 USA. [Malesani, D.] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, Juliane Maries Vej 30, DK-2100 Copenhagen O, Denmark. [Markwardt, C. B.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Palmer, D. M.] Los Alamos Natl Lab, B244, Los Alamos, NM 87545 USA. [Perri, M.] Osserv Astron Roma, INAF, Via Frascati 33, I-00040 Monte Porzio Catone, Italy. RP Evans, PA (reprint author), Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. EM pae9@leicester.ac.uk OI Sbarufatti, Boris/0000-0001-6620-8347 FU UK Space Agency; Italian Space Agency; National Aeronautics and Space Administration; National Science Foundation; SIMBAD data base FX This work made use of data supplied by the UK Swift Science Data Centre at the University of Leicester, and used the ALICE High Performance Computing Facility at the University of Leicester. This research has made use of the XRT Data Analysis Software (XRT-DAS) developed under the responsibility of the ASI Science Data Center (ASDC), Italy. PAE, APB, BM, KLP and JPO acknowledge UK Space Agency support. SC and GT acknowledge Italian Space Agency support. 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, and the SIMBAD data base, operated at CDS, Strasbourg, France. Fig. 1 was created using the KAPETYN package (Terlouw & Vogelaar 2015). We thank the anonymous referee for their helpful feedback on the original version of the Letter. NR 34 TC 11 Z9 11 U1 1 U2 6 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUL 21 PY 2016 VL 460 IS 1 BP L40 EP L44 DI 10.1093/mnrasl/slw065 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DR3VZ UT WOS:000379832000009 ER PT J AU Kumarasinghe, CS Premaratne, M Gunapala, SD Agrawal, GP AF Kumarasinghe, Chathurangi S. Premaratne, Malin Gunapala, Sarath D. Agrawal, Govind P. TI Theoretical analysis of hot electron injection from metallic nanotubes into a semiconductor interface SO PHYSICAL CHEMISTRY CHEMICAL PHYSICS LA English DT Article ID SURFACE-PLASMONS; NANOPARTICLES; AU; PHOTOEMISSION; DYNAMICS; NANORODS; CARRIERS; DEVICE; LIGHT AB Metallic nanostructures under optical illumination can generate a non-equilibrium high-energy electron gas (also known as hot electrons) capable of being injected into neighbouring media over a potential barrier at particle boundaries. The nature of this process is highly nanoparticle shape and size dependent. Here, we have derived an analytical expression for the frequency dependent rate of injection of these energetic electrons from a metallic nanotube into a semiconductor layer in contact with its inner boundary. In our derivation, we have considered the quantum mechanical motion of the electron gas confined by the particle boundaries in determining the electron energy spectrum and wave functions. We present a comprehensive theoretical analysis of how different geometric parameters such as the outer to inner radius ratio, length and thickness of a nanotube and illumination frequency affect the hot electron injection and internal quantum efficiency of the nanotube. We reveal that longer nanotubes with thin shells and high inner to outer radius ratios show better performance at visible and infrared frequencies. Our derivations and results provide the much needed theoretical insight for optimization of thin nanotubes for different hot electron based applications. C1 [Kumarasinghe, Chathurangi S.; Premaratne, Malin] Monash Univ, Adv Comp & Simulat Lab A L, Dept Elect & Comp Syst Engn, Clayton, Vic 3800, Australia. [Gunapala, Sarath D.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Agrawal, Govind P.] Univ Rochester, Inst Opt, Rochester, NY 14627 USA. RP Kumarasinghe, CS; Premaratne, M (reprint author), Monash Univ, Adv Comp & Simulat Lab A L, Dept Elect & Comp Syst Engn, Clayton, Vic 3800, Australia. EM chathurangi.kumarasinghe@monash.edu; malin.premaratne@monash.edu FU Monash University Institute of Graduate Research; Australian Research Council [DP140100883] FX The work of C. S. K. is supported by the Monash University Institute of Graduate Research. The work of M. P., S. D. G. and G. P. A. is supported by the Australian Research Council, through its Discovery Grant DP140100883. NR 47 TC 1 Z9 1 U1 3 U2 10 PU ROYAL SOC CHEMISTRY PI CAMBRIDGE PA THOMAS GRAHAM HOUSE, SCIENCE PARK, MILTON RD, CAMBRIDGE CB4 0WF, CAMBS, ENGLAND SN 1463-9076 EI 1463-9084 J9 PHYS CHEM CHEM PHYS JI Phys. Chem. Chem. Phys. PD JUL 21 PY 2016 VL 18 IS 27 BP 18227 EP 18236 DI 10.1039/c6cp03043b PG 10 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA DQ8UH UT WOS:000379486200051 PM 27332556 ER PT J AU Ackermann, M Ajello, M Baldini, L Ballet, J Barbiellini, G Bastieri, D Bellazzini, R Bissaldi, E Blandford, RD Bloom, ED Bonino, R Brandt, TJ Bregeon, J Bruel, P Buehler, R Buson, S Caliandro, GA Cameron, RA Caragiulo, M Caraveo, PA Cavazzuti, E Cecchi, C Charles, E Chekhtman, A Cheung, CC Chiaro, G Ciprini, S Cohen, JM Cohen-Tanugi, J Costanza, F Cutini, S D'Ammando, F Davis, DS de Angelis, A de Palma, F Desiante, R Digel, SW Di Lalla, N Di Mauro, M Di Venere, L Favuzzi, C Fegan, SJ Ferrara, EC Focke, WB Fukazawa, Y Funk, S Fusco, P Gargano, F Gasparrini, D Georganopoulos, M Giglietto, N Giordano, F Giroletti, M Godfrey, G Green, D Grenier, IA Guiriec, S Hays, E Hewitt, JW Hill, AB Jogler, T Johnnesson, G Kensei, S Kuss, M Larsson, S Latronico, L Li, J Li, L Longo, F Loparco, F Lubrano, P Magill, JD Maldera, S Manfreda, A Mayer, M Mazziotta, MN McConville, W McEnery, JE Michelson, PF Mitthumsiri, W Mizuno, T Monzani, ME Morselli, A Moskalenko, IV Murgia, S Negro, M Nuss, E Ohno, M Ohsugi, T 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 Reimer, A Reimer, O Schmid, J Sgro, C Simone, D Siskind, EJ Spada, F Spandre, G Spinelli, P Stawarz, L Takahashi, H Thayer, JB Thompson, DJ Torres, DF Tosti, G Troja, E Vianello, G Wood, KS Wood, M Zimmer, S AF Ackermann, M. Ajello, M. Baldini, L. Ballet, J. Barbiellini, G. Bastieri, D. Bellazzini, R. Bissaldi, E. Blandford, R. D. Bloom, E. D. Bonino, R. Brandt, T. J. Bregeon, J. Bruel, P. Buehler, R. Buson, S. Caliandro, G. A. Cameron, R. A. Caragiulo, M. Caraveo, P. A. Cavazzuti, E. Cecchi, C. Charles, E. Chekhtman, A. Cheung, C. C. Chiaro, G. Ciprini, S. Cohen, J. M. Cohen-Tanugi, J. Costanza, F. Cutini, S. D'Ammando, F. Davis, D. S. de Angelis, A. de Palma, F. Desiante, R. Digel, S. W. Di Lalla, N. Di Mauro, M. Di Venere, L. Favuzzi, C. Fegan, S. J. Ferrara, E. C. Focke, W. B. Fukazawa, Y. Funk, S. Fusco, P. Gargano, F. Gasparrini, D. Georganopoulos, M. Giglietto, N. Giordano, F. Giroletti, M. Godfrey, G. Green, D. Grenier, I. A. Guiriec, S. Hays, E. Hewitt, J. W. Hill, A. B. Jogler, T. Johnnesson, G. Kensei, S. Kuss, M. Larsson, S. Latronico, L. Li, J. Li, L. Longo, F. Loparco, F. Lubrano, P. Magill, J. D. Maldera, S. Manfreda, A. Mayer, M. Mazziotta, M. N. McConville, W. McEnery, J. E. Michelson, P. F. Mitthumsiri, W. Mizuno, T. Monzani, M. E. Morselli, A. Moskalenko, I. V. Murgia, S. Negro, M. Nuss, E. Ohno, M. Ohsugi, T. 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. Reimer, A. Reimer, O. Schmid, J. Sgro, C. Simone, D. Siskind, E. J. Spada, F. Spandre, G. Spinelli, P. Stawarz, L. Takahashi, H. Thayer, J. B. Thompson, D. J. Torres, D. F. Tosti, G. Troja, E. Vianello, G. Wood, K. S. Wood, M. Zimmer, S. TI FERMI LARGE AREA TELESCOPE DETECTION OF EXTENDED GAMMA-RAY EMISSION FROM THE RADIO GALAXY FORNAX A SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: individual (Fornax A); galaxies: jets; gamma rays: galaxies; radiation mechanisms: non-thermal ID EXTRAGALACTIC BACKGROUND LIGHT; ACTIVE GALACTIC NUCLEI; COMPTON X-RAYS; SOURCE CATALOG; EAST LOBE; SCALE; STRENGTHS; OUTBURST; NGC-1316; CLUSTER AB We report the Fermi Large Area Telescope detection of extended gamma-ray emission from the lobes of the radio galaxy Fornax. A using 6.1 years of Pass. 8 data. After Centaurus. A, this is now the second example of an extended gamma-ray source attributed to a radio galaxy. Both an extended flat disk morphology and a morphology following the extended radio lobes were preferred over a point-source description, and the core contribution was constrained to be < 14% of the total gamma-ray flux. A preferred alignment of the gamma-ray elongation with the radio lobes was demonstrated by rotating the radio lobes template. We found no significant evidence for variability on similar to 0.5 year timescales. Taken together, these results strongly suggest a lobe origin for the gamma-rays. With the extended nature of the > 100 MeV gamma-ray emission established, we model the source broadband emission considering currently available total lobe radio and millimeter flux measurements, as well as X-ray detections attributed to inverse Compton (IC) emission off the cosmic microwave background (CMB). Unlike the Centaurus. A case, we find that a leptonic model involving IC scattering of CMB and extragalactic background light (EBL) photons underpredicts the gamma-ray fluxes by factors of about similar to 2-3, depending on the EBL model adopted. An additional gamma-ray spectral component is thus required, and could be due to hadronic emission arising from proton-proton collisions of cosmic rays with thermal plasma within the radio lobes. C1 [Ackermann, M.; Buehler, R.; Mayer, M.] Deutsch Elektronen Synchrotron DESY, D-15738 Zeuthen, Germany. [Ajello, M.] Clemson Univ, Kinard Lab Phys, Dept Phys & Astron, Clemson, SC 29634 USA. [Baldini, L.] Univ Pisa, I-56127 Pisa, Italy. [Baldini, L.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy. [Baldini, L.; Blandford, R. D.; Bloom, E. D.; Caliandro, G. A.; Cameron, R. A.; Charles, E.; Digel, S. W.; Di Mauro, M.; Focke, W. B.; Godfrey, G.; Hill, A. B.; Jogler, T.; Michelson, P. F.; Monzani, M. E.; Moskalenko, I. V.; Orlando, E.; Paneque, D.; Pesce-Rollins, M.; Porter, T. A.; Reimer, A.; Reimer, O.; Thayer, J. B.; Vianello, G.; Wood, M.] Stanford Univ, Dept Phys, Kavli Inst Particle Astrophys & Cosmol, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA. [Baldini, L.; Blandford, R. D.; Bloom, E. D.; Caliandro, G. A.; Cameron, R. A.; Charles, E.; Digel, S. W.; Di Mauro, M.; Focke, W. B.; Godfrey, G.; Hill, A. B.; Jogler, T.; Michelson, P. F.; Monzani, M. E.; Moskalenko, I. V.; Orlando, E.; Paneque, D.; Pesce-Rollins, M.; Porter, T. A.; Reimer, A.; Reimer, O.; Thayer, J. B.; Vianello, G.; Wood, M.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA. [Ballet, J.; Grenier, I. A.; Schmid, J.] 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, Dipartimento Fis, I-34127 Trieste, Italy. [Bastieri, D.; Rando, R.] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy. [Bastieri, D.; Chiaro, G.; Rando, R.] Univ Padua, Dipartimento Fis & Astron G Galilei, I-35131 Padua, Italy. [Bellazzini, R.; Di Lalla, N.; Kuss, M.; Manfreda, A.; Pesce-Rollins, M.; Pivato, G.; Razzano, M.; Sgro, C.; Spada, F.; Spandre, G.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy. [Bissaldi, E.; Caragiulo, M.; Costanza, F.; de Palma, F.; Di Venere, L.; Favuzzi, C.; Fusco, P.; Gargano, F.; Giglietto, N.; Giordano, F.; Loparco, F.; Mazziotta, M. N.; Raino, S.; Simone, D.; Spinelli, P.] Ist Nazl Fis Nucl, Sez Bari, I-70126 Bari, Italy. [Bonino, R.; Desiante, R.; Latronico, L.; Maldera, S.; Negro, M.] Ist Nazl Fis Nucl, Sez Torino, I-10125 Turin, Italy. [Bonino, R.; Negro, M.] Univ Torino, Dipartimento Fis Gen Amadeo Avogadro, I-10125 Turin, Italy. [Brandt, T. J.; Buson, S.; Cohen, J. M.; Davis, D. S.; Ferrara, E. C.; Green, D.; Guiriec, S.; Hays, E.; McConville, W.; McEnery, J. E.; Perkins, J. S.; Thompson, D. J.; Troja, E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Bregeon, J.; Cohen-Tanugi, J.; Nuss, E.; Piron, F.] Univ Montpellier, Lab Univers & Particules Montpellier, CNRS IN2P3, F-34095 Montpellier, France. [Bruel, P.; Fegan, S. J.] Ecole Polytech, CNRS IN2P3, Lab Leprince Ringuet, F-91128 Palaiseau, France. [Buson, S.; Georganopoulos, M.] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA. [Buson, S.; Georganopoulos, M.] Univ Maryland Baltimore Cty, Ctr Space Sci & Technol, Baltimore, MD 21250 USA. [Buson, S.] CRESST, Greenbelt, MD 20771 USA. [Caliandro, G. A.] CIFS, I-10133 Turin, Italy. [Caragiulo, M.; Di Venere, L.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Giordano, F.; Loparco, F.; Raino, S.; Spinelli, P.] Univ Politecn Bari, Dipartimento Fis, I-70126 Bari, Italy. [Caraveo, P. A.] INAF Ist Astrofis Spaziale & Fis Cosm, I-20133 Milan, Italy. [Cavazzuti, E.; Ciprini, S.; Cutini, S.; Gasparrini, D.] Agenzia Spaziale Italiana ASI Sci Data Ctr, I-00133 Rome, Italy. [Cecchi, C.; Ciprini, S.; Cutini, S.; Gasparrini, D.; Lubrano, P.; Tosti, G.] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy. [Cecchi, C.; Tosti, G.] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy. [Chekhtman, A.] George Mason Univ, Coll Sci, Fairfax, VA 22030 USA. [Cheung, C. C.; Wood, K. S.] Naval Res Lab, Div Space Sci, Washington, DC 20375 USA. [Cheung, C. C.; Wood, K. S.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA. [Cohen, J. M.; Green, D.; Magill, J. D.; McConville, W.; McEnery, J. E.; Troja, E.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [D'Ammando, F.; Giroletti, M.; Orienti, M.] INAF Ist Radioastron, I-40129 Bologna, Italy. [D'Ammando, F.] Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy. [de Angelis, A.] Univ Udine, Dipartimento Fis, I-33100 Udine, Italy. [de Angelis, A.] Ist Nazl Fis Nucl, Sez Trieste, Grp Collegato Udine, I-33100 Udine, Italy. [de Palma, F.] Univ Telemat Pegaso, Piazza Trieste & Trento 48, I-80132 Naples, Italy. [Desiante, R.] Univ Udine, I-33100 Udine, Italy. [Fukazawa, Y.; Kensei, S.; Ohno, M.; Takahashi, H.] Hiroshima Univ, Dept Phys Sci, Higashihiroshima, Hiroshima 7398526, Japan. [Funk, S.] Erlangen Ctr Astroparticle Phys, D-91058 Erlangen, Germany. [Hewitt, J. W.] Univ North Florida, Dept Phys, 1 UNF Dr, Jacksonville, FL 32224 USA. [Hill, A. B.] Univ Southampton, Highfield, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Johnnesson, G.] Univ Iceland, Inst Sci, IS-107 Reykjavik, Iceland. [Larsson, S.; Li, L.] AlbaNova, KTH Royal Inst Technol, Dept Phys, SE-10691 Stockholm, Sweden. [Larsson, S.; Li, L.] AlbaNova, Oskar Klein Ctr Cosmoparticle Phys, SE-10691 Stockholm, Sweden. [Li, J.; Torres, D. F.] Inst Space Sci IEEC CSIC, Campus UAB, E-08193 Barcelona, Spain. [Mitthumsiri, W.] Mahidol Univ, Fac Sci, Dept Phys, Bangkok 10400, Thailand. [Mizuno, T.; Ohsugi, T.] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Higashihiroshima, Hiroshima 7398526, Japan. [Morselli, A.] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, I-00133 Rome, Italy. [Murgia, S.] Univ Calif Irvine, Ctr Cosmol, Dept Phys & Astron, Irvine, CA 92697 USA. [Ormes, J. F.] Univ Denver, Dept Phys & Astron, Denver, CO 80208 USA. [Paneque, D.] Max Planck Inst Phys & Astrophys, D-80805 Munich, Germany. [Reimer, A.; Reimer, O.] Leopold Franzens Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria. [Reimer, A.; Reimer, O.] Leopold Franzens Univ Innsbruck, Inst Theoret, A-6020 Innsbruck, Austria. [Siskind, E. J.] NYCB Real Time Comp Inc, Lattingtown, NY 11560 USA. [Stawarz, L.] Jagiellonian Univ, Astron Observ, PL-30244 Krakow, Poland. [Torres, D. F.] ICREA, Barcelona, Spain. [Zimmer, S.] Univ Geneva, DPNC, 24 Quai Ernest Ansermet, CH-1211 Geneva 4, Switzerland. [Chekhtman, A.] Naval Res Lab, Washington, DC 20375 USA. RP Cheung, CC (reprint author), Naval Res Lab, Div Space Sci, Washington, DC 20375 USA. EM Teddy.Cheung@nrl.navy.mil; georgano@umbc.edu; jmagill@umd.edu; wmcconvi@umd.edu; stawarz@oa.uj.edu.pl RI Reimer, Olaf/A-3117-2013; Orlando, E/R-5594-2016; Funk, Stefan/B-7629-2015; Bonino, Raffaella/S-2367-2016; Torres, Diego/O-9422-2016; Di Venere, Leonardo/C-7619-2017; OI Reimer, Olaf/0000-0001-6953-1385; Funk, Stefan/0000-0002-2012-0080; Torres, Diego/0000-0002-1522-9065; Di Venere, Leonardo/0000-0003-0703-824X; Hill, Adam/0000-0003-3470-4834; orienti, monica/0000-0003-4470-7094; DI MAURO, MATTIA/0000-0003-2759-5625; Mazziotta, Mario Nicola/0000-0001-9325-4672; Ajello, Marco/0000-0002-6584-1703 FU Istituto Nazionale di Astrofisica in Italy; Centre National d'Etudes Spatiales in France 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. NR 45 TC 2 Z9 2 U1 6 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 JUL 20 PY 2016 VL 826 IS 1 AR 1 DI 10.3847/0004-637X/826/1/1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DU1IU UT WOS:000381962200001 ER PT J AU Ajello, M Ghisellini, G Paliya, VS Kocevski, D Tagliaferri, G Madejski, G Rau, A Schady, P Greiner, J Massaro, F Balokovic, M Buhler, R Giomi, M Marcotulli, L D'Ammando, F Stern, D Boggs, SE Christensen, FE Craig, WW Hailey, CJ Harrison, FA Zhang, WW AF Ajello, M. Ghisellini, G. Paliya, V. S. Kocevski, D. Tagliaferri, G. Madejski, G. Rau, A. Schady, P. Greiner, J. Massaro, F. Balokovic, M. Buehler, R. Giomi, M. Marcotulli, L. D'Ammando, F. Stern, D. Boggs, S. E. Christensen, F. E. Craig, W. W. Hailey, C. J. Harrison, F. A. Zhang, W. W. TI NUSTAR, SWIFT, AND GROND OBSERVATIONS OF THE FLARING MEV BLAZAR PMN J0641-0320 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; quasars: general; quasars: individual (PMN J0641-0320); X-rays: general ID ACTIVE GALACTIC NUCLEI; LARGE-AREA TELESCOPE; SUPERMASSIVE BLACK-HOLES; BURST ALERT TELESCOPE; GAMMA-RAY SOURCES; RELATIVISTIC JETS; DISTANT BLAZAR; HOST GALAXIES; HIGH-REDSHIFT; EMISSION AB MeV blazars are a sub-population of the blazar family, exhibiting larger-than-average jet powers, accretion luminosities, and black hole masses. Because of their extremely hard X-ray continua, these objects are best studied in the X-ray domain. Here, we report on the discovery by the Fermi Large Area Telescope and subsequent follow-up observations with NuSTAR, Swift, and GROND of a new member of the MeV blazar family: PMN J0641-0320. Our optical spectroscopy provides confirmation that this is a flat-spectrum radio quasar located at a redshift of z = 1.196. Its very hard NuSTAR spectrum (power-law photon index of similar to 1 up to similar to 80 keV) indicates that the emission is produced via inverse Compton scattering off of photons coming from outside the jet. The overall spectral energy distribution of PMN J0641-0320 is typical of powerful blazars and, using a simple one-zone leptonic emission model, we infer that the emission region is located either inside the broad line region or within the dusty torus. C1 [Ajello, M.; Paliya, V. S.; Marcotulli, L.] Clemson Univ, Dept Phys & Astron, Kinard Lab Phys, Clemson, SC 29634 USA. [Ghisellini, G.] Ist Nazl Fis Nucl, Osservatorio Astronomico Brera, Via E Bianchi 46, I-23807 Merate, Italy. [Paliya, V. S.] Indian Inst Astrophys, Block 2 Koramangala, Bangalore 560034, Karnataka, India. [Kocevski, D.; Zhang, W. W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Madejski, G.] SLAC Natl Accelerator Lab, Kavli Inst Particle Astrophys & Cosmol, Menlo Pk, CA 94025 USA. [Rau, A.; Schady, P.; Greiner, J.] Max Planck Inst Extraterr Phys, Giessenbachstr 1, D-85748 Garching, Germany. [Massaro, F.] Univ Turin, Dipartimento Fis, Via Pietro Giuria 1, I-10125 Turin, Italy. [Balokovic, M.; Harrison, F. A.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Buehler, R.; Giomi, M.] DESY, D-15738 Zeuthen, Germany. [D'Ammando, F.] INAF, Ist Radioastron, I-40129 Bologna, Italy. [D'Ammando, F.] Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy. [Stern, D.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Boggs, S. E.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Christensen, F. E.; Craig, W. W.] Tech Univ Denmark, DTU Space Natl Space Inst, Elektrovej 327, DK-2800 Lyngby, Denmark. [Craig, W. W.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA. [Hailey, C. J.] Columbia Univ, Columbia Astrophys Lab, 538 W 120th St, New York, NY 10027 USA. RP Ajello, M (reprint author), Clemson Univ, Dept Phys & Astron, Kinard Lab Phys, Clemson, SC 29634 USA. EM majello@clemson.edu RI Massaro, Francesco/L-9102-2016; OI Massaro, Francesco/0000-0002-1704-9850; Ajello, Marco/0000-0002-6584-1703 FU NASA grant [NNH09ZDA001N]; International Fulbright Science and Technology Award; NASA Headquarters under the NASA Earth and Space Science Fellowship Program [NNX14AQ07H]; Istituto Nazionale di Astrofisica in Italy; Centre National d'Etudes Spatiales in France; NASA [NNG08FD60C]; National Aeronautics and Space Administration; Leibniz-Prize (DFG grant) [HA 1850/28-1] FX We thank the anonymous referee for useful comments. M.A. acknowledges generous support from NASA grant NNH09ZDA001N. M.B. acknowledges support from the International Fulbright Science and Technology Award and from NASA Headquarters under the NASA Earth and Space Science Fellowship Program, grant NNX14AQ07H.; 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 LAT as well as scientific data analysis. These include the National Aeronautics and Space Administration and the Department of Energy in the United States, the Commissariat a l'Energie Atomique and the Centre National de la Recherche Scientifique/Institut National de Physique Nucleaire et de Physique des Particules in France, the Agenzia Spaziale Italiana and the Istituto Nazionale di Fisica Nucleare in Italy, the Ministry of Education, Culture, Sports, Science, and Technology (MEXT), High Energy Accelerator Research Organization (KEK) and Japan Aerospace Exploration Agency (JAXA) in Japan, and the K. A. Wallenberg Foundation, the Swedish Research Council and the Swedish National Space Board in Sweden. Additional support for science analysis during the operations phase is gratefully acknowledged from the Istituto Nazionale di Astrofisica in Italy and the Centre National d'Etudes Spatiales in France.; This NuSTAR work was supported under NASA Contract No. NNG08FD60C, and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software, and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA).; Part of this work is based on archival data, software, or online services provided by the ASI Data Center (ASDC). This research has made use of the XRT Data Analysis Software (XRTDAS). Part of the funding for GROND (both hardware and personnel) was generously granted by the Leibniz-Prize to G. Hasinger (DFG grant HA 1850/28-1). NR 66 TC 0 Z9 0 U1 1 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 20 PY 2016 VL 826 IS 1 AR 76 DI 10.3847/0004-637X/826/1/76 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DU1IU UT WOS:000381962200076 ER PT J AU Brightman, M Masini, A Ballantyne, DR Balokovic, M Brandt, WN Chen, CT Comastri, A Farrah, D Gandhi, P Harrison, FA Ricci, C Stern, D Walton, DJ AF Brightman, M. Masini, A. Ballantyne, D. R. Balokovic, M. Brandt, W. N. Chen, C. -T. Comastri, A. Farrah, D. Gandhi, P. Harrison, F. A. Ricci, C. Stern, D. Walton, D. J. TI A GROWTH-RATE INDICATOR FOR COMPTON-THICK ACTIVE GALACTIC NUCLEI SO ASTROPHYSICAL JOURNAL LA English DT Article DE black hole physics; galaxies: general; galaxies: nuclei; galaxies: Seyfert; masers ID SUPERMASSIVE BLACK-HOLES; RAY SPECTRAL MODEL; H2O MASER EMISSION; X-RAY; CIRCINUS GALAXY; ACCRETION DISK; NGC 1068; BOLOMETRIC LUMINOSITIES; NUSTAR OBSERVATIONS; MEGAMASER DISKS AB Due to their heavily obscured central engines, the growth rate of Compton-thick (CT) active galactic nuclei (AGNs) is difficult to measure. A statistically significant correlation between the Eddington ratio, lambda(Edd), and the X-ray power-law index, Gamma, observed in unobscured AGNs offers an estimate of their growth rate from X-ray spectroscopy (albeit with large scatter). However, since X-rays undergo reprocessing by Compton scattering and photoelectric absorption when the line of sight to the central engine is heavily obscured, the recovery of the intrinsic Gamma is challenging. Here we study a sample of local, predominantly CT megamaser AGNs, where the black hole mass, and thus Eddington luminosity, are well known. We compile results of the X-ray spectral fitting of these sources with sensitive high-energy (E > 10 keV) NuSTAR data, where X-ray torus models, which take into account the reprocessing effects have been used to recover the intrinsic Gamma values and X-ray luminosities, L-X. With a simple bolometric correction to L-X to calculate lambda(Edd), we find a statistically significant correlation between Gamma and lambda(Edd) (p = 0.007). A linear fit to the data yields Gamma = (0.41 +/- 0.18)log(10)lambda(Edd) + (2.38 +/- 0.20), which is statistically consistent with results for unobscured AGNs. This result implies that torus modeling successfully recovers the intrinsic AGN parameters. Since the megamasers have low-mass black holes (M-BH approximate to 10(6)-10(7) M-circle dot) and are highly inclined, our results extend the Gamma-lambda(Edd) relationship to lower masses and argue against strong orientation effects in the corona, in support of AGN unification. Finally this result supports the use of Gamma as a growth-rate indicator for accreting black holes, even for CT AGNs. C1 [Brightman, M.; Balokovic, M.; Harrison, F. A.; Walton, D. J.] CALTECH, Cahill Ctr Astrophys, 1216 East Calif Blvd, Pasadena, CA 91125 USA. [Masini, A.; Comastri, A.] INAF Osservatorio Astron Bologna, Via Ranzani 1, I-40127 Bologna, Italy. [Masini, A.] Univ Bologna, Dipartimento Fis & Astron DIFA, Viale Berti Pichat 6-2, I-40127 Bologna, Italy. [Ballantyne, D. R.] Georgia Inst Technol, Sch Phys, Ctr Relativist Astrophys, Atlanta, GA 30332 USA. [Brandt, W. N.; Chen, C. -T.] Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA. [Farrah, D.] Virginia Tech, Dept Phys, Blacksburg, VA 24061 USA. [Gandhi, P.] Univ Southampton, Dept Phys & Astron, Southampton SO17 1BJ, Hants, England. [Ricci, C.] Pontificia Univ Catolica Chile, Fac Fis, Inst Astrofis, Casilla 306, Santiago 22, Chile. [Stern, D.; Walton, D. J.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. RP Brightman, M (reprint author), CALTECH, Cahill Ctr Astrophys, 1216 East Calif Blvd, Pasadena, CA 91125 USA. OI Comastri, Andrea/0000-0003-3451-9970 FU NASA [NNG08FD60C]; National Aeronautics and Space Administration; ASI/INAF [I/037/12/0-011/13]; STFC [ST/J003697/2]; NASA Headquarters under the NASA Earth and Space Science Fellowship Program [NNX14AQ07H] FX This work was supported under NASA Contract No. NNG08FD60C, and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software and Calibration teams for support with the execution and analysis of these observations. Furthermore, 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. A.M. and A.C. acknowledge support from the ASI/INAF grant I/037/12/0-011/13. P.G. acknowledges funding from STFC (ST/J003697/2). M.B. acknowledges support from NASA Headquarters under the NASA Earth and Space Science Fellowship Program, grant NNX14AQ07H. NR 66 TC 3 Z9 3 U1 5 U2 9 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 20 PY 2016 VL 826 IS 1 AR 93 DI 10.3847/0004-637X/826/1/93 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DU1IU UT WOS:000381962200093 ER PT J AU Darling, J Gerard, B Amiri, N Lawrence, K AF Darling, Jeremy Gerard, Benjamin Amiri, Nikta Lawrence, Kelsey TI WATER MASERS IN THE ANDROMEDA GALAXY. I. A SURVEY FOR WATER MASERS, AMMONIA, AND HYDROGEN RECOMBINATION LINES SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: individual (M31); galaxies: ISM; ISM: molecules; Local Group; masers; radio lines: galaxies ID STAR-FORMING REGIONS; PROPER-MOTION; LOCAL GROUP; NEARBY GALAXIES; MILKY-WAY; GALACTIC H-2-REGIONS; SPACE-TELESCOPE; MOLECULAR GAS; HOT AMMONIA; H2O MASERS AB We report the results of a Green Bank Telescope survey for water masers, ammonia (1, 1) and (2, 2), and the H66 alpha recombination line toward 506 luminous compact 24 mu m emitting regions in the Andromeda Galaxy (M31). We include the 206 sources observed in the Darling water maser survey for completeness. The survey was sensitive enough to detect any maser useful for similar to 10 mu as yr(-1) astrometry. No new water masers, ammonia lines, or H66 alpha recombination lines were detected individually or in spectral stacks reaching rms noise levels of similar to 3 mJy and similar to 0.2 mJy, respectively, in 3.1-3.3 km s(-1) channels. The lack of detections in individual spectra and in the spectral stacks is consistent with Galactic extrapolations. Contrary to previous assertions, there do not seem to be any additional bright water masers to be found in M31. The strong variability of water masers may enable new maser detections in the future, but variability may also limit the astrometric utility of known (or future) masers because flaring masers must also fade. C1 [Darling, Jeremy; Gerard, Benjamin; Amiri, Nikta; Lawrence, Kelsey] Univ Colorado, Dept Astrophys & Planetary Sci, Ctr Astrophys & Space Astron, 389 UCB, Boulder, CO 80309 USA. [Gerard, Benjamin] Univ Victoria, Dept Phys & Astron, 3800 Finnerty Rd, Victoria, BC V8P 5C2, Canada. [Amiri, Nikta] Jet Prop Lab, M-S 238-600,4800 Oak Grove Dr, Pasadena, CA 91109 USA. RP Darling, J (reprint author), Univ Colorado, Dept Astrophys & Planetary Sci, Ctr Astrophys & Space Astron, 389 UCB, Boulder, CO 80309 USA. EM jdarling@colorado.edu OI Gerard, Benjamin/0000-0003-3978-9195; Darling, Jeremy/0000-0003-2511-2060 FU NSF [AST-1109078] FX All authors acknowledge support from the NSF grant AST-1109078. The authors thank K. Gordon for the Spitzer map, M. Claussen and T. Beasley for sharing their results, and the anonymous referee for helpful comments. This research has made use of NASA's Astrophysics Data System Bibliographic Services and the NASA/IPAC Extragalactic Database (NED), and uses observations made with the Spitzer Space Telescope, both of which are operated by the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. NR 49 TC 1 Z9 1 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 20 PY 2016 VL 826 IS 1 AR 24 DI 10.3847/0004-637X/826/1/24 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DU1IU UT WOS:000381962200024 ER PT J AU Gotthelf, EV Mori, K Aliu, E Paredes, JM Tomsick, JA Boggs, SE Christensen, FE Craig, WW Hailey, CJ Harrison, FA Hong, JS Rahoui, F Stern, D Zhang, WW AF Gotthelf, E. V. Mori, K. Aliu, E. Paredes, J. M. Tomsick, J. A. Boggs, S. E. Christensen, F. E. Craig, W. W. Hailey, C. J. Harrison, F. A. Hong, J. S. Rahoui, F. Stern, D. Zhang, W. W. TI HARD X-RAY EMISSION FROM SH 2-104: A NuSTAR SEARCH FOR GAMMA-RAY COUNTERPARTS SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: individual objects (Sh 2-104, MGRO J2019+37, 3XMM J201744.7+365045, VER J2019+368); pulsars: individual (NuSTAR J201744.3+364812); stars: neutron ID GALACTIC PLANE; CLUSTER WESTERLUND-1; TEMPERATURE RELATION; MGRO J2019+37; XMM-NEWTON; TELESCOPE; DISCOVERY; REGION; YOUNG; PULSAR AB We present NuSTAR hard X-ray observations of Sh 2-104, a compact H II region containing several young massive stellar clusters (YMSCs). We have detected distinct hard X-ray sources coincident with localized VERITAS TeV emission recently resolved from the giant gamma-ray complex MGRO J2019+37 in the Cygnus region. Fainter, diffuse X-rays coincident with the eastern YMSC in Sh2-104 likely result from the colliding winds of a component star. Just outside the radio shell of Sh 2-104 lies 3XMM J201744.7+365045 and a nearby nebula, NuSTAR J201744.3+364812, whose properties are most consistent with extragalactic objects. The combined XMM-Newton and NuSTAR spectrum of 3XMM J201744.7+365045 is well-fit to an absorbed power-law model with N-H= (3.1 +/- 1.0) x 10(22) cm(-2) and a photon index Gamma= 2.1 +/- 0.1. Based on possible long-term flux variation and the lack of detected pulsations (<= 43% modulation), this object is likely a background active galactic nucleus rather than a Galactic pulsar. The spectrum of the NuSTAR nebula shows evidence of an emission line at E = 5.6 keV, suggesting an optically obscured galaxy cluster at z = 0.19 +/- 0.02 (d = 800 Mpc) and L-X = 1.2 x 10(44) erg s(-1). Follow-up Chandra observations of Sh 2-104 will help identify the nature of the X-ray sources and their relation to MGRO J2019+37. We also show that the putative VERITAS excess south of Sh 2-104, is most likely associated with the newly discovered Fermi pulsar PSR J2017+3625 and not the H II region. C1 [Gotthelf, E. V.; Mori, K.; Hailey, C. J.] Columbia Univ, Columbia Astrophys Lab, 550 West 120th St, New York, NY 10027 USA. [Gotthelf, E. V.; Aliu, E.; Paredes, J. M.] Univ Barcelona, IEEC UB, Dept Fis Quant & Astrofis, Inst Ciencies Cosmos, Marti i Franques 1, E-08028 Barcelona, Spain. [Tomsick, J. A.; Boggs, S. E.; Craig, W. W.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Christensen, F. E.] Tech Univ Denmark, DTU Space Natl Space Inst, Elektrovej 327, DK-2800 Lyngby, Denmark. [Craig, W. W.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA. [Harrison, F. A.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Hong, J. S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Rahoui, F.] Harvard Univ, Dept Astron, 60 Garden St, Cambridge, MA 02138 USA. [Stern, D.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Zhang, W. W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Rahoui, F.] European Southern Observ, Karl Schwarzchild Str 2, D-85748 Garching, Germany. RP Gotthelf, EV (reprint author), Columbia Univ, Columbia Astrophys Lab, 550 West 120th St, New York, NY 10027 USA.; Gotthelf, EV (reprint author), Univ Barcelona, IEEC UB, Dept Fis Quant & Astrofis, Inst Ciencies Cosmos, Marti i Franques 1, E-08028 Barcelona, Spain. EM eric@astro.columbia.edu FU NASA [NNG08FD60C]; National Aeronautics and Space Administration; National Aeronautics and Space Administration through XMM-Newton Award [NNX15AG28G]; Chandra Award [G05-16061X]; National Aeronautics Space Administration [NAS8-03060]; Spanish MINECO under grants of ICCUB (Unidad de Excelencia "Maria de Maeztu") [AYA2013-47447-C3-1-P, MDM-2014-0369]; Catalan DEC grant [SGR 86]; ICREA Academia FX This work was supported under NASA Contract No. NNG08FD60C and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR operations, software, and calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). E.V.G. acknowledges partial support by the National Aeronautics and Space Administration through XMM-Newton Award Number NNX15AG28G and Chandra Award Number G05-16061X, issued by the Chandra X-ray Observatory Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of the National Aeronautics Space Administration under contract NAS8-03060. J.M.P. acknowledges support by the Spanish MINECO under grants AYA2013-47447-C3-1-P, MDM-2014-0369 of ICCUB (Unidad de Excelencia "Maria de Maeztu"), and the Catalan DEC grant 2014 SGR 86 and ICREA Academia. NR 44 TC 0 Z9 0 U1 1 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 20 PY 2016 VL 826 IS 1 AR 25 DI 10.3847/0004-637X/826/1/25 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DU1IU UT WOS:000381962200025 ER PT J AU Grefenstette, BW Glesener, L Krucker, S Hudson, H Hannah, IG Smith, DM Vogel, JK White, SM Madsen, KK Marsh, AJ Caspi, A Chen, B Shih, A Kuhar, M Boggs, SE Christensen, FE Craig, WW Forster, K Hailey, CJ Harrison, FA Miyasaka, H Stern, D Zhang, WW AF Grefenstette, Brian W. Glesener, Lindsay Krucker, Sam Hudson, Hugh Hannah, Iain G. Smith, David M. Vogel, Julia K. White, Stephen M. Madsen, Kristin K. Marsh, Andrew J. Caspi, Amir Chen, Bin Shih, Albert Kuhar, Matej Boggs, Steven E. Christensen, Finn E. Craig, William W. Forster, Karl Hailey, Charles J. Harrison, Fiona A. Miyasaka, Hiromasa Stern, Daniel Zhang, William W. TI THE FIRST FOCUSED HARD X-RAY IMAGES OF THE SUN WITH NuSTAR SO ASTROPHYSICAL JOURNAL LA English DT Article DE acceleration of particles; methods: data analysis; Sun: X-rays, gamma rays ID SOLAR-FLARES; ACCELERATION REGION; ENERGY-DISTRIBUTION; QUIET SUN; MICROFLARES; NANOFLARES; TELESCOPE; MISSION; RHESSI; EMISSION AB We present results from the the first campaign of dedicated solar observations undertaken by the Nuclear Spectroscopic Telescope ARray (NuSTAR) hard X-ray (HXR) telescope. Designed as an astrophysics mission, NuSTAR nonetheless has the capability of directly imaging the Sun at HXR energies (>3 keV) with an increase in sensitivity of at least two magnitude compared to current non-focusing telescopes. In this paper we describe the scientific areas where NuSTAR will make major improvements on existing solar measurements. We report on the techniques used to observe the Sun with NuSTAR, their limitations and complications, and the procedures developed to optimize solar data quality derived from our experience with the initial solar observations. These first observations are briefly described, including the measurement of the Fe K-shell lines in a decaying X-class flare, HXR emission from high in the solar corona, and full-disk HXR images of the Sun. C1 [Grefenstette, Brian W.; Madsen, Kristin K.; Forster, Karl; Harrison, Fiona A.; Miyasaka, Hiromasa] CALTECH, Cahill Ctr Astrophys, 1216 E Calif Blvd, Pasadena, CA 91125 USA. [Glesener, Lindsay] Univ Minnesota Twin Cities, Sch Phys & Astron, Minneapolis, MN 55455 USA. [Glesener, Lindsay; Krucker, Sam; Hudson, Hugh; Boggs, Steven E.; Craig, William W.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Krucker, Sam; Kuhar, Matej] Univ Appl Sci & Arts Northwestern Switzerland, CH-5210 Windisch, Switzerland. [Hudson, Hugh; Hannah, Iain G.] Univ Glasgow, SUPA Sch Phys & Astron, Glasgow G12 8QQ, Lanark, Scotland. [Smith, David M.; Marsh, Andrew J.] Univ Calif Santa Cruz, Dept Phys, 1156 High St, Santa Cruz, CA 95064 USA. [Smith, David M.; Marsh, Andrew J.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, 1156 High St, Santa Cruz, CA 95064 USA. [Vogel, Julia K.] Lawrence Livermore Natl Lab, Phys & Life Sci Directorate, Div Phys, Livermore, CA 94550 USA. [White, Stephen M.] US Air Force, Res Lab, Albuquerque, NM USA. [Caspi, Amir] Southwest Res Inst, Boulder, CO 80302 USA. [Chen, Bin] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Shih, Albert] NASA, Goddard Space Flight Ctr, Solar Phys Lab, Greenbelt, MD 20771 USA. [Christensen, Finn E.] Tech Univ Denmark, Natl Space Inst, DTU Space, Elektrovej 327, DK-2800 Lyngby, Denmark. [Craig, William W.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA. [Hailey, Charles J.] Columbia Univ, Columbia Astrophys Lab, 538 W 120th St, New York, NY 10027 USA. [Stern, Daniel] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Zhang, William W.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. RP Grefenstette, BW (reprint author), CALTECH, Cahill Ctr Astrophys, 1216 E Calif Blvd, Pasadena, CA 91125 USA. EM bwgref@srl.caltech.edu RI Hannah, Iain/F-1972-2011; OI Hannah, Iain/0000-0003-1193-8603; Hudson, Hugh/0000-0001-5685-1283; Glesener, Lindsay/0000-0001-7092-2703; Madsen, Kristin/0000-0003-1252-4891; Caspi, Amir/0000-0001-8702-8273 FU NASA [NNX12AJ36G, NNX14AG07G, NNX15AK26G, NNX14AN84G]; Swiss National Science Foundation [200021-140308]; NASA Earth and Space Science Fellowship [NNX13AM41H]; U.S. Department of Energy by Lawrence Livermore National Laboratory [DE-AC52-07NA27344]; Royal Society University Research Fellowship FX This work was supported under NASA contract NNG08FD60C and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by NASA. Additional funding for this work was also provided under NASA grants NNX12AJ36G and NNX14AG07G. S.K. acknowledges funding from the Swiss National Science Foundation (200021-140308). A.J.M.'s participation was supported by NASA Earth and Space Science Fellowship award NNX13AM41H. Part of this work was performed under the auspices of the U.S. Department of Energy by Lawrence Livermore National Laboratory under Contract DE-AC52-07NA27344. A.C. was supported by NASA grants NNX15AK26G and NNX14AN84G. I.G.H. is supported by a Royal Society University Research Fellowship. NR 37 TC 3 Z9 3 U1 1 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 20 PY 2016 VL 826 IS 1 AR 20 DI 10.3847/0004-637X/826/1/20 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DU1IU UT WOS:000381962200020 ER PT J AU Kaplan, DL Kupfer, T Nice, DJ Irrgang, A Heber, U Arzoumanian, Z Beklen, E Crowter, K DeCesar, ME Demorest, PB Dolch, T Ellis, JA Ferdman, RD Ferrara, EC Fonseca, E Gentile, PA Jones, G Jones, ML Kreuzer, S Lam, MT Levin, L Lorimer, DR Lynch, RS McLaughlin, MA Miller, AA Ng, C Pennucci, TT Prince, TA Ransom, SM Ray, PS Spiewak, R Stairs, IH Stovall, K Swiggum, J Zhu, WW AF Kaplan, David L. Kupfer, Thomas Nice, David J. Irrgang, Andreas Heber, Ulrich Arzoumanian, Zaven Beklen, Elif Crowter, Kathryn DeCesar, Megan E. Demorest, Paul B. Dolch, Timothy Ellis, Justin A. Ferdman, Robert D. Ferrara, Elizabeth C. Fonseca, Emmanuel Gentile, Peter A. Jones, Glenn Jones, Megan L. Kreuzer, Simon Lam, Michael T. Levin, Lina Lorimer, Duncan R. Lynch, Ryan S. McLaughlin, Maura A. Miller, Adam A. Ng, Cherry Pennucci, Timothy T. Prince, Tom A. Ransom, Scott M. Ray, Paul S. Spiewak, Renee Stairs, Ingrid H. Stovall, Kevin Swiggum, Joseph Zhu, Weiwei TI PSR J1024-0719: A MILLISECOND PULSAR IN AN UNUSUAL LONG-PERIOD ORBIT SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: general; pulsars: individual (PSR J1024-0719); stars: distances ID SKY SURVEY 2MASS; GLOBULAR-CLUSTERS; MILKY-WAY; PROPER MOTIONS; NEUTRON-STARS; BINARY PULSAR; EVOLUTION; RESOLUTION; DISCOVERY; TELESCOPE AB PSR J1024-0719 is a millisecond pulsar that was long thought to be isolated. However, puzzling results concerning its velocity, distance, and low rotational period derivative have led to a reexamination of its properties. We present updated radio timing observations along with new and archival optical data which show that PSR J1024-0719 is most likely in a long-period (2-20 kyr) binary system with a low-mass (approximate to 0.4 M-circle dot), low-metallicity (Z approximate to -0.9 dex) main-sequence star. Such a system can explain most of the anomalous properties of this pulsar. We suggest that this system formed through a dynamical exchange in a globular cluster that ejected it into a halo orbit, which is consistent with the low observed metallicity for the stellar companion. Further astrometric and radio timing observations such as measurement of the third period derivative could strongly constrain the range of orbital parameters. C1 [Kaplan, David L.; DeCesar, Megan E.; Spiewak, Renee; Swiggum, Joseph] Univ Wisconsin, Dept Phys, Ctr Gravitat Cosmol & Astrophys, POB 413, Milwaukee, WI 53201 USA. [Kupfer, Thomas; Miller, Adam A.; Prince, Tom A.] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA. [Nice, David J.] Lafayette Coll, Dept Phys, Easton, PA 18042 USA. [Irrgang, Andreas; Heber, Ulrich; Kreuzer, Simon] Univ Erlangen Nurnberg, Astron Inst, Dr Karl Remeis Observ & ECAP, Sternwartstr 7, D-96049 Bamberg, Germany. [Arzoumanian, Zaven] NASA, Goddard Space Flight Ctr, Ctr Res & Explorat Space Sci & Technol, Code 662, Greenbelt, MD 20771 USA. [Arzoumanian, Zaven] NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, Code 662, Greenbelt, MD 20771 USA. [Beklen, Elif] Suleyman Demirel Univ, Dept Phys, TR-32260 Isparta, Turkey. [Beklen, Elif; Gentile, Peter A.; Jones, Megan L.; Levin, Lina; Lorimer, Duncan R.; McLaughlin, Maura A.] West Virginia Univ, Dept Phys & Astron, POB 6315, Morgantown, WV 26506 USA. [Crowter, Kathryn; Fonseca, Emmanuel; Ng, Cherry; Stairs, Ingrid H.] Univ British Columbia, Dept Phys & Astron, 6224 Agr Rd, Vancouver, BC V6T 1Z1, Canada. [Demorest, Paul B.] Natl Radio Astron Observ, 1003 Lopezville Rd, Socorro, NM 87801 USA. [Dolch, Timothy] Hillsdale Coll, Dept Phys, 33 E Coll St, Hillsdale, MI 49242 USA. [Ellis, Justin A.; Miller, Adam A.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Ferdman, Robert D.] McGill Univ, Dept Phys, 3600 Univ St, Montreal, PQ H3A 2T8, Canada. [Ferrara, Elizabeth C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Jones, Glenn] Columbia Univ, Dept Phys, New York, NY 10027 USA. [Lam, Michael T.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. [Lynch, Ryan S.] Natl Radio Astron Observ, POB 2, Green Bank, WV 24944 USA. [Pennucci, Timothy T.] Univ Virginia, Dept Astron, POB 400325, Charlottesville, VA 22904 USA. [Ransom, Scott M.] Natl Radio Astron Observ, 520 Edgemont Rd, Charlottesville, VA 22903 USA. [Ray, Paul S.] Naval Res Lab, Div Space Sci, Washington, DC 20375 USA. [Stairs, Ingrid H.] McGill Space Inst, 3550 Rue Univ, Montreal, PQ H3A 2A7, Canada. [Stovall, Kevin] Univ New Mexico, Dept Phys & Astron, Albuquerque, NM 87131 USA. [Miller, Adam A.; Zhu, Weiwei] Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany. RP Kaplan, DL (reprint author), Univ Wisconsin, Dept Phys, Ctr Gravitat Cosmol & Astrophys, POB 413, Milwaukee, WI 53201 USA. RI Heber, Ulrich/G-3306-2013; OI Heber, Ulrich/0000-0001-7798-6769; Kaplan, David/0000-0001-6295-2881 FU National Science Foundation (NSF) PIRE program [0968296]; NSF Physics Frontiers Center [1430284]; NSERC Discovery Grant; Canadian Institute for Advanced Research; NASA from a Hubble Fellowship [HST-HF-51325.01]; STScI; NASA [NAS 5-26555] FX We thank J. Creighton, C. Bassa, and S. Phinney for useful discussions. The NANOGrav project receives support from National Science Foundation (NSF) PIRE program award number 0968296 and NSF Physics Frontiers Center award number 1430284. P.S.R.'s work at NRL is supported by the Chief of Naval Research. Pulsar research at UBC is supported by an NSERC Discovery Grant and by the Canadian Institute for Advanced Research. A.A.M. acknowledges support for this work by NASA from a Hubble Fellowship grant: HST-HF-51325.01, awarded by STScI, operated by AURA, Inc., for NASA, under contract NAS 5-26555. Part of the research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. NR 67 TC 2 Z9 2 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 20 PY 2016 VL 826 IS 1 AR 86 DI 10.3847/0004-637X/826/1/86 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DU1IU UT WOS:000381962200086 ER PT J AU Keek, L Wolf, Z Ballantyne, DR AF Keek, L. Wolf, Z. Ballantyne, D. R. TI ACCRETION DISK SIGNATURES IN TYPE I X-RAY BURSTS: PROSPECTS FOR FUTURE MISSIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; stars: neutron; X-rays: binaries; X-rays: bursts ID EQUATION-OF-STATE; NEUTRON-STARS; TIMING-EXPLORER; THERMONUCLEAR BURSTS; ANGULAR-DISTRIBUTION; SPECTRAL EVOLUTION; MILLISECOND PULSAR; EXO 0748-676; 4U 1636-536; AQL X-1 AB Type I X-ray bursts and superbursts from accreting neutron stars illuminate the accretion disk and produce a reflection signal that evolves as the burst fades. Examining the evolution of reflection features in the spectra will provide insight into the burst-disk interaction, a potentially powerful probe of accretion disk physics. At present, reflection has been observed during only two bursts of exceptional duration. We investigate the detectability of reflection signatures with four of the latest well-studied X-ray observatory concepts: Hitomi, Neutron Star Interior Composition Explorer (NICER), Athena, and Large Observatory For X-ray Timing (LOFT). Burst spectra are modeled for different values for the flux, temperature, and the disk ionization parameter, which are representative for most known bursts and sources. The effective area and throughput of a Hitomi-like telescope are insufficient for characterizing burst reflection features. NICER and Athena will detect reflection signatures in Type I bursts with peak fluxes. greater than or similar to 10(-7.5) erg cm(-2) s(-1) and also effectively constrain the reflection parameters for bright bursts with fluxes of similar to 10(-7) erg cm(-2) s(-1) in exposures of several seconds. Thus, these observatories will provide crucial new insight into the interaction of accretion flows and X-ray bursts. For sources with low line-of-sight absorption, the wide bandpass of these instruments allows for the detection of soft X-ray reflection features, which are sensitive to the disk metallicity and density. The large collecting area that is part of the LOFT design would revolutionize the field by tracing the evolution of the accretion geometry in detail throughout short bursts. C1 [Keek, L.] NASA, CRESST, GSFC, Greenbelt, MD 20771 USA. [Keek, L.] NASA, Xray Astrophys Lab, GSFC, Greenbelt, MD 20771 USA. [Keek, L.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Wolf, Z.; Ballantyne, D. R.] Georgia Inst Technol, Sch Phys, Ctr Relativist Astrophys, 837 State St, Atlanta, GA 30332 USA. RP Keek, L (reprint author), NASA, CRESST, GSFC, Greenbelt, MD 20771 USA.; Keek, L (reprint author), NASA, Xray Astrophys Lab, GSFC, Greenbelt, MD 20771 USA.; Keek, L (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA. EM laurens.keek@nasa.gov FU NASA [NNG06EO90A] FX The authors thank R.E. Rutledge for encouraging to write this paper and T.E. Strohmayer for helpful comments. L.K. is supported by NASA under award number NNG06EO90A. L.K. thanks the International Space Science Institute in Bern, Switzerland for hosting an International Team on X-ray bursts. NR 77 TC 1 Z9 1 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 20 PY 2016 VL 826 IS 1 AR 79 DI 10.3847/0004-637X/826/1/79 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DU1IU UT WOS:000381962200079 ER PT J AU Kinch, BE Schnittman, JD Kallman, TR Krolik, JH AF Kinch, Brooks E. Schnittman, Jeremy D. Kallman, Timothy R. Krolik, Julian H. TI Fe K alpha PROFILES FROM SIMULATIONS OF ACCRETING BLACK HOLES SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; black hole physics; line: formation ID X-RAY REFLECTION; ACTIVE GALACTIC NUCLEI; SEYFERT-GALAXIES; RADIATION TRANSPORT; IRON LINES; GX 339-4; DISKS; EMISSION; SPECTRA; SPIN AB We present the first results from a new technique for the prediction of Fe K alpha profiles directly from general relativistic magnetohydrodynamic (GRMHD) simulations. Data from a GRMHD simulation are processed by a Monte Carlo global radiation transport code, which determines the X-ray flux irradiating the disk surface and the coronal electron temperature self-consistently. With that irradiating flux and the disk's density structure drawn from the simulation, we determine the reprocessed Fe K alpha emission from photoionization equilibrium and solution of the radiation transfer equation. We produce maps of the surface brightness of Fe K alpha emission over the disk surface, which-for our example of a 10M(circle dot) Schwarzschild black hole accreting at 1% the Eddington value-rises steeply one gravitational radius outside the radius of the innermost stable circular orbit and then falls alpha r(-2) at larger radii. We explain these features of the Fe K alpha radial surface brightness profile as consequences of the disk's ionization structure and an extended coronal geometry, respectively. We also present the corresponding Fe K alpha line profiles as would be seen by distant observers at several inclinations. Both the shapes of the line profiles and the equivalent widths of our predicted K alpha lines are qualitatively similar to those typically observed from accreting black holes. Most importantly, this work represents a direct link between theory and observation: in a fully self-consistent way, we produce observable results-iron fluorescence line profiles-from the theory of black hole accretion with almost no phenomenological assumptions. C1 [Kinch, Brooks E.; Krolik, Julian H.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Schnittman, Jeremy D.; Kallman, Timothy R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Kinch, BE (reprint author), Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. EM kinch@jhu.edu; jeremy.d.schnittman@nasa.gov; timothy.r.kallman@nasa.gov; jhk@jhu.edu FU NASA/ATP Grant [NNX14AB43G, 13-0077]; NSF Grant [AST-0908869]; NASA grant FX This work was partially supported by NASA/ATP Grant NNX14AB43G, NSF Grant AST-0908869, and NASA/ATP Grant 13-0077. We are particularly grateful to John Hawley for providing funds from the NSF grant and to John Baker for funds from the latter NASA grant. B.E.K. also thanks the GSFC Laboratory for High Energy Astrophysics for hospitality. NR 45 TC 0 Z9 0 U1 1 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 20 PY 2016 VL 826 IS 1 AR 52 DI 10.3847/0004-637X/826/1/52 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DU1IU UT WOS:000381962200052 ER PT J AU Lanz, L Ogle, PM Alatalo, K Appleton, PN AF Lanz, Lauranne Ogle, Patrick M. Alatalo, Katherine Appleton, Philip N. TI STAR FORMATION SUPPRESSION DUE TO JET FEEDBACK IN RADIO GALAXIES WITH SHOCKED WARM MOLECULAR GAS SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: evolution; galaxies: ISM; galaxies: jets; galaxies: star formation ID ACTIVE GALACTIC NUCLEI; SPITZER-SPACE-TELESCOPE; DIGITAL-SKY-SURVEY; SPECTRAL IRRADIANCE CALIBRATION; MULTIBAND IMAGING PHOTOMETER; CO-TO-H-2 CONVERSION FACTOR; INFRARED ARRAY CAMERA; SIMILAR-TO 0.1; X-RAY; HYDROGEN EMISSION AB We present Herschel observations of 22 radio galaxies, selected for the presence of shocked, warm molecular hydrogen emission. We measured and modeled spectral energy distributions in 33 bands from the ultraviolet to the far-infrared to investigate the impact of jet feedback on star formation activity. These galaxies are massive, early type galaxies with normal gas-to-dust ratios, covering a range of optical and infrared colors. We find that the star formation rate (SFR) is suppressed by a factor of similar to 3-6, depending on how molecular gas mass is estimated. We suggest that this suppression is due to the shocks driven by the radio jets injecting turbulence into the interstellar medium (ISM), which also powers the luminous warm H-2 line emission. Approximately 25% of the sample shows suppression by more than a factor of 10. However, the degree of SFR suppression does not correlate with indicators of jet feedback including jet power, diffuse X-ray emission, or intensity of warm molecular H-2 emission, suggesting that while injected turbulence likely impacts star formation, the process is not purely parameterized by the amount of mechanical energy dissipated into the ISM. Radio galaxies with shocked warm molecular gas cover a wide range in SFR stellar mass space, indicating that these galaxies are in a variety of evolutionary states, from actively star-forming and gas-rich to quiescent and gas-poor. SFR suppression appears to have the largest impact on the evolution of galaxies that are moderately gas-rich. C1 [Lanz, Lauranne; Ogle, Patrick M.; Appleton, Philip N.] CALTECH, Infrared Proc & Anal Ctr, MC100-22, Pasadena, CA 91125 USA. [Alatalo, Katherine] Observ Carnegie Inst Washington, 813 Santa Barbara St, Pasadena, CA 91101 USA. [Appleton, Philip N.] CALTECH, NASA, Herschel Sci Ctr, IPAC, MC100-22, Pasadena, CA 91125 USA. RP Lanz, L (reprint author), CALTECH, Infrared Proc & Anal Ctr, MC100-22, Pasadena, CA 91125 USA. EM llanz@ipac.caltech.edu OI Alatalo, Katherine/0000-0002-4261-2326 FU NASA through an award issued by JPL/Caltech; NASA through Hubble Fellowship grant - Space Telescope Science Institute [HST-HF2-51352.001]; NASA [NAS5-26555]; NASA; NSF; Sloan Digital Sky Survey (Sloan-III); Alfred P. Sloan Foundation; Participating Institutions; U.S. DOE Office of Science; Association of Universities for Research in Astronomy, Inc., under NASA [NAS5-26555]; NASA Office of Space Science [NNX09AF08G] FX We thank Mark Lacy for his advice and useful discussion with regards to the Sajina model, as well as George Helou for suggesting the extended Schmidt law as another point of analysis, and Yong Shi, Michael Brown, and Aditya Togi, whose comments improved the revised version of this paper. This work made use of the remote access computing accounts of the NASA Herschel Science Center, which were very helpful in reducing the Herschel data. L.L. and P.M.O. acknowledges support for this work provided by NASA through an award issued by JPL/Caltech. Support for K.A. is provided by NASA through Hubble Fellowship grant #HST-HF2-51352.001 awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS5-26555.; This work is based in part on observations made with Herschel, a European Space Agency Cornerstone Mission with significant participation by NASA. This publication used observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory (JPL)/California Institute of Technology (Caltech) under a contract with NASA. Observations from the Wide-field Iqrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and JPL/Caltech, funded by NASA, were also used. 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 (IPAC)/Caltech, funded by NASA and the NSF, as well as from the Sloan Digital Sky Survey (Sloan-III),whose funding has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the NSF, and the U.S. DOE Office of Science, and which is managed by the Astrophysical Research Consortium for the Participating Institutions of the Sloan-III Collaboration. Finally, this publication makes use of data from the Galaxy Evolution Explorer, retrieved from the Mikulski Archive for Space Telescopes (MAST), part of 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 MAST for non-HST data is provided by the NASA Office of Space Science via grant NNX09AF08G and by other grants and contracts. NR 132 TC 1 Z9 1 U1 3 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 20 PY 2016 VL 826 IS 1 AR 29 DI 10.3847/0004-637X/826/1/29 PG 40 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DU1IU UT WOS:000381962200029 ER PT J AU Lynch, BJ Edmondson, JK Kazachenko, MD Guidoni, SE AF Lynch, B. J. Edmondson, J. K. Kazachenko, M. D. Guidoni, S. E. TI RECONNECTION PROPERTIES OF LARGE-SCALE CURRENT SHEETS DURING CORONAL MASS EJECTION ERUPTIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE magnetic reconnection; magnetohydrodynamics (MHD); Sun: corona; Sun: coronal mass ejections (CMEs); Sun: flares; Sun: magnetic fields ID COLLISIONLESS MAGNETIC RECONNECTION; SUPRA-ARCADE DOWNFLOWS; SOLAR-FLARES; FLUX-ROPE; WAVELET ANALYSIS; 2-RIBBON FLARES; MODEL; CHALLENGE; FIELD; ACCELERATION AB We present a detailed analysis of the properties of magnetic reconnection at large-scale current sheets (CSs) in a high cadence version of the Lynch & Edmondson 2.5D MHD simulation of sympathetic magnetic breakout eruptions from a pseudostreamer source region. We examine the resistive tearing and break-up of the three main CSs into chains of X- and O-type null points and follow the dynamics of magnetic island growth, their merging, transit, and ejection with the reconnection exhaust. For each CS, we quantify the evolution of the length-to-width aspect ratio (up to similar to 100:1), Lundquist number (similar to 10(3)), and reconnection rate (inflow-to-outflow ratios reaching similar to 0.40). We examine the statistical and spectral properties of the fluctuations in the CSs resulting from the plasmoid instability, including the distribution of magnetic island area, mass, and flux content. We show that the temporal evolution of the spectral index of the reconnection-generated magnetic energy density fluctuations appear to reflect global properties of the CS evolution. Our results are in excellent agreement with recent, high-resolution reconnection-in-a-box simulations even though our CSs' formation, growth, and dynamics are intrinsically coupled to the global evolution of sequential sympathetic coronal mass ejection eruptions. C1 [Lynch, B. J.; Kazachenko, M. D.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Edmondson, J. K.] Univ Michigan, Climate & Space Sci & Engn Dept, Ann Arbor, MI 48109 USA. [Guidoni, S. E.] NASA, Heliophys Sci Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Lynch, BJ (reprint author), Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. RI Lynch, Benjamin/B-1300-2013; OI Lynch, Benjamin/0000-0001-6886-855X FU AFOSR YIP [FA9550-11-1-0048]; NASA HTP [NNX11AJ65G]; NSF AGS [1249150]; Coronal Global Evolutionary Model (CGEM) project NSF AGS [1321474]; NASA LWS [NNX10AQ616G]; NASA Postdoctoral Program at Goddard Space Flight Center FX The authors would like to thank the anonymous referee for valuable suggestions during the review process and acknowledge Drs. George Fisher, Spiro Antiochos, and Paul Cassak for helpful discussion during the preparation of the manuscript. B. J.L. and M.D.K. acknowledge support from AFOSR YIP FA9550-11-1-0048, NASA HTP NNX11AJ65G, NSF AGS 1249150, and the Coronal Global Evolutionary Model (CGEM) project NSF AGS 1321474. J.K.E. acknowledges support from NASA LWS NNX10AQ616G. S.E.G. acknowledges support from the NASA Postdoctoral Program at Goddard Space Flight Center, administered by Oak Ridge Associated Universities. NR 93 TC 2 Z9 2 U1 2 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 20 PY 2016 VL 826 IS 1 AR 43 DI 10.3847/0004-637X/826/1/43 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DU1IU UT WOS:000381962200043 ER PT J AU Racusin, JL Oates, SR de Pasquale, M Kocevski, D AF Racusin, J. L. Oates, S. R. de Pasquale, M. Kocevski, D. TI A CORRELATION BETWEEN THE INTRINSIC BRIGHTNESS AND AVERAGE DECAY RATE OF GAMMA-RAY BURST X-RAY AFTERGLOW LIGHT CURVES SO ASTROPHYSICAL JOURNAL LA English DT Article DE gamma-ray burst: general; X-rays: bursts ID SWIFT XRT DATA; OFF-AXIS; COMPREHENSIVE ANALYSIS; TEMPORAL PROPERTIES; OPTICAL AFTERGLOWS; EXTENDED EMISSION; PROMPT EMISSION; COMPLETE SAMPLE; LOW-LUMINOSITY; PLATEAU-PHASE AB We present a correlation between the average temporal decay (alpha(X,avg,> 200 s)) and early-time luminosity (L-X,L-200 (s)) of X-ray afterglows of gamma-ray bursts as observed by the Swift X-ray Telescope. Both quantities are measured relative to a rest-frame time of 200 s after the gamma-ray trigger. The luminosity-average decay correlation does not depend on specific temporal behavior and contains one scale-independent quantity minimizing the role of selection effects. This is a complementary correlation to that discovered by Oates et al. in the optical light curves observed by the Swift Ultraviolet Optical Telescope. The correlation indicates that, on average, more luminous X-ray afterglows decay faster than less luminous ones, indicating some relative mechanism for energy dissipation. The X-ray and optical correlations are entirely consistent once corrections are applied and contamination is removed. We explore the possible biases introduced by different light-curve morphologies and observational selection effects, and how either geometrical effects or intrinsic properties of the central engine and jet could explain the observed correlation. C1 [Racusin, J. L.; Kocevski, D.] NASAs Goddard Space Flight Ctr, Code 661, Greenbelt, MD 20771 USA. [Oates, S. R.] CSIC, Inst Astrofis Andalucia IAA, Glorieta Astron S-N, E-18008 Granada, Spain. [Oates, S. R.; de Pasquale, M.] Univ Coll London, Mullard Space Sci Lab, Holmbury St Mary, Dorking RH5 6NT, Surrey, England. RP Racusin, JL (reprint author), NASAs Goddard Space Flight Ctr, Code 661, Greenbelt, MD 20771 USA. EM judith.racusin@nasa.gov FU UK Space Agency; NASA Postdoctoral Program; [AYA2012-39727-C03-01] FX The authors thank the anonymous referee for helpful comments, as well as Brad Cenko and Raffaella Margutti for useful discussions. This work made use of data supplied by the UK Swift Science Data Centre at the University of Leicester. S.R.O. acknowledges the support of the Spanish Ministry, Project Number AYA2012-39727-C03-01. M.D.P. acknowledges the support of the UK Space Agency. D.K. acknowledges the support of the NASA Postdoctoral Program. NR 72 TC 0 Z9 0 U1 3 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 20 PY 2016 VL 826 IS 1 AR 45 DI 10.3847/0004-637X/826/1/45 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DU1IU UT WOS:000381962200045 ER PT J AU Sloan, GC Kraemer, KE McDonald, I Groenewegen, MAT Wood, PR Zijlstra, AA Lagadec, E Boyer, ML Kemper, F Matsuura, M Sahai, R Sargent, BA Srinivasan, S van Loon, JT Volk, K AF Sloan, G. C. Kraemer, K. E. McDonald, I. Groenewegen, M. A. T. Wood, P. R. Zijlstra, A. A. Lagadec, E. Boyer, M. L. Kemper, F. Matsuura, M. Sahai, R. Sargent, B. A. Srinivasan, S. van Loon, J. Th. Volk, K. TI THE INFRARED SPECTRAL PROPERTIES OF MAGELLANIC CARBON STARS SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; infrared: stars; stars: AGB and post-AGB; stars: carbon ID ASYMPTOTIC GIANT BRANCH; SPITZER-SPACE-TELESCOPE; LONG-PERIOD VARIABLES; GRAVITATIONAL LENSING EXPERIMENT.; SHORT-WAVELENGTH SPECTROMETER; AGE-METALLICITY RELATIONSHIP; CLOUDS PHOTOMETRIC SURVEY; POINT-SOURCE CATALOG; OGLE-III CATALOG; PLANETARY-NEBULAE AB The Infrared Spectrograph on the Spitzer Space Telescope observed 184 carbon stars in the Magellanic Clouds. This sample reveals that the dust-production rate (DPR) from carbon stars generally increases with the pulsation period of the star. The composition of the dust grains follows two condensation sequences, with more SiC condensing before amorphous carbon in metal-rich stars, and the order reversed in metal-poor stars. MgS dust condenses in optically thicker dust shells, and its condensation is delayed in more metal-poor stars. Metal-poor carbon stars also tend to have stronger absorption from C2H2 at 7.5 mu m. The relation between DPR and pulsation period shows significant apparent scatter, which results from the initial mass of the star, with more massive stars occupying a sequence parallel to lower-mass stars, but shifted to longer periods. Accounting for differences in the mass distribution between the carbon stars observed in the Small and Large Magellanic Clouds reveals a hint of a subtle decrease in the DPR at lower metallicities, but it is not statistically significant. The most deeply embedded carbon stars have lower variability amplitudes and show SiC in absorption. In some cases they have bluer colors at shorter wavelengths, suggesting that the central star is becoming visible. These deeply embedded stars may be evolving off of the asymptotic giant branch and/or they may have non-spherical dust geometries. C1 [Sloan, G. C.] Cornell Univ, Cornell Ctr Astrophys & Planetary Sci, Ithaca, NY 14853 USA. [Sloan, G. C.] Univ N Carolina, Dept Phys & Astron, Chapel Hill, NC 27599 USA. [Kraemer, K. E.] Boston Coll, Inst Sci Res, 140 Commonwealth Ave, Chestnut Hill, MA 02467 USA. [McDonald, I.; Zijlstra, A. A.] Univ Manchester, Jodrell Bank, Ctr Astrophys, Manchester M13 9PL, Lancs, England. [Groenewegen, M. A. T.] Koninklijke Sterrenwacht Belgie, Ringlaan 3, B-1180 Brussels, Belgium. [Wood, P. R.] Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT 2611, Australia. [Lagadec, E.] Observ Cote Azur, F-06300 Nice, France. [Boyer, M. L.] NASA, CRESST, Goddard Space Flight Ctr, Code 665, Greenbelt, MD 20771 USA. [Boyer, M. L.] NASA, Observat Cosmol Lab, Goddard Space Flight Ctr, Code 665, Greenbelt, MD 20771 USA. [Boyer, M. L.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Kemper, F.; Srinivasan, S.] Acad Sinica, Inst Astron & Astrophys, 11F Astron Math Bldg,NTU AS,1,Sect 4,Roosevelt Rd, Taipei 10617, Taiwan. [Matsuura, M.] Cardiff Univ, Sch Phys & Astron, Queens Bldg, Cardiff CF24 3AA, S Glam, Wales. [Sahai, R.] CALTECH, Jet Prop Lab, MS 183-900, Pasadena, CA 91109 USA. [Sargent, B. A.] Rochester Inst Technol, Ctr Imaging Sci, 54 Lomb Mem Dr, Rochester, NY 14623 USA. [Sargent, B. A.] Rochester Inst Technol, Lab Multiwavelength Astrophys, 54 Lomb Mem Dr, Rochester, NY 14623 USA. [van Loon, J. Th.] Keele Univ, Lennard Jones Labs, Keele ST5 5BG, Staffs, England. [Volk, K.] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA. RP Sloan, GC (reprint author), Cornell Univ, Cornell Ctr Astrophys & Planetary Sci, Ithaca, NY 14853 USA.; Sloan, GC (reprint author), Univ N Carolina, Dept Phys & Astron, Chapel Hill, NC 27599 USA. EM sloan@isc.astro.cornell.edu RI Kemper, Francisca/D-8688-2011; OI Kemper, Francisca/0000-0003-2743-8240; Zijlstra, Albert/0000-0002-3171-5469; Kraemer, Kathleen/0000-0002-2626-7155 FU NASA [1257184, 1407]; NSF [1108645]; Ministry of Science and Technology (MoST) of Taiwan [MOST104-2628-M-001-004-MY3] FX We thank the anonymous referee for helpful and constructive comments. GCS was supported by NASA through Contract Number 1257184 issued by the Jet Propulsion Laboratory, California Institute of Technology under NASA contract 1407 and the NSF through Award 1108645. FK received support from the Ministry of Science and Technology (MoST) of Taiwan, grant MOST104-2628-M-001-004-MY3. This research relied on the following resources: NASA's Astrophysics Data System, the Infrared Science Archive at the Infrared Processing and Analysis Center, operated by JPL, and the Simbad and VizieR databases, operated at the Centre de Donnees astronomiques de Strasbourg. NR 91 TC 2 Z9 2 U1 2 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 20 PY 2016 VL 826 IS 1 AR 44 DI 10.3847/0004-637X/826/1/44 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DU1IU UT WOS:000381962200044 ER PT J AU Ukwatta, TN Hurley, K MacGibbon, JH Svinkin, DS Aptekar, RL Golenetskii, SV Frederiks, DD Pal'shin, VD Goldsten, J Boynton, W Kozyrev, AS Rau, A von Kienlin, A Zhang, X Connaughton, V Yamaoka, K Ohno, M Ohmori, N Feroci, M Frontera, F Guidorzi, C Cline, T Gehrels, N Krimm, HA McTiernan, J AF Ukwatta, T. N. Hurley, K. MacGibbon, J. H. Svinkin, D. S. Aptekar, R. L. Golenetskii, S. V. Frederiks, D. D. Pal'shin, V. D. Goldsten, J. Boynton, W. Kozyrev, A. S. Rau, A. von Kienlin, A. Zhang, X. Connaughton, V. Yamaoka, K. Ohno, M. Ohmori, N. Feroci, M. Frontera, F. Guidorzi, C. Cline, T. Gehrels, N. Krimm, H. A. McTiernan, J. TI INVESTIGATION OF PRIMORDIAL BLACK HOLE BURSTS USING INTERPLANETARY NETWORK GAMMA-RAY BURSTS SO ASTROPHYSICAL JOURNAL LA English DT Article DE black hole physics; methods: observational ID 1ST 2 YEARS; SPECTRAL CATALOG; SHORT-DURATION; UPPER LIMITS; RATE-DENSITY; GIANT FLARE; SEARCH; EVAPORATION; EXPLOSIONS; BATSE AB The detection of a gamma-ray burst (GRB) in the solar neighborhood would have very important implications for GRB phenomenology. The leading theories for cosmological GRBs would not be able to explain such events. The final bursts of evaporating primordial black holes (PBHs), however, would be a natural explanation for local GRBs. We present a novel technique that can constrain the distance to GRBs using detections from widely separated, non-imaging spacecraft. This method can determine the actual distance to the burst if it is local. We applied this method to constrain distances to a sample of 36 short-duration GRBs detected by the Interplanetary Network (IPN) that show observational properties that are expected from PBH evaporations. These bursts have minimum possible distances in the 10(13)-10(18) cm (7-10(5) au) range, which are consistent with the expected PBH energetics and with a possible origin in the solar neighborhood, although none of the bursts can be unambiguously demonstrated to be local. Assuming that these bursts are real PBH events, we estimate lower limits on the PBH burst evaporation rate in the solar neighborhood. C1 [Ukwatta, T. N.] Los Alamos Natl Lab, Space & Remote Sensing ISR 2, Los Alamos, NM 87545 USA. [Hurley, K.; McTiernan, J.] Univ Calif Berkeley, Space Sci Lab, 7 Gauss Way, Berkeley, CA 94720 USA. [MacGibbon, J. H.] Univ North Florida, Dept Phys, Jacksonville, FL 32224 USA. [Svinkin, D. S.; Aptekar, R. L.; Golenetskii, S. V.; Frederiks, D. D.; Pal'shin, V. D.] Ioffe Phys Tech Inst, St Petersburg 194021, Russia. [Goldsten, J.] Johns Hopkins Univ, Appl Phys Lab, Johns Hopkins Rd, Laurel, MD 20723 USA. [Boynton, W.] Univ Arizona, Dept Planetary Sci, Tucson, AZ 85721 USA. [Kozyrev, A. S.] Space Res Inst, 84-32 Profsoyuznaya, Moscow 117997, Russia. [Rau, A.; von Kienlin, A.; Zhang, X.] Max Planck Inst Extraterr Phys, Giessenbachstr,Postfach 1312, D-85748 Garching, Germany. [Connaughton, V.] Univ Alabama Huntsville, NSSTC, 320 Sparkman Dr, Huntsville, AL 35805 USA. [Yamaoka, K.] Aoyama Gakuin Univ, Dept Math & Phys, 5-10-1 Fuchinobe, Sagamihara, Kanagawa 2298558, Japan. [Ohno, M.] Hiroshima Univ, Dept Phys, 1-3-1 Kagamiyama, Higashihiroshima, Hiroshima 7398526, Japan. [Ohmori, N.] Miyazaki Univ, Dept Appl Phys, 1-1 Gakuen Kibanadai Nishi, Miyazaki, Miyazaki 8892192, Japan. [Feroci, M.] IAPS Roma, INAF, Via Fosso Cavaliere 100, I-00133 Rome, Italy. [Frontera, F.; Guidorzi, C.] Univ Ferrara, Dept Phys & Earth Sci, Via Saragat 1, I-44122 Ferrara, Italy. [Cline, T.; Gehrels, N.] NASA, Goddard Space Flight Ctr, Code 661, Greenbelt, MD 20771 USA. [Krimm, H. A.] NASA, Goddard Space Flight Ctr, CRESST, USRA, Code 661, Greenbelt, MD 20771 USA. [Frontera, F.] INAF, Ist Astrofis Spaziale & Fis Cosm Bologna, Via Gobetti 101, I-40129 Bologna, Italy. [Krimm, H. A.] Univ Space Res Assoc, 10211 Wincopin Circle,Suite 500, Columbia, MD 21044 USA. RP Ukwatta, TN (reprint author), Los Alamos Natl Lab, Space & Remote Sensing ISR 2, Los Alamos, NM 87545 USA. EM tilan@lanl.gov FU NASA [NNX09AU03G, NNX10AU34G, NNX11AP96G, NNX13AP09G, NNG04GM50G, NNG06GE69G, NNX07AQ22G, NNX08AC90G, NNX08AX95G, NNX09AR28G, NNX08AN23G, NNX09AO97G, NNX12AD68G, NNX06AI36G, NNX08AB84G, NNX08AZ85G, NNX09AV61G, NNX10AR12G, NNX07AR71G, NAG5-3500]; JPL [1282043, Y503559, NNX12AE41G, NNX13AI54G, NNX15AE60G, NNX07AH52G, NAG5-13080, NAG5-7766, NAG5-9126, NAG5-10710, NNG06GI89G]; Laboratory Directed Research and Development program at the Los Alamos National Laboratory (LANL); Russian Space Agency contract and RFBR [15-02-00532, 13-02-12017-ofi-m] FX Support for the IPN was provided by NASA grants NNX09AU03G, NNX10AU34G, NNX11AP96G, and NNX13AP09G (Fermi); NNG04GM50G, NNG06GE69G, NNX07AQ22G, NNX08AC90G, NNX08AX95G, and NNX09AR28G (INTEGRAL); NNX08AN23G, NNX09AO97G, and NNX12AD68G (Swift); NNX06AI36G, NNX08AB84G, NNX08AZ85G, NNX09AV61G, and NNX10AR12G (Suzaku); NNX07AR71G (MESSENGER); NAG5-3500, and JPL Contracts 1282043 and Y503559 (Odyssey); NNX12AE41G, NNX13AI54G, and NNX15AE60G (ADA); NNX07AH52G (Konus); NAG5-13080 (RHESSI); NAG5-7766, NAG5-9126, and NAG5-10710, (BeppoSAX); and NNG06GI89G. T. N. U. acknowledges support from the Laboratory Directed Research and Development program at the Los Alamos National Laboratory (LANL). The Konus-Wind experiment is partially supported by a Russian Space Agency contract and RFBR grants 15-02-00532 and 13-02-12017-ofi-m. We also thank Jim Linnemann (MSU), Dan Stump (MSU), Brenda Dingus (LANL), and Pat Harding (LANL) for useful conversations on the analysis. NR 75 TC 0 Z9 0 U1 1 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 20 PY 2016 VL 826 IS 1 AR 98 DI 10.3847/0004-637X/826/1/98 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DU1IU UT WOS:000381962200098 ER PT J AU Walton, DJ Tomsick, JA Madsen, KK Grinberg, V Barret, D Boggs, SE Christensen, FE Clavel, M Craig, WW Fabian, AC Fuerst, F Hailey, CJ Harrison, FA Miller, JM Parker, ML Rahoui, F Stern, D Tao, L Wilms, J Zhang, W AF Walton, D. J. Tomsick, J. A. Madsen, K. K. Grinberg, V. Barret, D. Boggs, S. E. Christensen, F. E. Clavel, M. Craig, W. W. Fabian, A. C. Fuerst, F. Hailey, C. J. Harrison, F. A. Miller, J. M. Parker, M. L. Rahoui, F. Stern, D. Tao, L. Wilms, J. Zhang, W. TI THE SOFT STATE OF CYGNUS X-1 OBSERVED WITH NuSTAR: A VARIABLE CORONA AND A STABLE INNER DISK SO ASTROPHYSICAL JOURNAL LA English DT Article DE black hole physics; X-rays: binaries; X-rays: individual (Cygnus X-1) ID X-RAY REFLECTION; BLACK-HOLE SPIN; XMM-NEWTON OBSERVATIONS; ACTIVE GALACTIC NUCLEI; LONG-TERM VARIABILITY; ACCRETION DISK; STELLAR WIND; HARD STATE; SUZAKU OBSERVATIONS; SWIFT OBSERVATIONS AB We present a multi-epoch hard X-ray analysis of Cygnus X-1 in its soft state based on four observations with the Nuclear Spectroscopic Telescope Array (NuSTAR). Despite the basic similarity of the observed spectra, there is clear spectral variability between epochs. To investigate this variability, we construct a model incorporating both the standard disk-corona continuum and relativistic reflection from the accretion disk, based on prior work on Cygnus X-1, and apply this model to each epoch independently. We find excellent consistency for the black hole spin and the iron abundance of the accretion disk, which are expected to remain constant on observational timescales. In particular, we confirm that Cygnus X-1 hosts a rapidly rotating black hole, 0.93 less than or similar to a* less than or similar to 0.96, in broad agreement with the majority of prior studies of the relativistic disk reflection and constraints on the spin obtained through studies of the thermal accretion disk continuum. Our work also confirms the apparent misalignment between the inner disk and the orbital plane of the binary system reported previously, finding the magnitude of this warp to be similar to 10 degrees-15 degrees. This level of misalignment does not significantly change (and may even improve) the agreement between our reflection results and the thermal continuum results regarding the black hole spin. The spectral variability observed by NuSTAR is dominated by the primary continuum, implying variability in the temperature of the scattering electron plasma. Finally, we consistently observe absorption from ionized iron at similar to 6.7 keV, which varies in strength as a function of orbital phase in a manner consistent with the absorbing material being an ionized phase of the focused stellar wind from the supergiant companion star. C1 [Walton, D. J.; Stern, D.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Walton, D. J.; Madsen, K. K.; Fuerst, F.; Harrison, F. A.; Tao, L.] CALTECH, Space Radiat Lab, Pasadena, CA 91125 USA. [Tomsick, J. A.; Boggs, S. E.; Clavel, M.; Craig, W. W.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Grinberg, V.] MIT, MIT Kavli Inst Astrophys & Space Res, 70 Vassar St, Cambridge, MA 02139 USA. [Barret, D.] Univ Toulouse, UPS OMP, IRAP, Toulouse, France. [Barret, D.] CNRS, IRAP, 9 Ave Colonel Roche,BP 44346, F-31028 Toulouse 4, France. [Christensen, F. E.] Tech Univ Denmark, Natl Space Inst, DTU Space, Elektrovej 327, DK-2800 Lyngby, Denmark. [Fabian, A. C.; Parker, M. L.] Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England. [Hailey, C. J.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Miller, J. M.] Univ Michigan, Dept Astron, 1085 S Univ Ave, Ann Arbor, MI 48109 USA. [Rahoui, F.] European So Observ, K Schwarzschild Str 2, D-85748 Garching, Germany. [Rahoui, F.] Harvard Univ, Dept Astron, 60 Garden St, Cambridge, MA 02138 USA. [Wilms, J.] ECAP Erlangen Ctr Astroparticle Phys, Sternwartstr 7, D-96049 Bamberg, Germany. [Zhang, W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Walton, DJ (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.; Walton, DJ (reprint author), CALTECH, Space Radiat Lab, Pasadena, CA 91125 USA. RI Wilms, Joern/C-8116-2013; OI Wilms, Joern/0000-0003-2065-5410; Clavel, Maica/0000-0003-0724-2742 FU NASA through the Smithsonian Astrophysical Observatory (SAO) [SV3-73016]; NASA [NAS8-03060]; French Space Agency (CNES) FX The authors would like to thank the referee for prompt and useful feedback. DB acknowledges financial support from the French Space Agency (CNES). VG acknowledges financial support provided by NASA through the Smithsonian Astrophysical Observatory (SAO) contract SV3-73016 to MIT for Support of the Chandra X-Ray Center (CXC) and Science Instruments; CXC is operated by SAO for and on behalf of NASA under contract NAS8-03060. This research made use of data obtained with NuSTAR, a project led by Caltech, funded by NASA, and managed by NASA/JPL, and has utilized the NUSTARDAS software package, jointly developed by the ASI Science Data Center (ASDC, Italy) and Caltech (USA). Swift BAT transient monitor results are provided by the Swift BAT team. This research has also made use of MAXI data provided by RIKEN, JAXA, and the MAXI team. NR 89 TC 5 Z9 5 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 20 PY 2016 VL 826 IS 1 AR 87 DI 10.3847/0004-637X/826/1/87 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DU1IU UT WOS:000381962200087 ER PT J AU Yang, H Apai, D Marley, MS Karalidi, T Flateau, D Showman, AP Metchev, S Buenzli, E Radigan, J Artigau, E Lowrance, PJ Burgasser, AJ AF Yang, Hao Apai, Daniel Marley, Mark S. Karalidi, Theodora Flateau, Davin Showman, Adam P. Metchev, Stanimir Buenzli, Esther Radigan, Jacqueline Artigau, Etienne Lowrance, Patrick J. Burgasser, Adam J. TI EXTRASOLAR STORMS: PRESSURE-DEPENDENT CHANGES IN LIGHT-CURVE PHASE IN BROWN DWARFS FROM SIMULTANEOUS HST AND SPITZER OBSERVATIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE brown dwarfs; infrared: stars; stars: atmospheres; stars: low-mass ID HUBBLE-SPACE-TELESCOPE; INFRARED ARRAY CAMERA; PROPER-MOTION SURVEY; PECULIAR L DWARFS; ALL-SKY SURVEY; VERY-LOW MASS; T-DWARFS; PHOTOMETRIC VARIABILITY; ABSOLUTE CALIBRATION; EVOLVING WEATHER AB We present Spitzer/Infrared Array Camera Ch1 and Ch2 monitoring of six brown dwarfs during eight different epochs over the course of 20 months. For four brown dwarfs, we also obtained simulataneous Hubble Space Telescope (HST)/WFC3 G141 grism spectra during two epochs and derived light curves in five narrowband filters. Probing different pressure levels in the atmospheres, the multiwavelength light curves of our six targets all exhibit variations, and the shape of the light curves evolves over the timescale of a rotation period, ranging from 1.4 to 13 hr. We compare the shapes of the light curves and estimate the phase shifts between the light curves observed at different wavelengths by comparing the phase of the primary Fourier components. We use state-of-the-art atmosphere models to determine the flux contribution of different pressure layers to the observed flux in each filter. We find that the light curves that probe higher pressures are similar and in phase, but are offset and often different from the light curves that probe lower pressures. The phase differences between the two groups of light curves suggest that the modulations seen at lower and higher pressures may be introduced by different cloud layers. C1 [Yang, Hao; Apai, Daniel; Karalidi, Theodora] Univ Arizona, Dept Astron, 933 N Cherry Ave, Tucson, AZ 85721 USA. [Apai, Daniel; Flateau, Davin] Dept Planetary Sci, 1629 E Univ Blvd, Tucson, AZ 85721 USA. [Marley, Mark S.] NASA, Ames Res Ctr, Naval Air Stn, Mountain View, CA 94035 USA. [Showman, Adam P.] Univ Arizona, Dept Planetary Sci, 1629 Univ Blvd, Tucson, AZ 85721 USA. [Metchev, Stanimir] Univ Western Ontario, Dept Phys & Astron, Ctr Planetary Sci & Explorat, 1151 Richmond St, London, ON N6A 3K7, Canada. [Metchev, Stanimir] SUNY Stony Brook, Dept Phys & Astron, 100 Nicolls Rd, Stony Brook, NY 11794 USA. [Buenzli, Esther] Swiss Fed Inst Technol, Inst Astron, Wolfgang Pauli Str 27, CH-8093 Zurich, Switzerland. [Radigan, Jacqueline] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA. [Artigau, Etienne] Univ Montreal, Dep Phys, CP 6128 Succ Ctr ville, Montreal, PQ H3C 3J7, Canada. [Lowrance, Patrick J.] CALTECH, Infrared Proc & Anal Ctr, MS 100-22, Pasadena, CA 91125 USA. [Burgasser, Adam J.] Univ Calif San Diego, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA. RP Yang, H (reprint author), Univ Arizona, Dept Astron, 933 N Cherry Ave, Tucson, AZ 85721 USA. EM haoyang@email.arizona.edu; apai@arizona.edu OI Yang, Hao/0000-0002-9423-2333; Metchev, Stanimir/0000-0003-3050-8203 FU NASA; Universities for Research in Astronomy, Inc. under NASA [13176, NAS5-26555] FX This work is part of the Spitzer Cycle-9 Exploration Program, Extrasolar Storms. 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.; Support for HST GO programs 13176 was provided by Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. We acknowledge the outstanding help of Patricia Royle (STScI) and the Spitzer Science Center staff, especially Nancy Silbermann, for coordinating the HST and Spitzer observations. NR 54 TC 0 Z9 0 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 20 PY 2016 VL 826 IS 1 AR 8 DI 10.3847/0004-637X/826/1/8 PG 25 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DU1IU UT WOS:000381962200008 ER PT J AU Zurbuchen, TH Weberg, M von Steiger, R Mewaldt, RA Lepri, ST Antiochos, SK AF Zurbuchen, T. H. Weberg, M. von Steiger, R. Mewaldt, R. A. Lepri, S. T. Antiochos, S. K. TI COMPOSITION OF CORONAL MASS EJECTIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE acceleration of particles; solar wind; Sun: abundances; Sun: coronal mass ejections (CMEs) ID SOLAR ENERGETIC PARTICLES; ELEMENT ABUNDANCES; HELIUM ABUNDANCE; MAGNETIC-FIELD; ACTIVE-REGION; WIND; ACCELERATION; EVENTS; MODEL; SPEED AB We analyze the physical origin of plasmas that are ejected from the solar corona. To address this issue, we perform a comprehensive analysis of the elemental composition of interplanetary coronal mass ejections (ICMEs) using recently released elemental composition data for Fe, Mg, Si, S, C, N, Ne, and He as compared to O and H. We find that ICMEs exhibit a systematic abundance increase of elements with first ionization potential (FIP) < 10 eV, as well as a significant increase of Ne as compared to quasi-stationary solar wind. ICME plasmas have a stronger FIP effect than slow wind, which indicates either that an FIP process is active during the ICME ejection or that a different type of solar plasma is injected into ICMEs. The observed FIP fractionation is largest during times when the Fe ionic charge states are elevated above Q(Fe) > 12.0. For ICMEs with elevated charge states, the FIP effect is enhanced by 70% over that of the slow wind. We argue that the compositionally hot parts of ICMEs are active region loops that do not normally have access to the heliosphere through the processes that give rise to solar wind. We also discuss the implications of this result for solar energetic particles accelerated during solar eruptions and for the origin of the slow wind itself. C1 [Zurbuchen, T. H.; Weberg, M.; Lepri, S. T.] Univ Michigan, Dept Climate & Space Sci & Engn, Ann Arbor, MI 48109 USA. [von Steiger, R.] Int Space Sci Inst, Bern, Switzerland. [von Steiger, R.] Univ Bern, Phys Inst, CH-3012 Bern, Switzerland. [Mewaldt, R. A.] CALTECH, Pasadena, CA USA. [Antiochos, S. K.] NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Greenbelt, MD USA. RP Zurbuchen, TH (reprint author), Univ Michigan, Dept Climate & Space Sci & Engn, Ann Arbor, MI 48109 USA. FU NASA [NNX13AH66G, NNH13ZDA001N, NNX11A075G]; Catholic University of America [362496-Sub1] FX We acknowledge the work of the ACE SWICS team and particularly Paul Shearer for their dedication to producing high-quality compositional data. T.H.Z. acknowledges the hospitality of the staff of the International Space Science Institute where much of this work was performed. This work was supported, in part, by NASA grants NNX13AH66G, NNH13ZDA001N, and NNX11A075G, and the Catholic University of America contract 362496-Sub1. NR 54 TC 0 Z9 0 U1 5 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 20 PY 2016 VL 826 IS 1 AR 10 DI 10.3847/0004-637X/826/1/10 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DU1IU UT WOS:000381962200010 ER PT J AU Connaughton, V Burns, E Goldstein, A Blackburn, L Briggs, MS Zhang, BB Camp, J Christensen, N Hui, CM Jenke, P Littenberg, T McEnery, JE Racusin, J Shawhan, P Singer, L Veitch, J Wilson-Hodge, CA Bhat, PN Bissaldi, E Cleveland, W Fitzpatrick, G Giles, MM Gibby, MH von Kienlin, A Kippen, RM McBreen, S Mailyan, B Meegan, CA Paciesas, WS Preece, RD Roberts, OJ Sparke, L Stanbro, M Toelge, K Veres, P AF Connaughton, V. Burns, E. Goldstein, A. Blackburn, L. Briggs, M. S. Zhang, B. -B. Camp, J. Christensen, N. Hui, C. M. Jenke, P. Littenberg, T. McEnery, J. E. Racusin, J. Shawhan, P. Singer, L. Veitch, J. Wilson-Hodge, C. A. Bhat, P. N. Bissaldi, E. Cleveland, W. Fitzpatrick, G. Giles, M. M. Gibby, M. H. von Kienlin, A. Kippen, R. M. McBreen, S. Mailyan, B. Meegan, C. A. Paciesas, W. S. Preece, R. D. Roberts, O. J. Sparke, L. Stanbro, M. Toelge, K. Veres, P. TI FERMI GBM OBSERVATIONS OF LIGO GRAVITATIONAL-WAVE EVENT GW150914 SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE gamma-ray burst: general; gravitational waves ID GAMMA-RAY BURSTS; COMPACT OBJECT MERGERS; ELECTROMAGNETIC COUNTERPARTS; VIRGO; BATSE; CATALOG; MONITOR; GRBS; ERA AB With an instantaneous view of 70% of the sky, the Fermi Gamma-ray Burst Monitor (GBM) is an excellent partner in the search for electromagnetic counterparts to gravitational-wave (GW) events. GBM observations at the time of the Laser Interferometer Gravitational-wave Observatory (LIGO) event GW150914 reveal the presence of a weak transient above 50 keV, 0.4 s after the GW event, with a false-alarm probability of 0.0022 (2.9 sigma). This weak transient lasting 1 s was not detected by any other instrument and does not appear to be connected with other previously known astrophysical, solar, terrestrial, or magnetospheric activity. Its localization is ill-constrained but consistent with the direction of GW150914. The duration and spectrum of the transient event are consistent with a weak short gamma-ray burst (GRB) arriving at a large angle to the direction in which Fermi was pointing where the GBM detector response is not optimal. If the GBM transient is associated with GW150914, then this electromagnetic signal from a stellar mass black hole binary merger is unexpected. We calculate a luminosity in hard X-ray emission between 1 keV and 10 MeV of 1.8(-1.0)(+1.5) x 10(49) erg s(-1). Future joint observations of GW events by LIGO/Virgo and Fermi GBM could reveal whether the weak transient reported here is a plausible counterpart to GW150914 or a chance coincidence, and will further probe the connection between compact binary mergers and short GRBs. C1 [Connaughton, V.; Littenberg, T.; Cleveland, W.; Paciesas, W. S.] Univ Space Res Assoc, 320 Sparkman Dr, Huntsville, AL 35806 USA. [Burns, E.] Univ Alabama, Dept Phys, 320 Sparkman Dr, Huntsville, AL 35805 USA. [Goldstein, A.; Hui, C. M.; Wilson-Hodge, C. A.] NASA, Marshall Space Flight Ctr, Astrophys Off, ZP12, Huntsville, AL 35812 USA. [Blackburn, L.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Blackburn, L.] MIT, LIGO, 77 Massachusetts Ave, Cambridge, MA 02139 USA. [Briggs, M. S.; Preece, R. D.; Stanbro, M.] Univ Alabama, Dept Space Sci, 320 Sparkman Dr, Huntsville, AL 35805 USA. [Briggs, M. S.; Zhang, B. -B.; Jenke, P.; Bhat, P. N.; Fitzpatrick, G.; Mailyan, B.; Meegan, C. A.; Veres, P.] Univ Alabama, CSPAR, 320 Sparkman Dr, Huntsville, AL 35805 USA. [Zhang, B. -B.] IAA CSIC, POB 03004, E-18080 Granada, Spain. [Camp, J.; McEnery, J. E.; Racusin, J.; Singer, L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Christensen, N.] Carleton Coll, Phys & Astron, Northfield, MN 55057 USA. [Shawhan, P.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA. [Veitch, J.] Univ Birmingham, Birmingham B15 2TT, W Midlands, England. [Bissaldi, E.] Ist Nazl Fis Nucl, Sez Bari, I-70126 Bari, Italy. [Bissaldi, E.; Toelge, K.] Politecn Bari, Dipartimento Fis, I-70125 Bari, Italy. [Giles, M. M.; Gibby, M. H.] Jacobs Technol Inc, Huntsville, AL USA. [von Kienlin, A.] Max Planck Inst Extraterr Phys, Giessenbachstr 1, D-85748 Garching, Germany. [Kippen, R. M.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA. [McBreen, S.; Roberts, O. J.] Univ Coll Dublin, Sch Phys, Stillorgan Rd, Dublin 4, Ireland. [Sparke, L.] NASA Headquarters, Washington, DC USA. RP Connaughton, V (reprint author), Univ Space Res Assoc, 320 Sparkman Dr, Huntsville, AL 35806 USA. EM valerie@nasa.gov RI Roberts, Oliver/N-6284-2016 OI Roberts, Oliver/0000-0002-7150-9061 NR 56 TC 44 Z9 44 U1 5 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD JUL 20 PY 2016 VL 826 IS 1 AR L6 DI 10.3847/2041-8205/826/1/L6 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DS4GL UT WOS:000380739300006 ER PT J AU El-Batal, AM Miller, JM Reynolds, MT Boggs, SE Chistensen, FE Craig, WW Fuerst, F Hailey, CJ Harrison, FA Stern, DK Tomsick, J Walton, DJ Zhang, WW AF El-Batal, A. M. Miller, J. M. Reynolds, M. T. Boggs, S. E. Chistensen, F. E. Craig, W. W. Fuerst, F. Hailey, C. J. Harrison, F. A. Stern, D. K. Tomsick, J. Walton, D. J. Zhang, W. W. TI NuSTAR OBSERVATIONS OF THE BLACK HOLE GS 1354-645: EVIDENCE OF RAPID BLACK HOLE SPIN SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE accretion, accretion disks; black hole physics; X-rays: binaries ID INNER ACCRETION FLOW; HARD-STATE; REFLECTION; DISK; SPECTROSCOPY; OUTBURST; CONSTRAINTS; BINARIES; SPECTRA; SWIFT AB We present the results of a NuSTAR study of the dynamically confirmed stellar-mass black hole GS 1354-645. The source was observed during its 2015 "hard" state outburst; we concentrate on spectra from two relatively bright phases. In the higher-flux observation, the broadband NuSTAR spectra reveal a clear, strong disk reflection spectrum, blurred by a degree that requires a black hole spin of a = cf/GM(2) >= 0.98 (1 sigma statistical limits only). The fits also require a high inclination: 0 similar or equal to 75 (2)degrees. Strong "dips" are sometimes observed in the X-ray light curves of sources viewed at such an angle; these are absent, perhaps indicating that dips correspond to flared disk structures that only manifest at higher accretion rates. In the lower flux observation, there is evidence of radial truncation of the thin accretion disk. We discuss these results in the context of spin in stellar-mass black holes, and inner accretion flow geometries at moderate accretion rates. C1 [El-Batal, A. M.; Miller, J. M.; Reynolds, M. T.] Univ Michigan, Dept Astron, 1085 S Univ Ave, Ann Arbor, MI 48109 USA. [Boggs, S. E.; Craig, W. W.; Tomsick, J.] Univ Calif Berkeley, Space Sci Lab, 7 Gauss Way, Berkeley, CA 94720 USA. [Chistensen, F. E.] Danish Tech Univ, Lungby, Denmark. [Craig, W. W.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA. [Fuerst, F.; Harrison, F. A.] CALTECH, Cahill Ctr Astron & Astrophys, 1200 East Calif Blvd, Pasadena, CA 91125 USA. [Hailey, C. J.] Columbia Univ, Columbia Astrophys Lab, 550 West 120th St, New York, NY 10027 USA. [Hailey, C. J.] Columbia Univ, Dept Astron, 550 West 120th St, New York, NY 10027 USA. [Stern, D. K.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Zhang, W. W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Miller, JM (reprint author), Univ Michigan, Dept Astron, 1085 S Univ Ave, Ann Arbor, MI 48109 USA. EM jonmm@umich.edu FU NASA [NNG08FD60C]; NASA FX We thank the anonymous referee for comments that improved this manuscript. This work was supported under NASA contract No. NNG08FD60C, and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by NASA. NR 40 TC 0 Z9 0 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD JUL 20 PY 2016 VL 826 IS 1 AR L12 DI 10.3847/2041-8205/826/1/L12 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DS4GL UT WOS:000380739300012 ER PT J AU Zhang, X Sander, SP Cheng, L Thimmakondu, VS Stanton, JF AF Zhang, Xu Sander, Stanley P. Cheng, Lan Thimmakondu, Venkatesan S. Stanton, John F. TI Matrix-isolated infrared absorption spectrum of CH2BrOO radical SO CHEMICAL PHYSICS LETTERS LA English DT Article ID GAS-PHASE; ATMOSPHERIC CHEMISTRY; PEROXY-RADICALS; BASIS-SETS; KINETICS; ATOMS; POTENTIALS; GRADIENTS; ELECTRON; 298-K AB The bromomethylperoxy radical, CH2BrOO, has been generated in cryogenic matrices. Six fundamental bands for CH2BrOO have been observed in an argon matrix at 5 K. The experimental frequencies (cm (1)) are: v(4) = 1274.3, v(5) = 1229.4, v(6) = 1086.7, v(7) = 961.8, v(8) = 879.9, and v(10) = 515.4, two of which are detected for the first time. Ab initio calculations have been performed employing coupled-cluster methods. The experimental frequencies are shown to be in good agreement with the computation as well as the four bands (v(4), v(6), v(7) and v(8)) observed by Huang and Lee in the gas phase. (C) 2016 Elsevier B. V. All rights reserved. C1 [Zhang, Xu; Sander, Stanley P.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Cheng, Lan; Thimmakondu, Venkatesan S.; Stanton, John F.] Univ Texas Austin, Dept Chem, Inst Theoret Chem, Austin, TX 78712 USA. RP Zhang, X; Sander, SP (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.; Stanton, JF (reprint author), Univ Texas Austin, Dept Chem, Inst Theoret Chem, Austin, TX 78712 USA. EM xzxuzhang@gmail.com FU NASA; U.S. Department of Energy [DE-FG02-07ER15884]; Robert A. Welch Foundation of Houston, TX [F-1284]; National Aeronautics and Space Administration; California Institute of Technology FX This work was supported by the NASA Tropospheric Chemistry and Upper Atmosphere Research Programs. Additional support for this work to J.F.S. comes from the U.S. Department of Energy (Contract Number DE-FG02-07ER15884) and the Robert A. Welch Foundation of Houston, TX (Grant F-1284). The authors would also like to thank Dr. Kyle Bayes and Prof. Barney Ellison for their helpful discussions. The research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. Copyright 2016 California Institute of Technology. Government sponsorship is acknowledged. NR 25 TC 0 Z9 0 U1 2 U2 2 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0009-2614 EI 1873-4448 J9 CHEM PHYS LETT JI Chem. Phys. Lett. PD JUL 16 PY 2016 VL 657 BP 131 EP 134 DI 10.1016/j.cplett.2016.05.060 PG 4 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA DW2AG UT WOS:000383444700023 ER PT J AU Andre, M Li, W Toledo-Redondo, S Khotyaintsev, YV Vaivads, A Graham, DB Norgren, C Burch, J Lindqvist, PA Marklund, G Ergun, R Torbert, R Magnes, W Russell, CT Giles, B Moore, TE Chandler, MO Pollock, C Young, DT Avanov, LA Dorelli, JC Gershman, DJ Paterson, WR Lavraud, B Saito, Y AF Andre, M. Li, W. Toledo-Redondo, S. Khotyaintsev, Yu. V. Vaivads, A. Graham, D. B. Norgren, C. Burch, J. Lindqvist, P. -A. Marklund, G. Ergun, R. Torbert, R. Magnes, W. Russell, C. T. Giles, B. Moore, T. E. Chandler, M. O. Pollock, C. Young, D. T. Avanov, L. A. Dorelli, J. C. Gershman, D. J. Paterson, W. R. Lavraud, B. Saito, Y. TI Magnetic reconnection and modification of the Hall physics due to cold ions at the magnetopause SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE magnetic reconnection; magnetopause; electric fields; Hall current ID ART. NO. A03215; EARTHS MAGNETOSPHERE; OUTER MAGNETOSPHERE; PLASMASPHERIC PLUME; PLASMA; WIND; MULTISCALE; OUTFLOW; SPACE; SOLAR AB Observations by the four Magnetospheric Multiscale spacecraft are used to investigate the Hall physics of a magnetopause magnetic reconnection separatrix layer. Inside this layer of currents and strong normal electric fields, cold (eV) ions of ionospheric origin can remain frozen-in together with the electrons. The cold ions reduce the Hall current. Using a generalized Ohm's law, the electric field is balanced by the sum of the terms corresponding to the Hall current, the vxB drifting cold ions, and the divergence of the electron pressure tensor. A mixture of hot and cold ions is common at the subsolar magnetopause. A mixture of length scales caused by a mixture of ion temperatures has significant effects on the Hall physics of magnetic reconnection. C1 [Andre, M.; Li, W.; Khotyaintsev, Yu. V.; Vaivads, A.; Graham, D. B.; Norgren, C.] Swedish Inst Space Phys, Uppsala, Sweden. [Toledo-Redondo, S.] European Space Agcy ESAC, Madrid, Spain. [Norgren, C.] Uppsala Univ, Dept Phys & Astron, Uppsala, Sweden. [Burch, J.; Torbert, R.; Young, D. T.] Southwest Res Inst, San Antonio, TX USA. [Lindqvist, P. -A.; Marklund, G.] KTH, Stockholm, Sweden. [Ergun, R.] Univ Colorado, LASP, Boulder, CO 80309 USA. [Torbert, R.] Univ New Hampshire, Durham, NH 03824 USA. [Magnes, W.] Austrian Acad Sci, Space Res Inst, Graz, Austria. [Russell, C. T.] Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90024 USA. [Giles, B.; Moore, T. E.; Pollock, C.; Avanov, L. A.; Dorelli, J. C.; Gershman, D. J.; Paterson, W. R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA. [Chandler, M. O.] NASA, Marshall Space Flight Ctr, Huntsville, AL USA. [Gershman, D. J.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Lavraud, B.] Univ Toulouse, Inst Rech Astrophys & Planetol, Toulouse, France. [Lavraud, B.] CNRS, UMR 5277, Toulouse, France. [Saito, Y.] Inst Space & Astronaut Sci, JAXA, Chofu, Tokyo, Japan. RP Andre, M (reprint author), Swedish Inst Space Phys, Uppsala, Sweden. EM mats.andre@irfu.se RI NASA MMS, Science Team/J-5393-2013 OI NASA MMS, Science Team/0000-0002-9504-5214 FU Swedish National Space Board [SNSB 139/12, 164/14, 176/15]; CNES FX We thank the entire MMS team and instrument PIs for data access and support. MMS data are available at https://lasp.colorado.edu/mms/sdc/public/. We acknowledge support from the Swedish National Space Board contracts SNSB 139/12, 164/14, and 176/15. The IRAP contribution to MMS was supported by CNES. NR 52 TC 1 Z9 1 U1 8 U2 8 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD JUL 16 PY 2016 VL 43 IS 13 BP 6705 EP 6712 DI 10.1002/2016GL069665 PG 8 WC Geosciences, Multidisciplinary SC Geology GA DS6ON UT WOS:000380901600004 ER PT J AU Norgren, C Graham, DB Khotyaintsev, YV Andre, M Vaivads, A Chen, LJ Lindqvist, PA Marklund, GT Ergun, RE Magnes, W Strangeway, RJ Russell, CT Torbert, RB Paterson, WR Gershman, DJ Dorelli, JC Avanov, LA Lavraud, B Saito, Y Giles, BL Pollock, CJ Burch, JL AF Norgren, C. Graham, D. B. Khotyaintsev, Yu. V. Andre, M. Vaivads, A. Chen, L. -J. Lindqvist, P. -A. Marklund, G. T. Ergun, R. E. Magnes, W. Strangeway, R. J. Russell, C. T. Torbert, R. B. Paterson, W. R. Gershman, D. J. Dorelli, J. C. Avanov, L. A. Lavraud, B. Saito, Y. Giles, B. L. Pollock, C. J. Burch, J. L. TI Finite gyroradius effects in the electron outflow of asymmetric magnetic reconnection SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE magnetic reconnection; electron demagnetization; finite gyroradius effects; electron diffusion region ID DIFFUSION REGION AB We present observations of asymmetric magnetic reconnection showing evidence of electron demagnetization in the electron outflow. The observations were made at the magnetopause by the four Magnetospheric Multiscale (MMS) spacecraft, separated by approximate to 15km. The reconnecting current sheet has negligible guide field, and all four spacecraft likely pass close to the electron diffusion region just south of the X line. In the electron outflow near the X line, all four spacecraft observe highly structured electron distributions in a region comparable to a few electron gyroradii. The distributions consist of a core with T-vertical bar>T and a nongyrotropic crescent perpendicular to the magnetic field. The crescents are associated with finite gyroradius effects of partly demagnetized electrons. These observations clearly demonstrate the manifestation of finite gyroradius effects in an electron-scale reconnection current sheet. C1 [Norgren, C.; Graham, D. B.; Khotyaintsev, Yu. V.; Andre, M.; Vaivads, A.] Swedish Inst Space Phys, Uppsala, Sweden. [Norgren, C.] Uppsala Univ, Dept Phys & Astron, Uppsala, Sweden. [Chen, L. -J.; Paterson, W. R.; Gershman, D. J.; Dorelli, J. C.; Avanov, L. A.; Giles, B. L.; Pollock, C. J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA. [Chen, L. -J.; Gershman, D. J.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Lindqvist, P. -A.; Marklund, G. T.] KTH Royal Inst Technol, Sch Elect Engn, Space & Plasma Phys, Stockholm, Sweden. [Ergun, R. E.] Univ Colorado, Lab Atmospher & Space Phys, Boulder, CO 80309 USA. [Magnes, W.] Austrian Acad Sci, Space Res Inst, Graz, Austria. [Strangeway, R. J.; Russell, C. T.] Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA USA. [Torbert, R. B.] Univ New Hampshire, Ctr Space Sci, Durham, NH 03824 USA. [Lavraud, B.] Univ Toulouse, Inst Rech Astrophys & Planetol, Toulouse, France. [Lavraud, B.] CNRS, UMR 5277, Toulouse, France. [Saito, Y.] Inst Space & Astronaut Sci, JAXA, Sagamihara, Kanagawa, Japan. [Burch, J. L.] Southwest Res Inst, San Antonio, TX USA. RP Norgren, C (reprint author), Swedish Inst Space Phys, Uppsala, Sweden.; Norgren, C (reprint author), Uppsala Univ, Dept Phys & Astron, Uppsala, Sweden. EM cecilia.norgren@irfu.se RI NASA MMS, Science Team/J-5393-2013 OI NASA MMS, Science Team/0000-0002-9504-5214 FU Swedish National Space Board [23/12:2, 175/15]; CNES; CNRS FX We thank the entire MMS team and instrument PIs for data access and support. MMS data are available at https://lasp.colorado.edu/mms/sdc/public. This work was supported by the Swedish National Space Board, grants 23/12:2 and 175/15. The IRAP contribution was supported by CNES and CNRS. C.N. thanks the International Space Science Institute (ISSI) for supporting the team "from Cluster to MMS", from which this work was partly developed. NR 26 TC 3 Z9 3 U1 4 U2 5 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD JUL 16 PY 2016 VL 43 IS 13 BP 6724 EP 6733 DI 10.1002/2016GL069205 PG 10 WC Geosciences, Multidisciplinary SC Geology GA DS6ON UT WOS:000380901600006 ER PT J AU Poppe, AR Fillingim, MO Halekas, JS Raeder, J Angelopoulos, V AF Poppe, A. R. Fillingim, M. O. Halekas, J. S. Raeder, J. Angelopoulos, V. TI ARTEMIS observations of terrestrial ionospheric molecular ion outflow at the Moon SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE molecular ions; magnetotail; ion outflow; lunar volatiles; lunar exosphere ID INTERPLANETARY MAGNETIC-FIELD; COLD O+ BEAMS; ELECTRICAL-RESISTIVITY; LOBE/MANTLE REGIONS; EARTHS MAGNETOPAUSE; PLASMA SHEET; MAGNETOSPHERE; NITROGEN; OXYGEN; MODEL AB The Acceleration, Reconnection, Turbulence, and Electrodynamics of the Moon's Interaction with the Sun (ARTEMIS) spacecraft observes outflowing molecular ionospheric ions at lunar distances in the terrestrial magnetotail. The heavy ion fluxes are observed during geomagnetically disturbed times and consist of mainly molecular species ( N2+, NO+, and O2+, approximately masses 28-32amu) on the order of 10(5)-10(6)cm(-2)s(-1) at nearly identical velocities as concurrently present protons. By performing backward particle tracing in time-dependent electromagnetic fields from the magnetohydrodynamic Open Global Geospace Circulation Model of the terrestrial magnetosphere, we show that the ions escape the inner magnetosphere through magnetopause shadowing near noon and are subsequently accelerated to common velocities down the low-latitude boundary layer to lunar distances. At the Moon, the observed molecular ion outflow can sputter significant fluxes of neutral species into the lunar exosphere while also delivering nitrogen and oxygen to the lunar volatile inventory. C1 [Poppe, A. R.; Fillingim, M. O.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Poppe, A. R.; Halekas, J. S.] NASA, Ames Res Ctr, Solar Syst Explorat Res Virtual Inst, Moffett Field, CA 94035 USA. [Halekas, J. S.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. [Raeder, J.] Univ New Hampshire, Ctr Space Sci, Durham, NH 03824 USA. [Angelopoulos, V.] Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90024 USA. [Angelopoulos, V.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90024 USA. RP Poppe, AR (reprint author), Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.; Poppe, AR (reprint author), NASA, Ames Res Ctr, Solar Syst Explorat Res Virtual Inst, Moffett Field, CA 94035 USA. EM poppe@ssl.berkeley.edu FU NASA's Solar System Exploration Research Virtual Institute (SSERVI) [NNX14AG16A]; NASA LASER [NNX13AJ97G]; NSF [AGS-1143895]; NASA [NAS5-02099]; German Ministry for Economy and Technology; German Center for Aviation and Space (DLR) [50 OC 0302] FX A.R.P. and J.S.H. gratefully acknowledge support from NASA's Solar System Exploration Research Virtual Institute (SSERVI) grant NNX14AG16A and NASA LASER grant NNX13AJ97G. Work at UNH was supported by NSF grant AGS-1143895. The ARTEMIS mission is funded and operated under NASA grant NAS5-02099, and we specifically acknowledge J.P. McFadden for the use of ESA data and K.-H. Glassmeier, U. Auster, and W. Baumjohann for the use of FGM data provided under the lead of the Technical University of Braunschweig and with financial support through the German Ministry for Economy and Technology and the German Center for Aviation and Space (DLR) under contract 50 OC 0302. ARTEMIS data are publicly available at http://artemis.ssl.berkeley.edu. We thank the NASA Coordinated Community Modeling Center (CCMC) for use of the OpenGGCM model. Modeling results can be accessed by contacting the lead author. NR 49 TC 0 Z9 0 U1 3 U2 3 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD JUL 16 PY 2016 VL 43 IS 13 BP 6749 EP 6758 DI 10.1002/2016GL069715 PG 10 WC Geosciences, Multidisciplinary SC Geology GA DS6ON UT WOS:000380901600009 ER PT J AU Toledo-Redondo, S Andre, M Khotyaintsev, YV Vaivads, A Walsh, A Li, WY Graham, DB Lavraud, B Masson, A Aunai, N Divin, A Dargent, J Fuselier, S Gershman, DJ Dorelli, J Giles, B Avanov, L Pollock, C Saito, Y Moore, TE Coffey, V Chandler, MO Lindqvist, PA Torbert, R Russell, CT AF Toledo-Redondo, Sergio Andre, Mats Khotyaintsev, Yuri V. Vaivads, Andris Walsh, Andrew Li, Wenya Graham, Daniel B. Lavraud, Benoit Masson, Arnaud Aunai, Nicolas Divin, Andrey Dargent, Jeremy Fuselier, Stephen Gershman, Daniel J. Dorelli, John Giles, Barbara Avanov, Levon Pollock, Craig Saito, Yoshifumi Moore, Thomas E. Coffey, Victoria Chandler, Michael O. Lindqvist, Per-Arne Torbert, Roy Russell, Christopher T. TI Cold ion demagnetization near the X-line of magnetic reconnection SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE magnetic reconnection ID ART. NO. A03215; DAYSIDE MAGNETOPAUSE; PLASMASPHERIC PLUMES; STATISTICAL-ANALYSIS; OUTER MAGNETOSPHERE; EARTHS MAGNETOPAUSE; SPACECRAFT AB Although the effects of magnetic reconnection in magnetospheres can be observed at planetary scales, reconnection is initiated at electron scales in a plasma. Surrounding the electron diffusion region, there is an Ion-Decoupling Region (IDR) of the size of the ion length scales (inertial length and gyroradius). Reconnection at the Earth's magnetopause often includes cold magnetospheric (few tens of eV), hot magnetospheric (10keV), and magnetosheath (1keV) ions, with different gyroradius length scales. We report observations of a subregion inside the IDR of the size of the cold ion population gyroradius (approximate to 15km) where the cold ions are demagnetized and accelerated parallel to the Hall electric field. Outside the subregion, cold ions follow the E x B motion together with electrons, while hot ions are demagnetized. We observe a sharp cold ion density gradient separating the two regions, which we identify as the cold and hot IDRs. C1 [Toledo-Redondo, Sergio; Walsh, Andrew; Masson, Arnaud] European Space Agcy, Sci Directorate, ESAC, Madrid, Spain. [Andre, Mats; Khotyaintsev, Yuri V.; Vaivads, Andris; Li, Wenya; Graham, Daniel B.; Divin, Andrey] Swedish Inst Space Phys, Uppsala, Sweden. [Lavraud, Benoit; Dargent, Jeremy] Univ Toulouse UPS, Inst Rech Astrophys & Planetol, Toulouse, France. [Lavraud, Benoit; Dargent, Jeremy] CNRS, Toulouse, France. [Aunai, Nicolas; Dargent, Jeremy] Univ Paris 11, CNRS, Lab Plasma Phys, UPMC,Ecole Polytech, Paris, France. [Divin, Andrey] St Petersburg State Univ, Earth Phys Dept, Fac Phys, St Petersburg, Russia. [Fuselier, Stephen] Southwest Res Inst, San Antonio, TX USA. [Fuselier, Stephen] Univ Texas San Antonio, Dept Space Sci, San Antonio, TX USA. [Gershman, Daniel J.; Dorelli, John; Giles, Barbara; Avanov, Levon; Pollock, Craig; Moore, Thomas E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA. [Avanov, Levon] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Saito, Yoshifumi] Inst Space & Astronaut Sci, Sagamihara, Kanagawa, Japan. [Coffey, Victoria; Chandler, Michael O.] NASA, Marshall Space Flight Ctr, Huntsville, AL USA. [Lindqvist, Per-Arne] Royal Inst Technol, Dept Space & Plasma Phys, Stockholm, Sweden. [Torbert, Roy] Univ New Hampshire, Inst Study Earth Oceans & Space, Durham, NH 03824 USA. [Russell, Christopher T.] Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90024 USA. RP Toledo-Redondo, S (reprint author), European Space Agcy, Sci Directorate, ESAC, Madrid, Spain. EM sergiotr@ugr.es RI NASA MMS, Science Team/J-5393-2013; Divin, Andrey/E-4501-2015 OI NASA MMS, Science Team/0000-0002-9504-5214; Divin, Andrey/0000-0002-5579-3066 FU ESA Fellowship; science faculty of the European Space Astronomy Centre (ESAC) FX We would like to congratulate all the people involved in the MMS project for all their efforts during this early stage of the mission and the high quality achieved that will provide us great scientific return. S.T.R. holds an ESA Fellowship and acknowledges support from the science faculty of the European Space Astronomy Centre (ESAC). MMS data are available to the public in the MMS Science Data Center (https://lasp.colorado.edu/mms/sdc/public/). NR 33 TC 1 Z9 1 U1 4 U2 4 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD JUL 16 PY 2016 VL 43 IS 13 BP 6759 EP 6767 DI 10.1002/2016GL069877 PG 9 WC Geosciences, Multidisciplinary SC Geology GA DS6ON UT WOS:000380901600010 ER PT J AU Schorghofer, N Mazarico, E Platz, T Preusker, F Schroder, SE Raymond, CA Russell, CT AF Schorghofer, Norbert Mazarico, Erwan Platz, Thomas Preusker, Frank Schroeder, Stefan E. Raymond, Carol A. Russell, Christopher T. TI The permanently shadowed regions of dwarf planet Ceres SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE Ceres; cold traps; Dawn mission; planetary science ID WATER ICE; SURFACE VOLATILES; POLAR-REGIONS; LUNAR-SURFACE; MERCURY; CRATERS; FRACTIONATION; TEMPERATURE; STABILITY; MIGRATION AB Ceres has only a small spin axis tilt (4 degrees), and craters near its rotational poles can experience permanent shadow and trap volatiles, as is the case on Mercury and on Earth's Moon. Topography derived from stereo imaging by the Dawn spacecraft is used to calculate direct solar irradiance that defines the extent of the permanently shadowed regions (PSRs). In the northern polar region, PSRs cover approximate to 1800km(2) or 0.13% of the hemisphere, and most of the PSRs are cold enough to trap water ice over geological time periods. Based on modeling of the water exosphere, water molecules seasonally reside around the winter pole and ultimately an estimated 0.14% of molecules get trapped. Even for the lowest estimates of the amount of available water, this predicts accumulation rates in excess of loss rates, and hence, there should be fresh ice deposits in the cold traps. C1 [Schorghofer, Norbert] Univ Hawaii Manoa, Inst Astron, Honolulu, HI 96822 USA. [Mazarico, Erwan] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA. [Platz, Thomas] Max Planck Inst Solar Syst Res, Gottingen, Germany. [Preusker, Frank; Schroeder, Stefan E.] Deutsch Zentrum Luft & Raumfahrt DLR, Berlin, Germany. [Raymond, Carol A.] Jet Prop Lab, Pasadena, CA USA. [Russell, Christopher T.] Univ Calif Los Angeles, Dept Earth Planetary & Space Sci, Los Angeles, CA USA. RP Schorghofer, N (reprint author), Univ Hawaii Manoa, Inst Astron, Honolulu, HI 96822 USA. EM norbert@hawaii.edu RI Platz, Thomas/F-7539-2013; Schroder, Stefan/D-9709-2013 OI Platz, Thomas/0000-0002-1253-2034; Schroder, Stefan/0000-0003-0323-8324 FU National Aeronautics and Space Administration [NNX15AI38G]; DACGIP FX We thank the Dawn team for the acquisition and processing of data used in this work. N.S. was supported by the National Aeronautics and Space Administration under grant NNX15AI38G issued through the Dawn at Ceres Guest Investigator Program (DACGIP). E.M. also acknowledges support from DACGIP. NR 40 TC 3 Z9 3 U1 6 U2 6 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD JUL 16 PY 2016 VL 43 IS 13 BP 6783 EP 6789 DI 10.1002/2016GL069368 PG 7 WC Geosciences, Multidisciplinary SC Geology GA DS6ON UT WOS:000380901600013 ER PT J AU Hughes, CW Williams, J Hibbert, A Boening, C Oram, J AF Hughes, Chris W. Williams, Joanne Hibbert, Angela Boening, Carmen Oram, James TI A Rossby whistle: A resonant basin mode observed in the Caribbean Sea SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE Caribbean Sea; sea level; bottom pressure; Rossby wave; basin mode ID MESOSCALE VARIABILITY; OCEAN AB We show that an important source of coastal sea level variability around the Caribbean Sea is a resonant basin mode. The mode consists of a baroclinic Rossby wave which propagates westward across the basin and is rapidly returned to the east along the southern boundary as coastal shelf waves. Almost two wavelengths of the Rossby wave fit across the basin, and it has a period of 120days. The porous boundary of the Caribbean Sea results in this mode exciting a mass exchange with the wider ocean, leading to a dominant mode of bottom pressure variability which is almost uniform over the Grenada, Venezuela, and Colombia basins and has a sharp spectral peak at 120day period. As the Rossby waves have been shown to be excited by instability of the Caribbean Current, this resonant mode is dynamically equivalent to the operation of a whistle. C1 [Hughes, Chris W.; Oram, James] Univ Liverpool, Sch Environm Sci, Liverpool, Merseyside, England. [Hughes, Chris W.; Williams, Joanne; Hibbert, Angela] Natl Oceanog Ctr, Liverpool, Merseyside, England. [Boening, Carmen] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Hughes, CW (reprint author), Univ Liverpool, Sch Environm Sci, Liverpool, Merseyside, England.; Hughes, CW (reprint author), Natl Oceanog Ctr, Liverpool, Merseyside, England. EM cwh@liv.ac.uk FU National Oceanographic Partnership Program (NOPP); NERC through the National Oceanography Centre; NERC [NE/I023384/1] FX We thank the Permanent Service for Mean Sea Level for providing quality-controlled tide gauge and bottom pressure data, which can be found at http://www.psmsl.org/, and AVISO for provision of the ocean dynamic topography product at http://www.aviso.altimetry.fr/. The ECCO ocean state estimates were provided by the ECCO Consortium for Estimating the Circulation and Climate of the Ocean funded by the National Oceanographic Partnership Program (NOPP). NCEP Reanalysis data were provided by the NOAA/OAR/ESRL PSD, Boulder, Colorado, USA, from http://www.esrl.noaa.gov/psd/. The JPL GRACE Mascon data can be downloaded from http://grace.jpl.nasa.gov. Any other data used in this paper will be supplied by C.W.H. on request by e-mail. This work has been supported by NERC through the National Oceanography Centre, as well as through grant NE/I023384/1. The OCCAM and NEMO models were run and provided by the NOC Southampton modeling group. We thank them and particularly Andrew Coward and Beverly de Cuevas for their help with these data sets. NR 25 TC 0 Z9 0 U1 0 U2 0 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD JUL 16 PY 2016 VL 43 IS 13 BP 7036 EP 7043 DI 10.1002/2016GL069573 PG 8 WC Geosciences, Multidisciplinary SC Geology GA DS6ON UT WOS:000380901600043 ER PT J AU Dhomse, SS Chipperfield, MP Damadeo, RP Zawodny, JM Ball, WT Feng, W Hossaini, R Mann, GW Haigh, JD AF Dhomse, S. S. Chipperfield, M. P. Damadeo, R. P. Zawodny, J. M. Ball, W. T. Feng, W. Hossaini, R. Mann, G. W. Haigh, J. D. TI On the ambiguous nature of the 11year solar cycle signal in upper stratospheric ozone SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE solar signal; stratosphere; modeling ID CHEMICAL-TRANSPORT MODEL; QUASI-BIENNIAL OSCILLATION; MT. PINATUBO ERUPTION; SPECTRAL IRRADIANCE; CLIMATE MODEL; SAGE II; SIMULATIONS; VARIABILITY; CIRCULATION; VERSION AB Up to now our understanding of the 11year ozone solar cycle signal (SCS) in the upper stratosphere has been largely based on the Stratospheric Aerosol and Gas Experiment (SAGE) II (v6.2) data record, which indicated a large positive signal which could not be reproduced by models, calling into question our understanding of the chemistry of the upper stratosphere. Here we present an analysis of new v7.0 SAGE II data which shows a smaller upper stratosphere ozone SCS, due to a more realistic ozone-temperature anticorrelation. New simulations from a state-of-art 3-D chemical transport model show a small SCS in the upper stratosphere, which is in agreement with SAGE v7.0 data and the shorter Halogen Occultation Experiment and Microwave Limb Sounder records. However, despite these improvements in the SAGE II data, there are still large uncertainties in current observational and meteorological reanalysis data sets, so accurate quantification of the influence of solar flux variability on the climate system remains an open scientific question. C1 [Dhomse, S. S.; Chipperfield, M. P.; Feng, W.; Hossaini, R.; Mann, G. W.] Univ Leeds, Sch Earth & Environm, Leeds, W Yorkshire, England. [Dhomse, S. S.; Chipperfield, M. P.] Univ Leeds, Natl Ctr Earth Observat, Leeds, W Yorkshire, England. [Damadeo, R. P.; Zawodny, J. M.] NASA, Langley Res Ctr, Hampton, VA 23665 USA. [Ball, W. T.] PMOD WRC, Davos, Switzerland. [Feng, W.; Mann, G. W.] Univ Leeds, Natl Ctr Atmospher Sci, Leeds, W Yorkshire, England. [Haigh, J. D.] Imperial Coll, Grantham Inst, London, England. [Haigh, J. D.] Imperial Coll, Blackett Lab, London, England. RP Dhomse, SS (reprint author), Univ Leeds, Sch Earth & Environm, Leeds, W Yorkshire, England.; Dhomse, SS (reprint author), Univ Leeds, Natl Ctr Earth Observat, Leeds, W Yorkshire, England. EM S.S.Dhomse@leeds.ac.uk RI FENG, WUHU/B-8327-2008; Dhomse, Sandip/C-8198-2011 OI Ball, William/0000-0002-1005-3670; FENG, WUHU/0000-0002-9907-9120; Dhomse, Sandip/0000-0003-3854-5383 FU NERC SOLCLI [NE/D002753/1]; MAPLE [NE/J008621/1] FX This work was supported by the NERC SOLCLI (NE/D002753/1) and MAPLE (NE/J008621/1) projects. We thank the NASA/NOAA for the MLS and HALOE data. Model simulations were performed on the Archer and Leeds Arc1 HPC systems. NR 35 TC 2 Z9 2 U1 9 U2 9 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD JUL 16 PY 2016 VL 43 IS 13 BP 7241 EP 7249 DI 10.1002/2016GL069958 PG 9 WC Geosciences, Multidisciplinary SC Geology GA DS6ON UT WOS:000380901600067 ER PT J AU Sarangi, C Tripathi, SN Mishra, AK Goel, A Welton, EJ AF Sarangi, Chandan Tripathi, S. N. Mishra, A. K. Goel, A. Welton, E. J. TI Elevated aerosol layers and their radiative impact over Kanpur during monsoon onset period SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE elevated aerosol layer; radiative forcing efficiency; daytime variations; lower atmospheric cooling; atmospheric stability ID ASIAN SUMMER MONSOON; INDO-GANGETIC BASIN; REGIONAL CLIMATE MODEL; BLACK CARBON AEROSOLS; LONG-RANGE TRANSPORT; ENERGY SYSTEM CERES; MAJOR DUST STORMS; VERTICAL-DISTRIBUTION; SEASONAL-VARIATION; PREMONSOON SEASON AB Accurate information about aerosol vertical distribution is needed to reduce uncertainties in aerosol radiative forcing and its effect on atmospheric dynamics. The present study deals with synergistic analyses of aerosol vertical distribution and aerosol optical depth (AOD) with meteorological variables using multisatellite and ground-based remote sensors over Kanpur in central Indo-Gangetic Plain (IGP). Micro-Pulse Lidar Network-derived aerosol vertical extinction (sigma) profiles are analyzed to quantify the interannual and daytime variations during monsoon onset period (May-June) for 2009-2011. The mean aerosol profile is broadly categorized into two layers viz., a surface layer (SL) extending up to 1.5km (where sigma decreased exponentially with height) and an elevated aerosol layer (EAL) extending between 1.5 and 5.5km. The increase in total columnar aerosol loading is associated with relatively higher increase in contribution from EAL loading than that from SL. The mean contributions of EALs are about 60%, 51%, and 50% to total columnar AOD during 2009, 2010, and 2011, respectively. We observe distinct parabolic EALs during early morning and late evening but uniformly mixed EALs during midday. The interannual and daytime variations of EALs are mainly influenced by long-range transport and convective capacity of the local emissions, respectively. Radiative flux analysis shows that clear-sky incoming solar radiation at surface is reduced with increase in AOD, which indicates significant cooling at surface. Collocated analysis of atmospheric temperature and aerosol loading reveals that increase in AOD not only resulted in surface dimming but also reduced the temperature (approximate to 2-3 degrees C) of lower troposphere (below 3km altitude). Radiative transfer simulations indicate that the reduction of incoming solar radiation at surface is mainly due to increased absorption by EALs (with increase in total AOD). The observed cooling in lower troposphere in high aerosol loading scenario could be understood as a dynamical feedback of EAL-induced stratification of lower troposphere. Further, the observed radiative effect of EALs increases the stability of the lower troposphere, which could modulate the large-scale atmospheric dynamics during monsoon onset period. These findings encourage follow-up studies on the implication of EALs to the Indian summer monsoon dynamics using numerical models. C1 [Sarangi, Chandan; Tripathi, S. N.; Goel, A.] Indian Inst Technol, Dept Civil Engn, Kanpur, Uttar Pradesh, India. [Mishra, A. K.] Indian Inst Technol, Ctr Environm Sci & Engn, Kanpur, Uttar Pradesh, India. [Welton, E. J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA. RP Tripathi, SN (reprint author), Indian Inst Technol, Dept Civil Engn, Kanpur, Uttar Pradesh, India. EM snt@iitk.ac.in RI Tripathi, Sachchida/J-4840-2016 FU Earth System Science Organization, Ministry of Earth Sciences, Government of India [MM/NERC-MoES-03/2014/002] FX The authors gratefully acknowledge the financial support given by the Earth System Science Organization, Ministry of Earth Sciences, Government of India (grant MM/NERC-MoES-03/2014/002) to conduct this research under Monsoon Mission. The authors would like to thank B.N. Holben and staff at NASA GSFC for establishing and processing data of the AERONET and SolRad-Net site at IIT Kanpur, used in this study. We acknowledge the use of radiosonde data freely available from University of Wyoming, the NCEP Reanalysis data provided by the NOAA/OAR/ESRL USA, and use of HYSPLIT model of NOAA-ARL for back trajectory analysis. MODIS, MISR, CERES, CALIPSO, and AIRS data sets were obtained from the NASA Langley Research Centre Atmospheric Science Data Center. All data measured at IITK are available on request from author (snt@iitk.ac.in). We also appreciate help from V.P. Kanawade in Figure 3. NR 111 TC 0 Z9 0 U1 6 U2 6 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD JUL 16 PY 2016 VL 121 IS 13 BP 7936 EP 7957 DI 10.1002/2015JD024711 PG 22 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA DS4DB UT WOS:000380730500026 ER PT J AU Carey, LD Koshak, W Peterson, H Mecikalski, RM AF Carey, Lawrence D. Koshak, William Peterson, Harold Mecikalski, Retha M. TI The kinematic and microphysical control of lightning rate, extent, and NOX production SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE lightning; flash rate; flash extent; NOx production; radar; LMA ID PRECIPITATION DEVELOPMENT; POLARIMETRIC RADAR; TRANSPORT MODELS; MAPPING ARRAY; STORM; ELECTRIFICATION; THUNDERSTORMS; CONVECTION; ALABAMA; PARAMETERIZATION AB This study investigates the kinematic and microphysical control of lightning properties, particularly those that may govern the production of nitrogen oxides (NOX=NO+NO2) via lightning (LNOX), such as flash rate, type, and extent. The NASA Lightning Nitrogen Oxides Model (LNOM) is applied to lightning observations following multicell thunderstorms through their lifecycle in a Lagrangian sense over Northern Alabama on 21 May 2012 during the Deep Convective Clouds and Chemistry (DC3) experiment. LNOM provides estimates of flash rate, type, channel length distributions, channel segment altitude distributions (SADs), and LNOX production profiles. The LNOM-derived lightning characteristics and LNOX production are compared to the evolution of radar-inferred updraft and precipitation properties. Intercloud, intracloud (IC) flash SAD comprises a significant fraction of the total (IC+cloud-to-ground [CG]) SAD, while increased CG flash SAD at altitudes >6km occurs after the simultaneous peaks in several thunderstorm properties (i.e., total [IC+CG] and IC flash rate, graupel volume/mass, convective updraft volume, and maximum updraft speed). At heights <6km, the CG LNOX production dominates the column-integrated total LNOX production. Unlike the SAD, total LNOX production consists of a more equal contribution from IC and CG flashes for heights >6km. Graupel volume/mass, updraft volume, and maximum updraft speed are all well correlated to the total flash rate (correlation coefficient, 0.8) but are less correlated to total flash extent (0.6) and total LNOX production (0.5). Although LNOM transforms lightning observations into LNOX production values, these values are estimates and are subject to further independent validation. C1 [Carey, Lawrence D.; Mecikalski, Retha M.] Univ Alabama, Dept Atmospher Sci, Huntsville, AL 35899 USA. [Koshak, William] NASA, Earth Sci Off, Marshall Space Flight Ctr, Huntsville, AL USA. [Peterson, Harold] Bur Indian Affairs, Eastern Region Off, Nashville, TN USA. RP Carey, LD (reprint author), Univ Alabama, Dept Atmospher Sci, Huntsville, AL 35899 USA. EM larry.carey@nsstc.uah.edu FU National Science Foundation's Physical and Dynamical Meteorology (NSF PDM) Program [AGS-1063573] FX We wish to recognize funding from the National Science Foundation's Physical and Dynamical Meteorology (NSF PDM) Program (AGS-1063573), which has supported the DC3 field experiment and associated research. We want to acknowledge Lamont Bain for his time editing and gridding the ARMOR and KHTX data and for creating the dual-Doppler fields used in this and other manuscripts. We also wish to thank the many, many people who made the collection of DC3 observations possible. The data used herein can be obtained from the DC3 webpage located here: http://data.eol.ucar.edu/master_list/?project=DC3. Finally, we wish to thank three anonymous reviewers for comments that have substantially improved the quality of this research paper. NR 60 TC 2 Z9 2 U1 3 U2 4 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD JUL 16 PY 2016 VL 121 IS 13 BP 7975 EP 7989 DI 10.1002/2015JD024703 PG 15 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA DS4DB UT WOS:000380730500028 ER PT J AU Collow, ABM Miller, MA Trabachino, LC AF Collow, Allison B. Marquardt Miller, Mark A. Trabachino, Lynne C. TI Cloudiness over the Amazon rainforest: Meteorology and thermodynamics SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE thermodynamics; lifting condensation level; GoAmazon ID SOUTH-AMERICA; CLIMATE-CHANGE; WATER-VAPOR; DEFORESTATION; CONVECTION; CIRCULATION; SURFACE; BASIN; VARIABILITY; DYNAMICS AB Comprehensive meteorological observations collected during GOAmazon2014/15 using the Atmospheric Radiation Measurement Mobile Facility no. 1 and assimilated observations from the Modern-Era Retrospective Analysis for Research and Applications, Version 2 are used to document the seasonal cycle of cloudiness, thermodynamics, and precipitation above the Amazon rainforest. The reversal of synoptic-scale vertical motions modulates the transition between the wet and dry seasons. Ascending moist air during the wet season originates near the surface of the Atlantic Ocean and is advected into the Amazon rainforest, where it experiences convergence and, ultimately, precipitates. The dry season is characterized by weaker winds and synoptic-scale subsidence with little or no moisture convergence accompanying moisture advection. This combination results in the drying of the midtroposphere during June through October as indicated by a decrease in liquid water path, integrated water, and the vertical profile of water vapor mixing ratio. The vertical profile of cloud fraction exhibits a relatively consistent decline in cloud fraction from the lifting condensation level (LCL) to the freezing level where a minimum is observed, unlike many other tropical regions. Coefficients of determination between the LCL and cloud fractional coverage suggest a relatively robust relationship between the LCL and cloudiness beneath 5km during the dry season (R-2=0.42) but a weak relationship during the wet season (0.12). C1 [Collow, Allison B. Marquardt; Miller, Mark A.; Trabachino, Lynne C.] Rutgers State Univ, Inst Earth Ocean & Atmospher Sci, New Brunswick, NJ 08901 USA. [Collow, Allison B. Marquardt] Univ Space Res Assoc, Columbia, MD 21046 USA. [Collow, Allison B. Marquardt] NASA, Global Modeling & Assimilat Off, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Collow, ABM (reprint author), Rutgers State Univ, Inst Earth Ocean & Atmospher Sci, New Brunswick, NJ 08901 USA.; Collow, ABM (reprint author), Univ Space Res Assoc, Columbia, MD 21046 USA.; Collow, ABM (reprint author), NASA, Global Modeling & Assimilat Off, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM allison.collow@nasa.gov FU Department of Energy's Atmospheric System Research program [DE-FG02-08ER64531]; U.S. Department of Energy, Office of Science, Office of Biological and Environmental Research, Climate and Environmental Sciences Division; National Aeronautics and Space Administration FX This work is supported by the Department of Energy's Atmospheric System Research program award DE-FG02-08ER64531. Data used in this study were obtained from the Atmospheric Radiation Measurement Program sponsored by the U.S. Department of Energy, Office of Science, Office of Biological and Environmental Research, Climate and Environmental Sciences Division (http://www.archive.arm.gov/), and the National Aeronautics and Space Administration (http://ceres.larc.nasa.gov/order_data.php and http://daac.gsfc.nasa.gov/). We would like to thank Kathleen Schiro for sharing data quality concerns regarding the precipitation observations at the AMF11 and Ben Lintner for providing guidance throughout the study. NR 51 TC 1 Z9 1 U1 12 U2 12 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD JUL 16 PY 2016 VL 121 IS 13 BP 7990 EP 8005 DI 10.1002/2016JD024848 PG 16 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA DS4DB UT WOS:000380730500029 ER PT J AU Aquila, V Swartz, WH Waugh, DW Colarco, PR Pawson, S Polvani, LM Stolarski, RS AF Aquila, V. Swartz, W. H. Waugh, D. W. Colarco, P. R. Pawson, S. Polvani, L. M. Stolarski, R. S. TI Isolating the roles of different forcing agents in global stratospheric temperature changes using model integrations with incrementally added single forcings SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE stratospheric temperatures; ozone; volcanic eruptions; solar cycle; ODS; greenhouse gases ID OZONE-DEPLETING SUBSTANCES; CHEMISTRY-CLIMATE MODEL; ATMOSPHERIC-TEMPERATURE; GREENHOUSE GASES; SPECTRAL IRRADIANCE; VOLCANIC-ERUPTIONS; NATURAL INFLUENCES; SOLAR-CYCLE; IN-SITU; TRENDS AB Satellite instruments show a cooling of global stratospheric temperatures over the whole data record (1979-2014). This cooling is not linear and includes two descending steps in the early 1980s and mid-1990s. The 1979-1995 period is characterized by increasing concentrations of ozone-depleting substances (ODSs) and by the two major volcanic eruptions of El Chichon (1982) and Mount Pinatubo (1991). The 1995-present period is characterized by decreasing ODS concentrations and by the absence of major volcanic eruptions. Greenhouse gas (GHG) concentrations increase over the whole time period. In order to isolate the roles of different forcing agents in the global stratospheric temperature changes, we performed a set of simulations using the NASA Goddard Earth Observing System Chemistry-Climate Model with prescribed sea surface temperatures. We find that in our model simulations the cooling of the stratosphere from 1979 to present is mostly driven by changes in GHG concentrations in the middle and upper stratosphere and by GHG and ODS changes in the lower stratosphere. While the cooling trend caused by increasing GHGs is roughly constant over the satellite era, changing ODS concentrations cause a significant stratospheric cooling only up to the mid-1990s, when they start to decrease because of the implementation of the Montreal Protocol. Sporadic volcanic events and the solar cycle have a distinct signature in the time series of stratospheric temperature anomalies but do not play a statistically significant role in the long-term trends from 1979 to 2014. Several factors combine to produce the step-like behavior in the stratospheric temperatures: in the lower stratosphere, the flattening starting in the mid-1990s is due to the decrease in ozone-depleting substances; Mount Pinatubo and the solar cycle cause the abrupt steps through the aerosol-associated warming and the volcanically induced ozone depletion. In the middle and upper stratosphere, changes in solar irradiance are largely responsible for the step-like behavior of global temperature anomalies, together with volcanically induced ozone depletion and water vapor increases in the post-Pinatubo years. C1 [Aquila, V.] Goddard Earth Sci Technol & Res GESTAR, Columbia, MD 21046 USA. [Aquila, V.; Waugh, D. W.; Stolarski, R. S.] Johns Hopkins Univ, Dept Earth & Planetary Sci, Baltimore, MD 21218 USA. [Aquila, V.; Colarco, P. R.] NASA, Lab Atmospher Chem & Dynam Code 614, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Swartz, W. H.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA. [Pawson, S.] NASA, Global Modeling & Assimilat Off, Goddard Space Flight Ctr, Greenbelt, MD USA. [Polvani, L. M.] Columbia Univ, New York, NY USA. RP Aquila, V (reprint author), Goddard Earth Sci Technol & Res GESTAR, Columbia, MD 21046 USA.; Aquila, V (reprint author), Johns Hopkins Univ, Dept Earth & Planetary Sci, Baltimore, MD 21218 USA.; Aquila, V (reprint author), NASA, Lab Atmospher Chem & Dynam Code 614, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM valentina.aquila@jhu.edu RI Pawson, Steven/I-1865-2014; Swartz, William/A-1965-2010; Colarco, Peter/D-8637-2012 OI Pawson, Steven/0000-0003-0200-717X; Swartz, William/0000-0002-9172-7189; Colarco, Peter/0000-0003-3525-1662 FU NASA; U.S. National Science Foundation FX The authors would like to thank D. Seidel, L. Oman, and P. Newman for useful discussions and C. McLandress for providing the AMSU/SSU temperature data. We also thank the three reviewers for their comments. The model simulations were performed at the NASA Center for Climate Simulation. V.A. is funded, in part, by the NASA Model, Analysis, and Prediction program. W.H.S. is funded for this work by a grant from NASA's Living With a Star program. L.M.P. and D.W.W. are funded, in part, by a grant from the U.S. National Science Foundation. The MSU data record is available at http://www.remss.com/measurements/upper-air-temperature. The simulated temperature records are available upon request to the corresponding author. NR 61 TC 2 Z9 2 U1 7 U2 10 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD JUL 16 PY 2016 VL 121 IS 13 BP 8067 EP 8082 DI 10.1002/2015JD023841 PG 16 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA DS4DB UT WOS:000380730500034 ER PT J AU Li, Y Barth, MC Chen, G Patton, EG Kim, SW Wisthaler, A Mikoviny, T Fried, A Clark, R Steiner, AL AF Li, Yang Barth, Mary C. Chen, Gao Patton, Edward G. Kim, Si-Wan Wisthaler, Armin Mikoviny, Tomas Fried, Alan Clark, Richard Steiner, Allison L. TI Large-eddy simulation of biogenic VOC chemistry during the DISCOVER-AQ 2011 campaign SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE isoprene; segregation; turbulence; OH reactivity ID VOLATILE ORGANIC-COMPOUNDS; CONVECTIVE BOUNDARY-LAYER; MEXICO-CITY; ATMOSPHERIC CHEMISTRY; PHOTOOXIDATION PRODUCTS; VERTICAL-DISTRIBUTION; ISOPRENE OXIDATION; CHEMICAL-REACTIONS; SHALLOW CUMULUS; REGIONAL MODEL AB Biogenic volatile organic compounds (BVOCs) are oxidized quickly in the atmosphere to form oxygenated VOC (OVOC) and play crucial roles in the formation of ozone and secondary organic aerosols. We use the National Center for Atmospheric Research's large-eddy simulation model and Deriving Information on Surface Conditions from Column and Vertically Resolved Observations Relevant to Air Quality 2011 flight data to understand the role of boundary layer turbulence on the atmospheric chemistry of key BVOC species and their oxidation products. We simulate three distinct convective environments during the campaign, representing fair weather conditions (case 1: 1 July), a convective event dominated by southwesterly flow (case 2: 11 July), and a polluted event with high temperature and convection (case 3: 29 July). Isoprene segregation is greatest in the lower boundary layer under warm and convective conditions, reaching up to a 10% reduction in the isoprene-OH reaction rate. Under warm and convective conditions, the BVOC lifetimes lengthen due to increased isoprene emission, elevated initial chemical concentrations, and OH competition. Although turbulence-driven segregation has less influence on the OVOC species, convection mixes more OVOC into the upper atmospheric boundary layer (ABL) and increases the total OH reactivity. Production and loss rates of ozone above 2km in all the three cases indicate in situ ozone formation in addition to vertical convective transport of ozone from the surface and aloft, consistent with the increased contribution of OH reactivity from OVOC. Together, these results show that total OH reactivity in the ABL increases under warmer and stronger convective conditions due to enhanced isoprene emission and the OVOC contribution to ozone formation. C1 [Li, Yang; Steiner, Allison L.] Univ Michigan, Climate & Space Sci & Engn, Ann Arbor, MI 48109 USA. [Barth, Mary C.; Patton, Edward G.] Natl Ctr Atmospher Res, POB 3000, Boulder, CO 80307 USA. [Chen, Gao] NASA, Langley Res Ctr, Hampton, VA 23665 USA. [Kim, Si-Wan] NOAA, Div Chem Sci, Earth Syst Res Lab, Boulder, CO USA. [Kim, Si-Wan] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA. [Wisthaler, Armin] Univ Innsbruck, Inst Ion Phys & Appl Phys, Innsbruck, Austria. [Wisthaler, Armin; Mikoviny, Tomas] Univ Oslo, Dept Chem, Oslo, Norway. [Mikoviny, Tomas] ORAU, Oak Ridge, TN USA. [Fried, Alan] Univ Colorado, Inst Arctic & Alpine Res, Boulder, CO 80309 USA. [Clark, Richard] Millersville Univ Pennsylvania, Dept Earth Sci, Millersville, PA USA. RP Li, Y (reprint author), Univ Michigan, Climate & Space Sci & Engn, Ann Arbor, MI 48109 USA. EM yanglibj@umich.edu RI Manager, CSD Publications/B-2789-2015; Steiner, Allison/F-4942-2011; OI Patton, Edward/0000-0001-5431-9541 FU NASA [NNX13AN76H]; National Science Foundation; NASA FX This research is supported by NASA Earth and Space Science Fellowship NNX13AN76H. The National Center for Atmospheric Research is sponsored by the National Science Foundation. We gratefully acknowledge Kenneth Davis, Chin-Hoh Moeng, and Peter Sullivan for their initiation of the study and the development of the NCAR LES model. DISCOVER-AQ 2011 campaign data are obtained through DISCOVER-AQ doi:10.5067/Aircraft/DISCOVER-AQ/Aerosol-TraceGas. The PTR-MS measurements aboard the NASA P-3B were supported by the Austrian Federal Ministry for Transport, Innovation, and Technology through the Austrian Space Applications Programme of the Austrian Research Promotion Agency. Tomas Mikoviny was supported by an appointment to the NASA Postdoctoral Program at the Langley Research Center, administered by Oak Ridge Associated Universities through a contract with NASA. We gratefully acknowledge Si-Chee Tsay (NASA Goddard Space Flight Center) for providing the NOx measurements and Edwin Gluth (Maryland Department of the Environment) for providing the surface temperature in the Fair Hill site. MERRA IC/BC data are obtained through the Modeling and Assimilation Data and Information Services Center (http://disc.sci.gsfc.nasa.gov/daac-bin/DataHoldings.pl). For data from model runs in this paper, please contact Yang Li (University of Michigan; yanglibj@umich.edu). NR 74 TC 0 Z9 0 U1 8 U2 10 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD JUL 16 PY 2016 VL 121 IS 13 BP 8083 EP 8105 DI 10.1002/2016JD024942 PG 23 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA DS4DB UT WOS:000380730500035 ER PT J AU Barnes, EA Parazoo, N Orbe, C Denning, AS AF Barnes, Elizabeth A. Parazoo, Nicholas Orbe, Clara Denning, A. Scott TI Isentropic transport and the seasonal cycle amplitude of CO2 SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE carbon dioxide; synoptic transport; isentropic transport; seasonal cycle ID ATMOSPHERE-BIOSPHERE EXCHANGE; COLUMN CARBON-DIOXIDE; EARTH SYSTEM MODELS; TERRESTRIAL BIOSPHERE; NORTHERN ECOSYSTEMS; CLIMATE-CHANGE; PRODUCTIVITY; FOREST; VULNERABILITY; NITROGEN AB Carbon-concentration feedbacks and carbon-climate feedbacks constitute one of the largest sources of uncertainty in future climate. Since the beginning of the modern atmospheric CO2 record, seasonal variations in CO2 have been recognized as a signal of the metabolism of land ecosystems, and quantitative attribution of changes in the seasonal cycle amplitude (SCA) of CO2 to ecosystem processes is critical for understanding and projecting carbon-climate feedbacks far into the 21st Century. Here the impact of surface carbon fluxes on the SCA of CO2 throughout the Northern Hemisphere troposphere is investigated, paying particular attention to isentropic transport across latitudes. The analysis includes both a chemical transport model GOES-Chem and an idealized tracer in a gray-radiation aquaplanet. The results of the study can be summarized by two main conclusions: (1) the SCA of CO2 roughly follows surfaces of constant potential temperature, which can explain the observed increase in SCA with latitude along pressure surfaces and (2) increasing seasonal fluxes in lower latitudes have a larger impact on the SCA of CO2 throughout most of the troposphere compared to increasing seasonal fluxes in higher latitudes. These results provide strong evidence that recently observed changes in the SCA of CO2 at high northern latitudes (poleward of 60 degrees N) are likely driven by changes in midlatitude surface fluxes, rather than changes in Arctic fluxes. C1 [Barnes, Elizabeth A.; Denning, A. Scott] Colorado State Univ, Dept Atmospher Sci, Ft Collins, CO 80523 USA. [Parazoo, Nicholas] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Parazoo, Nicholas] Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA USA. [Orbe, Clara] Johns Hopkins Univ, Dept Earth & Planetary Sci, Goddard Earth Sci Technol & Res GESTAR, Baltimore, MD 21218 USA. [Orbe, Clara] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA. RP Barnes, EA (reprint author), Colorado State Univ, Dept Atmospher Sci, Ft Collins, CO 80523 USA. EM eabarnes@atmos.colostate.edu RI Barnes, Elizabeth/O-1790-2014 OI Barnes, Elizabeth/0000-0003-4284-9320 FU National Science Foundation [1419818]; NASA's Science Mission Directorate [NNX15AJ09G]; National Aeronautics and Space Administration FX The authors would like to thank three anonymous reviewers for their helpful comments on an earlier version of this manuscript. E.A.B. was supported by the Climate and Large-scale Dynamics Program of the National Science Foundation under grant 1419818. A.S.D. gratefully acknowledges support from NASA's Science Mission Directorate under the Atmospheric Carbon Transport project (NNX15AJ09G). Part of the research in this study was performed at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. We thank C. Koven for providing CLM4.5 CO2 surface flux fields, and the ODIAC fossil fuel CO2 emissions were provided by T. Oda. The model output supporting the conclusions of this article is available from the corresponding author upon request (eabarnes@atmos.colostate.edu). NR 66 TC 1 Z9 1 U1 7 U2 9 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD JUL 16 PY 2016 VL 121 IS 13 BP 8106 EP 8124 DI 10.1002/2016JD025109 PG 19 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA DS4DB UT WOS:000380730500036 ER PT J AU Cui, H Xiao, SH Zhou, CM Peng, YB Kaufman, AJ Plummer, RE AF Cui, Huan Xiao, Shuhai Zhou, Chuanming Peng, Yongbo Kaufman, Alan J. Plummer, Rebecca E. TI Phosphogenesis associated with the Shuram Excursion: Petrographic and geochemical observations from the Ediacaran Doushantuo Formation of South China SO SEDIMENTARY GEOLOGY LA English DT Article DE Phosphogenesis; Sulfate-methane transition zone; Microbial sulfate reduction; Authigenic carbonates; Shuram Excursion; C-S-P-Fe cycles ID PROTEROZOIC CYANOBACTERIAL BLOOMS; FOSSIL PRESERVATION; ATMOSPHERIC OXYGEN; PHOSPHORUS CYCLE; BIOGENIC METHANE; YANGTZE PLATFORM; EARLY EVOLUTION; TRACE FOSSIL; BLACK-SEA; OCEAN AB The Ediacaran Period witnessed one of the largest phosphogenic events in Earth's history. Coincidently, some phosphorite deposits in South China are associated with the largest-known carbon isotope negative excursion (i.e., Shuram Excursion), suggesting an intimate coupling of the biogeochemical carbon and phosphorous cycles. However, the geomicrobiological linkage between these anomalies remain poorly understood. In this study, we investigated the phosphorite samples from the uppermost Doushantuo Formation in South China. Carbon isotope compositions of authigenic calcite cements and nodules in the phosphorites are as low as -34 parts per thousand (VPDB). Petrographic and geochemical investigations indicate that the C-13-depleted carbonates likely formed as the result of microbial sulfate and iron reduction that released phosphorous from iron oxyhydroxide, concentrating phosphorous in pore waters, and thereby promoting phosphate mineralization. The timing of this event appears to coincide with enhanced sulfate delivery to seawater through continental weathering. The basin-scale distribution of Doushantuo phosphorites suggests a redox control on the availability of iron oxyhydroxide and the recycling of pore water phosphorous. Both inner and outer shelf regions were likely characterized by an oxic water column, and were the main loci for phosphogenesis; on the contrary, intra-shelf and slope regions, which are lean in phosphorite, were subjected to euxinic or ferruginous water column conditions. The intimate coupling between Ediacaran phosphogenesis and the Shuram Excursion suggests strong links among seawater redox conditions, C-S-P-Fe cycling, and fossil phosphatization. Increased microbial sulfate reduction driven by enhanced sulfate reservoir in the Ediacaran ocean may have played an essential role on these biogeochemical events. (C) 2016 Elsevier B.V. All rights reserved. C1 [Cui, Huan] Univ Wisconsin, Dept Geosci, Madison, WI 53706 USA. [Cui, Huan] Univ Wisconsin, NASA Astrobiol Inst, Madison, WI 53706 USA. [Cui, Huan; Kaufman, Alan J.; Plummer, Rebecca E.] Univ Maryland, Dept Geol, College Pk, MD 20742 USA. [Xiao, Shuhai] Virginia Tech, Dept Geosci, Blacksburg, VA 24061 USA. [Zhou, Chuanming] Chinese Acad Sci, Nanjing Inst Geol & Palaeontol, Key Lab Econ Stratig & Palaeogeog, Nanjing 210008, Jiangsu, Peoples R China. [Peng, Yongbo] Louisiana State Univ, Dept Geol & Geophys, Baton Rouge, LA 70803 USA. [Kaufman, Alan J.] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. RP Cui, H (reprint author), Univ Wisconsin, Dept Geosci, Madison, WI 53706 USA.; Cui, H (reprint author), Univ Wisconsin, NASA Astrobiol Inst, Madison, WI 53706 USA. EM Huan.Cui@Wisc.EDU RI Xiao, Shuhai/A-2190-2009; Zhou, Chuanming/E-5313-2010; OI Xiao, Shuhai/0000-0003-4655-2663; Cui, Huan/0000-0003-0705-3423 FU NASA Exobiology [NNX12AR91G, NNX15AL27G]; NSF Sedimentary Geology and Paleontology program [EAR-0844270, EAR-1528553]; Society of Economic Geologists Student Research Grant; Explorers Club Exploration Fund Grant; American Association of Petroleum Geologists; NASA Astrobiology Institute in the University of Wisconsin Madison FX We thank Mike Evans and Zhengting Wang for their assistance in the UMD Paleoclimate Co-Laboratory, and Timothy Rose for the guidance on using the Cathodoluminescence Microscope and Spectrometer in the Department of Mineral Sciences, Smithsonian Institution, Washington, DC. We also thank Drew Muscente, Xiao-Ming Liu and Zhenbing She for helpful comments. This research is supported by grants from the NASA Exobiology (NNX12AR91G to AJK and NNX15AL27G to SX), the NSF Sedimentary Geology and Paleontology program (EAR-0844270 to AJK and EAR-1528553 to SX), the Society of Economic Geologists Student Research Grant (to HC), the Explorers Club Exploration Fund Grant (to HC), and the American Association of Petroleum Geologists Grants-In-Aid Program (to HC). HC also thanks the NASA Astrobiology Institute in the University of Wisconsin Madison for support. The manuscript benefits from constructive reviews by James Schiffbauer and an anonymous reviewer. NR 121 TC 4 Z9 4 U1 13 U2 13 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0037-0738 EI 1879-0968 J9 SEDIMENT GEOL JI Sediment. Geol. PD JUL 15 PY 2016 VL 341 BP 134 EP 146 DI 10.1016/j.sedgeo.2016.05.008 PG 13 WC Geology SC Geology GA DT5RL UT WOS:000381540200009 ER PT J AU Han, JW Meyyappan, M AF Han, Jin-Woo Meyyappan, M. TI A Built-In Temperature Sensor in an Integrated Microheater SO IEEE SENSORS JOURNAL LA English DT Article DE Temperature sensing; built-in mechanism; microheater; Joule heating ID GAS SENSOR; ARRAY; FILM AB Chip-based microheaters have been widely used in many applications, including gas sensors, flow meters, mass sensors, and polymerase chain reaction chambers, where accurate monitoring of temperature is critical. The temperature measurement is conventionally done with the aid of a separate sensor, which may add to the cost and inaccuracy. In this paper, a built-in temperature sensing method is provided for the microheaters. The resistor-based microheater relies on Joule heating mechanism and its resistance is dependent upon its own body temperature, implying that the microheater has an inherent temperature sensing mechanism. It is found that an intermittent temperature sampling in the middle of the heating cycle does not disturb the body temperature if the temperature sampling voltage and pulsewidth are sufficiently low and short, respectively. The built-in temperature sensing is attributed to the electrical time constant being few orders of magnitude smaller than the thermal time constant. The temperature estimation results using the built-in method show excellent agreement with the benchmark measurements from an infrared pyrometer. C1 [Han, Jin-Woo; Meyyappan, M.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Han, JW (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM jin-woo.han@nasa.gov; m.meyyappan@nasa.gov NR 16 TC 1 Z9 1 U1 12 U2 15 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1530-437X EI 1558-1748 J9 IEEE SENS J JI IEEE Sens. J. PD JUL 15 PY 2016 VL 16 IS 14 BP 5543 EP 5547 DI 10.1109/JSEN.2016.2569445 PG 5 WC Engineering, Electrical & Electronic; Instruments & Instrumentation; Physics, Applied SC Engineering; Instruments & Instrumentation; Physics GA DR0MM UT WOS:000379601600007 ER PT J AU Sobel, AH Camargo, SJ Hall, TM Lee, CY Tippett, MK Wing, AA AF Sobel, Adam H. Camargo, Suzana J. Hall, Timothy M. Lee, Chia-Ying Tippett, Michael K. Wing, Allison A. TI Human influence on tropical cyclone intensity SO SCIENCE LA English DT Review ID GENESIS POTENTIAL INDEX; SEA-SURFACE TEMPERATURE; GLOBAL CLIMATE-CHANGE; HURRICANE ACTIVITY; MAXIMUM INTENSITY; REANALYSIS DATA; FUTURE CHANGES; CMIP5 MODELS; VARIABILITY; TRENDS AB Recent assessments agree that tropical cyclone intensity should increase as the climate warms. Less agreement exists on the detection of recent historical trends in tropical cyclone intensity. We interpret future and recent historical trends by using the theory of potential intensity, which predicts the maximum intensity achievable by a tropical cyclone in a given local environment. Although greenhouse gas-driven warming increases potential intensity, climate model simulations suggest that aerosol cooling has largely canceled that effect over the historical record. Large natural variability complicates analysis of trends, as do poleward shifts in the latitude of maximum intensity. In the absence of strong reductions in greenhouse gas emissions, future greenhouse gas forcing of potential intensity will increasingly dominate over aerosol forcing, leading to substantially larger increases in tropical cyclone intensities. C1 [Sobel, Adam H.; Tippett, Michael K.] Columbia Univ, Dept Appl Phys & Appl Math, New York, NY 10027 USA. [Sobel, Adam H.; Camargo, Suzana J.; Wing, Allison A.] Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY 10964 USA. [Hall, Timothy M.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Lee, Chia-Ying] Columbia Univ, Int Res Inst Climate & Soc, Palisades, NY 10964 USA. [Tippett, Michael K.] King Abdulaziz Univ, Dept Meteorol, Ctr Excellence Climate Res, Jeddah, Saudi Arabia. RP Sobel, AH (reprint author), Columbia Univ, Dept Appl Phys & Appl Math, New York, NY 10027 USA.; Sobel, AH (reprint author), Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY 10964 USA. EM ahs129@columbia.edu RI Camargo, Suzana/C-6106-2009; Sobel, Adam/K-4014-2015; Tippett, Michael/C-6286-2011; OI Camargo, Suzana/0000-0002-0802-5160; Sobel, Adam/0000-0003-3602-0567; Tippett, Michael/0000-0002-7790-5364; Wing, Allison/0000-0003-2194-8709 FU NSF [AGS-1143959]; Office of Naval Research [N00014-16-1-2073]; NSF Atmospheric and Geospace Sciences postdoctoral research fellowship [1433251] FX A.H.S. thanks J. Kossin, G. Vecchi, and K. Emanuel for helpful discussions. This work was supported by NSF grant AGS-1143959 and Office of Naval Research grant N00014-16-1-2073. A.A.W. is supported by a NSF Atmospheric and Geospace Sciences postdoctoral research fellowship under award no. 1433251. NR 83 TC 4 Z9 4 U1 41 U2 73 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 EI 1095-9203 J9 SCIENCE JI Science PD JUL 15 PY 2016 VL 353 IS 6296 BP 242 EP 246 DI 10.1126/science.aaf6574 PG 5 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA DR0EM UT WOS:000379580800038 PM 27418502 ER PT J AU Kulkarni, C Peteet, D Boger, R Heusser, L AF Kulkarni, Charuta Peteet, Dorothy Boger, Rebecca Heusser, Linda TI Exploring the role of humans and climate over the Balkan landscape: 500 years of vegetational history of Serbia SO QUATERNARY SCIENCE REVIEWS LA English DT Article DE Little Ice Age; Paleoecology; Human-environmental interactions; Serbia; Central Balkans ID TREE-RING WIDTHS; PALYNOLOGICAL RICHNESS; LAND-USE; FLORISTIC DIVERSITY; LAST MILLENNIUM; PLANT DIVERSITY; POLLEN ANALYSIS; EASTERN EUROPE; FOSSIL POLLEN; HUMAN IMPACT AB We present the first, well-dated, high-resolution record of vegetation and landscape change from Serbia, which spans the past 500 years. Biological proxies (pollen, spores, and charcoal), geochemical analysis through X-ray Fluorescence (XRF), and a detailed chronology based on AMS C-14 dating from a western Serbian sinkhole core suggest complex woodland-grassland dynamics and strong erosional signals throughout the Little Ice Age (LIA). An open landscape with prominent steppe vegetation (e.g. Poaceae, Chenopodiaceae) and minor woodland exists during 1540-1720 CE (early LIA), while the late LIA (1720-1850 CE) in this record shows higher tree percentages possibly due to increased moisture availability. The post LIA Era (1850-2012 CE) brings a disturbed type of vegetation with the presence of weedy genera and an increase in regional woodland. Anthropogenic indicators for agricultural, pastoral and fire practices in the region together attest to the dominant role of humans in shaping this Balkan landscape throughout the interval. The changing nature of human interference, potentially as a response to underlying climatic transitions, is evident through large-scale soil depletion resulting from grazing and land clearance during the early LIA and stabilization of arable lands during the late and post-LIA eras. (C) 2016 Elsevier Ltd. All rights reserved. C1 [Kulkarni, Charuta; Boger, Rebecca] CUNY, Grad Ctr, Dept Earth & Environm Sci, 365 Fifth Ave, New York, NY 10016 USA. [Peteet, Dorothy] NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA. [Peteet, Dorothy; Heusser, Linda] Lamont Doherty Earth Observ, 61 Rte 9W, Palisades, NY 10964 USA. [Boger, Rebecca] CUNY Brooklyn Coll, Dept Earth & Environm Sci, 2900 Bedford Ave, Brooklyn, NY 11210 USA. RP Kulkarni, C (reprint author), CUNY, Grad Ctr, Dept Earth & Environm Sci, 365 Fifth Ave, New York, NY 10016 USA. EM ckulkarni@gradcenter.cuny.edu OI Kulkarni, Charuta/0000-0002-4952-7765 FU PSC CUNY [66575-00-44] FX This research is funded by PSC CUNY Grant No. 66575-00-44. The authors are grateful to Dr. Branko Sikoparia and Dr. Predrag Radisic from the Laboratory of Palynology, University of Novi Sad, Serbia for providing necessary reference pollen slides. We also thank Mr. Marko Rucando and Ms. Tamara Dukic for their help in collecting detailed information on local vegetation. Special thanks to Dr. Jonathan Nichols for his insights into the age-depth modelling in this study. We are also grateful to the two anonymous reviewers and the editor, Dr. Jose S Carrion for constructive suggestions on earlier versions of the manuscript. This is LDEO contribution no. 8017. NR 119 TC 0 Z9 0 U1 10 U2 16 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0277-3791 J9 QUATERNARY SCI REV JI Quat. Sci. Rev. PD JUL 15 PY 2016 VL 144 BP 83 EP 94 DI 10.1016/j.quascirev.2016.05.021 PG 12 WC Geography, Physical; Geosciences, Multidisciplinary SC Physical Geography; Geology GA DQ3LW UT WOS:000379104800007 ER PT J AU Gupta, RK Pandya, R Sieffert, T Meyyappan, M Koehne, JE AF Gupta, Rakesh K. Pandya, Ruchi Sieffert, Theodore Meyyappan, M. Koehne, Jessica E. TI Multiplexed electrochemical immunosensor for label-free detection of cardiac markers using a carbon nanofiber array chip SO JOURNAL OF ELECTROANALYTICAL CHEMISTRY LA English DT Article DE Biosensors; Vertically aligned carbon nanofibers; Cardiac proteins; Nanoelectrode array; Differential pulse voltammetry; Electrochemical multianalyte immunosensor ID C-REACTIVE PROTEIN; ACUTE MYOCARDIAL-INFARCTION; ACUTE CORONARY SYNDROMES; CREATINE-KINASE-MB; TROPONIN-I; NANOELECTRODE ARRAYS; RISK STRATIFICATION; NATRIURETIC PEPTIDE; HUMAN SERUM; BIOMARKERS AB We present an electrochemical multianalyte or multiplexed immunosensor for simultaneous label free detection of cardiac markers panel, comprising of C-reactive protein, cardiac troponin-I and myoglobin. The multi electrode biosensor chip contains nine identical but electrically isolated microelectrodes arranged in a 3 x 3 array configuration. Each electrode contains carbon nanofiber nanoelectrodes grown vertically using plasma enhanced chemical vapor deposition. A hydrophobic photoresist layer, lithographically etched on the chip, exposes the electrodes and helps to selectively immobilize the antibody probes for the three target cardiac biomarkers using carbodiimide chemistry. The real-time label free detection of the three cardiac markers from a mixture is demonstrated with high sensitivity and selectivity. Detection in complex protein mixtures in human blood serum does not show any false positives from non-specific protein adsorption. The results show that the present sensor can serve as a miniaturized, low cost lab-on-a-chip system for the detection of various biomarkers in healthcare, environmental monitoring and security applications. Published by Elsevier B.V. C1 [Gupta, Rakesh K.; Pandya, Ruchi; Sieffert, Theodore; Meyyappan, M.; Koehne, Jessica E.] NASA, Ames Res Ctr, Ctr Nanotechnol, Moffett Field, CA 94035 USA. [Gupta, Rakesh K.] Univ Manchester, Manchester M13 9PL, Lancs, England. RP Koehne, JE (reprint author), NASA, Ames Res Ctr, Ctr Nanotechnol, Moffett Field, CA 94035 USA. EM Jessica.e.koehne@nasa.gov FU J&K Council for Science and Technology, Department of Higher Education, JK, India; University Grants Commission (UGC), New-Delhi, India FX JK acknowledges a Presidential Early Career Award. RKG acknowledges the financial support from the J&K Council for Science and Technology, Department of Higher Education, J&K, India and University Grants Commission (UGC), New-Delhi, India. TS was a graduate student intern from the Purdue University, School of Aeronautics and Astronautics and RP was a high school student intern from Lynbrook High School, San Jose, CA. NR 48 TC 0 Z9 0 U1 21 U2 37 PU ELSEVIER SCIENCE SA PI LAUSANNE PA PO BOX 564, 1001 LAUSANNE, SWITZERLAND SN 1572-6657 EI 1873-2569 J9 J ELECTROANAL CHEM JI J. Electroanal. Chem. PD JUL 15 PY 2016 VL 773 BP 53 EP 62 DI 10.1016/j.jelechem.2016.04.034 PG 10 WC Chemistry, Analytical; Electrochemistry SC Chemistry; Electrochemistry GA DP4JY UT WOS:000378463400008 ER PT J AU Schmitt, MP Harder, BJ Wolfe, DE AF Schmitt, Michael P. Harder, Bryan J. Wolfe, Douglas E. TI Process-structure-property relations for the erosion durability of plasma spray-physical vapor deposition (PS-PVD) thermal barrier coatings SO SURFACE & COATINGS TECHNOLOGY LA English DT Article DE Thermal barrier coatings; Erosion; Low k; Rare earth; PS-PVD; TBC ID YTTRIA-STABILIZED ZIRCONIA; MECHANICAL-PROPERTIES; TBC MORPHOLOGY; CONDUCTIVITY; ARCHITECTURES; INFILTRATION; DEGRADATION; SYSTEMS AB New thermal barrier coating (TBC) materials and microstructures are under development to increase gas turbine operating temperatures beyond the similar to 1200 degrees C threshold of standard 7 wt% yttria stabilized zirconia (7YSZ). To deposit these advanced coatings, a new thermal spray deposition technique is used: Plasma Spray - Physical Vapor Deposition (PS-PVD). PS-PVD is capable of depositing from the vapor phase to yield strain tolerant columnar microstructures similar to Electron Beam - Physical Vapor Deposition (EB-PVD) or, alternatively, the traditional splat-like lamellar microstructure common to Air Plasma Spray (APS). This study investigates the process-structure relationships and resulting erosion response for plasma gas flow, amperage, and feed rate. It was found that in the selected design space, porosity and surface roughness vary from similar to 12-26% and similar to 5-10 mu m, respectively. Erosion behavior is discussed and the mechanism is identified to be heavily dependent upon the intercolumnar spacing. The lowest erosion rates are similar to EB-PVD, while the highest erosion rates were closer to APS. This is attributed to the hybrid nature of the PS-PVD process and provides an opportunity to tailor coatings with a wide range of properties, and thus performance. Published by Elsevier B.V. C1 [Schmitt, Michael P.; Wolfe, Douglas E.] Penn State Univ, Dept Mat Sci & Engn, University Pk, PA 16802 USA. [Schmitt, Michael P.; Wolfe, Douglas E.] Penn State Univ, Appl Res Lab, University Pk, PA 16802 USA. [Schmitt, Michael P.; Harder, Bryan J.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. [Wolfe, Douglas E.] Penn State Univ, Dept Engn Sci & Mech, 227 Hammond Bldg, University Pk, PA 16802 USA. RP Harder, BJ (reprint author), NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. EM bryan.harder@nasa.gov FU NASA Graduate Student Researchers Program (GSRP) [NNX11AL02H]; Applied Resarch Lab (ARL)-Walker Fellowship program FX The authors would like to thank Dr. Rick Rogers and Dr. Brian Good for their thoughtful discussion. This work was supported under the NASA Graduate Student Researchers Program (GSRP) award No. NNX11AL02H and the Applied Resarch Lab (ARL)-Walker Fellowship program. The opinions and views expressed are those of the authors and do not necessarily reflect NASA or the US Navy. NR 35 TC 3 Z9 3 U1 18 U2 35 PU ELSEVIER SCIENCE SA PI LAUSANNE PA PO BOX 564, 1001 LAUSANNE, SWITZERLAND SN 0257-8972 J9 SURF COAT TECH JI Surf. Coat. Technol. PD JUL 15 PY 2016 VL 297 BP 11 EP 18 DI 10.1016/j.surfcoat.2016.04.029 PG 8 WC Materials Science, Coatings & Films; Physics, Applied SC Materials Science; Physics GA DO5JS UT WOS:000377820000002 ER PT J AU Keller, JW Gaddis, L Petro, NE AF Keller, John W. Gaddis, Lisa Petro, Noah E. TI Untitled SO ICARUS LA English DT Editorial Material C1 [Keller, John W.; Petro, Noah E.] NASA, Goddard Space Flight Ctr, Washington, DC 20010 USA. [Gaddis, Lisa] USGS, Astrogeol Sci Ctr, San Francisco, CA USA. RP Keller, JW (reprint author), NASA, Goddard Space Flight Ctr, Washington, DC 20010 USA. NR 2 TC 0 Z9 0 U1 0 U2 0 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD JUL 15 PY 2016 VL 273 SI SI BP 1 EP 1 DI 10.1016/j.icarus.2016.04.016 PG 1 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DL6FK UT WOS:000375734900001 ER PT J AU Keller, JW Petro, NE Vondrak, RR AF Keller, J. W. Petro, N. E. Vondrak, R. R. CA LRO Team TI The Lunar Reconnaissance Orbiter Mission - Six years of science and exploration at the Moon SO ICARUS LA English DT Article DE Moon; Moon, surface; Geological processes ID ALTIMETER LOLA DATA; LASER ALTIMETER; SOUTH-POLE; NEUTRON DETECTOR; RADIOMETER OBSERVATIONS; RADIATION ENVIRONMENT; COHERENT BACKSCATTER; COMPTON-BELKOVICH; SHACKLETON CRATER; SILICIC VOLCANISM AB Since entering lunar orbit on June 23, 2009 the Lunar Reconnaissance Orbiter (LRO) has made comprehensive measurements of the Moon and its environment. The seven LRO instruments use a variety of primarily remote sensing techniques to obtain a unique set of observations. These measurements provide new information regarding the physical properties of the lunar surface, the lunar environment, and the location of volatiles and other resources. Scientific interpretation of these observations improves our understanding of the geologic history of the Moon, its current state, and what its history can tell us about the evolution of the Solar System. Scientific results from LRO observations overturned existing paradigms and deepened our appreciation of the complex nature of our nearest neighbor. This paper summarizes the capabilities, measurements, and some of the science and exploration results of the first six years of the LRO mission. Published by Elsevier Inc. C1 [Keller, J. W.; Petro, N. E.; Vondrak, R. R.; LRO Team] NASA, Goddard Space Flight Ctr, Code 691,8800 Greenbelt Rd, Greenbelt, MD 20771 USA. RP Keller, JW (reprint author), NASA, Goddard Space Flight Ctr, Code 691,8800 Greenbelt Rd, Greenbelt, MD 20771 USA. EM John.W.Keller@nasa.gov NR 161 TC 3 Z9 3 U1 4 U2 14 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD JUL 15 PY 2016 VL 273 SI SI BP 2 EP 24 DI 10.1016/j.icarus.2015.11.024 PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DL6FK UT WOS:000375734900002 ER PT J AU Schwadron, NA Wilson, JK Looper, MD Jordan, AP Spence, HE Blake, JB Case, AW Iwata, Y Kasper, JC Farrell, WM Lawrence, DJ Livadiotis, G Mazur, J Petro, N Pieters, C Robinson, MS Smith, S Townsend, LW Zeitlin, C AF Schwadron, N. A. Wilson, J. K. Looper, M. D. Jordan, A. P. Spence, H. E. Blake, J. B. Case, A. W. Iwata, Y. Kasper, J. C. Farrell, W. M. Lawrence, D. J. Livadiotis, G. Mazur, J. Petro, N. Pieters, C. Robinson, M. S. Smith, S. Townsend, L. W. Zeitlin, C. TI Signatures of volatiles in the lunar proton albedo SO ICARUS LA English DT Article DE Moon, surface; Cosmic rays; Ices; Moon ID PROSPECTOR GAMMA-RAY; NEUTRON SPECTROMETERS; SPATIAL-DISTRIBUTION; EPITHERMAL NEUTRONS; WATER ICE; MOON; SURFACE; RADIATION; POLES AB We find evidence for hydrated material in the lunar regolith using "albedo protons" measured with the Cosmic Ray Telescope for the Effects of Radiation (CRaTER) on the Lunar Reconnaissance Orbiter (LRO). Fluxes of these albedo protons, which are emitted from the regolith due to steady bombardment by high energy radiation (Galactic Cosmic Rays), are observed to peak near the poles, and are inconsistent with the latitude trends of heavy element enrichment (e.g., enhanced Fe abundance). The latitudinal distribution of albedo protons anti-correlates with that of epithermal or high energy neutrons. The high latitude enhancement may be due to the conversion of upward directed secondary neutrons from the lunar regolith into tertiary protons due to neutron-proton collisions in hydrated regolith that is more prevalent near the poles. The CRaTER instrument may thus provide important measurements of volatile distributions within regolith at the Moon and potentially, with similar sensors and observations, at other bodies within the Solar System. (C) 2016 Published by Elsevier Inc. C1 [Schwadron, N. A.; Wilson, J. K.; Jordan, A. P.; Spence, H. E.; Smith, S.] Univ New Hampshire, Ctr Space Sci, Morse Hall,8 Coll Rd, Durham, NH 03824 USA. [Schwadron, N. A.; Wilson, J. K.; Jordan, A. P.; Spence, H. E.; Smith, S.] Univ New Hampshire, Inst Earth Oceans & Space, Morse Hall,8 Coll Rd, Durham, NH 03824 USA. [Looper, M. D.; Blake, J. B.; Mazur, J.] Aerosp Corp, El Segundo, CA 90245 USA. [Case, A. W.; Kasper, J. C.] Harvard Smithsonian Ctr Astrophys, Div High Energy Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Kasper, J. C.] Univ Michigan, Dept Climate & Space Sci & Engn, Ann Arbor, MI 48109 USA. [Iwata, Y.] NIRS, Inage Ku, 4-9-1 Anagawa, Chiba 2638555, Japan. [Lawrence, D. J.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Farrell, W. M.; Petro, N.] Goddard Space Flight Ctr, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA. [Pieters, C.] Brown Univ, Planetary Geosciences Grp, Dept Earth Environm & Planetary Sci, 324 Brook St, Providence, RI 02912 USA. [Robinson, M. S.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [Townsend, L. W.] Univ Tennessee, Knoxville, TN 37996 USA. [Livadiotis, G.; Zeitlin, C.] Univ New Hampshire, SW Res Inst, Earth Oceans & Space Sci, Durham, NH 03824 USA. RP Schwadron, NA (reprint author), Univ New Hampshire, Ctr Space Sci, Morse Hall,8 Coll Rd, Durham, NH 03824 USA.; Schwadron, NA (reprint author), Univ New Hampshire, Inst Earth Oceans & Space, Morse Hall,8 Coll Rd, Durham, NH 03824 USA. RI Farrell, William/I-4865-2013 FU LRO program [NNG11PA03C]; SSERVI; DREAM2 (NASA) [NNX14AG13A] FX We thank all those who made CRaTER possible. CRaTER is primarily funded by the LRO program (contract NNG11PA03C). This work was also funded by SSERVI and DREAM2 (NASA Grant NNX14AG13A). CRaTER data are available at http://crater-web.sr.unh.edu. NR 42 TC 0 Z9 0 U1 6 U2 14 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD JUL 15 PY 2016 VL 273 SI SI BP 25 EP 35 DI 10.1016/j.icarus.2015.12.003 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DL6FK UT WOS:000375734900003 ER PT J AU Hurley, DM Cook, JC Benna, M Halekas, JS Feldman, PD Retherford, KD Hodges, RR Grava, C Mahaffy, P Gladstone, GR Greathouse, T Kaufmann, DE Elphic, RC Stern, SA AF Hurley, Dana M. Cook, Jason C. Benna, Mehdi Halekas, Jasper S. Feldman, Paul D. Retherford, Kurt D. Hodges, R. Richard Grava, Cesare Mahaffy, Paul Gladstone, G. Randall Greathouse, Thomas Kaufmann, David E. Elphic, Richard C. Stern, S. Alan TI Understanding temporal and spatial variability of the lunar helium atmosphere using simultaneous observations from LRO, LADEE, and ARTEMIS SO ICARUS LA English DT Article DE Moon; Atmospheres, evolution; Spectroscopy; Solar wind ID SOLAR-WIND; MERCURY; MOON; INSTRUMENT; HYDROGEN; MISSION; ARGON; LAMP AB Simultaneous measurements of helium in the exosphere of the Moon are made from the Lunar Reconnaissance Orbiter (LRO) Lyman Alpha Mapping Project (LAMP) and the Lunar Atmosphere and Dust Environment Explorer (LADEE) Neutral Mass Spectrometer (NMS) through the entire 5-month span of the LADEE mission. In addition, the ARTEMIS mission monitored the solar wind alpha particle flux to the Moon. Modeling the lunar helium exosphere, we relate the LAMP polar observations to the LADEE equatorial observations. Further, using the ARTEMIS alpha flux in the Monte Carlo model reproduces the temporal variations in helium density. Comparing the LAMP data to the LADEE data shows excellent agreement. Comparing those with the ARTEMIS data reveals that the solar wind alpha flux is the primary driver to variability in the helium exosphere throughout the LADEE mission. Using a decay time for exospheric helium of 5 days, we determine that the solar wind contributes 64 +/- 5% of the helium to the lunar exosphere. The remaining 36 +/- 5% is presumed to come from outgassing of radiogenic helium from the interior of the Moon. Furthermore, the model reproduces the measurements if 63 +/- 6% of the incident alpha particles are converted to thermalized helium atoms through the interaction between the alphas and the lunar surface. However, these values are dependent on both inferred source rates from LAMP and LADEE observations and on the assumed time constant of the exospheric decay rate. (C) 2015 Elsevier Inc. All rights reserved. C1 [Hurley, Dana M.] Johns Hopkins Univ, Appl Phys Lab, Johns Hopkins Rd, Laurel, MD 20723 USA. [Cook, Jason C.; Stern, S. Alan] SW Res Inst, Boulder, CO 80302 USA. [Benna, Mehdi; Mahaffy, Paul] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Halekas, Jasper S.] Univ Iowa, Iowa City, IA 52242 USA. [Feldman, Paul D.] Johns Hopkins Univ, Baltimore, MD 21218 USA. [Retherford, Kurt D.; Grava, Cesare; Gladstone, G. Randall; Greathouse, Thomas] SW Res Inst, 6220 Culebra Rd, San Antonio, TX 78228 USA. [Hodges, R. Richard] Univ Colorado, Boulder, CO 80303 USA. [Elphic, Richard C.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Hurley, DM (reprint author), Johns Hopkins Univ, Appl Phys Lab, Johns Hopkins Rd, Laurel, MD 20723 USA. RI Hurley, Dana/F-4488-2015; OI Hurley, Dana/0000-0003-1052-1494; Halekas, Jasper/0000-0001-5258-6128 FU NASA through the LADEE mission; NASA through LADEE Guest Investigator Program [NNX13AO70G]; NASA through LRO LAMP mission [NNG05EC87C]; NASA through ARTEMIS mission FX We acknowledge NASA for support through the LADEE mission, LADEE Guest Investigator Program (NNX13AO70G), LRO LAMP mission (NNG05EC87C), and ARTEMIS mission. We are grateful to the many operations folks involved in all three of these mission teams that helped facilitate our campaigns to coordinate investigations during the LADEE era. NR 29 TC 0 Z9 0 U1 6 U2 8 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD JUL 15 PY 2016 VL 273 SI SI BP 45 EP 52 DI 10.1016/j.icarus.2015.09.011 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DL6FK UT WOS:000375734900005 ER PT J AU Barker, MK Sun, X Mazarico, E Neumann, GA Zuber, MT Smith, DE AF Barker, M. K. Sun, X. Mazarico, E. Neumann, G. A. Zuber, M. T. Smith, D. E. TI Lunar phase function at 1064 nm from Lunar Orbiter Laser Altimeter passive and active radiometry SO ICARUS LA English DT Article DE Photometry; Moon; surface; Regoliths ID BIDIRECTIONAL REFLECTANCE SPECTROSCOPY; PHOTOMETRIC PROPERTIES; MAGNETIC-ANOMALIES; CLEMENTINE DATA; ONE MOON; SURFACE; REGOLITH; MISSION; ALBEDO; MODEL AB We present initial calibration and results of passive radiometry collected by the Lunar Orbiter Laser Altimeter onboard the Lunar Reconnaissance Orbiter over the course of 12 months. After correcting for time- and temperature-dependent dark noise and detector responsivity variations, the LOLA passive radiometry measurements are brought onto the absolute radiance scale of the SELENE Spectral Profiler. The resulting photometric precision is estimated to be similar to 5%. We leverage the unique ability of LOLA to measure normal albedo to explore the 1064 nm phase function's dependence on various geologic parameters. On a global scale, we find that iron abundance and optical maturity (quantified by FeO and OMAT) are the dominant controlling parameters. Titanium abundance (TiO2), surface roughness on decimeter to decameter scales, and soil thermophysical properties have a smaller effect, but the latter two are correlated with GMAT, indicating that exposure age is the driving force behind their effects in a globally-averaged sense. The phase function also exhibits a dependence on surface slope at 300 m baselines, possibly the result of mass wasting exposing immature material and/or less space weathering due to reduced sky visibility. Modeling the photometric function in the Hapke framework, we find that, relative to the highlands, the maria exhibit decreased backscattering, a smaller opposition effect (GE) width, and a smaller OE amplitude. Immature highlands regolith has a higher backscattering fraction and a larger OE width compared to mature highlands regolith. Within the maria, the backscattering fraction and OE width show little dependence on TiO2 and GMAT. Variations in the phase function shape at large phase angles are observed in and around the Copernican-aged Jackson crater, including its dark halo, a putative impact melt deposit. Finally, the phase function of the Reiner Gamma Formation behaves more optically immature than is typical for its composition and GMAT, suggesting the visible-to-near-infrared spectrum and phase function respond differently to the unusual regolith evolution and properties at this location. (C) 2016 Elsevier Inc. All rights reserved. C1 [Barker, M. K.] Sigma Space Corp, 4600 Forbes Blvd, Lanham, MD 20706 USA. [Sun, X.; Mazarico, E.; Neumann, G. A.] Goddard Space Flight Ctr, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA. [Zuber, M. T.; Smith, D. E.] MIT, Deptartment Earth Atmospher & Planetary Sci, 77 Massachusetts Ave, Cambridge, MA 02139 USA. RP Barker, MK (reprint author), Sigma Space Corp, 4600 Forbes Blvd, Lanham, MD 20706 USA. EM michael.k.barker@nasa.gov RI Neumann, Gregory/I-5591-2013; Mazarico, Erwan/N-6034-2014 OI Neumann, Gregory/0000-0003-0644-9944; Mazarico, Erwan/0000-0003-3456-427X NR 74 TC 1 Z9 1 U1 1 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 EI 1090-2643 J9 ICARUS JI Icarus PD JUL 15 PY 2016 VL 273 SI SI BP 96 EP 113 DI 10.1016/j.icarus.2016.02.008 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DL6FK UT WOS:000375734900010 ER PT J AU Baker, DMH Head, JW Collins, GS Potter, RWK AF Baker, David M. H. Head, James W. Collins, Gareth S. Potter, Ross W. K. TI The formation of peak-ring basins: Working hypotheses and path forward in using observations to constrain models of impact-basin formation SO ICARUS LA English DT Article DE Moon; Moon, surface; Impact processes; Cratering ID COMPLEX CRATER FORMATION; LUNAR MASCON BASINS; SCHRODINGER-BASIN; ACOUSTIC FLUIDIZATION; CHICXULUB CRATER; MOON; ORIGIN; MELT; CRUST; SIMULATIONS AB Impact basins provide windows into the crustal structure and stratigraphy of planetary bodies; however, interpreting the stratigraphic origin of basin materials requires an understanding of the processes controlling basin formation and morphology. Peak-ring basins (exhibiting a rim crest and single interior ring of peaks) provide important insight into the basin-formation process, as they are transitional between complex craters with central peaks and larger multi-ring basins. New image and altimetry data from the Lunar Reconnaissance Orbiter as well as a suite of remote sensing datasets have permitted a reassessment of the origin of lunar peak-ring basins. We synthesize morphometric, spectroscopic, and gravity observations of lunar peak-ring basins and describe two working hypotheses for the formation of peak rings that involve interactions between inward collapsing walls of the transient cavity and large central uplifts of the crust and mantle. Major facets of our observations are then compared and discussed in the context of numerical simulations of peak-ring basin formation in order to plot a course for future model refinement and development. (C) 2015 Elsevier Inc. All rights reserved. C1 [Baker, David M. H.; Head, James W.; Potter, Ross W. K.] Brown Univ, Dept Earth Environm & Planetary Sci, Providence, RI 02912 USA. [Baker, David M. H.] NASA, Goddard Space Flight Ctr, 8800 Greenbelt Rd,Code 698, Greenbelt, MD 20771 USA. [Collins, Gareth S.] Univ London Imperial Coll Sci Technol & Med, Dept Earth Sci & Engn, London, England. RP Baker, DMH (reprint author), NASA, Goddard Space Flight Ctr, 8800 Greenbelt Rd,Code 698, Greenbelt, MD 20771 USA. EM david.m.hollibaughbaker@nasa.gov OI Collins, Gareth/0000-0002-6087-6149 FU NASA Lunar Reconnaissance Orbiter (LRO) Mission, Lunar Orbiter Laser Altimeter (LOLA) Experiment Team [NNX11AK29G, NNX13AO77G]; NASA Gravity Recovery and Interior Laboratory (GRAIL) Mission Guest Scientist Program [NNX12AL07G]; NASA Solar System Exploration Research Virtual Institute (SSERVI) grant for Evolution and Environment of Exploration Destinations [NNA14AB01A]; Science and Facilities Research Council (STFC) [ST/J001260/1] FX Thank you to an anonymous reviewer and to Mark Cintala for their comprehensive reviews that greatly improved the quality of the manuscript. We gratefully acknowledge financial support from the NASA Lunar Reconnaissance Orbiter (LRO) Mission, Lunar Orbiter Laser Altimeter (LOLA) Experiment Team (Grants NNX11AK29G and NNX13AO77G), the NASA Gravity Recovery and Interior Laboratory (GRAIL) Mission Guest Scientist Program (Grant NNX12AL07G) and the NASA Solar System Exploration Research Virtual Institute (SSERVI) grant for Evolution and Environment of Exploration Destinations under cooperative agreement number NNA14AB01A at Brown University. We gratefully acknowledge the developers of the iSALE shock physics code (www.isale-code.de). GSC was funded by Science and Facilities Research Council (STFC) grant ST/J001260/1. NR 116 TC 5 Z9 5 U1 6 U2 11 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD JUL 15 PY 2016 VL 273 SI SI BP 146 EP 163 DI 10.1016/j.icarus.2015.11.033 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DL6FK UT WOS:000375734900014 ER PT J AU Ghent, RR Carter, LM Bandfield, JL Udovicic, CJT Campbell, BA AF Ghent, R. R. Carter, L. M. Bandfield, J. L. Udovicic, C. J. Tai Campbell, B. A. TI Lunar crater ejecta: Physical properties revealed by radar and thermal infrared observations SO ICARUS LA English DT Article DE Moon; Regoliths; Radar observations; Infrared observations; Cratering ID IMPACT CRATERS; 70-CM WAVELENGTH; MOON; AGES; CONSTRAINTS; REGOLITH; DEPOSITS; BASIN; MARS AB We investigate the physical properties, and changes through time, of lunar impact ejecta using radar and thermal infrared data. We use data from two instruments on the Lunar Reconnaissance Orbiter (LRO) - the Diviner thermal radiometer and the Miniature Radio Frequency (Mini-RF) radar instrument - together with Earth-based radar observations. We use this multiwavelength intercomparison to constrain block sizes and to distinguish surface from buried rocks in proximal ejecta deposits. We find that radar detectable rocks buried within the upper meter of regolith can remain undisturbed by surface processes such as micrometeorite bombardment for >3 Gyr. We also investigate the thermophysical properties of radar-dark haloes, comprised of fine-grained, rock-poor ejecta distal to the blocky proximal ejecta. Using Diviner data, we confirm that the halo material is depleted in surface rocks, but show that it is otherwise thermophysically indistinct from background regolith. We also find that radar-dark haloes, like the blocky ejecta, remain visible in radar observations for craters with ages >3 Ga, indicating that regolith overturn processes cannot replenish their block populations on that timescale. (C) 2015 Elsevier Inc. All rights reserved. C1 [Ghent, R. R.; Udovicic, C. J. Tai] Univ Toronto, Dept Earth Sci, 22 Russell St, Toronto, ON M5S 3B1, Canada. [Ghent, R. R.] Planetary Sci Inst, Tucson, AZ 85719 USA. [Carter, L. M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Bandfield, J. L.] Space Sci Inst, Boulder, CO 80301 USA. [Campbell, B. A.] Smithsonian Inst, Ctr Earth & Planetary Studies, Washington, DC 20013 USA. RP Ghent, RR (reprint author), Univ Toronto, Dept Earth Sci, 22 Russell St, Toronto, ON M5S 3B1, Canada. RI Carter, Lynn/D-2937-2012 NR 53 TC 2 Z9 2 U1 5 U2 9 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD JUL 15 PY 2016 VL 273 SI SI BP 182 EP 195 DI 10.1016/j.icarus.2015.12.014 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DL6FK UT WOS:000375734900016 ER PT J AU Greenhagen, BT Neish, CD Williams, JP Cahill, JTS Ghent, RR Hayne, PO Lawrence, SJ Petro, NE Bandfield, JL AF Greenhagen, Benjamin T. Neish, Catherine D. Williams, Jean-Pierre Cahill, Joshua T. S. Ghent, Rebecca R. Hayne, Paul O. Lawrence, Samuel J. Petro, Noah E. Bandfield, Joshua L. TI Origin of the anomalously rocky appearance of Tsiolkovskiy crater SO ICARUS LA English DT Article DE Moon, surface; Cratering; Impact processes; Geological processes; Regoliths ID LUNAR FARSIDE; GIORDANO BRUNO; IMPACT MELT; AGE; FLOWS; MOON; MARE AB Rock abundance maps derived from the Diviner Lunar Radiometer instrument on the Lunar Reconnaissance Orbiter (LRO) show Tsiolkovskiy crater to have high surface rock abundance and relatively low regolith thickness. The location of the enhanced rock abundance to the southeast of the crater is consistent with a massive, well-preserved impact melt deposit apparent in LRO Miniature Radio Frequency instrument circular polarization ratio data. A new model crater age using LRO Lunar Reconnaissance Orbiter Camera imagery suggests that while it originated in the Late Imbrian, Tsiolkovskiy may be the youngest lunar crater of its size (similar to 180 km diameter). Together these data show that Tsiolkovskiy has a unique surface rock population and regolith properties for a crater of its size and age. Explanation of these observations requires mechanisms that produce more large blocks, preserve boulders and large blocks from degradation to regolith, and/or uncover buried rocks. These processes have important implications for formation of regolith on the Moon. (C) 2016 Elsevier Inc. All rights reserved. C1 [Greenhagen, Benjamin T.; Cahill, Joshua T. S.] Johns Hopkins Univ, Appl Phys Lab, 11100 Johns Hopkins Rd, Laurel, MD 20723 USA. [Neish, Catherine D.] Univ Western Ontario, Dept Earth Sci, Biol & Geol Sci Bldg,Room 1026 1151 Richmond St N, London, ON N6A 5B7, Canada. [Williams, Jean-Pierre] Univ Calif Los Angeles, Dept Earth Planetary & Space Sci, 595 Charles Young Dr East,Box 951567, Los Angeles, CA 90095 USA. [Ghent, Rebecca R.] Ctr Earth Sci, Dept Earth Sci, 22 Russell St, Toronto, ON M5S 3B1, Canada. [Ghent, Rebecca R.] Planetary Sci Inst, 1700 East Ft Lowell,Suite 106, Tucson, AZ 85719 USA. [Hayne, Paul O.] CALTECH, Jet Prop Lab, ASU, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Lawrence, Samuel J.] Sch Earth & Space Explorat, POB 871404, Tempe, AZ 85287 USA. [Petro, Noah E.] NASA, Goddard Space Flight Ctr, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA. [Bandfield, Joshua L.] Space Sci Inst, 4750 Walnut St,Suite 205, Boulder, CO 80301 USA. RP Greenhagen, BT (reprint author), Johns Hopkins Univ, Appl Phys Lab, 11100 Johns Hopkins Rd, Laurel, MD 20723 USA. EM benjamin.greenhagen@jhuapl.edu RI Williams, Jean-Pierre/C-3531-2009 OI Williams, Jean-Pierre/0000-0003-4163-2760 FU LRO project; Diviner science investigation; NASA FX We thank the LRO, Diviner, Mini-RF, and LROC operations teams for their effort in returning the data presented here. We also wish to thank the Diviner and Mini-RF science teams for helpful discussion in the early stages of this work. This work was supported by the LRO project and the Diviner science investigation, under contract with NASA. NR 39 TC 1 Z9 1 U1 4 U2 5 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD JUL 15 PY 2016 VL 273 SI SI BP 237 EP 247 DI 10.1016/j.icarus.2016.02.041 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DL6FK UT WOS:000375734900021 ER PT J AU Ashley, JW Robinson, MS Stopar, JD Glotch, TD Hawke, BR van der Bogert, CH Hiesinger, H Lawrence, SJ Jolliff, BL Greenhagen, BT Giguere, TA Paige, DA AF Ashley, J. W. Robinson, M. S. Stopar, J. D. Glotch, T. D. Hawke, B. Ray van der Bogert, C. H. Hiesinger, H. Lawrence, S. J. Jolliff, B. L. Greenhagen, B. T. Giguere, T. A. Paige, D. A. TI The Lassell massif-A silicic lunar volcano SO ICARUS LA English DT Article DE Moon, surface; Moon, interior; Volcanism; Infrared observations; Image processing ID COMPOSITIONAL ANALYSES; PYROCLASTIC DEPOSITS; MAIRAN DOMES; MARE BASALTS; MARIUS HILLS; RED SPOTS; MOON; SURFACE; GRUITHUISEN; EMPLACEMENT AB Lunar surface volcanic processes are dominated by mare-producing basaltic extrusions. However, spectral anomalies, landform morphology, and granitic or rhyolitic components found in the Apollo sample suites indicate limited occurrences of non-mare, geochemically evolved (Si-enriched) volcanic deposits. Recent thermal infrared spectroscopy, high-resolution imagery, and topographic data from the Lunar Reconnaissance Orbiter (LRO) show that most of the historic "red spots" and other, less well-known locations on the Moon, are indeed silica rich (relative to basalt). Here we present a geologic investigation of the Lassell massif (14.65 degrees S, 350.96 degrees E) near the center of Alphonsus A basin in Mare Nubium, where high silica thermal emission signals correspond with morphological indications of viscous (possibly also explosive) extrusion, and small-scale, low-reflectance deposits occur in a variety of stratigraphic relationships. Multiple layers with stair-step lobate forms suggest different eruption events or pulsing within a single eruption. Absolute model ages derived from crater size-frequency distributions (CSFDs) indicate that the northern parts of the massif were emplaced at similar to 4 Ga, before the surrounding mare. However, CSFDs also indicate the possibility of more recent resurfacing events. The complex resurfacing history might be explained by either continuous resurfacing due to mass wasting and/or the emplacement of pyroclastics. Relatively low-reflectance deposits are visible at meter-scale resolutions (below detection limits for compositional analysis) at multiple locations across the massif, suggestive of pyroclastic activity, a quenched flow surface, or late-stage mafic materials. Compositional evidence from 7-band UV/VIS spectral data at the kilometer-scale and morphologic evidence for possible caldera collapse and/or explosive venting support the interpretation of a complex volcanic history for the Lassell massif. (C) 2016 Elsevier Inc. All rights reserved. C1 [Ashley, J. W.; Robinson, M. S.; Stopar, J. D.; Lawrence, S. J.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85281 USA. [Ashley, J. W.] CALTECH, Jet Prop Lab, Mail Stop 183-301,4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Glotch, T. D.] SUNY Stony Brook, Dept Geosci, Stony Brook, NY 11794 USA. [Hawke, B. Ray; Giguere, T. A.] Univ Hawaii, Sch Ocean & Earth Sci & Technol, Hawaii Inst Geophys & Planetol, Honolulu, HI 96822 USA. [van der Bogert, C. H.; Hiesinger, H.] Univ Munster, Inst Planetol, D-48149 Munster, Germany. [Jolliff, B. L.] Washington Univ, Dept Earth & Planetary Sci, St Louis, MO 63105 USA. [Greenhagen, B. T.] Johns Hopkins Univ, Appl Phys Lab, 11100 Johns Hopkins Rd, Laurel, MD 20723 USA. [Paige, D. A.] Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90095 USA. RP Ashley, JW (reprint author), CALTECH, Jet Prop Lab, Mail Stop 183-301,4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM james.w.ashley@jpl.nasa.gov OI Ashley, James/0000-0003-0723-0987; Stopar, Julie/0000-0003-1578-3688 FU Lunar Reconnaissance Orbiter Camera (LROC) project; German Space Agency (DLR) FX We would like to thank Dr. Debra Hurwitz and Dr. Briony Horgan, who provided insightful reviews. This work was supported by the Lunar Reconnaissance Orbiter Camera (LROC) project. The authors gratefully acknowledge the contributions of the Lunar Reconnaissance Orbiter and LROC Teams. H. Hiesinger and C.H. van der Bogert were funded by the German Space Agency (DLR). The final draft of this paper is submitted in fond memory of co-author Dr. Bernard Ray Hawke. NR 70 TC 2 Z9 2 U1 3 U2 6 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD JUL 15 PY 2016 VL 273 SI SI BP 248 EP 261 DI 10.1016/j.icarus.2015.12.036 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DL6FK UT WOS:000375734900022 ER PT J AU Bennett, KA Horgan, BHN Gaddis, LR Greenhagen, BT Allen, CC Hayne, PO Bell, JF Paige, DA AF Bennett, Kristen A. Horgan, Briony H. N. Gaddis, Lisa R. Greenhagen, Benjamin T. Allen, Carlton C. Hayne, Paul O. Bell, James F., III Paige, David A. TI Complex explosive volcanic activity on the Moon within Oppenheimer crater SO ICARUS LA English DT Article DE Volcanism; Spectroscopy; Infrared observations; Mineralogy; Moon; Moon, surface ID LUNAR PYROCLASTIC DEPOSITS; NEAR-INFRARED SPECTRA; MINERALOGY MAPPER M-3; COMPOSITIONAL ANALYSES; SURFACE LAYER; GLASS-BEADS; IDENTIFICATION; CLEMENTINE; THICKNESS; MIXTURES AB Oppenheimer crater is a floor-fractured crater located within the South Pole-Aitken basin on the Moon, and exhibits more than a dozen localized pyroclastic deposits associated with the fractures. Localized pyroclastic volcanism on the Moon is thought to form as a result of intermittently explosive Vulcanian eruptions under low effusion rates, in contrast to the higher-effusion rate, Hawaiian-style fire fountaining inferred to form larger regional deposits. We use Lunar Reconnaissance Orbiter Camera images and Diviner Radiometer mid-infrared data, Chandrayaan-1 orbiter Moon Mineralogy Mapper near-infrared spectra, and Clementine orbiter Ultraviolet/visible camera images to test the hypothesis that the pyroclastic deposits in Oppenheimer crater were emplaced via Vulcanian activity by constraining their composition and mineralogy. Mineralogically, we find that the deposits are variable mixtures of orthopyroxene and minor clinopyroxene sourced from the crater floor, juvenile clinopyroxene, and juvenile iron-rich glass, and that the mineralogy of the pyroclastics varies both across the Oppenheimer deposits as a whole and within individual deposits. We observe similar variability in the inferred iron content of pyroclastic glasses, and note in particular that the northwest deposit, associated with Oppenheimer U crater, contains the most iron-rich volcanic glass thus far identified on the Moon, which could be a useful future resource. We propose that this variability in mineralogy indicates variability in eruption style, and that it cannot be explained by a simple Vulcanian eruption. A Vulcanian eruption should cause significant country rock to be incorporated into the pyroclastic deposit; however, large areas within many of the deposits exhibit spectra consistent with high abundances of juvenile phases and very little floor material. Thus, we propose that at least the most recent portion of these deposits must have erupted via a Strombolian or more continuous fire fountaining eruption, and in some cases may have included an effusive component. These results suggest that localized lunar pyroclastic deposits may have a more complex origin and mode of emplacement than previously thought. (C) 2016 Elsevier Inc. All rights reserved. C1 [Bennett, Kristen A.; Bell, James F., III] Arizona State Univ, Sch Earth & Space Explorat, ISTB4 Room 795,781 Terrace Mall, Tempe, AZ 85287 USA. [Horgan, Briony H. N.] Purdue Univ, Dept Earth Atmospher & Planetary Sci, 550 Stadium Mall Dr, W Lafayette, IN 47907 USA. [Gaddis, Lisa R.] US Geol Survey, Astrogeol Sci Ctr, 2255 N Gemini Dr, Flagstaff, AZ 86001 USA. [Greenhagen, Benjamin T.] Johns Hopkins Univ, Appl Phys Lab, 11100 Johns Hopkins Rd, Laurel, MD 20723 USA. [Allen, Carlton C.] NASA, Lyndon B Johnson Space Ctr, 2101 NASA Rd 1, Houston, TX 77058 USA. [Hayne, Paul O.] NASA, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Paige, David A.] Univ Calif Los Angeles, Dept Earth Planetary & Space Sci, 595 Charles E Young Dr E, Los Angeles, CA 90095 USA. RP Bennett, KA (reprint author), Arizona State Univ, Sch Earth & Space Explorat, ISTB4 Room 795,781 Terrace Mall, Tempe, AZ 85287 USA. EM kristen.a.bennett@asu.edu NR 63 TC 0 Z9 0 U1 3 U2 7 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD JUL 15 PY 2016 VL 273 SI SI BP 296 EP 314 DI 10.1016/j.icarus.2016.02.007 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DL6FK UT WOS:000375734900025 ER PT J AU Lemelin, M Lucey, PG Neumann, GA Mazarico, EM Barker, MK Kakazu, A Trang, D Smith, DE Zuber, MT AF Lemelin, M. Lucey, P. G. Neumann, G. A. Mazarico, E. M. Barker, M. K. Kakazu, A. Trang, D. Smith, D. E. Zuber, M. T. TI Improved calibration of reflectance data from the LRO Lunar Orbiter Laser Altimeter (LOLA) and implications for space weathering SO ICARUS LA English DT Article DE Moon; Moon, surface; Image processing; Infrared observations; Solar wind ID KAGUYA MULTIBAND IMAGER; PROSPECTOR; NEUTRONS; SURFACE; MOON AB The Lunar Orbiter Laser Altimeter (LOLA) experiment on Lunar Reconnaissance Orbiter (LRO) is a laser altimeter that also measures the strength of the return pulse from the lunar surface. These data have been used to estimate the reflectance of the lunar surface, including regions lacking direct solar illumination. A new calibration of these data is presented that features lower uncertainties overall and more consistent results in the polar regions. We use these data, along with newly available maps of the distribution of lunar maria, also derived from LRO instrument data, to investigate a newly discovered dependence of the albedo of the lunar maria on latitude (Hemingway et al., [2015]). We confirm that there is an increase in albedo with latitude in the lunar maria, and confirm that this variation is not an artifact arising from the distribution of compositions within the lunar maria, using data from the Lunar Prospector Neutron Spectrometer. Radiative transfer modeling of the albedo dependence within the lunar maria is consistent with the very weak to absent dependence of albedo on latitude in the lunar highlands; the lower abundance of the iron source for space weathering products in the lunar highlands weakens the latitude dependence to the extent that it is only weakly detectable in current data. In addition, photometric models and normalization may take into account the fact that the lunar albedo is latitude dependent, but this dependence can cause errors in normalized reflectance of at most 2% for the majority of near-nadir geometries. We also investigate whether the latitude dependent albedo may have obscured detection of small mare deposits at high latitudes. We find that small regions at high latitudes with low roughness similar to the lunar maria are not mare deposits that may have been misclassified owing to high albedos imposed by the latitude dependence. Finally, we suggest that the only modest correlations among space weathering indicators defined for the lunar samples may be due to mixing of soils from distinct latitudes. (C) 2016 Elsevier Inc. All rights reserved. C1 [Lemelin, M.; Lucey, P. G.; Kakazu, A.; Trang, D.] Univ Hawaii Manoa, Dept Geol & Geophys, Hawaii Inst Geophys & Planetol, 1680 East West Rd,Post 602, Honolulu, HI 96822 USA. [Neumann, G. A.; Mazarico, E. M.] NASA, Goddard Space Flight Ctr, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA. [Barker, M. K.] Sigma Space Corp, 4600 Forbes Blvd, Lanham, MD 20706 USA. [Smith, D. E.; Zuber, M. T.] MIT, Dept Earth Atmospher & Planetary Sci, 77 Massachusetts Ave, Cambridge, MA 02139 USA. RP Lemelin, M (reprint author), Univ Hawaii Manoa, Dept Geol & Geophys, Hawaii Inst Geophys & Planetol, 1680 East West Rd,Post 602, Honolulu, HI 96822 USA. EM mlemelin@hawaii.edu RI Neumann, Gregory/I-5591-2013; Mazarico, Erwan/N-6034-2014 OI Neumann, Gregory/0000-0003-0644-9944; Mazarico, Erwan/0000-0003-3456-427X FU Lunar Reconnaissance Orbiter Lunar Orbiter Laser Altimeter Experiment; Hawaii Institute of Geophysics and Planetology [2185, 9582]; Natural Sciences and Engineering Research Council of Canada (NSERC) through the Alexander Graham Bell Graduate Scholarship (PGS D) FX This work was supported in part by the Lunar Reconnaissance Orbiter Lunar Orbiter Laser Altimeter Experiment, David E. Smith Principal Investigator, by the Hawaii Institute of Geophysics and Planetology (HIGP Publication 2185, SOEST Publication 9582), and by the Natural Sciences and Engineering Research Council of Canada (NSERC) through the Alexander Graham Bell Graduate Scholarship (PGS D). NR 27 TC 2 Z9 2 U1 1 U2 2 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD JUL 15 PY 2016 VL 273 SI SI BP 315 EP 328 DI 10.1016/j.icarus.2016.02.006 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DL6FK UT WOS:000375734900026 ER PT J AU Barker, MK Mazarico, E Neumann, GA Zuber, MT Haruyama, J Smith, DE AF Barker, M. K. Mazarico, E. Neumann, G. A. Zuber, M. T. Haruyama, J. Smith, D. E. TI A new lunar digital elevation model from the Lunar Orbiter Laser Altimeter and SELENE Terrain Camera SO ICARUS LA English DT Article DE Moon; Moon, interior; Moon, surface ID GRAIL; MISSION; CRUST; MOON; DIMENSIONS; TOPOGRAPHY AB We present an improved lunar digital elevation model (DEM) covering latitudes within 60, at a horizontal resolution of 512 pixels per degree (similar to 60 m at the equator) and a typical vertical accuracy similar to 3 to 4 m. This DEM is constructed from similar to 4.5 x 10(9) geodetically-accurate topographic heights from the Lunar Orbiter Laser Altimeter (LOLA) onboard the Lunar Reconnaissance Orbiter, to which we co-registered 43,200 stereo-derived DEMs (each 1 degrees x 1 degrees) from the SELENE Terrain Camera (TC) (similar to 10(10) pixels total). After co-registration, approximately 90% of the TC DEMs show root-mean-square vertical residuals with the LOLA data of <5 m compared to similar to 50% prior to co-registration. We use the co-registered TC data to estimate and correct orbital and pointing geolocation errors from the LOLA altimetric profiles (typically amounting to <10 m horizontally and <1 m vertically). By combining both co-registered datasets, we obtain a near-global DEM with high geodetic accuracy, and without the need for surface interpolation. We evaluate the resulting LOLA + TC merged DEM (designated as "SLDEM2015") with particular attention to quantifying seams and crossover errors. (C) 2015 The Authors. Published by Elsevier Inc. C1 [Barker, M. K.] Sigma Space Corp, 4600 Forbes Blvd, Lanham, MD 20706 USA. [Mazarico, E.; Neumann, G. A.] NASA, Goddard Space Flight Ctr, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA. [Zuber, M. T.; Smith, D. E.] MIT, Dept Earth Atmospher & Planetary Sci, 77 Massachusetts Ave, Cambridge, MA 02139 USA. [Haruyama, J.] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Tokyo, Japan. RP Barker, MK (reprint author), Sigma Space Corp, 4600 Forbes Blvd, Lanham, MD 20706 USA. EM michael.k.barker@nasa.gov RI Neumann, Gregory/I-5591-2013; Mazarico, Erwan/N-6034-2014 OI Neumann, Gregory/0000-0003-0644-9944; Mazarico, Erwan/0000-0003-3456-427X FU NASA's Lunar Reconnaissance Orbiter Project; NASA's Planetary Geology and Geophysics Program FX This work was supported by NASA's Lunar Reconnaissance Orbiter Project and Planetary Geology and Geophysics Program. We thank the SELENE (Kaguya) TC team and the SELENE Data Archive for providing the SELENE (Kaguya) data. SELENE is a Japanese mission developed and operated by JAXA. We also thank the LRO Mission Operations Center and LOLA science teams for their hard work in producing the LOLA data used in this study. We are grateful to the anonymous reviewers for constructive feedback which improved the quality of this paper. NR 39 TC 2 Z9 2 U1 4 U2 9 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD JUL 15 PY 2016 VL 273 SI SI BP 346 EP 355 DI 10.1016/j.icarus.2015.07.039 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DL6FK UT WOS:000375734900029 ER PT J AU Rizzardi, LF Kunz, H Rubins, K Chouker, A Quiriarte, H Sams, C Crucian, BE Feinberg, AP AF Rizzardi, Lindsay F. Kunz, Hawley Rubins, Kathleen Chouker, Alexander Quiriarte, Heather Sams, Clarence Crucian, Brian E. Feinberg, Andrew P. TI Evaluation of techniques for performing cellular isolation and preservation during microgravity conditions SO NPJ MICROGRAVITY LA English DT Article ID BUBBLE FORMATION; GRAVITY AB Genomic and epigenomic studies require the precise transfer of microliter volumes among different types of tubes in order to purify DNA, RNA, or protein from biological samples and subsequently perform analyses of DNA methylation, RNA expression, and chromatin modifications on a genome-wide scale. Epigenomic and transcriptional analyses of human blood cells, for example, require separation of purified cell types to avoid confounding contributions of altered cellular proportions, and long-term preservation of these cells requires their isolation and transfer into appropriate freezing media. There are currently no protocols for these cellular isolation procedures on the International Space Station (ISS). Currently human blood samples are either frozen as mixed cell populations (within the CPT collection tubes) with poor yield of viable cells required for cell-type isolations, or returned under ambient conditions, which requires timing with Soyuz missions. Here we evaluate the feasibility of translating terrestrial cell purification techniques to the ISS. Our evaluations were performed in microgravity conditions during parabolic atmospheric flight. The pipetting of open liquids in microgravity was evaluated using analog-blood fluids and several types of pipette hardware. The best-performing pipettors were used to evaluate the pipetting steps required for peripheral blood mononuclear cell (PBMC) isolation following terrestrial density-gradient centrifugation. Evaluation of actual blood products was performed for both the overlay of diluted blood, and the transfer of isolated PBMCs. We also validated magnetic purification of cells. We found that positive-displacement pipettors avoided air bubbles, and the tips allowed the strong surface tension of water, glycerol, and blood to maintain a patent meniscus and withstand robust pipetting in microgravity. These procedures will greatly increase the breadth of research that can be performed on board the ISS, and allow improvised experimentation by astronauts on extraterrestrial missions. C1 [Rizzardi, Lindsay F.; Feinberg, Andrew P.] Johns Hopkins Univ, Sch Med, Ctr Epigenet, Baltimore, MD 21218 USA. [Kunz, Hawley] Wyle, Sci Technol & Engn Grp, Houston, TX USA. [Rubins, Kathleen] NASA, Johnson Space Ctr, Astronaut Off, Houston, TX USA. [Chouker, Alexander] Hosp Ludwig Maximilians Univ, Dept Anesthesiol, Munich, Germany. [Quiriarte, Heather] JES Tech, Houston, TX USA. [Sams, Clarence] NASA, Johnson Space Ctr, Space & Clin Operat Div, Houston, TX USA. [Crucian, Brian E.] NASA, Johnson Space Ctr, Biomed Res & Environm Sci Div, Houston, TX 77058 USA. [Feinberg, Andrew P.] Johns Hopkins Univ, Sch Med, Dept Med, Baltimore, MD 21205 USA. [Feinberg, Andrew P.] Johns Hopkins Univ, Sch Med, Dept Biomed Engn, Baltimore, MD 21205 USA. [Feinberg, Andrew P.] Johns Hopkins Univ, Sch Med, Dept Mental Hlth, Baltimore, MD 21218 USA. [Feinberg, Andrew P.] Johns Hopkins Univ, Dept Med, Sch Engn, Baltimore, MD 21218 USA. [Feinberg, Andrew P.] Johns Hopkins Univ, Dept Biomed Engn, Sch Engn, Baltimore, MD 21218 USA. [Feinberg, Andrew P.] Johns Hopkins Univ, Dept Mental Hlth, Sch Engn, Baltimore, MD 21218 USA. [Feinberg, Andrew P.] Johns Hopkins Univ, Sch Publ Hlth, Dept Med, Baltimore, MD 21218 USA. [Feinberg, Andrew P.] Johns Hopkins Univ, Sch Publ Hlth, Dept Biomed Engn, Baltimore, MD 21218 USA. [Feinberg, Andrew P.] Johns Hopkins Univ, Sch Publ Hlth, Dept Mental Hlth, Baltimore, MD 21218 USA. RP Feinberg, AP (reprint author), Johns Hopkins Univ, Sch Med, Ctr Epigenet, Baltimore, MD 21218 USA.; Crucian, BE (reprint author), NASA, Johnson Space Ctr, Biomed Res & Environm Sci Div, Houston, TX 77058 USA.; Feinberg, AP (reprint author), Johns Hopkins Univ, Sch Med, Dept Med, Baltimore, MD 21205 USA.; Feinberg, AP (reprint author), Johns Hopkins Univ, Sch Med, Dept Biomed Engn, Baltimore, MD 21205 USA.; Feinberg, AP (reprint author), Johns Hopkins Univ, Sch Med, Dept Mental Hlth, Baltimore, MD 21218 USA.; Feinberg, AP (reprint author), Johns Hopkins Univ, Dept Med, Sch Engn, Baltimore, MD 21218 USA.; Feinberg, AP (reprint author), Johns Hopkins Univ, Dept Biomed Engn, Sch Engn, Baltimore, MD 21218 USA.; Feinberg, AP (reprint author), Johns Hopkins Univ, Dept Mental Hlth, Sch Engn, Baltimore, MD 21218 USA.; Feinberg, AP (reprint author), Johns Hopkins Univ, Sch Publ Hlth, Dept Med, Baltimore, MD 21218 USA.; Feinberg, AP (reprint author), Johns Hopkins Univ, Sch Publ Hlth, Dept Biomed Engn, Baltimore, MD 21218 USA.; Feinberg, AP (reprint author), Johns Hopkins Univ, Sch Publ Hlth, Dept Mental Hlth, Baltimore, MD 21218 USA. EM brian.crucian-1@nasa.gov; afeinberg@jhu.edu NR 4 TC 1 Z9 1 U1 5 U2 5 PU NATURE PUBLISHING GROUP PI NEW YORK PA 75 VARICK ST, 9TH FLR, NEW YORK, NY 10013-1917 USA SN 2373-8065 J9 NPJ MICROGRAVITY JI NPJ Microgravity PD JUL 14 PY 2016 VL 2 AR 16025 DI 10.1038/npjmgrav.2016.25 PG 10 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA DR9IT UT WOS:000380211000001 ER PT J AU Hajra, R Chakraborty, SK Tsurutani, BT DasGupta, A Echer, E Brum, CGM Gonzalez, WD Sobral, JHA AF Hajra, Rajkumar Chakraborty, Shyamal Kumar Tsurutani, Bruce T. DasGupta, Ashish Echer, Ezequiel Brum, Christiano G. M. Gonzalez, Walter D. Andrade Sobral, Jose Humberto TI An empirical model of ionospheric total electron content (TEC) near the crest of the equatorial ionization anomaly (EIA) SO JOURNAL OF SPACE WEATHER AND SPACE CLIMATE LA English DT Article DE Ionosphere (equatorial); Solar activity; Solar cycle; Total electron content; Forecasting ID LOW-LATITUDE; SOLAR MINIMUM; SEMIANNUAL VARIATIONS; AMBIENT IONIZATION; SUNSPOT MINIMUM; INDIAN ZONE; REGION; IRI; PREDICTIONS; SATELLITE AB We present a geomagnetic quiet time (Dst > -50 nT) empirical model of ionospheric total electron content (TEC) for the northern equatorial ionization anomaly (EIA) crest over Calcutta, India. The model is based on the 1980-1990 TEC measurements from the geostationary Engineering Test Satellite-2 (ETS-2) at the Haringhata (University of Calcutta, India: 22.58 degrees N, 88.38 degrees E geographic; 12.09 degrees N, 160.46 degrees E geomagnetic) ionospheric field station using the technique of Faraday rotation of plane polarized VHF (136.11 MHz) signals. The ground station is situated virtually underneath the northern EIA crest. The monthly mean TEC increases linearly with F-10.7 solar ionizing flux, with a significantly high correlation coefficient (r - 0.89-0.99) between the two. For the same solar flux level, the TEC values are found to be significantly different between the descending and ascending phases of the solar cycle. This ionospheric hysteresis effect depends on the local time as well as on the solar flux level. On an annual scale, TEC exhibits semiannual variations with maximum TEC values occurring during the two equinoxes and minimum at summer solstice. The semiannual variation is strongest during local noon with a summer-to-equinox variability of similar to 50-100 TEC units. The diurnal pattern of TEC is characterized by a pre-sunrise (0400-0500 LT) minimum and near-noon (1300-1400 LT) maximum. Equatorial electrodynamics is dominated by the equatorial electrojet which in turn controls the daytime TEC variation and its maximum. We combine these long-term analyses to develop an empirical model of monthly mean TEC. The model is validated using both ETS-2 measurements and recent GNSS measurements. It is found that the present model efficiently estimates the TEC values within a 1-sigma range from the observed mean values. C1 [Hajra, Rajkumar; Echer, Ezequiel; Gonzalez, Walter D.; Andrade Sobral, Jose Humberto] Inst Nacl Pesquisas Espaciais, Av Astronautas, BR-12227010 Sao Jose Dos Campos, SP, Brazil. [Hajra, Rajkumar; Brum, Christiano G. M.] SRI Int, Natl Astron & Ionosphere Ctr, Space & Atmospher Sci Dept, Arecibo Observ, HC3 Box 53995, Arecibo, PR 00612 USA. [Hajra, Rajkumar] CNRS, Lab Phys & Chim Environm & Espace LPC2E, F-45100 Orleans, France. [Chakraborty, Shyamal Kumar] Raja Peary Mohan Coll, Dept Phys, Uttarpara 712258, Hooghly, India. [Tsurutani, Bruce T.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr Pasadena, Pasadena, CA 91109 USA. [DasGupta, Ashish] Univ Calcutta, SK Mitra Ctr Res Space Environm, Kolkata 700009, W Bengal, India. RP Hajra, R (reprint author), Inst Nacl Pesquisas Espaciais, Av Astronautas, BR-12227010 Sao Jose Dos Campos, SP, Brazil.; Hajra, R (reprint author), SRI Int, Natl Astron & Ionosphere Ctr, Space & Atmospher Sci Dept, Arecibo Observ, HC3 Box 53995, Arecibo, PR 00612 USA.; Hajra, R (reprint author), CNRS, Lab Phys & Chim Environm & Espace LPC2E, F-45100 Orleans, France. EM rajkumarhajra@yahoo.co.in OI Hajra, Rajkumar/0000-0003-0447-1531 FU Fundacao de Amparo a Pesquisa do Estado de Sao Paulo (FAPESP) through post-doctoral research fellowship at INPE; DST SERB Project, Govt. of India; Brazilian CNPq agency [302583/2015-7]; NASA; National Science Foundation (NSF) [1160876] FX The work of R.H. is financially supported by Fundacao de Amparo a Pesquisa do Estado de Sao Paulo (FAPESP) through post-doctoral research fellowship at INPE. The work of S.K.C. is supported by DST SERB Project, Govt. of India. E.E. would like to thank the Brazilian CNPq (302583/2015-7) agency for financial support. Portions of this research were performed at the Jet Propulsion Laboratory, California Institute of Technology under contract with NASA. The Arecibo Observatory is operated by SRI International in collaboration with the Universities Space Research Association (USRA) and the Universidad Metropolitana (UMET) under a cooperative agreement with the National Science Foundation (NSF), Award Number 1160876. We would like to thank the referees and the editors for valuable suggestions leading to substantial improvement of the manuscript. The editor thanks three anonymous referees for their assistance in evaluating this paper. NR 69 TC 0 Z9 0 U1 3 U2 6 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 2115-7251 J9 J SPACE WEATHER SPAC JI J. Space Weather Space Clim. PD JUL 14 PY 2016 VL 6 AR A29 DI 10.1051/swsc/2016023 PG 9 WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences GA DR9CM UT WOS:000380194700001 ER PT J AU Wang, J Kaseman, D Lee, K Sen, S Kovnir, K AF Wang, Jian Kaseman, Derrick Lee, Kathleen Sen, Sabyasachi Kovnir, Kirin TI Enclathration of X@La-4 Tetrahedra in Channels of Zn-P Frameworks in La3Zn4P6X (X = Cl, Br) SO CHEMISTRY OF MATERIALS LA English DT Article ID MATPASS/CPMG NMR-SPECTROSCOPY; STRUCTURAL CHEMISTRY; CRYSTAL-STRUCTURES; ELECTRON LOCALIZATION; PHYSICAL-PROPERTIES; PHOSPHIDES; POLYPHOSPHIDES; ANIONS; PHOSPHORUS; LANTHANUM AB Two new quaternary lanthanum zinc phosphide-halides were synthesized via high-temperature solid-state reactions. Their complex crystal structures were determined by a combination of X-ray diffraction and advanced solid-state 31P NMR spectroscopy. La3Zn4P6Cl and La3Zn4P6.6Br0.8 share a common structural feature: a polyanionic Zn-P framework with large channels hosting complex one-dimensional cations. The cations are built from X@La4 tetrahedral chains with X = Cl (La3Zn4P6Cl) or Br0.8P0.2 (La3Zn4P6.6Br0.8). The X@La4 tetrahedra share two vertices forming one-dimensional chains. To accommodate larger bromine-containing cations the Zn-P framework is rearranged by breaking and forming several Zn-P and P-P bonds. This results in the formation of a unique [P3]3- cycle, which is isoelectronic to cyclopropane. Analysis of the electron localization and orbital overlaps confirmed the presence of different chemical bonding in the Zn-P networks in the Cl- and Br-containing compounds. La3Zn4P6Cl was predicted to be a narrow bandgap semiconductor, while the formation of the [P3]3- units in the structure of La3Zn4P6.6Br0.8 was shown to lead to a narrowing of the bandgap. Characterization of the transport properties confirmed both La3Zn4P6Cl and La3Zn4P6.6Br0.8 to be narrow bandgap semiconductors with electrons as dominating charge carriers at low temperatures. La3Zn4P6Cl exhibits a n-p transition around 250 K. Due to the complex crystal structure and segregation of the areas of different chemical bonding, both title compounds exhibit ultralow thermal conductivities of 0.7 Wm(-1) K-1 and 1.5 Wm(-1) K-1 at 400 K for La3Zn4P6Cl and La3Zn4P6.6Br0.8, respectively. C1 [Wang, Jian; Lee, Kathleen; Kovnir, Kirin] Univ Calif Davis, Dept Chem, One Shields Ave, Davis, CA 95616 USA. [Kaseman, Derrick; Sen, Sabyasachi] Univ Calif Davis, Dept Mat Sci, One Shields Ave, Davis, CA 95616 USA. [Lee, Kathleen] Jet Prop Lab, Thermal Energy Convers Technol Grp, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. RP Kovnir, K (reprint author), Univ Calif Davis, Dept Chem, One Shields Ave, Davis, CA 95616 USA. EM kkovnir@ucdavis.edu OI Wang, Jian/0000-0003-1326-4470 FU GAANN; ARCS; U.S. Department of Energy, Office of Basic Energy Sciences, Division of Materials Sciences and Engineering [DE-SC0008931] FX The authors would like to thank Prof. S. M. Kauzlarich for access to the SPS. K.L. acknowledges the GAANN and ARCS fellowships. This research is supported by the U.S. Department of Energy, Office of Basic Energy Sciences, Division of Materials Sciences and Engineering under Award DE-SC0008931. NR 70 TC 2 Z9 2 U1 4 U2 6 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0897-4756 EI 1520-5002 J9 CHEM MATER JI Chem. Mat. PD JUL 12 PY 2016 VL 28 IS 13 BP 4741 EP 4750 DI 10.1021/acs.chemmater.6b01752 PG 10 WC Chemistry, Physical; Materials Science, Multidisciplinary SC Chemistry; Materials Science GA DR1ZJ UT WOS:000379704100026 ER PT J AU Parazoo, NC Commane, R Wofsy, SC Koven, CD Sweeney, C Lawrence, DM Lindaas, J Chang, RYW Miller, CE AF Parazoo, Nicholas C. Commane, Roisin Wofsy, Steven C. Koven, Charles D. Sweeney, Colm Lawrence, David M. Lindaas, Jakob Chang, Rachel Y. -W. Miller, Charles E. TI Detecting regional patterns of changing CO2 flux in Alaska SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE carbon cycle; permafrost thaw; climate; Earth system models; remote sensing ID NORTHERN ECOSYSTEMS; SATELLITE-OBSERVATIONS; CARBON-DIOXIDE; PERMAFROST; CLIMATE; CYCLE; AIRCRAFT; DYNAMICS; EXCHANGE; FEEDBACK AB With rapid changes in climate and the seasonal amplitude of carbon dioxide (CO2) in the Arctic, it is critical that we detect and quantify the underlying processes controlling the changing amplitude of CO2 to better predict carbon cycle feedbacks in the Arctic climate system. We use satellite and airborne observations of atmospheric CO2 with climatically forced CO2 flux simulations to assess the detectability of Alaskan carbon cycle signals as future warming evolves. We find that current satellite remote sensing technologies can detect changing uptake accurately during the growing season but lack sufficient cold season coverage and near-surface sensitivity to constrain annual carbon balance changes at regional scale. Airborne strategies that target regular vertical profile measurements within continental interiors are more sensitive to regional flux deeper into the cold season but currently lack sufficient spatial coverage throughout the entire cold season. Thus, the current CO2 observing network is unlikely to detect potentially large CO2 sources associated with deep permafrost thaw and cold season respiration expected over the next 50 y. Although continuity of current observations is vital, strategies and technologies focused on cold season measurements (active remote sensing, aircraft, and tall towers) and systematic sampling of vertical profiles across continental interiors over the full annual cycle are required to detect the onset of carbon release from thawing permafrost. C1 [Parazoo, Nicholas C.; Miller, Charles E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Parazoo, Nicholas C.] Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA 90095 USA. [Commane, Roisin; Wofsy, Steven C.; Lindaas, Jakob] Harvard Univ, Dept Earth & Planetary Sci, Cambridge, MA 02138 USA. [Commane, Roisin; Wofsy, Steven C.] Harvard Univ, Harvard Sch Engn & Appl Sci, Cambridge, MA 02138 USA. [Koven, Charles D.] Lawrence Berkeley Natl Lab, Climate & Ecosyst Sci Div, Berkeley, CA 94720 USA. [Sweeney, Colm] NOAA, Earth Syst Res Lab, Boulder, CO 80305 USA. [Sweeney, Colm] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA. [Lawrence, David M.] Natl Ctr Atmospher Res, Climate & Global Dynam Lab, Boulder, CO 80302 USA. [Lindaas, Jakob] Colorado State Univ, Dept Atmospher Sci, Ft Collins, CO 80523 USA. [Chang, Rachel Y. -W.] Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS B3H 4R2, Canada. RP Parazoo, NC (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.; Parazoo, NC (reprint author), Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA 90095 USA. EM nicholas.c.parazoo@jpl.nasa.gov RI Koven, Charles/N-8888-2014; OI Koven, Charles/0000-0002-3367-0065; Lindaas, Jakob/0000-0003-1872-3162; Commane, Roisin/0000-0003-1373-1550 FU NASA; Office of Science, Office of Biological and Environmental Research (BER) of the US Department of Energy (DOE) [DE-AC02-05CH11231]; US DOE, BER [DE-FC03-97ER62402/A010]; NSF [PLR-1304220] FX Some of the research described was performed for CARVE, an Earth Ventures (EV-1) investigation, under contract with NASA. A portion of this research was carried out at the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. C.D.K. was supported by the Director, Office of Science, Office of Biological and Environmental Research (BER) of the US Department of Energy (DOE) Contract DE-AC02-05CH11231 as part of their Regional and Global Climate Modeling (BGC-Feedbacks SFA) and Terrestrial Ecosystem Science (NGEE-Arctic) Programs. D.M.L. was supported by the US DOE, BER as part of Climate Change Prediction Program Cooperative Agreement DE-FC03-97ER62402/A010 and by NSF Grant PLR-1304220. NR 36 TC 0 Z9 0 U1 13 U2 20 PU NATL ACAD SCIENCES PI WASHINGTON PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA SN 0027-8424 J9 P NATL ACAD SCI USA JI Proc. Natl. Acad. Sci. U. S. A. PD JUL 12 PY 2016 VL 113 IS 28 BP 7733 EP 7738 DI 10.1073/pnas.1601085113 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA DR1VX UT WOS:000379694100032 PM 27354511 ER PT J AU McKinna, LIW Werdell, PJ Proctor, CW AF McKinna, Lachlan I. W. Werdell, P. Jeremy Proctor, Christopher W. TI Implementation of an analytical Raman scattering correction for satellite ocean-color processing SO OPTICS EXPRESS LA English DT Article ID INHERENT OPTICAL-PROPERTIES; RADIANCE MODEL; NATURAL-WATERS; CHLOROPHYLL-A; TIME-SERIES; PURE WATER; ABSORPTION; INVERSION; SURFACE; BACKSCATTERING AB Raman scattering of photons by seawater molecules is an inelastic scattering process. This effect can contribute significantly to the water-leaving radiance signal observed by space-borne ocean-color spectroradiometers. If not accounted for during ocean-color processing, Raman scattering can cause biases in derived inherent optical properties (IOPs). Here we describe a Raman scattering correction (RSC) algorithm that has been integrated within NASA's standard ocean-color processing software. We tested the RSC with NASA's Generalized Inherent Optical Properties algorithm (GIOP). A comparison between derived IOPs and in situ data revealed that the magnitude of the derived backscattering coefficient and the phytoplankton absorption coefficient were reduced when the RSC was applied, whilst the absorption coefficient of colored dissolved and detrital matter remained unchanged. Importantly, our results show that the RSC did not degrade the retrieval skill of the GIOP. In addition, a time-series study of oligotrophic waters near Bermuda showed that the RSC did not introduce unwanted temporal trends or artifacts into derived IOPs. (C) 2016 Optical Society of America C1 [McKinna, Lachlan I. W.] Sci Applicat Int Corp, 1710 SAIC Dr, Mclean, VA 22102 USA. [McKinna, Lachlan I. W.; Werdell, P. Jeremy; Proctor, Christopher W.] NASA, Goddard Space Flight Ctr, Code 616, Greenbelt, MD 20771 USA. [Proctor, Christopher W.] Sci Syst & Applicat Inc, 10210 Greenbelt Rd,Suite 600, Lanham, MD 20706 USA. RP McKinna, LIW (reprint author), Sci Applicat Int Corp, 1710 SAIC Dr, Mclean, VA 22102 USA.; McKinna, LIW (reprint author), NASA, Goddard Space Flight Ctr, Code 616, Greenbelt, MD 20771 USA. EM lachlan.i.mckinna@nasa.gov FU NASA Ocean Biology and Biogeochemistry Program FX A NASA Ocean Biology and Biogeochemistry Program award for the Science of Terra and Aqua supported this work. We thank Tommy Owens for time-series data processing support. Ivona Cetinic, Amir Ibrahim and other members of the NASA OBPG are also duly acknowledged for providing valuable scientific advice. We also wish to recognize the efforts of Emmanuel Boss who kindly reviewed this paper. NR 46 TC 0 Z9 0 U1 1 U2 1 PU OPTICAL SOC AMER PI WASHINGTON PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA SN 1094-4087 J9 OPT EXPRESS JI Opt. Express PD JUL 11 PY 2016 VL 24 IS 14 BP A1123 EP A1137 DI 10.1364/OE.24.0A1123 PG 15 WC Optics SC Optics GA DT8UF UT WOS:000381770500011 PM 27410899 ER PT J AU Underwood, DS Tennyson, J Yurchenko, SN Huang, XC Schwenke, DW Lee, TJ Clausen, S Fateev, A AF Underwood, Daniel S. Tennyson, Jonathan Yurchenko, Sergei N. Huang, Xinchuan Schwenke, David W. Lee, Timothy J. Clausen, Sonnik Fateev, Alexander TI ExoMol molecular line lists - XIV. The rotation-vibration spectrum of hot SO2 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE molecular data; opacity; astronomical data bases: miscellaneous; planets and satellites: atmospheres ID CROSS-SECTION MEASUREMENTS; ROVIBRATIONAL BOUND-STATES; POTENTIAL-ENERGY SURFACE; HIGH-RESOLUTION; SULFUR-DIOXIDE; TRIATOMIC-MOLECULES; WAVELENGTH REGION; ORION-KL; INTENSITIES; ABSORPTION AB Sulphur dioxide is well-known in the atmospheres of planets and satellites, where its presence is often associated with volcanism, and in circumstellar envelopes of young and evolved stars as well as the interstellar medium. This work presents a line list of 1.3 billion (SO2)-S-32-O-16 vibration-rotation transitions computed using an empirically adjusted potential energy surface and an ab initio dipole moment surface. The list gives complete coverage up to 8000 cm(-1) (wavelengths longer than 1.25 mu m) for temperatures below 2000 K. Infrared absorption cross-sections are recorded at 300 and 500 C are used to validated the resulting ExoAmes line list. The line list is made available in electronic form as supplementary data to this article and at www.exomol.com. C1 [Underwood, Daniel S.; Tennyson, Jonathan; Yurchenko, Sergei N.] UCL, Dept Phys & Astron, London WC1E 6BT, England. [Huang, Xinchuan] SETI Inst, Mountain View, CA 94043 USA. [Schwenke, David W.] NASA, Ames Res Ctr, NAS Facil, Moffett Field, CA 94035 USA. [Lee, Timothy J.] NASA, Ames Res Ctr, Space Sci & Astrobiol Div, Moffett Field, CA 94035 USA. [Clausen, Sonnik; Fateev, Alexander] Tech Univ Denmark, Dept Chem & Biochem Engn, Frederiksborgvej 399, DK-4000 Roskilde, Denmark. RP Tennyson, J (reprint author), UCL, Dept Phys & Astron, London WC1E 6BT, England. EM j.tennyson@ucl.ac.uk RI Tennyson, Jonathan/I-2222-2012; Yurchenko, Sergey/G-9929-2012; Lee, Timothy/K-2838-2012; HUANG, XINCHUAN/A-3266-2013 OI Tennyson, Jonathan/0000-0002-4994-5238; Yurchenko, Sergey/0000-0001-9286-9501; FU Energinet.dk project [2010-1-10442]; ERC [267219]; STFC; BIS; NASA [12-APRA12-0107]; NASA/SETI Institute Cooperative Agreement [NNX15AF45A] FX This work was supported by Energinet.dk project 2010-1-10442 'Sulfur trioxide measurement technique for energy systems' and the ERC under the Advanced Investigator Project 267219. It made use of the DiRAC@Darwin HPC cluster which is part of the DiRAC UK HPC facility for particle physics, astrophysics and cosmology and is supported by STFC and BIS. XH, DWS, and TJL gratefully acknowledge funding support from the NASA Grant 12-APRA12-0107. XH also acknowledges support from the NASA/SETI Institute Cooperative Agreement NNX15AF45A. NR 89 TC 8 Z9 8 U1 5 U2 8 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUL 11 PY 2016 VL 459 IS 4 BP 3890 EP 3899 DI 10.1093/mnras/stw849 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DR3VM UT WOS:000379830700038 ER PT J AU Knowles, K Intema, HT Baker, AJ Bharadwaj, V Bond, JR Cress, C Gupta, N Hajian, A Hilton, M Hincks, AD Hlozek, R Hughes, JP Lindner, RR Marriage, TA Menanteau, F Moodley, K Niemack, MD Reese, ED Sievers, J Sifon, C Srianand, R Wollack, EJ AF Knowles, K. Intema, H. T. Baker, A. J. Bharadwaj, V. Bond, J. R. Cress, C. Gupta, N. Hajian, A. Hilton, M. Hincks, A. D. Hlozek, R. Hughes, J. P. Lindner, R. R. Marriage, T. A. Menanteau, F. Moodley, K. Niemack, M. D. Reese, E. D. Sievers, J. Sifon, C. Srianand, R. Wollack, E. J. TI A giant radio halo in a low-mass SZ-selected galaxy cluster: ACT-CL J0256.5+0006 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: clusters: individual: (ACT-CL J0256.5+0006); galaxies: clusters: intracluster medium; radio continuum: general; X-rays: individual: ACT-CL J0256.5+0006 ID X-RAY-CLUSTERS; SUNYAEV-ZELDOVICH; SIMULATED CLUSTERS; SCALING RELATIONS; MERGING CLUSTER; ABELL CLUSTERS; SKY SURVEY; FOLLOW-UP; EMISSION; SUBSTRUCTURE AB We present the detection of a giant radio halo (GRH) in the Sunyaev-Zel'dovich (SZ)-selected merging galaxy cluster ACT-CL J0256.5+0006 (z = 0.363), observed with the Giant Metrewave Radio Telescope at 325 and 610 MHz. We find this cluster to host a faint (S-610 = 5.6 +/- 1.4 mJy) radio halo with an angular extent of 2.6 arcmin, corresponding to 0.8 Mpc at the cluster redshift, qualifying it as a GRH. J0256 is one of the lowest mass systems, M-500,M- SZ = (5.0 +/- 1.2) x 10(14) M-aS (TM), found to host a GRH. We measure the GRH at lower significance at 325 MHz (S-325 = 10.3 +/- 5.3 mJy), obtaining a spectral index measurement of $\alpha <^>{610}_{325} = 1.0<^>{+0.7}_{-0.9}$. This result is consistent with the mean spectral index of the population of typical radio haloes, alpha = 1.2 +/- 0.2. Adopting the latter value, we determine a 1.4 GHz radio power of P-1.4 GHz = (1.0 +/- 0.3) x 10(24) W Hz(-1), placing this cluster within the scatter of known scaling relations. Various lines of evidence, including the intracluster medium morphology, suggest that ACT-CL J0256.5+0006 is composed of two subclusters. We determine a merger mass ratio of 7:4, and a line-of-sight velocity difference of v(aSyen) = 1880 +/- 210 km s(-1). We construct a simple merger model to infer relevant time-scales in the merger. From its location on the P-1.4 GHz-L-X scaling relation, we infer that we observe ACT-CL J0256.5+0006 just before first core crossing. C1 [Knowles, K.; Bharadwaj, V.; Hilton, M.; Moodley, K.] Univ KwaZulu Natal, Astrophys & Cosmol Res Unit, Sch Math Stat & Comp Sci, ZA-4041 Durban, South Africa. [Intema, H. T.] Natl Radio Astron Observ, 1003 Lopezville Rd, Socorro, NM 87801 USA. [Baker, A. J.; Hughes, J. P.; Lindner, R. R.] Rutgers State Univ, Dept Phys & Astron, 136 Frelinghuysen Rd, Piscataway, NJ 08854 USA. [Bond, J. R.; Hajian, A.] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada. [Cress, C.] Ctr High Performance Comp, CSIR Campus,15 Lower Hope Rd, Cape Town, South Africa. [Cress, C.] Univ Western Cape, Dept Phys, Modderdam Rd, ZA-7535 Bellville, South Africa. [Gupta, N.; Srianand, R.] IUCAA, Post Bag 4, Pune 411007, Maharashtra, India. [Hincks, A. D.] Univ British Columbia, Dept Phys & Astron, 6224 Agr Rd, Vancouver, BC V6T 1Z1, Canada. [Hlozek, R.] Princeton Univ, Dept Astrophys Sci, Peyton Hall, Princeton, NJ 08544 USA. [Lindner, R. R.] Univ Wisconsin, Dept Astron, 475 N Charter St, Madison, WI 53706 USA. [Marriage, T. A.] Johns Hopkins Univ, Dept Phys & Astron, 3400 N Charles St, Baltimore, MD 21218 USA. [Menanteau, F.] Univ Illinois, Natl Ctr Supercomp Applicat, 1205 W Clark St, Urbana, IL 61801 USA. [Menanteau, F.] Univ Illinois, Dept Astron, W Green St, Urbana, IL 61801 USA. [Niemack, M. D.] Cornell Univ, Dept Phys, Ithaca, NY 14853 USA. [Reese, E. D.] Moorpk Coll, Dept Phys Astron & Engn, 7075 Campus Rd, Moorpark, CA 93021 USA. [Sievers, J.] Univ KwaZulu Natal, Astrophys & Cosmol Res Unit, Sch Chem & Phys, ZA-4041 Durban, South Africa. [Sievers, J.] Univ KwaZulu Natal, Natl Inst Theoret Phys NITheP, Private Bag X54001, ZA-4000 Durban, South Africa. [Sifon, C.] Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands. [Wollack, E. J.] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA. RP Knowles, K (reprint author), Univ KwaZulu Natal, Astrophys & Cosmol Res Unit, Sch Math Stat & Comp Sci, ZA-4041 Durban, South Africa. EM kendaknowles.astro@gmail.com RI Wollack, Edward/D-4467-2012; OI Wollack, Edward/0000-0002-7567-4451; Menanteau, Felipe/0000-0002-1372-2534; Sifon, Cristobal/0000-0002-8149-1352 FU NRF/SKA South Africa Project; National Radio Astronomy Observatory, a facility of the National Science Foundation; National Science Foundation [AST 0955810] FX KK acknowledges post-graduate support from the NRF/SKA South Africa Project. HTI is financially supported by the National Radio Astronomy Observatory, a facility of the National Science Foundation operated under Associated Universities Inc. AJB acknowledges support from National Science Foundation grant AST 0955810. NR 73 TC 1 Z9 1 U1 0 U2 0 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUL 11 PY 2016 VL 459 IS 4 BP 4240 EP 4258 DI 10.1093/mnras/stw795 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DR3VM UT WOS:000379830700065 ER PT J AU Kuhn, RB Rodriguez, JE Collins, KA Lund, MB Siverd, RJ Colon, KD Pepper, J Stassun, KG Cargile, PA James, DJ Penev, K Zhou, G BaylisS, D Tan, TG Curtis, IA Udry, S Segransan, D Mawet, D Dhita, S Soutter, J Hart, R Carter, B Gaudi, BS Myers, G Beatty, TG Eastman, JD Reichart, DE Haislip, JB Kielkopf, J Bieryla, A Latham, DW Jensen, ELN Oberst, TE StevensI, DJ AF Kuhn, Rudolf B. Rodriguez, Joseph E. Collins, Karen A. Lund, Michael B. Siverd, Robert J. Colon, Knicole D. Pepper, Joshua Stassun, Keivan G. Cargile, Phillip A. James, David J. Penev, Kaloyan Zhou, George Bayliss, Daniel Tan, T. G. Curtis, Ivan A. Udry, Stephane Segransan, Damien Mawet, Dimitri Dhital, Saurav Soutter, Jack Hart, Rhodes Carter, Brad Gaudi, B. Scott Myers, Gordon Beatty, Thomas G. Eastman, Jason D. Reichart, Daniel E. Haislip, Joshua B. Kielkopf, John Bieryla, Allyson Latham, David W. Jensen, Eric L. N. Oberst, Thomas E. Stevens, Daniel J. TI KELT-10b: the first transiting exoplanet from the KELT-South survey -a hot sub-Jupiter transiting a V=10.7 early G-star SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE techniques: photometric; techniques: radial velocities; techniques: spectroscopic; stars: individual: KELT-10; planetary systems ID SPECTRAL-LINE BISECTORS; IMAGE SUBTRACTION; EXTRASOLAR PLANET; STELLAR PHOTOMETRY; RADIAL-VELOCITIES; VARIABLE-STARS; LIGHT CURVES; SHORT-PERIOD; SPACED DATA; COOL STARS AB We report the discovery of KELT-10b, the first transiting exoplanet discovered using the KELT-South telescope. KELT-10b is a highly inflated sub-Jupiter mass planet transiting a relatively bright V = 10.7 star (TYC 8378-64-1), with T-eff = 5948 +/- 74 K, log g = $4.319_{-0.030}<^>{+0.020}$ and [Fe/H] = $0.09_{-0.10}<^>{+0.11}$, an inferred mass M-* = $1.112_{-0.061}<^>{+0.055}$ M-aS (TM) and radius R-* = $1.209_{-0.035}<^>{+0.047}$ R-aS (TM). The planet has a radius R-p = $1.399_{-0.049}<^>{+0.069}$ R-J and mass M-p = $0.679_{-0.038}<^>{+0.039}$ M-J. The planet has an eccentricity consistent with zero and a semimajor axis a = $0.052\,50_{-0.000\,97}<^>{+0.000\,86}$ au. The best-fitting linear ephemeris is T-0 = 2457 066.720 45 +/- 0.000 27 BJD(TDB) and P = 4.166 2739 +/- 0.000 0063 d. This planet joins a group of highly inflated transiting exoplanets with a larger radius and smaller mass than that of Jupiter. The planet, which boasts deep transits of 1.4 per cent, has a relatively high equilibrium temperature of T-eq = $1377_{-23}<^>{+28}$ K, assuming zero albedo and perfect heat redistribution. KELT-10b receives an estimated insolation of $0.817_{-0.054}<^>{+0.068}$ x 10(9) erg s(-1) cm(-2), which places it far above the insolation threshold above which hot Jupiters exhibit increasing amounts of radius inflation. Evolutionary analysis of the host star suggests that KELT-10b may not survive beyond the current subgiant phase, depending on the rate of in-spiral of the planet over the next few Gyr. The planet transits a relatively bright star and exhibits the third largest transit depth of all transiting exoplanets with V < 11 in the Southern hemisphere, making it a promising candidate for future atmospheric characterization studies. C1 [Kuhn, Rudolf B.] S African Astron Observ, POB 9, ZA-7935 Cape Town, South Africa. [Rodriguez, Joseph E.; Collins, Karen A.; Lund, Michael B.; Stassun, Keivan G.] Vanderbilt Univ, Dept Phys & Astron, 6301 Stevenson Ctr, Nashville, TN 37235 USA. [Collins, Karen A.; Kielkopf, John] Univ Louisville, Dept Phys & Astron, Louisville, KY 40292 USA. [Siverd, Robert J.] Las Cumbres Observ, Global Telescope Network, 6740 Cortona Dr,Suite 102, Santa Barbara, CA 93117 USA. [Colon, Knicole D.; Pepper, Joshua] Lehigh Univ, Dept Phys, Bethlehem, PA 18015 USA. [Colon, Knicole D.] NASA Ames Res Ctr, M-S 244-30, Moffett Field, CA 94035 USA. [Colon, Knicole D.] Bay Area Environm Res Inst, 625 2nd St Ste 209, Petaluma, CA 94952 USA. [Stassun, Keivan G.] Fisk Univ, Dept Phys, 1000 17thAve North, Nashville, TN 37208 USA. [Cargile, Phillip A.; Eastman, Jason D.; Bieryla, Allyson; Latham, David W.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [James, David J.] Cerro Tololo Interamer Observ, Colina El Pino S-N,Casilla 603, La Serena, Chile. [Penev, Kaloyan] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Zhou, George] Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT 2611, Australia. [Bayliss, Daniel; Udry, Stephane; Segransan, Damien] Univ Geneva, Astron Observ, Chemin Maillettes 51, CH-1290 Sauverny, Switzerland. [Bayliss, Daniel] Australia Telescope Natl Facil, Acton, ACT 2601, Australia. [Tan, T. G.] Perth Exoplanet Survey Telescope, Perth, WA, Australia. [Curtis, Ivan A.] 2 Yandra St,Vale Pk, Adelaide, SA 5081, Australia. [Mawet, Dimitri] CALTECH, Dept Astron, Mail Code 249-17,1200 E Calif Blvd, Pasadena, CA 91125 USA. [Mawet, Dimitri] European So Observ, Alonso Coniova 3107, Santiago, Chile. [Dhital, Saurav] Boston Univ, Dept Astron, 725 Commonwealth Ave, Boston, MA 02215 USA. [Soutter, Jack; Hart, Rhodes; Carter, Brad] Univ So Queensland, Computat Engn & Sci Res Ctr, Toowoomba, Qld 4350, Australia. [Gaudi, B. Scott; Stevens, Daniel J.] Ohio State Univ, Dept Astron, 140 West 18th Ave, Columbus, OH 43210 USA. [Myers, Gordon] 5 Inverness Way, Hillsborough, CA 94010 USA. [Myers, Gordon] AAVSO, 49 Bay State Rd, Cambridge, MA 02138 USA. [Beatty, Thomas G.] Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA. [Beatty, Thomas G.] Penn State Univ, Ctr Exoplanets & Habitable Worlds, 525 Davey Lab, University Pk, PA 16802 USA. [Reichart, Daniel E.; Haislip, Joshua B.] Univ N Carolina, Dept Phys & Astron, Chapel Hill, NC 27599 USA. [Jensen, Eric L. N.] Swarthmore Coll, Dept Phys & Astron, Swarthmore, PA 19081 USA. [Oberst, Thomas E.] Westminster Coll, Dept Phys, Wilmington, PA 16172 USA. RP Kuhn, RB (reprint author), S African Astron Observ, POB 9, ZA-7935 Cape Town, South Africa.; Rodriguez, JE (reprint author), Vanderbilt Univ, Dept Phys & Astron, 6301 Stevenson Ctr, Nashville, TN 37235 USA.; Pepper, J (reprint author), Lehigh Univ, Dept Phys, Bethlehem, PA 18015 USA. EM rudi@saao.ac.za; rodriguez.jr.joey@gmail.com; joshua.pepper@lehigh.edu OI Jensen, Eric/0000-0002-4625-7333; Tan, Thiam-Guan/0000-0001-5603-6895; Pepper, Joshua/0000-0002-3827-8417 FU NASA [NNX13AQ62G]; NSF CAREER [AST-1056524] FX KELT-South is hosted by the South African Astronomical Observatory and we are grateful for their ongoing support and assistance. KP acknowledges support from NASA grant NNX13AQ62G. Work by BSG and DJS was partially supported by NSF CAREER Grant AST-1056524. NR 103 TC 5 Z9 5 U1 3 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 JUL 11 PY 2016 VL 459 IS 4 BP 4281 EP 4298 DI 10.1093/mnras/stw880 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DR3VM UT WOS:000379830700067 ER PT J AU Kromer, M Fremling, C Pakmor, R Taubenberger, S Amanullah, R Cenko, SB Fransson, C Goobar, A Leloudas, G Taddia, F Ropke, FK Seitenzahl, IR Sim, SA Sollerman, J AF Kromer, M. Fremling, C. Pakmor, R. Taubenberger, S. Amanullah, R. Cenko, S. B. Fransson, C. Goobar, A. Leloudas, G. Taddia, F. Roepke, F. K. Seitenzahl, I. R. Sim, S. A. Sollerman, J. TI The peculiar Type Ia supernova iPTF14atg: Chandrasekhar-mass explosion or violent merger? SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE hydrodynamics; nuclear reactions, nucleosynthesis, abundances; radiative transfer; methods: numerical; supernovae: individual: iPTF14atg ID WHITE-DWARF MODELS; LATE-TIME SPECTROSCOPY; SN 2011FE; PROGENITOR SYSTEM; LIGHT CURVES; SYNTHETIC OBSERVABLES; SPECTRUM SYNTHESIS; STELLAR COMPANION; NEBULAR SPECTRA; SHOCK BREAKOUT AB iPTF14atg, a subluminous peculiar Type Ia supernova (SN Ia) similar to SN 2002es, is the first SN Ia for which a strong UV flash was observed in the early-time light curves. This has been interpreted as evidence for a single-degenerate (SD) progenitor system, where such a signal is expected from interactions between the SN ejecta and the non-degenerate companion star. Here, we compare synthetic observables of multidimensional state-of-the-art explosion models for different progenitor scenarios to the light curves and spectra of iPTF14atg. From our models, we have difficulties explaining the spectral evolution of iPTF14atg within the SD progenitor channel. In contrast, we find that a violent merger of two carbon-oxygen white dwarfs with 0.9 and 0.76 M-aS (TM), respectively, provides an excellent match to the spectral evolution of iPTF14atg from 10 d before to several weeks after maximum light. Our merger model does not naturally explain the initial UV flash of iPTF14atg. We discuss several possibilities like interactions of the SN ejecta with the circumstellar medium and surface radioactivity from an He-ignited merger that may be able to account for the early UV emission in violent merger models. C1 [Kromer, M.; Fremling, C.; Fransson, C.; Taddia, F.; Sollerman, J.] Stockholm Univ, Dept Astron, Oskar Klein Ctr, AlbaNova, SE-10691 Stockholm, Sweden. [Pakmor, R.; Roepke, F. K.] Heidelberger Inst Theoret Studien, Schloss Wolfsbrunnenweg 35, D-69118 Heidelberg, Germany. [Taubenberger, S.] European Southern Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany. [Taubenberger, S.] Max Planck Inst Astrophys, Karl Schwarzschild Str 1, D-85748 Garching, Germany. [Amanullah, R.; Goobar, A.] Stockholm Univ, Dept Phys, Oskar Klein Ctr, AlbaNova, SE-10691 Stockholm, Sweden. [Cenko, S. B.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Mail Code 661, Greenbelt, MD 20771 USA. [Leloudas, G.] Weizmann Inst Sci, Dept Particle Phys & Astrophys, IL-7610001 Rehovot, Israel. [Leloudas, G.] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, Juliane Maries Vej 30, DK-2100 Copenhagen, Denmark. [Roepke, F. K.] Heidelberg Univ, Zentrum Astron, Inst Theoret Astrophys, Philosophenweg 12, D-69120 Heidelberg, Germany. [Seitenzahl, I. R.] Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT 2611, Australia. [Seitenzahl, I. R.; Sim, S. A.] ARC Ctr Excellence All Sky Astrophys CAASTRO, Redfern, NSW, Australia. [Sim, S. A.] Queens Univ Belfast, Sch Math & Phys, Astrophys Res Ctr, Belfast BT7 1NN, Antrim, North Ireland. RP Kromer, M (reprint author), Stockholm Univ, Dept Astron, Oskar Klein Ctr, AlbaNova, SE-10691 Stockholm, Sweden. EM markus.kromer@astro.su.se OI Sollerman, Jesper/0000-0003-1546-6615 FU Knut and Alice Wallenberg Foundation; Swedish Research Council; Klaus Tschira Foundation; European Research Council under ERC-StG [EXAGAL-308037]; Deutsche Forschungsgemeinschaft via the Transregional Collaborative Research Center [TRR 33]; Swedish National Space Board; Australian Research Council [FL0992131]; German Federal Ministry of Education and Research (BMBF); German State Ministries for Research of Baden-Wurttemberg (MWK); Bayern (StMWFK); Nordrhein-Westfalen (MIWF) FX We gratefully acknowledge support from the Knut and Alice Wallenberg Foundation. The Oskar Klein Centre is funded by the Swedish Research Council. The work of RP and FKR is supported by the Klaus Tschira Foundation. RP also acknowledges support by the European Research Council under ERC-StG grant EXAGAL-308037. ST is supported by the Deutsche Forschungsgemeinschaft via the Transregional Collaborative Research Center TRR 33 'The Dark Universe'. AG and RA acknowledge support from the Swedish Research Council and the Swedish National Space Board. IRS was supported by the Australian Research Council Laureate Grant FL0992131.; The authors gratefully acknowledge the Gauss Centre for Super computing (GCS) for providing computing time through the John von Neumann Institute for Computing (NIC) on the GCS share of the supercomputer JUQUEEN (Stephan & Docter 2015) at Julich Supercomputing Centre (JSC). GCS is the alliance of the three national supercomputing centres HLRS (Universitat Stuttgart), JSC (Forschungszentrum Julich), and LRZ (Bayerische Akademie der Wissenschaften), funded by the German Federal Ministry of Education and Research (BMBF) and the German State Ministries for Research of Baden-Wurttemberg (MWK), Bayern (StMWFK), and Nordrhein-Westfalen (MIWF). 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 94 TC 2 Z9 2 U1 1 U2 2 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUL 11 PY 2016 VL 459 IS 4 BP 4428 EP 4439 DI 10.1093/mnras/stw962 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DR3VM UT WOS:000379830700077 ER PT J AU Gacesa, M Montgomery, JA Michels, HH Cote, R AF Gacesa, Marko Montgomery, John A., Jr. Michels, H. Harvey Cote, Robin TI Production of NaCa+ molecular ions in the ground state from cold atom-ion mixtures by photoassociation via an intermediate state SO PHYSICAL REVIEW A LA English DT Article ID LONG-RANGE MOLECULES; CHARGE-EXCHANGE; COLLISIONS; ELECTRON; EQUATION; CURVES; TRAP AB We present a theoretical analysis of optical pathways for formation of cold ground-state (NaCa)(+) molecular ions via an intermediate state. The formation schemes are based on ab initio potential energy curves and transition dipole moments calculated using effective-core-potential methods of quantum chemistry. In the proposed approach, starting from a mixture of cold trapped Ca+ ions immersed into an ultracold gas of Na atoms, (NaCa)(+) molecular ions are photoassociated in the excited E-1 Sigma(+) electronic state and allowed to spontaneously decay either to the ground electronic state or an intermediate state from which the population is transferred to the ground state via an additional optical excitation. By analyzing all possible pathways, we find that the efficiency of a two-photon scheme, via either the B-1 Sigma(+) or C-1 Sigma(+) potential, is sufficient to produce significant quantities of ground-state (NaCa)(+) molecular ions. A single-step process results in lower formation rates that would require either a high-density sample or a very intense photoassociation laser to be viable. C1 [Gacesa, Marko] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Gacesa, Marko; Montgomery, John A., Jr.; Michels, H. Harvey; Cote, Robin] Univ Connecticut, Dept Phys, Storrs, CT 06268 USA. RP Gacesa, M (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.; Gacesa, M (reprint author), Univ Connecticut, Dept Phys, Storrs, CT 06268 USA. EM marko.gacesa@nasa.gov FU MURI US Army Research Office [W911NF-14-1-0378]; National Science Foundation [PHY-1415560] FX The authors wish to thank W. W. Smith for useful discussions and an anonymous reviewer for suggestions that led to significant improvements of the manuscript. This work was partially supported by the MURI US Army Research Office Grant No. W911NF-14-1-0378 (MG) and by the PIF program of the National Science Foundation Grant No. PHY-1415560 (RC). NR 66 TC 1 Z9 1 U1 9 U2 12 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 JUL 11 PY 2016 VL 94 IS 1 AR 013407 DI 10.1103/PhysRevA.94.013407 PG 12 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA DQ8XV UT WOS:000379495900006 ER PT J AU Hitlin, DG Kim, JH Trevor, J Hoenk, M Hennessy, J Jewell, A Farrell, R McClish, M AF Hitlin, D. G. Kim, J. H. Trevor, J. Hoenk, M. Hennessy, J. Jewell, A. Farrell, R. McClish, M. TI An APD for the efficient detection of the fast scintillation component of BaF2 SO NUCLEAR INSTRUMENTS & METHODS IN PHYSICS RESEARCH SECTION A-ACCELERATORS SPECTROMETERS DETECTORS AND ASSOCIATED EQUIPMENT LA English DT Article DE Barium fluoride; Photosensors; APD; Solar blind; Superlattice; Atomic layer deposition AB Barium fluoride crystals are the baseline choice for the calorimeter of the Mu2e experiment at Fermilab. By the fast (decay time 0.9 ns) 220 nm scintillation component and discriminating against the larger slow (decay time 630 ns) 300 nm component, it is possible to build a radiation-hard calorimeter with good energy and time resolution and high rate capability. This requires a solid state photosensor with high quantum efficiency at 220 nm, discrimination against the 300 nm component and good rise and decay times. Progress on the development of such a sensor is presented. (C) 2015 Elsevier B.V. All rights reserved. C1 [Hitlin, D. G.; Kim, J. H.; Trevor, J.] CALTECH, Lauritsen Lab, Pasadena, CA 91125 USA. [Hoenk, M.; Hennessy, J.; Jewell, A.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Farrell, R.; McClish, M.] RMD Inc, Watertown, MA USA. RP Hitlin, DG (reprint author), CALTECH, Lauritsen Lab, Pasadena, CA 91125 USA. EM hitlin@caltech.edu OI Jung, Kyuhyun/0000-0001-8631-610X FU SBIR grant [DE-SC0011316] FX The development of this UV sensitive, solar-blind APD a collaborative effort of Caltech, Jet Propulsion Laboratory and RMD Inc., under SBIR grant DE-SC0011316 and with NASA and DOE funds. NR 10 TC 0 Z9 0 U1 3 U2 7 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0168-9002 EI 1872-9576 J9 NUCL INSTRUM METH A JI Nucl. Instrum. Methods Phys. Res. Sect. A-Accel. Spectrom. Dect. Assoc. Equip. PD JUL 11 PY 2016 VL 824 BP 119 EP 122 DI 10.1016/j.nima.2015.11.074 PG 4 WC Instruments & Instrumentation; Nuclear Science & Technology; Physics, Nuclear; Physics, Particles & Fields SC Instruments & Instrumentation; Nuclear Science & Technology; Physics GA DL1RD UT WOS:000375408700042 ER PT J AU Barlis, A Aguirre, J Stevenson, T AF Barlis, A. Aguirre, J. Stevenson, T. TI Kinetic inductance detectors for far-infrared spectroscopy SO NUCLEAR INSTRUMENTS & METHODS IN PHYSICS RESEARCH SECTION A-ACCELERATORS SPECTROMETERS DETECTORS AND ASSOCIATED EQUIPMENT LA English DT Article DE Kinetic inductance detectors; Superconducting detectors; Applied superconductivity AB The star formation mechanisms at work in the early universe remain one of the major unsolved problems of modern astrophysics. Many of the luminous galaxies present during the period of peak star formation (at redshift of about 2.5) were heavily enshrouded in dust, which makes observing their properties difficult at optical wavelengths. However, many spectral lines exist at far-infrared wavelengths that serve as tracers of star formation. Here, we describe a detector system suitable for a balloon-borne spectroscopic intensity mapping experiment at far-infrared wavelengths. The system uses lumped-element kinetic inductance detectors (KIDs), which have the potential to achieve high sensitivity and low noise levels. KIDs consist of separate capacitive and inductive elements, and use the inductive element as the radiation absorber. We describe the design considerations, fabrication process, and readout scheme for a prototype LEKID array of 1600 pixels. (C) 2015 Elsevier B.V. All rights reserved. C1 [Barlis, A.; Aguirre, J.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. [Stevenson, T.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA. RP Barlis, A (reprint author), Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. EM abarlis@physics.upenn.edu FU NASA Space Technology Research Fellowship [NNX13AL68H] FX This work was supported by a NASA Space Technology Research Fellowship (grant #NNX13AL68H). The authors thank the members of the Detector Development Laboratory at NASA Goddard Space Flight Center for sharing their expertise on the KID fabrication process. NR 2 TC 0 Z9 0 U1 3 U2 5 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0168-9002 EI 1872-9576 J9 NUCL INSTRUM METH A JI Nucl. Instrum. Methods Phys. Res. Sect. A-Accel. Spectrom. Dect. Assoc. Equip. PD JUL 11 PY 2016 VL 824 BP 165 EP 167 DI 10.1016/j.nima.2015.12.022 PG 3 WC Instruments & Instrumentation; Nuclear Science & Technology; Physics, Nuclear; Physics, Particles & Fields SC Instruments & Instrumentation; Nuclear Science & Technology; Physics GA DL1RD UT WOS:000375408700057 ER PT J AU Nucciotti, A Alpert, B Becker, D Bennett, D Biasotti, M Brofferio, C Ceriale, V Ceruti, G Corsini, D Day, P De Gerone, M Dressler, R Faverzani, M Ferri, E Fowler, J Fumagalli, E Gard, J Gatti, F Giachero, A Hays-Wehle, J Heinitz, S Hilton, G Koester, U Lusignoli, M Maino, M Mates, J Nisi, S Nizzolo, R Orlando, A Parodi, L Pessina, G Pizzigoni, G Puiu, A Ragazzi, S Reintsema, C Ribeiro-Gomes, M Schmidt, D Schumann, D Siccardi, F Sisti, M Swetz, D Terranova, F Ullom, J Vale, L AF Nucciotti, A. Alpert, B. Becker, D. Bennett, D. Biasotti, M. Brofferio, C. Ceriale, V. Ceruti, G. Corsini, D. Day, P. De Gerone, M. Dressler, R. Faverzani, M. Ferri, E. Fowler, J. Fumagalli, E. Gard, J. Gatti, F. Giachero, A. Hays-Wehle, J. Heinitz, S. Hilton, G. Koester, U. Lusignoli, M. Maino, M. Mates, J. Nisi, S. Nizzolo, R. Orlando, A. Parodi, L. Pessina, G. Pizzigoni, G. Puiu, A. Ragazzi, S. Reintsema, C. Ribeiro-Gomes, M. Schmidt, D. Schumann, D. Siccardi, F. Sisti, M. Swetz, D. Terranova, F. Ullom, J. Vale, L. TI Status of the HOLMES detector development SO NUCLEAR INSTRUMENTS & METHODS IN PHYSICS RESEARCH SECTION A-ACCELERATORS SPECTROMETERS DETECTORS AND ASSOCIATED EQUIPMENT LA English DT Article DE Neutrino mass; Ho-163; Electron capture; Low temperature detectors ID ELECTRON NEUTRINO MASS; HO-163; DECAY AB HOLMES is a new experiment to directly measure the neutrino mass with a sensitivity as low as 0.4 eV. HOLMES will perform a calorimetric measurement of the energy released in the electron capture decay of Ho-163. HOLMES will deploy a large array of low temperature microcalorimeters with implanted Ho-163 nuclei. HOLMES baseline detector is an array of 1000 microcalorimeters each with an implanted Ho-163 activity of about 300 Bq, an energy resolution FVVHM of about 1 eV at the spectrum end-point (Q approximate to 2.5 keV), and a time resolution of about 1 mu s. Matching these performances requires a careful optimization of all components, from the microcalorimeters to the signal processing algorithms. We outline here the project technical challenges and the present status of the development. (C) 2015 Elsevier B.V. All rights reserved. C1 [Nucciotti, A.; Brofferio, C.; Faverzani, M.; Ferri, E.; Nizzolo, R.; Puiu, A.; Ragazzi, S.; Sisti, M.; Terranova, F.] Univ Milano Bicocca, Dipartimento Fis, Milan, Italy. [Nucciotti, A.; Brofferio, C.; Ceruti, G.; Faverzani, M.; Ferri, E.; Giachero, A.; Maino, M.; Pessina, G.; Puiu, A.; Ragazzi, S.; Sisti, M.; Terranova, F.] Ist Nazl Fis Nucl, Sezi Milano Bicocca, Via Celoria 16, I-20133 Milan, Italy. [Biasotti, M.; Ceriale, V.; Corsini, D.; De Gerone, M.; Fumagalli, E.; Gatti, F.; Orlando, A.; Parodi, L.; Pizzigoni, G.; Schumann, D.; Siccardi, F.] Ist Nazl Fis Nucl, Sez Genova, Via Dodecaneso 33, I-16146 Genoa, Italy. [Day, P.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Dressler, R.; Heinitz, S.] Paul Scherrer Inst, Villigen, Switzerland. [Alpert, B.; Becker, D.; Bennett, D.; Fowler, J.; Gard, J.; Hays-Wehle, J.; Hilton, G.; Mates, J.; Reintsema, C.; Schmidt, D.; Swetz, D.; Ullom, J.; Vale, L.] NIST, Boulder, CO USA. [Koester, U.] Inst Laue Langevin, Grenoble, France. [Nisi, S.] Ist Nazl Fis Nucl, Lab Nazl Gran Sasso, Assergi, AQ, Italy. [Lusignoli, M.] Ist Nazl Fis Nucl, Sez Roma 1, Rome, Italy. [Ribeiro-Gomes, M.] Univ Lisbon, Multidisciplinary Ctr Astrophysics CENTRA IST, P-1699 Lisbon, Portugal. RP Nucciotti, A (reprint author), Univ Milano Bicocca, Dipartimento Fis, Milan, Italy. EM angelo.nucciotti@mib.infn.it RI Giachero, Andrea/I-1081-2013; Sisti, Monica/B-7550-2013; Ferri, Elena/L-8531-2014; Biasotti, Michele/C-7890-2017 OI Giachero, Andrea/0000-0003-0493-695X; Sisti, Monica/0000-0003-2517-1909; De Gerone, Matteo/0000-0002-5489-6581; Ferri, Elena/0000-0003-1425-3669; Pessina, Gianluigi Ezio/0000-0003-3700-9757; Biasotti, Michele/0000-0002-7241-8479 FU European Research Council under the European Union's Seventh Framework Programme (FP7)/ERC [340321]; NIST Innovations in Measurement Science program for the TES detector development FX The HOLMES experiment is funded by the European Research Council under the European Union's Seventh Framework Programme (FP7/2007-2013)/ERC Grant Agreement no. 340321. We also acknowledge support from the NIST Innovations in Measurement Science program for the TES detector development. NR 6 TC 0 Z9 0 U1 3 U2 6 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0168-9002 EI 1872-9576 J9 NUCL INSTRUM METH A JI Nucl. Instrum. Methods Phys. Res. Sect. A-Accel. Spectrom. Dect. Assoc. Equip. PD JUL 11 PY 2016 VL 824 BP 182 EP 183 DI 10.1016/j.nima.2015.09.066 PG 2 WC Instruments & Instrumentation; Nuclear Science & Technology; Physics, Nuclear; Physics, Particles & Fields SC Instruments & Instrumentation; Nuclear Science & Technology; Physics GA DL1RD UT WOS:000375408700062 ER PT J AU Pizzigoni, G Alpert, B Balata, M Bennett, D Biasotti, M Boragno, C Brofferio, C De Gerone, M Dressler, R Faverazani, M Ferri, E Folwer, J Gatti, F Giachero, A Heinitz, S Hilton, G Koster, U Lusignoli, M Maino, M Mates, J Nisi, S Nizzolo, R Nucciotti, A Pessina, G Puiu, A Ragazzi, S Reintsema, C Gomes, MR Shmidt, D Schumann, D Sisti, M Swetz, D Terranova, F Ullom, J Day, PK AF Pizzigoni, G. Alpert, B. Balata, M. Bennett, D. Biasotti, M. Boragno, C. Brofferio, C. De Gerone, M. Dressler, R. Faverazani, M. Ferri, E. Folwer, J. Gatti, F. Giachero, A. Heinitz, S. Hilton, G. Koster, U. Lusignoli, M. Maino, M. Mates, J. Nisi, S. Nizzolo, R. Nucciotti, A. Pessina, G. Puiu, A. Ragazzi, S. Reintsema, C. Ribeiro Gomes, M. Shmidt, D. Schumann, D. Sisti, M. Swetz, D. Terranova, F. Ullom, J. Day, P. K. TI Inside HOLMES experiment: Ho-163 metallic target production for the micro-calorimeter absorber SO NUCLEAR INSTRUMENTS & METHODS IN PHYSICS RESEARCH SECTION A-ACCELERATORS SPECTROMETERS DETECTORS AND ASSOCIATED EQUIPMENT LA English DT Article DE Neutrino mass; Holmes experiment; Reduction and distillation process AB The main goal in the HOLMES experiment is the neutrino mass measurement using an array of 1000 micro-calorimeters with standard metallic absorber. A good isotope for such measurement is the Ho-163, those isotopes embedded in the metallic absorber will be 10(11)-10(13). Since Ho-163 is not available in nature, a dedicated process must be set up to produce the amount needed for this neutrino mass experiment. The process with the highest born-up cross-section is the neutron irradiation of Er2O3 enriched in Er-162: Er-162(n,gamma)Er-163 -> Ho-163 +v(e), where the decay is an EC with half-life of about 75 min and the (n,gamma) is about 20 barns for thermal neutron. After the neutron irradiation in the oxide powder there are several radioactive isotopes which are potentially disturbing because of the background that they cause below 5 keV. The chemical separation of holmium from the irradiation enriched Er2O3 powder is therefore mandatory and will be performed by means of ion exchange chromatography. On the end of those processes the oxide powder enriched in 162Er will have the 163Ho isotope number required. The holmium chemical state influences the end point of the EC spectrum, in order to avoid such effect it is necessary to embed in the absorber only the metallic isotope. Reduction and distillation technique allowed us to obtain a pure metallic holmium, starting from natural oxide holmium. This technique will be applied on the irradiated oxide powder to obtain the metallic Ho-163, ready to be embedded in the micro-calorimeter absorber. (C) 2015 Elsevier B.V. All rights reserved. C1 [Pizzigoni, G.; Biasotti, M.; Boragno, C.; De Gerone, M.; Gatti, F.] Univ Genoa, Dipartimento Fis, Genoa, Italy. [Pizzigoni, G.; Biasotti, M.; Boragno, C.; De Gerone, M.; Gatti, F.] Ist Nazl Fis Nucl, Sez Genova, Via Dodecaneso 33, I-16146 Genoa, Italy. [Alpert, B.; Bennett, D.; Folwer, J.; Mates, J.; Reintsema, C.; Shmidt, D.; Swetz, D.; Ullom, J.] NIST, Boulder, CO USA. [Balata, M.; Nisi, S.] Ist Nazl Fis Nucl, Lab Nazl Gran Sasso, Assergi, AQ, Italy. [Brofferio, C.; Faverazani, M.; Ferri, E.; Giachero, A.; Maino, M.; Nizzolo, R.; Nucciotti, A.; Puiu, A.; Ragazzi, S.; Sisti, M.; Terranova, F.] Univ Milano Bicocca, Dipartimento Fis, Milan, Italy. [Brofferio, C.; Faverazani, M.; Ferri, E.; Giachero, A.; Maino, M.; Nizzolo, R.; Nucciotti, A.; Pessina, G.; Puiu, A.; Ragazzi, S.; Sisti, M.; Terranova, F.] Ist Nazl Fis Nucl, Sez Milano Bicocca, Via Celoria 16, I-20133 Milan, Italy. [Day, P. K.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Dressler, R.; Heinitz, S.; Hilton, G.; Schumann, D.] Paul Scherrer Inst, Villigen, Switzerland. [Lusignoli, M.] Inst Laue Langevin, Grenoble, France. [Koster, U.] Ist Nazl Fis Nucl, Sez Roma 1, Rome, Italy. [Ribeiro Gomes, M.] Univ Lisbon, Multidisciplinary Ctr Astrophys CENTRA IST, P-1699 Lisbon, Portugal. RP Pizzigoni, G (reprint author), Univ Genoa, Dipartimento Fis, Genoa, Italy. EM giulio.pizzigoni@ge.infn.it RI Giachero, Andrea/I-1081-2013; Ferri, Elena/L-8531-2014; Biasotti, Michele/C-7890-2017; Sisti, Monica/B-7550-2013 OI Giachero, Andrea/0000-0003-0493-695X; Ferri, Elena/0000-0003-1425-3669; Biasotti, Michele/0000-0002-7241-8479; Sisti, Monica/0000-0003-2517-1909 FU European Research Council under the European Union's Seventh Framework Programme (FP7)/ERC Grant [340321] FX The HOLMES experiment is funded by the European Research Council under the European Union's Seventh Framework Programme (FP7/2007-2013)/ERC Grant Agreement no. 340321. We would like to thank Professor P. Manfrinetti for his useful contributions. NR 6 TC 2 Z9 2 U1 3 U2 7 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0168-9002 EI 1872-9576 J9 NUCL INSTRUM METH A JI Nucl. Instrum. Methods Phys. Res. Sect. A-Accel. Spectrom. Dect. Assoc. Equip. PD JUL 11 PY 2016 VL 824 BP 223 EP 225 DI 10.1016/j.nima.2015.11.020 PG 3 WC Instruments & Instrumentation; Nuclear Science & Technology; Physics, Nuclear; Physics, Particles & Fields SC Instruments & Instrumentation; Nuclear Science & Technology; Physics GA DL1RD UT WOS:000375408700078 ER PT J AU Benford, JN Benford, DJ AF Benford, James N. Benford, Dominic J. TI POWER BEAMING LEAKAGE RADIATION AS A SETI OBSERVABLE SO ASTROPHYSICAL JOURNAL LA English DT Article DE extraterrestrial intelligence; space vehicles; stars: individual (KIC 8462852) ID DEEP SPACE EXPLORATION; INTERSTELLAR COMMUNICATION; ENERGY; EARTH AB The most observable leakage radiation from an advanced civilization may well be from the use of power beaming to transfer energy and accelerate spacecraft. Applications suggested for power beaming involve launching spacecraft to orbit, raising satellites to a higher orbit, and interplanetary concepts involving space-to-space transfers of cargo or passengers. We also quantify beam-driven launch to the outer solar system, interstellar precursors, and ultimately starships. We estimate the principal observable parameters of power beaming leakage. Extraterrestrial civilizations would know their power beams could be observed, and so could put a message on the power beam and broadcast it for our receipt at little additional energy or cost. By observing leakage from power beams we may find a message embedded on the beam. Recent observations of the anomalous star KIC 8462852 by the Allen Telescope Array (ATA) set some limits on extraterrestrial power beaming in that system. We show that most power beaming applications commensurate with those suggested for our solar system would be detectable if using the frequency range monitored by the ATA, and so the lack of detection is a meaningful, if modest, constraint on extraterrestrial power beaming in that system. Until more extensive observations are made, the limited observation time and frequency coverage are not sufficiently broad in frequency and duration to produce firm conclusions. Such beams would be visible over large interstellar distances. This implies a new approach to the SETI search: instead of focusing on narrowband beacon transmissions generated by another civilization, look for more powerful beams with much wider bandwidth. This requires a new approach for their discovery by telescopes on Earth. Further studies of power beaming applications should be performed, potentially broadening the parameter space of the observable features that we have discussed here. C1 [Benford, James N.] Microwave Sci, 1041 Los Arabis Lane, Lafayette, CA 94549 USA. [Benford, Dominic J.] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA. RP Benford, JN (reprint author), Microwave Sci, 1041 Los Arabis Lane, Lafayette, CA 94549 USA. EM jimbenford@gmail.com RI Benford, Dominic/D-4760-2012 OI Benford, Dominic/0000-0002-9884-4206 NR 28 TC 0 Z9 0 U1 1 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 10 PY 2016 VL 825 IS 2 AR 101 DI 10.3847/0004-637X/825/2/101 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DU1BM UT WOS:000381940800019 ER PT J AU Dwek, E AF Dwek, Eli TI IRON: A KEY ELEMENT FOR UNDERSTANDING THE ORIGIN AND EVOLUTION OF INTERSTELLAR DUST SO ASTROPHYSICAL JOURNAL LA English DT Article DE dust, extinction; Galaxy: abundances; ISM: abundances; nuclear reactions, nucleosynthesis, abundances; supernovae: general; solar neighborhood ID KEPLERS SUPERNOVA REMNANT; CORE-COLLAPSE SUPERNOVAE; SPITZER-SPACE-TELESCOPE; IA SUPERNOVAE; SOLAR NEIGHBORHOOD; CHEMICAL EVOLUTION; NUMERICAL SIMULATIONS; INFRARED-EMISSION; GALACTIC-CENTER; MASSIVE SINGLE AB The origin and depletion of iron differ from all other abundant refractory elements that make up the composition of interstellar dust. Iron is primarily synthesized in Type Ia supernovae (SNe Ia) and in core collapse supernovae (CCSN), and is present in the outflows from AGB stars. Only the latter two are observed to be sources of interstellar dust since searches for dust in SN Ia have provided strong evidence for the absence of any significant mass of dust in their ejecta. Consequently, more than 65% of the iron is injected into the ISM in gaseous form. Yet ultraviolet and X-ray observations along many lines of sight in the ISM show that iron is severely depleted in the gas phase as compared to expected solar abundances. The missing iron, comprising about 90% of the total, is believed to be locked up in interstellar dust. This suggests that most of the missing iron must have precipitated from the ISM gas by a cold accretion onto preexisting silicate, carbon, or composite grains. Iron is thus the only element that requires most of its growth to occur outside the traditional stellar condensation sources. This is a robust statement that does not depend on our evolving understanding of the dust destruction efficiency in the ISM. Reconciling the physical, optical, and chemical properties of such composite grains with their many observational manifestations is a major challenge for understanding the nature and origin of interstellar dust. C1 [Dwek, Eli] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Code 665, Greenbelt, MD 20771 USA. RP Dwek, E (reprint author), NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Code 665, Greenbelt, MD 20771 USA. EM eli.dwek@nasa.gov FU NASA's research grants [12-ADP12-0145, 13-ADAP13-0094] FX In writing this paper I have benefited from many enlightening conversations with Joe Nuth, and useful references provided by Steven Rodney. J.N. and Rick Arendt provided useful comments on an early version of the manuscript. I thank the referees, Xander Tielens and Anthony Jones, for their critical comments, which led to improvements in the manuscript. This work was supported by NASA's 12-ADP12-0145 and 13-ADAP13-0094 research grants. NR 74 TC 3 Z9 3 U1 3 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 10 PY 2016 VL 825 IS 2 AR 136 DI 10.3847/0004-637X/825/2/136 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DU1BM UT WOS:000381940800054 ER PT J AU Eingorn, M AF Eingorn, Maxim TI FIRST-ORDER COSMOLOGICAL PERTURBATIONS ENGENDERED BY POINT-LIKE MASSES SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmological parameters; cosmology: theory; dark energy; dark matter; gravitation; large-scale structure of universe ID UNIVERSE; SIMULATIONS; HOMOGENEITY; SCALE AB In the framework of the concordance cosmological model, the first-order scalar and vector perturbations of the homogeneous background are derived in the weak gravitational field limit without any supplementary approximations. The sources of these perturbations (inhomogeneities) are presented in the discrete form of a system of separate point-like gravitating masses. The expressions found for the metric corrections are valid at all (sub-horizon and super-horizon) scales and converge at all points except at the locations of the sources. The average values of these metric corrections are zero (thus, first-order backreaction effects are absent). Both the Minkowski background limit and the Newtonian cosmological approximation are reached under certain well-defined conditions. An important feature of the velocity-independent part of the scalar perturbation is revealed: up to an additive constant, this part represents a sum of Yukawa potentials produced by inhomogeneities with the same finite time-dependent Yukawa interaction range. The suggested connection between this range and the homogeneity scale is briefly discussed along with other possible physical implications. C1 [Eingorn, Maxim] North Carolina Cent Univ, CREST, Fayetteville St 1801, Durham, NC 27707 USA. [Eingorn, Maxim] NASA, Res Ctr, Fayetteville St 1801, Durham, NC 27707 USA. RP Eingorn, M (reprint author), North Carolina Cent Univ, CREST, Fayetteville St 1801, Durham, NC 27707 USA.; Eingorn, M (reprint author), NASA, Res Ctr, Fayetteville St 1801, Durham, NC 27707 USA. EM maxim.eingorn@gmail.com RI Eingorn, Maxim/L-1543-2014 OI Eingorn, Maxim/0000-0002-1545-7818 FU NSF CREST award [HRD-1345219]; NASA grant [NNX09AV07A] FX This work was supported by NSF CREST award HRD-1345219 and NASA grant NNX09AV07A. I would like to thank the anonymous referee for valuable comments that have considerably improved the discussion of the derived results. I am also grateful to my colleague Prof. Diane Markoff for the careful review of their presentation. NR 46 TC 5 Z9 5 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 10 PY 2016 VL 825 IS 2 AR 84 DI 10.3847/0004-637X/825/2/84 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DU1BM UT WOS:000381940800002 ER PT J AU Elmegreen, DM Elmegreen, BG Almeida, JS Munoz-Tunon, C Mendez-Abreu, J Gallagher, JS Rafelski, M Filho, M Ceverino, D AF Elmegreen, Debra Meloy Elmegreen, Bruce G. Sanchez Almeida, Jorge Munoz-Tunon, Casiana Mendez-Abreu, Jairo Gallagher, John S. Rafelski, Marc Filho, Mercedes Ceverino, Daniel TI HUBBLE SPACE TELESCOPE OBSERVATIONS OF ACCRETION-INDUCED STAR FORMATION IN THE TADPOLE GALAXY KISO 5639 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: dwarf; galaxies: individual (Kiso 5639); galaxies: photometry; galaxies: star clusters: general; galaxies: star formation; H II regions ID COMPACT DWARF GALAXIES; ULTRA DEEP FIELD; ALPHA ESCAPE FRACTION; METAL-POOR GALAXIES; I ZW 18; FORMING GALAXIES; NEARBY GALAXIES; FORMATION LAW; INTEGRATED PHOTOMETRY; IRREGULAR GALAXIES AB The tadpole galaxy Kiso 5639 has a slowly rotating disk with a drop in metallicity at its star-forming head, suggesting that star formation was triggered by the accretion of metal-poor gas. We present multi-wavelength Hubble Space Telescope Wide Field Camera 3 images of UV through I band plus H alpha to search for peripheral emission and determine the properties of various regions. The head has a mass in young stars of similar to 10(6) M-circle dot and an ionization rate of 6.4 x 10(51) s(-1), equivalent to similar to 2100 O9-type stars. There are four older star-forming regions in the tail, and an underlying disk with a photometric age of similar to 1 Gyr. The mass distribution function of 61 star clusters is a power law with a slope of -1.73 +/- 0.51. Fourteen young clusters in the head are more massive than 10(4) M-circle dot, suggesting a clustering fraction of 30%-45%. Wispy filaments of Ha emission and young stars extend away from the galaxy. Shells and holes in the head H II region could be from winds and supernovae. Gravity from the disk should limit the expansion of the H II region, although hot gas might escape through the holes. The star formation surface density determined from Ha in the head is compared to that expected from likely pre-existing and accreted gas. Unless the surface density of the accreted gas is a factor of similar to 3 or more larger than what was in the galaxy before, the star formation rate has to exceed the usual Kennicutt-Schmidt rate by a factor of >= 5. C1 [Elmegreen, Debra Meloy] Vassar Coll, Dept Phys & Astron, Poughkeepsie, NY 12604 USA. [Elmegreen, Bruce G.] IBM Res Div, TJ Watson Res Ctr, Yorktown Hts, NY 10598 USA. [Sanchez Almeida, Jorge; Munoz-Tunon, Casiana; Filho, Mercedes] Inst Astrofis Canarias, C Via Lactea S-N, E-38205 Tenerife, Spain. [Sanchez Almeida, Jorge; Munoz-Tunon, Casiana; Filho, Mercedes] Univ La Laguna, Dept Astrofis, E-38207 San Cristobal la Laguna, Spain. [Mendez-Abreu, Jairo] Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland. [Gallagher, John S.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. [Rafelski, Marc] Goddard Space Flight Ctr, Astrophys Sci Div, Code 665, Greenbelt, MD 20771 USA. [Ceverino, Daniel] Heidelberg Univ, Zentrum Astron, Inst Theoret Astrophys, Albert Ueberle Str 2, D-69120 Heidelberg, Germany. RP Elmegreen, DM (reprint author), Vassar Coll, Dept Phys & Astron, Poughkeepsie, NY 12604 USA. OI Elmegreen, Debra/0000-0002-1392-3520; Mendez Abreu, Jairo/0000-0002-8766-2597 FU NASA; STScI; Spanish Ministry of Economy and Competitiveness [AYA2013-47742-C4-2-P]; European Research Council Starting Grant (SEDmorph); European Research Council Advanced Grant (STARLIGHT); National Aeronautics and Space Administration; Jesus Serra Foundation; [HST-GO-13723.002-A]; [HST-GO-13723.001-A] FX We thank NASA and STScI for observing time and grant support. DME is supported by HST-GO-13723.002-A and BGE is supported by HST-GO-13723.001-A; both are grateful to the Severo Ochoa and Jesus Serra Foundation for support during a visit to the Instituto de Astrofisica de Canarias. The work of JSA, CMT, and MF has been partly funded by the Spanish Ministry of Economy and Competitiveness, project AYA2013-47742-C4-2-P. JMA acknowledges support from the European Research Council Starting Grant (SEDmorph; P. I. V. Wild). MR acknowledges support from an appointment to the NASA Postdoctoral Program at Goddard Space Flight Center. DC acknowledges support from the European Research Council Advanced Grant (STARLIGHT; P. I. Ralf Klessen) 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 74 TC 1 Z9 1 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 10 PY 2016 VL 825 IS 2 AR 145 DI 10.3847/0004-637X/825/2/145 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DU1BM UT WOS:000381940800063 ER PT J AU Farr, B Berry, CPL Farr, WM Haster, CJ Middleton, H Cannon, K Graff, PB Hanna, C Mandel, I Pankow, C Price, LR Sidery, T Singer, LP Urban, AL Vecchio, A Veitch, J Vitale, S AF Farr, Ben Berry, Christopher P. L. Farr, Will M. Haster, Carl-Johan Middleton, Hannah Cannon, Kipp Graff, Philip B. Hanna, Chad Mandel, Ilya Pankow, Chris Price, Larry R. Sidery, Trevor Singer, Leo P. Urban, Alex L. Vecchio, Alberto Veitch, John Vitale, Salvatore TI PARAMETER ESTIMATION ON GRAVITATIONAL WAVES FROM NEUTRON-STAR BINARIES WITH SPINNING COMPONENTS SO ASTROPHYSICAL JOURNAL LA English DT Article DE gravitational waves; methods: data analysis; stars: neutron; surveys ID COMPACT-OBJECT BINARIES; BLACK-HOLES; MASS-DISTRIBUTION; ADVANCED LIGO; FOLLOW-UP; RADIATION; MERGERS; VIRGO; COALESCENCE; TRANSIENTS AB Inspiraling binary neutron stars (BNSs) are expected to be one of the most significant sources of gravitational-wave signals for the new generation of advanced ground-based detectors. We investigate how well we could hope to measure properties of these binaries using the Advanced LIGO detectors, which began operation in September 2015. We study an astrophysically motivated population of sources (binary components with masses 1.2 M-circle dot-1.6 M-circle dot and spins of less than 0.05) using the full LIGO analysis pipeline. While this simulated population covers the observed range of potential BNS sources, we do not exclude the possibility of sources with parameters outside these ranges; given the existing uncertainty in distributions of mass and spin, it is critical that analyses account for the full range of possible mass and spin configurations. We find that conservative prior assumptions on neutron-star mass and spin lead to average fractional uncertainties in component masses of similar to 16%, with little constraint on spins (the median 90% upper limit on the spin of the more massive component is similar to 0.7). Stronger prior constraints on neutron-star spins can further constrain mass estimates but only marginally. However, we find that the sky position and luminosity distance for these sources are not influenced by the inclusion of spin; therefore, if LIGO detects a low-spin population of BNS sources, less computationally expensive results calculated neglecting spin will be sufficient for guiding electromagnetic follow-up. C1 [Farr, Ben] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [Farr, Ben] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Berry, Christopher P. L.; Farr, Will M.; Haster, Carl-Johan; Middleton, Hannah; Mandel, Ilya; Sidery, Trevor; Vecchio, Alberto; Veitch, John] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. [Cannon, Kipp] Univ Toronto, Canadian Inst Theoret Astrophys, 60 St George St, Toronto, ON M5S 3H8, Canada. [Graff, Philip B.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA. [Graff, Philip B.] NASA, Goddard Space Flight Ctr, Gravitat Astrophys Lab, Greenbelt, MD 20771 USA. [Hanna, Chad] Penn State Univ, University Pk, PA 16802 USA. [Pankow, Chris; Urban, Alex L.] Univ Wisconsin, Leonard E Parker Ctr Gravitat Cosmol & Astrophys, Milwaukee, WI 53201 USA. [Price, Larry R.] CALTECH, LIGO Lab, Pasadena, CA 91125 USA. [Singer, Leo P.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Code 661, Greenbelt, MD 20771 USA. [Vitale, Salvatore] MIT, 185 Albany St, Cambridge, MA 02139 USA. RP Farr, B (reprint author), Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA.; Farr, B (reprint author), Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. EM farr@uchicago.edu RI Vecchio, Alberto/F-8310-2015; OI Vecchio, Alberto/0000-0002-6254-1617; Farr, Will/0000-0003-1540-8562; Berry, Christopher/0000-0003-3870-7215; Mandel, Ilya/0000-0002-6134-8946; Veitch, John/0000-0002-6508-0713 FU Enrico Fermi Institute at the University of Chicago as a McCormick Fellow; Science and Technology Facilities Council; NASA [NNX12AN10G]; National Science Foundation; LIGO Laboratory; STFC [ST/K005014/1]; National Science Foundation [PHY-0757058]; NSF [PHY-1126812]; LIGO Data Grid including: the Nemo computing cluster at the Center for Gravitation and Cosmology at the University of Wisconsin-Milwaukee under NSF [PHY-0923409, PHY-0600953]; Atlas computing cluster at the Albert Einstein Institute, Hannover; LIGO computing clusters at Caltech FX B.F. was supported by the Enrico Fermi Institute at the University of Chicago as a McCormick Fellow. This work was supported in part by the Science and Technology Facilities Council. P.B.G. acknowledges NASA grant NNX12AN10G. S.V. acknowledges the support of the National Science Foundation and the LIGO Laboratory. J.V. was supported by STFC grant ST/K005014/1. LIGO was constructed by the California Institute of Technology and Massachusetts Institute of Technology with funding from the National Science Foundation and operates under cooperative agreement PHY-0757058.; This work used computing resources at CIERA funded by NSF PHY-1126812, as well as the computing facilities of the LIGO Data Grid including: the Nemo computing cluster at the Center for Gravitation and Cosmology at the University of Wisconsin-Milwaukee under NSF Grants PHY-0923409 and PHY-0600953; the Atlas computing cluster at the Albert Einstein Institute, Hannover; the LIGO computing clusters at Caltech, and the facilities of the Advanced Research Computing @ Cardiff (ARCCA) Cluster at Cardiff University. NR 63 TC 3 Z9 3 U1 1 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 10 PY 2016 VL 825 IS 2 AR 116 DI 10.3847/0004-637X/825/2/116 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DU1BM UT WOS:000381940800034 ER PT J AU Hong, J Mori, K Hailey, CJ Nynka, M Zhang, S Gotthelf, E Fornasini, FM Krivonos, R Bauer, F Perez, K Tomsick, JA Bodaghee, A Chiu, JL Clavel, M Stern, D Grindlay, JE Alexander, DM Aramaki, T Baganoff, FK Barret, D Barriere, N Boggs, SE Canipe, AM Christensen, FE Craig, WW Desai, MA Forster, K Giommi, P Grefenstette, BW Harrison, FA Hong, D Hornstrup, A Kitaguchi, T Koglin, JE Madsen, KK Mao, PH Miyasaka, H Perri, M Pivovaroff, MJ Puccetti, S Rana, V Westergaard, NJ Zhang, WW Zoglauer, A AF Hong, JaeSub Mori, Kaya Hailey, Charles J. Nynka, Melania Zhang, Shuo Gotthelf, Eric Fornasini, Francesca M. Krivonos, Roman Bauer, Franz Perez, Kerstin Tomsick, John A. Bodaghee, Arash Chiu, Jeng-Lun Clavel, Maica Stern, Daniel Grindlay, Jonathan E. Alexander, David M. Aramaki, Tsuguo Baganoff, Frederick K. Barret, Didier Barriere, Nicolas Boggs, Steven E. Canipe, Alicia M. Christensen, Finn E. Craig, William W. Desai, Meera A. Forster, Karl Giommi, Paolo Grefenstette, Brian W. Harrison, Fiona A. Hong, Dooran Hornstrup, Allan Kitaguchi, Takao Koglin, Jason E. Madsen, Kristen K. Mao, Peter H. Miyasaka, Hiromasa Perri, Matteo Pivovaroff, Michael J. Puccetti, Simonetta Rana, Vikram Westergaard, Niels J. Zhang, William W. Zoglauer, Andreas TI NuSTAR HARD X-RAY SURVEY OF THE GALACTIC CENTER REGION. II. X-RAY POINT SOURCES SO ASTROPHYSICAL JOURNAL LA English DT Article DE Galaxy: center; X-rays: binaries; X-rays: diffuse background; X-rays: general ID MAGNETIC CATACLYSMIC VARIABLES; SUPERNOVA-REMNANT SAGITTARIUS; XMM-NEWTON OBSERVATIONS; BURSTING PULSAR; CHANDRA CATALOG; LIMITING WINDOW; GRS 1741.9-2853; NUMBER COUNTS; V404 CYGNI; A-ASTERISK AB We present the first survey results of hard X-ray point sources in the Galactic Center (GC) region by NuSTAR. We have discovered 70 hard (3-79 keV) X-ray point sources in a 0.6 deg(2) region around Sgr A* with a total exposure of 1.7 Ms, and 7 sources in the Sgr B2 field with 300 ks. We identify clear Chandra counterparts for 58 NuSTAR sources and assign candidate counterparts for the remaining 19. The NuSTAR survey reaches X-ray luminosities of similar to 4x and similar to 8 x 10(32) erg s(-1) at the GC (8 kpc) in the 3-10 and 10-40 keV bands, respectively. The source list includes three persistent luminous X-ray binaries (XBs) and the likely run-away pulsar called the Cannonball. New source-detection significance maps reveal a cluster of hard (>10 keV) X-ray sources near the Sgr. A diffuse complex with no clear soft X-ray counterparts. The severe extinction observed in the Chandra spectra indicates that all the NuSTAR sources are in the central bulge or are of extragalactic origin. Spectral analysis of relatively bright NuSTAR sources suggests that magnetic cataclysmic variables constitute a large fraction (>40%-60%). Both spectral analysis and logN-logS distributions of the NuSTAR sources indicate that the X-ray spectra of the NuSTAR sources should have kT > 20 keV on average for a single temperature thermal plasma model or an average photon index of Gamma = 1.5-2 for a power-law model. These findings suggest that the GC X-ray source population may contain a larger fraction of XBs with high plasma temperatures than the field population. C1 [Hong, JaeSub; Grindlay, Jonathan E.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Mori, Kaya; Hailey, Charles J.; Nynka, Melania; Zhang, Shuo; Gotthelf, Eric; Canipe, Alicia M.; Desai, Meera A.; Hong, Dooran] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Gotthelf, Eric] Univ Barcelona, Dept Fis Quant & Astrofis, Inst Ciencies Cosmos, IEEC UB, Marti & Franques 1, Barcelona 08028, Spain. [Fornasini, Francesca M.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Krivonos, Roman] Russian Acad Sci, Space Res Inst, Profsoyuznaya 84-32, Moscow 117997, Russia. [Bauer, Franz] Pontificia Univ Catolica Chile, Fac Fis, Inst Astrofis, Santiago 22, Chile. [Bauer, Franz] Millennium Inst Astrophys, Santiago, Chile. [Bauer, Franz] Space Sci Inst, 4750 Walnut St,Suite 205, Boulder, CO 80301 USA. [Perez, Kerstin] Haverford Coll, 370 Lancaster Ave,KINSC L109, Haverford, PA 19041 USA. [Tomsick, John A.; Chiu, Jeng-Lun; Clavel, Maica; Barriere, Nicolas; Boggs, Steven E.; Craig, William W.; Zoglauer, Andreas] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Bodaghee, Arash] Georgia Coll, 231 W Hancock St, Milledgeville, GA 31061 USA. [Stern, Daniel] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Alexander, David M.] Univ Durham, Dept Phys, Durham DH1 3LE, England. [Aramaki, Tsuguo] Standford Natl Accelerator Lab, 2575 Sand Hill Rd, Menlo Pk, CA 94025 USA. [Baganoff, Frederick K.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Barret, Didier; Christensen, Finn E.] Univ Toulouse, UPS OMP, IRAP, Toulouse, France. [Barret, Didier] Inst Rech Astrophys & Planetol, CNRS, 9Av Colonel Roche,BP 44346, F-31028 Toulouse 4, France. [Craig, William W.; Pivovaroff, Michael J.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA. [Forster, Karl; Grefenstette, Brian W.; Harrison, Fiona A.; Madsen, Kristen K.; Mao, Peter H.; Miyasaka, Hiromasa; Rana, Vikram] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Giommi, Paolo; Perri, Matteo; Puccetti, Simonetta] ASI Sci Data Ctr, Via Politecn Snc, I-00133 Rome, Italy. [Hornstrup, Allan; Westergaard, Niels J.] Tech Univ Denmark, DTU Space Natl Space Inst, Elektrovej 327, DK-2800 Lyngby, Denmark. [Kitaguchi, Takao] Hiroshima Univ, Dept Phys Sci, Higashihiroshima, Hiroshima 7398526, Japan. [Kitaguchi, Takao] Hiroshima Univ, Core Res Energet Universe, Higashihiroshima, Hiroshima 7398526, Japan. [Koglin, Jason E.] Kavli Inst Particle Astrophys & Cosmol, SLAC Natl Accelerator Lab, Menlo Pk, CA 94025 USA. [Perri, Matteo; Puccetti, Simonetta] INAF Astron Roma, Via Frascati 33, I-00040 Monte Porzio Catone, Italy. [Zhang, William W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Hong, J (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM jaesub@head.cfa.harvard.edu OI Clavel, Maica/0000-0003-0724-2742; Krivonos, Roman/0000-0003-2737-5673 FU NASA [NASA Contract No. NNG08FD60C]; National Aeronautics and Space Administration; NASA/APRA grant [NNX14AD59G]; Russian Science Foundation [14-22-00271]; CONICYT-Chile (Basal-CATA) [PFB-06/2007]; CONICYT-Chile (FONDECYT) [1141218]; CONICYT-Chile ("EMBIGGEN" Anillo) [ACT1101]; Ministry of Economy, Development, and Tourism's Millennium Science Initiative [IC120009]; NASA Headquarters under the NASA Earth and Space Science Fellowship Program-Grant [NNX13AM31]; French Space Agency (CNES) FX This work was supported under NASA Contract No. NNG08FD60C, and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software and Calibration teams for support with the execution and analysis of these observations. We thank G. Ponti for careful reading and suggestions of the manuscript. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). J. Hong acknowledges support from NASA/APRA grant NNX14AD59G. R. Krivonos acknowledges support from Russian Science Foundation through grant 14-22-00271. F.E. Bauer acknowledges support from CONICYT-Chile (Basal-CATA PFB-06/2007, FONDECYT 1141218, "EMBIGGEN" Anillo ACT1101), and the Ministry of Economy, Development, and Tourism's Millennium Science Initiative through grant IC120009, awarded to The Millennium Institute of Astrophysics, MAS. S. Zhang is supported by NASA Headquarters under the NASA Earth and Space Science Fellowship Program-Grant NNX13AM31. D. Barret acknowledges support from the French Space Agency (CNES). NR 89 TC 3 Z9 3 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 10 PY 2016 VL 825 IS 2 AR 132 DI 10.3847/0004-637X/825/2/132 PG 31 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DU1BM UT WOS:000381940800050 ER PT J AU Karalidi, T Apai, D Marley, MS Buenzli, E AF Karalidi, Theodora Apai, Daniel Marley, Mark S. Buenzli, Esther TI MAPS OF EVOLVING CLOUD STRUCTURES IN LUHMAN 16AB FROM HST TIME-RESOLVED SPECTROSCOPY SO ASTROPHYSICAL JOURNAL LA English DT Article DE methods: statistical; stars: individual (WISE J104915.57-531906.1); techniques: photometric ID BINARY BROWN DWARF; 2 PC; WISE J104915.57-531906.1AB; AMPLITUDE VARIABILITY; L/T TRANSITION; T DWARFS; ATMOSPHERE; WEATHER; DISCOVERY; ROTATION AB WISE J104915.57-531906.1 is the nearest brown dwarf binary to our solar system, consisting of two brown dwarfs in the L/T transition: Luhman 16A and B. In this paper, we present the first map of Luhman 16A, and maps of Luhman 16B for two epochs. Our maps were created by applying Aeolus, a Markov-Chain Monte Carlo code that maps the top-of-the-atmosphere (TOA) structure of brown dwarf and other ultracool atmospheres, to light curves of Luhman 16A and B using the Hubble Space Telescope's G141 and G102 grisms. Aeolus retrieved three or four spots in the TOA of Luhman 16A and B, with a surface coverage of 19%-32% (depending on an assumed rotational period of 5 hr or 8 hr) or 21%-38.5% (depending on the observational epoch), respectively. The brightness temperature of the spots of the best-fit models was similar to 200 K hotter than the background TOA. We compared our Luhman 16B map with the only previously published map. Interestingly, our map contained a large TOA spot that was cooler (Delta T similar to 51 K) than the background, which lay at low latitudes, in agreement with the previous Luhman 16B map. Finally, we report the detection of a feature reappearing in Luhman 16B light curves that are separated by tens of hundreds of rotations from each other. We speculate that this feature is related to TOA structures of Luhman 16B. C1 [Karalidi, Theodora; Apai, Daniel] Univ Arizona, Dept Astron, Steward Observ, 933 North Cherry Ave, Tucson, AZ 85721 USA. [Apai, Daniel] Univ Arizona, Lunar & Planetary Lab, 1629 East Univ Blvd, Tucson, AZ 85721 USA. [Marley, Mark S.] NASA, Ames Res Ctr, MS-245-3, Moffett Field, CA 94035 USA. [Buenzli, Esther] ETH, Inst Astron, Wolfgang Pauli Str 27, CH-8093 Zurich, Switzerland. RP Karalidi, T (reprint author), Univ Arizona, Dept Astron, Steward Observ, 933 North Cherry Ave, Tucson, AZ 85721 USA. EM tkaralidi@email.arizona.edu OI Marley, Mark/0000-0002-5251-2943 FU Spitzer Cycle-9 Exploration Program Extrasolar Storms [90063]; NASA by JPL/Caltech; NASA from the Space Telescope Science Institute [12314]; NASA [NAS5-26555, NAS 526555]; National Aeronautics and Space Administration [NNX15AD94G] FX This work is part of the Spitzer Cycle-9 Exploration Program Extrasolar Storms (program No. 90063). Support for this work was provided by NASA through an award issued by JPL/Caltech. Support for Program number 12314 was provided by NASA through a grant from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555. An allocation of computer time from the UA Research Computing High Performance Computing (HTC) and High Throughput Computing (HTC) at the University of Arizona is gratefully acknowledged. This study, in part, is based on observations made with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 526555. D. Apai acknowledges support by the National Aeronautics and Space Administration under agreement No. NNX15AD94G for the program Earths in Other Solar Systems. We thank I.J.M. Crossfield for providing us with the previously published Luhman 16B map data set. We thank Ben W.P. Lew for providing us with a best-fit exoplanet period for the PPCS-1 in Luhman 16B light curves. We thank the anonymous referee for a helpful report. NR 32 TC 1 Z9 1 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 10 PY 2016 VL 825 IS 2 AR 90 DI 10.3847/0004-637X/825/2/90 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DU1BM UT WOS:000381940800008 ER PT J AU Koss, MJ Assef, R Balokovic, M Stern, D Gandhi, P Lamperti, I Alexander, DM Ballantyne, DR Bauer, FE Berney, S Brandt, WN Comastri, A Gehrels, N Harrison, FA Lansbury, G Markwardt, C Ricci, C Rivers, E Schawinski, K Trakhtenbrot, B Treister, E Urry, CM AF Koss, Michael J. Assef, R. Balokovic, M. Stern, D. Gandhi, P. Lamperti, I. Alexander, D. M. Ballantyne, D. R. Bauer, F. E. Berney, S. Brandt, W. N. Comastri, A. Gehrels, N. Harrison, F. A. Lansbury, G. Markwardt, C. Ricci, C. Rivers, E. Schawinski, K. Trakhtenbrot, B. Treister, E. Urry, C. Megan TI A NEW POPULATION OF COMPTON-THICK AGNs IDENTIFIED USING THE SPECTRAL CURVATURE ABOVE 10 keV SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: Seyfert; X-rays: galaxies ID ACTIVE GALACTIC NUCLEI; SEYFERT 2 GALAXIES; SUPERMASSIVE BLACK-HOLES; X-RAY SPECTROSCOPY; SWIFT-BAT SURVEY; DEEP FIELD-SOUTH; XMM-NEWTON; MIDINFRARED SELECTION; MU-M; NUSTAR AB We present a new metric that uses the spectral curvature (SC) above 10 keV to identify Compton-thick active galactic nuclei (AGNs) in low-quality Swift/Burst Alert Telescope (BAT) X-ray data. Using NuSTAR, we observe nine high SC-selected AGNs. We find that high-sensitivity spectra show that the majority are Compton-thick (78% or 7/9) and the remaining two are nearly Compton-thick (NH similar or equal to (5-8) x 10(23) cm(-2)). We find that the SCBAT and SCNuSTAR measurements are consistent, suggesting that this technique can be applied to future telescopes. We tested the SC method on well-known Compton-thick AGNs and found that it is much more effective than broadband ratios (e.g., 100% using SC versus 20% using 8-24 keV/3-8 keV). Our results suggest that using the > 10 keV emission may be the only way to identify this population since only two sources show Compton-thick levels of excess in the Balmer decrement corrected [O III] to observed X-ray emission ratio (F-[O III]/F-2-10(obs) keV > 1) and WISE colors do not identify most of them as AGNs. Based on this small sample, we find that a higher fraction of these AGNs are in the final merger stage (< 10 kpc) than typical BAT AGNs. Additionally, these nine obscured AGNs have, on average, approximate to 4 x higher accretion rates than other BAT-detected AGNs ( = 0.068 +/- 0.023 compared to = 0.016 +/- 0.004). The robustness of SC at identifying Compton-thick AGNs implies that a higher fraction of nearby AGNs may be Compton-thick (approximate to 22%) and the sum of black hole growth in Compton-thick AGNs (Eddington ratio times population percentage) is nearly as large as mildly obscured and unobscured AGNs. C1 [Koss, Michael J.; Lamperti, I.; Berney, S.; Schawinski, K.; Trakhtenbrot, B.] Swiss Fed Inst Technol, Inst Astron, Dept Phys, Wolfgang Pauli Str 27, CH-8093 Zurich, Switzerland. [Koss, Michael J.] Univ Hawaii, Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA. [Assef, R.] Univ Diego Portales, Nucleo Astron Fac Ingn, Av Ejercito 441, Santiago, Chile. [Balokovic, M.; Harrison, F. A.; Rivers, E.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Stern, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Gandhi, P.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Alexander, D. M.] Univ Durham, Dept Phys, S Rd, Durham DH1 3LE, England. [Ballantyne, D. R.] Georgia Inst Technol, Sch Phys, Ctr Relativist Astrophys, Atlanta, GA 30332 USA. [Bauer, F. E.; Ricci, C.] Pontificia Univ Catolica Chile, Inst Astrofis, Fac Fis, Casilla 306, Santiago 22, Chile. [Bauer, F. E.] Space Sci Inst, 4750 Walnut St,Suite 205, Boulder, CO 80301 USA. [Brandt, W. N.] Penn State Univ, Davey Lab 525, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Brandt, W. N.] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA. [Brandt, W. N.] Penn State Univ, Dept Phys, Davey Lab 104, University Pk, PA 16802 USA. [Comastri, A.] INAF, Osservatorio Astron Bologna, Via Ranzani 1, I-40127 Bologna, Italy. [Gehrels, N.; Markwardt, C.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD USA. [Treister, E.] Univ Concepcion, Dept Astron, Casilla 160-C, Concepcion, Chile. [Urry, C. Megan] Yale Univ, Dept Phys, Yale Ctr Astron & Astrophys, POB 208120, New Haven, CT 06520 USA. RP Koss, MJ (reprint author), Swiss Fed Inst Technol, Inst Astron, Dept Phys, Wolfgang Pauli Str 27, CH-8093 Zurich, Switzerland.; Koss, MJ (reprint author), Univ Hawaii, Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA. EM mkoss@phys.ethz.ch OI Koss, Michael/0000-0002-7998-9581; Trakhtenbrot, Benny/0000-0002-3683-7297 FU Ambizione fellowship grant [PZ00P2_154799/1]; Swiss National Science Foundation (NSF) grant [PP00P2 138979/1]; Center of Excellence in Astrophysics and Associated Technologies [PFB 06]; FONDECYT regular grant [1120061]; CONICYT Anillo project [ACT1101]; NASA Headquarters under the NASA Earth and Space Science Fellowship Program [NNX14AQ07H]; NSF award [AST 1008067]; Caltech NuSTAR sub-contract [44A-1092750]; NASA ADP grant [NNX10AC99G]; ASI/INAF grant [I/037/12/0011/13]; Caltech Kingsley visitor program; National Aeronautics and Space Administration through Chandra Award [AR3-14010X]; National Aeronautics Space Administration [NAS8-03060]; NASA [NNG08FD60C]; ESA Member States FX We acknowledge financial support from Ambizione fellowship grant PZ00P2_154799/1 (M.K.), the Swiss National Science Foundation (NSF) grant PP00P2 138979/1 (M.K. and K.S.), the Center of Excellence in Astrophysics and Associated Technologies (PFB 06), by the FONDECYT regular grant 1120061 and by the CONICYT Anillo project ACT1101 (E.T.), NASA Headquarters under the NASA Earth and Space Science Fellowship Program, grant NNX14AQ07H (M.B.), NSF award AST 1008067 (D.B.), Caltech NuSTAR sub-contract 44A-1092750 and NASA ADP grant NNX10AC99G (W. N.B.), and the ASI/INAF grant I/037/12/0011/13 and the Caltech Kingsley visitor program (A.C.). M.K. also acknowledges that support for this work was provided by the National Aeronautics and Space Administration through Chandra Award Number AR3-14010X issued by the Chandra X-ray Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of the National Aeronautics Space Administration under contract NAS8-03060. This work was supported under NASA Contract No. NNG08FD60C and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). This research made use of the XRT Data Analysis Software (XRTDAS), archival data, software, and online services provided by the ASDC. This work made use of data supplied by the UK Swift Science Data Centre at the University of Leicester. The scientific results reported in this article are based on data obtained from the Chandra Data Archive (Obs ID = 4078, 4868, 12290, 13895). This work is based on observations obtained with XMM-Newton (Obs ID = 0110930201, 0147760101, 0200430201), an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA. NR 87 TC 3 Z9 3 U1 1 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 10 PY 2016 VL 825 IS 2 AR 85 DI 10.3847/0004-637X/825/2/85 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DU1BM UT WOS:000381940800003 ER PT J AU Rafelski, M Gardner, JP Fumagalli, M Neeleman, M Teplitz, HI Grogin, N Koekemoer, AM Scarlata, C AF Rafelski, Marc Gardner, Jonathan P. Fumagalli, Michele Neeleman, Marcel Teplitz, Harry I. Grogin, Norman Koekemoer, Anton M. Scarlata, Claudia TI THE STAR FORMATION RATE EFFICIENCY OF NEUTRAL ATOMIC-DOMINATED HYDROGEN GAS IN THE OUTSKIRTS OF STAR-FORMING GALAXIES FROM z similar to 1 TO z similar to 3 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: evolution; galaxies: high-redshift; galaxies: photometry; galaxies: star formation; galaxies: structure; quasars: absorption lines ID LY-ALPHA SYSTEMS; DAMPED LYMAN-ALPHA; ULTRA-DEEP FIELD; CO-TO-H-2 CONVERSION FACTOR; KENNICUTT-SCHMIDT RELATION; DWARF IRREGULAR GALAXIES; SURFACE BRIGHTNESS GALAXIES; EXTRAGALACTIC LEGACY SURVEY; II-ASTERISK ABSORPTION; DARK-MATTER UNIVERSE AB Current observational evidence suggests that the star formation rate (SFR) efficiency of neutral atomic hydrogen gas measured in damped Lya systems (DLAs) at z similar to 3 is more than 10 times lower than predicted by the Kennicutt-Schmidt (KS) relation. To understand the origin of this deficit, and to investigate possible evolution with redshift and galaxy properties, we measure the SFR efficiency of atomic gas at z similar to 1, z similar to 2, and z similar to 3 around star-forming galaxies. We use new robust photometric redshifts in the Hubble Ultra Deep Field to create galaxy stacks in these three redshift bins, and measure the SFR efficiency by combining DLA absorber statistics with the observed rest-frame UV emission in the galaxies' outskirts. We find that the SFR efficiency of H I gas at z > 1 is similar to 1%-3% of that predicted by the KS relation. Contrary to simulations and models that predict a reduced SFR efficiency with decreasing metallicity and thus with increasing redshift, we find no significant evolution in the SFR efficiency with redshift. Our analysis instead suggests that the reduced SFR efficiency is driven by the low molecular content of this atomic-dominated phase, with metallicity playing a secondary effect in regulating the conversion between atomic and molecular gas. This interpretation is supported by the similarity between the observed SFR efficiency and that observed in local atomic-dominated gas, such as in the outskirts of local spiral galaxies and local dwarf galaxies. C1 [Rafelski, Marc; Gardner, Jonathan P.] Goddard Space Flight Ctr, Code 665, Greenbelt, MD 20771 USA. [Fumagalli, Michele] Univ Durham, Inst Computat Cosmol, South Rd, Durham DH1 3LE, England. [Fumagalli, Michele] Univ Durham, Ctr Extragalact Astron, Dept Phys, South Rd, Durham DH1 3LE, England. [Neeleman, Marcel] Univ Calif Santa Cruz, Dept Astron & Astrophys, UCO Lick Observ, 1156 High St, Santa Cruz, CA 95064 USA. [Teplitz, Harry I.] CALTECH, Infrared Proc & Anal Ctr, MS 100-22, Pasadena, CA 91125 USA. [Grogin, Norman; Koekemoer, Anton M.] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA. [Scarlata, Claudia] Univ Minnesota, Minnesota Inst Astrophys, Sch Phys & Astron, Minneapolis, MN 55455 USA. RP Rafelski, M (reprint author), Goddard Space Flight Ctr, Code 665, Greenbelt, MD 20771 USA. EM marc.a.rafelski@nasa.gov RI Fumagalli, Michele/K-9510-2015; OI Fumagalli, Michele/0000-0001-6676-3842; Koekemoer, Anton/0000-0002-6610-2048 FU Science and Technology Facilities Council [ST/L00075X/1]; NASA from the Space Telescope Science Institute [GO-12534]; NASA [NAS5-26555]; NASA Postdoctoral Program at Goddard Space Flight Center FX We would like to thank Rachel Somerville, Mark Krumholz, and Bruce Elmegreen for useful discussions on interpreting the results. We also thank the referee for useful comments that improved the clarity of the paper. M.R. acknowledges support from an appointment to the NASA Postdoctoral Program at Goddard Space Flight Center. M.F. acknowledges support by the Science and Technology Facilities Council (grant number ST/L00075X/1). Support for HST Program GO-12534 was provided by NASA through grants from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. NR 140 TC 3 Z9 3 U1 2 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 10 PY 2016 VL 825 IS 2 AR 87 DI 10.3847/0004-637X/825/2/87 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DU1BM UT WOS:000381940800005 ER PT J AU Ryu, T Sato, B Kuzuhara, M Narita, N Takahashi, YH Uyama, T Kudo, T Kusakabe, N Hashimoto, J Omiya, M Harakawa, H Abe, L Ando, H Brandner, W Brandt, TD Carson, JC Currie, T Egner, S Feldt, M Goto, M Grady, CA Guyon, O Hayano, Y Hayashi, M Hayashi, SS Helminiak, KG Henning, T Hodapp, KW Ida, S Ishii, M Itoh, Y Iye, M Izumiura, H Janson, M Kambe, E Kandori, R Knapp, GR Kokubo, E Kwon, J Matsuo, T Mayama, S McElwain, MW Mede, K Miyama, S Morino, JI Moro-Martin, A Nishimura, T Pyo, TS Serabyn, E Suenaga, T Suto, H Suzuki, R Takami, M Takato, N Takeda, Y Terada, H Thalmann, C Turner, EL Watanabe, M Wisniewski, J Yamada, T Yoshida, M Takami, H Usuda, T Tamura, M AF Ryu, Tsuguru Sato, Bun'ei Kuzuhara, Masayuki Narita, Norio Takahashi, Yasuhiro H. Uyama, Taichi Kudo, Tomoyuki Kusakabe, Nobuhiko Hashimoto, Jun Omiya, Masashi Harakawa, Hiroki Abe, Lyu Ando, Hiroyasu Brandner, Wolfgang Brandt, Timothy D. Carson, Joseph C. Currie, Thayne Egner, Sebastian Feldt, Markus Goto, Miwa Grady, Carol A. Guyon, Olivier Hayano, Yutaka Hayashi, Masahiko Hayashi, Saeko S. Helminiak, Krzysztof G. Henning, Thomas Hodapp, Klaus W. Ida, Shigeru Ishii, Miki Itoh, Yoichi Iye, Masanori Izumiura, Hideyuki Janson, Markus Kambe, Eiji Kandori, Ryo Knapp, Gillian R. Kokubo, Eiichiro Kwon, Jungmi Matsuo, Taro Mayama, Satoshi McElwain, Michael W. Mede, Kyle Miyama, Shoken Morino, Jun-Ichi Moro-Martin, Amaya Nishimura, Tetsuo Pyo, Tae-Soo Serabyn, Eugene Suenaga, Takuya Suto, Hiroshi Suzuki, Ryuji Takami, Michihiro Takato, Naruhisa Takeda, Yoichi Terada, Hiroshi Thalmann, Christian Turner, Edwin L. Watanabe, Makoto Wisniewski, John Yamada, Toru Yoshida, Michitoshi Takami, Hideki Usuda, Tomonori Tamura, Motohide TI HIGH-CONTRAST IMAGING OF INTERMEDIATE-MASS GIANTS WITH LONG-TERM RADIAL VELOCITY TRENDS SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: general; methods: observational; planetary systems; techniques: high angular resolution; techniques: radial velocities ID EXOPLANET HOST STARS; EVOLUTIONARY MODELS; STELLAR COMPANIONS; K-GIANT; SUBSTELLAR COMPANION; PLANETARY COMPANIONS; DWARF COMPANION; IOTA DRACONIS; OKAYAMA HIDES; BROWN DWARFS AB A radial velocity (RV) survey for intermediate-mass giants has been in operation for over a decade at Okayama Astrophysical Observatory (OAO). The OAO survey has revealed that some giants show long-term linear RV accelerations (RV trends), indicating the presence of outer companions. Direct-imaging observations can help clarify what objects generate these RV trends. We present the results of high-contrast imaging observations of six intermediate-mass giants with long-term RV trends using the Subaru Telescope and HiCIAO camera. We detected co-moving companions to gamma Hya B (0.61(-0.14)(+0.12)M(circle dot)), HD 5608 B (0.10 +/- 0.01M(circle dot)), and HD 109272 B (0.28 +/- 0.06M(circle dot)). For the remaining targets (iota Dra, 18 Del, and HD 14067), we exclude companions more massive than 30-60 M-Jup at projected separations of 1 ''-7 ''. We examine whether these directly imaged companions or unidentified long-period companions can account for the RV trends observed around the six giants. We find that the Kozai mechanism can explain the high eccentricity of the inner planets iota Dra b, HD 5608 b, and HD 14067 b. C1 [Ryu, Tsuguru; Narita, Norio; Izumiura, Hideyuki; Kokubo, Eiichiro; Mayama, Satoshi; Suenaga, Takuya; Takeda, Yoichi] Grad Univ Adv Studies, SOKENDAI, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan. [Ryu, Tsuguru; Narita, Norio; Omiya, Masashi; Harakawa, Hiroki; Ando, Hiroyasu; Hayashi, Masahiko; Ishii, Miki; Iye, Masanori; Kandori, Ryo; Kokubo, Eiichiro; Morino, Jun-Ichi; Suenaga, Takuya; Suto, Hiroshi; Suzuki, Ryuji; Takeda, Yoichi; Terada, Hiroshi; Takami, Hideki; Usuda, Tomonori; Tamura, Motohide] Natl Astron Observ Japan, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan. [Sato, Bun'ei; Kuzuhara, Masayuki; Ida, Shigeru] Tokyo Inst Technol, Dept Earth & Planetary Sci, Meguro Ku, Tokyo 1528551, Japan. [Narita, Norio; Kusakabe, Nobuhiko; Hashimoto, Jun; Suto, Hiroshi; Tamura, Motohide] Astrobiol Ctr, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan. [Takahashi, Yasuhiro H.; Uyama, Taichi; Kwon, Jungmi; Mede, Kyle; Tamura, Motohide] Univ Tokyo, Dept Astron, Bunkyo Ku, 7-3-1 Hongo, Tokyo 1130033, Japan. [Kudo, Tomoyuki; Currie, Thayne; Egner, Sebastian; Guyon, Olivier; Hayano, Yutaka; Hayashi, Saeko S.; Helminiak, Krzysztof G.; Nishimura, Tetsuo; Pyo, Tae-Soo; Takato, Naruhisa] Natl Astron Observ Japan, Subaru Telescope, 650 North Aohoku Pl, Hilo, HI 96720 USA. [Abe, Lyu] Univ Nice Sophia Antipolis, Observ Cote Azur, CNRS, Lab Lagrange UMR 7293, 28 Ave Valrose, F-06108 Nice 2, France. [Brandner, Wolfgang; Carson, Joseph C.; Feldt, Markus; Henning, Thomas] Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany. [Brandt, Timothy D.] Inst Adv Study, Dept Astrophys, Olden Lane, Princeton, NJ 08540 USA. [Carson, Joseph C.] Coll Charleston, Dept Phys & Astron, 58 Coming St, Charleston, SC 29424 USA. [Goto, Miwa] Univ Munich, Univ Sternwarte, Scheinerstr 1, D-81679 Munich, Germany. [Grady, Carol A.; McElwain, Michael W.] Goddard Space Flight Ctr, Exoplanets & Stellar Astrophys Lab, Code 667, Greenbelt, MD 20771 USA. [Grady, Carol A.] Eureka Sci, 2452 Delmer,Suite 100, Oakland, CA 96002 USA. [Grady, Carol A.] Goddard Ctr Astrobiol, Washington, DC USA. [Hodapp, Klaus W.] Univ Hawaii, Inst Astron, 640 N Aohoku Pl, Hilo, HI 96720 USA. [Itoh, Yoichi] Univ Hyogo, Ctr Astron, Nishi Harima Astron Observ, 407-2 Nishigaichi, Sayo, Hyogo 6795313, Japan. [Izumiura, Hideyuki; Kambe, Eiji] Natl Astron Observ Japan, Okayama Astrophys Observ, Kamogata, Okayama 7190232, Japan. [Janson, Markus; Knapp, Gillian R.] Stockholm Univ, AlbaNova Univ Ctr, Dept Astron, SE-10691 Stockholm, Sweden. [Matsuo, Taro; Turner, Edwin L.] Kyoto Univ, Dept Astron, Sakyo Ku, Kitashirakawa Oiwake Cho, Kyoto, Kyoto 6068502, Japan. [Miyama, Shoken] Hiroshima Univ, 1-3-2 Kagamiyama, Higashihiroshima, Hiroshima 7398511, Japan. [Moro-Martin, Amaya] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA. [Moro-Martin, Amaya] Johns Hopkins Univ, Ctr Astrophys Sci, Baltimore, MD 21218 USA. [Serabyn, Eugene] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Takami, Michihiro] Acad Sinica, Inst Astron & Astrophys, POB 23-141, Taipei 10617, Taiwan. [Thalmann, Christian] ETH, Inst Astron, Wolfgang Pauli Str 27, CH-8093 Zurich, Switzerland. [Turner, Edwin L.] Univ Tokyo, Kavli Inst Phys & Math Universe, 5-1-5 Kashiwanoha, Kashiwa, Chiba 2778568, Japan. [Watanabe, Makoto] Hokkaido Univ, Dept Cosmosci, Kita Ku, Sapporo, Hokkaido 0600810, Japan. [Wisniewski, John] Univ Oklahoma, HL Dodge Dept Phys & Astron, 440 W Brooks St, Norman, OK 73019 USA. [Yamada, Toru] Tohoku Univ, Astron Inst, Aoba Ku, Sendai, Miyagi 9808578, Japan. [Yoshida, Michitoshi] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Higashihiroshima, Hiroshima 7398526, Japan. RP Ryu, T (reprint author), Grad Univ Adv Studies, SOKENDAI, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan.; Ryu, T (reprint author), Natl Astron Observ Japan, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan. EM tsuguru.ryu@nao.ac.jp RI MIYAMA, Shoken/A-3598-2015 FU NAOJ Fellowship; Inoue Science Research Award; JSPS KAKENHI [25247026]; U.S. National Science Foundation [1009203]; Center for the Promotion of Integrated Sciences (CPIS) of SOKENDAI; [25-8826] FX The data analysis was carried out using a common use data analysis computer system at the Astronomy Data Center of the National Astronomical Observatory of Japan. This research made use of the SIMBAD database, operated at CDS, Strasbourg, France. Our analysis is also based on observations made with the NASA/ESA Hubble Space Telescope, and obtained from the Hubble Legacy Archive, which is a collaboration between the Space Telescope Science Institute, the Space Telescope European Coordinating Facility (ST-ECF/ESA), and the Canadian Astronomy Data Centre (CADC/NRC/CSA). N.N. acknowledges support from the NAOJ Fellowship, Inoue Science Research Award, and a Grant-in-Aid for Scientific Research (A) (JSPS KAKENHI Grant Number 25247026). J.C.C. acknowledges support from the U.S. National Science Foundation under Award No. 1009203. This work was partially supported by a Grant-in-Aid for JSPS Fellows (Grant Number 25-8826). This work was supported in part by the Center for the Promotion of Integrated Sciences (CPIS) of SOKENDAI. NR 65 TC 1 Z9 1 U1 1 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 10 PY 2016 VL 825 IS 2 AR 127 DI 10.3847/0004-637X/825/2/127 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DU1BM UT WOS:000381940800045 ER PT J AU Sumi, T Udalski, A Bennett, DP Gould, A Poleski, R Bond, IA Skowron, J Rattenbury, N Pogge, RW Bensby, T Beaulieu, JP Marquette, JB Batista, V Brillant, S Abe, F Asakura, Y Bhattacharya, A Donachie, M Freeman, M Fukui, A Hirao, Y Itow, Y Koshimoto, N Li, MCA Ling, CH Masuda, K Matsubara, Y Muraki, Y Nagakane, M Ohnishi, K Oyokawa, H Saito, T Sharan, A Sullivan, DJ Suzuki, D Tristram, PJ Yonehara, A Szymanski, MK Ulaczyk, K Kozlowski, S Wyrzykowski, L Kubiak, M Pietrukowicz, P Pietrzynski, G Soszynski, I Han, C Jung, YK Shin, IG Lee, CU AF Sumi, T. Udalski, A. Bennett, D. P. Gould, A. Poleski, R. Bond, I. A. Skowron, J. Rattenbury, N. Pogge, R. W. Bensby, T. Beaulieu, J. P. Marquette, J. B. Batista, V. Brillant, S. Abe, F. Asakura, Y. Bhattacharya, A. Donachie, M. Freeman, M. Fukui, A. Hirao, Y. Itow, Y. Koshimoto, N. Li, M. C. A. Ling, C. H. Masuda, K. Matsubara, Y. Muraki, Y. Nagakane, M. Ohnishi, K. Oyokawa, H. Saito, To. Sharan, A. Sullivan, D. J. Suzuki, D. Tristram, P. J. Yonehara, A. Szymanski, M. K. Ulaczyk, K. Kozlowski, S. Wyrzykowski, L. Kubiak, M. Pietrukowicz, P. Pietrzynski, G. Soszynski, I. Han, C. Jung, Y-K. Shin, I-G Lee, C-U. CA MOA Collaboration OGLE Collaboration TI THE FIRST NEPTUNE ANALOG OR SUPER-EARTH WITH A NEPTUNE-LIKE ORBIT: MOA-2013-BLG-605LB SO ASTROPHYSICAL JOURNAL LA English DT Article DE Galaxy: bulge; gravitational lensing: micro; planetary systems ID GRAVITATIONAL LENSING EXPERIMENT; PARALLAX MICROLENS DEGENERACY; DIFFERENCE IMAGE-ANALYSIS; SAGITTARIUS-A-ASTERISK; LOW-MASS STARS; GALACTIC BULGE; GIANT PLANETS; PROPER MOTION; SNOW LINE; JUPITER/SATURN ANALOG AB We present the discovery of the first Neptune analog exoplanet or super-Earth with a Neptune-like orbit, MOA-2013-BLG-605Lb. This planet has a mass similar to that of Neptune or a super-Earth and it orbits at 9 similar to 14 times the expected position of the snow line, a(snow), which is similar to Neptune's separation of 11 a(snow) from the Sun. The planet/host-star mass ratio is q = (3.6 +/- 0.7) x 10(-4) and the projected separation normalized by the Einstein radius is s = 2.39 +/- 0.05. There are three degenerate physical solutions and two of these are due to a new type of degeneracy in the microlensing parallax parameters, which we designate "the wide degeneracy." The three models have (i) a Neptune-mass planet with a mass of M-p = 21(-7)(+6)M(circle plus) orbiting a low-mass M-dwarf with a mass of M-h = 0.19(-0.06)(+0.05)M(circle dot), (ii) a mini-Neptune with M-p = 7.9(-1.2)(+1.8)M(circle plus) orbiting a brown dwarf host with M-h = 0.068(-0.011)(+0.019)M(circle dot), and (iii) a super-Earth with M-p = 3.2(-0.3)(+0.5)M(circle plus) orbiting a low-mass brown dwarf host with M-h = 0.025(-0.004)(+0.005)M(circle dot), which is slightly favored. The 3D planet-host separations are 4.6(-1.2)(+4.7) au, 2.1(-0.2) (+1.0) au, and 0.94(-0.02)(+0.67) au, which are 8.9(-1.4)(+10.5), 12(-1)(+7), or 14(-1)(+11) times larger than a(snow) for these models, respectively. Keck adaptive optics observations confirm that the lens is faint. This discovery suggests that low-mass planets with Neptune-like orbits are common. Therefore processes similar to the one that formed Neptune in our own solar system or cold super-Earths may be common in other solar systems. C1 [Sumi, T.; Hirao, Y.; Koshimoto, N.; Nagakane, M.] Osaka Univ, Grad Sch Sci, Dept Earth & Space Sci, Toyonaka, Osaka 5600043, Japan. [Udalski, A.; Poleski, R.; Skowron, J.; Szymanski, M. K.; Ulaczyk, K.; Kozlowski, S.; Wyrzykowski, L.; Kubiak, M.; Pietrukowicz, P.; Pietrzynski, G.; Soszynski, I.] Univ Warsaw Observ, Al Ujazdowskie 4, PL-00478 Warsaw, Poland. [Bennett, D. P.; Bhattacharya, A.; Suzuki, D.] Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA. [Bennett, D. P.] NASA, Goddard Space Flight Ctr, Lab Exoplanets & Stellar Astrophys, Greenbelt, MD 20771 USA. [Gould, A.; Poleski, R.; Pogge, R. W.] Ohio State Univ, Dept Astron, 140 W 18th Ave, Columbus, OH 43210 USA. [Bond, I. A.; Ling, C. H.] Massey Univ, Inst Informat & Math Sci, Private Bag 102-904,North Shore Mail Ctr, Auckland, New Zealand. [Rattenbury, N.; Donachie, M.; Freeman, M.; Li, M. C. A.; Sharan, A.] Univ Auckland, Dept Phys, Private Bag 92019, Auckland, New Zealand. [Bensby, T.] Lund Observ, Dept Astron & Theoret Phys, Box 43, SE-22100 Lund, Sweden. [Beaulieu, J. P.; Marquette, J. B.; Batista, V.] Univ Paris 06, Inst Astrophys Paris, CNRS, UMR7095, F-75014 Paris, France. [Brillant, S.] ESO, Karl Schwarzschildst 2, D-85748 Garching, Germany. [Abe, F.; Asakura, Y.; Itow, Y.; Masuda, K.; Matsubara, Y.; Muraki, Y.; Oyokawa, H.] Nagoya Univ, Inst Space Earth Environm Res, Nagoya, Aichi 4648601, Japan. [Fukui, A.] Natl Astron Observ Japan, Okayama Astrophys Observ, 3037-5 Honjo, Asakuchi, Okayama 7190232, Japan. [Ohnishi, K.] Nagano Natl Coll Technol, Nagano 3818550, Japan. [Saito, To.] Tokyo Metropolitan Coll Aeronaut, Tokyo 1168523, Japan. [Sullivan, D. J.] Victoria Univ, Sch Chem & Phys Sci, Wellington, New Zealand. [Tristram, P. J.] Mt John Univ Observ, POB 56, Lake Tekapo 8770, New Zealand. [Yonehara, A.] Kyoto Sangyo Univ, Dept Phys, Fac Sci, Kyoto 6038555, Japan. [Han, C.; Jung, Y-K.; Shin, I-G] Chungbuk Natl Univ, Inst Astrophys, Dept Phys, Cheongju 371763, South Korea. [Lee, C-U.] Korea Astron & Space Sci Inst, Daejeon 305348, South Korea. RP Sumi, T (reprint author), Osaka Univ, Grad Sch Sci, Dept Earth & Space Sci, Toyonaka, Osaka 5600043, Japan. EM sumi@ess.sci.osaka-u.ac.jp; udalski@astrouw.edu.pl; bennett@nd.edu; i.a.bond@massey.ac.nz; n.rattenbury@auckland.ac.nz; mdon849@aucklanduni.ac.nz; mli351@auckland.ac.nz; c.h.ling@massey.ac.nz; asha583@aucklanduni.ac.nz; msz@astrouw.edu.pl; kulaczyk@astrouw.edu.pl; mk@astrouw.edu.pl; pietrzyn@astrouw.edu.pl; soszynsk@astrouw.edu.pl RI Kozlowski, Szymon/G-4799-2013; Skowron, Jan/M-5186-2014; OI Kozlowski, Szymon/0000-0003-4084-880X; Skowron, Jan/0000-0002-2335-1730; Pogge, Richard/0000-0003-1435-3053 FU JSPS [JSPS23103002, JSPS24253004, JSPS26247023]; National Science Centre, Poland [MAESTRO 2014/14/A/ST9/00121]; NSF grants [AST-1009621, AST-1211875, AST 1103471]; NASA grants [NNX12AF54G, NNX13AF64G, NNX12AB99G]; Marsden Fund of the Royal Society of New Zealand [MAU1104]; ESO's DGDF; Programme National de Planetologie, CNRS; PERSU Sorbonne Universite; Creative Research Initiative Program of National Research Foundation of Korea [2009-0081561]; [JSPS25103508]; [23340064] FX T.S. acknowledges financial support from the JSPS, JSPS23103002, JSPS24253004, and JSPS26247023. The MOA project is supported by the grant JSPS25103508 and 23340064. The OGLE project has received funding from the National Science Centre, Poland, grant MAESTRO 2014/14/A/ST9/00121 to A.U.. D.P.B. acknowledges support from NSF grants AST-1009621 and AST-1211875, as well as NASA grants NNX12AF54G and NNX13AF64G. Work by I.A.B. and P.Y. was supported by the Marsden Fund of the Royal Society of New Zealand, contract no. MAU1104. N.J.R. is a Royal Society of New Zealand Rutherford Discovery Fellow. A.S., M.L. and M.D. acknowledge support from the Royal Society of New Zealand. A.S. is a University of Auckland Doctoral Scholar. A.G. was supported by NSF grant AST 1103471 and NASA grant NNX12AB99G. J.P.B., S.B., and J.B.M. gratefully acknowledge support from ESO's DGDF 2014. J.P.B. and J.B. acknowledge the support of the Programme National de Planetologie, CNRS, and from PERSU Sorbonne Universite. The work by C.H. was supported by the Creative Research Initiative Program (2009-0081561) of National Research Foundation of Korea. NR 95 TC 3 Z9 3 U1 2 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 10 PY 2016 VL 825 IS 2 AR 112 DI 10.3847/0004-637X/825/2/112 PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DU1BM UT WOS:000381940800030 ER PT J AU Tsuge, M Bahou, M Wu, YJ Allamandola, L Lee, YP AF Tsuge, Masashi Bahou, Mohammed Wu, Yu-Jong Allamandola, Louis Lee, Yuan-Pern TI THE INFRARED SPECTRUM OF PROTONATED OVALENE IN SOLID PARA-HYDROGEN AND ITS POSSIBLE CONTRIBUTION TO INTERSTELLAR UNIDENTIFIED INFRARED EMISSION SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrochemistry; infrared: ISM; ISM: lines and bands; ISM: molecules ID POLYCYCLIC AROMATIC-HYDROCARBONS; ELECTRONIC-ABSORPTION-SPECTRA; PHASE PAH MOLECULES; GAS-PHASE; ASTROPHYSICAL IMPLICATIONS; NEUTRAL COUNTERPART; DETAILED MODEL; BANDS; SPECTROSCOPY; CATIONS AB The mid-infrared emission from galactic objects, including reflection nebulae, planetary nebulae, proto-planetary nebulae, molecular clouds, etc, as well as external galaxies, is dominated by the unidentified infrared (UIR) emission bands. Large protonated polycyclic aromatic hydrocarbons (H(+)PAHs) were proposed as possible carriers, but no spectrum of an H(+)PAH has been shown to exactly match the UIR bands. Here, we report the IR spectrum of protonated ovalene (7-C32H15+) measured in a para-hydrogen (p-H-2) matrix at 3.2 K, generated by bombarding a mixture of ovalene and p-H-2 with electrons during matrix deposition. Spectral assignments were made based on the expected chemistry and on the spectra simulated with the wavenumbers and infrared intensities predicted with the B3PW91/6-311++G(2d, 2p) method. The close resemblance of the observed spectral pattern to that of the UIR bands suggests that protonated ovalene may contribute to the UIR emission, particularly from objects that emit Class A spectra, such as the IRIS reflection nebula, NGC 7023. C1 [Tsuge, Masashi; Bahou, Mohammed; Lee, Yuan-Pern] Natl Chiao Tung Univ, Dept Appl Chem, 1001 Ta Hsueh Rd, Hsinchu 30010, Taiwan. [Tsuge, Masashi; Bahou, Mohammed; Lee, Yuan-Pern] Natl Chiao Tung Univ, Inst Mol Sci, 1001 Ta Hsueh Rd, Hsinchu 30010, Taiwan. [Wu, Yu-Jong] Natl Synchrotron Radiat Res Ctr, 101 Hsin Ann Rd, Hsinchu 30076, Taiwan. [Allamandola, Louis] NASA, Ames Res Ctr, Astrophys & Astrochem Lab, Moffett Field, CA 94035 USA. [Lee, Yuan-Pern] Acad Sinica, Inst Mol Sci, Taipei 10617, Taiwan. RP Tsuge, M (reprint author), Natl Chiao Tung Univ, Dept Appl Chem, 1001 Ta Hsueh Rd, Hsinchu 30010, Taiwan.; Tsuge, M (reprint author), Natl Chiao Tung Univ, Inst Mol Sci, 1001 Ta Hsueh Rd, Hsinchu 30010, Taiwan. EM tsuge@nctu.edu.tw; yplee@mail.nctu.edu.tw RI Lee, Yuan-Pern/F-7938-2012; OI Lee, Yuan-Pern/0000-0001-6418-7378; Tsuge, Masashi/0000-0001-9669-1288 FU Ministry of Science and Technology, Taiwan [MOST104-2745-M009-001-ASP, MOST104-2113-M-213-004]; Ministry of Education, Taiwan ("ATU Plan" of National Chiao Tung University); NASA's Astrophysics Data Analysis Program FX The Ministry of Science and Technology, Taiwan (grants MOST104-2745-M009-001-ASP and MOST104-2113-M-213-004), and Ministry of Education, Taiwan ("ATU Plan" of National Chiao Tung University) supported this work. The National Center for High-Performance Computing provided the computer time. L.A. gratefully acknowledges support from NASA's Astrophysics Data Analysis Program. We thank Christiaan Boersma for providing the Red Rectangle spectrum. NR 53 TC 4 Z9 4 U1 3 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 10 PY 2016 VL 825 IS 2 AR 96 DI 10.3847/0004-637X/825/2/96 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DU1BM UT WOS:000381940800014 ER PT J AU Folatelli, G Van Dyk, SD Kuncarayakti, H Maeda, K Bersten, MC Nomoto, K Pignata, G Hamuy, M Quimby, RM Zheng, WK Filippenko, AV Clubb, KI Smith, N Elias-Rosa, N Foley, RJ Miller, AA AF Folatelli, Gaston Van Dyk, Schuyler D. Kuncarayakti, Hanindyo Maeda, Keiichi Bersten, Melina C. Nomoto, Ken'ichi Pignata, Giuliano Hamuy, Mario Quimby, Robert M. Zheng, WeiKang Filippenko, Alexei V. Clubb, Kelsey I. Smith, Nathan Elias-Rosa, Nancy Foley, Ryan J. Miller, Adam A. TI DISAPPEARANCE OF THE PROGENITOR OF SUPERNOVA iPTF13bvn SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE galaxies: individual (NGC 5806); stars: evolution; supernovae: general; supernovae: individual (iPTF13bvn) ID CORE-COLLAPSE SUPERNOVA; BINARY PROGENITOR; LIGHT CURVES; IB SUPERNOVA; SN 2011DH; SUPERGIANT PROGENITOR; STELLAR PHOTOMETRY; DUST EXTINCTION; IA SUPERNOVAE; COMPANION AB Supernova (SN) iPTF13bvn in NGC 5806 was the first Type Ib SN to have been tentatively associated with a progenitor in pre-explosion images. We performed deep ultraviolet (UV) and optical Hubble Space Telescope observations of the SN site similar to 740 days after explosion. We detect an object in the optical bands that is fainter than the pre-explosion object. This dimming is likely not produced by dust absorption in the ejecta; thus, our finding confirms the connection of the progenitor candidate with the SN. The object in our data is likely dominated by the fading SN, implying that the pre-SN flux is mostly due to the progenitor. We compare our revised pre-SN photometry with previously proposed models. Although binary progenitors are favored, models need to be refined. In particular, to comply with our deep UV detection limit, any companion star must be less luminous than a late-O star or substantially obscured by newly formed dust. A definitive progenitor characterization will require further observations to disentangle the contribution of a much fainter SN and its environment. C1 [Folatelli, Gaston; Bersten, Melina C.] Univ Nacl La Plata, IALP, Fac Ciencias Astron & Geofis, CONICET, Paseo Bosque S-N,B1900FWA, La Plata, Buenos Aires, Argentina. [Folatelli, Gaston; Maeda, Keiichi; Bersten, Melina C.; Nomoto, Ken'ichi; Quimby, Robert M.] Univ Tokyo, Kavli Inst Phys & Math Universe WPI, Kashiwa, Chiba 2778583, Japan. [Van Dyk, Schuyler D.] CALTECH, IPAC, Mailcode 100-22, Pasadena, CA 91125 USA. [Kuncarayakti, Hanindyo; Pignata, Giuliano; Hamuy, Mario] Millennium Inst Astrophys MAS, Santiago, Chile. [Kuncarayakti, Hanindyo; Hamuy, Mario] Univ Chile, Dept Astron, Casilla 36-D, Santiago, Chile. [Maeda, Keiichi] Kyoto Univ, Dept Astron, Sakyo Ku, Kitashirakawa Oiwake Cho, Kyoto 6068502, Japan. [Pignata, Giuliano] Univ Andres Bello, Dept Ciencias Fis, Avda Republ 252, Santiago, Chile. [Quimby, Robert M.] San Diego State Univ, Dept Astron, 5500 Campanile Dr, San Diego, CA 92182 USA. [Zheng, WeiKang; Filippenko, Alexei V.; Clubb, Kelsey I.] Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA. [Smith, Nathan] Univ Arizona, Steward Observ, 933 N Cherry Ave, Tucson, AZ 85721 USA. [Elias-Rosa, Nancy] INAF, Osservatorio Astron Padova, Vicolo Osservatorio 5, I-35122 Padua, Italy. [Foley, Ryan J.] Univ Illinois, Dept Astron, 1002 W Green St, Urbana, IL 61801 USA. [Foley, Ryan J.] Univ Illinois, Dept Phys, 1110 W Green St, Urbana, IL 61801 USA. [Miller, Adam A.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,MS 169-506, Pasadena, CA 91109 USA. RP Folatelli, G (reprint author), Univ Nacl La Plata, IALP, Fac Ciencias Astron & Geofis, CONICET, Paseo Bosque S-N,B1900FWA, La Plata, Buenos Aires, Argentina.; Folatelli, G (reprint author), Univ Tokyo, Kavli Inst Phys & Math Universe WPI, Kashiwa, Chiba 2778583, Japan. EM gaston.folatelli@ipmu.jp RI Elias-Rosa, Nancy/D-3759-2014; OI Elias-Rosa, Nancy/0000-0002-1381-9125; Van Dyk, Schuyler/0000-0001-9038-9950 FU STScI [GO-13684, GO-13822, AR-14295]; NASA [NAS5-26555, HST-HF-51325.01, NAS 5-26555]; NSF [AST-1211916, AST-1518052]; TABASGO Foundation (KAIT and research support); Sylvia & Jim Katzman Foundation; Clark and Sharon Winslow; Christopher R. Redlich Fund; WPI Initiative MEXT (Japan); Japan Society for the Promotion of Science (JSPS) KAKENHI [26800100, 23224004, 26400222]; JSPS Open Partnership Bilateral Joint Research Project between Japan and Chile; Millennium Institute of Astrophysics [IC120009]; FONDECYT [3140563]; PRIN-INAF; Alfred P. Sloan Foundation FX This research is supported by grants GO-13684, GO-13822, and AR-14295 from STScI, which is operated by AURA, Inc., under NASA contract NAS5-26555. A.V.F.'s group is also grateful for funding through NSF grant AST-1211916, the TABASGO Foundation (KAIT and research support), the Sylvia & Jim Katzman Foundation, Clark and Sharon Winslow, and the Christopher R. Redlich Fund. This research is supported by the WPI Initiative MEXT (Japan), the Japan Society for the Promotion of Science (JSPS) KAKENHI grants 26800100 (K.M.) 23224004, and 26400222 (K.N.), and by the JSPS Open Partnership Bilateral Joint Research Project between Japan and Chile (K.M.). M.H., G.P., and H.K. acknowledge support from the Millennium Institute of Astrophysics (grant IC120009). H.K. also acknowledges FONDECYT grant 3140563. N.E.R. is supported by PRIN-INAF 2014. R.J.F. acknowledges support from NSF grant AST-1518052 and the Alfred P. Sloan Foundation. A.A.M. acknowledges support by NASA (Hubble Fellowship grant HST-HF-51325.01, under contract NAS 5-26555). Many UC Berkeley undergraduate students helped obtain Lick/Nickel data. Research at Lick Observatory is partially supported by a generous gift from Google. NR 38 TC 4 Z9 4 U1 4 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD JUL 10 PY 2016 VL 825 IS 2 AR L22 DI 10.3847/2041-8205/825/2/L22 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DS4GG UT WOS:000380738800006 ER PT J AU Parks, GK Lee, E Fu, SY Kim, HE Ma, YQ Yang, ZW Liu, Y Lin, N Hong, J Canu, P Dandouras, I Reme, H Goldstein, ML AF Parks, G. K. Lee, E. Fu, S. Y. Kim, H. E. Ma, Y. Q. Yang, Z. W. Liu, Y. Lin, N. Hong, J. Canu, P. Dandouras, I. Reme, H. Goldstein, M. L. TI TRANSPORT OF SOLAR WIND H+ AND He++ IONS ACROSS EARTH'S BOW SHOCK SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE shock waves; solar wind ID QUASI-PERPENDICULAR SHOCKS; HEAT-CONDUCTION; MAGNETIC-FIELD; MACH NUMBER; TEMPERATURE; MODEL; MAGNETOSHEATH; REFORMATION; ANISOTROPY AB We have investigated the dependence of mass, energy, and charge of solar wind ( SW) transport across Earth's bow shock. An examination of 111 crossings during quiet SW in both quasi-perpendicular and quasi-parallel shock regions shows that 64 crossings had various degrees of heating and thermalization of SW. We found 22 crossings where the SW speed was <400 km s(-1). The shock potential of a typical supercritical quasi-perpendicular shock estimated from deceleration of the SW and cutoff energy of electron flat top distribution is similar to 50 Volts. We find that the temperatures of H+ and He++ beams that penetrate the shock can sometimes be nearly the same in the upstream and downstream regions, indicating little or no heating had occurred crossing the bow shock. None of the models predict that the SW can cross the bow shock without heating. Our observations are important constraints for new models of collisionless shocks. C1 [Parks, G. K.; Lin, N.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Lee, E.] Kyung Hee Univ, Sch Space Res, Yongin, South Korea. [Lee, E.] Kyung Hee Univ, Inst Nat Sci, Yongin, South Korea. [Fu, S. Y.; Ma, Y. Q.] Peking Univ, Inst Space Sci, Beijing, Peoples R China. [Kim, H. E.; Hong, J.] Kyung Hee Univ, Sch Space Res, Yongin, South Korea. [Yang, Z. W.; Liu, Y.] Chinese Acad Sci, Key Lab Space Weather, Beijing, Peoples R China. [Canu, P.] Ecole Polytech, Plasma Phys Lab, Paris, France. [Dandouras, I.; Reme, H.] Univ Toulouse 3, IRAP, Toulouse, France. [Dandouras, I.; Reme, H.] CNRS, Toulouse, France. [Goldstein, M. L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA. RP Parks, GK (reprint author), Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. EM parks@ssl.berkeley.edu FU NASA [NNX07AP96G]; National Research Foundation - Ministry of Education of Korea [NRF-2013R1A1A2010711] FX The research at UC Berkeley was performed under NASA Grant No. NNX07AP96G. Cluster is a joint project of the ESA and NASA. The research work by E. Lee was supported in part by the BK21 Plus Program and the Basic Science Research Program (NRF-2013R1A1A2010711) through the National Research Foundation funded by the Ministry of Education of Korea. NR 35 TC 0 Z9 0 U1 1 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD JUL 10 PY 2016 VL 825 IS 2 AR L27 DI 10.3847/2041-8205/825/2/L27 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DS4GG UT WOS:000380738800011 ER PT J AU Kuleshov, MV Jones, MR Rouillard, AD Fernandez, NF Duan, QN Wang, ZC Koplev, S Jenkins, SL Jagodnik, KM Lachmann, A McDermott, MG Monteiro, CD Gundersen, GW Ma'ayan, A AF Kuleshov, Maxim V. Jones, Matthew R. Rouillard, Andrew D. Fernandez, Nicolas F. Duan, Qiaonan Wang, Zichen Koplev, Simon Jenkins, Sherry L. Jagodnik, Kathleen M. Lachmann, Alexander McDermott, Michael G. Monteiro, Caroline D. Gundersen, Gregory W. Ma'ayan, Avi TI Enrichr: a comprehensive gene set enrichment analysis web server 2016 update SO NUCLEIC ACIDS RESEARCH LA English DT Article ID FUNCTIONAL INTERPRETATION; ONTOLOGY TERMS; HUMAN PROTEOME; TOOL; DATABASE; PATHWAY; LIST; INFORMATION; BIOLOGY; SYSTEM AB Enrichment analysis is a popular method for analyzing gene sets generated by genome-wide experiments. Here we present a significant update to one of the tools in this domain called Enrichr. Enrichr currently contains a large collection of diverse gene set libraries available for analysis and download. In total, Enrichr currently contains 180 184 annotated gene sets from 102 gene set libraries. New features have been added to Enrichr including the ability to submit fuzzy sets, upload BED files, improved application programming interface and visualization of the results as clustergrams. Overall, Enrichr is a comprehensive resource for curated gene sets and a search engine that accumulates biological knowledge for further biological discoveries. Enrichr is freely available at: http://amp.pharm.mssm.edu/Enrichr. C1 [Kuleshov, Maxim V.; Jones, Matthew R.; Rouillard, Andrew D.; Fernandez, Nicolas F.; Duan, Qiaonan; Wang, Zichen; Koplev, Simon; Jenkins, Sherry L.; Lachmann, Alexander; McDermott, Michael G.; Monteiro, Caroline D.; Gundersen, Gregory W.; Ma'ayan, Avi] Icahn Sch Med Mt Sinai, Dept Pharmacol & Syst Therapeut, LINCS Data Coordinat & Integrat Ctr BD2K, One Gustave L Levy Pl,Box 1215, New York, NY 10029 USA. [Jagodnik, Kathleen M.] NASA Glenn Res Ctr, Fluid Phys & Transport Proc Branch, 21000 Brookpk Rd, Cleveland, OH 44135 USA. RP Ma'ayan, A (reprint author), Icahn Sch Med Mt Sinai, Dept Pharmacol & Syst Therapeut, LINCS Data Coordinat & Integrat Ctr BD2K, One Gustave L Levy Pl,Box 1215, New York, NY 10029 USA. EM avi.maayan@mssm.edu FU NIH [R01GM098316, U54HL127624, U54CA189201] FX NIH [R01GM098316, U54HL127624 and U54CA189201 to A.M.]. Funding for open access charge: Institutional funds. NR 43 TC 32 Z9 32 U1 6 U2 8 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0305-1048 EI 1362-4962 J9 NUCLEIC ACIDS RES JI Nucleic Acids Res. PD JUL 8 PY 2016 VL 44 IS W1 BP W90 EP W97 DI 10.1093/nar/gkw377 PG 8 WC Biochemistry & Molecular Biology SC Biochemistry & Molecular Biology GA DR3FA UT WOS:000379786800016 PM 27141961 ER PT J AU Xu, LT Dunning, TH AF Xu, Lu T. Dunning, Thom H., Jr. TI Variations in the Nature of Triple Bonds: The N-2, HCN, and HC2H Series SO JOURNAL OF PHYSICAL CHEMISTRY A LA English DT Article ID CASSCF WAVE-FUNCTIONS; SPACE SCF METHOD; POLYATOMIC-MOLECULES; ELECTRONIC-STRUCTURES; QUANTUM-THEORY; VALENCE; BENT; C-2; REPRESENTATIONS; OPTIMIZATION AB The inertness of molecular nitrogen and the reactivity of acetylene suggest there are significant variations in the nature of triple bonds. To understand these differences, we performed generalized valence bond as well as more accurate electronic structure calculations on three molecules with putative triple bonds: N-2, HCN, and HC2H. The calculations predict that the triple bond in HC2H is quite different from the triple bond in N-2 with HCN being an intermediate case but closer to N-2 than HC2H. The triple bond in N-2 is a traditional triple bond with the spins of the electrons in the bonding orbital pairs predominantly singlet coupled in the GVB wave function (92%). In HC2H, however, there is a substantial amount of residual CH(a(4)Sigma(-)) fragment coupling in the triple bond at its equilibrium geometry with the contribution of the perfect pairing spin function dropping to 82% (77% in a full valence GVB calculation). This difference in the nature of the triple bond in N-2 and HC2H may well be responsible for the differences in the reactivities of N-2 and HC2H. C1 [Xu, Lu T.; Dunning, Thom H., Jr.] Univ Illinois, Dept Chem, 600 S Mathews Ave, Urbana, IL 61801 USA. [Xu, Lu T.] Univ Illinois, Dept Aerosp Engn, 104 S Wright St, Urbana, IL 61801 USA. [Xu, Lu T.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Dunning, Thom H., Jr.] Univ Washington, NIAC, Pacific Northwest Natl Lab, Sieg Hall,3960 Benton Lane NE, Seattle, WA 98195 USA. [Dunning, Thom H., Jr.] Univ Washington, Dept Chem, Seattle, WA 98195 USA. RP Dunning, TH (reprint author), Univ Illinois, Dept Chem, 600 S Mathews Ave, Urbana, IL 61801 USA.; Dunning, TH (reprint author), Univ Washington, NIAC, Pacific Northwest Natl Lab, Sieg Hall,3960 Benton Lane NE, Seattle, WA 98195 USA.; Dunning, TH (reprint author), Univ Washington, Dept Chem, Seattle, WA 98195 USA. EM thdjr@illinois.edu FU Distinguished Chair for Research Excellence in Chemistry at the University of Illinois at Urbana-Champaign FX This work was supported by funding from the Distinguished Chair for Research Excellence in Chemistry at the University of Illinois at Urbana-Champaign. NR 39 TC 1 Z9 1 U1 3 U2 5 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 1089-5639 J9 J PHYS CHEM A JI J. Phys. Chem. A PD JUL 7 PY 2016 VL 120 IS 26 BP 4526 EP 4533 DI 10.1021/acs.jpca.6b03631 PG 8 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA DQ8JM UT WOS:000379457100011 PM 27299373 ER PT J AU Aharonian, F Akamatsu, H Akimoto, F Allen, SW Anabuki, N Angelini, L Arnaud, K Audard, M Awaki, H Axelsson, M Bamba, A Bautz, M Blandford, R Brenneman, L Brown, GV Bulbul, E Cackett, E Chernyakova, M Chiao, M Coppi, P Costantini, E de Plaa, J den Herder, JW Done, C Dotani, T Ebisawa, K Eckart, M Enoto, T Ezoe, Y Fabian, AC Ferrigno, C Foster, A Fujimoto, R Fukazawa, Y Furuzawa, A Galeazzi, M Gallo, L Gandhi, P Giustini, M Goldwurm, A Gu, L Guainazzi, M Haba, Y Hagino, K Hamaguchi, K Harrus, I Hatsukade, I Hayashi, K Hayashi, T Hayashida, K Hiraga, J Hornschemeier, A Hoshino, A Hughes, J Iizuka, R Inoue, H Inoue, Y Ishibashi, K Ishida, M Ishikawa, K Ishisaki, Y Itoh, M Iyomoto, N Kaastra, J Kallman, T Kamae, T Kara, E Kataoka, J Katsuda, S Katsuta, J Kawaharada, M Kawai, N Kelley, R Khangulyan, D Kilbourne, C King, A Kitaguchi, T Kitamoto, S Kitayama, T Kohmura, T Kokubun, M Koyama, S Koyama, K Kretschmar, P Krimm, H Kubota, A Kunieda, H Laurent, P Lebrun, F Lee, SH Leutenegger, M Limousin, O Loewenstein, M Long, KS Lumb, D Madejski, G Maeda, Y Maier, D Makishima, K Markevitch, M Matsumoto, H Matsushita, K McCammon, D McNamara, B Mehdipour, M Miller, E Miller, J Mineshige, S Mitsuda, K Mitsuishi, I Miyazawa, T Mizuno, T Mori, H Mori, K Moseley, H Mukai, K Murakami, H Murakami, T Mushotzky, R Nagino, R Nakagawa, T Nakajima, H Nakamori, T Nakano, T Nakashima, S Nakazawa, K Nobukawa, M Noda, H Nomachi, M O'Dell, S Odaka, H Ohashi, T Ohno, M Okajima, T Ota, N Ozaki, M Paerels, F Paltani, S Parmar, A Petre, R Pinto, C Pohl, M Porter, FS Pottschmidt, K Ramsey, B Reynolds, C Russell, H Safi-Harb, S Saito, S Sakai, K Sameshima, H Sato, G Sato, K Sato, R Sawada, M Schartel, N Serlemitsos, P Seta, H Shidatsu, M Simionescu, A Smith, R Soong, Y Stawarz, L Sugawara, Y Sugita, S Szymkowiak, A Tajima, H Takahashi, H Takahashi, T Takeda, S Takei, Y Tamagawa, T Tamura, K Tamura, T Tanaka, T Tanaka, Y Tanaka, Y Tashiro, M Tawara, Y Terada, Y Terashima, Y Tombesi, F Tomida, H Tsuboi, Y Tsujimoto, M Tsunemi, H Tsuru, T Uchida, H Uchiyama, H Uchiyama, Y Ueda, S Ueda, Y Ueno, S Uno, S Urry, M Ursino, E De Vries, C Watanabe, S Werner, N Wik, D Wilkins, D Williams, B Yamada, S Yamaguchi, H Yamaoka, K Yamasaki, NY Yamauchi, M Yamauchi, S Yaqoob, T Yatsu, Y Yonetoku, D Yoshida, A Yuasa, T Zhuravleva, I Zoghbi, A AF Aharonian, Felix Akamatsu, Hiroki Akimoto, Fumie Allen, Steven W. Anabuki, Naohisa Angelini, Lorella Arnaud, Keith Audard, Marc Awaki, Hisamitsu Axelsson, Magnus Bamba, Aya Bautz, Marshall Blandford, Roger Brenneman, Laura Brown, Gregory V. Bulbul, Esra Cackett, Edward Chernyakova, Maria Chiao, Meng Coppi, Paolo Costantini, Elisa de Plaa, Jelle den Herder, Jan-Willem Done, Chris Dotani, Tadayasu Ebisawa, Ken Eckart, Megan Enoto, Teruaki Ezoe, Yuichiro Fabian, Andrew C. Ferrigno, Carlo Foster, Adam Fujimoto, Ryuichi Fukazawa, Yasushi Furuzawa, Akihiro Galeazzi, Massimiliano Gallo, Luigi Gandhi, Poshak Giustini, Margherita Goldwurm, Andrea Gu, Liyi Guainazzi, Matteo Haba, Yoshito Hagino, Kouichi Hamaguchi, Kenji Harrus, Ilana Hatsukade, Isamu Hayashi, Katsuhiro Hayashi, Takayuki Hayashida, Kiyoshi Hiraga, Junko Hornschemeier, Ann Hoshino, Akio Hughes, John Iizuka, Ryo Inoue, Hajime Inoue, Yoshiyuki Ishibashi, Kazunori Ishida, Manabu Ishikawa, Kumi Ishisaki, Yoshitaka Itoh, Masayuki Iyomoto, Naoko Kaastra, Jelle Kallman, Timothy Kamae, Tuneyoshi Kara, Erin Kataoka, Jun Katsuda, Satoru Katsuta, Junichiro Kawaharada, Madoka Kawai, Nobuyuki Kelley, Richard Khangulyan, Dmitry Kilbourne, Caroline King, Ashley Kitaguchi, Takao Kitamoto, Shunji Kitayama, Tetsu Kohmura, Takayoshi Kokubun, Motohide Koyama, Shu Koyama, Katsuji Kretschmar, Peter Krimm, Hans Kubota, Aya Kunieda, Hideyo Laurent, Philippe Lebrun, Francois Lee, Shiu-Hang Leutenegger, Maurice Limousin, Olivier Loewenstein, Michael Long, Knox S. Lumb, David Madejski, Grzegorz Maeda, Yoshitomo Maier, Daniel Makishima, Kazuo Markevitch, Maxim Matsumoto, Hironori Matsushita, Kyoko McCammon, Dan McNamara, Brian Mehdipour, Missagh Miller, Eric Miller, Jon Mineshige, Shin Mitsuda, Kazuhisa Mitsuishi, Ikuyuki Miyazawa, Takuya Mizuno, Tsunefumi Mori, Hideyuki Mori, Koji Moseley, Harvey Mukai, Koji Murakami, Hiroshi Murakami, Toshio Mushotzky, Richard Nagino, Ryo Nakagawa, Takao Nakajima, Hiroshi Nakamori, Takeshi Nakano, Toshio Nakashima, Shinya Nakazawa, Kazuhiro Nobukawa, Masayoshi Noda, Hirofumi Nomachi, Masaharu O'Dell, Steve Odaka, Hirokazu Ohashi, Takaya Ohno, Masanori Okajima, Takashi Ota, Naomi Ozaki, Masanobu Paerels, Frits Paltani, Stephane Parmar, Arvind Petre, Robert Pinto, Ciro Pohl, Martin Porter, F. Scott Pottschmidt, Katja Ramsey, Brian Reynolds, Christopher Russell, Helen Safi-Harb, Samar Saito, Shinya Sakai, Kazuhiro Sameshima, Hiroaki Sato, Goro Sato, Kosuke Sato, Rie Sawada, Makoto Schartel, Norbert Serlemitsos, Peter Seta, Hiromi Shidatsu, Megumi Simionescu, Aurora Smith, Randall Soong, Yang Stawarz, Lukasz Sugawara, Yasuharu Sugita, Satoshi Szymkowiak, Andrew Tajima, Hiroyasu Takahashi, Hiromitsu Takahashi, Tadayuki Takeda, Shin'ichiro Takei, Yoh Tamagawa, Toru Tamura, Keisuke Tamura, Takayuki Tanaka, Takaaki Tanaka, Yasuo Tanaka, Yasuyuki Tashiro, Makoto Tawara, Yuzuru Terada, Yukikatsu Terashima, Yuichi Tombesi, Francesco Tomida, Hiroshi Tsuboi, Yohko Tsujimoto, Masahiro Tsunemi, Hiroshi Tsuru, Takeshi Uchida, Hiroyuki Uchiyama, Hideki Uchiyama, Yasunobu Ueda, Shutaro Ueda, Yoshihiro Ueno, Shiro Uno, Shin'ichiro Urry, Meg Ursino, Eugenio De Vries, Cor Watanabe, Shin Werner, Norbert Wik, Daniel Wilkins, Dan Williams, Brian Yamada, Shinya Yamaguchi, Hiroya Yamaoka, Kazutaka Yamasaki, Noriko Y. Yamauchi, Makoto Yamauchi, Shigeo Yaqoob, Tahir Yatsu, Yoichi Yonetoku, Daisuke Yoshida, Atsumasa Yuasa, Takayuki Zhuravleva, Irina Zoghbi, Abderahmen CA Hitomi Collaboration TI The quiescent intracluster medium in the core of the Perseus cluster SO NATURE LA English DT Article ID X-RAY SPECTROSCOPY; GALAXY CLUSTERS; XMM-NEWTON; TURBULENT VELOCITY; NGC 1275; NGC-1275; LINE; CONSTRAINTS; FEEDBACK; PLASMAS AB Clusters of galaxies are the most massive gravitationally bound objects in the Universe and are still forming. They are thus important probes(1) of cosmological parameters and many astrophysical processes. However, knowledge of the dynamics of the pervasive hot gas, the mass of which is much larger than the combined mass of all the stars in the cluster, is lacking. Such knowledge would enable insights into the injection of mechanical energy by the central supermassive black hole and the use of hydrostatic equilibrium for determining cluster masses. X-rays from the core of the Perseus cluster are emitted by the 50-million-kelvin diffuse hot plasma filling its gravitational potential well. The active galactic nucleus of the central galaxy NGC 1275 is pumping jetted energy into the surrounding intracluster medium, creating buoyant bubbles filled with relativistic plasma. These bubbles probably induce motions in the intracluster medium and heat the inner gas, preventing runaway radiative cooling-a process known as active galactic nucleus feedback(2-6). Here we report X-ray observations of the core of the Perseus cluster, which reveal a remarkably quiescent atmosphere in which the gas has a line-of-sight velocity dispersion of 164 +/- 10 kilometres per second in the region 30-60 kiloparsecs from the central nucleus. A gradient in the line-of-sight velocity of 150 +/- 70 kilometres per second is found across the 60-kiloparsec image of the cluster core. Turbulent pressure support in the gas is four per cent of the thermodynamic pressure, with large-scale shear at most doubling this estimate. We infer that a total cluster mass determined from hydrostatic equilibrium in a central region would require little correction for turbulent pressure. C1 [Aharonian, Felix; Chernyakova, Maria] Dublin Inst Adv Studies, Astron & Astrophys Sect, Dublin 2, Ireland. [Aharonian, Felix] Natl Res Nucl Univ MEPHI, Moscow 115409, Russia. [Akamatsu, Hiroki; Costantini, Elisa; de Plaa, Jelle; den Herder, Jan-Willem; Giustini, Margherita; Gu, Liyi; Kaastra, Jelle; Mehdipour, Missagh; De Vries, Cor] SRON Netherlands Inst Space Res, Utrecht, Netherlands. [Akimoto, Fumie; Furuzawa, Akihiro; Hayashi, Takayuki; Ishibashi, Kazunori; Kunieda, Hideyo; Mitsuishi, Ikuyuki; Miyazawa, Takuya; Tamura, Keisuke; Tawara, Yuzuru; Yamaoka, Kazutaka] Nagoya Univ, Dept Phys, Nagoya, Aichi 4648602, Japan. [Allen, Steven W.; Blandford, Roger; Kamae, Tuneyoshi; King, Ashley; Madejski, Grzegorz; Werner, Norbert; Zhuravleva, Irina] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA. [Allen, Steven W.; Blandford, Roger; King, Ashley; Werner, Norbert; Zhuravleva, Irina] Stanford Univ, Dept Phys, 382 Via Pueblo Mall, Stanford, CA 94305 USA. [Allen, Steven W.; Blandford, Roger; Madejski, Grzegorz] SLAC Natl Accelerator Lab, 2575 Sand Hill Rd, Menlo Pk, CA 94025 USA. [Anabuki, Naohisa; Hayashida, Kiyoshi; Nagino, Ryo; Nakajima, Hiroshi; Tsunemi, Hiroshi] Osaka Univ, Dept Earth & Space Sci, Osaka 5600043, Japan. [Angelini, Lorella; Arnaud, Keith; Chiao, Meng; Eckart, Megan; Hamaguchi, Kenji; Harrus, Ilana; Hornschemeier, Ann; Kallman, Timothy; Kelley, Richard; Kilbourne, Caroline; Krimm, Hans; Leutenegger, Maurice; Loewenstein, Michael; Markevitch, Maxim; Mori, Hideyuki; Moseley, Harvey; Mukai, Koji; Okajima, Takashi; Petre, Robert; Porter, F. Scott; Pottschmidt, Katja; Sakai, Kazuhiro; Serlemitsos, Peter; Soong, Yang; Tombesi, Francesco; Wik, Daniel; Williams, Brian; Yamaguchi, Hiroya; Yaqoob, Tahir] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Arnaud, Keith; Kara, Erin; Loewenstein, Michael; Mushotzky, Richard; Reynolds, Christopher] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Audard, Marc; Ferrigno, Carlo; Paltani, Stephane; Pohl, Martin] Univ Geneva, CH-1211 Geneva 4, Switzerland. [Awaki, Hisamitsu; Terashima, Yuichi] Ehime Univ, Dept Phys, Matsuyama, Ehime 7908577, Japan. [Axelsson, Magnus; Ezoe, Yuichiro; Ishisaki, Yoshitaka; Ohashi, Takaya; Seta, Hiromi; Yamada, Shinya] Tokyo Metropolitan Univ, Dept Phys, Tokyo 1920397, Japan. [Bamba, Aya; Nakazawa, Kazuhiro] Univ Tokyo, Dept Phys, Tokyo 1130033, Japan. [Bautz, Marshall; Bulbul, Esra; Miller, Eric] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Brenneman, Laura; Foster, Adam; Smith, Randall] Smithsonian Astrophys Observ, 60 Garden St,MS-4, Cambridge, MA 02138 USA. [Brown, Gregory V.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA. [Cackett, Edward; Fabian, Andrew C.; Pinto, Ciro; Russell, Helen] Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England. [Coppi, Paolo; Szymkowiak, Andrew; Urry, Meg] Yale Univ, Yale Ctr Astron & Astrophys, New Haven, CT 06520 USA. [Done, Chris] Univ Durham, Dept Phys, Durham DH1 3LE, England. [Dotani, Tadayasu; Ebisawa, Ken; Guainazzi, Matteo; Hagino, Kouichi; Hayashi, Katsuhiro; Iizuka, Ryo; Inoue, Hajime; Inoue, Yoshiyuki; Ishida, Manabu; Kokubun, Motohide; Koyama, Shu; Lee, Shiu-Hang; Maeda, Yoshitomo; Mitsuda, Kazuhisa; Nakagawa, Takao; Nakashima, Shinya; Odaka, Hirokazu; Ozaki, Masanobu; Sameshima, Hiroaki; Sato, Goro; Sato, Rie; Simionescu, Aurora; Takahashi, Tadayuki; Takei, Yoh; Tamura, Takayuki; Tanaka, Yasuo; Tomida, Hiroshi; Tsujimoto, Masahiro; Ueda, Shutaro; Ueno, Shiro; Watanabe, Shin; Yamasaki, Noriko Y.] Japan Aerosp Explorat Agcy JAXA, ISAS, Sagamihara, Kanagawa 2525210, Japan. [Enoto, Teruaki; Mineshige, Shin; Ueda, Yoshihiro] Kyoto Univ, Dept Astron, Kyoto 6068502, Japan. [Enoto, Teruaki] Kyoto Univ, Hakubi Ctr Adv Res, Kyoto 6068302, Japan. [Fujimoto, Ryuichi; Murakami, Toshio; Yonetoku, Daisuke] Kanazawa Univ, Fac Math & Phys, Kanazawa, Ishikawa 9201192, Japan. [Fukazawa, Yasushi; Katsuta, Junichiro; Kitaguchi, Takao; Mizuno, Tsunefumi; Ohno, Masanori; Takahashi, Hiromitsu; Tanaka, Yasuyuki] Hiroshima Univ, Dept Phys Sci, Hiroshima 7398526, Japan. [Galeazzi, Massimiliano; Ursino, Eugenio] Univ Miami, Dept Phys, Miami, FL 33124 USA. [Gallo, Luigi; Wilkins, Dan] St Marys Univ, Dept Phys & Astron, Halifax, NS B3H 3C3, Canada. [Gandhi, Poshak] Univ Southampton, Dept Phys & Astron, Southampton SO17 1BJ, Hants, England. [Goldwurm, Andrea; Laurent, Philippe; Lebrun, Francois; Limousin, Olivier; Maier, Daniel] CEA Saclay, IRFU Serv Astrophys, F-91191 Gif Sur Yvette, France. [Guainazzi, Matteo; Kretschmar, Peter; Schartel, Norbert] ESAC, ESA, Madrid, Spain. [Haba, Yoshito] Aichi Univ Educ, Dept Phys & Astron, Kariya, Aichi 4488543, Japan. [Hamaguchi, Kenji; Harrus, Ilana; Mukai, Koji; Pottschmidt, Katja; Yaqoob, Tahir] Univ Maryland Baltimore Cty, Dept Phys, 1000 Hilltop Circle, Baltimore, MD 21250 USA. [Hatsukade, Isamu; Mori, Koji; Yamauchi, Makoto] Miyazaki Univ, Dept Appl Phys & Elect Engn, Miyazaki 8892192, Japan. [Hiraga, Junko] Kwansei Gakuin Univ, Sch Sci & Technol, Dept Phys, Nishinomiya, Hyogo 6691337, Japan. [Hoshino, Akio; Khangulyan, Dmitry; Kitamoto, Shunji; Saito, Shinya; Uchiyama, Yasunobu] Rikkyo Univ, Dept Phys, Tokyo 1718501, Japan. [Hughes, John] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. [Ishikawa, Kumi; Nakano, Toshio; Noda, Hirofumi; Tamagawa, Toru; Yuasa, Takayuki] RIKEN, Nishina Ctr, 2-1 Hirosawa, Wako, Saitama 3510198, Japan. [Itoh, Masayuki] Kobe Univ, Fac Human Dev, Kobe, Hyogo 6578501, Japan. [Iyomoto, Naoko] Kyushu Univ, Fukuoka 8190395, Japan. [Kataoka, Jun] Waseda Univ, Res Inst Sci & Engn, Tokyo 1698555, Japan. [Katsuda, Satoru; Sugawara, Yasuharu; Tsuboi, Yohko] Chuo Univ, Dept Phys, Tokyo 1128551, Japan. [Kawaharada, Madoka] Japan Aerosp Explorat Agcy JAXA, Tsukuba Space Ctr TKSC, Tsukuba, Ibaraki 3058505, Japan. [Kawai, Nobuyuki; Sugita, Satoshi; Yatsu, Yoichi] Tokyo Inst Technol, Dept Phys, Tokyo 1528551, Japan. [Kitayama, Tetsu] Toho Univ, Dept Phys, Chiba 2748510, Japan. [Kohmura, Takayoshi] Tokyo Univ Sci, Dept Phys, Chiba 2788510, Japan. [Koyama, Katsuji; Tanaka, Takaaki; Tsuru, Takeshi; Uchida, Hiroyuki] Kyoto Univ, Dept Phys, Kyoto 6068502, Japan. [Krimm, Hans] Univ Space Res Assoc, 7178 Columbia Gateway Dr, Columbia, MD 21046 USA. [Kubota, Aya] Shibaura Inst Technol, Dept Elect Informat Syst, Saitama 3378570, Japan. [Long, Knox S.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Lumb, David; Parmar, Arvind] ESTEC, ESA, NL-2200 AG Noordwijk, Netherlands. [Makishima, Kazuo; Shidatsu, Megumi] RIKEN, 2-1 Hirosawa, Wako, Saitama 3510198, Japan. [Matsumoto, Hironori] Nagoya Univ, Kobayashi Maskawa Inst, Nagoya, Aichi 4648602, Japan. [Matsushita, Kyoko; Sato, Kosuke] Tokyo Univ Sci, Dept Phys, Tokyo 1628601, Japan. [McCammon, Dan] Univ Wisconsin, Dept Phys, Madison, WI 53706 USA. [McNamara, Brian] Univ Waterloo, Waterloo, ON N2L 3G1, Canada. [Miller, Jon; Zoghbi, Abderahmen] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Murakami, Hiroshi] Tohoku Gakuin Univ, Fac Liberal Arts, Dept Informat Sci, Sendai, Miyagi 9813193, Japan. [Nakamori, Takeshi] Yamagata Univ, Dept Phys, Fac Sci, Yamagata 9908560, Japan. [Nobukawa, Masayoshi] Nara Univ Educ, Dept Teacher Training, Takabatake Cho, Nara 6308528, Japan. [Nobukawa, Masayoshi] Nara Univ Educ, Sch Educ, Takabatake Cho, Nara 6308528, Japan. [Nomachi, Masaharu] Osaka Univ, Res Ctr Nucl Phys Toyonaka, 1-1 Machikaneyama Machi, Toyonaka, Osaka 5600043, Japan. [O'Dell, Steve; Ramsey, Brian] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. [Ota, Naomi; Yamauchi, Shigeo] Nara Womens Univ, Fac Sci, Dept Phys, Nara 6308506, Japan. [Paerels, Frits] Columbia Univ, Dept Astron, New York, NY 10027 USA. [Safi-Harb, Samar] Univ Manitoba, Dept Phys & Astron, Winnipeg, MB R3T 2N2, Canada. [Sawada, Makoto; Yoshida, Atsumasa] Aoyama Gakuin Univ, Dept Math & Phys, Sagamihara, Kanagawa 2525258, Japan. [Stawarz, Lukasz] Jagiellonian Univ, Astron Observ, PL-30244 Krakow, Poland. [Tajima, Hiroyasu] Nagoya Univ, Inst Space Earth Environm Res, Nagoya, Aichi 4648601, Japan. [Takeda, Shin'ichiro] Grad Univ OIST, Okinawa Inst Sci & Technol, Adv Med Instrumentat Unit, Okinawa 9040495, Japan. [Tashiro, Makoto; Terada, Yukikatsu] Saitama Univ, Dept Phys, Saitama 3388570, Japan. [Uchiyama, Hideki] Shizuoka Univ, Fac Educ, Sci Educ, Shizuoka 4228529, Japan. [Uno, Shin'ichiro] Nihon Fukushi Univ, Fac Hlth Sci, Mihama, Aichi 4750012, Japan. [Wik, Daniel] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. RP Fabian, AC (reprint author), Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England. EM acf@ast.cam.ac.uk RI Yamasaki, Noriko/C-2252-2008; Porter, Frederick/D-3501-2012; Zoghbi, Abderahmen/A-8445-2017; Shidatsu, Megumi/C-5742-2017; OI Porter, Frederick/0000-0002-6374-1119; Zoghbi, Abderahmen/0000-0002-0572-9613; Kretschmar, Peter/0000-0001-9840-2048; , kouichi/0000-0003-4235-5304; De Coppi, Paolo/0000-0002-1659-0207 FU NASA Science Mission Directorate; DoE [DE-AC3-76SF00515]; NASA [NNX15AM19G]; US DoE by LLNL [DE-AC52-07NA27344]; NASA; European Space Agency; CNES; Centre National d'Etudes Spatiales; NWO, the Netherlands Organization for Scientific Research; Swiss Secretariat for Education, Research and Innovation SERI; ESA's PRODEX programme; Canadian Space Agency; JSPS/MEXT KAKENHI [15H02070, 15K05107, 23340071, 26109506, 24103002, 25400236, 25800119, 25400237, 25287042, 24540229, 25105516, 23540280, 25400235, 25247028, 26800095, 25400231, 26220703, 24105007, 23340055, 15H00773, 23000004, 15H02090, 15K17610, 15H05438, 15H00785, 24540232]; NWO via a Veni grant; JSPS; STFC [ST/L00075X/1]; JAXA; UK Science and Technology Funding Council (STFC) [ST/J003697/2]; ERC [340442]; JAXA/ISAS; JAXA/TKSC; NASA/GSFC; Noqsi Aerospace Ltd; Stanford U/KIPAC; ESA (Netherlands); SRON; CSA FX We acknowledge all the JAXA members who have contributed to the ASTRO-H (Hitomi) project. All US members gratefully acknowledge support through the NASA Science Mission Directorate. Stanford and SLAC members acknowledge support via DoE contract to SLAC National Accelerator Laboratory DE-AC3-76SF00515 and NASA grant NNX15AM19G. Part of this work was performed under the auspices of the US DoE by LLNL under contract DE-AC52-07NA27344 and also supported by NASA grants to LLNL. Support from the European Space Agency is gratefully acknowledged. French members acknowledge support from CNES, the Centre National d'Etudes Spatiales. SRON is supported by NWO, the Netherlands Organization for Scientific Research. The Swiss team acknowledges support of the Swiss Secretariat for Education, Research and Innovation SERI and ESA's PRODEX programme. The Canadian Space Agency is acknowledged for the support of Canadian members. We acknowledge support from JSPS/MEXT KAKENHI grant numbers 15H02070, 15K05107, 23340071, 26109506, 24103002, 25400236, 25800119, 25400237, 25287042, 24540229, 25105516, 23540280, 25400235, 25247028, 26800095, 25400231, 25247028, 26220703, 24105007, 23340055, 15H00773, 23000004, 15H02090, 15K17610, 15H05438, 15H00785 and 24540232. H. Akamatsu acknowledges support of NWO via a Veni grant. M. Axelsson acknowledges a JSPS International Research Fellowship. C. Done acknowledges STFC funding under grant ST/L00075X/1. P. Gandhi acknowledges a JAXA International Top Young Fellowship and UK Science and Technology Funding Council (STFC) grant ST/J003697/2. H. Russell, A. C. Fabian and C. Pinto acknowledge support from ERC Advanced Grant Feedback 340442. We thank contributions by many companies, including, in particular, NEC, Mitsubishi Heavy Industries, Sumitomo Heavy Industries and Japan Aviation Electronics Industry. Finally, we acknowledge strong support from the following engineers. JAXA/ISAS: C. Baluta, N. Bando, A. Harayama, K. Hirose, K. Ishimura, N. Iwata, T. Kawano, S. Kawasaki, K. Minesugi, C. Natsukari, H. Ogawa, M. Ogawa, M. Ohta, T. Okazaki, S.-i. Sakai, Y. Shibano, M. Shida, T. Shimada, A. Wada, T. Yamada; JAXA/TKSC: A. Okamoto, Y. Sato, K. Shinozaki, H. Sugita; Chubu U: Y. Namba; Ehime U: K. Ogi; Kochi U of Technology: T. Kosaka; Miyazaki U: Y. Nishioka; Nagoya U: H. Nagano; NASA/GSFC: T. Bialas, K. Boyce, E. Canavan, M. DiPirro, M. Kimball, C. Masters, D. Mcguinness, J. Miko, T. Muench, J. Pontius, P. Shirron, C. Simmons, G. Sneiderman, T. Watanabe; Noqsi Aerospace Ltd: J. Doty; Stanford U/KIPAC: M. Asai, K. Gilmore; ESA (Netherlands): C. Jewell; SRON: D. Haas, M. Frericks, P. Laubert, P. Lowes; U of Geneva: P. Azzarello; CSA: A. Koujelev, F. Moroso. NR 37 TC 7 Z9 7 U1 11 U2 19 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 EI 1476-4687 J9 NATURE JI Nature PD JUL 7 PY 2016 VL 535 IS 7610 BP 117 EP + DI 10.1038/nature18627 PG 15 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA DQ2EU UT WOS:000379015600035 ER PT J AU Abbott, BP Abbott, R Abbott, TD Abernathy, MR Acernese, F Ackley, K Adamo, M Adams, C Adams, T Addesso, P Adhikari, RX Adya, VB Affeldt, C Agathos, M Agatsuma, K Aggarwal, N Aguiar, OD Aiello, L Ain, A Ajith, P Allen, B Allocca, A Altin, PA Anderson, SB Anderson, WG Arai, K Araya, MC Arceneaux, CC Areeda, JS Arnaud, N Arun, KG Ascenzi, S Ashton, G Ast, M Aston, SM Astone, P Aufmuth, P Aulbert, C Babak, S Bacon, P Bader, MKM Baker, PT Baldaccini, F Ballardin, G Ballmer, SW Barayoga, JC Barclay, SE Barish, BC Barker, D Barone, F Barr, B Barsotti, L Barsuglia, M Barta, D Bartlett, J Bartos, I Bassiri, R Basti, A Batch, JC Baune, C 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Vahlbruch, H. Vajente, G. Valdes, G. van Bakel, N. van Beuzekom, M. van den Brand, J. F. J. Van den Broeck, C. Vander-Hyde, D. C. van der Schaaf, L. van Heijningen, J. V. van Veggel, A. A. Vardaro, M. Vass, S. Vasuth, M. Vaulin, R. Vecchio, A. Vedovato, G. Veitch, J. Veitch, P. J. Venkateswara, K. Verkindt, D. Vetrano, F. Vicere, A. Vinciguerra, S. Vine, D. J. Vinet, J-Y Vitale, S. Vo, T. Vocca, H. Vorvick, C. Voss, D. Vousden, W. D. Vyatchanin, S. P. Wade, A. R. Wade, L. E. Wade, M. Walker, M. Wallace, L. Walsh, S. Wang, G. Wang, H. Wang, M. Wang, X. Wang, Y. Ward, R. L. Warner, J. Was, M. Weaver, B. Wei, L-W Weinert, M. Weinstein, A. J. Weiss, R. Welborn, T. Wen, L. Wessels, P. Westphal, T. Wette, K. Whelan, J. T. Whitcomb, S. White, D. J. Whiting, B. F. Williams, R. D. Williamson, A. R. Willis, J. L. Willke, B. Wimmer, M. H. Winkler, W. Wipf, C. C. Wittel, H. Woan, G. Worden, J. Wright, J. L. Wu, G. Yablon, J. Yam, W. Yamamoto, H. Yancey, C. C. Yap, M. J. Yu, H. Yvert, M. Zadrozny, A. Zangrando, L. Zanolin, M. Zendri, J-P Zevin, M. Zhang, F. Zhang, L. Zhang, M. Zhang, Y. Zhao, C. Zhou, M. Zhou, Z. Zhu, X. J. Zotov, N. Zucker, M. E. Zuraw, S. E. Zweizig, J. CA LIGO Sci Collaboration Virgo Collaboration TI Characterization of transient noise in Advanced LIGO relevant to gravitational wave signal GW150914 SO CLASSICAL AND QUANTUM GRAVITY LA English DT Article DE gravitational waves; detector characterization; GW150914 AB On 14 September 2015, a gravitational wave signal from a coalescing black hole binary system was observed by the Advanced LIGO detectors. This paper describes the transient noise backgrounds used to determine the significance of the event (designated GW150914) and presents the results of investigations into potential correlated or uncorrelated sources of transient noise in the detectors around the time of the event. The detectors were operating nominally at the time of GW150914. 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[Hoak, D.; Lombardi, A. L.; Nedkova, K.; Zuraw, S. E.] Univ Massachusetts, Amherst, MA 01003 USA. [Hollitt, S. E.; Hosken, D. J.; Munch, J.; Ottaway, D. J.; Veitch, P. J.] Univ Adelaide, Adelaide, SA 5005, Australia. [Huerta, E. A.; McWilliams, S. T.] W Virginia Univ, Morgantown, WV 26506 USA. [Jaranowski, P.] Univ Bialystok, PL-15424 Bialystok, Poland. [Jawahar, S.; Lockerbie, N. A.; Tokmakov, K. V.] Univ Strathclyde, SUPA, Glasgow G1 1XQ, Lanark, Scotland. [Haris, K.; Pai, A.; Saleem, M.] IISER TVM, CET Campus, Trivandrum 695016, Kerala, India. [Khazanov, E. A.; Palashov, O.; Sergeev, A.] Inst Appl Phys, Nizhnii Novgorod 603950, Russia. [Kim, J.; Kim, Y-M; Lee, C. H.] Pusan Natl Univ, Pusan 609735, South Korea. [Kim, K.; Lee, H. K.] Hanyang Univ, Seoul 133791, South Korea. [Krolak, A.; Kutynia, A.; Zadrozny, A.] NCBJ, PL-05400 Otwock, Poland. [Krolak, A.] IM PAN, PL-00956 Warsaw, Poland. [Lange, J.; O'Shaughnessy, R.; Whelan, J. 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H.] Whitman Coll, 345 Boyer Ave, Walla Walla, WA 99362 USA. [Oh, J. J.; Oh, S. H.; Son, E. J.] Natl Inst Math Sci, Daejeon 305390, South Korea. [Penn, S.] Hobart & William Smith Coll, Geneva, NY 14456 USA. [Rosinska, D.] Univ Zielona Gora, Janusz Gil Inst Astron, PL-65265 Zielona Gora, Poland. [Summerscales, T. Z.] Andrews Univ, Berrien Springs, MI 49104 USA. [Trozzo, L.] Univ Siena, Via Laterina 8, I-53100 Siena, Italy. [Bozzi, A.; Ugolini, D.] Trinity Univ, San Antonio, TX 78212 USA. [Venkateswara, K.] Univ Washington, Seattle, WA 98195 USA. [Wade, L. E.; Wade, M.] Kenyon Coll, Gambier, OH 43022 USA. [Willis, J. L.] Abilene Christian Univ, Abilene, TX 79699 USA. [Zotov, N.] Louisiana Tech Univ, Ruston, LA 71272 USA. RP Abbott, BP (reprint author), CALTECH, LIGO, Pasadena, CA 91125 USA. RI Zhu, Xingjiang/E-1501-2016; Pinto, Innocenzo/L-3520-2016; Conti, Livia/F-8565-2013; Vicere, Andrea/J-1742-2012; Sigg, Daniel/I-4308-2015; Rocchi, Alessio/O-9499-2015; Costa, Cesar/G-7588-2012; Gemme, Gianluca/C-7233-2008; Strain, Kenneth/D-5236-2011; Kumar, Prem/B-6691-2009; Lazzaro, Claudia/L-2986-2016; Stratta, Maria Giuliana/L-3045-2016; De Laurentis, Martina/L-3022-2016; Chow, Jong/A-3183-2008; Frey, Raymond/E-2830-2016; Prokhorov, Leonid/I-2953-2012; Di Virgilio, Angela Dora Vittoria/E-9078-2015; Sergeev, Alexander/F-3027-2017; Harms, Jan/J-4359-2012; McClelland, David/E-6765-2010; Losurdo, Giovanni/K-1241-2014; Iyer, Bala R./E-2894-2012; Travasso, Flavio/J-9595-2016; Tiwari, Shubhanshu/R-8546-2016; Bartos, Imre/A-2592-2017; Punturo, Michele/I-3995-2012; Cella, Giancarlo/A-9946-2012; Leonardi, Matteo/G-9694-2015; Cesarini, Elisabetta/C-4507-2017; Danilishin, Stefan/K-7262-2012; Hild, Stefan/A-3864-2010; Steinlechner, Sebastian/D-5781-2013; Groot, Paul/K-4391-2016; Vecchio, Alberto/F-8310-2015; Graef, Christian/J-3167-2015; Branchesi, Marica/P-2296-2015; prodi, giovanni/B-4398-2010; Ciani, Giacomo/G-1036-2011; Gammaitoni, Luca/B-5375-2009; Ferrante, Isidoro/F-1017-2012; Sorrentino, Fiodor/M-6662-2016; Bell, Angus/E-7312-2011; Garufi, Fabio/K-3263-2015; Marchesoni, Fabio/A-1920-2008; Strigin, Sergey/I-8337-2012 OI Zhu, Xingjiang/0000-0001-7049-6468; Conti, Livia/0000-0003-2731-2656; Vicere, Andrea/0000-0003-0624-6231; Sigg, Daniel/0000-0003-4606-6526; Rocchi, Alessio/0000-0002-1382-9016; Gemme, Gianluca/0000-0002-1127-7406; Strain, Kenneth/0000-0002-2066-5355; Lazzaro, Claudia/0000-0001-5993-3372; Stratta, Maria Giuliana/0000-0003-1055-7980; De Laurentis, Martina/0000-0002-3815-4078; Mandel, Ilya/0000-0002-6134-8946; Murphy, David/0000-0002-8538-815X; Pitkin, Matthew/0000-0003-4548-526X; Veitch, John/0000-0002-6508-0713; Davies, Gareth/0000-0002-4289-3439; Principe, Maria/0000-0002-6327-0628; Gendre, Bruce/0000-0002-9077-2025; Granata, Massimo/0000-0003-3275-1186; Berry, Christopher/0000-0003-3870-7215; Kanner, Jonah/0000-0001-8115-0577; Freise, Andreas/0000-0001-6586-9901; Nelemans, Gijs/0000-0002-0752-2974; Naticchioni, Luca/0000-0003-2918-0730; Khan, Sebastian/0000-0003-4953-5754; Scott, Jamie/0000-0001-6701-6515; Callister, Thomas/0000-0001-9892-177X; Sorazu, Borja/0000-0002-6178-3198; Bondu, Francois/0000-0001-6487-5197; Zweizig, John/0000-0002-1521-3397; Del Pozzo, Walter/0000-0003-3978-2030; Chow, Jong/0000-0002-2414-5402; Frey, Raymond/0000-0003-0341-2636; Di Virgilio, Angela Dora Vittoria/0000-0002-2237-7533; O'Shaughnessy, Richard/0000-0001-5832-8517; Dolique, Vincent/0000-0001-5644-9905; Boschi, Valerio/0000-0001-8665-2293; Papa, M.Alessandra/0000-0002-1007-5298; Vocca, Helios/0000-0002-1200-3917; Farr, Ben/0000-0002-2916-9200; Guidi, Gianluca/0000-0002-3061-9870; McClelland, David/0000-0001-6210-5842; Losurdo, Giovanni/0000-0003-0452-746X; Iyer, Bala R./0000-0002-4141-5179; Travasso, Flavio/0000-0002-4653-6156; Tiwari, Shubhanshu/0000-0003-1611-6625; Punturo, Michele/0000-0001-8722-4485; Cella, Giancarlo/0000-0002-0752-0338; Cesarini, Elisabetta/0000-0001-9127-3167; Danilishin, Stefan/0000-0001-7758-7493; Steinlechner, Sebastian/0000-0003-4710-8548; Groot, Paul/0000-0002-4488-726X; Vecchio, Alberto/0000-0002-6254-1617; Graef, Christian/0000-0002-4535-2603; prodi, giovanni/0000-0001-5256-915X; Ciani, Giacomo/0000-0003-4258-9338; Gammaitoni, Luca/0000-0002-4972-7062; Ferrante, Isidoro/0000-0002-0083-7228; Sorrentino, Fiodor/0000-0002-9605-9829; Bell, Angus/0000-0003-1523-0821; Garufi, Fabio/0000-0003-1391-6168; Marchesoni, Fabio/0000-0001-9240-6793; FU Australian Research Council; Council of Scientific and Industrial Research of India; Department of Science and Technology, India; Science AMP; Engineering Research Board (SERB), India; Ministry of Human Resource Development, India; Spanish Ministerio de Economia y Competitividad; Conselleria d'Economia i Competitivitat of the Govern de les Illes Balears; Conselleria d'Educacio Cultura i Universitats of the Govern de les Illes Balears; National Science Centre of Poland; European Commission; Royal Society; Scottish Funding Council; Scottish Universities Physics Alliance; Hungarian Scientific Research Fund (OTKA); Lyon Institute of Origins (LIO); National Research Foundation of Korea; Industry Canada; Province of Ontario through the Ministry of Economic Development and Innovation; Natural Science and Engineering Research Council Canada; Canadian Institute for Advanced Research; Brazilian Ministry of Science, Technology, and Innovation; Fundacao de Amparo a Pesquisa do Estado de Sao Paulo (FAPESP); Russian Foundation for Basic Research; Leverhulme Trust; Research Corporation; Ministry of Science and Technology (MOST), Taiwan; Kavli Foundation FX The authors gratefully acknowledge the support of the United States National Science Foundation (NSF) for the construction and operation of the LIGO Laboratory and Advanced LIGO as well as the Science and Technology Facilities Council (STFC) of the United Kingdom, the Max-Planck-Society (MPS), and the State of Niedersachsen/Germany for support of the construction of Advanced LIGO and construction and operation of the GEO600 detector. Additional support for Advanced LIGO was provided by the Australian Research Council. The authors gratefully acknowledge the Italian Istituto Nazionale di Fisica Nucleare (INFN), the French Centre National de la Recherche Scientifique (CNRS) and the Foundation for Fundamental Research on Matter supported by the Netherlands Organisation for Scientific Research, for the construction and operation of the Virgo detector and the creation and support of the EGO consortium. The authors also gratefully acknowledge research support from these agencies as well as by the Council of Scientific and Industrial Research of India, Department of Science and Technology, India, Science & Engineering Research Board (SERB), India, Ministry of Human Resource Development, India, the Spanish Ministerio de Economia y Competitividad, the Conselleria d'Economia i Competitivitat and Conselleria d'Educacio Cultura i Universitats of the Govern de les Illes Balears, the National Science Centre of Poland, the European Commission, the Royal Society, the Scottish Funding Council, the Scottish Universities Physics Alliance, the Hungarian Scientific Research Fund (OTKA), the Lyon Institute of Origins (LIO), the National Research Foundation of Korea, Industry Canada and the Province of Ontario through the Ministry of Economic Development and Innovation, the Natural Science and Engineering Research Council Canada, Canadian Institute for Advanced Research, the Brazilian Ministry of Science, Technology, and Innovation, Fundacao de Amparo a Pesquisa do Estado de Sao Paulo (FAPESP), Russian Foundation for Basic Research, the Leverhulme Trust, the Research Corporation, Ministry of Science and Technology (MOST), Taiwan and the Kavli Foundation. The authors gratefully acknowledge the support of the NSF, STFC, MPS, INFN, CNRS and the State of Niedersachsen/Germany for provision of computational resources. NR 43 TC 12 Z9 12 U1 28 U2 54 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0264-9381 EI 1361-6382 J9 CLASSICAL QUANT GRAV JI Class. Quantum Gravity PD JUL 7 PY 2016 VL 33 IS 13 AR 134001 DI 10.1088/0264-9381/33/13/134001 PG 34 WC Astronomy & Astrophysics; Physics, Multidisciplinary; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA DP2QM UT WOS:000378334600003 ER PT J AU Abbott, T Abdalla, FB Allam, S Amara, A Annis, J Armstrong, R Bacon, D Banerji, M Bauer, AH Baxter, E Becker, MR Benoit-Levy, A Bernstein, RA Bernstein, GM Bertin, E Blazek, J Bonnett, C Bridle, SL Brooks, D Bruderer, C Buckley-Geer, E Burke, DL Busha, MT Capozzi, D Rosell, AC Kind, MC Carretero, J Castander, FJ Chang, C Clampitt, J Crocce, M Cunha, CE D'Andrea, CB da Costa, LN Das, R DePoy, DL Desai, S Diehl, HT Dietrich, JP Dodelson, S Doel, P Drlica-Wagner, A Efstathiou, G Eifler, TF Erickson, B Estrada, J Evrard, AE Neto, AF Fernandez, E Finley, DA Flaugher, B Fosalba, P Friedrich, O Frieman, J Gangkofner, C Garcia-Bellido, J Gaztanaga, E Gerdes, DW Gruen, D Gruendl, RA Gutierrez, G Hartley, W Hirsch, M Honscheid, K Huff, EM Jain, B James, DJ Jarvis, M Kacprzak, T Kent, S Kirk, D Krause, E Kravtsov, A Kuehn, K Kuropatkin, N Kwan, J Lahav, O Leistedt, B Li, TS Lima, M Lin, H MacCrann, N March, M Marshall, JL Martini, P McMahon, RG Melchior, P Miller, CJ Miquel, R Mohr, JJ Neilsen, E Nichol, RC Nicola, A Nord, B Ogando, R Palmese, A Peiris, HV Plazas, AA Refregier, A Roe, N Romer, AK Roodman, A Rowe, B Rykoff, ES Sabiu, C Sadeh, I Sako, M Samuroff, S Sanchez, E Sanchez, C Seo, H Sevilla-Noarbe, I Sheldon, E Smith, RC Soares-Santos, M Sobreira, F Suchyta, E Swanson, MEC Tarle, G Thaler, J Thomas, D Troxel, MA Vikram, V Walker, AR Wechsler, RH Weller, J Zhang, Y Zuntz, J AF Abbott, T. Abdalla, F. B. Allam, S. Amara, A. Annis, J. Armstrong, R. Bacon, D. Banerji, M. Bauer, A. H. Baxter, E. Becker, M. R. Benoit-Levy, A. Bernstein, R. A. Bernstein, G. M. Bertin, E. Blazek, J. Bonnett, C. Bridle, S. L. Brooks, D. Bruderer, C. Buckley-Geer, E. Burke, D. L. Busha, M. T. Capozzi, D. Rosell, A. Carnero Kind, M. Carrasco Carretero, J. Castander, F. J. Chang, C. Clampitt, J. Crocce, M. Cunha, C. E. D'Andrea, C. B. da Costa, L. N. Das, R. DePoy, D. L. Desai, S. Diehl, H. T. Dietrich, J. P. Dodelson, S. Doel, P. Drlica-Wagner, A. Efstathiou, G. Eifler, T. F. Erickson, B. Estrada, J. Evrard, A. E. Fausti Neto, A. Fernandez, E. Finley, D. A. Flaugher, B. Fosalba, P. Friedrich, O. Frieman, J. Gangkofner, C. Garcia-Bellido, J. Gaztanaga, E. Gerdes, D. W. Gruen, D. Gruendl, R. A. Gutierrez, G. Hartley, W. Hirsch, M. Honscheid, K. Huff, E. M. Jain, B. James, D. J. Jarvis, M. Kacprzak, T. Kent, S. Kirk, D. Krause, E. Kravtsov, A. Kuehn, K. Kuropatkin, N. Kwan, J. Lahav, O. Leistedt, B. Li, T. S. Lima, M. Lin, H. MacCrann, N. March, M. Marshall, J. L. Martini, P. McMahon, R. G. Melchior, P. Miller, C. J. Miquel, R. Mohr, J. J. Neilsen, E. Nichol, R. C. Nicola, A. Nord, B. Ogando, R. Palmese, A. Peiris, H. V. Plazas, A. A. Refregier, A. Roe, N. Romer, A. K. Roodman, A. Rowe, B. Rykoff, E. S. Sabiu, C. Sadeh, I. Sako, M. Samuroff, S. Sanchez, E. Sanchez, C. Seo, H. Sevilla-Noarbe, I. Sheldon, E. Smith, R. C. Soares-Santos, M. Sobreira, F. Suchyta, E. Swanson, M. E. C. Tarle, G. Thaler, J. Thomas, D. Troxel, M. A. Vikram, V. Walker, A. R. Wechsler, R. H. Weller, J. Zhang, Y. Zuntz, J. CA Dark Energy Survey Collaboration TI Cosmology from cosmic shear with Dark Energy Survey Science Verification data SO PHYSICAL REVIEW D LA English DT Article ID MATTER POWER SPECTRUM; WEAK-LENSING TOMOGRAPHY; LARGE-SCALE STRUCTURE; BARYON ACOUSTIC-OSCILLATIONS; INTRINSIC ALIGNMENTS; PARAMETER CONSTRAINTS; GALAXY ELLIPTICITIES; PRECISION COSMOLOGY; COVARIANCE-MATRIX; HUBBLE CONSTANT AB We present the first constraints on cosmology from the Dark Energy Survey (DES), using weak lensing measurements from the preliminary Science Verification (SV) data. We use 139 square degrees of SV data, which is less than 3% of the full DES survey area. Using cosmic shear 2-point measurements over three redshift bins we find sigma(8)(Omega(m)/0.3)(0.5) = 0.81 +/- 0.06 (68% confidence), after marginalizing over 7 systematics parameters and 3 other cosmological parameters. We examine the robustness of our results to the choice of data vector and systematics assumed, and find them to be stable. About 20% of our error bar comes from marginalizing over shear and photometric redshift calibration uncertainties. The current state-of-the-art cosmic shear measurements from CFHTLenS are mildly discrepant with the cosmological constraints from Planck CMB data; our results are consistent with both data sets. Our uncertainties are similar to 30% larger than those from CFHTLenS when we carry out a comparable analysis of the two data sets, which we attribute largely to the lower number density of our shear catalogue. We investigate constraints on dark energy and find that, with this small fraction of the full survey, the DES SV constraints make negligible impact on the Planck constraints. The moderate disagreement between the CFHTLenS and Planck values of sigma(8)(Omega(m)/0.3)(0.5) is present regardless of the value of w. C1 [Abbott, T.; James, D. J.; Smith, R. C.; Walker, A. R.] Natl Opt Astron Observ, Cerro Tololo Interamer Observ, Casilla 603, La Serena, Chile. [Abdalla, F. B.; Benoit-Levy, A.; Brooks, D.; Doel, P.; Hirsch, M.; Kirk, D.; Lahav, O.; Leistedt, B.; Palmese, A.; Peiris, H. V.; Rowe, B.; Sadeh, I.] UCL, Dept Phys & Astron, Gower St, London WC1E 6BT, England. [Allam, S.; Annis, J.; Buckley-Geer, E.; Diehl, H. T.; Dodelson, S.; Drlica-Wagner, A.; Estrada, J.; Finley, D. A.; Flaugher, B.; Frieman, J.; Gutierrez, G.; Kent, S.; Kuropatkin, N.; Lin, H.; Neilsen, E.; Nord, B.; Soares-Santos, M.; Sobreira, F.] Fermilab Natl Accelerator Lab, POB 500, Batavia, IL 60510 USA. [Amara, A.; Bruderer, C.; Chang, C.; Hartley, W.; Kacprzak, T.; Nicola, A.; Refregier, A.] ETH, Dept Phys, Wolfgang Pauli Str 16, CH-8093 Zurich, Switzerland. [Armstrong, R.] Princeton Univ, Dept Astrophys Sci, Peyton Hall, Princeton, NJ 08544 USA. [Bacon, D.; Capozzi, D.; D'Andrea, C. B.; Nichol, R. C.; Thomas, D.] Univ Portsmouth, Inst Cosmol & Gravitat, Portsmouth PO1 3FX, Hants, England. [Banerji, M.; Efstathiou, G.; McMahon, R. G.] Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England. [Banerji, M.; Efstathiou, G.; McMahon, R. G.] Univ Cambridge, Kavli Inst Cosmol, Madingley Rd, Cambridge CB3 0HA, England. [Bauer, A. H.; Carretero, J.; Castander, F. J.; Crocce, M.; Fosalba, P.; Gaztanaga, E.] IEEC CSIC, Inst Ciencies Espai, Campus UAB,Carrer Can Magrans S-N, Barcelona 08193, Spain. [Baxter, E.; Bernstein, G. M.; Clampitt, J.; Eifler, T. F.; Jain, B.; March, M.; Sako, M.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. [Becker, M. R.; Burke, D. L.; Busha, M. T.; Cunha, C. E.; Krause, E.; Roodman, A.; Rykoff, E. S.; Wechsler, R. H.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, POB 2450, Stanford, CA 94305 USA. [Becker, M. R.; Busha, M. T.; Wechsler, R. H.] Stanford Univ, Dept Phys, 382 Via Pueblo Mall, Stanford, CA 94305 USA. [Bernstein, R. A.] Carnegie Observ, 813 Santa Barbara St, Pasadena, CA 91101 USA. [Bertin, E.] Univ Paris 06, Sorbonne Univ, Inst Astrophys Paris, UMR 7095, F-75014 Paris, France. [Bertin, E.] CNRS, UMR 7095, Inst Astrophys Paris, F-75014 Paris, France. [Blazek, J.; Honscheid, K.; Huff, E. M.; Martini, P.; Melchior, P.; Seo, H.; Suchyta, E.] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA. [Bonnett, C.; Carretero, J.; Fernandez, E.; Miquel, R.; Sanchez, C.] Univ Autonoma Barcelona, Inst Fis Altes Energies, E-08193 Barcelona, Spain. [Bridle, S. L.; MacCrann, N.; Samuroff, S.; Troxel, M. A.; Zuntz, J.] Univ Manchester, Sch Phys & Astron, Jodrell Bank, Ctr Astrophys, Oxford Rd, Manchester M13 9PL, Lancs, England. [Burke, D. L.; Roodman, A.; Rykoff, E. S.; Wechsler, R. H.] SLAC Natl Accelerator Lab, Menlo Pk, CA 94025 USA. [Rosell, A. Carnero; da Costa, L. N.; Jarvis, M.; Ogando, R.] Observ Nacl, Rua Gal Jose Cristino 77, BR-20921400 Rio De Janeiro, RJ, Brazil. [Rosell, A. Carnero; da Costa, L. N.; Fausti Neto, A.; Lima, M.; Ogando, R.; Sobreira, F.] Lab Interinst E Astron LIneA, Rua Gal Jose Cristino 77, BR-20921400 Rio De Janeiro, RJ, Brazil. [Kind, M. Carrasco; Gruendl, R. A.; Swanson, M. E. C.] Natl Ctr Supercomp Applicat, 1205 West Clark St, Urbana, IL 61801 USA. [Kind, M. Carrasco; Gruendl, R. A.; Sevilla-Noarbe, I.] Univ Illinois, Dept Astron, 1002 W Green St, Urbana, IL 61801 USA. [Das, R.; Erickson, B.; Evrard, A. E.; Gerdes, D. W.; Miller, C. J.; Tarle, G.; Zhang, Y.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA. [DePoy, D. L.; Li, T. S.; Marshall, J. L.] Texas A&M Univ, George P & Cynthia Woods Mitchell Inst Fundamenta, College Stn, TX 77843 USA. [DePoy, D. L.; Li, T. S.; Marshall, J. L.] Texas A&M Univ, Dept Phys & Astron, College Stn, TX 77843 USA. [Desai, S.; Dietrich, J. P.; Gangkofner, C.; Mohr, J. J.] Univ Munich, Fac Phys, Scheinerstr 1, D-81679 Munich, Germany. [Desai, S.; Dietrich, J. P.; Gangkofner, C.; Mohr, J. J.; Weller, J.] Excellence Cluster Universe, Boltzmannstr 2, D-85748 Garching, Germany. [Dodelson, S.; Frieman, J.; Kravtsov, A.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Eifler, T. F.; Plazas, A. A.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Evrard, A. E.; Miller, C. J.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Friedrich, O.; Gruen, D.; Mohr, J. J.; Weller, J.] Max Planck Inst Extraterr Phys, Giessenbachstr, D-85748 Garching, Germany. [Friedrich, O.; Gruen, D.; Weller, J.] Univ Munich, Fak Phys, Univ Sternwarte, Scheinerstr 1, D-81679 Munich, Germany. [Garcia-Bellido, J.] Univ Autonoma Madrid, Inst Fis Teor IFT UAM CSIC, E-28049 Madrid, Spain. [Honscheid, K.; Huff, E. M.; Melchior, P.; Suchyta, E.] Ohio State Univ, Dept Phys, 174 W 18th Ave, Columbus, OH 43210 USA. [Kuehn, K.] Australian Astron Observ, N Ryde, NSW 2113, Australia. [Kwan, J.; Vikram, V.] Argonne Natl Lab, 9700 South Cass Ave, Lemont, IL 60439 USA. [Lima, M.] Univ Sao Paulo, Inst Fis, Dept Fis Matemat, CP 66318, BR-05314970 Sao Paulo, Brazil. [Martini, P.] Ohio State Univ, Dept Astron, 174 W 18Th Ave, Columbus, OH 43210 USA. [Miquel, R.] Inst Catalana Recerca & Estudis Avancats, E-08010 Barcelona, Spain. [Roe, N.] Lawrence Berkeley Natl Lab, 1 Cyclotron Rd, Berkeley, CA 94720 USA. [Romer, A. K.] Univ Sussex, Dept Phys & Astron, Pevensey Bldg, Brighton BN1 9QH, E Sussex, England. [Sabiu, C.] Korea Astron & Space Sci Inst, Daejeon 305348, South Korea. [Sanchez, E.; Sevilla-Noarbe, I.] Ctr Invest Energet Medioambient & Tecnol CIEMAT, Madrid, Spain. [Seo, H.] Ohio Univ, Dept Phys & Astron, 251B Clippinger Labs, Athens, OH 45701 USA. [Sheldon, E.] Brookhaven Natl Lab, Bldg 510, Upton, NY 11973 USA. [Thaler, J.] Univ Illinois, Dept Phys, 1110 W Green St, Urbana, IL 61801 USA. RP MacCrann, N (reprint author), Univ Manchester, Sch Phys & Astron, Jodrell Bank, Ctr Astrophys, Oxford Rd, Manchester M13 9PL, Lancs, England. EM niall.maccrann@postgrad.manchester.ac.uk; joseph.zuntz@manchester.ac.uk RI Lima, Marcos/E-8378-2010; Ogando, Ricardo/A-1747-2010; Sobreira, Flavia/F-4168-2015; Fernandez, Enrique/L-5387-2014; Gaztanaga, Enrique/L-4894-2014; OI Garcia-Bellido, Juan/0000-0002-9370-8360; Ogando, Ricardo/0000-0003-2120-1154; Sobreira, Flavia/0000-0002-7822-0658; Fernandez, Enrique/0000-0002-6405-9488; Gaztanaga, Enrique/0000-0001-9632-0815; McMahon, Richard/0000-0001-8447-8869; Stern, Corvin/0000-0003-4406-6127; Rowe, Barnaby/0000-0002-7042-9174; Abdalla, Filipe/0000-0003-2063-4345 FU DoE [DE-AC02-98CH10886, DE-SC0007901, DE-FG02-91ER40690]; SFB-Transregio 33 'The Dark Universe' by the Deutsche Forschungsgemeinschaft (DFG); DFG cluster of excellence 'Origin and Structure of the Universe'; NSF [AST-0812790, AST-1138729]; JPL; U.S. Department of Energy; U.S. National Science Foundation; Ministry of Science and Education of Spain; Science and Technology Facilities Council of the United Kingdom; Higher Education Funding Council for England; National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign; Kavli Institute of Cosmological Physics at the University of Chicago; Center for Cosmology and Astro-Particle Physics at the Ohio State University; Mitchell Institute for Fundamental Physics and Astronomy at Texas AM University; Financiadora de Estudos e Projetos; Fundacao Carlos Chagas Filho de Amparo a Pesquisa do Estado do Rio de Janeiro; Conselho Nacional de Desenvolvimento Cientifico e Tecnologico; Ministerio da Ciencia, Tecnologia e Inovacao; Deutsche Forschungsgemeinschaft; Collaborating Institutions in the Dark Energy Survey; National Science Foundation [AST-1138766]; MINECO [AYA2012-39559, ESP2013-48274, FPA2013-47986]; Centro de Excelencia Severo Ochoa [SEV-2012-0234, SEV-2012-0249]; European Research Council under European Union Seventh Framework Programme; ERC grant [240672, 291329, 306478] FX We are grateful for the extraordinary contributions of our CTIO colleagues and the DECam Construction, Commissioning and Science Verification teams in achieving the excellent instrument and telescope conditions that have made this work possible. The success of this project also relies critically on the expertise and dedication of the DES Data Management group. We are very grateful to Iain Murray for advice on importance sampling. We thank Catherine Heymans, Martin Kilbinger, Antony Lewis and Adam Moss for helpful discussion. This paper is DES paper DES-2015-0076 and FermiLab preprint number FERMILAB-PUB-15-285-AE. Sheldon is supported by DoE Grant No. DE-AC02-98CH10886. Gruen was supported by SFB-Transregio 33 'The Dark Universe' by the Deutsche Forschungsgemeinschaft (DFG) and the DFG cluster of excellence 'Origin and Structure of the Universe'. Gangkofner acknowledges the support by the DFG Cluster of Excellence 'Origin and Structure of the Universe'. Jarvis has been supported on this project by NSF Grants No. AST-0812790 and AST-1138729. Jarvis, Bernstein, and Jain are partially supported by DoE Grant No. DE-SC0007901. Melchior was supported by DoE Grant No. DE-FG02-91ER40690. Plazas was supported by DoE Grant No. DE-AC02-98CH10886 and by JPL, run by Caltech under a contract for NASA. Funding for the DES Projects has been provided by the U.S. Department of Energy, the U.S. National Science Foundation, the Ministry of Science and Education of Spain, the Science and Technology Facilities Council of the United Kingdom, the Higher Education Funding Council for England, the National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign, the Kavli Institute of Cosmological Physics at the University of Chicago, the Center for Cosmology and Astro-Particle Physics at the Ohio State University, the Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M University, Financiadora de Estudos e Projetos, Fundacao Carlos Chagas Filho de Amparo a Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Cientifico e Tecnologico and the Ministerio da Ciencia, Tecnologia e Inovacao, the Deutsche Forschungsgemeinschaft and the Collaborating Institutions in the Dark Energy Survey. The DES data management system is supported by the National Science Foundation under Grant No. AST-1138766. The Collaborating Institutions are Argonne National Laboratory, the University of California at Santa Cruz, the University of Cambridge, Centro de Investigaciones Energeticas, Medioambientales y Tecnologicas-Madrid, the University of Chicago, University College London, the DES-Brazil Consortium, the University of Edinburgh, the Eidgenossische Technische Hochschule (ETH) Zurich, Fermi National Accelerator Laboratory, the University of Illinois at Urbana-Champaign, the Institut de Ciencies de l'Espai (IEEC/CSIC), the Institut de Fisica d'Altes Energies, Lawrence Berkeley National Laboratory, the Ludwig-Maximilians Universitat Munchen and the associated Excellence Cluster Universe, the University of Michigan, the National Optical Astronomy Observatory, the University of Nottingham, The Ohio State University, the University of Pennsylvania, the University of Portsmouth, SLAC National Accelerator Laboratory, Stanford University, the University of Sussex, and Texas A&M University. The DES participants from Spanish institutions are partially supported by MINECO under Grants No. AYA2012-39559, ESP2013-48274, FPA2013-47986, and Centro de Excelencia Severo Ochoa SEV-2012-0234 and SEV-2012-0249.; r Research leading to these results has received funding from the European Research Council under the European Union Seventh Framework Programme (FP7/2007-2013) including ERC grant agreements 240672, 291329, and 306478. This paper has gone through internal review by the DES collaboration. NR 118 TC 8 Z9 8 U1 1 U2 6 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 2470-0010 EI 2470-0029 J9 PHYS REV D JI Phys. Rev. D PD JUL 6 PY 2016 VL 94 IS 2 AR 022001 DI 10.1103/PhysRevD.94.022001 PG 22 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA DR1RJ UT WOS:000379682300001 ER PT J AU Becker, MR Troxel, MA MacCrann, N Krause, E Eifler, TF Friedrich, O Nicola, A Refregier, A Amara, A Bacon, D Bernstein, GM Bonnett, C Bridle, SL Busha, MT Chang, C Dodelson, S Erickson, B Evrard, AE Frieman, J Gaztanaga, E Gruen, D Hartley, W Jain, B Jarvis, M Kacprzak, T Kirk, D Kravtsov, A Leistedt, B Peiris, HV Rykoff, ES Sabiu, C Sanchez, C Seo, H Sheldon, E Wechsler, RH Zuntz, J Abbott, T Abdalla, FB Allam, S Armstrong, R Banerji, M Bauer, AH Benoit-Levy, A Bertin, E Brooks, D Buckley-Geer, E Burke, DL Capozzi, D Rosell, AC Kind, MC Carretero, J Castander, FJ Crocce, M Cunha, CE D'Andrea, CB da Costa, LN DePoy, DL Desai, S Diehl, HT Dietrich, JP Doel, P Neto, AF Fernandez, E Finley, DA Flaugher, B Fosalba, P Gerdes, DW Gruendl, RA Gutierrez, G Honscheid, K James, DJ Kuehn, K Kuropatkin, N Lahav, O Li, TS Lima, M Maia, MAG March, M Martini, P Melchior, P Miller, CJ Miquel, R Mohr, JJ Nichol, RC Nord, B Ogando, R Plazas, AA Reil, K Romer, AK Roodman, A Sako, M Sanchez, E Scarpine, V Schubnell, M Sevilla-Noarbe, I Smith, RC Soares-Santos, M Sobreira, F Suchyta, E Swanson, MEC Tarle, G Thaler, J Thomas, D Vikram, V Walker, AR AF Becker, M. R. Troxel, M. A. MacCrann, N. Krause, E. Eifler, T. F. Friedrich, O. Nicola, A. Refregier, A. Amara, A. Bacon, D. Bernstein, G. M. Bonnett, C. Bridle, S. L. Busha, M. T. Chang, C. Dodelson, S. Erickson, B. Evrard, A. E. Frieman, J. Gaztanaga, E. Gruen, D. Hartley, W. Jain, B. Jarvis, M. Kacprzak, T. Kirk, D. Kravtsov, A. Leistedt, B. Peiris, H. V. Rykoff, E. S. Sabiu, C. Sanchez, C. Seo, H. Sheldon, E. Wechsler, R. H. Zuntz, J. Abbott, T. Abdalla, F. B. Allam, S. Armstrong, R. Banerji, M. Bauer, A. H. Benoit-Levy, A. Bertin, E. Brooks, D. Buckley-Geer, E. Burke, D. L. Capozzi, D. Carnero Rosell, A. Kind, M. Carrasco Carretero, J. Castander, F. J. Crocce, M. Cunha, C. E. D'Andrea, C. B. da Costa, L. N. DePoy, D. L. Desai, S. Diehl, H. T. Dietrich, J. P. Doel, P. Fausti Neto, A. Fernandez, E. Finley, D. A. Flaugher, B. Fosalba, P. Gerdes, D. W. Gruendl, R. A. Gutierrez, G. Honscheid, K. James, D. J. Kuehn, K. Kuropatkin, N. Lahav, O. Li, T. S. Lima, M. Maia, M. A. G. March, M. Martini, P. Melchior, P. Miller, C. J. Miquel, R. Mohr, J. J. Nichol, R. C. Nord, B. Ogando, R. Plazas, A. A. Reil, K. Romer, A. K. Roodman, A. Sako, M. Sanchez, E. Scarpine, V. Schubnell, M. Sevilla-Noarbe, I. Smith, R. C. Soares-Santos, M. Sobreira, F. Suchyta, E. Swanson, M. E. C. Tarle, G. Thaler, J. Thomas, D. Vikram, V. Walker, A. R. CA Dark Energy Survey Collaboration TI Cosmic shear measurements with Dark Energy Survey Science Verification data SO PHYSICAL REVIEW D LA English DT Article ID WEAK LENSING SURVEYS; POLARIZATION POWER SPECTRA; GALAXY SHAPE MEASUREMENT; LARGE-SCALE STRUCTURE; COVARIANCE-MATRIX; DISTANT GALAXIES; NOISE BIAS; STATISTICS; IMPACT; SIMULATIONS AB We present measurements of weak gravitational lensing cosmic shear two-point statistics using Dark Energy Survey Science Verification data. We demonstrate that our results are robust to the choice of shear measurement pipeline, either NGMIX or IM3SHAPE, and robust to the choice of two-point statistic, including both real and Fourier-space statistics. Our results pass a suite of null tests including tests for B-mode contamination and direct tests for any dependence of the two-point functions on a set of 16 observing conditions and galaxy properties, such as seeing, airmass, galaxy color, galaxy magnitude, etc. We furthermore use a large suite of simulations to compute the covariance matrix of the cosmic shear measurements and assign statistical significance to our null tests. We find that our covariance matrix is consistent with the halo model prediction, indicating that it has the appropriate level of halo sample variance. We compare the same jackknife procedure applied to the data and the simulations in order to search for additional sources of noise not captured by the simulations. We find no statistically significant extra sources of noise in the data. The overall detection significance with tomography for our highest source density catalog is 9.7 sigma. Cosmological constraints from the measurements in this work are presented in a companion paper. C1 [Becker, M. R.; Busha, M. T.; Wechsler, R. H.] Stanford Univ, Dept Phys, 382 Via Pueblo Mall, Stanford, CA 94305 USA. [Becker, M. R.; Krause, E.; Busha, M. T.; Rykoff, E. S.; Wechsler, R. H.; Burke, D. L.; Cunha, C. E.; Reil, K.; Roodman, A.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, POB 2450, Stanford, CA 94305 USA. [Troxel, M. A.; MacCrann, N.; Bridle, S. L.; Zuntz, J.] Univ Manchester, Sch Phys & Astron, Ctr Astrophys, Jodrell Bank, Oxford Rd, Manchester M13 9PL, Lancs, England. [Eifler, T. F.; Bernstein, G. M.; Jain, B.; Jarvis, M.; March, M.; Sako, M.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. [Eifler, T. F.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Friedrich, O.; Gruen, D.; Mohr, J. J.] Max Planck Inst Extraterr Phys, Giessenbachstr, D-85748 Garching, Germany. [Friedrich, O.; Gruen, D.; Dietrich, J. P.] Univ Munich, Fak Phys, Univ Sternwarte, Scheinerstr 1, D-81679 Munich, Germany. [Nicola, A.; Refregier, A.; Amara, A.; Chang, C.; Hartley, W.; Kacprzak, T.] ETH, Dept Phys, Wolfgang Pauli Str 16, CH-8093 Zurich, Switzerland. [Bacon, D.; Capozzi, D.; D'Andrea, C. B.; Nichol, R. C.; Thomas, D.] Univ Portsmouth, Inst Cosmol & Gravitat, Portsmouth PO1 3FX, Hants, England. [Bonnett, C.; Sanchez, C.; Carretero, J.; Fernandez, E.; Miquel, R.] Univ Autonoma Barcelona, Inst Fis Altes Energies, E-08193 Barcelona, Spain. [Dodelson, S.; Frieman, J.; Allam, S.; Buckley-Geer, E.; Diehl, H. T.; Finley, D. A.; Flaugher, B.; Gutierrez, G.; Kuropatkin, N.; Nord, B.; Scarpine, V.; Soares-Santos, M.; Sobreira, F.] Fermilab Natl Accelerator Lab, POB 500, Batavia, IL 60510 USA. [Dodelson, S.; Frieman, J.; Kravtsov, A.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Erickson, B.; Evrard, A. E.; Gerdes, D. W.; Miller, C. J.; Schubnell, M.; Tarle, G.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA. [Evrard, A. E.; Miller, C. J.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Gaztanaga, E.; Bauer, A. H.; Carretero, J.; Castander, F. J.; Crocce, M.; Fosalba, P.] IEEC CSIC, Inst Ciencies Espai, Campus UAB,Carrer Can Magrans S-N, Barcelona 08193, Spain. [Kirk, D.; Leistedt, B.; Peiris, H. V.; Abdalla, F. B.; Benoit-Levy, A.; Brooks, D.; Doel, P.; Lahav, O.] UCL, Dept Phys & Astron, Gower St, London WC1E 6BT, England. [Rykoff, E. S.; Wechsler, R. H.; Burke, D. L.; Reil, K.; Roodman, A.] SLAC Natl Accelerator Lab, Menlo Pk, CA 94025 USA. [Sabiu, C.] Korea Astron & Space Sci Inst, Daejeon 305348, South Korea. [Seo, H.; Honscheid, K.; Melchior, P.; Suchyta, E.] Ohio State Univ, Dept Phys, 174 W 18th Ave, Columbus, OH 43210 USA. [Sheldon, E.] Brookhaven Natl Lab, Bldg 510, Upton, NY 11973 USA. [Abbott, T.; James, D. J.; Smith, R. C.; Walker, A. R.] Natl Opt Astron Observ, Cerro Tololo Interamer Observ, Casilla 603, La Serena, Chile. [Abdalla, F. B.] Rhodes Univ, Dept Phys & Elect, POB 94, ZA-6140 Grahamstown, South Africa. [Armstrong, R.] Princeton Univ, Dept Astrophys Sci, Peyton Hall, Princeton, NJ 08544 USA. [Banerji, M.] Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England. [Banerji, M.] Univ Cambridge, Kavli Inst Cosmol, Madingley Rd, Cambridge CB3 0HA, England. [Bertin, E.] CNRS, UMR 7095, Inst Astrophys Paris, F-75014 Paris, France. [Bertin, E.] Univ Paris 06, Sorbonne Univ, Inst Astrophys Paris, UMR 7095, F-75014 Paris, France. [Carnero Rosell, A.; da Costa, L. N.; Fausti Neto, A.; Lima, M.; Maia, M. A. G.; Ogando, R.; Sobreira, F.] Lab Interinst E Astron LIneA, Rua Gal Jose Cristino 77, BR-20921400 Rio De Janeiro, RJ, Brazil. [Carnero Rosell, A.; da Costa, L. N.; Maia, M. A. G.; Ogando, R.] Observ Nacl, Rua Gal Jose Cristino 77, BR-20921400 Rio De Janeiro, RJ, Brazil. [Kind, M. Carrasco; Gruendl, R. A.; Sevilla-Noarbe, I.] Univ Illinois, Dept Astron, 1002 W Green St, Urbana, IL 61801 USA. [Kind, M. Carrasco; Gruendl, R. A.; Swanson, M. E. C.] Natl Ctr Supercomp Applicat, 1205 West Clark St, Urbana, IL 61801 USA. [DePoy, D. L.; Li, T. S.] Texas A&M Univ, George P & Cynthia Woods Mitchell Inst Fundamenta, College Stn, TX 77843 USA. [DePoy, D. L.; Li, T. S.] Texas A&M Univ, Dept Phys & Astron, College Stn, TX 77843 USA. [Desai, S.; Mohr, J. J.] Univ Munich, Fac Phys, Scheinerstr 1, D-81679 Munich, Germany. [Desai, S.; Dietrich, J. P.; Mohr, J. J.] Excellence Cluster Universe, Boltzmannstr 2, D-85748 Garching, Germany. [Honscheid, K.; Martini, P.; Melchior, P.; Suchyta, E.] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA. [Kuehn, K.] Australian Astron Observ, N Ryde, NSW 2113, Australia. [Lima, M.] Univ Sao Paulo, Inst Fis, Dept Fis Matemat, CP 66318, BR-05314970 Sao Paulo, SP, Brazil. [Martini, P.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Miquel, R.] Inst Catalana Recerca & Estudis Avancats, E-08010 Barcelona, Spain. [Plazas, A. A.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Romer, A. K.] Univ Sussex, Dept Phys & Astron, Pevensey Bldg, Brighton BN1 9QH, E Sussex, England. [Sanchez, E.; Sevilla-Noarbe, I.] Ctr Invest Energet Medioambientales & Tecnol CIEM, Madrid, Spain. [Thaler, J.] Univ Illinois, Dept Phys, 1110 W Green St, Urbana, IL 61801 USA. [Thomas, D.] Www Sepnet Ac Uk, South East Phys Network, SEPnet, Southampton, Hants, England. [Vikram, V.] Argonne Natl Lab, 9700 South Cass Ave, Lemont, IL 60439 USA. RP Becker, MR (reprint author), Stanford Univ, Dept Phys, 382 Via Pueblo Mall, Stanford, CA 94305 USA.; Becker, MR (reprint author), Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, POB 2450, Stanford, CA 94305 USA. EM beckermr@stanford.edu RI Lima, Marcos/E-8378-2010; Ogando, Ricardo/A-1747-2010; Sobreira, Flavia/F-4168-2015; Fernandez, Enrique/L-5387-2014; Gaztanaga, Enrique/L-4894-2014; OI Ogando, Ricardo/0000-0003-2120-1154; Sobreira, Flavia/0000-0002-7822-0658; Fernandez, Enrique/0000-0002-6405-9488; Gaztanaga, Enrique/0000-0001-9632-0815; Abdalla, Filipe/0000-0003-2063-4345 FU University of Chicago Research Computing Center; National Science Foundation [ACI-1053575, AST-1138766]; European Research Council [240672]; DOE SciDAC grant; SFB-Transregio 33 "The Dark Universe" by the Deutsche Forschungsgemeinaft (DFG); DFG cluster of excellence "Origin and Structure of the Universe"; Swiss National Foundation [20021_14944, 20021_1439606]; NSF [AST-0812790, AST-1138729]; DoE [DE-SC0007901]; FAPESP; CNPq; NASA Astrophysics Data System; U.S. Department of Energy; U.S. National Science Foundation; Ministry of Science and Education of Spain; Science and Technology Facilities Council of the United Kingdom; Higher Education Funding Council for England; National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign; Kavli Institute of Cosmological Physics at the University of Chicago; Center for Cosmology and Astro-Particle Physics at the Ohio State University; Mitchell Institute for Fundamental Physics and Astronomy at Texas AM University; Financiadora de Estudos e Projetos; Fundacao Carlos Chagas Filho de Amparo a Pesquisa do Estado do Rio de Janeiro; Conselho Nacional de Desenvolvimento Cientifico e Tecnologico; Ministerio da Ciencia e Tecnologia; Deutsche Forschungsgemeinschaft; Collaborating Institutions in the Dark Energy Survey; MINECO [AYA2012-39559, ESP2013-48274, FPA2013-47986]; Centro de Excelencia Severo Ochoa [SEV-2012-0234]; ERDF funds from European Union; [NSF-AST-1211838] FX We are grateful for the extraordinary contributions of our CTIO colleagues and the DECam Construction, Commissioning and Science Verification teams in achieving the excellent instrument and telescope conditions that have made this work possible. The success of this project also relies critically on the expertise and dedication of the DES Data Management group. M. R. B. is grateful for the support of the University of Chicago Research Computing Center, and especially Doug Rudd, for the time used to carry out the N-body simulations carried out in this work. M. R. B. would also like to thank Stewart Marshall for his ongoing assistance in using SLAC computing resources. This work used the Extreme Science and Engineering Discovery Environment (XSEDE), which is supported by National Science Foundation grant number ACI-1053575. J. A. Z., M. A. T., S. L. B. acknowledge support from the European Research Council in the form of a Starting Grant with number 240672. M. R. B. and R. H. W. received partial support from NSF-AST-1211838 and from a DOE SciDAC grant. O. F. and D. G. were supported by SFB-Transregio 33 "The Dark Universe" by the Deutsche Forschungsgemeinaft (DFG) and the DFG cluster of excellence "Origin and Structure of the Universe." A.A., A.R., A.N. are supported in part by Grants No. 20021_14944 and No. 20021_1439606 from the Swiss National Foundation. Jarvis has been supported on this project by NSF Grants No. AST-0812790 and No. AST-1138729. Jarvis, Bernstein, and Jain are partially supported by DoE grant DE-SC0007901. M. L. is partially supported by FAPESP and CNPq. This work made extensive use of the NASA Astrophysics Data System and arXiv.org preprint server. Funding for the DES Projects has been provided by the U.S. Department of Energy, the U.S. National Science Foundation, the Ministry of Science and Education of Spain, the Science and Technology Facilities Council of the United Kingdom, the Higher Education Funding Council for England, the National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign, the Kavli Institute of Cosmological Physics at the University of Chicago, the Center for Cosmology and Astro-Particle Physics at the Ohio State University, the Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M University, Financiadora de Estudos e Projetos, Fundacao Carlos Chagas Filho de Amparo a Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Cientifico e Tecnologico and the Ministerio da Ciencia e Tecnologia, the Deutsche Forschungsgemeinschaft and the Collaborating Institutions in the Dark Energy Survey. The DES data management system is supported by the National Science Foundation under Grant Number AST-1138766. The DES participants from Spanish institutions are partially supported by MINECO under grants AYA2012-39559, ESP2013-48274, FPA2013-47986, and Centro de Excelencia Severo Ochoa SEV-2012-0234, some of which include ERDF funds from the European Union.; r The Collaborating Institutions are Argonne National Laboratory, the University of California at Santa Cruz, the University of Cambridge, Centro de Investigaciones Energeticas, Medioambientales y Tecnologicas-Madrid, the University of Chicago, University College London, the DES-Brazil Consortium, the Eidgenossische Technische Hochschule (ETH) Zurich, Fermi National Accelerator Laboratory, the University of Edinburgh, the University of Illinois at Urbana-Champaign, the Institut de Ciencies de l'Espai (IEEC/CSIC), the Institut de Fisica d'Altes Energies, Lawrence Berkeley National Laboratory, the Ludwig-Maximilians Universitat and the associated Excellence Cluster Universe, the University of Michigan, the National Optical Astronomy Observatory, the University of Nottingham, The Ohio State University, the University of Pennsylvania, the University of Portsmouth, SLAC National Accelerator Laboratory, Stanford University, the University of Sussex, and Texas A&M University. This paper is Fermilab publication FERMILAB-PUB-15-303-AE and DES publication DES-2015-0061. This paper has gone through internal review by the DES collaboration. NR 78 TC 16 Z9 16 U1 1 U2 5 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 2470-0010 EI 2470-0029 J9 PHYS REV D JI Phys. Rev. D PD JUL 6 PY 2016 VL 94 IS 2 AR 022002 DI 10.1103/PhysRevD.94.022002 PG 24 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA DR1RJ UT WOS:000379682300002 ER PT J AU Leonard, CD Bull, P Allison, R AF Leonard, C. Danielle Bull, Philip Allison, Rupert TI Spatial curvature endgame: Reaching the limit of curvature determination SO PHYSICAL REVIEW D LA English DT Article ID BARYON ACOUSTIC-OSCILLATION; MATTER POWER SPECTRUM; DARK ENERGY; DISTANCE MEASUREMENTS; CROSS-CORRELATION; COSMIC SHEAR; UNIVERSE; COSMOLOGY; SCALE; RECONSTRUCTION AB Current constraints on spatial curvature show that it is dynamically negligible: vertical bar Omega(K)vertical bar less than or similar to 5 x 10(-3) (95% C.L.). Neglecting it as a cosmological parameter would be premature however, as more stringent constraints on Omega(K) at around the 10(-4) level would offer valuable tests of eternal inflation models and probe novel large-scale structure phenomena. This precision also represents the "curvature floor," beyond which constraints cannot be meaningfully improved due to the cosmic variance of horizon-scale perturbations. In this paper, we discuss what future experiments will need to do in order to measure spatial curvature to this maximum accuracy. Our conservative forecasts show that the curvature floor is unreachable-by an order of magnitude-even with Stage IV experiments, unless strong assumptions are made about dark energy evolution and the Lambda CDM parameter values. We also discuss some of the novel problems that arise when attempting to constrain a global cosmological parameter like Omega(K) with such high precision. Measuring curvature down to this level would be an important validation of systematics characterization in high-precision cosmological analyses. C1 [Leonard, C. Danielle; Allison, Rupert] Univ Oxford, Astrophys, Denys Wilkinson Bldg,Keble Rd, Oxford OX1 3RH, England. [Bull, Philip] CALTECH, Pasadena, CA 91125 USA. [Bull, Philip] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA USA. RP Leonard, CD (reprint author), Univ Oxford, Astrophys, Denys Wilkinson Bldg,Keble Rd, Oxford OX1 3RH, England. EM danielle.leonard@physics.ox.ac.uk FU Natural Sciences and Engineering Research Council of Canada; NASA; ERC [259505] FX We would like to thank Pedro Ferreira and Jo Dunkley for helpful discussions. We also thank the authors of CAMB, which was used in this work. C. D. L. is supported by the Natural Sciences and Engineering Research Council of Canada. P. B.'s research was supported by an appointment to the NASA Postdoctoral Program at the Jet Propulsion Laboratory, California Institute of Technology, administered by Universities Space Research Association under contract with NASA. R. A. is supported by ERC Grant No. 259505. NR 91 TC 0 Z9 0 U1 0 U2 0 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 2470-0010 EI 2470-0029 J9 PHYS REV D JI Phys. Rev. D PD JUL 5 PY 2016 VL 94 IS 2 AR 023502 DI 10.1103/PhysRevD.94.023502 PG 9 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA DR2GK UT WOS:000379722800005 ER PT J AU Chakraborty, S Fu, R Massie, ST Stephens, G AF Chakraborty, Sudip Fu, Rong Massie, Steven T. Stephens, Graeme TI Relative influence of meteorological conditions and aerosols on the lifetime of mesoscale convective systems SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE mesoscale convective systems; aerosols; meteorological parameters ID LIGHTNING ACTIVITY; CLOUDS; PRECIPITATION; INVIGORATION; RETRIEVAL; IMPACTS; LIQUID; AMAZON; RADAR; FLOOD AB Using collocated measurements from geostationary and polar-orbital satellites over tropical continents, we provide a large-scale statistical assessment of the relative influence of aerosols and meteorological conditions on the lifetime of mesoscale convective systems (MCSs). Our results show that MCSs' lifetime increases by 3-24 h when vertical wind shear (VWS) and convective available potential energy (CAPE) are moderate to high and ambient aerosol optical depth (AOD) increases by 1 SD (1s). However, this influence is not as strong as that of CAPE, relative humidity, and VWS, which increase MCSs' lifetime by 3-30 h, 3-27 h, and 3-30 h per 1s of these variables and explain up to 36%, 45%, and 34%, respectively, of the variance of the MCSs' lifetime. AOD explains up to 24% of the total variance of MCSs' lifetime during the decay phase. This result is physically consistent with that of the variation of the MCSs' ice water content (IWC) with aerosols, which accounts for 35% and 27% of the total variance of the IWC in convective cores and anvil, respectively, during the decay phase. The effect of aerosols on MCSs' lifetime varies between different continents. AOD appears to explain up to 20-22% of the total variance of MCSs' lifetime over equatorial South America compared with 8% over equatorial Africa. Aerosols over the Indian Ocean can explain 20% of total variance of MCSs' lifetime over South Asia because such MCSs form and develop over the ocean. These regional differences of aerosol impacts may be linked to different meteorological conditions. C1 [Chakraborty, Sudip; Fu, Rong] Univ Texas Austin, Jackson Sch Geosci, Austin, TX 78712 USA. [Massie, Steven T.] Univ Colorado Boulder, Lab Atmospher & Space Phys, Boulder, CO 80309 USA. [Stephens, Graeme] Jet Prop Lab, Pasadena, CA 91109 USA. RP Chakraborty, S (reprint author), Univ Texas Austin, Jackson Sch Geosci, Austin, TX 78712 USA. EM sudipm@utexas.edu FU NASA [NNX1172G]; Office of Biological & Environmental Research within Department of Energy, Office of Science [DE-SC0011117]; NASA CALIPSO/CLOUDSAT [NNX14AO85G] FX We acknowledge the providers of the ISCCP, CloudSat, TRMM, Aura MLS, Aqua MODIS, and MERRA datasets. S.C. and R.F. were supported by NASA Aura Science Team Grant (NNX1172G) and the Office of Biological & Environmental Research within the Department of Energy, Office of Science Grant (DE-SC0011117). S.T.M. and S.C. are supported by NASA CALIPSO/CLOUDSAT Grant NNX14AO85G. The supercomputer at the University of Texas has been used to store and analyze the data. NR 43 TC 2 Z9 2 U1 5 U2 9 PU NATL ACAD SCIENCES PI WASHINGTON PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA SN 0027-8424 J9 P NATL ACAD SCI USA JI Proc. Natl. Acad. Sci. U. S. A. PD JUL 5 PY 2016 VL 113 IS 27 BP 7426 EP 7431 DI 10.1073/pnas.1601935113 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA DQ2GW UT WOS:000379021700050 PM 27313203 ER PT J AU Saghaian, SM Karaca, HE Souri, M Turabi, AS Noebe, RD AF Saghaian, S. M. Karaca, H. E. Souri, M. Turabi, A. S. Noebe, R. D. TI Tensile shape memory behavior of Ni50.3Ti29.7Hf20 high temperature shape memory alloys SO MATERIALS & DESIGN LA English DT Article DE Shape memory alloys; NiTiHf; Tensile testing; Heat treatments ID INDUCED MARTENSITIC-TRANSFORMATION; SINGLE-CRYSTALS; COMPRESSION ASYMMETRY; POLYCRYSTALLINE NITI; PSEUDOELASTIC NITI; DAMPING CAPACITY; STRESS; STATE; SHEAR AB The effects of heat treatment on the shape memory characteristics of a polycrystalline Ni50.3Ti29.7Hf20 alloy were studied via thermal cycling under stress and isothermal stress cycling experiments in tension. It was revealed that transformation temperatures could be increased above 100 degrees C with aging at temperature above 500 degrees C and in particular were stabilized against stress-free thermal cycling after aging at 500 degrees C. Recoverable strain of similar to 5% was observed for the as-extruded samples and decreased to similar to 4% after aging due to the formation of non-transformable precipitates. The aged alloys demonstrated near perfect shape memory effect under tensile stresses as high as 700 MPa and perfect superelasticity at temperatures up to 230 degrees C. Finally, the tension-compression asymmetry observed in NiTiHf alloys was discussed. (C) 2016 Elsevier Ltd. All rights reserved. C1 [Saghaian, S. M.; Karaca, H. E.; Souri, M.; Turabi, A. S.] Univ Kentucky, Dept Mech Engn, Lexington, KY 40506 USA. [Noebe, R. D.] NASA, Glenn Res Ctr, Mat & Struct Div, Cleveland, OH USA. RP Karaca, HE (reprint author), Univ Kentucky, Dept Mech Engn, Lexington, KY 40506 USA. EM karacahaluk@uky.edu FU NASA EPSCoR [NNX11AQ31A]; NSF [CMMI-1538665]; NASA Transformative Aeronautics Concepts Program (TACP), Transformational Tools & Technologies Project; [KSEF-148-502-15-355] FX This work was supported in part by the NASA EPSCoR NNX11AQ31A, KSEF-148-502-15-355, NSF CMMI-1538665 programs and NASA Transformative Aeronautics Concepts Program (TACP), Transformational Tools & Technologies Project (Dale Hopkins, Technical Lead for Structures & Materials Discipline). NR 30 TC 2 Z9 2 U1 10 U2 33 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0264-1275 EI 1873-4197 J9 MATER DESIGN JI Mater. Des. PD JUL 5 PY 2016 VL 101 BP 340 EP 345 DI 10.1016/j.matdes.2016.03.163 PG 6 WC Materials Science, Multidisciplinary SC Materials Science GA DL1SS UT WOS:000375413100043 ER PT J AU Zuidema, P Redemann, J Haywood, J Wood, R Piketh, S Hipondoka, M Formenti, P AF Zuidema, Paquita Redemann, Jens Haywood, James Wood, Robert Piketh, Stuart Hipondoka, Martin Formenti, Paola TI Smoke and Clouds above the Southeast Atlantic Upcoming Field Campaigns Probe Absorbing Aerosol's Impact on Climate SO BULLETIN OF THE AMERICAN METEOROLOGICAL SOCIETY LA English DT Editorial Material C1 [Zuidema, Paquita] Univ Miami, Miami, FL USA. [Redemann, Jens] NASA, Ames Res Ctr, Mountain View, CA USA. [Haywood, James] Univ Exeter, Exeter, Devon, England. [Wood, Robert] Univ Washington, Seattle, WA 98195 USA. [Piketh, Stuart] North West Univ, Potchefstroom, South Africa. [Hipondoka, Martin] Univ Namibia, Windhoek, Namibia. [Formenti, Paola] Lab Interuniv Syst Atmospher, Creteil, France. RP Zuidema, P (reprint author), Univ Miami, Rosenstiel Sch Marine & Atmospher Sci, 4600 Rickenbacker Causeway, Miami, FL 33149 USA. EM pzuidema@rsmas.miami.edu RI Zuidema, Paquita/C-9659-2013; Wood, Robert/A-2989-2008 OI Zuidema, Paquita/0000-0003-4719-372X; Wood, Robert/0000-0002-1401-3828 NR 2 TC 2 Z9 2 U1 1 U2 1 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0003-0007 EI 1520-0477 J9 B AM METEOROL SOC JI Bull. Amer. Meteorol. Soc. PD JUL PY 2016 VL 97 IS 7 BP 1131 EP 1135 DI 10.1175/BAMS-D-15-00082.1 PG 5 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA DT7GF UT WOS:000381654400006 ER PT J AU Shui, JL Lin, Y Connell, JW Xu, JT Fan, XL Dai, LM AF Shui, Jianglan Lin, Yi Connell, John W. Xu, Jiantie Fan, Xueliu Dai, Liming TI Nitrogen-Doped Holey Graphene for High-Performance Rechargeable Li-O-2 Batteries SO ACS ENERGY LETTERS LA English DT Article ID LITHIUM-OXYGEN BATTERIES; LI-AIR BATTERIES; CATHODE CATALYSTS; POROUS GRAPHENE; REDUCTION; NANOPARTICLES; COMPOSITE; ELECTRODE; OXIDE; ELECTROCATALYST AB Li-air batteries represent cutting edge electrochemical energy storage devices, but their practical applications have been precluded by the high cathode cost, the low discharge/charge efficiency, and/or the short battery lifetime. Here, we developed a low-cost, but very efficient, air electrode from porous nitrogen-doped holey graphene for rechargeable nonaqueous Li-O-2 cells. The resultant Li-O-2 cell can deliver a high round-trip efficiency (85%) and a long cycling life (>100 cycles) under controlled discharge/charge depths or a high capacity of 17 000 mAh/g under the full discharge/charge condition, superior to most other carbonaceous air cathodes. The observed superb performance for the air electrode based on the nitrogen-doped holey graphene can be attributed to its efficient metal-free catalytic activity and three-dimensional mass transport pathway. Therefore, this work represents a new approach to low-cost, efficient, metal-free, binder-free, and hierarchically porous air electrodes useful for energy conversion and storage from N-doped holey graphene. C1 [Shui, Jianglan; Xu, Jiantie; Fan, Xueliu; Dai, Liming] Case Western Reserve Univ, Case Sch Engn, Dept Macromol Sci & Engn, 10900 Euclid Ave, Cleveland, OH 44106 USA. [Lin, Yi] Natl Inst Aerosp, 100 Explorat Way, Hampton, VA 23666 USA. [Lin, Yi] Coll William & Mary, Dept Appl Sci, Williamsburg, VA 23185 USA. [Connell, John W.] NASA, Langley Res Ctr, Adv Mat & Proc Branch, Mail Stop 226, Hampton, VA 23681 USA. [Shui, Jianglan] Beihang Univ, Sch Mat Sci & Engn, Beijing 100191, Peoples R China. RP Dai, LM (reprint author), Case Western Reserve Univ, Case Sch Engn, Dept Macromol Sci & Engn, 10900 Euclid Ave, Cleveland, OH 44106 USA.; Lin, Y (reprint author), Natl Inst Aerosp, 100 Explorat Way, Hampton, VA 23666 USA.; Lin, Y (reprint author), Coll William & Mary, Dept Appl Sci, Williamsburg, VA 23185 USA.; Connell, JW (reprint author), NASA, Langley Res Ctr, Adv Mat & Proc Branch, Mail Stop 226, Hampton, VA 23681 USA. EM yi.lin@nianet.org; john.w.connell@nasa.gov; liming.dai@case.edu FU AFOSR [FA9550-12-1-0037]; NSF-AIR [HP-1343270]; NSF [CMMI-1400274]; Internal Research and Development (IRAD) funds at NASA Langley Research Center FX We acknowledge support from AFOSR (FA9550-12-1-0037), NSF-AIR (HP-1343270), and NSF (CMMI-1400274). Y.L. and J.W.C are grateful for support from Internal Research and Development (IRAD) funds at NASA Langley Research Center. NR 45 TC 1 Z9 1 U1 29 U2 29 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 2380-8195 J9 ACS ENERGY LETT JI ACS Energy Lett. PD JUL PY 2016 VL 1 IS 1 BP 260 EP 265 DI 10.1021/acsenergylett.6b00128 PG 6 WC Chemistry, Physical; Electrochemistry; Energy & Fuels; Nanoscience & Nanotechnology; Materials Science, Multidisciplinary SC Chemistry; Electrochemistry; Energy & Fuels; Science & Technology - Other Topics; Materials Science GA EE5AS UT WOS:000389617700042 ER PT J AU Fang, K Shen, C Fisher, JB Niu, J AF Fang, Kuai Shen, Chaopeng Fisher, Joshua B. Niu, Jie TI Improving Budyko curve-based estimates of long-term water partitioning using hydrologic signatures from GRACE SO WATER RESOURCES RESEARCH LA English DT Article ID SURFACE PROCESSES MODEL; GROUNDWATER DEPLETION; CLIMATE-CHANGE; ANNUAL RUNOFF; EVAPOTRANSPIRATION; FRAMEWORK; BALANCES; CONSTRAINTS; VARIABILITY; SATELLITES AB The Budyko hypothesis provides a first-order estimate of water partitioning into runoff (Q) and evapotranspiration (E). Observations, however, often show significant departures from the Budyko curve; moreover, past improvements to Budyko curve tend to lose predictive power when migrated between regions or to small scales. Here to estimate departures from the Budyko curve, we use hydrologic signatures extracted from Gravity Recovery And Climate Experiment (GRACE) terrestrial water storage anomalies. The signatures include GRACE amplitude as a fraction of precipitation (A/P), interannual variability, and 1-month lag autocorrelation. We created a group of linear models embodying two alternate hypotheses that departures can be predicted by (a) Taylor series expansion based on the deviation of physical characteristics (seasonality, snow fraction, and vegetation index) from reference conditions and (b) surrogate indicators covarying with E, e.g., A/P. These models are fitted using a mesoscale USA data set (HUC4) and then evaluated using world data sets and USA basins <1 x 10(5) km(2). The model with A/P could reduce error by 50% compared to Budyko itself. We found that seasonality and fraction of precipitation as snow account for a major portion of the predictive power of A/P, while the remainder is attributed to unexplained basin characteristics. When migrated to a global data set, type b models performed better than type a. This contrast in transferability is argued to be due to data set limitations and catchment coevolution. The GRACE-based correction performs well for USA basins >1000 km(2) and, according to comparison with other global data sets, is suitable for data fusion purposes, with GRACE error as estimates of uncertainty. C1 [Fang, Kuai; Shen, Chaopeng] Penn State Univ, Dept Civil & Environm Engn, State Coll, PA 16801 USA. [Fisher, Joshua B.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Niu, Jie] Lawrence Berkeley Natl Lab, Berkeley, CA USA. [Niu, Jie] Univ Calif Santa Barbara, Santa Barbara, CA 93106 USA. RP Shen, C (reprint author), Penn State Univ, Dept Civil & Environm Engn, State Coll, PA 16801 USA. EM cshen@engr.psu.edu OI Fisher, Joshua/0000-0003-4734-9085; Shen, Chaopeng/0000-0002-0685-1901 FU Office of Biological and Environmental Research of the US Department of Energy [DE-SC0010620] FX This work was supported by Office of Biological and Environmental Research of the US Department of Energy under contract DE-SC0010620. We thank David Wolock from USGS for providing shapefiles for the USGS basins. Data generated from this study are presented in figure format in the paper, and the data sets can be requested from the corresponding author. We thank Murugesu Sivapalan for some useful discussion about incomplete coevolution. J.B.F. contributed to this work from the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. Constructive comments from anonymous reviewers and the Associate Editor have helped to improve the manuscript. NR 77 TC 1 Z9 1 U1 10 U2 10 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0043-1397 EI 1944-7973 J9 WATER RESOUR RES JI Water Resour. Res. PD JUL PY 2016 VL 52 IS 7 BP 5537 EP 5554 DI 10.1002/2016WR018748 PG 18 WC Environmental Sciences; Limnology; Water Resources SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Water Resources GA DW5KO UT WOS:000383683800035 ER PT J AU Tenenbaum, LF AF Tenenbaum, Laura Faye TI Between a rock and a cold place SO PHYSICS WORLD LA English DT Editorial Material C1 [Tenenbaum, Laura Faye] NASA, Jet Prop Lab, Washington, DC 20546 USA. RP Tenenbaum, LF (reprint author), NASA, Jet Prop Lab, Washington, DC 20546 USA. EM laura.f.tenenbaum@jpl.nasa.gov NR 0 TC 0 Z9 0 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0953-8585 J9 PHYS WORLD JI Phys. World PD JUL PY 2016 VL 29 IS 7 BP 32 EP 35 PG 4 WC Physics, Multidisciplinary SC Physics GA EB7MD UT WOS:000387570800025 ER PT J AU Olkin, C AF Olkin, Cathy TI Our new view of Pluto SO PHYSICS WORLD LA English DT Editorial Material C1 [Olkin, Cathy] Southwest Res Inst, Boulder, CO 80302 USA. [Olkin, Cathy] NASA, New Horizons Mission, Washington, DC 20546 USA. RP Olkin, C (reprint author), Southwest Res Inst, Boulder, CO 80302 USA.; Olkin, C (reprint author), NASA, New Horizons Mission, Washington, DC 20546 USA. EM colkin@boulder.swri.edu NR 0 TC 0 Z9 0 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0953-8585 J9 PHYS WORLD JI Phys. World PD JUL PY 2016 VL 29 IS 7 BP 40 EP 43 PG 4 WC Physics, Multidisciplinary SC Physics GA EB7MD UT WOS:000387570800027 ER PT J AU Bottom, M Shelton, JC Wallace, JK Bartos, R Kuhn, J Mawet, D Mennesson, B Burruss, R Serabyn, E AF Bottom, Michael Shelton, J. Chris Wallace, James K. Bartos, Randall Kuhn, Jonas Mawet, Dimitri Mennesson, Bertrand Burruss, Rick Serabyn, Eugene TI Stellar Double Coronagraph: A Multistage Coronagraphic Platform at Palomar Observatory SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article DE instrumentation: adaptive optics; instrumentation: high angular resolution; planets and satellites: detection ID VORTEX CORONAGRAPH; LABORATORY DEMONSTRATION; MASK; ASTROMETRY; IMAGE AB We present a new instrument, the "Stellar Double Coronagraph," a flexible coronagraphic platform. Designed for Palomar Observatory's 200 '' Hale telescope, its two focal and pupil planes allow for a number of different observing configurations, including multiple vortex coronagraphs in series for improved contrast at small angles. We describe the motivation, design, observing modes, wavefront control approaches, data reduction pipeline, and early science results. We also discuss future directions for the instrument. C1 [Bottom, Michael; Mawet, Dimitri] CALTECH, MC 249-17, Pasadena, CA 91125 USA. [Shelton, J. Chris; Wallace, James K.; Bartos, Randall; Kuhn, Jonas; Mawet, Dimitri; Mennesson, Bertrand; Burruss, Rick; Serabyn, Eugene] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Kuhn, Jonas] ETH, Inst Astron, Wolfgang Pauli Str 27, CH-8093 Zurich, Switzerland. RP Bottom, M (reprint author), CALTECH, MC 249-17, Pasadena, CA 91125 USA. EM mbottom@caltech.edu FU NASA [NNX13AN42H]; National Aeronautics and Space Administration (NASA) FX We are pleased to acknowledge the Palomar Observatory staff for their enthusiastic and excellent support. We thank the referee for a careful and thorough read, and comments which improved the paper. MB is supported by a NASA Space Technology Research Fellowship, grant NNX13AN42H. 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 (NASA). NR 30 TC 3 Z9 3 U1 1 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6280 EI 1538-3873 J9 PUBL ASTRON SOC PAC JI Publ. Astron. Soc. Pac. PD JUL PY 2016 VL 128 IS 965 AR 075003 DI 10.1088/1538-3873/128/965/075003 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EB1LD UT WOS:000387112300010 ER PT J AU Mullally, F Coughlin, JL Thompson, SE Christiansen, J Burke, C Clarke, BD Haas, MR AF Mullally, F. Coughlin, Jeffery L. Thompson, Susan E. Christiansen, Jessie Burke, Christopher Clarke, Bruce D. Haas, Michael R. TI Identifying False Alarms in the Kepler Planet Candidate Catalog SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article DE methods: data analysis; planets and satellites: detection; binaries: eclipsing ID SYSTEMATIC-ERROR CORRECTION; LIGHT CURVES; VALIDATION; POSITIVES; SAMPLE; IDENTIFICATION; SIGNALS AB We present a new automated method to identify instrumental features masquerading as small, long-period planets in the Kepler planet candidate catalog. These systematics, mistakenly identified as planet transits, can have a strong impact on occurrence rate calculations because they cluster in a region of parameter space where Kepler's sensitivity to planets is poor. We compare individual transit-like events to a variety of models of real transits and systematic events and use a Bayesian information criterion to evaluate the likelihood that each event is real. We describe our technique and test its performance on simulated data. Results from this technique are incorporated in the Kepler Q1-Q17 DR24 planet candidate catalog of Coughlin et al. C1 [Mullally, F.; Coughlin, Jeffery L.; Thompson, Susan E.; Burke, Christopher; Clarke, Bruce D.] NASA, Ames Res Ctr, SETI, Moffett Field, CA 94035 USA. [Christiansen, Jessie] CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA. [Haas, Michael R.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Mullally, F (reprint author), NASA, Ames Res Ctr, SETI, Moffett Field, CA 94035 USA. EM fergal.mullally@nasa.gov FU NASA's Science Mission Directorate; NASA [NAS5-26555]; NASA Office of Space Science [NNX13AC07G]; National Aeronautics and Space Administration FX Funding for this Discovery mission is provided by NASA's Science Mission Directorate. All of the data presented in this paper were obtained from the Mikulski Archive for Space Telescopes (MAST). STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. Support for MAST for non-HST data is provided by the NASA Office of Space Science via grant NNX13AC07G and by other grants and contracts. This research has made use of the NASA Exoplanet Archive, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. NR 27 TC 6 Z9 6 U1 1 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6280 EI 1538-3873 J9 PUBL ASTRON SOC PAC JI Publ. Astron. Soc. Pac. PD JUL PY 2016 VL 128 IS 965 AR 074502 DI 10.1088/1538-3873/128/965/074502 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EB1LD UT WOS:000387112300006 ER PT J AU Placek, B Knuth, KH Angerhausen, D AF Placek, Ben Knuth, Kevin H. Angerhausen, Daniel TI Combining Photometry from Kepler and TESS to Improve Short-period Exoplanet Characterization SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article DE methods: data analysis; techniques: photometric ID EXTRASOLAR GIANT PLANETS; LIGHT CURVES; ELLIPSOIDAL VARIATIONS; PHASE CURVES; HOT JUPITER; ORBIT; CONFIRMATION; COMPANIONS; EFFICIENT; EXONEST AB Planets emit thermal radiation and reflect incident light that they receive from their host stars. As a planet orbits its host star the photometric variations associated with these two effects produce very similar phase curves. If observed through only a single bandpass, this leads to a degeneracy between certain planetary parameters that hinder the precise characterization of such planets. However, observing the same planet through two different bandpasses gives much more information about the planet. Here we develop a Bayesian methodology for combining photometry from both Kepler and the Transiting Exoplanet Survey Satellite. In addition, we demonstrate via simulations that one can disentangle the reflected and thermally emitted light from the atmosphere of a hot-Jupiter as well as more precisely constrain both the geometric albedo and day-side temperature of the planet. This methodology can further be employed using various combinations of photometry from the James Webb Space Telescope, the Characterizing ExOplanet Satellite, or the PLATO mission. C1 [Placek, Ben; Knuth, Kevin H.] SUNY Albany, Dept Phys, Albany, NY 12222 USA. [Angerhausen, Daniel] NASA, Goddard Space Flight Ctr, Exoplanets & Stellar Astrophys Lab, Code 667, Greenbelt, MD 20771 USA. [Placek, Ben] Schenectady Cty Community Coll, Ctr Sci & Technol, Schenectady, NY 12305 USA. [Knuth, Kevin H.] SUNY Albany, Dept Informat, Albany, NY 12222 USA. RP Placek, B (reprint author), SUNY Albany, Dept Phys, Albany, NY 12222 USA.; Placek, B (reprint author), Schenectady Cty Community Coll, Ctr Sci & Technol, Schenectady, NY 12305 USA. EM placekbh@sunysccc.edu; kknuth@albany.edu; daniel.angerhausen@nasa.gov FU National Aeronautics and Space Administration FX This research has made use of the Exoplanet Orbit Database and the Exoplanet Data Explorer at exoplanets.org. This research has also made use of the NASA Exoplanet Archive, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. Finally, the authors would like to thank the anonymous reviewer for the very constructive comments on the paper. NR 37 TC 0 Z9 0 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6280 EI 1538-3873 J9 PUBL ASTRON SOC PAC JI Publ. Astron. Soc. Pac. PD JUL PY 2016 VL 128 IS 965 AR 074503 DI 10.1088/1538-3873/128/965/074503 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EB1LD UT WOS:000387112300007 ER PT J AU Van Cleve, JE Howell, SB Smith, JC Clarke, BD Thompson, SE Bryson, ST Lund, MN Handberg, R Chaplin, WJ AF Van Cleve, Jeffrey E. Howell, Steve B. Smith, Jeffrey C. Clarke, Bruce D. Thompson, Susan E. Bryson, Stephen T. Lund, Mikkel N. Handberg, Rasmus Chaplin, William J. TI That's How We Roll: The NASA K2 Mission Science Products and Their Performance Metrics SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article DE asteroseismology; instrumentation: photometers; methods: data analysis; planetary systems; stars: variables: general ID SYSTEMATIC-ERROR CORRECTION; INSTRUMENT NOISE PROPERTIES; SOLAR-TYPE STARS; KEPLER MISSION; PLANETARY CANDIDATES; STELLAR; PHOTOMETRY; CATALOG; ASTEROSEISMOLOGY; CLASSIFICATION AB NASA's exoplanet Discovery mission Kepler was reconstituted as the K2 mission a year after the failure of the second of Kepler's four. reaction wheels in 2013 May. Fine control of the spacecraft pointing is now accomplished through the use of the two remaining well-functioning reaction wheels and balancing the pressure of sunlight on the solar panels, which constrains K2 observations to fields in the ecliptic for up to approximately 80 days each. This pseudo-stable mechanism gives typical roll motion in the focal plane of 1.0 pixels peak-to-peak over 6 hr at the edges of the field, two orders of magnitude greater than typical 6 hr pointing errors in the Kepler primary mission. Despite these roll errors, the joint performance of the flight system and its modified science data processing pipeline restores much of the photometric precision of the primary mission while viewing a wide variety of targets, thus turning adversity into diversity. We define K2 performance metrics for data compression and pixel budget available in each campaign; the photometric noise on exoplanet transit and stellar activity timescales; residual correlations in corrected long-cadence light curves; and the protection of test sinusoidal signals from overfitting in the systematic error removal process. We find that data compression and noise both increase linearly with radial distance from the center of the field of view, with the data compression proportional to star count as well. At the center, where roll motion is nearly negligible, the limiting 6 hr photometric precision for a quiet 12th magnitude star can be as low as 30 ppm, only 25% higher than that of Kepler. This noise performance is achieved without sacrificing signal fidelity; test sinusoids injected into the data are attenuated by less than 10% for signals with periods upto 15 days, so that a wide range of stellar rotation and variability signatures are preserved by the K2 pipeline. At timescales relevant to asteroseismology, light curves derived from K2 archive calibrated pixels have high-frequency noise amplitude within 40% of that achieved by Kepler. The improvements in K2 operations and science data analysis resulting from 1.5 years of experience with this new mission concept, and quantified by the metrics in this paper, will support continuation of K2's already high level of scientific productivity in an extended K2 mission. C1 [Van Cleve, Jeffrey E.; Howell, Steve B.; Smith, Jeffrey C.; Clarke, Bruce D.; Thompson, Susan E.; Bryson, Stephen T.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Van Cleve, Jeffrey E.; Smith, Jeffrey C.; Clarke, Bruce D.; Thompson, Susan E.] SETI Inst, 189 Bernardo Ave, Mountain View, CA 94043 USA. [Lund, Mikkel N.; Chaplin, William J.] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. [Lund, Mikkel N.; Handberg, Rasmus; Chaplin, William J.] Aarhus Univ, Dept Phys & Astron, SAC, Ny Munkegade 120, DK-8000 Aarhus C, Denmark. RP Van Cleve, JE (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.; Van Cleve, JE (reprint author), SETI Inst, 189 Bernardo Ave, Mountain View, CA 94043 USA. EM jeffrey.vancleve@nasa.gov OI Handberg, Rasmus/0000-0001-8725-4502 FU NASA's Science Mission Directorate; NASA [NNX13AD01A] FX Funding for this Discovery Mission is provided by NASA's Science Mission Directorate. We thank the Kepler Science Operation Center and Science Office staff whose efforts led to the data products discussed in this work. We thank in particular Tom Barclay and Fergal Mullally for reading early drafts and making helpful comments; Wendy Stenzel for Figure 1; Mike Haas and Charlie Sobeck for K2 project support of the preparation of this manuscript; Daniel Huber for the EPIC stellar properties in advance of publication; and Ball Aerospace and LASP for making the operational improvements that led to these results. This work was supported by NASA grant NNX13AD01A. NR 37 TC 6 Z9 6 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6280 EI 1538-3873 J9 PUBL ASTRON SOC PAC JI Publ. Astron. Soc. Pac. PD JUL PY 2016 VL 128 IS 965 AR 075002 DI 10.1088/1538-3873/128/965/075002 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EB1LD UT WOS:000387112300009 ER PT J AU Shen, Y Fichot, CG Liang, SK Benner, R AF Shen, Yuan Fichot, Cedric G. Liang, Sheng-Kang Benner, Ronald TI Biological hot spots and the accumulation of marine dissolved organic matter in a highly productive ocean margin SO LIMNOLOGY AND OCEANOGRAPHY LA English DT Article ID GULF-OF-MEXICO; MISSISSIPPI RIVER PLUME; WESTERN ARCTIC-OCEAN; PHYTOPLANKTON GROWTH; INTERMEDIATE SALINITIES; AQUATIC ECOSYSTEMS; COASTAL ECOSYSTEM; SURFACE WATERS; AMINO-ACIDS; FRESH-WATER AB Concentrations of dissolved organic carbon (DOC) and major biochemicals (amino acids and carbohydrates) were measured during five cruises (2009-2010) to the Louisiana margin in the northern Gulf of Mexico. Concentrations of amino acids and carbohydrates were elevated at mid-salinities and were indicative of plankton production of dissolved organic matter (DOM) in surface waters. Hot spots of two compositionally distinct types of labile DOM were identified based on the relative abundances of amino acids and carbohydrates. Amino acid-rich hot spots occurred sporadically in regions of high phytoplankton biomass and were mostly observed between dusk and dawn, reflecting a grazing source. In contrast, carbohydrate-rich hot spots were more widespread and were often found in nutrient-poor waters, indicating the production of carbon-rich DOM associated with nutrient limitation. Major biochemical indicators and bioassay experiments indicated labile DOM comprised a relatively small fraction of the DOC. Most DOM was degraded and had a semi-labile nature. Substantial accumulations of marine (plankton-derived) DOC were observed in surface waters, particularly at mid-salinities during the summer. Microbial alteration of marine DOC and nutrient limitation of microbial utilization of carbon-rich DOM appeared largely responsible for the accumulation of DOC. The reservoir of accumulated marine DOC in the shelf surface mixed layer ranged from 0.11 Tg C to 0.23 Tg C, with the lowest and highest values occurring during winter and summer. Substantial cross-shelf export of semi-labile marine DOM occurred during the summer and provided a major carbon and energy subsidy to microbial food webs in offshore waters. C1 [Shen, Yuan; Fichot, Cedric G.; Liang, Sheng-Kang; Benner, Ronald] Univ South Carolina, Marine Sci Program, Columbia, SC 29208 USA. [Liang, Sheng-Kang] Minist Educ, Key Lab Marine Chem Theory & Technol, Qingdao, Peoples R China. [Benner, Ronald] Univ South Carolina, Dept Biol Sci, Columbia, SC 29208 USA. [Fichot, Cedric G.] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Shen, Y (reprint author), Univ South Carolina, Marine Sci Program, Columbia, SC 29208 USA. EM shen2@email.sc.edu OI Shen, Yuan/0000-0001-6618-4226 FU U.S. National Science Foundation [0850653]; 111 Project of China [B13030] FX l We are grateful to Steven E. Lohrenz and Wei-Jun Cai for providing the opportunity to participate in the GulfCarbon cruises. We appreciate the sampling assistance by Leanne Powers and the crews of the R/V Cape Hatteras and the R/V Hugh Sharp. We thank the anonymous reviewers for their comments and suggestions. This research was funded by a grant from the U.S. National Science Foundation (0850653 to RB) and by the 111 Project of China (B13030 to SKL). NR 66 TC 1 Z9 1 U1 4 U2 4 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0024-3590 EI 1939-5590 J9 LIMNOL OCEANOGR JI Limnol. Oceanogr. PD JUL PY 2016 VL 61 IS 4 BP 1287 EP 1300 DI 10.1002/lno.10290 PG 14 WC Limnology; Oceanography SC Marine & Freshwater Biology; Oceanography GA DW4OO UT WOS:000383622900011 ER PT J AU Rademacher, KR Campbell, MD Gledhill, CT Fitzhugh, G Driggers, WB Caillouet, R Switzer, TS AF Rademacher, Kevin R. Campbell, Matthew D. Gledhill, Christopher T. Fitzhugh, Gary Driggers, William B. Caillouet, Ryan Switzer, Theodore S. TI Male color phase in gag: implications for monitoring sex ratio via visual underwater surveys and port sample observations SO BULLETIN OF MARINE SCIENCE LA English DT Article ID GULF-OF-MEXICO; MYCTEROPERCA-MICROLEPIS SERRANIDAE; SOUTHEASTERN UNITED-STATES; SOCIAL-CONTROL; REPRODUCTIVE-BIOLOGY; BLUEHEAD WRASSE; GROUPER; PISCES; FISHES; REEF AB Fishing of gag (Mycteroperca microlepis Goode and Bean, 1879) spawning aggregations in the northern Gulf of Mexico has reduced the percentage of males in the population from approximately 17% to 2% since the 1970s. This is critical as gag are monandric, protogynous hermaphrodites, and accurate estimation of size-attransition and sex ratio is necessary for proper management. Presence of darkened pigmentation on the abdomen was thought to indicate transition from female to male, and thus, video observations of gag with dark pigmentation were used to estimate sex ratios and indices of abundance. Recent video observations of gag demonstrate that they can change pigmentation patterns within seconds, which could be leading to misidentification of males in those surveys. Results of our investigation showed that males observed in the video survey, as determined by pigmentation only, are significantly shorter than males observed in the commercial fishery, which were determined using both pigmentation and histological examination. Significant differences were detected between pigmented and non-pigmented gag in the commercial data, but not in the video survey data. Additionally, size at which 50% of females had transitioned to male was significantly larger when estimated using commercial fishery data vs the video survey data. Due to significant differences in length distributions and estimates of size-at-transition, and evidence of rapid changes in pigmentation patterns, it is inadvisable to estimate sex ratios or relative indices of abundance by sex for gag from video observations. To address potential shifts in size- and age-at-transition, continued monitoring of sex ratios using histological techniques is recommended. C1 [Rademacher, Kevin R.; Campbell, Matthew D.; Driggers, William B.] Natl Marine Fisheries Serv, Southeast Fisheries Sci Ctr, Mississippi Labs, 3209 Freder St, Pascagoula, MS 39567 USA. [Gledhill, Christopher T.] Natl Marine Fisheries Serv, Southeast Fisheries Sci Ctr, Stennis Branch, Mississippi Labs, Stennis Space Ctr, MS 39529 USA. [Fitzhugh, Gary] Natl Marine Fisheries Serv, Southeast Fisheries Sci Ctr, Panama City Lab, Panama City, FL 32408 USA. [Caillouet, Ryan; Switzer, Theodore S.] Florida Fish & Wildlife Conservat Commiss, Fish & Wildlife Res Inst, St Petersburg, FL 33701 USA. RP Campbell, MD (reprint author), Natl Marine Fisheries Serv, Southeast Fisheries Sci Ctr, Mississippi Labs, 3209 Freder St, Pascagoula, MS 39567 USA. EM matthew.d.campbell@noaa.gov NR 45 TC 0 Z9 0 U1 2 U2 2 PU ROSENSTIEL SCH MAR ATMOS SCI PI MIAMI PA 4600 RICKENBACKER CAUSEWAY, MIAMI, FL 33149 USA SN 0007-4977 EI 1553-6955 J9 B MAR SCI JI Bull. Mar. Sci. PD JUL PY 2016 VL 92 IS 3 BP 305 EP 319 DI 10.5343/bms.2015.1060 PG 15 WC Marine & Freshwater Biology; Oceanography SC Marine & Freshwater Biology; Oceanography GA DZ4CB UT WOS:000385804300002 ER PT J AU Norris, PM da Silva, AM AF Norris, Peter M. da Silva, Arlindo M. TI Monte Carlo Bayesian inference on a statistical model of sub-gridcolumn moisture variability using high-resolution cloud observations. Part 1: Method SO QUARTERLY JOURNAL OF THE ROYAL METEOROLOGICAL SOCIETY LA English DT Article DE cloud data assimilation; statistical cloud parametrizations; Bayesian inference; Markov chain Monte Carlo ID SATELLITE CLOUD; WATER-VAPOR; FIELDS; MODIS; ASSIMILATION AB A method is presented to constrain a statistical model of sub-gridcolumn moisture variability using high-resolution satellite cloud data. The method can be used for large-scale model parameter estimation or cloud data assimilation. The gridcolumn model includes assumed probability density function (PDF) intra-layer horizontal variability and a copula-based inter-layer correlation model. The observables used in the current study are Moderate Resolution Imaging Spectroradiometer (MODIS) cloud-top pressure, brightness temperature and cloud optical thickness, but the method should be extensible to direct cloudy radiance assimilation for a small number of channels. The algorithm is a form of Bayesian inference with a Markov chain Monte Carlo (MCMC) approach to characterizing the posterior distribution. This approach is especially useful in cases where the background state is clear but cloudy observations exist. In traditional linearized data assimilation methods, a subsaturated background cannot produce clouds via any infinitesimal equilibrium perturbation, but the Monte Carlo approach is not gradient-based and allows jumps into regions of non-zero cloud probability. The current study uses a skewed-triangle distribution for layer moisture. The article also includes a discussion of the Metropolis and multiple-try Metropolis versions of MCMC. C1 [Norris, Peter M.] Univ Space Res Assoc, Goddard Earth Sci Technol & Res, Columbia, MD USA. [Norris, Peter M.; da Silva, Arlindo M.] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Code 610-1, Greenbelt, MD 20771 USA. RP Norris, PM (reprint author), NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Code 610-1, Greenbelt, MD 20771 USA. EM peter.m.norris@nasa.gov FU NASA [NNH08ZDA001N-MAP] FX This work was supported by a NASA grant from the Modeling, Analysis, and Prediction program (solicitation NNH08ZDA001N-MAP, proposal title: 'Assimilation of A-Train satellite data for constraining a new PDF-based cloud parametrization in GEOS-5', PI: Arlindo da Silva). The authors thank Steven Platnick and Gala Wind for much useful information on the inner workings of the MODIS cloud algorithms and the characteristics of their retrievals. The authors also thank Dr Chris Snyder and an anonymous reviewer for their reviews, which helped to improve this article substantially. Resources supporting this work were provided by the NASA High-End Computing (HEC) Program through the NASA Center for Climate Simulation (NCCS) at Goddard Space Flight Center. NR 23 TC 0 Z9 0 U1 0 U2 0 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0035-9009 EI 1477-870X J9 Q J ROY METEOR SOC JI Q. J. R. Meteorol. Soc. PD JUL PY 2016 VL 142 IS 699 BP 2505 EP 2527 DI 10.1002/qj.2843 PN B PG 23 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA DY8GL UT WOS:000385367000025 ER PT J AU Norris, PM da Silva, AM AF Norris, Peter M. da Silva, Arlindo M. TI Monte Carlo Bayesian inference on a statistical model of sub-gridcolumn moisture variability using high-resolution cloud observations. Part 2: Sensitivity tests and results SO QUARTERLY JOURNAL OF THE ROYAL METEOROLOGICAL SOCIETY LA English DT Article DE cloud data assimilation; Monte Carlo Bayesian inference; correlation models ID DENSITY-FUNCTIONS; ARAKAWA-SCHUBERT; WATER; PARAMETERIZATION; SCHEME; SCALE; CONVECTION; AGCM AB Part 1 of this series presented a Monte Carlo Bayesian method for constraining a complex statistical model of global circulation model (GCM) sub-gridcolumn moisture variability using high-resolution Moderate Resolution Imaging Spectroradiometer (MODIS) cloud data, thereby permitting parameter estimation and cloud data assimilation for large-scale models. This article performs some basic testing of this new approach, verifying that it does indeed reduce mean and standard deviation biases significantly with respect to the assimilated MODIS cloud optical depth, brightness temperature and cloud-top pressure and that it also improves the simulated rotational-Raman scattering cloud optical centroid pressure (OCP) against independent (non-assimilated) retrievals from the Ozone Monitoring Instrument (OMI). Of particular interest, the Monte Carlo method does show skill in the especially difficult case where the background state is clear but cloudy observations exist. In traditional linearized data assimilation methods, a subsaturated background cannot produce clouds via any infinitesimal equilibrium perturbation, but the Monte Carlo approach allows non-gradient-based jumps into regions of non-zero cloud probability. In the example provided, the method is able to restore marine stratocumulus near the Californian coast, where the background state has a clear swath. This article also examines a number of algorithmic and physical sensitivities of the new method and provides guidance for its cost-effective implementation. One obvious difficulty for the method, and other cloud data assimilation methods as well, is the lack of information content in passive-radiometer-retrieved cloud observables on cloud vertical structure, beyond cloud-top pressure and optical thickness, thus necessitating strong dependence on the background vertical moisture structure. It is found that a simple flow-dependent correlation modification from Riishojgaard provides some help in this respect, by better honouring inversion structures in the background state. C1 [Norris, Peter M.] Univ Space Res Assoc, Goddard Earth Sci Technol & Res, Columbia, MD USA. [Norris, Peter M.; da Silva, Arlindo M.] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Code 610-1, Greenbelt, MD 20771 USA. RP Norris, PM (reprint author), NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Code 610-1, Greenbelt, MD 20771 USA. EM peter.m.norris@nasa.gov FU NASA [NNH08ZDA001N-MAP, NNH12ZDA001N-MAP] FX This work was supported by NASA grants from the Modeling, Analysis, and Prediction program (solicitation NNH08ZDA001N-MAP, proposal title: 'Assimilation of A-Train satellite data for constraining a new PDF-based cloud parametrization in GEOS-5', PI: Arlindo da Silva, and solicitation NNH12ZDA001N-MAP, proposal title: 'Using Near-Real Time Satellite Retrieved Cloud and Surface Properties to Validate and Improve GEOS-5 Analyses and Forecasts', PIs: P. Minnis and M. Rienecker). NR 17 TC 0 Z9 0 U1 1 U2 1 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0035-9009 EI 1477-870X J9 Q J ROY METEOR SOC JI Q. J. R. Meteorol. Soc. PD JUL PY 2016 VL 142 IS 699 BP 2528 EP 2540 DI 10.1002/qj.2844 PN B PG 13 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA DY8GL UT WOS:000385367000026 ER PT J AU Abbott, BP Abbott, R Abbott, TD Abernathy, MR Acernese, F Ackley, K Adams, C Adams, T Addesso, P Adhikari, RX Adya, VB Affeldt, C Agathos, M Agatsuma, K Aggarwal, N Aguiar, OD Aiello, L Ain, A Ajith, P Allen, B Allocca, A Altin, PA Anderson, SB Anderson, WG Arai, K Araya, MC Arceneaux, CC Areeda, JS Arnaud, N Arun, KG Ascenzi, S Ashton, G Ast, M Aston, SM Astone, P Aufmuth, P Aulbert, C Babak, S Bacon, P Bader, MKM Baker, PT Baldaccini, F Ballardin, G Ballmer, SW Barayoga, JC Barclay, SE Barish, BC Barker, D Barone, F Barr, B Barsotti, L Barsuglia, M Barta, D Barthelmy, S Bartlett, J Bartos, I Bassiri, R Basti, A Batch, JC Baune, C Bavigadda, V Bazzan, M Behnke, B Bejger, M Bell, AS Bell, CJ Berger, BK Bergman, J Bergmann, G Berry, CPL Bersanetti, D Bertolini, A Betzwieser, J Bhagwat, S Bhandare, R Bilenko, IA Billingsley, G Birch, J Birney, R Biscans, S Bisht, A Bitossi, M Biwer, C Bizouard, MA Blackburn, JK Blair, CD Blair, DG Blair, RM Bloemen, S Bock, O Bodiya, TP Boer, M Bogaert, G Bogan, C Bohe, A Bojtos, P Bond, C Bondu, F Bonnand, R Boom, BA Bork, R Boschi, V Bose, S Bouffanais, Y Bozzi, A Bradaschia, C Brady, PR Braginsky, VB Branchesi, M Brau, JE Briant, T Brillet, A Brinkmann, M Brisson, V Brockill, P Brooks, AF Brown, DA Brown, DD Brown, NM Buchanan, CC Buikema, A Bulik, T Bulten, HJ Buonanno, A Buskulic, D Buy, C Byer, RL Cadonati, L Cagnoli, G Cahillane, C Bustillo, JC Callister, T Calloni, E Camp, JB Cannon, KC Cao, J Capano, CD Capocasa, E Carbognani, F Caride, S Diaz, JC Casentini, C Caudill, S Cavaglia, M Cavalier, F Cavalieri, R Cella, G Cepeda, CB Baiardi, LC Cerretani, G Cesarini, E Chakraborty, R Chalermsongsak, T Chamberlin, SJ Chan, M Chao, S Charlton, P Chassande-Mottin, E Chen, HY Chen, Y Cheng, C Chincarini, A Chiummo, A Cho, HS Cho, M Chow, JH Christensen, N Chu, Q Chua, S Chung, S Ciani, G Clara, F Clark, JA Cleva, F Coccia, E Cohadon, PF Colla, A Collette, CG Cominsky, L Constancio, M Conte, A Conti, L Cook, D Corbitt, TR Cornish, N Corsi, A Cortese, S Costa, CA Coughlin, MW Coughlin, SB Coulon, JP Countryman, ST Couvares, P Cowan, EE Coward, DM Cowart, MJ Coyne, DC Coyne, R Craig, K Creighton, JDE Cripe, J Crowder, SG Cumming, A Cunningham, L Cuoco, E Dal Canton, T Danilishin, SL D'Antonio, S Danzmann, K Darman, NS Dattilo, V Dave, I Daveloza, HP Davier, M Davies, GS Daw, EJ Day, R DeBra, D Debreczeni, G Degallaix, J De Laurentis, M Deleglise, S Del Pozzo, W Denker, T Dent, T Dereli, H Dergachev, V DeRosa, RT De Rosa, R DeSalvo, R Dhurandhar, S Diaz, MC Di Fiore, L Di Giovanni, M Di Lieto, A Di Pace, S Di Palma, I Di Virgilio, A Dojcinoski, G Dolique, V Donovan, F Dooley, KL Doravari, S Douglas, R Downes, TP Drago, M Drever, RWP Driggers, JC Du, Z Ducrot, M Dwyer, SE Edo, TB Edwards, MC Effler, A Eggenstein, HB Ehrens, P Eichholz, J Eikenberry, SS Engels, W Essick, RC Etzel, T Evans, M Evans, TM Everett, R Factourovich, M Fafone, V Fair, H Fairhurst, S Fan, X Fang, Q Farinon, S Farr, B Farr, WM Favata, M Fays, M Fehrmann, H Fejer, MM Ferrante, I Ferreira, EC Ferrini, F Fidecaro, F Fiori, I Fiorucci, D Fisher, RP Flaminio, R Fletcher, M Fournier, JD Franco, S Frasca, S Frasconi, F Frei, Z Freise, A Frey, R Frey, V Fricke, TT Fritschel, P Frolov, VV Fulda, P Fyffe, M Gabbard, HAG Gair, JR Gammaitoni, L Gaonkar, SG Garufi, F Gatto, A Gaur, G Gehrels, N Gemme, G Gendre, B Genin, E Gennai, A George, J Gergely, L Germain, V Ghosh, A Ghosh, S Giaime, JA Giardina, KD Giazotto, A Gill, K Glaefke, A Goetz, E Goetz, R Gondan, L Gonzalez, G Castro, JMG Gopakumar, A Gordon, NA Gorodetsky, ML Gossan, SE Gosselin, M Gouaty, R Graef, C Graff, PB Granata, M Grant, A Gras, S Gray, C Greco, G Green, AC Groot, P Grote, H Grunewald, S Guidi, GM Guo, X Gupta, A Gupta, MK Gushwa, KE Gustafson, EK Gustafson, R Hacker, JJ Hall, BR Hall, ED Hammond, G Haney, M Hanke, MM Hanks, J Hanna, C Hannam, MD Hanson, J Hardwick, T Haris, K Harms, J Harry, GM Harry, IW Hart, MJ Hartman, MT Haster, CJ Haughian, K Heidmann, A Heintze, MC Heitmann, H Hello, P Hemming, G Hendry, M Heng, IS Hennig, J Heptonstall, AW Heurs, M Hild, S Hoak, D Hodge, KA Hofman, D Hollitt, SE Holt, K Holz, DE Hopkins, P Hosken, DJ Hough, J Houston, EA Howell, EJ Hu, YM Huang, S Huerta, EA Huet, D Hughey, B Husa, S Huttner, SH Huynh-Dinh, T Idrisy, A Indik, N Ingram, DR Inta, R Isa, HN Isac, JM Isi, M Islas, G Isogai, T Iyer, BR Izumi, K Jacqmin, T Jang, H Jani, K Jaranowski, P Jawahar, S Jimenez-Forteza, F Johnson, WW Jones, DI Jones, R Jonker, RJG Ju, L Kalaghatgi, CV Kalogera, V Kandhasamy, S Kang, G Kanner, JB Karki, S Kasprzack, M Katsavounidis, E Katzman, W Kaufer, S Kaur, T Kawabe, K Kawazoe, F Kefelian, F Kehl, MS Keitel, D Kelley, DB Kells, W Kennedy, R Key, JS Khalaidovski, A Khalili, FY Khan, I Khan, S Khan, Z Khazanov, EA 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CA LIGO Sci Collaboration Virgo Colla ASKAP Collaboration BOOTES Collaboration Dark Energy Survey Collaboration Dark Energy Camera GW-EM Collabor Fermi GBM Collaboration FERMI LAT Collaboration GRAvitational Wave Inaf TeAm GRAWI INTEGRAL Collaboration IPTF Collaboration InterPlanetary Network J-GEM Collaboration LA Silla-QUEST Survey Liverpool Telescope Collaboration Low Frequency Array LOFAR Collabo MASTER Collaboration MAXI Collaboration MWA Collaboration Pan-STARRS Collaboration PESSTO Collaboration Pi Sky Collaboration SkyMapper Collaboration Swift Collaboration Tarot Zadko Algerian Natl Observ C TOROS Collaboration VISTA Collaboration TI SUPPLEMENT: "LOCALIZATION AND BROADBAND FOLLOW-UP OF THE GRAVITATIONAL-WAVE TRANSIENT GW150914" (2016, ApJL, 826, L13) SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE gravitational waves; methods: observational ID ADVANCED LIGO; ELECTROMAGNETIC COUNTERPARTS; DARK ENERGY; TELESCOPE; MISSION; VIRGO; EVENTS; SEARCH; CAMERA AB This Supplement provides supporting material for Abbott et al. (2016a). We briefly summarize past electromagnetic (EM) follow-up efforts as well as the organization and policy of the current EM follow-up program. We compare the four probability sky maps produced for the gravitational-wave transient GW150914, and provide additional details of the EM follow-up observations that were performed in the different bands. C1 [Abbott, B. P.; Abbott, R.; Abernathy, M. R.; Adhikari, R. X.; Anderson, S. B.; Arai, K.; Araya, M. C.; Barayoga, J. C.; Barish, B. C.; Berger, B. K.; Billingsley, G.; Blackburn, J. K.; Bork, R.; Brooks, A. F.; Cahillane, C.; Callister, T.; Cepeda, C. B.; Chakraborty, R.; Chalermsongsak, T.; Couvares, P.; Coyne, D. C.; Dergachev, V.; Drever, R. W. P.; Ehrens, P.; Etzel, T.; Gossan, S. E.; Gushwa, K. E.; Gustafson, E. K.; Hall, E. D.; Heptonstall, A. W.; Hodge, K. A.; Isi, M.; Kanner, J. B.; Kells, W.; Kondrashov, V.; Korth, W. Z.; Kozak, D. B.; Lazzarini, A.; Li, T. G. F.; Mageswaran, M.; Maros, E.; Martynov, D. V.; Marx, J. 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EM lsc-spokesperson@ligo.org RI Prokhorov, Leonid/I-2953-2012; Gammaitoni, Luca/B-5375-2009; Ciani, Giacomo/G-1036-2011; Sigg, Daniel/I-4308-2015; Di Virgilio, Angela Dora Vittoria/E-9078-2015; Garufi, Fabio/K-3263-2015; Sergeev, Alexander/F-3027-2017; Vitek, Stanislav/B-3332-2015; Harms, Jan/J-4359-2012; Jelinek, Martin/E-5290-2016; Marchesoni, Fabio/A-1920-2008; Cesarini, Elisabetta/C-4507-2017; Costa, Cesar/G-7588-2012; Hild, Stefan/A-3864-2010; Roberts, Oliver/N-6284-2016; Mihara, Tatehiro/C-5536-2017; Di Venere, Leonardo/C-7619-2017; Chow, Jong/A-3183-2008; Hudec, Rene/G-9018-2014; Frey, Raymond/E-2830-2016; Serino, Motoko/D-3890-2017; Caballero-Garcia, Maria/D-5659-2017; Bartos, Imre/A-2592-2017; Punturo, Michele/I-3995-2012; Gaztanaga, Enrique/L-4894-2014; zhou, hua/A-6862-2017; Cella, Giancarlo/A-9946-2012; prodi, giovanni/B-4398-2010; Ogando, Ricardo/A-1747-2010; Leonardi, Matteo/G-9694-2015; Galbany, Lluis/A-8963-2017; Elias-Rosa, Nancy/D-3759-2014; Reimer, Olaf/A-3117-2013; Ferrante, Isidoro/F-1017-2012; Pata, Petr/D-5817-2013; Gemme, Gianluca/C-7233-2008; Vecchio, Alberto/F-8310-2015; Losurdo, Giovanni/K-1241-2014; Lima, Marcos/E-8378-2010; Strigin, Sergey/I-8337-2012; Iyer, Bala R./E-2894-2012; Sorrentino, Fiodor/M-6662-2016; Orlando, E/R-5594-2016; Wayth, Randall/B-2444-2013; Travasso, Flavio/J-9595-2016; Tiwari, Shubhanshu/R-8546-2016; Funk, Stefan/B-7629-2015; Bonino, Raffaella/S-2367-2016 OI Gammaitoni, Luca/0000-0002-4972-7062; Ciani, Giacomo/0000-0003-4258-9338; Sigg, Daniel/0000-0003-4606-6526; Di Virgilio, Angela Dora Vittoria/0000-0002-2237-7533; Garufi, Fabio/0000-0003-1391-6168; Vitek, Stanislav/0000-0002-3185-1495; Jelinek, Martin/0000-0003-3922-7416; Gorbovskoy, Evgeny/0000-0002-4368-9237; Bondu, Francois/0000-0001-6487-5197; Marchesoni, Fabio/0000-0001-9240-6793; Cesarini, Elisabetta/0000-0001-9127-3167; Roberts, Oliver/0000-0002-7150-9061; Mihara, Tatehiro/0000-0002-6337-7943; Di Venere, Leonardo/0000-0003-0703-824X; Chow, Jong/0000-0002-2414-5402; Frey, Raymond/0000-0003-0341-2636; Caballero-Garcia, Maria/0000-0001-7920-4564; Scalzo, Richard/0000-0003-3740-1214; Kotak, Rubina/0000-0001-5455-3653; Abdalla, Filipe/0000-0003-2063-4345; Piccinni, Ornella Juliana/0000-0001-5478-3950; Nelemans, Gijs/0000-0002-0752-2974; Pitkin, Matthew/0000-0003-4548-526X; Croft, Steve/0000-0003-4823-129X; Principe, Maria/0000-0002-6327-0628; Macri, Lucas/0000-0002-1775-4859; Lares, Marcelo/0000-0001-8180-5780; Getman, Fedor/0000-0003-1550-0182; Zweizig, John/0000-0002-1521-3397; Horesh, Assaf/0000-0002-5936-1156; Schmidt, Brian/0000-0001-6589-1287; Hill, Adam/0000-0003-3470-4834; Onken, Christopher/0000-0003-0017-349X; Gendre, Bruce/0000-0002-9077-2025; McMahon, Richard/0000-0001-8447-8869; orienti, monica/0000-0003-4470-7094; Granata, Massimo/0000-0003-3275-1186; Axelsson, Magnus/0000-000